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"count": 257459,
"next": "https://hermes.lco.global/api/v0/messages/?format=api&limit=100&offset=1200&ordering=topic",
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"results": [
{
"id": 4195,
"topic": "gcn.circular",
"uuid": "7d1fc87d-8d8f-476a-bf1d-8c27ba4c23fd",
"title": "IPN triangulation of GRB 231020A",
"submitter": "Hop gcn.circular",
"authors": "Dmitry Svinkin at Ioffe Institute <svinkin@mail.ioffe.ru>",
"data": {
"date": "23/10/30 20:36:49 GMT",
"from": "Dmitry Svinkin at Ioffe Institute <svinkin@mail.ioffe.ru>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34917"
},
"title": "GCN CIRCULAR",
"number": "34917",
"subject": "IPN triangulation of GRB 231020A"
},
"message_text": "A.S. Kozyrev, D.V. Golovin, M.L. Litvak, I.G. Mitrofanov, and A.B. Sanin\non behalf of the MGNS/BepiColombo and HEND/Mars Odyssey teams,\n\nJ. Benkhoff on behalf of the BepiColombo team,\n\nD. Svinkin, D. Frederiks, A. Ridnaia, A. Lysenko,\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\nS. Barthelmy, J. Cummings, H. Krimm, D. Palmer, and A. Tohuvavohu\non behalf of the Swift-BAT team,\n\nand\n\nW. Boynton, C. Fellows, K. Harshman, H. Enos, R. Starr,\nand A.S. Gardner on on behalf of the GRS-Odyssey GRB team,\nreport:\n\nThe long-duration GRB 231020A\n(Fermi-GBM detection: The Fermi GBM team, GCN Circ. 34856;\nBala et al., GCN Circ. 34869;\nBALROG localization: Preis et al., GCN Circ. 34861;\nAstroSat-CZTI detection: Navaneeth et al., GCN Circ. 34880;\nGRID detection: Wang and Yang, GCN Circ. 34903)\nwas detected by Fermi (GBM trigger 719521023), INTEGRAL (SPI-ACS),\nKonus-Wind, Swift (BAT), Mars-Odyssey (HEND), BepiColombo (MGNS),\nAstroSat (CZTI), and GRID, at about 68218 s UT (18:56:58).\nThe burst was outside the coded field of view of the BAT.\n\nWe have triangulated it to a preliminary, 3 sigma error box\nwhose coordinates are:\n ---------------------------------------------\n RA(2000), deg Dec(2000), deg\n ---------------------------------------------\n Center:\n 314.493 (20h 57m 58s) -29.254 (-29d 15' 15\")\n Corners:\n 314.061 (20h 56m 15s) -28.067 (-28d 04' 02\")\n 314.696 (20h 58m 47s) -29.893 (-29d 53' 33\")\n 314.881 (20h 59m 31s) -30.286 (-30d 17' 09\")\n 314.275 (20h 57m 06s) -28.562 (-28d 33' 43\")\n ---------------------------------------------\nThe error box area is 247 sq. arcmin, and its maximum\ndimension is 2.3 deg (the minimum one is 2.2 arcmin).\nThe Sun distance was 101 deg.\n\nThis localization may be improved.\n\nThe IPN localization is consistent with, but reduces the area of,\nthe Fermi-GBM final localization.\n\nA triangulation map and HEALPix FITS file are posted at\nhttp://www.ioffe.ru/LEA/GRBs/GRB231020_T68224/IPN\n\nThe Konus-Wind time history and spectrum will be given\nin a forthcoming GCN Circular.\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34917.",
"published": "2023-10-31T23:26:58.706639Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-31T23:26:58.706656Z",
"modified": "2023-10-31T23:26:58.711583Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 3870,
"topic": "gcn.circular",
"uuid": "307ce196-21c5-4fe8-b844-d42662f2afc1",
"title": "IceCube-231014A - IceCube observation of a high-energy neutrino candidate track-like event",
"submitter": "Hop gcn.circular",
"authors": "Marcos Santander at U of Alabama <jmsantander@ua.edu>",
"data": {
"date": "23/10/14 23:19:35 GMT",
"from": "Marcos Santander at U of Alabama <jmsantander@ua.edu>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34817"
},
"title": "GCN CIRCULAR",
"number": "34817",
"subject": "IceCube-231014A - IceCube observation of a high-energy neutrino candidate track-like event"
},
"message_text": "The IceCube Collaboration (http://icecube.wisc.edu/) reports:\n\nOn 2023-10-14 at 22:00:06.27 UT IceCube detected a track-like event with a high probability of being of astrophysical origin. The event was selected by the ICECUBE_Astrotrack_BRONZE alert stream. The average astrophysical neutrino purity for Bronze alerts is 30%. This alert has an estimated false alarm rate of 4.853 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/138449_20481611.amon) more sophisticated reconstruction algorithms have been applied offline, with the direction refined to:\n\nDate: 2023-10-14\nTime: 22:00:06.27 UT\nRA: 297.16 (+2.73 / -4.32 deg 90% PSF containment) J2000\nDec: +1.34 (+1.24 / -1.11 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\nTwo Fermi 4FGL-DR4 sources are located in the 90% uncertainty region of the event. The sources are 4FGL J1947.0+0031 at RA = 296.76 deg, Dec = +0.52 and 4FGL J1955.7+0214 at RA = 298.94 deg, Dec = +2.24, located 0.91 and 1.99 deg away from the best fit position, respectively.\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\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34817.",
"published": "2023-10-14T23:19:50.694469Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-14T23:19:50.694497Z",
"modified": "2023-10-14T23:19:50.701592Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 3879,
"topic": "gcn.circular",
"uuid": "d250d6bc-b0f6-4c9e-8aa9-03d00821167a",
"title": "Discovery of an optical transient with strong flaring activity: a new blazar candidate in the Messier 31 field.",
"submitter": "Hop gcn.circular",
"authors": "Gianluca Masi at Bellatrix Astronomical Obs <gianluca@bellatrixobservatory.org>",
"data": {
"date": "23/10/15 16:23:11 GMT",
"from": "Gianluca Masi at Bellatrix Astronomical Obs <gianluca@bellatrixobservatory.org>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34818"
},
"title": "GCN CIRCULAR",
"number": "34818",
"subject": "Discovery of an optical transient with strong flaring activity: a new blazar candidate in the Messier 31 field."
},
"message_text": "On 15 Aug. 2023, during a regular survey work on the Messier 31 (NGC 224) field, performed with the 0.25m-f/4.5 robotic unit part of the Virtual Telescope Project facility in Manciano, Italy, we discovered a bright object on several unfiltered images, located at RA,DEC=00 43 54.36, +40 46 34.0 (J2000.0 astrometry from the discovery image). On 15.07 Aug. 2023 we estimated it at R=18.2 (R-mags for the reference stars from the Gaia DR2 catalogue). We have found the source by comparing the 15 Aug. images with 10.91 Aug. ones, taken via the same equipment. On the 10.91 Aug. images, the source was at R=18.9. We labelled this source as VTP J004354.36+404634.0 within our survey program. \n\nWe queried Simbad at the mentioned coordinates, concluding it is most likely an optical counterpart to a nearby ( r < 1â)Â radio source NVSS J004354+404634. At the same position, Vizier reports a few entries for X-ray sources. \n\nSDSS (DR16) reports an optical source at two different epochs at the mentioned coordinates: \n2002.7634: g=22.6 and r=22.5 (errors: 0.2 mags)\n2002.7584: g=23.8 and r=23.4 (errors: 0.9 and 0.6 mags, respectively) \n\nPan-STARRS DR1 reports an optical source, too: \n11 July 2012: g=22.08 and r=21.24 (errors: 0.08 and 0.07 mags, respectively) \n\nOn 22 Aug. 2023, the MASTER survey detected a mag. 18.2 (clear) object, reporting it as a probable nova in M31, with no follow-up:\nhttps://www.wis-tns.org/object/2023qhf\n\nThe CRTS archival light curve shows evident optical variability in V-band between 2006 and 2013, never brighter than V=18.6 (with detection limit at about V=21). \n\nOur data, from 10 Aug. 2023 to 13 Oct. 2023 likely covers an unprecedented bright flare reaching R=17.6 on 19.82 Aug. 2023 (UT). The source has been brighter than R=19.0 for more than 60 days in a row now. Detailed photometry is provided below (dates/times are UT, year is 2023): \n\n10.91 Aug.: 18.9\n11.91 Aug.: 18.7 \n15.07 Aug.: 18.2 \n20.88 Aug.: 18.3 \n09.84 Sept.: 18.0 \n10.82 Sept.: 18.0 \n11.82 Sept.: 17.9 \n15.86 Sept.: 18.0 \n16.96 Sept.: 17.9 \n19.82 Sept.: 17.6 \n20.87 Sept.: 17.8 \n23.82 Sept.: 17.9 (bright Moon in the sky) \n24.96 Sept.: 18.2 \n27.08 Sept.: 18.7 (very bright Moon in the sky) \n01.76 Oct.: 18.4 \n02.76 Oct.: 18.8 \n03.77 Oct.: 18.6 \n05.82 Oct.: 18.9 \n06.78 Oct.: 18.6 \n08.00 Oct.: 18.8\n08.80 Oct.: 18.8 \n09.77 Oct.: 18.9 \n11.85 Oct.: 18.8 \n12.85 Oct.: 18.7 \n13.76 Oct.: 18.5 \n \nErrors are around 0.1 mag. for the brighter values and around 0.3 mags for the fainter ones. \n \nThe scenario summarized above suggests that the variable optical source we have discovered is the optical counterpart of a blazar. \n \nA spectrum taken on 24 Sept. 2023 upon our request at the Copernico telescope operated by INAF Osservatorio Astronomico di Padova in Asiago-Ekar under poor sky conditions, with a resulting low S/N ration, does not show obvious, strong features, this supporting our hypothesis of the blazar nature for this transient.\n \nMulti-wavelength observations are strongly encouraged. \n \nWe wish to thank Lina Tomasella, Osservatorio Astronomico di Padova, Makoto Uemura, Hiroshima University, and Telescope Live for the precious support and fruitful discussion. \n \nDetails about our work are available here: \nhttps://www.virtualtelescope.eu/2023/08/16/discovery-of-variability-of-the-optical-counterpart-of-the-nvss-j004354404634-radio-source-in-the-messier-31-field/\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34818.",
"published": "2023-10-15T16:23:28.306864Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-15T16:23:28.306888Z",
"modified": "2023-10-15T16:23:28.314550Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 3880,
"topic": "gcn.circular",
"uuid": "7ea86a64-e13c-4584-9d5d-a34422041ab4",
"title": "(correction) Discovery of an optical transient with strong flaring activity: a new blazar candidate in the Messier 31 field",
"submitter": "Hop gcn.circular",
"authors": "Gianluca Masi at Bellatrix Astronomical Obs <gianluca@bellatrixobservatory.org>",
"data": {
"date": "23/10/15 16:25:55 GMT",
"from": "Gianluca Masi at Bellatrix Astronomical Obs <gianluca@bellatrixobservatory.org>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34819"
},
"title": "GCN CIRCULAR",
"number": "34819",
"subject": "(correction) Discovery of an optical transient with strong flaring activity: a new blazar candidate in the Messier 31 field"
},
"message_text": "On 15 Aug. 2023, during a regular survey work on the Messier 31 (NGC 224) field, performed with the 0.25m-f/4.5 robotic unit part of the Virtual Telescope Project facility in Manciano, Italy, we discovered a bright object on several unfiltered images, located at RA,DEC=00 43 54.36, +40 46 34.0 (J2000.0 astrometry from the discovery image). On 15.07 Aug. 2023 we estimated it at R=18.2 (R-mags for the reference stars from the Gaia DR2 catalogue). We have found the source by comparing the 15 Aug. images with 10.91 Aug. ones, taken via the same equipment. On the 10.91 Aug. images, the source was at R=18.9. We labelled this source as VTP J004354.36+404634.0 within our survey program. \n\nWe queried Simbad at the mentioned coordinates, concluding it is most likely an optical counterpart to a nearby ( r < 1â)Â radio source NVSS J004354+404634. At the same position, Vizier reports a few entries for X-ray sources. \n\nSDSS (DR16) reports an optical source at two different epochs at the mentioned coordinates: \n2002.7634: g=22.6 and r=22.5 (errors: 0.2 mags)\n2002.7584: g=23.8 and r=23.4 (errors: 0.9 and 0.6 mags, respectively) \n\nPan-STARRS DR1 reports an optical source, too: \n11 July 2012: g=22.08 and r=21.24 (errors: 0.08 and 0.07 mags, respectively) \n\nOn 22 Aug. 2023, the MASTER survey detected a mag. 18.2 (clear) object, reporting it as a probable nova in M31, with no follow-up:\nhttps://www.wis-tns.org/object/2023qhf\n\nThe CRTS archival light curve shows evident optical variability in V-band between 2006 and 2013, never brighter than V=18.6 (with detection limit at about V=21). \n\nOur data, from 10 Aug. 2023 to 13 Oct. 2023 likely covers an unprecedented bright flare reaching R=17.6 on 19.82 Aug. 2023 (UT). The source has been brighter than R=19.0 for more than 60 days in a row now. Detailed photometry is provided below (dates/times are UT, year is 2023): \n\n10.91 Aug.: 18.9\n11.91 Aug.: 18.7 \n15.07 Aug.: 18.2 \n20.88 Aug.: 18.3 \n09.84 Sept.: 18.0 \n10.82 Sept.: 18.0 \n11.82 Sept.: 17.9 \n15.86 Sept.: 18.0 \n16.96 Sept.: 17.9 \n19.82 Sept.: 17.6 \n20.87 Sept.: 17.8 \n23.82 Sept.: 17.9 (bright Moon in the sky) \n24.96 Sept.: 18.2 \n27.08 Sept.: 18.7 (very bright Moon in the sky) \n01.76 Oct.: 18.4 \n02.76 Oct.: 18.8 \n03.77 Oct.: 18.6 \n05.82 Oct.: 18.9 \n06.78 Oct.: 18.6 \n08.00 Oct.: 18.8\n08.80 Oct.: 18.8 \n09.77 Oct.: 18.9 \n11.85 Oct.: 18.8 \n12.85 Oct.: 18.7 \n13.76 Oct.: 18.5 \n \nErrors are around 0.1 mag. for the brighter values and around 0.3 mags for the fainter ones. \n \nThe scenario summarized above suggests that the variable optical source we have discovered is the optical counterpart of a blazar. \n \nA spectrum taken on 24 Sept. 2023 upon our request at the Copernico telescope operated by INAF Osservatorio Astronomico di Padova in Asiago-Ekar under poor sky conditions, with a resulting low S/N ration, does not show obvious, strong features, this supporting our hypothesis of the blazar nature for this transient.\n \nMulti-wavelength observations are strongly encouraged. \n \nWe wish to thank Lina Tomasella, Osservatorio Astronomico di Padova, Makoto Uemura, Hiroshima University, and Telescope Live for the precious support and fruitful discussion. \n \nDetails about our work are available here: \nhttps://www.virtualtelescope.eu/2023/08/16/discovery-of-variability-of-the-optical-counterpart-of-the-nvss-j004354404634-radio-source-in-the-messier-31-field/\n\nGianluca Masi\nVirtual Telescope Project\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34819.",
"published": "2023-10-15T16:26:03.128593Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-15T16:26:03.128622Z",
"modified": "2023-10-15T16:26:03.142850Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4199,
"topic": "gcn.circular",
"uuid": "2e502e3a-aa63-42ce-a222-9bc8b9d34b3d",
"title": "GRB 231024A: AKO Optical Counterpart Candidate",
"submitter": "Hop gcn.circular",
"authors": "Mohammad Odeh at Al Khatim Observatory M44 <mshodeh@gmail.com>",
"data": {
"date": "23/10/30 12:04:57 GMT",
"from": "Mohammad Odeh at Al Khatim Observatory M44 <mshodeh@gmail.com>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34910"
},
"title": "GCN CIRCULAR",
"number": "34910",
"subject": "GRB 231024A: AKO Optical Counterpart Candidate"
},
"message_text": "Mohammad Odeh (Al-Khatim Observatory, AKO, operated by the International\nAstronomical Center in Abu Dhabi, UAE), and Dalya Akl, Ilmah Abdi, and\nNidhal Guessoum (American University of Sharjah, UAE), report:\n\nWe observed the field of GRB 231024A (Fermi GBM Team, GCN 34876; Gompertz\net al., GCN 34878; Iglesias-López et al., GCN 34881; Saccardi et al., GCN\n34882; Scotton et. al., GCN 34885) with our 0.36m f/7.7 robotic telescope.\n\nThe observation was done on 29 October 2023 from 17:31 UT to 19:14 UT, 5.21\ndays after the trigger. We obtained 32x180 sec. images using (Ic) filter.\n\nWe detected the optical afterglow candidate of GRB 231024A in our stacked\nimages at the coordinates (J2000.0): R.A.: 00:55:07.28, Dec.: -15:15:19.6,\nwhich is consistent with the observation of (Gompertz et al., GCN 34878).\n\nThe following magnitude was calculated using the Atlas catalogue as a\nreference:\n-----------------------------------------------------------------------------\nObsTime (mid), Exposure (sec), Filter, Mag, MagRMS\n-----------------------------------------------------------------------------\n2023-10-29T18:24:01Z, 32x180s (stacked), Ic, 18.3, 0.16\n-----------------------------------------------------------------------------\n\nThe magnitude is not corrected for galactic extinction.\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34910.",
"published": "2023-10-31T23:26:58.939886Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-31T23:26:58.939905Z",
"modified": "2023-10-31T23:26:58.944617Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4200,
"topic": "gcn.circular",
"uuid": "926e8dca-9760-429b-acf3-ebe72ef29ff8",
"title": "GRB 231028A: Swift-BAT refined analysis",
"submitter": "Hop gcn.circular",
"authors": "Tyler Parsotan at NASA GSFC <tyler.parsotan@nasa.gov>",
"data": {
"date": "23/10/30 17:03:43 GMT",
"from": "Tyler Parsotan at NASA GSFC <tyler.parsotan@nasa.gov>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34914"
},
"title": "GCN CIRCULAR",
"number": "34914",
"subject": "GRB 231028A: Swift-BAT refined analysis"
},
"message_text": "H. A. Krimm (NSF), S. D. Barthelmy (GSFC),\nS. Laha (GSFC/UMBC), A. Y. Lien (U Tampa),\nC. B. Markwardt (GSFC), D. M. Palmer (LANL),\nT. Parsotan (GSFC/UMBC), T. Sakamoto (AGU),\nM. Stamatikos (OSU) (i.e. the Swift-BAT team):\n\nUsing the data set from T-240 to T+962 sec from the recent telemetry downlink,\nwe report further analysis of BAT GRB 231028A (trigger #1193078)\n(Williams et al., GCN Circ. 34894). The BAT ground-calculated position is\nRA, Dec = 214.016, 20.897 deg which is\n RA(J2000) = 14h 16m 03.8s\n Dec(J2000) = +20d 53' 47.8\"\nwith an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).\nThe partial coding was 68%.\n\nThe mask-weighted lightcurve shows a broad initial pulse with subsequent\nextended emission.\nT90 (15-350 keV) is 37.23 +- 0.98 sec (estimated error including systematics).\n\nThe time-averaged spectrum from T-6.86 to T+41.95 sec is best fit by a simple\npower-law model. The power law index of the time-averaged spectrum is\n1.40 +- 0.04. The fluence in the 15-150 keV band is 7.2 +- 0.2 x 10^-06 erg/cm2.\nThe 1-sec peak photon flux measured from T+1.06 sec in the 15-150 keV band\nis 8.6 +- 0.4 ph/cm2/sec. All the quoted errors are at the 90% confidence\nlevel.\n\nThe results of the batgrbproduct analysis are available at\nhttp://gcn.gsfc.nasa.gov/notices_s/1193078/BA/\n\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34914.",
"published": "2023-10-31T23:26:58.950900Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-31T23:26:58.950919Z",
"modified": "2023-10-31T23:26:58.956541Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6316,
"topic": "gcn.circular",
"uuid": "719d9f09-08f6-40d1-9351-49ed92f9596e",
"title": "X-ray transient EP240331A: GRANDMA-Kilonova catcher optical upper limit",
"submitter": "Hop gcn.circular",
"authors": "Sarah Antier at OCA <sarah.antier@oca.eu>",
"data": {
"date": "24/04/02 13:41:41 GMT",
"from": "Sarah Antier at OCA <sarah.antier@oca.eu>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/36010"
},
"title": "GCN CIRCULAR",
"number": "36010",
"subject": "X-ray transient EP240331A: GRANDMA-Kilonova catcher optical upper limit"
},
"message_text": "M. Freeberg (KNC), S. Antier (OCA), X. Wang (Tsinghua), W. M Yuan (NAOC), D. Turpin (CEA-Saclay/Irfu), M. Masek (FZU), M. Prouza (FZU), S. Karpov (FZU), I. Tosta e Melo (UniCT-DFA), P. Hello (IJCLAB), T. Pradier (Unistra/IPHC), M. Coughlin (UMN), C. Andrade (UMN), P-A Duverne (APC), N. Guessoum (AUS), H-B Eggenstein (KNC):\n\non behalf of the GRANDMA collaboration:\n\nWe performed a target of opportunity observations with GRANDMA and its citizen science project Kilonova-catcher (KNC) on the X-ray flare EP20240331a detected by Einstein Probe (EP) WXT on T0 = 2024-03-31T22:07:17 (Pan et al.,2024, ATel #16564).\n\nWe did not find any optical counterpart :\n\na) using FRAM-CTA-N within 25 arcmin error box centered at 11:17:39.36 -20:02:31.20 (RA,DEC= 169.414, -20.042) on 2024-04-01 23:59:15.000 (1.07 day post T0). Our image limiting magnitudes are Rc = 19 and V = 19 (Vega)\nb) using KNC-T72 (Chile) within a 20 arcmin error box centered at 11:17:39.36 -20:02:31.20 (RA,DEC= 169.414, -20.042) on 2024-04-02 02:01:20.00 (1.16 day post T0). Our image limiting magnitude is Rc = 20.5 (Vega)\n\nImages were calibrated with Gaïa Catalog, using STDpipe (Karpov, 2020).\n\nThese results are consistent with Groot et al., GCN 36007 and Lipunov et al., GCN 36009.\n\nWe thank the Einstein Probe team for useful communication.\n\nGRANDMA is a worldwide telescope network (grandma.ijclab.in2p3.fr) devoted to the observation of transients in the context of multi-messenger astrophysics (Antier et al. 2020 MNRAS 497, 5518). Kilonova-Catcher (KNC) is the citizen science program of GRANDMA (http://kilonovacatcher.in2p3.fr/).\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/36010.",
"published": "2024-04-02T13:41:58.930706Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-04-02T13:41:58.930737Z",
"modified": "2024-04-02T13:41:58.938428Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 3903,
"topic": "gcn.circular",
"uuid": "a926b479-5aa6-42b0-9e31-fb6380aa0d40",
"title": "LIGO/Virgo/KAGRA S231014r: Upper limits from Swift/BAT-GUANO",
"submitter": "Hop gcn.circular",
"authors": "Samuele Ronchini at PSU <sjs8171@psu.edu>",
"data": {
"date": "23/10/16 13:49:41 GMT",
"from": "Samuele Ronchini at PSU <sjs8171@psu.edu>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34820"
},
"title": "GCN CIRCULAR",
"number": "34820",
"subject": "LIGO/Virgo/KAGRA S231014r: Upper limits from Swift/BAT-GUANO"
},
"message_text": "Samuele Ronchini (PSU), Tyler Parsotan (NASA GSFC), James DeLaunay (U Alabama), Gayathri Raman (PSU), Jamie A. Kennea (PSU), Aaron Tohuvavohu (U Toronto) report:\n\nSwift/BAT was observing 84.9% of the GW localization probability (bayestar.multiorder.fits) at merger time. A fraction 24.4 % of the GW localization posterior is contained inside the BAT coded FoV.\n\nThe LVK 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\nUsing the NITRATES analysis (DeLaunay + Tohuvavohu 2022, ApJ, 941, 169), we searched for emission on 8 timescales from 0.128s to 16.384s in the interval [-20,+20] seconds around the merger time. We find no evidence for a signal, and derive the following upper limits.\n\nWe quote the 5-sigma flux upper limits in the 15-350 keV band, weighted over the GW localization, for four spectral templates (soft, normal, and hard GRB-like templates described in [arXiv:1612.02395], and spectral shape from GRB170817A [arXiv:1710.05446]) and for four time bins.\nIn units of 10^-7 erg/s/cm^2:\n\ntime_bin (s) soft normal hard GRB170817\n------------------------------------\n0.256 14.1 9.87 8.93 10.8\n1.024 8.81 6.16 5.57 6.76\n4.096 6.89 4.82 4.36 5.29\n16.38 5.73 4.01 3.63 4.40\n\nThe upper limits as function of sky position are plotted here, alongside the GW localization:\nhttps://doi.org/10.5281/zenodo.10005469\nThe solid and dashed lines indicate the 90% and 50% GW contour levels, respectively.\n\nThe corresponding fits file can be found here:\nhttps://doi.org/10.5281/zenodo.10005473\n\nGUANO is a fully autonomous, extremely low latency, spacecraft\ncommanding pipeline designed for targeted recovery of BAT event mode\ndata around the times of compelling astrophysical events to enable\nmore sensitive GRB searches.\n\nA live reporting of Swift/BAT event data recovered by GUANO can be\nfound at: https://www.swift.psu.edu/guano/\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34820.",
"published": "2023-10-16T13:49:53.549166Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-16T13:49:53.549203Z",
"modified": "2023-10-16T13:49:53.559250Z",
"nonlocalizedevents": [
{
"event_id": "S231014r"
}
],
"targets": []
},
{
"id": 6317,
"topic": "gcn.circular",
"uuid": "23c7726a-8a79-4489-bc1f-3bd4cf9ca0f3",
"title": "X-ray transient EP240331a: Kinder optical upper limits",
"submitter": "Hop gcn.circular",
"authors": "Janet Chen at National Central University <janetstars@gmail.com>",
"data": {
"date": "24/04/02 19:06:39 GMT",
"from": "Janet Chen at National Central University <janetstars@gmail.com>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/36011"
},
"title": "GCN CIRCULAR",
"number": "36011",
"subject": "X-ray transient EP240331a: Kinder optical upper limits"
},
"message_text": "T.-W. Chen (NCUIA), S. Yang (HNAS), S. Smartt (Oxford), H.-Y. Hsiao, W.-J. Hou, A. Sankar.K, Y.-C. Pan, M.-H. Lee, C.-H. Lai, C.-C. Ngeow, C.-S. Lin, H.-C. Lin, J.-K. Guo (all NCUIA), S. Srivastav (Oxford) and M. Fulton, T. Moore, C. Angus, A. Aamer (all QUB) report:\n\nWe observed the field of EP240331a (Pan et al. 2024, ATel #16564) using several telescopes at the Lulin Observatory, Taiwan as part of the Kinder collaboration (Chen et al., AstroNote 2021-92), including the Lulin One-meter Telescope (LOT) with r band, 40cm Super Light Telescope (SLT) with g band, and 50cm Lulin-ASIAA Telescope for Transients and Education (LATTE) with B band.\n\nThe first LOT epoch started at 15:55 UT on April 1, 2024 (MJD = 60401.663), 0.74 days (\u0017.8 hours) after the discovery of the X-ray transient, EP240331a. We observed 4 pointings in order to cover its reported 20 arcmin error box. Each pointing were observed for 4 times, with 300-second exposure time each, taken under seeing conditions averaging 1\".7 and at a median airmass of 1.63.\n\nWe used the Kinder pipeline (Yang et al. A&A 646, A22) to stack the images with same pointing and subtract the stacked images with the Pan-STARRS1 template images. We found a possible variable at the location of RA = 11:17:32.8593, Dec = -20:06:28.335 in the difference images. The object was measured to have an r-band magnitude of 20.61+/-0.08 mag. We then cross checked it with several archived catalogs and found it was clearly detected in the Legacy Survey DR10 image, marked as a star with r = 20.75 mag. We measured this source in the Pan-STARRS1 image and obtained r = 21.00 +/- 0.15 mag. The variation indicates a possible variable star, but we cannot rule out AGN either.\n\nBesides this variable, we do not detect any other significant optical counterpart candidates. In 2.5 sigma level, we obtained the following preliminary upper limits (in the AB system):\n\ng > 21.2 and\nr > 21.9 mag.\n\nThe given limits are 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). Our B-band images are shallower and not calibrated so we do not report the limits here.\n\nOur result is consistent with MeerLICHT (Groot et al., GCN 36007), MASTER (Lipunov et al., GCN 36009) and GRANDMA (Freeberg et al., ATel #16567; GCN 36010); our optical upper limit is deeper than these reports and confirm there is no significant optical counterpart within the first day after the X-ray trigger.\n\nWe thank ASIAA for providing LATTE for the observations, and thank the Einstein Probe team for useful communication.\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/36011.",
"published": "2024-04-02T19:06:59.539434Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-04-02T19:06:59.539450Z",
"modified": "2024-04-02T19:06:59.547673Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 3908,
"topic": "gcn.circular",
"uuid": "26885cc1-acd0-429b-b7df-5ab23ec8c26f",
"title": "IceCube-231014A: 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": "23/10/16 17:12:25 GMT",
"from": "Jessie Thwaites at IceCube/U Wisc-Madison <thwaites@wisc.edu>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34821"
},
"title": "GCN CIRCULAR",
"number": "34821",
"subject": "IceCube-231014A: 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-231014A (https://gcn.nasa.gov/circulars/34817) in a time range of 1000 seconds centered on the alert event time (2023-10-14 21:51:46.260 UTC to 2023-10-14 22:08:26.260 UTC) during which IceCube was collecting good quality data. Excluding the event that prompted the alert, zero track-like events are found within the 90% containment region of IceCube-231014A.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-231014A ranges from 1.4e-01 to 1.5e-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 3e+02 GeV and 2e+05 GeV.\n\nA subsequent search was performed including 2 days of data centered on the alert event time (2023-10-13 22:00:06.260 UTC to 2023-10-15 22:00:06.260 UTC). In this case, we report a p-value of 1.00, 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-231014A is 1.6e-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/34821.",
"published": "2023-10-16T17:12:40.984008Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-16T17:12:40.984030Z",
"modified": "2023-10-16T17:12:40.991055Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 3937,
"topic": "gcn.circular",
"uuid": "e8b6370f-873e-4dc1-a030-757cbff0a029",
"title": "GRB 231017A: Swift/BAT-GUANO candidate arcminute localization of a burst",
"submitter": "Hop gcn.circular",
"authors": "Jimmy DeLaunay at University of Alabama <delauj2@gmail.com>",
"data": {
"date": "23/10/17 15:30:08 GMT",
"from": "Jimmy DeLaunay at University of Alabama <delauj2@gmail.com>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34824"
},
"title": "GCN CIRCULAR",
"number": "34824",
"subject": "GRB 231017A: Swift/BAT-GUANO candidate arcminute localization of a burst"
},
"message_text": "James DeLaunay (U Alabama, PSU), Aaron Tohuvavohu (U Toronto), Gayathri Raman (PSU), Jamie A. Kennea (PSU), Tyler Parsotan (NASA GSFC) report:\n\nSwift/BAT did not localize GRB 231017A onboard (T0: 2023-10-17T08:05:03.30 UTC, Fermi/GBM GCN 34822, Trigger 719222708).\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 15 in a 2.048 s analysis time bin, starting at T0 - 0.512 s. \n\nA candidate arcminute localization is found with DeltaLLHOut of 17 and a DeltaLLHPeak of 6.\n\nSee Section 9.1 and Figures 10 and 17 in the NITRATES paper for brief descriptions and interpretations of sqrt(TS), DeltaLLHPeak, and DeltaLLHOut.\n\nThe BAT position is\nRA, Dec = 86.191, +56.666 deg which is\n RA(J2000) = 05 44m 45.84s\n Dec(J2000) = +56d 39â² 57.6â³\nwith an estimated uncertainty of 6 arcmin radius.\n\nXRT and UVOT follow-up has been requested.\nResults of follow-up observations will be reported in future circulars.\n\nGUANO is a fully autonomous, extremely low latency, spacecraft\ncommanding pipeline designed for targeted recovery of BAT event mode\ndata around the times of compelling astrophysical events to enable\nmore sensitive GRB searches.\n\nA live reporting of Swift/BAT event data recovered by GUANO can be\nfound at: https://www.swift.psu.edu/guano/\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34824.",
"published": "2023-10-17T15:30:15.914983Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-17T15:30:15.915016Z",
"modified": "2023-10-17T15:30:15.921487Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4201,
"topic": "gcn.circular",
"uuid": "1c3df3d6-b076-4843-9424-8813e3d6590a",
"title": "GRB 231030B: 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": "23/10/30 20:08:47 GMT",
"from": "Fermi GBM Team at MSFC/Fermi-GBM <do_not_reply@GIOC.nsstc.nasa.gov>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34915"
},
"title": "GCN CIRCULAR",
"number": "34915",
"subject": "GRB 231030B: Fermi GBM Final Real-time Localization"
},
"message_text": "The Fermi GBM team reports the detection of a likely LONG GRB\n\nAt 19:58:19 UT on 30 Oct 2023, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 231030B (trigger 720388704.937126 / 231030832).\n\nThe on-ground calculated location, using the Fermi GBM trigger data, is RA = 244.0, Dec = 56.5 (J2000 degrees, equivalent to J2000 16h 15m, 56d 30'), with a statistical uncertainty of 1.1 degrees.\n\nThe angle from the Fermi LAT boresight is 47.0 degrees.\n\nThe skymap can be found here:\nhttps://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn231030832/quicklook/glg_skymap_all_bn231030832.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/2023/bn231030832/quicklook/glg_healpix_all_bn231030832.fit\n\nThe GBM light curve can be found here:\nhttps://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn231030832/quicklook/glg_lc_medres34_bn231030832.gif\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34915.",
"published": "2023-10-31T23:26:58.971249Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-31T23:26:58.971286Z",
"modified": "2023-10-31T23:26:58.977002Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 3935,
"topic": "gcn.circular",
"uuid": "55401341-e348-4a1c-a97d-139485b5a75d",
"title": "GRB231017A: Fermi GBM Final Localization",
"submitter": "Hop gcn.circular",
"authors": "Joe Mangan at IJCLab <joseph.mangan@ijclab.in2p3.fr>",
"data": {
"date": "23/10/17 14:51:29 GMT",
"from": "Joe Mangan at IJCLab <joseph.mangan@ijclab.in2p3.fr>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34822"
},
"title": "GCN CIRCULAR",
"number": "34822",
"subject": "GRB231017A: Fermi GBM Final Localization"
},
"message_text": "The Fermi GBM team reports the detection of a likely Long GRB.\n\nAt 08:05:03.30 UT on 17 October 2023, the Fermi Gamma-Ray Burst Monitor (GBM) triggered and located GRB231017A (trigger 719222708 / 231017337).\n\nThe on-ground calculated location, using the GBM trigger data, is RA = 88.8, DEC = 57.2 (J2000 degrees, equivalent to 5h 55m, 57d 09'), with a statistical uncertainty of 5.7 degrees (radius, 1-sigma containment, statistical only; there is additionally a systematic error which we have characterized as a core-plus-tail model, with 90% of GRBs having a 3.7 deg error and a small tail suffering a larger than 10 deg systematic error. [Connaughton et al. 2015, ApJS, 216, 32] ).\n\nThe angle from the Fermi LAT boresight at the GBM trigger time is 58 degrees.\n\nThe skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn231017337/quicklook/glg_skymap_all_bn231017337.png\n\nThe HEALPix FITS file, including the estimated localization systematic, can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn231017337/quicklook/glg_healpix_all_bn231017337.fit\n\nThe GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn231017337/quicklook/glg_lc_medres34_bn231017337.gif\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34822.",
"published": "2023-10-17T14:51:45.304091Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-17T14:51:45.304122Z",
"modified": "2023-10-17T14:51:45.331366Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 3936,
"topic": "gcn.circular",
"uuid": "e77286e0-b9bb-4fe1-b59c-70bb87d9ce1c",
"title": "Fermi-LAT gamma-ray observations of IceCube-231014A",
"submitter": "Hop gcn.circular",
"authors": "Simone Garrappa at DESY <simone.garrappa@desy.de>",
"data": {
"date": "23/10/17 15:25:12 GMT",
"from": "Simone Garrappa at DESY <simone.garrappa@desy.de>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34823"
},
"title": "GCN CIRCULAR",
"number": "34823",
"subject": "Fermi-LAT gamma-ray observations of IceCube-231014A"
},
"message_text": "S. Garrappa (Weizmann Institute of Science), C. Bartolini (INFN Bari), S. Buson (Uni Wuerzburg) and J. Sinapius (DESY) on behalf of the Fermi-LAT collaboration:\n\nWe report an analysis of observations of the vicinity of the IC231014A high-energy neutrino event (GCN 34817) 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 2023-10-14 at 22:00:06.27 UT (T0) with J2000 position RA = 297.16 (+2.73, -4.32) deg, Decl. = +1.34 (+1.24, -1.11) deg (90% PSF containment). There are three Fermi 4FGL-DR4 cataloged gamma-ray (>100 MeV; The Fermi-LAT collaboration 2022, ApJS, 260, 53) sources in the 90% IC231014A uncertainty localization region. Based on a preliminary analysis of the LAT data over a month and day timescale prior T0, these objects are not significantly detected at gamma rays.\n\nWe searched for intermediate (days to years) timescale emission from a new gamma-ray source. Preliminary analysis indicates no significant (> 5 sigma) new excess emission (> 100 MeV) at the IC231014A best-fit position. Assuming a power-law spectrum (photon index = 2.0 fixed) for a point source at the IC231014A best-fit position, the >100 MeV flux upper limit (95% confidence) is < 3.1e-10 ph cm^-2 s^-1 for ~15-years (2008-08-04 to 2023-10-14 UTC), and < 1.8e-8 (< 1.1e-7) ph cm^-2 s^-1 for a 1-month (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 are S. Garrappa (simone.garrappa at weizmann.ac.il), C. Bartolini (chiara.bartolini at ba.infn.it), S. Buson (sara.buson at uni-wuerzburg.de) and J. Sinapius (jonas.sinapius at desy.de).\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\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34823.",
"published": "2023-10-17T15:25:23.943863Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-17T15:25:23.943884Z",
"modified": "2023-10-17T15:25:23.953699Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 3938,
"topic": "gcn.circular",
"uuid": "5bb281db-c7e6-42b7-bcf3-fb6a5b5f7713",
"title": "GRB 231017A: Swift ToO observations",
"submitter": "Hop gcn.circular",
"authors": "Phil Evans at U of Leicester <pae9@star.le.ac.uk>",
"data": {
"date": "23/10/17 17:27:04 GMT",
"from": "Phil Evans at U of Leicester <pae9@star.le.ac.uk>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34825"
},
"title": "GCN CIRCULAR",
"number": "34825",
"subject": "GRB 231017A: Swift ToO observations"
},
"message_text": "P. A. Evans (U. Leicester) reports on behalf of the Swift team:\n\nSwift has initiated a ToO observation of the Swift/BAT-GUANO GRB 231017A.\nAutomated analysis of the XRT data will be presented online at\nhttps://www.swift.ac.uk/ToO_GRBs/00021623\n\nAny uncatalogued X-ray sources detected in this analysis will be\nreported on this website and via GCN COUNTERPART notices. These are\nnot necessarily related to the Swift/BAT-GUANO event. Any X-ray source\nconsidered to be a probable afterglow candidate will be reported via a\nGCN Circular after manual consideration.\n\nDetails of the XRT automated analysis methods are detailed in Evans et\nal. (2007, A&A, 469, 379; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8).\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/34825.",
"published": "2023-10-17T17:27:15.700674Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-17T17:27:15.700695Z",
"modified": "2023-10-17T17:27:15.708684Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4202,
"topic": "gcn.circular",
"uuid": "402b95c1-ea50-4bb4-8bad-1cfeee131e11",
"title": "GRB 231028B: VZLUSAT-2 detection",
"submitter": "Hop gcn.circular",
"authors": "Marianna DafÄÃková at Masaryk University <500025@mail.muni.cz>",
"data": {
"date": "23/10/31 19:20:48 GMT",
"from": "Marianna DafÄÃková at Masaryk University <500025@mail.muni.cz>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34922"
},
"title": "GCN CIRCULAR",
"number": "34922",
"subject": "GRB 231028B: 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 231028B (Fermi/GBM detection: trigger no. 720224759; Konus/WIND detection at 2023-10-28 22:25:55.024 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 2023-10-28 22:25:58 (22:26:31) UTC. The T90 duration is 43 s (37 s) and the significance during T90 reaches 13 sigma (8 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/GRB231028B_GCN_VZLUSAT2.pdf\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\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34922.",
"published": "2023-10-31T23:26:58.990757Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-31T23:26:58.990825Z",
"modified": "2023-10-31T23:26:58.997399Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 3947,
"topic": "gcn.circular",
"uuid": "da41655c-856f-4372-80be-caf9890d8946",
"title": "GRB 231018A: 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": "23/10/18 12:40:39 GMT",
"from": "Fermi GBM Team at MSFC/Fermi-GBM <do_not_reply@GIOC.nsstc.nasa.gov>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34826"
},
"title": "GCN CIRCULAR",
"number": "34826",
"subject": "GRB 231018A: Fermi GBM Final Real-time Localization"
},
"message_text": "The Fermi GBM team reports the detection of a likely LONG GRB\n\nAt 12:30:10 UT on 18 Oct 2023, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 231018A (trigger 719325015.663762 / 231018521).\n\nThe on-ground calculated location, using the Fermi GBM trigger data, is RA = 3.0, Dec = 50.7 (J2000 degrees, equivalent to J2000 00h 12m, 50d 42'), with a statistical uncertainty of 1.0 degrees.\n\nThe angle from the Fermi LAT boresight is 131.0 degrees.\n\nThe skymap can be found here:\nhttps://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn231018521/quicklook/glg_skymap_all_bn231018521.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/2023/bn231018521/quicklook/glg_healpix_all_bn231018521.fit\n\nThe GBM light curve can be found here:\nhttps://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn231018521/quicklook/glg_lc_medres34_bn231018521.gif\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34826.",
"published": "2023-10-18T12:40:49.675734Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-18T12:40:49.675767Z",
"modified": "2023-10-18T12:40:49.686838Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 3948,
"topic": "gcn.circular",
"uuid": "b23f27f8-b23a-4022-94dd-30fc573eaf5d",
"title": "GRB 231018A: BALROG localization (Fermi Trigger / GRB 231018521)",
"submitter": "Hop gcn.circular",
"authors": "Jochen Greiner at MPE <jcgrog@mpe.mpg.de>",
"data": {
"date": "23/10/18 13:15:13 GMT",
"from": "Jochen Greiner at MPE <jcgrog@mpe.mpg.de>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34827"
},
"title": "GCN CIRCULAR",
"number": "34827",
"subject": "GRB 231018A: BALROG localization (Fermi Trigger / GRB 231018521)"
},
"message_text": "T. Preis, B. Biltzinger, J. Burgess & J. Greiner (all MPE Garching) report:\n\nThe public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger\n at 12:30:10 on 18 Oct. 2023 were automatically fitted for spectrum\nand sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427;\nBerlato et al. 2019, ApJ 873, 60).\n\nThe best-fit position (1 sigma statistical errors) is:\nRA(2000.0) = 1.2+/-0.5 deg\nDecl.(2000.0) = 51.5+/-0.2 deg\nWe estimate an additional systematic error of 1 deg.\n\nFurther details are available at:\nhttps://grb.mpe.mpg.de/grb/GRB231018521/\n\nThe Healpix map can be downloaded from:\nhttps://grb.mpe.mpg.de/grb/GRB231018521/healpix\n\nThe location parameters are available as JSON at:\nhttps://grb.mpe.mpg.de/grb/GRB231018521/json\n\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34827.",
"published": "2023-10-18T13:15:24.462961Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-18T13:15:24.462983Z",
"modified": "2023-10-18T13:15:24.470019Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4203,
"topic": "gcn.circular",
"uuid": "199568ec-b213-4d8f-984a-16920a5e4bff",
"title": "LIGO/Virgo/KAGRA S231029y: Upper limits from Swift/BAT-GUANO",
"submitter": "Hop gcn.circular",
"authors": "Samuele Ronchini at PSU <sjs8171@psu.edu>",
"data": {
"date": "23/10/30 13:44:36 GMT",
"from": "Samuele Ronchini at PSU <sjs8171@psu.edu>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34912"
},
"title": "GCN CIRCULAR",
"number": "34912",
"subject": "LIGO/Virgo/KAGRA S231029y: Upper limits from Swift/BAT-GUANO"
},
"message_text": "Samuele Ronchini (PSU), Tyler Parsotan (NASA GSFC), James DeLaunay (PSU), Gayathri Raman (PSU), Jamie A. Kennea (PSU), Aaron Tohuvavohu (U Toronto) report:\n\nSwift/BAT was observing 70.4% of the GW localization probability (bayestar.multiorder.fits) at merger time. A fraction 14.3 % of the GW localization posterior is contained inside the BAT coded FoV.\n\nThe LVK 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\nUsing the NITRATES analysis (DeLaunay + Tohuvavohu 2022, ApJ, 941, 169), we searched for emission on 8 timescales from 0.128s to 16.384s in the interval [-20,+20] seconds around the merger time. We find no evidence for a signal, and derive the following upper limits.\n\nWe quote the 5-sigma flux upper limits in the 15-350 keV band, weighted over the GW localization, for four spectral templates (soft, normal, and hard GRB-like templates described in [arXiv:1612.02395], and spectral shape from GRB170817A [arXiv:1710.05446]) and for four time bins.\nIn units of 10^-7 erg/s/cm^2:\n\ntime_bin (s) soft normal hard GRB170817\n------------------------------------\n0.256 13.4 9.6 8.6 10.6\n1.024 6.8 4.9 4.4 5.4\n4.096 3.7 2.7 2.4 3.0\n16.38 2.4 1.7 1.5 1.9\n\n\nThe upper limits as function of sky position are plotted here, alongside the GW localization:\nhttps://doi.org/10.5281/zenodo.10051951\nThe solid and dashed lines indicate the 90% and 50% GW contour levels, respectively.\n\nThe corresponding fits file can be found here:\nhttps://doi.org/10.5281/zenodo.10051953\n\nGUANO is a fully autonomous, extremely low latency, spacecraft\ncommanding pipeline designed for targeted recovery of BAT event mode\ndata around the times of compelling astrophysical events to enable\nmore sensitive GRB searches.\n\nA live reporting of Swift/BAT event data recovered by GUANO can be\nfound at: https://www.swift.psu.edu/guano/\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34912.",
"published": "2023-10-31T23:26:59.009220Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-31T23:26:59.009239Z",
"modified": "2023-10-31T23:26:59.014221Z",
"nonlocalizedevents": [
{
"event_id": "S231029y"
}
],
"targets": []
},
{
"id": 3951,
"topic": "gcn.circular",
"uuid": "619a096d-b9ee-428b-9eee-922991600391",
"title": "GRB 231012B may not be a GRB",
"submitter": "Hop gcn.circular",
"authors": "Vidushi Sharma at NASA GSFC/UMBC <vidushi.sharma@nasa.gov>",
"data": {
"date": "23/10/18 14:37:59 GMT",
"from": "Vidushi Sharma at NASA GSFC/UMBC <vidushi.sharma@nasa.gov>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34828"
},
"title": "GCN CIRCULAR",
"number": "34828",
"subject": "GRB 231012B may not be a GRB"
},
"message_text": "V. Sharma (NASA GSFC/UMBC) reports on behalf of the Fermi Gamma-ray Burst Monitor Team:\n\nThe Fermi Gamma-ray Burst Monitor (GBM) trigger 718822496/231012705, which occurred at 16:54:51 UT on 12 October 2023, was tentatively classified as GRB 231012B (GCN 34815). However, we are uncertain about its classification as a GRB and can likely be due to distant particles.\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34828.",
"published": "2023-10-18T14:38:10.176660Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-18T14:38:10.176691Z",
"modified": "2023-10-18T14:38:10.185027Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 3956,
"topic": "gcn.circular",
"uuid": "418070dc-1a75-4621-b644-3ed8a742c951",
"title": "GRB 231017A: Swift-XRT observations",
"submitter": "Hop gcn.circular",
"authors": "Phil Evans at U of Leicester <pae9@star.le.ac.uk>",
"data": {
"date": "23/10/18 15:56:18 GMT",
"from": "Phil Evans at U of Leicester <pae9@star.le.ac.uk>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34829"
},
"title": "GCN CIRCULAR",
"number": "34829",
"subject": "GRB 231017A: Swift-XRT observations"
},
"message_text": "S. Dichiara (PSU), J.A. Kennea (PSU), J.P. Osborne (U. Leicester), K.L.\nPage (U. Leicester), A.P. Beardmore (U. Leicester), E. Ambrosi\n(INAF-IASFPA) , M. Capalbi (INAF-IASFPA), M. Perri (SSDC & INAF-OAR),\nA. Tohuvavohu (U. Toronto) and P.A. Evans (U. Leicester) reports on\nbehalf of the Swift-XRT team:\n\nSwift-XRT has performed follow-up observations of the\nSwift/BAT-GUANO-detected burst GRB 231017A (GCN Circ. 34824, DeLaunay\net al.), collecting 4.2 ks of Photon Counting (PC) mode data between\nT0+32.7 ks and T0+101.7 ks.\n\nOne uncatalogued X-ray source has been detected consistent with being\nwithin 493 arcsec of the Swift/BAT-GUANO position, it is below the RASS\nlimit and shows no definitive signs of fading. Therefore, at the\npresent time we cannot confirm this as the afterglow. Details of this\nsource are given below:\n\nSource 2:\n RA (J2000.0): 86.1666 = 05:44:39.99\n Dec (J2000.0): +56.7487 = +56:44:55.3\n Error: 8.4 arcsec (radius, 90% conf.)\n Count-rate: (2.09 [+1.11, -0.84])e-3 ct s^-1\n Distance: 301 arcsec from Swift/BAT-GUANO position.\n Flux: (3.3 [+1.8, -1.3])e-14 erg cm^-2 s^-1 (observed, 0.3-10 keV)\n\nTwo uncatalogued sources were also detected too far from the GRB\nposition to be likely afterglow candidates.\n\nThe results of the XRT-team automatic analysis of the XRT observations,\nincluding a position-specific upper limit calculator, are available at\nhttps://www.swift.ac.uk/ToO_GRBs/00021623.\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/34829.",
"published": "2023-10-18T15:56:33.831401Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-18T15:56:33.831438Z",
"modified": "2023-10-18T15:56:33.840349Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 3957,
"topic": "gcn.circular",
"uuid": "816d6b10-d1ed-4ec4-8f64-4fe14f6ba97c",
"title": "GRB 231017A: Fermi GBM Detection",
"submitter": "Hop gcn.circular",
"authors": "Joe Mangan at IJCLab <joseph.mangan@ijclab.in2p3.fr>",
"data": {
"date": "23/10/18 16:19:02 GMT",
"from": "Joe Mangan at IJCLab <joseph.mangan@ijclab.in2p3.fr>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34830"
},
"title": "GCN CIRCULAR",
"number": "34830",
"subject": "GRB 231017A: Fermi GBM Detection"
},
"message_text": "J.Mangan (CNRS/IJCLab), E. Bissaldi (Politecnico and INFN Bari) and C. Meegan (UAH) report on behalf of the Fermi Gamma-ray Burst Monitor Team:\n\n\"At 08:05:03.30 UT on 17 October 2023, the Fermi Gamma-ray Burst Monitor (GBM)\ntriggered and located GRB 231017A (trigger 719222708/231017337), which was also\ndetected by the Swift/BAT-GUANO (DeLaunay et al. 2023, GCN 34824).\n\nThe Fermi GBM Final Real-time Localization is reported in GCN 34822.\n\nThe GBM light curve consists of a single emission episode with a duration (T90)\nof about 4.8 s (50-300 keV). The time-averaged spectrum\nfrom T0-3.5 to T0+4.7 s is best fit by\na power law function with an exponential high-energy cutoff.\nThe power law index is -1.1 +/- 0.2 and the cutoff energy,\nparameterized as Epeak, is 270 +/- 82 keV.\n\nA Band function fits the spectrum equally well\nwith Epeak= 175 +/- 92 keV, alpha = -0.9 +/- 0.3 and beta = -1.9 +/- 0.3.\n\nThe event fluence (10-1000 keV) in this time interval is\n(1.7 +/- 0.2)E-06 erg/cm^2. The 64-msec peak photon flux measured\nstarting from T0+0.77 s in the 10-1000 keV band is 7.8 +/- 1.6 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/34830.",
"published": "2023-10-18T16:19:13.555609Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-18T16:19:13.555641Z",
"modified": "2023-10-18T16:19:13.563054Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6318,
"topic": "gcn.circular",
"uuid": "dd1d542d-9cb1-47b2-87a6-336c0fe2e7f6",
"title": "GRB 240402A: 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": "24/04/02 23:54:34 GMT",
"from": "Fermi GBM Team at MSFC/Fermi-GBM <do_not_reply@GIOC.nsstc.nasa.gov>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/36012"
},
"title": "GCN CIRCULAR",
"number": "36012",
"subject": "GRB 240402A: Fermi GBM Final Real-time Localization"
},
"message_text": "The Fermi GBM team reports the detection of a likely LONG GRB\n\nAt 23:44:04 UT on 2 Apr 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 240402A (trigger 733794249.222788 / 240402989).\n\nThe on-ground calculated location, using the Fermi GBM trigger data, is RA = 220.9, Dec = 29.3 (J2000 degrees, equivalent to J2000 14h 43m, 29d 18'), with a statistical uncertainty of 25.0 degrees.\n\nThe angle from the Fermi LAT boresight is 98.0 degrees.\n\nThe skymap can be found here:\nhttps://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240402989/quicklook/glg_skymap_all_bn240402989.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/bn240402989/quicklook/glg_healpix_all_bn240402989.fit\n\nThe GBM light curve can be found here:\nhttps://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240402989/quicklook/glg_lc_medres34_bn240402989.gif\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/36012.",
"published": "2024-04-02T23:54:51.504680Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-04-02T23:54:51.504698Z",
"modified": "2024-04-02T23:54:51.513873Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 3960,
"topic": "gcn.circular",
"uuid": "d6f47339-0b8d-4808-a74c-4e66dc1cf702",
"title": "GRB 231018A: Fermi GBM Detection",
"submitter": "Hop gcn.circular",
"authors": "Stephen Lesage at Fermi-GBM Team <sjl0014@uah.edu>",
"data": {
"date": "23/10/18 17:36:50 GMT",
"from": "Stephen Lesage at Fermi-GBM Team <sjl0014@uah.edu>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34831"
},
"title": "GCN CIRCULAR",
"number": "34831",
"subject": "GRB 231018A: Fermi GBM Detection"
},
"message_text": "S. Lesage (UAH), E. Bissaldi (Politecnico and INFN Bari) and C. Meegan (UAH)\nreport on behalf of the Fermi Gamma-ray Burst Monitor Team:\n\n\"At 12:30:10 UT on 18 October 2023, the Fermi Gamma-ray Burst Monitor (GBM)\ntriggered and located GRB 231018A (trigger 719325015/231018521).\nThe Fermi GBM Final Real-time Localization is reported in GCN 34826.\n\nThe angle from the Fermi LAT boresight is 131 degrees.\n\nThe GBM light curve consists of multiple multiple pulses with a duration (T90)\nof about 39.4 s (50-300 keV). The time-averaged spectrum\nfrom T0-4.6 to T0+92.7 s is best fit by\na Band function with Epeak = 109 +/- 3 keV,\nalpha = -1.24 +/- 0.02, and beta = -2.56 +/- 0.05.\n\nThe event fluence (10-1000 keV) in this time interval is\n(1.192 +/- 0.009)E-04 erg/cm^2. The 1-sec peak photon flux measured\nstarting from T0+57 s in the 10-1000 keV band is 75 +/- 1 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/34831.",
"published": "2023-10-18T17:37:01.665349Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-18T17:37:01.665380Z",
"modified": "2023-10-18T17:37:01.677748Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 3961,
"topic": "gcn.circular",
"uuid": "e9c54eaa-1436-4f6b-976c-23167c925797",
"title": "GRB 231015A: AstroSat CZTI detection",
"submitter": "Hop gcn.circular",
"authors": "Gaurav Waratkar at IIT Bombay <gauravwaratkar@iitb.ac.in>",
"data": {
"date": "23/10/18 17:40:44 GMT",
"from": "Gaurav Waratkar at IIT Bombay <gauravwaratkar@iitb.ac.in>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34832"
},
"title": "GCN CIRCULAR",
"number": "34832",
"subject": "GRB 231015A: AstroSat CZTI detection"
},
"message_text": "P. K. Navaneeth (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 GRB 231015A which was also detected by Konus-Wind (reported in IPN_RAW GCN notices).\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 2023-10-15 23:49:53.50 UTC. The measured peak count rate associated with the burst is 477 (+43, -43) counts/s above the background in the combined data of two quadrants (out of four), with a total of 5641 (+323, -329) counts. The local mean background count rate was 239 (+3, -3) counts/s. Using cumulative rates, we measure a T90 of 24 (+1, -1) 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 2023-10-15 23:49:53.42 UTC. The measured peak count rate associated with the burst is 864 (+76, -87) counts/s above the background in the combined data of all quadrants, with a total of 10039 (+610, -910) counts. The local mean background count rate was 1514 (+7, -6) counts/s. We measure a T90 of 25 (+4, -2) 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\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34832.",
"published": "2023-10-18T17:40:52.330826Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-18T17:40:52.330848Z",
"modified": "2023-10-18T17:40:52.336447Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4204,
"topic": "gcn.circular",
"uuid": "ff496119-470d-4360-95fd-75ad2309e138",
"title": "GRB 231028A: AstroSat CZTI detection",
"submitter": "Hop gcn.circular",
"authors": "Gaurav Waratkar at IIT Bombay <gauravwaratkar@iitb.ac.in>",
"data": {
"date": "23/10/29 03:47:02 GMT",
"from": "Gaurav Waratkar at IIT Bombay <gauravwaratkar@iitb.ac.in>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34901"
},
"title": "GCN CIRCULAR",
"number": "34901",
"subject": "GRB 231028A: AstroSat CZTI detection"
},
"message_text": "P. K. Navaneeth (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 GRB 231028A which was also detected by Fermi-GBM (Fermi GBM Team, GCN Circ. 34893, Veres et al., GCN Circ. 34899), Swift-BAT (Williams et al., GCN Circ. 34894), and Glowbug (Kerr et al., GCN Circ. 34900).\n\nThe source was clearly detected in the CZT detectors in the 20-200 keV energy range. The light curve peaks at 2023-10-28 04:09:14.25 UTC. The measured peak count rate associated with the burst is 66 (+42, -4) counts/s above the background in the combined data of two quadrants (out of four), with a total of 273 (+88, -85) counts. The local mean background count rate was 156 (+1, -4) counts/s. Using cumulative rates, we measure a T90 of 7.8 (+0.9, -3.0) s. We caution that there was a 0.3 s readout dead time in CZTI after the detection of the burst. Hence, the T90 can be as large as 8.7 s for this GRB, with a lower limit of 4.8 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 2023-10-28 04:09:13.77 UTC. The measured peak count rate associated with the burst is 605 (+74, -72) counts/s above the background in the combined data of all quadrants, with a total of 2924 (+529, -560) counts. The local mean background count rate was 1508 (+6, -7) counts/s. We measure a T90 of 6.2 (+2.3, -1.3) 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/34901.",
"published": "2023-10-31T23:26:59.031568Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-31T23:26:59.031586Z",
"modified": "2023-10-31T23:26:59.036385Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 3975,
"topic": "gcn.circular",
"uuid": "622dada4-7638-499d-a4d9-d5f1e75d10fd",
"title": "LIGO/Virgo/KAGRA S231018cb: One counterpart neutrino candidate event from an IceCube neutrino search",
"submitter": "Hop gcn.circular",
"authors": "Erik Blaufuss at University of Maryland, College Park <blaufuss@umd.edu>",
"data": {
"date": "23/10/19 02:06:25 GMT",
"from": "Erik Blaufuss at University of Maryland, College Park <blaufuss@umd.edu>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34838"
},
"title": "GCN CIRCULAR",
"number": "34838",
"subject": "LIGO/Virgo/KAGRA S231018cb: One counterpart neutrino candidate event from an IceCube neutrino search"
},
"message_text": "IceCube Collaboration (http://icecube.wisc.edu/) reports:\n\nWe have performed a search for track-like muon neutrino events detected by IceCube consistent with the sky localization of the low-significance gravitational-wave candidate event S231018cb in a time range of 1000 seconds centered on the alert event time (2023-10-18T23:40:06 UTC to 2023-10-18T23:56:46 UTC) [1,2] .\nDuring this time period IceCube was collecting good quality data. A single hypothesis test\nwas conducted, using a Bayesian approach to quantify the joint GW + neutrino event significance, which assumes a binary merger scenario and accounts for known astrophysical priors, such as GW source distance, in the statistical significance estimation [3].\n\nOne track-like event is found in spatial and temporal coincidence with the gravitational-wave\nCandidate S231018cb calculated from the map circulated in the S231018cb-2-Preliminary notice. This represents an overall p-value of 0.003 for the Bayesian search. The p-value\nmeasures the consistency of the observed track-like events with the known atmospheric backgrounds for this single map (not accounting for statistical trials from multiple GW events).\n\nFurther details are available at https://gcn.nasa.gov/missions/icecube and at https://roc.icecube.wisc.edu/public/LvkNuTrackSearch.\n\nProperties of the coincident events are shown below:\n\n dt(s) RA(deg) Dec(deg) Angular uncertainty(deg) p-value(Bayesian)\n-----------------------------------------------------------------------------------------------------\n-24.13 170.53 +11.11 0.53 0.0031\n\nwhere:\ndt = Time of track event minus time of GW trigger (sec)\nAngular uncertainty = Angular uncertainty of track event: the radius of a circle\n representing 90% CL containment by area.\np-value = the p-value for this specific track event from this search.\n\nThe IceCube Neutrino Observatory is a cubic-kilometer neutrino detector operating at the\ngeographic South Pole, Antarctica. The IceCube realtime alert point of contact can be\nreached at roc@icecube.wisc.edu\n\n[1] M. G. Aartsen et al 2020 ApJL 898 L10\n[2] Abbasi et al. Astrophys.J. 944 (2023) 1, 80\n[3] I. Bartos et al. 2019 Phys. Rev. D 100, 083017\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34838.",
"published": "2023-10-19T02:06:35.015248Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-19T02:06:35.015287Z",
"modified": "2023-10-19T02:06:35.111781Z",
"nonlocalizedevents": [
{
"event_id": "S231018c"
}
],
"targets": []
},
{
"id": 3962,
"topic": "gcn.circular",
"uuid": "083e8569-0a65-4d09-94da-b1f56e38b97c",
"title": "GRB231017A: GROWTH-India upper limits on the optical afterglow",
"submitter": "Hop gcn.circular",
"authors": "Anirudh Salgundi <salgundi.anirudh@gmail.com>",
"data": {
"date": "23/10/18 20:23:19 GMT",
"from": "Anirudh Salgundi <salgundi.anirudh@gmail.com>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34833"
},
"title": "GCN CIRCULAR",
"number": "34833",
"subject": "GRB231017A: GROWTH-India upper limits on the optical afterglow"
},
"message_text": "R. Kumar, A. Salgundi, R. Sharma, Y. Wagh, V. Swain, V. Bhalerao (IIT Bombay), S. Barway, G. C. Anupama (IIA), K. Angail (IAO)\n\nWe observed the field of GRB 231017A detected by Fermi (Fermi GBM team GCN 34822) with 0.7m GROWTH-India Telescope (GIT). GIT was triggered at 2023-10-18 15:49:46.29 UT, i.e., 1.32 days after the Fermi trigger, as a response to the Swift/GUANO trigger (J DeLaunay et al., GCN 34824). We obtained multiple frames in the g' and r' bands, covering the localisation reported by Swift/XRT (P. A. Evans et al., GCN 34825). We searched individual images and the stacked image for an afterglow, but do not detect any. Our upper limits on the magnitude of the afterglow are:\n\nJD (mid) | t_mid-t0 (days)| Filter | Exposure (s) | Limiting Magnitude (5 sigma) |\n\n2460236.187750 | 1.351 | g' | 3 x 300 | 19.27 |\n2460236.171885 | 1.335 | r' | 6 x 300 | 21.08 |\n2460236.250104 | 1.413 | g' | 2 x 400 | 19.98 |\n\nThe magnitudes are calibrated against PanSTARRS DR1 (Chambers et al., 2016) and not corrected for Galactic extinction.\n\nThe GROWTH India Telescope (GIT; Kumar et al. 2022) is a 70-cm telescope with a 0.7-degree field of view, set up by the Indian Institute of Astrophysics (IIA) and the Indian Institute of Technology Bombay (IITB) with funding from DST-SERB and IUSSTF. It is located at the Indian Astronomical Observatory (Hanle), operated by IIA. We acknowledge funding by the IITB alumni batch of 1994, which partially supports the operations of the telescope. Telescope technical details are available at https://sites.google.com/view/growthindia/.\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34833.",
"published": "2023-10-18T20:23:31.358600Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-18T20:23:31.358624Z",
"modified": "2023-10-18T20:23:31.369520Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 3963,
"topic": "gcn.circular",
"uuid": "a5dddb84-996f-4f36-96a9-f72af6078cb0",
"title": "GRB 231017A: LCOGT Optical Upper Limits",
"submitter": "Hop gcn.circular",
"authors": "Robert Strausbaugh at Eastern Illinois University <rstrausbaugh@eiu.edu>",
"data": {
"date": "23/10/18 20:47:26 GMT",
"from": "Robert Strausbaugh at Eastern Illinois University <rstrausbaugh@eiu.edu>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34834"
},
"title": "GCN CIRCULAR",
"number": "34834",
"subject": "GRB 231017A: LCOGT Optical Upper Limits"
},
"message_text": "R. Strausbaugh (Eastern Illinois University), A. Cucchiara (NASA) report on behalf of a larger collaboration:\n\nWe observed the Fermi GRB 231017A field (Fermi GBM team, GCN 34822) with the LCOGT 1-meter Sinistro instrument at the Teide Observatory, Tenerife site, on October 18, from 01:01 to 01:34 UT (corresponding to 15.93 to 16.48 hours from the GRB trigger time) with the SDSS r and i filters.\n\nWe performed a series of 3x300s exposures in each band. We do not detect a source within the Swift-XRT error region around the candidate X-ray source (Dichiara et al., GCN 34829) in either band.\n\nThe following upper limits are calculated using the PanSTARRS catalog as reference:\n\nr > 23.0\ni > 22.6\n\nThese magnitudes are not corrected for galactic extinction.\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34834.",
"published": "2023-10-18T20:47:36.246427Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-18T20:47:36.246461Z",
"modified": "2023-10-18T20:47:36.257853Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 3964,
"topic": "gcn.circular",
"uuid": "c9fcb347-f47f-487c-af4b-4de5876c49bb",
"title": "GRB 231015A: Glowbug gamma-ray detection",
"submitter": "Hop gcn.circular",
"authors": "C.C. Cheung at Naval Research Lab <Teddy.Cheung@nrl.navy.mil>",
"data": {
"date": "23/10/18 22:27:07 GMT",
"from": "C.C. Cheung at Naval Research Lab <Teddy.Cheung@nrl.navy.mil>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34835"
},
"title": "GCN CIRCULAR",
"number": "34835",
"subject": "GRB 231015A: Glowbug gamma-ray detection"
},
"message_text": "M. Kerr, C.C. Cheung, J. E. Grove, R. Woolf (NRL), A. Goldstein (USRA), C.A. Wilson-Hodge (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 231015A, which was also detected by AstroSat and Konus-Wind (GCN 34832). AstroSat CZTI detected multiple peaks of emission with the strongest peak at 2023-10-15 23:49:53.50 UTC.\n\nUsing an adaptive window with a resolution of 32-ms, the onset for the multi-peaked emission reported by AstroSat is determined to be 2023-10-15 23:49:21.128 with a duration of 36.9 s and a total significance of about 95.4 sigma. The light curve comprises two primary peaks separated by about 15 s.\n\nUsing a standard power-law function with an exponential high-energy cutoff [3] to model the emission over this duration results in a photon index dN/dE~E^x of x=0.1 and a cutoff energy (\"Epeak\") of 292 keV. The modeled 10-10000 keV fluence is 3.4e-05 erg/cm^2.\n\nAdditional analysis of Glowbug data revealed an earlier component to the two main emission peaks. Using an adaptive window with a resolution of 32-ms, the burst onset of this earlier emission is determined to be 2023-10-15 23:47:03.912 with a duration of 10.3 s and a total significance of about 13.4 sigma. The light curve comprises a single broad peak.\n\nUsing a standard power-law function with an exponential high-energy cutoff [3] to model the emission in the earlier component over this duration results in a photon index dN/dE~E^x of x=2.0 and a cutoff energy (\"Epeak\") of 193 keV. The modeled 10-10000 keV fluence is 8.9e-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\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34835.",
"published": "2023-10-18T22:27:19.080139Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-18T22:27:19.080171Z",
"modified": "2023-10-18T22:27:19.094392Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4205,
"topic": "gcn.circular",
"uuid": "5db738a4-3622-407c-b254-ff48f17285a7",
"title": "IceCube-231027A: 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": "23/10/30 16:53:28 GMT",
"from": "Jessie Thwaites at IceCube/U Wisc-Madison <thwaites@wisc.edu>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34913"
},
"title": "GCN CIRCULAR",
"number": "34913",
"subject": "IceCube-231027A: 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-231027A (https://gcn.nasa.gov/circulars/34891) in a time range of 1000 seconds centered on the alert event time (2023-10-27 04:07:50.440 UTC to 2023-10-27 04:24:30.440 UTC) during which IceCube was collecting good quality data. Excluding the event that prompted the alert, zero track-like events are found within the 90% containment region of IceCube-231027A. 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-231027A is 1.5e-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 5e+04 GeV.\n\nA subsequent search was performed including 2 days of data centered on the alert event time (2023-10-26 04:16:10.440 UTC to 2023-10-28 04:16:10.440 UTC). In this case, we report a p-value of 1.00, 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-231027A is 1.8e-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\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34913.",
"published": "2023-10-31T23:26:59.042517Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-31T23:26:59.042535Z",
"modified": "2023-10-31T23:26:59.047298Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6319,
"topic": "gcn.circular",
"uuid": "7618181c-fc4c-4aec-b971-890fa84c9301",
"title": "Fermi GRB 240402A: 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": "24/04/03 00:31:29 GMT",
"from": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/36013"
},
"title": "GCN CIRCULAR",
"number": "36013",
"subject": "Fermi GRB 240402A: 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) started inspect of the Fermi GRB 240402A ( Fermi GBM team, GCN 36012) errorbox 56 sec after notice time and 92 sec after trigger time at 2024-04-02 23:45:36 UT, with upper limit up to 19.8 mag. The observations began at zenith distance = 17 deg. The sun altitude is -30.8 deg.\n\nMASTER-SAAO robotic telescope located in South Africa (South African Astronomical Observatory) started inspect of the Fermi GRB 240402A errorbox 283 sec after notice time and 318 sec after trigger time at 2024-04-02 23:49:23 UT, with upper limit up to 18.5 mag. The observations began at zenith distance = 78 deg. The sun altitude is -59.0 deg.\n\nThe galactic latitude b = 65 deg., longitude l = 44 deg.\n\n\nReal time updated cover map and OT discovered available here:\nhttps://master.sai.msu.ru/site/master2/observ.php?id$13376\n\nWe obtain a following upper limits.\n\nTmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment\n_________|_____________________|_____________________|____________________________________|_____|_______|_______|________\n\n 182 | 2024-04-02 23:45:36 | MASTER-Kislovodsk | (15h 12m 58.69s , +25d 58m 16.1s) | C | 180 | 19.2 |\n 182 | 2024-04-02 23:45:36 | MASTER-Kislovodsk | (15h 08m 03.72s , +26d 20m 19.6s) | C | 180 | 19.8 |\n 330 | 2024-04-02 23:49:03 | MASTER-Kislovodsk | (16h 13m 25.97s , +37d 31m 16.3s) | C | 60 | 18.3 |\n 330 | 2024-04-02 23:49:03 | MASTER-Kislovodsk | (16h 19m 02.25s , +37d 08m 45.3s) | C | 60 | 19.1 |\n 349 | 2024-04-02 23:49:23 | MASTER-SAAO | (16h 19m 55.22s , +38d 58m 47.5s) | C | 60 | 16.1 |\n 421 | 2024-04-02 23:50:35 | MASTER-Kislovodsk | (16h 14m 08.44s , +35d 13m 37.9s) | C | 60 | 19.0 |\n 425 | 2024-04-02 23:50:39 | MASTER-Kislovodsk | (16h 08m 40.42s , +35d 36m 13.1s) | C | 60 | 18.1 |\n 443 | 2024-04-02 23:50:57 | MASTER-SAAO | (16h 00m 22.97s , +39d 01m 30.8s) | C | 60 | 17.7 |\n 505 | 2024-04-02 23:51:59 | MASTER-Kislovodsk | (16h 27m 17.68s , +41d 17m 25.8s) | C | 60 | 18.2 |\n 505 | 2024-04-02 23:51:59 | MASTER-Kislovodsk | (16h 33m 11.34s , +40d 54m 41.2s) | C | 60 | 19.1 |\n 535 | 2024-04-02 23:52:29 | MASTER-SAAO | (15h 54m 33.78s , +37d 07m 14.2s) | C | 60 | 17.8 |\n 585 | 2024-04-02 23:53:19 | MASTER-Kislovodsk | (16h 27m 18.43s , +35d 35m 04.3s) | C | 60 | 18.1 |\n 586 | 2024-04-02 23:53:19 | MASTER-Kislovodsk | (16h 32m 45.73s , +35d 12m 25.9s) | C | 60 | 18.9 |\n 628 | 2024-04-02 23:54:02 | MASTER-SAAO | (16h 05m 06.50s , +33d 19m 48.0s) | C | 60 | 17.9 |\n 666 | 2024-04-02 23:54:39 | MASTER-Kislovodsk | (16h 15m 46.11s , +43d 13m 38.4s) | C | 60 | 18.2 |\n 666 | 2024-04-02 23:54:39 | MASTER-Kislovodsk | (16h 21m 50.67s , +42d 50m 47.1s) | C | 60 | 19.0 |\n 720 | 2024-04-02 23:55:34 | MASTER-SAAO | (15h 50m 12.26s , +35d 13m 34.4s) | C | 60 | 17.9 |\n 746 | 2024-04-02 23:56:00 | MASTER-Kislovodsk | (16h 23m 15.40s , +33d 41m 08.3s) | C | 60 | 18.0 |\n 746 | 2024-04-02 23:56:00 | MASTER-Kislovodsk | (16h 28m 35.35s , +33d 18m 27.6s) | C | 60 | 19.0 |\n 815 | 2024-04-02 23:57:09 | MASTER-SAAO | (15h 55m 25.17s , +42d 48m 09.2s) | C | 60 | 15.9 |\n 826 | 2024-04-02 23:57:20 | MASTER-Kislovodsk | (16h 36m 37.66s , +43d 13m 21.7s) | C | 60 | 17.9 |\n 907 | 2024-04-02 23:58:40 | MASTER-Kislovodsk | (15h 40m 20.30s , +39d 24m 34.9s) | C | 60 | 18.3 |\n 907 | 2024-04-02 23:58:40 | MASTER-Kislovodsk | (15h 46m 05.32s , +39d 01m 06.7s) | C | 60 | 19.1 |\n 909 | 2024-04-02 23:58:43 | MASTER-SAAO | (16h 02m 45.99s , +31d 24m 25.4s) | C | 60 | 18.1 |\n 988 | 2024-04-03 00:00:02 | MASTER-Kislovodsk | (16h 20m 24.70s , +31d 48m 55.2s) | C | 60 | 18.1 |\n 988 | 2024-04-03 00:00:02 | MASTER-Kislovodsk | (16h 25m 37.89s , +31d 25m 23.4s) | C | 60 | 19.1 |\n 1001 | 2024-04-03 00:00:15 | MASTER-SAAO | (15h 46m 56.79s , +33d 20m 42.9s) | C | 60 | 18.1 |\n 1068 | 2024-04-03 00:01:22 | MASTER-Kislovodsk | (16h 04m 35.13s , +45d 07m 13.7s) | C | 60 | 18.0 |\n 1068 | 2024-04-03 00:01:22 | MASTER-Kislovodsk | (16h 10m 52.08s , +44d 43m 13.8s) | C | 60 | 19.0 |\n 1105 | 2024-04-03 00:01:59 | MASTER-SAAO | (16h 46m 04.76s , +35d 10m 14.6s) | C | 60 | 16.8 |\n 1149 | 2024-04-03 00:02:42 | MASTER-Kislovodsk | (16h 41m 26.99s , +33d 40m 45.2s) | C | 60 | 18.1 |\n 1149 | 2024-04-03 00:02:42 | MASTER-Kislovodsk | (16h 46m 46.14s , +33d 17m 15.8s) | C | 60 | 19.0 |\n 1201 | 2024-04-03 00:03:35 | MASTER-SAAO | (15h 35m 39.18s , +37d 09m 08.1s) | C | 60 | 17.9 |\n 1391 | 2024-04-03 00:06:45 | MASTER-SAAO | (14h 53m 45.28s , +14d 23m 05.9s) | C | 60 | 18.5 |\n 1493 | 2024-04-03 00:07:27 | MASTER-Kislovodsk | (14h 58m 58.63s , +24d 04m 51.1s) | C | 180 | 18.9 |\n 1493 | 2024-04-03 00:07:27 | MASTER-Kislovodsk | (14h 54m 12.44s , +24d 27m 07.2s) | C | 180 | 19.5 |\n 1488 | 2024-04-03 00:08:22 | MASTER-SAAO | (16h 20m 04.04s , +39d 00m 18.3s) | C | 60 | 16.8 |\n 1581 | 2024-04-03 00:09:55 | MASTER-SAAO | (16h 00m 22.64s , +39d 00m 24.8s) | C | 60 | 17.7 |\n 1640 | 2024-04-03 00:10:54 | MASTER-Kislovodsk | (16h 13m 26.45s , +37d 29m 49.3s) | C | 60 | 18.4 |\n 1640 | 2024-04-03 00:10:54 | MASTER-Kislovodsk | (16h 19m 02.71s , +37d 07m 14.4s) | C | 60 | 19.1 |\n 1673 | 2024-04-03 00:11:27 | MASTER-SAAO | (15h 54m 43.06s , +37d 07m 09.0s) | C | 60 | 18.0 |\n 1721 | 2024-04-03 00:12:14 | MASTER-Kislovodsk | (16h 08m 38.80s , +35d 37m 20.6s) | C | 60 | 18.1 |\n 1721 | 2024-04-03 00:12:14 | MASTER-Kislovodsk | (16h 14m 06.47s , +35d 13m 52.5s) | C | 60 | 19.0 |\n 1765 | 2024-04-03 00:12:59 | MASTER-SAAO | (16h 05m 12.80s , +33d 20m 02.1s) | C | 60 | 17.7 |\n 1801 | 2024-04-03 00:13:35 | MASTER-Kislovodsk | (16h 27m 14.87s , +41d 18m 41.7s) | C | 60 | 17.9 |\n 1801 | 2024-04-03 00:13:35 | MASTER-Kislovodsk | (16h 33m 08.42s , +40d 54m 57.1s) | C | 60 | 18.8 |\n 1857 | 2024-04-03 00:14:31 | MASTER-SAAO | (15h 50m 14.26s , +35d 13m 11.9s) | C | 60 | 17.7 |\n 1857 | 2024-04-03 00:14:31 | MASTER-SAAO | (15h 48m 06.98s , +35d 26m 14.8s) | C | 60 | 17.2 |\n 1881 | 2024-04-03 00:14:55 | MASTER-Kislovodsk | (16h 27m 12.81s , +35d 37m 13.4s) | C | 60 | 18.1 |\n 1881 | 2024-04-03 00:14:55 | MASTER-Kislovodsk | (16h 32m 40.09s , +35d 13m 39.0s) | C | 60 | 19.0 |\n 1937 | 2024-04-03 00:15:51 | MASTER-SAAO | (15h 53m 16.83s , +43d 03m 43.3s) | C | 60 | 16.0 |\n 1937 | 2024-04-03 00:15:51 | MASTER-SAAO | (15h 55m 37.69s , +42d 50m 39.4s) | C | 60 | 16.4 |\n 1968 | 2024-04-03 00:16:22 | MASTER-Kislovodsk | (16h 15m 48.39s , +43d 12m 59.3s) | C | 60 | 18.2 |\n 1968 | 2024-04-03 00:16:22 | MASTER-Kislovodsk | (16h 21m 53.26s , +42d 49m 15.1s) | C | 60 | 19.0 |\n 2016 | 2024-04-03 00:17:10 | MASTER-SAAO | (16h 00m 41.87s , +31d 38m 28.9s) | C | 60 | 17.4 |\n 2016 | 2024-04-03 00:17:10 | MASTER-SAAO | (16h 02m 43.92s , +31d 25m 26.0s) | C | 60 | 17.8 |\n 2048 | 2024-04-03 00:17:42 | MASTER-Kislovodsk | (16h 23m 10.32s , +33d 41m 12.0s) | C | 60 | 18.0 |\n 2048 | 2024-04-03 00:17:42 | MASTER-Kislovodsk | (16h 28m 30.12s , +33d 17m 37.9s) | C | 60 | 19.0 |\n 2096 | 2024-04-03 00:18:30 | MASTER-SAAO | (15h 44m 53.33s , +33d 34m 17.4s) | C | 60 | 17.4 |\n 2096 | 2024-04-03 00:18:30 | MASTER-SAAO | (15h 46m 57.91s , +33d 21m 14.9s) | C | 60 | 17.6 |\n 2128 | 2024-04-03 00:19:02 | MASTER-Kislovodsk | (16h 36m 35.85s , +43d 12m 09.6s) | C | 60 | 18.0 |\n 2176 | 2024-04-03 00:19:49 | MASTER-SAAO | (16h 44m 02.30s , +35d 24m 23.6s) | C | 60 | 16.1 |\n 2176 | 2024-04-03 00:19:49 | MASTER-SAAO | (16h 46m 09.16s , +35d 11m 18.5s) | C | 60 | 16.4 |\n 2212 | 2024-04-03 00:20:26 | MASTER-Kislovodsk | (15h 42m 05.91s , +39d 17m 26.2s) | C | 60 | 18.3 |\n 2212 | 2024-04-03 00:20:26 | MASTER-Kislovodsk | (15h 36m 18.02s , +39d 39m 32.1s) | C | 60 | 19.1 |\n 2255 | 2024-04-03 00:21:09 | MASTER-SAAO | (15h 33m 24.47s , +37d 20m 59.2s) | C | 60 | 17.2 |\n 2255 | 2024-04-03 00:21:09 | MASTER-SAAO | (15h 35m 34.79s , +37d 07m 56.8s) | C | 60 | 17.3 |\n 2298 | 2024-04-03 00:21:51 | MASTER-Kislovodsk | (16h 25m 40.93s , +31d 23m 52.6s) | C | 60 | 19.1 |\n 2298 | 2024-04-03 00:21:51 | MASTER-Kislovodsk | (16h 20m 27.98s , +31d 47m 16.2s) | C | 60 | 18.1 |\n 2335 | 2024-04-03 00:22:29 | MASTER-SAAO | (16h 16m 59.52s , +29d 43m 12.7s) | C | 60 | 17.4 |\n 2378 | 2024-04-03 00:23:12 | MASTER-Kislovodsk | (16h 04m 34.59s , +45d 07m 57.2s) | C | 60 | 18.1 |\n 2378 | 2024-04-03 00:23:12 | MASTER-Kislovodsk | (16h 10m 51.11s , +44d 44m 45.0s) | C | 60 | 18.9 |\n 2458 | 2024-04-03 00:24:32 | MASTER-Kislovodsk | (16h 41m 25.01s , +33d 41m 59.4s) | C | 60 | 18.1 |\n 2458 | 2024-04-03 00:24:32 | MASTER-Kislovodsk | (16h 46m 44.92s , +33d 19m 30.3s) | C | 60 | 19.0 |\n 2538 | 2024-04-03 00:25:52 | MASTER-Kislovodsk | (16h 13m 23.00s , +37d 31m 10.7s) | C | 60 | 18.3 |\n 2538 | 2024-04-03 00:25:52 | MASTER-Kislovodsk | (16h 18m 58.79s , +37d 07m 57.4s) | C | 60 | 19.1 |\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/36013.",
"published": "2024-04-03T00:31:45.562432Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-04-03T00:31:45.562444Z",
"modified": "2024-04-03T00:31:45.571075Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6320,
"topic": "gcn.circular",
"uuid": "20a39136-00ea-4ca0-8bcc-ef30f2356723",
"title": "Fermi trigger No 733808041: 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": "24/04/03 05:46:31 GMT",
"from": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/36014"
},
"title": "GCN CIRCULAR",
"number": "36014",
"subject": "Fermi trigger No 733808041: 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 GRB240403.15 (trigger No 733808041,15h 03m 19.20s , +39d 09m 36.0s, R=5.79) errorbox 5 sec after trigger time at 2024-04-03 03:34:02 UT, with upper limit up to 17.8 mag. The observations began at zenith distance = 79 deg. The sun altitude is -17.2 deg.\n\nThe galactic latitude b = 60 deg., longitude l = 65 deg.\n\n\nReal time updated cover map and OT discovered available here:\nhttps://master.sai.msu.ru/site/master2/observ.php?id$13499\n\nWe obtain a following upper limits.\n\nTmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment\n_________|_____________________|_____________________|____________________________________|_____|_______|_______|________\n\n 36 | 2024-04-03 03:34:02 | MASTER-SAAO | (15h 20m 07.21s , +39d 22m 12.9s) | C | 60 | 17.4 |\n 36 | 2024-04-03 03:34:02 | MASTER-SAAO | (15h 22m 18.15s , +39d 09m 00.4s) | C | 60 | 17.8 |\n 674 | 2024-04-03 03:44:39 | MASTER-SAAO | (15h 17m 31.00s , +37d 15m 40.2s) | C | 60 | 17.6 |\n 674 | 2024-04-03 03:44:39 | MASTER-SAAO | (15h 15m 23.12s , +37d 28m 50.8s) | C | 60 | 17.1 |\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/36014.",
"published": "2024-04-03T05:46:47.481210Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-04-03T05:46:47.481223Z",
"modified": "2024-04-03T05:46:47.487845Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 3965,
"topic": "gcn.circular",
"uuid": "a4cb5311-582f-4c49-bf7e-b7983a5d91a2",
"title": "GRB 231017A: Las Cumbres optical upper limit",
"submitter": "Hop gcn.circular",
"authors": "Manisha Shrestha at University of Arizona <mshrestha1@arizona.edu>",
"data": {
"date": "23/10/18 23:23:48 GMT",
"from": "Manisha Shrestha at University of Arizona <mshrestha1@arizona.edu>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34836"
},
"title": "GCN CIRCULAR",
"number": "34836",
"subject": "GRB 231017A: Las Cumbres optical upper limit"
},
"message_text": "M. Shrestha (Univ. of Arizona), D. Sand (Univ. of Arizona), K. D. Alexander (Univ. of Arizona), J. Andrews (Gemini), J. Pearson (Univ. of Arizona), N. Smith (Univ. of Arizona), K. Bostroem (Univ. of Arizona) D. A. Howell (LCO/UCSB), C. McCully (LCO/UCSB), M. Newsome (LCO/UCSB), E Padilla Gonzalez (LCO/UCSB), C. Pellegrino (LCO/UCSB), G. Terreran (LCO/UCSB), J. Farah (LCO/UCSB) report on behalf of a wider Global Supernova Project collaboration:\n\nWe observed the field of GRB 231017A (Fermi GBM team GCN 34822, Trigger 719222708) localized by Swift/BAT-GUANO (DeLaunay et al. GCN 34824) with the 1-m telescope, on 2023-10-18T02:56:38.021 UT (60235.12 MJD, ~0.8 days after the trigger) using the Sinistro instrument in V, g, r, i bands. We do not detect any new optical counterpart within the error region of BAT-GUANO with upper limit of:\n\ng> 22.5\nr> 21.2\ni> 20.9\n\nThese values were calculated with respect to ATLAS-REFCAT2 (Tonry et al. 2018, ApJ 867 105) catalog are not corrected for galactic extinction. This non-detection is in agreement with Strausbaugh et al., GCN 34834 and Kumar et al., GCN 34833.\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34836.",
"published": "2023-10-18T23:23:58.962475Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-18T23:23:58.962506Z",
"modified": "2023-10-18T23:23:58.971093Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 3971,
"topic": "gcn.circular",
"uuid": "990ffb89-dbe2-45d7-ad63-d0326ae00490",
"title": "IC231004A: Classification of AT2023uqf/ZTF23abidzvf as a rapidly-evolving supernova with CSM interaction",
"submitter": "Hop gcn.circular",
"authors": "Robert Stein at Caltech <rdstein@astro.caltech.edu>",
"data": {
"date": "23/10/18 23:57:27 GMT",
"from": "Robert Stein at Caltech <rdstein@astro.caltech.edu>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34837"
},
"title": "GCN CIRCULAR",
"number": "34837",
"subject": "IC231004A: Classification of AT2023uqf/ZTF23abidzvf as a rapidly-evolving supernova with CSM interaction"
},
"message_text": "Robert Stein (Caltech), Jannis Necker (DESY), Simeon Reusch (DESY), Anna Franckowiak (RUB), Vikram Ravi (Caltech), Anna Y. Q. Ho (Cornell), Daniel Perley (LJMU), Mansi Kasliwal (Caltech), Jesper Sollerman (OKC), Kaustav Das (Caltech) and Jean Somalwar (Caltech) report:\n\nAT2023uqf/ZTF23abidzvf was first reported by ZTF (Reusch et al., GCN 34810) as a possible optical counterpart to neutrino IC231004A (Lincetto et al., GCN 34797), as part of the broader ZTF neutrino follow-up program (Stein et al. 2023). After the initial report, our ZTF observations showed that AT2023uqf rapidly brightened, rising by ~1 mag in the first 2 days. There was a 5-day gap in ZTF observations, and the source has since been fading at a rate of > 0.1 mag per day.\n\nWe obtained spectroscopic observations of this source at the Nordic Optical Telescope with ALFOSC (PI: Franckowiak), and the Low Resolution Imaging Spectrometer at the Keck observatory (LRIS; Oke et al 1995, PI: Ravi). Observations were conducted on 2013-10-14, 12 days after the transient was first detected.\n\nThe spectra show a hot and mostly featureless blue continuum with numerous narrow host-galaxy emission features (H-alpha, H-beta, [OIII], [OII]) at a consistent redshift of z=0.1503) , At this redshift, the implied absolute g-band magnitude is at least M =-19.7. There are intermediate-width emission features at rest-frame wavelengths of ~4470 and ~5880 Angstroms consistent with redshifted He-I also visible, but no other individually-identifiable features from the transient. We highlight in particular the lack of any H lines in the spectrum (except those associated with the host galaxy). Based on these observations, and the general similarity of the spectra to Type Ibn events from the literature such as iPTF14aki (Hosseinzadeh et al. 2017) at a similar rest-frame epoch, we classify AT2023uqf as a Type Ibn supernova. The rapidly evolving light curve, blue colour and high peak luminosity of AT2023uqf is similar to that of other Type Ibn supernovae in the literature (e.g., Ho et al. 2023) as well as to luminous fast blue optical transients (LFBOTs) such as AT2020mrf (Yao et al. 2022). \n\nIn any case, the narrow He lines present in the spectra of AT2023uqf confirm the presence of CSM interaction in this source. AT2023uqf thus unambiguously exhibits all the expected spectroscopic and temporal behaviour expected for the popular CSM neutrino production models (see e.g Murase et al. 2011, Zirakashvili & Ptuskin 2016, Petropoulou et al. 2017, Sarmah et al. 2022, Pitik et al. 2023). However, somewhat surprisingly, AT2023uqf does not belong to the canonical Type IIn class of CSM-interacting supernovae. Our spectra show that AT2023uqf experienced substantial mass loss prior to explosion, with the hydrogen shell being entirely stripped. The AT2023uqf supernova shock collided with a dense He-rich/H-poor CSM, rather than the H-rich CSM seen in Type IIn sources.\n\nWe are planning multi-wavelength observations to better characterise AT2023uqf, and additional community follow-up is encouraged.\n\n\nZTF and GROWTH are worldwide collaborations comprising Caltech, USA; IPAC, USA; WIS, Israel; OKC, Sweden; JSI/UMd, USA; DESY, Germany; TANGO, Taiwan; UW Milwaukee, USA; LANL, USA; TCD, Ireland; IN2P3, France.\n\nSome of the data presented herein were obtained at Keck Observatory, which is a private 501(c)3 non-profit organization operated as a scientific partnership among the California Institute of Technology, the University of California, and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. \n\nThe authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the Native Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.\n\nBased on observations made with the Nordic Optical Telescope, owned in collaboration by the University of Turku and Aarhus University, and operated jointly by Aarhus University, the University of Turku and the University of Oslo, representing Denmark, Finland and Norway, the University of Iceland and Stockholm University at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias.\n\nThe data presented here were obtained in part with ALFOSC, which is provided by the Instituto de Astrofisica de Andalucia (IAA) under a joint agreement with the University of Copenhagen and NOT.\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34837.",
"published": "2023-10-18T23:57:38.168038Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-18T23:57:38.168068Z",
"modified": "2023-10-18T23:57:38.175098Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 3980,
"topic": "gcn.circular",
"uuid": "e6dd3316-335e-4aaa-9486-39a08b306be2",
"title": "GRB 231018A: GROWTH-India Follow-Up of a Fermi Long GRB",
"submitter": "Hop gcn.circular",
"authors": "Varun Bhalerao at IIT Bombay <varunb@iitb.ac.in>",
"data": {
"date": "23/10/19 07:33:47 GMT",
"from": "Varun Bhalerao at IIT Bombay <varunb@iitb.ac.in>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34839"
},
"title": "GCN CIRCULAR",
"number": "34839",
"subject": "GRB 231018A: GROWTH-India Follow-Up of a Fermi Long GRB"
},
"message_text": "R. Kumar, Y. Wagh, R. Sharma, A. Salgundi, V. Swain, D. Raman, T. Roychowdhury, V. Bhalerao (IIT Bombay), S. Barway, G. C. Anupama (IIA), K. Angail (IAO)\n\nWe observed the field of GRB 231018A detected by Fermi (Fermi GBM Team, GCN Circ. 34826; GCN Circ. 34831) with 0.7m GROWTH-India Telescope (GIT). GIT started observing the field at 2023-10-18 17:28:08.912 UT, i.e., 4.96 hours after the Fermi trigger. We obtained a series of 25 r' band images each of 300s exposure, covering 9.44 square degrees. This corresponds to 21.7% of the probability enclosed in the Fermi GBM Final Real-time Localisation (Fermi GBM Team, GCN Circ. 34826) and 20.17% of the probability enclosed in the BALROG localization (Preis et al., GCN Circ. 34827). Where available, PanSTARRS images (Chambers et al., 2016) were used as references for image subtraction. In other fields, we looked for new point sources absent in the GSC2.3 catalog. We did not find any suitable afterglow candidate, reaching a median limiting magnitude of 18.95 in the r' band. The detailed observing log is:\n\n| Tile ID | RA (deg) | Dec (deg) | Lim Mag (AB) | Method |\n\n| 54910 | 0.12 | 50.1 | 18.54 | Catalog |\n| 55565 | 1.25 | 51.5 | 18.93 | Subtraction |\n| 55567 | 3.51 | 51.5 | 18.96 | Subtraction |\n| 55883 | 0.13 | 51.5 | 18.82 | Catalog |\n| 54579 | 3.36 | 49.4 | 18.66 | Subtraction |\n| 55238 | 0.12 | 50.1 | 18.25 | Catalog |\n| 54912 | 2.32 | 50.1 | 19.02 | Subtraction |\n| 55241 | 2.35 | 50.8 | 19.01 | Subtraction |\n| 55564 | 0.13 | 51.5 | 18.74 | Catalog |\n| 55242 | 3.46 | 50.8 | 18.96 | Subtraction |\n| 55240 | 1.24 | 50.8 | 19.02 | Subtraction |\n| 55243 | 4.57 | 50.8 | 18.98 | Subtraction |\n| 54577 | 1.20 | 49.4 | 18.22 | Subtraction |\n| 54914 | 4.51 | 50.1 | 17.48 | Subtraction |\n| 54578 | 2.28 | 49.4 | 18.76 | Subtraction |\n| 56201 | 2.45 | 52.9 | 15.70 | Subtraction |\n| 55885 | 1.27 | 52.2 | 18.97 | Subtraction |\n| 55887 | 3.56 | 52.2 | 19.03 | Subtraction |\n| 55568 | 4.64 | 51.5 | 18.85 | Subtraction |\n| 55886 | 2.42 | 52.2 | 18.97 | Subtraction |\n| 54913 | 3.42 | 50.1 | 19.05 | Subtraction |\n| 55563 | 0.13 | 50.8 | 18.64 | Catalog |\n| 54911 | 1.22 | 50.1 | 19.12 | Subtraction |\n\nThe magnitudes are calibrated against PanSTARRS DR1 (Chambers et al., 2016) and not corrected for Galactic extinction.\n\nThe GROWTH India Telescope (GIT; Kumar et al. 2022) is a 70-cm telescope with a 0.7-degree field of view, set up by the Indian Institute of Astrophysics (IIA) and the Indian Institute of Technology Bombay (IITB) with funding from DST-SERB and IUSSTF. It is located at the Indian Astronomical Observatory (Hanle), operated by IIA. We acknowledge funding by the IITB alumni batch of 1994, which partially supports the operations of the telescope. Telescope technical details are available at https://sites.google.com/view/growthindia/.\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34839.",
"published": "2023-10-19T07:33:58.577260Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-19T07:33:58.577281Z",
"modified": "2023-10-19T07:33:58.586595Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6321,
"topic": "gcn.circular",
"uuid": "b175563e-b900-4fb3-add3-94468c1bfe4f",
"title": "GRB 240403A: BALROG localization (Fermi Trigger 733838255 / GRB 240403498)",
"submitter": "Hop gcn.circular",
"authors": "Jochen Greiner at MPE <jcgrog@mpe.mpg.de>",
"data": {
"date": "24/04/03 15:15:04 GMT",
"from": "Jochen Greiner at MPE <jcgrog@mpe.mpg.de>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/36015"
},
"title": "GCN CIRCULAR",
"number": "36015",
"subject": "GRB 240403A: BALROG localization (Fermi Trigger 733838255 / GRB 240403498)"
},
"message_text": "T. Preis, B. Biltzinger, J. Burgess & J. Greiner (all MPE Garching) report:\n\nThe public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger\n733838255 at 11:57:30 on 03 April 2024 were automatically fitted for spectrum\nand sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427;\nBerlato et al. 2019, ApJ 873, 60).\n\nThe best-fit position is:\nRA(2000.0) = 9.0 deg\nDecl.(2000.0) = -17.6 deg\nThe 1 sigma statistical error radius is 0.8 deg.\nWe estimate an additional systematic error of 1 deg.\n\nFurther details are available at:\nhttps://grb.mpe.mpg.de/grb/GRB240403498/\n\nThe Healpix map can be downloaded from:\nhttps://grb.mpe.mpg.de/grb/GRB240403498/healpix\n\nThe location parameters are available as JSON at:\nhttps://grb.mpe.mpg.de/grb/GRB240403498/json\n\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/36015.",
"published": "2024-04-03T15:15:22.879131Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-04-03T15:15:22.879146Z",
"modified": "2024-04-03T15:15:22.885913Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 3987,
"topic": "gcn.circular",
"uuid": "ae78bfef-b807-4e3d-8a2e-1db6636969cd",
"title": "GRB 231017A: JinShan optical upper limit",
"submitter": "Hop gcn.circular",
"authors": "Dong Xu at NAOC/CAS <dxu@nao.cas.cn>",
"data": {
"date": "23/10/19 13:18:13 GMT",
"from": "Dong Xu at NAOC/CAS <dxu@nao.cas.cn>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34840"
},
"title": "GCN CIRCULAR",
"number": "34840",
"subject": "GRB 231017A: JinShan optical upper limit"
},
"message_text": "D. Xu, X. Liu, S.Q. Jiang, Z.P. Zhu, S.Y. Fu, J. An, T.H. Lu (NAOC), J.Z. Liu (XAO) report on behalf of a large collaboration:\n\nWe observed the field of GRB 231017A detected by Fermi/GBM (Fermi GBM team, GCN 34822) and Swift/BAT-GUANO (DeLaunay et al. GCN 34824) using the No.2 50cm telescope (50B) located at Altay, Xinjiang, China. We obtained 20x180 s frames in the Sloan r-band, starting at 15:41:21 UT on 2023-10-17, i.e. 7.6 hr after the trigger.\n\nNo optical transient is detected in our stacked image within the error region of the Swift/BAT-GUANO, with the Swift-XRT Source 2 candidate inside the error region (Dichiara et al. GCN 34829), down to a limiting magnitude of r>20.5, calibrated with the nearby PanSTARRS field.\n\nAltay Astronomical Time-Domain Project (JinShan Project for short) is located on the southern side of the Altay mountains in Xinjiang, China. It has geographical Longitude 88 43 35 E, Latitude +47 35 24 N, and Altitude 1025 meters. Altay and JinShan have the same meaning of Gold Mountain. The project consists of four 50cm telescopes with FOV of 1.7x1.7 deg^2 for each (50A, 50B, 50C, and 50D), two 100cm telescopes with FOV of 1.4x1.4 deg^2 for each (100A and 100B), and one 100cm telescope with FOV of 14x14 arcmin^2 (100C). Each telescope has different filters. JinShan is now at its early commissioning stage.\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34840.",
"published": "2023-10-19T13:18:25.045110Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-19T13:18:25.045142Z",
"modified": "2023-10-19T13:18:25.053294Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 3990,
"topic": "gcn.circular",
"uuid": "3a77c65f-9be2-4381-950f-53d3e9d5cc93",
"title": "GRB 231017A: GOTO optical upper limits",
"submitter": "Hop gcn.circular",
"authors": "Ben Gompertz at U of Birmingham <b.gompertz@bham.ac.uk>",
"data": {
"date": "23/10/19 16:24:59 GMT",
"from": "Ben Gompertz at U of Birmingham <b.gompertz@bham.ac.uk>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34841"
},
"title": "GCN CIRCULAR",
"number": "34841",
"subject": "GRB 231017A: GOTO optical upper limits"
},
"message_text": "S. Belkin; K. Ackley; A. Kumar; B. P. Gompertz; B. Godson; R. Starling; M. J. Dyer; J. Lyman; K. Ulaczyk; F. Jimenez-Ibarra; D. O'Neill; D. Steeghs; 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 231017A (Fermi GBM team, GCN 34822). Targeted observations were performed between 00:20:50 UT on 2023-10-18 and 02:37:04 UT on 2023-10-18 (starting ~16.25 hours after trigger). Each observation consisted of 4x90s exposures in the GOTO L-band (400-700 nm).\n\nWe identify no candidate optical counterparts within the Swift/BAT-GUANO localisation region (DeLaunay et al., GCN 34824) or at the positions of the 9 sources identified in XRT pointed observations (Evans et al., GCN 34825; Dichiara et al., GCN 34829). The mean 5-sigma limiting magnitude was L > 20.2 mag. This result is consistent with other observations (ââKumar et al., GCN 34833; Strausbaugh et al., GCN 34834; Shrestha et al., GCN 34836; Xu et al., GCN 34840).\n\nMagnitudes were calibrated using ATLAS-REFCAT2 (Tonry et al. 2018) and are not corrected for Galactic extinction.\nGOTO (https://goto-observatory.org<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\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34841.",
"published": "2023-10-19T16:25:16.158280Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-19T16:25:16.158313Z",
"modified": "2023-10-19T16:25:16.168749Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 3991,
"topic": "gcn.circular",
"uuid": "fb94f92d-968d-4fce-94e6-3aa09e55b2ae",
"title": "GRB 231019A: 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": "23/10/19 17:20:27 GMT",
"from": "Fermi GBM Team at MSFC/Fermi-GBM <do_not_reply@GIOC.nsstc.nasa.gov>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34842"
},
"title": "GCN CIRCULAR",
"number": "34842",
"subject": "GRB 231019A: Fermi GBM Final Real-time Localization"
},
"message_text": "The Fermi GBM team reports the detection of a likely LONG GRB\n\nAt 17:09:58 UT on 19 Oct 2023, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 231019A (trigger 719428203.333452 / 231019715).\n\nThe on-ground calculated location, using the Fermi GBM trigger data, is RA = 343.1, Dec = 45.7 (J2000 degrees, equivalent to J2000 22h 52m, 45d 42'), with a statistical uncertainty of 7.2 degrees.\n\nThe angle from the Fermi LAT boresight is 92.0 degrees.\n\nThe skymap can be found here:\nhttps://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn231019715/quicklook/glg_skymap_all_bn231019715.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/2023/bn231019715/quicklook/glg_healpix_all_bn231019715.fit\n\nThe GBM light curve can be found here:\nhttps://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn231019715/quicklook/glg_lc_medres34_bn231019715.gif\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34842.",
"published": "2023-10-19T17:20:37.981620Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-19T17:20:37.981642Z",
"modified": "2023-10-19T17:20:37.992094Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6322,
"topic": "gcn.circular",
"uuid": "c0a04f4f-a0b8-4931-b372-e5d3ac2c0742",
"title": "X-ray transient LXT 240402A: LEIA detection",
"submitter": "Hop gcn.circular",
"authors": "EP Team at NAOC/CAS <ep_ta@bao.ac.cn>",
"data": {
"date": "24/04/03 16:20:48 GMT",
"from": "EP Team at NAOC/CAS <ep_ta@bao.ac.cn>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/36016"
},
"title": "GCN CIRCULAR",
"number": "36016",
"subject": "X-ray transient LXT 240402A: LEIA detection"
},
"message_text": "X. P. Xu , Z. X. Ling , Y. Liu , C. Zhang , W. Chen , H. Q. Cheng , C. Z. Cui , D. W. Fan , H. B. Hu , J. W. Hu , M. H. Huang , C. C. Jin , 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 , Y. F. Xu , H. N. Yang , M. Zhang , W. D. Zhang , W. J. Zhang , , D. H. Zhao (NAOC, CAS), D. M. Li, Q. X. Li (BNU)ï¼C. Y. Wang, Y. J. Zhang (THU), and W. Yuan (NAOC, CAS) on behalf of the LEIA and Einstein Probe team\n\n\n\nWe report on a fast X-ray transient LXT 240402A detected by LEIA (Lobster Eye Imager for Astronomy) in 0.5-4 keV. The position of the source is R.A. = 245.438 deg, DEC = 25.800 deg with an uncertainty of 1.5 arcmin (radius, 90%C.L. statistical and systematic). The source was detected by LEIA at 2024-04-02T08:47:41 (UTC). The averaged 0.5-4 keV spectrum can be fitted with an absorbed power law (with the column density fixed to the galactic value of 3.4e20 cm^-2) with a photon index of 0.8 (-0.2/+0.2), giving an unabsorbed flux of ~2.6 (-0.4/+0.5) e-9 erg/s/cm2 in the 0.5-4 keV band. There are two peaks observed in the light curve. The transient event lasted for approximately 200 seconds with a peak flux of ~3e-8 erg/s/cm2 in 0.5-4 keV band. \n\nWithin the error circle of LXT 240402A, there is a radio galaxy (NVSS J162146+254915) at a redshift of ~0.05 with a ROSAT flux of 2.3e-12 erg/s/cm2, which is fainter than the peak flux detected by LEIA by more than three orders of magnitude. Assuming that LXT 240402A is associated with NVSS J162146+254915, the average luminosity of the X-ray transient is esitimated to be 1.5e46 erg/s. More follow-up observations are encouraged to help explore the nature of this transient.\n\nLEIA (Zhang et al. 2022, ApJL, 941, 2; Ling et al. 2023, RAA, 23, 095007) is a soft X-ray Lobster-eye imager (0.5 - 4.0keV) with a FoV of 340 square degrees aboard the experimental satellite SATech-01 of the CAS, launched on July 27, 2022. The above result is preliminary and the final result will be published elsewhere.\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/36016.",
"published": "2024-04-03T16:21:05.685775Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-04-03T16:21:05.685794Z",
"modified": "2024-04-03T16:21:05.691514Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 3992,
"topic": "gcn.circular",
"uuid": "87a3fa3e-2f83-4c32-9e04-4cf907668724",
"title": "GRB 230911C: ATCA detection of possible radio counterpart",
"submitter": "Hop gcn.circular",
"authors": "Sarah Chastain at University of New Mexico <sarahichastain@gmail.com>",
"data": {
"date": "23/10/19 17:29:14 GMT",
"from": "Sarah Chastain at University of New Mexico <sarahichastain@gmail.com>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34843"
},
"title": "GCN CIRCULAR",
"number": "34843",
"subject": "GRB 230911C: ATCA detection of possible radio counterpart"
},
"message_text": "S. Chastain (UNM), G. E. Anderson (Curtin), J. K. Leung (UofT/HUJI), S. D. Ryder (Macquarie), A. J. van der Horst (GWU), A. Gulati (USyd), and L. Rhodes (Oxford) on behalf of the ATCA PanRadio GRB collaboration\n\nThe Australia Telescope Compact Array (ATCA) observed long GRB 230911C (E. Sonbas et al., GCN 34655) as part of the ATCA \"PanRadio GRB\" Large Project C3542 (PI: G. Anderson) on 2023-09-11 UT, 2023-09-13 UT, 2023-09-26 UT, and 2023-10-16 UT.\n\nWe detect a possible radio afterglow at 9 GHz in the second epoch, which continues to brighten in the third, and fourth epoch. At 5.5 GHz this source is not detected in any of the observations.\nIn the fourth epoch at 5.5 GHz, we find 3-sigma upper limit of 105 microJy/beam. In the fourth epoch at 9.0 GHz, the source detected in the previous observations is detected at 150 +/- 35 microJy/beam.\nThe fitted position is:\nRAJ2000 = 15:07:13 +/- 8 arcseconds\nDECJ2000 = -41:19:51 +/- 1 arcsecond\nThis is approximately 18 arcseconds away from the reported Swift/XRT enhanced position (P. A. Evans et al., GCN 34658).\n\n\n\nFurther observations are planned.\n\nWe thank the CSIRO Space and Astronomy staff for supporting these observations.\nWe 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/34843.",
"published": "2023-10-19T17:29:25.096934Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-19T17:29:25.096972Z",
"modified": "2023-10-19T17:29:25.105735Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 3993,
"topic": "gcn.circular",
"uuid": "3c089b33-6f39-4bc2-aa34-7258e7c5c131",
"title": "GRB 231017A: Swift/UVOT Upper Limit",
"submitter": "Hop gcn.circular",
"authors": "Alice Breeveld at MSSL-UCL <a.breeveld@ucl.ac.uk>",
"data": {
"date": "23/10/19 18:34:36 GMT",
"from": "Alice Breeveld at MSSL-UCL <a.breeveld@ucl.ac.uk>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34844"
},
"title": "GCN CIRCULAR",
"number": "34844",
"subject": "GRB 231017A: Swift/UVOT Upper Limit"
},
"message_text": "A. A. Breeveld (UCL-MSSL) and T. Parsotan (GSFC/UMBC) report on behalf of the Swift/UVOT team:\n\nThe Swift/UVOT began settled observations of the field of GRB 231017A 73640 s after the GBM trigger (Mangan et al., GCN Circ. 34822).\nNo new sources are seen in the UVOT data.\nA preliminary 3-sigma upper limit using the UVOT photometric system, (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) at the position of the XRT candidate (Source 2) given by Dichiara et al. (GCN Circ. 34829) is:\n\nFilter T_start(s) T_stop(s) Exp(s) Mag\n\nu 73640 101690 4839 >21.0\n\nThe magnitude in the table is not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.252 in the direction of the burst (Schlegel et al. 1998).\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34844.",
"published": "2023-10-19T18:34:47.741482Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-19T18:34:47.741502Z",
"modified": "2023-10-19T18:34:47.759643Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 3994,
"topic": "gcn.circular",
"uuid": "2f657d10-ef3c-47e6-b7b7-6939ae8db26f",
"title": "IPN triangulation of GRB 231018A",
"submitter": "Hop gcn.circular",
"authors": "Dmitry Svinkin at Ioffe Institute <svinkin@mail.ioffe.ru>",
"data": {
"date": "23/10/19 18:41:19 GMT",
"from": "Dmitry Svinkin at Ioffe Institute <svinkin@mail.ioffe.ru>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34845"
},
"title": "GCN CIRCULAR",
"number": "34845",
"subject": "IPN triangulation of GRB 231018A"
},
"message_text": "D. 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\nS. Barthelmy, J. Cummings, H. Krimm, D. Palmer, and A. Tohuvavohu\non behalf of the Swift-BAT team,\nreport:\n\nThe bright, long-duration GRB 231018A\n(Fermi-GBM detection: The Fermi GBM team, GCN Circ. 34826;\nBALROG localization: Preis et al., GCN Circ. 34827)\nhas been detected by Fermi (GBM trigger 719325015), CALET (GBM),\nGECAM-B, INTEGRAL (SPI-ACS), Konus-Wind, and Swift (BAT),\nso far, at about 45010 s UT (12:30:10).\nThe burst was outside the coded field of view of the BAT.\n\nWe have triangulated it to a preliminary, 3 sigma error box\nwhose coordinates are:\n ---------------------------------------------\n RA(2000), deg Dec(2000), deg\n ---------------------------------------------\n Center:\n 1.122 (00h 04m 29s) +47.410 (+47d 24' 36\")\n Corners:\n 6.422 (00h 25m 41s) +50.650 (+50d 39' 01\")\n 356.061 (23h 44m 15s) +43.842 (+43d 50' 31\")\n 357.865 (23h 51m 28s) +44.479 (+44d 28' 43\")\n 10.820 (00h 43m 17s) +51.565 (+51d 33' 55\")\n ---------------------------------------------\nThe error box area is 6.6 sq. deg, and its maximum\ndimension is 12.54 deg (the minimum one is 38 arcmin).\nThe Sun distance was 137 deg.\n\nThe IPN localization is consistent with, but reduces the area of,\nthe final Fermi-GBM and the BALROG localizations.\n\nThis localization may be improved.\n\nA triangulation map and HEALPix FITS files are posted at\nhttp://www.ioffe.ru/LEA/GRBs/GRB231018_T45043/IPN\n\nThe Konus-Wind time history and spectrum will be given\nin a forthcoming GCN Circular.\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34845.",
"published": "2023-10-19T18:41:29.400324Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-19T18:41:29.400354Z",
"modified": "2023-10-19T18:41:29.409739Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4000,
"topic": "gcn.circular",
"uuid": "9ce40a2a-d478-455b-b91c-4015e6abcd13",
"title": "GRB 231018A: Glowbug gamma-ray detection",
"submitter": "Hop gcn.circular",
"authors": "C.C. Cheung at Naval Research Lab <Teddy.Cheung@nrl.navy.mil>",
"data": {
"date": "23/10/19 21:07:59 GMT",
"from": "C.C. Cheung at Naval Research Lab <Teddy.Cheung@nrl.navy.mil>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34847"
},
"title": "GCN CIRCULAR",
"number": "34847",
"subject": "GRB 231018A: Glowbug gamma-ray detection"
},
"message_text": "C.C. Cheung, M. Kerr, J. E. Grove, R. Woolf (NRL), A. Goldstein (USRA), C.A. Wilson-Hodge (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 231018A, which was also detected by Fermi/GBM, Konus-Wind, CALET, GECAM-B, INTEGRAL/SPI-ACS, and Swift/BAT, resulting in an IPN localization (GCN 34826, 34845, 34846).\n \nUsing an adaptive window with a resolution of 32-ms, the burst onset is determined to be 2023-10-18 12:30:07.824 with a duration of 87.6 s and a total significance of about 159 sigma. The Glowbug light curve comprises multiple peaks and is generally similar to the Konus-Wind light curve (GCN 34846).\n \nUsing a standard power-law function with an exponential high-energy cutoff [3] to model the emission over this duration results in a photon index dN/dE~E^x of x=1.0 and a cutoff energy (\"Epeak\") of 193 keV. The modeled 10-10000 keV fluence is 3.4e-05 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/34847.",
"published": "2023-10-19T21:08:10.550876Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-19T21:08:10.550897Z",
"modified": "2023-10-19T21:08:10.556931Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 3995,
"topic": "gcn.circular",
"uuid": "2f6e089a-7b5b-4c37-831b-c2034238418d",
"title": "Konus-Wind detection of GRB 231018A",
"submitter": "Hop gcn.circular",
"authors": "Dmitry Frederiks at Ioffe Institute <fred@mail.ioffe.ru>",
"data": {
"date": "23/10/19 18:44:04 GMT",
"from": "Dmitry Frederiks at Ioffe Institute <fred@mail.ioffe.ru>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34846"
},
"title": "GCN CIRCULAR",
"number": "34846",
"subject": "Konus-Wind detection of GRB 231018A"
},
"message_text": "D. Frederiks, A.Lysenko, A. Ridnaia, D. Svinkin,\nYu. Temiraev, A. Tsvetkova, M. Ulanov, and T. Cline,\non behalf of the Konus-Wind team, report:\n\nThe long, bright GRB 231018A (Fermi GBM detection: Lesage et al., GCN 34831;\nIPN triangulation: Svinkin et al., GCN 34845)\ntriggered Konus-Wind (KW) at T0=45043.083 s UT (12:30:43.083).\n\nThe burst light curve shows a multi-peaked emission complex,\nwhich starts at ~T0-32 s, peaks at ~T0+28 s,\nand has a total duration of ~90 s.\nThe emission is seen up to ~10 MeV.\n\nThe Konus-Wind light curve of this GRB is available at\nhttp://www.ioffe.ru/LEA/GRBs/GRB231018_T45043/\n\nAs observed by Konus-Wind, the burst had\na fluence of (1.17 ± 0.04)x10^-4 erg/cm^2 and\na 64-ms peak energy flux, measured from T0 + 28.352 s,\nof (2.44 ± 0.10)x10^-5 erg/cm^2/s (both in the 20 keV - 10 MeV energy range).\n\nThe time-integrated spectrum (measured from T0 to T0+38.912 s)\nis best fit in the 20 keV - 15 MeV range\nby a GRB (Band) function with the following model parameters:\nthe low-energy photon index alpha = -1.34 (-0.05,+0.05),\nthe high energy photon index beta = -2.92 (-0.17,+0.12),\nthe peak energy Ep = 114 (-4,+4) keV,\nchi2 = 90/96 dof.\n\nThe spectrum near the peak count rate (measured from T0+24.576 to T0+29.696 s)\nis best fit in the 20 keV - 15 MeV range\nby a GRB (Band) function with the following model parameters:\nthe low-energy photon index alpha = -1.19 (-0.05,+0.06),\nthe high energy photon index beta = -3.15 (-0.37,+0.24),\nthe peak energy Ep = 146 (-7,+8) keV,\nchi2 = 67/73 dof.\n\nAll the quoted errors are estimated at the 90% confidence level.\nAll the presented results are preliminary.\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34846.",
"published": "2023-10-19T18:44:11.423681Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-19T18:44:11.423702Z",
"modified": "2023-10-19T18:44:11.429988Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4214,
"topic": "gcn.circular",
"uuid": "91b2368a-548e-4209-9ff5-4a7248cb7412",
"title": "GRB 231030B: AstroSat CZTI detection",
"submitter": "Hop gcn.circular",
"authors": "Gaurav Waratkar at IIT Bombay <gauravwaratkar@iitb.ac.in>",
"data": {
"date": "23/10/31 14:01:12 GMT",
"from": "Gaurav Waratkar at IIT Bombay <gauravwaratkar@iitb.ac.in>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34919"
},
"title": "GCN CIRCULAR",
"number": "34919",
"subject": "GRB 231030B: AstroSat CZTI detection"
},
"message_text": "P. K. Navaneeth (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 likely long GRB 231030B which was also detected by Fermi-GBM (Fermi GBM Team, GCN Circ. 34915).\n\nThe source was clearly detected in the CZT detectors in the 20-200 keV energy range. The light curve peaks at 2023-10-30 19:58:21.25 UTC. The measured peak count rate associated with the burst is 356 (+57, -41) counts/s above the background in the combined data of three quadrants (out of four), with a total of 1131 (+128, -178) counts. The local mean background count rate was 242 (+2, -4) counts/s. Using cumulative rates, we measure a T90 of 6.4 (+2.1, -2.3) s.\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 2023-10-30 19:58:20.73 UTC. The measured peak count rate associated with the burst is 705 (+74, -78) counts/s above the background in the combined data of all quadrants, with a total of 2538 (+365, -401) counts. The local mean background count rate was 1484 (+6, -7) counts/s. We measure a T90 of 7.4 (+3.6, -3.1) 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/34919.",
"published": "2023-10-31T23:27:06.233140Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-31T23:27:06.233158Z",
"modified": "2023-10-31T23:27:06.238068Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4007,
"topic": "gcn.circular",
"uuid": "af85b061-6a35-4af4-8b4c-cf6937090a07",
"title": "Fermi GRB 231019A: 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": "23/10/20 00:00:57 GMT",
"from": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34848"
},
"title": "GCN CIRCULAR",
"number": "34848",
"subject": "Fermi GRB 231019A: 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 231019A ( Fermi GBM team, GCN 34842) errorbox 816 sec after notice time and 850 sec after trigger time at 2023-10-19 17:24:09 UT, with upper limit up to 17.5 mag. The observations began at zenith distance = 46 deg. The sun altitude is -42.0 deg.\n\nThe galactic latitude b = -12 deg., longitude l = 103 deg.\n\n\nReal time updated cover map and OT discovered available here:\nhttps://master.sai.msu.ru/site/master2/observ.php?id\"88694\n\nWe obtain a following upper limits.\n\nTmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment\n_________|_____________________|_____________________|____________________________________|_____|_______|_______|________\n\n 881 | 2023-10-19 17:24:09 | MASTER-Amur | (22h 54m 16.71s , +46d 46m 10.5s) | C | 60 | 17.4 |\n 961 | 2023-10-19 17:25:28 | MASTER-Amur | (23h 05m 59.53s , +46d 44m 56.9s) | C | 60 | 17.5 |\n 1040 | 2023-10-19 17:26:48 | MASTER-Amur | (22h 59m 27.09s , +48d 37m 55.9s) | C | 60 | 17.5 |\n 1120 | 2023-10-19 17:28:08 | MASTER-Amur | (23h 11m 28.93s , +48d 39m 20.4s) | C | 60 | 17.4 |\n 1200 | 2023-10-19 17:29:28 | MASTER-Amur | (22h 36m 34.03s , +48d 40m 14.4s) | C | 60 | 17.1 |\n 1279 | 2023-10-19 17:30:47 | MASTER-Amur | (22h 48m 32.17s , +48d 39m 03.7s) | C | 60 | 17.4 |\n 1370 | 2023-10-19 17:32:18 | MASTER-Amur | (22h 42m 41.86s , +50d 33m 03.9s) | C | 60 | 17.2 |\n 1450 | 2023-10-19 17:33:38 | MASTER-Amur | (22h 55m 09.57s , +50d 31m 51.8s) | C | 60 | 17.4 |\n 1530 | 2023-10-19 17:34:58 | MASTER-Amur | (22h 54m 23.63s , +46d 44m 22.5s) | C | 60 | 17.1 |\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/34848.",
"published": "2023-10-20T00:01:09.136076Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-20T00:01:09.136108Z",
"modified": "2023-10-20T00:01:09.150487Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6323,
"topic": "gcn.circular",
"uuid": "865d924a-4510-415a-9a6b-4cd450174d11",
"title": "GRB 240402B: GECAM-C detection",
"submitter": "Hop gcn.circular",
"authors": "Kai <wcxuemail@gmail.com>",
"data": {
"date": "24/04/03 17:01:02 GMT",
"from": "Kai <wcxuemail@gmail.com>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/36017"
},
"title": "GCN CIRCULAR",
"number": "36017",
"subject": "GRB 240402B: GECAM-C detection"
},
"message_text": "Wang-Chen Xue, Shao-Lin Xiong, Chao Zheng, Yanqiu Zhang, and Chengkui Li,\nreport on behalf of the GECAM team:\n\nGECAM-C observed a long burst, GRB 240402A at\n2024-04-02T08:47:46 UTC (denoted as T0), which has been\ndetected by LEIA (GCN 36016) and Konus-Wind.\n\nAccording to the observation data of GECAM-C, this burst mainly consists\nof two peaks with a duration (T90) of 6.55 +/- 0.52 sec (15-350 keV).\n\nThe GECAM-C localization is consistent with the LEIA localization\n(GCN 36016) within the error.\n\nThe time-averaged spectrum of GECAM-C data from T0-7.0 to T0+7.0 s could be\nadequately fit by a cut-off power-law with photon index alpha of -0.62 (-0.14, +0.13),\nand peak energy Ep of 66 (-3, +3) keV. The corresponding burst fluence is\n7.69 (-0.24, +0.25) * 10^-7 erg/cm^2 in 15-350 keV.\n\nWe note that these results are preliminary and refined analysis will be reported later.\n\nGravitational wave high-energy Electromagnetic Counterpart All-sky Monitor\n(GECAM) mission originally consists of two micro-satellites (GECAM-A and GECAM-B)\nlaunched in Dec. 2020. As the third member of GECAM constellation,\nGECAM-C was launched onboard SATech-01 experimental satellite in July 2022.\nGECAM mission is funded by the Chinese Academy of Sciences (CAS).\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/36017.",
"published": "2024-04-03T17:01:20.304200Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-04-03T17:01:20.304212Z",
"modified": "2024-04-03T17:01:20.309819Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4020,
"topic": "gcn.circular",
"uuid": "426b7955-3bb7-4eba-8e98-4dead6c51399",
"title": "GRB 231018A: CALET Gamma-Ray Burst Monitor detection",
"submitter": "Hop gcn.circular",
"authors": "Yuta Kawakubo at Louisiana State University <kawakubo1@lsu.edu>",
"data": {
"date": "23/10/20 04:35:30 GMT",
"from": "Yuta Kawakubo at Louisiana State University <kawakubo1@lsu.edu>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34849"
},
"title": "GCN CIRCULAR",
"number": "34849",
"subject": "GRB 231018A: CALET Gamma-Ray Burst Monitor detection"
},
"message_text": "P. S. Marrocchesi (U of Siena), A. Yoshida, T. Sakamoto,\nS. Sugita (AGU), Y. Kawakubo (LSU), K. Yamaoka (Nagoya U),\nS. Nakahira (JAXA), Y. Asaoka (ICRR), S. Torii, Y. Akaike,\nK. Kobayashi (Waseda U), Y. Shimizu, T. Tamura (Kanagawa U),\nN. Cannady (GSFC/UMBC), M. L. Cherry (LSU),\nS. Ricciarini (U of Florence),\nand the CALET collaboration:\n\nThe long GRB 231018A (Fermi GBM Final Real-time Localization: Fermi\nGBM team, GCN Circ. 34826; BALROG localization: Preis et al.,\nGCN Circ 34827; Fermi GBM Detection: Lesage et al., GCN Circ 34831;\nIPN triangulation: Svinkin et al., GCN Circ 34845; Konus-Wind detection:\nFrederiks et al., GCN Circ 34846; Glowbug gamma-ray detection: Cheung\net al., GCN Circ 34847) triggered the CALET Gamma-ray Burst Monitor (CGBM)\nat 12:30:52.87 UTC on 18 October 2023\n(http://cgbm.calet.jp/cgbm_trigger/flight/1381667434/index.html).\nThe burst signal was seen by only the SGM detector.\n\nThe burst light curve shows a multi-peaked structure that ends T+46 sec.\nSince CGBM was in the HV-on sequence, the whole episode was not observed by CGBM.\nThe ground-processed light curve is available at\n\nhttp://cgbm.calet.jp/cgbm_trigger/ground/1381667434/\n\nThe CALET data used in this analysis are provided by\nthe Waseda CALET Operation Center located at Waseda University.\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34849.",
"published": "2023-10-20T04:35:41.213674Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-20T04:35:41.213706Z",
"modified": "2023-10-20T04:35:41.220825Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4027,
"topic": "gcn.circular",
"uuid": "6dd2c4a5-8116-427f-90f0-2d1a600b5422",
"title": "GRB 231018A: GRBAlpha detection",
"submitter": "Hop gcn.circular",
"authors": "Marianna DafÄÃková at Masaryk University <500025@mail.muni.cz>",
"data": {
"date": "23/10/20 10:02:38 GMT",
"from": "Marianna DafÄÃková at Masaryk University <500025@mail.muni.cz>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34850"
},
"title": "GCN CIRCULAR",
"number": "34850",
"subject": "GRB 231018A: GRBAlpha detection"
},
"message_text": "M. Dafcikova, J. Ripa (Masaryk U.), A. Pal (Konkoly Observatory), N. Werner (Masaryk U.), M. Ohno, H. Takahashi (Hiroshima U.), L. Meszaros, B. Csak (Konkoly Observatory), N. Husarikova, F. Munz , M. Topinka, M. Kolar, J.-P. Breuer, F. Hroch (Masaryk U.), T. Urbanec, M. Kasal, A. Povalac (Brno U. of Technology), J. Hudec, J. Kapus, M. Frajt (Spacemanic s.r.o), R. Laszlo, M. Koleda (Needronix s.r.o), M. Smelko, P. Hanak, P. Lipovsky (Technical U. of Kosice), G. Galgoczi (Wigner Research Center/Eotvos U.), Y. Uchida, H. Poon, H. Matake (Hiroshima U.), N. Uchida (ISAS/JAXA), T. Bozoki (Eotvos U.), G. Dalya (Eotvos U.), yyT. Enoto (Kyoto U.), Zs. Frei (Eotvos U.), G. Friss (Eotvos U.), Y. Fukazawa, K. Hirose (Hiroshima U.), S. Hisadomi (Nagoya U.), Y. Ichinohe (Rikkyo U.), K. Kapas (Eotvos U.), L. L. Kiss (Konkoly Observatory), T. Mizuno (Hiroshima U.), K. Nakazawa (Nagoya U.), H. Odaka (Univ of Tokyo), J. Takatsy (Eotvos U.), K. Torigoe (Hiroshima U.), N. Kogiso, M. Yoneyama (Osaka Metropolitan U.), M. Moritaki (U. Tokyo), T. Kano (U. Michigan) -- the GRBAlpha collaboration.\n\nThe long-duration GRB 231018A (Fermi/GBM detection: GCN 34831; Konus/Wind detection: GCN 34846; Glowbug detection: GCN 34847; CALET/CGBM detection: GCN 34849; INTEGRAL/SPI-ACS peak detection at 2023-10-18 ~12:31:08 UT) was observed by the GRBAlpha 1U CubeSat (Pal et al. 2023, A&A, 677, 40; arXiv:2302.10048).\n\nThe detection was confirmed at the peak time 2023-10-18 12:31:08 UTC. The T90 duration measured by GRBAlpha is 32 s and the overall significance during T90 reaches 91 sigma.\n\nThe light curve obtained by GRBAlpha is available here: \nhttps://grbalpha.konkoly.hu/static/share/GRB231018A_GCN.pdf\n\nAll GRBAlpha detections are listed at: https://monoceros.physics.muni.cz/hea/GRBAlpha/ \nGRBAlpha, launched on 2021 March 22, is a demonstration mission for a future CubeSat constellation (Werner et al. Proc. SPIE 2018). The detector of GRBAlpha consists of a 75 x 75 x 5 mm3 CsI scintillator read out by a SiPM array, covering the energy range from ~50 keV to ~1000 keV. To increase the duty cycle and the downlink rate, the upgrade of the on-board data acquisition software stack is in progress. The ground segment is also supported by the radio amateur community and it takes advantage of the SatNOGS network for increased data downlink volume. \n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34850.",
"published": "2023-10-20T10:02:49.399689Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-20T10:02:49.399725Z",
"modified": "2023-10-20T10:02:49.413236Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4040,
"topic": "gcn.circular",
"uuid": "ccc1f3aa-13d5-45c7-a96d-8104454a4c69",
"title": "IceCube-231004A: Upper limits from Fermi-GBM Observations",
"submitter": "Hop gcn.circular",
"authors": "Joshua Wood at NASA/MSFC <joshua.r.wood@nasa.gov>",
"data": {
"date": "23/10/20 15:50:36 GMT",
"from": "Joshua Wood at NASA/MSFC <joshua.r.wood@nasa.gov>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34851"
},
"title": "GCN CIRCULAR",
"number": "34851",
"subject": "IceCube-231004A: Upper limits from Fermi-GBM Observations"
},
"message_text": "J. Wood (NASA/MSFC), Eric Burns (LSU), Michelle Hui (NASA/MSFC) report on behalf of the Fermi-GBM team:\n\nFor the IceCube high-energy neutrino candidate event IceCube-231004A\n(GCN 34797), at the event time Fermi-GBM was observing the reported\nneutrino location at:\n\nRA: 143.79 (+1.10, -1.01 deg 90% PSF containment) J2000\nDec: -25.04 (+1.03, -1.21 deg 90% PSF containment) J2000\n\nThere was no Fermi-GBM onboard trigger around the event time of the\nneutrino candidate. An automated, blind search for short gamma-ray\nbursts below the onboard triggering threshold in Fermi-GBM also\nidentified no counterpart candidates. The GBM targeted search,\nthe most sensitive, coherent search for GRB-like signals,\nwas run from +/-30 s around the neutrino candidate time.\nFrom this search, no significant signal was found related\nto IceCube-231004A.\n\nWe set upper limits on impulsive gamma-ray emission to aid\ntheoretical modeling of the potential optical counterpart\nAT2023uqf/ZTF23abidzvf (GCN 34837). Using the representative\nsoft, normal, and hard GRB-like templates described in\narXiv:2308.13666, we set the following 3 sigma flux upper limits over\n10-1000 keV (in units of 10^-7 erg/s/cm^2):\n\nTimescale Soft Normal Hard\n-------------------------------------------\n0.128 s: 2.9 4.2 7.3\n1.024 s: 0.9 1.4 2.3\n8.192 s: 0.3 0.4 0.6\n\nAssuming the reported redshift z = 0.1503 (GCN 34837), we estimate\nthe following intrinsic luminosity upper limits over\nthe 1 keV-10 MeV energy range (in units of 10^49 erg/s):\n\nTimescale Soft Normal Hard\n------------------------------------\n0.128s: 2.8 3.7 10.6\n1.024s: 0.8 1.2 3.3\n8.192s: 0.3 0.3 0.9\n\nThese results are preliminary.\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34851.",
"published": "2023-10-20T15:50:52.146866Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-20T15:50:52.146896Z",
"modified": "2023-10-20T15:50:52.152591Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4042,
"topic": "gcn.circular",
"uuid": "1ee9cfa0-f287-4e09-b792-e31bd1ed6d7c",
"title": "LIGO/Virgo/KAGRA S231020ba: Identification of a GW compact binary merger candidate",
"submitter": "Hop gcn.circular",
"authors": "Paul Stevens at IJCLab, Paris <paul.stevens@ligo.org>",
"data": {
"date": "23/10/20 15:52:30 GMT",
"from": "Paul Stevens at IJCLab, Paris <paul.stevens@ligo.org>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34852"
},
"title": "GCN CIRCULAR",
"number": "34852",
"subject": "LIGO/Virgo/KAGRA S231020ba: Identification of a GW compact binary merger candidate"
},
"message_text": "The LIGO Scientific Collaboration, the Virgo Collaboration, and the KAGRA Collaboration report:\n\nWe identified the compact binary merger candidate S231020ba during real-time processing of data from LIGO Hanford Observatory (H1) and LIGO Livingston Observatory (L1) at 2023-10-20 14:29:47.583 UTC (GPS time: 1381847405.583). The candidate was found by the GstLAL [1], MBTA [2], PyCBC Live [3], and SPIIR [4] analysis pipelines.\n\nS231020ba is an event of interest because its false alarm rate, as estimated by the online analysis, is 1.3e-09 Hz, or about one in 25 years. The event's properties can be found at this URL:\n\nhttps://gracedb.ligo.org/superevents/S231020ba\n\nThe classification of the GW signal, in order of descending probability, is BBH (91%), NSBH (8%), Terrestrial (<1%), or BNS (<1%).\n\nThere was a high rate of noise transients (glitches) in the LIGO Hanford detector which may affect the parameters or the significance of the candidate.\n\nAssuming the candidate is astrophysical in origin, the probability that the lighter compact object is consistent with a neutron star mass (HasNS) is <1%. [5] Using the masses and spins inferred from the signal, the probability of matter outside the final compact object (HasRemnant) is <1%. [5] Both HasNS and HasRemnant consider the support of several neutron star equations of state. The probability that either of the binary components lies between 3 and 5 solar masses (HasMassGap) is 7%.\n\nTwo sky maps are available at this time and can be retrieved from the GraceDB event page:\n * bayestar.multiorder.fits,1, an initial localization generated by BAYESTAR [6], distributed via GCN notice about 27 seconds after the candidate event time.\n * bayestar.multiorder.fits,2, an initial localization generated by BAYESTAR [6], distributed via GCN notice about 5 minutes after the candidate event time.\n\nThe preferred sky map at this time is bayestar.multiorder.fits,2. For the bayestar.multiorder.fits,2 sky map, the 90% credible region is 1444 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 1111 +/- 404 Mpc (a posteriori mean +/- standard deviation).\n\nFor further information about analysis methodology and the contents of this alert, refer to the LIGO/Virgo/KAGRA Public Alerts User Guide https://emfollow.docs.ligo.org/userguide/.\n\n [1] Tsukada et al. PRD 108, 043004 (2023) and Ewing et al. arXiv:2305.05625 (2023)\n [2] Aubin et al. CQG 38, 095004 (2021)\n [3] Dal Canton et al. ApJ 923, 254 (2021)\n [4] Chu et al. PRD 105, 024023 (2022)\n [5] Chatterjee et al. ApJ 896, 54 (2020)\n [6] Singer & Price PRD 93, 024013 (2016)\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34852.",
"published": "2023-10-20T15:52:37.477178Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-20T15:52:37.477214Z",
"modified": "2023-10-20T15:52:37.483810Z",
"nonlocalizedevents": [
{
"event_id": "S231020b"
}
],
"targets": []
},
{
"id": 4045,
"topic": "gcn.circular",
"uuid": "400c545a-ca1d-4f97-8a93-8d231de49b19",
"title": "GRB 231017A: 1.3m DFOT Optical upper limit",
"submitter": "Hop gcn.circular",
"authors": "Amit Kumar Ror at ARIES <mitturor77894@gmail.com>",
"data": {
"date": "23/10/20 17:12:08 GMT",
"from": "Amit Kumar Ror at ARIES <mitturor77894@gmail.com>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34853"
},
"title": "GCN CIRCULAR",
"number": "34853",
"subject": "GRB 231017A: 1.3m DFOT Optical upper limit"
},
"message_text": "Amit K. Ror, Rahul Gupta, Amar Aryan, Shashi B. Pandey, Rishi C., and\nNeelam Panwar (ARIES) report:\n\nWe observed the field of Fermi, and Swift detected GRB 231017A (Fermi GCM\nTeam GCN 34822; Mangan et al. 2023, GCN 34830; DeLaunay et al. 2023, GCN\n34824; and Swift team GCN 34825) with the 1.3m Devasthal Fast Optical\nTelescope (DFOT), located at the Devasthal Observatory of the Aryabhatta\nResearch Institute of Observational Sciences (ARIES), India. The\nobservations were started on 2023-10-18 at 22:19:07 UT, i.e., ~ 1.6 days\nafter the GBM trigger. We have taken multiple frames with an exposure time\nof 100 s in the R filter. We stacked the images after the alignment. We did\nnot detect any optical afterglow in our stacked image within the error box\nof Swift-XRT observation (Dichiara et al., 2023, GCN 34829). We obtain the\nfollowing preliminary 3-sigma upper limit in the stacked image:\n\n\nDate Start_UT T_start-T0 (days) Filter Exp time (s) Limiting magnitude\n\n========================================================\n2023-10-18 22:19:07 1.6 R 100*36 > 21.6\n\nOur non-detection is consistent with Kumar et al. 2023, GCN 34833;\nStrausbaugh et al. 2023, GCN 34834; Shrestha et al. 2023, GCN 34836; Xu et\nal. 2023, GCN 34840; and Belkin et al. 2023, GCN 34841.\n\nThe magnitude is not corrected for the Galactic extinction in the direction\nof the burst. Photometric calibration is performed using the standard stars\nfrom the USNO-B1.0 catalog. This circular may be cited.\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34853.",
"published": "2023-10-20T17:12:23.452076Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-20T17:12:23.452106Z",
"modified": "2023-10-20T17:12:23.462562Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4046,
"topic": "gcn.circular",
"uuid": "b2fc81ab-be5e-47b5-b585-ecfad80cb1f7",
"title": "LIGO/Virgo/KAGRA S231020ba: Coverage and upper limits from MAXI/GSC observations",
"submitter": "Hop gcn.circular",
"authors": "Yuta Kawakubo at Louisiana State University <kawakubo1@lsu.edu>",
"data": {
"date": "23/10/20 17:24:16 GMT",
"from": "Yuta Kawakubo at Louisiana State University <kawakubo1@lsu.edu>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34854"
},
"title": "GCN CIRCULAR",
"number": "34854",
"subject": "LIGO/Virgo/KAGRA S231020ba: Coverage and upper limits from MAXI/GSC observations"
},
"message_text": "Y. Kawakubo (LSU),\nH. Negoro, M. Nakajima (Nihon U.),\nT. Mihara (RIKEN), N. Kawai (RIKEN),\nS. Sugita, M. Serino, H. Hiramatsu, H. Nishikawa, Y. Kondo (AGU),\nreport on behalf of the MAXI team:\n\nWe examined MAXI/GSC all-sky X-ray images (2-20 keV)\nafter compact binary merger candidate S231020ba at 2023-10-20 14:29:47.000 UTC (GCN #34852).\n\nAt the trigger time of S231020ba, the high-voltage of MAXI/GSC was off,\nand it was turned on at T0+1153 sec (+19.2 min).\nThe first one-orbit (92 min) scan observation with GSC after the event covered 90%\nof the 90% credible region of the bayestar skymap from 14:51:52 to 16:00:18 UTC (T0+1325 to T0+5431 sec).\n\nNo significant new source was found in the region in the one-orbit scan observation.\nA typical 1-sigma averaged upper limit obtained in one scan observation\nis 20 mCrab at 2-20 keV.\n\nIf you require information about X-ray flux by MAXI/GSC at specific coordinates,\nplease contact the submitter of this circular by email.\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34854.",
"published": "2023-10-20T17:24:27.586952Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-10-20T17:24:27.586972Z",
"modified": "2023-10-20T17:24:27.595735Z",
"nonlocalizedevents": [
{
"event_id": "S231020b"
}
],
"targets": []
},
{
"id": 6324,
"topic": "gcn.circular",
"uuid": "6409174d-a1a0-4538-8bd0-0d99a2fd373e",
"title": "GRB 240402B: GWAC-F50A optical upper limit",
"submitter": "Hop gcn.circular",
"authors": "Liping Xin at NAOC, SVOM <xlp@nao.cas.cn>",
"data": {
"date": "24/04/03 22:56:22 GMT",
"from": "Liping Xin at NAOC, SVOM <xlp@nao.cas.cn>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/36018"
},
"title": "GCN CIRCULAR",
"number": "36018",
"subject": "GRB 240402B: GWAC-F50A optical upper limit"
},
"message_text": "\nL.P.Xin(NAOC), Y.G.Yang(HNU), C.WU(NAOC), Y.L.Qiu(NAOC), J.Wang(GXU/NAOC),\nL.H.Li(NAOC), C.Wu(NAOC), E.W.Liang(GXU), X.H.Han (NAOC), X.M.Lu(NAOC),\nR.S.Zhang(NAOC), Y.Xu(NAOC), Y.J.Xiao(NAOC), P.P.Zhang(NAOC), L.Lan(NAOC),\nJ.Y.Wei(NAOC) on behalf of the SVOM/GWAC team:\n\nWe began to observe X-ray transient LXT 240402A (Xu et all., GCN 36106) detected by LEIA,\nwhich was also detected by GECAME-C as GRB 240402B (Xue et al., GCN 36107),\nwith GWAC-F50A telescope, at Xinglong station, China, at 19:22:13 (UT), 03. April. 2024,\nabout 34.57 hours after the burst. The weather was not good.\n\nAfter stacking 5*200 seconds, no any new sources were detected in our stacked image\ndown to a limit magnitude of 18.0 mag in R band comparing to several nearby USNO B1.0 stars.\n\nWe acknowledge the excellent support from observation assistant Yangtong Zheng.\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/36018.",
"published": "2024-04-03T22:56:42.444417Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-04-03T22:56:42.444433Z",
"modified": "2024-04-03T22:56:42.452839Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6325,
"topic": "gcn.circular",
"uuid": "735e4c37-4cf2-49d1-9f6e-0c4a6cfdfff8",
"title": "LXT 240402A: MASTER optical observations with AGN in error-box",
"submitter": "Hop gcn.circular",
"authors": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"data": {
"date": "24/04/03 23:16:13 GMT",
"from": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/36019"
},
"title": "GCN CIRCULAR",
"number": "36019",
"subject": "LXT 240402A: MASTER optical observations with AGN in error-box"
},
"message_text": "\nV.Lipunov, P.Balanutsa (Lomonosov MSU), D.Buckley (SAAO), O.Gress, N.Budnev(ISU), K.Zhirkov, A.Kuznetsov,\nG.Antipov, N.Tiurina, E.Gorbovskoy, Ya.Kechin, D.Vlasenko, Yu.Tselik, I.Gorbunov,\nV.Vladimirov,D.Zimnukhov, V.Senik, A.Yudin,A.Chasovnikov, D.Cheryasov(Lomonosov MSU,SAI,PhysicsDepartment),\nA.Sosnovskij (Crimean Astrophysical Observatory, RAS),\nC.Francile. F. Podesta, R.Podesta (Observatorio Astronomico Felix AguilarOAFA),\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 LXT 240402A (Xu et al. GCN 36016, Triggertime 24-04-02 08:47:41UT, Notice$/04/03 16:20:48;\nCenter R.A.,Dec. = 245.438 +25.800 +-1.5 arcmin; also detected by GECAM-C (GCN 36017 Wang-Chen Xue et al.))\nobservation at 2024-04-03 02:48:45 (optical observations also started by GWAC-F50A (Xin et al. GCN 36018))\n\nMASTER-SAAO robotic telescope located in South Africa was pointed to errorbox\n64864 sec after trigger time at 2024-04-03 02:48:45 UT (by own observational program), with upper limit up to 19.3 mag.\nThe observations began at zenith distance = 60 deg. The sun altitude is -26.7 deg.\n\nMASTER-Tunka robotic telescope (Russia, Baikal) was pointed 1 days 28326 sec after trigger time at 2024-04-03 16:39:47 UT, with upper limit up to 20.0 mag.\nThe observations began at zenith distance = 52 deg. The sun altitude is -33.1 deg.\n\nMASTER-Amur robotic telescope (Russia, Blagoveschensk) was pointed 1 days 28367 sec after trigger time at\n2024-04-03 16:40:28 UT, with upper limit up to 19.0 mag.\nThe observations began at zenith distance = 37 deg. The sun altitude is -32.6 deg.\n\nThe analysis of LERG AGN (Comerford et al. 2020), locate in 75\" frin the errir-box center) light curve in MASTER database will be continued.\n\nThe galactic latitude b = 43 deg., longitude l = 44 deg.\n\nReal time updated cover map and possibly OT, that can be discovered, will be available here:\nhttps://master.sai.msu.ru/site/master2/observ.php?id$13927\n\nWe obtain the following upper limits.\n\nTmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment\n_________|_____________________|_____________________|____________________________________|_____|_______|_______|________\n\n 64894 | 2024-04-03 02:48:45 | MASTER-SAAO | (16h 19m 12.57s , +27d 40m 03.0s) | C | 60 | 18.2 |\n 65856 | 2024-04-03 03:04:47 | MASTER-SAAO | (16h 19m 18.33s , +27d 39m 39.9s) | C | 60 | 18.1 |\n 66812 | 2024-04-03 03:20:43 | MASTER-SAAO | (16h 19m 23.87s , +27d 41m 06.6s) | C | 60 | 18.4 |\n 67771 | 2024-04-03 03:36:41 | MASTER-SAAO | (16h 17m 58.29s , +25d 59m 53.5s) | C | 60 | 18.3 |\n 67831 | 2024-04-03 03:36:41 | MASTER-SAAO | (16h 17m 58.29s , +25d 59m 53.3s) | C | 180 | 17.3 | Coadd\n 67771 | 2024-04-03 03:36:41 | MASTER-SAAO | (16h 19m 52.88s , +25d 46m 41.7s) | C | 60 | 18.5 |\n 67831 | 2024-04-03 03:36:41 | MASTER-SAAO | (16h 19m 52.89s , +25d 46m 41.7s) | C | 180 | 17.4 | Coadd\n 68729 | 2024-04-03 03:52:39 | MASTER-SAAO | (16h 18m 01.18s , +26d 01m 18.6s) | C | 60 | 17.8 |\n 68729 | 2024-04-03 03:52:39 | MASTER-SAAO | (16h 19m 56.33s , +25d 48m 07.4s) | C | 60 | 18.2 |\n 69688 | 2024-04-03 04:08:39 | MASTER-SAAO | (16h 18m 00.35s , +26d 02m 44.4s) | C | 60 | 16.0 |\n 69688 | 2024-04-03 04:08:39 | MASTER-SAAO | (16h 19m 55.57s , +25d 49m 31.9s) | C | 60 | 16.1 |\n 114741 | 2024-04-03 16:39:47 | MASTER-Tunka | (16h 21m 42.47s , +25d 05m 39.5s) | C | 30 | 18.5 |\n 114742 | 2024-04-03 16:39:47 | MASTER-Tunka | (16h 22m 52.93s , +25d 47m 55.4s) | C | 30 | 19.0 |\n 114772 | 2024-04-03 16:39:47 | MASTER-Tunka | (16h 22m 52.93s , +25d 47m 55.4s) | C | 90 | 19.7 | Coadd\n 114783 | 2024-04-03 16:40:28 | MASTER-Amur | (16h 23m 12.57s , +25d 41m 12.4s) | C | 30 | 18.4 |\n 114783 | 2024-04-03 16:40:28 | MASTER-Amur | (16h 22m 57.71s , +26d 02m 22.2s) | C | 30 | 17.4 |\n 114816 | 2024-04-03 16:41:02 | MASTER-Tunka | (16h 21m 36.76s , +25d 04m 43.0s) | C | 30 | 18.6 |\n 114817 | 2024-04-03 16:41:02 | MASTER-Tunka | (16h 22m 47.20s , +25d 46m 58.9s) | C | 30 | 19.1 |\n 114846 | 2024-04-03 16:41:32 | MASTER-Amur | (16h 23m 07.00s , +25d 40m 05.4s) | C | 30 | 18.4 |\n 114846 | 2024-04-03 16:41:32 | MASTER-Amur | (16h 22m 52.04s , +26d 01m 14.7s) | C | 30 | 17.2 |\n 114891 | 2024-04-03 16:42:16 | MASTER-Tunka | (16h 21m 42.59s , +25d 05m 02.4s) | C | 30 | 18.5 |\n 114891 | 2024-04-03 16:42:16 | MASTER-Tunka | (16h 22m 53.03s , +25d 47m 18.5s) | C | 30 | 19.2 |\n 114910 | 2024-04-03 16:42:36 | MASTER-Amur | (16h 22m 57.77s , +26d 01m 20.4s) | C | 30 | 17.3 |\n 114910 | 2024-04-03 16:42:36 | MASTER-Amur | (16h 23m 12.81s , +25d 40m 11.5s) | C | 30 | 18.5 |\n 114960 | 2024-04-03 16:43:25 | MASTER-Tunka | (16h 21m 39.39s , +25d 06m 34.5s) | C | 30 | 18.4 |\n 114960 | 2024-04-03 16:43:26 | MASTER-Tunka | (16h 22m 49.83s , +25d 48m 50.6s) | C | 30 | 19.0 |\n 114990 | 2024-04-03 16:43:26 | MASTER-Tunka | (16h 22m 49.83s , +25d 48m 50.7s) | C | 90 | 19.4 | Coadd\n 114973 | 2024-04-03 16:43:39 | MASTER-Amur | (16h 23m 09.88s , +25d 41m 33.3s) | C | 30 | 18.5 |\n 114973 | 2024-04-03 16:43:39 | MASTER-Amur | (16h 22m 54.77s , +26d 02m 41.6s) | C | 30 | 17.4 |\n 115036 | 2024-04-03 16:44:42 | MASTER-Amur | (16h 23m 10.10s , +25d 40m 13.1s) | C | 30 | 18.5 |\n 115037 | 2024-04-03 16:44:42 | MASTER-Amur | (16h 22m 54.96s , +26d 01m 20.9s) | C | 30 | 17.3 |\n 115038 | 2024-04-03 16:44:44 | MASTER-Tunka | (16h 21m 39.42s , +25d 05m 05.1s) | C | 30 | 18.2 |\n 115038 | 2024-04-03 16:44:44 | MASTER-Tunka | (16h 22m 49.83s , +25d 47m 21.3s) | C | 30 | 18.8 |\n 115100 | 2024-04-03 16:45:46 | MASTER-Amur | (16h 23m 12.16s , +25d 41m 27.8s) | C | 30 | 18.4 |\n 115100 | 2024-04-03 16:45:46 | MASTER-Amur | (16h 22m 56.99s , +26d 02m 35.4s) | C | 30 | 17.4 |\n 115113 | 2024-04-03 16:45:58 | MASTER-Tunka | (16h 21m 43.49s , +25d 06m 49.9s) | C | 30 | 18.3 |\n 115113 | 2024-04-03 16:45:59 | MASTER-Tunka | (16h 22m 53.89s , +25d 49m 05.9s) | C | 30 | 18.8 |\n 115163 | 2024-04-03 16:46:49 | MASTER-Amur | (16h 23m 07.27s , +25d 40m 36.5s) | C | 30 | 18.5 |\n 115163 | 2024-04-03 16:46:49 | MASTER-Amur | (16h 22m 52.06s , +26d 01m 43.8s) | C | 30 | 17.3 |\n 115189 | 2024-04-03 16:47:14 | MASTER-Tunka | (16h 21m 35.99s , +25d 05m 59.2s) | C | 30 | 18.3 |\n 115189 | 2024-04-03 16:47:15 | MASTER-Tunka | (16h 22m 46.37s , +25d 48m 15.2s) | C | 30 | 18.8 |\n 115219 | 2024-04-03 16:47:15 | MASTER-Tunka | (16h 22m 46.37s , +25d 48m 15.2s) | C | 90 | 19.3 | Coadd\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/36019.",
"published": "2024-04-03T23:16:28.503860Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-04-03T23:16:28.503876Z",
"modified": "2024-04-03T23:16:28.510520Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4299,
"topic": "gcn.circular",
"uuid": "9a137263-9ac9-497e-854d-e00c5b9a6f63",
"title": "GRB 231101A: 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": "23/11/01 02:33:51 GMT",
"from": "Fermi GBM Team at MSFC/Fermi-GBM <do_not_reply@GIOC.nsstc.nasa.gov>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34924"
},
"title": "GCN CIRCULAR",
"number": "34924",
"subject": "GRB 231101A: Fermi GBM Final Real-time Localization"
},
"message_text": "The Fermi GBM team reports the detection of a likely LONG GRB\n\nAt 02:23:16 UT on 1 Nov 2023, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 231101A (trigger 720498201.799648 / 231101099).\n\nThe on-ground calculated location, using the Fermi GBM trigger data, is RA = 137.1, Dec = 13.3 (J2000 degrees, equivalent to J2000 09h 08m, 13d 18'), with a statistical uncertainty of 13.2 degrees.\n\nThe angle from the Fermi LAT boresight is 86.0 degrees.\n\nThe skymap can be found here:\nhttps://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn231101099/quicklook/glg_skymap_all_bn231101099.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/2023/bn231101099/quicklook/glg_healpix_all_bn231101099.fit\n\nThe GBM light curve can be found here:\nhttps://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn231101099/quicklook/glg_lc_medres34_bn231101099.gif\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34924.",
"published": "2023-11-01T02:34:01.962243Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-11-01T02:34:01.962267Z",
"modified": "2023-11-01T02:34:01.968526Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4300,
"topic": "gcn.circular",
"uuid": "92052616-d540-4412-90ab-ff6ae6dc1e9f",
"title": "Fermi trigger No 720498201: 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": "23/11/01 02:46:02 GMT",
"from": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34925"
},
"title": "GCN CIRCULAR",
"number": "34925",
"subject": "Fermi trigger No 720498201: 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) started inspect of the Fermi GRB231101.10 (trigger No 720498201,09h 08m 14.40s , +13d 15m 36.0s, R\u0013.18) errorbox 90 sec after notice time and 123 sec after trigger time at 2023-11-01 02:25:20 UT, with upper limit up to 17.4 mag. Observations started at twilight. The observations began at zenith distance = 45 deg. The sun altitude is -14.9 deg.\n\nMASTER-Tavrida robotic telescope located in Russia (Lomonosov MSU, SAI Crimea astronomical station) started inspect of the Fermi GRB231101.10 errorbox 308 sec after notice time and 341 sec after trigger time at 2023-11-01 02:28:58 UT, with upper limit up to 18.1 mag. The observations began at zenith distance = 38 deg. The sun altitude is -20.1 deg.\n\nThe galactic latitude b = 37 deg., longitude l = 217 deg.\n\n\nReal time updated cover map and OT discovered available here:\nhttps://master.sai.msu.ru/site/master2/observ.php?id\"93558\n\nWe obtain a following upper limits.\n\nTmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment\n_________|_____________________|_____________________|____________________________________|_____|_______|_______|________\n\n 154 | 2023-11-01 02:25:20 | MASTER-Kislovodsk | (09h 42m 58.56s , +04d 46m 59.7s) | C | 60 | 17.3 |\n 236 | 2023-11-01 02:26:43 | MASTER-Kislovodsk | (08h 52m 53.45s , +12d 25m 15.9s) | C | 60 | 17.3 |\n 317 | 2023-11-01 02:28:03 | MASTER-Kislovodsk | (09h 08m 26.97s , +12d 23m 35.0s) | C | 60 | 17.2 |\n 372 | 2023-11-01 02:28:58 | MASTER-Tavrida | (08h 54m 24.41s , +10d 59m 50.1s) | C | 60 | 17.6 |\n 399 | 2023-11-01 02:29:25 | MASTER-Kislovodsk | (08h 57m 14.59s , +14d 19m 37.3s) | C | 60 | 17.3 |\n 444 | 2023-11-01 02:30:10 | MASTER-Tavrida | (08h 51m 26.54s , +09d 05m 37.5s) | C | 60 | 17.6 |\n 518 | 2023-11-01 02:31:24 | MASTER-Tavrida | (09h 09m 49.90s , +11d 00m 29.9s) | C | 60 | 17.6 |\n 591 | 2023-11-01 02:32:38 | MASTER-Tavrida | (09h 04m 15.19s , +07d 10m 19.4s) | C | 60 | 17.9 |\n 885 | 2023-11-01 02:37:31 | MASTER-Kislovodsk | (08h 49m 13.80s , +10d 31m 19.6s) | C | 60 | 17.2 |\n 966 | 2023-11-01 02:38:53 | MASTER-Kislovodsk | (08h 41m 29.96s , +14d 18m 20.2s) | C | 60 | 17.4 |\n 1046 | 2023-11-01 02:40:13 | MASTER-Kislovodsk | (08h 57m 14.79s , +14d 19m 34.6s) | C | 60 | 17.1 |\n 1112 | 2023-11-01 02:41:18 | MASTER-Tavrida | (08h 54m 26.42s , +10d 58m 53.5s) | C | 60 | 18.1 |\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/34925.",
"published": "2023-11-01T02:46:13.695800Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-11-01T02:46:13.695821Z",
"modified": "2023-11-01T02:46:13.701632Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4301,
"topic": "gcn.circular",
"uuid": "019e12b0-ff32-4085-a409-cebf53f7d517",
"title": "New Swift-BAT/GUANO and IceCube Notices Available via GCN Kafka",
"submitter": "Hop gcn.circular",
"authors": "Judith Racusin at NASA/GSFC <judith.racusin@nasa.gov>",
"data": {
"date": "23/11/01 15:36:15 GMT",
"from": "Judith Racusin at NASA/GSFC <judith.racusin@nasa.gov>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34926"
},
"title": "GCN CIRCULAR",
"number": "34926",
"subject": "New Swift-BAT/GUANO and IceCube Notices Available via GCN Kafka"
},
"message_text": "Swift-BAT/GUANO, IceCube, and GCN teams report:\n\nThe Swift-BAT/GUANO, IceCube, and GCN teams are pleased to announce the availability of new GCN notice types via the new GCN in JSON format. JSON format notices can be streamed via Kafka (https://gcn.nasa.gov/quickstart) These new notice types are not available via GCN Classic.\n\nSwift-BAT/GUANO: gcn.notices.swift.bat.guano (https://gcn.nasa.gov/missions/swift)\n- Summary: GUANO is a ground-based analysis of data from Swift BAT, significantly enhancing the sensitivity and sky area covered as compared to Swift's onboard triggering.\n- Occurence Rate: The Swift/BAT-GUANO notices occur at a rate of 50 times per year.\n- Time Delay: The post-event processing and communication of alert is distributed to GCN within 10 minutes to 5 hours of detection, depending on data downlink method and space-to-ground communications resource availability.\n- Notice Type: The new Swift/BAT-GUANO notice type (gcn.notices.swift.bat.guano) provides timestamps, sky locations, durations, and other supplementary information on gamma-ray transients discovered through this system, to enable prompt follow-up by observers and other instruments. The 'initial' notice distributed for any detection will not include localization information. In the majority of cases later 'update' notices will follow with a localization attached. ~1/4 of GUANO bursts will have arcminute-scale localizations, distributed in the form [RA, Dec, Error] the remainder will be more poorly localized and may be distributed as HEALPix maps.\n\nIceCube LVK Neutrino Track Search:gcn.notices.icecube.lvk_nu_track_search (https://gcn.nasa.gov/missions/icecube)\n- Summary: IceCube is a is a cubic-kilometer Cherenkov particle detector deployed in the Antarctic ice beneath the Amundsen-Scott South Pole Station. IceCube detects neutrinos by observing the light produced by relativistic charged particles created by neutrino interactions in or near the instrumented volume of ice.\n- Occurrence Rate: The LVK Nu Track Search notices are triggered by LIGO/Virgo/KAGRA alerts and occur at the same rate of these alerts, searching for neutrino signals from both significant and low significance LVK alerts.\n- Time Delay: Neutrino searches are performed in a +/- 500 second time window about the LVK alert, and Nu Track search results are generally available within ~1000 seconds of the LVK GW event time.\n- Notice Type: The new LVK Nu Track Search notice type (gcn.notices.icecube.lvk_nu_track_search) provides results from realtime searches for coincident neutrino signals from all LIGO/Virgo/KAGRA gravitational-wave alerts, using a realtime muon neutrino track-like event selection and the sky maps from gravitational wave detectors. Search results will include neutrino directions for observed coincident events with the aim to identify multi-messenger transient sources and seed electromagnetic followup up observations.\n\nNotice Schema and Examples: The JSON schema defining the notice format and examples can be viewed in the Schema Browser (https://gcn.nasa.gov/docs/schema/latest/gcn/notices) or the GCN schema repository (https://github.com/nasa-gcn/gcn-schema).\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34926.",
"published": "2023-11-01T15:36:29.890058Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-11-01T15:36:29.890081Z",
"modified": "2023-11-01T15:36:29.897204Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4309,
"topic": "gcn.circular",
"uuid": "6cb776b9-2adc-4a52-9672-3cb04081959a",
"title": "LIGO/Virgo/KAGRA S231102w: Identification of a GW compact binary merger candidate",
"submitter": "Hop gcn.circular",
"authors": "Gaël Servignat at LUTH <gael.servignat@obspm.fr>",
"data": {
"date": "23/11/02 08:31:34 GMT",
"from": "Gaël Servignat at LUTH <gael.servignat@obspm.fr>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34927"
},
"title": "GCN CIRCULAR",
"number": "34927",
"subject": "LIGO/Virgo/KAGRA S231102w: Identification of a GW compact binary merger candidate"
},
"message_text": "The LIGO Scientific Collaboration, the Virgo Collaboration, and the KAGRA Collaboration report:\n\nWe identified the compact binary merger candidate S231102w during real-time processing of data from LIGO Hanford Observatory (H1) and LIGO Livingston Observatory (L1) at 2023-11-02 07:17:36.371 UTC (GPS time: 1382944674.371). The candidate was found by the CWB [1], GstLAL [2], MBTA [3], PyCBC Live [4], and SPIIR [5] analysis pipelines.\n\nS231102w is an event of interest because its false alarm rate, as estimated by the online analysis, is 5.8e-23 Hz, or about one in 1e15 years. The event's properties can be found at this URL:\n\nhttps://gracedb.ligo.org/superevents/S231102w\n\nThe classification of the GW signal, in order of descending probability, is BBH (>99%), Terrestrial (<1%), BNS (<1%), or NSBH (<1%).\n\nAssuming the candidate is astrophysical in origin, the probability that the lighter compact object is consistent with a neutron star mass (HasNS) is <1%. [6] Using the masses and spins inferred from the signal, the probability of matter outside the final compact object (HasRemnant) is <1%. [6] Both HasNS and HasRemnant consider the support of several neutron star equations of state. The probability that either of the binary components lies between 3 and 5 solar masses (HasMassGap) is <1%.\n\nTwo sky maps are available at this time and can be retrieved from the GraceDB event page:\n * bayestar.multiorder.fits,0, an initial localization generated by BAYESTAR [7], distributed via GCN notice about 27 seconds after the candidate event time.\n * bayestar.multiorder.fits,1, an initial localization generated by BAYESTAR [7], distributed via GCN notice about 5 minutes after the candidate event time.\n\nThe preferred sky map at this time is bayestar.multiorder.fits,1. For the bayestar.multiorder.fits,1 sky map, the 90% credible region is 2555 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 4123 +/- 1317 Mpc (a posteriori mean +/- standard deviation).\n\nFor further information about analysis methodology and the contents of this alert, refer to the LIGO/Virgo/KAGRA Public Alerts User Guide https://emfollow.docs.ligo.org/userguide/.\n\n [1] Klimenko et al. PRD 93, 042004 (2016)\n [2] Tsukada et al. PRD 108, 043004 (2023) and Ewing et al. arXiv:2305.05625 (2023)\n [3] Aubin et al. CQG 38, 095004 (2021)\n [4] Dal Canton et al. ApJ 923, 254 (2021)\n [5] Chu et al. PRD 105, 024023 (2022)\n [6] Chatterjee et al. ApJ 896, 54 (2020)\n [7] Singer & Price PRD 93, 024013 (2016)\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34927.",
"published": "2023-11-02T08:31:45.320674Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-11-02T08:31:45.320703Z",
"modified": "2023-11-02T08:31:45.329047Z",
"nonlocalizedevents": [
{
"event_id": "S231102w"
}
],
"targets": []
},
{
"id": 6328,
"topic": "gcn.circular",
"uuid": "2f7277c8-b472-4d3d-a236-9a73c3b57972",
"title": "GRB 240404A: 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": "24/04/04 02:46:02 GMT",
"from": "Fermi GBM Team at MSFC/Fermi-GBM <do_not_reply@GIOC.nsstc.nasa.gov>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/36020"
},
"title": "GCN CIRCULAR",
"number": "36020",
"subject": "GRB 240404A: Fermi GBM Final Real-time Localization"
},
"message_text": "The Fermi GBM team reports the detection of a likely SHORT GRB\n\nAt 02:38:04 UT on 4 Apr 2024, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 240404A (trigger 733891089.631386 / 240404110).\n\nThe on-ground calculated location, using the Fermi GBM trigger data, is RA = 257.0, Dec = -27.3 (J2000 degrees, equivalent to J2000 17h 07m, -27d 18'), with a statistical uncertainty of 13.3 degrees.\n\nThe angle from the Fermi LAT boresight is 93.0 degrees.\n\nThe skymap can be found here:\nhttps://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240404110/quicklook/glg_skymap_all_bn240404110.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/bn240404110/quicklook/glg_healpix_all_bn240404110.fit\n\nThe GBM light curve can be found here:\nhttps://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2024/bn240404110/quicklook/glg_lc_medres34_bn240404110.gif\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/36020.",
"published": "2024-04-04T02:46:19.972799Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-04-04T02:46:19.972812Z",
"modified": "2024-04-04T02:46:19.978609Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4319,
"topic": "gcn.circular",
"uuid": "a1c2d745-aad8-4cdf-bf32-a145c4cb341b",
"title": "GRB 231101A: Glowbug gamma-ray detection",
"submitter": "Hop gcn.circular",
"authors": "C.C. Cheung at Naval Research Lab <Teddy.Cheung@nrl.navy.mil>",
"data": {
"date": "23/11/02 15:13:39 GMT",
"from": "C.C. Cheung at Naval Research Lab <Teddy.Cheung@nrl.navy.mil>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34929"
},
"title": "GCN CIRCULAR",
"number": "34929",
"subject": "GRB 231101A: Glowbug gamma-ray detection"
},
"message_text": "C.C. Cheung, M. Kerr, J. E. Grove, R. Woolf (NRL), A. Goldstein (USRA), C.A. Wilson-Hodge (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 231101A, which was also detected by Fermi/GBM (GCN 34924).\n \nUsing an adaptive window with a resolution of 32-ms, the burst onset is determined to be 2023-11-01 02:23:14.776 with a duration of about 4 s and a total significance of about 6.4 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 photon index dN/dE~E^x of x=-0.8 and a cutoff energy (\"Epeak\") of 1023 keV. The modeled 10-10000 keV fluence is 4.1e-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/34929.",
"published": "2023-11-02T15:13:53.930411Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-11-02T15:13:53.930442Z",
"modified": "2023-11-02T15:13:53.936311Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4320,
"topic": "gcn.circular",
"uuid": "d68a55ca-18d3-4262-8d10-476a842daec0",
"title": "LIGO/Virgo/KAGRA S231102i: 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": "23/11/02 15:17:08 GMT",
"from": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34930"
},
"title": "GCN CIRCULAR",
"number": "34930",
"subject": "LIGO/Virgo/KAGRA S231102i: 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 LIGO/Virgo/KAGRA S231102i errorbox 38402 sec after notice time and 38635 sec after trigger time at 2023-11-02 14:45:39 UT, with upper limit up to 16.5 mag. The observations began at zenith distance = 13 deg. The sun altitude is -45.9 deg.\n\nThe galactic latitude b = -10 deg., longitude l = 271 deg.\n\n\nReal time updated cover map and OT discovered available here:\nhttps://master.sai.msu.ru/site/master2/ligo_1.php?id\u0017224\n\nWe obtain a following upper limits.\n\nTmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment\n_________|_____________________|_____________________|____________________________________|_____|_______|_______|________\n\n 38665 | 2023-11-02 14:45:39 | MASTER-Tunka | (00h 38m 11.42s , +38d 30m 50.9s) | C | 60 | 16.5 |\n 38744 | 2023-11-02 14:47:05 | MASTER-Tunka | (00h 28m 26.71s , +38d 40m 03.4s) | C | 45 | 14.4 |\n 38815 | 2023-11-02 14:48:16 | MASTER-Tunka | (00h 38m 10.99s , +38d 29m 56.3s) | C | 45 | 15.7 |\n 38816 | 2023-11-02 14:48:16 | MASTER-Tunka | (00h 28m 33.82s , +38d 40m 08.3s) | C | 45 | 14.2 |\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/34930.",
"published": "2023-11-02T15:17:16.349821Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-11-02T15:17:16.349841Z",
"modified": "2023-11-02T15:17:16.355212Z",
"nonlocalizedevents": [
{
"event_id": "S231102i"
}
],
"targets": []
},
{
"id": 6329,
"topic": "gcn.circular",
"uuid": "9f11b616-73be-458f-ab95-78a27480b3f2",
"title": "Fermi GRB 240404A: 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": "24/04/04 03:16:11 GMT",
"from": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/36021"
},
"title": "GCN CIRCULAR",
"number": "36021",
"subject": "Fermi GRB 240404A: 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 240404A ( Fermi GBM team, GCN 36020) errorbox 1191 sec after notice time and 1229 sec after trigger time at 2024-04-04 02:58:34 UT, with upper limit up to 18.5 mag. The observations began at zenith distance = 10 deg. The sun altitude is -24.8 deg.\n\nThe galactic latitude b = 7 deg., longitude l = 357 deg.\n\n\nReal time updated cover map and OT discovered available here:\nhttps://master.sai.msu.ru/site/master2/observ.php?id$14151\n\nWe obtain a following upper limits.\n\nTmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment\n_________|_____________________|_____________________|____________________________________|_____|_______|_______|________\n\n 1260 | 2024-04-04 02:58:34 | MASTER-SAAO | (16h 31m 03.20s , -27d 28m 14.7s) | C | 60 | 18.5 |\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/36021.",
"published": "2024-04-04T03:16:29.687767Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-04-04T03:16:29.687790Z",
"modified": "2024-04-04T03:16:29.695375Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4602,
"topic": "gcn.circular",
"uuid": "899748af-3cc2-4383-b6db-a94e7b5c9e6e",
"title": "GRB 231110A: Glowbug gamma-ray detection",
"submitter": "Hop gcn.circular",
"authors": "C.C. Cheung at Naval Research Lab <Teddy.Cheung@nrl.navy.mil>",
"data": {
"date": "23/11/13 02:43:32 GMT",
"from": "C.C. Cheung at Naval Research Lab <Teddy.Cheung@nrl.navy.mil>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/35006"
},
"title": "GCN CIRCULAR",
"number": "35006",
"subject": "GRB 231110A: Glowbug gamma-ray detection"
},
"message_text": "C.C. Cheung, M. Kerr, J. E. Grove, R. Woolf (NRL), A. Goldstein (USRA), C.A. Wilson-Hodge (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 231110A, which was also detected by Swift/BAT, GECAM-B, and AstroSat/CZTI (GCN 34977, 34992, 35005). \n\nUsing an adaptive window with a resolution of 32-ms, the burst onset is determined to be 2023-11-10 21:19:32.008 with a duration of 8.2 s and a total significance of about 38 sigma. The light curve comprises the single peak observed by Swift/BAT, GECAM-B, and AstroSat/CZTI.\n\nUsing a standard power-law function with an exponential high-energy cutoff [3] to model the emission over this duration results in a photon index dN/dE~E^x of x=1.2 and a cutoff energy (\"Epeak\") of 271 keV. The modeled 10-10000 keV fluence is 2.4e-06 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/35006.",
"published": "2023-11-13T02:43:42.562067Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-11-13T02:43:42.562085Z",
"modified": "2023-11-13T02:43:42.567813Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4330,
"topic": "gcn.circular",
"uuid": "cdd7803d-65ba-4420-ae92-96807c54d406",
"title": "LIGO/Virgo/KAGRA S231102w: Updated Sky localization",
"submitter": "Hop gcn.circular",
"authors": "Charlie Hoy at University of Portsmouth <charlie.hoy@port.ac.uk>",
"data": {
"date": "23/11/03 01:01:38 GMT",
"from": "Charlie Hoy at University of Portsmouth <charlie.hoy@port.ac.uk>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34931"
},
"title": "GCN CIRCULAR",
"number": "34931",
"subject": "LIGO/Virgo/KAGRA S231102w: Updated Sky localization"
},
"message_text": "The LIGO Scientific Collaboration, the Virgo Collaboration, and the KAGRA Collaboration report:\n\nWe have conducted further analysis of the LIGO Hanford Observatory (H1) and LIGO Livingston Observatory (L1) data around the time of the compact binary merger (CBC) candidate S231102w (GCN Circular 34927). Parameter estimation has been performed using Bilby [1] and a new sky map, Bilby.multiorder.fits, distributed via GCN Notice, is available for retrieval from the GraceDB event page:\n\nhttps://gracedb.ligo.org/superevents/S231102w\n\nFor the Bilby.multiorder.fits sky map, the 90% credible region is 2343 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 3493 +/- 1015 Mpc (a posteriori mean +/- standard deviation).\n\nFor further information about analysis methodology and the contents of this alert, refer to the LIGO/Virgo/KAGRA Public Alerts User Guide https://emfollow.docs.ligo.org/userguide/.\n\n [1] Ashton et al. ApJS 241, 27 (2019) and Morisaki et al. arXiv:2307.13380 (2023)\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34931.",
"published": "2023-11-03T01:01:49.181901Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-11-03T01:01:49.181936Z",
"modified": "2023-11-03T01:01:49.188023Z",
"nonlocalizedevents": [
{
"event_id": "S231102w"
}
],
"targets": []
},
{
"id": 4331,
"topic": "gcn.circular",
"uuid": "1bfd772c-8f57-406a-b44e-9cd29ae60b83",
"title": "Fermi-LAT gamma-ray observations of IceCube-231027A",
"submitter": "Hop gcn.circular",
"authors": "Sara Buson at GSFC/Fermi <sara.buson@gmail.com>",
"data": {
"date": "23/11/03 09:05:01 GMT",
"from": "Sara Buson at GSFC/Fermi <sara.buson@gmail.com>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34932"
},
"title": "GCN CIRCULAR",
"number": "34932",
"subject": "Fermi-LAT gamma-ray observations of IceCube-231027A"
},
"message_text": "S. Buson (Uni Wuerzburg), S. Garrappa (Weizmann Institute of Science), C. Bartolini (INFN Bari) and J. Sinapius (DESY) on behalf of the Fermi-LAT collaboration:\nWe report an analysis of observations of the vicinity of the IC231027A high-energy neutrino event (GCN 34891) 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 2023-10-27 at 04:16:10.44 UT (T0) with J2000 position RA = 267.16 (+3.35, -3.40) deg, Decl. = +46.96 (+2.25, -2.88) deg (90% PSF containment). According to the fourth Fermi LAT source catalog (4FGL-DR4), there are eight 4FGL-DR4 cataloged gamma-ray (>100 MeV; The Fermi-LAT collaboration 2022, ApJS, 260, 53) sources in the 90% IC231027A uncertainty localization region. \nWe searched for intermediate (days to years) timescale emission from a new gamma-ray source. Preliminary analysis indicates no significant (> 5 sigma) new excess emission (> 100 MeV) at the IC231027A best-fit position. Assuming a power-law spectrum (photon index = 2.0 fixed) for a point source at the IC231027A best-fit position, the >100 MeV flux upper limit (95% confidence) is < 7.0e-10 ph cm^-2 s^-1 for ~15-years (2008-08-04 to 2023-10-27 UTC), and < 5.2e-9 (< 1.4e-7) ph cm^-2 s^-1 for a 1-month (1-day) integration time before T0.\nThe gamma-ray source nearest to the best-fit position of IC231027A is the blazar 4FGL J1747.9+4704 (a.k.a. B3 1746+470, 5BZB J1747+4658), at a 0.16deg separation. Close to the neutrino-event best-fit position, at 0.29deg separation, there is also the unassociated gamma-ray source 4FGL J1749.6+4716. Preliminary analysis indicates that these gamma-ray sources are ongoing a prolonged, enhanced activity state. The year-binned gamma-ray light curves show that they entered the high state in 2021. During the last year, i.e. 1-year integration time before T0, the observed flux (E>100 MeV) of 4FGL J1747.9+4704 is (1.2 +/- 0.3) x 10^-9 photons cm^-2 s^-1 (statistical uncertainty only), more than three times greater than the average flux reported in the 4FGL-DR4; the flux (E>100 MeV) observed for 4FGL J1749.6+4716 during this same period is of (2.3 +/- 0.3) x 10^-8 photons cm^-2 s^-1 (statistical uncertainty only), more than ten times greater than the 4FGL-DR4 average flux. We encourage multiwavelength observations of these sources. \nWe performed an analysis of the region selecting only the LAT higher energy events (>1GeV) in order to achieve an improved localisation of the unassociated source 4FGL J1749.6+4716, and obtain as best-fit position RA = 267.3962, Decl. = 47.3276 (0.04 deg 68% containment, 0.07 deg 95% containment). A plausible association is the flat-spectrum radio source B3 1748+473 (GB6 B1748+4720), located 0.01deg away from the best-fit position.\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 are S. Buson (sara.buson at uni-wuerzburg.de <http://uni-wuerzburg.de/>), S. Garrappa (simone.garrappa at weizmann.ac.il <http://weizmann.ac.il/>), J. Sinapius (jonas.sinapius at desy.de <http://desy.de/>), C. Bartolini (chiara.bartolini at ba.infn.it <http://ba.infn.it/>).\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\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34932.",
"published": "2023-11-03T09:05:11.655580Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-11-03T09:05:11.655599Z",
"modified": "2023-11-03T09:05:11.662364Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4333,
"topic": "gcn.circular",
"uuid": "4ef2f83b-b1c5-4001-bd99-a8785c79d897",
"title": "IceCube-231103A - IceCube observation of a high-energy neutrino candidate track-like event",
"submitter": "Hop gcn.circular",
"authors": "Erik Blaufuss at University of Maryland, College Park <blaufuss@umd.edu>",
"data": {
"date": "23/11/03 14:13:16 GMT",
"from": "Erik Blaufuss at University of Maryland, College Park <blaufuss@umd.edu>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34933"
},
"title": "GCN CIRCULAR",
"number": "34933",
"subject": "IceCube-231103A - IceCube observation of a high-energy neutrino candidate track-like event"
},
"message_text": "The IceCube Collaboration (http://icecube.wisc.edu/) reports:\n\nOn 23-11-03 at 09:17:35.29 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 0.1472 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/138515_8773328.amon) more sophisticated reconstruction algorithms have been applied offline, with the direction refined to:\n\nDate: 23-11-03\nTime: 09:17:35.29 UT\nRA: 105.67 (+3.15 / -2.94 deg 90% PSF containment) J2000\nDec: +47.85 (+ 1.95 / -1.78 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\nSeveral Fermi 4FGL-DR4 sources are located in the 90% uncertainty region of the event. The closest source is 4FGL J0708.9+4839 at RA = 107.25 deg, Dec = +48.66 located 1.32 deg away from the best fit 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\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34933.",
"published": "2023-11-03T14:13:28.319015Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-11-03T14:13:28.319034Z",
"modified": "2023-11-03T14:13:28.324878Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4337,
"topic": "gcn.circular",
"uuid": "61b85641-2675-4c91-b974-3bda878884ec",
"title": "GRB 231103A: 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": "23/11/03 14:52:04 GMT",
"from": "Fermi GBM Team at MSFC/Fermi-GBM <do_not_reply@GIOC.nsstc.nasa.gov>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34934"
},
"title": "GCN CIRCULAR",
"number": "34934",
"subject": "GRB 231103A: Fermi GBM Final Real-time Localization"
},
"message_text": "The Fermi GBM team reports the detection of a likely LONG GRB\n\nAt 14:41:30 UT on 3 Nov 2023, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 231103A (trigger 720715295.24961 / 231103612).\n\nThe on-ground calculated location, using the Fermi GBM trigger data, is RA = 14.0, Dec = -55.3 (J2000 degrees, equivalent to J2000 00h 56m, -55d 17'), with a statistical uncertainty of 5.2 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/2023/bn231103612/quicklook/glg_skymap_all_bn231103612.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/2023/bn231103612/quicklook/glg_healpix_all_bn231103612.fit\n\nThe GBM light curve can be found here:\nhttps://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn231103612/quicklook/glg_lc_medres34_bn231103612.gif\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34934.",
"published": "2023-11-03T14:52:19.299781Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-11-03T14:52:19.299814Z",
"modified": "2023-11-03T14:52:19.306028Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4338,
"topic": "gcn.circular",
"uuid": "6f3049ba-50cf-439d-a22a-ef22a0886394",
"title": "IceCube Alert 231103.39: 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": "23/11/03 16:40:11 GMT",
"from": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34935"
},
"title": "GCN CIRCULAR",
"number": "34935",
"subject": "IceCube Alert 231103.39: 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 IceCube Alert 231103.39 (trigger No 8773328,06h 57m 00.48s , +46d 34m 51.6s, R=1.08) errorbox 25857 sec after notice time and 25909 sec after trigger time at 2023-11-03 16:29:24 UT, with upper limit up to 18.0 mag. The observations began at zenith distance = 31 deg. The sun altitude is -51.8 deg.\n\nThe galactic latitude b = 21 deg., longitude l = 170 deg.\n\n\nReal time updated cover map and OT discovered available here:\nhttps://master.sai.msu.ru/site/master2/observ.php?id\"94588\n\nWe obtain a following upper limits.\n\nTmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment\n_________|_____________________|_____________________|____________________________________|_____|_______|_______|________\n\n 25999 | 2023-11-03 16:29:24 | MASTER-Amur | (07h 01m 07.02s , +47d 50m 23.7s) | C | 180 | 18.0 |\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/34935.",
"published": "2023-11-03T16:40:22.483063Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-11-03T16:40:22.483081Z",
"modified": "2023-11-03T16:40:22.490489Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4343,
"topic": "gcn.circular",
"uuid": "199ad46d-f390-4cd5-8159-b2b2818eb6cb",
"title": "Swift GRB231104.07: 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": "23/11/04 01:57:24 GMT",
"from": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34936"
},
"title": "GCN CIRCULAR",
"number": "34936",
"subject": "Swift GRB231104.07: 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) was pointed to the Swift GRB231104.07 (trigger No 1194500,01h 35m 09.36s , +83d 47m 27.6s, R=0.05) errorbox 15 sec after notice time and 35 sec after trigger time at 2023-11-04 01:48:15 UT, with upper limit up to 14.7 mag. The observations began at zenith distance = 45 deg. The sun altitude is -28.0 deg.\n\nThe galactic latitude b = 21 deg., longitude l = 124 deg.\n\n\nReal time updated cover map and OT discovered available here:\nhttps://master.sai.msu.ru/site/master2/observ.php?id\"94743\n\nWe obtain a following upper limits.\n\nTmid-T0 | Site |Filt.| Expt. | Limit| Comment\n_________|_____________________|_____|_______|______|________\n\n 40 | MASTER-Tavrida | C | 10 | 13.8 |\n 57 | MASTER-Tavrida | C | 10 | 13.8 |\n 75 | MASTER-Tavrida | C | 10 | 13.9 |\n 98 | MASTER-Tavrida | C | 20 | 14.5 |\n 125 | MASTER-Tavrida | C | 20 | 14.3 |\n 157 | MASTER-Tavrida | C | 30 | 14.6 |\n 200 | MASTER-Tavrida | C | 40 | 14.7 |\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/34936.",
"published": "2023-11-04T01:57:35.743093Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-11-04T01:57:35.743116Z",
"modified": "2023-11-04T01:57:35.751110Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6332,
"topic": "gcn.circular",
"uuid": "dd989362-dda2-4ba9-ae90-a90b3d86793d",
"title": "LXT 240402A: 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": "24/04/04 09:00:26 GMT",
"from": "EP Team at NAOC/CAS <ep_ta@bao.ac.cn>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/36022"
},
"title": "GCN CIRCULAR",
"number": "36022",
"subject": "LXT 240402A: EP-FXT detection of the X-ray afterglow"
},
"message_text": "S. M. Jia (IHEP, CAS), H. Sun (NAOC, CAS), C. K. Li, Y. Chen, W. W. Cui, H. Feng, J. Guan, D. W. Han, W. Li, C. Z. Liu, F. J. Lu, L. M. Song, J. Wang, J. J. Xu, J. Zhang, S. N. Zhang, H. S. Zhao, X. F. Zhao, (IHEP, CAS), E. Kuulkers, A. Santovincenzo (ESA), P. O'Brien (Univ. of Leicester), K. Nandra, A. Rau (MPE), B. Cordier (CEA), X. F. Wu (PMO, CAS), X. P. Xu, Z. X. Ling , Y. Liu , C. Zhang , C. C. Jin , J. W. Hu , D. Y. Li , H. Y. Liu , H. W. Pan , W. Yuan (NAOC, CAS), on behalf of the LEIA and Einstein Probe team\n\n\nFollowing the detection of the fast X-ray transient LXT 240402A (Xu et al., GCN 36016) and the associated GRB 240402B (Wang et al., GCN 36017), we performed observations of LXT 240402A with the Follow-up X-ray Telescope (FXT) on board Einstein Probe (EP). The observations began at 2024-04-03T19:45:00, about 35 hours after the LEIA detection. The exposure time was 12 ks. An X-ray source was detected at R.A. = 245.451 deg, DEC = 25.763 deg, with an uncertainty of 10 arcsec (radius, 90% C.L. statistical and systematic), 2.4 arcmin away from the LEIA source.\n\nThere is no cataloged X-ray source within the error circle, consistent with this source being the afterglow of LXT240402A. The spectrum can be fitted with an absorbed power-law model with NH fixed at the Galactic value of 4.3e20 cm-2 and a photon index of 1.7(+/-0.1) (90% C.L.). The derived flux in 0.5-10 keV is 7.8(+/-0.8)e-13 erg/s/cm2 (90% C.L.). Further monitoring of this source with FXT is planned for 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/36022.",
"published": "2024-04-04T09:00:43.076707Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-04-04T09:00:43.076725Z",
"modified": "2024-04-04T09:00:43.084423Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4344,
"topic": "gcn.circular",
"uuid": "01f4d9c2-26de-4f50-a6a3-8a0b05faa82c",
"title": "GRB 231104A: 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": "23/11/04 01:57:53 GMT",
"from": "Fermi GBM Team at MSFC/Fermi-GBM <do_not_reply@GIOC.nsstc.nasa.gov>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34937"
},
"title": "GCN CIRCULAR",
"number": "34937",
"subject": "GRB 231104A: Fermi GBM Final Real-time Localization"
},
"message_text": "The Fermi GBM team reports the detection of a likely LONG GRB\n\nAt 01:47:28 UT on 4 Nov 2023, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 231104A (trigger 720755253.13875 / 231104075).\n\nThe on-ground calculated location, using the Fermi GBM trigger data, is RA = 8.0, Dec = 82.1 (J2000 degrees, equivalent to J2000 00h 32m, 82d 05'), with a statistical uncertainty of 1.0 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/2023/bn231104075/quicklook/glg_skymap_all_bn231104075.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/2023/bn231104075/quicklook/glg_healpix_all_bn231104075.fit\n\nThe GBM light curve can be found here:\nhttps://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn231104075/quicklook/glg_lc_medres34_bn231104075.gif\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34937.",
"published": "2023-11-04T01:57:58.797507Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-11-04T01:57:58.797525Z",
"modified": "2023-11-04T01:57:58.803403Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4345,
"topic": "gcn.circular",
"uuid": "cbb0e822-7686-4e08-a634-f948517934bc",
"title": "GRB 231104A: Swift detection of a bright burst",
"submitter": "Hop gcn.circular",
"authors": "David Palmer at LANL <palmer@lanl.gov>",
"data": {
"date": "23/11/04 02:34:58 GMT",
"from": "David Palmer at LANL <palmer@lanl.gov>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34938"
},
"title": "GCN CIRCULAR",
"number": "34938",
"subject": "GRB 231104A: Swift detection of a bright burst"
},
"message_text": "\nK. L. Page (U Leicester), J.D. Gropp (PSU), D. M. Palmer (LANL) and\nM. H. Siegel (PSU) report on behalf of the Neil Gehrels Swift\nObservatory Team:\n\nAt 01:47:39 UT, the Swift Burst Alert Telescope (BAT) triggered and\nlocated GRB 231104A (trigger\u001194500). Swift slewed immediately to the burst.\nThe BAT on-board calculated location is\nRA, Dec 23.789, +83.791 which is\n RA(J2000) = 01h 35m 09s\n Dec(J2000) = +83d 47' 27\"\nwith an uncertainty of 3 arcmin (radius, 90% containment, including\nsystematic uncertainty). The available BAT light curve (up to T+8s)\nshowed a complex structure with a duration of at least 12 sec.\nThe peak count rate was ~50,000 counts/sec (15-350 keV),\nat ~0 sec after the trigger.\n\nThe XRT began observing the field at 01:49:10 UT, 90.2 seconds after\nthe BAT trigger. Using promptly downlinked data we find an\nuncatalogued X-ray source with an enhanced position: RA, Dec 23.8113,\n83.7912 which is equivalent to:\n RA(J2000) = 01h 35m 14.7s\n Dec(J2000) = +83d 47' 28\"\nwith an uncertainty of 3.8 arcseconds (radius, 90% containment). This\nlocation is 9 arcseconds from the BAT onboard position. This position\nmay be improved as more data are received; the latest position is\navailable at https://www.swift.ac.uk/sper.\n\nUVOT took a finding chart exposure of 150 seconds with the White filter\nstarting 860 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 25% of\nthe BAT 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\nBAT 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\n0.157.\n\nBurst Advocate for this burst is K. L. Page (klp5 AT leicester.ac.uk).\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/34938.",
"published": "2023-11-04T02:35:09.849663Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-11-04T02:35:09.849682Z",
"modified": "2023-11-04T02:35:09.857018Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4346,
"topic": "gcn.circular",
"uuid": "7aa153b7-c73e-4645-a59f-c59c2ceed5ea",
"title": "GRB231104A: LCOGT Optical Upper Limits",
"submitter": "Hop gcn.circular",
"authors": "Robert Strausbaugh at Eastern Illinois University <rstrausbaugh@eiu.edu>",
"data": {
"date": "23/11/04 04:09:15 GMT",
"from": "Robert Strausbaugh at Eastern Illinois University <rstrausbaugh@eiu.edu>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34939"
},
"title": "GCN CIRCULAR",
"number": "34939",
"subject": "GRB231104A: LCOGT Optical Upper Limits"
},
"message_text": "R. Strausbaugh (Eastern Illinois University), A. Cucchiara (NASA) report on behalf of a larger collaboration:\n\nWe observed the Fermi GRB 231104A field (Fermi GBM team, GCN 34937) with the LCOGT 1-meter Sinistro instrument at the McDonald Observatory, USA site, on November 4, from 02:53 to 03:25 UT (corresponding to 1.10 to 1.63 hours from the GRB trigger time) with the SDSS r and i filters.\n\nWe performed a series of 3x300s exposures in each band. We do not detect a source within the Swift-XRT error region around the candidate X-ray source (Page et al., GCN 34938) in either band.\n\nThe following 5-sigma upper limits are calculated using the PanSTARRS catalog as reference:\n\nr > 22.6\ni > 21.8\n\nThese magnitudes are not corrected for galactic extinction.\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34939.",
"published": "2023-11-04T04:09:27.240358Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-11-04T04:09:27.240378Z",
"modified": "2023-11-04T04:09:27.248290Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4353,
"topic": "gcn.circular",
"uuid": "8c1c9670-6f33-47f4-ab82-d17b8ecf50a6",
"title": "GRB 231104A: Enhanced Swift-XRT position",
"submitter": "Hop gcn.circular",
"authors": "Phil Evans at U of Leicester <pae9@star.le.ac.uk>",
"data": {
"date": "23/11/04 08:03:51 GMT",
"from": "Phil Evans at U of Leicester <pae9@star.le.ac.uk>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34940"
},
"title": "GCN CIRCULAR",
"number": "34940",
"subject": "GRB 231104A: 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 1654 s of XRT Photon Counting mode data and 2 UVOT\nimages for GRB 231104A, 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 = 23.80633, +83.79348 which is equivalent\nto:\n\nRA (J2000): 01h 35m 13.52s\nDec (J2000): +83d 47' 36.5\"\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/34940.",
"published": "2023-11-04T08:04:02.139111Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-11-04T08:04:02.139145Z",
"modified": "2023-11-04T08:04:02.145734Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4370,
"topic": "gcn.circular",
"uuid": "c7d74c43-ce14-4bb7-a825-eb7165b59550",
"title": "GRB 231104A: AKO Upper Limit",
"submitter": "Hop gcn.circular",
"authors": "Mohammad Odeh at Al Khatim Observatory M44 <mshodeh@gmail.com>",
"data": {
"date": "23/11/04 19:20:58 GMT",
"from": "Mohammad Odeh at Al Khatim Observatory M44 <mshodeh@gmail.com>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34946"
},
"title": "GCN CIRCULAR",
"number": "34946",
"subject": "GRB 231104A: 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 Fermi GRB 231104A field (Fermi GBM team, GCN 34937) with\nwith our 0.36m f/7.7 robotic telescope on November 4, from 17:12 to 18:22\nUT (corresponding to 16.6 hours from the GRB trigger time) using (Ic)\nfilter. We obtained 24x180 second images.\n\nWe do not detect a source within the Swift-XRT error region around the\ncandidate X-ray source (Page et al., GCN 34938).\n\nThe following 5-sigma upper limit is calculated using the ATLAS catalog as\nreference:\nIc = 19.7\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34946.",
"published": "2023-11-04T19:21:08.974341Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-11-04T19:21:08.974375Z",
"modified": "2023-11-04T19:21:08.982232Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4360,
"topic": "gcn.circular",
"uuid": "28d1f9ec-e384-475d-834f-2cef61c27d54",
"title": "GRB 231104A: Swift/UVOT Upper Limits",
"submitter": "Hop gcn.circular",
"authors": "Paul Kuin at MSSL <npkuin@gmail.com>",
"data": {
"date": "23/11/04 12:44:11 GMT",
"from": "Paul Kuin at MSSL <npkuin@gmail.com>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34941"
},
"title": "GCN CIRCULAR",
"number": "34941",
"subject": "GRB 231104A: Swift/UVOT Upper Limits"
},
"message_text": "N. P. M. Kuin (UCL/MSSL) and K. L. Page (U. Leicester) report on behalf\nof the Swift/UVOT team:\n\nThe Swift/UVOT began settled observations of the field of GRB 231104A\n91 s after the BAT trigger (Page et al., GCN Circ. 34940). No optical\nafterglow consistent with the XRT position (Goad et al., GCN Circ. 34940)\nis detected in the initial UVOT exposures.\nPreliminary 3-sigma upper limits using the UVOT photometric system\n(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first\nfinding chart (FC) exposure and subsequent exposures are:\n\nFilter T_start(s) T_stop(s) Exp(s) Mag\n\nwhite_FC 91 241 147 >21.7\nu_FC 304 553 246 >20.7\nwhite 91 1709 411 >21.8\nv 633 1758 117 >19.3\nb 559 1684 117 >20.4\nu 304 1659 343 >20.9\nw1 683 1808 117 >19.7\nm2 659 679 20 >18.6\n\nThe magnitudes in the table are not corrected for the Galactic extinction\ndue to the reddening of E(B-V) = 0.156 in the direction of the burst\n(Schlegel et al. 1998).\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34941.",
"published": "2023-11-04T12:44:21.462787Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-11-04T12:44:21.462819Z",
"modified": "2023-11-04T12:44:21.472058Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4364,
"topic": "gcn.circular",
"uuid": "6267837d-d7c6-4868-993d-0e90ca7ad00f",
"title": "LIGO/Virgo/KAGRA S231104ac: Identification of a GW compact binary merger candidate",
"submitter": "Hop gcn.circular",
"authors": "massimo.lenti@fi.infn.it",
"data": {
"date": "23/11/04 14:53:03 GMT",
"from": "massimo.lenti@fi.infn.it",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34942"
},
"title": "GCN CIRCULAR",
"number": "34942",
"subject": "LIGO/Virgo/KAGRA S231104ac: Identification of a GW compact binary merger candidate"
},
"message_text": "The LIGO Scientific Collaboration, the Virgo Collaboration, and the KAGRA Collaboration report:\n\nWe identified the compact binary merger candidate S231104ac during real-time processing of data from LIGO Hanford Observatory (H1) and LIGO Livingston Observatory (L1) at 2023-11-04 13:34:18.945 UTC (GPS time: 1383140076.945). The candidate was found by the GstLAL [1], PyCBC Live [2], and SPIIR [3] analysis pipelines.\n\nS231104ac is an event of interest because its false alarm rate, as estimated by the online analysis, is 3.2e-10 Hz, or about one in 1e2 years. The event's properties can be found at this URL:\n\nhttps://gracedb.ligo.org/superevents/S231104ac\n\nThe classification of the GW signal, in order of descending probability, is BBH (>99%), NSBH (<1%), Terrestrial (<1%), or BNS (<1%).\n\nAssuming the candidate is astrophysical in origin, the probability that the lighter compact object is consistent with a neutron star mass (HasNS) is <1%. [4] Using the masses and spins inferred from the signal, the probability of matter outside the final compact object (HasRemnant) is <1%. [4] Both HasNS and HasRemnant consider the support of several neutron star equations of state. The probability that either of the binary components lies between 3 and 5 solar masses (HasMassGap) is <1%.\n\nTwo sky maps are available at this time and can be retrieved from the GraceDB event page:\n * bayestar.multiorder.fits,1, an initial localization generated by BAYESTAR [5], distributed via GCN notice about 29 seconds after the candidate event time.\n * bayestar.multiorder.fits,2, an initial localization generated by BAYESTAR [5], distributed via GCN notice about 5 minutes after the candidate event time.\n\nThe preferred sky map at this time is bayestar.multiorder.fits,2. For the bayestar.multiorder.fits,2 sky map, the 90% credible region is 922 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 1388 +/- 369 Mpc (a posteriori mean +/- standard deviation).\n\nFor further information about analysis methodology and the contents of this alert, refer to the LIGO/Virgo/KAGRA Public Alerts User Guide https://emfollow.docs.ligo.org/userguide/.\n\n [1] Tsukada et al. PRD 108, 043004 (2023) and Ewing et al. arXiv:2305.05625 (2023)\n [2] Dal Canton et al. ApJ 923, 254 (2021)\n [3] Chu et al. PRD 105, 024023 (2022)\n [4] Chatterjee et al. ApJ 896, 54 (2020)\n [5] Singer & Price PRD 93, 024013 (2016)\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34942.",
"published": "2023-11-04T14:53:18.737547Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-11-04T14:53:18.737566Z",
"modified": "2023-11-04T14:53:18.743019Z",
"nonlocalizedevents": [
{
"event_id": "S231104a"
}
],
"targets": []
},
{
"id": 6337,
"topic": "gcn.circular",
"uuid": "668d3c9b-4801-4afc-a96f-e98ae7b872a2",
"title": "X-ray transient LXT240402A: AST3-3 optical upper limits",
"submitter": "Hop gcn.circular",
"authors": "Tianrui Sun at Purple Mountain Obs,CAS <trsun@pmo.ac.cn>",
"data": {
"date": "24/04/04 13:02:10 GMT",
"from": "Tianrui Sun at Purple Mountain Obs,CAS <trsun@pmo.ac.cn>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/36023"
},
"title": "GCN CIRCULAR",
"number": "36023",
"subject": "X-ray transient LXT240402A: AST3-3 optical upper limits"
},
"message_text": "Following the detection of LXT 240402A by Leia (Xu et al. GCN 36016) and FXT on board âEinstein Probe (Jia et al. GCN 36022) ,\nwe use Antarctic Survey Telescope 3-3 at YaoAn Astronomy Observation Station (China, Yunnan) for follow-up.\nOur observation started on 2024-04-03T16:28:21.084 . \nNo new optical source was detected within the error box (Jia et al. GCN 36022) down to 22.1 mag in the coadd image (total 60x180s, g-band).\n\nOur non-detection is consistent with the results from the GWAC-F50A (Xin et al., GCN 36018), MASTER (Lipunov et al. GCN 36019) limits.\n\nWe thank the staff at YaoAn Astronomy Observation Station for their excellent support.\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/36023.",
"published": "2024-04-04T13:02:26.017789Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-04-04T13:02:26.017803Z",
"modified": "2024-04-04T13:02:26.025374Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4365,
"topic": "gcn.circular",
"uuid": "58decf7c-e42d-41e1-b8b4-a2da5050c527",
"title": "GRB 231104A: Fermi-LAT detection",
"submitter": "Hop gcn.circular",
"authors": "N. Di Lalla at Stanford University <niccolo.dilalla@stanford.edu>",
"data": {
"date": "23/11/04 16:29:52 GMT",
"from": "N. Di Lalla at Stanford University <niccolo.dilalla@stanford.edu>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34943"
},
"title": "GCN CIRCULAR",
"number": "34943",
"subject": "GRB 231104A: Fermi-LAT detection"
},
"message_text": "G. Principe (University of Trieste), F. Longo (University of Trieste), N. Di Lalla (Stanford University), D. Tak (Seoul National University) report on behalf of the Fermi-LAT Collaboration:\n\nAt 01:47:28 on November 04, 2023 Fermi-LAT detected high-energy emission from GRB 231104A, which was also detected by Fermi-GBM (trigger 720755253.13875 / 231104075, GCN 34937) and Swift (GCN 34938).\n\nThe best LAT on-ground location is found to be\n\nRA, Dec = 24.1, 84.0 (degrees, J2000)\n\nwith an error radius of 0.7 deg (90 % containment, statistical error only). This was 29 deg from the LAT boresight at the time of the trigger.\n\nThe data from the Fermi-LAT show a significant increase in the event rate that is spatially and temporally correlated with the trigger with high significance. The 100 MeV - 1 GeV photon flux in the time interval 0-400 s after the GBM trigger is (6.6 ± 2.2) E-06 ph/cm2/s.\n\nThe estimated integrated photon index above 100 MeV is -2.7 +/- 0.5. The highest-energy photon is a 530 MeV event which is observed 120 seconds after the GBM trigger.\n\nThe Fermi-LAT point of contact for this burst is Giacomo Principe (giacomo.principe@ts.infn.it).\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\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34943.",
"published": "2023-11-04T16:30:02.729005Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-11-04T16:30:02.729026Z",
"modified": "2023-11-04T16:30:02.736321Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4366,
"topic": "gcn.circular",
"uuid": "83f52b8c-48a3-4372-a45d-648e51446ec0",
"title": "GRB 231104A: Swift-XRT refined Analysis",
"submitter": "Hop gcn.circular",
"authors": "Phil Evans at U of Leicester <pae9@star.le.ac.uk>",
"data": {
"date": "23/11/04 16:55:30 GMT",
"from": "Phil Evans at U of Leicester <pae9@star.le.ac.uk>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34944"
},
"title": "GCN CIRCULAR",
"number": "34944",
"subject": "GRB 231104A: Swift-XRT refined Analysis"
},
"message_text": "J.A. Kennea (PSU), K.L. Page (U. Leicester), A.P. Beardmore (U.\nLeicester), M. Capalbi (INAF-IASFPA), M. Perri (SSDC & INAF-OAR), V.\nD'Elia (SSDC & INAF-OAR), A. Tohuvavohu (U. Toronto), D.N. Burrows\n(PSU) and P.A. Evans report on behalf of the Swift-XRT team:\n\nWe have analysed 6.6 ks of XRT data for GRB 231104A, from 72 s to 34.5\nks after the BAT trigger. The data comprise 62 s in Windowed Timing\n(WT) mode (the first 9 s were taken while Swift was slewing) with the\nremainder in Photon Counting (PC) mode.\n\nThe late-time light curve (from T0+10.9 ks) can be modelled with a\npower-law decay with a decay index of alpha=1.08 (+/-0.22).\n\nA spectrum formed from the PC mode data can be fitted with an absorbed\npower-law with a photon spectral index of 1.93 (+0.28, -0.27). The\nbest-fitting absorption column is 7.9 (+1.1, -1.0) x 10^22 cm^-2, in\nexcess of the Galactic value of 1.3 x 10^21 cm^-2 (Willingale et al.\n2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion\nfactor deduced from this spectrum is 9.9 x 10^-11 (3.0 x 10^-10) erg\ncm^-2 count^-1.\n\nA summary of the PC-mode spectrum is thus:\nTotal column:\t 7.9 (+1.1, -1.0) x 10^22 cm^-2\nGalactic foreground: 1.3 x 10^21 cm^-2\nExcess significance: 12.5 sigma\nPhoton index:\t 1.93 (+0.28, -0.27)\n\nIf the light curve continues to decay with a power-law decay index of\n1.08, the count rate at T+24 hours will be 0.017 count s^-1,\ncorresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.7 x\n10^-12 (5.0 x 10^-12) erg cm^-2 s^-1.\n\nThe results of the XRT-team automatic analysis are available at\nhttp://www.swift.ac.uk/xrt_products/01194500.\n\nThis circular is an official product of the Swift-XRT team.\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34944.",
"published": "2023-11-04T16:55:41.262118Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-11-04T16:55:41.262137Z",
"modified": "2023-11-04T16:55:41.268424Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4367,
"topic": "gcn.circular",
"uuid": "93e5e352-24fe-418e-9ce5-d0a7064ada38",
"title": "GRB 231104A: AstroSat CZTI detection",
"submitter": "Hop gcn.circular",
"authors": "Gaurav Waratkar at IIT Bombay <gauravwaratkar@iitb.ac.in>",
"data": {
"date": "23/11/04 17:12:40 GMT",
"from": "Gaurav Waratkar at IIT Bombay <gauravwaratkar@iitb.ac.in>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34945"
},
"title": "GCN CIRCULAR",
"number": "34945",
"subject": "GRB 231104A: AstroSat CZTI detection"
},
"message_text": "P. K. Navaneeth (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 bright long-duration GRB 231104A which was also detected by Fermi-GBM (Fermi GBM Team, GCN Circ. 34937), and Swift-BAT (Page et al., GCN Circ. 34938).\n\nThe source was clearly detected in the CZT detectors in the 20-200 keV energy range. The light curve peaks at 2023-11-04 01:47:40.35 UTC. The measured peak count rate associated with the burst is 1905 (+239, -231) counts/s above the background in the combined data of three quadrants (out of four), with a total of 2144 (+214, -227) counts. The local mean background count rate was 232 (+6, -7) counts/s. Using cumulative rates, we measure a T90 of 5 (+1, -1) s. We note that the total count measurements are affected by a 0.3s housekeeping dead time window that coincided with the burst. We also see a faint second peak, consistent with the light curve from Fermi-GBM and Swift-BAT, which is more prominently seen in the Veto detectors as reported below. However, the peak is too weak to make any contribution to the T90 measurements in the CZT lightcurve.\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 2023-11-04 01:47:38.43 UTC. The measured peak count rate associated with the burst is 3448 (+108, -118) counts/s above the background in the combined data of all quadrants, with a total of 14749 (+818, -888) counts. The local mean background count rate was 1357 (+7, -8) counts/s. We measure a T90 of 24 (+1, -18) s from the cumulative Veto light curve. This longer T90 arises from a clear detection of the second peak of the GRB.\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/34945.",
"published": "2023-11-04T17:12:50.372005Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-11-04T17:12:50.372023Z",
"modified": "2023-11-04T17:12:50.378055Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4372,
"topic": "gcn.circular",
"uuid": "2bcaaada-6ed7-4196-8fcd-41aa5cd696ed",
"title": "LIGO/Virgo/KAGRA S231104ac: Updated Sky localization",
"submitter": "Hop gcn.circular",
"authors": "Anjali Yelikar at Rochester Institute of Technology <ay2016@g.rit.edu>",
"data": {
"date": "23/11/04 20:10:57 GMT",
"from": "Anjali Yelikar at Rochester Institute of Technology <ay2016@g.rit.edu>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34947"
},
"title": "GCN CIRCULAR",
"number": "34947",
"subject": "LIGO/Virgo/KAGRA S231104ac: Updated Sky localization"
},
"message_text": "The LIGO Scientific Collaboration, the Virgo Collaboration, and the KAGRA Collaboration report:\n\nWe have conducted further analysis of the LIGO Hanford Observatory (H1) and LIGO Livingston Observatory (L1) data around the time of the compact binary merger (CBC) candidate S231104ac (GCN Circular 34942). Parameter estimation has been performed using Bilby [1] and a new sky map, Bilby.multiorder.fits, distributed via GCN Notice, is available for retrieval from the GraceDB event page:\n\nhttps://gracedb.ligo.org/superevents/S231104ac\n\nFor the Bilby.multiorder.fits sky map, the 90% credible region is 759 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 1357 +/- 321 Mpc (a posteriori mean +/- standard deviation).\n\nFor further information about analysis methodology and the contents of this alert, refer to the LIGO/Virgo/KAGRA Public Alerts User Guide https://emfollow.docs.ligo.org/userguide/.\n\n [1] Ashton et al. ApJS 241, 27 (2019) and Morisaki et al. arXiv:2307.13380 (2023)\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34947.",
"published": "2023-11-04T20:11:07.739877Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-11-04T20:11:07.739897Z",
"modified": "2023-11-04T20:11:07.749282Z",
"nonlocalizedevents": [
{
"event_id": "S231104a"
}
],
"targets": []
},
{
"id": 4375,
"topic": "gcn.circular",
"uuid": "3a83b3b2-fe15-4b53-9b11-be8674b58ded",
"title": "Fermi GRB 231103A: 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": "23/11/04 21:31:35 GMT",
"from": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34948"
},
"title": "GCN CIRCULAR",
"number": "34948",
"subject": "Fermi GRB 231103A: 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 231103A ( Fermi GBM team, GCN 34934) errorbox 1 days 13914 sec after notice time and 1 days 13948 sec after trigger time at 2023-11-04 18:33:59 UT, with upper limit up to 19.5 mag. The observations began at zenith distance = 32 deg. The sun altitude is -17.7 deg.\n\nThe galactic latitude b = -62 deg., longitude l = 301 deg.\n\n\nReal time updated cover map and OT discovered available here:\nhttps://master.sai.msu.ru/site/master2/observ.php?id\"94659\n\nWe obtain a following upper limits.\n\nTmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment\n_________|_____________________|_____________________|____________________________________|_____|_______|_______|________\n\n 100379 | 2023-11-04 18:33:59 | MASTER-SAAO | (00h 48m 05.20s , -55d 59m 13.2s) | C | 60 | 18.1 |\n 100470 | 2023-11-04 18:35:30 | MASTER-SAAO | (01h 02m 13.02s , -56d 00m 21.6s) | C | 60 | 17.9 |\n 100550 | 2023-11-04 18:36:50 | MASTER-SAAO | (00h 45m 39.68s , -54d 04m 42.2s) | C | 60 | 17.9 |\n 100642 | 2023-11-04 18:38:22 | MASTER-SAAO | (00h 59m 18.30s , -54d 06m 09.5s) | C | 60 | 16.9 |\n 100722 | 2023-11-04 18:39:42 | MASTER-SAAO | (00h 50m 32.32s , -57d 53m 12.0s) | C | 60 | 16.6 |\n 100813 | 2023-11-04 18:41:12 | MASTER-SAAO | (01h 05m 34.52s , -57d 52m 15.4s) | C | 60 | 17.4 |\n 100903 | 2023-11-04 18:42:43 | MASTER-SAAO | (00h 43m 33.08s , -52d 12m 15.4s) | C | 60 | 17.1 |\n 100983 | 2023-11-04 18:44:02 | MASTER-SAAO | (00h 56m 41.87s , -52d 11m 49.5s) | C | 60 | 17.8 |\n 101073 | 2023-11-04 18:45:33 | MASTER-SAAO | (01h 11m 34.45s , -54d 06m 01.8s) | C | 60 | 17.8 |\n 101153 | 2023-11-04 18:46:53 | MASTER-SAAO | (01h 25m 15.58s , -54d 04m 38.8s) | C | 60 | 17.4 |\n 101244 | 2023-11-04 18:48:23 | MASTER-SAAO | (00h 20m 41.61s , -55d 57m 53.2s) | C | 60 | 18.1 |\n 101323 | 2023-11-04 18:49:43 | MASTER-SAAO | (00h 35m 06.42s , -55d 59m 02.0s) | C | 60 | 18.1 |\n 101414 | 2023-11-04 18:51:14 | MASTER-SAAO | (00h 47m 51.52s , -56d 00m 07.4s) | C | 60 | 18.0 |\n 101494 | 2023-11-04 18:52:34 | MASTER-SAAO | (01h 02m 17.63s , -56d 00m 07.2s) | C | 60 | 17.4 |\n 101574 | 2023-11-04 18:53:54 | MASTER-SAAO | (00h 45m 36.77s , -54d 04m 35.5s) | C | 60 | 17.2 |\n 101665 | 2023-11-04 18:55:25 | MASTER-SAAO | (00h 59m 15.26s , -54d 05m 54.2s) | C | 60 | 17.6 |\n 101745 | 2023-11-04 18:56:44 | MASTER-SAAO | (00h 50m 34.14s , -57d 52m 15.6s) | C | 60 | 17.1 |\n 101835 | 2023-11-04 18:58:15 | MASTER-SAAO | (01h 05m 31.65s , -57d 53m 04.8s) | C | 60 | 17.6 |\n 101915 | 2023-11-04 18:59:35 | MASTER-SAAO | (00h 43m 29.81s , -52d 10m 03.6s) | C | 60 | 18.8 |\n 102006 | 2023-11-04 19:01:06 | MASTER-SAAO | (00h 56m 38.27s , -52d 11m 07.4s) | C | 60 | 18.4 |\n 102090 | 2023-11-04 19:02:30 | MASTER-SAAO | (01h 11m 28.41s , -54d 06m 08.1s) | C | 60 | 18.0 |\n 102180 | 2023-11-04 19:04:00 | MASTER-SAAO | (01h 25m 13.83s , -54d 06m 05.7s) | C | 60 | 17.6 |\n 102260 | 2023-11-04 19:05:20 | MASTER-SAAO | (00h 20m 42.61s , -55d 57m 57.1s) | C | 60 | 17.8 |\n 102340 | 2023-11-04 19:06:40 | MASTER-SAAO | (00h 35m 00.69s , -55d 59m 37.9s) | C | 60 | 18.5 |\n 102431 | 2023-11-04 19:08:11 | MASTER-SAAO | (00h 47m 56.37s , -55d 58m 10.0s) | C | 60 | 18.6 |\n 102511 | 2023-11-04 19:09:30 | MASTER-SAAO | (01h 02m 08.10s , -55d 58m 57.3s) | C | 60 | 18.8 |\n 102601 | 2023-11-04 19:11:01 | MASTER-SAAO | (00h 45m 32.38s , -54d 03m 51.1s) | C | 60 | 18.7 |\n 102681 | 2023-11-04 19:12:21 | MASTER-SAAO | (00h 59m 16.65s , -54d 04m 56.3s) | C | 60 | 18.9 |\n 102772 | 2023-11-04 19:13:52 | MASTER-SAAO | (00h 50m 26.68s , -57d 53m 45.1s) | C | 60 | 18.7 |\n 102863 | 2023-11-04 19:15:23 | MASTER-SAAO | (01h 05m 35.49s , -57d 53m 43.3s) | C | 60 | 18.7 |\n 102943 | 2023-11-04 19:16:43 | MASTER-SAAO | (00h 43m 31.08s , -52d 10m 08.2s) | C | 60 | 18.5 |\n 103034 | 2023-11-04 19:18:14 | MASTER-SAAO | (00h 56m 34.06s , -52d 11m 33.8s) | C | 60 | 18.3 |\n 103114 | 2023-11-04 19:19:34 | MASTER-SAAO | (01h 11m 32.86s , -54d 04m 11.9s) | C | 60 | 18.4 |\n 103205 | 2023-11-04 19:21:04 | MASTER-SAAO | (01h 25m 04.73s , -54d 04m 55.3s) | C | 60 | 18.7 |\n 103285 | 2023-11-04 19:22:24 | MASTER-SAAO | (00h 20m 38.65s , -55d 57m 19.5s) | C | 60 | 19.0 |\n 103375 | 2023-11-04 19:23:55 | MASTER-SAAO | (00h 35m 01.28s , -55d 58m 30.0s) | C | 60 | 18.6 |\n 103455 | 2023-11-04 19:25:14 | MASTER-SAAO | (01h 15m 05.16s , -55d 59m 28.4s) | C | 60 | 18.4 |\n 103546 | 2023-11-04 19:26:45 | MASTER-SAAO | (01h 29m 20.63s , -55d 57m 55.9s) | C | 60 | 18.3 |\n 103636 | 2023-11-04 19:28:16 | MASTER-SAAO | (00h 21m 53.42s , -57d 51m 21.9s) | C | 60 | 18.4 |\n 103716 | 2023-11-04 19:29:36 | MASTER-SAAO | (00h 36m 50.52s , -57d 52m 23.0s) | C | 60 | 18.8 |\n 103807 | 2023-11-04 19:31:06 | MASTER-SAAO | (00h 53m 25.90s , -59d 46m 31.6s) | C | 60 | 18.7 |\n 103886 | 2023-11-04 19:32:26 | MASTER-SAAO | (01h 09m 13.38s , -59d 47m 38.3s) | C | 60 | 19.0 |\n 103977 | 2023-11-04 19:33:57 | MASTER-SAAO | (00h 19m 37.16s , -54d 03m 39.3s) | C | 60 | 19.1 |\n 104057 | 2023-11-04 19:35:16 | MASTER-SAAO | (00h 33m 15.26s , -54d 05m 07.0s) | C | 60 | 19.1 |\n 104148 | 2023-11-04 19:36:48 | MASTER-SAAO | (01h 08m 13.21s , -52d 10m 43.1s) | C | 60 | 19.1 |\n 104240 | 2023-11-04 19:38:19 | MASTER-SAAO | (01h 21m 17.37s , -52d 09m 45.3s) | C | 60 | 19.2 |\n 104319 | 2023-11-04 19:39:39 | MASTER-SAAO | (01h 18m 58.93s , -57d 53m 35.1s) | C | 60 | 18.8 |\n 104411 | 2023-11-04 19:41:11 | MASTER-SAAO | (01h 34m 08.78s , -57d 53m 34.5s) | C | 60 | 18.7 |\n 104491 | 2023-11-04 19:42:30 | MASTER-SAAO | (01h 15m 00.67s , -55d 57m 36.8s) | C | 60 | 18.5 |\n 104582 | 2023-11-04 19:44:02 | MASTER-SAAO | (01h 29m 18.81s , -55d 59m 26.5s) | C | 60 | 18.3 |\n 104673 | 2023-11-04 19:45:32 | MASTER-SAAO | (00h 21m 52.25s , -57d 51m 04.0s) | C | 60 | 18.9 |\n 104753 | 2023-11-04 19:46:52 | MASTER-SAAO | (00h 36m 49.52s , -57d 52m 06.7s) | C | 60 | 18.8 |\n 104843 | 2023-11-04 19:48:23 | MASTER-SAAO | (00h 53m 16.53s , -59d 45m 16.1s) | C | 60 | 18.8 |\n 104923 | 2023-11-04 19:49:43 | MASTER-SAAO | (01h 09m 18.63s , -59d 46m 23.5s) | C | 60 | 19.0 |\n 105014 | 2023-11-04 19:51:13 | MASTER-SAAO | (00h 19m 31.76s , -54d 04m 54.5s) | C | 60 | 18.6 |\n 105093 | 2023-11-04 19:52:33 | MASTER-SAAO | (00h 33m 16.45s , -54d 04m 48.7s) | C | 60 | 19.2 |\n 105184 | 2023-11-04 19:54:04 | MASTER-SAAO | (01h 08m 14.92s , -52d 09m 37.7s) | C | 60 | 19.5 |\n 105264 | 2023-11-04 19:55:24 | MASTER-SAAO | (01h 21m 18.05s , -52d 11m 16.2s) | C | 60 | 19.5 |\n 105355 | 2023-11-04 19:56:55 | MASTER-SAAO | (01h 19m 01.73s , -57d 51m 26.8s) | C | 60 | 19.1 |\n 105435 | 2023-11-04 19:58:14 | MASTER-SAAO | (01h 34m 00.07s , -57d 52m 23.9s) | C | 60 | 18.9 |\n 105514 | 2023-11-04 19:59:34 | MASTER-SAAO | (01h 14m 54.50s , -55d 57m 22.2s) | C | 60 | 19.1 |\n 105619 | 2023-11-04 20:01:19 | MASTER-SAAO | (01h 29m 18.65s , -55d 58m 24.7s) | C | 60 | 19.1 |\n 105699 | 2023-11-04 20:02:39 | MASTER-SAAO | (00h 21m 43.13s , -57d 52m 37.0s) | C | 60 | 18.6 |\n 105790 | 2023-11-04 20:04:09 | MASTER-SAAO | (00h 36m 51.46s , -57d 52m 23.3s) | C | 60 | 19.0 |\n 105869 | 2023-11-04 20:05:29 | MASTER-SAAO | (00h 53m 17.74s , -59d 45m 15.4s) | C | 60 | 18.9 |\n 105961 | 2023-11-04 20:07:01 | MASTER-SAAO | (01h 09m 11.95s , -59d 47m 01.1s) | C | 60 | 19.0 |\n 106052 | 2023-11-04 20:08:32 | MASTER-SAAO | (00h 19m 35.58s , -54d 02m 43.3s) | C | 60 | 19.0 |\n 106132 | 2023-11-04 20:09:52 | MASTER-SAAO | (00h 32m 14.43s , -54d 03m 46.8s) | C | 60 | 19.0 |\n 106223 | 2023-11-04 20:11:23 | MASTER-SAAO | (01h 08m 10.21s , -52d 09m 11.5s) | C | 60 | 19.0 |\n 106303 | 2023-11-04 20:12:43 | MASTER-SAAO | (01h 21m 18.10s , -52d 10m 15.4s) | C | 60 | 19.2 |\n 106393 | 2023-11-04 20:14:13 | MASTER-SAAO | (01h 18m 53.89s , -57d 53m 04.3s) | C | 60 | 18.5 |\n 106484 | 2023-11-04 20:15:44 | MASTER-SAAO | (01h 34m 02.61s , -57d 52m 46.8s) | C | 60 | 18.5 |\n 106564 | 2023-11-04 20:17:03 | MASTER-SAAO | (00h 41m 35.25s , -50d 16m 46.0s) | C | 60 | 19.3 |\n 106654 | 2023-11-04 20:18:34 | MASTER-SAAO | (00h 54m 08.61s , -50d 15m 02.8s) | C | 60 | 19.3 |\n 106734 | 2023-11-04 20:19:54 | MASTER-SAAO | (00h 16m 58.41s , -52d 08m 19.0s) | C | 60 | 18.4 |\n 106825 | 2023-11-04 20:21:24 | MASTER-SAAO | (00h 30m 04.44s , -52d 09m 31.0s) | C | 60 | 19.0 |\n 106904 | 2023-11-04 20:22:44 | MASTER-SAAO | (00h 21m 07.37s , -59d 46m 04.0s) | C | 60 | 19.2 |\n 106995 | 2023-11-04 20:24:15 | MASTER-SAAO | (00h 36m 56.76s , -59d 44m 33.0s) | C | 60 | 19.1 |\n 107075 | 2023-11-04 20:25:35 | MASTER-SAAO | (01h 05m 24.62s , -50d 15m 24.1s) | C | 60 | 19.3 |\n 107165 | 2023-11-04 20:27:05 | MASTER-SAAO | (01h 17m 49.62s , -50d 16m 02.4s) | C | 60 | 19.5 |\n 107245 | 2023-11-04 20:28:25 | MASTER-SAAO | (00h 56m 40.30s , -61d 39m 32.1s) | C | 60 | 19.0 |\n 107325 | 2023-11-04 20:29:45 | MASTER-SAAO | (01h 13m 25.52s , -61d 40m 41.4s) | C | 60 | 19.0 |\n 107416 | 2023-11-04 20:31:16 | MASTER-SAAO | (01h 23m 27.45s , -59d 45m 16.8s) | C | 60 | 19.0 |\n 107587 | 2023-11-04 20:34:07 | MASTER-SAAO | (00h 41m 11.05s , -50d 14m 59.2s) | C | 60 | 19.4 |\n 107667 | 2023-11-04 20:35:27 | MASTER-SAAO | (00h 53m 39.84s , -50d 15m 41.7s) | C | 60 | 19.4 |\n 107757 | 2023-11-04 20:36:57 | MASTER-SAAO | (00h 17m 01.97s , -52d 07m 57.7s) | C | 60 | 18.8 |\n 107837 | 2023-11-04 20:38:17 | MASTER-SAAO | (00h 30m 06.80s , -52d 09m 10.8s) | C | 60 | 19.4 |\n 107928 | 2023-11-04 20:39:47 | MASTER-SAAO | (00h 21m 04.50s , -59d 45m 47.4s) | C | 60 | 18.9 |\n 108018 | 2023-11-04 20:41:18 | MASTER-SAAO | (00h 36m 55.09s , -59d 45m 56.9s) | C | 60 | 19.2 |\n 108097 | 2023-11-04 20:42:37 | MASTER-SAAO | (01h 04m 07.89s , -50d 14m 42.3s) | C | 60 | 19.5 |\n 108189 | 2023-11-04 20:44:09 | MASTER-SAAO | (01h 17m 51.31s , -50d 16m 44.4s) | C | 60 | 19.5 |\n 108269 | 2023-11-04 20:45:29 | MASTER-SAAO | (00h 56m 35.62s , -61d 38m 14.1s) | C | 60 | 19.0 |\n 108359 | 2023-11-04 20:46:59 | MASTER-SAAO | (01h 13m 21.67s , -61d 39m 23.0s) | C | 60 | 19.1 |\n 108438 | 2023-11-04 20:48:18 | MASTER-SAAO | (01h 23m 20.98s , -59d 44m 30.4s) | C | 60 | 19.1 |\n 108609 | 2023-11-04 20:51:09 | MASTER-SAAO | (00h 40m 02.48s , -50d 16m 11.9s) | C | 60 | 19.5 |\n 108689 | 2023-11-04 20:52:28 | MASTER-SAAO | (00h 52m 34.36s , -50d 16m 04.4s) | C | 60 | 19.4 |\n 108780 | 2023-11-04 20:53:59 | MASTER-SAAO | (00h 17m 11.16s , -52d 07m 59.9s) | C | 60 | 19.2 |\n 108859 | 2023-11-04 20:55:19 | MASTER-SAAO | (00h 30m 08.49s , -52d 09m 20.1s) | C | 60 | 19.5 |\n 108951 | 2023-11-04 20:56:50 | MASTER-SAAO | (00h 21m 16.72s , -59d 43m 37.0s) | C | 60 | 18.7 |\n 109030 | 2023-11-04 20:58:10 | MASTER-SAAO | (00h 36m 56.57s , -59d 44m 40.3s) | C | 60 | 19.1 |\n 109121 | 2023-11-04 20:59:41 | MASTER-SAAO | (01h 03m 42.75s , -50d 14m 18.9s) | C | 60 | 19.3 |\n 109211 | 2023-11-04 21:01:11 | MASTER-SAAO | (01h 16m 20.36s , -50d 15m 24.5s) | C | 60 | 19.5 |\n 109291 | 2023-11-04 21:02:31 | MASTER-SAAO | (00h 54m 25.41s , -61d 39m 50.6s) | C | 60 | 19.0 |\n 109382 | 2023-11-04 21:04:01 | MASTER-SAAO | (01h 11m 22.74s , -61d 39m 33.8s) | C | 60 | 19.0 |\n 109461 | 2023-11-04 21:05:21 | MASTER-SAAO | (01h 21m 25.85s , -59d 44m 13.6s) | C | 60 | 19.0 |\n 109552 | 2023-11-04 21:06:52 | MASTER-SAAO | (01h 37m 19.41s , -59d 45m 45.6s) | C | 60 | 19.2 |\n 109723 | 2023-11-04 21:09:42 | MASTER-SAAO | (00h 39m 43.02s , -61d 37m 13.9s) | C | 60 | 19.0 |\n 109802 | 2023-11-04 21:11:02 | MASTER-SAAO | (01h 35m 49.54s , -54d 04m 06.7s) | C | 60 | 19.0 |\n 110064 | 2023-11-04 21:15:23 | MASTER-SAAO | (00h 29m 18.96s , -50d 13m 13.1s) | C | 60 | 19.5 |\n 110224 | 2023-11-04 21:18:04 | MASTER-SAAO | (00h 50m 56.80s , -48d 20m 34.3s) | C | 60 | 19.4 |\n 110314 | 2023-11-04 21:19:34 | MASTER-SAAO | (01h 01m 43.99s , -48d 21m 25.6s) | C | 60 | 19.4 |\n 110485 | 2023-11-04 21:22:25 | MASTER-SAAO | (01h 31m 34.54s , -52d 08m 09.8s) | C | 60 | 19.4 |\n 110735 | 2023-11-04 21:26:35 | MASTER-SAAO | (00h 40m 00.46s , -61d 37m 53.3s) | C | 60 | 19.0 |\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/34948.",
"published": "2023-11-04T21:31:46.158697Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-11-04T21:31:46.158730Z",
"modified": "2023-11-04T21:31:46.166345Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4376,
"topic": "gcn.circular",
"uuid": "f2f0c803-d0c4-4915-9681-d30061199089",
"title": "GRB 231104B: 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": "23/11/04 23:21:14 GMT",
"from": "Fermi GBM Team at MSFC/Fermi-GBM <do_not_reply@GIOC.nsstc.nasa.gov>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34949"
},
"title": "GCN CIRCULAR",
"number": "34949",
"subject": "GRB 231104B: Fermi GBM Final Real-time Localization"
},
"message_text": "The Fermi GBM team reports the detection of a likely LONG GRB\n\nAt 23:10:39 UT on 4 Nov 2023, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 231104B (trigger 720832244.521916 / 231104966).\n\nThe on-ground calculated location, using the Fermi GBM trigger data, is RA = 10.9, Dec = -41.8 (J2000 degrees, equivalent to J2000 00h 43m, -41d 47'), with a statistical uncertainty of 3.3 degrees.\n\nThe angle from the Fermi LAT boresight is 124.0 degrees.\n\nThe skymap can be found here:\nhttps://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn231104966/quicklook/glg_skymap_all_bn231104966.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/2023/bn231104966/quicklook/glg_healpix_all_bn231104966.fit\n\nThe GBM light curve can be found here:\nhttps://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn231104966/quicklook/glg_lc_medres34_bn231104966.gif\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34949.",
"published": "2023-11-04T23:21:25.198901Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-11-04T23:21:25.198922Z",
"modified": "2023-11-04T23:21:25.206262Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4381,
"topic": "gcn.circular",
"uuid": "da48e118-b0d7-404f-b8b9-3c3f7e88858c",
"title": "GRB 231104A: Fermi GBM Observation",
"submitter": "Hop gcn.circular",
"authors": "sumanbala2210@gmail.com",
"data": {
"date": "23/11/05 05:31:07 GMT",
"from": "sumanbala2210@gmail.com",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34950"
},
"title": "GCN CIRCULAR",
"number": "34950",
"subject": "GRB 231104A: Fermi GBM Observation"
},
"message_text": "S. Bala (USRA) and C. Meegan (UAH) report on behalf of\nthe Fermi Gamma-ray Burst Monitor Team:\n\n\"At 01:47:28.14 UT on 04 November 2023, the Fermi Gamma-ray Burst Monitor (GBM)\ntriggered and located GRB 231104A (trigger 720755253/231104075).\nwhich was also detected by Swift BAT (K. L. Page et al. 2023, GCN 34938) and\nFermi LAT (G. Principe. et al. 2023, GCN 34943).\nThe Fermi GBM on-ground location is consistent with the Swift BAT position.\n\nThe angle from the Fermi LAT boresight is 32 degrees.\n\nThe GBM light curve Consist of three distinguishable pick with a duration (T90)\nof about 44 s (50-300 keV). The time-averaged spectrum\nfrom T0-3.6 to T0+62.0 s is best fit by\na power law function with an exponential high-energy cutoff.\nThe power law index is -1.07 +/- 0.01 and the cutoff energy,\nparameterized as Epeak, is 539 +/- 22 keV.\n\nThe event fluence (10-1000 keV) in this time interval is\n(5.59 +/- 0.06)E-05 erg/cm^2. The 1-sec peak photon flux measured\nstarting from T0+3.6 s in the 10-1000 keV band is 2 +/- 0.2 ph/s/cm^2.\n\nA Band function fits the spectrum equally well\nwith Epeak= 490 +/- 20 keV, alpha = -1.05 +/- 0.02 and beta = -2.6 +/- 0.2.\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/34950.",
"published": "2023-11-05T05:31:17.753378Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-11-05T05:31:17.753413Z",
"modified": "2023-11-05T05:31:17.761980Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4382,
"topic": "gcn.circular",
"uuid": "5708279c-21df-414d-8a51-6af857df6c46",
"title": "GRB 231104A: NOT upper limit",
"submitter": "Hop gcn.circular",
"authors": "Zipei Zhu at NAOC <zpzhu@nao.cas.cn>",
"data": {
"date": "23/11/05 11:47:50 GMT",
"from": "Zipei Zhu at NAOC <zpzhu@nao.cas.cn>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34951"
},
"title": "GCN CIRCULAR",
"number": "34951",
"subject": "GRB 231104A: NOT upper limit"
},
"message_text": "Z. Zhu, D. Xu (NAOC), D.B. Malesani (Radboud Univ. and DAWN/NBI), A. de Ugarte Postigo (OCA-CNRS), Z. Gray (NOT) report on behalf of a larger collaboration:\n\nWe observed the field of GRB 231104A detected by Swift (Page et al., GCN 34938) and Fermi (Fermi GBM team, GCN 34937) using the the 2.56 m Nordic Optical Telescope (NOT) equipped with the ALFOSC camera. Observations started at 01:57:16 UT on 2023-11-05, i.e., ~ 1.0 day after the Swift/BAT trigger, and 9x200 s Sloan i-filter images were obtained.\n\nNo optical source is detected within or at the border of the Swift/XRT enhanced error circle (Goad et al., GCN 34940) down to upper limits of i > 24.2 mag (3-sigma), calibrated with the nearby Pan-STARRS stars and not corrected for Galactic extinction.\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34951.",
"published": "2023-11-05T11:48:00.578632Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-11-05T11:48:00.578651Z",
"modified": "2023-11-05T11:48:00.587514Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4397,
"topic": "gcn.circular",
"uuid": "bba6b3bd-359e-4e59-a628-db0215a255fd",
"title": "Fermi-LAT gamma-ray observations of IceCube-231103A",
"submitter": "Hop gcn.circular",
"authors": "chiara.bartolini-1@unitn.it",
"data": {
"date": "23/11/06 11:48:23 GMT",
"from": "chiara.bartolini-1@unitn.it",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34952"
},
"title": "GCN CIRCULAR",
"number": "34952",
"subject": "Fermi-LAT gamma-ray observations of IceCube-231103A"
},
"message_text": "C. Bartolini (INFN Bari), S. Buson (Uni Wuerzburg), S. Garrappa (Weizmann Institute of Science), and J. Sinapius (DESY) on behalf of the Fermi-LAT collaboration:\n\nWe report an analysis of observations of the vicinity of the IC231103A high-energy neutrino event (GCN 34933) 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 2023-11-03 at 09:17:35.29 UT (T0) with J2000 position RA = 105.67 (+3.15, -2.94) deg, Decl. = +47.85 (+1.95, -1.78) deg (90% PSF containment). According to the fourth Fermi LAT source catalog (4FGL-DR4), there are several 4FGL-DR4 cataloged gamma-ray (>100 MeV; The Fermi-LAT collaboration 2022, ApJS, 260, 53) sources in the 90% IC231103A uncertainty localization region. Based on a preliminary analysis of the LAT data over a month and day timescale prior T0, these objects are not significantly detected at gamma rays.\n\nWe searched for intermediate (days to years) timescale emission from a new gamma-ray source. Preliminary analysis indicates no significant (> 5 sigma) new excess emission (> 100 MeV) at the IC231103A best-fit position. Assuming a power-law spectrum (photon index = 2.0 fixed) for a point source at the IC231103A best-fit position, the >100 MeV flux upper limit (95% confidence) is <4.3e-10 ph cm^-2 s^-1 for ~15-years (2008-08-04 to 2023-11-03 UTC), and < 1.3e-8 (<7.2 e-8) ph cm^-2 s^-1 for a 1-month (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 are S. Garrappa (simone.garrappa at weizmann.ac.il), C. Bartolini (chiara.bartolini at ba.infn.it), S. Buson (sara.buson at uni-wuerzburg.de) and J. Sinapius (jonas.sinapius at desy.de).\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\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34952.",
"published": "2023-11-06T11:48:40.524859Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-11-06T11:48:40.524878Z",
"modified": "2023-11-06T11:48:40.531868Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4404,
"topic": "gcn.circular",
"uuid": "c1d115cd-0949-4491-8ffa-f81185a9bb3f",
"title": "LIGO/Virgo/KAGRA S231106y: one counterpart neutrino candidate from IceCube neutrino searches",
"submitter": "Hop gcn.circular",
"authors": "Erik Blaufuss at University of Maryland, College Park <blaufuss@umd.edu>",
"data": {
"date": "23/11/06 16:07:24 GMT",
"from": "Erik Blaufuss at University of Maryland, College Park <blaufuss@umd.edu>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34953"
},
"title": "GCN CIRCULAR",
"number": "34953",
"subject": "LIGO/Virgo/KAGRA S231106y: one counterpart neutrino candidate from IceCube neutrino searches"
},
"message_text": "The IceCube Collaboration (http://icecube.wisc.edu/) reports:\n\nA search for track-like muon neutrino events detected by IceCube consistent with the sky localization of the low-significance gravitational wave candidate S231106y in a time range of 1000 seconds centered on the alert event time (2023-11-06 06:48:08 UTC to 2023-11-06 07:04:48 UTC) has been performed [1,2]. During this time period IceCube was collecting good quality data. One hypothesis test was conducted for this low-significance gravitational wave event. The search uses a Bayesian approach to quantify the joint GW + neutrino event significance, which assumes a binary merger scenario and accounts for known astrophysical priors, such as GW source distance, in the significance estimate [3].\n\nOne track-like event was found in spatial and temporal coincidence with the gravitational-wave\ncandidate S231106y calculated from the map circulated by LVK as S231106y-2-Preliminary. This\nrepresents an overall pre-trial p-value of 0.0090 for the Bayesian search.\n\nThe reported p-value here does not account for any trials correction (multiple hypotheses testing). The false alarm rate of this coincidence can be obtained by multiplying the p-value with the corresponding GW trigger rate. Further details are available at https://gcn.nasa.gov/missions/icecube and at https://roc.icecube.wisc.edu/public/LvkNuTrackSearch.\n.\n\nProperties of the coincident event(s) are shown below.\n\ndt(s)\tRA(deg)\t\tDec(deg)\tAngular uncertainty(deg) p-value(generic transient) p-value(Bayesian)\n-----------------------------------------------------------------------------------------------------\n41.78 318.15 \t69.01 6.54 not applicable\t\t0.0090\n\n\n\nwhere:\ndt = Time of track event minus time of GW trigger (sec)\nAngular uncertainty = Angular uncertainty of track event: the radius of a circle\n \trepresenting 90% CL containment by area.\np-value = the p-value for this specific track event from each search.\n\nThe IceCube Neutrino Observatory is a cubic-kilometer neutrino detector operating at the\ngeographic South Pole, Antarctica. The IceCube realtime alert point of contact can be\nreached at roc@icecube.wisc.edu\n\n\n[1] M. G. Aartsen et al 2020 ApJL 898 L10\n[2] Abbasi et al. Astrophys.J. 944 (2023) 1, 80\n[3] I. Bartos et al. 2019 Phys. Rev. D 100, 083017\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34953.",
"published": "2023-11-06T16:07:39.876557Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-11-06T16:07:39.876575Z",
"modified": "2023-11-06T16:07:39.882096Z",
"nonlocalizedevents": [
{
"event_id": "S231106y"
}
],
"targets": []
},
{
"id": 6342,
"topic": "gcn.circular",
"uuid": "0b6156f2-cf2d-4bf0-893e-cb5fa0f4129e",
"title": "GRB 240403A: Fermi GBM Detection",
"submitter": "Hop gcn.circular",
"authors": "rachel.hamburg@ijclab.in2p3.fr",
"data": {
"date": "24/04/04 14:27:05 GMT",
"from": "rachel.hamburg@ijclab.in2p3.fr",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/36024"
},
"title": "GCN CIRCULAR",
"number": "36024",
"subject": "GRB 240403A: Fermi GBM Detection"
},
"message_text": "R. Hamburg (CNRS/IN2P3/IJCLab), S. Dalessi (UAH) and C. Meegan (UAH) report on behalf of\nthe Fermi Gamma-ray Burst Monitor Team:\n\n\"At 11:57:30.58 UT on 03 April 2024, the Fermi Gamma-ray Burst Monitor (GBM)\ntriggered and located GRB 240403A (trigger 733838255/240403498).\n\nThe on-ground calculated location, using the Fermi GBM trigger data,\nis RA = 6.5, Dec = -17.3 (J2000 degrees, equivalent to\nJ2000 +00h 26m, -17d 17'), with a statistical uncertainty of 1.77 degrees.\nThere is additionally a systematic error which we have characterized\nas a core-plus-tail model, with 90% of GRBs having a 3.7 deg error and a\nsmall tail suffering a larger than 10 deg systematic error (Connaughton\net al. 2015, ApJS, 216, 32).\n\nThe angle from the Fermi LAT boresight is 62 degrees.\n\nThe GBM light curve shows a precursor, a main emission peak\nand third weaker peak, yielding a duration (T90)\nof about 35.6 s (50-300 keV). The time-averaged spectrum\nfrom T0-1.2 to T0+76.7 s is best fit by\na power law function with an exponential high-energy cutoff.\nThe power law index is -1.11 +/- 0.01 and the cutoff energy,\nparameterized as Epeak, is 350 +/- 10 keV.\nA Band function also fits well with Epeak = 322 +/- 14 keV,\nalpha = -1.08 +/- 0.02, and beta = -2.40 +/- 0.13.\n\nThe event fluence (10-1000 keV) in this time interval is\n(3.6 +/- 0.4)E-05 erg/cm^2. The 1-sec peak photon flux measured\nstarting from T0+26 s in the 10-1000 keV band is 39.1 +/- 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/36024.",
"published": "2024-04-04T14:27:22.983263Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-04-04T14:27:22.983282Z",
"modified": "2024-04-04T14:27:22.991259Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4405,
"topic": "gcn.circular",
"uuid": "089d7adf-79f6-48c1-9ec2-c159c3979711",
"title": "IceCube-231103A: 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": "23/11/06 16:45:29 GMT",
"from": "Jessie Thwaites at IceCube/U Wisc-Madison <thwaites@wisc.edu>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34954"
},
"title": "GCN CIRCULAR",
"number": "34954",
"subject": "IceCube-231103A: 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-231103A (https://gcn.nasa.gov/circulars/34933) in a time range of 1000 seconds centered on the alert event time (2023-11-03 09:09:15.290 UTC to 2023-11-03 09:25:55.290 UTC) during which IceCube was collecting good quality data. Excluding the event that prompted the alert, zero track-like events are found within the 90% containment region of IceCube-231103A. 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-231103A is 1.5e-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 5e+04 GeV.\n\nA subsequent search was performed including 2 days of data centered on the alert event time (2023-11-02 09:17:35.290 UTC to 2023-11-04 09:17:35.290 UTC). In this case, we report a p-value of 0.07, 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-231103A is 1.8e-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/34954.",
"published": "2023-11-06T16:45:39.630776Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-11-06T16:45:39.630817Z",
"modified": "2023-11-06T16:45:39.638335Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4406,
"topic": "gcn.circular",
"uuid": "154b391b-8b3a-403f-8921-c3599b171b7e",
"title": "GRB 231104A: 3.6m DOT optical upper limit",
"submitter": "Hop gcn.circular",
"authors": "Rahul Gupta at Aryabhatta Research Institute of Observational Sciences (ARIES) India <rahulbhu.c157@gmail.com>",
"data": {
"date": "23/11/06 18:02:21 GMT",
"from": "Rahul Gupta at Aryabhatta Research Institute of Observational Sciences (ARIES) India <rahulbhu.c157@gmail.com>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34955"
},
"title": "GCN CIRCULAR",
"number": "34955",
"subject": "GRB 231104A: 3.6m DOT optical upper limit"
},
"message_text": "Rahul Gupta, Amit K. Ror, Amar Aryan, and S. B. Pandey (ARIES) report on\nbehalf of a larger collaboration:\n\nWe observed the field of GRB 231104A detected by Fermi (Fermi GBM team, GCN\n34937; Principe et al., GCN 34943), Swift (Page et al., GCN 34938), and\nAstroSat (Navaneeth et al., GCN 34945) using the 3.6m Devasthal Optical\nTelescope of ARIES Nainital. We have taken multiple frames having an\nexposure time of 100 sec in the r and i filters, respectively. We do not\nfind any evidence of an afterglow candidate inside the Swift/XRT enhanced\nerror circle (Goad et al., GCN 34940), consistent with other non-detections\n(Strausbaugh et al., GCN 34939; Kuin et al., GCN 34941; Odeh et al., GCN\n34946; and Zhu et al., GCN 34951). We obtained the limiting mag of ~ 24 mag\n(r-band) at ~ 0.9 days post-detection.\n\nThe limiting magnitudes quoted are not corrected for the Galactic\nextinction in the direction of the burst. Photometric calibration is\nperformed using the standard stars from the Pan-STARRS catalog.\n\nThis circular may be cited. 3.6m Devasthal Optical Telescope (DOT) is\nthe recently commissioned facility in the Northern Himalayan region of\nIndia (long:79 41 04E, lat:29 21 40N, alt:2540m) owned and operated by the\nAryabhatta Research Institute of Observational Sciences (ARIES), Nainital (\nhttps://www.aries.res.in). Authors of this GCN circular thankfully\nacknowledge consistent support from the staff members to run and maintain\nthe 3.6m DOT.\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34955.",
"published": "2023-11-06T18:02:32.668584Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-11-06T18:02:32.668603Z",
"modified": "2023-11-06T18:02:32.675667Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4407,
"topic": "gcn.circular",
"uuid": "cf663ff6-804f-44c7-99a3-6866e453540f",
"title": "GRB 231106A: 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": "23/11/06 18:24:51 GMT",
"from": "Fermi GBM Team at MSFC/Fermi-GBM <do_not_reply@GIOC.nsstc.nasa.gov>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34956"
},
"title": "GCN CIRCULAR",
"number": "34956",
"subject": "GRB 231106A: Fermi GBM Final Real-time Localization"
},
"message_text": "The Fermi GBM team reports the detection of a likely LONG GRB\n\nAt 18:13:23 UT on 6 Nov 2023, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 231106A (trigger 720987208.394416 / 231106759).\n\nThe on-ground calculated location, using the Fermi GBM trigger data, is RA = 113.8, Dec = 25.6 (J2000 degrees, equivalent to J2000 07h 35m, 25d 36'), with a statistical uncertainty of 3.4 degrees.\n\nThe angle from the Fermi LAT boresight is 120.0 degrees.\n\nThe skymap can be found here:\nhttps://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn231106759/quicklook/glg_skymap_all_bn231106759.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/2023/bn231106759/quicklook/glg_healpix_all_bn231106759.fit\n\nThe GBM light curve can be found here:\nhttps://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn231106759/quicklook/glg_lc_medres34_bn231106759.gif\n\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34956.",
"published": "2023-11-06T18:25:02.561682Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-11-06T18:25:02.561720Z",
"modified": "2023-11-06T18:25:02.569293Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4408,
"topic": "gcn.circular",
"uuid": "616aeff4-dccf-4a8d-ad99-b91b5cbb4017",
"title": "GRB 231104A: NuSTAR Observation of the prompt emission",
"submitter": "Hop gcn.circular",
"authors": "Brian Grefenstette at Caltech/NuSTAR <bwgref@srl.caltech.edu>",
"data": {
"date": "23/11/06 19:21:51 GMT",
"from": "Brian Grefenstette at Caltech/NuSTAR <bwgref@srl.caltech.edu>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34957"
},
"title": "GCN CIRCULAR",
"number": "34957",
"subject": "GRB 231104A: NuSTAR Observation of the prompt emission"
},
"message_text": "B. Grefenstette reports on behalf of the NuSTAR Search for INteresting Gamma-ray Signals (SINGS) working group:\n\nThe NuSTAR SINGS working group reports the discovery of prompt emission from a potential GRB 231104A in the NuSTAR CsI anti-coincidence shields and the CdZnTe imagers. This GRB was identified through a blind search using the CsI shield rates. Details of the search algorithm will be described in a future paper. \n\nThe CsI data are recorded at 1 Hz and show a broad burst with multiple peaks. The initial NuSTAR trigger had a T0 of 2023-11-04T01:47:31, though offline analysis shows that a initial rise in the shield of 2023-11-04T01:47:37, which is consistent with the onset time reported by Ferm GBM (Bala et al, GCN Circ 34950). Peak 1-sec count rates were ~4,000 counts per second in both the FPMA and FPMB shield units. Typical background rates are ~1,000 counts per second. The burst was detected in both the CdZnTe detectors as well as in the shields.\n\nUsing the localization from Swift (Palmer et al, GCN Circ 34938):\n\n RA(J2000) = 01h 35m 09s\n Dec(J2000) = +83d 47' 27\"\n\nâ¦the burst was ~100-degrees from the instrument boresight.\n\nThe main burst lasts for ~6-s. Two narrow (<1-s) peaks can be seen in both the 1-Hz CsI shield rates and in the CdZnTe detectors.\n\nThe automated light curve report for this GRB, discovery report, off-line analysis of the shield data, and the CdZnTe lightcurves can be found here:\n\nhttps://nustarsoc.caltech.edu/NuSTAR_Public/grbs/reports/2023/231104A/\n\nInformation on NuSTAR SINGS can be found here: \n\nhttps://nustarsoc.caltech.edu/NuSTAR_Public/grbs/\n\nNuSTAR is a NASA Small Explorer mission led by Caltech and managed by JPL for NASAâs Science Mission Directorate in Washington. \n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34957.",
"published": "2023-11-06T19:22:02.789674Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-11-06T19:22:02.789699Z",
"modified": "2023-11-06T19:22:02.796880Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4421,
"topic": "gcn.circular",
"uuid": "4ec8ca25-7028-4fed-b895-1f24fbab45b3",
"title": "LIGO/Virgo/KAGRA S231102w: Upper limits from Swift/BAT-GUANO",
"submitter": "Hop gcn.circular",
"authors": "Samuele Ronchini at PSU <sjs8171@psu.edu>",
"data": {
"date": "23/11/07 02:59:50 GMT",
"from": "Samuele Ronchini at PSU <sjs8171@psu.edu>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34960"
},
"title": "GCN CIRCULAR",
"number": "34960",
"subject": "LIGO/Virgo/KAGRA S231102w: Upper limits from Swift/BAT-GUANO"
},
"message_text": "Samuele Ronchini (PSU), Jamie A. Kennea (PSU), James DeLaunay (PSU), Gayathri Raman (PSU), Aaron Tohuvavohu (U Toronto), Tyler Parsotan (NASA GSFC) report:\n\nSwift/BAT was observing 55% of the GW localization probability (bayestar.multiorder.fits) at merger time. A fraction 24.3 % of the GW localization posterior is contained inside the BAT coded FoV.\n\nThe LVK 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\nUsing the NITRATES analysis (DeLaunay + Tohuvavohu 2022, ApJ, 941, 169), we searched for emission on 8 timescales from 0.128s to 16.384s in the interval [-20,+20] seconds around the merger time. We find no evidence for a signal, and derive the following upper limits.\n\nWe quote the 5-sigma flux upper limits in the 15-350 keV band, weighted over the GW localization, for four spectral templates (soft, normal, and hard GRB-like templates described in [arXiv:1612.02395], and spectral shape from GRB170817A [arXiv:1710.05446]) and for four time bins.\nIn units of 10^-7 erg/s/cm^2:\n\ntime_bin (s) soft normal hard GRB170817\n------------------------------------\n0.256 7.3 5.4 4.9 5.9\n1.024 3.7 2.7 2.5 3.0\n4.096 2.0 1.5 1.3 1.6\n16.38 1.2 0.9 0.8 1.0\n\n\nThe upper limits as function of sky position are plotted here, alongside the GW localization:\nhttps://doi.org/10.5281/zenodo.10069919\nThe solid and dashed lines indicate the 90% and 50% GW contour levels, respectively.\n\nThe corresponding fits file can be found here:\nhttps://doi.org/10.5281/zenodo.10069923\n\nGUANO is a fully autonomous, extremely low latency, spacecraft\ncommanding pipeline designed for targeted recovery of BAT event mode\ndata around the times of compelling astrophysical events to enable\nmore sensitive GRB searches.\n\nA live reporting of Swift/BAT event data recovered by GUANO can be\nfound at: https://www.swift.psu.edu/guano/\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34960.",
"published": "2023-11-07T03:00:02.622826Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-11-07T03:00:02.622848Z",
"modified": "2023-11-07T03:00:02.634929Z",
"nonlocalizedevents": [
{
"event_id": "S231102w"
}
],
"targets": []
},
{
"id": 4411,
"topic": "gcn.circular",
"uuid": "45b78c94-e04d-4f9f-ae61-2048b9f7a5d0",
"title": "GRB 231104A: Wendelstein Optical/Infrared Observations",
"submitter": "Hop gcn.circular",
"authors": "m.busmann@physik.lmu.de",
"data": {
"date": "23/11/06 20:45:59 GMT",
"from": "m.busmann@physik.lmu.de",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34958"
},
"title": "GCN CIRCULAR",
"number": "34958",
"subject": "GRB 231104A: Wendelstein Optical/Infrared Observations"
},
"message_text": "Malte Busman (LMU), Daniel Gruen (LMU), Brendan OâConnor (CMU), Julius Gassert (LMU), Lei Hu (CMU), Antonella Palmese (CMU), Christoph Ries (LMU), Arno Riffeser (LMU/MPE), Michael Schmidt (LMU), Ananya Shankar (LMU):\n\nWe observed the position of GRB 231104A (Fermi GBM team, GCN 34937; Page et al., GCN 34938) with the 2m Fraunhofer telescope at Wendelstein Observatory, Germany. Observations were obtained using the 3kk imager in the r, z, and K bands simultaneously starting on 2023-11-06 at 12:09:53 UT with a total exposure of 6,021 seconds.\n\nAt the position of the XRT source (Goad et al., GCN 34940) we do not detect any source within 15â to depth r> 23.6 and K>21.0 AB mag at 2.4 days after the GRB trigger. The magnitudes are not corrected for Milky Way extinction and the photometry was calibrated against nearby stars in the PS1 and 2MASS catalogs.\n\nWe thank the staff of the Wendelstein Observatory for obtaining these observations.\n\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/34958.",
"published": "2023-11-06T20:46:10.164767Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-11-06T20:46:10.164798Z",
"modified": "2023-11-06T20:46:10.173057Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 4412,
"topic": "gcn.circular",
"uuid": "86afac4d-d679-4fc9-a1a8-4f6ec8f5c9e0",
"title": "Fermi GRB 231106A: 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": "23/11/06 22:01:20 GMT",
"from": "Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>",
"urls": {
"gcn": "https://gcn.nasa.gov/circulars/34959"
},
"title": "GCN CIRCULAR",
"number": "34959",
"subject": "Fermi GRB 231106A: 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 231106A ( Fermi GBM team, GCN 34956) errorbox 7435 sec after notice time and 7476 sec after trigger time at 2023-11-06 20:18:00 UT, with upper limit up to 19.0 mag. The observations began at zenith distance = 68 deg. The sun altitude is -58.5 deg.\n\nThe galactic latitude b = 21 deg., longitude l = 194 deg.\n\n\nReal time updated cover map and OT discovered available here:\nhttps://master.sai.msu.ru/site/master2/observ.php?id\"96397\n\nWe obtain a following upper limits.\n\nTmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment\n_________|_____________________|_____________________|____________________________________|_____|_______|_______|________\n\n 7507 | 2023-11-06 20:18:00 | MASTER-Tavrida | (07h 18m 58.76s , +28d 01m 31.6s) | C | 60 | 16.6 |\n 7579 | 2023-11-06 20:19:12 | MASTER-Tavrida | (07h 11m 43.66s , +26d 07m 24.0s) | C | 60 | 16.1 |\n 8169 | 2023-11-06 20:29:02 | MASTER-Tavrida | (07h 27m 01.04s , +29d 55m 54.0s) | C | 60 | 17.4 |\n 8317 | 2023-11-06 20:31:30 | MASTER-Tavrida | (07h 36m 13.30s , +28d 00m 34.7s) | C | 60 | 15.6 |\n 8390 | 2023-11-06 20:32:43 | MASTER-Tavrida | (07h 45m 13.60s , +28d 02m 01.0s) | C | 60 | 13.5 |\n 8610 | 2023-11-06 20:36:22 | MASTER-Tavrida | (07h 18m 54.71s , +28d 00m 53.6s) | C | 60 | 17.7 |\n 9277 | 2023-11-06 20:47:30 | MASTER-Tavrida | (07h 28m 03.37s , +28d 00m 48.0s) | C | 60 | 17.8 |\n 9351 | 2023-11-06 20:48:43 | MASTER-Tavrida | (07h 11m 38.63s , +26d 07m 42.0s) | C | 60 | 18.0 |\n 9423 | 2023-11-06 20:49:56 | MASTER-Tavrida | (07h 20m 32.94s , +26d 06m 27.4s) | C | 60 | 17.8 |\n 9642 | 2023-11-06 20:53:35 | MASTER-Tavrida | (07h 28m 30.97s , +26d 08m 26.4s) | C | 60 | 17.5 |\n 9714 | 2023-11-06 20:54:47 | MASTER-Tavrida | (07h 37m 30.51s , +26d 07m 36.6s) | C | 60 | 17.3 |\n 9788 | 2023-11-06 20:56:01 | MASTER-Tavrida | (07h 21m 38.45s , +24d 12m 21.0s) | C | 60 | 17.4 |\n 9861 | 2023-11-06 20:57:14 | MASTER-Tavrida | (07h 30m 29.86s , +24d 12m 54.8s) | C | 60 | 17.0 |\n 9935 | 2023-11-06 20:58:28 | MASTER-Tavrida | (07h 27m 01.91s , +29d 55m 58.0s) | C | 60 | 18.5 |\n 10007 | 2023-11-06 20:59:40 | MASTER-Tavrida | (07h 36m 15.07s , +29d 54m 58.4s) | C | 60 | 18.2 |\n 10159 | 2023-11-06 21:02:12 | MASTER-Tavrida | (07h 24m 04.95s , +22d 19m 29.7s) | C | 60 | 17.1 |\n 10234 | 2023-11-06 21:03:27 | MASTER-Tavrida | (07h 36m 06.69s , +28d 02m 41.0s) | C | 60 | 18.2 |\n 10306 | 2023-11-06 21:04:39 | MASTER-Tavrida | (07h 45m 14.82s , +28d 01m 51.3s) | C | 60 | 17.7 |\n 10379 | 2023-11-06 21:05:52 | MASTER-Tavrida | (07h 38m 17.32s , +24d 12m 47.6s) | C | 60 | 17.3 |\n 10452 | 2023-11-06 21:07:05 | MASTER-Tavrida | (07h 47m 07.78s , +24d 13m 19.4s) | C | 60 | 16.2 |\n 10526 | 2023-11-06 21:08:19 | MASTER-Tavrida | (07h 18m 57.19s , +28d 02m 21.1s) | C | 60 | 18.3 |\n 11903 | 2023-11-06 21:31:16 | MASTER-Tavrida | (07h 27m 56.23s , +28d 02m 55.0s) | C | 60 | 18.3 |\n 11975 | 2023-11-06 21:32:28 | MASTER-Tavrida | (07h 11m 40.50s , +26d 07m 34.7s) | C | 60 | 18.6 |\n 12048 | 2023-11-06 21:33:41 | MASTER-Tavrida | (07h 20m 28.35s , +26d 06m 44.0s) | C | 60 | 18.5 |\n 12121 | 2023-11-06 21:34:54 | MASTER-Tavrida | (07h 31m 55.79s , +22d 19m 23.2s) | C | 60 | 18.1 |\n 12193 | 2023-11-06 21:36:06 | MASTER-Tavrida | (07h 40m 32.06s , +22d 21m 04.8s) | C | 60 | 18.2 |\n 12266 | 2023-11-06 21:37:19 | MASTER-Tavrida | (07h 37m 26.81s , +26d 07m 27.4s) | C | 60 | 18.7 |\n 12338 | 2023-11-06 21:38:31 | MASTER-Tavrida | (07h 30m 29.80s , +24d 14m 40.3s) | C | 60 | 18.5 |\n 12411 | 2023-11-06 21:39:44 | MASTER-Tavrida | (07h 26m 57.61s , +29d 55m 51.6s) | C | 60 | 18.9 |\n 12483 | 2023-11-06 21:40:56 | MASTER-Tavrida | (07h 36m 10.40s , +29d 57m 03.1s) | C | 60 | 18.7 |\n 12628 | 2023-11-06 21:43:21 | MASTER-Tavrida | (07h 24m 02.93s , +22d 18m 52.3s) | C | 60 | 18.3 |\n 12702 | 2023-11-06 21:44:35 | MASTER-Tavrida | (07h 45m 14.98s , +28d 01m 29.2s) | C | 60 | 18.8 |\n 12774 | 2023-11-06 21:45:47 | MASTER-Tavrida | (07h 47m 05.00s , +24d 15m 07.1s) | C | 60 | 18.5 |\n 12848 | 2023-11-06 21:47:00 | MASTER-Tavrida | (07h 27m 58.96s , +28d 01m 19.4s) | C | 60 | 18.9 |\n 13142 | 2023-11-06 21:51:54 | MASTER-Tavrida | (07h 20m 26.86s , +26d 08m 02.8s) | C | 60 | 19.0 |\n 13215 | 2023-11-06 21:53:08 | MASTER-Tavrida | (07h 40m 28.08s , +22d 21m 25.6s) | C | 60 | 18.7 |\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/34959.",
"published": "2023-11-06T22:01:31.096443Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2023-11-06T22:01:31.096463Z",
"modified": "2023-11-06T22:01:31.104157Z",
"nonlocalizedevents": [],
"targets": []
},
{
"id": 6862,
"topic": "gcn.circular",
"uuid": "5ab3ccf3-601b-4f21-bd76-6f163a54672c",
"title": "LIGO/Virgo/KAGRA S240422ed: GW-MMADS DECam observations",
"submitter": "Hop gcn.circular",
"authors": "Igor Andreoni at JSI/UMD/NASA <igor.andreoni@gmail.com>",
"data": {
"date": "24/04/23 06:14:10 GMT",
"from": "Igor Andreoni at JSI/UMD/NASA <igor.andreoni@gmail.com>",
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/36245"
},
"title": "GCN CIRCULAR",
"number": "36245",
"subject": "LIGO/Virgo/KAGRA S240422ed: GW-MMADS DECam observations"
},
"message_text": "Antonella Palmese (CMU), Lei Hu (CMU), Tomás Cabrera (CMU), Brendan O'Connor (CMU), Keerthi Kunnumkai (CMU), Igor Andreoni (UMD) report on behalf of the GW-MMADS team:\n\nWe observed the high probability area of the LVK gravitational wave candidate S240422ed (GCN 36236, GCN 36240) using the wide-field Dark Energy Camera (DECam) on the 4m Blanco telescope, as part of the Gravitational Wave Multi-Messenger Astronomy DECam Survey (GW-MMADS; PI: Andreoni & Palmese). Observations were carried out between 2023-04-22 23:37 and 2024-04-23 03:40 UTC in r and z band using 60s exposures.\n\nOur pointings have been reported to the TreasureMap (Wyatt et al., 2020): https://treasuremap.space/alerts?graceids=S240422ed\n\nData reduction is underway.\n\nWe thank the CTIO and NOIRLab staff for supporting these observations and the data calibrations.\n\n\nView this GCN Circular online at https://gcn.nasa.gov/circulars/36245.",
"published": "2024-04-23T06:14:25.651139Z",
"message_parser": "GCN Circular Parser v1",
"retracted": false,
"created": "2024-04-23T06:14:25.651154Z",
"modified": "2024-04-23T06:14:25.657103Z",
"nonlocalizedevents": [
{
"event_id": "S240422e"
}
],
"targets": []
}
]
}
