TITLE: GCN CIRCULAR
NUMBER: 39910
SUBJECT: GRB 250328A: SVOM detection of a burst
DATE: 25/03/28 17:32:16 GMT
FROM: SVOM_group <svomgroup(a)bao.ac.cn>
M. Brunet, J. Malzac, L. Bouchet, O. Godet (IRAP), C. Plasse (CEA), L.P. Xin (NAOC)
on behalf of the SVOM mission team.
SVOM/ECLAIRs triggered on the gamma-ray burst GRB 250328A (SVOM burst-id sb25032803) starting at 2025-03-28T16:56:56.3 UTC (Tb). The following trigger information was received on the ground with low latency by …
[View More]the SVOM VHF Alert Network.
The burst was only detected by the Count-Rate Trigger (CRT), which produced a sequence of 1 alerts. CRT provided the alert with the best signal-to-noise-ratio (SNR) of 6.85 in the [8-120] keV energy band over a time window of 20.48 seconds starting at Tb.
The light curve showed a single structure with a duration of about 15s
The localization of the best alert is R.A., Dec 215.9771, 25.8825 degrees:
RA (J2000) = 14h23m54.51s
Dec (J2000) = 25d52m56.83s
with a 90% C.L. radius of 11.42 arcmin (including systematic error of 2 arcmin added in quadrature).
No immediate slew was performed on this burst, because its significance was below the slew threshold. A SVOM ToO will be performed.
The Space-based multi-band astronomical Variable Objects Monitor (SVOM) is a China-France joint mission led by the Chinese National Space Administration (CNSA), French Space Agency (CNES), and the Chinese Academy of Sciences (CAS), which is dedicated to observing gamma-ray bursts and other transient phenomena in the energetic universe.
The Burst Advocate (BA) on shift for this burst is Marius Brunet: marius.brunet(a)irap.omp.eu.
Please contact the BA by email if you require additional information regarding the SVOM follow-up of this burst.
View this GCN Circular online at https://gcn.nasa.gov/circulars/39910.
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TITLE: GCN CIRCULAR
NUMBER: 39909
SUBJECT: FRB 20250316A: FTW optical observations
DATE: 25/03/28 16:50:28 GMT
FROM: Malte Busmann at Ludwig-Maximilians-Universität München <m.busmann(a)physik.lmu.de>
Malte Busmann, Jennifer Fabà, Daniel Gruen, Mathias Mucke, Xiaoxiong Zuo (LMU), Brendan O'Connor, and Antonella Palmese (CMU) report on behalf of a larger collaboration:
We observed the localization of FRB 20250316A (Ng et al., ATel #17081; Andrew et al., GCN 39886). With the …
[View More]Three Channel Imager (3KK) at the Fraunhofer Telescope at Wendelstein Observatory (FTW) in the g and i band on multiple nights. Observations started 2.53d after the FRB or 5.8h after the discovery of an uncataloged X-ray source EP J120944.2+585060 by Einstein Probe (GCN 39834).
| Time (UT) | t - t0 (d) | Band | Exposures | Depth (3 sigma, AB mag) | Depth Diff (3 sigma, AB mag) |
|---------------------|------------|------|-----------|-------------------------|------------------------------|
| 2025-03-18T21:14:03 | 2.53 | g | 10x 180 s | 24.3 | Used as Reference |
| 2025-03-18T21:14:03 | 2.53 | i | 10x 180 s | 23.7 | Used as Reference |
| 2025-03-22T20:05:28 | 6.48 | g | 16x 180 s | 21.9 | - |
| 2025-03-22T20:05:28 | 6.48 | i | 16x 180 s | 21.6 | - |
| 2025-03-23T23:11:05 | 7.61 | g | 15x 180 s | 24.4 | 23.5 |
| 2025-03-23T23:11:05 | 7.61 | i | 15x 180 s | 23.8 | 23.0 |
| 2025-03-28T03:33:48 | 11.79 | g | 10x 180 s | 23.0 | 22.9 |
| 2025-03-28T03:33:48 | 11.79 | i | 10x 180 s | 22.5 | 22.5 |
We performed difference imaging against templates from the LegacySurvey (g) and PS1 (i). We also used our first observation as a template and do not detect any excess flux at the FRB location in either case. This is consistent with the observations of Becerra et al. (ATel #17082, GCN 39843, 39853), Niino et al.(ATel #17084), Hashimoto (ATel #17095), Yang et al. (ATel #17101), Troja et al. (ATel #17109, GCN 39869), Dong et al. (ATel #17112), Aryan et al. (GCN 39839), Pereyra et al. (GCN 39858), Jiang et al. (GCN 39864), Gillanders et al. (GCN 39883), and Simha et al. (ATel #17116, GCN 39887).
The magnitudes are calibrated against the PS1 catalog and are not corrected for galactic extinction.
We thank Christoph Ries and Michael Schmidt from the Wendelstein Observatory staff for obtaining these observations.
View this GCN Circular online at https://gcn.nasa.gov/circulars/39909.
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TITLE: GCN CIRCULAR
NUMBER: 39908
SUBJECT: LIGO/Virgo/KAGRA S250328ae: NED Galaxies in the 4-Update Localization Volume
DATE: 25/03/28 15:33:03 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 …
[View More]the LVK S250328ae-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 839 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/S250328ae/4
Top 20 List Download: https://ned.ipac.caltech.edu/uri/NED::GWFglist/fits/S250328ae/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 J094227.03+110047.4| 145.61266| 11.01318| G| 612.35| null| null| null| 12.661| 0.096| 10.577| 0.006|2.63e-06| 5.47e-08|
|WISEA J093435.61+082700.3| 143.64838| 8.45010| G| 507.10| 0.11| null| null| 13.186| 0.203| 10.854| 0.006|3.85e-06| 4.28e-08|
|WISEA J093458.83+094902.6| 143.74516| 9.81741| G| 564.56| 0.09| null| null| 14.250| 0.157| 10.944| 0.007|2.12e-06| 2.69e-08|
|WISEA J093555.60+093752.8| 143.98169| 9.63134| G| 589.67| 0.08| null| null| 13.465| 0.202| 11.501| 0.007|2.87e-06| 2.37e-08|
|WISEA J093938.05+110947.9| 144.90857| 11.16332| G| 482.07| 0.08| null| null| 13.597| 0.141| 12.972| 0.014|1.58e-05| 2.25e-08|
|WISEA J094028.13+111733.4| 145.11722| 11.29263| G| 556.24| 0.11| null| null| 13.110| 0.111| 12.941| 0.015|9.93e-06| 1.94e-08|
|WISEA J094035.77+103104.6| 145.14905| 10.51795| G| 495.66| 0.07| null| null| 13.045| 0.080| 12.298| 0.012|6.77e-06| 1.90e-08|
|WISEA J093657.39+085125.0| 144.23916| 8.85696| G| 557.28| 0.06| null| null| null| null| 11.769| 0.007|3.22e-06| 1.86e-08|
|WISEA J094109.87+105038.6| 145.29116| 10.84407| G| 439.67| 0.07| null| null| 12.109| 0.080| 12.120| 0.012|6.55e-06| 1.70e-08|
|WISEA J094121.23+112617.1| 145.33849| 11.43811| G| 564.36| 0.09| null| null| 13.311| 0.123| 13.095| 0.017|9.76e-06| 1.70e-08|
|WISEA J094025.05+111347.9| 145.10441| 11.23000| G| 557.91| 0.09| null| null| 13.243| 0.108| 13.078| 0.020|9.62e-06| 1.66e-08|
|WISEA J093619.16+091944.6| 144.07983| 9.32906| G| 588.58| 0.11| null| null| 13.919| 0.167| 12.015| 0.007|3.16e-06| 1.62e-08|
|WISEA J093619.13+091936.4| 144.07971| 9.32680| G| 591.85| 0.08| null| null| 12.365| 0.106| 12.060| 0.010|3.00e-06| 1.49e-08|
|WISEA J093747.49+101024.7| 144.44789| 10.17354| G| 432.26| 0.05| null| null| 12.881| 0.108| 12.438| 0.013|7.81e-06| 1.46e-08|
|WISEA J093417.20+081006.5| 143.57167| 8.16848| G| 347.36| 0.08| 21.156| 0.071| 13.681| 0.191| 10.002| 0.006|1.22e-06| 1.39e-08|
|WISEA J094125.76+110548.3| 145.35737| 11.09678| G| 557.02| 0.07| null| null| 13.696| 0.126| 13.350| 0.021|9.58e-06| 1.28e-08|
|WISEA J094051.38+102028.4| 145.21409| 10.34125| G| 444.19| 0.03| null| null| 15.275| 0.145| 12.091| 0.007|4.61e-06| 1.25e-08|
|WISEA J094106.66+105024.2| 145.27777| 10.84008| G| 487.71| null| null| null| 14.219| 0.109| 13.198| 0.021|1.00e-05| 1.18e-08|
|WISEA J093537.73+091115.6| 143.90721| 9.18768| G| 552.71| 0.11| null| null| 13.648| 0.222| 12.528| 0.013|4.10e-06| 1.16e-08|
|WISEA J093620.06+092335.0| 144.08362| 9.39307| G| 582.84| 0.07| 20.401| 0.231| 13.508| 0.189| 12.534| 0.014|3.60e-06| 1.12e-08|
Table 1: Top 20 galaxies in NED-LVS that fall in the 90% probability volume for S250328ae 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/39908.
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TITLE: GCN CIRCULAR
NUMBER: 39907
SUBJECT: EP250302a: upper limit of SPI-ACS/INTEGRAL
DATE: 25/03/28 13:40:48 GMT
FROM: Alexei Pozanenko at IKI, Moscow <grb.alex(a)gmail.com>
P. Minaev (IKI), A. Pozanenko (IKI), S. Grebenev (IKI), I. Chelovekov (IKI)
and IKI GRB-FuN
We searched the INTEGRAL dataset for gamma-ray emission from the X-ray
transient EP250302a, detected with WXT EP (Dai et al., GCN 39556). No
significant excess above the background was detected during the EP250302a
…
[View More]in any of the detectors. The source EP250302a is located 71 degrees
off-axis of the INTEGRAL telescopes' field of view. In particular, for the
SPI-ACS detector, the upper limit (3-sigma) for the fluence from an event
with a duration of 100 sec (during the first and second EP250302a episodes)
is 3.2e-6 erg*cm^-2 using the softest simulated CPL spectrum with Ep = 20
keV. The SPI-ACS estimating is based on the calibration given in the paper
https://ui.adsabs.harvard.edu/abs/2023MNRAS.525.2411M
We thank the INTEGRAL Observatory and all the staff who have served it for
over 22 years. Blessed be the memory of its deeds.
View this GCN Circular online at https://gcn.nasa.gov/circulars/39907.
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TITLE: GCN CIRCULAR
NUMBER: 39906
SUBJECT: GRB 250327B: CrAO and SAO RAS Optical Observations
DATE: 25/03/28 13:37:10 GMT
FROM: Alexei Pozanenko at IKI, Moscow <grb.alex(a)gmail.com>
N. Pankov (HSE, IKI), A. Moskvitin (SAO RAS), V. Rumyantsev (CrAO), O. I.
Spiridonova (SAO RAS), A. Pozanenko (IKI) report on behalf of IKI-GRB-FuN:
We performed optical observations of the field of GRB 250327A (Bouchet et.
al, GCN 39888; Page et. al, GCN 39895) at the redshift of z = 3.035
(…
[View More]Malesani et. al, GCN 39893; Dennefeld et al., GCN 39905) with the
2.6-meter Shajn telescope (ZTSh) of the Crimean Astrophysical Observatory
(CrAO) and the 1-meter Zeiss-1000 telescope of the Special Astrophysical
Observatory of the RAS (SAO RAS). The observations started on (UT)
2025-03-27 22:24:22 at CrAO, i.e. about 0.05 days since GBM trigger. We
obtained the series of frames in the VRI filters with ZTSh and the series
of frames in the BVRI filters with Zeiss-1000. We clearly detect the bright
optical afterglow (Moskvitin et. al, GCN 39889; Xin et. al, GCN 39890;
O’Neill et. al, GCN 39891; Malesani et. al, GCN 39893; Lian et. al, GCN
39894; Shrestha et. al, GCN 39896; Ducoin et. al, GCN 39897; Perley &
Bochenek, GCN 39902) in the images from both telescopes. The preliminary
photometry of the afterglow in the end of each series is as follows:
Date UT start t-T0 Exp. Filter OT Err Telescope
(mid, days) (s)
2025-03-27 23:12:18 0.08410 30 I 16.45 0.07 ZTSh
2025-03-27 23:13:36 0.08500 30 R 17.15 0.08 ZTSh
2025-03-27 23:12:59 0.08457 30 V 17.80 0.10 ZTSh
2025-03-27 00:25:24 0.14229 4*300 Rc 18.22 0.05 Zeiss-1000
The photometry is based on nearby stars of USNO-B1.0 (R2 magnitudes; same
as in Moskvitin et. al, GCN 39889) and has not been corrected for the
Galactic extinction. Using the R-filter photometry between 0.01 and 0.1
days after trigger, we estimate a power law decay of the light curve to be
alpha = -1.87 +/- 0.03.
View this GCN Circular online at https://gcn.nasa.gov/circulars/39906.
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TITLE: GCN CIRCULAR
NUMBER: 39905
SUBJECT: GRB 250327B: OHP/T193 spectroscopic observations and redshift confirmation
DATE: 25/03/28 12:49:52 GMT
FROM: Benjamin Schneider at MIT <bschn(a)mit.edu>
M. Dennefeld (IAP/CNRS/Sorbonne U.), B. Schneider (LAM), C. Adami (LAM/Pytheas/AMU), E. Le Floc'h (CEA/Irfu), A. Saccardi (CEA/Irfu), S. Vergani (CNRS, Obs. de Paris, LUX), S. Basa (Pytheas/OHP/LAM) report on behalf of the MISTRAL-GRB collaboration:
We observed the SVOM/ECLAIRs GRB …
[View More]250327B (Bouchet et al., GCN 39888) using the T193cm telescope at Observatoire de Haute-Provence (France) equipped with the MISTRAL spectro-imager in red setting.
We obtained 1x60 s in the r’, i’, z’ and Y bands starting at 22:44:30 UT on 2025-03-27 (T0+1.55 h after the trigger). The optical afterglow reported by Moskvitin et al. GCN 39889; Xin et al. GCN 39890; O’Neill et al. GCN 39891; Malesani et al. GCN 39893; Lian et al. GCN 39894; Shrestha et al. GCN 39896; Ducoin et al., GCN39897; Perley et al., GCN 39902; and Kumar et al., GCN 39904 is well detected at r = 17.25 +/- 0.05 mag (AB). The photometric calibration was performed using nearby stars from the PanSTARRS catalog and the magnitude is not corrected for Galactic extinction.
In addition, we obtained 3x15 min of spectroscopic observations covering from 6400 to 9950 AA starting at 2025-03-27 22:52:55 UT (T0+1.69 h). In the stacked spectrum, we clearly detect multiple absorption features, which we interpret as being due to Si II, Si II*, C IV, Fe II, Fe II*, Al II, Al III, Mg I, Ni II* at a common redshift of z = 3.038 +/- 0.005. The detection of fine-structure lines robustly associates this system to the high-energy transient. This value is also consistent with the value reported by Malesani et al. (GCN 39893).
We acknowledge the excellent support from the Observatoire de Haute-Provence and in particular Stéphane Favard.
View this GCN Circular online at https://gcn.nasa.gov/circulars/39905.
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TITLE: GCN CIRCULAR
NUMBER: 39904
SUBJECT: GRB 250327B: further optical observations by LCOGT
DATE: 25/03/28 12:22:25 GMT
FROM: Amit Kumar at Royal Holloway - UoL/ U of Warwick, UK <amitkundu515(a)gmail.com>
Amit Kumar (RHUL/Warwick), Raya Dastidar (UNAB), Giuliano Pignata (UTA), Danny Steeghs, Thomas Killestein (Warwick), David O’Neill (Birmingham), Jonathan Andrés Pineda García (UNAB) and Mauricio Ramirez (UNAB) report on behalf of the wider collaboration:
We conducted …
[View More]optical follow-up observations of the optical counterpart to the SVOM/ECLAIRs-detected GRB 250327B (Bouchet et al., GCN 39888) using the LCOGT 0.4-m telescope at the Las Cumbres Observatory Global Telescope (LCOGT) node located at Teide Observatory, Tenerife, Spain, equipped with the SCICAM-QHY600 camera. Observations were carried out on 2025-03-28 between 02:18:54 UT and 03:34:29 UT, corresponding to approximately 5.1 to 6.4 hours post-burst.
Each epoch comprised a series of 6 × 300 sec exposures in the B-band. In the stacked image, we clearly detect the optical counterpart with a B-band magnitude of ~21.9 ± 0.2. The detected position is consistent with the location of the optical counterpart reported by Moskvitin et al. GCN 39889 (a.k.a. GOTO25bhx, AT 2025gcz), with supporting detections from Xin et al. (GCN 39890), O’Neill et al. (GCN 39891), Malesani et al. (GCN 39893), Lian et al. (GCN 39894), Shrestha et al. (GCN 39896), Ducoin et al. (GCN 39897), and Perley & Bochenek (GCN 39902).
The reported magnitude is calibrated against the USNO-B1 catalog and is not corrected for Galactic extinction in the direction of the event.
Further analysis and follow-up observations are ongoing. This circular may be cited.
View this GCN Circular online at https://gcn.nasa.gov/circulars/39904.
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TITLE: GCN CIRCULAR
NUMBER: 39903
SUBJECT: EP250315a: Pan-STARRS r and i-band imaging and photometry
DATE: 25/03/28 10:04:31 GMT
FROM: James Gillanders at University of Oxford <jhgillanders.astro(a)gmail.com>
J. H. Gillanders (Oxford), M. Huber, K. C. Chambers (IfA, Univ. Hawaii), S. J. Smartt, K. W. Smith, S. Srivastav (Oxford), M. Nicholl, D. Young, M. Fulton (QUB), T.-W. Chen (NCU, Taiwan) A. S. B. Schultz, T. de Boer, J. Fairlamb, G. Paek, C. C. Lin, T. Lowe, E. Magnier, P. …
[View More]Minguez, I. A. Smith, R. J. Wainscoat (IfA, Univ. Hawaii).
We observed the optical counterpart of EP250315a (Peng et al., GCN 39731; Quirola-Vasquez et al., GCN 39733), using the Pan-STARRS telescope system (Chambers et al., 2016, arXiv e-prints, 1612.05560) on MJD 60755.50 (2025-03-21 12:00 UTC), approximately 6.25 days after the EP-WXT detection (Peng et al., GCN 39731). The Pan-STARRS system consists of two 1.8m telescope units located at the summit of Haleakala on the Hawaiian island of Maui, employing an SDSS-like filter system denoted as grizy, and a broad w-filter, which is a composite of the gri-filters.
Our observation consisted of 6x150s exposures in both the r and i filters with Pan-STARRS1. The images were processed with the Pan-STARRS pipeline. After astrometric and photometric calibration, reference images were subtracted from the target stacked images (Magnier et al., 2020a, ApJS, 251, 3; Magnier et al., 2020b, ApJS, 251, 6; Waters et al., 2020, ApJS, 251, 4).
From these difference images, we do not detect the optical counterpart discovered by Quirola-Vasquez et al., GCN 39733. At the reported optical counterpart position, we measure 3.5-sigma limiting AB magnitudes of r~21.7 and i~21.7.
View this GCN Circular online at https://gcn.nasa.gov/circulars/39903.
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TITLE: GCN CIRCULAR
NUMBER: 39902
SUBJECT: GRB 250327b: Liverpool Telescope optical observations
DATE: 25/03/28 09:30:33 GMT
FROM: A. Bochenek at Liverpool John Moores University <a.m.bochenek(a)2023.ljmu.ac.uk>
D. A. Perley and A.Bochenek (LJMU) report:
We observed the field of GRB250327b (Bouchet et al., GCN 39888) using the IO:O optical camera on the 2m robotic Liverpool Telescope. We obtained 1x100s exposures in the SDSS g, r, i, and z filters, starting at 2025-03-28 00:17:…
[View More]25 UT, approximately 3.1 hours after the trigger.
We report a detection in all our images at the position of the optical counterpart (Moskvitin et al., GCN 39889), given in the table below. Our results agree with previous optical observations (Moskvitin et al. GCN 39889; Xin et al. GCN 39890; O’Neill et al. GCN 39891; Malesani et al. GCN 39893; Lian et al. GCN 39894; Shrestha et al. GCN 39896; Ducoin et al., GCN39897).
MJD (mid) T_mid - T_0 Filter Mag. (AB)
60762.01268 3.11 hours r 18.47 ± 0.02
60762.01412 3.14 hours i 17.98 ± 0.04
60762.01556 3.18 hours g 19.87 ± 0.05
60762.01706 3.21 hours z 17.82 ± 0.06
The photometry was calibrated using nearby PanSTARRS secondary standards and was not corrected for extinction.
View this GCN Circular online at https://gcn.nasa.gov/circulars/39902.
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TITLE: GCN CIRCULAR
NUMBER: 39901
SUBJECT: GRB 250322A: GRANDMA/TNOT optical upper limits
DATE: 25/03/28 09:01:10 GMT
FROM: duverne(a)apc.in2p3.fr
E. Elhosseiny (NRIAG), N. Kochiashvili (AbAO), O. Pyshna (Caltech), Haichang Zhu (THU), A. Iskandar(XAO), Xiaofeng Wang (THU), Letian Wang (XAO) C. Andrade (UMN), S. Antier (OCA/IJCLAB), M. Coughlin (UMN), P-A. Duverne (APC), N. Guessoum (AUS), P. Hello (IJCLAB), S. Karpov (FZU), T. Pradier (Unistra/IPHC), D. Turpin (CEA-Saclay/Irfu) on …
[View More]behalf of the GRANDMA and Kilonova-Catcher collaborations:
The field of GRB 250322A (Gupta et al., GCN 39835, Goad et al. GCN 39841, Perri et al. GCN 39855, Sadaula et al. GCN 39867) has been imaged with the 80~cm Tsinghua-Nanshan Optical Telescope (TNOT) located at Nanshan Station of Xinjiang Astronomy observatory 1.1h post trigger with the r' filter for a total exposure of 100s.
We do not detect any new source at the enhanced Swift-XRT position (Goad et al. GCN 39841) down to r<21.2 AB mag (5-sigma) calibrated with nearby Pan-STARRS stars and without Galactic extinction correction.
All the data have been reduced by a single data processing pipeline, STDPipe (Karpov et al., 2025 Acta Polytechnica, 65(1), 50-64).
We use the SkyPortal application (skyportal.io) to monitor our observational campaign (Coughlin et al. 2023).
GRANDMA is a worldwide telescope network (grandma.ijclab.in2p3.fr) devoted to the observation of transients in the context of multi-messenger astrophysics (Antier et al. 2020 MNRAS 497, 5518). Kilonova-Catcher (KNC) is the citizen science program of GRANDMA (http://kilonovacatcher.in2p3.fr/).
View this GCN Circular online at https://gcn.nasa.gov/circulars/39901.
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