July 2025 - vsnet-grb-info - ooruri.kusastro.kyoto-u.ac.jp

[vsnet-grb-info 39230] LIGO/Virgo/KAGRA S250726ak: Updated Sky localization
by GCN Circulars 27 Jul '25

27 Jul '25

TITLE: GCN CIRCULAR NUMBER: 41174 SUBJECT: LIGO/Virgo/KAGRA S250726ak: Updated Sky localization DATE: 25/07/27 10:32:41 GMT FROM: Lorenzo Pompili at Max Planck Institute for Gravitational Physics <lorenzo.pompili(a)aei.mpg.de> The LIGO Scientific Collaboration, the Virgo Collaboration, and the KAGRA Collaboration report: We 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 S250726ak (GCN Circular 41171). 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: https://gracedb.ligo.org/superevents/S250726ak For the Bilby.multiorder.fits,0 sky map, the 90% credible region is 361 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 3333 +/- 1448 Mpc (a posteriori mean +/- standard deviation). For 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/. [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 View this GCN Circular online at https://gcn.nasa.gov/circulars/41174. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 39229] The EP-WXT trigger 01709195487 is likely a flaring star
by GCN Circulars 27 Jul '25

27 Jul '25

TITLE: GCN CIRCULAR NUMBER: 41173 SUBJECT: The EP-WXT trigger 01709195487 is likely a flaring star DATE: 25/07/27 09:47:00 GMT FROM: EP Team at NAOC/CAS <ep_ta(a)bao.ac.cn> R. D. Liang (NAO, CAS), Y.-H. I. Yin (NJU), Z. X. Ling (NAO, CAS) on behalf of the Einstein Probe (EP) team: The EP-WXT trigger 01709195487 at the time of 2025-07-27T07:34:04, is likely a stellar flare associated with UPM J1905-2819. The estimated flux of the flare is around 1.2 x 10^-10 erg/s/cm^2 in 0.5-4.0 keV. The autonomous follow-up observation with the Follow-up X-ray Telescope (FXT) detected a source at R.A. = 286.3565, DEC = -28.3311 deg (J2000) with an uncertainty of 20 arcsec in radius (90% C.L. statistical and systematic) within the WXT error circle, whose position is around 9 arcsec away from the high proper motion star UPM J1905-2819. Launched on January 9, 2024, EP is a space X-ray observatory to monitor the soft X-ray sky with X-ray follow-up capability (Yuan et al. 2022, Handbook of X-ray and Gamma-ray Astrophysics). View this GCN Circular online at https://gcn.nasa.gov/circulars/41173. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 39228] Swift detection of the Soft Gamma Repeater PSR J1647-4552
by GCN Circulars 26 Jul '25

26 Jul '25

TITLE: GCN CIRCULAR NUMBER: 41172 SUBJECT: Swift detection of the Soft Gamma Repeater PSR J1647-4552 DATE: 25/07/26 23:21:53 GMT FROM: David Palmer at LANL <palmer(a)lanl.gov> S. Dichiara (PSU), R. Gupta (NASA GSFC) and D. M. Palmer (LANL) report on behalf of the Neil Gehrels Swift Observatory Team: At 2025-07-26 22:49:05 UT, the Swift Burst Alert Telescope (BAT) triggered and located Soft Gamma Repeater (SGR) PSR J1647-4552 (trigger=1337165). For this previously-known source, Swift is configured to NOT automatically slew to the location. The BAT on-board calculated location is RA, Dec 251.779, -45.871 which is RA(J2000) = 16h 47m 07s Dec(J2000) = -45d 52' 14" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). This position is within 34 arcseconds of the SGR catalogued location. The BAT light curve showed a single spike structure (at the 64 ms resolution of the immediately-available lightcurve) with a duration of about 128 ms sec. The peak count rate was ~2700 counts/sec (15-350 keV), at ~0 sec after the trigger. There have been 12 previous detections of bursts from this source by BAT, most recently in Feb 2020. The detections have come singly or in clusters of 2-3 within minutes to hours. View this GCN Circular online at https://gcn.nasa.gov/circulars/41172. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 39227] LIGO/Virgo/KAGRA S250726ak: Identification of a GW compact binary merger candidate
by GCN Circulars 26 Jul '25

26 Jul '25

TITLE: GCN CIRCULAR NUMBER: 41171 SUBJECT: LIGO/Virgo/KAGRA S250726ak: Identification of a GW compact binary merger candidate DATE: 25/07/26 09:16:48 GMT FROM: Cassius Melo at Universidade Federal de Alfenas - UNIFAL-MG <cassiusanderson.melo(a)ligo.org> The LIGO Scientific Collaboration, the Virgo Collaboration, and the KAGRA Collaboration report: We identified the compact binary merger candidate S250726ak during real-time processing of data from LIGO Hanford Observatory (H1), LIGO Livingston Observatory (L1), and Virgo Observatory (V1) at 2025-07-26 08:28:15.370 UTC (GPS time: 1437553713.370). The candidate was found by the cWB [1], cWB BBH [2], GstLAL [3], MBTA [4], PyCBC Live [5], and SPIIR [6] analysis pipelines. S250726ak is an event of interest because its false alarm rate, as estimated by the online analysis, is 4.7e-12 Hz, or about one in 1e4 years. The event's properties can be found at this URL: https://gracedb.ligo.org/superevents/S250726ak The classification of the GW signal, in order of descending probability, is BBH (>99%), Terrestrial (<1%), BNS (<1%), or NSBH (<1%). Assuming 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%. [7] Using the masses and spins inferred from the signal, the probability of matter outside the final compact object (HasRemnant) is <1%. [7] 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%. The source chirp mass falls with highest probability in the bin (22.0, 44.0) solar masses, assuming the candidate is astrophysical in origin. Two sky maps are available at this time and can be retrieved from the GraceDB event page: * bayestar.multiorder.fits,0, an initial localization generated by BAYESTAR [8], distributed via GCN and SCiMMA notices about 24 seconds after the candidate event time. * bayestar.multiorder.fits,1, an initial localization generated by BAYESTAR [8], distributed via GCN and SCiMMA notices about 4 minutes after the candidate event time. The preferred sky map at this time is bayestar.multiorder.fits,1. For the bayestar.multiorder.fits,1 sky map, the 90% credible region is 1027 deg2. Marginalized over the whole sky, the a posteriori luminosity distance estimate is 3384 +/- 1067 Mpc (a posteriori mean +/- standard deviation). For 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/. [1] Klimenko et al. PRD 93, 042004 (2016) doi:10.1103/PhysRevD.93.042004 [2] T. Mishra et al. PRD 105, 083018 (2022) doi:10.1103/PhysRevD.105.083018 [3] 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 [4] Alléné et al. CQG 42, 105009 (2025) doi:10.1088/1361-6382/add234 [5] Dal Canton et al. ApJ 923, 254 (2021) doi:10.3847/1538-4357/ac2f9a [6] Chu et al. PRD 105, 024023 (2022) doi:10.1103/PhysRevD.105.024023 [7] Chatterjee et al. ApJ 896, 54 (2020) doi:10.3847/1538-4357/ab8dbe [8] Singer & Price PRD 93, 024013 (2016) doi:10.1103/PhysRevD.93.024013 View this GCN Circular online at https://gcn.nasa.gov/circulars/41171. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 39226] GRB 250725A: Swift-XRT refined Analysis
by GCN Circulars 25 Jul '25

25 Jul '25

TITLE: GCN CIRCULAR NUMBER: 41170 SUBJECT: GRB 250725A: Swift-XRT refined Analysis DATE: 25/07/25 19:07:22 GMT FROM: Phil Evans at U of Leicester <pae9(a)star.le.ac.uk> S. Dichiara (PSU), J.A. Kennea (PSU), D.N. Burrows (PSU), K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester), V. D'Elia (SSDC & INAF-OAR), B. Sbarufatti (INAF-OAB), C. Salvaggio (INAF-OAB) and P.A. Evans report on behalf of the Swift-XRT team: We have analysed 7.4 ks of XRT data for GRB 250725A, from 828 s to 53.2 ks after the trigger. The data comprise 64 s in Windowed Timing (WT) mode with the remainder in Photon Counting (PC) mode. The light curve can be modelled with an initial power-law decay with an index of alpha=1.14 (+/-0.06), followed by a break at T+13.4 ks to an alpha of 2.2 (+0.4, -0.3). A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 1.72 (+0.09, -0.08). The best-fitting absorption column is 2.7 (+2.3, -2.1) x 10^22 cm^-2, at a redshift of 5.26, in addition to the Galactic value of 9.2 x 10^20 cm^-2 (Willingale et al. 2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 4.0 x 10^-11 (4.7 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Galactic foreground: 9.2 x 10^20 cm^-2 Intrinsic column: 2.7 (+2.3, -2.1) x 10^22 cm^-2 at z=5.26 Photon index: 1.72 (+0.09, -0.08) If the light curve continues to decay with a power-law decay index of 2.2, the count rate at T+24 hours will be 4.0 x 10^-3 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.6 x 10^-13 (1.9 x 10^-13) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/01336720. This circular is an official product of the Swift-XRT team. View this GCN Circular online at https://gcn.nasa.gov/circulars/41170. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 39225] GRB 250725A: Fermi GBM Observation
by GCN Circulars 25 Jul '25

25 Jul '25

TITLE: GCN CIRCULAR NUMBER: 41169 SUBJECT: GRB 250725A: Fermi GBM Observation DATE: 25/07/25 17:08:33 GMT FROM: Matt Godwin <msg0028(a)uah.edu> Matt Godwin (UAH), R. Sonawane (IISER TVM) and C. Meegan (UAH) report on behalf of the Fermi Gamma-ray Burst Monitor Team: "At 01:51:34.81 UT on 25 July 2025, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 250725A (trigger 775101099/250725077). which was also detected by Swift XRT (Evans et al. 2025, GCN 41152), Konus-Wind (Frederiks et al. 2025, GCN 41166), and Fermi LAT (Airasca et al. 2025, GCN 41161). The Fermi GBM on-ground location is consistent with the Swift XRT position. The redshift observed by VLT (Thakur et al. 2025, GCN 41160) is z = 5.26. The angle from the Fermi LAT boresight is 24 degrees. The GBM light curve consists of one main peak and a weaker secondary peak with a duration (T90) of about 9.5 s (50-300 keV). The time-averaged spectrum from T0+0.003 to T0+11.904 s is best fit by a Band function with Epeak = 161 +/- 7 keV, alpha = -0.47 +/- 0.05, and beta = -2.7 +/- 0.2. The event fluence (10-1000 keV) in this time interval is (1.18 +/- 0.03)E-05 erg/cm^2. The 1-sec peak photon flux measured starting from T0+1.7 s in the 10-1000 keV band is 18 +/- 0.4 ph/s/cm^2. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog: https://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html For Fermi GBM data and info, please visit the official Fermi GBM Support Page: https://fermi.gsfc.nasa.gov/ssc/data/access/gbm/" View this GCN Circular online at https://gcn.nasa.gov/circulars/41169. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 39224] LIGO/Virgo/KAGRA S250725j: Updated Sky localization
by GCN Circulars 25 Jul '25

25 Jul '25

TITLE: GCN CIRCULAR NUMBER: 41168 SUBJECT: LIGO/Virgo/KAGRA S250725j: Updated Sky localization DATE: 25/07/25 17:04:56 GMT FROM: Lorenzo Pompili at Max Planck Institute for Gravitational Physics <lorenzo.pompili(a)aei.mpg.de> The LIGO Scientific Collaboration, the Virgo Collaboration, and the KAGRA Collaboration report: We 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 S250725j (GCN Circular 41154). 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: https://gracedb.ligo.org/superevents/S250725j For the Bilby.multiorder.fits,0 sky map, the 90% credible region is well fit by an ellipse with an area of 19 deg2 described by the following DS9 region (right ascension, declination, semi-major axis, semi-minor axis, position angle of the semi-minor axis): icrs; ellipse(15h32m, -36d06m, 3.23d, 1.84d, 158.46d) Marginalized over the whole sky, the a posteriori luminosity distance estimate is 380 +/- 93 Mpc (a posteriori mean +/- standard deviation). For 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/. [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 View this GCN Circular online at https://gcn.nasa.gov/circulars/41168. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 39223] GRB 250725A: Swift-BAT refined analysis
by GCN Circulars 25 Jul '25

25 Jul '25

TITLE: GCN CIRCULAR NUMBER: 41167 SUBJECT: GRB 250725A: Swift-BAT refined analysis DATE: 25/07/25 16:18:21 GMT FROM: Rahul Gupta at NASA GSFC <rahul.gupta(a)nasa.gov> T. Parsotan (GSFC), S. D. Barthelmy (GSFC), P. A. Evans (U Leicester), R. Gupta (GSFC), H. A. Krimm (NSF), S. Laha (GSFC/UMBC), A. Y. Lien (U Tampa), C. B. Markwardt (GSFC), M. J. Moss (GSFC), D. M. Palmer (LANL), D. Sadaula (GSFC/UMBC), T. Sakamoto (AGU) (i.e. the Swift-BAT team): Using the data set from T-239 to T+963 sec from the recent telemetry downlink, we report further analysis of BAT GRB 250725A (trigger #1336720) (Evans, et al., GCN Circ. 41152). The BAT ground-calculated position is RA, Dec = 35.459, -82.786 deg which is RA(J2000) = 02h 21m 50.1s Dec(J2000) = -82d 47' 10.4" with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment). The partial coding was 34%. The mask-weighted BAT light curve shows multi-peaked emission episode starting ~T-2 sec, with a sharp rise and a structured decay extending over ~12 seconds. T90 (15-350 keV) is 9.58 +- 0.25 sec (estimated error including systematics). The time-averaged spectrum from T-1.77 to T+9.50 sec is best fit by a power law with an exponential cutoff. This fit gives a photon index 0.81 +- 0.19, and Epeak of 207.2 +- 105.6 keV (chi squared 38.63 for 56 d.o.f.). For this model the total fluence in the 15-150 keV band is 5.0 +- 0.1 x 10^-06 erg/cm2 and the 1-sec peak flux measured from T+0.06 sec in the 15-150 keV band is 12.5 +- 0.6 ph/cm2/sec. A fit to a simple power law gives a photon index of 1.15 +- 0.05 (chi squared 49.20 for 57 d.o.f.). All the quoted errors are at the 90% confidence level. The results of the batgrbproduct analysis are available at https://swift.gsfc.nasa.gov/results/batgrbcat/BAT_refined_circular/1336720 View this GCN Circular online at https://gcn.nasa.gov/circulars/41167. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 39222] Konus-Wind detection of GRB 250725A
by GCN Circulars 25 Jul '25

25 Jul '25

TITLE: GCN CIRCULAR NUMBER: 41166 SUBJECT: Konus-Wind detection of GRB 250725A DATE: 25/07/25 15:53:14 GMT FROM: Dmitry Frederiks at Ioffe Institute <fred(a)mail.ioffe.ru> D. Frederiks, A.Lysenko, A. Ridnaia, D. Svinkin, A. Tsvetkova, M. Ulanov, and T. Cline, on behalf of the Konus-Wind team, report: The long GRB 250525A (Fermi-GBM detection: The Fermi GBM team, GCN 41150; Swift detection: Evans et al., GCN 41152; SVOM/GRM observation: Wang et al., GCN 41164) triggered Konus-Wind (KW) at T0=6698.029 s UT (01:51:38.029). The burst shows a multi-peaked structure with a total duration of ~12 s. The emission is seen up to ~1.5 MeV. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB250725_T06698/ As observed by Konus-Wind, the burst had a fluence of (1.19 ± 0.10)x10^-5 erg/cm^2 and a 64-ms peak energy flux, measured from T0 + 0.512 s, of (4.16 ± 0.41)x10^-6 erg/cm^2/s (both in the 20 keV - 10 MeV energy range). The time-integrated spectrum (measured from T0 to T0+16.640 s) is best fit in the 20 keV - 15 MeV range by a GRB (Band) function with the following model parameters: the low-energy photon index alpha = -0.41 (-0.13,+0.15), the high energy photon index beta = -2.75 (-0.25,+0.18), the peak energy Ep = 155 (-9,+9) keV, chi2 = 89/97 dof. Assuming the redshift z=5.26 (Thakur et al., GCN 41160) and a standard cosmology with H_0 = 67.3 km/s/Mpc, Omega_M = 0.315, and Omega_Lambda = 0.685 (Planck Collaboration, 2014), we estimate the burst isotropic energy release E_iso to (5.85 ± 0.49)x10^53 erg, the isotropic peak luminosity L_iso to (1.30 ± 0.13)x10^52 erg/s, and the rest-frame peak spectral energy Ep,z to (970 ± 56) keV. With the obtained estimates, GRB 250725A is consistent with 68% prediction bands of both 'Amati' and 'Yonetoku' relations for the sample of >300 long KW GRBs with known redshifts (Tsvetkova et al., 2017; Tsvetkova et al., 2021), see http://www.ioffe.ru/LEA/GRBs/GRB250725_T06698/GRB250725A_rest_frame.pdf All the quoted errors are estimated at the 68% confidence level. All the presented results are preliminary. View this GCN Circular online at https://gcn.nasa.gov/circulars/41166. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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[vsnet-grb-info 39221] LIGO/Virgo/KAGRA S250725j: NED Galaxies in the 3-Initial Localization Volume
by GCN Circulars 25 Jul '25

25 Jul '25

TITLE: GCN CIRCULAR NUMBER: 41165 SUBJECT: LIGO/Virgo/KAGRA S250725j: NED Galaxies in the 3-Initial Localization Volume DATE: 25/07/25 15:34:28 GMT FROM: David Cook at Caltech/IPAC-NED <dcook(a)ipac.caltech.edu> 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) On behalf of the NASA/IPAC Extragalactic Database (NED) Team. We spatially cross-matched the LVK S250725j-3-Initial sky localization with the NED Local Volume Sample (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 594 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: Full List Download: https://ned.ipac.caltech.edu/uri/NED::GWFglist/fits/S250725j/3 Top 20 List Download: https://ned.ipac.caltech.edu/uri/NED::GWFglist/fits/S250725j/3/20 The 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. | 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| |-------------------------|--------------|--------------|-------|-----------|-----------|-------|---------|------------|------------|------------|------------|--------|----------| |WISEA J152748.68-355739.1| 231.95286| -35.96088| G| 452.82| null| null| null| 13.128| 0.132| 10.686| 0.006|4.47e-06| 4.56e-08| |WISEA J153844.18-344009.1| 234.68409| -34.66922| G| 480.22| null| null| null| 12.995| 0.143| 10.976| 0.010|3.62e-06| 3.52e-08| |WISEA J153525.42-344743.9| 233.85592| -34.79554| G| 524.15| null| null| null| 13.715| 0.214| 11.189| 0.018|3.34e-06| 2.91e-08| |WISEA J152653.58-355046.3| 231.72329| -35.84620| G| 431.02| null| null| null| 13.223| 0.157| 10.966| 0.009|4.06e-06| 2.89e-08| |WISEA J154628.27-340002.3| 236.61826| -34.00070| G| 425.21| null| null| null| 13.479| 0.169| 9.563| 0.006|1.10e-06| 2.79e-08| |WISEA J153024.70-351033.1| 232.60293| -35.17588| G| 529.76| null| null| null| 12.578| 0.113| 11.182| 0.008|2.90e-06| 2.58e-08| |WISEA J153324.20-354028.6| 233.35085| -35.67462| G| 435.53| null| null| null| 13.377| 0.171| 11.600| 0.011|5.94e-06| 2.45e-08| |WISEA J153416.18-351536.7| 233.56786| -35.26055| G| 415.65| null| null| null| 13.472| 0.230| 11.551| 0.011|5.56e-06| 2.18e-08| |WISEA J153550.83-352815.7| 233.96181| -35.47105| G| 452.48| null| null| null| 12.155| 0.114| 11.835| 0.011|5.59e-06| 2.01e-08| |WISEA J152918.46-355636.4| 232.32692| -35.94346| G| 469.28| null| null| null| 13.745| 0.216| 11.703| 0.011|4.59e-06| 1.97e-08| |WISEA J153406.90-352554.3| 233.52878| -35.43177| G| 444.26| 0.49| null| null| 12.177| 0.090| 12.031| 0.023|5.84e-06| 1.68e-08| |WISEA J153130.18-350639.3| 232.87576| -35.11092| G| 419.28| 0.79| null| null| 12.607| 0.111| 11.785| 0.011|4.73e-06| 1.49e-08| |WISEA J153144.43-352246.2| 232.93514| -35.37951| G| 474.13| null| null| null| 12.991| 0.145| 12.199| 0.016|4.99e-06| 1.38e-08| |WISEA J153031.02-350955.4| 232.62929| -35.16539| G| 478.85| null| null| null| 13.515| 0.194| 12.117| 0.015|4.17e-06| 1.28e-08| |WISEA J153512.75-350712.9| 233.80314| -35.12027| G| 470.25| null| null| null| 13.554| 0.177| 12.400| 0.011|5.07e-06| 1.18e-08| |WISEA J152932.42-350115.2| 232.38508| -35.02090| G| 538.67| null| null| null| 13.523| 0.198| 11.824| 0.007|2.30e-06| 1.16e-08| |WISEA J154625.51-332529.0| 236.60631| -33.42475| G| 445.85| null| null| null| 12.552| 0.113| 10.145| 0.007|6.91e-07| 1.13e-08| |WISEA J153354.06-351626.2| 233.47529| -35.27397| G| 397.36| null| null| null| 13.103| 0.132| 12.174| 0.012|5.35e-06| 1.08e-08| |WISEA J153959.24-350547.6| 234.99684| -35.09658| G| 378.08| null| null| null| 13.710| 0.194| 11.652| 0.010|3.45e-06| 1.05e-08| |WISEA J153052.19-345946.7| 232.71748| -34.99631| G| 454.26| 0.79| null| null| 12.909| 0.128| 12.253| 0.014|4.22e-06| 1.01e-08| Table 1: Top 20 galaxies in NED-LVS that fall in the 90% probability volume for S250725j 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). View this GCN Circular online at https://gcn.nasa.gov/circulars/41165. --- To unsubscribe, open this link in a web browser: https://gcn.nasa.gov/unsubscribe/eyJhbGciOiJIUzI1NiJ9.eyJlbWFpbCI6InZzbmV0L…

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