TITLE: GCN CIRCULAR
NUMBER: 37617
SUBJECT: NuEm-240926A / IC240926A: BZQJ0955+4532 ~0.6m optical decay and rebrightening detection by MASTER
DATE: 24/09/27 10:49:56 GMT
FROM: Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov(a)xray.sai.msu.ru>
V.Lipunov, K.Zhirkov, D.Vlasenko, I.Panchenko, A.Kuznetsov (Lomonosov MSU), A.Sosnovskij (CrAO RAS), P.Balanutsa, G.Antipov, N.Tiurina, E.Gorbovskoy, M.Gulyaev, Ya.Kechin, V.Senik (Lomonosov MSU),
O.Gress, N.Budnev(ISU),
D.Buckley (…
[View More]SAAO),
C.Francile. F. Podesta, R.Podesta (Observatorio Astronomico Felix AguilarOAFA),
R. Rebolo (The Instituto de Astrofisica de Canarias),
A. Tlatov, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory),
A. Gabovich, V.Yurkov (Blagoveschensk Educational StateUniversity)
MASTER Global robotic net (http://observ.pereplet.ru Lipunov et al.,2010,Advances in Astronomy,2010,30L)
started observation of NuEm-240926A / IC240926A alert (Ayala et al. GCN 37614,
The HAWC transit interval: 2024/09/26 13:12:19-19:01:26 UT, socket notice=19:10:33 ) at MASTER-Amur (2024-09-26 19:16:05, clouds, summary reduction) and at MASTER-Tavrida (just after the error-box rise since 21:59:06).
We found the blazar BZQJ0955+4532 to be in the off-state in first hours and then switched to the on-state no later than several hours (so as trigger time is not known now)
after the event. The amplitude of this variability is about 0.6m (calibrated by field stars from our 4 square degrees field of view).
This effect is observed the same as for TXS 0506+056, also found by MASTER for IC170922
(Lipunov et al. ApJL 896, 2, L19 https://ui.adsabs.harvard.edu/abs/2020ApJ...896L..19L/abstract )
Observations and reduction will be continued.
View this GCN Circular online at https://gcn.nasa.gov/circulars/37617.
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TITLE: GCN CIRCULAR
NUMBER: 37616
SUBJECT: GRB 240926A: SVOM/GRM observation
DATE: 24/09/27 07:55:33 GMT
FROM: wenlongzhang2018(a)163.com
SVOM/GRM team: Wen-Long Zhang, Yue Huang, Yan-Ting Zhang, Jia-Cong Liu, Yong-Wei Dong, Jiang-Tao Liu, Shi-Jie Zheng, Jian-Chao Sun, Wen-Jun Tan, Jiang He, Chen-Wei Wang, Min Gao, Hao-Xuan Guo, Lu Li, Yong-Ye Li, Hong-Wei Liu, Xin Liu, Hao-Li Shi, Li-Ming Song, You-Li Tuo, Hao-Xi Wang, Jin Wang, Jin-Zhou Wang, Ping Wang, Rui-Jie Wang, Yu-Xi Wang, Bo-…
[View More]Bing Wu, Shao-Lin Xiong, Jian-Ying Ye, Yi-Tao Yin, Wen-Hui Yu, Fan Zhang, Li Zhang, Peng Zhang, Shuang-Nan Zhang, Shu-Min Zhao, Xiao-Yun Zhao, Chao Zheng (IHEP), Maria-Grazia Bernardini (LUPM/INAF-OAB), Laurent Bouchet (IRAP), David Corre (CEA), Tais Maiolino (LUPM), Frédéric Piron (LUPM), Stéphane Schanne (CEA), Jingwei Wang (IAP)
SVOM JSWG: Jian-Yan Wei (NAOC), Bertrand Cordier (CEA), Shuang-Nan Zhang (IHEP), Stéphane Basa (LAM), JeanLuc Attéia (IRAP), Arnaud Claret (CEA), Zi-Gao Dai (USTC), Frédéric Daigne (IAP), Jin-Song Deng (NAOC), Andrea Goldwurm (APC), Diego Götz (CEA), Xu-Hui Han (NAOC), Cyril Lachaud (APC), En-Wei Liang (GXU), Yu-Lei Qiu (NAOC), Susanna Vergani (Obs.Paris), Jing Wang (NAOC), Chao Wu (NAOC), Li-Ping Xin (NAOC), Bing Zhang (UNLV)
report on behalf of the SVOM team:
During the commissioning phase, the SVOM/GRM was triggered in-flight by GRB 240926A (SVOM trigger reference: sb24092601) at 2024-09-26T11:42:45.000 UT (T0).
The real-time alert data and light curves of SVOM/GRM were downlinked to the ground through the VHF system with low latency. The light curves show that this burst consists of multiple pulses with a T90 of 55.54 s -0.39/+0.48 s.
The SVOM/GRM light curve can be found here:
https://www.bursthub.cn//admin/static/svgrb240926A.png
The SVOM/GRM on-ground localization of this burst is (J2000):
RA: 241.92 deg
DEC: 40.31 deg
Error: 3.78 deg (1 sigma, statistical only)
We caution that the calibration of SVOM/GRM is undergoing and this localization is subject to systematic errors. The localization may be improved in the refined analysis.
At the time of the burst ECLAIRs was not in operational mode.
The Space Variable Objects Monitor (SVOM) is a China-France joint mission led by the Chinese National Space Administration (CNSA, China), National Center for Space Studies (CNES, France) and the Chinese Academy of Sciences (CAS, China), which is dedicated to observing gamma-ray bursts and other transient phenomena in the energetic universe. GRM is developed by the Institute of High Energy Physics (IHEP) of CAS.
The SVOM/GRM point of contact for this burst is: Wen-Long Zhang (IHEP)(zhangwl(a)ihep.ac.cn)
View this GCN Circular online at https://gcn.nasa.gov/circulars/37616.
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TITLE: GCN CIRCULAR
NUMBER: 37615
SUBJECT: EP trigger ID 01709061302: the X-ray transient is likely a stellar flare event
DATE: 24/09/27 02:48:42 GMT
FROM: EP Team at NAOC/CAS <ep_ta(a)bao.ac.cn>
Q. C. Shui (IHEP, CAS), D. Y. Li (NAOC, CAS), C. Zhou (HUST), G. Y. Zhao (SYSU), T. C. Zheng (PMO, CAS), and W. Yuan (NAOC, CAS) on behalf of the Eintein Probe team
The Follow-up X-ray Telescope (FXT) on board the Einstein Probe (EP) mission performed an autonomous observation on the X-…
[View More]ray transient detected by EP-WXT (trigger ID 01709061302). The observation started at 2024-09-27 01:08:38.0 (UTC), about 5 minutes after the EP-WXT trigger time. The FXT onboard data processing system detected a source at R.A. = 350.5437 deg, DEC = -3.0283 deg (J2000) with an uncertainty of about 20 arcsec (radius, 90% C.L. statistical and systematic), consistent with the position of the WXT transient within the uncertainties. The FXT source is associated with a K-type star, PM J23221-0301, at a distance of about 46 pc and located about 8 arcsec away from the FXT position. We suggest that this X-ray transient is likely a stellar flare event.
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/37615.
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TITLE: GCN CIRCULAR
NUMBER: 37614
SUBJECT: AMON Coincidence Alert from the sub-threshold IceCube-HAWC search NuEm-240926A
DATE: 24/09/26 19:34:25 GMT
FROM: Hugo Ayala at Pennsylvania State University <hgayala(a)psu.edu>
The AMON, IceCube, and HAWC collaborations report:
The AMON NuEm stream channel found a coincidence alert from the
IceCube online neutrino selection + HAWC daily monitoring analysis.
The analysis looks for IceCube neutrino events -mostly atmospheric
in origin- …
[View More]around the position and transit time of a HAWC cluster of
likely gamma rays, as identified in the integrated observations from
a single transit, in this case having a duration of 6.06 hours.
The HAWC transit interval starts from 2024/09/26 13:12:19 UT to
2024/09/26 19:01:26 UT
(End of the HAWC transit time)
The location of the coincidence is reported as
RA (J2000): 149.97 deg
Dec (J2000): 46.22 deg
Location uncertainty (50% containment): 0.22 deg (statistical only).
Location uncertainty (90% containment): 0.41 deg (statistical only).
The false alarm rate (FAR) of this coincidence is 3.41 per year.
We encourage follow-up observations of the alert region contingent on
the availability of resources and interest, given the quoted FAR.
A quick search in the region reveals the 4FGL source J0959.6+4606
it's ~0.1 deg away from the coincidence position.
Other 4FGL sources that appear nearby are J0958.0+4728, J1008.1+4706
and J0950.2+4553
AMON seeks to perform a real-time correlation analysis of the
high-energy signals across all known astronomical messengers. More
information about AMON can be found in https://www.amon.psu.edu/
Information on the IceCube collaboration: http://icecube.wisc.edu/
Information on the HAWC collaboration: https://www.hawc-observatory.org
View this GCN Circular online at https://gcn.nasa.gov/circulars/37614.
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TITLE: GCN CIRCULAR
NUMBER: 37613
SUBJECT: Konus-Wind detection of GRB 240905B
DATE: 24/09/26 15:50:34 GMT
FROM: Dmitry Svinkin at Ioffe Institute <svinkin(a)mail.ioffe.ru>
D. Svinkin, D. Frederiks, M. Ulanov, A. Tsvetkova,
A. Lysenko, A. Ridnaia, and T. Cline
on behalf of the Konus-Wind team, report:
The short-duration GRB 240905B
(Fermi-GBM detection: The Fermi GBM team, GCN 37389; Dalessi et al., GCN 37436;
AstroSat-CZTI detection: Joshi et al, GCN 37391;
Fermi-LAT detection:…
[View More] Gupta et al., GCN 37418;
IPN triangulation: Kozyrev et al., GCN 37455;
VZLUSAT-2 detection: Dafcikova et al., GCN 37601)
triggered Konus-Wind at T0=16038.558 s UT (04:27:18.558).
The burst light curve shows a multipeaked structure
which starts at ~T0-0.1 s and has a total duration of ~1 s.
The emission is seen up ~5 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB240905_T16038/
As observed by Konus-Wind, the burst
had a fluence of 1.68(-0.28,+0.35)x10^-5 erg/cm2,
and a 16-ms peak flux, measured from T0+0.432 s,
of 4.13(-1.05,+1.17)x10^-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).
The time-averaged spectrum of the burst
(measured from T0 to T0+8.448 s)
is best fit in the 20 keV - 10 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with alpha = -0.54(-0.18,+0.21)
and Ep = 1229(-251,+357) keV (chi2 = 92/87 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.2
(chi2 = 92/86 dof).
All the quoted errors are at the 90% confidence level.
All the quoted values are preliminary.
View this GCN Circular online at https://gcn.nasa.gov/circulars/37613.
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TITLE: GCN CIRCULAR
NUMBER: 37612
SUBJECT: GRB 240529A: FRAM-ORM early optical afterglow observations reveal plateau and rebrightening
DATE: 24/09/26 15:18:39 GMT
FROM: Martin Jelinek at Astro.Inst-AVCR,Ondrejov <martin.jelinek(a)asu.cas.cz>
Martin Jelinek, Alzbeta Malenakova, Jan Strobl (ASU CAS Ondrejov, CZ), Sergey Karpov, Martin Masek, Petr Janecek, Jakub Jurysek, Jan Ebr, Ronan Cunniffe, Petr Travnicek and Michael Prouza (Institute of Physics, Prague, CZ)
report:
The 25cm …
[View More]robotic telescope FRAM-ORM at La Palma (Spain) responded automatically to the Swift alert of GRB 240529A (Eyles-Ferris et al., GCN 36556; Osborne et al., GCN 36557; Dichiara et al., GCN 36564; Markwardt et al., GCN 36566). We obtained a series of unfiltered 20s and 60s exposures starting at 02:59:07.8 UT, (37s post-trigger) and covering two hours of the afterglow evolution.
Due to an ongoing focusing run at the time of the alert, initial frames were out of focus. Nevertheless, the optical afterglow was clearly detected in all focused and defocused images, allowing for a comprehensive early-time light curve from an early plateau through initial decay to the start of a substantial rebrightening.
Combining our data with published measurements (Dutton et al., GCN 36568; Mo et al., GCN 36569), we reconstruct the overall light curve behavior:
a) Initial plateau: The afterglow maintained a nearly constant brightness, declining marginally from r~15.2 to 15.5 during the first 2ks post-trigger.
b) Gradual decay: The initial plateau gradually transitioned to a decay with the decay index consistent with the later decay.
c) Rebrightening: The trend reverses suddenly at ~4.2ks and the afterglow nearly reaches its initial brightness at a second peak of r~15.8 at t~10ks.
d) Final decay: after 10ks, the afterglow decays with a power-law index alpha ~ 1.85, consistent with multiple team reports (Kumar et al., GCN 36559; Fu et al., GCN 36561; Shilling et al., GCN 36562; Perez-Garcia et al., GCN 36563; Dutton et al., GCN 36568; Mo et al., GCN 36569)
View this GCN Circular online at https://gcn.nasa.gov/circulars/37612.
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TITLE: GCN CIRCULAR
NUMBER: 37611
SUBJECT: GW S240915b and S240919bn : Swift UVOT follow-up
DATE: 24/09/26 14:41:09 GMT
FROM: Alice Breeveld at MSSL-UCL <a.breeveld(a)ucl.ac.uk>
A.A. Breeveld (UCL-MSSL), F.E. Marshall (NASA/GSFC), S.R. Oates (Lancaster U.), N.P.M. Kuin (UCL-MSSL), C. Gronwall (PSU), N.J. Klingler (NASA/GSFC UMBC CRESST II), M. De Pasquale (University of Messina), M.J. Page (UCL-MSSL), S. Shilling (Lancaster U.), M.H. Siegel (PSU), A. D’Aì (INAF-IASFPA), P. D’…
[View More]Avanzo (INAF-OAB), A.P. Beardmore (U. Leicester), M.G. Bernardini (INAF-OAB), S. Campana (INAF-OAB), S.B. Cenko (NASA/GSFC), J.J. Delaunay (PSU), S. Dichiara (PSU), V. D’Elia (ASI-SSDC & INAF-OAR), R.A.J.Eyles-Ferris (U. Leicester), P.A. Evans (U. Leicester), R. Gayathri (PSU), D. Hartmann (Clemson University), J.A. Kennea (PSU), S. Laha (NASA/GSFC), H.A. Krimm (NSF), D. B. Malesani (DTU Space), P. O’Brien (U. Leicester), J.P. Osborne (U. Leicester), T. Partosan (NASA/GSFC), M. Perri (ASDC),K.L. Page (U. Leicester), D.M. Palmer (LANL), S. Ronchini (PSU), T. Sbarrato (INAF-OAB), B. Sbarufatti (INAF-OAB), G. Tagliaferri (INAF-OAB), E. Troja (U. Tor Vergata, INAF), A. Tohuvavohu (U. Toronto) on behalf of the Swift team:
We report on the analysis of the Swift UVOT follow-up of two GW events S240915b and S240919bn.
The procedure of the UVOT follow-up has been described in Oates et al.,2021, MNRAS, 507, 12960.
We examined the UVOT data for all fields pointed at by Swift through the planned tiling exposures (310 for S240915b; 217 for S240919bn) in either the U or UVW1 band. The exposures were typically around 70s long and reached upper limits around 19-19.3 in U and 18.2-18.7 in UVW1.
No credible candidates associated with S240915b or S240919bn were identified.
View this GCN Circular online at https://gcn.nasa.gov/circulars/37611.
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TITLE: GCN CIRCULAR
NUMBER: 37610
SUBJECT: EP240919a / GRB 240919A: SVOM/VT upper limit
DATE: 24/09/26 04:01:58 GMT
FROM: Liping Xin at NAOC, SVOM <xlp(a)nao.cas.cn>
SVOM/VT commissioning team: Y. L. Qiu, L. P. Xin, H. L. Li, C. Wu, X. H. Han, W. J. Xie, H. B. Cai, Y. Xu, Y. J. Xiao, P. P. Zhang, J. S. Deng, L. Lan, X. M. Lu, R. S. Zhang (NAOC), J. Zhang, L. J. Dan, G. Y. Zou, C. J. Wang, Y. F. Du, C. Huang (XIOPM) and Shaolin Xiong (IHEP).
SVOM JSWG: Jian-Yan Wei (NAOC), …
[View More]Bertrand Cordier (CEA), Shuang-Nan Zhang (IHEP), Stéphane Basa (LAM), Jean-Luc Atteia (IRAP), Arnaud Claret (CEA), Zi-Gao Dai (USTC), Frédéric Daigne (IAP), Jin-Song Deng (NAOC), Andrea Goldwurm (APC), Diego Götz (CEA), Xu-Hui Han (NAOC), Cyril Lachaud (APC), En-Wei Liang (GXU), Yu-Lei Qiu (NAOC), Susanna Vergani (Obs.Paris), Jing Wang (NAOC), Chao Wu (NAOC), Li-Ping Xin (NAOC), Bing Zhang (UNLV)
report on behalf of the SVOM team:
During the commissioning phase of SVOM mission, we observed the field of the EP240919a (Liang et al., GCN 37561) which is also confirmed as GRB 240919A (Liang et al., GCN 37563; Rodi et al., GCN 37572; Wang et al., GCN 37574) with SVOM/VT telescope in ToO mode. The observation started at 2024-09-21T14:12:58 UT, about 47.5 hours after the burst, and the total exposure time was 6160 seconds. VT made the observations with two channels simultaneously, VT_B (400nm-650nm) and VT_R (650nm-1000nm).
No any uncatalogued sources were detected in the 5.5 ks stacked images within the error circles of EP/FXT(Liang et al., GCN 37561) compared to DESI Legacy DR10 catalog, down to the following 3 sigma upper limit of VT_B=24.0 mag and VT_R=24.0 mag in AB magnitude.
The Space Variable Objects Monitor (SVOM) is a China-France joint mission led by the Chinese National Space Administration (CNSA, China), National Center for Space Studies (CNES, France) and the Chinese Academy of Sciences (CAS, China), which is dedicated to observing gamma-ray bursts and other transient phenomena in the energetic universe. VT was jointly developed by Xi'an Institute of Optics and Precision Mechanics (XIOPM), CAS and National astronomical observatories (NAOC),CAS.
View this GCN Circular online at https://gcn.nasa.gov/circulars/37610.
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TITLE: GCN CIRCULAR
NUMBER: 37609
SUBJECT: LIGO/Virgo/KAGRA S240925n: NED Galaxies in the Localization Volume
DATE: 24/09/25 15:52:55 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 …
[View More]S240925n-4-Update 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 42329 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/S240925n/4
Top 20 List Download: https://ned.ipac.caltech.edu/uri/NED::GWFglist/fits/S240925n/4/20
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 J062805.37-433822.4| 97.02237| -43.63942| G| 353.30| null| null| null| 13.407| 0.166| 10.531| 0.006|8.65e-07| 1.65e-10|
|WISEA J082912.08+093324.3| 127.30033| 9.55669| G| 300.62| 0.10| null| null| 13.544| 0.318| 9.710| 0.006|3.75e-07| 1.11e-10|
|WISEA J071238.60-372350.1| 108.16138| -37.39731| G| 390.44| null| null| null| 13.392| 0.189| 9.730| 0.006|2.07e-07| 1.08e-10|
|WISEA J070803.77-354236.4| 107.01575| -35.71003| G| 328.72| null| null| null| 12.425| 0.144| 10.393| 0.006|5.43e-07| 1.07e-10|
|WISEA J061819.45-434436.6| 94.58121| -43.74347| G| 370.50| 0.65| 20.752| 0.288| 11.534| 0.065| 11.355| 0.008|1.07e-06| 1.04e-10|
| LCSB S1127P| 124.68167| -5.27042| G| 288.80| 0.79| 19.041| 0.091| 12.474| 0.142| 9.606| 0.006|3.23e-07| 9.65e-11|
|WISEA J081327.05-104947.3| 123.36275| -10.82981| G| 334.80| null| 21.777| 0.343| 12.588| 0.130| 9.678| 0.006|2.52e-07| 9.54e-11|
|WISEA J073059.04-315148.7| 112.74613| -31.86356| G| 346.09| null| null| null| 13.600| 0.199| 10.124| 0.006|3.04e-07| 8.52e-11|
|WISEA J070820.06-363048.2| 107.08383| -36.51381| G| 379.19| null| null| null| 13.096| 0.187| 11.119| 0.006|6.00e-07| 8.29e-11|
|WISEA J061611.50-442317.6| 94.04800| -44.38825| G| 294.82| 0.65| null| null| 12.556| 0.098| 10.622| 0.006|6.79e-07| 8.28e-11|
|WISEA J060209.36-452357.6| 90.53908| -45.39936| G| 384.51| null| 19.583| 0.110| 13.598| 0.217| 11.579| 0.007|8.76e-07| 7.51e-11|
|WISEA J061409.91-454035.8| 93.54125| -45.67661| G| 402.08| null| null| null| 13.766| 0.117| 10.605| 0.006|3.24e-07| 7.45e-11|
|WISEA J051216.45-480857.2| 78.06850| -48.14919| G| 337.91| 0.65| null| null| 12.125| 0.095| 10.653| 0.006|4.79e-07| 7.40e-11|
|WISEA J075243.04-243418.1| 118.17925| -24.57167| G| 429.53| null| null| null| 13.189| 0.220| 9.554| 0.006|9.88e-08| 7.27e-11|
|WISEA J063117.86-431255.9| 97.82442| -43.21550| G| 300.09| 0.65| null| null| 12.542| 0.092| 10.771| 0.006|6.19e-07| 6.84e-11|
|WISEA J055703.16-455202.4| 89.26317| -45.86731| G| 370.68| null| null| null| 13.004| 0.146| 11.788| 0.007|9.80e-07| 6.44e-11|
|WISEA J080912.41-155827.8| 122.30163| -15.97442| G| 363.85| null| null| null| 13.237| 0.167| 9.611| 0.006|1.36e-07| 6.43e-11|
|WISEA J061604.66-444741.9| 94.01942| -44.79497| G| 363.27| 0.65| null| null| 12.326| 0.099| 11.531| 0.006|8.01e-07| 6.41e-11|
|WISEA J072410.09-335347.5| 111.04196| -33.89656| G| 367.11| null| null| null| 12.437| 0.112| 10.727| 0.007|3.60e-07| 6.35e-11|
|WISEA J082326.29-051125.1| 125.85971| -5.19033| G| 265.27| null| 19.749| 0.112| 13.018| 0.169| 9.675| 0.006|2.64e-07| 6.23e-11|
Table 1: Top 20 galaxies in NED-LVS that fall in the 90% probability volume for S240925n 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).
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TITLE: GCN CIRCULAR
NUMBER: 37608
SUBJECT: EP240918b and EP240918c: EP-FXT follow-up observations
DATE: 24/09/25 11:33:40 GMT
FROM: EP Team at NAOC/CAS <ep_ta(a)bao.ac.cn>
M. J. Liu (NAOC ,CAS), Y. F. Liang (PMO, CAS), Z. J. Zhang (HKU), X. P. Xu, C. C. Jin, Z. X. Ling, W. M. Yuan, Y. Liu, C. Zhang, W. Chen, H. Q. Cheng, C. Z. Cui, D. W. Fan, H. B. Hu, J. W. Hu, M. H. Huang, D. Y. Li, H. Y. Liu, Z. Z. Lv, T. Y. Lian, X. Mao, H. W. Pan, X. Pan, H. Sun, W. X. Wang, Y. L. Wang, Y. …
[View More]F. Xu, H. N. Yang, M. Zhang, W. D. Zhang, W. J. Zhang, Z. Zhang, D. H. Zhao (NAOC, CAS), Y. Chen, S. M. Jia, W. W. Cui, D. W. Han, C. K. Li, L. M. Song, X. F. Zhao, J. Zhang, S. N. Zhang (IHEP, CAS), E. Kuulkers, A. Santovincenzo (ESA), P. O'Brien (Univ. of Leicester), K. Nandra, A. Rau (MPE), B. Cordier (CEA) on behalf of the Einstein Probe team
We have reported the detection of two fast X-ray transients EP240918b and EP240918c by the Einstein Probe (EP) mission (Liang et al. GCN 37555).
The follow-up observation with the EP-FXT for EP240918b was performed, starting at 2024-09-19T11:25:26 (UTC), about 20 hours after the detection of the source by WXT. No X-ray source was detected within the 3 arcmin radius region around the WXT position of EP240918b.
The follow-up observations with the EP-FXT for EP240918c were performed, starting at 2024-09-19T12:40:28 (UTC) and 2024-09-24T13:01:28 (UTC), respectively. Two X-ray sources were detected within the 3 arcmin radius region around the WXT position of EP240918c in each observation. EP J184515.3-131115 is detected at R.A. = 281.3138 deg, DEC = -13.1875 deg (J2000) with an uncertainty of 10 arcsec in radius (90% C.L. statistical and systematic). EP J184516.2-130819 locates at R.A. = 281.3187 deg, DEC = -13.1371 deg (J2000) with an uncertainty of 10 arcsec in radius (90% C.L. statistical and systematic), being consistent with the position of the star TYC 5704-6-1. No rapid dimming was found for two sources.
Further follow-up observations are encouraged to identify the nature of EP240918b and EP240918c.
Launched on January 9, 2024, EP is a space X-ray observatory to monitor the soft X-ray sky with onboard 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/37608.
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