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"duration": null,
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},
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},
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},
"alert_type": "PRELIMINARY",
"sequence_num": 1,
"time_created": "2025-11-16T23:22:46Z",
"superevent_id": "S251116en",
"external_coinc": null
},
"message_text": "",
"published": "2025-11-16T23:28:35.746791Z",
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"retracted": false,
"created": "2025-11-16T23:28:35.746819Z",
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{
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"message": {
"id": 5799946,
"topic": "igwn.gwalert",
"uuid": "3853eb7d-e3a3-4cf4-864e-f1cc344be0ea",
"title": "S251116en - PRELIMINARY",
"submitter": "cody.messick-30d512c8",
"authors": "LVK",
"data": {
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},
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],
"significant": true,
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"Terrestrial": 1.830139914937856e-05
},
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"central_frequency": null
},
"alert_type": "PRELIMINARY",
"sequence_num": 2,
"time_created": "2025-11-16T23:27:20Z",
"superevent_id": "S251116en",
"external_coinc": null
},
"message_text": "",
"published": "2025-11-16T23:29:27.059898Z",
"message_parser": "IGWN Alert Avro Parser v1",
"retracted": false,
"created": "2025-11-16T23:29:27.059924Z",
"modified": "2025-11-16T23:29:27.116460Z"
}
},
{
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"sequence_number": 3,
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"message": {
"id": 5799982,
"topic": "igwn.gwalert",
"uuid": "4ad74580-450e-4aad-abaa-1687b5acd31e",
"title": "S251116en - INITIAL",
"submitter": "cody.messick-30d512c8",
"authors": "LVK",
"data": {
"urls": {
"skymap": "https://gracedb.ligo.org/api/superevents/S251116en/files/bayestar.multiorder.fits,1",
"gracedb": "https://gracedb.ligo.org/superevents/S251116en/view/"
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"event": {
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"time": "2025-11-16T23:22:21.761Z",
"group": "CBC",
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},
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"sequence_num": 3,
"time_created": "2025-11-16T23:52:30Z",
"superevent_id": "S251116en",
"external_coinc": null
},
"message_text": "",
"published": "2025-11-16T23:54:21.359398Z",
"message_parser": "IGWN Alert Avro Parser v1",
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"modified": "2025-11-16T23:54:21.380229Z"
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"references": [
{
"id": 5799985,
"topic": "gcn.circulars",
"uuid": "012b5579-04c5-436f-83b0-a3fcc604d94b",
"title": "LIGO/Virgo/KAGRA S251116en: Identification of a GW compact binary merger candidate",
"submitter": "Jyotirmaya Mohanta at University of Tsukuba <s2430161@u.tsukuba.ac.jp>",
"authors": "Jyotirmaya Mohanta at University of Tsukuba <s2430161@u.tsukuba.ac.jp>",
"data": {
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/42708"
},
"format": "text/plain",
"$schema": "https://gcn.nasa.gov/schema/v6.0.0/gcn/circulars.schema.json",
"eventId": "LIGO/Virgo/KAGRA S251116en",
"subject": "LIGO/Virgo/KAGRA S251116en: Identification of a GW compact binary merger candidate",
"createdOn": 1763337899432,
"submitter": "Jyotirmaya Mohanta at University of Tsukuba <s2430161@u.tsukuba.ac.jp>",
"circularId": 42708,
"submittedHow": "web"
},
"message_text": "The LIGO Scientific Collaboration, the Virgo Collaboration, and the KAGRA Collaboration report:\n\nWe identified the compact binary merger candidate S251116en during real-time processing of data from LIGO Hanford Observatory (H1) and LIGO Livingston Observatory (L1) at 2025-11-16 23:22:21.761 UTC (GPS time: 1447370559.761). The candidate was found by the Aframe [1], cWB [2], cWB BBH [3], GstLAL [4], MBTA [5], MLy [6], PyCBC Live [7], and SPIIR [8] analysis pipelines.\n\nS251116en is an event of interest because its false alarm rate, as estimated by the online analysis, is 1.3e-12 Hz, or about one in 1e4 years. The event's properties can be found at this URL:\n\nhttps://gracedb.ligo.org/superevents/S251116en\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 at least one of the compact objects is consistent with a neutron star mass (HasNS) is <1%. [9] Using the masses and spins inferred from the signal, the probability of matter outside the final compact object (HasRemnant) is <1%. [9] Both HasNS and HasRemnant consider the support of several neutron star equations of state for maximum neutron star mass. The probability that either of the binary components lies between 3 and 5 solar masses (HasMassGap) is <1%.\n\nThe source chirp mass falls with highest probability in the bin (22.0, 44.0) solar masses, assuming the candidate is astrophysical in origin.\n\nTwo sky maps are available at this time and can be retrieved from the GraceDB event page:\n * amplfi.multiorder.fits,0, an initial localization generated by AMPLFI [10], distributed via GCN and SCiMMA notices about 25 seconds after the candidate event time.\n * bayestar.multiorder.fits,0, an initial localization generated by BAYESTAR [11], distributed via GCN and SCiMMA notices about 4 minutes after the candidate event time.\n\nThe preferred sky map at this time is bayestar.multiorder.fits,0. For the bayestar.multiorder.fits,0 sky map, the 90% credible region is 788 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 1741 +/- 490 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/.\n\n [1] Marx et al. PRD 111, 042010 (2025) doi:10.1103/PhysRevD.111.042010\n [2] Klimenko et al. PRD 93, 042004 (2016) doi:10.1103/PhysRevD.93.042004\n [3] T. Mishra et al. PRD 105, 083018 (2022) doi:10.1103/PhysRevD.105.083018\n [4] Tsukada et al. PRD 108, 043004 (2023) doi:10.1103/PhysRevD.108.043004 and Ewing et al. PRD 109, 042008 (2024) doi:10.1103/PhysRevD.109.042008\n [5] Alléné et al. CQG 42, 105009 (2025) doi:10.1088/1361-6382/add234\n [6] Skliris et al. PRD 110, 104034 (2024) doi:10.1103/PhysRevD.110.104034\n [7] Dal Canton et al. ApJ 923, 254 (2021) doi:10.3847/1538-4357/ac2f9a\n [8] Chu et al. PRD 105, 024023 (2022) doi:10.1103/PhysRevD.105.024023\n [9] Chatterjee et al. ApJ 896, 54 (2020) doi:10.3847/1538-4357/ab8dbe\n [10] Chatterjee et al. MLST 5, 045030 (2024) doi:10.1088/2632-2153/ad8982\n [11] Singer & Price PRD 93, 024013 (2016) doi:10.1103/PhysRevD.93.024013\n",
"published": "2025-11-17T00:05:06.759072Z",
"message_parser": "GCN Circular Parser v2",
"retracted": false,
"created": "2025-11-17T00:05:06.759091Z",
"modified": "2025-11-17T00:05:06.787540Z",
"targets": []
}
]
},
{
"event_id": "141518_18513107",
"sequences": [
{
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"message": {
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"topic": "gcn.classic.text.ICECUBE_ASTROTRACK_BRONZE",
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"title": "GCN/AMON NOTICE",
"submitter": "",
"authors": "",
"data": {
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"title": "GCN/AMON NOTICE",
"energy": "1.1337e+02 [TeV]",
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"comments": "IceCube Bronze event.\nThe position error is statistical only, there is no systematic added.",
"revision": "0",
"sun_dist": "69.21 [deg] Sun_angle= 4.3 [hr] (West of Sun)",
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"sun_postn": "210.21d {+14h 00m 51s} -12.30d {-12d 18' 15\"}",
"ecl_coords": "142.84, 1.51 [deg] ecliptic lon,lat of the event",
"gal_coords": "218.08, 44.76 [deg] galactic lon,lat of the event",
"moon_postn": "254.97d {+16h 59m 53s} -27.87d {-27d 52' 27\"}",
"signalness": "3.4222e-01 [dn]",
"notice_date": "Sat 25 Oct 25 13:48:32 UT",
"notice_type": "ICECUBE Astrotrack Bronze",
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"discovery_date": "20973 TJD; 298 DOY; 25/10/25 (yy/mm/dd)",
"discovery_time": "49673 SOD {13:47:53.26} UT"
},
"message_text": "TITLE: GCN/AMON NOTICE\nNOTICE_DATE: Sat 25 Oct 25 13:48:32 UT\nNOTICE_TYPE: ICECUBE Astrotrack Bronze \nSTREAM: 25\nRUN_NUM: 141518\nEVENT_NUM: 18513107\nSRC_RA: 145.6970d {+09h 42m 47s} (J2000),\n 146.0498d {+09h 44m 12s} (current),\n 145.0128d {+09h 40m 03s} (1950)\nSRC_DEC: +15.3302d {+15d 19' 49\"} (J2000),\n +15.2112d {+15d 12' 40\"} (current),\n +15.5592d {+15d 33' 33\"} (1950)\nSRC_ERROR: 71.21 [arcmin radius, stat-only, 90% containment]\nSRC_ERROR50: 27.74 [arcmin radius, stat-only, 50% containment]\nDISCOVERY_DATE: 20973 TJD; 298 DOY; 25/10/25 (yy/mm/dd)\nDISCOVERY_TIME: 49673 SOD {13:47:53.26} UT\nREVISION: 0\nENERGY: 1.1337e+02 [TeV]\nSIGNALNESS: 3.4222e-01 [dn]\nFAR: 2.3507 [yr^-1]\nSUN_POSTN: 210.21d {+14h 00m 51s} -12.30d {-12d 18' 15\"}\nSUN_DIST: 69.21 [deg] Sun_angle= 4.3 [hr] (West of Sun)\nMOON_POSTN: 254.97d {+16h 59m 53s} -27.87d {-27d 52' 27\"}\nMOON_DIST: 113.53 [deg]\nGAL_COORDS: 218.08, 44.76 [deg] galactic lon,lat of the event\nECL_COORDS: 142.84, 1.51 [deg] ecliptic lon,lat of the event\nCOMMENTS: IceCube Bronze event. \nCOMMENTS: The position error is statistical only, there is no systematic added. \n",
"published": "2025-10-25T13:48:32Z",
"message_parser": "Icecube Notice Plaintext Parser v1",
"retracted": false,
"created": "2025-10-25T13:48:33.530301Z",
"modified": "2025-10-25T13:48:33.538571Z"
}
},
{
"id": 10984,
"sequence_number": 1,
"sequence_type": "UPDATE",
"message": {
"id": 5791187,
"topic": "gcn.classic.text.ICECUBE_ASTROTRACK_BRONZE",
"uuid": "d4d96a70-a9e4-4cfb-9280-b93200d29775",
"title": "GCN/AMON NOTICE",
"submitter": "",
"authors": "",
"data": {
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"urls": {
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},
"title": "GCN/AMON NOTICE",
"energy": "1.1337e+02 [TeV]",
"src_ra": "145.6299d {+09h 42m 31s} (J2000),\n145.9823d {+09h 43m 56s} (current),\n144.9464d {+09h 39m 47s} (1950)",
"stream": "25",
"run_num": "141518",
"src_dec": "+15.0600d {+15d 03' 36\"} (J2000),\n+14.9411d {+14d 56' 28\"} (current),\n+15.2889d {+15d 17' 20\"} (1950)",
"comments": "IceCube Bronze event.\nThe position error is statistical only, there is no systematic added.",
"revision": "1",
"sun_dist": "69.23 [deg] Sun_angle= 4.3 [hr] (West of Sun)",
"event_num": "18513107",
"moon_dist": "114.06 [deg]",
"src_error": "45.60 [arcmin radius, stat-only, 90% containment]",
"sun_postn": "210.26d {+14h 01m 02s} -12.32d {-12d 19' 16\"}",
"ecl_coords": "142.87, 1.23 [deg] ecliptic lon,lat of the event",
"gal_coords": "218.39, 44.59 [deg] galactic lon,lat of the event",
"moon_postn": "255.63d {+17h 02m 31s} -27.93d {-27d 56' 02\"}",
"signalness": "3.4222e-01 [dn]",
"notice_date": "Sat 25 Oct 25 14:59:32 UT",
"notice_type": "ICECUBE Astrotrack Bronze",
"src_error50": "24.59 [arcmin radius, stat-only, 50% containment]",
"discovery_date": "20973 TJD; 298 DOY; 25/10/25 (yy/mm/dd)",
"discovery_time": "49673 SOD {13:47:53.26} UT"
},
"message_text": "TITLE: GCN/AMON NOTICE\nNOTICE_DATE: Sat 25 Oct 25 14:59:32 UT\nNOTICE_TYPE: ICECUBE Astrotrack Bronze \nSTREAM: 25\nRUN_NUM: 141518\nEVENT_NUM: 18513107\nSRC_RA: 145.6299d {+09h 42m 31s} (J2000),\n 145.9823d {+09h 43m 56s} (current),\n 144.9464d {+09h 39m 47s} (1950)\nSRC_DEC: +15.0600d {+15d 03' 36\"} (J2000),\n +14.9411d {+14d 56' 28\"} (current),\n +15.2889d {+15d 17' 20\"} (1950)\nSRC_ERROR: 45.60 [arcmin radius, stat-only, 90% containment]\nSRC_ERROR50: 24.59 [arcmin radius, stat-only, 50% containment]\nDISCOVERY_DATE: 20973 TJD; 298 DOY; 25/10/25 (yy/mm/dd)\nDISCOVERY_TIME: 49673 SOD {13:47:53.26} UT\nREVISION: 1\nENERGY: 1.1337e+02 [TeV]\nSIGNALNESS: 3.4222e-01 [dn]\nFAR: 2.3507 [yr^-1]\nSUN_POSTN: 210.26d {+14h 01m 02s} -12.32d {-12d 19' 16\"}\nSUN_DIST: 69.23 [deg] Sun_angle= 4.3 [hr] (West of Sun)\nMOON_POSTN: 255.63d {+17h 02m 31s} -27.93d {-27d 56' 02\"}\nMOON_DIST: 114.06 [deg]\nGAL_COORDS: 218.39, 44.59 [deg] galactic lon,lat of the event\nECL_COORDS: 142.87, 1.23 [deg] ecliptic lon,lat of the event\nCOMMENTS: IceCube Bronze event. \nCOMMENTS: The position error is statistical only, there is no systematic added. \n",
"published": "2025-10-25T14:59:32Z",
"message_parser": "Icecube Notice Plaintext Parser v1",
"retracted": false,
"created": "2025-10-25T14:59:33.002485Z",
"modified": "2025-10-25T14:59:33.014113Z"
}
}
],
"references": [
{
"id": 5791187,
"topic": "gcn.classic.text.ICECUBE_ASTROTRACK_BRONZE",
"uuid": "d4d96a70-a9e4-4cfb-9280-b93200d29775",
"title": "GCN/AMON NOTICE",
"submitter": "",
"authors": "",
"data": {
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"urls": {
"gcn": "https://gcn.gsfc.nasa.gov/notices_amon_g_b/141518_18513107.amon"
},
"title": "GCN/AMON NOTICE",
"energy": "1.1337e+02 [TeV]",
"src_ra": "145.6299d {+09h 42m 31s} (J2000),\n145.9823d {+09h 43m 56s} (current),\n144.9464d {+09h 39m 47s} (1950)",
"stream": "25",
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"src_dec": "+15.0600d {+15d 03' 36\"} (J2000),\n+14.9411d {+14d 56' 28\"} (current),\n+15.2889d {+15d 17' 20\"} (1950)",
"comments": "IceCube Bronze event.\nThe position error is statistical only, there is no systematic added.",
"revision": "1",
"sun_dist": "69.23 [deg] Sun_angle= 4.3 [hr] (West of Sun)",
"event_num": "18513107",
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"moon_postn": "255.63d {+17h 02m 31s} -27.93d {-27d 56' 02\"}",
"signalness": "3.4222e-01 [dn]",
"notice_date": "Sat 25 Oct 25 14:59:32 UT",
"notice_type": "ICECUBE Astrotrack Bronze",
"src_error50": "24.59 [arcmin radius, stat-only, 50% containment]",
"discovery_date": "20973 TJD; 298 DOY; 25/10/25 (yy/mm/dd)",
"discovery_time": "49673 SOD {13:47:53.26} UT"
},
"message_text": "TITLE: GCN/AMON NOTICE\nNOTICE_DATE: Sat 25 Oct 25 14:59:32 UT\nNOTICE_TYPE: ICECUBE Astrotrack Bronze \nSTREAM: 25\nRUN_NUM: 141518\nEVENT_NUM: 18513107\nSRC_RA: 145.6299d {+09h 42m 31s} (J2000),\n 145.9823d {+09h 43m 56s} (current),\n 144.9464d {+09h 39m 47s} (1950)\nSRC_DEC: +15.0600d {+15d 03' 36\"} (J2000),\n +14.9411d {+14d 56' 28\"} (current),\n +15.2889d {+15d 17' 20\"} (1950)\nSRC_ERROR: 45.60 [arcmin radius, stat-only, 90% containment]\nSRC_ERROR50: 24.59 [arcmin radius, stat-only, 50% containment]\nDISCOVERY_DATE: 20973 TJD; 298 DOY; 25/10/25 (yy/mm/dd)\nDISCOVERY_TIME: 49673 SOD {13:47:53.26} UT\nREVISION: 1\nENERGY: 1.1337e+02 [TeV]\nSIGNALNESS: 3.4222e-01 [dn]\nFAR: 2.3507 [yr^-1]\nSUN_POSTN: 210.26d {+14h 01m 02s} -12.32d {-12d 19' 16\"}\nSUN_DIST: 69.23 [deg] Sun_angle= 4.3 [hr] (West of Sun)\nMOON_POSTN: 255.63d {+17h 02m 31s} -27.93d {-27d 56' 02\"}\nMOON_DIST: 114.06 [deg]\nGAL_COORDS: 218.39, 44.59 [deg] galactic lon,lat of the event\nECL_COORDS: 142.87, 1.23 [deg] ecliptic lon,lat of the event\nCOMMENTS: IceCube Bronze event. \nCOMMENTS: The position error is statistical only, there is no systematic added. \n",
"published": "2025-10-25T14:59:32Z",
"message_parser": "Icecube Notice Plaintext Parser v1",
"retracted": false,
"created": "2025-10-25T14:59:33.002485Z",
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{
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"declination": 15.06,
"declination_sexagesimal": "15:03:36"
}
]
},
{
"id": 5791174,
"topic": "gcn.classic.text.ICECUBE_ASTROTRACK_BRONZE",
"uuid": "5ee3bcb5-8cd0-4af8-8a54-198b3c3fdb6f",
"title": "GCN/AMON NOTICE",
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"authors": "",
"data": {
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"title": "GCN/AMON NOTICE",
"energy": "1.1337e+02 [TeV]",
"src_ra": "145.6970d {+09h 42m 47s} (J2000),\n146.0498d {+09h 44m 12s} (current),\n145.0128d {+09h 40m 03s} (1950)",
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"comments": "IceCube Bronze event.\nThe position error is statistical only, there is no systematic added.",
"revision": "0",
"sun_dist": "69.21 [deg] Sun_angle= 4.3 [hr] (West of Sun)",
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{
"id": 5792310,
"topic": "gcn.circulars",
"uuid": "43f76abf-9fc4-4aac-a038-ec74ccc48b51",
"title": "LIGO/Virgo/KAGRA S251018bi: Identification of a GW compact binary merger candidate",
"submitter": "shoki.iwaguchi@ligo.org",
"authors": "shoki.iwaguchi@ligo.org",
"data": {
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"bibcode": "2025GCN.42357....1L",
"eventId": "LIGO/Virgo/KAGRA S251018bi",
"subject": "LIGO/Virgo/KAGRA S251018bi: Identification of a GW compact binary merger candidate",
"createdOn": 1760803511626,
"submitter": "shoki.iwaguchi@ligo.org",
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"message_text": "The LIGO Scientific Collaboration, the Virgo Collaboration, and the KAGRA Collaboration report:\n\nWe identified the compact binary merger candidate S251018bi during real-time processing of data from LIGO Hanford Observatory (H1), LIGO Livingston Observatory (L1), and Virgo Observatory (V1) at 2025-10-18 15:25:47.021 UTC (GPS time: 1444836365.021). The candidate was found by the Aframe [1], cWB [2], cWB BBH [3], GstLAL [4], MBTA [5], PyCBC Live [6], and SPIIR [7] analysis pipelines.\n\nS251018bi 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/S251018bi\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 at least one of the compact objects is consistent with a neutron star mass (HasNS) is <1%. [8] Using the masses and spins inferred from the signal, the probability of matter outside the final compact object (HasRemnant) is <1%. [8] Both HasNS and HasRemnant consider the support of several neutron star equations of state for maximum neutron star mass. The probability that either of the binary components lies between 3 and 5 solar masses (HasMassGap) is <1%.\n\nThe source chirp mass falls with highest probability in the bin (22.0, 44.0) solar masses, assuming the candidate is astrophysical in origin.\n\nTwo sky maps are available at this time and can be retrieved from the GraceDB event page:\n * amplfi.multiorder.fits,0, an initial localization generated by AMPLFI [9], distributed via GCN and SCiMMA notices about 23 seconds after the candidate event time.\n * bayestar.multiorder.fits,0, an initial localization generated by BAYESTAR [10], distributed via GCN and SCiMMA notices about 5 minutes after the candidate event time.\n\nThe preferred sky map at this time is bayestar.multiorder.fits,0. For the bayestar.multiorder.fits,0 sky map, the 90% credible region is 1463 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 5450 +/- 1489 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/.\n\n [1] Marx et al. PRD 111, 042010 (2025) doi:10.1103/PhysRevD.111.042010\n [2] Klimenko et al. PRD 93, 042004 (2016) doi:10.1103/PhysRevD.93.042004\n [3] T. Mishra et al. PRD 105, 083018 (2022) doi:10.1103/PhysRevD.105.083018\n [4] Tsukada et al. PRD 108, 043004 (2023) doi:10.1103/PhysRevD.108.043004 and Ewing et al. PRD 109, 042008 (2024) doi:10.1103/PhysRevD.109.042008\n [5] Alléné et al. CQG 42, 105009 (2025) doi:10.1088/1361-6382/add234\n [6] Dal Canton et al. ApJ 923, 254 (2021) doi:10.3847/1538-4357/ac2f9a\n [7] Chu et al. PRD 105, 024023 (2022) doi:10.1103/PhysRevD.105.024023\n [8] Chatterjee et al. ApJ 896, 54 (2020) doi:10.3847/1538-4357/ab8dbe\n [9] Chatterjee et al. MLST 5, 045030 (2024) doi:10.1088/2632-2153/ad8982\n [10] Singer & Price PRD 93, 024013 (2016) doi:10.1103/PhysRevD.93.024013",
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{
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"uuid": "7c328b33-188c-4ceb-8c46-33f8866b9981",
"title": "LIGO/Virgo/KAGRA S251018bi: Updated Sky localization",
"submitter": "Nihar.Gupte@aei.mpg.de",
"authors": "Nihar.Gupte@aei.mpg.de",
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"bibcode": "2025GCN.42372....1L",
"eventId": "LIGO/Virgo/KAGRA S251018bi",
"subject": "LIGO/Virgo/KAGRA S251018bi: Updated Sky localization",
"createdOn": 1760990294934,
"submitter": "Nihar.Gupte@aei.mpg.de",
"circularId": 42372,
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"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), LIGO Livingston Observatory (L1), and Virgo Observatory (V1) data around the time of the compact binary merger (CBC) candidate S251018bi (GCN Circular 42357). Parameter estimation has been performed using Bilby [1] and a new sky map, Bilby.multiorder.fits,0, distributed via GCN and SCiMMA notices, is available for retrieval from the GraceDB event page:\n\nhttps://gracedb.ligo.org/superevents/S251018bi\n\nFor the Bilby.multiorder.fits,0 sky map, the 90% credible region is 883 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 4502 +/- 1313 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/.\n\n [1] Ashton et al. ApJS 241, 27 (2019) doi:10.3847/1538-4365/ab06fc and Morisaki et al. PRD 108, 123040 (2023) doi:10.1103/PhysRevD.108.123040",
"published": "2025-11-03T08:10:29.134138Z",
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{
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"title": "LIGO/Virgo/KAGRA S251018bi: Updated Sky localization",
"submitter": "Nihar.Gupte@aei.mpg.de",
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"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), LIGO Livingston Observatory (L1), and Virgo Observatory (V1) data around the time of the compact binary merger (CBC) candidate S251018bi (GCN Circular 42357). Parameter estimation has been performed using Bilby [1] and a new sky map, Bilby.multiorder.fits,0, distributed via GCN and SCiMMA notices, is available for retrieval from the GraceDB event page:\n\nhttps://gracedb.ligo.org/superevents/S251018bi\n\nFor the Bilby.multiorder.fits,0 sky map, the 90% credible region is 883 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 4502 +/- 1313 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/.\n\n [1] Ashton et al. ApJS 241, 27 (2019) doi:10.3847/1538-4365/ab06fc and Morisaki et al. PRD 108, 123040 (2023) doi:10.1103/PhysRevD.108.123040",
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{
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"uuid": "737e75e4-13e0-4552-993d-8828afe6a07a",
"title": "LIGO/Virgo/KAGRA S251018bi: Identification of a GW compact binary merger candidate",
"submitter": "shoki.iwaguchi@ligo.org",
"authors": "shoki.iwaguchi@ligo.org",
"data": {
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"eventId": "LIGO/Virgo/KAGRA S251018bi",
"subject": "LIGO/Virgo/KAGRA S251018bi: Identification of a GW compact binary merger candidate",
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"message_text": "The LIGO Scientific Collaboration, the Virgo Collaboration, and the KAGRA Collaboration report:\n\nWe identified the compact binary merger candidate S251018bi during real-time processing of data from LIGO Hanford Observatory (H1), LIGO Livingston Observatory (L1), and Virgo Observatory (V1) at 2025-10-18 15:25:47.021 UTC (GPS time: 1444836365.021). The candidate was found by the Aframe [1], cWB [2], cWB BBH [3], GstLAL [4], MBTA [5], PyCBC Live [6], and SPIIR [7] analysis pipelines.\n\nS251018bi 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/S251018bi\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 at least one of the compact objects is consistent with a neutron star mass (HasNS) is <1%. [8] Using the masses and spins inferred from the signal, the probability of matter outside the final compact object (HasRemnant) is <1%. [8] Both HasNS and HasRemnant consider the support of several neutron star equations of state for maximum neutron star mass. The probability that either of the binary components lies between 3 and 5 solar masses (HasMassGap) is <1%.\n\nThe source chirp mass falls with highest probability in the bin (22.0, 44.0) solar masses, assuming the candidate is astrophysical in origin.\n\nTwo sky maps are available at this time and can be retrieved from the GraceDB event page:\n * amplfi.multiorder.fits,0, an initial localization generated by AMPLFI [9], distributed via GCN and SCiMMA notices about 23 seconds after the candidate event time.\n * bayestar.multiorder.fits,0, an initial localization generated by BAYESTAR [10], distributed via GCN and SCiMMA notices about 5 minutes after the candidate event time.\n\nThe preferred sky map at this time is bayestar.multiorder.fits,0. For the bayestar.multiorder.fits,0 sky map, the 90% credible region is 1463 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 5450 +/- 1489 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/.\n\n [1] Marx et al. PRD 111, 042010 (2025) doi:10.1103/PhysRevD.111.042010\n [2] Klimenko et al. PRD 93, 042004 (2016) doi:10.1103/PhysRevD.93.042004\n [3] T. Mishra et al. PRD 105, 083018 (2022) doi:10.1103/PhysRevD.105.083018\n [4] Tsukada et al. PRD 108, 043004 (2023) doi:10.1103/PhysRevD.108.043004 and Ewing et al. PRD 109, 042008 (2024) doi:10.1103/PhysRevD.109.042008\n [5] Alléné et al. CQG 42, 105009 (2025) doi:10.1088/1361-6382/add234\n [6] Dal Canton et al. ApJ 923, 254 (2021) doi:10.3847/1538-4357/ac2f9a\n [7] Chu et al. PRD 105, 024023 (2022) doi:10.1103/PhysRevD.105.024023\n [8] Chatterjee et al. ApJ 896, 54 (2020) doi:10.3847/1538-4357/ab8dbe\n [9] Chatterjee et al. MLST 5, 045030 (2024) doi:10.1088/2632-2153/ad8982\n [10] Singer & Price PRD 93, 024013 (2016) doi:10.1103/PhysRevD.93.024013",
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]
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{
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{
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"message": {
"id": 5800025,
"topic": "igwn.gwalert",
"uuid": "d97959dd-1586-4bbc-8d5d-7e723b3b7a04",
"title": "S251117z - PRELIMINARY",
"submitter": "cody.messick-30d512c8",
"authors": "LVK",
"data": {
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"time": "2025-11-17T03:38:38.813Z",
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"area_50": 530.2237603621547,
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"time_created": "2025-11-17T03:39:17Z",
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},
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"published": "2025-11-17T03:39:18.342621Z",
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{
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"message": {
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"topic": "igwn.gwalert",
"uuid": "90fa34c1-b1cc-4137-9f5f-a7899bff2288",
"title": "S251117z - PRELIMINARY",
"submitter": "cody.messick-30d512c8",
"authors": "LVK",
"data": {
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"time_created": "2025-11-17T03:43:50Z",
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],
"references": []
},
{
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"sequences": [],
"references": [
{
"id": 5792362,
"topic": "gcn.circulars",
"uuid": "6fb3fc3b-4390-437f-b330-abfa47893baf",
"title": "LIGO/Virgo/KAGRA S251017di: Retraction of GW compact binary merger candidate",
"submitter": "shoki.iwaguchi@ligo.org",
"authors": "shoki.iwaguchi@ligo.org",
"data": {
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"bibcode": "2025GCN.42337....1L",
"eventId": "LIGO/Virgo/KAGRA S251017di",
"subject": "LIGO/Virgo/KAGRA S251017di: Retraction of GW compact binary merger candidate",
"createdOn": 1760737125760,
"submitter": "shoki.iwaguchi@ligo.org",
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},
"message_text": "The LIGO Scientific Collaboration, the Virgo Collaboration, and the KAGRA Collaboration report:\n\nThe trigger S251017di is no longer considered to be a candidate of interest. This candidate was initially identified by one or more early-warning analyses by matching partial signal templates to the data. Analysis of additional data up to the putative merger time, with full signal templates, did not make a significant detection, indicating that the initial candidate was likely due to transient noise.",
"published": "2025-11-03T08:10:43.703617Z",
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"created": "2025-11-03T08:10:43.703639Z",
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{
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"topic": "gcn.circulars",
"uuid": "39dda453-89bd-456e-ac9f-f9a7fb63260e",
"title": "LIGO/Virgo/KAGRA S251017di: Retraction of GW compact binary merger candidate",
"submitter": "shoki.iwaguchi@ligo.org",
"authors": "shoki.iwaguchi@ligo.org",
"data": {
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"subject": "LIGO/Virgo/KAGRA S251017di: Retraction of GW compact binary merger candidate",
"createdOn": 1760737125760,
"submitter": "shoki.iwaguchi@ligo.org",
"circularId": 42337,
"submittedHow": "web"
},
"message_text": "The LIGO Scientific Collaboration, the Virgo Collaboration, and the KAGRA Collaboration report:\n\nThe trigger S251017di is no longer considered to be a candidate of interest. This candidate was initially identified by one or more early-warning analyses by matching partial signal templates to the data. Analysis of additional data up to the putative merger time, with full signal templates, did not make a significant detection, indicating that the initial candidate was likely due to transient noise.",
"published": "2025-10-17T21:38:54.470490Z",
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"retracted": false,
"created": "2025-10-17T21:38:54.470556Z",
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"sequences": [],
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{
"id": 5792401,
"topic": "gcn.circulars",
"uuid": "7258c8a6-8aeb-400e-a1ca-8e95c2097d3f",
"title": "LIGO/Virgo/KAGRA S251021u: Updated Sky localization",
"submitter": "mattia.emma.2022@live.rhul.ac.uk",
"authors": "mattia.emma.2022@live.rhul.ac.uk",
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"bibcode": "2025GCN.42375....1L",
"eventId": "LIGO/Virgo/KAGRA S251021u",
"subject": "LIGO/Virgo/KAGRA S251021u: Updated Sky localization",
"createdOn": 1761063504891,
"submitter": "mattia.emma.2022@live.rhul.ac.uk",
"circularId": 42375,
"submittedHow": "web"
},
"message_text": "\n\nThe 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 S251021u (GCN Circular 42373). Parameter estimation has been performed using Bilby [1] and a new sky map, Bilby.multiorder.fits,0, distributed via GCN and SCiMMA notices, is available for retrieval from the GraceDB event page:\n\nhttps://gracedb.ligo.org/superevents/S251021u\n\nFor the Bilby.multiorder.fits,0 sky map, the 90% credible region is 3859 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 5884 +/- 2089 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/.\n\n [1] Ashton et al. ApJS 241, 27 (2019) doi:10.3847/1538-4365/ab06fc and Morisaki et al. PRD 108, 123040 (2023) doi:10.1103/PhysRevD.108.123040",
"published": "2025-11-03T08:10:54.149451Z",
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"retracted": false,
"created": "2025-11-03T08:10:54.149480Z",
"modified": "2025-11-03T08:10:54.183390Z",
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},
{
"id": 5792314,
"topic": "gcn.circulars",
"uuid": "96d1806a-77a7-42c3-89e7-b2683b0fdd73",
"title": "LIGO/Virgo/KAGRA S251021u: Identification of a GW compact binary merger candidate",
"submitter": "alvinli@g.ecc.u-tokyo.ac.jp",
"authors": "alvinli@g.ecc.u-tokyo.ac.jp",
"data": {
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},
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"bibcode": "2025GCN.42373....1L",
"eventId": "LIGO/Virgo/KAGRA S251021u",
"subject": "LIGO/Virgo/KAGRA S251021u: Identification of a GW compact binary merger candidate",
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"submitter": "alvinli@g.ecc.u-tokyo.ac.jp",
"circularId": 42373,
"submittedHow": "web"
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"message_text": "The LIGO Scientific Collaboration, the Virgo Collaboration, and the KAGRA Collaboration report:\n\nWe identified the compact binary merger candidate S251021u during real-time processing of data from LIGO Hanford Observatory (H1) and LIGO Livingston Observatory (L1) at 2025-10-21 03:22:15.181 UTC (GPS time: 1445052153.181). The candidate was found by the Aframe [1], cWB [2], cWB BBH [3], GstLAL [4], MBTA [5], PyCBC Live [6], and SPIIR [7] analysis pipelines.\n\nS251021u is an event of interest because its false alarm rate, as estimated by the online analysis, is 2.2e-09 Hz, or about one in 14 years. The event's properties can be found at this URL:\n\nhttps://gracedb.ligo.org/superevents/S251021u\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 at least one of the compact objects is consistent with a neutron star mass (HasNS) is <1%. [8] Using the masses and spins inferred from the signal, the probability of matter outside the final compact object (HasRemnant) is <1%. [8] Both HasNS and HasRemnant consider the support of several neutron star equations of state for maximum neutron star mass. The probability that either of the binary components lies between 3 and 5 solar masses (HasMassGap) is <1%.\n\nThe source chirp mass falls with highest probability in the bin (44.0, 88.0) solar masses, assuming the candidate is astrophysical in origin.\n\nTwo sky maps are available at this time and can be retrieved from the GraceDB event page:\n * amplfi.multiorder.fits,0, an initial localization generated by AMPLFI [9], distributed via GCN and SCiMMA notices about 25 seconds after the candidate event time.\n * bayestar.multiorder.fits,0, an initial localization generated by BAYESTAR [10], distributed via GCN and SCiMMA notices about 4 minutes after the candidate event time.\n\nThe preferred sky map at this time is bayestar.multiorder.fits,0. For the bayestar.multiorder.fits,0 sky map, the 90% credible region is 3742 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 7164 +/- 2185 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/.\n\n [1] Marx et al. PRD 111, 042010 (2025) doi:10.1103/PhysRevD.111.042010\n [2] Klimenko et al. PRD 93, 042004 (2016) doi:10.1103/PhysRevD.93.042004\n [3] T. Mishra et al. PRD 105, 083018 (2022) doi:10.1103/PhysRevD.105.083018\n [4] Tsukada et al. PRD 108, 043004 (2023) doi:10.1103/PhysRevD.108.043004 and Ewing et al. PRD 109, 042008 (2024) doi:10.1103/PhysRevD.109.042008\n [5] Alléné et al. CQG 42, 105009 (2025) doi:10.1088/1361-6382/add234\n [6] Dal Canton et al. ApJ 923, 254 (2021) doi:10.3847/1538-4357/ac2f9a\n [7] Chu et al. PRD 105, 024023 (2022) doi:10.1103/PhysRevD.105.024023\n [8] Chatterjee et al. ApJ 896, 54 (2020) doi:10.3847/1538-4357/ab8dbe\n [9] Chatterjee et al. MLST 5, 045030 (2024) doi:10.1088/2632-2153/ad8982\n [10] Singer & Price PRD 93, 024013 (2016) doi:10.1103/PhysRevD.93.024013",
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"targets": []
},
{
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"topic": "gcn.circulars",
"uuid": "541a8514-1f3e-4a33-9838-c3e9805f849e",
"title": "LIGO/Virgo/KAGRA S251021u: Updated Sky localization",
"submitter": "mattia.emma.2022@live.rhul.ac.uk",
"authors": "mattia.emma.2022@live.rhul.ac.uk",
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},
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},
"message_text": "\n\nThe 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 S251021u (GCN Circular 42373). Parameter estimation has been performed using Bilby [1] and a new sky map, Bilby.multiorder.fits,0, distributed via GCN and SCiMMA notices, is available for retrieval from the GraceDB event page:\n\nhttps://gracedb.ligo.org/superevents/S251021u\n\nFor the Bilby.multiorder.fits,0 sky map, the 90% credible region is 3859 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 5884 +/- 2089 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/.\n\n [1] Ashton et al. ApJS 241, 27 (2019) doi:10.3847/1538-4365/ab06fc and Morisaki et al. PRD 108, 123040 (2023) doi:10.1103/PhysRevD.108.123040",
"published": "2025-10-23T23:33:37.065434Z",
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"created": "2025-10-23T23:33:37.065479Z",
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{
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"title": "LIGO/Virgo/KAGRA S251021u: Identification of a GW compact binary merger candidate",
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"authors": "alvinli@g.ecc.u-tokyo.ac.jp",
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"message_text": "The LIGO Scientific Collaboration, the Virgo Collaboration, and the KAGRA Collaboration report:\n\nWe identified the compact binary merger candidate S251021u during real-time processing of data from LIGO Hanford Observatory (H1) and LIGO Livingston Observatory (L1) at 2025-10-21 03:22:15.181 UTC (GPS time: 1445052153.181). The candidate was found by the Aframe [1], cWB [2], cWB BBH [3], GstLAL [4], MBTA [5], PyCBC Live [6], and SPIIR [7] analysis pipelines.\n\nS251021u is an event of interest because its false alarm rate, as estimated by the online analysis, is 2.2e-09 Hz, or about one in 14 years. The event's properties can be found at this URL:\n\nhttps://gracedb.ligo.org/superevents/S251021u\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 at least one of the compact objects is consistent with a neutron star mass (HasNS) is <1%. [8] Using the masses and spins inferred from the signal, the probability of matter outside the final compact object (HasRemnant) is <1%. [8] Both HasNS and HasRemnant consider the support of several neutron star equations of state for maximum neutron star mass. The probability that either of the binary components lies between 3 and 5 solar masses (HasMassGap) is <1%.\n\nThe source chirp mass falls with highest probability in the bin (44.0, 88.0) solar masses, assuming the candidate is astrophysical in origin.\n\nTwo sky maps are available at this time and can be retrieved from the GraceDB event page:\n * amplfi.multiorder.fits,0, an initial localization generated by AMPLFI [9], distributed via GCN and SCiMMA notices about 25 seconds after the candidate event time.\n * bayestar.multiorder.fits,0, an initial localization generated by BAYESTAR [10], distributed via GCN and SCiMMA notices about 4 minutes after the candidate event time.\n\nThe preferred sky map at this time is bayestar.multiorder.fits,0. For the bayestar.multiorder.fits,0 sky map, the 90% credible region is 3742 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 7164 +/- 2185 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/.\n\n [1] Marx et al. PRD 111, 042010 (2025) doi:10.1103/PhysRevD.111.042010\n [2] Klimenko et al. PRD 93, 042004 (2016) doi:10.1103/PhysRevD.93.042004\n [3] T. Mishra et al. PRD 105, 083018 (2022) doi:10.1103/PhysRevD.105.083018\n [4] Tsukada et al. PRD 108, 043004 (2023) doi:10.1103/PhysRevD.108.043004 and Ewing et al. PRD 109, 042008 (2024) doi:10.1103/PhysRevD.109.042008\n [5] Alléné et al. CQG 42, 105009 (2025) doi:10.1088/1361-6382/add234\n [6] Dal Canton et al. ApJ 923, 254 (2021) doi:10.3847/1538-4357/ac2f9a\n [7] Chu et al. PRD 105, 024023 (2022) doi:10.1103/PhysRevD.105.024023\n [8] Chatterjee et al. ApJ 896, 54 (2020) doi:10.3847/1538-4357/ab8dbe\n [9] Chatterjee et al. MLST 5, 045030 (2024) doi:10.1088/2632-2153/ad8982\n [10] Singer & Price PRD 93, 024013 (2016) doi:10.1103/PhysRevD.93.024013",
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{
"id": 5792471,
"topic": "gcn.circulars",
"uuid": "3c6968da-66df-4585-bc7c-e0724b7766f0",
"title": "LIGO/Virgo/KAGRA S251013x: Updated Sky localization and Source Classification",
"submitter": "Nihar.Gupte@aei.mpg.de",
"authors": "Nihar.Gupte@aei.mpg.de",
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"bibcode": "2025GCN.42220....1L",
"eventId": "LIGO/Virgo/KAGRA S251013x",
"subject": "LIGO/Virgo/KAGRA S251013x: Updated Sky localization and Source Classification",
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"submitter": "Nihar.Gupte@aei.mpg.de",
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"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), LIGO Livingston Observatory (L1), and Virgo Observatory (V1) data around the time of the compact binary merger (CBC) candidate S251013x (GCN Circular 42212). Parameter estimation has been performed using Bilby [1] and a new sky map, Bilby.multiorder.fits,0, distributed via GCN and SCiMMA notices, is available for retrieval from the GraceDB event page:\n\nhttps://gracedb.ligo.org/superevents/S251013x\n\nFor the Bilby.multiorder.fits,0 sky map, the 90% credible region is 1361 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 3775 +/- 1200 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/.\n\n [1] Ashton et al. ApJS 241, 27 (2019) doi:10.3847/1538-4365/ab06fc and Morisaki et al. PRD 108, 123040 (2023) doi:10.1103/PhysRevD.108.123040",
"published": "2025-11-03T08:12:05.348009Z",
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{
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"title": "LIGO/Virgo/KAGRA S251013x: Identification of a GW compact binary merger candidate",
"submitter": "Kento IMAI <kent0311p@g.ecc.u-tokyo.ac.jp>",
"authors": "Kento IMAI <kent0311p@g.ecc.u-tokyo.ac.jp>",
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"message_text": "The LIGO Scientific Collaboration, the Virgo Collaboration, and the KAGRA Collaboration report:\n\nWe identified the compact binary merger candidate S251013x during real-time processing of data from LIGO Hanford Observatory (H1), LIGO Livingston Observatory (L1), and Virgo Observatory (V1) at 2025-10-13 02:44:14.281 UTC (GPS time: 1444358672.281). The candidate was found by the Aframe [1], GstLAL [2], MBTA [3], and PyCBC Live [4] analysis pipelines.\n\nS251013x is an event of interest because its false alarm rate, as estimated by the online analysis, is 1.5e-08 Hz, or about one in 2 years. The event's properties can be found at this URL:\n\nhttps://gracedb.ligo.org/superevents/S251013x\n\nThe classification of the GW signal, in order of descending probability, is BBH (99%), Terrestrial (1%), NSBH (<1%), or BNS (<1%).\n\nAssuming the candidate is astrophysical in origin, the probability that at least one of the compact objects 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 for maximum neutron star mass. The probability that either of the binary components lies between 3 and 5 solar masses (HasMassGap) is <1%.\n\nThe source chirp mass falls with highest probability in the bin (22.0, 44.0) solar masses, assuming the candidate is astrophysical in origin.\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 and SCiMMA notices about 30 seconds after the candidate event time.\n * bayestar.multiorder.fits,2, an initial localization generated by BAYESTAR [6], distributed via GCN and SCiMMA notices 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 1589 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 1946 +/- 505 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/.\n\n [1] Marx et al. PRD 111, 042010 (2025) doi:10.1103/PhysRevD.111.042010\n [2] Tsukada et al. PRD 108, 043004 (2023) doi:10.1103/PhysRevD.108.043004 and Ewing et al. PRD 109, 042008 (2024) doi:10.1103/PhysRevD.109.042008\n [3] Alléné et al. CQG 42, 105009 (2025) doi:10.1088/1361-6382/add234\n [4] Dal Canton et al. ApJ 923, 254 (2021) doi:10.3847/1538-4357/ac2f9a\n [5] Chatterjee et al. ApJ 896, 54 (2020) doi:10.3847/1538-4357/ab8dbe\n [6] Singer & Price PRD 93, 024013 (2016) doi:10.1103/PhysRevD.93.024013\n",
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{
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"title": "LIGO/Virgo/KAGRA S251013x: Updated Sky localization and Source Classification",
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"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), LIGO Livingston Observatory (L1), and Virgo Observatory (V1) data around the time of the compact binary merger (CBC) candidate S251013x (GCN Circular 42212). Parameter estimation has been performed using Bilby [1] and a new sky map, Bilby.multiorder.fits,0, distributed via GCN and SCiMMA notices, is available for retrieval from the GraceDB event page:\n\nhttps://gracedb.ligo.org/superevents/S251013x\n\nFor the Bilby.multiorder.fits,0 sky map, the 90% credible region is 1361 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 3775 +/- 1200 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/.\n\n [1] Ashton et al. ApJS 241, 27 (2019) doi:10.3847/1538-4365/ab06fc and Morisaki et al. PRD 108, 123040 (2023) doi:10.1103/PhysRevD.108.123040",
"published": "2025-10-13T16:23:13.083820Z",
"message_parser": "GCN Circular Parser v2",
"retracted": false,
"created": "2025-10-13T16:23:13.083832Z",
"modified": "2025-10-13T16:23:13.100190Z",
"targets": []
},
{
"id": 5787134,
"topic": "gcn.circulars",
"uuid": "ee160ebe-1852-49ca-958f-663b371c6a82",
"title": "LIGO/Virgo/KAGRA S251013x: Identification of a GW compact binary merger candidate",
"submitter": "Kento IMAI <kent0311p@g.ecc.u-tokyo.ac.jp>",
"authors": "Kento IMAI <kent0311p@g.ecc.u-tokyo.ac.jp>",
"data": {
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},
"format": "text/plain",
"$schema": "https://gcn.nasa.gov/schema/v4.5.0/gcn/circulars.schema.json",
"eventId": "LIGO/Virgo/KAGRA S251013x",
"subject": "LIGO/Virgo/KAGRA S251013x: Identification of a GW compact binary merger candidate",
"createdOn": 1760326293113,
"submitter": "Kento IMAI <kent0311p@g.ecc.u-tokyo.ac.jp>",
"circularId": 42212,
"submittedHow": "web"
},
"message_text": "The LIGO Scientific Collaboration, the Virgo Collaboration, and the KAGRA Collaboration report:\n\nWe identified the compact binary merger candidate S251013x during real-time processing of data from LIGO Hanford Observatory (H1), LIGO Livingston Observatory (L1), and Virgo Observatory (V1) at 2025-10-13 02:44:14.281 UTC (GPS time: 1444358672.281). The candidate was found by the Aframe [1], GstLAL [2], MBTA [3], and PyCBC Live [4] analysis pipelines.\n\nS251013x is an event of interest because its false alarm rate, as estimated by the online analysis, is 1.5e-08 Hz, or about one in 2 years. The event's properties can be found at this URL:\n\nhttps://gracedb.ligo.org/superevents/S251013x\n\nThe classification of the GW signal, in order of descending probability, is BBH (99%), Terrestrial (1%), NSBH (<1%), or BNS (<1%).\n\nAssuming the candidate is astrophysical in origin, the probability that at least one of the compact objects 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 for maximum neutron star mass. The probability that either of the binary components lies between 3 and 5 solar masses (HasMassGap) is <1%.\n\nThe source chirp mass falls with highest probability in the bin (22.0, 44.0) solar masses, assuming the candidate is astrophysical in origin.\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 and SCiMMA notices about 30 seconds after the candidate event time.\n * bayestar.multiorder.fits,2, an initial localization generated by BAYESTAR [6], distributed via GCN and SCiMMA notices 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 1589 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 1946 +/- 505 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/.\n\n [1] Marx et al. PRD 111, 042010 (2025) doi:10.1103/PhysRevD.111.042010\n [2] Tsukada et al. PRD 108, 043004 (2023) doi:10.1103/PhysRevD.108.043004 and Ewing et al. PRD 109, 042008 (2024) doi:10.1103/PhysRevD.109.042008\n [3] Alléné et al. CQG 42, 105009 (2025) doi:10.1088/1361-6382/add234\n [4] Dal Canton et al. ApJ 923, 254 (2021) doi:10.3847/1538-4357/ac2f9a\n [5] Chatterjee et al. ApJ 896, 54 (2020) doi:10.3847/1538-4357/ab8dbe\n [6] Singer & Price PRD 93, 024013 (2016) doi:10.1103/PhysRevD.93.024013\n",
"published": "2025-10-13T03:31:40.920496Z",
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"retracted": false,
"created": "2025-10-13T03:31:40.920506Z",
"modified": "2025-10-13T03:31:40.931573Z",
"targets": []
}
]
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"title": "S251117au - PRELIMINARY",
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"topic": "igwn.gwalert",
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"title": "S251117bc - PRELIMINARY",
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"time_created": "2025-11-17T08:27:14Z",
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},
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"published": "2025-11-17T10:18:25.996051Z",
"message_parser": "IGWN Alert Avro Parser v1",
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"created": "2025-11-17T10:18:25.996072Z",
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}
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{
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"message": {
"id": 5800257,
"topic": "igwn.gwalert",
"uuid": "677f286b-a66a-435e-9c9b-04e51d2732f9",
"title": "S251117bc - PRELIMINARY",
"submitter": "cody.messick-30d512c8",
"authors": "LVK",
"data": {
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"sequence_num": 2,
"time_created": "2025-11-17T08:31:47Z",
"superevent_id": "S251117bc",
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},
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"published": "2025-11-17T10:18:32.326983Z",
"message_parser": "IGWN Alert Avro Parser v1",
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"created": "2025-11-17T10:18:32.327003Z",
"modified": "2025-11-17T10:18:32.332721Z"
}
}
],
"references": []
},
{
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"sequence_number": 1,
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"message": {
"id": 5788055,
"topic": "igwn.gwalert",
"uuid": "ed9edb4a-7b7a-4839-9402-7af0849ed14b",
"title": "S251014cn - PRELIMINARY",
"submitter": "cody.messick-30d512c8",
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"data": {
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"BNS": 2.9095750477763796e-109,
"NSBH": 2.6227783475393e-107,
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"time_created": "2025-10-14T11:33:48Z",
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"published": "2025-10-14T11:33:48.668152Z",
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}
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{
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"message": {
"id": 5788056,
"topic": "igwn.gwalert",
"uuid": "93ac48b9-1aa2-4564-84db-1d3de1223056",
"title": "S251014cn - PRELIMINARY",
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"data": {
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"title": "S251014cn - INITIAL",
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"authors": "LVK",
"data": {
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],
"references": [
{
"id": 5792512,
"topic": "gcn.circulars",
"uuid": "66025454-b683-4742-a819-0b44a106178f",
"title": "LIGO/Virgo/KAGRA S251014cn: Updated Sky localization",
"submitter": "Nihar.Gupte@aei.mpg.de",
"authors": "Nihar.Gupte@aei.mpg.de",
"data": {
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/42306"
},
"format": "text/plain",
"$schema": "https://gcn.nasa.gov/schema/v4.5.0/gcn/circulars.schema.json",
"bibcode": "2025GCN.42306....1L",
"eventId": "LIGO/Virgo/KAGRA S251014cn",
"subject": "LIGO/Virgo/KAGRA S251014cn: Updated Sky localization",
"createdOn": 1760601103704,
"submitter": "Nihar.Gupte@aei.mpg.de",
"circularId": 42306,
"submittedHow": "web"
},
"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 S251014cn (GCN Circular 42255. Parameter estimation has been performed using Bilby [1] and a new sky map, Bilby.multiorder.fits,0, distributed via GCN and SCiMMA notices, is available for retrieval from the GraceDB event page:\n\nhttps://gracedb.ligo.org/superevents/S251014cn\n\nFor the Bilby.multiorder.fits,0 sky map, the 90% credible region is 172 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 607 +/- 164 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/.\n\n [1] Ashton et al. ApJS 241, 27 (2019) doi:10.3847/1538-4365/ab06fc and Morisaki et al. PRD 108, 123040 (2023) doi:10.1103/PhysRevD.108.123040",
"published": "2025-11-03T08:12:16.870941Z",
"message_parser": "GCN Circular Parser v2",
"retracted": false,
"created": "2025-11-03T08:12:16.870958Z",
"modified": "2025-11-03T08:12:16.875795Z",
"targets": []
},
{
"id": 5792506,
"topic": "gcn.circulars",
"uuid": "8751ead6-efc6-4dcd-bc69-4b37f9cf4ce0",
"title": "LIGO/Virgo/KAGRA S251014cn: NED Galaxies in the 3-Initial Localization Volume",
"submitter": "David Cook at Caltech/IPAC-NED <dcook@ipac.caltech.edu>",
"authors": "David Cook at Caltech/IPAC-NED <dcook@ipac.caltech.edu>",
"data": {
"urls": {
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},
"format": "text/markdown",
"$schema": "https://gcn.nasa.gov/schema/v4.5.0/gcn/circulars.schema.json",
"bibcode": "2025GCN.42260....1C",
"eventId": "LIGO/Virgo/KAGRA S251014cn",
"subject": "LIGO/Virgo/KAGRA S251014cn: NED Galaxies in the 3-Initial Localization Volume",
"createdOn": 1760456735147,
"submitter": "David Cook at Caltech/IPAC-NED <dcook@ipac.caltech.edu>",
"circularId": 42260,
"submittedHow": "web"
},
"message_text": "David O. Cook (Caltech/IPAC), Rick Ebert (Caltech/IPAC), George Helou (Caltech/IPAC), Joseph M. Mazzarella (Caltech/IPAC), Marion Schmitz (Caltech/IPAC), and Leo Singer (NASA/GSFC)\n\nOn behalf of the NASA/IPAC Extragalactic Database (NED) Team.\n\nWe spatially cross-matched the LVK S251014cn-3-Initial sky localization with the [NED Local Volume Sample](https://ned.ipac.caltech.edu/NED::LVS/) (NED-LVS; Cook et al. 2023), which is a subset of NED with a redshift or redshift-independent distance less than 1000 Mpc. We find 10691 galaxies within the 90% containment volume, and we list here the top 20 galaxies sorted by the joint probability of the 3D localization and the WISE W1 luminosity (an observable proxy for stellar mass). For the full or top 20 list of galaxies in the 90% volume go either to the NED Gravitational Wave Followup service at https://ned.ipac.caltech.edu/uri/NED::GWF/ or click on the following links:\n\nFull List Download: https://ned.ipac.caltech.edu/uri/NED::GWFglist/fits/S251014cn/3 \nTop 20 List Download: https://ned.ipac.caltech.edu/uri/NED::GWFglist/fits/S251014cn/3/20\n\nThe NED-GWF service provides downloadable galaxy lists and visualizations for candidate host galaxies. For each GW alert, these products are automatically generated and made available within minutes to expedite efficient electromagnetic follow-up observations. The NED top 20 list is sorted by the joint probability of the 3D localization and the WISE W1 luminosity, but users can sort on additional pre-computed prioritization metrics (star formation rate, P_3D * P_SFR; and specific star formation rate, P_3D * P_sSFR; etc.) which are available via downloading the entire galaxy list inside the event's probability volume.\n\n| objname| ra| dec|objtype| DistMpc|DistMpc_unc| m_NUV| m_NUV_unc| m_Ks| m_Ks_unc| m_W1| m_W1_unc| P_3D|P_3D_LumW1|\n|-------------------------|--------------|--------------|-------|-----------|-----------|------------|------------|------------|------------|------------|------------|--------|----------|\n|WISEA J204706.11-222948.1| 311.77550| -22.49672| G| 727.73| 4.31| null| null| 14.677| 0.171| 9.127| 0.006|1.25e-07| 1.19e-09|\n|WISEA J210442.39-250658.2| 316.17666| -25.11619| G| 632.49| 0.65| null| null| 12.233| 0.093| 9.702| 0.006|1.67e-07| 7.14e-10|\n| [HB89] 2155-304| 329.71694| -30.22559| QSO| 546.26| 0.43| 13.401| 0.001| 10.101| 0.013| 9.233| 0.006|8.29e-08| 4.03e-10|\n|WISEA J203200.13-212013.9| 308.00055| -21.33721| G| 686.01| null| null| null| 13.471| 0.172| 11.048| 0.007|2.64e-07| 3.82e-10|\n|WISEA J195711.85-155450.4| 299.29942| -15.91401| G| 464.26| null| null| null| 13.148| 0.182| 9.223| 0.006|9.41e-08| 3.41e-10|\n|WISEA J210053.37-260056.2| 315.22239| -26.01562| G| 523.86| null| 20.640| 0.211| 13.660| 0.182| 10.671| 0.006|2.12e-07| 2.55e-10|\n|WISEA J202657.64-194510.3| 306.74020| -19.75287| G| 536.72| 0.65| null| null| 12.502| 0.088| 10.962| 0.006|2.42e-07| 2.33e-10|\n|WISEA J233456.39-265518.6| 353.73499| -26.92184| G| 280.74| 0.65| null| null| 11.229| 0.056| 8.467| 0.005|8.37e-08| 2.18e-10|\n|WISEA J195521.91-151547.2| 298.84130| -15.26312| G| 485.70| null| null| null| 13.338| 0.163| 10.223| 0.007|1.19e-07| 1.91e-10|\n|WISEA J211913.50-272622.9| 319.80626| -27.43970| G| 533.96| null| 21.251| 0.278| 13.385| 0.135| 11.169| 0.007|2.33e-07| 1.84e-10|\n|WISEA J201311.18-190314.5| 303.29661| -19.05404| G| 572.05| null| null| null| 13.451| 0.145| 11.150| 0.007|1.75e-07| 1.62e-10|\n|WISEA J202635.83-202306.5| 306.64930| -20.38515| G| 735.83| 0.65| null| null| 12.556| 0.102| 11.879| 0.008|2.08e-07| 1.62e-10|\n|WISEA J202559.97-203159.0| 306.49991| -20.53307| G| 732.69| 0.65| null| null| 12.200| 0.114| 11.897| 0.012|2.03e-07| 1.54e-10|\n|WISEA J214110.24-264550.3| 325.29269| -26.76397| QSO| 608.68| null| 16.698| 0.017| 11.077| 0.012| 9.482| 0.006|3.03e-08| 1.46e-10|\n|WISEA J204622.40-223419.0| 311.59335| -22.57195| G| 685.98| 4.31| null| null| 15.453| 0.346| 11.646| 0.007|1.74e-07| 1.46e-10|\n|WISEA J200050.95-154454.3| 300.21230| -15.74842| G| 688.87| null| null| null| 13.684| 0.252| 11.792| 0.008|1.90e-07| 1.41e-10|\n|WISEA J193249.64-101803.3| 293.20684| -10.30092| G| 410.47| 0.65| null| null| 12.248| 0.139| 9.373| 0.006|5.53e-08| 1.39e-10|\n|WISEA J210524.13-254016.4| 316.35056| -25.67124| G| 492.45| null| null| null| 13.568| 0.159| 11.429| 0.007|2.62e-07| 1.38e-10|\n|WISEA J202206.73-184638.7| 305.52808| -18.77742| G| 497.59| 0.65| 19.597| 0.097| 12.293| 0.055| 11.011| 0.007|1.75e-07| 1.38e-10|\n|WISEA J201415.46-192535.3| 303.56468| -19.42654| G| 602.46| null| null| null| 13.720| 0.165| 11.210| 0.007|1.39e-07| 1.35e-10|\n\nTable 1: Top 20 galaxies in NED-LVS that fall in the 90% probability volume for S251014cn sorted by the joint probability of 3D position and WISE W1 luminosity (P_3D * P_LumW1). Galaxy is the NED preferred name. RA and Dec are the Equatorial coordinates in degrees (J2000). Objtype is the object type of the galaxy candidate. Distance is the distance to the galaxy in Mpc. m_NUV and mErr_NUV are the apparent magnitude and error from GALEX. m_Ks and mErr_Ks are the apparent magnitude and error from 2MASS. m_W1 and mErr_W1 are the apparent magnitude and error from AllWISE. P_3D is the probability that the galaxy is in the volume given the distance of GW event. P_3D_LumW1 is the joint probability within the volume weighted by the WISE1 luminosity of the galaxy (P_3D * P_LumW1). ",
"published": "2025-11-03T08:12:15.786270Z",
"message_parser": "GCN Circular Parser v2",
"retracted": false,
"created": "2025-11-03T08:12:15.786285Z",
"modified": "2025-11-03T08:12:15.791156Z",
"targets": []
},
{
"id": 5792427,
"topic": "gcn.circulars",
"uuid": "413f25ab-5346-47cf-87da-6a5fb349d49f",
"title": "LIGO/Virgo/KAGRA S251014cn: Identification of a GW compact binary merger candidate",
"submitter": "Matteo Tagliazucchi at University of Bologna - INFN Bologna <matteo.tagliazucchi2@unibo.it>",
"authors": "Matteo Tagliazucchi at University of Bologna - INFN Bologna <matteo.tagliazucchi2@unibo.it>",
"data": {
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/42255"
},
"format": "text/plain",
"$schema": "https://gcn.nasa.gov/schema/v4.5.0/gcn/circulars.schema.json",
"bibcode": "2025GCN.42255....1L",
"eventId": "LIGO/Virgo/KAGRA S251014cn",
"subject": "LIGO/Virgo/KAGRA S251014cn: Identification of a GW compact binary merger candidate",
"createdOn": 1760445173338,
"submitter": "Matteo Tagliazucchi at University of Bologna - INFN Bologna <matteo.tagliazucchi2@unibo.it>",
"circularId": 42255,
"submittedHow": "web"
},
"message_text": "The LIGO Scientific Collaboration, the Virgo Collaboration, and the KAGRA Collaboration report:\n\nWe identified the compact binary merger candidate S251014cn during real-time processing of data from LIGO Hanford Observatory (H1) and LIGO Livingston Observatory (L1) at 2025-10-14 11:33:23.373 UTC (GPS time: 1444476821.373). The candidate was found by the Aframe [1], cWB [2], cWB BBH [3], GstLAL [4], MBTA [5], MLy [6], PyCBC Live [7], and SPIIR [8] analysis pipelines.\n\nS251014cn 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/S251014cn\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 at least one of the compact objects is consistent with a neutron star mass (HasNS) is <1%. [9] Using the masses and spins inferred from the signal, the probability of matter outside the final compact object (HasRemnant) is <1%. [9] Both HasNS and HasRemnant consider the support of several neutron star equations of state for maximum neutron star mass. The probability that either of the binary components lies between 3 and 5 solar masses (HasMassGap) is <1%.\n\nThe source chirp mass falls with highest probability in the bin (11.0, 22.0) solar masses, assuming the candidate is astrophysical in origin.\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 [10], distributed via GCN and SCiMMA notices about 24 seconds after the candidate event time.\n * bayestar.multiorder.fits,1, an initial localization generated by BAYESTAR [10], distributed via GCN and SCiMMA notices 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 233 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 610 +/- 172 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/.\n\n [1] Marx et al. PRD 111, 042010 (2025) doi:10.1103/PhysRevD.111.042010\n [2] Klimenko et al. PRD 93, 042004 (2016) doi:10.1103/PhysRevD.93.042004\n [3] T. Mishra et al. PRD 105, 083018 (2022) doi:10.1103/PhysRevD.105.083018\n [4] Tsukada et al. PRD 108, 043004 (2023) doi:10.1103/PhysRevD.108.043004 and Ewing et al. PRD 109, 042008 (2024) doi:10.1103/PhysRevD.109.042008\n [5] Alléné et al. CQG 42, 105009 (2025) doi:10.1088/1361-6382/add234\n [6] Skliris et al. PRD 110, 104034 (2024) doi:10.1103/PhysRevD.110.104034\n [7] Dal Canton et al. ApJ 923, 254 (2021) doi:10.3847/1538-4357/ac2f9a\n [8] Chu et al. PRD 105, 024023 (2022) doi:10.1103/PhysRevD.105.024023\n [9] Chatterjee et al. ApJ 896, 54 (2020) doi:10.3847/1538-4357/ab8dbe\n [10] Singer & Price PRD 93, 024013 (2016) doi:10.1103/PhysRevD.93.024013\n",
"published": "2025-11-03T08:11:13.634659Z",
"message_parser": "GCN Circular Parser v2",
"retracted": false,
"created": "2025-11-03T08:11:13.634674Z",
"modified": "2025-11-03T08:11:13.639550Z",
"targets": []
},
{
"id": 5788616,
"topic": "gcn.circulars",
"uuid": "b61b8dca-561a-4772-a9a7-c53eaaea2ddc",
"title": "LIGO/Virgo/KAGRA S251014cn: Updated Sky localization",
"submitter": "Nihar.Gupte@aei.mpg.de",
"authors": "Nihar.Gupte@aei.mpg.de",
"data": {
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/42306"
},
"format": "text/plain",
"$schema": "https://gcn.nasa.gov/schema/v4.5.0/gcn/circulars.schema.json",
"eventId": "LIGO/Virgo/KAGRA S251014cn",
"subject": "LIGO/Virgo/KAGRA S251014cn: Updated Sky localization",
"createdOn": 1760601103704,
"submitter": "Nihar.Gupte@aei.mpg.de",
"circularId": 42306,
"submittedHow": "web"
},
"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 S251014cn (GCN Circular 42255. Parameter estimation has been performed using Bilby [1] and a new sky map, Bilby.multiorder.fits,0, distributed via GCN and SCiMMA notices, is available for retrieval from the GraceDB event page:\n\nhttps://gracedb.ligo.org/superevents/S251014cn\n\nFor the Bilby.multiorder.fits,0 sky map, the 90% credible region is 172 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 607 +/- 164 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/.\n\n [1] Ashton et al. ApJS 241, 27 (2019) doi:10.3847/1538-4365/ab06fc and Morisaki et al. PRD 108, 123040 (2023) doi:10.1103/PhysRevD.108.123040",
"published": "2025-10-16T07:51:51.392119Z",
"message_parser": "GCN Circular Parser v2",
"retracted": false,
"created": "2025-10-16T07:51:51.392141Z",
"modified": "2025-10-16T07:51:51.413797Z",
"targets": []
},
{
"id": 5788097,
"topic": "gcn.circulars",
"uuid": "90ca13c7-ac3b-4c92-b262-9e3bc69d5531",
"title": "LIGO/Virgo/KAGRA S251014cn: NED Galaxies in the 3-Initial Localization Volume",
"submitter": "David Cook at Caltech/IPAC-NED <dcook@ipac.caltech.edu>",
"authors": "David Cook at Caltech/IPAC-NED <dcook@ipac.caltech.edu>",
"data": {
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/42260"
},
"format": "text/markdown",
"$schema": "https://gcn.nasa.gov/schema/v4.5.0/gcn/circulars.schema.json",
"eventId": "LIGO/Virgo/KAGRA S251014cn",
"subject": "LIGO/Virgo/KAGRA S251014cn: NED Galaxies in the 3-Initial Localization Volume",
"createdOn": 1760456735147,
"submitter": "David Cook at Caltech/IPAC-NED <dcook@ipac.caltech.edu>",
"circularId": 42260,
"submittedHow": "web"
},
"message_text": "David O. Cook (Caltech/IPAC), Rick Ebert (Caltech/IPAC), George Helou (Caltech/IPAC), Joseph M. Mazzarella (Caltech/IPAC), Marion Schmitz (Caltech/IPAC), and Leo Singer (NASA/GSFC)\n\nOn behalf of the NASA/IPAC Extragalactic Database (NED) Team.\n\nWe spatially cross-matched the LVK S251014cn-3-Initial sky localization with the [NED Local Volume Sample](https://ned.ipac.caltech.edu/NED::LVS/) (NED-LVS; Cook et al. 2023), which is a subset of NED with a redshift or redshift-independent distance less than 1000 Mpc. We find 10691 galaxies within the 90% containment volume, and we list here the top 20 galaxies sorted by the joint probability of the 3D localization and the WISE W1 luminosity (an observable proxy for stellar mass). For the full or top 20 list of galaxies in the 90% volume go either to the NED Gravitational Wave Followup service at https://ned.ipac.caltech.edu/uri/NED::GWF/ or click on the following links:\n\nFull List Download: https://ned.ipac.caltech.edu/uri/NED::GWFglist/fits/S251014cn/3 \nTop 20 List Download: https://ned.ipac.caltech.edu/uri/NED::GWFglist/fits/S251014cn/3/20\n\nThe NED-GWF service provides downloadable galaxy lists and visualizations for candidate host galaxies. For each GW alert, these products are automatically generated and made available within minutes to expedite efficient electromagnetic follow-up observations. The NED top 20 list is sorted by the joint probability of the 3D localization and the WISE W1 luminosity, but users can sort on additional pre-computed prioritization metrics (star formation rate, P_3D * P_SFR; and specific star formation rate, P_3D * P_sSFR; etc.) which are available via downloading the entire galaxy list inside the event's probability volume.\n\n| objname| ra| dec|objtype| DistMpc|DistMpc_unc| m_NUV| m_NUV_unc| m_Ks| m_Ks_unc| m_W1| m_W1_unc| P_3D|P_3D_LumW1|\n|-------------------------|--------------|--------------|-------|-----------|-----------|------------|------------|------------|------------|------------|------------|--------|----------|\n|WISEA J204706.11-222948.1| 311.77550| -22.49672| G| 727.73| 4.31| null| null| 14.677| 0.171| 9.127| 0.006|1.25e-07| 1.19e-09|\n|WISEA J210442.39-250658.2| 316.17666| -25.11619| G| 632.49| 0.65| null| null| 12.233| 0.093| 9.702| 0.006|1.67e-07| 7.14e-10|\n| [HB89] 2155-304| 329.71694| -30.22559| QSO| 546.26| 0.43| 13.401| 0.001| 10.101| 0.013| 9.233| 0.006|8.29e-08| 4.03e-10|\n|WISEA J203200.13-212013.9| 308.00055| -21.33721| G| 686.01| null| null| null| 13.471| 0.172| 11.048| 0.007|2.64e-07| 3.82e-10|\n|WISEA J195711.85-155450.4| 299.29942| -15.91401| G| 464.26| null| null| null| 13.148| 0.182| 9.223| 0.006|9.41e-08| 3.41e-10|\n|WISEA J210053.37-260056.2| 315.22239| -26.01562| G| 523.86| null| 20.640| 0.211| 13.660| 0.182| 10.671| 0.006|2.12e-07| 2.55e-10|\n|WISEA J202657.64-194510.3| 306.74020| -19.75287| G| 536.72| 0.65| null| null| 12.502| 0.088| 10.962| 0.006|2.42e-07| 2.33e-10|\n|WISEA J233456.39-265518.6| 353.73499| -26.92184| G| 280.74| 0.65| null| null| 11.229| 0.056| 8.467| 0.005|8.37e-08| 2.18e-10|\n|WISEA J195521.91-151547.2| 298.84130| -15.26312| G| 485.70| null| null| null| 13.338| 0.163| 10.223| 0.007|1.19e-07| 1.91e-10|\n|WISEA J211913.50-272622.9| 319.80626| -27.43970| G| 533.96| null| 21.251| 0.278| 13.385| 0.135| 11.169| 0.007|2.33e-07| 1.84e-10|\n|WISEA J201311.18-190314.5| 303.29661| -19.05404| G| 572.05| null| null| null| 13.451| 0.145| 11.150| 0.007|1.75e-07| 1.62e-10|\n|WISEA J202635.83-202306.5| 306.64930| -20.38515| G| 735.83| 0.65| null| null| 12.556| 0.102| 11.879| 0.008|2.08e-07| 1.62e-10|\n|WISEA J202559.97-203159.0| 306.49991| -20.53307| G| 732.69| 0.65| null| null| 12.200| 0.114| 11.897| 0.012|2.03e-07| 1.54e-10|\n|WISEA J214110.24-264550.3| 325.29269| -26.76397| QSO| 608.68| null| 16.698| 0.017| 11.077| 0.012| 9.482| 0.006|3.03e-08| 1.46e-10|\n|WISEA J204622.40-223419.0| 311.59335| -22.57195| G| 685.98| 4.31| null| null| 15.453| 0.346| 11.646| 0.007|1.74e-07| 1.46e-10|\n|WISEA J200050.95-154454.3| 300.21230| -15.74842| G| 688.87| null| null| null| 13.684| 0.252| 11.792| 0.008|1.90e-07| 1.41e-10|\n|WISEA J193249.64-101803.3| 293.20684| -10.30092| G| 410.47| 0.65| null| null| 12.248| 0.139| 9.373| 0.006|5.53e-08| 1.39e-10|\n|WISEA J210524.13-254016.4| 316.35056| -25.67124| G| 492.45| null| null| null| 13.568| 0.159| 11.429| 0.007|2.62e-07| 1.38e-10|\n|WISEA J202206.73-184638.7| 305.52808| -18.77742| G| 497.59| 0.65| 19.597| 0.097| 12.293| 0.055| 11.011| 0.007|1.75e-07| 1.38e-10|\n|WISEA J201415.46-192535.3| 303.56468| -19.42654| G| 602.46| null| null| null| 13.720| 0.165| 11.210| 0.007|1.39e-07| 1.35e-10|\n\nTable 1: Top 20 galaxies in NED-LVS that fall in the 90% probability volume for S251014cn sorted by the joint probability of 3D position and WISE W1 luminosity (P_3D * P_LumW1). Galaxy is the NED preferred name. RA and Dec are the Equatorial coordinates in degrees (J2000). Objtype is the object type of the galaxy candidate. Distance is the distance to the galaxy in Mpc. m_NUV and mErr_NUV are the apparent magnitude and error from GALEX. m_Ks and mErr_Ks are the apparent magnitude and error from 2MASS. m_W1 and mErr_W1 are the apparent magnitude and error from AllWISE. P_3D is the probability that the galaxy is in the volume given the distance of GW event. P_3D_LumW1 is the joint probability within the volume weighted by the WISE1 luminosity of the galaxy (P_3D * P_LumW1). ",
"published": "2025-10-14T15:45:43.564942Z",
"message_parser": "GCN Circular Parser v2",
"retracted": false,
"created": "2025-10-14T15:45:43.564950Z",
"modified": "2025-10-14T15:45:43.588017Z",
"targets": []
},
{
"id": 5788065,
"topic": "gcn.circulars",
"uuid": "22ac1556-5309-444d-9986-8f68261153ce",
"title": "LIGO/Virgo/KAGRA S251014cn: Identification of a GW compact binary merger candidate",
"submitter": "Matteo Tagliazucchi at University of Bologna - INFN Bologna <matteo.tagliazucchi2@unibo.it>",
"authors": "Matteo Tagliazucchi at University of Bologna - INFN Bologna <matteo.tagliazucchi2@unibo.it>",
"data": {
"urls": {
"gcn_circular": "https://gcn.nasa.gov/circulars/42255"
},
"format": "text/plain",
"$schema": "https://gcn.nasa.gov/schema/v4.5.0/gcn/circulars.schema.json",
"eventId": "LIGO/Virgo/KAGRA S251014cn",
"subject": "LIGO/Virgo/KAGRA S251014cn: Identification of a GW compact binary merger candidate",
"createdOn": 1760445173338,
"submitter": "Matteo Tagliazucchi at University of Bologna - INFN Bologna <matteo.tagliazucchi2@unibo.it>",
"circularId": 42255,
"submittedHow": "web"
},
"message_text": "The LIGO Scientific Collaboration, the Virgo Collaboration, and the KAGRA Collaboration report:\n\nWe identified the compact binary merger candidate S251014cn during real-time processing of data from LIGO Hanford Observatory (H1) and LIGO Livingston Observatory (L1) at 2025-10-14 11:33:23.373 UTC (GPS time: 1444476821.373). The candidate was found by the Aframe [1], cWB [2], cWB BBH [3], GstLAL [4], MBTA [5], MLy [6], PyCBC Live [7], and SPIIR [8] analysis pipelines.\n\nS251014cn 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/S251014cn\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 at least one of the compact objects is consistent with a neutron star mass (HasNS) is <1%. [9] Using the masses and spins inferred from the signal, the probability of matter outside the final compact object (HasRemnant) is <1%. [9] Both HasNS and HasRemnant consider the support of several neutron star equations of state for maximum neutron star mass. The probability that either of the binary components lies between 3 and 5 solar masses (HasMassGap) is <1%.\n\nThe source chirp mass falls with highest probability in the bin (11.0, 22.0) solar masses, assuming the candidate is astrophysical in origin.\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 [10], distributed via GCN and SCiMMA notices about 24 seconds after the candidate event time.\n * bayestar.multiorder.fits,1, an initial localization generated by BAYESTAR [10], distributed via GCN and SCiMMA notices 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 233 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 610 +/- 172 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/.\n\n [1] Marx et al. PRD 111, 042010 (2025) doi:10.1103/PhysRevD.111.042010\n [2] Klimenko et al. PRD 93, 042004 (2016) doi:10.1103/PhysRevD.93.042004\n [3] T. Mishra et al. PRD 105, 083018 (2022) doi:10.1103/PhysRevD.105.083018\n [4] Tsukada et al. PRD 108, 043004 (2023) doi:10.1103/PhysRevD.108.043004 and Ewing et al. PRD 109, 042008 (2024) doi:10.1103/PhysRevD.109.042008\n [5] Alléné et al. CQG 42, 105009 (2025) doi:10.1088/1361-6382/add234\n [6] Skliris et al. PRD 110, 104034 (2024) doi:10.1103/PhysRevD.110.104034\n [7] Dal Canton et al. ApJ 923, 254 (2021) doi:10.3847/1538-4357/ac2f9a\n [8] Chu et al. PRD 105, 024023 (2022) doi:10.1103/PhysRevD.105.024023\n [9] Chatterjee et al. ApJ 896, 54 (2020) doi:10.3847/1538-4357/ab8dbe\n [10] Singer & Price PRD 93, 024013 (2016) doi:10.1103/PhysRevD.93.024013\n",
"published": "2025-10-14T12:33:01.431182Z",
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"sequences": [],
"references": [
{
"id": 5792531,
"topic": "gcn.circulars",
"uuid": "6483e63b-cdb5-4d5e-a876-889913564d94",
"title": "LIGO/Virgo/KAGRA S251026bn: Identification of a GW compact binary merger candidate",
"submitter": "joan-rene.merou@ligo.org",
"authors": "joan-rene.merou@ligo.org",
"data": {
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"bibcode": "2025GCN.42462....1L",
"eventId": "LIGO/Virgo/KAGRA S251026bn",
"subject": "LIGO/Virgo/KAGRA S251026bn: Identification of a GW compact binary merger candidate",
"createdOn": 1761516675840,
"submitter": "joan-rene.merou@ligo.org",
"circularId": 42462,
"submittedHow": "web"
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"message_text": "The LIGO Scientific Collaboration, the Virgo Collaboration, and the KAGRA Collaboration report:\n\nWe identified the compact binary merger candidate S251026bn during real-time processing of data from LIGO Hanford Observatory (H1) and LIGO Livingston Observatory (L1) at 2025-10-26 21:16:05.296 UTC (GPS time: 1445548583.296). The candidate was found by the Aframe [1], cWB [2], cWB BBH [3], GstLAL [4], MBTA [5], PyCBC Live [6], and SPIIR [7] analysis pipelines.\n\nS251026bn is an event of interest because its false alarm rate, as estimated by the online analysis, is 4.8e-12 Hz, or about one in 1e4 years. The event's properties can be found at this URL:\n\nhttps://gracedb.ligo.org/superevents/S251026bn\n\nThe classification of the GW signal, in order of descending probability, is BBH (>99%), Terrestrial (<1%), NSBH (<1%), or BNS (<1%).\n\nAssuming the candidate is astrophysical in origin, the probability that at least one of the compact objects is consistent with a neutron star mass (HasNS) is <1%. [8] Using the masses and spins inferred from the signal, the probability of matter outside the final compact object (HasRemnant) is <1%. [8] Both HasNS and HasRemnant consider the support of several neutron star equations of state for maximum neutron star mass. The probability that either of the binary components lies between 3 and 5 solar masses (HasMassGap) is 8%.\n\nThe source chirp mass falls with highest probability in the bin (5.5, 11.0) solar masses, assuming the candidate is astrophysical in origin.\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 [9], distributed via GCN and SCiMMA notices about 29 seconds after the candidate event time.\n * bayestar.multiorder.fits,1, an initial localization generated by BAYESTAR [9], distributed via GCN and SCiMMA notices 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 956 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 1254 +/- 349 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/.\n\n [1] Marx et al. PRD 111, 042010 (2025) doi:10.1103/PhysRevD.111.042010\n [2] Klimenko et al. PRD 93, 042004 (2016) doi:10.1103/PhysRevD.93.042004\n [3] T. Mishra et al. PRD 105, 083018 (2022) doi:10.1103/PhysRevD.105.083018\n [4] Tsukada et al. PRD 108, 043004 (2023) doi:10.1103/PhysRevD.108.043004 and Ewing et al. PRD 109, 042008 (2024) doi:10.1103/PhysRevD.109.042008\n [5] Alléné et al. CQG 42, 105009 (2025) doi:10.1088/1361-6382/add234\n [6] Dal Canton et al. ApJ 923, 254 (2021) doi:10.3847/1538-4357/ac2f9a\n [7] Chu et al. PRD 105, 024023 (2022) doi:10.1103/PhysRevD.105.024023\n [8] Chatterjee et al. ApJ 896, 54 (2020) doi:10.3847/1538-4357/ab8dbe\n [9] Singer & Price PRD 93, 024013 (2016) doi:10.1103/PhysRevD.93.024013\n\n",
"published": "2025-11-03T08:12:19.100649Z",
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{
"id": 5792491,
"topic": "gcn.circulars",
"uuid": "ec779507-8121-4f40-980a-30a902568c78",
"title": "LIGO/Virgo/KAGRA S251026bn: Updated Sky localization",
"submitter": "lucy.thomas@ligo.org",
"authors": "lucy.thomas@ligo.org",
"data": {
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"bibcode": "2025GCN.42465....1L",
"eventId": "LIGO/Virgo/KAGRA S251026bn",
"subject": "LIGO/Virgo/KAGRA S251026bn: Updated Sky localization",
"createdOn": 1761532822153,
"submitter": "lucy.thomas@ligo.org",
"circularId": 42465,
"submittedHow": "web"
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"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 S251026bn (GCN Circular 42462). Parameter estimation has been performed using Bilby [1] and a new sky map, Bilby.multiorder.fits,0, distributed via GCN and SCiMMA notices, is available for retrieval from the GraceDB event page:\n\nhttps://gracedb.ligo.org/superevents/S251026bn\n\nFor the Bilby.multiorder.fits,0 sky map, the 90% credible region is 744 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 1202 +/- 347 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/.\n\n [1] Ashton et al. ApJS 241, 27 (2019) doi:10.3847/1538-4365/ab06fc and Morisaki et al. PRD 108, 123040 (2023) doi:10.1103/PhysRevD.108.123040",
"published": "2025-11-03T08:12:07.586903Z",
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"retracted": false,
"created": "2025-11-03T08:12:07.586918Z",
"modified": "2025-11-03T08:12:07.591291Z",
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"sequences": [
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"message": {
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"topic": "gcn.classic.text.ICECUBE_CASCADE",
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"message_text": "TITLE: GCN/AMON NOTICE\nNOTICE_DATE: Fri 07 Nov 25 21:03:32 UT\nNOTICE_TYPE: ICECUBE Cascade \nEVENT_NAME: IceCubeCascade-251107a\nSTREAM: 26\nRUN_NUM: 141568\nEVENT_NUM: 42562719\nSRC_RA: 285.1968d {+19h 00m 47s} (J2000),\n 285.6746d {+19h 02m 42s} (current),\n 284.2713d {+18h 57m 05s} (1950)\nSRC_DEC: -46.5855d {-46d 35' 07\"} (J2000),\n -46.5472d {-46d 32' 49\"} (current),\n -46.6563d {-46d 39' 22\"} (1950)\nSRC_ERROR: 13.58 [deg radius, stat+systematic, 90% containment]\nSRC_ERROR50: 7.45 [deg radius, stat+systematic, 50% containment]\nDISCOVERY_DATE: 20986 TJD; 311 DOY; 25/11/07 (yy/mm/dd)\nDISCOVERY_TIME: 75705 SOD {21:01:45.88} UT\nREVISION: 0\nENERGY: 106.19 [TeV]\nSIGNALNESS: 9.0012e-01 [dn]\nFAR: 0.3110 [yr^-1]\nSUN_POSTN: 223.24d {+14h 52m 58s} -16.54d {-16d 32' 21\"}\nSUN_DIST: 59.22 [deg] Sun_angle= -4.2 [hr] (East of Sun)\nMOON_POSTN: 77.00d {+05h 08m 01s} +27.96d {+27d 57' 25\"}\nMOON_DIST: 150.85 [deg]\nGAL_COORDS: 350.23,-20.87 [deg] galactic lon,lat of the event\nECL_COORDS: 281.35,-23.74 [deg] ecliptic lon,lat of the event\nSKYMAP_FITS_URL: https://roc.icecube.wisc.edu/public/hese_cascades/hese_60986_run00141568.evt000042562719.fits\nSKYMAP_PNG_URL: https://roc.icecube.wisc.edu/public/hese_cascades/hese_60986_run00141568.evt000042562719.png\nCOMMENTS: IceCube Cascade event. \nCOMMENTS: The position error is the combined statistical and the systematic. \n",
"published": "2025-11-07T21:03:32Z",
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"energy": "106.19 [TeV]",
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"message_text": "TITLE: GCN/AMON NOTICE\nNOTICE_DATE: Fri 07 Nov 25 21:03:32 UT\nNOTICE_TYPE: ICECUBE Cascade \nEVENT_NAME: IceCubeCascade-251107a\nSTREAM: 26\nRUN_NUM: 141568\nEVENT_NUM: 42562719\nSRC_RA: 285.1968d {+19h 00m 47s} (J2000),\n 285.6746d {+19h 02m 42s} (current),\n 284.2713d {+18h 57m 05s} (1950)\nSRC_DEC: -46.5855d {-46d 35' 07\"} (J2000),\n -46.5472d {-46d 32' 49\"} (current),\n -46.6563d {-46d 39' 22\"} (1950)\nSRC_ERROR: 13.58 [deg radius, stat+systematic, 90% containment]\nSRC_ERROR50: 7.45 [deg radius, stat+systematic, 50% containment]\nDISCOVERY_DATE: 20986 TJD; 311 DOY; 25/11/07 (yy/mm/dd)\nDISCOVERY_TIME: 75705 SOD {21:01:45.88} UT\nREVISION: 0\nENERGY: 106.19 [TeV]\nSIGNALNESS: 9.0012e-01 [dn]\nFAR: 0.3110 [yr^-1]\nSUN_POSTN: 223.24d {+14h 52m 58s} -16.54d {-16d 32' 21\"}\nSUN_DIST: 59.22 [deg] Sun_angle= -4.2 [hr] (East of Sun)\nMOON_POSTN: 77.00d {+05h 08m 01s} +27.96d {+27d 57' 25\"}\nMOON_DIST: 150.85 [deg]\nGAL_COORDS: 350.23,-20.87 [deg] galactic lon,lat of the event\nECL_COORDS: 281.35,-23.74 [deg] ecliptic lon,lat of the event\nSKYMAP_FITS_URL: https://roc.icecube.wisc.edu/public/hese_cascades/hese_60986_run00141568.evt000042562719.fits\nSKYMAP_PNG_URL: https://roc.icecube.wisc.edu/public/hese_cascades/hese_60986_run00141568.evt000042562719.png\nCOMMENTS: IceCube Cascade event. \nCOMMENTS: The position error is the combined statistical and the systematic. \n",
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"message": {
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"topic": "igwn.gwalert",
"uuid": "9cf6057a-9e24-45aa-b203-30404989ed95",
"title": "S251108cr - PRELIMINARY",
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"data": {
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"title": "S251108cr - PRELIMINARY",
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"data": {
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"message_text": "Shreya Anand (Stanford), Anirudh Salgundi (UNC), Robert Stein (UMD), Vishwajeet Swain (IIT-B), Yogesh Wagh (IIT-B), Xander J. Hall (CMU), Mansi Kasliwal (Caltech), Eric Bellm (UW), Michael Coughlin (UMN), Theophile Jegou du Laz (Caltech), and Antonella Palmese (CMU) report,\n\nOn behalf of the Zwicky Transient Facility (ZTF) and Global Relay of Observatories Watching Transients Happen (GROWTH) collaborations: \n\nWe observed the localization region of the LVK low-significance burst trigger S251031dw with the Palomar 48-inch telescope, equipped with the 47 square degree ZTF camera (Bellm et al. 2019, Graham et al. 2019). We started observations in the g- and r-band beginning at 2025-11-01 12:22 UTC, approximately 15.2 hours after merger. We covered 23.1% of the reported localization region on 2025-10-31 and 60.9% of the localization on 2025-11-01. This estimate accounts for chip gaps. ~30% of the tiled localization was at a low galactic latitude. Each exposure was 200s with a median r-band depth of 21.1 mag. \n \nThe images were processed in real-time through the ZTF reduction and image subtraction pipelines at IPAC to search for potential counterparts (Masci et al. 2019). AMPEL (Nordin et al. 2019, Stein et al. 2021) was used to search the alerts database for candidates. We reject stellar sources (Tachibana and Miller 2018) and moving objects, and apply machine learning algorithms (Mahabal et al. 2019), removing candidates with history of variability prior to the merger time. \n\nAfter filtering, 58 transient candidates remain, all within the 95.0% localization of the skymap. None of these candidates have fast evolution consistent with kilonovae. We perform additional vetting of these candidates, and highlight 9 candidates that appear to be young and SN-like, or AGN-like, as candidates of interest in the burst search, in the table below: \n\n\n| ZTF Name | IAU Name | RA (deg) | DEC (deg) | MJD | Filt | Mag | MagErr | Note |\n| ------------ | ---------- | ---------- | ---------- | -------- | ---- | ----- | ------ | -------- |\n| ZTF25acchitl | -- | 127.996770 | -27.778576 | 60980.52 | r | 20.63 | 0.11 | AGN-like |\n| ZTF25accnabz | -- | 128.305827 | -23.858020 | 60980.52 | r | 21.60 | 0.19 | AGN-like |\n| ZTF25acchdbq | -- | 121.061164 | -19.087422 | 60980.50 | r | 20.35 | 0.21 | AGN-like |\n| ZTF25acchjjz | -- | 127.829510 | -20.792424 | 60980.52 | r | 20.88 | 0.12 | AGN-like |\n| ZTF25acchljm | -- | 130.363870 | -23.822309 | 60980.52 | r | 20.87 | 0.13 | AGN-like |\n| ZTF25accniqx | -- | 131.262056 | -20.691176 | 60980.54 | r | 20.16 | 0.15 | AGN-like |\n| ZTF25acchigq | -- | 128.491126 | -24.746190 | 60980.52 | r | 21.26 | 0.15 | AGN-like |\n| ZTF25acchszc | AT2025acno | 137.799671 | -22.017226 | 60980.54 | r | 20.93 | 0.13 | SN-like |\n| ZTF25acchppz | AT2025acep | 135.228502 | -23.983061 | 60980.54 | r | 19.48 | 0.05 | SN-like |\n\nZTF25acchszc appears to be a rising young, blue supernova in a host galaxy (no redshift available). ZTF25acchppz is offset 9\" from a potential host galaxy at z=0.082, and is therefore unlikely to be associated with the burst source. Further follow-up is encouraged.\n\nBased on observations obtained with the Samuel Oschin Telescope 48-inch and the 60-inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. ZTF is supported by the National Science Foundation under Award #2407588 and a partnership including Caltech, USA; Caltech/IPAC, USA; University of Maryland, USA; University of California, Berkeley, USA; University of Wisconsin at Milwaukee, USA; Cornell University, USA; Drexel University, USA; University of North Carolina at Chapel Hill, USA; Institute of Science and Technology, Austria; National Central University, Taiwan; Operations are conducted by Caltech's Optical Observatory (COO) and Caltech/IPAC. GROWTH acknowledges the generous support of the NSF under PIRE Grant No 1545949. Alert database searches are done by AMPEL (Nordin et al. 2019) and Kowalski (Duev et al. 2019). The GROWTH India Telescope (GIT, Kumar et al., 2022) is set up by the Indian Institute of Astrophysics (IIA) and the Indian Institute of Technology Bombay (IITB) with funding from DST-SERB and IUSSTF. Its operations are partially supported by funding from the IIT Bombay alumni batch of 1994. The Fritz and SkyPortal projects acknowledge the generous support of The Gordon and Betty Moore Foundation.",
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"message_text": "Shreya Anand (Stanford), Anirudh Salgundi (UNC), Robert Stein (UMD), Vishwajeet Swain (IIT-B), Yogesh Wagh (IIT-B), Xander J. Hall (CMU), Mansi Kasliwal (Caltech), Eric Bellm (UW), Michael Coughlin (UMN), Theophile Jegou du Laz (Caltech), and Antonella Palmese (CMU) report,\n\nOn behalf of the Zwicky Transient Facility (ZTF) and Global Relay of Observatories Watching Transients Happen (GROWTH) collaborations: \n\nWe observed the localization region of the LVK low-significance burst trigger S251031dw with the Palomar 48-inch telescope, equipped with the 47 square degree ZTF camera (Bellm et al. 2019, Graham et al. 2019). We started observations in the g- and r-band beginning at 2025-11-01 12:22 UTC, approximately 15.2 hours after merger. We covered 23.1% of the reported localization region on 2025-10-31 and 60.9% of the localization on 2025-11-01. This estimate accounts for chip gaps. ~30% of the tiled localization was at a low galactic latitude. Each exposure was 200s with a median r-band depth of 21.1 mag. \n \nThe images were processed in real-time through the ZTF reduction and image subtraction pipelines at IPAC to search for potential counterparts (Masci et al. 2019). AMPEL (Nordin et al. 2019, Stein et al. 2021) was used to search the alerts database for candidates. We reject stellar sources (Tachibana and Miller 2018) and moving objects, and apply machine learning algorithms (Mahabal et al. 2019), removing candidates with history of variability prior to the merger time. \n\nAfter filtering, 58 transient candidates remain, all within the 95.0% localization of the skymap. None of these candidates have fast evolution consistent with kilonovae. We perform additional vetting of these candidates, and highlight 9 candidates that appear to be young and SN-like, or AGN-like, as candidates of interest in the burst search, in the table below: \n\n\n| ZTF Name | IAU Name | RA (deg) | DEC (deg) | MJD | Filt | Mag | MagErr | Note |\n| ------------ | ---------- | ---------- | ---------- | -------- | ---- | ----- | ------ | -------- |\n| ZTF25acchitl | -- | 127.996770 | -27.778576 | 60980.52 | r | 20.63 | 0.11 | AGN-like |\n| ZTF25accnabz | -- | 128.305827 | -23.858020 | 60980.52 | r | 21.60 | 0.19 | AGN-like |\n| ZTF25acchdbq | -- | 121.061164 | -19.087422 | 60980.50 | r | 20.35 | 0.21 | AGN-like |\n| ZTF25acchjjz | -- | 127.829510 | -20.792424 | 60980.52 | r | 20.88 | 0.12 | AGN-like |\n| ZTF25acchljm | -- | 130.363870 | -23.822309 | 60980.52 | r | 20.87 | 0.13 | AGN-like |\n| ZTF25accniqx | -- | 131.262056 | -20.691176 | 60980.54 | r | 20.16 | 0.15 | AGN-like |\n| ZTF25acchigq | -- | 128.491126 | -24.746190 | 60980.52 | r | 21.26 | 0.15 | AGN-like |\n| ZTF25acchszc | AT2025acno | 137.799671 | -22.017226 | 60980.54 | r | 20.93 | 0.13 | SN-like |\n| ZTF25acchppz | AT2025acep | 135.228502 | -23.983061 | 60980.54 | r | 19.48 | 0.05 | SN-like |\n\nZTF25acchszc appears to be a rising young, blue supernova in a host galaxy (no redshift available). ZTF25acchppz is offset 9\" from a potential host galaxy at z=0.082, and is therefore unlikely to be associated with the burst source. Further follow-up is encouraged.\n\nBased on observations obtained with the Samuel Oschin Telescope 48-inch and the 60-inch Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. ZTF is supported by the National Science Foundation under Award #2407588 and a partnership including Caltech, USA; Caltech/IPAC, USA; University of Maryland, USA; University of California, Berkeley, USA; University of Wisconsin at Milwaukee, USA; Cornell University, USA; Drexel University, USA; University of North Carolina at Chapel Hill, USA; Institute of Science and Technology, Austria; National Central University, Taiwan; Operations are conducted by Caltech's Optical Observatory (COO) and Caltech/IPAC. GROWTH acknowledges the generous support of the NSF under PIRE Grant No 1545949. Alert database searches are done by AMPEL (Nordin et al. 2019) and Kowalski (Duev et al. 2019). The GROWTH India Telescope (GIT, Kumar et al., 2022) is set up by the Indian Institute of Astrophysics (IIA) and the Indian Institute of Technology Bombay (IITB) with funding from DST-SERB and IUSSTF. Its operations are partially supported by funding from the IIT Bombay alumni batch of 1994. The Fritz and SkyPortal projects acknowledge the generous support of The Gordon and Betty Moore Foundation.",
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