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"count": 257791,
"next": "https://hermes.lco.global/api/v0/messages/?format=api&limit=100&offset=2400&ordering=topic",
"previous": "https://hermes.lco.global/api/v0/messages/?format=api&limit=100&offset=2200&ordering=topic",
"results": [
{
"id": 6275,
"topic": "gcn.circular",
"uuid": "6833318c-1cd6-4f87-99b8-9175a55ec2a9",
"title": "GRB 240320A: Glowbug gamma-ray detection",
"submitter": "Hop gcn.circular",
"authors": "C.C. Cheung at Naval Research Lab <Teddy.Cheung@nrl.navy.mil>",
"data": {
"date": "24/03/25 15:16:54 GMT",
"from": "C.C. Cheung at Naval Research Lab <Teddy.Cheung@nrl.navy.mil>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35976"
},
"title": "GCN CIRCULAR",
"number": "35976",
"subject": "GRB 240320A: Glowbug gamma-ray detection"
},
"message_text": "C.C. Cheung, R. Woolf, M. Kerr, J.E. Grove (NRL), A. Goldstein (USRA), C.A. Wilson-Hodge, D. Kocevski (MSFC), and M.S. Briggs (UAH) report:\n\nThe Glowbug gamma-ray telescope [1,2], operating on the International Space Station, reports the detection of GRB 240320A, which was also detected by Fermi GBM (GCN 35967).\n\nUsing an adaptive window with a resolution of 32-ms, the burst onset is determined to be 2024-03-20 17:29:44.176 with a duration of 5.1 s and a total significance of about 14.9 sigma. The light curve comprises two primary peaks at ~T0+1s and ~T0+3.5s.\n\nUsing a standard power-law function with an exponential high-energy cutoff [3] to model the emission over this duration results in a poorly constrained power-law index and a cutoff energy (\"Epeak\") of 191 keV. The modeled 10-10000 keV fluence is 4.5e-07 erg/cm^2.\n\nThe analysis results presented here are preliminary and use a response function that lacks a detailed characterization of the surrounding passive structure of the ISS.\n\nGlowbug is a NASA-funded technology demonstrator for sensitive, low-cost gamma-ray transient telescopes developed, built, and operated by the U.S. Naval Research Laboratory (NRL) with support from the University of Alabama in Huntsville, USRA, and NASA MSFC. It was launched on 2023 March 15 aboard the Department of Defense Space Test Programâs STP-H9 to the ISS. The detector comprises 12 large-area (15 cm x 15 cm) CsI:Tl panels covering the surface of a half cube, and two hexagonal (5-cm diameter, 10-cm length) CLLB scintillators, giving it a large field of view (instantaneous FoV ~2/3 sky) over a wide energy band of 50 keV to >2 MeV.\n\n[1] Grove, J.E. et al. 2020, Proc. Yamada Conf. LXXI, arXiv:2009.11959\n[2] Woolf, R.S. et al. 2022, Proc. SPIE, 12181, id. 121811O\n[3] Goldstein, A. et al. 2020, ApJ 895, 40, arXiv :1909.03006\n\nDistribution Statement A: Approved for public release. Distribution is unlimited.\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35976.",
"published": "2024-03-25T15:17:10.226649Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-25T15:17:10.226661Z",
"modified": "2024-03-25T15:17:10.235739Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6204,
"topic": "gcn.circular",
"uuid": "5a87afca-bc5f-4339-a3f7-ed249e506b69",
"title": "IceCube-240307A: Upper limits from a search for additional neutrino events in IceCube",
"submitter": "Hop gcn.circular",
"authors": "Jessie Thwaites at IceCube/U Wisc-Madison <thwaites@wisc.edu>",
"data": {
"date": "24/03/08 17:18:14 GMT",
"from": "Jessie Thwaites at IceCube/U Wisc-Madison <thwaites@wisc.edu>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35905"
},
"title": "GCN CIRCULAR",
"number": "35905",
"subject": "IceCube-240307A: Upper limits from a search for additional neutrino events in IceCube"
},
"message_text": "The IceCube Collaboration (http://icecube.wisc.edu/) reports:\n\nIceCube has performed a search [1] for additional track-like muon neutrino events arriving from the direction of IceCube-240307A (https://gcn.nasa.gov/circulars/35898) in a time range of 1000 seconds centered on the alert event time (2024-03-07 07:36:37.380 UTC to 2024-03-07 07:53:17.380 UTC) during which IceCube was collecting good quality data. Excluding the event that prompted the alert, one track-like event is found within the 90% containment region of IceCube-240307A. We find that this additional event is well described by atmospheric background expectations, with a p-value of 0.07. The IceCube sensitivity to neutrino point sources with an E^-2.5 spectrum (E^2 dN/dE at 1 TeV) within the locations spanned by the 90% spatial containment region of IceCube-240307A ranges from 1.4e-01 to 1.7e-01 GeV cm^-2 in a 1000 second time window. 90% of events IceCube would detect from a source at this declination with an E^-2.5 spectrum have energies in the approximate energy range between 2e+02 GeV and 7e+04 GeV. \n\nA subsequent search was performed including 2 days of data centered on the alert event time (2024-03-06 07:44:57.380 UTC to 2024-03-08 07:44:57.380 UTC). In this case, we report a p-value of 0.75, consistent with no significant excess of track events. The IceCube sensitivity to neutrino point sources with an E^-2.5 spectrum (E^2 dN/dE at 1 TeV) within the locations spanned by the 90% spatial containment region of IceCube-240307A ranges from 1.6e-01 to 2.0e-01 GeV cm^-2 in a 2 day time window. \n\nThe IceCube Neutrino Observatory is a cubic-kilometer neutrino detector operating at the geographic South Pole, Antarctica. The IceCube realtime alert point of contact can be reached at roc@icecube.wisc.edu.\n\n[1] IceCube Collaboration, R. Abbasi et al., ApJ 910 4 (2021)\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35905.",
"published": "2024-03-08T17:18:30.668789Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-08T17:18:30.668805Z",
"modified": "2024-03-08T17:18:30.676318Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6205,
"topic": "gcn.circular",
"uuid": "21094556-83db-4c30-b18b-e972b9495ee2",
"title": "Swift Trigger 1219325 is not a GRB",
"submitter": "Hop gcn.circular",
"authors": "P.A. Evans at U. Leicester <pae9@leicester.ac.uk>",
"data": {
"date": "24/03/09 14:55:03 GMT",
"from": "P.A. Evans at U. Leicester <pae9@leicester.ac.uk>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35906"
},
"title": "GCN CIRCULAR",
"number": "35906",
"subject": "Swift Trigger 1219325 is not a GRB"
},
"message_text": "\nP. A. Evans (U Leicester) and K. L. Page (U Leicester) report on\nbehalf of the Neil Gehrels Swift Observatory Team:\n\nSwift-BAT trigger 1219325 was caused by Cyg X-1 while the star trackers had\nlost lock. It is not an astrophysical transient.\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35906.",
"published": "2024-03-09T14:55:16.607355Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-09T14:55:16.607372Z",
"modified": "2024-03-09T14:55:16.616643Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6206,
"topic": "gcn.circular",
"uuid": "9958df05-e19d-460c-bd05-00b1f09ed7f6",
"title": "GRB 240309A: MAXI/GSC detection",
"submitter": "Hop gcn.circular",
"authors": "Motoko Serino at Aoyama Gakuin U. <serino@phys.aoyama.ac.jp>",
"data": {
"date": "24/03/10 00:51:38 GMT",
"from": "Motoko Serino at Aoyama Gakuin U. <serino@phys.aoyama.ac.jp>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35907"
},
"title": "GCN CIRCULAR",
"number": "35907",
"subject": "GRB 240309A: MAXI/GSC detection"
},
"message_text": "M. Shidatsu (Ehime U.), M. Serino (AGU), M. Nakajima (Nihon U.), Y. Kawakubo (LSU),\nH. Negoro, K. Kobayashi, M. Tanaka, Y. Soejima, Y. Kudo (Nihon U.),\nT. Mihara, T. Kawamuro, S. Yamada, S. Wang, T. Tamagawa, N. Kawai, M. Matsuoka (RIKEN),\nT. Sakamoto, S. Sugita, H. Hiramatsu, H. Nishikawa, A. Yoshida (AGU),\nY. Tsuboi, S. Urabe, S. Nawa, N. Nemoto, E.Goto (Chuo U.),\nY. Niida (Ehime U.),\nI. Takahashi, M. Niwano, S. Sato, N. Higuchi, Y. Yatsu (Tokyo Tech),\nS. Nakahira, S. Ueno, H. Tomida, M. Ishikawa, S. Ogawa, T. Kurihara (JAXA),\nY. Ueda, K. Setoguchi, T. Yoshitake, Y. Nakatani, Y. Okada (Kyoto U.),\nM. Yamauchi, Y. Hagiwara, Y. Otsuki, T. Hasegawa, M. Nishio (Miyazaki U.),\nK. Yamaoka (Nagoya U.),\nM. Sugizaki (NAOC),\nW. Iwakiri (Chiba U.)\nreport on behalf of the MAXI team:\n\nThe MAXI/GSC nova alert system triggered a bright uncatalogued X-ray transient source\nat 21:33:07 UT on March 9, 2024.\nAssuming that the source flux was constant over the transit,\nwe obtain the source position at\n(R.A., Dec) = (241.601 deg, -69.000 deg) = (16 06 24, -69 00 00) (J2000)\nwith a statistical 90% C.L. elliptical error region\nwith long and short radii of 0.34 deg and 0.23 deg, respectively.\nThe roll angle of long axis from the north direction is 99.0 deg counterclockwise.\nThere is an additional systematic uncertainty of 0.1 deg (90% containment radius).\nThe X-ray flux averaged over the scan was 158 +- 29 mCrab\n(4.0-10.0keV, 1 sigma error).\nWithout assumptions on the source constancy, we obtain a rectangular error\nbox for the transient source with the following corners:\n(R.A., Dec) = (242.811, -67.736) deg = (16 11 14, -67 44 09) (J2000)\n(R.A., Dec) = (241.055, -67.657) deg = (16 04 13, -67 39 25) (J2000)\n(R.A., Dec) = (240.086, -70.134) deg = (16 00 20, -70 08 02) (J2000)\n(R.A., Dec) = (242.048, -70.222) deg = (16 08 11, -70 13 19) (J2000)\nThere was no significant excess flux in the previous transit at 20:00 UT\nand in the next transit at 23:06 UT with an upper limit of 20 mCrab for each.\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35907.",
"published": "2024-03-10T00:51:53.589855Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-10T00:51:53.589875Z",
"modified": "2024-03-10T00:51:53.597857Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6207,
"topic": "gcn.circular",
"uuid": "24c2df36-2977-4056-be21-86483c970f95",
"title": "GRB 240310A: Fermi GBM Final Real-time Localization",
"submitter": "Hop gcn.circular",
"authors": "Fermi GBM Team at MSFC/Fermi-GBM <do_not_reply@GIOC.nsstc.nasa.gov>",
"data": {
"date": "24/03/10 05:50:42 GMT",
"from": "Fermi GBM Team at MSFC/Fermi-GBM <do_not_reply@GIOC.nsstc.nasa.gov>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35908"
},
"title": "GCN CIRCULAR",
"number": "35908",
"subject": "GRB 240310A: Fermi GBM Final Real-time Localization"
},
"message_text": "The Fermi GBM team reports the detection of a likely LONG GRB\n\nAt 05:40:08 UT on 10 Mar 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 240310A (trigger 731742013.593492 / 240310236).\n\nThe on-ground calculated location, using the Fermi GBM trigger data, is RA = 312.5, Dec = -4.9 (J2000 degrees, equivalent to J2000 20h 49m, -4d 54'), with a statistical uncertainty of 10.5 degrees.\n\nThe angle from the Fermi LAT boresight is 87.0 degrees.\n\nThe skymap can be found here:\nhttps://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240310236/quicklook/glg_skymap_all_bn240310236.png\n\nThe HEALPix FITS file, including the estimated localization systematic, can be found here:\nhttps://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240310236/quicklook/glg_healpix_all_bn240310236.fit\n\nThe GBM light curve can be found here:\nhttps://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240310236/quicklook/glg_lc_medres34_bn240310236.gif\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35908.",
"published": "2024-03-10T05:50:57.598334Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-10T05:50:57.598354Z",
"modified": "2024-03-10T05:50:57.605539Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6208,
"topic": "gcn.circular",
"uuid": "9c1006d1-fe73-4c85-8d01-d0098b90e55a",
"title": "Swift GRB240309.61: Global MASTER-Net observations report",
"submitter": "Hop gcn.circular",
"authors": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"data": {
"date": "24/03/10 06:42:53 GMT",
"from": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35909"
},
"title": "GCN CIRCULAR",
"number": "35909",
"subject": "Swift GRB240309.61: Global MASTER-Net observations report"
},
"message_text": "V. Lipunov, V.Kornilov, E. Gorbovskoy, K. Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, V.Senik, D. Vlasenko,\nG.Antipov, D.Zimnukhov, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov, D. Cheryasov, Ya.Kechin, Yu.Tselik, A. Sosnovskij\n(Lomonosov Moscow State University, SAI, Physics Department),\n\nR. Podesta, C.Lopez, F. Podesta, C.Francile\n(Observatorio Astronomico Felix Aguilar OAFA),\n\nR. Rebolo, M. Serra\n(The Instituto de Astrofisica de Canarias),\n\nD. Buckley\n(South African Astronomical Observatory),\n\nO.A. Gress, N.M. Budnev, O.Ershova\n(Irkutsk State University, API),\n\nL.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez,\nA.R.Corella, L.H.Rodriguez\n(INAOE, Guillermo Haro Astrophysics Observatory),\n\nA. Tlatov, D. Dormidontov\n(Kislovodsk Solar Station of the Pulkovo Observatory),\n\nV. Yurkov, A. Gabovich\n(Blagoveschensk Educational State University)\n\nMASTER-Amur robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Blagoveshchensk State Pedagogical University) was pointed to the Swift GRB240309.61 (trigger No 1219325,19h 59m 15.60s , +35d 08m 34.8s, R=0.00130556) errorbox 11103 sec after notice time and 11141 sec after trigger time at 2024-03-09 17:37:59 UT, with upper limit up to 17.0 mag. The observations began at zenith distance = 70 deg. The sun altitude is -38.0 deg.\n\nMASTER-Tavrida robotic telescope located in Russia (Lomonosov MSU, SAI Crimea astronomical station) was pointed to the Swift GRB240309.61 errorbox 28115 sec after notice time and 28152 sec after trigger time at 2024-03-09 22:21:31 UT, with upper limit up to 18.0 mag. The observations began at zenith distance = 85 deg. The sun altitude is -49.7 deg.\n\nThe galactic latitude b = 3 deg., longitude l = 72 deg.\n\n\nReal time updated cover map and OT discovered available here:\nhttps://master.sai.msu.ru/site/master2/observ.php?id#95242\n\nWe obtain a following upper limits.\n\nTmid-T0 | Site |Filt.| Expt. | Limit| Comment\n_________|_____________________|_____|_______|______|________\n\n 11231 | MASTER-Amur | C | 180 | 16.7 |\n 12469 | MASTER-Amur | C | 180 | 17.0 |\n 12994 | MASTER-Amur | C | 180 | 16.8 |\n 28243 | MASTER-Tavrida | C | 180 | 15.1 |\n 29478 | MASTER-Tavrida | C | 180 | 16.5 |\n 30724 | MASTER-Tavrida | C | 180 | 17.0 |\n 31962 | MASTER-Tavrida | C | 180 | 17.2 |\n 32915 | MASTER-Tavrida | C | 180 | 17.2 |\n 33203 | MASTER-Tavrida | C | 180 | 17.4 |\n 34088 | MASTER-Tavrida | C | 180 | 16.8 |\n 34456 | MASTER-Tavrida | C | 180 | 16.9 |\n 35699 | MASTER-Tavrida | C | 180 | 17.2 |\n 35992 | MASTER-Tavrida | C | 180 | 17.4 |\n 36937 | MASTER-Tavrida | C | 180 | 17.4 |\n 38183 | MASTER-Tavrida | C | 180 | 17.7 |\n 39465 | MASTER-Tavrida | C | 180 | 17.8 |\n 40756 | MASTER-Tavrida | C | 180 | 17.9 |\n 41963 | MASTER-Tavrida | C | 180 | 18.0 |\n 43190 | MASTER-Tavrida | C | 180 | 17.9 |\n 44486 | MASTER-Tavrida | C | 180 | 17.8 |\n 45715 | MASTER-Tavrida | C | 180 | 16.7 |\nFilter C is a clear (unfiltred) band.\n\n\nThe observation and reduction will continue.\nThe message may be cited.\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35909.",
"published": "2024-03-10T06:43:08.580580Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-10T06:43:08.580596Z",
"modified": "2024-03-10T06:43:08.587540Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6209,
"topic": "gcn.circular",
"uuid": "b7f96253-8dde-4a3f-9688-b93a0b800666",
"title": "Fermi GRB 240310A: Global MASTER-Net observations report",
"submitter": "Hop gcn.circular",
"authors": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"data": {
"date": "24/03/10 22:45:52 GMT",
"from": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35910"
},
"title": "GCN CIRCULAR",
"number": "35910",
"subject": "Fermi GRB 240310A: Global MASTER-Net observations report"
},
"message_text": "V. Lipunov, V.Kornilov, E. Gorbovskoy, K. Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, V.Senik, D. Vlasenko,\nG.Antipov, D.Zimnukhov, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov, D. Cheryasov, Ya.Kechin, Yu.Tselik, A. Sosnovskij\n(Lomonosov Moscow State University, SAI, Physics Department),\n\nR. Podesta, C.Lopez, F. Podesta, C.Francile\n(Observatorio Astronomico Felix Aguilar OAFA),\n\nR. Rebolo, M. Serra\n(The Instituto de Astrofisica de Canarias),\n\nD. Buckley\n(South African Astronomical Observatory),\n\nO.A. Gress, N.M. Budnev, O.Ershova\n(Irkutsk State University, API),\n\nL.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez,\nA.R.Corella, L.H.Rodriguez\n(INAOE, Guillermo Haro Astrophysics Observatory),\n\nA. Tlatov, D. Dormidontov\n(Kislovodsk Solar Station of the Pulkovo Observatory),\n\nV. Yurkov, A. Gabovich\n(Blagoveschensk Educational State University)\n\nMASTER-Amur robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Blagoveshchensk State Pedagogical University) started inspect of the Fermi GRB 240310A ( Fermi GBM team, GCN 35908) errorbox 52875 sec after notice time and 52908 sec after trigger time at 2024-03-10 20:21:56 UT, with upper limit up to 17.3 mag. Observations started at twilight. The observations began at zenith distance = 69 deg. The sun altitude is -15.5 deg.\n\nThe galactic latitude b = -29 deg., longitude l = 43 deg.\n\n\nReal time updated cover map and OT discovered available here:\nhttps://master.sai.msu.ru/site/master2/observ.php?id#95738\n\nWe obtain a following upper limits.\n\nTmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment\n_________|_____________________|_____________________|____________________________________|_____|_______|_______|________\n\n 52938 | 2024-03-10 20:21:56 | MASTER-Amur | (20h 20m 04.50s , +05d 01m 00.9s) | C | 60 | 17.3 |\n 53018 | 2024-03-10 20:23:16 | MASTER-Amur | (20h 28m 04.31s , +05d 02m 38.3s) | C | 60 | 17.2 |\n 53177 | 2024-03-10 20:25:55 | MASTER-Amur | (20h 08m 44.97s , +01d 12m 42.5s) | C | 60 | 16.8 |\n 53895 | 2024-03-10 20:37:53 | MASTER-Amur | (20h 19m 59.07s , +05d 01m 44.8s) | C | 60 | 17.0 |\n 53975 | 2024-03-10 20:39:13 | MASTER-Amur | (20h 28m 08.06s , +05d 01m 08.4s) | C | 60 | 16.9 |\n 54136 | 2024-03-10 20:41:54 | MASTER-Amur | (20h 08m 48.83s , +01d 10m 54.5s) | C | 60 | 16.1 |\n 54215 | 2024-03-10 20:43:14 | MASTER-Amur | (20h 15m 59.12s , +01d 11m 14.5s) | C | 60 | 16.5 |\n 54295 | 2024-03-10 20:44:33 | MASTER-Amur | (20h 24m 02.80s , +01d 13m 22.6s) | C | 60 | 16.3 |\n 54375 | 2024-03-10 20:45:53 | MASTER-Amur | (20h 32m 30.33s , +03d 07m 57.2s) | C | 60 | 16.4 |\n 54455 | 2024-03-10 20:47:13 | MASTER-Amur | (20h 40m 37.56s , +03d 07m 22.0s) | C | 60 | 16.4 |\n 54694 | 2024-03-10 20:51:12 | MASTER-Amur | (20h 31m 12.01s , +01d 11m 40.1s) | C | 60 | 15.9 |\n 54774 | 2024-03-10 20:52:32 | MASTER-Amur | (20h 39m 14.65s , +01d 13m 39.3s) | C | 60 | 15.8 |\n 54854 | 2024-03-10 20:53:52 | MASTER-Amur | (20h 19m 58.98s , +04d 59m 44.6s) | C | 60 | 16.0 |\n 54933 | 2024-03-10 20:55:12 | MASTER-Amur | (20h 27m 59.97s , +05d 01m 09.9s) | C | 60 | 15.7 |\n 55093 | 2024-03-10 20:57:51 | MASTER-Amur | (20h 08m 44.79s , +01d 09m 45.4s) | C | 60 | 14.9 |\nFilter C is a clear (unfiltred) band.\n\n\nThe observation and reduction will continue.\nThe message may be cited.\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35910.",
"published": "2024-03-10T22:46:09.176398Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-10T22:46:09.176424Z",
"modified": "2024-03-10T22:46:09.184176Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6210,
"topic": "gcn.circular",
"uuid": "2fd4aadc-904d-4429-9744-7536b7439b57",
"title": "GRB 240310B: Glowbug gamma-ray detection",
"submitter": "Hop gcn.circular",
"authors": "C.C. Cheung at Naval Research Lab <Teddy.Cheung@nrl.navy.mil>",
"data": {
"date": "24/03/11 15:31:04 GMT",
"from": "C.C. Cheung at Naval Research Lab <Teddy.Cheung@nrl.navy.mil>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35911"
},
"title": "GCN CIRCULAR",
"number": "35911",
"subject": "GRB 240310B: Glowbug gamma-ray detection"
},
"message_text": "C.C. Cheung, R. Woolf, M. Kerr, J.E. Grove (NRL), A. Goldstein (USRA), C.A. Wilson-Hodge, D. Kocevski (MSFC), and M.S. Briggs (UAH) report:\n \nThe Glowbug gamma-ray telescope [1,2], operating on the International Space Station, reports the detection of GRB 240310B, which was also detected by CALET (Trigger 1394110412).\n \nUsing an adaptive window with a resolution of 32-ms, the burst onset is determined to be 2024-03-10 12:58:14.336 with a duration of 12.3 s and a total significance of about 19.3 sigma. The light curve comprises a single peak.\n \nUsing a standard power-law function with an exponential high-energy cutoff [3] to model the emission over this duration results in a poorly constrained power-law index and a cutoff energy (\"Epeak\") of 126 keV. The modeled 10-10000 keV fluence is 8.1e-07 erg/cm^2.\n \nThe best-fit localization is RA, Decl. (J2000, deg) = 234.5, 87.9 with a radius of 15.9 deg (95% confidence), with a highly uncertain systematic uncertainty.\n \nThe analysis results presented here are preliminary and use a response function that lacks a detailed characterization of the surrounding passive structure of the ISS.\n \nGlowbug is a NASA-funded technology demonstrator for sensitive, low-cost gamma-ray transient telescopes developed, built, and operated by the U.S. Naval Research Laboratory (NRL) with support from the University of Alabama in Huntsville, USRA, and NASA MSFC. It was launched on 2023 March 15 aboard the Department of Defense Space Test Programâs STP-H9 to the ISS. The detector comprises 12 large-area (15 cm x 15 cm) CsI:Tl panels covering the surface of a half cube, and two hexagonal (5-cm diameter, 10-cm length) CLLB scintillators, giving it a large field of view (instantaneous FoV ~2/3 sky) over a wide energy band of 50 keV to >2 MeV.\n \n[1] Grove, J.E. et al. 2020, Proc. Yamada Conf. LXXI, arXiv:2009.11959\n[2] Woolf, R.S. et al. 2022, Proc. SPIE, 12181, id. 121811O\n[3] Goldstein, A. et al. 2020, ApJ 895, 40, arXiv :1909.03006\n \nDistribution Statement A: Approved for public release. Distribution is unlimited.\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35911.",
"published": "2024-03-11T15:31:21.931446Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-11T15:31:21.931465Z",
"modified": "2024-03-11T15:31:21.940831Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6276,
"topic": "gcn.circular",
"uuid": "a9ba279e-dfcd-4b7c-91d0-fbbebf1a3cee",
"title": "Fermi trigger No 733092476: Global MASTER-Net observations report",
"submitter": "Hop gcn.circular",
"authors": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"data": {
"date": "24/03/25 23:31:02 GMT",
"from": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35977"
},
"title": "GCN CIRCULAR",
"number": "35977",
"subject": "Fermi trigger No 733092476: Global MASTER-Net observations report"
},
"message_text": "V. Lipunov, V.Kornilov, E. Gorbovskoy, K. Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, V.Senik, D. Vlasenko,\nG.Antipov, D.Zimnukhov, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov, D. Cheryasov, Ya.Kechin, Yu.Tselik, A. Sosnovskij\n(Lomonosov Moscow State University, SAI, Physics Department),\n\nR. Podesta, C.Lopez, F. Podesta, C.Francile\n(Observatorio Astronomico Felix Aguilar OAFA),\n\nR. Rebolo, M. Serra\n(The Instituto de Astrofisica de Canarias),\n\nD. Buckley\n(South African Astronomical Observatory),\n\nO.A. Gress, N.M. Budnev, O.Ershova\n(Irkutsk State University, API),\n\nL.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez,\nA.R.Corella, L.H.Rodriguez\n(INAOE, Guillermo Haro Astrophysics Observatory),\n\nA. Tlatov, D. Dormidontov\n(Kislovodsk Solar Station of the Pulkovo Observatory),\n\nV. Yurkov, A. Gabovich\n(Blagoveschensk Educational State University)\n\nMASTER-Tunka robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Applied Physics Institute, Irkutsk State University) started inspect of the Fermi GRB240325.87 (trigger No 733092476,23h 52m 16.08s , +12d 55m 58.8s, R&.23) errorbox 2625 sec after notice time and 2658 sec after trigger time at 2024-03-25 21:32:10 UT, with upper limit up to 15.0 mag. Observations started at twilight. The observations began at zenith distance = 64 deg. The sun altitude is -13.7 deg.\n\nThe galactic latitude b = -47 deg., longitude l = 102 deg.\n\n\nReal time updated cover map and OT discovered available here:\nhttps://master.sai.msu.ru/site/master2/observ.php?id$06760\n\nWe obtain a following upper limits.\n\nTmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment\n_________|_____________________|_____________________|____________________________________|_____|_______|_______|________\n\n 2689 | 2024-03-25 21:32:10 | MASTER-Tunka | (22h 40m 57.63s , +34d 24m 37.9s) | C | 60 | 14.7 |\n 2782 | 2024-03-25 21:33:43 | MASTER-Tunka | (22h 53m 51.34s , +30d 36m 29.5s) | C | 60 | 13.9 |\n 2876 | 2024-03-25 21:35:17 | MASTER-Tunka | (22h 28m 39.00s , +32d 33m 13.4s) | C | 60 | 15.0 |\n 2972 | 2024-03-25 21:36:53 | MASTER-Tunka | (22h 55m 29.91s , +36d 18m 16.9s) | C | 60 | 14.8 |\n 3647 | 2024-03-25 21:48:09 | MASTER-Tunka | (22h 41m 06.08s , +34d 25m 20.8s) | C | 60 | 14.6 |\n 3903 | 2024-03-25 21:52:24 | MASTER-Tunka | (22h 28m 41.31s , +32d 32m 29.2s) | C | 60 | 13.1 |\nFilter C is a clear (unfiltred) band.\n\n\nThe observation and reduction will continue.\nThe message may be cited.\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35977.",
"published": "2024-03-25T23:31:20.348549Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-25T23:31:20.348570Z",
"modified": "2024-03-25T23:31:20.356251Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6211,
"topic": "gcn.circular",
"uuid": "23549429-6212-430e-9c58-ac0ac360c3b3",
"title": "Fermi-LAT gamma-ray observations of IceCube-240307A",
"submitter": "Hop gcn.circular",
"authors": "Simone Garrappa at DESY <simone.garrappa@desy.de>",
"data": {
"date": "24/03/11 17:46:08 GMT",
"from": "Simone Garrappa at DESY <simone.garrappa@desy.de>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35912"
},
"title": "GCN CIRCULAR",
"number": "35912",
"subject": "Fermi-LAT gamma-ray observations of IceCube-240307A"
},
"message_text": "S. Garrappa (Weizmann Institute of Science), C. Bartolini (INFN Bari), S. Buson (DESY; Univ. of Wuerzburg), L. Pfeiffer (Univ. of Wuerzburg) and J. Sinapius (DESY) on behalf of the Fermi-LAT collaboration:\n\nWe report an analysis of observations of the vicinity of the IC240229A high-energy neutrino event (GCN 35898) with all-sky survey data from the Large Area Telescope (LAT), on board the Fermi Gamma-ray Space Telescope. The IceCube event was detected on 2024-03-07 at 07:44:57.38 UT (T0) with J2000 position RA = 239.63 (+13.20, -15.22) deg, Decl. = +39.94 (+18.18, -14.92 ) deg (90% PSF containment). Several catalogued gamma-ray (>100 MeV; The Fermi-LAT collaboration 2022, ApJS, 260, 53) sources are located within the 90% IC240307A localization region. Based on a preliminary analysis of the LAT data over the timescale of 1-day prior to T0, these objects are not significantly detected (> 5 sigma).\n\nWe searched for intermediate (days to years) timescale emission from a new gamma-ray transient source. Preliminary analysis indicates no significant (> 5 sigma) new excess emission (> 100 MeV) at the IC240307A best-fit position. Assuming a power-law spectrum (photon index = 2.0 fixed) for a point source at the IC240307A best-fit position, the >100 MeV flux upper limit (95% confidence) is < 3.8e-8 ph cm^-2 s^-1 for a 1-day integration time before T0.\n\nSince Fermi normally operates in an all-sky scanning mode, regular monitoring of this region will continue. For these observations the Fermi-LAT contact persons is S. Garrappa (simone.garrappa at weizmann.ac.il).\n\nThe Fermi-LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.\n\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35912.",
"published": "2024-03-11T17:46:24.431191Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-11T17:46:24.431207Z",
"modified": "2024-03-11T17:46:24.439874Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6212,
"topic": "gcn.circular",
"uuid": "496ea964-5c39-4ec7-b755-0893f3e83401",
"title": "Fermi trigger No 731839490: Global MASTER-Net observations report",
"submitter": "Hop gcn.circular",
"authors": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"data": {
"date": "24/03/11 20:45:48 GMT",
"from": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35913"
},
"title": "GCN CIRCULAR",
"number": "35913",
"subject": "Fermi trigger No 731839490: Global MASTER-Net observations report"
},
"message_text": "V. Lipunov, V.Kornilov, E. Gorbovskoy, K. Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, V.Senik, D. Vlasenko,\nG.Antipov, D.Zimnukhov, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov, D. Cheryasov, Ya.Kechin, Yu.Tselik, A. Sosnovskij\n(Lomonosov Moscow State University, SAI, Physics Department),\n\nR. Podesta, C.Lopez, F. Podesta, C.Francile\n(Observatorio Astronomico Felix Aguilar OAFA),\n\nR. Rebolo, M. Serra\n(The Instituto de Astrofisica de Canarias),\n\nD. Buckley\n(South African Astronomical Observatory),\n\nO.A. Gress, N.M. Budnev, O.Ershova\n(Irkutsk State University, API),\n\nL.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez,\nA.R.Corella, L.H.Rodriguez\n(INAOE, Guillermo Haro Astrophysics Observatory),\n\nA. Tlatov, D. Dormidontov\n(Kislovodsk Solar Station of the Pulkovo Observatory),\n\nV. Yurkov, A. Gabovich\n(Blagoveschensk Educational State University)\n\nMASTER-Amur robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Blagoveshchensk State Pedagogical University) started inspect of the Fermi GRB240311.36 (trigger No 731839490,22h 18m 24.00s , +05d 37m 58.8s, R3.28) errorbox 38228 sec after notice time and 38263 sec after trigger time at 2024-03-11 19:22:28 UT, with upper limit up to 18.0 mag. The observations began at zenith distance = 68 deg. The sun altitude is -24.2 deg.\n\nThe galactic latitude b = -41 deg., longitude l = 69 deg.\n\n\nReal time updated cover map and OT discovered available here:\nhttps://master.sai.msu.ru/site/master2/observ.php?id#96720\n\nWe obtain a following upper limits.\n\nTmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment\n_________|_____________________|_____________________|____________________________________|_____|_______|_______|________\n\n 38293 | 2024-03-11 19:22:28 | MASTER-Amur | (19h 59m 58.79s , +14d 32m 34.9s) | C | 60 | 17.7 |\n 38373 | 2024-03-11 19:23:47 | MASTER-Amur | (20h 18m 24.64s , +16d 29m 01.3s) | C | 60 | 17.8 |\n 38452 | 2024-03-11 19:25:07 | MASTER-Amur | (20h 26m 46.01s , +16d 27m 41.8s) | C | 60 | 17.8 |\n 38612 | 2024-03-11 19:27:47 | MASTER-Amur | (20h 07m 24.85s , +14d 34m 35.0s) | C | 60 | 17.9 |\n 38692 | 2024-03-11 19:29:07 | MASTER-Amur | (20h 15m 47.37s , +14d 33m 57.0s) | C | 60 | 17.9 |\n 39107 | 2024-03-11 19:36:02 | MASTER-Amur | (20h 23m 06.76s , +14d 33m 50.8s) | C | 60 | 17.6 |\n 39388 | 2024-03-11 19:40:43 | MASTER-Amur | (20h 31m 29.25s , +14d 34m 14.1s) | C | 60 | 17.8 |\n 39479 | 2024-03-11 19:42:13 | MASTER-Amur | (19h 59m 57.86s , +14d 31m 24.7s) | C | 60 | 17.8 |\n 39558 | 2024-03-11 19:43:33 | MASTER-Amur | (20h 18m 28.20s , +16d 26m 34.8s) | C | 60 | 17.8 |\n 39638 | 2024-03-11 19:44:53 | MASTER-Amur | (20h 26m 45.20s , +16d 28m 09.5s) | C | 60 | 17.9 |\n 39798 | 2024-03-11 19:47:32 | MASTER-Amur | (20h 07m 29.07s , +14d 33m 26.0s) | C | 60 | 17.9 |\n 39877 | 2024-03-11 19:48:52 | MASTER-Amur | (20h 15m 39.60s , +14d 32m 50.9s) | C | 60 | 17.6 |\n 40117 | 2024-03-11 19:52:51 | MASTER-Amur | (20h 23m 05.99s , +14d 32m 01.3s) | C | 60 | 17.7 |\n 40197 | 2024-03-11 19:54:11 | MASTER-Amur | (20h 29m 10.05s , +12d 39m 53.0s) | C | 60 | 17.9 |\n 40276 | 2024-03-11 19:55:31 | MASTER-Amur | (20h 37m 22.40s , +12d 38m 52.7s) | C | 60 | 18.0 |\n 40357 | 2024-03-11 19:56:51 | MASTER-Amur | (20h 31m 30.06s , +14d 33m 56.2s) | C | 60 | 18.0 |\n 40545 | 2024-03-11 20:00:00 | MASTER-Amur | (19h 59m 57.42s , +14d 32m 13.2s) | C | 60 | 17.8 |\n 40631 | 2024-03-11 20:01:26 | MASTER-Amur | (20h 18m 27.01s , +16d 26m 08.0s) | C | 60 | 17.7 |\n 40712 | 2024-03-11 20:02:46 | MASTER-Amur | (20h 26m 40.19s , +16d 25m 29.8s) | C | 60 | 17.7 |\n 40792 | 2024-03-11 20:04:06 | MASTER-Amur | (20h 07m 29.74s , +14d 30m 28.8s) | C | 60 | 17.7 |\n 40872 | 2024-03-11 20:05:26 | MASTER-Amur | (20h 15m 42.70s , +14d 32m 44.1s) | C | 60 | 17.6 |\n 40952 | 2024-03-11 20:06:46 | MASTER-Amur | (20h 36m 29.07s , +10d 45m 47.6s) | C | 60 | 17.8 |\n 41032 | 2024-03-11 20:08:06 | MASTER-Amur | (20h 44m 31.53s , +10d 45m 11.2s) | C | 60 | 17.8 |\n 41111 | 2024-03-11 20:09:26 | MASTER-Amur | (20h 23m 05.57s , +14d 32m 56.8s) | C | 60 | 17.7 |\nFilter C is a clear (unfiltred) band.\n\n\nThe observation and reduction will continue.\nThe message may be cited.\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35913.",
"published": "2024-03-11T20:46:05.552314Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-11T20:46:05.552331Z",
"modified": "2024-03-11T20:46:05.559382Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6213,
"topic": "gcn.circular",
"uuid": "0be74210-6e1a-4f8d-8d7a-4097036b8b8c",
"title": "GRB 240310A: MASTER OT J200702.72-263928.7 inside 3sigma",
"submitter": "Hop gcn.circular",
"authors": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"data": {
"date": "24/03/12 09:59:24 GMT",
"from": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35914"
},
"title": "GCN CIRCULAR",
"number": "35914",
"subject": "GRB 240310A: MASTER OT J200702.72-263928.7 inside 3sigma"
},
"message_text": "\nV.Lipunov, V.Shumkov (Lomonosov MSU),D.Buckley (SAAO),D.Svinkin (Ioffe Institute, Konus-Wind),\nA.Kuznetsov, P.Balanutsa, K.Zhirkov, N.Tiurina, G.Antipov, E.Gorbovskoy (Lomonosov MSU),\nYa.Kechin, D.Vlasenko, Yu.Tselik, V.Topolev, B.Rudenko, M.Gulyaev, V.Vladimirov, D.Zimnukhov,\nV.Senik, A.Yudin, A.Chasovnikov, D.Cheryasov (Lomonosov MSU,SAI,PhysicsDepartment),\nO.A. Gress, N.M. Budnev (Irkutsk State University, API),\nC.Francile. F. Podesta, R.Podesta (Observatorio Astronomico Felix Aguilar OAFA),\nA.Sosnovskij (Crimean Astrophysical Observatory, RAS),\nR. Rebolo, M. Serra(The Instituto de Astrofisica de Canarias),\nA. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory),\nA. Gabovich, V.Yurkov (Blagoveschensk Educational StateUniversity)\n\nMASTER Global robotic net (http://observ.pereplet.ru Lipunov et al.,2010,Advances in Astronomy,2010,30L)\nstarted Fermi (GCN 35908,trig\u0005:40:08) GRB 240310A inspection (cover map in Lipunov et al. GCN 35910)\nin MASTER-Amur, MASTER-SAAO, AMSTER-Tunka, MASTER-Kislovodsk, MASTER-Tavrida\n\nDuring inspection inside 3-sigma error-box (see map in GCN35910)\nMASTER auto-detection system found new OT, not presented in MASTER database since 2003, in VIZIER, in CRTS database\n\nMASTER OT J200702.72-263928.7 / AT2024efb discovery\n\nOT source at (RA, Dec) = 20h 07m 02.72s -26d 39m 28.7s on 2024-03-12.06429 UT.\n\nThe OT unfiltered magnitude is 16.8m at 3 images (mlim\u0018.7).\n\nThere is no minor planet at this place (we excluded 1999CO47 with m_V .8m in 14.4\"W,0.6\"N ).\n\nWe used reference image on 2018-10-07.86227 UT with unfiltered mlim\u0019.9m between thousands archive images.\n\nSpectral observations are required.\n\nthe association of this object with the gamma ray burst is not obvious\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35914.",
"published": "2024-03-12T09:59:42.327723Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-12T09:59:42.327740Z",
"modified": "2024-03-12T09:59:42.339012Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6214,
"topic": "gcn.circular",
"uuid": "095ba4d0-0be5-4eac-988f-58e7bab7c878",
"title": "GRB 240303C: VZLUSAT-2 detection",
"submitter": "Hop gcn.circular",
"authors": "Marianna DafÄÃková at Masaryk University <500025@mail.muni.cz>",
"data": {
"date": "24/03/12 19:07:08 GMT",
"from": "Marianna DafÄÃková at Masaryk University <500025@mail.muni.cz>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35915"
},
"title": "GCN CIRCULAR",
"number": "35915",
"subject": "GRB 240303C: VZLUSAT-2 detection"
},
"message_text": "M. Dafcikova, J. Ripa (Masaryk U.), A. Pal (Konkoly Observatory), N. Werner (Masaryk U.), M. Ohno (Hiroshima U.), L. Meszaros, B. Csak (Konkoly Observatory), H. Takahashi (Hiroshima U.), F. Munz , M. Topinka, F. Hroch, N. Husarikova, J.-P. Breuer (Masaryk U.), J. Hudec, J. Kapus, M. Frajt, M. Rezenov (Spacemanic s.r.o), R. Laszlo (Needronix), G. Galgoczi (Wigner Research Center/Eotvos U.), N. Uchida (ISAS/JAXA), T. Enoto (Kyoto U.), Zs. Frei (Eotvos U.), Y. Fukazawa, K. Hirose, H. Matake (Hiroshima U.), S. Hisadomi (Nagoya U.), Y. Ichinohe (Rikkyo U.), L. L. Kiss (Konkoly Observatory), T. Mizuno (Hiroshima U.), K. Nakazawa (Nagoya U.), H. Odaka (Univ of Tokyo), K. Torigoe (Hiroshima U.), P. Svoboda, V. Daniel, J. Dudas, M. Junas, J. Gromes (VZLU), I. Vertat (FEL ZCU) -- the VZLUSAT-2/GRB payload collaboration.\n\nThe long-duration GRB 240303C (Fermi/GBM detection: trigger no. 731189113; Konus/Wind detection trigger at 2024-03-03 20:05:07.253 UT) was detected by the GRB detectors on board of the VZLUSAT-2 3U CubeSat (https://www.vzlusat2.cz/en/).\n\nThe data acquisition was performed by the GRB detector units no. 0 and no. 1. The detection was confirmed at the peak time 2024-03-03 20:04:53 (20:04:52) UTC. The T90 duration is 5 s (3 s) and the significance during T90 reaches 7.8 sigma (5.7 sigma) for detector unit no. 0 (no. 1).\n\nThe light curve obtained by VZLUSAT-2 is available here:\nhttps://vzlusat2.konkoly.hu/static/share/GRB240303C_GCN_VZLUSAT2.pdf\n\nWe note that the light curve measured by VZLUSAT-2 is shifted by approximately 18 s with respect to light curves obtained by other missions. At the moment, the cause of this discrepancy is being investigated.\n\nAll VZLUSAT-2 detections are listed at: https://monoceros.physics.muni.cz/hea/VZLUSAT-2/\nThe GRB detectors on VZLUSAT-2 are a demonstration payload for a future CubeSat constellation (Werner et al. Proc. SPIE 2018). Two GRB modules of VZLUSAT-2 are placed in a perpendicular manner and each consists of a 75 x 75 x 5 mm3 CsI scintillator read out by a SiPM array, covering the energy range from ~30 keV to ~1000 keV. VZLUSAT-2 was launched on 2022 January 13 from Cape Canaveral.\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35915.",
"published": "2024-03-12T19:07:25.829946Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-12T19:07:25.829970Z",
"modified": "2024-03-12T19:07:25.840905Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6215,
"topic": "gcn.circular",
"uuid": "c757d056-40a2-467b-ab4a-4354d924e88c",
"title": "Swift Trigger 1219874 is not astrophysical",
"submitter": "Hop gcn.circular",
"authors": "Boris Sbarufatti at INAF-OAB <boris.sbarufatti@inaf.it>",
"data": {
"date": "24/03/12 21:03:44 GMT",
"from": "Boris Sbarufatti at INAF-OAB <boris.sbarufatti@inaf.it>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35916"
},
"title": "GCN CIRCULAR",
"number": "35916",
"subject": "Swift Trigger 1219874 is not astrophysical"
},
"message_text": "\nB. Sbarufatti (INAF-OAB) report on behalf of the Neil Gehrels Swift\nObservatory Team:\n\nSwift Trigger 1219874 is due to an outage of the star trackers, and therefore is not astrophysical.\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35916.",
"published": "2024-03-12T21:04:07.501226Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-12T21:04:07.501246Z",
"modified": "2024-03-12T21:04:07.509222Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6216,
"topic": "gcn.circular",
"uuid": "256a4b6c-56b1-413a-bcd7-cc8dd4c705cf",
"title": "GRB 240312A: GECAM detection of a long burst",
"submitter": "Hop gcn.circular",
"authors": "wenlongzhang2018@163.com",
"data": {
"date": "24/03/13 03:12:08 GMT",
"from": "wenlongzhang2018@163.com",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35917"
},
"title": "GCN CIRCULAR",
"number": "35917",
"subject": "GRB 240312A: GECAM detection of a long burst"
},
"message_text": "Wen-Long Zhang, Shao-Lin Xiong, Xiao-Yun Zhao report on behalf of the GECAM team:\n\nGECAM-B was triggered in-flight by a long burst, GRB 240312A, at 2024-03-12T14:02:10.550 UTC (T0). INTEGRAL/SPI-ACS was also triggered by this burst.\n\nAccording to the GECAM-B light curves, this burst shows single-pulses with a total duration of ~5 sec.\n\nAccording to the in-flight software, GECAM-B localized this burst to the following position (J2000):\nRa: 13.86 deg\nDec: 2.45 deg\nErr: 2.74 deg (1-sigma, statistical only)\n\nThe time-averaged spectrum of GECAM-B realtime data from about T0-0.2 to T0+3.8 s could be\nadequately fit by a Band function with a flux about 2.09E-6 erg/cm^2/s in 20-1000 keV.\n\nWe note that these results are very preliminary. Refined analysis will be reported later.\n\nGravitational wave high-energy Electromagnetic Counterpart All-sky Monitor (GECAM) mission originally consists of two microsatellites (GECAM-A and GECAM-B) launched in December 2020. As the third member of GECAM constellation, GECAM-C was launched onboard SATech-01 experimental satellite in July 2022. GECAM mission is funded by the Chinese Academy of Sciences (CAS).\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35917.",
"published": "2024-03-13T03:12:26.379214Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-13T03:12:26.379228Z",
"modified": "2024-03-13T03:12:26.388035Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6217,
"topic": "gcn.circular",
"uuid": "b34a5f57-1d09-4380-bcde-166620da69a7",
"title": "Swift Trigger 1219905 is not a GRB",
"submitter": "Hop gcn.circular",
"authors": "Boris Sbarufatti at INAF-OAB <boris.sbarufatti@inaf.it>",
"data": {
"date": "24/03/13 03:56:31 GMT",
"from": "Boris Sbarufatti at INAF-OAB <boris.sbarufatti@inaf.it>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35918"
},
"title": "GCN CIRCULAR",
"number": "35918",
"subject": "Swift Trigger 1219905 is not a GRB"
},
"message_text": "\nB. Sbarufatti (INAF-OAB) report on behalf of the Neil Gehrels Swift\nObservatory Team:\n\nSwift Trigger 1219905 is due to an outage of the star trackers, and therefore is not astrophysical.\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35918.",
"published": "2024-03-13T03:56:47.360739Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-13T03:56:47.360757Z",
"modified": "2024-03-13T03:56:47.366959Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6218,
"topic": "gcn.circular",
"uuid": "4954829f-9c1b-46ba-abdb-31a7ba5b8374",
"title": "Swift Trigger 1219909 and 1219910 are not a astrophysical",
"submitter": "Hop gcn.circular",
"authors": "Boris Sbarufatti at INAF-OAB <boris.sbarufatti@inaf.it>",
"data": {
"date": "24/03/13 04:51:58 GMT",
"from": "Boris Sbarufatti at INAF-OAB <boris.sbarufatti@inaf.it>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35919"
},
"title": "GCN CIRCULAR",
"number": "35919",
"subject": "Swift Trigger 1219909 and 1219910 are not a astrophysical"
},
"message_text": "\nB. Sbarufatti (INAF-OAB) report on behalf of the Neil Gehrels Swift\nObservatory Team:\n\nSwift Trigger 1219909 and 1219910 are due to an outage of the star trackers, and therefore are not astrophysical.\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35919.",
"published": "2024-03-13T04:52:14.453448Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-13T04:52:14.453464Z",
"modified": "2024-03-13T04:52:14.463475Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6219,
"topic": "gcn.circular",
"uuid": "1d155975-2ed8-4055-bffd-58b8769fa017",
"title": "Swift triggers 1219917, 1219917 and 1219922 were not astrophysical",
"submitter": "Hop gcn.circular",
"authors": "Boris Sbarufatti at INAF-OAB <boris.sbarufatti@inaf.it>",
"data": {
"date": "24/03/13 10:16:10 GMT",
"from": "Boris Sbarufatti at INAF-OAB <boris.sbarufatti@inaf.it>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35920"
},
"title": "GCN CIRCULAR",
"number": "35920",
"subject": "Swift triggers 1219917, 1219917 and 1219922 were not astrophysical"
},
"message_text": "\nB. Sbarufatti (INAF-OAB) report on behalf of the Neil Gehrels Swift\nObservatory Team:\n\nTriggers 1219917, 1219917 and 1219922 were due to an outage of the star trackers, and therefore are not astrophysical\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35920.",
"published": "2024-03-13T10:16:26.346538Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-13T10:16:26.346558Z",
"modified": "2024-03-13T10:16:26.354350Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6220,
"topic": "gcn.circular",
"uuid": "8f08d6c4-27e6-496e-b6c4-b45ef2808968",
"title": "GRB 240312A: Glowbug gamma-ray detection",
"submitter": "Hop gcn.circular",
"authors": "C.C. Cheung at Naval Research Lab <Teddy.Cheung@nrl.navy.mil>",
"data": {
"date": "24/03/13 19:21:31 GMT",
"from": "C.C. Cheung at Naval Research Lab <Teddy.Cheung@nrl.navy.mil>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35921"
},
"title": "GCN CIRCULAR",
"number": "35921",
"subject": "GRB 240312A: Glowbug gamma-ray detection"
},
"message_text": "C.C. Cheung, R. Woolf, M. Kerr, J.E. Grove (NRL), A. Goldstein (USRA), C.A. Wilson-Hodge, D. Kocevski (MSFC), and M.S. Briggs (UAH) report:\n \nThe Glowbug gamma-ray telescope [1,2], operating on the International Space Station, reports the detection of GRB 240312A, which was also detected by GECAM-B (GCN 35917) and INTEGRAL/SPI-ACS (Trigger 10625).\n \nUsing an adaptive window with a resolution of 32-ms, the burst onset is determined to be 2024-03-12 14:02:09.584 with a duration of 2.0 s and a total significance of about 8.1 sigma. The light curve comprises a single peak.\n \nUsing a standard power-law function with an exponential high-energy cutoff [3] to model the emission over this duration results in a poorly constrained power-law index and a cutoff energy (\"Epeak\") of 185 keV. The modeled 10-10000 keV fluence is 2.7e-07 erg/cm^2.\n \nThe analysis results presented here are preliminary and use a response function that lacks a detailed characterization of the surrounding passive structure of the ISS.\n \nGlowbug is a NASA-funded technology demonstrator for sensitive, low-cost gamma-ray transient telescopes developed, built, and operated by the U.S. Naval Research Laboratory (NRL) with support from the University of Alabama in Huntsville, USRA, and NASA MSFC. It was launched on 2023 March 15 aboard the Department of Defense Space Test Programâs STP-H9 to the ISS. The detector comprises 12 large-area (15 cm x 15 cm) CsI:Tl panels covering the surface of a half cube, and two hexagonal (5-cm diameter, 10-cm length) CLLB scintillators, giving it a large field of view (instantaneous FoV ~2/3 sky) over a wide energy band of 50 keV to >2 MeV.\n \n[1] Grove, J.E. et al. 2020, Proc. Yamada Conf. LXXI, arXiv:2009.11959\n[2] Woolf, R.S. et al. 2022, Proc. SPIE, 12181, id. 121811O\n[3] Goldstein, A. et al. 2020, ApJ 895, 40, arXiv :1909.03006\n \nDistribution Statement A: Approved for public release. Distribution is unlimited\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35921.",
"published": "2024-03-13T19:21:49.384137Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-13T19:21:49.384153Z",
"modified": "2024-03-13T19:21:49.393246Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6646,
"topic": "gcn.circular",
"uuid": "592737b0-07fb-4720-a636-dc89c4151b01",
"title": "LIGO/Virgo/KAGRA S240413p: DECam GW-MMADS candidates",
"submitter": "Hop gcn.circular",
"authors": "Antonella Palmese at Carnegie Mellon University <apalmese@andrew.cmu.edu>",
"data": {
"date": "24/04/18 03:51:55 GMT",
"from": "Antonella Palmese at Carnegie Mellon University <apalmese@andrew.cmu.edu>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/36153"
},
"title": "GCN CIRCULAR",
"number": "36153",
"subject": "LIGO/Virgo/KAGRA S240413p: DECam GW-MMADS candidates"
},
"message_text": "LIGO/Virgo/KAGRA S240413p: DECam GW-MMADS candidates\n\nAntonella Palmese (CMU), Lei Hu (CMU), Tomás Cabrera (CMU), Igor Andreoni (UMD), Malte Busman (LMU), Saavik Ford (AMNH/CUNY), Julius Gassert (LMU), Matthew Graham (Caltech), Daniel Gruen (LMU), Brendan O'Connor (CMU), Jake Postiglione (CUNY), Julian Sommer (LMU) report on behalf of the GW-MMADS team:\n\nThe high probability area of the LVK gravitational wave candidate S240413p (GCN 36075, 36082) was observed using the wide-field Dark Energy Camera (DECam) on the 4m Blanco telescope, as part of the âSearch, discovery and follow up of electromagnetic counterparts of gravitational wave eventsâ program\n(PI: Soares-Santos). We reduced exposures taken starting at 2024-04-16 00:53 UTC on the first night and 2024-04-16 23:25 UTC on the second night of the follow-up. The first nightâs observations covered r and i band, and the second nightâs observations were performed in i band. \n\nWe run the SFFT difference imaging (Hu et al. 2022) on the available images, filter out likely stars and moving objects, and visually inspect the remaining transients. We report new transients within the LVK 99% CI area that we do not currently exclude as candidate counterparts based on available redshift information. \n\n+-------------------------+----------+----------+------------+-------------+-----------+\n| id | ra | dec | mjd | mag±err (ab)| filter |\n|-------------------------+----------+----------+------------+-------------+-----------|\n| C202404161101539p095533 | 165.4746 | 9.9258 | 60416.04736 | 21.31±0.08 | i |\n| T202404161055381p073155 | 163.9089 | 7.5319 | 60416.15488 | 21.14±0.08 | i |\n| T202404161035468p033742 | 158.9451 | 3.6284 | 60416.09484 | 21.41±0.04 | r |\n| T202404161046169p084925 | 161.5702 | 8.8237 | 60416.13789 | 21.2±0.05 | i |\n| T202404161030235p040944 | 157.5978 | 4.1621. | 60416.13357 | 21.43±0.06 | i |\n|-------------------------+----------+----------+------------+-------------+-----------+\n\nFurther inspection of candidate counterparts is underway.\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/36153.",
"published": "2024-04-18T03:52:13.782884Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-04-18T03:52:13.782899Z",
"modified": "2024-04-18T03:52:13.791337Z",
"nonlocalizedevents": [
{
"event_id": "S240413p"
}
],
"targets": []
},
{
"id": 6221,
"topic": "gcn.circular",
"uuid": "bde75503-f3e0-4d91-88f9-eb4d790b1ed8",
"title": "GRB240204A: VIRT optical upper limit",
"submitter": "Hop gcn.circular",
"authors": "Priya Gokuldass at ERAU <gokuldap@my.erau.edu>",
"data": {
"date": "24/03/14 00:11:58 GMT",
"from": "Priya Gokuldass at ERAU <gokuldap@my.erau.edu>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35922"
},
"title": "GCN CIRCULAR",
"number": "35922",
"subject": "GRB240204A: VIRT optical upper limit"
},
"message_text": "K. Smith (UVI), P. Gokuldass (ERAU), N. Orange (OrangeWave Innovative Science, LLC), D. Morris (NASA), T. Lombardi (Eckerd College), K. Noonan (UVI), R. Querrard (UVI), D. Smith (UVI) report:\n\nWe observed the field of GRB240204A (Cenko et al., GCN 35666) with the 0.5m Virgin Island Robotic Telescope (VIRT) at the University of the Virgin Islands' Etelman Observatory on 02-05-2024 starting at 00:36:35 (T+10.04 hrs). We performed a series of exposures in an R filter with a total exposure of 4000s. The weather conditions were clear during the hours of observation with an average airmass of 1.08.\n\nWe do not detect any source within the enhanced XRT position (Beardmore et al. GCN 35671). This non-detection is consistent with the upper limits and detections of the faint optical transient reported by Master (Lipunov et al., GCN 35668), Mondy (Pozanenko et al., GCN 35670), Montarrenti Observatory (Leonini et al., GCN 35672), LCOGT (Perez-Fournon and Poidevin, GCN 35673), Osservatorio Nastro Verde (Ruocco et al., GCN 35677), Liverpool Telescope (Bochenek et al., GCN 35678), and Observatoire de Haute-Provence (Adami et al., GCN 35690). We report the following 3-sigma upper limit:\n\nT_mid ||Exposure ||Filter ||Limit\nT+ 10.04 hrs || 4000s || R || >20.9\n\nThe limit is estimated from comparison to nearby USNO B1 stars and is not corrected for Galactic extinction. The VIRT is still in the commissioning phase.\n\nWe acknowledge financial support from NASA MUREP MIRO award 80NSSC21M0001 and NASA EPSCoR award 80NNSC22M0063. R.Q and N.B.O also acknowledge financial support from South Carolina Space Grant award 80NSSC20M0054. This message can be cited.\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35922.",
"published": "2024-03-14T00:12:18.702929Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-14T00:12:18.702944Z",
"modified": "2024-03-14T00:12:18.709992Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6222,
"topic": "gcn.circular",
"uuid": "702f0773-a023-43c7-927e-1ace11f30f3f",
"title": "GRB 240314A: Fermi GBM Final Real-time Localization",
"submitter": "Hop gcn.circular",
"authors": "Fermi GBM Team at MSFC/Fermi-GBM <do_not_reply@GIOC.nsstc.nasa.gov>",
"data": {
"date": "24/03/14 11:41:45 GMT",
"from": "Fermi GBM Team at MSFC/Fermi-GBM <do_not_reply@GIOC.nsstc.nasa.gov>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35923"
},
"title": "GCN CIRCULAR",
"number": "35923",
"subject": "GRB 240314A: Fermi GBM Final Real-time Localization"
},
"message_text": "The Fermi GBM team reports the detection of a likely LONG GRB\n\nAt 11:31:07 UT on 14 Mar 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 240314A (trigger 732108672.455724 / 240314480).\n\nThe on-ground calculated location, using the Fermi GBM trigger data, is RA = 142.2, Dec = 22.0 (J2000 degrees, equivalent to J2000 09h 28m, 22d 00'), with a statistical uncertainty of 6.3 degrees.\n\nThe angle from the Fermi LAT boresight is 32.0 degrees.\n\nThe skymap can be found here:\nhttps://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240314480/quicklook/glg_skymap_all_bn240314480.png\n\nThe HEALPix FITS file, including the estimated localization systematic, can be found here:\nhttps://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240314480/quicklook/glg_healpix_all_bn240314480.fit\n\nThe GBM light curve can be found here:\nhttps://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240314480/quicklook/glg_lc_medres34_bn240314480.gif\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35923.",
"published": "2024-03-14T11:42:01.998835Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-14T11:42:01.998851Z",
"modified": "2024-03-14T11:42:02.012607Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6223,
"topic": "gcn.circular",
"uuid": "5ef87cc7-3100-445e-9bea-e4d5dd7818e0",
"title": "Fermi GRB 240314A: Global MASTER-Net observations report",
"submitter": "Hop gcn.circular",
"authors": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"data": {
"date": "24/03/14 12:45:42 GMT",
"from": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35924"
},
"title": "GCN CIRCULAR",
"number": "35924",
"subject": "Fermi GRB 240314A: Global MASTER-Net observations report"
},
"message_text": "V. Lipunov, V.Kornilov, E. Gorbovskoy, K. Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, V.Senik, D. Vlasenko,\nG.Antipov, D.Zimnukhov, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov, D. Cheryasov, Ya.Kechin, Yu.Tselik, A. Sosnovskij\n(Lomonosov Moscow State University, SAI, Physics Department),\n\nR. Podesta, C.Lopez, F. Podesta, C.Francile\n(Observatorio Astronomico Felix Aguilar OAFA),\n\nR. Rebolo, M. Serra\n(The Instituto de Astrofisica de Canarias),\n\nD. Buckley\n(South African Astronomical Observatory),\n\nO.A. Gress, N.M. Budnev, O.Ershova\n(Irkutsk State University, API),\n\nL.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez,\nA.R.Corella, L.H.Rodriguez\n(INAOE, Guillermo Haro Astrophysics Observatory),\n\nA. Tlatov, D. Dormidontov\n(Kislovodsk Solar Station of the Pulkovo Observatory),\n\nV. Yurkov, A. Gabovich\n(Blagoveschensk Educational State University)\n\nMASTER-Tunka robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Applied Physics Institute, Irkutsk State University) started inspect of the Fermi GRB 240314A ( Fermi GBM team, GCN 35923) errorbox 2094 sec after notice time and 2130 sec after trigger time at 2024-03-14 12:06:38 UT, with upper limit up to 21.0 mag. Observations started at twilight. The observations began at zenith distance = 49 deg. The sun altitude is -9.8 deg.\n\nThe galactic latitude b = 44 deg., longitude l = 208 deg.\n\n\nReal time updated cover map and OT discovered available here:\nhttps://master.sai.msu.ru/site/master2/observ.php?id#99137\n\nWe obtain a following upper limits.\n\nTmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment\n_________|_____________________|_____________________|____________________________________|_____|_______|_______|________\n\n 2161 | 2024-03-14 12:06:38 | MASTER-Tunka | (09h 38m 21.12s , +19d 35m 30.4s) | C | 60 | 14.0 |\n 2240 | 2024-03-14 12:07:57 | MASTER-Tunka | (09h 46m 47.30s , +19d 34m 19.2s) | C | 60 | 13.9 |\n 2319 | 2024-03-14 12:09:16 | MASTER-Tunka | (09h 47m 39.13s , +17d 41m 52.7s) | C | 60 | 14.3 |\n 2636 | 2024-03-14 12:14:33 | MASTER-Tunka | (09h 54m 28.40s , +19d 34m 23.7s) | C | 60 | 13.9 |\n 2795 | 2024-03-14 12:17:12 | MASTER-Tunka | (09h 54m 09.79s , +23d 22m 51.5s) | C | 60 | 13.2 |\n 2874 | 2024-03-14 12:18:31 | MASTER-Tunka | (10h 02m 58.51s , +23d 23m 58.1s) | C | 60 | 13.7 |\n 2954 | 2024-03-14 12:19:51 | MASTER-Tunka | (09h 36m 11.27s , +13d 55m 07.8s) | C | 60 | 14.0 |\n 3270 | 2024-03-14 12:25:07 | MASTER-Tunka | (09h 47m 39.73s , +17d 42m 53.7s) | C | 60 | 14.1 |\n 3349 | 2024-03-14 12:26:26 | MASTER-Tunka | (09h 56m 05.28s , +17d 41m 17.0s) | C | 60 | 14.4 |\n 3588 | 2024-03-14 12:30:25 | MASTER-Tunka | (09h 54m 28.29s , +19d 37m 08.1s) | C | 60 | 14.4 |\n 3746 | 2024-03-14 12:33:03 | MASTER-Tunka | (09h 54m 06.55s , +23d 23m 18.0s) | C | 60 | 15.5 |\n 3825 | 2024-03-14 12:34:22 | MASTER-Tunka | (10h 02m 58.89s , +23d 23m 11.0s) | C | 60 | 13.8 |\n 3905 | 2024-03-14 12:35:42 | MASTER-Tunka | (09h 36m 15.10s , +13d 55m 44.7s) | C | 60 | 14.8 |\n 4063 | 2024-03-14 12:38:20 | MASTER-Tunka | (09h 38m 21.67s , +19d 37m 46.3s) | C | 60 | 14.8 |\n 4142 | 2024-03-14 12:39:39 | MASTER-Tunka | (09h 46m 48.16s , +19d 36m 46.6s) | C | 60 | 21.0 |\nFilter C is a clear (unfiltred) band.\n\n\nThe observation and reduction will continue.\nThe message may be cited.\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35924.",
"published": "2024-03-14T12:45:57.210662Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-14T12:45:57.210679Z",
"modified": "2024-03-14T12:45:57.218458Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6224,
"topic": "gcn.circular",
"uuid": "78a296af-93d4-4797-a692-fcfd1668c56b",
"title": "Swift Triggers 1220090, 1220091 and 1220092 are not astrophysical",
"submitter": "Hop gcn.circular",
"authors": "Boris Sbarufatti at INAF-OAB <boris.sbarufatti@inaf.it>",
"data": {
"date": "24/03/14 22:57:02 GMT",
"from": "Boris Sbarufatti at INAF-OAB <boris.sbarufatti@inaf.it>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35925"
},
"title": "GCN CIRCULAR",
"number": "35925",
"subject": "Swift Triggers 1220090, 1220091 and 1220092 are not astrophysical"
},
"message_text": "\nB. Sbarufatti (INAF-OAB) report on behalf of the Neil Gehrels Swift\nObservatory Team:\n\nSwift Triggers 1220090, 1220091 and 1220092 were due to an outage of the star trackers, and therefore are not astrophysical\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35925.",
"published": "2024-03-14T22:57:16.627504Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-14T22:57:16.627527Z",
"modified": "2024-03-14T22:57:16.635834Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6226,
"topic": "gcn.circular",
"uuid": "1f868d96-b97b-4e96-bca0-a05c613e8f46",
"title": "GRB 240315A: Fermi GBM Final Real-time Localization",
"submitter": "Hop gcn.circular",
"authors": "Fermi GBM Team at MSFC/Fermi-GBM <do_not_reply@GIOC.nsstc.nasa.gov>",
"data": {
"date": "24/03/15 11:18:06 GMT",
"from": "Fermi GBM Team at MSFC/Fermi-GBM <do_not_reply@GIOC.nsstc.nasa.gov>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35927"
},
"title": "GCN CIRCULAR",
"number": "35927",
"subject": "GRB 240315A: Fermi GBM Final Real-time Localization"
},
"message_text": "The Fermi GBM team reports the detection of a likely LONG GRB\n\nAt 11:07:29 UT on 15 Mar 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 240315A (trigger 732193654.441586 / 240315464).\n\nThe on-ground calculated location, using the Fermi GBM trigger data, is RA = 199.5, Dec = 21.9 (J2000 degrees, equivalent to J2000 13h 18m, 21d 53'), with a statistical uncertainty of 14.1 degrees.\n\nThe angle from the Fermi LAT boresight is 77.0 degrees.\n\nThe skymap can be found here:\nhttps://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240315464/quicklook/glg_skymap_all_bn240315464.png\n\nThe HEALPix FITS file, including the estimated localization systematic, can be found here:\nhttps://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240315464/quicklook/glg_healpix_all_bn240315464.fit\n\nThe GBM light curve can be found here:\nhttps://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240315464/quicklook/glg_lc_medres34_bn240315464.gif\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35927.",
"published": "2024-03-15T11:18:21.638643Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-15T11:18:21.638659Z",
"modified": "2024-03-15T11:18:21.647657Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6227,
"topic": "gcn.circular",
"uuid": "898289bc-d7dd-49b0-8e91-ddda5796c570",
"title": "Swift Triggers 1220155, 1220156, 1220157, 1220158, 1220160 and 1220161 were not astrophysical",
"submitter": "Hop gcn.circular",
"authors": "Boris Sbarufatti at INAF-OAB <boris.sbarufatti@inaf.it>",
"data": {
"date": "24/03/15 12:27:50 GMT",
"from": "Boris Sbarufatti at INAF-OAB <boris.sbarufatti@inaf.it>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35928"
},
"title": "GCN CIRCULAR",
"number": "35928",
"subject": "Swift Triggers 1220155, 1220156, 1220157, 1220158, 1220160 and 1220161 were not astrophysical"
},
"message_text": "\nB. Sbarufatti (INAF-OAB) report on behalf of the Neil Gehrels Swift\nObservatory Team:\n\nSwift Triggers 1220155, 1220156, 1220157, 1220158, 1220160 and 1220161 were due to an outage of the star trackers, and therefore are not astrophysical.\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35928.",
"published": "2024-03-15T12:28:07.769187Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-15T12:28:07.769208Z",
"modified": "2024-03-15T12:28:07.776573Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6649,
"topic": "gcn.circular",
"uuid": "12a8b711-943b-4d80-b438-b451c4c1978b",
"title": "EP240414a: GSP detects optical candidate counterpart AT2024gsa",
"submitter": "Hop gcn.circular",
"authors": "Wenxiong Li <liwenxiong1992@gmail.com>",
"data": {
"date": "24/04/18 05:19:43 GMT",
"from": "Wenxiong Li <liwenxiong1992@gmail.com>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/36154"
},
"title": "GCN CIRCULAR",
"number": "36154",
"subject": "EP240414a: GSP detects optical candidate counterpart AT2024gsa"
},
"message_text": "W. X. Li, S. J. Xue, H. Sun (NAOC), X. F. Wang (THU), M. Andrews, J. Farrah, D. A. Howell, M. Newsome, E. Padilla Gonzalez, C. McCully, and G. Terreran (Las Cumbres Observatory), on behalf of a larger collaboration, report the optical follow-up observations of AT2024gsa (Aryan et al., GCN 36094, Xu et al., GCN 36105, Srivastav et al. GCN 36150). This transient was identified as the optical counterpart to the fast X-ray transient EP240414a (Lian et al., GCN 36091; Guan et al., GCN 36129).\n\nOur observations were conducted on 2024 April 18.065 UT using the 1-meter telescope at the Las Cumbres Observatory node located at Cerro Tololo Interamerican Observatory in Chile. AT2024gsa is detected in all BVgri band images.\nThe photometric results are:\nB ~ 21.3m\nV ~ 20.9m\ng ~ 21.1m\nr ~ 20.7m\ni ~ 20.6m\n\nFurther followup observations are encouraged.\n\nThese observations were taken as part of the Global Supernova Project.\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/36154.",
"published": "2024-04-18T05:20:07.889567Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-04-18T05:20:07.889583Z",
"modified": "2024-04-18T05:20:07.898982Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6228,
"topic": "gcn.circular",
"uuid": "137c3834-c028-460a-9823-3cc460fa2d81",
"title": "Changes to the Fermi-GBM Triggering Thresholds",
"submitter": "Hop gcn.circular",
"authors": "Oliver J Roberts at USRA/NASA <oliver.roberts@nasa.gov>",
"data": {
"date": "24/03/15 18:28:40 GMT",
"from": "Oliver J Roberts at USRA/NASA <oliver.roberts@nasa.gov>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35929"
},
"title": "GCN CIRCULAR",
"number": "35929",
"subject": "Changes to the Fermi-GBM Triggering Thresholds"
},
"message_text": "O.J. Roberts reports on behalf of the GBM Team\n\nAt 15:00 UTC on March 14th, 2024, the triggering thresholds on Fermi-GBM triggering algorithms 8-11, were reduced from 4.5 sigma to 4.0 sigma. These algorithms are designed to trigger on short (256 and 512 ms) timescales over 50-300 keV. More information on these and other triggering algorithms that Fermi-GBM uses can be found in Table 1 of the first GBM Catalog [1]. This was undertaken to obtain additional short GRBs that will be rapidly down-linked for multi messenger science. The external coincidence search RAVEN [2,3] will automatically ingest the GBM localizations from these GRBs and issue joint GW-GRB detection skymaps through the LVK alert stream.\n\nFurther testing is ongoing, during which time, these and possibly other triggering algorithm thresholds may be reduced further. Consequently, Fermi-GBM may trigger and localize spurious events. We note that the trigger algorithm and significance are listed in the Fermi-GBM Alert GCN notice type. We will report on any spurious events, and provide a final update on the threshold values of the triggering algorithms that were amended, in a further GCN notice once testing has concluded.\n\n[1] Paciesas, W.S., et al., 2012 ApJS 199 18, https://iopscience.iop.org/article/10.1088/0067-0049/199/1/18/pdf\n[2] Urban, A.L., 2016, Ph.D. Thesis. https://dc.uwm.edu/etd/1218/\n[3] Piotrzkowski, B.J., 2022, Ph.D. Thesis https://dc.uwm.edu/etd/3060\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35929.",
"published": "2024-03-15T18:28:56.397682Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-15T18:28:56.397698Z",
"modified": "2024-03-15T18:28:56.406836Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6229,
"topic": "gcn.circular",
"uuid": "cdd22bbb-6b88-4f75-b1e5-d691d2fb2c16",
"title": "GRID detection of GRB 240306A",
"submitter": "Hop gcn.circular",
"authors": "GRID Student Team at Tsinghua University <grid@tsinghua.edu.cn>",
"data": {
"date": "24/03/16 12:53:36 GMT",
"from": "GRID Student Team at Tsinghua University <grid@tsinghua.edu.cn>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35930"
},
"title": "GCN CIRCULAR",
"number": "35930",
"subject": "GRID detection of GRB 240306A"
},
"message_text": "Chenyu Wang, Zirui Yang and Longhao Li report on behalf of the GRID Collaboration: \n\nGRID-03B reports the detection of the long-duration GRB 240306A, which was also detected by Fermi/GBM, Swift/BAT-GUANO and AstroSat CZTI (GCN Circular 35885, 35889 and 35892).\n\nThe event was triggered with GRID on 2024-03-06 at 06:45:48 UTC. The measured burst duration (T90) in the 30-2000 keV range is approximately 10.0 ± 1.0 seconds. Due to its proximity to Earth's atmosphere in the view of GRID-03B, the spectral data from GRID for this event may not be accurate.\n\nThe GRID light curve of this event can be found at https://mirrors.tuna.tsinghua.edu.cn/GRID/data/GRID-GCN/GRB240306A/GRID_GRB240306A_ltcv.pdf.\n\nGRID is a student-led project to monitor the transient gamma-ray sky with multiple detectors onboard different nanosatellites in the era of multi-messenger astronomy. For more information about GRID, please refer to the following references: https://doi.org/10.1007/s10686-019-09636-w and https://doi.org/10.1007/s10686-021-09819-4.\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35930.",
"published": "2024-03-16T12:53:53.827024Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-16T12:53:53.827039Z",
"modified": "2024-03-16T12:53:53.834960Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6230,
"topic": "gcn.circular",
"uuid": "40d4e162-bbc1-4158-a4f7-5366ffbbe834",
"title": "Einstein Probe detected of a fast X-ray transient EP240315a",
"submitter": "Hop gcn.circular",
"authors": "EP Team at NAOC/CAS <ep_ta@bao.ac.cn>",
"data": {
"date": "24/03/16 15:49:37 GMT",
"from": "EP Team at NAOC/CAS <ep_ta@bao.ac.cn>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35931"
},
"title": "GCN CIRCULAR",
"number": "35931",
"subject": "Einstein Probe detected of a fast X-ray transient EP240315a"
},
"message_text": "W. J. Zhang (NAOC, CAS), X. Mao (NAOC, CAS), W. D. Zhang (NAOC, CAS), H. Y. Liu (NAOC, CAS), Y. Liu (NAOC, CAS), C. Zhang (NAOC, CAS),\n\nZ. X. Ling (NAOC, CAS), C. C. Jin (NAOC, CAS), H. Q. Cheng (NAOC, CAS), W. Chen (NAOC, CAS), C. Z. Cui (NAOC, CAS), D. W. Fan (NAOC, CAS),\n\nH. B. Hu (NAOC, CAS), J. W. Hu (NAOC, CAS), M. H. Huang (NAOC, CAS), D. Y. Li (NAOC, CAS), T. Y. Lian (NAOC, CAS), M. J. Liu (NAOC, CAS),\n\nZ. Z. Lv (NAOC, CAS), H. W. Pan (NAOC, CAS), X. Pan (NAOC, CAS), H. Sun (NAOC, CAS), W. X. Wang (NAOC, CAS),Y. L. Wang (NAOC, CAS),\n\nQ. Y. Wu (NAOC, CAS), X. P. Xu (NAOC, CAS), Y. F. Xu (NAOC, CAS), H. N. Yang (NAOC, CAS), M. Zhang (NAOC, CAS), S. N. Zhang (IHEP, CAS),\n\nZ. Zhang (NAOC, CAS), D. H. Zhao (NAOC, CAS), E. Kuulkers (ESA), P. O'Brien (Univ. of Leicester) and W. Yuan (NAOC, CAS), on behalf of the Einstein Probe team\n\n\n\n\n\n\n We report on the detection of a fast X-ray transient EP240315a at 2024-03-15T20:10:44 (UTC) by the Wide-field X-ray Telescope (WXT) on board\n\nthe Einstein Probe (EP) mission during a calibration observation. The position of the source is R.A. = 141.644 deg, DEC = -9.547 deg (J2000)\n\nwith an uncertainty of 3 arcmin (radius, 90% C.L. statistical and systematic). The light curve of the source shows a multi-peak profile.\n\nThe transient event lasts for ~1600 seconds and has a peak flux of ~3e-9 erg/s/cm^2 in the 0.5-4 keV band. The averaged spectrum can be fitted\n\nby an absorbed power-law with NH = 1.5(-0.9/+1.0) x 10^21 cm^-2 and a photon index of 1.7(-0.4/+0.4). The derived average unabsorbed 0.5 - 4.0 keV\n\nflux is 5.3(-0.7/+1.0) x 10^-10 erg/s/cm^2. However, we note that the derived source parameters may be subject to larger uncertainties than those\n\nquoted here since in-orbit calibration of the instrument is still in progress.\n\n\n\n\n No previously known bright X-ray sources have been found within the 3 arcmin region around the source position, with only one optical counterpart\n\nof white dwarf candidate located at the distance of ~380 pc. Based on the shape and timescale of the observed flare light curve, we tend to consider\n\nthat the source is not a stellar flare, although this cannot be ruled out. A Swift target of opportunity observation has been proposed, and further\n\nfollow-up observations are strongly encouraged to identify the nature of this X-ray flare.\n\n\n\n\n\n The above observation was made with the WXT instrument during the commissioning phase of EP. Launched on January 9, 2024, EP is a space X-ray observatory\n\nto monitor the soft X-ray sky with X-ray follow-up capability (Yuan et al. 2022, Handbook of X-ray and Gamma-ray Astrophysics). EP is a mission of the Chinese\n\nAcademy of Sciences in collaboration with ESA, MPE and CNES.\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35931.",
"published": "2024-03-16T15:49:53.984745Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-16T15:49:53.984762Z",
"modified": "2024-03-16T15:49:53.992154Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6231,
"topic": "gcn.circular",
"uuid": "2698740c-2cb1-4153-b8e5-136ca5782014",
"title": "X-ray transient EP240315a: ATLAS detection of a possible optical counterpart AT2024eju",
"submitter": "Hop gcn.circular",
"authors": "S. Srivastav at Oxford <shubhamsrivastav@gmail.com>",
"data": {
"date": "24/03/16 22:08:06 GMT",
"from": "S. Srivastav at Oxford <shubhamsrivastav@gmail.com>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35932"
},
"title": "GCN CIRCULAR",
"number": "35932",
"subject": "X-ray transient EP240315a: ATLAS detection of a possible optical counterpart AT2024eju"
},
"message_text": "S. Srivastav, S. J. Smartt (Oxford), M. D. Fulton, K. W. Smith, A. Aamer, C. R. Angus, M. McCollum, T. Moore, M. Nicholl, X. Sheng, J. Weston, D. R. Young (QUB), P. Ramsden (QUB/Birmingham), L. Shingles (GSI/QUB), A. Andersson, J. H. Gillanders, L. Rhodes, H. Stevance (Oxford), J. Sommer (LMU/QUB), L. Denneau, J. Tonry, H. Weiland, A. Lawrence, R. Siverd (IfA, University of Hawaii), N. Erasmus, W. Koorts (South African Astronomical Observatory), A. Jordan, V. Suc (UAI, Obstech), A. Rest (STScI), T.-W. Chen (NCU), C. Stubbs (Harvard):\n\nHere we report the ATLAS detection of an optical transient AT2024eju, discovered within the error circle of the fast X-ray transient EP240315a reported by the Einstein Probe mission (Zhang et al, GCN 35931).\n\nATLAS is a quadruple 0.5-m telescope system with two units in Hawaii, one in Chile and one in South Africa (see Tonry et al. 2018, PASP, 130:064505), routinely surveying the visible sky on a daily basis. We promptly process all data with our transient science server (Smith et al. 2020, PASP, 132:085002).\n\nATLAS detected AT2024eju (TNS Astronomical Transient Report No. 205383) during normal survey mode observations at an AB magnitude of 19.37 +/- 0.14 in the ATLAS-cyan band on MJD 60384.887, around 1.1 hrs following the detection of the X-ray transient. The position of AT2024eju is 0.8 arcmin offset from the coordinates reported by Zhang et al. We found no historical detections of any excess optical flux in ATLAS at this position through forced photometry.\n\nSpectroscopic classification of this transient is encouraged.\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35932.",
"published": "2024-03-16T22:08:24.515215Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-16T22:08:24.515231Z",
"modified": "2024-03-16T22:08:24.522910Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6232,
"topic": "gcn.circular",
"uuid": "193c9adb-f24d-4974-9411-3c6dd9d62612",
"title": "AT2024eju: followup observations with Liverpool Telescope suggest a fading transient",
"submitter": "Hop gcn.circular",
"authors": "S. Srivastav at Oxford <shubhamsrivastav@gmail.com>",
"data": {
"date": "24/03/17 00:38:27 GMT",
"from": "S. Srivastav at Oxford <shubhamsrivastav@gmail.com>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35933"
},
"title": "GCN CIRCULAR",
"number": "35933",
"subject": "AT2024eju: followup observations with Liverpool Telescope suggest a fading transient"
},
"message_text": "S. Srivastav, S. J. Smartt (Oxford), M. D. Fulton and K. W. Smith (QUB) report on behalf of a larger collaboration:\n\nWe report follow-up photometry of AT2024eju, the possible optical counterpart (Srivastav et al., GCN 35932) of the fast X-ray transient EP240315a (Zhang et al., GCN 35931). The images were obtained with the 2m Liverpool Telescope in g, r and i bands starting on MJD 60385.848, 1.01 days following the discovery of the X-ray transient.\n\nThe transient was not detected in any of the 3 bands with the following upper limits:\n\nMJD\tFilter\tLimit (AB mag)\n60385.848\tg\t>19.55\n60385.851\tr\t>19.72\n60385.853\ti\t>20.02\n\nThis suggests that AT2024eju has likely faded since the ATLAS detection ~1 day ago, further follow-up observations are encouraged.\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35933.",
"published": "2024-03-17T00:38:41.887594Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-17T00:38:41.887609Z",
"modified": "2024-03-17T00:38:41.894473Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6233,
"topic": "gcn.circular",
"uuid": "03b04ffa-c57e-4d09-beed-91a29a554897",
"title": "Fermi trigger No 732299243: Global MASTER-Net observations report",
"submitter": "Hop gcn.circular",
"authors": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"data": {
"date": "24/03/17 02:15:39 GMT",
"from": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35934"
},
"title": "GCN CIRCULAR",
"number": "35934",
"subject": "Fermi trigger No 732299243: Global MASTER-Net observations report"
},
"message_text": "V. Lipunov, V.Kornilov, E. Gorbovskoy, K. Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, V.Senik, D. Vlasenko,\nG.Antipov, D.Zimnukhov, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov, D. Cheryasov, Ya.Kechin, Yu.Tselik, A. Sosnovskij\n(Lomonosov Moscow State University, SAI, Physics Department),\n\nR. Podesta, C.Lopez, F. Podesta, C.Francile\n(Observatorio Astronomico Felix Aguilar OAFA),\n\nR. Rebolo, M. Serra\n(The Instituto de Astrofisica de Canarias),\n\nD. Buckley\n(South African Astronomical Observatory),\n\nO.A. Gress, N.M. Budnev, O.Ershova\n(Irkutsk State University, API),\n\nL.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez,\nA.R.Corella, L.H.Rodriguez\n(INAOE, Guillermo Haro Astrophysics Observatory),\n\nA. Tlatov, D. Dormidontov\n(Kislovodsk Solar Station of the Pulkovo Observatory),\n\nV. Yurkov, A. Gabovich\n(Blagoveschensk Educational State University)\n\nMASTER-Amur robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Blagoveshchensk State Pedagogical University) started inspect of the Fermi GRB240316.69 (trigger No 732299243,14h 56m 04.08s , -04d 39m 00.0s, RP) errorbox 82 sec after notice time and 90 sec after trigger time at 2024-03-16 16:28:48 UT, with upper limit up to 18.8 mag. The observations began at zenith distance = 52 deg. The sun altitude is -40.4 deg.\n\nMASTER-Tunka robotic telescope located in Russia (Applied Physics Institute, Irkutsk State University) started inspect of the Fermi GRB240316.69 errorbox 219 sec after notice time and 227 sec after trigger time at 2024-03-16 16:31:05 UT, with upper limit up to 17.1 mag. The observations began at zenith distance = 29 deg. The sun altitude is -39.6 deg.\n\nMASTER-SAAO robotic telescope located in South Africa (South African Astronomical Observatory) started inspect of the Fermi GRB240316.69 errorbox 15653 sec after notice time and 15661 sec after trigger time at 2024-03-16 20:48:20 UT, with upper limit up to 19.8 mag. The observations began at zenith distance = 57 deg. The sun altitude is -46.3 deg.\n\nThe galactic latitude b = 46 deg., longitude l = 352 deg.\n\n\nReal time updated cover map and OT discovered available here:\nhttps://master.sai.msu.ru/site/master2/observ.php?id$00236\n\nWe obtain a following upper limits.\n\nTmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment\n_________|_____________________|_____________________|____________________________________|_____|_______|_______|________\n\n 181 | 2024-03-16 16:28:48 | MASTER-Amur | (16h 06m 46.77s , +18d 16m 17.0s) | C | 180 | 18.2 |\n 257 | 2024-03-16 16:31:05 | MASTER-Tunka | (13h 27m 34.20s , +36d 44m 47.4s) | C | 60 | 16.5 |\n 381 | 2024-03-16 16:32:08 | MASTER-Amur | (15h 58m 20.26s , +18d 16m 28.0s) | C | 180 | 18.2 |\n 580 | 2024-03-16 16:35:28 | MASTER-Amur | (16h 06m 52.31s , +18d 15m 48.4s) | C | 180 | 18.2 |\n 780 | 2024-03-16 16:38:47 | MASTER-Amur | (16h 04m 34.75s , +16d 20m 54.5s) | C | 180 | 17.8 |\n 733 | 2024-03-16 16:39:00 | MASTER-Tunka | (13h 32m 07.39s , +40d 34m 02.3s) | C | 60 | 16.8 |\n 892 | 2024-03-16 16:41:40 | MASTER-Tunka | (13h 32m 13.58s , +40d 33m 00.1s) | C | 60 | 16.9 |\n 979 | 2024-03-16 16:42:07 | MASTER-Amur | (16h 12m 51.86s , +16d 22m 45.0s) | C | 180 | 17.8 |\n 1179 | 2024-03-16 16:45:27 | MASTER-Amur | (16h 04m 31.81s , +16d 20m 21.8s) | C | 180 | 17.9 |\n 1289 | 2024-03-16 16:48:16 | MASTER-Tunka | (13h 17m 13.22s , +32d 58m 37.3s) | C | 60 | 16.6 |\n 1379 | 2024-03-16 16:48:47 | MASTER-Amur | (16h 12m 54.64s , +16d 21m 56.4s) | C | 180 | 18.0 |\n 1686 | 2024-03-16 16:54:54 | MASTER-Tunka | (13h 45m 20.90s , +34d 51m 15.4s) | C | 60 | 16.5 |\n 1856 | 2024-03-16 16:56:43 | MASTER-Amur | (16h 11m 31.26s , +14d 27m 53.9s) | C | 180 | 17.6 |\n 2055 | 2024-03-16 17:00:03 | MASTER-Amur | (16h 19m 55.52s , +14d 27m 11.5s) | C | 180 | 17.9 |\n 2003 | 2024-03-16 17:00:10 | MASTER-Tunka | (13h 27m 40.18s , +31d 04m 46.7s) | C | 60 | 15.5 |\n 2254 | 2024-03-16 17:03:22 | MASTER-Amur | (16h 11m 32.54s , +14d 25m 22.3s) | C | 180 | 18.0 |\n 2454 | 2024-03-16 17:06:42 | MASTER-Amur | (16h 19m 55.51s , +14d 25m 43.2s) | C | 180 | 18.1 |\n 2478 | 2024-03-16 17:08:06 | MASTER-Tunka | (12h 57m 33.81s , +27d 19m 32.5s) | C | 60 | 16.3 |\n 2654 | 2024-03-16 17:10:02 | MASTER-Amur | (16h 09m 21.09s , +20d 06m 53.5s) | C | 180 | 18.4 |\n 2637 | 2024-03-16 17:10:45 | MASTER-Tunka | (13h 14m 50.30s , +27d 18m 20.3s) | C | 60 | 16.7 |\n 2716 | 2024-03-16 17:12:04 | MASTER-Tunka | (13h 02m 37.62s , +29d 13m 32.9s) | C | 60 | 16.3 |\n 2854 | 2024-03-16 17:13:22 | MASTER-Amur | (16h 17m 56.91s , +20d 08m 32.8s) | C | 180 | 18.1 |\n 2796 | 2024-03-16 17:13:24 | MASTER-Tunka | (13h 14m 47.48s , +27d 17m 47.5s) | C | 60 | 16.1 |\n 2875 | 2024-03-16 17:14:43 | MASTER-Tunka | (13h 02m 36.55s , +29d 11m 37.3s) | C | 60 | 16.3 |\n 2954 | 2024-03-16 17:16:02 | MASTER-Tunka | (13h 11m 56.34s , +29d 11m 14.5s) | C | 60 | 16.3 |\n 3053 | 2024-03-16 17:16:41 | MASTER-Amur | (16h 09m 18.18s , +20d 07m 01.1s) | C | 180 | 18.6 |\n 3034 | 2024-03-16 17:17:21 | MASTER-Tunka | (12h 45m 06.68s , +29d 12m 28.5s) | C | 60 | 16.7 |\n 3253 | 2024-03-16 17:20:00 | MASTER-Amur | (16h 17m 50.04s , +20d 08m 24.0s) | C | 180 | 18.4 |\n 3272 | 2024-03-16 17:21:20 | MASTER-Tunka | (12h 54m 17.26s , +29d 14m 25.4s) | C | 60 | 15.8 |\n 3351 | 2024-03-16 17:22:39 | MASTER-Tunka | (12h 31m 12.24s , +27d 19m 42.7s) | C | 60 | 16.4 |\n 3452 | 2024-03-16 17:23:20 | MASTER-Amur | (15h 59m 58.59s , +25d 46m 37.5s) | C | 180 | 18.5 |\n 3431 | 2024-03-16 17:23:58 | MASTER-Tunka | (12h 54m 22.42s , +29d 12m 43.0s) | C | 60 | 15.8 |\n 3510 | 2024-03-16 17:25:17 | MASTER-Tunka | (12h 31m 14.52s , +27d 21m 38.6s) | C | 60 | 16.1 |\n 3589 | 2024-03-16 17:26:37 | MASTER-Tunka | (12h 40m 18.15s , +27d 19m 37.8s) | C | 60 | 16.1 |\n 3652 | 2024-03-16 17:26:40 | MASTER-Amur | (16h 08m 58.53s , +25d 47m 30.0s) | C | 180 | 18.4 |\n 3668 | 2024-03-16 17:27:56 | MASTER-Tunka | (12h 27m 30.73s , +29d 15m 08.5s) | C | 60 | 16.1 |\n 3747 | 2024-03-16 17:29:15 | MASTER-Tunka | (12h 40m 15.86s , +27d 21m 30.7s) | C | 60 | 16.1 |\n 3852 | 2024-03-16 17:30:00 | MASTER-Amur | (16h 00m 02.66s , +25d 47m 54.9s) | C | 180 | 18.5 |\n 3827 | 2024-03-16 17:30:34 | MASTER-Tunka | (12h 27m 37.15s , +29d 15m 19.6s) | C | 60 | 16.0 |\n 3985 | 2024-03-16 17:33:13 | MASTER-Tunka | (12h 35m 36.28s , +25d 27m 47.7s) | C | 60 | 16.1 |\n 4051 | 2024-03-16 17:33:19 | MASTER-Amur | (16h 08m 56.69s , +25d 46m 55.3s) | C | 180 | 18.4 |\n 4143 | 2024-03-16 17:35:51 | MASTER-Tunka | (12h 35m 39.40s , +25d 27m 59.9s) | C | 60 | 17.0 |\n 4251 | 2024-03-16 17:36:39 | MASTER-Amur | (16h 33m 47.86s , +25d 49m 06.8s) | C | 180 | 18.6 |\n 4302 | 2024-03-16 17:38:30 | MASTER-Tunka | (12h 52m 34.84s , +25d 26m 14.2s) | C | 60 | 16.0 |\n 4451 | 2024-03-16 17:39:59 | MASTER-Amur | (16h 42m 41.70s , +25d 50m 30.7s) | C | 180 | 18.6 |\n 4461 | 2024-03-16 17:41:09 | MASTER-Tunka | (12h 52m 34.35s , +25d 25m 35.1s) | C | 60 | 15.5 |\n 4540 | 2024-03-16 17:42:28 | MASTER-Tunka | (13h 01m 26.43s , +25d 26m 43.1s) | C | 60 | 16.7 |\n 4651 | 2024-03-16 17:43:18 | MASTER-Amur | (16h 33m 53.58s , +25d 48m 39.1s) | C | 180 | 18.5 |\n 4699 | 2024-03-16 17:45:06 | MASTER-Tunka | (13h 01m 23.06s , +25d 26m 04.6s) | C | 60 | 16.3 |\n 4850 | 2024-03-16 17:46:38 | MASTER-Amur | (16h 42m 41.85s , +25d 48m 01.2s) | C | 180 | 18.6 |\n 5175 | 2024-03-16 17:53:03 | MASTER-Tunka | (13h 45m 35.47s , +31d 07m 01.6s) | C | 60 | 16.6 |\n 5311 | 2024-03-16 17:54:18 | MASTER-Amur | (16h 50m 28.47s , +27d 43m 44.1s) | C | 180 | 18.0 |\n 5528 | 2024-03-16 17:57:56 | MASTER-Amur | (16h 59m 31.54s , +27d 42m 45.4s) | C | 180 | 18.3 |\n 5492 | 2024-03-16 17:58:20 | MASTER-Tunka | (14h 03m 19.41s , +32d 58m 40.3s) | C | 60 | 16.5 |\n 5651 | 2024-03-16 18:00:59 | MASTER-Tunka | (14h 03m 19.69s , +32d 59m 53.7s) | C | 60 | 16.1 |\n 5734 | 2024-03-16 18:01:22 | MASTER-Amur | (16h 50m 32.42s , +27d 42m 56.1s) | C | 180 | 18.3 |\n 5730 | 2024-03-16 18:02:18 | MASTER-Tunka | (13h 35m 19.65s , +33d 01m 11.8s) | C | 60 | 16.3 |\n 5934 | 2024-03-16 18:04:42 | MASTER-Amur | (16h 59m 28.57s , +27d 42m 47.6s) | C | 180 | 18.2 |\n 5888 | 2024-03-16 18:04:56 | MASTER-Tunka | (13h 36m 32.91s , +36d 47m 56.1s) | C | 60 | 15.3 |\n 6133 | 2024-03-16 18:08:01 | MASTER-Amur | (16h 52m 07.62s , +23d 54m 15.0s) | C | 180 | 18.4 |\n 6127 | 2024-03-16 18:08:54 | MASTER-Tunka | (13h 46m 39.80s , +36d 47m 55.5s) | C | 60 | 15.7 |\n 6206 | 2024-03-16 18:10:14 | MASTER-Tunka | (13h 55m 41.15s , +36d 47m 59.0s) | C | 60 | 15.3 |\n 6333 | 2024-03-16 18:11:21 | MASTER-Amur | (17h 00m 46.80s , +23d 53m 38.7s) | C | 180 | 18.4 |\n 6285 | 2024-03-16 18:11:33 | MASTER-Tunka | (13h 46m 36.06s , +36d 49m 38.0s) | C | 60 | 15.4 |\n 6365 | 2024-03-16 18:12:52 | MASTER-Tunka | (13h 55m 46.76s , +36d 48m 06.7s) | C | 60 | 14.9 |\n 6533 | 2024-03-16 18:14:41 | MASTER-Amur | (16h 52m 07.65s , +23d 52m 48.4s) | C | 180 | 18.5 |\n 6732 | 2024-03-16 18:18:00 | MASTER-Amur | (17h 00m 50.55s , +23d 55m 00.2s) | C | 180 | 18.3 |\n 6761 | 2024-03-16 18:19:29 | MASTER-Tunka | (14h 22m 41.91s , +34d 53m 01.7s) | C | 60 | 16.5 |\n 6841 | 2024-03-16 18:20:48 | MASTER-Tunka | (14h 12m 48.50s , +29d 11m 33.8s) | C | 60 | 16.6 |\n 6932 | 2024-03-16 18:21:20 | MASTER-Amur | (16h 51m 22.88s , +29d 35m 46.2s) | C | 180 | 18.4 |\n 6920 | 2024-03-16 18:22:08 | MASTER-Tunka | (14h 22m 41.39s , +34d 52m 07.9s) | C | 60 | 16.5 |\n 7000 | 2024-03-16 18:23:27 | MASTER-Tunka | (14h 12m 48.69s , +29d 10m 47.5s) | C | 60 | 16.6 |\n 7132 | 2024-03-16 18:24:40 | MASTER-Amur | (17h 00m 30.22s , +29d 35m 24.6s) | C | 180 | 18.4 |\n 7079 | 2024-03-16 18:24:47 | MASTER-Tunka | (14h 21m 58.63s , +29d 11m 46.1s) | C | 60 | 16.4 |\n 7332 | 2024-03-16 18:27:59 | MASTER-Amur | (16h 51m 16.18s , +29d 35m 29.9s) | C | 180 | 18.3 |\n 7396 | 2024-03-16 18:30:04 | MASTER-Tunka | (14h 06m 24.95s , +27d 18m 22.4s) | C | 60 | 16.4 |\n 7531 | 2024-03-16 18:31:19 | MASTER-Amur | (17h 00m 35.26s , +29d 34m 56.2s) | C | 180 | 18.3 |\n 7635 | 2024-03-16 18:34:03 | MASTER-Tunka | (14h 00m 13.67s , +25d 24m 15.8s) | C | 60 | 16.4 |\n 7731 | 2024-03-16 18:34:38 | MASTER-Amur | (16h 56m 39.82s , +33d 21m 28.6s) | C | 180 | 18.3 |\n 7714 | 2024-03-16 18:35:22 | MASTER-Tunka | (14h 09m 12.17s , +25d 25m 14.3s) | C | 60 | 16.3 |\n 7794 | 2024-03-16 18:36:42 | MASTER-Tunka | (13h 43m 13.42s , +25d 27m 02.4s) | C | 60 | 15.1 |\n 7930 | 2024-03-16 18:37:58 | MASTER-Amur | (17h 06m 12.67s , +33d 23m 14.4s) | C | 180 | 18.3 |\n 8031 | 2024-03-16 18:40:39 | MASTER-Tunka | (13h 52m 15.09s , +25d 24m 47.7s) | C | 60 | 16.9 |\n 8130 | 2024-03-16 18:41:18 | MASTER-Amur | (16h 56m 38.14s , +33d 21m 06.2s) | C | 180 | 18.3 |\n 8111 | 2024-03-16 18:41:58 | MASTER-Tunka | (13h 47m 16.40s , +23d 30m 37.8s) | C | 60 | 15.6 |\n 8330 | 2024-03-16 18:44:37 | MASTER-Amur | (17h 06m 15.61s , +33d 23m 01.8s) | C | 180 | 18.3 |\n 8348 | 2024-03-16 18:45:56 | MASTER-Tunka | (13h 56m 01.30s , +23d 32m 42.4s) | C | 60 | 16.6 |\n 8428 | 2024-03-16 18:47:16 | MASTER-Tunka | (14h 03m 53.26s , +23d 30m 15.6s) | C | 60 | 16.7 |\n 8587 | 2024-03-16 18:49:54 | MASTER-Tunka | (14h 03m 57.13s , +23d 32m 20.0s) | C | 60 | 16.7 |\n 8794 | 2024-03-16 18:52:22 | MASTER-Amur | (17h 11m 10.52s , +31d 28m 56.6s) | C | 180 | 18.2 |\n 8745 | 2024-03-16 18:52:33 | MASTER-Tunka | (14h 17m 03.20s , +25d 24m 13.7s) | C | 60 | 16.3 |\n 8825 | 2024-03-16 18:53:52 | MASTER-Tunka | (14h 12m 39.91s , +23d 32m 00.9s) | C | 60 | 16.5 |\n 8904 | 2024-03-16 18:55:12 | MASTER-Tunka | (14h 17m 11.35s , +25d 24m 49.6s) | C | 60 | 16.5 |\n 8994 | 2024-03-16 18:55:41 | MASTER-Amur | (17h 20m 41.84s , +31d 28m 21.1s) | C | 180 | 18.4 |\n 9062 | 2024-03-16 18:57:50 | MASTER-Tunka | (14h 20m 36.85s , +23d 31m 16.3s) | C | 60 | 16.5 |\n 9194 | 2024-03-16 18:59:01 | MASTER-Amur | (17h 11m 10.87s , +31d 26m 23.8s) | C | 180 | 18.4 |\n 9221 | 2024-03-16 19:00:28 | MASTER-Tunka | (14h 20m 37.51s , +23d 31m 31.2s) | C | 60 | 15.7 |\n 9300 | 2024-03-16 19:01:48 | MASTER-Tunka | (14h 29m 20.02s , +23d 29m 46.7s) | C | 60 | 14.9 |\n 9396 | 2024-03-16 19:02:23 | MASTER-Amur | (17h 20m 39.88s , +31d 27m 04.5s) | C | 180 | 18.4 |\n 9379 | 2024-03-16 19:03:07 | MASTER-Tunka | (14h 14m 32.79s , +27d 19m 24.2s) | C | 60 | 14.9 |\n 9595 | 2024-03-16 19:05:43 | MASTER-Amur | (17h 08m 51.90s , +29d 32m 08.5s) | C | 180 | 18.4 |\n 9538 | 2024-03-16 19:05:46 | MASTER-Tunka | (14h 14m 30.63s , +27d 18m 14.1s) | C | 60 | 15.3 |\n 9697 | 2024-03-16 19:08:24 | MASTER-Tunka | (14h 30m 16.50s , +29d 13m 35.6s) | C | 60 | 16.9 |\n 9795 | 2024-03-16 19:09:03 | MASTER-Amur | (17h 18m 06.28s , +29d 34m 06.9s) | C | 180 | 18.3 |\n 9855 | 2024-03-16 19:11:03 | MASTER-Tunka | (14h 30m 10.00s , +29d 13m 44.7s) | C | 60 | 15.8 |\n 9934 | 2024-03-16 19:12:22 | MASTER-Tunka | (14h 39m 29.05s , +29d 11m 46.1s) | C | 60 | 16.7 |\n 10029 | 2024-03-16 19:12:57 | MASTER-Amur | (17h 08m 49.88s , +29d 32m 23.9s) | C | 180 | 18.3 |\n 10014 | 2024-03-16 19:13:41 | MASTER-Tunka | (14h 37m 18.53s , +23d 29m 41.2s) | C | 60 | 14.5 |\n 10093 | 2024-03-16 19:15:01 | MASTER-Tunka | (14h 39m 26.80s , +29d 12m 39.3s) | C | 60 | 15.5 |\n 10229 | 2024-03-16 19:16:16 | MASTER-Amur | (17h 18m 01.75s , +29d 33m 48.2s) | C | 180 | 18.3 |\n 10172 | 2024-03-16 19:16:20 | MASTER-Tunka | (14h 37m 14.73s , +23d 29m 04.0s) | C | 60 | 15.4 |\n 10428 | 2024-03-16 19:19:36 | MASTER-Amur | (16h 50m 43.31s , +25d 41m 57.8s) | C | 180 | 18.7 |\n 10411 | 2024-03-16 19:20:18 | MASTER-Tunka | (14h 46m 04.69s , +23d 29m 31.5s) | C | 60 | 14.8 |\n 10490 | 2024-03-16 19:21:38 | MASTER-Tunka | (14h 50m 53.99s , +25d 22m 46.8s) | C | 60 | 16.5 |\n 10627 | 2024-03-16 19:22:55 | MASTER-Amur | (16h 59m 42.99s , +25d 42m 44.9s) | C | 180 | 18.4 |\n 10569 | 2024-03-16 19:22:57 | MASTER-Tunka | (14h 59m 55.58s , +25d 22m 15.3s) | C | 60 | 16.6 |\n 10648 | 2024-03-16 19:24:16 | MASTER-Tunka | (15h 22m 48.97s , +29d 09m 08.9s) | C | 60 | 16.8 |\n 10827 | 2024-03-16 19:26:15 | MASTER-Amur | (16h 50m 47.90s , +25d 43m 23.5s) | C | 180 | 18.7 |\n 10966 | 2024-03-16 19:29:34 | MASTER-Tunka | (15h 07m 49.29s , +25d 21m 27.7s) | C | 60 | 15.6 |\n 11027 | 2024-03-16 19:29:35 | MASTER-Amur | (16h 59m 40.53s , +25d 42m 00.2s) | C | 180 | 18.5 |\n 11045 | 2024-03-16 19:30:53 | MASTER-Tunka | (15h 32m 04.19s , +29d 08m 13.2s) | C | 60 | 16.6 |\n 11226 | 2024-03-16 19:32:54 | MASTER-Amur | (16h 53m 22.05s , +31d 23m 55.4s) | C | 180 | 18.4 |\n 11283 | 2024-03-16 19:34:50 | MASTER-Tunka | (15h 23m 15.61s , +27d 16m 01.6s) | C | 60 | 16.2 |\n 11426 | 2024-03-16 19:36:14 | MASTER-Amur | (17h 02m 45.67s , +31d 25m 20.9s) | C | 180 | 18.5 |\n 11441 | 2024-03-16 19:37:29 | MASTER-Tunka | (15h 23m 20.57s , +27d 16m 08.7s) | C | 60 | 16.1 |\n 11629 | 2024-03-16 19:39:36 | MASTER-Amur | (16h 53m 28.51s , +31d 23m 30.3s) | C | 180 | 18.4 |\n 11679 | 2024-03-16 19:41:27 | MASTER-Tunka | (15h 32m 22.34s , +27d 14m 56.1s) | C | 60 | 17.0 |\n 11828 | 2024-03-16 19:42:56 | MASTER-Amur | (17h 02m 45.12s , +31d 22m 54.1s) | C | 180 | 18.5 |\n 12265 | 2024-03-16 19:50:13 | MASTER-Amur | (16h 54m 54.34s , +38d 58m 36.7s) | C | 180 | 18.8 |\n 12247 | 2024-03-16 19:50:55 | MASTER-Tunka | (14h 53m 55.90s , +23d 31m 43.7s) | C | 60 | 15.8 |\n 12326 | 2024-03-16 19:52:14 | MASTER-Tunka | (15h 33m 39.84s , +25d 22m 03.7s) | C | 60 | 16.7 |\n 12405 | 2024-03-16 19:53:33 | MASTER-Tunka | (14h 53m 50.84s , +23d 31m 59.7s) | C | 60 | 16.4 |\n 12485 | 2024-03-16 19:54:52 | MASTER-Tunka | (15h 02m 43.89s , +23d 30m 25.0s) | C | 60 | 16.1 |\n 12564 | 2024-03-16 19:56:11 | MASTER-Tunka | (15h 40m 22.65s , +29d 08m 53.1s) | C | 60 | 16.6 |\n 12643 | 2024-03-16 19:57:31 | MASTER-Tunka | (15h 02m 39.12s , +23d 31m 13.1s) | C | 60 | 15.6 |\n 12703 | 2024-03-16 19:57:31 | MASTER-Amur | (16h 55m 01.38s , +38d 57m 06.3s) | C | 180 | 18.8 |\n 12722 | 2024-03-16 19:58:50 | MASTER-Tunka | (15h 40m 19.63s , +29d 09m 06.4s) | C | 60 | 16.8 |\n 12960 | 2024-03-16 20:02:48 | MASTER-Tunka | (15h 49m 34.74s , +29d 09m 27.9s) | C | 60 | 16.5 |\n 13119 | 2024-03-16 20:05:27 | MASTER-Tunka | (16h 06m 48.59s , +27d 13m 35.1s) | C | 60 | 16.5 |\n 13198 | 2024-03-16 20:06:46 | MASTER-Tunka | (16h 15m 20.85s , +29d 06m 53.8s) | C | 60 | 16.2 |\n 13278 | 2024-03-16 20:08:05 | MASTER-Tunka | (16h 06m 48.72s , +27d 14m 37.8s) | C | 60 | 14.5 |\n 13436 | 2024-03-16 20:10:44 | MASTER-Tunka | (16h 24m 31.50s , +29d 07m 58.6s) | C | 60 | 16.4 |\n 13515 | 2024-03-16 20:12:03 | MASTER-Tunka | (16h 01m 19.73s , +32d 55m 38.4s) | C | 60 | 15.1 |\n 13595 | 2024-03-16 20:13:22 | MASTER-Tunka | (16h 24m 36.81s , +29d 06m 27.3s) | C | 60 | 16.7 |\n 13754 | 2024-03-16 20:16:01 | MASTER-Tunka | (16h 10m 59.70s , +32d 55m 57.5s) | C | 60 | 16.0 |\n 13912 | 2024-03-16 20:18:40 | MASTER-Tunka | (16h 10m 55.30s , +32d 57m 12.4s) | C | 60 | 15.0 |\n 13991 | 2024-03-16 20:19:59 | MASTER-Tunka | (15h 58m 38.95s , +25d 20m 59.8s) | C | 60 | 14.7 |\n 14071 | 2024-03-16 20:21:19 | MASTER-Tunka | (16h 07m 28.91s , +25d 19m 49.8s) | C | 60 | 16.5 |\n 14230 | 2024-03-16 20:23:57 | MASTER-Tunka | (16h 07m 31.32s , +25d 20m 24.8s) | C | 60 | 16.4 |\n 14309 | 2024-03-16 20:25:17 | MASTER-Tunka | (15h 43m 54.44s , +23d 29m 33.4s) | C | 60 | 16.0 |\n 14547 | 2024-03-16 20:29:15 | MASTER-Tunka | (15h 52m 33.37s , +23d 26m 51.6s) | C | 60 | 15.5 |\n 14626 | 2024-03-16 20:30:34 | MASTER-Tunka | (16h 14m 56.15s , +27d 13m 27.0s) | C | 60 | 15.5 |\n 14706 | 2024-03-16 20:31:53 | MASTER-Tunka | (16h 23m 57.52s , +27d 14m 50.8s) | C | 60 | 17.0 |\n 14785 | 2024-03-16 20:33:12 | MASTER-Tunka | (16h 15m 33.55s , +25d 21m 45.4s) | C | 60 | 16.7 |\n 14864 | 2024-03-16 20:34:32 | MASTER-Tunka | (16h 23m 52.65s , +27d 13m 45.3s) | C | 60 | 17.1 |\n 15023 | 2024-03-16 20:37:10 | MASTER-Tunka | (16h 24m 28.19s , +25d 20m 16.1s) | C | 60 | 17.1 |\n 15182 | 2024-03-16 20:39:49 | MASTER-Tunka | (16h 24m 25.64s , +25d 21m 04.4s) | C | 60 | 17.0 |\n 15420 | 2024-03-16 20:43:47 | MASTER-Tunka | (16h 50m 19.64s , +29d 07m 35.9s) | C | 60 | 16.3 |\n 15499 | 2024-03-16 20:45:06 | MASTER-Tunka | (16h 09m 21.44s , +23d 27m 45.0s) | C | 60 | 14.2 |\n 15657 | 2024-03-16 20:47:45 | MASTER-Tunka | (16h 59m 37.26s , +29d 05m 06.4s) | C | 60 | 16.5 |\n 15692 | 2024-03-16 20:48:20 | MASTER-SAAO | (14h 13m 20.24s , -27d 25m 16.8s) | C | 60 | 18.7 |\n 15752 | 2024-03-16 20:48:20 | MASTER-SAAO | (14h 13m 20.24s , -27d 25m 16.8s) | C | 180 | 19.5 | Coadd\n 15692 | 2024-03-16 20:48:20 | MASTER-SAAO | (14h 11m 18.64s , -27d 12m 21.6s) | C | 60 | 19.0 |\n 15752 | 2024-03-16 20:48:20 | MASTER-SAAO | (14h 11m 18.64s , -27d 12m 21.6s) | C | 180 | 19.7 | Coadd\n 15737 | 2024-03-16 20:49:04 | MASTER-Tunka | (16h 32m 26.16s , +25d 19m 12.7s) | C | 60 | 16.5 |\n 15771 | 2024-03-16 20:49:39 | MASTER-SAAO | (14h 13m 26.71s , -27d 24m 59.1s) | C | 60 | 18.9 |\n 15771 | 2024-03-16 20:49:39 | MASTER-SAAO | (14h 11m 25.04s , -27d 12m 04.6s) | C | 60 | 19.0 |\n 15816 | 2024-03-16 20:50:24 | MASTER-Tunka | (16h 59m 37.10s , +29d 06m 26.8s) | C | 60 | 14.4 |\n 15851 | 2024-03-16 20:50:59 | MASTER-SAAO | (14h 13m 23.12s , -27d 23m 36.7s) | C | 60 | 18.7 |\n 15851 | 2024-03-16 20:50:59 | MASTER-SAAO | (14h 11m 21.49s , -27d 10m 42.5s) | C | 60 | 19.0 |\n 15895 | 2024-03-16 20:51:43 | MASTER-Tunka | (16h 32m 21.46s , +25d 19m 51.5s) | C | 60 | 14.7 |\n 15931 | 2024-03-16 20:52:18 | MASTER-SAAO | (13h 48m 15.82s , -17d 54m 48.5s) | C | 60 | 17.8 |\n 15991 | 2024-03-16 20:52:18 | MASTER-SAAO | (13h 48m 15.82s , -17d 54m 48.5s) | C | 180 | 18.8 | Coadd\n 15931 | 2024-03-16 20:52:18 | MASTER-SAAO | (13h 46m 22.02s , -17d 41m 53.0s) | C | 60 | 17.9 |\n 15991 | 2024-03-16 20:52:18 | MASTER-SAAO | (13h 46m 22.02s , -17d 41m 53.0s) | C | 180 | 18.9 | Coadd\n 16010 | 2024-03-16 20:53:38 | MASTER-SAAO | (13h 48m 17.55s , -17d 53m 11.2s) | C | 60 | 17.7 |\n 16010 | 2024-03-16 20:53:38 | MASTER-SAAO | (13h 46m 23.75s , -17d 40m 16.4s) | C | 60 | 17.8 |\n 16054 | 2024-03-16 20:54:22 | MASTER-Tunka | (16h 49m 14.86s , +27d 11m 39.8s) | C | 60 | 15.3 |\n 16090 | 2024-03-16 20:54:58 | MASTER-SAAO | (13h 48m 12.09s , -17d 53m 57.2s) | C | 60 | 18.6 |\n 16090 | 2024-03-16 20:54:58 | MASTER-SAAO | (13h 46m 18.28s , -17d 41m 02.0s) | C | 60 | 18.8 |\n 16134 | 2024-03-16 20:55:41 | MASTER-Tunka | (16h 41m 22.12s , +25d 19m 03.1s) | C | 60 | 16.9 |\n 16213 | 2024-03-16 20:57:01 | MASTER-Tunka | (16h 49m 16.58s , +27d 13m 43.8s) | C | 60 | 16.0 |\n 16292 | 2024-03-16 20:58:20 | MASTER-Tunka | (16h 58m 19.97s , +27d 11m 10.6s) | C | 60 | 15.3 |\n 16372 | 2024-03-16 20:59:39 | MASTER-Tunka | (16h 56m 02.13s , +32d 54m 33.7s) | C | 60 | 15.0 |\n 16644 | 2024-03-16 21:03:12 | MASTER-SAAO | (14h 03m 22.06s , -23d 37m 01.3s) | C | 180 | 19.6 |\n 16644 | 2024-03-16 21:03:12 | MASTER-SAAO | (14h 01m 23.62s , -23d 24m 07.5s) | C | 180 | 19.6 |\n 16609 | 2024-03-16 21:03:37 | MASTER-Tunka | (17h 05m 39.83s , +32d 52m 57.4s) | C | 60 | 14.9 |\n 16688 | 2024-03-16 21:04:56 | MASTER-Tunka | (17h 10m 29.19s , +31d 01m 02.7s) | C | 60 | 16.7 |\n 16768 | 2024-03-16 21:06:15 | MASTER-Tunka | (17h 05m 42.85s , +32d 53m 56.9s) | C | 60 | 16.7 |\n 16844 | 2024-03-16 21:06:31 | MASTER-SAAO | (13h 24m 12.09s , -16d 00m 12.6s) | C | 180 | 19.7 |\n 16844 | 2024-03-16 21:06:31 | MASTER-SAAO | (13h 22m 18.43s , -15d 47m 17.7s) | C | 180 | 19.7 |\n 16847 | 2024-03-16 21:07:35 | MASTER-Tunka | (17h 10m 31.39s , +31d 00m 30.6s) | C | 60 | 15.4 |\n 16926 | 2024-03-16 21:08:54 | MASTER-Tunka | (17h 19m 50.55s , +30d 59m 27.0s) | C | 60 | 16.7 |\n 16984 | 2024-03-16 21:09:51 | MASTER-SAAO | (14h 28m 45.29s , -29d 17m 33.8s) | C | 60 | 18.8 |\n 17044 | 2024-03-16 21:09:51 | MASTER-SAAO | (14h 28m 45.29s , -29d 17m 33.9s) | C | 180 | 19.6 | Coadd\n 16984 | 2024-03-16 21:09:51 | MASTER-SAAO | (14h 26m 40.83s , -29d 04m 41.1s) | C | 60 | 19.0 |\n 17044 | 2024-03-16 21:09:51 | MASTER-SAAO | (14h 26m 40.83s , -29d 04m 41.1s) | C | 180 | 19.8 | Coadd\n 17005 | 2024-03-16 21:10:13 | MASTER-Tunka | (17h 07m 55.98s , +29d 06m 26.6s) | C | 60 | 16.5 |\n 17063 | 2024-03-16 21:11:11 | MASTER-SAAO | (14h 28m 45.20s , -29d 19m 01.8s) | C | 60 | 18.8 |\n 17063 | 2024-03-16 21:11:11 | MASTER-SAAO | (14h 26m 40.68s , -29d 06m 09.0s) | C | 60 | 19.1 |\n 17085 | 2024-03-16 21:11:33 | MASTER-Tunka | (17h 19m 49.75s , +30d 58m 05.1s) | C | 60 | 15.0 |\n 17143 | 2024-03-16 21:12:31 | MASTER-SAAO | (14h 28m 47.30s , -29d 17m 38.0s) | C | 60 | 18.8 |\n 17143 | 2024-03-16 21:12:31 | MASTER-SAAO | (14h 26m 42.76s , -29d 04m 45.3s) | C | 60 | 19.1 |\n 17164 | 2024-03-16 21:12:52 | MASTER-Tunka | (17h 07m 54.57s , +29d 05m 34.0s) | C | 60 | 14.7 |\n 17222 | 2024-03-16 21:13:50 | MASTER-SAAO | (14h 38m 23.92s , -10d 18m 44.7s) | C | 60 | 18.9 |\n 17282 | 2024-03-16 21:13:50 | MASTER-SAAO | (14h 38m 23.92s , -10d 18m 44.8s) | C | 180 | 19.5 | Coadd\n 17222 | 2024-03-16 21:13:50 | MASTER-SAAO | (14h 36m 34.39s , -10d 05m 46.3s) | C | 60 | 19.1 |\n 17282 | 2024-03-16 21:13:50 | MASTER-SAAO | (14h 36m 34.39s , -10d 05m 46.3s) | C | 180 | 19.7 | Coadd\n 17244 | 2024-03-16 21:14:11 | MASTER-Tunka | (17h 17m 05.16s , +29d 05m 57.8s) | C | 60 | 14.5 |\n 17302 | 2024-03-16 21:15:10 | MASTER-SAAO | (14h 38m 23.88s , -10d 17m 44.4s) | C | 60 | 18.8 |\n 17302 | 2024-03-16 21:15:10 | MASTER-SAAO | (14h 36m 34.31s , -10d 04m 46.0s) | C | 60 | 19.1 |\n 17323 | 2024-03-16 21:15:31 | MASTER-Tunka | (16h 49m 21.48s , +25d 20m 26.4s) | C | 60 | 14.5 |\n 17382 | 2024-03-16 21:16:30 | MASTER-SAAO | (14h 38m 31.03s , -10d 18m 44.5s) | C | 60 | 18.9 |\n 17382 | 2024-03-16 21:16:30 | MASTER-SAAO | (14h 36m 41.42s , -10d 05m 45.8s) | C | 60 | 19.0 |\n 17402 | 2024-03-16 21:16:50 | MASTER-Tunka | (17h 17m 02.08s , +29d 05m 31.4s) | C | 60 | 15.2 |\n 17522 | 2024-03-16 21:17:49 | MASTER-SAAO | (14h 03m 20.65s , -23d 37m 03.8s) | C | 180 | 19.6 |\n 17522 | 2024-03-16 21:17:49 | MASTER-SAAO | (14h 01m 21.51s , -23d 24m 10.5s) | C | 180 | 19.7 |\n 17481 | 2024-03-16 21:18:09 | MASTER-Tunka | (16h 49m 17.34s , +25d 21m 15.3s) | C | 60 | 16.9 |\n 17561 | 2024-03-16 21:19:28 | MASTER-Tunka | (16h 58m 16.41s , +25d 19m 34.7s) | C | 60 | 16.8 |\n 17721 | 2024-03-16 21:21:09 | MASTER-SAAO | (13h 24m 11.57s , -16d 00m 28.6s) | C | 180 | 19.6 |\n 17721 | 2024-03-16 21:21:09 | MASTER-SAAO | (13h 22m 17.36s , -15d 47m 33.1s) | C | 180 | 19.7 |\n 17719 | 2024-03-16 21:22:07 | MASTER-Tunka | (16h 58m 12.76s , +25d 19m 51.7s) | C | 60 | 12.7 |\n 17921 | 2024-03-16 21:24:29 | MASTER-SAAO | (14h 29m 56.17s , -19d 47m 57.8s) | C | 180 | 19.5 |\n 17921 | 2024-03-16 21:24:29 | MASTER-SAAO | (14h 28m 00.56s , -19d 35m 01.7s) | C | 180 | 19.6 |\n 17878 | 2024-03-16 21:24:46 | MASTER-Tunka | (17h 02m 03.33s , +31d 01m 55.3s) | C | 60 | 15.1 |\n 18036 | 2024-03-16 21:27:24 | MASTER-Tunka | (17h 02m 01.85s , +31d 01m 45.0s) | C | 60 | 16.1 |\n 18121 | 2024-03-16 21:27:48 | MASTER-SAAO | (14h 18m 20.20s , -08d 25m 24.5s) | C | 180 | 19.5 |\n 18121 | 2024-03-16 21:27:48 | MASTER-SAAO | (14h 16m 30.42s , -08d 12m 25.7s) | C | 180 | 19.5 |\n 18116 | 2024-03-16 21:28:43 | MASTER-Tunka | (16h 34m 39.57s , +31d 02m 38.4s) | C | 60 | 15.0 |\n 18234 | 2024-03-16 21:30:42 | MASTER-Tunka | (16h 44m 06.44s , +31d 03m 27.4s) | C | 60 | 14.3 |\n 18260 | 2024-03-16 21:31:08 | MASTER-SAAO | (14h 13m 24.62s , -27d 23m 35.5s) | C | 60 | 18.7 |\n 18320 | 2024-03-16 21:31:08 | MASTER-SAAO | (14h 13m 24.62s , -27d 23m 35.5s) | C | 180 | 19.6 | Coadd\n 18260 | 2024-03-16 21:31:08 | MASTER-SAAO | (14h 11m 21.31s , -27d 10m 41.9s) | C | 60 | 18.8 |\n 18313 | 2024-03-16 21:32:01 | MASTER-Tunka | (16h 50m 29.73s , +23d 26m 47.8s) | C | 60 | 15.5 |\n 18340 | 2024-03-16 21:32:27 | MASTER-SAAO | (14h 13m 17.69s , -27d 24m 13.5s) | C | 60 | 18.8 |\n 18340 | 2024-03-16 21:32:27 | MASTER-SAAO | (14h 11m 14.34s , -27d 11m 19.8s) | C | 60 | 18.9 |\n 18413 | 2024-03-16 21:33:40 | MASTER-Tunka | (16h 44m 03.39s , +31d 03m 27.7s) | C | 60 | 16.2 |\n 18419 | 2024-03-16 21:33:47 | MASTER-SAAO | (14h 13m 16.53s , -27d 23m 13.9s) | C | 60 | 18.9 |\n 18419 | 2024-03-16 21:33:47 | MASTER-SAAO | (14h 11m 13.13s , -27d 10m 20.2s) | C | 60 | 19.0 |\n 18492 | 2024-03-16 21:35:00 | MASTER-Tunka | (16h 50m 23.60s , +23d 27m 44.8s) | C | 60 | 16.1 |\n 18499 | 2024-03-16 21:35:07 | MASTER-SAAO | (13h 48m 17.53s , -17d 53m 54.7s) | C | 60 | 18.8 |\n 18559 | 2024-03-16 21:35:07 | MASTER-SAAO | (13h 48m 17.53s , -17d 53m 54.7s) | C | 180 | 19.6 | Coadd\n 18499 | 2024-03-16 21:35:07 | MASTER-SAAO | (13h 46m 22.16s , -17d 40m 58.6s) | C | 60 | 18.8 |\n 18571 | 2024-03-16 21:36:19 | MASTER-Tunka | (16h 59m 16.00s , +23d 26m 06.7s) | C | 60 | 16.6 |\n 18579 | 2024-03-16 21:36:27 | MASTER-SAAO | (13h 48m 11.32s , -17d 54m 54.2s) | C | 60 | 18.9 |\n 18579 | 2024-03-16 21:36:27 | MASTER-SAAO | (13h 46m 15.91s , -17d 41m 58.0s) | C | 60 | 18.9 |\n 18659 | 2024-03-16 21:37:46 | MASTER-SAAO | (13h 48m 17.35s , -17d 54m 25.9s) | C | 60 | 18.9 |\n 18659 | 2024-03-16 21:37:46 | MASTER-SAAO | (13h 46m 21.94s , -17d 41m 30.0s) | C | 60 | 19.0 |\n 18730 | 2024-03-16 21:38:57 | MASTER-Tunka | (16h 59m 13.01s , +23d 26m 47.1s) | C | 60 | 16.2 |\n 18738 | 2024-03-16 21:39:06 | MASTER-SAAO | (14h 53m 53.47s , -10d 18m 32.6s) | C | 60 | 18.7 |\n 18798 | 2024-03-16 21:39:06 | MASTER-SAAO | (14h 53m 53.47s , -10d 18m 32.6s) | C | 180 | 19.4 | Coadd\n 18738 | 2024-03-16 21:39:06 | MASTER-SAAO | (14h 52m 03.44s , -10d 05m 32.4s) | C | 60 | 18.7 |\n 18818 | 2024-03-16 21:40:26 | MASTER-SAAO | (14h 53m 53.41s , -10d 19m 54.7s) | C | 60 | 18.8 |\n 18818 | 2024-03-16 21:40:26 | MASTER-SAAO | (14h 52m 03.34s , -10d 06m 54.2s) | C | 60 | 18.8 |\n 18898 | 2024-03-16 21:41:45 | MASTER-SAAO | (14h 53m 56.98s , -10d 18m 10.6s) | C | 60 | 18.7 |\n 18898 | 2024-03-16 21:41:45 | MASTER-SAAO | (14h 52m 06.87s , -10d 05m 10.5s) | C | 60 | 18.9 |\n 19037 | 2024-03-16 21:43:05 | MASTER-SAAO | (14h 29m 51.16s , -19d 48m 38.7s) | C | 180 | 19.5 |\n 19037 | 2024-03-16 21:43:05 | MASTER-SAAO | (14h 27m 55.00s , -19d 35m 41.8s) | C | 180 | 19.5 |\n 19237 | 2024-03-16 21:46:25 | MASTER-SAAO | (14h 18m 15.58s , -08d 23m 30.8s) | C | 180 | 19.3 |\n 19237 | 2024-03-16 21:46:25 | MASTER-SAAO | (14h 16m 25.25s , -08d 10m 31.4s) | C | 180 | 19.4 |\n 19230 | 2024-03-16 21:47:18 | MASTER-Tunka | (16h 27m 28.08s , +24d 47m 46.1s) | C | 60 | 16.0 |\n 19437 | 2024-03-16 21:49:45 | MASTER-SAAO | (14h 52m 09.05s , -17d 55m 07.6s) | C | 180 | 19.4 |\n 19437 | 2024-03-16 21:49:45 | MASTER-SAAO | (14h 50m 14.43s , -17d 42m 09.3s) | C | 180 | 19.2 |\n 19389 | 2024-03-16 21:49:56 | MASTER-Tunka | (16h 27m 28.95s , +24d 48m 54.4s) | C | 60 | 15.8 |\n 19562 | 2024-03-16 21:52:50 | MASTER-Tunka | (16h 04m 51.87s , +22d 57m 09.5s) | C | 60 | 15.8 |\n 19577 | 2024-03-16 21:53:05 | MASTER-SAAO | (14h 28m 39.54s , -29d 19m 30.5s) | C | 60 | 18.7 |\n 19577 | 2024-03-16 21:53:05 | MASTER-SAAO | (14h 26m 33.43s , -29d 06m 36.6s) | C | 60 | 18.8 |\n 19657 | 2024-03-16 21:54:25 | MASTER-SAAO | (14h 26m 39.81s , -29d 06m 11.5s) | C | 60 | 18.7 |\n 19737 | 2024-03-16 21:55:44 | MASTER-SAAO | (14h 28m 42.25s , -29d 17m 51.4s) | C | 60 | 18.5 |\n 19737 | 2024-03-16 21:55:44 | MASTER-SAAO | (14h 26m 36.12s , -29d 04m 57.4s) | C | 60 | 18.6 |\n 19816 | 2024-03-16 21:57:04 | MASTER-SAAO | (14h 38m 25.66s , -10d 19m 43.0s) | C | 60 | 18.7 |\n 19816 | 2024-03-16 21:57:04 | MASTER-SAAO | (14h 36m 34.68s , -10d 06m 44.0s) | C | 60 | 18.7 |\n 19880 | 2024-03-16 21:58:07 | MASTER-Tunka | (15h 59m 20.50s , +30d 32m 27.6s) | C | 60 | 15.1 |\n 19896 | 2024-03-16 21:58:24 | MASTER-SAAO | (14h 38m 28.49s , -10d 18m 10.8s) | C | 60 | 18.6 |\n 19896 | 2024-03-16 21:58:24 | MASTER-SAAO | (14h 36m 37.45s , -10d 05m 11.8s) | C | 60 | 18.5 |\n 19959 | 2024-03-16 21:59:27 | MASTER-Tunka | (16h 08m 35.71s , +30d 33m 29.0s) | C | 60 | 14.5 |\n 19976 | 2024-03-16 21:59:44 | MASTER-SAAO | (14h 38m 23.07s , -10d 18m 56.4s) | C | 60 | 18.6 |\n 19976 | 2024-03-16 21:59:44 | MASTER-SAAO | (14h 36m 32.02s , -10d 05m 57.2s) | C | 60 | 18.6 |\n 20039 | 2024-03-16 22:00:46 | MASTER-Tunka | (16h 00m 29.27s , +32d 28m 00.6s) | C | 60 | 15.2 |\n 20122 | 2024-03-16 22:01:09 | MASTER-SAAO | (14h 52m 02.76s , -17d 54m 10.1s) | C | 180 | 19.4 |\n 20122 | 2024-03-16 22:01:09 | MASTER-SAAO | (14h 50m 07.81s , -17d 41m 12.5s) | C | 180 | 19.4 |\n 20118 | 2024-03-16 22:02:06 | MASTER-Tunka | (16h 08m 37.59s , +30d 32m 57.8s) | C | 60 | 14.0 |\n 20197 | 2024-03-16 22:03:25 | MASTER-Tunka | (16h 00m 29.03s , +32d 26m 05.6s) | C | 60 | 15.6 |\n 20321 | 2024-03-16 22:04:29 | MASTER-SAAO | (14h 57m 15.24s , -21d 43m 15.8s) | C | 180 | 19.3 |\n 20321 | 2024-03-16 22:04:29 | MASTER-SAAO | (14h 55m 17.33s , -21d 30m 18.8s) | C | 180 | 19.2 |\n 20277 | 2024-03-16 22:04:44 | MASTER-Tunka | (16h 10m 00.47s , +32d 26m 08.1s) | C | 60 | 13.9 |\n 20435 | 2024-03-16 22:07:23 | MASTER-Tunka | (16h 10m 00.93s , +32d 27m 42.2s) | C | 60 | 13.7 |\n 20521 | 2024-03-16 22:07:49 | MASTER-SAAO | (14h 11m 12.58s , -29d 19m 06.2s) | C | 180 | 19.6 |\n 20521 | 2024-03-16 22:07:49 | MASTER-SAAO | (14h 09m 05.62s , -29d 06m 13.1s) | C | 180 | 19.5 |\n 20514 | 2024-03-16 22:08:42 | MASTER-Tunka | (16h 06m 23.43s , +36d 15m 03.7s) | C | 60 | 15.4 |\n 20593 | 2024-03-16 22:10:01 | MASTER-Tunka | (16h 16m 13.94s , +36d 15m 31.4s) | C | 60 | 14.9 |\n 20721 | 2024-03-16 22:11:08 | MASTER-SAAO | (14h 57m 15.61s , -21d 43m 51.7s) | C | 180 | 19.4 |\n 20721 | 2024-03-16 22:11:08 | MASTER-SAAO | (14h 55m 17.44s , -21d 30m 54.7s) | C | 180 | 19.4 |\n 20673 | 2024-03-16 22:11:20 | MASTER-Tunka | (16h 11m 13.22s , +38d 08m 00.4s) | C | 60 | 14.8 |\n 20832 | 2024-03-16 22:13:59 | MASTER-Tunka | (16h 11m 14.87s , +38d 10m 15.0s) | C | 60 | 13.5 |\n 20920 | 2024-03-16 22:14:28 | MASTER-SAAO | (14h 11m 15.75s , -29d 17m 13.4s) | C | 180 | 19.4 |\n 20920 | 2024-03-16 22:14:28 | MASTER-SAAO | (14h 09m 08.67s , -29d 04m 19.8s) | C | 180 | 19.4 |\n 20911 | 2024-03-16 22:15:18 | MASTER-Tunka | (16h 21m 18.40s , +38d 07m 44.1s) | C | 60 | 14.6 |\n 20990 | 2024-03-16 22:16:38 | MASTER-Tunka | (16h 37m 00.87s , +40d 01m 53.4s) | C | 60 | 14.2 |\n 21069 | 2024-03-16 22:17:57 | MASTER-Tunka | (16h 21m 15.95s , +38d 10m 03.0s) | C | 60 | 13.5 |\n 21131 | 2024-03-16 22:17:58 | MASTER-SAAO | (13h 53m 03.61s , -31d 15m 34.2s) | C | 180 | 19.2 |\n 21131 | 2024-03-16 22:17:58 | MASTER-SAAO | (13h 50m 56.23s , -31d 02m 28.4s) | C | 180 | 19.1 |\n 21148 | 2024-03-16 22:19:16 | MASTER-Tunka | (16h 37m 07.41s , +40d 01m 59.9s) | C | 60 | 13.6 |\n 21228 | 2024-03-16 22:20:36 | MASTER-Tunka | (16h 47m 20.89s , +40d 00m 17.5s) | C | 60 | 14.0 |\n 21330 | 2024-03-16 22:21:18 | MASTER-SAAO | (13h 50m 21.69s , -32d 54m 41.3s) | C | 180 | 19.3 |\n 21330 | 2024-03-16 22:21:18 | MASTER-SAAO | (13h 52m 31.66s , -33d 07m 48.4s) | C | 180 | 19.4 |\n 21483 | 2024-03-16 22:24:50 | MASTER-SAAO | (14h 53m 46.82s , -10d 19m 25.9s) | C | 60 | 18.7 |\n 21483 | 2024-03-16 22:24:50 | MASTER-SAAO | (14h 51m 56.30s , -10d 06m 19.9s) | C | 60 | 18.8 |\n 21562 | 2024-03-16 22:26:10 | MASTER-SAAO | (14h 53m 47.65s , -10d 18m 24.1s) | C | 60 | 18.8 |\n 21562 | 2024-03-16 22:26:10 | MASTER-SAAO | (14h 51m 57.07s , -10d 05m 18.4s) | C | 60 | 18.8 |\n 21642 | 2024-03-16 22:27:30 | MASTER-SAAO | (14h 53m 53.46s , -10d 19m 23.1s) | C | 60 | 18.8 |\n 21642 | 2024-03-16 22:27:30 | MASTER-SAAO | (14h 52m 02.83s , -10d 06m 17.4s) | C | 60 | 18.9 |\n 21797 | 2024-03-16 22:29:05 | MASTER-SAAO | (13h 50m 43.92s , -31d 02m 20.7s) | C | 180 | 19.2 |\n 21797 | 2024-03-16 22:29:05 | MASTER-SAAO | (13h 52m 51.97s , -31d 15m 30.8s) | C | 180 | 19.3 |\n 21997 | 2024-03-16 22:32:25 | MASTER-SAAO | (13h 50m 11.73s , -32d 55m 53.1s) | C | 180 | 19.2 |\n 21997 | 2024-03-16 22:32:25 | MASTER-SAAO | (13h 52m 22.44s , -33d 09m 04.2s) | C | 180 | 19.3 |\n 22197 | 2024-03-16 22:35:45 | MASTER-SAAO | (13h 50m 24.45s , -34d 48m 22.5s) | C | 180 | 19.4 |\n 22197 | 2024-03-16 22:35:45 | MASTER-SAAO | (13h 52m 38.04s , -35d 01m 34.6s) | C | 180 | 19.5 |\n 31289 | 2024-03-17 01:07:17 | MASTER-SAAO | (15h 53m 05.79s , +39d 38m 12.2s) | C | 180 | 14.1 |\n 31289 | 2024-03-17 01:07:17 | MASTER-SAAO | (15h 55m 20.49s , +39d 25m 07.2s) | C | 180 | 14.2 |\n 31713 | 2024-03-17 01:14:21 | MASTER-SAAO | (15h 52m 52.74s , +39d 38m 29.7s) | C | 180 | 13.0 |\n 31713 | 2024-03-17 01:14:21 | MASTER-SAAO | (15h 55m 10.90s , +39d 25m 28.2s) | C | 180 | 13.0 |\nFilter C is a clear (unfiltred) band.\n\n\nThe observation and reduction will continue.\nThe message may be cited.\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35934.",
"published": "2024-03-17T02:15:57.139692Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-17T02:15:57.139706Z",
"modified": "2024-03-17T02:15:57.147228Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6234,
"topic": "gcn.circular",
"uuid": "0258fe9f-93d3-47f4-97e6-c7eb424bd689",
"title": "X-ray transient EP240315a: Nanshan/HMT optical upper limit",
"submitter": "Hop gcn.circular",
"authors": "Dong Xu at NAOC/CAS <dxu@nao.cas.cn>",
"data": {
"date": "24/03/17 06:52:41 GMT",
"from": "Dong Xu at NAOC/CAS <dxu@nao.cas.cn>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35935"
},
"title": "GCN CIRCULAR",
"number": "35935",
"subject": "X-ray transient EP240315a: Nanshan/HMT optical upper limit"
},
"message_text": "S.Q. Jiang, Z.P. Zhu, X. Liu, J. An, S.Y. Fu, T.H. Lu, D. Xu (NAOC), X. Gao (Urumqi No.1 Senior High School), J.Z. Liu (XAO) report on behalf of a large collaboration:\n\nWe observed the field of EP240315a detected by Einstein Probe (EP, Zhang et al., GCN 35931) using the HMT-0.5m telescope located at Nanshan, Xinjiang, China. We obtained 30 x 90 s frames without any filter.\n\nNo uncatalogued optical transient is detected within or near the EP/WXT error circle, down to a limiting magnitude of r ~ 20.9 at a median time of 20.44 hr post-trigger, calibrated with the nearby PanSTAR field.\n\nThe previously reported ATLAS optical counterpart candidate, AT2024eju, (Srivastav et al., GCN 35932) is not present in the HMT co-added image, indicating that it has decayed significantly. Our non-detection is consistent with that from LT (Srivastav et al., GCN 35933).\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35935.",
"published": "2024-03-17T06:52:55.610436Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-17T06:52:55.610451Z",
"modified": "2024-03-17T06:52:55.618560Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6650,
"topic": "gcn.circular",
"uuid": "c051aae3-a720-4749-b8db-bb5ccfa2fa8c",
"title": "EP240416a: BOOTES-2/TELMA Optical Upper Limit",
"submitter": "Hop gcn.circular",
"authors": "Dingrong Xiong at Yunnan Observatories of CAS, China <xiongdingrong@ynao.ac.cn>",
"data": {
"date": "24/04/18 09:25:48 GMT",
"from": "Dingrong Xiong at Yunnan Observatories of CAS, China <xiongdingrong@ynao.ac.cn>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/36155"
},
"title": "GCN CIRCULAR",
"number": "36155",
"subject": "EP240416a: BOOTES-2/TELMA Optical Upper Limit"
},
"message_text": "D. R. Xiong, J. M. Bai, J. R. Mao, Y. F. Fan, K. Ye, C. J. Wang, Y. X. Xin, B. L. Lun, J. J. Zhang, X. H. Zhao, L. Xu, K. X. Lu, X. Ding, X. G. Yu, D. Q. Wang, S. S. He, X. L. Zhang, J. G. Wang (Yunnan Observatories/CAS), A. J. Castro-Tirado, E. Fernandez-Garcia, Y. D. Hu (IAA-CSIC) and C. J. Perez del Pulgar (UMA) on behalf of the BOOTES team report:\n\nWe observed the X-ray transient EP 240416a (Cheng et al., GCN 36138), and did not found any optical counterpart within an uncertainty of 3 arcmin in radius compared to the PanSTARRS DR1 image. The upper limits of magnitudes (without being corrected for Galactic extinction) are given as follows.\n\nTmid-T0 (day) | UT (start) | Upper Limit (error) | Exposure Time | Filter\n\n--------------------------------------------------------------------------------------------------------------\n\n0.96 | 24-04-17T01:50:42 | 19.56 (0.2) | 100s*10 | Clear\n\n-------------------------------------------------------------------------------------------------------------\n\nThe Burst Optical Observer and Transient Exploring System (BOOTES) is a world-wide automatic telescope network which aims to repaid follow-up of transient and astrophysical sources in the sky for which the first station was installed in 1998 (Castro-Tirado et al. 1999; Hu et al. 2021). The BOOTES-2/TELMA robotic telescope at IHSM La Mayora (UMA-CSIC) in Algarrobo Costa (Malaga, Spain). We acknowledge the support of these staffs from the BOOTES telescope networks.\n\n=================================================================\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/36155.",
"published": "2024-04-18T09:26:07.182990Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-04-18T09:26:07.183002Z",
"modified": "2024-04-18T09:26:07.190543Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6235,
"topic": "gcn.circular",
"uuid": "9864aaa1-2db8-487c-b693-371b53d449c0",
"title": "X-ray transient EP240315a: VLT/X-shooter spectroscopic redshift of z = 4.859",
"submitter": "Hop gcn.circular",
"authors": "Andrea Saccardi at Observatoire de Paris <andrea.saccardi@obspm.fr>",
"data": {
"date": "24/03/17 06:54:26 GMT",
"from": "Andrea Saccardi at Observatoire de Paris <andrea.saccardi@obspm.fr>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35936"
},
"title": "GCN CIRCULAR",
"number": "35936",
"subject": "X-ray transient EP240315a: VLT/X-shooter spectroscopic redshift of z = 4.859"
},
"message_text": "A. Saccardi (GEPI/Obs. de Paris), A. J. Levan (Radboud Univ. & Warwick Univ.), Z. Zhu (NAOC), B. P. Gompertz (U. Birmingham), S. D. Vergani (GEPI/Obs. de Paris & IAP & INAF/OABr), G. Pugliese (API), D. Xu (NAOC), D. B. Malesani (DAWN/NBI and Radboud Univ.), report on behalf of the Stargate collaboration:\n\nWe observed the field of the ATLAS optical counterpart AT2024eju (Srivastav et al., GCN 35932) of the fast X-ray transient EP240315a reported by the WXT instrument during the commissioning phase of the Einstein Probe mission (Zhang et al, GCN 35931) using the ESO/VLT UT3 (Melipal) equipped with the X-shooter spectrograph. Our spectra cover the wavelength range 3000-21000 AA, and consist of 4 exposures of 1200 s each. Observations started at 01:02:52 UT on Mar 17 2024 (~29 hr after the trigger). We detect a clear continuum across both VIS and NIR arms. From the detection of a Lya absorption at ~7120 AA and multiple absorption features, which we interpret as being due to OI, SiII, NV, CIV and SiIV, we infer a redshift of z = 4.859. We also note the presence of additional absorption features likely due to multiple intervening systems. The high redshift of the transient suggests a highly energetic event and potentially links this Fast X-ray Transient to a GRB-like phenomena.\n\nWe acknowledge the excellent support from the ESO staff in Paranal, in particular Joe Anderson and Matias Jones.\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35936.",
"published": "2024-03-17T06:54:33.720409Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-17T06:54:33.720425Z",
"modified": "2024-03-17T06:54:33.728630Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6236,
"topic": "gcn.circular",
"uuid": "e9a69637-cd35-46bf-9cfc-91d04d9fffca",
"title": "X-ray transient EP240315a: GROND J-band detection",
"submitter": "Hop gcn.circular",
"authors": "Arne Rau at MPE <arau@mpe.mpg.de>",
"data": {
"date": "24/03/17 07:54:44 GMT",
"from": "Arne Rau at MPE <arau@mpe.mpg.de>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35937"
},
"title": "GCN CIRCULAR",
"number": "35937",
"subject": "X-ray transient EP240315a: GROND J-band detection"
},
"message_text": "Arne Rau (MPE):\n\nThe location of the optical transient AT2024eju (Srivastav et al., GCN35932), discovered within the error circle of the fast X-ray transient EP240315a reported by Einstein Probe n (Zhang et al., GCN 35931), was observed with the optical/NIR imager GROND (Greiner et al. 2008) at the MPG 2.2m telescope at the ESO La Silla Observatory on 2024 March 17th 02:50:23 UT (MJD 60386.118).\n\nWith an exposure of 1200s, the source is detected in the J-band at m_vega\u0019.6+/-0.2 (m_AB .5+/-0.2).\n\nWe thank the 2.2m staff member, Paul Eigenthaler, for the rapid execution of the observation.\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35937.",
"published": "2024-03-17T07:54:59.553231Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-17T07:54:59.553248Z",
"modified": "2024-03-17T07:54:59.562382Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6237,
"topic": "gcn.circular",
"uuid": "ba5fc54d-8e95-47ff-b657-1792521eaebc",
"title": "X-ray transient EP240315a: Kinder follow-up observations for AT 2024eju with Lulin observatory",
"submitter": "Hop gcn.circular",
"authors": "Janet Chen at National Central University <janetstars@gmail.com>",
"data": {
"date": "24/03/17 08:26:16 GMT",
"from": "Janet Chen at National Central University <janetstars@gmail.com>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35938"
},
"title": "GCN CIRCULAR",
"number": "35938",
"subject": "X-ray transient EP240315a: Kinder follow-up observations for AT 2024eju with Lulin observatory"
},
"message_text": "T.-W. Chen (NCUIA), S. Yang (HNAS), M.-H. Lee, H.-Y. Hsiao, C.-H. Lai, A. Sankar.K, C.-C. Ngeow, Y.-C. Pan, C.-S. Lin, W.-J. Hou, H.-C. Lin, J.-K. Guo (all NCUIA), S. Srivastav, S. Smartt (both Oxford) and M. Fulton, T. Moore, C. Angus, A. Aamer (all QUB) report:\n\nWe observed the field of AT 2024eju (Srivastav et al., GCN 35932), a possible optical counterpart for the EP240315a (Zhang et al., GCN 35931) found by ATLAS, using the 40cm SLT at Lulin Observatory, Taiwan as part of the Kinder collaboration (Chen et al., AstroNote 2021-92).\n\nThe first SLT epoch of observations started at 16:09 UT on 16 of March 2024 (MJD = 60385.673), 0.83 days after the discovery of the X-ray transient. The r-band images were combined from 6 frames, each with a 300-second exposure time, taken under seeing conditions averaging 2.0\" and at a median airmass of 1.61.\n\nWe used the Kinder pipeline (Yang et al. A&A 646, A22) to measure the PSF photometry on the source location, after subtracted with the Pan-STARRS1 template image. We obtained the following preliminary upper limit (in the AB system):\n\nr > 21.5 mag (SNR = 2.2 sigma).\n\nThe given limit is derived based on calibrating against Pan-STARRS1 field stars and is not corrected for the expected Galactic foreground extinction corresponding to a reddening of E_(B-V) = 0.04 mag in the direction of the burst (Schlafly & Finkbeiner 2011).\n\nOur r-band limit is deeper than the LT follow-up observations on MJD 60385.848 (Srivastav et al., GCN 35933) and the Nanshan/HMT limit on MJD 60385.69 (Jiang et al., GCN 35935). By direct comparison with the ATLAS o band detection of AT 2024eju, we deduce that the source experienced a rapid fade of more than 1.86 magnitudes within a span of 0.78 days.\n\nDespite the SNR of the measurement being only 2.2 sigma, which falls below our threshold, we were still able to see a slightly faint source in the subtracted image by eye at the position of AT 2024eju. We thus chose to measure the faint source using a lower threshold and obtained an r-band magnitude of 21.45 +/- 0.22.\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35938.",
"published": "2024-03-17T08:26:32.458490Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-17T08:26:32.458505Z",
"modified": "2024-03-17T08:26:32.466757Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6651,
"topic": "gcn.circular",
"uuid": "d24a57ed-f33e-46c6-9cb9-8a943e687119",
"title": "Improved IPN triangulation of GRB 240411A",
"submitter": "Hop gcn.circular",
"authors": "Dmitry Svinkin at Ioffe Institute <svinkin@mail.ioffe.ru>",
"data": {
"date": "24/04/18 10:47:24 GMT",
"from": "Dmitry Svinkin at Ioffe Institute <svinkin@mail.ioffe.ru>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/36156"
},
"title": "GCN CIRCULAR",
"number": "36156",
"subject": "Improved IPN triangulation of GRB 240411A"
},
"message_text": "A.S. Kozyrev, D.V. Golovin, M.L. Litvak, I.G. Mitrofanov, and A.B. Sanin\non behalf of the MGNS/BepiColombo team,\n\nJ. Benkhoff on behalf of the BepiColombo team,\n\nD. Svinkin, D. Frederiks, A. Lysenko, A. Ridnaia,\nand T. Cline on behalf of the Konus-Wind team,\n\nA. Goldstein, M. S. Briggs, C. Wilson-Hodge,\nand E. Burns on behalf of the Fermi GBM team,\n\nE. Bozzo and C. Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team,\n\nand\n\nS. Barthelmy, J. Cummings, H. Krimm, D. Palmer, and A. Tohuvavohu\non behalf of the Swift-BAT team, report:\n\nUsing the BepiColombo (MGNS) data we have improved\nthe previous IPN error box (Svinkin et al., GCN 36090).\n\nThe coordinates of the updated 3 sigma error box are:\n ---------------------------------------------\n RA(2000), deg Dec(2000), deg\n ---------------------------------------------\n Center:\n 248.823 (16h 35m 17s) +43.618 (+43d 37' 03\")\n Corners:\n 248.867 (16h 35m 28s) +43.236 (+43d 14' 08\")\n 248.814 (16h 35m 15s) +43.972 (+43d 58' 19\")\n 248.777 (16h 35m 07s) +43.999 (+43d 59' 57\")\n 248.831 (16h 35m 20s) +43.263 (+43d 15' 47\")\n ---------------------------------------------\nThe error box area is 65 sq. arcmin, and its maximum\ndimension is 46 arcmin (the minimum one is 1 arcmin).\nThe Sun distance was 111 deg.\n\nThis box may be further improved.\n\nUpdated triangulation map and HEALPix FITS files are posted at\nhttp://www.ioffe.ru/LEA/GRBs/GRB240411_T06302/IPN/\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/36156.",
"published": "2024-04-18T10:47:42.939257Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-04-18T10:47:42.939271Z",
"modified": "2024-04-18T10:47:42.947725Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6238,
"topic": "gcn.circular",
"uuid": "a2a8ee7c-a906-4d78-8c1a-07d5e2d1fd7d",
"title": "GRB 240317A: Fermi GBM Final Real-time Localization",
"submitter": "Hop gcn.circular",
"authors": "Fermi GBM Team at MSFC/Fermi-GBM <do_not_reply@GIOC.nsstc.nasa.gov>",
"data": {
"date": "24/03/17 09:54:24 GMT",
"from": "Fermi GBM Team at MSFC/Fermi-GBM <do_not_reply@GIOC.nsstc.nasa.gov>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35939"
},
"title": "GCN CIRCULAR",
"number": "35939",
"subject": "GRB 240317A: Fermi GBM Final Real-time Localization"
},
"message_text": "The Fermi GBM team reports the detection of a likely LONG GRB\n\nAt 09:43:55 UT on 17 Mar 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 240317A (trigger 732361440.302272 / 240317405).\n\nThe on-ground calculated location, using the Fermi GBM trigger data, is RA = 223.9, Dec = 19.1 (J2000 degrees, equivalent to J2000 14h 55m, 19d 06'), with a statistical uncertainty of 4.5 degrees.\n\nThe angle from the Fermi LAT boresight is 75.0 degrees.\n\nThe skymap can be found here:\nhttps://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240317405/quicklook/glg_skymap_all_bn240317405.png\n\nThe HEALPix FITS file, including the estimated localization systematic, can be found here:\nhttps://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240317405/quicklook/glg_healpix_all_bn240317405.fit\n\nThe GBM light curve can be found here:\nhttps://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240317405/quicklook/glg_lc_medres34_bn240317405.gif\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35939.",
"published": "2024-03-17T09:54:41.497738Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-17T09:54:41.497751Z",
"modified": "2024-03-17T09:54:41.507559Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6239,
"topic": "gcn.circular",
"uuid": "1388d9f7-c971-4bb1-9436-9d085c46b8a6",
"title": "X-ray transient EP240315a: orphan FXT?",
"submitter": "Hop gcn.circular",
"authors": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"data": {
"date": "24/03/17 10:04:11 GMT",
"from": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35940"
},
"title": "GCN CIRCULAR",
"number": "35940",
"subject": "X-ray transient EP240315a: orphan FXT?"
},
"message_text": "\nV.Lipunov (Lomonosov MSU, Perevoschikov Moscow Observatory)\n\nThe recently launched space mission of the Chinese Academy of Sciences in collaboration with ESA, MPE and CNES Einstein Probe mission (Yuan et al. 2022, Handbook of X-ray and Gamma-ray Astrophysics) reported the discovery of the fast soft X-ray transient (FXT) EP240315a (Zhagn et al., GCN 35931).\n\nPublication is about an event lasting ~1600 seconds. The spectrum of the ATLAS optical counterpart AT2024eju (Srivastav et al., GCN 35932) unambiguously establishes the cosmological nature of EP240315a with redshift z = 4.859 and a possible connection with Gamma Ray Bursts (Saccardi et al., GCN 35936).\n\nNote that the phenomenon of fast X-ray flares was actually predicted within the framework of the Spinar paradigm (Lipunov & Gorbovskoy, 2007, ApJ, v.665, L97; Lipunov & Gorbovskoy, 2008, MNRAS, v.383, 1397.; Lipunova et al., 2009, MNRAS, v.397,1695).\n\nIn the case of core collapse, which has an increased spin monentum and a weak magnetic field, the phenomenon of fast X-ray bursts can occur without the phenomenon of a gamma-ray burst at all. The corresponding diagram is available at http://observ.pereplet.ru/images/spinar_dogma.jpg)\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35940.",
"published": "2024-03-17T10:04:24.303511Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-17T10:04:24.303523Z",
"modified": "2024-03-17T10:04:24.309401Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6652,
"topic": "gcn.circular",
"uuid": "cf11fba0-07ce-4a36-8fb6-8315a0a140fb",
"title": "EP240416A: Khureltogoot optical upper limit",
"submitter": "Hop gcn.circular",
"authors": "Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>",
"data": {
"date": "24/04/18 12:29:15 GMT",
"from": "Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/36157"
},
"title": "GCN CIRCULAR",
"number": "36157",
"subject": "EP240416A: Khureltogoot optical upper limit"
},
"message_text": "N. Pankov (HSE,IKI), L. Elenin (KIAM), A. Pozanenko (IKI), N. Tungalag (IAG), A. Volnova (IKI), S. Belkin (IKI) report on behalf of GRB IKI FuN:\n\nWe observed the EP240416A (Cheng et al., GCN 36138) with the ORI-40 telescope of Khureltogoot observatory in Clear filter starting on 2024-04-16 (UT) 17:57:07. We did not detect the optical counterpart (Chen et al., GCN 36139; An et al., GCN 36144). Preliminary photometry of a stacked image is the following\n\nDate UT start t-T0 Exp. Filter OT Err. UL(3sigma)\n (mid, days) (s)\n\n2024-04-16 17:57:07 0.65409 54*60 Clear n/d n/d 19.7\n\nThe photometry is based on nearby USNO-B1.0 (R2) stars.\n\nThe given results is in agreement with the upper limit obtained by (Xiong et al., GCN 36155).\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/36157.",
"published": "2024-04-18T12:29:32.176958Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-04-18T12:29:32.176973Z",
"modified": "2024-04-18T12:29:32.184744Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6653,
"topic": "gcn.circular",
"uuid": "2439a266-477b-4f18-8e51-f384afeb62d2",
"title": "EP240416A: Terskol Zeiss-2000 optical upper limit",
"submitter": "Hop gcn.circular",
"authors": "Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>",
"data": {
"date": "24/04/18 12:40:39 GMT",
"from": "Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/36158"
},
"title": "GCN CIRCULAR",
"number": "36158",
"subject": "EP240416A: Terskol Zeiss-2000 optical upper limit"
},
"message_text": "S. Belkin (IKI), I. Sokolov (INASAN, KIAM), A. Pozanenko (IKI), N. Pankov (HSE) report on behalf of GRB IKI FuN:\n\nWe observed the EP240416A (Cheng et al., GCN 36138) with the Zeiss-2000 telescope of Terskol observatory in R-filter starting on on 2024-04-16 (UT) 21:21:18. We did not detect the optical counterpart (Chen et al., GCN 36139; An et al., GCN 36144) down to the limiting magnitude of R~21.9. Preliminary photometry of a stacked image is the following\n\nDate UT start t-T0 Exp. Filter OT Err. UL(3sigma)\n (mid, days) (s)\n\n2024-04-16 21:21:18 0.79832 70x90 R n/d n/d 21.9\n\nThe photometry is based on nearby USNO-B1.0 stars.\nUSNO-B1.0\nRA DEC R2\n13:32:30.1848000 -13:36:51.350400 13.67\n13:32:25.6521600 -13:39:02.671200 14.26\n13:32:19.2355200 -13:39:27.943200 13.96\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/36158.",
"published": "2024-04-18T12:40:59.224238Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-04-18T12:40:59.224256Z",
"modified": "2024-04-18T12:40:59.230283Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6240,
"topic": "gcn.circular",
"uuid": "02c08ebb-7da3-4b70-8d37-6cff7af9809e",
"title": "GRB 240317B: Fermi GBM Final Real-time Localization",
"submitter": "Hop gcn.circular",
"authors": "Fermi GBM Team at MSFC/Fermi-GBM <do_not_reply@GIOC.nsstc.nasa.gov>",
"data": {
"date": "24/03/17 11:04:59 GMT",
"from": "Fermi GBM Team at MSFC/Fermi-GBM <do_not_reply@GIOC.nsstc.nasa.gov>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35941"
},
"title": "GCN CIRCULAR",
"number": "35941",
"subject": "GRB 240317B: Fermi GBM Final Real-time Localization"
},
"message_text": "The Fermi GBM team reports the detection of a likely LONG GRB\n\nAt 10:54:24 UT on 17 Mar 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 240317B (trigger 732365669.017448 / 240317454).\n\nThe on-ground calculated location, using the Fermi GBM trigger data, is RA = 274.5, Dec = 49.6 (J2000 degrees, equivalent to J2000 18h 18m, 49d 36'), with a statistical uncertainty of 8.8 degrees.\n\nThe angle from the Fermi LAT boresight is 96.0 degrees.\n\nThe skymap can be found here:\nhttps://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240317454/quicklook/glg_skymap_all_bn240317454.png\n\nThe HEALPix FITS file, including the estimated localization systematic, can be found here:\nhttps://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240317454/quicklook/glg_healpix_all_bn240317454.fit\n\nThe GBM light curve can be found here:\nhttps://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240317454/quicklook/glg_lc_medres34_bn240317454.gif\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35941.",
"published": "2024-03-17T11:05:17.175037Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-17T11:05:17.175052Z",
"modified": "2024-03-17T11:05:17.181575Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6241,
"topic": "gcn.circular",
"uuid": "6a3c6396-fc71-44cb-a2f4-1a80950f116a",
"title": "Fermi GRB 240317A: Global MASTER-Net observations report",
"submitter": "Hop gcn.circular",
"authors": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"data": {
"date": "24/03/17 13:31:01 GMT",
"from": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35942"
},
"title": "GCN CIRCULAR",
"number": "35942",
"subject": "Fermi GRB 240317A: Global MASTER-Net observations report"
},
"message_text": "V. Lipunov, V.Kornilov, E. Gorbovskoy, K. Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, V.Senik, D. Vlasenko,\nG.Antipov, D.Zimnukhov, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov, D. Cheryasov, Ya.Kechin, Yu.Tselik, A. Sosnovskij\n(Lomonosov Moscow State University, SAI, Physics Department),\n\nR. Podesta, C.Lopez, F. Podesta, C.Francile\n(Observatorio Astronomico Felix Aguilar OAFA),\n\nR. Rebolo, M. Serra\n(The Instituto de Astrofisica de Canarias),\n\nD. Buckley\n(South African Astronomical Observatory),\n\nO.A. Gress, N.M. Budnev, O.Ershova\n(Irkutsk State University, API),\n\nL.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez,\nA.R.Corella, L.H.Rodriguez\n(INAOE, Guillermo Haro Astrophysics Observatory),\n\nA. Tlatov, D. Dormidontov\n(Kislovodsk Solar Station of the Pulkovo Observatory),\n\nV. Yurkov, A. Gabovich\n(Blagoveschensk Educational State University)\n\nMASTER-Amur robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Blagoveshchensk State Pedagogical University) started inspect of the Fermi GRB 240317A ( Fermi GBM team, GCN 35939) errorbox 12523 sec after notice time and 12555 sec after trigger time at 2024-03-17 13:13:10 UT, with upper limit up to 17.8 mag. The observations began at zenith distance = 69 deg. The sun altitude is -32.2 deg.\n\nMASTER-Tunka robotic telescope located in Russia (Applied Physics Institute, Irkutsk State University) started inspect of the Fermi GRB 240317A errorbox 13217 sec after notice time and 13249 sec after trigger time at 2024-03-17 13:24:45 UT, with upper limit up to 13.5 mag. The observations began at zenith distance = 80 deg. The sun altitude is -20.7 deg.\n\nThe galactic latitude b = 60 deg., longitude l = 24 deg.\n\n\nReal time updated cover map and OT discovered available here:\nhttps://master.sai.msu.ru/site/master2/observ.php?id$00638\n\nWe obtain a following upper limits.\n\nTmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment\n_________|_____________________|_____________________|____________________________________|_____|_______|_______|________\n\n 12585 | 2024-03-17 13:13:10 | MASTER-Amur | (14h 48m 33.06s , +20d 16m 10.5s) | C | 60 | 17.7 |\n 12665 | 2024-03-17 13:14:30 | MASTER-Amur | (14h 57m 03.77s , +20d 17m 46.4s) | C | 60 | 17.4 |\n 12745 | 2024-03-17 13:15:50 | MASTER-Amur | (14h 59m 54.03s , +22d 11m 46.7s) | C | 60 | 17.6 |\n 12825 | 2024-03-17 13:17:10 | MASTER-Amur | (15h 08m 25.81s , +22d 11m 31.4s) | C | 60 | 17.4 |\n 13067 | 2024-03-17 13:21:11 | MASTER-Amur | (14h 38m 28.91s , +18d 21m 26.0s) | C | 60 | 17.8 |\n 13146 | 2024-03-17 13:22:31 | MASTER-Amur | (14h 46m 52.55s , +18d 23m 18.1s) | C | 60 | 17.7 |\n 13280 | 2024-03-17 13:24:45 | MASTER-Tunka | (14h 41m 05.02s , +21d 19m 39.8s) | C | 60 | 13.5 |\nFilter C is a clear (unfiltred) band.\n\n\nThe observation and reduction will continue.\nThe message may be cited.\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35942.",
"published": "2024-03-17T13:31:16.885609Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-17T13:31:16.885628Z",
"modified": "2024-03-17T13:31:16.893512Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6242,
"topic": "gcn.circular",
"uuid": "022a0cdc-3d5b-49b8-b114-8648c1b0213a",
"title": "Fermi GRB 240317B: Global MASTER-Net observations report",
"submitter": "Hop gcn.circular",
"authors": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"data": {
"date": "24/03/17 13:31:09 GMT",
"from": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35943"
},
"title": "GCN CIRCULAR",
"number": "35943",
"subject": "Fermi GRB 240317B: Global MASTER-Net observations report"
},
"message_text": "V. Lipunov, V.Kornilov, E. Gorbovskoy, K. Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, V.Senik, D. Vlasenko,\nG.Antipov, D.Zimnukhov, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov, D. Cheryasov, Ya.Kechin, Yu.Tselik, A. Sosnovskij\n(Lomonosov Moscow State University, SAI, Physics Department),\n\nR. Podesta, C.Lopez, F. Podesta, C.Francile\n(Observatorio Astronomico Felix Aguilar OAFA),\n\nR. Rebolo, M. Serra\n(The Instituto de Astrofisica de Canarias),\n\nD. Buckley\n(South African Astronomical Observatory),\n\nO.A. Gress, N.M. Budnev, O.Ershova\n(Irkutsk State University, API),\n\nL.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez,\nA.R.Corella, L.H.Rodriguez\n(INAOE, Guillermo Haro Astrophysics Observatory),\n\nA. Tlatov, D. Dormidontov\n(Kislovodsk Solar Station of the Pulkovo Observatory),\n\nV. Yurkov, A. Gabovich\n(Blagoveschensk Educational State University)\n\nMASTER-Amur robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Blagoveshchensk State Pedagogical University) started inspect of the Fermi GRB 240317B ( Fermi GBM team, GCN 35941) errorbox 465 sec after notice time and 497 sec after trigger time at 2024-03-17 11:02:41 UT, with upper limit up to 17.7 mag. Observations started at twilight. The observations began at zenith distance = 69 deg. The sun altitude is -14.2 deg.\n\nMASTER-Tunka robotic telescope located in Russia (Applied Physics Institute, Irkutsk State University) started inspect of the Fermi GRB 240317B errorbox 5026 sec after notice time and 5058 sec after trigger time at 2024-03-17 12:18:42 UT, with upper limit up to 14.5 mag. Observations started at twilight. The observations began at zenith distance = 78 deg. The sun altitude is -10.9 deg.\n\nThe galactic latitude b = 25 deg., longitude l = 78 deg.\n\n\nReal time updated cover map and OT discovered available here:\nhttps://master.sai.msu.ru/site/master2/observ.php?id$00679\n\nWe obtain a following upper limits.\n\nTmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment\n_________|_____________________|_____________________|____________________________________|_____|_______|_______|________\n\n 527 | 2024-03-17 11:02:41 | MASTER-Amur | (18h 08m 33.84s , +60d 12m 29.5s) | C | 60 | 17.0 |\n 607 | 2024-03-17 11:04:01 | MASTER-Amur | (18h 24m 41.82s , +60d 10m 12.2s) | C | 60 | 17.1 |\n 5088 | 2024-03-17 12:18:42 | MASTER-Tunka | (18h 40m 58.76s , +51d 03m 11.4s) | C | 60 | 13.3 |\n 5247 | 2024-03-17 12:21:20 | MASTER-Tunka | (18h 38m 56.08s , +52d 56m 32.7s) | C | 60 | 13.1 |\n 5326 | 2024-03-17 12:22:39 | MASTER-Tunka | (18h 11m 57.74s , +54d 49m 55.0s) | C | 60 | 13.6 |\n 5405 | 2024-03-17 12:23:59 | MASTER-Tunka | (18h 25m 29.46s , +54d 49m 03.5s) | C | 60 | 13.1 |\n 5484 | 2024-03-17 12:25:18 | MASTER-Tunka | (18h 44m 12.61s , +49d 08m 38.9s) | C | 60 | 12.8 |\n 5723 | 2024-03-17 12:29:16 | MASTER-Tunka | (18h 10m 46.74s , +56d 42m 59.1s) | C | 60 | 13.9 |\n 5809 | 2024-03-17 12:30:42 | MASTER-Tunka | (18h 25m 14.42s , +56d 44m 15.4s) | C | 60 | 13.9 |\n 5888 | 2024-03-17 12:32:02 | MASTER-Tunka | (18h 37m 57.53s , +54d 50m 37.3s) | C | 60 | 13.9 |\n 5967 | 2024-03-17 12:33:21 | MASTER-Tunka | (18h 51m 38.66s , +54d 48m 51.4s) | C | 60 | 13.8 |\n 6093 | 2024-03-17 12:35:27 | MASTER-Tunka | (17h 32m 14.76s , +47d 49m 22.3s) | C | 60 | 12.0 |\n 6173 | 2024-03-17 12:36:46 | MASTER-Tunka | (17h 45m 53.62s , +51d 38m 34.6s) | C | 60 | 13.6 |\n 6252 | 2024-03-17 12:38:05 | MASTER-Tunka | (17h 58m 51.51s , +51d 37m 38.5s) | C | 60 | 13.5 |\n 6331 | 2024-03-17 12:39:25 | MASTER-Tunka | (18h 08m 20.83s , +53d 30m 31.9s) | C | 60 | 13.5 |\n 6411 | 2024-03-17 12:40:44 | MASTER-Tunka | (18h 22m 07.75s , +53d 30m 45.1s) | C | 60 | 13.3 |\n 6490 | 2024-03-17 12:42:03 | MASTER-Tunka | (17h 42m 29.98s , +53d 33m 01.3s) | C | 60 | 13.7 |\n 6569 | 2024-03-17 12:43:22 | MASTER-Tunka | (17h 56m 03.03s , +53d 31m 31.5s) | C | 60 | 14.2 |\n 6648 | 2024-03-17 12:44:42 | MASTER-Tunka | (18h 07m 12.93s , +55d 25m 21.8s) | C | 60 | 13.5 |\n 6727 | 2024-03-17 12:46:01 | MASTER-Tunka | (18h 21m 30.03s , +55d 25m 53.4s) | C | 60 | 13.9 |\n 6807 | 2024-03-17 12:47:20 | MASTER-Tunka | (18h 10m 40.47s , +51d 38m 42.8s) | C | 60 | 12.5 |\n 6886 | 2024-03-17 12:48:40 | MASTER-Tunka | (18h 34m 27.86s , +53d 30m 56.9s) | C | 60 | 13.1 |\n 7045 | 2024-03-17 12:51:19 | MASTER-Tunka | (18h 23m 52.08s , +51d 35m 59.6s) | C | 60 | 12.9 |\n 7125 | 2024-03-17 12:52:38 | MASTER-Tunka | (17h 45m 52.05s , +51d 36m 29.1s) | C | 60 | 13.2 |\n 7283 | 2024-03-17 12:55:16 | MASTER-Tunka | (18h 08m 31.13s , +53d 32m 30.1s) | C | 60 | 12.0 |\n 7362 | 2024-03-17 12:56:36 | MASTER-Tunka | (18h 22m 06.54s , +53d 30m 53.0s) | C | 60 | 12.2 |\n 7442 | 2024-03-17 12:57:55 | MASTER-Tunka | (17h 42m 28.24s , +53d 30m 30.9s) | C | 60 | 13.5 |\n 7521 | 2024-03-17 12:59:15 | MASTER-Tunka | (17h 56m 14.41s , +53d 31m 12.9s) | C | 60 | 12.3 |\n 7600 | 2024-03-17 13:00:34 | MASTER-Tunka | (18h 07m 15.33s , +55d 25m 54.0s) | C | 60 | 13.1 |\n 7680 | 2024-03-17 13:01:53 | MASTER-Tunka | (18h 21m 35.22s , +55d 24m 10.8s) | C | 60 | 13.4 |\n 7838 | 2024-03-17 13:04:32 | MASTER-Tunka | (18h 34m 26.84s , +53d 30m 37.4s) | C | 60 | 12.8 |\n 7997 | 2024-03-17 13:07:11 | MASTER-Tunka | (18h 01m 01.79s , +45d 53m 48.3s) | C | 60 | 13.1 |\n 8116 | 2024-03-17 13:09:09 | MASTER-Amur | (18h 08m 32.38s , +60d 15m 05.1s) | C | 60 | 17.6 |\n 8168 | 2024-03-17 13:10:01 | MASTER-Tunka | (17h 38m 59.01s , +45d 54m 53.6s) | C | 60 | 12.7 |\n 8195 | 2024-03-17 13:10:29 | MASTER-Amur | (18h 24m 43.45s , +60d 15m 58.2s) | C | 60 | 17.7 |\n 8334 | 2024-03-17 13:12:48 | MASTER-Tunka | (17h 26m 26.99s , +49d 44m 57.1s) | C | 60 | 13.3 |\n 8414 | 2024-03-17 13:14:07 | MASTER-Tunka | (17h 39m 06.53s , +49d 43m 35.7s) | C | 60 | 13.6 |\n 8493 | 2024-03-17 13:15:26 | MASTER-Tunka | (18h 23m 15.91s , +45d 53m 39.0s) | C | 60 | 13.4 |\n 8572 | 2024-03-17 13:16:46 | MASTER-Tunka | (17h 40m 10.09s , +55d 26m 08.0s) | C | 60 | 13.2 |\n 8651 | 2024-03-17 13:18:05 | MASTER-Tunka | (17h 54m 24.83s , +55d 25m 12.8s) | C | 60 | 13.1 |\n 8730 | 2024-03-17 13:19:24 | MASTER-Tunka | (17h 46m 22.65s , +44d 01m 00.9s) | C | 60 | 14.5 |\n 8889 | 2024-03-17 13:22:03 | MASTER-Tunka | (17h 21m 14.66s , +51d 37m 48.6s) | C | 60 | 14.5 |\n 8968 | 2024-03-17 13:23:22 | MASTER-Tunka | (17h 34m 22.92s , +51d 38m 11.6s) | C | 60 | 13.6 |\nFilter C is a clear (unfiltred) band.\n\n\nThe observation and reduction will continue.\nThe message may be cited.\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35943.",
"published": "2024-03-17T13:31:19.906566Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-17T13:31:19.906591Z",
"modified": "2024-03-17T13:31:19.917143Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6654,
"topic": "gcn.circular",
"uuid": "26b5c1b8-bdf7-44a8-a5ef-8331d570fbaa",
"title": "LIGO/Virgo/KAGRA S240413p: X-ray upper limits from EP-WXT for the candidate AGN counterpart",
"submitter": "Hop gcn.circular",
"authors": "EP Team at NAOC/CAS <ep_ta@bao.ac.cn>",
"data": {
"date": "24/04/18 13:34:02 GMT",
"from": "EP Team at NAOC/CAS <ep_ta@bao.ac.cn>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/36159"
},
"title": "GCN CIRCULAR",
"number": "36159",
"subject": "LIGO/Virgo/KAGRA S240413p: X-ray upper limits from EP-WXT for the candidate AGN counterpart"
},
"message_text": "J. W. Hu, W. Chen, S. Q. Jiang, D. Y. Li, C. C. Jin, Y. Liu, Z. X. Ling, C. Zhang, H. Q. Cheng, C. Z. Cui, D. W. Fan, H. B. Hu, M. H. Huang, T. Y. Lian, H. Y. Liu, M. J. Liu, Z. Z. Lv, X. Mao, H. W. Pan, X. Pan, H. Sun, W. X. Wang, Y. L. Wang, Q. Y. Wu, X. P. Xu, Y. F. Xu, H. N. Yang, W. Yuan, M. Zhang, W. D. Zhang, W. J. Zhang, Z. Zhang, D. H. Zhao (NAOC, CAS), E. Kuulkers, A. Santovincenzo (ESA), P. O'Brien (Univ. of Leicester), K. Nandra, A. Rau (MPE), B. Cordier (CEA), on behalf of the Einstein Probe team \n\nC.R. Bom et al. (GCN 36146) reported a candidate optical counterpart associated with a known AGN for the binary black hole merger S240413p (GCN 36075). The position of this AGN was covered by EP-WXT in four observations from 2024-04-13 to 2024-04-17. No significant X-ray counterpart was detected in these observations, and a flux upper limit at the 90% confidence level is estimated for each of the observations.\n\nThe details of these observations are:\nNo. | Start time (UTC) | End time (UTC) | Exposure (s) | Upper limit (erg/s/cm2) \n-------------------------------------------------------------------------------------------\n1 | 2024-04-13 20:45:36 | 2024-04-13 21:35:22 | 2986 | 5.2 x 10^-12\n2 | 2024-04-15 01:36:51 | 2024-04-15 01:57:31 | 1240 | 2.8 x 10^-11\n3 | 2024-04-15 06:25:48 | 2024-04-15 06:37:08 | 680 | 3.4 x 10^-11\n4 | 2024-04-15 12:52:24 | 2024-04-15 23:21:34 | 18776 | 4.6 x 10^-12\n\nFurthermore, no X-ray sources were detected in the above observations at the nearby positions mentioned by Antonella Palmese et al. (GCN 36153) with similar upper limits. No new transients were found in these EP-WXT fields, either.\n\nThe above observations were made with the WXT instrument during the commissioning phase of EP. Launched on January 9, 2024, EP is a space X-ray observatory to monitor the soft X-ray sky with X-ray follow-up capability (Yuan et al. 2022, Handbook of X-ray and Gamma-ray Astrophysics). EP is a mission of the Chinese Academy of Sciences in collaboration with ESA, MPE and CNES.\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/36159.",
"published": "2024-04-18T13:34:27.032457Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-04-18T13:34:27.032471Z",
"modified": "2024-04-18T13:34:27.040603Z",
"nonlocalizedevents": [
{
"event_id": "S240413p"
}
],
"targets": []
},
{
"id": 6657,
"topic": "gcn.circular",
"uuid": "a468af4a-629c-46aa-988a-738da4f1f33e",
"title": "Fermi GRB 240417A: Global MASTER-Net observations report",
"submitter": "Hop gcn.circular",
"authors": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"data": {
"date": "24/04/18 15:15:59 GMT",
"from": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/36160"
},
"title": "GCN CIRCULAR",
"number": "36160",
"subject": "Fermi GRB 240417A: Global MASTER-Net observations report"
},
"message_text": "V. Lipunov, V.Kornilov, E. Gorbovskoy, K. Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, V.Senik, D. Vlasenko,\nG.Antipov, D.Zimnukhov, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov, D. Cheryasov, Ya.Kechin, Yu.Tselik, A. Sosnovskij\n(Lomonosov Moscow State University, SAI, Physics Department),\n\nR. Podesta, C.Lopez, F. Podesta, C.Francile\n(Observatorio Astronomico Felix Aguilar OAFA),\n\nR. Rebolo, M. Serra\n(The Instituto de Astrofisica de Canarias),\n\nD. Buckley\n(South African Astronomical Observatory),\n\nO.A. Gress, N.M. Budnev, O.Ershova\n(Irkutsk State University, API),\n\nL.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez,\nA.R.Corella, L.H.Rodriguez\n(INAOE, Guillermo Haro Astrophysics Observatory),\n\nA. Tlatov, D. Dormidontov\n(Kislovodsk Solar Station of the Pulkovo Observatory),\n\nV. Yurkov, A. Gabovich\n(Blagoveschensk Educational State University)\n\nMASTER-SAAO robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in South Africa (South African Astronomical Observatory) started inspect of the Fermi GRB 240417A ( Fermi GBM team, GCN 36151) errorbox 774 sec after notice time and 811 sec after trigger time at 2024-04-17 18:59:41 UT, with upper limit up to 18.2 mag. The observations began at zenith distance = 81 deg. The sun altitude is -35.5 deg.\n\nThe galactic latitude b = -64 deg., longitude l = 276 deg.\n\n\nReal time updated cover map and OT discovered available here:\nhttps://master.sai.msu.ru/site/master2/observ.php?id$25683\n\nWe obtain a following upper limits.\n\nTmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment\n_________|_____________________|_____________________|____________________________________|_____|_______|_______|________\n\n 841 | 2024-04-17 18:59:41 | MASTER-SAAO | (02h 19m 40.07s , -49d 59m 17.6s) | C | 60 | 16.7 |\n 841 | 2024-04-17 18:59:41 | MASTER-SAAO | (02h 22m 25.63s , -50d 12m 18.9s) | C | 60 | 18.0 |\n 921 | 2024-04-17 19:01:01 | MASTER-SAAO | (02h 25m 31.14s , -51d 54m 11.0s) | C | 60 | 17.6 |\n 921 | 2024-04-17 19:01:01 | MASTER-SAAO | (02h 28m 23.59s , -52d 07m 10.2s) | C | 60 | 18.2 |\n 1001 | 2024-04-17 19:02:21 | MASTER-SAAO | (02h 06m 24.22s , -53d 47m 21.4s) | C | 60 | 17.3 |\n 1001 | 2024-04-17 19:02:21 | MASTER-SAAO | (02h 09m 24.03s , -54d 00m 23.9s) | C | 60 | 17.9 |\n 1081 | 2024-04-17 19:03:41 | MASTER-SAAO | (02h 37m 07.92s , -48d 05m 50.6s) | C | 60 | 17.1 |\n 1081 | 2024-04-17 19:03:41 | MASTER-SAAO | (02h 39m 47.00s , -48d 18m 52.3s) | C | 60 | 18.0 |\n 1161 | 2024-04-17 19:05:01 | MASTER-SAAO | (02h 12m 39.18s , -55d 43m 14.3s) | C | 60 | 17.7 |\n 1161 | 2024-04-17 19:05:01 | MASTER-SAAO | (02h 15m 47.66s , -55d 56m 15.5s) | C | 60 | 17.8 |\n 1240 | 2024-04-17 19:06:20 | MASTER-SAAO | (02h 32m 17.11s , -53d 48m 54.6s) | C | 60 | 17.8 |\n 1240 | 2024-04-17 19:06:20 | MASTER-SAAO | (02h 35m 16.99s , -54d 01m 54.5s) | C | 60 | 18.1 |\n 1320 | 2024-04-17 19:07:40 | MASTER-SAAO | (02h 43m 18.37s , -49d 59m 03.5s) | C | 60 | 17.6 |\n 1320 | 2024-04-17 19:07:40 | MASTER-SAAO | (02h 46m 03.49s , -50d 12m 05.0s) | C | 60 | 18.1 |\n 1399 | 2024-04-17 19:09:00 | MASTER-SAAO | (02h 50m 14.83s , -51d 54m 15.6s) | C | 60 | 17.9 |\n 1399 | 2024-04-17 19:09:00 | MASTER-SAAO | (02h 53m 06.96s , -52d 07m 15.0s) | C | 60 | 18.1 |\n 1479 | 2024-04-17 19:10:19 | MASTER-SAAO | (02h 39m 45.84s , -55d 41m 02.2s) | C | 60 | 17.9 |\n 1479 | 2024-04-17 19:10:19 | MASTER-SAAO | (02h 42m 54.28s , -55d 54m 01.9s) | C | 60 | 18.1 |\n 2049 | 2024-04-17 19:19:50 | MASTER-SAAO | (02h 19m 50.95s , -57d 36m 10.4s) | C | 60 | 17.6 |\n 2049 | 2024-04-17 19:19:50 | MASTER-SAAO | (02h 23m 09.63s , -57d 49m 11.0s) | C | 60 | 18.0 |\n 2129 | 2024-04-17 19:21:09 | MASTER-SAAO | (02h 12m 43.89s , -55d 43m 12.1s) | C | 60 | 17.4 |\n 2129 | 2024-04-17 19:21:09 | MASTER-SAAO | (02h 15m 52.54s , -55d 56m 16.3s) | C | 60 | 17.7 |\n 2209 | 2024-04-17 19:22:29 | MASTER-SAAO | (02h 32m 20.62s , -53d 48m 34.2s) | C | 60 | 17.4 |\n 2209 | 2024-04-17 19:22:29 | MASTER-SAAO | (02h 35m 20.64s , -54d 01m 37.3s) | C | 60 | 18.0 |\n 2289 | 2024-04-17 19:23:49 | MASTER-SAAO | (02h 58m 03.34s , -53d 47m 56.0s) | C | 60 | 17.7 |\n 2289 | 2024-04-17 19:23:49 | MASTER-SAAO | (03h 01m 03.63s , -54d 00m 55.3s) | C | 60 | 17.8 |\n 2368 | 2024-04-17 19:25:09 | MASTER-SAAO | (02h 50m 21.71s , -51d 52m 51.9s) | C | 60 | 17.5 |\n 2368 | 2024-04-17 19:25:09 | MASTER-SAAO | (02h 53m 13.93s , -52d 05m 54.1s) | C | 60 | 17.9 |\n 2448 | 2024-04-17 19:26:28 | MASTER-SAAO | (02h 39m 43.88s , -55d 41m 38.1s) | C | 60 | 17.6 |\n 2448 | 2024-04-17 19:26:28 | MASTER-SAAO | (02h 42m 52.44s , -55d 54m 40.0s) | C | 60 | 18.0 |\n 2528 | 2024-04-17 19:27:48 | MASTER-SAAO | (02h 59m 53.48s , -48d 04m 10.7s) | C | 60 | 17.1 |\n 2528 | 2024-04-17 19:27:48 | MASTER-SAAO | (03h 02m 32.38s , -48d 17m 15.3s) | C | 60 | 18.0 |\n 2608 | 2024-04-17 19:29:08 | MASTER-SAAO | (03h 07m 05.82s , -49d 59m 07.5s) | C | 60 | 17.4 |\n 2608 | 2024-04-17 19:29:08 | MASTER-SAAO | (03h 09m 51.00s , -50d 12m 09.4s) | C | 60 | 18.1 |\n 2688 | 2024-04-17 19:30:28 | MASTER-SAAO | (01h 57m 51.98s , -59d 31m 22.7s) | C | 60 | 17.7 |\n 2688 | 2024-04-17 19:30:28 | MASTER-SAAO | (02h 01m 20.89s , -59d 44m 30.9s) | C | 60 | 17.9 |\n 2767 | 2024-04-17 19:31:47 | MASTER-SAAO | (02h 48m 18.36s , -57d 36m 03.2s) | C | 60 | 17.7 |\n 2767 | 2024-04-17 19:31:47 | MASTER-SAAO | (02h 51m 36.68s , -57d 49m 04.8s) | C | 60 | 17.8 |\n 2847 | 2024-04-17 19:33:07 | MASTER-SAAO | (02h 27m 51.47s , -59d 28m 57.3s) | C | 60 | 17.9 |\n 2847 | 2024-04-17 19:33:07 | MASTER-SAAO | (02h 31m 20.55s , -59d 42m 00.7s) | C | 60 | 18.1 |\n 3026 | 2024-04-17 19:36:06 | MASTER-SAAO | (02h 19m 50.18s , -57d 36m 53.1s) | C | 60 | 17.6 |\n 3026 | 2024-04-17 19:36:06 | MASTER-SAAO | (02h 23m 08.30s , -57d 49m 58.3s) | C | 60 | 17.9 |\n 3106 | 2024-04-17 19:37:26 | MASTER-SAAO | (03h 06m 49.57s , -55d 40m 25.7s) | C | 60 | 17.7 |\n 3106 | 2024-04-17 19:37:26 | MASTER-SAAO | (03h 09m 58.14s , -55d 53m 25.1s) | C | 60 | 17.9 |\n 3186 | 2024-04-17 19:38:46 | MASTER-SAAO | (03h 15m 03.12s , -51d 52m 17.0s) | C | 60 | 17.6 |\n 3186 | 2024-04-17 19:38:46 | MASTER-SAAO | (03h 17m 55.06s , -52d 05m 17.5s) | C | 60 | 17.9 |\n 3266 | 2024-04-17 19:40:06 | MASTER-SAAO | (02h 58m 04.42s , -53d 46m 10.0s) | C | 60 | 17.4 |\n 3266 | 2024-04-17 19:40:06 | MASTER-SAAO | (03h 01m 03.86s , -53d 59m 12.9s) | C | 60 | 17.6 |\n 3346 | 2024-04-17 19:41:26 | MASTER-SAAO | (02h 05m 15.46s , -61d 25m 16.1s) | C | 60 | 17.7 |\n 3346 | 2024-04-17 19:41:26 | MASTER-SAAO | (02h 08m 56.84s , -61d 38m 22.5s) | C | 60 | 18.0 |\n 3426 | 2024-04-17 19:42:46 | MASTER-SAAO | (02h 39m 54.65s , -55d 42m 06.4s) | C | 60 | 17.5 |\n 3426 | 2024-04-17 19:42:46 | MASTER-SAAO | (02h 43m 02.68s , -55d 55m 12.1s) | C | 60 | 17.9 |\n 3505 | 2024-04-17 19:44:06 | MASTER-SAAO | (02h 57m 52.33s , -59d 29m 44.7s) | C | 60 | 17.8 |\n 3506 | 2024-04-17 19:44:06 | MASTER-SAAO | (03h 01m 21.54s , -59d 42m 45.4s) | C | 60 | 18.0 |\n 3681 | 2024-04-17 19:47:01 | MASTER-SAAO | (02h 48m 21.96s , -57d 35m 18.3s) | C | 60 | 17.5 |\n 3681 | 2024-04-17 19:47:01 | MASTER-SAAO | (02h 51m 40.07s , -57d 48m 21.0s) | C | 60 | 17.8 |\n 3760 | 2024-04-17 19:48:21 | MASTER-SAAO | (02h 27m 54.17s , -59d 30m 45.3s) | C | 60 | 17.5 |\n 3760 | 2024-04-17 19:48:21 | MASTER-SAAO | (02h 31m 23.18s , -59d 43m 50.1s) | C | 60 | 17.8 |\n 3840 | 2024-04-17 19:49:40 | MASTER-SAAO | (02h 37m 08.32s , -61d 24m 32.3s) | C | 60 | 17.7 |\n 3840 | 2024-04-17 19:49:40 | MASTER-SAAO | (02h 40m 50.22s , -61d 37m 34.9s) | C | 60 | 17.8 |\n 3920 | 2024-04-17 19:51:00 | MASTER-SAAO | (03h 23m 55.07s , -53d 47m 16.4s) | C | 60 | 17.6 |\n 3920 | 2024-04-17 19:51:00 | MASTER-SAAO | (03h 26m 54.82s , -54d 00m 16.9s) | C | 60 | 17.6 |\n 3999 | 2024-04-17 19:52:19 | MASTER-SAAO | (03h 16m 46.82s , -57d 34m 09.9s) | C | 60 | 17.5 |\n 3999 | 2024-04-17 19:52:19 | MASTER-SAAO | (03h 20m 04.98s , -57d 47m 09.9s) | C | 60 | 17.7 |\n 4079 | 2024-04-17 19:53:39 | MASTER-SAAO | (03h 06m 50.03s , -55d 40m 54.8s) | C | 60 | 17.4 |\n 4079 | 2024-04-17 19:53:39 | MASTER-SAAO | (03h 09m 58.28s , -55d 53m 57.4s) | C | 60 | 17.7 |\n 4158 | 2024-04-17 19:54:59 | MASTER-SAAO | (03h 15m 00.23s , -51d 51m 42.3s) | C | 60 | 14.3 |\n 4158 | 2024-04-17 19:54:59 | MASTER-SAAO | (03h 17m 51.89s , -52d 04m 46.8s) | C | 60 | 15.1 |\n 4238 | 2024-04-17 19:56:18 | MASTER-SAAO | (02h 58m 15.68s , -53d 47m 01.1s) | C | 60 | 16.3 |\n 4238 | 2024-04-17 19:56:18 | MASTER-SAAO | (03h 01m 15.00s , -54d 00m 08.3s) | C | 60 | 16.6 |\n 4318 | 2024-04-17 19:57:38 | MASTER-SAAO | (02h 05m 23.14s , -61d 25m 20.2s) | C | 60 | 16.1 |\n 4318 | 2024-04-17 19:57:38 | MASTER-SAAO | (02h 09m 04.28s , -61d 38m 30.0s) | C | 60 | 16.6 |\n 4398 | 2024-04-17 19:58:58 | MASTER-SAAO | (02h 13m 52.27s , -63d 18m 45.2s) | C | 60 | 17.4 |\n 4398 | 2024-04-17 19:58:58 | MASTER-SAAO | (02h 17m 48.14s , -63d 31m 52.1s) | C | 60 | 17.6 |\n 4478 | 2024-04-17 20:00:18 | MASTER-SAAO | (02h 57m 58.29s , -59d 29m 40.0s) | C | 60 | 15.1 |\n 4478 | 2024-04-17 20:00:18 | MASTER-SAAO | (03h 01m 27.24s , -59d 42m 43.2s) | C | 60 | 15.9 |\n 4576 | 2024-04-17 20:01:56 | MASTER-SAAO | (01h 40m 22.93s , -63d 29m 31.1s) | C | 60 | 16.5 |\n 4576 | 2024-04-17 20:01:56 | MASTER-SAAO | (01h 36m 52.94s , -63d 16m 04.8s) | C | 60 | 16.1 |\n 4668 | 2024-04-17 20:03:28 | MASTER-SAAO | (02h 48m 31.38s , -57d 35m 15.9s) | C | 60 | 16.8 |\n 4668 | 2024-04-17 20:03:28 | MASTER-SAAO | (02h 51m 45.99s , -57d 48m 17.9s) | C | 60 | 17.2 |\n 4748 | 2024-04-17 20:04:48 | MASTER-SAAO | (03h 30m 49.13s , -49d 59m 18.4s) | C | 60 | 14.4 |\n 4748 | 2024-04-17 20:04:48 | MASTER-SAAO | (03h 33m 31.29s , -50d 12m 19.1s) | C | 60 | 16.2 |\n 5251 | 2024-04-17 20:13:11 | MASTER-SAAO | (02h 37m 21.09s , -61d 23m 37.4s) | C | 60 | 14.3 |\n 5251 | 2024-04-17 20:13:11 | MASTER-SAAO | (02h 40m 58.78s , -61d 36m 39.4s) | C | 60 | 15.0 |\n 5331 | 2024-04-17 20:14:31 | MASTER-SAAO | (03h 24m 00.11s , -53d 47m 23.3s) | C | 60 | 15.2 |\n 5331 | 2024-04-17 20:14:31 | MASTER-SAAO | (03h 26m 56.37s , -54d 00m 25.0s) | C | 60 | 15.9 |\n 5410 | 2024-04-17 20:15:51 | MASTER-SAAO | (03h 16m 56.49s , -57d 35m 08.1s) | C | 60 | 16.6 |\n 5410 | 2024-04-17 20:15:51 | MASTER-SAAO | (03h 20m 10.64s , -57d 48m 08.3s) | C | 60 | 16.7 |\n 5510 | 2024-04-17 20:17:30 | MASTER-SAAO | (03h 07m 04.39s , -55d 39m 51.6s) | C | 60 | 16.6 |\n 5510 | 2024-04-17 20:17:30 | MASTER-SAAO | (03h 10m 08.60s , -55d 52m 56.1s) | C | 60 | 16.9 |\n 5590 | 2024-04-17 20:18:50 | MASTER-SAAO | (02h 14m 02.20s , -63d 18m 18.2s) | C | 60 | 13.0 |\n 5590 | 2024-04-17 20:18:50 | MASTER-SAAO | (02h 17m 53.23s , -63d 31m 28.1s) | C | 60 | 14.1 |\n 5669 | 2024-04-17 20:20:09 | MASTER-SAAO | (02h 58m 06.27s , -59d 27m 57.6s) | C | 60 | 16.4 |\n 5669 | 2024-04-17 20:20:09 | MASTER-SAAO | (03h 01m 30.82s , -59d 41m 04.8s) | C | 60 | 16.6 |\n 6169 | 2024-04-17 20:28:30 | MASTER-SAAO | (02h 37m 24.10s , -61d 22m 39.0s) | C | 60 | 12.7 |\n 6169 | 2024-04-17 20:28:30 | MASTER-SAAO | (02h 41m 01.66s , -61d 35m 49.8s) | C | 60 | 13.2 |\n 6593 | 2024-04-17 20:35:33 | MASTER-SAAO | (03h 17m 04.62s , -57d 33m 41.0s) | C | 60 | 17.3 |\n 6593 | 2024-04-17 20:35:33 | MASTER-SAAO | (03h 20m 18.38s , -57d 46m 44.5s) | C | 60 | 17.6 |\n 6685 | 2024-04-17 20:37:05 | MASTER-SAAO | (02h 14m 27.70s , -63d 28m 51.0s) | C | 60 | 17.1 |\n 6685 | 2024-04-17 20:37:05 | MASTER-SAAO | (02h 10m 56.62s , -63d 15m 23.0s) | C | 60 | 16.8 |\nFilter C is a clear (unfiltred) band.\n\n\nThe observation and reduction will continue.\nThe message may be cited.\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/36160.",
"published": "2024-04-18T15:16:15.627817Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-04-18T15:16:15.627832Z",
"modified": "2024-04-18T15:16:15.636232Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6658,
"topic": "gcn.circular",
"uuid": "10a65f4d-c44f-4f1d-aa80-7665fbd826f8",
"title": "EP240417a: EP-WXT detection of a fast X-ray transient ",
"submitter": "Hop gcn.circular",
"authors": "EP Team at NAOC/CAS <ep_ta@bao.ac.cn>",
"data": {
"date": "24/04/18 16:56:42 GMT",
"from": "EP Team at NAOC/CAS <ep_ta@bao.ac.cn>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/36161"
},
"title": "GCN CIRCULAR",
"number": "36161",
"subject": "EP240417a: EP-WXT detection of a fast X-ray transient "
},
"message_text": "J. W. Hu, W. Chen, S. Q. Jiang, C. C. Jin, Y. Liu, Z. X. Ling, C. Zhang, H. Q. Cheng, C. Z. Cui, D. W. Fan, H. B. Hu, M. H. Huang, D. Y. Li, T. Y. Lian, H. Y. Liu, M. J. Liu, Z. Z. Lv, X. Mao, H. W. Pan, X. Pan, H. Sun, W. X. Wang, Y. L. Wang, Q. Y. Wu, X. P. Xu, Y. F. Xu, H. N. Yang, W. Yuan, M. Zhang, W. D. Zhang, W. J. Zhang, Z. Zhang, D. H. Zhao (NAOC, CAS), E. Kuulkers, A. Santovincenzo (ESA), P. O'Brien (Univ. of Leicester), K. Nandra, A. Rau (MPE), B. Cordier (CEA), on behalf of the Einstein Probe team. \n\nWe report on the detection of a fast X-ray transient EP240417a at 2024-04-17T15:12:33 (UTC) by the Wide-field X-ray Telescope (WXT) onboard the Einstein Probe (EP) mission during a calibration observation. The position of the source is R.A. = 177.442 deg, DEC = -15.438 deg (J2000) with an uncertainty of 3 arcmin (radius, 90% C.L. statistical and systematic). The flare lasted for at least 1500 seconds, with the tail of the fading light curve undetected due to the interruption of the observation. The peak flux reached ~3 x 10^-10 erg/s/cm^2 in the 0.5-4.0 keV band. The averaged 0.5-4.0 keV spectrum can be well fitted with a single power law of photon index 1.15(-0.26/+0.27), and the best-fit absorption column density is consistent with 0. The derived average 0.5-4.0 keV flux is 9.8(-0.8/+0.8) x 10^-11 erg/s/cm^2. The uncertainties are at the 90% confidence level for the above parameters.\n \nNo previously known bright X-ray sources are found within the error circle around the source position. The derived source parameters may be subject to larger uncertainties than those quoted here since the in-orbit calibration of the instrument is still in progress.\n\nFurther follow-up observations are encouraged to identify the nature of this X-ray transient.\n\nThe above observation was made with EP-WXT during the commissioning phase. Launched on January 9, 2024, EP is a space X-ray observatory to monitor the soft X-ray sky with X-ray follow-up capability (Yuan et al. 2022, Handbook of X-ray and Gamma-ray Astrophysics). EP is a mission of the Chinese Academy of Sciences in collaboration with ESA, MPE and CNES.\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/36161.",
"published": "2024-04-18T16:57:00.645726Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-04-18T16:57:00.645738Z",
"modified": "2024-04-18T16:57:00.652965Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6659,
"topic": "gcn.circular",
"uuid": "30f2b1c0-3d03-4a4d-8452-380a2701c51e",
"title": "GRB 240418A: Swift detection of a burst",
"submitter": "Hop gcn.circular",
"authors": "Simone Dichiara at Pennsylvania State University <sbd5667@psu.edu>",
"data": {
"date": "24/04/18 20:36:44 GMT",
"from": "Simone Dichiara at Pennsylvania State University <sbd5667@psu.edu>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/36162"
},
"title": "GCN CIRCULAR",
"number": "36162",
"subject": "GRB 240418A: Swift detection of a burst"
},
"message_text": "\nM. H. Siegel (PSU), S. Dichiara (PSU), J.D. Gropp (PSU),\nF. E. Marshall (NASA/GSFC), D. M. Palmer (LANL) and\nM. A. Williams (PSU) report on behalf of the Neil Gehrels Swift\nObservatory Team:\n\nAt 20:24:08 UT, the Swift Burst Alert Telescope (BAT) triggered and\nlocated GRB 240418A (trigger\u001222885). Swift slewed immediately to the burst.\nThe BAT on-board calculated location is\nRA, Dec 239.322, +23.607 which is\n RA(J2000) = 15h 57m 17s\n Dec(J2000) = +23d 36' 26\"\nwith an uncertainty of 3 arcmin (radius, 90% containment, including\nsystematic uncertainty). The BAT light curve showed a complex\nstructure with a duration of at least 20 sec. The peak count rate\nwas ~700 counts/sec (15-350 keV), at ~7 sec after the trigger.\n\nThe XRT began observing the field at 20:26:10.4 UT, 122.2 seconds after\nthe BAT trigger. Using promptly downlinked data we find an uncatalogued\nX-ray source located at RA, Dec 239.37228, 23.59581 which is equivalent\nto:\n RA(J2000) = 15h 57m 29.35s\n Dec(J2000) = +23d 35' 44.9\"\nwith an uncertainty of 6.5 arcseconds (radius, 90% containment). This\nlocation is 170 arcseconds from the BAT onboard position, within the\nBAT error circle. This position may be improved as more data are\nreceived; the latest position is available at\nhttps://www.swift.ac.uk/sper. We cannot determine whether the source\nis fading at the present time.\n\nA power-law fit to a spectrum formed from promptly downlinked event\ndata gives a column density consistent with the Galactic value of 5.26\nx 10^20 cm^-2 (Willingale et al. 2013).\n\nUVOT took a finding chart exposure of 150 seconds with the White filter\nstarting 125 seconds after the BAT trigger. No credible afterglow candidate has\nbeen found in the initial data products. The 2.7'x2.7' sub-image covers none of\nthe XRT error circle. The 8'x8' region for the list of sources generated\non-board covers 100% of the XRT error circle. The list of sources is typically\ncomplete to about 18 mag. No correction has been made for the expected\nextinction corresponding to E(B-V) of 0.058.\n\nBurst Advocate for this burst is M. H. Siegel (siegel AT swift.psu.edu).\nPlease contact the BA by email if you require additional information\nregarding Swift followup of this burst. In extremely urgent cases, after\ntrying the Burst Advocate, you can contact the Swift PI by phone (see\nSwift TOO web site for information: http://www.swift.psu.edu/)\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/36162.",
"published": "2024-04-18T20:37:00.293342Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-04-18T20:37:00.293354Z",
"modified": "2024-04-18T20:37:00.322641Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6243,
"topic": "gcn.circular",
"uuid": "ca9be883-47e9-411c-8b0d-8bd1f72271e0",
"title": "X-ray transient EP240315a: Montarrenti Observatory optical upper limit",
"submitter": "Hop gcn.circular",
"authors": "Simone Leonini at Montarrenti Observatory (Siena, Italy) <s.leonini@iol.it>",
"data": {
"date": "24/03/17 14:48:52 GMT",
"from": "Simone Leonini at Montarrenti Observatory (Siena, Italy) <s.leonini@iol.it>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35944"
},
"title": "GCN CIRCULAR",
"number": "35944",
"subject": "X-ray transient EP240315a: Montarrenti Observatory optical upper limit"
},
"message_text": "S. Leonini, M. Conti, P. Rosi, L.M. Tinjaca Ramirez (Montarrenti Observatory, Siena, Italy, part of UAI/SSV-GRB section), M.G. Dainotti (National Astronomical Observatory of Japan), Y. Niino (Tokyo University, Institute of Astronomy), K. Kalinowski (Aarhus University, Department of Physics and Astronomy) and B. De Simone (Universita' degli Studi Di Salerno) report:\n\nWe observed the field of the possible optical countepart of the X-ray transient EP240315a (Einstein Probe, GCN 35931, Zhang et al.; GCN 35932, GCN 35933, Srivastav et al.; GCN 35935, Jiang et al.; GCN 35937, Rau; GCN 35938, Chen et al.) with the automated and remoted 0.53m Ritchey-Chretien telescope at Montarrenti Observatory (Siena, Italy, IAU code C88).\n\nThe observations were started at 2024-03-16 20:10:21 UT (approximately 24 hours after the discovery of the X-ray transient) stacking 32x40s V and Rc-band CCD images.\n\nWe have not found any optical transient candidate within the error-box of the EP mission position with the following upper limit:\n\n MJD Filter Limit SNR\n60385.8572 V > 20.43 6.9\n60385.8578 Rc > 20.90 5.4\n\nMagnitude was calibrated with the nearby PanSTAR stars converted using Lupton (2005) equations. No correction for galactic dust extinction was applied.\n\n\n\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35944.",
"published": "2024-03-17T14:49:13.897678Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-17T14:49:13.897693Z",
"modified": "2024-03-17T14:49:13.904022Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6244,
"topic": "gcn.circular",
"uuid": "5d761e4a-b863-4d15-8724-f977d80eeecb",
"title": "X-ray transient EP240315a: Kitab observatory optical upper limitns",
"submitter": "Hop gcn.circular",
"authors": "Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>",
"data": {
"date": "24/03/17 16:17:06 GMT",
"from": "Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35945"
},
"title": "GCN CIRCULAR",
"number": "35945",
"subject": "X-ray transient EP240315a: Kitab observatory optical upper limitns"
},
"message_text": "N. Pankov (HSE, IKI), A. Schmalz (KIAM), A. Pozanenko (IKI), S. Belkin (IKI), A. Volnova (IKI), A. Novichonok (Petrozavodsk State University, KIAM) report on behalf of IKI GRB FuN:\n\nWe observed the field of the optical counterpart of the X-ray transient EP240315a (Einstein Probe, GCN 35931, Zhang et al.; GCN 35932, GCN 35933, Srivastav et al.; GCN 35935, Jiang et al.; GCN 35937, Rau; GCN 35938, Chen et al.; GCN 35944, Leonini et al.) with Kitab-ISON RC-36 telescope starting on 2024-03-16 (UT) 18:00:00 in Clear filter. We do not detect the optical afterglow (Srivastav et al., GCN 35932) at redshift of z = 4.859 (Saccardi et al., GCN 35936). Preliminary photometry of the filed is following\n\nDate UT start t-T0 Filter Exp. OT Err. UL(3sigma)\n (mid, days) (s)\n\n2024-03-16 18:00:00 0.91685 Clear 22*60 n/d n/d 19.2\n\nThe photometry is based on the nearby USNO-B1.0 (R2) stars.\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35945.",
"published": "2024-03-17T16:17:19.447537Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-17T16:17:19.447551Z",
"modified": "2024-03-17T16:17:19.455132Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6660,
"topic": "gcn.circular",
"uuid": "ec5642a8-0f73-496e-87bf-f7fd6285d8e3",
"title": "Swift GRB240418.85: Global MASTER-Net observations report",
"submitter": "Hop gcn.circular",
"authors": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"data": {
"date": "24/04/18 20:37:07 GMT",
"from": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/36163"
},
"title": "GCN CIRCULAR",
"number": "36163",
"subject": "Swift GRB240418.85: Global MASTER-Net observations report"
},
"message_text": "V. Lipunov, V.Kornilov, E. Gorbovskoy, K. Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, V.Senik, D. Vlasenko,\nG.Antipov, D.Zimnukhov, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov, D. Cheryasov, Ya.Kechin, Yu.Tselik, A. Sosnovskij\n(Lomonosov Moscow State University, SAI, Physics Department),\n\nR. Podesta, C.Lopez, F. Podesta, C.Francile\n(Observatorio Astronomico Felix Aguilar OAFA),\n\nR. Rebolo, M. Serra\n(The Instituto de Astrofisica de Canarias),\n\nD. Buckley\n(South African Astronomical Observatory),\n\nO.A. Gress, N.M. Budnev, O.Ershova\n(Irkutsk State University, API),\n\nL.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez,\nA.R.Corella, L.H.Rodriguez\n(INAOE, Guillermo Haro Astrophysics Observatory),\n\nA. Tlatov, D. Dormidontov\n(Kislovodsk Solar Station of the Pulkovo Observatory),\n\nV. Yurkov, A. Gabovich\n(Blagoveschensk Educational State University)\n\nMASTER-Kislovodsk robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) was pointed to the Swift GRB240418.85 (trigger No 1222885,15h 57m 17.26s , +23d 36m 26.3s, R=0.05) errorbox 18 sec after notice time and 78 sec after trigger time at 2024-04-18 20:25:26 UT, with upper limit up to 17.8 mag. The observations began at zenith distance = 41 deg. The sun altitude is -34.9 deg.\n\nThe galactic latitude b = 48 deg., longitude l = 39 deg.\n\n\nReal time updated cover map and OT discovered available here:\nhttps://master.sai.msu.ru/site/master2/observ.php?id$26906\n\nWe obtain a following upper limits.\n\nTmid-T0 | Site |Filt.| Expt. | Limit| Comment\n_________|_____________________|_____|_______|______|________\n\n 88 | MASTER-Kislovodsk | P| | 20 | 17.0 |\n 98 | MASTER-Kislovodsk | P| | 40 | 17.3 | Coadd\n 171 | MASTER-Kislovodsk | P| | 10 | 16.5 |\n 202 | MASTER-Kislovodsk | P| | 10 | 16.5 |\n 236 | MASTER-Kislovodsk | P| | 20 | 17.0 |\n 275 | MASTER-Kislovodsk | P| | 30 | 17.3 |\n 331 | MASTER-Kislovodsk | P| | 40 | 17.5 |\n 395 | MASTER-Kislovodsk | P| | 50 | 17.5 |\n 470 | MASTER-Kislovodsk | P| | 60 | 17.8 |\n\n\nThe observation and reduction will continue.\nThe message may be cited.\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/36163.",
"published": "2024-04-18T20:37:12.357757Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-04-18T20:37:12.357768Z",
"modified": "2024-04-18T20:37:12.363447Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6661,
"topic": "gcn.circular",
"uuid": "7761a7b8-d77e-4979-a1c8-8524b83406c3",
"title": "GRB 240411A: GOTO early optical upper limits",
"submitter": "Hop gcn.circular",
"authors": "Ben Gompertz at U of Birmingham <b.gompertz@bham.ac.uk>",
"data": {
"date": "24/04/18 20:43:43 GMT",
"from": "Ben Gompertz at U of Birmingham <b.gompertz@bham.ac.uk>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/36164"
},
"title": "GCN CIRCULAR",
"number": "36164",
"subject": "GRB 240411A: GOTO early optical upper limits"
},
"message_text": "B. P. Gompertz, D. Steeghs, B. Godson; R. Starling, K. Ackley; M. J. Dyer; J. Lyman; K. Ulaczyk; F. Jimenez-Ibarra; A. Kumar; D. O'Neill; D. K. Galloway; V. Dhillon; P. O'Brien; G. Ramsay; K. Noysena; R. Kotak; R. P. Breton; L. K. Nuttall; E. Pall'e and D. Pollacco report on behalf of the GOTO collaboration:\n\nWe report on observations with the Gravitational-wave Optical Transient Observer (GOTO; Steeghs et al. 2022) in response to GRB 240411A (Fermi GBM Team, GCN 36061; Pal et al., GCN 36068; Cheung et al., 36141). Targeted observations began at 01:57:29 UT on 2024-04-11, 12 minutes after the GBM trigger. Each observation consisted of 4x90s exposures in the GOTO L-band (400-700 nm).\n\nImages were processed immediately after acquisition using the GOTO pipeline. Difference imaging was performed using recent survey observations of the same pointings. Source candidates were initially filtered using a classifier (Killestein et al. 2021) and cross-matched against a variety of contextual and minor planet catalogues. Human vetting was carried out in real time on any candidates that passed the above checks.\n\nNo new candidate transient events are identified within the refined IPN error box (Kozyrev et al., GCN 36156). The 5-sigma limiting magnitude of the image is L > 19.7 at 12 minutes after trigger.\n\nMagnitudes were calibrated using ATLAS-REFCAT2 (Tonry et al. 2018) and are not corrected for Galactic extinction.\n\nGOTO (https://goto-observatory.org) is a network of telescopes that is principally funded by the STFC and operated at the Roque de los Muchachos Observatory on La Palma, Spain, and Siding Spring Observatory in NSW, Australia, on behalf of a consortium including the University of Warwick, Monash University, Armagh Observatory & Planetarium, the University of Leicester, the University of Sheffield, the National Astronomical Research Institute of Thailand (NARIT), the University of Turku, the University of Portsmouth, the University of Manchester and the Instituto de Astrofisica de Canarias (IAC).\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/36164.",
"published": "2024-04-18T20:43:53.103664Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-04-18T20:43:53.103678Z",
"modified": "2024-04-18T20:43:53.110019Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6245,
"topic": "gcn.circular",
"uuid": "d92ca493-1e1d-43ce-861f-9093f6448ddb",
"title": "GRB 240315B: AstroSat CZTI detection",
"submitter": "Hop gcn.circular",
"authors": "Gaurav Waratkar at IIT Bombay <gauravwaratkar24@gmail.com>",
"data": {
"date": "24/03/17 16:20:24 GMT",
"from": "Gaurav Waratkar at IIT Bombay <gauravwaratkar24@gmail.com>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35946"
},
"title": "GCN CIRCULAR",
"number": "35946",
"subject": "GRB 240315B: AstroSat CZTI detection"
},
"message_text": "J. Joshi (IUCAA), G. Waratkar (IITB), A. Vibhute (IUCAA), V. Bhalerao (IITB), D. Bhattacharya (Ashoka University/IUCAA), A. R. Rao (IUCAA/TIFR), and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:\n\nAnalysis of AstroSat CZTI data with the CIFT framework (Sharma et al., 2021, JApA, 42, 73) showed the detection of a long-duration GRB 240315B.\n\nThe source was clearly detected in the CZT detectors in the 20-200 keV energy range. The light curve showed multiple peaks of emission with the strongest peak at 2024-03-15 21:46:05.50 UTC. The measured peak count rate associated with the burst is 74 (+33, -6) counts/s above the background in the combined data of three quadrants (out of four), with a total of 1069 (+247, -264) counts. The local mean background count rate was 209 (+2, -2) counts/s. Using cumulative rates, we measure a T90 of 34 (+3, -6) s.\n\nThe source was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range. The light curve showed multiple peaks of emission with the strongest peak at 2024-03-15 21:45:58.81 UTC. The measured peak count rate associated with the burst is 224 (+66, -32) counts/s above the background in the combined data of all quadrants, with a total of 2900 (+431, -469) counts. The local mean background count rate was 1256 (+4, -5) counts/s. We measure a T90 of 28 (+2, -3) s from the cumulative Veto light curve.\n\nCZTI is built by a TIFR-led consortium of institutes across India, including VSSC, URSC, IUCAA, SAC, and PRL. The Indian Space Research Organisation funded, managed, and facilitated the project.\n\nCZTI GRB detections are reported regularly on the payload site at:\nhttp://astrosat.iucaa.in/czti/?q=grb\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35946.",
"published": "2024-03-17T16:20:38.696359Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-17T16:20:38.696372Z",
"modified": "2024-03-17T16:20:38.702757Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6246,
"topic": "gcn.circular",
"uuid": "ebd581e3-7592-4b8a-9744-f1ea74fb48d3",
"title": "GRB 240317A: AstroSat CZTI detection",
"submitter": "Hop gcn.circular",
"authors": "Gaurav Waratkar at IIT Bombay <gauravwaratkar24@gmail.com>",
"data": {
"date": "24/03/17 16:22:39 GMT",
"from": "Gaurav Waratkar at IIT Bombay <gauravwaratkar24@gmail.com>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35947"
},
"title": "GCN CIRCULAR",
"number": "35947",
"subject": "GRB 240317A: AstroSat CZTI detection"
},
"message_text": "J. Joshi (IUCAA), G. Waratkar (IITB), A. Vibhute (IUCAA), V. Bhalerao (IITB), D. Bhattacharya (Ashoka University/IUCAA), A. R. Rao (IUCAA/TIFR), and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:\n\nAnalysis of AstroSat CZTI data with the CIFT framework (Sharma et al., 2021, JApA, 42, 73) showed the detection of a long-duration GRB 240317A which was also detected by Fermi GBM (Fermi-GBM team, GCN Circ. 35939).\n\nThe source was clearly detected in the CZT detectors in the 20-200 keV energy range. The light curve peaks at 2024-03-17 09:44:00.50 UTC. The measured peak count rate associated with the burst is 216 (+47, -19) counts/s above the background in the combined data of all quadrants, with a total of 1230 (+201, -216) counts. The local mean background count rate was 383 (+3, -3) counts/s. Using cumulative rates, we measure a T90 of 10 (+2, -4) s. We caution that there is a 0.3 s readout dead time in CZTI data just after the burst. Hence, the T90 can be as large as 13 s for this GRB, with a lower limit of 6 s as estimated above by cumulative rates.\n\nThe source was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range. The light curve peaks at 2024-03-17 09:43:58.74 UTC. The measured peak count rate associated with the burst is 408 (+77, -67) counts/s above the background in the combined data of all quadrants, with a total of 2969 (+539, -536) counts. The local mean background count rate was 1833 (+8, -9) counts/s. We measure a T90 of 17 (+3, -4) s from the cumulative Veto light curve.\n\nCZTI is built by a TIFR-led consortium of institutes across India, including VSSC, URSC, IUCAA, SAC, and PRL. The Indian Space Research Organisation funded, managed, and facilitated the project.\n\nCZTI GRB detections are reported regularly on the payload site at:\nhttp://astrosat.iucaa.in/czti/?q=grb\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35947.",
"published": "2024-03-17T16:22:46.925479Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-17T16:22:46.925491Z",
"modified": "2024-03-17T16:22:46.931538Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6662,
"topic": "gcn.circular",
"uuid": "1d6fc255-7977-404e-bd30-1a4521450c0e",
"title": "GRB 240418A: AKO Upper Limit",
"submitter": "Hop gcn.circular",
"authors": "Mohammad Odeh at Al Khatim Observatory M44 <mshodeh@gmail.com>",
"data": {
"date": "24/04/18 21:54:58 GMT",
"from": "Mohammad Odeh at Al Khatim Observatory M44 <mshodeh@gmail.com>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/36165"
},
"title": "GCN CIRCULAR",
"number": "36165",
"subject": "GRB 240418A: AKO Upper Limit"
},
"message_text": "Mohammad Odeh (Al-Khatim Observatory, AKO, operated by the International\nAstronomical Center in Abu Dhabi, UAE) and Nidhal Guessoum (American\nUniversity of Sharjah, UAE), report:\n\nWe observed the field of GRB 240418A (Siegel et al., GCN 36162) with our\n0.36m f/7.7 robotic telescope.\n\nWe obtained 13x180s images using Ic filter on 18 April 2024, starting at\n21:06UT, 42 minutes after the GRB trigger.\n\nWe did not detect any credible afterglow candidate within the updated XRT\nposition (Trigger number 1222885), down to the magnitude = 20.0 for the\nstacked images.\n\nThe magnitude was estimated using the Atlas catalogue as a reference, and\nit is not corrected for galactic extinction.\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/36165.",
"published": "2024-04-18T21:55:14.140148Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-04-18T21:55:14.140162Z",
"modified": "2024-04-18T21:55:14.148020Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6248,
"topic": "gcn.circular",
"uuid": "e25c3755-c38a-4821-b860-997ed29a5cf3",
"title": "GRB 240318A: Fermi GBM Final Real-time Localization",
"submitter": "Hop gcn.circular",
"authors": "Fermi GBM Team at MSFC/Fermi-GBM <do_not_reply@GIOC.nsstc.nasa.gov>",
"data": {
"date": "24/03/18 03:01:31 GMT",
"from": "Fermi GBM Team at MSFC/Fermi-GBM <do_not_reply@GIOC.nsstc.nasa.gov>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35949"
},
"title": "GCN CIRCULAR",
"number": "35949",
"subject": "GRB 240318A: Fermi GBM Final Real-time Localization"
},
"message_text": "The Fermi GBM team reports the detection of a likely LONG GRB\n\nAt 02:51:01 UT on 18 Mar 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 240318A (trigger 732423066.81932 / 240318119).\n\nThe on-ground calculated location, using the Fermi GBM trigger data, is RA = 275.1, Dec = -5.0 (J2000 degrees, equivalent to J2000 18h 20m, -5d 00'), with a statistical uncertainty of 4.8 degrees.\n\nThe angle from the Fermi LAT boresight is 53.0 degrees.\n\nThe skymap can be found here:\nhttps://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240318119/quicklook/glg_skymap_all_bn240318119.png\n\nThe HEALPix FITS file, including the estimated localization systematic, can be found here:\nhttps://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240318119/quicklook/glg_healpix_all_bn240318119.fit\n\nThe GBM light curve can be found here:\nhttps://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240318119/quicklook/glg_lc_medres34_bn240318119.gif\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35949.",
"published": "2024-03-18T03:01:47.102635Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-18T03:01:47.102654Z",
"modified": "2024-03-18T03:01:47.109071Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6249,
"topic": "gcn.circular",
"uuid": "02e18e18-03b5-431f-af4e-43032b80983d",
"title": "Fermi GRB 240318A: Global MASTER-Net observations report",
"submitter": "Hop gcn.circular",
"authors": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"data": {
"date": "24/03/18 03:30:37 GMT",
"from": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35950"
},
"title": "GCN CIRCULAR",
"number": "35950",
"subject": "Fermi GRB 240318A: Global MASTER-Net observations report"
},
"message_text": "V. Lipunov, V.Kornilov, E. Gorbovskoy, K. Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, V.Senik, D. Vlasenko,\nG.Antipov, D.Zimnukhov, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov, D. Cheryasov, Ya.Kechin, Yu.Tselik, A. Sosnovskij\n(Lomonosov Moscow State University, SAI, Physics Department),\n\nR. Podesta, C.Lopez, F. Podesta, C.Francile\n(Observatorio Astronomico Felix Aguilar OAFA),\n\nR. Rebolo, M. Serra\n(The Instituto de Astrofisica de Canarias),\n\nD. Buckley\n(South African Astronomical Observatory),\n\nO.A. Gress, N.M. Budnev, O.Ershova\n(Irkutsk State University, API),\n\nL.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez,\nA.R.Corella, L.H.Rodriguez\n(INAOE, Guillermo Haro Astrophysics Observatory),\n\nA. Tlatov, D. Dormidontov\n(Kislovodsk Solar Station of the Pulkovo Observatory),\n\nV. Yurkov, A. Gabovich\n(Blagoveschensk Educational State University)\n\nMASTER-Tavrida robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Lomonosov MSU, SAI Crimea astronomical station) started inspect of the Fermi GRB 240318A ( Fermi GBM team, GCN 35949) errorbox 45 sec after notice time and 77 sec after trigger time at 2024-03-18 02:52:19 UT, with upper limit up to 16.6 mag. Observations started at twilight. The observations began at zenith distance = 55 deg. The sun altitude is -11.1 deg.\n\nMASTER-SAAO robotic telescope located in South Africa (South African Astronomical Observatory) started inspect of the Fermi GRB 240318A errorbox 52 sec after notice time and 84 sec after trigger time at 2024-03-18 02:52:25 UT, with upper limit up to 17.6 mag. The observations began at zenith distance = 47 deg. The sun altitude is -23.4 deg.\n\nThe galactic latitude b = 4 deg., longitude l = 25 deg.\n\n\nReal time updated cover map and OT discovered available here:\nhttps://master.sai.msu.ru/site/master2/observ.php?id$01036\n\nWe obtain a following upper limits.\n\nTmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment\n_________|_____________________|_____________________|____________________________________|_____|_______|_______|________\n\n 88 | 2024-03-18 02:52:19 | MASTER-Tavrida | (18h 47m 01.74s , -04d 52m 07.6s) | C | 20 | 16.5 |\n 94 | 2024-03-18 02:52:25 | MASTER-SAAO | (18h 42m 40.28s , -05d 38m 11.7s) | C | 20 | 17.5 |\n 94 | 2024-03-18 02:52:25 | MASTER-SAAO | (18h 40m 48.53s , -05d 24m 58.7s) | C | 20 | 17.4 |\n 117 | 2024-03-18 02:52:48 | MASTER-Tavrida | (18h 47m 05.23s , -04d 51m 08.3s) | C | 20 | 16.5 |\n 134 | 2024-03-18 02:53:05 | MASTER-SAAO | (18h 42m 40.33s , -05d 38m 08.3s) | C | 20 | 17.5 |\n 134 | 2024-03-18 02:53:05 | MASTER-SAAO | (18h 40m 48.53s , -05d 24m 54.8s) | C | 20 | 17.4 |\n 149 | 2024-03-18 02:53:16 | MASTER-Tavrida | (18h 46m 58.27s , -04d 51m 41.1s) | C | 30 | 16.6 |\n 178 | 2024-03-18 02:53:44 | MASTER-SAAO | (18h 42m 40.38s , -05d 38m 05.3s) | C | 30 | 17.6 |\n 178 | 2024-03-18 02:53:44 | MASTER-SAAO | (18h 40m 48.53s , -05d 24m 51.9s) | C | 30 | 17.6 |\n 187 | 2024-03-18 02:53:53 | MASTER-Tavrida | (18h 46m 58.14s , -04d 50m 44.1s) | C | 30 | 16.6 |\n 228 | 2024-03-18 02:54:29 | MASTER-Tavrida | (18h 47m 04.89s , -04d 51m 46.9s) | C | 40 | 16.6 |\n 232 | 2024-03-18 02:54:34 | MASTER-SAAO | (18h 42m 40.45s , -05d 38m 02.3s) | C | 40 | 17.6 |\n 232 | 2024-03-18 02:54:34 | MASTER-SAAO | (18h 40m 48.53s , -05d 24m 48.9s) | C | 40 | 17.6 |\n 282 | 2024-03-18 02:55:18 | MASTER-Tavrida | (18h 46m 57.52s , -04d 52m 50.5s) | C | 50 | 16.5 |\n 345 | 2024-03-18 02:56:16 | MASTER-Tavrida | (18h 47m 03.45s , -04d 52m 44.2s) | C | 60 | 16.5 |\n 648 | 2024-03-18 03:00:49 | MASTER-Tavrida | (18h 22m 27.68s , -04d 26m 36.6s) | C | 120 | 16.4 |\n 787 | 2024-03-18 03:02:59 | MASTER-Tavrida | (18h 22m 25.32s , -04d 25m 45.6s) | C | 140 | 16.3 |\nFilter C is a clear (unfiltred) band.\n\n\nThe observation and reduction will continue.\nThe message may be cited.\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35950.",
"published": "2024-03-18T03:30:52.422210Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-18T03:30:52.422225Z",
"modified": "2024-03-18T03:30:52.427514Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6250,
"topic": "gcn.circular",
"uuid": "a425dd73-be6a-4991-acdd-06274e584daa",
"title": "X-ray transient EP240315a: EP-FXT detection of the X-ray afterglow",
"submitter": "Hop gcn.circular",
"authors": "EP Team at NAOC/CAS <ep_ta@bao.ac.cn>",
"data": {
"date": "24/03/18 13:38:26 GMT",
"from": "EP Team at NAOC/CAS <ep_ta@bao.ac.cn>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35951"
},
"title": "GCN CIRCULAR",
"number": "35951",
"subject": "X-ray transient EP240315a: EP-FXT detection of the X-ray afterglow"
},
"message_text": "Y. Chen, S.M. Jia, W.W. Cui, C.K. Li, D.W. Han, J. Wang, W. Li, X.F. Zhao, J.J. Xu, H.S. Zhao, J. Guan, J. Zhang, L.M. Song, F.J. Lu, C.Z. Liu, S.N. Zhang (IHEP, CAS), W.J. Zhang, X. Mao, W.D. Zhang, D.Y. Li, T.Y. Lian, Y. Liu, W. Yuan (NAOC, CAS), K. Nandra, A. Rau, P. Friedrich, N. Meidinger, V. Burwitz (MPE), E. Kuulkers, Andrea Santovincenzo (ESA), P. O'Brien (UoL) and B. Cordier (CEA) on behalf of the Einstein Probe team\n\n\nFollowing the detection of the fast X-ray transient EP240315a (Zhang et al., GCN 35931) and its optical counterpart (Srivastav et al., GCN 35932, 35933; Jiang et al., GCN 35935; Saccardi et al., GCN 35936; Rau GCN 35937; Chen GCN 35938; Lipunov, GCN 35940; Leonini et al., GCN 35944; Pankov et al., GCN 35945), we performed observations of EP240315a with the Follow-up X-ray Telescope (FXT) on board the Einstein Probe mission. The observations began at 2024-03-17T14:10:00, about 42 hours after the EP-WXT detection. The exposure time is 3758 seconds. An X-ray afterglow was detected at R.A. = 141.6483 deg, DEC = -9.5335 deg, with an uncertainty of 10 arcsec (radius, 90% C.L. statistical and systematic), 3.2 arcsec away from the position of the optical counterpart AT2024eju (Srivastav et al., GCN 35932). The spectrum can be fitted with an absorbed power-law model with NH fixed at the Galactic value of 4.2E20 cm-2 and a photon index of 1.4(-0.5, +0.5). The derived flux in 0.3-10 keV is 1.8(-0.7, +1.4)E-13 erg/s/cm2 (90% C.L.). There is no cataloged X-ray source within the error circle, consistent with this source being the afterglow of EP240315a. Daily monitoring of the source with FXT is planned over the next few days. \n \nPlease note that EP-FXT is currently undergoing in-flight calibration. The derived source parameters may be subject to larger uncertainties, so please use them with caution. Launched on January 9, 2024, EP is a space X-ray observatory to monitor the soft X-ray sky with X-ray follow-up capability (Yuan et al. 2022, Handbook of X-ray and Gamma-ray Astrophysics). EP is a mission of the Chinese Academy of Sciences in collaboration with ESA, MPE and CNES.\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35951.",
"published": "2024-03-18T13:38:41.874513Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-18T13:38:41.874527Z",
"modified": "2024-03-18T13:38:41.883633Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6251,
"topic": "gcn.circular",
"uuid": "e87c732a-836f-44d2-b83b-0023cf1413ed",
"title": "X-ray transient EP240315a/AT2024eju: TShAO (Zeiss-1000) observatory optical upper limit",
"submitter": "Hop gcn.circular",
"authors": "Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>",
"data": {
"date": "24/03/18 14:52:47 GMT",
"from": "Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35952"
},
"title": "GCN CIRCULAR",
"number": "35952",
"subject": "X-ray transient EP240315a/AT2024eju: TShAO (Zeiss-1000) observatory optical upper limit"
},
"message_text": "N. Pankov (HSE, IKI), I. Reva (FAI), A. Pozanenko (IKI), S. Belkin (IKI), A. Volnova (IKI) report on behalf of IKI GRB FuN:\n\nWe observed the field of the X-ray transient EP240315a (Zhang et al., GCN 35931) till now also detected by Follow-up X-ray Telescope of Einstein Probe (Chen et al., GCN 35951). The optical counterpart AT2024eju discovered by ATLAS (Srivastav et al., GCN 35932, 35933) and observed in optic (Jiang et al., GCN 35935; Saccardi et al., GCN 35936; Rau GCN 35937; Chen GCN 35938; Leonini et al., GCN 35944; Pankov et al., GCN 35945) was observed with Zeiss-1000 telescope of Tien Shan Astronomical Observatory stating on 2024-03-17 (UT) 14:12:06 in R filter. We do not detect the optical counterpart. Preliminary photometry of the filed is following\n\nDate UT start t-T0 Filter Exp. OT Err. UL(3sigma)\n (mid, days) (s)\n\n2024-03-17 14:12:06 1.77526 R 35*120 n/d n/d 22.3\n\nThe photometry is based on nearby USNO-B1.0 (R2) stars.\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35952.",
"published": "2024-03-18T14:53:04.948111Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-18T14:53:04.948147Z",
"modified": "2024-03-18T14:53:04.953869Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6252,
"topic": "gcn.circular",
"uuid": "9662d6aa-4181-4280-9a50-7b33257d9f52",
"title": "Swift satellite in safe mode",
"submitter": "Hop gcn.circular",
"authors": "Brad Cenko at NASA/GSFC <brad.cenko@nasa.gov>",
"data": {
"date": "24/03/18 15:02:24 GMT",
"from": "Brad Cenko at NASA/GSFC <brad.cenko@nasa.gov>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35953"
},
"title": "GCN CIRCULAR",
"number": "35953",
"subject": "Swift satellite in safe mode"
},
"message_text": "For a number of months the Swift team has been tracking increased noise in one of the three on-board gyroscopes (e.g., GCN 34633). On Friday March 15, the performance of this gyroscope degraded significantly, making it difficult for the spacecraft to acquire star tracker lock and execute successful pointed science observations. Thus the spacecraft was put into safe mode.\n\nThe Swift spacecraft was designed to accommodate the failure of one gyroscope and still meet all mission requirements. However, the on-board flight software requires a patch to allow the satellite to operate properly in two-gyroscope mode.\n\nWe are working to upload and install this patch, which we expect will return the spacecraft to full functionality, in as rapid and safe a manner as possible. Until the patch has been successfully deployed, science observations are expected to be very limited.\n\nWe will provide updates to the community as available.\n\nIf you have further questions, please feel free to reach out to the Swift PI, Brad Cenko, at brad.cenko@nasa.gov.\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35953.",
"published": "2024-03-18T15:02:36.065409Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-18T15:02:36.065436Z",
"modified": "2024-03-18T15:02:36.070162Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6253,
"topic": "gcn.circular",
"uuid": "9127ded8-e763-4392-8214-5bf568fa1d9b",
"title": "X-ray transient EP240315a: 3.6 m TNG NIR detection",
"submitter": "Hop gcn.circular",
"authors": "Youdong HU at INAF-OAB <huyoudong072@hotmail.com>",
"data": {
"date": "24/03/18 15:24:39 GMT",
"from": "Youdong HU at INAF-OAB <huyoudong072@hotmail.com>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35954"
},
"title": "GCN CIRCULAR",
"number": "35954",
"subject": "X-ray transient EP240315a: 3.6 m TNG NIR detection"
},
"message_text": "Y.-D. Hu, P. D'Avanzo, M. Ferro, R. Brivio, S. Covino, D. Fugazza, S. Campana (INAF-OAB), A. Rossi (INAF-OAS), D. B. Malesani (DAWN/NBI & Radboud Univ.), A. Melandri (INAF-OAR), L. Di Fabrizio, C. Padilla (INAF-TNG) on behalf of the CIBO collaboration report:\n\nWe observed the field of the fast X-ray transient EP240315a detected by the Einstein Probe mission (Zhang et al., GCNC 35931; Chen et al. GCNC 35951) with the Italian 3.6m TNG telescope equipped with the near-infrared camera NICS to follow up its optical counterpart AT2024eju (TNS Astronomical Transient Report No. 205383). A series of images were obtained with the H filter starting on 2024-03-17 19:58:11 UT (i.e. 2.02 days post T0). The optical counterpart (Srivastav et al., GCN 35932, 35933; Jiang et al., GCN 35935; Saccardi et al., GCN 35936; Rau GCN 35937; Chen GCN 35938; Lipunov, GCN 35940; Leonini et al., GCN 35944; Pankov et al., GCN 35945, Pankov et al. GCNC 35952) is clearly detected in the co-added image with a preliminary result of H(Vega)~19.8 mag (calibrated against the 2MASS catalogue).\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35954.",
"published": "2024-03-18T15:24:56.569265Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-18T15:24:56.569306Z",
"modified": "2024-03-18T15:24:56.580616Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6254,
"topic": "gcn.circular",
"uuid": "a677f968-98d5-4c35-b7de-854343ee87a3",
"title": "GRB 240317B: Fermi GBM Observation",
"submitter": "Hop gcn.circular",
"authors": "rachel.hamburg@ijclab.in2p3.fr",
"data": {
"date": "24/03/18 16:26:15 GMT",
"from": "rachel.hamburg@ijclab.in2p3.fr",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35955"
},
"title": "GCN CIRCULAR",
"number": "35955",
"subject": "GRB 240317B: Fermi GBM Observation"
},
"message_text": "R. Hamburg (CNRS/IN2P3/IJCLab) and C. Meegan (UAH) report on behalf of\nthe Fermi Gamma-ray Burst Monitor Team:\n\n\"At 10:54:24.02 UT on 17 March 2024, the Fermi Gamma-ray Burst Monitor (GBM)\ntriggered and located GRB 240317B (trigger 732365669/240317454),\nwhich was also detected by Swift/BAT-GUANO (DeLaunay et al. 2024, GCN 35948).\nThe Fermi GBM on-ground location is consistent with the Swift position.\n\nThe angle from the Fermi LAT boresight is 89 degrees.\n\nThe GBM light curve shows one main emission episode with a duration (T90)\nof about 35 s (50-300 keV). The time-averaged spectrum\nfrom T0-6.1 to T0+32.8 s is best fit by\na power law function with an exponential high-energy cutoff.\nThe power law index is -0.6 +/- 0.3 and the cutoff energy,\nparameterized as Epeak, is 76 +/- 9 keV.\n\nThe event fluence (10-1000 keV) in this time interval is\n(1.9 +/- 0.2)E-06 erg/cm^2. The 1-sec peak photon flux measured\nstarting from T0+3.0 s in the 10-1000 keV band is 2.3 +/- 0.4 ph/s/cm^2.\n\nThe spectral analysis results presented above are preliminary;\nfinal results will be published in the GBM GRB Catalog:\nhttps://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html\n\nFor Fermi GBM data and info, please visit the official Fermi GBM Support Page:\nhttps://fermi.gsfc.nasa.gov/ssc/data/access/gbm/\"\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35955.",
"published": "2024-03-18T16:26:31.265122Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-18T16:26:31.265144Z",
"modified": "2024-03-18T16:26:31.271077Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6665,
"topic": "gcn.circular",
"uuid": "c887e5b7-da4d-440a-8bcd-e04874ea54aa",
"title": "GRB 240418A: Enhanced Swift-XRT position",
"submitter": "Hop gcn.circular",
"authors": "Phil Evans at U of Leicester <pae9@star.le.ac.uk>",
"data": {
"date": "24/04/19 00:11:49 GMT",
"from": "Phil Evans at U of Leicester <pae9@star.le.ac.uk>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/36166"
},
"title": "GCN CIRCULAR",
"number": "36166",
"subject": "GRB 240418A: Enhanced Swift-XRT position"
},
"message_text": "P.A. Evans, M.R. Goad, J.P. Osborne and A.P. Beardmore (U. Leicester)\nreport on behalf of the Swift-XRT team.\n\nUsing 463 s of XRT Photon Counting mode data and 1 UVOT\nimages for GRB 240418A, we find an astrometrically corrected X-ray\nposition (using the XRT-UVOT alignment and matching UVOT field sources\nto the USNO-B1 catalogue): RA, Dec = 239.37529, +23.59582 which is equivalent\nto:\n\nRA (J2000): 15h 57m 30.07s\nDec (J2000): +23d 35' 45.0\"\n\nwith an uncertainty of 3.6 arcsec (radius, 90% confidence).\n\nThis position may be improved as more data are received. The latest\nposition can be viewed at http://www.swift.ac.uk/xrt_positions. Position\nenhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans\net al. (2009, MNRAS, 397, 1177).\n\nThis circular was automatically generated, and is an official product of the\nSwift-XRT team.\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/36166.",
"published": "2024-04-19T00:12:10.433425Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-04-19T00:12:10.433445Z",
"modified": "2024-04-19T00:12:10.442425Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6255,
"topic": "gcn.circular",
"uuid": "eba32280-c8d3-4a3f-81ea-a6d161963f85",
"title": "X-ray transient EP240315a: PRIME near infrared detection",
"submitter": "Hop gcn.circular",
"authors": "Joe Durbak at UMD <gcn.joedurbak@gmail.com>",
"data": {
"date": "24/03/18 18:35:29 GMT",
"from": "Joe Durbak at UMD <gcn.joedurbak@gmail.com>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35956"
},
"title": "GCN CIRCULAR",
"number": "35956",
"subject": "X-ray transient EP240315a: PRIME near infrared detection"
},
"message_text": "O. Guiffreda (UMD), J. Durbak (UMD), A. S. Kutyrev (NASA/GSFC), E. Troja (U Rome), K. De (MIT), S. B. Cenko (NASA/GSFC)\n\nFollowing the Einstein Probe detection (GCN 35931) of EP240315a, we observed the transient field in the J filter with PRIME ~1 day after the Einstein Probe detection.\n\nAt the position of the optical transient AT2024eju reported by ATLAS (Srivastav et al. GCN 35932), we detect an uncatalogued source in J band. Using nearby VISTA Hemispherical Survey (VHS) stars for preliminary calibration we derive the following magnitude, not corrected for Galactic extinction:\n\nFilter | Mag(VISTA) | SNR | Seeing | Total exposure time (s) | UT Date-time at start\n-------|----------------|-----|--------|------------------------------------------------\nJ | 19.7 +/- 0.3 | 6.0 | 1.3â | 675 | 2024-03-16T19:14:20\n\nThis result is consistent with GROND detection (Rau GCN 35937). Conditions were intermittently cloudy, resulting in higher than usual photometric error.\n\nPRIME is a 1.8m telescope with 1.56 square degree FOV (0.5 arcsec/pixel) located in Sutherland, South Africa.\n\nFurther observations are planned.\n\nWe thank the Osaka University observers at PRIME and the staff at SAAO for their support with these observations.\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35956.",
"published": "2024-03-18T18:35:45.620645Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-18T18:35:45.620664Z",
"modified": "2024-03-18T18:35:45.627624Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6256,
"topic": "gcn.circular",
"uuid": "075a10f0-906c-427e-97a1-44628badaa59",
"title": "GRB 240318B: Glowbug gamma-ray detection",
"submitter": "Hop gcn.circular",
"authors": "C.C. Cheung at Naval Research Lab <Teddy.Cheung@nrl.navy.mil>",
"data": {
"date": "24/03/18 18:58:31 GMT",
"from": "C.C. Cheung at Naval Research Lab <Teddy.Cheung@nrl.navy.mil>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35957"
},
"title": "GCN CIRCULAR",
"number": "35957",
"subject": "GRB 240318B: Glowbug gamma-ray detection"
},
"message_text": "C.C. Cheung, R. Woolf, M. Kerr, J.E. Grove (NRL), A. Goldstein (USRA), C.A. Wilson-Hodge, D. Kocevski (MSFC), and M.S. Briggs (UAH) report:\n \nThe Glowbug gamma-ray telescope [1,2], operating on the International Space Station, reports the detection of GRB 240318B.\n \nUsing an adaptive window with a resolution of 32-ms, the burst onset is determined to be 2024-03-18 06:50:23.312 with a duration of 12.3 s and a total significance of about 17.8 sigma. The light curve comprises a single peak.\n \nUsing a standard power-law function with an exponential high-energy cutoff [3] to model the emission over this duration results in a poorly constrained power-law index and a cutoff energy (\"Epeak\") of ~1 MeV. The modeled 10-10000 keV fluence is 2.3e-06 erg/cm^2.\n \nThe best-fit localization is RA, Decl. (J2000, deg) = 261.8, -12.0 with a radius of 19.9 deg (95% confidence), with a highly uncertain systematic uncertainty.\n \nThe analysis results presented here are preliminary and use a response function that lacks a detailed characterization of the surrounding passive structure of the ISS.\n \nGlowbug is a NASA-funded technology demonstrator for sensitive, low-cost gamma-ray transient telescopes developed, built, and operated by the U.S. Naval Research Laboratory (NRL) with support from the University of Alabama in Huntsville, USRA, and NASA MSFC. It was launched on 2023 March 15 aboard the Department of Defense Space Test Programâs STP-H9 to the ISS. The detector comprises 12 large-area (15 cm x 15 cm) CsI:Tl panels covering the surface of a half cube, and two hexagonal (5-cm diameter, 10-cm length) CLLB scintillators, giving it a large field of view (instantaneous FoV ~2/3 sky) over a wide energy band of 50 keV to >2 MeV.\n \n[1] Grove, J.E. et al. 2020, Proc. Yamada Conf. LXXI, arXiv:2009.11959\n[2] Woolf, R.S. et al. 2022, Proc. SPIE, 12181, id. 121811O\n[3] Goldstein, A. et al. 2020, ApJ 895, 40, arXiv :1909.03006\n \nDistribution Statement A: Approved for public release. Distribution is unlimited.\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35957.",
"published": "2024-03-18T18:58:50.793255Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-18T18:58:50.793298Z",
"modified": "2024-03-18T18:58:50.800166Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6257,
"topic": "gcn.circular",
"uuid": "8c4f1602-aa4f-4f2d-8ee2-541a2ce8b256",
"title": "GRB 240317C: Glowbug gamma-ray detection",
"submitter": "Hop gcn.circular",
"authors": "C.C. Cheung at Naval Research Lab <Teddy.Cheung@nrl.navy.mil>",
"data": {
"date": "24/03/18 18:59:53 GMT",
"from": "C.C. Cheung at Naval Research Lab <Teddy.Cheung@nrl.navy.mil>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35958"
},
"title": "GCN CIRCULAR",
"number": "35958",
"subject": "GRB 240317C: Glowbug gamma-ray detection"
},
"message_text": "C.C. Cheung, R. Woolf, M. Kerr, J.E. Grove (NRL), A. Goldstein (USRA), C.A. Wilson-Hodge, D. Kocevski (MSFC), and M.S. Briggs (UAH) report:\n \nThe Glowbug gamma-ray telescope [1,2], operating on the International Space Station, reports the detection of GRB 240317C.\n \nUsing an adaptive window with a resolution of 32-ms, the burst onset is determined to be 2024-03-17 20:20:25.304 with a duration of 8.2 s and a total significance of about 25.8 sigma. The light curve comprises a single peak.\n \nUsing a standard power-law function with an exponential high-energy cutoff [3] to model the emission over this duration results in a poorly constrained power-law index and a cutoff energy (\"Epeak\") of 216 keV. The modeled 10-10000 keV fluence is 1.1e-06 erg/cm^2.\n \nThe best-fit localization is RA, Decl. (J2000, deg) = 314.8, -60.6 with a radius of 18.9 deg (95% confidence), with a highly uncertain systematic uncertainty.\n \nThe analysis results presented here are preliminary and use a response function that lacks a detailed characterization of the surrounding passive structure of the ISS.\n \nGlowbug is a NASA-funded technology demonstrator for sensitive, low-cost gamma-ray transient telescopes developed, built, and operated by the U.S. Naval Research Laboratory (NRL) with support from the University of Alabama in Huntsville, USRA, and NASA MSFC. It was launched on 2023 March 15 aboard the Department of Defense Space Test Programâs STP-H9 to the ISS. The detector comprises 12 large-area (15 cm x 15 cm) CsI:Tl panels covering the surface of a half cube, and two hexagonal (5-cm diameter, 10-cm length) CLLB scintillators, giving it a large field of view (instantaneous FoV ~2/3 sky) over a wide energy band of 50 keV to >2 MeV.\n \n[1] Grove, J.E. et al. 2020, Proc. Yamada Conf. LXXI, arXiv:2009.11959\n[2] Woolf, R.S. et al. 2022, Proc. SPIE, 12181, id. 121811O\n[3] Goldstein, A. et al. 2020, ApJ 895, 40, arXiv :1909.03006\n \nDistribution Statement A: Approved for public release. Distribution is unlimited.\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35958.",
"published": "2024-03-18T19:00:01.219519Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-18T19:00:01.219541Z",
"modified": "2024-03-18T19:00:01.264785Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6258,
"topic": "gcn.circular",
"uuid": "2eb9b637-489e-4ea6-9af5-efee9ce428b2",
"title": "GRB 240318A: Glowbug gamma-ray detection",
"submitter": "Hop gcn.circular",
"authors": "C.C. Cheung at Naval Research Lab <Teddy.Cheung@nrl.navy.mil>",
"data": {
"date": "24/03/18 19:01:13 GMT",
"from": "C.C. Cheung at Naval Research Lab <Teddy.Cheung@nrl.navy.mil>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35959"
},
"title": "GCN CIRCULAR",
"number": "35959",
"subject": "GRB 240318A: Glowbug gamma-ray detection"
},
"message_text": "C.C. Cheung, R. Woolf, M. Kerr, J.E. Grove (NRL), A. Goldstein (USRA), C.A. Wilson-Hodge, D. Kocevski (MSFC), and M.S. Briggs (UAH) report:\n \nThe Glowbug gamma-ray telescope [1,2], operating on the International Space Station, reports the detection of GRB 240318A, which was also detected by Fermi/GBM (GCN 35949).\n\nUsing an adaptive window with a resolution of 32-ms, the burst onset is determined to be 2024-03-18 02:51:00.832 with a duration of 5.2 s and a total significance of about 14.4 sigma. The light curve comprises a single peak.\n\nUsing a standard power-law function with an exponential high-energy cutoff [3] to model the emission over this duration results in a poorly constrained power-law index and a cutoff energy (\"Epeak\") of 163 keV. The modeled 10-10000 keV fluence is 7.6e-07 erg/cm^2.\n\nThe analysis results presented here are preliminary and use a response function that lacks a detailed characterization of the surrounding passive structure of the ISS.\n \nGlowbug is a NASA-funded technology demonstrator for sensitive, low-cost gamma-ray transient telescopes developed, built, and operated by the U.S. Naval Research Laboratory (NRL) with support from the University of Alabama in Huntsville, USRA, and NASA MSFC. It was launched on 2023 March 15 aboard the Department of Defense Space Test Programâs STP-H9 to the ISS. The detector comprises 12 large-area (15 cm x 15 cm) CsI:Tl panels covering the surface of a half cube, and two hexagonal (5-cm diameter, 10-cm length) CLLB scintillators, giving it a large field of view (instantaneous FoV ~2/3 sky) over a wide energy band of 50 keV to >2 MeV.\n \n[1] Grove, J.E. et al. 2020, Proc. Yamada Conf. LXXI, arXiv:2009.11959\n[2] Woolf, R.S. et al. 2022, Proc. SPIE, 12181, id. 121811O\n[3] Goldstein, A. et al. 2020, ApJ 895, 40, arXiv :1909.03006\n \nDistribution Statement A: Approved for public release. Distribution is unlimited.\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35959.",
"published": "2024-03-18T19:01:19.440599Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-18T19:01:19.440623Z",
"modified": "2024-03-18T19:01:19.444081Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6666,
"topic": "gcn.circular",
"uuid": "94489996-7f45-457f-8703-767594f48538",
"title": "GRB 240418A: NOT optical upper limits",
"submitter": "Hop gcn.circular",
"authors": "Daniele B. Malesani at IMAPP / Radboud University <d.malesani@astro.ru.nl>",
"data": {
"date": "24/04/19 00:50:40 GMT",
"from": "Daniele B. Malesani at IMAPP / Radboud University <d.malesani@astro.ru.nl>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/36167"
},
"title": "GCN CIRCULAR",
"number": "36167",
"subject": "GRB 240418A: NOT optical upper limits"
},
"message_text": "D. B. Malesani (DAWN/NBI and Radboud Univ.) and A. C. Casasbuenas (Univ. La Laguna and NOT) report on behalf of a larger collaboration.\n\nWe have observed the field of GRB 240418A (Siegel et al., GCN 36162) using the Nordic Optical Telescope (NOT) equipped with the ALFOSC camera. Observations were carried out under poor sky transparency, and consisted of images in the SDSS r and z bands (mean epochs 3.19 and 3.37 hr after trigger, respectively).\n\nWithin or close to the localization error circle of the X-ray afterglow (Evans et al., GCN 36166), we detect no object in either filter, down to limiting AB magnitudes r > 22, z > 20.4, calibrated against nearby stars from the Pan-STARRS catalog.\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/36167.",
"published": "2024-04-19T00:50:56.254288Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-04-19T00:50:56.254303Z",
"modified": "2024-04-19T00:50:56.262499Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6667,
"topic": "gcn.circular",
"uuid": "d7c5c845-3c0c-4360-b822-6474227ce3f2",
"title": "GRB 240418A: TSHAO Zeiss-1000 optical upper limit",
"submitter": "Hop gcn.circular",
"authors": "Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>",
"data": {
"date": "24/04/19 01:36:41 GMT",
"from": "Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/36168"
},
"title": "GCN CIRCULAR",
"number": "36168",
"subject": "GRB 240418A: TSHAO Zeiss-1000 optical upper limit"
},
"message_text": "A. Pozanenko (IKI), I. Reva (FAI), N.Pankov (HSE), S. Belkin (IKI) report on behalf of GRB-IKI-FuN:\n\nWe have observed the field of GRB 240418A (Siegel et al., GCN 36162) with Zeiss-1000 telescope of Tien Shan Astronomical Observatory starting on 2024-04-18 (UT) 21:47:25.\n\nWe do not detect any object within Enhanced Swift-XRT position (Evans et al., GCN 36166) up to R!.6. Preliminary photometry of the field in a stacked image is following.\n\nDate UT start t-T0 Filter Exp. OT Err. UL(3 sigma)\n (mid, days) (s)\n2024-04-18 21:47:25 - R 21*120 n/d n/d 21.6\n\nThe photometry is based on nearby USNO-B1.0 stars.\nNon detection of the OT is in agreement with the observations (Lipunov et al., GCN 36163; Odeh et al., GCN 36165; Malesani et al., GCN 36167).\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/36168.",
"published": "2024-04-19T01:36:56.898692Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-04-19T01:36:56.898709Z",
"modified": "2024-04-19T01:36:56.905994Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6668,
"topic": "gcn.circular",
"uuid": "85c7f41e-714d-4a53-b1fe-8e8c92d9e1dc",
"title": "GRB 240419A: Swift detection of a burst",
"submitter": "Hop gcn.circular",
"authors": "Simone Dichiara at Pennsylvania State University <sbd5667@psu.edu>",
"data": {
"date": "24/04/19 02:03:17 GMT",
"from": "Simone Dichiara at Pennsylvania State University <sbd5667@psu.edu>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/36169"
},
"title": "GCN CIRCULAR",
"number": "36169",
"subject": "GRB 240419A: Swift detection of a burst"
},
"message_text": "\nM. H. Siegel (PSU), S. Dichiara (PSU), R. Gupta (NASA/GSFC),\nJ. A. Kennea (PSU), S. Laha (GSFC/UMBC), D. M. Palmer (LANL) and\nM. A. Williams (PSU) report on behalf of the Neil Gehrels Swift\nObservatory Team:\n\nAt 01:48:01 UT, the Swift Burst Alert Telescope (BAT) triggered and\nlocated GRB 240419A (trigger\u001222955). Swift slewed immediately to the burst.\nThe BAT on-board calculated location is\nRA, Dec 94.568, -45.011 which is\n RA(J2000) = 06h 18m 16s\n Dec(J2000) = -45d 00' 40\"\nwith an uncertainty of 3 arcmin (radius, 90% containment, including\nsystematic uncertainty). The BAT light curve showed a complex\nstructure with a duration of about 4 sec. The peak count rate\nwas ~1500 counts/sec (15-350 keV), at ~1 sec after the trigger.\n\nThe XRT began observing the field at 01:49:51.1 UT, 110.1 seconds after\nthe BAT trigger. Using promptly downlinked data we find a fading,\nuncatalogued X-ray source located at RA, Dec 94.53468, -45.00073 which\nis equivalent to:\n RA(J2000) = 06h 18m 08.32s\n Dec(J2000) = -45d 00' 02.6\"\nwith an uncertainty of 3.5 arcseconds (radius, 90% containment). This\nlocation is 92 arcseconds from the BAT onboard position, within the BAT\nerror circle. This position may be improved as more data are received;\nthe latest position is available at https://www.swift.ac.uk/sper.\n\nA power-law fit to a spectrum formed from promptly downlinked event\ndata gives a column density consistent with the Galactic value of 6.63\nx 10^20 cm^-2 (Willingale et al. 2013).\n\nUVOT took a finding chart exposure of 150 seconds with the White filter\nstarting 113 seconds after the BAT trigger. No credible afterglow candidate has\nbeen found in the initial data products. The 2.7'x2.7' sub-image covers 100% of\nthe XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag.\nThe 8'x8' region for the list of sources generated on-board covers 100% of the\nXRT error circle. The list of sources is typically complete to about 18 mag. No\ncorrection has been made for the expected extinction corresponding to E(B-V) of\n0.069.\n\nBurst Advocate for this burst is M. H. Siegel (siegel AT swift.psu.edu).\nPlease contact the BA by email if you require additional information\nregarding Swift followup of this burst. In extremely urgent cases, after\ntrying the Burst Advocate, you can contact the Swift PI by phone (see\nSwift TOO web site for information: http://www.swift.psu.edu/)\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/36169.",
"published": "2024-04-19T02:03:39.512395Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-04-19T02:03:39.512413Z",
"modified": "2024-04-19T02:03:39.521388Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6259,
"topic": "gcn.circular",
"uuid": "278c2b03-ebe2-4e81-8c3c-dc777d7ab800",
"title": "X-ray transient EP240315a: GTC/OSIRIS spectroscopic redshift confirmation",
"submitter": "Hop gcn.circular",
"authors": "P.G. Jonker at Radboud University <p.jonker@astro.ru.nl>",
"data": {
"date": "24/03/18 21:46:12 GMT",
"from": "P.G. Jonker at Radboud University <p.jonker@astro.ru.nl>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35960"
},
"title": "GCN CIRCULAR",
"number": "35960",
"subject": "X-ray transient EP240315a: GTC/OSIRIS spectroscopic redshift confirmation"
},
"message_text": "J. Quirola-Vásquez (Radboud Univ.), P.G. Jonker (Radboud Univ.), A. J. Levan (Radboud Univ. & Warwick Univ.), F. E. Bauer (PUC), D. B. Malesani (DAWN/NBI and Radboud Univ.), Maria E. Ravasio (Radboud Univ.), M.A.P. Torres (IAC), A. M. GarcÃa (GTC) on behalf of a larger collaboration:\n\nWe observed the optical counterpart AT2024eju (Srivastav et al., GCN 35932) of the fast X-ray transient EP240315a reported by the Einstein Probe WXT instrument (Zhang et al., GCN 35931) and followed-up by its FXT instrument (Chen et al., GCN 35951), using the GTC/OSIRIS spectrograph. Our spectra cover the wavelength range 5100-10000 AA and consist of 3 exposures of 1200 seconds each. Observations started at 22:54:51 UT on Mar 16, 2024 (~27 hr after the X-ray trigger). We detect a faint trace, with the Lyman break and several absorption features which we identify as due to OIλ1302.17, SiIIλ1304.37, and SiIVλλ1393.76/1402.77. Therefore, we confirm the redshift identification of z = 4.859 determined by Saccardi et al. (GCN 35936) using VLT/X-shooter.\n\nWe acknowledge the excellent support from the GTC staff.\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35960.",
"published": "2024-03-18T21:46:30.416908Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-18T21:46:30.416932Z",
"modified": "2024-03-18T21:46:30.433493Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6260,
"topic": "gcn.circular",
"uuid": "f878e1c4-908f-4514-a0c0-2345f4e34c0d",
"title": "X-ray transient EP240315a: MeerKAT radio detection",
"submitter": "Hop gcn.circular",
"authors": "Francesco Carotenuto at University of Oxford <francesco.carotenuto@physics.ox.ac.uk>",
"data": {
"date": "24/03/18 21:47:26 GMT",
"from": "Francesco Carotenuto at University of Oxford <francesco.carotenuto@physics.ox.ac.uk>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35961"
},
"title": "GCN CIRCULAR",
"number": "35961",
"subject": "X-ray transient EP240315a: MeerKAT radio detection"
},
"message_text": "F. Carotenuto, J. Bright (Oxford), P. G. Jonker (Radboud), R. Fender, L. Rhodes (Oxford) report on behalf of a larger collaboration:\n\nWe observed the new Fast X-ray Transient EP240315a (Zhang et al., GCN 35931) with the MeerKAT radio telescope at 3.0 GHz for a total of 1 hour starting on 18 March 2024 at 16:53 UTC. J1939-6342 and 3C237 were used as flux and complex gain calibrators, respectively. Using the South African Radio Astronomy Observatory Science Data Pipeline image, we find an unresolved source at the position of the optical counterpart of the FXT AT2024eju (Srivastav et al., GCN 35932) with a flux density of ~30uJy/beam. The rms noise in the field is 8.5 uJy/beam. Further MeerKAT observations are planned.\n\nWe thank the staff at the South African Radio Astronomy Observatory for the rapid scheduling of these observations.\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35961.",
"published": "2024-03-18T21:47:32.624418Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-18T21:47:32.624445Z",
"modified": "2024-03-18T21:47:32.629009Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6261,
"topic": "gcn.circular",
"uuid": "75fdf51b-4de7-42ea-a5eb-6025bbf235e4",
"title": "X-ray transient EP240315a: GTC/HiPERCAM photometry",
"submitter": "Hop gcn.circular",
"authors": "P.G. Jonker at Radboud University <p.jonker@astro.ru.nl>",
"data": {
"date": "24/03/18 22:39:47 GMT",
"from": "P.G. Jonker at Radboud University <p.jonker@astro.ru.nl>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35962"
},
"title": "GCN CIRCULAR",
"number": "35962",
"subject": "X-ray transient EP240315a: GTC/HiPERCAM photometry"
},
"message_text": "P. G. Jonker (Radboud Univ.), S. Littlefair (Sheffield Uni.), F. E. Bauer (PUC), A. J. Levan (Radboud Univ. & Warwick Univ.), D. B. Malesani (DAWN/NBI and Radboud Univ.), Maria E. Ravasio (Radboud Univ.), M.A.P. Torres (IAC), V. Dhillon (Sheffield Uni.), D. GarcÃa Ãlvarez (GTC), A. M. GarcÃa (GTC), on behalf of a larger collaboration:\n\nWe observed the optical counterpart AT2024eju (Srivastav et al., GCN 35932) of the fast X-ray transient EP240315a reported by the Einstein Probe WXT instrument (Zhang et al., GCN 35931), using the GTC/HiPERCAM imager. We obtained 80 exposures of 30 seconds each in uâgârâiâzâ simultaneously. The observations started at 21:10 UT on Mar 17, 2024. We clearly detected the source in the râ, iâ, and zâ bands. \nThe zâ-band magnitude was 22 (AB mag). \n\nWe acknowledge the excellent support from the GTC staff.\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35962.",
"published": "2024-03-18T22:40:04.909768Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-18T22:40:04.909786Z",
"modified": "2024-03-18T22:40:04.915865Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6669,
"topic": "gcn.circular",
"uuid": "6b0e356a-6d89-45cf-be31-2436f5bfb166",
"title": "GRB 240419A: Prompt enhanced Swift-XRT position",
"submitter": "Hop gcn.circular",
"authors": "Phil Evans at U of Leicester <pae9@star.le.ac.uk>",
"data": {
"date": "24/04/19 02:37:35 GMT",
"from": "Phil Evans at U of Leicester <pae9@star.le.ac.uk>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/36170"
},
"title": "GCN CIRCULAR",
"number": "36170",
"subject": "GRB 240419A: Prompt enhanced Swift-XRT position"
},
"message_text": "P.A. Evans (U. Leicester) reports on behalf of the Swift-XRT team:\n\nUsing promptly downlinked XRT event data for GRB 240419A, we find an\nenhanced XRT position of the afterglow: RA, Dec: 94.53358, -44.99999\nwhich is equivalent to:\n RA (J2000) = 06 18 08.06\n Dec (J2000) = -44 59 60.0\nwith an uncertainty of 1.9 arcseconds (radius, 90% confidence).\nAnalysis of the promptly available data is online at\nhttp://www.swift.ac.uk/sper/1222955.\n\nPosition enhancement is is described by Goad et al. (2007, A&A, 476,\n1401) and Evans et al. (2009, MNRAS, 397, 1177).\n\nThis circular is an official product of the Swift-XRT team.\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/36170.",
"published": "2024-04-19T02:37:50.997024Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-04-19T02:37:50.997071Z",
"modified": "2024-04-19T02:37:51.011983Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6262,
"topic": "gcn.circular",
"uuid": "974a83cd-daa3-4a6a-94d3-7f59c95ef6ac",
"title": "X-ray transient EP 240315a: Chandra observations",
"submitter": "Hop gcn.circular",
"authors": "Andrew Levan at Radboud University <a.levan@astro.ru.nl>",
"data": {
"date": "24/03/19 11:31:23 GMT",
"from": "Andrew Levan at Radboud University <a.levan@astro.ru.nl>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35963"
},
"title": "GCN CIRCULAR",
"number": "35963",
"subject": "X-ray transient EP 240315a: Chandra observations"
},
"message_text": "A.J. Levan (Radboud & Warwick), P.G. Jonker (Radboud), D.B. Malesani (DAWN/NBI & Radboud), N.R. Tanvir (Leicester), B.P. Gompertz (Birmingham), A. Saccardi (GEPI/Obs. de Paris), A. de Ugarte Postigo (CNRS/OCA & LAM), A. Martin-Carrillo (UCD), D. Perley (LJMU), D. Xu (NAOC), G. Tagliaferri (INAF, Brera), J. Palmerio (GEPI/Obs. de Paris)), K.E. Heintz (DAWN/NBI), K. Wiersema (Hertfordshire), M. Grazia Bernardini (INAF, Brera), M. Ferro (INAF, Brera), P. Jakobbson (U. Iceland), P. DâAvanzo (INAF, Brera), R. Salvaterra (INAF, Milan), S. Vergani (GEPI/Obs. de Paris), G. Pugliese (API, Amsterdam), Y. Julakanti (Leicester) report for the Stargate collaboration: \n\nWe obtained observations of EP240315a (Zhang et al., GCN 35931) with the Chandra X-ray observatory. Observations began at 20:13 on 18 March 2024, 72 hours after the flare detection. The source was placed at the default aim point on the S3 chip for a total exposure time of 10 ks. At the location of AT2024eju (Srivastav et al., GCN 35932) we clearly detect an X-ray counterpart with a source flux of (3.3+/- 0.5)e-3 cps. \n\nFor the same spectral parameters inferred from the EP follow-up telescope observations, and at z = 4.859 (Saccardi et al., GCN 35936; Quirola-Vásquez et al., GCN 35960) the source has an X-ray luminosity of L_X ~ 2e46 erg/s . The decay from the EP follow-up telescope observations at t+42 hours (Chen et al. GCN 35951) to the Chandra exposure at t+72 hours post burst is ~t^-1.6. Both of these are typical of the properties seen in long GRBs, although the luminosity is towards the higher end.\n\nWe thank Pat Slane, Vinay Kashyap and the staff of the CXC for their excellent support and rapid scheduling of these observations.\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35963.",
"published": "2024-03-19T11:31:41.518616Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-19T11:31:41.518652Z",
"modified": "2024-03-19T11:31:41.526854Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6263,
"topic": "gcn.circular",
"uuid": "c40de39f-2ecc-4cbc-914f-2e63af79210a",
"title": "Fermi Gamma-ray Burst Monitor trigger 732299243/240316686 is not a GRB",
"submitter": "Hop gcn.circular",
"authors": "Peter Veres at University of Alabama in Huntsville <veresp@gmail.com>",
"data": {
"date": "24/03/19 14:58:43 GMT",
"from": "Peter Veres at University of Alabama in Huntsville <veresp@gmail.com>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35964"
},
"title": "GCN CIRCULAR",
"number": "35964",
"subject": "Fermi Gamma-ray Burst Monitor trigger 732299243/240316686 is not a GRB"
},
"message_text": "P. Veres (UAH) reports on behalf of the Fermi Gamma-ray Burst Monitor Team:\n\n\"The Fermi Gamma-ray Burst Monitor (GBM) trigger 732299243/240316686 at 16:27:18.18 UT on 16 March 2024, tentatively classified as a GRB, is in fact not due to a GRB. This trigger is due to a solar flare.\"\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35964.",
"published": "2024-03-19T14:58:59.549436Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-19T14:58:59.549456Z",
"modified": "2024-03-19T14:58:59.556434Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6264,
"topic": "gcn.circular",
"uuid": "f4ed3d79-c00f-454d-941e-8f4fb5824de3",
"title": "GRB 240317B: Swift/BAT-GUANO Angular Error Correction",
"submitter": "Hop gcn.circular",
"authors": "Jimmy DeLaunay at Penn State <delauj2@gmail.com>",
"data": {
"date": "24/03/19 19:07:34 GMT",
"from": "Jimmy DeLaunay at Penn State <delauj2@gmail.com>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35965"
},
"title": "GCN CIRCULAR",
"number": "35965",
"subject": "GRB 240317B: Swift/BAT-GUANO Angular Error Correction"
},
"message_text": "James DeLaunay (PSU), Aaron Tohuvavohu (U Toronto), Samuele Ronchini (PSU), Gayathri Raman (PSU), Jamie A. Kennea (PSU), Tyler Parsotan (NASA GSFC) report:\n\nDuring the detection of GRB 240317B, Swift was in safe point mode and had an unstable pointing. Due to this, the angular error is larger than previously reported (GCN 35948). We have performed an imaging analysis at the time of the GRB and found Cyg X-1 at an angular offset of ~1 deg. We also attempt to approximately correct the best fit position. \n\nThe updated BAT position and error is,\nRA, Dec = 271.95, +38.4 deg which is\n RA(J2000) = 18h 07m 48.0s\n Dec(J2000) = +38d 24â² 00.0â³\nwith an estimated uncertainty of ~1 deg radius\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35965.",
"published": "2024-03-19T19:07:51.998815Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-19T19:07:51.998833Z",
"modified": "2024-03-19T19:07:52.013407Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6265,
"topic": "gcn.circular",
"uuid": "f948cee0-3ef2-4fea-b840-c2681a3e6bca",
"title": "IPN triangulation of GRB 240315C (consistent with a fast X-ray transient EP240315a)",
"submitter": "Hop gcn.circular",
"authors": "Dmitry Svinkin at Ioffe Institute <svinkin@mail.ioffe.ru>",
"data": {
"date": "24/03/19 23:33:06 GMT",
"from": "Dmitry Svinkin at Ioffe Institute <svinkin@mail.ioffe.ru>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35966"
},
"title": "GCN CIRCULAR",
"number": "35966",
"subject": "IPN triangulation of GRB 240315C (consistent with a fast X-ray transient EP240315a)"
},
"message_text": "D. Svinkin, D. Frederiks, A. Ridnaia, A. Lysenko,\nand T. Cline on behalf of the Konus-Wind team,\n\nE. Burns on behalf of the IPN,\n\nand\n\nJ. DeLaunay, A. Tohuvavohu, S. Barthelmy, J. Cummings, H. Krimm,\nand D. Palmer on behalf of the Swift-BAT team, report:\n\nThe long-duration GRB 240315C has been detected by\nKonus-Wind, in the waiting mode, and Swift (BAT),\nso far, at about 73000 s UT (20:16:40).\nThe burst was outside the coded field of view of the BAT.\n\nWe have triangulated it to a Konus-BAT annulus centered at\nRA(2000)\u00159.341 deg (10h 37m 22s) Dec(2000)=+10.835 deg (+10d 50' 04\")\nwhose radius is 26.696 +/- 26.696 deg (3 sigma).\n\nThis localization may be improved.\n\nThe fast X-ray transient EP240315a (Zhang et al., GCN 35931) is inside the annulus and is consisted with the Konus-Wind ecliptic latitude response, lending support to the association of GRB 240315C and the transient.\n\nA triangulation map is posted at\nhttp://www.ioffe.ru/LEA/GRBs/GRB240315_T73000/IPN/\n\nThe Konus-Wind time history and spectrum will be given in a forthcoming\nGCN circular.\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35966.",
"published": "2024-03-19T23:33:21.387225Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-19T23:33:21.387244Z",
"modified": "2024-03-19T23:33:21.393242Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6266,
"topic": "gcn.circular",
"uuid": "e57dad93-81bb-4c01-ad8f-19a88d4b51e7",
"title": "GRB 240320A: Fermi GBM Final Real-time Localization",
"submitter": "Hop gcn.circular",
"authors": "Fermi GBM Team at MSFC/Fermi-GBM <do_not_reply@GIOC.nsstc.nasa.gov>",
"data": {
"date": "24/03/20 17:40:23 GMT",
"from": "Fermi GBM Team at MSFC/Fermi-GBM <do_not_reply@GIOC.nsstc.nasa.gov>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35967"
},
"title": "GCN CIRCULAR",
"number": "35967",
"subject": "GRB 240320A: Fermi GBM Final Real-time Localization"
},
"message_text": "The Fermi GBM team reports the detection of a likely LONG GRB\n\nAt 17:29:47 UT on 20 Mar 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 240320A (trigger 732648592.559252 / 240320729).\n\nThe on-ground calculated location, using the Fermi GBM trigger data, is RA = 150.8, Dec = 63.4 (J2000 degrees, equivalent to J2000 10h 03m, 63d 23'), with a statistical uncertainty of 14.5 degrees.\n\nThe angle from the Fermi LAT boresight is 55.0 degrees.\n\nThe skymap can be found here:\nhttps://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240320729/quicklook/glg_skymap_all_bn240320729.png\n\nThe HEALPix FITS file, including the estimated localization systematic, can be found here:\nhttps://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240320729/quicklook/glg_healpix_all_bn240320729.fit\n\nThe GBM light curve can be found here:\nhttps://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240320729/quicklook/glg_lc_medres34_bn240320729.gif\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35967.",
"published": "2024-03-20T17:40:42.123462Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-20T17:40:42.123479Z",
"modified": "2024-03-20T17:40:42.132408Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6267,
"topic": "gcn.circular",
"uuid": "f947b694-fa10-4263-a483-dba62215a5d6",
"title": "X-ray transient EP240315a: ATCA detection of radio counterpart",
"submitter": "Hop gcn.circular",
"authors": "James Leung at U. Toronto / HUJI <jamesk.leung@utoronto.ca>",
"data": {
"date": "24/03/20 22:45:33 GMT",
"from": "James Leung at U. Toronto / HUJI <jamesk.leung@utoronto.ca>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35968"
},
"title": "GCN CIRCULAR",
"number": "35968",
"subject": "X-ray transient EP240315a: ATCA detection of radio counterpart"
},
"message_text": "J. K. Leung (U. Toronto/HUJI), R. Ricci (INAF-IRA), D. Dobie (Swinburne/OzGrav), E. Troja (U. Rome)\n\nWe observed the field of AT2024eju (Srivastav et al., GCN35932), the likely optical counterpart to the fast X-ray transient EP240315a (Zhang et al., GCN35931), with the Australia Telescope Compact Array (ATCA) under project code CX564. The observations were taken on two consecutive days, from 2024-03-19 06:30 UT to 2024-03-19 09:00 UT and from 2024-03-20 06:30 UT to 2024-03-20 09:30 UT, both at 5.5 and 9 GHz.\n\nIn our preliminary analysis, we detect a radio source at both 5.5 and 9 GHz, with a flux density of ~0.1mJy. The position of the source is consistent with that of EP240315a (Zhang et al., GCN35931), AT2024eju (Srivastav et al., GCN35932), and the radio counterpart detected at 3 GHz by MeerKAT (Carotenuto et al., GCN35961).\n\nFurther ATCA observations are planned.\n\nWe thank the CSIRO Space and Astronomy staff, in particular Jamie Stevens, for supporting these observations in a timely manner. We acknowledge the Gomeroi people as the traditional owners of the Observatory site. The Australia Telescope Compact Array is part of the Australia Telescope National Facility (https://ror.org/05qajvd42) which is funded by the Australian Government for operation as a National Facility managed by CSIRO.\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35968.",
"published": "2024-03-20T22:45:48.837674Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-20T22:45:48.837697Z",
"modified": "2024-03-20T22:45:48.845764Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6268,
"topic": "gcn.circular",
"uuid": "af9d1ad3-e9db-4040-a3c9-0bf114aa6060",
"title": "GRB 240318A: Swift/BAT-GUANO detection of a burst outside the coded FOV",
"submitter": "Hop gcn.circular",
"authors": "Jimmy DeLaunay at Penn State <delauj2@gmail.com>",
"data": {
"date": "24/03/21 14:50:33 GMT",
"from": "Jimmy DeLaunay at Penn State <delauj2@gmail.com>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35969"
},
"title": "GCN CIRCULAR",
"number": "35969",
"subject": "GRB 240318A: Swift/BAT-GUANO detection of a burst outside the coded FOV"
},
"message_text": "James DeLaunay (PSU), Samuele Ronchini (PSU), Gayathri Raman (PSU), Aaron Tohuvavohu (U Toronto), Jamie A. Kennea (PSU), Tyler Parsotan (NASA GSFC) report:\n\nSwift/BAT did not localize GRB 240318A onboard (T0: 2024-03-18T02:51:01.82 UTC, Fermi trig 732423066)\n\nThe Fermi notice, distributed in near real-time, triggered the Swift Mission Operations Center operated Gamma-ray Urgent Archiver for Novel Opportunities (GUANO; Tohuvavohu et al. 2020, ApJ, 900, 1).\n\nUpon trigger by this notice, GUANO sent a command to the Swift Burst Alert Telescope (BAT) to save 200 seconds of BAT event-mode data from [-50,+150] seconds around the time of the burst. All the requested event mode data was delivered to the ground.\n\nThe BAT likelihood search, NITRATES (DeLaunay + Tohuvavohu 2022, ApJ, 941, 169), performed on the temporal window [T0-20 s, T0+20 s], detects the burst with a sqrt(TS) of 69.4 in a 4.096 s analysis time bin, starting at T0.\n\nNITRATES results are consistent with a burst coming from outside the FOV, with DeltaLLHOut of -292.\n\nSee Section 9.1 and Figures 10 and 17 in the NITRATES paper for brief descriptions and interpretation of sqrt(TS), DeltaLLHPeak, and DeltaLLHOut.\n\nGUANO is a fully autonomous, extremely low latency, spacecraft commanding pipeline designed for targeted recovery of BAT event mode data around the times of compelling astrophysical events to enable more sensitive GRB searches.\n\nA live reporting of Swift/BAT event data recovered by GUANO can be found at: https://www.swift.psu.edu/guano/\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35969.",
"published": "2024-03-21T14:50:48.442415Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-21T14:50:48.442429Z",
"modified": "2024-03-21T14:50:48.449890Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6269,
"topic": "gcn.circular",
"uuid": "278b339b-ca8a-4047-b648-7091cc8ea05f",
"title": "Fermi trigger No 732657380: Global MASTER-Net observations report",
"submitter": "Hop gcn.circular",
"authors": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"data": {
"date": "24/03/21 15:45:44 GMT",
"from": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35970"
},
"title": "GCN CIRCULAR",
"number": "35970",
"subject": "Fermi trigger No 732657380: Global MASTER-Net observations report"
},
"message_text": "V. Lipunov, V.Kornilov, E. Gorbovskoy, K. Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, V.Senik, D. Vlasenko,\nG.Antipov, D.Zimnukhov, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov, D. Cheryasov, Ya.Kechin, Yu.Tselik, A. Sosnovskij\n(Lomonosov Moscow State University, SAI, Physics Department),\n\nR. Podesta, C.Lopez, F. Podesta, C.Francile\n(Observatorio Astronomico Felix Aguilar OAFA),\n\nR. Rebolo, M. Serra\n(The Instituto de Astrofisica de Canarias),\n\nD. Buckley\n(South African Astronomical Observatory),\n\nO.A. Gress, N.M. Budnev, O.Ershova\n(Irkutsk State University, API),\n\nL.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez,\nA.R.Corella, L.H.Rodriguez\n(INAOE, Guillermo Haro Astrophysics Observatory),\n\nA. Tlatov, D. Dormidontov\n(Kislovodsk Solar Station of the Pulkovo Observatory),\n\nV. Yurkov, A. Gabovich\n(Blagoveschensk Educational State University)\n\nMASTER-SAAO robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in South Africa (South African Astronomical Observatory) started inspect of the Fermi GRB240320.83 (trigger No 732657380,18h 20m 40.80s , -34d 13m 12.0s, R=3.14) errorbox 9088 sec after trigger time at 2024-03-20 22:27:43 UT, with upper limit up to 17.0 mag. The observations began at zenith distance = 78 deg. The sun altitude is -57.9 deg.\n\nThe galactic latitude b = -10 deg., longitude l = 359 deg.\n\n\nReal time updated cover map and OT discovered available here:\nhttps://master.sai.msu.ru/site/master2/observ.php?id$03918\n\nWe obtain a following upper limits.\n\nTmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment\n_________|_____________________|_____________________|____________________________________|_____|_______|_______|________\n\n 9119 | 2024-03-20 22:27:43 | MASTER-SAAO | (18h 28m 13.21s , -38d 52m 59.6s) | C | 60 | 16.6 |\n 9119 | 2024-03-20 22:27:43 | MASTER-SAAO | (18h 25m 58.91s , -38d 40m 19.5s) | C | 60 | 17.0 |\n 9199 | 2024-03-20 22:29:03 | MASTER-SAAO | (18h 19m 02.96s , -37d 00m 13.3s) | C | 60 | 16.3 |\nFilter C is a clear (unfiltred) band.\n\n\nThe observation and reduction will continue.\nThe message may be cited.\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35970.",
"published": "2024-03-21T15:46:01.961060Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-21T15:46:01.961074Z",
"modified": "2024-03-21T15:46:01.969972Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6270,
"topic": "gcn.circular",
"uuid": "d9ba437b-f081-4dd6-a695-e0b8ea34a4ef",
"title": "GRB 240315C / X-ray transient EP240315a: Swift/BAT detection",
"submitter": "Hop gcn.circular",
"authors": "Jimmy DeLaunay at Penn State <delauj2@gmail.com>",
"data": {
"date": "24/03/21 15:47:43 GMT",
"from": "Jimmy DeLaunay at Penn State <delauj2@gmail.com>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35971"
},
"title": "GCN CIRCULAR",
"number": "35971",
"subject": "GRB 240315C / X-ray transient EP240315a: Swift/BAT detection"
},
"message_text": "James DeLaunay (PSU), Aaron Tohuvavohu (U Toronto), Dmitry Svinkin (Ioffe Institute), Samuele Ronchini (PSU), Gayathri Raman (PSU), Jamie A. Kennea (PSU), Tyler Parsotan (NASA GSFC) report:\n\nSwift/BAT did not localize GRB 240315C onboard (T0: 2024-03-15T20:10:44 UTC, EP240315a GCN 35931, GRB 240315C GCN 35966).\n\nSwift/BAT detects the emission starting at ~T0 + 350 s and lasts for ~70 s. The rates data shows the emission through all energy bins, ranging from 15 keV to 350 keV. No formal spectral analysis has been performed, but the hardness seems to be in the typical range for GRBs.\n\nNo event mode or survey mode data was available at the time due to being in a slew, so no imaging localization is possible.\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35971.",
"published": "2024-03-21T15:47:53.124795Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-21T15:47:53.124817Z",
"modified": "2024-03-21T15:47:53.129777Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6271,
"topic": "gcn.circular",
"uuid": "07795aaa-d7ee-4622-b343-38d4c735a390",
"title": "Konus-Wind detection of GRB 240315C (possible counterpart of EP240315a)",
"submitter": "Hop gcn.circular",
"authors": "Dmitry Svinkin at Ioffe Institute <svinkin@mail.ioffe.ru>",
"data": {
"date": "24/03/21 16:05:26 GMT",
"from": "Dmitry Svinkin at Ioffe Institute <svinkin@mail.ioffe.ru>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35972"
},
"title": "GCN CIRCULAR",
"number": "35972",
"subject": "Konus-Wind detection of GRB 240315C (possible counterpart of EP240315a)"
},
"message_text": "D. Svinkin, D. Frederiks, A.Lysenko, A. Ridnaia,\nA. Tsvetkova, M. Ulanov, and T. Cline,\non behalf of the Konus-Wind team, report:\n\nThe long-duration GRB 240315C\n(IPN triangulation: Svinkin et al., GCN 35966;\nSwift-BAT detection: DeLaunay et al., GCN 35971)\nwas detected by Konus-Wind (KW) in the waiting mode\nat T0=73018 s UT (20:16:58).\n\nThe burst was observed over the high and variable background\ndue to a solar particle event. A Bayesian block analysis of the KW waiting mode data in the 20-1600 keV band reveals a >20 sigma count rate increase in the interval from T0 to T0+47 s.\nThe burst light curve shows a multi-peaked structure with the brightest peak around ~T0+24 s (we note a 6 s gap in the data starting from ~T0+47 s).\n\nThe Konus-Wind light curve of this GRB is available at\nhttp://www.ioffe.ru/LEA/GRBs/GRB240315_T73000/\n\nThe spectrum of the burst, measured from T0 to T0+47 s,\ncan be described by a power law with exponential cutoff (CPL) model\ndN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)\nwith alpha = -1.09(-0.25,+0.36) and Ep = 410(-159,+388) keV.\n\nThe spectrum near the peak count rate, measured from T0+15 s to T0+29 s,\ncan be described by a CPL model with\nalpha = -0.80(-0.30,+0.38) and Ep = 459(-155,+304) keV.\n\nThe total burst fluence is 1.63(-0.40,+0.64)x10^-5 erg/cm^2,\nand the 2.944 s peak energy flux, measured from T0+23 s,\nis 9.13(-2.84,+3.65)x10^-7 erg/cm^2.\n(both in the 20 keV - 10 MeV energy range).\n\nThe burst was detected ~374 s after the start time of the fast X-ray transient EP240315a (T0(EP)=20:10:44 UT; Zhang et al., GCN 35931) and during the ~1600 s interval of the transient activity. The positional (GCN 35966) and temporal coincidence of this burst with the transient\nsupports the conclusion that the EP240315a is the GRB counterpart.\nDimmer emission episodes of GRB 240315C may be missed by Konus-Wind due to the high and variable background.\n\nAssuming GRB 240315C is indeed connected with EP240315a at\nredshift z=4.859 (Saccardi et al., GCN 35936; Quirola-Vásquez et al., GCN 35960) and a standard cosmology model with H_0 = 67.3 km/s/Mpc, Omega_M = 0.315, and Omega_Lambda = 0.685 (Planck Collaboration, 2014),\nwe estimate the following rest-frame parameters:\nthe isotropic energy release E_iso is 7.1(-1.7,+2.8)x10^53 erg,\nthe peak luminosity L_iso is 2.3(-0.7,+0.9)x10^53 erg/s,\nand the rest-frame peak energies of the time-integrated and\npeak spectra, Ep,i,z = 2402(-932,+2273) keV and Ep,p,z = 2689(-902,+1781) keV, respectively.\n\nWith the obtained estimates, GRB 240315C is inside 90% prediction band for the 'Amati' relation and inside 90% prediction band for the 'Yonetoku' relation derived for the sample of >300 long KW GRBs with known redshifts (Tsvetkova et al., 2017; Tsvetkova et al., 2021),\nsee http://www.ioffe.ru/LEA/GRBs/GRB240315_T73000/GRB240315C_rest_frame.pdf\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35972.",
"published": "2024-03-21T16:05:42.943065Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-21T16:05:42.943077Z",
"modified": "2024-03-21T16:05:42.949798Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6272,
"topic": "gcn.circular",
"uuid": "51b64c79-c476-45b6-8484-6f26b39ca77d",
"title": "Fermi GRB 240320A: Global MASTER-Net observations report",
"submitter": "Hop gcn.circular",
"authors": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"data": {
"date": "24/03/21 17:46:02 GMT",
"from": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35973"
},
"title": "GCN CIRCULAR",
"number": "35973",
"subject": "Fermi GRB 240320A: Global MASTER-Net observations report"
},
"message_text": "V. Lipunov, V.Kornilov, E. Gorbovskoy, K. Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, V.Senik, D. Vlasenko,\nG.Antipov, D.Zimnukhov, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov, D. Cheryasov, Ya.Kechin, Yu.Tselik, A. Sosnovskij\n(Lomonosov Moscow State University, SAI, Physics Department),\n\nR. Podesta, C.Lopez, F. Podesta, C.Francile\n(Observatorio Astronomico Felix Aguilar OAFA),\n\nR. Rebolo, M. Serra\n(The Instituto de Astrofisica de Canarias),\n\nD. Buckley\n(South African Astronomical Observatory),\n\nO.A. Gress, N.M. Budnev, O.Ershova\n(Irkutsk State University, API),\n\nL.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez,\nA.R.Corella, L.H.Rodriguez\n(INAOE, Guillermo Haro Astrophysics Observatory),\n\nA. Tlatov, D. Dormidontov\n(Kislovodsk Solar Station of the Pulkovo Observatory),\n\nV. Yurkov, A. Gabovich\n(Blagoveschensk Educational State University)\n\nMASTER-Tunka robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Applied Physics Institute, Irkutsk State University) started inspect of the Fermi GRB 240320A ( Fermi GBM team, GCN 35967) errorbox 69145 sec after notice time and 69181 sec after trigger time at 2024-03-21 12:42:48 UT, with upper limit up to 18.2 mag. Observations started at twilight. The observations began at zenith distance = 15 deg. The sun altitude is -13.5 deg.\n\nMASTER-Amur robotic telescope located in Russia (Blagoveshchensk State Pedagogical University) started inspect of the Fermi GRB 240320A errorbox 80725 sec after notice time and 80760 sec after trigger time at 2024-03-21 15:55:48 UT, with upper limit up to 17.3 mag. The observations began at zenith distance = 30 deg. The sun altitude is -39.4 deg.\n\nThe galactic latitude b = 45 deg., longitude l = 148 deg.\n\n\nReal time updated cover map and OT discovered available here:\nhttps://master.sai.msu.ru/site/master2/observ.php?id$03375\n\nWe obtain a following upper limits.\n\nTmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment\n_________|_____________________|_____________________|____________________________________|_____|_______|_______|________\n\n 69211 | 2024-03-21 12:42:48 | MASTER-Tunka | (09h 10m 24.61s , +52d 39m 34.5s) | C | 60 | 14.4 |\n 69335 | 2024-03-21 12:44:52 | MASTER-Tunka | (09h 11m 55.93s , +50d 44m 36.9s) | C | 60 | 14.3 | Coadd\n 69600 | 2024-03-21 12:49:17 | MASTER-Tunka | (08h 45m 24.19s , +52d 40m 17.4s) | C | 60 | 15.9 | Coadd\n 69698 | 2024-03-21 12:50:55 | MASTER-Tunka | (09h 09m 31.06s , +54d 32m 15.0s) | C | 60 | 16.5 | Coadd\n 69797 | 2024-03-21 12:52:34 | MASTER-Tunka | (08h 45m 26.41s , +52d 40m 09.6s) | C | 60 | 16.9 | Coadd\n 70044 | 2024-03-21 12:56:41 | MASTER-Tunka | (09h 35m 38.76s , +54d 33m 26.0s) | C | 60 | 16.1 | Coadd\n 70162 | 2024-03-21 12:58:40 | MASTER-Tunka | (08h 43m 21.21s , +54d 33m 41.9s) | C | 60 | 15.6 | Coadd\n 70282 | 2024-03-21 13:00:39 | MASTER-Tunka | (09h 35m 39.14s , +54d 31m 37.8s) | C | 60 | 14.8 | Coadd\n 71463 | 2024-03-21 13:20:20 | MASTER-Tunka | (09h 13m 48.63s , +48d 52m 15.6s) | C | 60 | 13.9 | Coadd\n 71922 | 2024-03-21 13:28:19 | MASTER-Tunka | (08h 35m 26.53s , +60d 30m 49.8s) | C | 20 | 18.2 |\n 72059 | 2024-03-21 13:30:16 | MASTER-Tunka | (08h 49m 27.90s , +60d 06m 51.9s) | C | 60 | 12.8 | Coadd\n 72144 | 2024-03-21 13:31:41 | MASTER-Tunka | (09h 12m 34.32s , +60d 05m 50.6s) | C | 60 | 17.6 | Coadd\n 72230 | 2024-03-21 13:33:07 | MASTER-Tunka | (08h 44m 16.89s , +59d 00m 23.4s) | C | 60 | 14.7 | Coadd\n 72313 | 2024-03-21 13:34:30 | MASTER-Tunka | (08h 49m 20.66s , +58d 52m 02.7s) | C | 60 | 12.9 | Coadd\n 80766 | 2024-03-21 15:55:48 | MASTER-Amur | (09h 02m 06.67s , +67d 36m 52.7s) | C | 10 | 15.8 |\n 80766 | 2024-03-21 15:55:48 | MASTER-Amur | (09h 01m 59.37s , +67d 58m 27.7s) | C | 10 | 16.1 |\n 80805 | 2024-03-21 15:56:27 | MASTER-Amur | (09h 02m 06.57s , +67d 35m 07.2s) | C | 10 | 15.8 |\n 80805 | 2024-03-21 15:56:27 | MASTER-Amur | (09h 01m 59.52s , +67d 56m 43.7s) | C | 10 | 16.0 |\n 80834 | 2024-03-21 15:56:56 | MASTER-Amur | (08h 41m 37.71s , +67d 35m 50.6s) | C | 10 | 15.8 |\n 80834 | 2024-03-21 15:56:56 | MASTER-Amur | (08h 41m 31.44s , +67d 57m 26.9s) | C | 10 | 16.0 |\n 80864 | 2024-03-21 15:57:26 | MASTER-Amur | (08h 41m 32.86s , +67d 34m 59.8s) | C | 10 | 15.7 |\n 80864 | 2024-03-21 15:57:26 | MASTER-Amur | (08h 41m 26.59s , +67d 56m 42.7s) | C | 10 | 15.9 |\n 80893 | 2024-03-21 15:57:55 | MASTER-Amur | (08h 41m 33.39s , +67d 35m 44.6s) | C | 10 | 15.8 |\n 80893 | 2024-03-21 15:57:55 | MASTER-Amur | (08h 41m 27.16s , +67d 57m 27.9s) | C | 10 | 15.9 |\n 80923 | 2024-03-21 15:58:25 | MASTER-Amur | (08h 41m 39.41s , +67d 34m 30.6s) | C | 10 | 15.8 |\n 80923 | 2024-03-21 15:58:25 | MASTER-Amur | (08h 41m 33.20s , +67d 56m 14.3s) | C | 10 | 16.1 |\n 80963 | 2024-03-21 15:58:55 | MASTER-Amur | (08h 41m 33.61s , +67d 33m 14.3s) | C | 30 | 16.3 |\n 80963 | 2024-03-21 15:58:55 | MASTER-Amur | (08h 41m 27.54s , +67d 54m 59.0s) | C | 30 | 16.6 |\n 81013 | 2024-03-21 15:59:45 | MASTER-Amur | (08h 41m 40.23s , +67d 35m 41.2s) | C | 30 | 15.4 |\n 81013 | 2024-03-21 15:59:45 | MASTER-Amur | (08h 41m 34.15s , +67d 57m 26.4s) | C | 30 | 15.7 |\n 81062 | 2024-03-21 16:00:34 | MASTER-Amur | (08h 41m 37.02s , +67d 36m 44.4s) | C | 30 | 15.8 |\n 81062 | 2024-03-21 16:00:34 | MASTER-Amur | (08h 41m 30.97s , +67d 58m 30.1s) | C | 30 | 16.3 |\n 81127 | 2024-03-21 16:01:24 | MASTER-Amur | (08h 41m 37.50s , +67d 34m 57.2s) | C | 60 | 15.5 |\n 81127 | 2024-03-21 16:01:24 | MASTER-Amur | (08h 41m 31.42s , +67d 56m 43.6s) | C | 60 | 16.0 |\n 81207 | 2024-03-21 16:02:44 | MASTER-Amur | (08h 41m 42.72s , +67d 35m 45.5s) | C | 60 | 15.5 |\n 81207 | 2024-03-21 16:02:44 | MASTER-Amur | (08h 41m 36.68s , +67d 57m 33.0s) | C | 60 | 16.0 |\n 81287 | 2024-03-21 16:04:05 | MASTER-Amur | (08h 41m 37.54s , +67d 34m 19.1s) | C | 60 | 15.5 |\n 81287 | 2024-03-21 16:04:05 | MASTER-Amur | (08h 41m 32.01s , +67d 56m 06.4s) | C | 60 | 15.8 |\n 82177 | 2024-03-21 16:18:54 | MASTER-Amur | (08h 41m 37.32s , +67d 59m 35.7s) | C | 60 | 17.3 |\n 82177 | 2024-03-21 16:18:54 | MASTER-Amur | (08h 41m 47.95s , +67d 37m 53.7s) | C | 60 | 16.6 |\n 82257 | 2024-03-21 16:20:14 | MASTER-Amur | (08h 41m 43.13s , +67d 58m 37.2s) | C | 60 | 17.2 |\n 82257 | 2024-03-21 16:20:14 | MASTER-Amur | (08h 41m 53.19s , +67d 36m 50.6s) | C | 60 | 16.6 |\nFilter C is a clear (unfiltred) band.\n\n\nThe observation and reduction will continue.\nThe message may be cited.\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35973.",
"published": "2024-03-21T17:46:17.887519Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-21T17:46:17.887533Z",
"modified": "2024-03-21T17:46:17.895412Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6672,
"topic": "gcn.circular",
"uuid": "3576063c-d867-4188-9598-711577532258",
"title": "EP240414a: GMG observation",
"submitter": "Hop gcn.circular",
"authors": "wangbaiting@ynao.ac.cn",
"data": {
"date": "24/04/19 03:57:39 GMT",
"from": "wangbaiting@ynao.ac.cn",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/36171"
},
"title": "GCN CIRCULAR",
"number": "36171",
"subject": "EP240414a: GMG observation"
},
"message_text": "B.-T. Wang, R.-Z. Li, J. Mao, H.-C. Feng, J.-M. Bai (YNAO) report:\n\nWe observed the field of EP240414a (Lian et al., GCN 36091) by the 2.4 meter GMG telescope in Yunnan observatories. The observation began from UT 18:42:44.276 April 18, 2024, about 4.4 days from the trigger. A optical countpart was marginally detected. The preliminary results are shown as\n\n-----------------------------------------------------------------------------\nUT exptime\t filter\t mag\n-----------------------------------------------------------------------------\n2024-04-18T18:42:44.276 \t900s\t sdssr\t 20.8 ± 0.3\n-----------------------------------------------------------------------------\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/36171.",
"published": "2024-04-19T03:57:53.491950Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-04-19T03:57:53.491963Z",
"modified": "2024-04-19T03:57:53.497521Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6273,
"topic": "gcn.circular",
"uuid": "cc917c66-8d3e-4a3d-a8ff-94c855635f6c",
"title": "GRB 240318A: Fermi GBM Observation",
"submitter": "Hop gcn.circular",
"authors": "Lorenzo Scotton at UAH <lscottongcn@outlook.com>",
"data": {
"date": "24/03/21 21:31:30 GMT",
"from": "Lorenzo Scotton at UAH <lscottongcn@outlook.com>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35974"
},
"title": "GCN CIRCULAR",
"number": "35974",
"subject": "GRB 240318A: Fermi GBM Observation"
},
"message_text": "L. Scotton (UAH) and C. Meegan (UAH) report on behalf of\nthe Fermi Gamma-ray Burst Monitor Team:\n\n\"At 02:51:01.82 UT on 18 March 2024, the Fermi Gamma-ray Burst Monitor (GBM)\ntriggered and located GRB 240318A (trigger 732423066/240318119),\nwhich was also detected by Glowbug (Cheung et al. 2024, GCN 35959)\nand Swift/BAT-GUANO (DeLaunay et al. 2024, GCN 35969).\nThe Fermi GBM Final Real-time Localization was provided in GCN 35949.\n\nThe angle from the Fermi LAT boresight is 53 degrees.\n\nThe GBM light curve consists of a single emission episode with a duration (T90)\nof about 8 s (50-300 keV). The time-averaged spectrum\nfrom T0-2.0 to T0+11.0 s is best fit by\na power law function with an exponential high-energy cutoff.\nThe power law index is -0.5 +/- 0.2 and the cutoff energy,\nparameterized as Epeak, is 112 +/- 8 keV.\n\nThe event fluence (10-1000 keV) in this time interval is\n(2.1 +/- 0.1)E-06 erg/cm^2. The 1-sec peak photon flux measured\nstarting from T0+1.1 s in the 10-1000 keV band is 4.5 +/- 0.3 ph/s/cm^2.\n\nThe spectral analysis results presented above are preliminary;\nfinal results will be published in the GBM GRB Catalog:\nhttps://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html\n\nFor Fermi GBM data and info, please visit the official Fermi GBM Support Page:\nhttps://fermi.gsfc.nasa.gov/ssc/data/access/gbm/\"\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35974.",
"published": "2024-03-21T21:31:46.978174Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-21T21:31:46.978195Z",
"modified": "2024-03-21T21:31:46.984083Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6277,
"topic": "gcn.circular",
"uuid": "4888b84a-891a-4e4b-9790-6e7a7aa1e90f",
"title": "Transient EPW20240219aa: REM optical/NIR further observations",
"submitter": "Hop gcn.circular",
"authors": "Matteo Ferro <matteo.ferro@inaf.it>",
"data": {
"date": "24/03/26 09:04:38 GMT",
"from": "Matteo Ferro <matteo.ferro@inaf.it>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35978"
},
"title": "GCN CIRCULAR",
"number": "35978",
"subject": "Transient EPW20240219aa: REM optical/NIR further observations"
},
"message_text": "M. Ferro, Y.-D. Hu, P. DâAvanzo, R. Brivio, S. Covino, D. Fugazza (INAF-OAB) on behalf of the REM team, report:\n\nWe observed for a second epoch the field of the transient EPW20240219aa (Zhang et al., ATel 16463; Zhang et al., ATel 16472; Zhang et al., GCN 35773) with the REM 60cm robotic telescope located at the ESO observatory of La Silla (Chile). The observations were carried in the g, r, i, z, H bands, starting on 2024 March 15 at 23:53:40 UT (i.e. 25.73 days after the event), and lasting for about 30 minutes.\nIn order to identify a possible supernova we performed image subtraction between these observations and the first epoch (taken 5.75 days after the event, Ferro et al., GCN 35803). We find no clear transient candidate within the Einstein Probe error circle, nor at the positions of the radio sources reported by Ho et al. (GCN 35788), down to the following 3sigma magnitude upper limits:\n\nH > 18.1 (Vega; calibrated against the 2MASS catalogue)\n\nr > 19.8 (AB; calibrated against the Pan-STARRS catalogue)\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35978.",
"published": "2024-03-26T09:04:57.638037Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-26T09:04:57.638054Z",
"modified": "2024-03-26T09:04:57.645983Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6278,
"topic": "gcn.circular",
"uuid": "c9477814-af48-4151-a3ff-dcf21594d142",
"title": "X-ray transient EP240315a: Ondrejov D50 optical limit",
"submitter": "Hop gcn.circular",
"authors": "Martin Jelinek at Astro.Inst-AVCR,Ondrejov <martin.jelinek@asu.cas.cz>",
"data": {
"date": "24/03/26 11:07:49 GMT",
"from": "Martin Jelinek at Astro.Inst-AVCR,Ondrejov <martin.jelinek@asu.cas.cz>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35979"
},
"title": "GCN CIRCULAR",
"number": "35979",
"subject": "X-ray transient EP240315a: Ondrejov D50 optical limit"
},
"message_text": "Alzbeta Malenakova, Jan Strobl, Martin Jelinek, Rene Hudec and Cyril Polasek\n(ASU CAS Ondrejov, CZ), report:\n\nWe observed the field of the fast X-ray transient EP240315a detected by Einstein Probe (Zhang et al., GCN 35931) and its optical counterpart AT2024eju detected by ATLAS (Srivastav et al., GCN 35932) with the 50 cm robotic telescope (D50) of Ondrejov observatory in Czech Republic. We obtained a set of 120s SDSS-r' exposures starting at 23:03 UT on March 16.\n\nWe measure the optical limit r' > 21.1 in a combined 26x120s image with a mean time T-T0 27.43h post detection, which is in agreement with other observations at similar epoch (e.g. Chen et al., GCN 35938, Leonini et al., 35944).\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35979.",
"published": "2024-03-26T11:08:10.619095Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-26T11:08:10.619114Z",
"modified": "2024-03-26T11:08:10.625761Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6279,
"topic": "gcn.circular",
"uuid": "636fccb9-4413-4cba-91d0-5cd5a40a77c9",
"title": "X-ray transient EP240315a: e-MERLIN radio observations",
"submitter": "Hop gcn.circular",
"authors": "Gabriele Bruni at INAF <gabriele.bruni@inaf.it>",
"data": {
"date": "24/03/26 14:45:28 GMT",
"from": "Gabriele Bruni at INAF <gabriele.bruni@inaf.it>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35980"
},
"title": "GCN CIRCULAR",
"number": "35980",
"subject": "X-ray transient EP240315a: e-MERLIN radio observations"
},
"message_text": "G. Bruni (INAF-IAPS), L. Rhodes (Oxford), L. Piro, G. Gianfagna, A.L. Thakur (INAF-IAPS), J. Bright, F. Carotenuto, S. Smartt, R. Fender (Oxford), P. Jonker (Radboud) report:\n\nWe observed the new Fast X-ray Transient EP240315a (Zhang et al., GCN 35931) with the e-Merlin radio telescope under the projects DD17003 (PI: Piro) and DD17004 (PI: Rhodes) at 5 GHz for a total of ~16 hours using a combination of two runs in two consecutive nights (from ~17:30 UT to ~02.00 UT, on March 20 and 21, 2024).\n\n3C286 was used for flux scale calibration, and 0933-0819 for complex gain, respectively. The beam size was 275x104 milli-arcsec. Data was reduced with the e-MERLIN pipeline and imaged with CASA. The image RMS was 15 uJy/beam.\n\nWe did not find statistically significant emission at a level above 5-sigma at the position of the optical counterpart (AT2024eju, Srivastav et al., GCN 35932). Thus, we estimated a 5-sigma upper limit of 75 uJy at 5 GHz. Scintillation could be a possible explanation for the large variability with respect to the previous radio detection at the same frequency (Leung et al., GCN 35968).\n\nFurther e-Merlin observations are planned. We thank the e-Merlin staff for their excellent support.\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35980.",
"published": "2024-03-26T14:45:51.775331Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-26T14:45:51.775358Z",
"modified": "2024-03-26T14:45:51.781514Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6280,
"topic": "gcn.circular",
"uuid": "78781052-8080-42d1-a532-d96c7b5a9939",
"title": "Fermi trigger No 733097506: Global MASTER-Net observations report",
"submitter": "Hop gcn.circular",
"authors": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"data": {
"date": "24/03/26 17:30:56 GMT",
"from": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35981"
},
"title": "GCN CIRCULAR",
"number": "35981",
"subject": "Fermi trigger No 733097506: Global MASTER-Net observations report"
},
"message_text": "V. Lipunov, V.Kornilov, E. Gorbovskoy, K. Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, V.Senik, D. Vlasenko,\nG.Antipov, D.Zimnukhov, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov, D. Cheryasov, Ya.Kechin, Yu.Tselik, A. Sosnovskij\n(Lomonosov Moscow State University, SAI, Physics Department),\n\nR. Podesta, C.Lopez, F. Podesta, C.Francile\n(Observatorio Astronomico Felix Aguilar OAFA),\n\nR. Rebolo, M. Serra\n(The Instituto de Astrofisica de Canarias),\n\nD. Buckley\n(South African Astronomical Observatory),\n\nO.A. Gress, N.M. Budnev, O.Ershova\n(Irkutsk State University, API),\n\nL.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez,\nA.R.Corella, L.H.Rodriguez\n(INAOE, Guillermo Haro Astrophysics Observatory),\n\nA. Tlatov, D. Dormidontov\n(Kislovodsk Solar Station of the Pulkovo Observatory),\n\nV. Yurkov, A. Gabovich\n(Blagoveschensk Educational State University)\n\nMASTER-Tunka robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Applied Physics Institute, Irkutsk State University) started inspect of the Fermi GRB240325.92 (trigger No 733097506,01h 55m 00.00s , +01d 54m 00.0s, R0.45) errorbox 54024 sec after notice time and 54058 sec after trigger time at 2024-03-26 13:12:40 UT, with upper limit up to 14.7 mag. Observations started at twilight. The observations began at zenith distance = 72 deg. The sun altitude is -16.4 deg.\n\nMASTER-Kislovodsk robotic telescope located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) started inspect of the Fermi GRB240325.92 errorbox 65955 sec after notice time and 65989 sec after trigger time at 2024-03-26 16:31:31 UT, with upper limit up to 18.0 mag. Observations started at twilight. The observations began at zenith distance = 62 deg. The sun altitude is -11.9 deg.\n\nThe galactic latitude b = -57 deg., longitude l = 154 deg.\n\n\nReal time updated cover map and OT discovered available here:\nhttps://master.sai.msu.ru/site/master2/observ.php?id$06794\n\nWe obtain a following upper limits.\n\nTmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment\n_________|_____________________|_____________________|____________________________________|_____|_______|_______|________\n\n 54088 | 2024-03-26 13:12:40 | MASTER-Tunka | (02h 55m 06.52s , +17d 04m 35.9s) | C | 60 | 13.8 |\n 54089 | 2024-03-26 13:12:40 | MASTER-Tunka | (02h 53m 52.29s , +16d 28m 26.9s) | C | 60 | 14.7 |\n 66020 | 2024-03-26 16:31:31 | MASTER-Kislovodsk | (02h 30m 22.81s , +28d 07m 21.0s) | C | 60 | 14.9 |\n 66261 | 2024-03-26 16:35:32 | MASTER-Kislovodsk | (02h 32m 11.32s , +25d 51m 11.9s) | C | 60 | 16.1 |\n 66261 | 2024-03-26 16:35:32 | MASTER-Kislovodsk | (02h 27m 55.78s , +26d 12m 05.8s) | C | 60 | 16.4 |\n 66341 | 2024-03-26 16:36:52 | MASTER-Kislovodsk | (02h 54m 37.58s , +16d 22m 18.5s) | C | 60 | 16.1 |\n 66341 | 2024-03-26 16:36:52 | MASTER-Kislovodsk | (02h 50m 39.80s , +16d 43m 12.7s) | C | 60 | 16.7 |\n 66983 | 2024-03-26 16:47:34 | MASTER-Kislovodsk | (02h 34m 50.66s , +27d 45m 12.9s) | C | 60 | 17.2 |\n 66983 | 2024-03-26 16:47:34 | MASTER-Kislovodsk | (02h 30m 31.07s , +28d 06m 05.3s) | C | 60 | 18.0 |\n 67223 | 2024-03-26 16:51:34 | MASTER-Kislovodsk | (02h 32m 17.68s , +25d 52m 26.7s) | C | 60 | 17.4 |\n 67223 | 2024-03-26 16:51:34 | MASTER-Kislovodsk | (02h 28m 03.93s , +26d 13m 16.7s) | C | 60 | 17.9 |\n 67303 | 2024-03-26 16:52:54 | MASTER-Kislovodsk | (02h 54m 31.95s , +16d 22m 24.3s) | C | 60 | 17.2 |\n 67303 | 2024-03-26 16:52:54 | MASTER-Kislovodsk | (02h 50m 35.97s , +16d 43m 13.4s) | C | 60 | 17.9 |\n 67944 | 2024-03-26 17:03:35 | MASTER-Kislovodsk | (02h 34m 44.27s , +27d 45m 18.2s) | C | 60 | 17.3 |\n 67944 | 2024-03-26 17:03:35 | MASTER-Kislovodsk | (02h 30m 26.14s , +28d 06m 06.7s) | C | 60 | 18.0 |\n 68185 | 2024-03-26 17:07:36 | MASTER-Kislovodsk | (02h 32m 10.21s , +25d 50m 06.1s) | C | 60 | 16.9 |\n 68185 | 2024-03-26 17:07:36 | MASTER-Kislovodsk | (02h 27m 58.10s , +26d 10m 51.5s) | C | 60 | 17.6 |\n 68265 | 2024-03-26 17:08:56 | MASTER-Kislovodsk | (02h 54m 36.53s , +16d 21m 19.8s) | C | 60 | 16.9 |\n 68265 | 2024-03-26 17:08:56 | MASTER-Kislovodsk | (02h 50m 42.00s , +16d 42m 04.9s) | C | 60 | 17.5 |\n 68345 | 2024-03-26 17:10:16 | MASTER-Kislovodsk | (02h 51m 38.04s , +12d 34m 19.1s) | C | 60 | 16.8 |\n 68345 | 2024-03-26 17:10:16 | MASTER-Kislovodsk | (02h 47m 49.51s , +12d 54m 58.2s) | C | 60 | 17.1 |\n 68425 | 2024-03-26 17:11:37 | MASTER-Kislovodsk | (02h 52m 59.66s , +14d 27m 09.9s) | C | 60 | 17.0 |\n 68425 | 2024-03-26 17:11:37 | MASTER-Kislovodsk | (02h 49m 08.58s , +14d 47m 49.7s) | C | 60 | 17.5 |\n 68666 | 2024-03-26 17:15:37 | MASTER-Kislovodsk | (03h 12m 19.95s , +18d 17m 12.4s) | C | 60 | 17.0 |\n 68666 | 2024-03-26 17:15:37 | MASTER-Kislovodsk | (03h 08m 20.63s , +18d 38m 03.1s) | C | 60 | 17.6 |\nFilter C is a clear (unfiltred) band.\n\n\nThe observation and reduction will continue.\nThe message may be cited.\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35981.",
"published": "2024-03-26T17:31:15.741220Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-26T17:31:15.741235Z",
"modified": "2024-03-26T17:31:15.748315Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6675,
"topic": "gcn.circular",
"uuid": "f5a38059-4dd5-420e-8d8d-2e3a5b604efc",
"title": "EP240416a: J-band observations with WINTER",
"submitter": "Hop gcn.circular",
"authors": "Geoffrey Mo at MIT <gmo@mit.edu>",
"data": {
"date": "24/04/19 05:07:16 GMT",
"from": "Geoffrey Mo at MIT <gmo@mit.edu>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/36172"
},
"title": "GCN CIRCULAR",
"number": "36172",
"subject": "EP240416a: J-band observations with WINTER"
},
"message_text": "Geoffrey Mo (MIT), Viraj Karambelkar (Caltech), Danielle Frostig (MIT), Robert Stein (Caltech), Nathan Lourie (MIT), Tomas Ahumada (Caltech), Robert Simcoe (MIT), and Mansi Kasliwal (Caltech) report:\n\nWe observed the field of the EP-WXT X-ray transient EP240416a (Cheng et al., GCN 36138) in the near-infrared J-band with the Palomar 1-m telescope, equipped with the 1 square degree WINTER camera (Lourie et al. 2020).\n\nObservations began at 2024-04-17T14:01:04.438 UTC (~1.5 days after the X-ray transient) and consisted of 15 x 120 s exposures. The images were processed using the WINTER data reduction pipeline (https://github.com/winter-telescope/mirar).\n\nWe do not detect the optical counterpart discovered by Kinder and confirmed by Xinglong and NOT (Chen et al., GCN 36139, An et al., GCN 36144, Antipov et al., GCN 36142, Xiong et al., GCN 36155, Pankov et al., GCN 36157, Belkin et al., GCN 36158), setting the following upper limit: J ~ 19.4 mag (AB).\n\nWINTER (Wide-field INfrared Transient ExploreR) is a partnership between MIT and Caltech, housed at Palomar Observatory, and funded by NSF MRI, NSF AAG, the David and Lucille Packard Foundation, and the MIT Kavli Institute for Astrophysics and Space Research.\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/36172.",
"published": "2024-04-19T05:07:33.057578Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-04-19T05:07:33.057593Z",
"modified": "2024-04-19T05:07:33.067859Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6281,
"topic": "gcn.circular",
"uuid": "122900b8-a242-4309-95c3-29a985f09e0a",
"title": "X-ray transient EP 240315a: Second epoch Chandra observations",
"submitter": "Hop gcn.circular",
"authors": "Andrew Levan at Radboud University <a.levan@astro.ru.nl>",
"data": {
"date": "24/03/27 09:06:39 GMT",
"from": "Andrew Levan at Radboud University <a.levan@astro.ru.nl>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35982"
},
"title": "GCN CIRCULAR",
"number": "35982",
"subject": "X-ray transient EP 240315a: Second epoch Chandra observations"
},
"message_text": "A.J. Levan (Radboud & Warwick), P.G. Jonker (Radboud), D.B. Malesani (DAWN/NBI & Radboud), N.R. Tanvir (Leicester), B.P. Gompertz (Birmingham), A. Saccardi (GEPI/Obs. de Paris), A. de Ugarte Postigo (CNRS/OCA & LAM), A. Martin-Carrillo (UCD), D. Perley (LJMU), D. Xu (NAOC), G. Tagliaferri (INAF, Brera), J. Palmerio (GEPI/Obs. de Paris)), K.E. Heintz (DAWN/NBI), K. Wiersema (Hertfordshire), M. Grazia Bernardini (INAF, Brera), M. Ferro (INAF, Brera), P. Jakobbson (U. Iceland), P. DâAvanzo (INAF, Brera), R. Salvaterra (INAF, Milan), S. Vergani (GEPI/Obs. de Paris), G. Pugliese (API, Amsterdam), Y. Julakanti (Leicester) report for the Stargate collaboration:\n\nWe obtained a second epoch of Chandra observations of EP240315a (Zhang et al., GCN 35931; Chen et al., GCN 35951) beginning at 04:34 on 26 March 2024, approximately 10.4 days after the transient detection and 6 days from the first epoch of observations (Levan et al., GCN 35963). A total of 18.5 ks of observations were obtained (compared to 10 ks at the first epoch). At the location of AT2024eju (Srivastav et al. GCN 35932) we do not detect any source. More formally, we identify a single photon at the source location, and set a 2-sigma upper limit of <2.4e-4 count s^-1 at this epoch.\n\nThe inferred decay rate from 3 days to 10.4 days is steeper than t^-2.1, and suggests a relatively rapid decay. This is consistent with the post-jet break decay rate for a GRB afterglow.\n\nWe again thank Pat Slane, Vinay Kashyap and the staff of the CXC for their excellent support and rapid scheduling of these observations.\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35982.",
"published": "2024-03-27T09:06:56.977051Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-27T09:06:56.977066Z",
"modified": "2024-03-27T09:06:56.984327Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6677,
"topic": "gcn.circular",
"uuid": "7a171286-3fb4-4837-9c0e-d891edb90bc0",
"title": "Fermi trigger No 735089036: Global MASTER-Net observations report",
"submitter": "Hop gcn.circular",
"authors": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"data": {
"date": "24/04/19 06:45:59 GMT",
"from": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/36173"
},
"title": "GCN CIRCULAR",
"number": "36173",
"subject": "Fermi trigger No 735089036: Global MASTER-Net observations report"
},
"message_text": "V. Lipunov, V.Kornilov, E. Gorbovskoy, K. Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, V.Senik, D. Vlasenko,\nG.Antipov, D.Zimnukhov, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov, D. Cheryasov, Ya.Kechin, Yu.Tselik, A. Sosnovskij\n(Lomonosov Moscow State University, SAI, Physics Department),\n\nR. Podesta, C.Lopez, F. Podesta, C.Francile\n(Observatorio Astronomico Felix Aguilar OAFA),\n\nR. Rebolo, M. Serra\n(The Instituto de Astrofisica de Canarias),\n\nD. Buckley\n(South African Astronomical Observatory),\n\nO.A. Gress, N.M. Budnev, O.Ershova\n(Irkutsk State University, API),\n\nL.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez,\nA.R.Corella, L.H.Rodriguez\n(INAOE, Guillermo Haro Astrophysics Observatory),\n\nA. Tlatov, D. Dormidontov\n(Kislovodsk Solar Station of the Pulkovo Observatory),\n\nV. Yurkov, A. Gabovich\n(Blagoveschensk Educational State University)\n\nMASTER-SAAO robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in South Africa (South African Astronomical Observatory) started inspect of the Fermi GRB240417.97 (trigger No 735089036,02h 10m 19.92s , -03d 31m 58.8s, R!.22) errorbox 63251 sec after notice time and 63285 sec after trigger time at 2024-04-18 16:58:36 UT, with upper limit up to 17.0 mag. Observations started at twilight. The observations began at zenith distance = 71 deg. The sun altitude is -10.2 deg.\n\nThe galactic latitude b = -59 deg., longitude l = 166 deg.\n\n\nReal time updated cover map and OT discovered available here:\nhttps://master.sai.msu.ru/site/master2/observ.php?id$25848\n\nWe obtain a following upper limits.\n\nTmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment\n_________|_____________________|_____________________|____________________________________|_____|_______|_______|________\n\n 63316 | 2024-04-18 16:58:36 | MASTER-SAAO | (03h 17m 20.19s , -08d 12m 54.6s) | C | 60 | 14.3 |\n 63395 | 2024-04-18 16:59:56 | MASTER-SAAO | (03h 31m 11.88s , -04d 25m 53.4s) | C | 60 | 14.7 |\n 63850 | 2024-04-18 17:07:31 | MASTER-SAAO | (03h 18m 29.94s , -10d 08m 18.3s) | C | 60 | 16.2 |\n 63850 | 2024-04-18 17:07:31 | MASTER-SAAO | (03h 20m 16.37s , -10d 20m 55.8s) | C | 60 | 16.9 |\n 63930 | 2024-04-18 17:08:50 | MASTER-SAAO | (03h 04m 26.97s , -12d 00m 30.8s) | C | 60 | 14.2 |\n 63930 | 2024-04-18 17:08:50 | MASTER-SAAO | (03h 06m 13.89s , -12d 13m 09.8s) | C | 60 | 16.6 |\n 64009 | 2024-04-18 17:10:10 | MASTER-SAAO | (03h 31m 48.88s , -06d 19m 29.0s) | C | 60 | 16.1 |\n 64009 | 2024-04-18 17:10:10 | MASTER-SAAO | (03h 33m 34.13s , -06d 32m 06.3s) | C | 60 | 17.0 |\n 64737 | 2024-04-18 17:22:18 | MASTER-SAAO | (03h 19m 29.66s , -08d 26m 39.1s) | C | 60 | 17.0 |\n 64817 | 2024-04-18 17:23:38 | MASTER-SAAO | (03h 33m 15.06s , -04d 36m 56.4s) | C | 60 | 17.0 |\n 65502 | 2024-04-18 17:35:03 | MASTER-SAAO | (03h 20m 39.07s , -10d 20m 17.5s) | C | 60 | 17.0 |\nFilter C is a clear (unfiltred) band.\n\n\nThe observation and reduction will continue.\nThe message may be cited.\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/36173.",
"published": "2024-04-19T06:46:19.489546Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-04-19T06:46:19.489563Z",
"modified": "2024-04-19T06:46:19.497152Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6284,
"topic": "gcn.circular",
"uuid": "2a518c4e-4189-4a51-98c3-cdb8649dbd6d",
"title": "IceCube-240327A - IceCube observation of a high-energy neutrino candidate track-like event",
"submitter": "Hop gcn.circular",
"authors": "A. Zegarelli at Ruhr University Bochum <azegarelli@icecube.wisc.edu>",
"data": {
"date": "24/03/27 13:44:38 GMT",
"from": "A. Zegarelli at Ruhr University Bochum <azegarelli@icecube.wisc.edu>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35983"
},
"title": "GCN CIRCULAR",
"number": "35983",
"subject": "IceCube-240327A - IceCube observation of a high-energy neutrino candidate track-like event"
},
"message_text": "The IceCube Collaboration (http://icecube.wisc.edu/) reports:\n\nOn 2024-03-27 at 11:04:49.50 UT IceCube detected a track-like event with a high probability of being of astrophysical origin. The event was selected by the ICECUBE_Astrotrack_GOLD alert stream. The average astrophysical neutrino purity for Gold alerts is 50%. This alert has an estimated false alarm rate of 1.0306 events per year due to atmospheric backgrounds. The IceCube detector was in a normal operating state at the time of detection.\n\nAfter the initial automated alert (https://gcn.gsfc.nasa.gov/notices_amon_g_b/139204_39158985.amon) more sophisticated reconstruction algorithms have been applied offline, with the direction refined to:\n\nDate: 2024-03-27\nTime: 11:04:49.50 UT\nRA: 25.40 (+1.86, -2.36 deg 90% PSF containment) J2000\nDec: 7.78 (+0.69, -0.68 deg 90% PSF containment) J2000\n\nWe encourage follow-up by ground and space-based instruments to help identify a possible astrophysical source for the candidate neutrino.\n\nNo known gamma-ray sources listed in the Fermi 4FGL-DR4 or 3FHL catalogs are located within the 90% uncertainty region of the event.\n\nThe IceCube Neutrino Observatory is a cubic-kilometer neutrino detector operating at the geographic South Pole, Antarctica. The IceCube realtime alert point of contact can be reached at roc@icecube.wisc.edu\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35983.",
"published": "2024-03-27T13:44:54.567072Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-27T13:44:54.567092Z",
"modified": "2024-03-27T13:44:54.575153Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6288,
"topic": "gcn.circular",
"uuid": "8921bd56-3eef-4fda-b808-d38c39d72298",
"title": "IceCube-240327B - IceCube observation of a high-energy neutrino candidate track-like event",
"submitter": "Hop gcn.circular",
"authors": "Giacomo Sommani at Ruhr-Universität Bochum <gsommani@icecube.wisc.edu>",
"data": {
"date": "24/03/27 18:11:03 GMT",
"from": "Giacomo Sommani at Ruhr-Universität Bochum <gsommani@icecube.wisc.edu>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/35984"
},
"title": "GCN CIRCULAR",
"number": "35984",
"subject": "IceCube-240327B - IceCube observation of a high-energy neutrino candidate track-like event"
},
"message_text": "The IceCube Collaboration (http://icecube.wisc.edu/) reports:\n\nOn 2024-03-27, at 16:12:30.47 UT IceCube detected a track-like event with a moderate probability of being of astrophysical origin. The event was selected by the ICECUBE_Astrotrack_BRONZE alert stream. The average astrophysical neutrino purity for Gold alerts is 30%. This alert has an estimated false alarm rate of 2.420 events per year due to atmospheric backgrounds. The IceCube detector was in a normal operating state at the time of detection.\n\nAfter the initial automated alert (https://gcn.gsfc.nasa.gov/notices_amon_g_b/139205_9784024.amon) more sophisticated reconstruction algorithms have been applied offline, with the direction refined to:\n\nDate: 2024-03-27\nTime: 16:12:30.47 UT\nRA: 89.21 (+1.36, -1.55 deg 90% PSF containment) J2000\nDec: 0.93 (+1.23, -1.47 deg 90% PSF containment) J2000\n\nWe encourage follow-up by ground and space-based instruments to help identify a possible astrophysical source for the candidate neutrino.\n\nFive known gamma-ray sources listed in the Fermi 4FGL-DR4 or 3FHL catalogs are located within the 90% uncertainty region of the event. The nearest one to the neutrino alert position is 4FGL J0555.9+0030, located at RA = 89.00 deg, Dec = 0.51 deg J2000, 0.47 deg away from the best-fit alert position.\n\nThe IceCube Neutrino Observatory is a cubic-kilometer neutrino detector operating at the geographic South Pole, Antarctica. The IceCube realtime alert point of contact can be reached at roc@icecube.wisc.edu\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/35984.",
"published": "2024-03-27T18:11:22.347797Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-03-27T18:11:22.347817Z",
"modified": "2024-03-27T18:11:22.355797Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6679,
"topic": "gcn.circular",
"uuid": "a9126f4d-edeb-455a-b1ca-897f22c9742a",
"title": "GRB 240419A: Enhanced Swift-XRT position",
"submitter": "Hop gcn.circular",
"authors": "Phil Evans at U of Leicester <pae9@star.le.ac.uk>",
"data": {
"date": "24/04/19 08:08:55 GMT",
"from": "Phil Evans at U of Leicester <pae9@star.le.ac.uk>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/36174"
},
"title": "GCN CIRCULAR",
"number": "36174",
"subject": "GRB 240419A: Enhanced Swift-XRT position"
},
"message_text": "M.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester)\nreport on behalf of the Swift-XRT team.\n\nUsing 977 s of XRT Photon Counting mode data and 1 UVOT\nimages for GRB 240419A, we find an astrometrically corrected X-ray\nposition (using the XRT-UVOT alignment and matching UVOT field sources\nto the USNO-B1 catalogue): RA, Dec = 94.53406, -44.99952 which is equivalent\nto:\n\nRA (J2000): 06h 18m 8.17s\nDec (J2000): -44d 59' 58.3\"\n\nwith an uncertainty of 2.2 arcsec (radius, 90% confidence).\n\nThis position may be improved as more data are received. The latest\nposition can be viewed at http://www.swift.ac.uk/xrt_positions. Position\nenhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans\net al. (2009, MNRAS, 397, 1177).\n\nThis circular was automatically generated, and is an official product of the\nSwift-XRT team.\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/36174.",
"published": "2024-04-19T08:09:13.533480Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-04-19T08:09:13.533502Z",
"modified": "2024-04-19T08:09:13.542148Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6680,
"topic": "gcn.circular",
"uuid": "a94e787f-1596-48b7-9efc-c5cf6f826909",
"title": "GRB 240419A: VLT optical afterglow detection",
"submitter": "Hop gcn.circular",
"authors": "Daniele B. Malesani at IMAPP / Radboud University <d.malesani@astro.ru.nl>",
"data": {
"date": "24/04/19 08:17:24 GMT",
"from": "Daniele B. Malesani at IMAPP / Radboud University <d.malesani@astro.ru.nl>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/36175"
},
"title": "GCN CIRCULAR",
"number": "36175",
"subject": "GRB 240419A: VLT optical afterglow detection"
},
"message_text": "B. Schneider (MIT), N. Gaspari (Radboud Univ.), N. R. Tanvir (Univ. Leicester), S. Covino (INAF/Brera), D. B. Malesani (DAWN/NBI and Radboud Univ.), L. Izzo (INAF/Napoli and DARK/NBI), A. Saccardi (GEPI/Obs. Paris), report on behalf of the Stargate collaboration.\n\nWe observed the field of GRB 240419A (Siegel et al., GCN 36169) using the ESO VLT UT1 equipped with the FORS2 camera. Observations were commenced automatically in rapid-response mode (RRM). The first image was acquired on April 19.0895 UT, that is, 20.9 min after the GRB, and consisted of a 20 s image in the R filter. At a relatively high airmass of 2.1, the delivered PSF was 1.4\".\n\nA source, not present in archival images, is detected within the UVOT-enhanced XRT error circle (Goad et al., GCN 36174), at coordinates (J2000):\n\nRA = 06:18:08.17\nDec = -44:59:57.3\n\nUsing FORS2 zeropoints, we measure for the source a magnitude R = 19.88 +- 0.05 (Vega), in excellent agreement with photometry calibrated against nearby stars from the SkyMapper catalog.\n\nFurther observations have been secured and will be reported at a later time. We acknowledge excellent support from the ESO observing staff in Paranal.\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/36175.",
"published": "2024-04-19T08:17:34.355268Z",
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"created": "2024-04-19T08:17:34.355285Z",
"modified": "2024-04-19T08:17:34.361520Z",
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