GRB 240529A
GCN Circular 36556
Subject
GRB 240529A: Swift detection of a burst with an optical counterpart
Date
2024-05-29T03:38:03Z (a year ago)
From
David Palmer at LANL <palmer@lanl.gov>
Via
email
R. A. J. Eyles-Ferris (U Leicester), R. Gupta (NASA/GSFC),
A. Y. Lien (U Tampa), K. L. Page (U Leicester), D. M. Palmer (LANL)
and T. M. Parsotan (GSFC) report on behalf of the Neil Gehrels Swift
Observatory Team:
At 02:58:31 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 240529A (trigger=1231488). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 335.322, +51.555 which is
RA(J2000) = 22h 21m 17s
Dec(J2000) = +51d 33' 19"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve showed a single-peaked
structure with a duration of at least 20 sec since we are missing data
after ~8 sec. The peak count rate was ~4000 counts/sec (15-350 keV),
at ~0 sec after the trigger.
The XRT began observing the field at 03:06:22.0 UT, 471.2 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source located at RA, Dec 335.35696, 51.56207 which
is equivalent to:
RA(J2000) = 22h 21m 25.67s
Dec(J2000) = +51d 33' 43.5"
with an uncertainty of 3.5 arcseconds (radius, 90% containment). This
location is 82 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at https://www.swift.ac.uk/sper.
A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 4.06
x 10^21 cm^-2 (Willingale et al. 2013).
UVOT took a finding chart exposure of 150 seconds with the White filter
starting 128 seconds after the BAT trigger. There is a candidate afterglow in
the list of sources generated on-board at
RA(J2000) = 22:21:26.04 = 335.35851
DEC(J2000) = +51:33:43.4 = 51.56205
with a 90%-confidence error radius of about 1.10 arc sec. This position is 2.7
arc sec. from the center of the XRT error circle. The estimated magnitude is
17.84. No correction has been made for the large, but uncertain, extinction
expected.
Burst Advocate for this burst is R. A. J. Eyles-Ferris (raje1 AT leicester.ac.uk).
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/)
GCN Circular 36557
Subject
GRB 240529A: Enhanced Swift-XRT position
Date
2024-05-29T05:48:24Z (a year ago)
From
Phil Evans at U of Leicester <pae9@star.le.ac.uk>
Via
email
J.P. Osborne, A.P. Beardmore, P.A. Evans and M.R. Goad (U. Leicester)
report on behalf of the Swift-XRT team.
Using 1384 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 240529A, we find an astrometrically corrected X-ray
position (using the XRT-UVOT alignment and matching UVOT field sources
to the USNO-B1 catalogue): RA, Dec = 335.35741, +51.56166 which is equivalent
to:
RA (J2000): 22h 21m 25.78s
Dec (J2000): +51d 33' 42.0"
with an uncertainty of 2.2 arcsec (radius, 90% confidence).
This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).
This circular was automatically generated, and is an official product of the
Swift-XRT team.
GCN Circular 36559
Subject
GRB 240529A: GOTO optical afterglow detection
Date
2024-05-29T07:47:25Z (a year ago)
From
Amit Kundu at University of Warwick, UK <amitkundu515@gmail.com>
Via
Web form
A. Kumar, B. P. Gompertz, S. Belkin, G. Ramsay, Y. Julakanti, R. Starling, K. Ackley, M. J. Dyer, J. Lyman, K. Ulaczyk, F. Jimenez-Ibarra, D. O'Neill, D. Steeghs, D. K. Galloway, V. Dhillon, P. O'Brien, K. Noysena, R. Kotak, R. P. Breton, L. K. Nuttall, E. Palle and D. Pollacco report on behalf of the GOTO collaboration:
The Gravitational-wave Optical Transient Observer (GOTO, Steeghs et al., 2022) performed targeted observations in response to Swift-detected GRB 240529A (Eyles-Ferris et al., GCN 36556). Three epochs of targeted observations were performed by GOTO-North starting at 2024-05-29UT03:02:10.4 (3.67 minutes after the trigger). The first two targeted observations consisted of 4x90s exposures in the GOTO L-band (400-700 nm), whereas the third pointing was covered during the serendipitous survey pointing and had exposure times of 4x45 sec.
We detect the optical afterglow in all three epochs, with L-band magnitudes of 16.06 +/- 0.01, 17.55 +/- 0.03 and 17.30 +/- 0.04 at 4.5 minutes, 1.22 hours and 1.72 hours (mid-points) after trigger, respectively.
Magnitudes were calibrated using ATLAS-REFCAT2 (Tonry et al. 2018) and are not corrected for Galactic extinction.
GOTO (https://goto-observatory.org) is a network of telescopes that is principally funded by the STFC and operated at the Roque de los Muchachos Observatory on La Palma, Spain, and Siding Spring Observatory in NSW, Australia, on behalf of a consortium including the University of Warwick, Monash University, Armagh Observatory & Planetarium, the University of Leicester, the University of Sheffield, the National Astronomical Research Institute of Thailand (NARIT), the University of Turku, the University of Portsmouth, the University of Manchester and the Instituto de Astrofisica de Canarias (IAC).
GCN Circular 36560
Subject
GRB 240529A: AstroSat CZTI detection
Date
2024-05-29T09:32:31Z (a year ago)
From
Gaurav Waratkar at IIT Bombay <gauravwaratkar@iitb.ac.in>
Via
Web form
J. Joshi (IUCAA), G. Waratkar (IITB), A. Vibhute (IUCAA), V. Bhalerao (IITB), D. Bhattacharya (Ashoka University/IUCAA), A. R. Rao (IUCAA/TIFR), and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:
Analysis of AstroSat CZTI data with the CIFT framework (Sharma et al., 2021, JApA, 42, 73) showed the detection of a long-duration GRB 240529A which was also detected by Swift-BAT (Eyles-Ferris et al., GCN Circ. 36556).
The source was clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range. The light curve showed multiple peaks of emission with the strongest peak at 2024-05-29 02:58:30.46 UTC. The measured peak count rate associated with the burst is 372 (+67, -60) counts/s above the background in the combined data of all quadrants, with a total of 6548 (+660, -731) counts. The local mean background count rate was 1334 (+5, -6) counts/s. We measure a T90 of 40 (+-2) s from the cumulative Veto light curve.
The source was also faintly detected in the CZT detectors in the 20-200 keV energy range.
CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, URSC, IUCAA, SAC, and PRL. The Indian Space Research Organisation funded, managed, and facilitated the project.
CZTI GRB detections are reported regularly on the payload site at:
http://astrosat.iucaa.in/czti/?q=grb
GCN Circular 36561
Subject
GRB 240529A: NOT optical observations
Date
2024-05-29T10:55:16Z (a year ago)
From
Dong Xu at NAOC/CAS <dxu@nao.cas.cn>
Via
Web form
S.Y. Fu, J. An, Z.P. Zhu, X. Liu, S.Q. Jiang, D. Xu (NAOC), D. B. Malesani (DAWN/NBI and Radboud), J. Terwel (NOT) report on behalf of a large collaboration:
We observed the field of GRB 240529A detected by Swift (Eyles-Ferris et al., GCN 36556) using the 2.56-m Nordic Optical Telescope (NOT) equipped with the ALFOSC camera, and obtained 3 x 100 s frames in the Sloan r-band and 3 x 100 s frames in z-band, starting at 04:51:50.7 UT on 2024-05-29, i.e., 1.89 hr after the BAT trigger.
The optical afterglow (Eyles-Ferris et al., GCN 36556; Kumar et al. GCN 36559) of the burst is clearly detected in our stacked images. Preliminary photometry results are as follows:
Tmid (UT) Tmid-T0(hr) Mag MagErr Filter
2024-05-29T04:54:47 1.94 16.48 0.05 r
2024-05-29T05:01:30 2.05 15.40 0.05 z
calibrated with nearby PanSTARRS stars.
GCN Circular 36562
Subject
GRB 240529A: Swift/UVOT Detection
Date
2024-05-29T13:07:35Z (a year ago)
From
Sam Shilling at Lancaster University <shilling.sam@gmail.com>
Via
Web form
S.P.R. Shilling (Lancaster U.) and Eyles-Ferris (U. Leicester)
report on behalf of the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 240529A
128 s after the BAT trigger (Eyles-Ferris et al., GCN Circ. 36556).
A source consistent with the enhanced XRT position
(Osborne et al., GCN Circ. 36557) is detected in the initial UVOT exposures.
The preliminary UVOT position is:
RA (J2000) = 22:21:25.97 = 335.35822 (deg.)
Dec (J2000) = +51:33:43.0 = 51.56194 (deg.)
with an estimated uncertainty of 0.43 arc sec. (radius, 90% confidence).
Preliminary detections and 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the early exposures are:
Filter T_start(s) T_stop(s) Exp(s) Mag
white 128 278 147 17.07 +/- 0.04
v 671 691 19 16.16 +/- 0.14
b 598 617 19 17.44 +/- 0.16
u 341 591 246 18.27 +/- 0.10
w1 720 1642 97 >18.8
m2 695 1617 97 >18.7
w2 647 1568 117 >19.1
The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.332 in the direction of the burst
(Schlegel et al. 1998).
GCN Circular 36563
Subject
GRB240529A: BOOTES-6/DPRT optical detection
Date
2024-05-29T13:24:36Z (a year ago)
From
Youdong HU at INAF-OAB <huyoudong072@hotmail.com>
Via
Web form
I. Perez-Garcia, E. Fernandez-Garcia, M.D. Caballero-Garcia, R. Sanchez-Ramirez, S. Guziy, S.-Y. Wu and A. J. Castro-Tirado (IAA-CSIC, Granada), Y.-D. Hu (INAF-OAB), P. J. Meintjes and H. J. van Heerden (UFS, South Africa), A. Martin-Carrillo and L. Hanlon (UCD, Ireland), C. J. Perez del Pulgar (UMA, Malaga) and D.-R. Xiong (YNAO) on behalf of a larger collaboration, report:
Following the detection of GRB 240529A by Swift (Eyles-Ferris et al. GCNC 36556), the BOOTES-6/DPRT 0.6m robotic telescope at Boyden Observatory in Maselspoort (South Africa) observed the GRB location starting on May. 29, 03:05 UT (~ 7 min after trigger). A series of images in clear filter were gathered and the optical afterglow was detected within the enhanced Swift/XRT position (Osborne et al. GCNC 36557) for which we measure a preliminary magnitude of 15.2 +- 0.1 on the first co-added 10 s x 4 image, which is consistent with the detections of GOTO (Kumar et al. GCNC 36559), NOT (Fu et al. GCNC 36561) and UVOT (Shilling et al. GCNC 36562). Further imaging is ongoing.
We thank the staff at Boyden Observatory for their excellent support.
GCN Circular 36564
Subject
GRB 240529A: Swift-XRT refined Analysis
Date
2024-05-29T14:50:35Z (a year ago)
From
Phil Evans at U of Leicester <pae9@star.le.ac.uk>
Via
email
S. Dichiara (PSU), J.A. Kennea (PSU), K.L. Page (U. Leicester), A.P.
Beardmore (U. Leicester), A. Melandri (INAF-OAR), T. Sbarrato
(INAF-OAB), P. D'Avanzo (INAF-OAB), A. Tohuvavohu (U. Toronto) and P.A.
Evans report on behalf of the Swift-XRT team:
We have analysed 5.8 ks of XRT data for GRB 240529A, from 107 s to 19.1
ks after the BAT trigger. The data comprise 344 s in Windowed Timing
(WT) mode (the first 10 s were taken while Swift was slewing) with the
remainder in Photon Counting (PC) mode. A spectrum formed from the WT
mode data can be fitted with an absorbed power-law with a photon
spectral index of 1.945 (+0.015, -0.025). The best-fitting absorption
column is consistent with the Galactic value of 4.1 x 10^21 cm^-2
(Willingale et al. 2013). The PC mode spectrum has a photon index of
2.07 (+0.05, -0.04) and a best-fitting absorption column consistent
with the Galactic value. The counts to observed (unabsorbed) 0.3-10 keV
flux conversion factor deduced from this spectrum is 3.8 x 10^-11 (6.0
x 10^-11) erg cm^-2 count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 4.06 (+0.15, -0.00) x 10^21 cm^-2
Galactic foreground: 4.1 x 10^21 cm^-2
Excess significance: <1.6 sigma
Photon index: 2.07 (+0.05, -0.04)
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/01231488.
This circular is an official product of the Swift-XRT team.
GCN Circular 36566
Subject
GRB 240529A: Swift-BAT refined analysis
Date
2024-05-29T17:19:11Z (a year ago)
From
Tyler Parsotan at NASA GSFC <tyler.parsotan@nasa.gov>
Via
email
C. B. Markwardt (GSFC), S. D. Barthelmy (GSFC),
R. Gupta (GSFC), H. A. Krimm (NSF),
S. Laha (GSFC/UMBC), A. Y. Lien (U Tampa),
M. J. Moss (GSFC), D. M. Palmer (LANL),
T. Parsotan (GSFC), 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 240529A (trigger #1231488)
(Eyles-Ferris et al., GCN 36556). The BAT ground-calculated position is
RA, Dec = 335.341, 51.557 deg which is
RA(J2000) = 22h 21m 22.0s
Dec(J2000) = +51d 33' 25.2"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 26%.
The mask weighted lightcurve shows a complex lightcurve structure with a relatively
gradual rise to the peak at trigger time and multiple pulses present at late times,
at t ~30 and ~50 sec after the trigger time.
T90 (15-350 keV) is 160.67 +- 14.52 sec (estimated error including systematics).
The time-averaged spectrum from -74.8 to 226.4 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
1.68 +- 0.04. The fluence in the 15-150 keV band is 2.1 +- 0.0 x 10^-05 erg/cm2.
The 1-sec peak photon flux measured from T+0.17 sec in the 15-150 keV band
is 7.7 +- 0.6 ph/cm2/sec. 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/1231488
GCN Circular 36568
Subject
GRB 240529A: Skynet Optical Observations
Date
2024-05-29T18:07:59Z (a year ago)
From
Dylan Dutton at UNC Chapel Hill <ddutton59@gmail.com>
Via
Web form
Dylan Dutton, Daniel Reichart, Joshua Haislip, Vladimir Kouprianov, Megan Dubay, Ruide Fu, Donovan Schlekat, Logan Selph, James Davidson, Edward Murphy, and Carlos Salgado report on behalf of the Skynet Robotic Telescope Network at the University of North Carolina at Chapel Hill.
We observed the field of GRB 240529A with Skynet's 0.6m RRRT telecope located in Virginia. The observation began at 05:19:30 UTC on May, 29 2024 approximately 2.3 hours after the trigger reported by Swift (Eyeles-Ferris et al., GCN 36556) and lasted until 08:33:52 UTC.
We obtained multiple expsoures in the B, V, and R filters. Exposure lengths were calculated using our automated exposure length scaling model.
We clearly detected a bright object within the uncertainty radius of the Swift localization that is consistent with detections from GOTO (Kumar et al. GCN 36559), NOT (Fu et al. GCN 36561), UVOT (Shilling et al. GCN 36562), and BOOTES-6 (Perez-Garcia et al. GCN 36563) at:
R.A. (J2000): 22:21:25.904
Dec. (J2000): 51:33:42.512
We report the photometry below.
ExpLen | Filter | Mag | MagErr | Date | UTC
---------------------------------------------------------
100s | V | 16.557 | 0.116 | May 29, 2023 | 05:19:30
111s | R | 15.838 | 0.032 | May 29, 2023 | 05:21:40
297s | B | 17.587 | 0.032 | May 29, 2024 | 06:11:34
222s | V | 16.537 | 0.015 | May 29, 2024 | 06:16:41
155s | R | 15.669 | 0.011 | May 29, 2024 | 06:20:32
419s | B | 17.635 | 0.029 | May 29, 2024 | 06:23:25
313s | V | 16.618 | 0.014 | May 29, 2024 | 06:30:33
166s | R | 15.839 | 0.012 | May 29, 2024 | 06:35:55
451s | B | 17.883 | 0.034 | May 29, 2024 | 06:38:59
337s | V | 16.764 | 0.015 | May 29, 2024 | 06:46:39
179s | R | 15.916 | 0.012 | May 29, 2024 | 06:52:25
485s | B | 17.833 | 0.031 | May 29, 2024 | 06:55:41
362s | V | 16.960 | 0.017 | May 29, 2024 | 07:03:55
192s | R | 16.212 | 0.015 | May 29, 2024 | 07:10:06
522s | B | 18.377 | 0.048 | May 29, 2024 | 07:13:35
389s | V | 17.119 | 0.018 | May 29, 2024 | 07:22:26
207s | R | 16.297 | 0.015 | May 29, 2024 | 07:29:04
561s | B | 18.320 | 0.043 | May 29, 2024 | 07:32:48
419s | V | 17.090 | 0.017 | May 29, 2024 | 07:42:18
222s | R | 16.315 | 0.014 | May 29, 2024 | 07:49:27
600s | B | 18.366 | 0.042 | May 29, 2024 | 07:53:25
450s | V | 17.192 | 0.017 | May 29, 2024 | 08:03:34
239s | R | 16.372 | 0.014 | May 29, 2024 | 08:11:14
600s | B | 18.440 | 0.046 | May 29, 2024 | 08:15:30
484s | V | 17.417 | 0.021 | May 29, 2024 | 08:25:39
256s | R | 16.624 | 0.018 | May 29, 2024 | 08:33:52
Our images have been calibrated using stars from the APASS catalog.
GCN Circular 36569
Subject
GRB 240529A: J-band detections with WINTER
Date
2024-05-29T19:37:47Z (a year ago)
From
Geoffrey Mo at MIT <gmo@mit.edu>
Via
Web form
Geoffrey Mo (MIT), Viraj Karambelkar (Caltech), Robert Stein (Caltech), Danielle Frostig (MIT), Nathan Lourie (MIT), Tomas Ahumada (Caltech), Benjamin Schneider (MIT), Robert Simcoe (MIT), and Mansi Kasliwal (Caltech) report:
We observed the field of GRB 240529A (Eyles-Ferris et al., GCN 36556; Osborne et al., GCN 36557; Gropp et al., GCN 36558; Joshi et al., GCN 36560; Dichiara et al., GCN 36564; Markwardt et al., GCN 36566) in the near-infrared J-band with the Palomar 1-m telescope, equipped with the 1-square degree WINTER camera (Lourie et al. 2020).
Two epochs of observations were performed. The first epoch began at 2024-05-29T10:18:49 UTC (~7.3 hours after the GRB) and consisted of 29 x 120 s exposures. The second epoch began at 2024-05-29T11:47:42 UTC (~8.8 hours after the GRB) and consisted of 10 x 120 s exposures. The images were processed using the WINTER data reduction pipeline (https://github.com/winter-telescope/mirar, https://doi.org/10.5281/zenodo.10888436), with image subtraction performed relative to J-band images from the UKIRT Hemisphere survey (Dye et al., 2017).
We detect the counterpart (Eyles-Ferris et al., GCN 36556; 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) in both epochs. The (AB) magnitude is J ~ 16.1 mag in the first epoch, and J ~ 16.5 mag in the second epoch.
WINTER (Wide-field INfrared Transient ExploreR) is a partnership between MIT and Caltech, housed at Palomar Observatory, and funded by NSF MRI, NSF AAG, the David and Lucile Packard Foundation, and the MIT Kavli Institute for Astrophysics and Space Research.
GCN Circular 36573
Subject
GRB 240529A: AKO Optical Afterglow Detection
Date
2024-05-30T07:19:31Z (a year ago)
From
Mohammad Odeh at Al Khatim Observatory M44 <mshodeh@gmail.com>
Via
legacy email
Mohammad Odeh (Al-Khatim Observatory, AKO, operated by the International
Astronomical Center in Abu Dhabi, UAE), Nidhal Guessoum, Dalya Akl, Ilmah
Aabdi, and Shaikha AlShamsi (American University of Sharjah, UAE), report:
We observed the field of GRB 240529A (Eyles-Ferris et al., GCN 36556), with
our 0.36m f/7.7 robotic telescope. The observation started on 29 May 2024 at
21:57 (UT) to 30 May 2024 at 00:23 (UT), about 20.2 hours from the trigger.
We obtained multiple 180-sec exposures in Ic and Clear filters. We clearly
detected the optical afterglow at:
R.A. (J2000): 22:21:25.97
Dec. (J2000): +51:33:42.6
Our detection is consistent with the results of (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).
The following observations were calculated using Atlas catalogue as a
reference:
----------------------------------------------------------------------------
-
ObsTime (mid), Exposure (sec), Filter, Mag
----------------------------------------------------------------------------
-
2024-05-29T23:08:00Z, 24 x 180s (stacked), Ic, 17.9 +/- 0.10
2024-05-29T23:11:00Z, 24 x 180s (stacked), C, Sr = 18.9 +/- 0.07
----------------------------------------------------------------------------
-
The magnitudes are not corrected for galactic extinction.
GCN Circular 36574
Subject
GRB 240529A: Redshift from GTC/OSIRIS+
Date
2024-05-30T11:30:32Z (a year ago)
Edited On
2024-05-30T16:51:04Z (a year ago)
From
Antonio de Ugarte Postigo at OCA <deugarte@oca.eu>
Edited By
Vidushi Sharma at NASA GSFC/UMBC <vidushi.sharma@nasa.gov> on behalf of Antonio de Ugarte Postigo at OCA <deugarte@oca.eu>
Via
email
A. de Ugarte Postigo (CNRS, OCA/LAM), C. C. Thoene (ASU-CAS), J. F. Agui Fernandez (CAHA), D. B. Malesani (DAWN/NBI and Radboud U.), Rakotondrainibe (LAM), N. R. Tanvir (U. Leicester), J. P. U. Fynbo (DAWN/NBI), L. Izzo (INAF-OACn & DARK/NBI), G. Lombardi (GTC), S. Geier (GTC), A. Cabrera Lavers (GTC), F. Perez-Toledo (GTC), A. Tejero (GTC) report:
We obtained spectroscopy of the afterglow of GRB 240529A (Eyles-Ferris et al. GCN 36556; Kumar et al. GCN 36559; Joshi et al. GCN 36560; 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; Odeh et al. GCN 36573) using OSIRIS+ at the 10.4 m GTC telescope in the Roque de los Muchachos Observatory (La Palma, Spain). The observation consisted of 3x900s exposures using grism R1000B, covering the range between 3600 and 7800 AA at a resolving power of around 600. The observation had a mean epoch 2024-05-30T04:05:55 UT (1.0468 days after the burst onset). At the time of the afterglow acquisition we measure a magnitude of r(AB) = 19.59 +/- 0.05 mag, as compared to PanSTARRS field stars.
In spite of the late observation, the spectrum still shows a bright continuum with many strong spectral features, which we identify as due to at least three absorption systems. The highest redshift one, which we identify as the one corresponding to the redshift of the GRB is at z=2.695. For this system we identify features of HI, SII, SiII SiII*,SiIV, OI, CI, CII, CIV, FeII, AlII and AlIII.
Additionally we detect two strong intervening systems. The highest redshift one has the most prominent features, corresponding to CIV, AlII, AlIII, and FeII at a redshift of z=2.035. The second system, at z=1.695 has features of CIV, AlIII, FeII, MgI, MgII.
GCN Circular 36575
Subject
GRB 240529A: T193/MISTRAL observations
Date
2024-05-30T13:23:17Z (a year ago)
From
Antonio de Ugarte Postigo at OCA <deugarte@oca.eu>
Via
email
C. Adami, S. Basa (LAM/Pytheas/AMU), A. de Ugarte Postigo (CNRS, OCA/LAM), E. Le Floc'h (CEA Paris-Saclay), J. Palmerio (GEPI, Obs. de Paris), F. Schussler (CEA Paris-Saclay) report:
We performed imaging of the field of GRB 240529A (Eyles-Ferris et al. GCN 36556; Kumar et al. GCN 36559; Joshi et al. GCN 36560; 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; Odeh et al. GCN 36573; de Ugarte Postigo et al. GCN 36574) with MISTRAL mounted on the 1.93 m telescope at Observatoire du Haut Provence (OHP, France). The observations consisted of 2 sets of 10x60s exposures in r-band under poor weather conditions, through passing clouds. Using a stack of the 6 only useable frames, we detect the afterglow close to the detection limit. Using as reference field stars from the Pan-STARRS catalogue, we determine a brightness of r(AB) = 19.8 +/- 0.3 mag at a mean date of 2024-05-30T01:52:00 UT, 0.9542 days after the burst. We note that this is slightly fainter but consistent with the value measured by GTC 1.75 hrs later (de Ugarte Postigo et al. GCN 36574).
We acknowledge the excellent support from Observatoire de Haute-Provence and in particular S. Favard for the MISTRAL observations and A. Radcliffe.
GCN Circular 36576
Subject
GRB 240529A: GROWTH-India optical follow-up
Date
2024-05-30T17:30:52Z (a year ago)
From
vishwajeet.s@iitb.ac.in
Via
Web form
T. Mohan, V. Swain, A. Salgundi, R. Kumar, V. Bhalerao (IITB), G.C. Anupama, S. Barway (IIA) and K. Angail (IAO) report on behalf of the GIT team:
We observed the field of GRB 240529A detected by Swift (Eyles-Ferris et al., GCN 36556) with 0.7m GROWTH-India Telescope (GIT). We started the observation at 2024-05-29 19:54:44 UT, i.e., 16.93 hours after the Swift trigger. We obtained multiple exposures of 400 seconds in the r', g' and i' filters. In our stacked images, we clearly detected the afterglow at the coordinates reported by Swift/UVOT Detection (Shilling et al., GCN 36562). The photometry results follow as:
---------------------------------------------------------------------------------
| JD (mid) | t-t0 (days) | Filter | Total Exposure (s) | Magnitude (AB) |
| ----------------- | ----------- |------- | ------------------ | -------------- |
| 2460460.425332341 | 0.801 | g' | 7x400 | 20.43 +/- 0.09 |
| 2460460.349607928 | 0.725 | r' | 8x400 | 19.14 +/- 0.05 |
| 2460460.386415344 | 0.762 | i' | 7x400 | 18.46 +/- 0.08 |
---------------------------------------------------------------------------------
The measurement is calibrated against PanSTARRS DR1 (Chambers et al., 2016) and not corrected for Galactic extinction.
Based on the publicly avialable photometry (Fu et al., GCN Circ. 36561; Postigo et al., GCN Circ. 36574; Adami et al., GCN Circ. 36575) and our measurements, we find that the source in r'-filter is fading as a power-law with flux proportional to (t−t0)^−alpha where t0 is Swift/BAT triggered time and calculated alpha = 1.12 +/- 0.01.
The GROWTH India Telescope (GIT; Kumar et al. 2022) is a 70-cm telescope with a 0.7-degree field of view, set up by the Indian Institute of Astrophysics (IIA) and the Indian Institute of Technology Bombay (IITB) with funding from DST-SERB and IUSSTF. It is located at the Indian Astronomical Observatory (Hanle), operated by IIA. We acknowledge funding by the IITB alumni batch of 1994, which partially supports the operations of the telescope. Telescope technical details are available at https://sites.google.com/view/growthindia/.
GCN Circular 36577
Subject
GRB 240529A: optical photometry from Konkoly
Date
2024-05-30T20:41:31Z (a year ago)
From
Jozsef Vinko at Konkoly Observator <vinko@konkoly.hu>
Via
legacy email
GRB 240529A: optical photometry from Konkoly
J. Vinko, A. Sodor, R. Konyves-Toth, L. Kriskovics, A. Pal, R. Szakats
(Konkoly Observatory, Hungary)
We report detection and photometry of the optical afterglow of GRB 240529A
(Eyles-Ferris et al. GCN 36556; Osborne et al. GCN 36557; Dichiara et al.
GCN 36564; Markwardt et al. GCN 36566) taken with the RC80 robotic telescope
at Piszkesteto Station of Konkoly Observatory, Hungary. The observations
started on 2024-05-29 22:40:46.49 UT. 5 sets of 300 sec frames were collected
through Sloan g', r'- and i' bands.
The optical afterglow (Kumar et al. GCN 36559; Joshi et al. GCN 36560; 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; Odeh et al. GCN 36573;
de Ugarte Postigo et al. GCN 36574; Adami et al. GCN 36575; Mohan et al. GCN 36576)
was detected on the stacked frames with the following magnitudes, calibrated
via nearby PS1 stars:
Date UT-middle t-T0(days) Exp(s) g'(AB) r'(AB) i'(AB)
2024-05-29 23:11:35.78 0.842 5x300 20.28 (0.21) 19.08 (0.09) 18.62 (0.09)
The magnitudes above are not corrected for galactic extinction.
GCN Circular 36578
Subject
GRB 240529A: Insight-HXMT/HE detection
Date
2024-05-31T02:38:28Z (a year ago)
From
tanwj@ihep.ac.cn
Via
Web form
Wenjun Tan, Shaolin Xiong , Xiaobo Li and Chengkui Li
report on behalf of the Insight-HXMT team:
At 2024-05-29T02:58:31.000 (T0), Insight-HXMT/HE detected
GRB 240529A(trigger ID: HEB240529123) in a routine search of the data,
which was also observed by Swift (Eyles-Ferris et al. GCN 36556; C. B. Markwardt et al. GCN 36566).
The Insight-HXMT/HE light curve consists of multiple
pulses with a duration (T90) of 66.23s measured from T0-37.26 s.
The 1s peak rate, measured from T0-0.159 s, is 3138 cnts/sec.
The total counts from this burst is 53027 counts.
URL_LC: https://twikinew.ihep.ac.cn/pubhxmt/HXMT/GRBList/HEB240529123_lc.jpg
All measurements above are made with the CsI detectors operating in the
regular mode with the energy range of about 80-800 keV (deposited energy).
Only gamma-rays with energy greater than about 200 keV can penetrate
the spacecraft and leave signals in the CsI detectors installed inside
the telescope.
Insight-HXMT is the first Chinese space X-ray telescope, which was
funded jointly by the China National Space Administration (CNSA) and
the Chinese Academy of Sciences (CAS).
More information about it could be found at:
http://hxmtweb.ihep.ac.cn/
GCN Circular 36579
Subject
GRB 240529A: MAAO 0.7m telescope optical afterglow detection
Date
2024-05-31T06:20:31Z (a year ago)
From
Gu Lim at Pusan National University <lim9gu@gmail.com>
Via
Web form
Lim, Gu (PNU), Kim, Dohyeong (PNU), Im, Myungshin (SNU), Park, Keun-Hong (MAAO), and Choi, Changmin (MAAO) report on behalf of the GECKO team
We searched for the optical afterglow of GRB 240529A (Eyles-Ferris et al., GCN 36556) with a 0.7m telescope at Miryang Arirang Astronomical Observatory (MAAO; Lim et al. 2024), one of the facilities of the GW EM-Counterpart Korean Observatory (GECKO). We started the observation at 2024-05-29T17:18:13 UT and obtained 10 images of each 120s with I-band 14.3 hours after the Swift detection (GCN 36556). The photometry is performed using 2xFWHM diameter aperture. The flux is calibrated using the APASS DR9 catalog (Henden et al. 2016) by converting the Vega system to the AB system using the Lupton (2005) transformation equation. After the image subtraction using HOTPANTS (Becker et al. 2015), we detected the optical afterglow at:
R.A (J2000): 22:21:25.92
Dec. (J2000): +51:33:43.46
This coordinate is within the uncertainty radius of the enhanced Swift-XRT report (Evans et al., GCN 36557). We determine a magnitude of I=17.46+/-0.19 AB mag without galactic extinction correction. Our detection is agreed with the results of (Odeh et al., GCN 36573).
T0 = 2024-05-29T02:58:31 UT (Eyles-Ferris et al., GCN 36556)
Tmid(UT) Exptime(s) Tmid-T0(hr) FWHM(") Mag+/-Magerr Depth_3sigma Filter
---------------------------------------------------------------------------------------
2024-05-29T17:32:38 180sx10 +14.3 5.6 17.46+/-0.19 18.40 I
Gravitational-wave EM Counterpart Korean Observatory (GECKO; Im et al. 2023, Proceedings of IAU Symp. Vol. 363, pp. 207.; Paek et al. 2024, The Astrophysical Journal, Vol. 960, Number 2, 113.) is a network of 0.5m to 1m class telescopes worldwide.
GCN Circular 36582
Subject
GRB 240529A: SAO RAS optical observations
Date
2024-05-31T19:24:45Z (a year ago)
From
Moskvitin Alexander at SAO RAS <mosk@sao.ru>
Via
legacy email
A. S. Moskvitin, O. I. Spiridonova and V. V. Vlasyuk (SAO RAS),
report on behalf of the GRB follow-up team.
We observed the field of the GRB 240529A (Eyles-Ferris et al.
GCN 36556; Osborne et al. GCN 36557; Joshi et al. GCN 36560;
Dichiara et al. GCN 36564; Markwardt et al. GCN 36566; Tan et al.
GCN 36578) with the SAO RAS 1m telescope Zeiss-1000 equipped
with CCD-photometer. We obtained 4 x 300 sec frames in Rc band
on May 30, 23:35:04--23:56:50 UT (t_mid - T0 = 1.8663 days).
The OT (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; Odeh et al. GCN 36573; de Ugarte Postigo et al.
GCN 36574; Adami et al. GCN 36575; Mohan et al. GCN 36576;
Vinko et al., GCN 36577; Lim et al. GCN 36579) is clearly detected
in the stacked frame with the brightness of R = 20.02 +/- 0.10.
The magnitudes were calibrated using R2 magnitudes of nearby USNO-B1.0
stars.
GCN Circular 36583
Subject
IPN triangulation of the initial episode of GRB 240529A
Date
2024-05-31T22:31:27Z (a year ago)
From
Dmitry Svinkin at Ioffe Institute <svinkin@mail.ioffe.ru>
Via
legacy email
A.S. Kozyrev, D.V. Golovin, M.L. Litvak, I.G. Mitrofanov, and A.B. Sanin
on behalf of the HEND/Mars Odyssey team,
D. Svinkin, D. Frederiks, A. Ridnaia, A. Lysenko,
and T. Cline on behalf of the Konus-Wind team,
E. Burns, on behalf of the IPN,
S. Barthelmy, J. Cummings, H. Krimm, D. Palmer, and A. Tohuvavohu
on behalf of the Swift-BAT team,
and
W. Boynton, C. Fellows, K. Harshman, H. Enos, R. Starr,
and A.S. Gardner on on behalf of the GRS-Odyssey GRB team,
report:
The long-duration GRB 240529A
(Swift-BAT detection: Eyles-Ferris et al., GCN 36556;
AstroSat-CZTI detection: Joshi et al., GCN 36560;
Insight-HXMT/HE detection: Tan et al., GCN 36578)
was detected by Swift (BAT), Konus-Wind, AstroSat (CZTI),
Insight-HXMT (HE), and Mars-Odyssey (HEND).
The burst triggered Swift-BAT at T0(BAT) = 10710.788 s UT (02:58:30.788).
The Konus-Wind lightcurve shows two emission episodes at ~T0(BAT)-400 s and ~T0(BAT)-300 s. These episodes was also detected by Swift (BAT), probably outside the coded FoV, and Mars-Odyssey (HEND).
We have triangulated the most intense episode (at ~T0(BAT)-400 s)
to a preliminary, 3 sigma error box whose coordinates are:
---------------------------------------------
RA(2000), deg Dec(2000), deg
---------------------------------------------
Center:
336.181 (22h 24m 43s) +52.215 (+52d 12' 55")
Corners:
341.510 (22h 46m 02s) +56.219 (+56d 13' 07")
331.787 (22h 07m 09s) +47.993 (+47d 59' 34")
332.038 (22h 08m 09s) +47.767 (+47d 46' 02")
341.743 (22h 46m 58s) +55.982 (+55d 58' 54")
---------------------------------------------
The error box area is 2.61 sq. deg, and its maximum
dimension is 10.2 deg (the minimum one is 15 arcmin).
The Sun distance was 73 deg.
Triangulation of the less intense episode (at ~T0(BAT)-400 s) is consistent with this IPN localization.
This localization is consistent with the Swift localization of
GRB 240529A, implying the episodes belong to GRB 240529A and extending the burst duration up to ~600 s.
A triangulation map and HEALPix FITS file are posted at
http://www.ioffe.ru/LEA/GRBs/GRB240529_T10304/IPN
The HEALPix triangulation map is the multi-order HEALPix in units of probability density.
The Konus-Wind time history and spectrum will be given in a forthcoming GCN Circular.
GCN Circular 36584
Subject
Konus-Wind detection of GRB 240529A
Date
2024-05-31T22:37:34Z (a year ago)
From
Dmitry Svinkin at Ioffe Institute <svinkin@mail.ioffe.ru>
Via
legacy email
D. Svinkin, D. Frederiks, M. Ulanov, A. Tsvetkova,
A. Lysenko, A. Ridnaia, and T. Cline
on behalf of the Konus-Wind team, report:
The long-duration GRB 240529A
(Swift-BAT detection: Eyles-Ferris et al., GCN 36556;
AstroSat-CZTI detection: Joshi et al., GCN 36560;
Insight-HXMT/HE detection: Tan et al., GCN 36578;
IPN triangulation: Kozyrev et al., GCN 36583)
triggered Konus-Wind at T0=10304.829 s UT (02:51:44.829).
The burst light curve shows two separated multipeaked emission episodes.
The first episode starts at ~T0-14.1 s and has a total duration of ~150 s,
the second (detected by Swift-BAT) starts at ~T0+344 s and lasts up to ~T0+520 s.
The emission is seen up to ~3 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB240529_T10304/
As observed by Konus-Wind, the burst
had a fluence of 1.3(-0.5,+0.4)x10^-4 erg/cm2,
and a 64-ms peak flux, measured from T0+6.960 s,
of 3.40(-0.93,+1.10)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).
The time-averaged spectrum of the burst
(measured from T0 to T0+491.264 s)
is best fit in the 20 keV - 3 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -1.11(-0.36,+1.61),
the high energy photon index beta = -2.02(-7.98,+0.22),
the peak energy Ep = 161(-100,+203) keV
(chi2 = 56/66 dof).
The spectrum near the maximum count rate
(measured from T0 to T0+7.936 s)
is best fit in the 20 keV - 3 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -1.00(-0.10,+0.15),
the high energy photon index beta = -2.85(-1.37,+0.50),
the peak energy Ep = 210(-33,+26) keV
(chi2 = 61/66 dof).
Assuming the redshift z=2.695 (Ugarte Postigo et al., GCN 36574)
and a standard cosmology model with H_0 = 67.3 km/s/Mpc,
Omega_M = 0.315, and Omega_Lambda = 0.685 (Planck Collaboration, 2014),
we estimate the following rest-frame parameters:
the isotropic energy release E_iso is 2.2(-0.8,+0.7)x10^54 erg,
the peak luminosity L_iso is 2.1(-0.6,+0.7)x10^53 erg/s,
the rest-frame peak energy of the time-integrated spectrum Ep,i,z is 595(-370,+750) keV,
and the rest-frame peak energy at the peak of the emission Ep,p,z is 776(-122,+96) keV.
With the obtained estimates, GRB 240529A is inside 90% prediction band
for the 'Amati' relation and inside 68% prediction band
for the 'Yonetoku' relation derived 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/GRB240529_T10304/GRB240529A_rest_frame.pdf
All the quoted errors are at the 90% confidence level.
All the quoted values are preliminary.
GCN Circular 36585
Subject
GRB 240529A : Mondy optical observations
Date
2024-06-01T02:27:03Z (a year ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
Via
legacy email
N. Pankov (HSE, IKI), A. Pozanenko (IKI), E. Klunko (ISTP), S. Belkin (IKI) report on behalf of GRB IKI FuN:
We observed the field of GRB 240529A (Eyles-Ferris et al.GCN 36556; Osborne et al. GCN 36557; Joshi et al. GCN 36560; Dichiara et al. GCN 36564; Markwardt et al. GCN 36566; Tan et al. GCN 36578) with AZT-33IK telescope of Mondy observatory in R-filter starting 2024-05-30 (UT) 17:12:21. The optical afterglow (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; Odeh et al. GCN 36573; de Ugarte Postigo et al.GCN 36574; Adami et al. GCN 36575; Mohan et al. GCN 36576; Vinko et al., GCN 36577; Lim et al. GCN 36579; Moskvitin et al. GCN 36582) is clearly detected in a stacked image.
Date UT start t-T0 Exp. Filter OT Err. UL(3 sigma)
(mid, days) (s)
2024-05-30 17:12:21 1.61308 29x120 R 19.67 0.11 21.6
The photometry is based on nearby USNO-B1.0 R2 stars.
GCN Circular 36589
Subject
GRB 240529A: 1.3m DFOT Optical observations
Date
2024-06-01T10:34:44Z (a year ago)
From
Amit Kumar Ror at ARIES <mitturor77894@gmail.com>
Via
email
Amit K. Ror, Anshika Gupta, Rishi C., Shashi B. Pandey, and Kuntal Misra
(ARIES) report:
We observed the field of GRB 240529A detected by Swift (Eyles-Ferris et
al., 2024 GCN 36556) with the 1.3m Devasthal Fast Optical Telescope (DFOT),
located at the Devasthal Observatory of the Aryabhatta Research Institute
of Observational Sciences (ARIES), India. The observations were started on
2024-05-30 at 21:11:46 UT, i.e., ~ 1.76 days after the BAT trigger. We have
taken multiple frames with an exposure time of 300 s in the R filter. A
similar set of observations was also performed on 2024-05-31 at 20:34:36
UT, i.e., ~ 2.734 days after the BAT trigger. We stacked the images after
the alignment. We clearly detected an optical afterglow in our final
stacked image within the error box of enhanced Swift-XRT and UVOT
observations (Osborne et al., 2024, GCN 36557; Shilling et al., 2024, GCN
36562). The estimated preliminary magnitude is as follows:
Date Start_UT T_start-T0 (days) Filter Exp time (s) Magnitude
=================================================
2024-05-30 21:11:46 UT 1.76 R 300*20 20.15 +/- 0.04
The detection of the GRB afterglow is consistent with the observations of
Kumar et al., 2024, GCN 36559; Fu et al., 2024, GCN 36561; Shilling et al.,
2024, GCN 36562; Perez-Garcia et al., 2024, GCN 36563; Dutton et al., 2024,
GCN 36568; Mo et al., 2024, GCN 36569; Odeh et al., 2024, GCN 36573;
Postigo et al., 2024, GCN 36574; Adami et al., 2024, GCN 36575; Mohan et
al., 2024, GCN 36576; Vinko et al., 2024, GCN 36577; Lim et al., 2024, GCN
36579; Moskvitin et al., 2024, GCN 36582; and Pankov et al., 2024, GCN
36585.
By combining our magnitudes with the observations of Moskvitin et al.
(2024, GCN 36582) and Pankov et al. (2024, GCN 36585), we have calculated
the decay index ~ 1.44 of the R-band light curve at late time.
The given magnitude value is not corrected for the Galactic and host
extinctions in the direction of the GRB afterglow. Photometric calibration
is performed using the standard stars from the USNO-B1.0 catalog. This
circular may be cited.
GCN Circular 36592
Subject
GRB 240529A: AKO Optical Afterglow Follow-Up Observations
Date
2024-06-01T12:17:07Z (a year ago)
From
Mohammad Odeh at Al Khatim Observatory M44 <mshodeh@gmail.com>
Via
legacy email
Mohammad Odeh (Al-Khatim Observatory, AKO, operated by the International
Astronomical Center in Abu Dhabi, UAE), Nidhal Guessoum, Dalya Akl, Ilmah
Aabdi, and Shaikha AlShamsi (American University of Sharjah, UAE), report:
As a follow-up to our first observation performed on May 29, 2024 (GCN 36573
<https://gcn.nasa.gov/circulars/36573>), we report further observations of
the field of GRB 240529A (Eyles-Ferris et al., GCN 36556) with our 0.36m
f/7.7 robotic telescope, on May. 30, starting at 22:09 UT.
We obtained multiple 180-sec exposures in the Ic filter, where we
marginally detected the GRB afterglow.
Our detection is consistent with the results of (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; Odeh et al. GCN
36573; Adami et al., GCN 36575; Mohan et al., GCN 36576; Vinko et al., GCN
36577; Gu et al., GCN 36579; Moskvitin et al., GCN 36582; Pankov et al.,
GCN 36585; Ror et al., GCN 36589).
The following table summarizes the results of the two nights, calculated
using the Atlas catalog as a reference:
-----------------------------------------------------------------
ObsTime (mid), Exposure, Filter, Mag, S/N, Lim. Mag.
-----------------------------------------------------------------
2024-05-29T23:08:00Z, 24 x 180s (stacked), Ic, 17.9 +/- 0.10, 16.1, 19.8
2024-05-30T23:15:55Z, 21 x 180s (stacked), Ic, 18.8 +/- 0.17, 8.0, 19.7
-----------------------------------------------------------------
The magnitudes are not corrected for galactic extinction.
For reference, cutouts of the GRB, as visible in our images for both
nights, can be found below:
Night 1
<https://astronomycenter.net/images/GRB/GRB%20240529A_Seen_20240529.png>
Night 2
<https://astronomycenter.net/images/GRB/GRB%20240529A_Seen_20240530.png>
GCN Circular 36597
Subject
GRB 240529A: further SAO RAS optical observations
Date
2024-06-02T13:30:58Z (a year ago)
From
Moskvitin Alexander at SAO RAS <mosk@sao.ru>
Via
legacy email
A. S. Moskvitin, O. I. Spiridonova, O. A. Maslennikova (SAO RAS),
report on behalf of the GRB follow-up team.
We observed the field of the GRB 240529A (Eyles-Ferris et al.
GCN 36556; Osborne et al. GCN 36557; Joshi et al. GCN 36560;
Dichiara et al. GCN 36564; Markwardt et al. GCN 36566; Tan et al.
GCN 36578) with the SAO RAS 1m telescope Zeiss-1000 equipped
with CCD-photometer. We obtained 8 x 300 sec frames in the Rc band
on June 1, 23:30:20 -- June 2, 00:16:50 UT (t_mid - T0 = 3.8716 days).
The OT (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; Odeh et al. GCNs 36573, 36592;
de Ugarte Postigo et al. GCN 36574; Adami et al. GCN 36575;
Mohan et al. GCN 36576; Vinko et al. GCN 36577; Lim et al. GCN 36579;
Pankov et al. GCN 36585; Ror et al., 36589) is clearly detected
in the stacked frame with the brightness of R = 20.7 +/- 0.1.
The magnitudes were calibrated using R2 magnitudes of nearby USNO-B1.0
stars.
GCN Circular 36599
Subject
GRB 240529A: OSN optical detection
Date
2024-06-02T20:53:59Z (a year ago)
From
Youdong HU at INAF-OAB <huyoudong072@hotmail.com>
Via
Web form
Y.-D. Hu (INAF-OAB), F. Aceituno, E. Fernandez-Garcia, A. J. Castro-Tirado, I. Perez-Garcia, S.-Y. Wu， M.D. Caballero-Garcia, R. Sanchez-Ramirez, S. Guziy (IAA-CSIC), on behalf of a larger collaboration, report:
Following the detection of GRB 240529A by Swift (Eyles-Ferris et al. GCNC 36556), we triggered the 1.5m telescope of the Observatiorio Sierra Nevada (OSN) near Granada, Spain. Observations in the RI bands began on Jun. 1 at 01:06 UT (~ 2.9 days post burst). The afterglow is clearly detected with 19.4+-0.1 mag in the I-band image (exposure 300 s) within the enhanced XRT/Swift position (Osborne et al. GCNC 36557). Our result is consistent with previous reports from GOTO (Kumar et al. GCNC 36559), NOT (Fu et al. GCNC 36561), UVOT (Shilling et al. GCNC 36562), BOOTES (Perez-Garcia et al., GCNC 36563), Skynet (Dutton et al., GCNC 36568), WINTER (Mo et al., GCNC 36569), AKO (Odeh et al. GCNC 36573), GTC (de Ugarte Postigo et al., GCNC 36574), T193/MISTRAL (Adami et al., GCNC 36575), GROWTH (Mohan et al., GCNC 36576), Konkoly (Vinko et al., GCNC 36577), MAAO (Gu et al., GCNC 36579), SAO (Moskvitin et al., GCNC 36582, GCNC 36594), Mondy (Pankov et al., GCNC 36585) and DFOT (Ror et al., GCNC 36589). Further imaging is ongoing.
We thank the staff at OSN for their excellent support.
GCN Circular 36601
Subject
GRB 240529A: continued SAO RAS optical observations
Date
2024-06-03T02:31:13Z (a year ago)
From
Moskvitin Alexander at SAO RAS <mosk@sao.ru>
Via
legacy email
A. S. Moskvitin, O. A. Maslennikova, O. I. Spiridonova (SAO RAS),
report on behalf of the GRB follow-up team.
We observed the field of the GRB 240529A (Eyles-Ferris et al.
GCN 36556; Osborne et al. GCN 36557; Joshi et al. GCN 36560;
Dichiara et al. GCN 36564; Markwardt et al. GCN 36566; Tan et al.
GCN 36578; Kozyrev et al. GCN 36583; Svinkin et al. GCN 36584)
with the SAO RAS 1m telescope Zeiss-1000 equipped with CCD-photometer.
We obtained 11 x 300 sec frames in the Rc band on June 2, 23:09:06 --
June 3, 00:12:47 UT (t_mid - T0 = 4.8628 days).
The OT (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; Odeh et al. GCNs 36573, 36592;
de Ugarte Postigo et al. GCN 36574; Adami et al. GCN 36575;
Mohan et al. GCN 36576; Vinko et al. GCN 36577; Lim et al. GCN 36579;
Moskvitin et al. GCNs 36582, 36597; Pankov et al. GCN 36585;
Ror et al., 36589; Hu et al. GCN 36599) is clearly detected
in the stacked frame almost with the same brightness as the day before
R = 20.72 +/- 0.09.
The magnitudes were calibrated using R2 magnitudes of nearby USNO-B1.0
stars.
GCN Circular 36603
Subject
GRB 240529A: MASTER prompt OT detection
Date
2024-06-03T05:40:18Z (a year ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>
Via
legacy email
V.Lipunov (MSU), D.Buckley (SAAO),
K.Zhirkov, G.Antipov, E.Gorbovskoy, A.Kuznetsov, D.Vlasenko, P.Balanutsa,
N.Tiurina, Ya.Kechin, Yu.Tselik, D.Zimnukhov, V.Senik, A.Yudin, V.Topolev,
A.Chasovnikov,D.Cheryasov(Lomonosov MSU,SAI,PhysicsDepartment),
O.Gress, N.Budnev(ISU),
A.Sosnovskij (Crimean Astrophysical Observatory, RAS),
C.Francile. F. Podesta, R.Podesta (Observatorio Astronomico Felix AguilarOAFA),
R. Rebolo, M. Serra(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 etal.,2010,Advances in Astronomy,2010,30L)
started observation (Lipunov et al. GCN 36555) of Swift GRB240529A (Eyles-Ferris et al. GCN36556, Ttrigger= 02:58:31UT)
in MASTER-SAAO at 3 degrees altitude at 2024-05-29 02:59:20 by wide-field MASTER-II camera and
at 2024-05-29 02:59:16 (44s after GRB time) by very wide field MASTER-VWF camera.
The optical transient MASTER OT J222126.06+513344.6 clearly detected since
03:00:20 with m_OT~14.5 at first maximum and with possible second maximum at light curve
during prompt emission of this GRB (Swift-BAT lightcurve Markwardt,Barthelmy et al. GCN36566)
The reduction of first 40 images from MASTER-VWFC since 2024-05-29 02:59:16 with OT substraction will be continued.
Observations started at zenith distance = 87 deg. The sun altitude was -31.0deg.
The galactic latitude b = -5 deg., longitude l = 101 deg.
Real time updated cover map and OT discovered available here:
https://master.sai.msu.ru/site/master2/observ.php?id=2474976
GCN Circular 36613
Subject
GRB 240529A: SAO RAS optical observations
Date
2024-06-04T15:21:45Z (a year ago)
From
Moskvitin Alexander at SAO RAS <mosk@sao.ru>
Via
legacy email
A. S. Moskvitin, O. A. Maslennikova, O. I. Spiridonova (SAO RAS),
report on behalf of the GRB follow-up team.
We observed the field of the GRB 240529A (Eyles-Ferris et al.
GCN 36556; Osborne et al. GCN 36557; Joshi et al. GCN 36560;
Dichiara et al. GCN 36564; Markwardt et al. GCN 36566; Tan et al.
GCN 36578; Kozyrev et al. GCN 36583; Svinkin et al. GCN 36584)
with the SAO RAS 1m telescope Zeiss-1000 equipped with CCD-photometer.
We obtained 15 x 200 sec frames in the Rc band on June 3, 23:17:01 --
June 4, 00:16:47 UT (t_mid - T0 = 5.8669 days).
The OT (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; Odeh et al. GCNs 36573, 36592;
de Ugarte Postigo et al. GCN 36574; Adami et al. GCN 36575;
Mohan et al. GCN 36576; Vinko et al. GCN 36577; Lim et al. GCN 36579;
Moskvitin et al. GCNs 36582, 36597; 36601; Pankov et al. GCN 36585;
Ror et al., 36589; Hu et al. GCN 36599; Lipunov et al., GCN 36603)
is clearly detected in the stacked frame with the brightness of
R = 20.96 +/- 0.09.
The magnitudes were calibrated using R2 magnitudes of nearby USNO-B1.0
stars.
GCN Circular 36636
Subject
GRB 240529A: radio detection with AMI-LA
Date
2024-06-07T11:47:28Z (a year ago)
From
Lauren Rhodes at Oxford <lauren.rhodes@physics.ox.ac.uk>
Via
Web form
Lauren Rhodes, Rob Fender (Oxford), Dave Green, Dave Titterington (Cambridge) report:
We observed the field of GRB 240529A (GCN 36556) with the Arcminute Microkelvin Imager - Large Array (AMI-LA) at 15.5 GHz beginning at UT 04:11:39 on 02-June-2024 for a total of 4 hours. The flux standard 3c286 was used to calibrate the bandpass response and flux scale of the AMI-LA and J2202+4216 was used as an interleaved complex gain calibrator.
We detected an unresolved radio source at the position of the afterglow candidate (also reported in GCN 36556) with a peak flux density of ~1mJy/beam. The rms noise in the field is about 40uJy/beam.
More observations are ongoing.
We thank the staff at the Mullard Radio Astronomy Observatory for carrying out these observations and operating the AMI-LA.
GCN Circular 36642
Subject
GRB 240529A: NOEMA detection
Date
2024-06-07T21:34:41Z (a year ago)
From
Antonio de Ugarte Postigo at OCA <deugarte@oca.eu>
Via
email
A. de Ugarte Postigo (CNRS/OCA & LAM), J.M. Winters (IRAM), M. Bremer (IRAM), C. C. Thoene (ASU-CAS), J. F. Agui Fernandez (CAHA), S. Antier (OCA), S. Basa (LAM), M. Michalowski (AOI-AMU), D. A. Perley (LJMU), J.-G. Ducoin (CPPM) report:
We observed the afterglow of GRB 240529A (Eyles-Ferris et al. GCN 36556, ) with the NOEMA interferometer, located at Plateau de Bure (France). The observation was performed on the 3rd June 2024 at around 11:00 UT, 5.3 days after the burst onset at the 3 mm band.
The afterglow is detected at a flux density of ~2 mJy, indicating that the peak emission is still at higher frequencies than the 15 GHz detection by AMI-LA (Rhodes et al. GCN 36636).
Based on observations carried out under project number W23DI with the IRAM NOEMA Interferometer. IRAM is supported by INSU/CNRS (France), MPG (Germany) and IGN (Spain).
GCN Circular 36654
Subject
GRB 240529A : MITSuME Akeno optical afterglow detection
Date
2024-06-10T11:17:09Z (a year ago)
From
Masafumi Niwano at Tokyo Institute of Technology <niwano@hp.phys.titech.ac.jp>
Via
Web form
M. Niwano, I. Takahashi, M. Sasada, N. Higuchi, S. Hayatsu, H. Seki, S. Joshima, Y. Kubo, H. Hagio, Y. Yatsu and N. Kawai (Tokyo Tech) report on behalf of the MITSuME collaboration:
We observed the field of GRB 240529A (Eyles-Ferris et al. GCN 36556) with the optical three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm telescope Akeno.
The observation with a series of 60 sec exposures started at 2024-05-29 15:11:22 UT (12.2 hrs after the Swift trigger). We stacked the images in good conditions. Then we detected point source in the Ic-band image at the Swift/UVOT position (Eyles-Ferris et al. GCN 36556). Here we report the Ic-band photometry on the image subtracted with a reference image taken at 2024-06-04 (5 days after the trigger), and the 5-sigma upper-limits as follows.
T0+[hrs] | MID-UT | T-EXP[sec] | magnitudes of aperture photometry
----------------------------------------------------------------------------------------------------------------
12.3 | 2024-05-29 16:10:25 | 1080 | g’>18.1, Rc>17.9, Ic=17.5+/-0.2
----------------------------------------------------------------------------------------------------------------
T0+ : Elapsed time after the trigger
T-EXP: Total Exposure time
We used the PS1 catalog for flux calibration. The catalog magnitudes in PS1 g, r and i bands were converted to our g'-, Rc- and Ic-band magnitudes following Tonry et al. (2012), Table 6. The magnitudes are expressed in the AB system. The images were processed in real-time through the MITSuME GPU reduction pipeline (Niwano et al. 2021, PASJ; https://github.com/MNiwano/Eclaire).
GCN Circular 36655
Subject
GRB 240529A: LBT optical detection and late temporal decay
Date
2024-06-10T13:22:57Z (a year ago)
From
Andrea Rossi at INAF <andrea.rossi@inaf.it>
Via
Web form
A. Rossi, E. Maiorano (INAF-OAS), A. Melandri (INAF-OAR), D. B. Malesani (DAWN/NBI and Radboud), L. Izzo (INAF-OACn & DARK/NBI) and M . De Pasquale (Univ. of Messina) report on behalf of the CIBO collaboration:
We observed the field of GRB 240529A (Eyles-Ferris et al., GCN 36556; Joshi et al., GCN 36560; Tan et al., GCN 36578; Kozyrev et al., GCN 36583 et al. GCN 36583; Svinkin et al., GCN 36584) with the LBC camera mounted on LBT (Mt Graham, AZ, USA) in u'g'r'i'z' bands approximately at midtime 9:55 UT on 2024-06-05 and 7.3 days after the burst trigger.
The optical transient (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; Odeh et al. GCNs 36573, 36592; de Ugarte Postigo et al. GCN 36574; Adami et al. GCN 36575; Mohan et al. GCN 36576; Vinko et al. GCN 36577; Lim et al. GCN 36579; Moskvitin et al. GCNs 36582, 36597, 36601 ; Pankov et al. GCN 36585; Ror et al., 36589; Hu et al. GCN 36599; Lipunov et al. GCN 36603) is well detected in r’i’z’ bands. The good seeing (0.8") allows us to detect the afterglow and separate it from a brighter star which is only 1 arcsec away and visible also in PanSTARRS archival images. Using PSF photometry, we measure a preliminary AB magnitude of r'=23.9+-0.1, calibrated against PanSTARRS field stars, and not corrected for the foreground Galactic extinction.
This detection together with the early photometry reported in the GCNs (selected between 5 and 30 hours after the trigger to be less contaminated by the near-by bright-star) are well fitted by a power-law decay with index -1.9, in agreement with the Swift/XRT late-time decay behavior.
We acknowledge the excellent support from the LBTO and LBT-INAF staff, particularly J. Rupert, S. Allanson, F. Cusano, E. Marini, D. Paris, and E. O. Kishka in obtaining these observations.
GCN Circular 36656
Subject
GRB240529A: 3.6m TNG NIR detection 8d after the burst
Date
2024-06-10T17:25:40Z (a year ago)
From
Youdong HU at INAF-OAB <huyoudong072@hotmail.com>
Via
Web form
Y.-D. Hu, P. D'Avanzo, M. Ferro, R. Brivio, S. Covino, D. Fugazza, S. Campana (INAF-OAB), A. Rossi (INAF-OAS), D. B. Malesani (DAWN/NBI & Radboud Univ.), A. Melandri (INAF-OAR), L. Di Fabrizio, H. Stoev (INAF-TNG) on behalf of the CIBO collaboration report:
We observed the field of the GRB240529A detected by the Swift (Eyles-Ferris et al., GCNC 36556), AstroSat (Joshi et al., GCNC 36560), Insight-HXMT (Tan et al., GCNC 36578), IPN (Kozyrev et al., GCNC 36583) and Konus-Wind (Svinkin et al., GCNC 36584) with the Italian 3.6m TNG telescope equipped with the near-infrared camera NICS to follow up its afterglow. A series of images were obtained with the J filter starting on 2024-06-06 04:42:44 UT (i.e. 8.1 days post T0). The afterglow (Kumar et al. GCNC 36559, Fu et al. GCNC 36561, Shilling et al. GCNC 36562, Perez-Garcia et al., GCNC 36563, Dutton et al., GCNC 36568, Mo et al., GCNC 36569, Odeh et al. GCNC 36573, GCNC 36592, de Ugarte Postigo et al., GCNC 36574, Adami et al., GCNC 36575, Mohan et al., GCNC 36576, Vinko et al., GCNC 36577, Gu et al., GCNC 36579, Moskvitin et al., GCNC 36582, GCNC 36594, GCNC 36597, GCNC 36601, GCNC 36613, Pankov et al., GCNC 36585, Ror et al., GCNC 36589, Hu et al., GCNC 36599, Lipunov et al., GCNC 36603, Rhodes et al., GCNC 36636, Niwano et al., GCNC 36654, Rossi et al., GCNC 36655) is faintly detected in the co-added image with a preliminary result of J(Vega)~20.4 mag (calibrated against the 2MASS catalogue).
GCN Circular 36734
Subject
GRB 240529A: JinShan optical observations
Date
2024-06-22T14:23:13Z (a year ago)
From
Dong Xu at NAOC/CAS <dxu@nao.cas.cn>
Via
Web form
J. An, X. Liu, Z.P. Zhu, S.Q. Jiang, S.Y. Fu, T.H. Lu, D. Xu (NAOC), J.Z. Liu (XAO) report on behalf of a large collaboration:
We observed the field of GRB 240529A by Swift (Eyles-Ferris et al. GCN 36556) using the 50cm-B, 50cm-C, 100cm-C telescopes (50B,50C,100C) of the JinShan project located at Altay, Xinjiang, China.
Observations were carried out between 16:14:18 UT and 17:55:39 UT on 2024-05-29 in the g, r, i, and z filters. The previously reported optical afterglow, e.g., by Swift/UVOT (Eyles-Ferris et al. GCN 36556; Shilling et al., GCN 36562) was clearly detected in our images.
Photometric results are reported as follows
T-T0(d) | Filter | Mag | MagErr
---------------------------------
0.5639 | g | 19.76 | 0.18
0.5691 | r | 18.56 | 0.06
0.5639 | i | 17.80 | 0.05
0.6037 | z | 17.65 | 0.06
calibrated with nearby PanSTARRS stars and not corrected for Galactic extinction.
Furthers observations have also been done by JinShan.
We acknowledge the excellent support from S.W Luo, M.M. Yang, Z. K. Feng, and L.F. Huo for enabling these observations.
GCN Circular 36947
Subject
GRB240529A: VIRT optical transient detection
Date
2024-07-27T17:41:52Z (a year ago)
From
Priya Gokuldass at ERAU <gokuldap@my.erau.edu>
Via
Web form
K. Smith (UVI), P. Gokuldass (ERAU), N. Orange (OrangeWave Innovative Science, LLC), D. Morris (NASA), T. Lombardi (Eckerd College), K. Noonan (UVI), D. Smith (UVI), R. Querrard (UVI) report:
We observed the field of GRB240529A (Eyles-Ferris et al., GCN 36556; Joshi et al., GCN 36560; Tan et al., GCN 36578; Kozyrev et al., GCN 36583; Svinkin et al., GCN 36584) with the 0.5m Virgin Islands Robotic Telescope (VIRT) at the University of the Virgin Islands' Etelman Observatory on 2024-05-30 starting at 7:10:12 UT (with Tmid as T+ 28.19 hrs). We performed a series of exposures in R filter with a total exposure of 2630s. The weather conditions were partly cloudy during the hours of observation with an average airmass of ~1.36.
We detect the optical transient reported by others (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; Odeh et al. GCNs 36573, 36592; de Ugarte Postigo et al. GCN 36574; Adami et al. GCN 36575; Mohan et al. GCN 36576; Vinko et al. GCN 36577; Lim et al. GCN 36579; Moskvitin et al. GCNs 36582, 36597, 36601 ; Pankov et al. GCN 36585; Ror et al., GCN 36589; Hu et al. GCN 36599; Lipunov et al. GCN 36603). Our data are consistent with the slow decay suggested through earlier reports (Odeh et al. GCN 36573, 36592; Lim et al. GCN 36579; Ror et al. GCN 36589; Moskvitin et al. GCNs 36582, 36597, 36601; Rossi et al. GCN 36655). We report the following magnitude:
T_mid. ||Exposure ||Filter ||Magnitude
T+ 28.19 hrs ||2630s ||R ||19.4 +/- 0.1
The limit is estimated from comparison to nearby PANSTAARS and is not corrected for Galactic extinction. The VIRT is still in the commissioning phase.
We acknowledge financial support from NASA MUREP MIRO awad 80NSSC21M001, NASA EPSCoR award 80NNSC22M0063, and NSF PAARE award 2319415. We also acknowledge the use of STDWeb interface to verify our result.
GCN Circular 37612
Subject
GRB 240529A: FRAM-ORM early optical afterglow observations reveal plateau and rebrightening
Date
2024-09-26T15:18:39Z (9 months ago)
From
Martin Jelinek at Astro.Inst-AVCR,Ondrejov <martin.jelinek@asu.cas.cz>
Via
legacy email
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 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)