TITLE: GCN CIRCULAR
NUMBER: 36661
SUBJECT: GRB 240607A: GECAM detection of a bright long burst
DATE: 24/06/11 16:27:47 GMT
FROM: wenlongzhang2018(a)163.com
Wen-Long Zhang, Shao-Lin Xiong and Wen-Jun Tan report on behalf of the GECAM team:
GECAM-C detected a long burst, GRB 240607A, at 2024-06-07T11:01:14.31 UTC (T0), which was also detected by Fermi/GBM (GCN #36634), AstroSat-CZTI (GCN #36638), Konus-Wind (GCN #36659) .
According to the GECAM-C light curve, this burst shows multiple pulses with a total duration of ~30 sec.
We note that these results are very preliminary. Refined analysis will be reported later.
Gravitational wave high-energy Electromagnetic Counterpart All-sky Monitor (GECAM) mission originally consists of two microsatellites (GECAM-A and GECAM-B) launched in December 2020. As the third member of GECAM constellation, GECAM-C was launched onboard SATech-01 experimental satellite in July 2022. GECAM mission is funded by the Chinese Academy of Sciences (CAS).
View this GCN Circular online at https://gcn.nasa.gov/circulars/36661.
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TITLE: GCN CIRCULAR
NUMBER: 36660
SUBJECT: Fermi GRB 240611A: Global MASTER-Net observations report
DATE: 24/06/11 14:15:22 GMT
FROM: Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov(a)xray.sai.msu.ru>
V. Lipunov, V.Kornilov, E. Gorbovskoy, K. Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov, V.Senik, D. Vlasenko,
G.Antipov, D.Zimnukhov, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov, D. Cheryasov, Ya.Kechin, Yu.Tselik, A. Sosnovskij
(Lomonosov Moscow State University, SAI, Physics Department),
R. Podesta, C.Lopez, F. Podesta, C.Francile
(Observatorio Astronomico Felix Aguilar OAFA),
R. Rebolo, M. Serra
(The Instituto de Astrofisica de Canarias),
D. Buckley
(South African Astronomical Observatory),
O.A. Gress, N.M. Budnev, O.Ershova
(Irkutsk State University, API),
L.Carrasco, J.R.Valdes, V.Chavushyan, V.M.Patino Alvarez, J.Martinez,
A.R.Corella, L.H.Rodriguez
(INAOE, Guillermo Haro Astrophysics Observatory),
A. Tlatov, D. Dormidontov
(Kislovodsk Solar Station of the Pulkovo Observatory),
V. Yurkov, A. Gabovich
(Blagoveschensk Educational State University)
MASTER-Amur robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Blagoveshchensk State Pedagogical University) started inspect of the Fermi GRB 240611A ( Fermi GBM team, GCN 36658) errorbox 9612 sec after notice time and 9643 sec after trigger time at 2024-06-11 13:19:42 UT, with upper limit up to 13.2 mag. Observations started at twilight. The observations began at zenith distance = 29 deg. The sun altitude is -11.4 deg.
The galactic latitude b = 30 deg., longitude l = 107 deg.
Real time updated cover map and OT discovered available here:
https://master.sai.msu.ru/site/master2/observ.php?id=2489453
We obtain a following upper limits.
Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment
_________|_____________________|_____________________|____________________________________|_____|_______|_______|________
9673 | 2024-06-11 13:19:42 | MASTER-Amur | (17h 31m 13.12s , +75d 32m 05.7s) | C | 60 | 13.2 |
Filter C is a clear (unfiltred) band.
The observation and reduction will continue.
The message may be cited.
View this GCN Circular online at https://gcn.nasa.gov/circulars/36660.
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TITLE: GCN CIRCULAR
NUMBER: 36659
SUBJECT: Konus-Wind detection of GRB 240607A
DATE: 24/06/11 13:55:10 GMT
FROM: Anna Ridnaia at Ioffe Institute <ridnaia(a)mail.ioffe.ru>
A. Ridnaia, D. Frederiks, A. Lysenko, D. Svinkin,
A. Tsvetkova, M. Ulanov, and T. Cline,
on behalf of the Konus-Wind team, report:
The very bright, long-duration GRB 240607A
(Fermi-GBM detection: The Fermi GBM team, GCN 36634;
Dalessi, GCN 36637; Dalessi and Meegan, GCN 36641;
BALROG localization: Preis et al., GCN 36635;
AstroSat-CZTI detection: Waratkar et al., GCN 36638;
IPN triangulation: Kozyrev at al., GCN 36650)
triggered Konus-Wind at T0=39674.62 s UT (11:01:14.620).
The burst light curve shows a multipeaked structure
which starts at ~T0-0.2 s and has a total duration of ~24.7 s.
The emission is seen up to ~6 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB240607_T39674/
As observed by Konus-Wind, the burst
had a fluence of 1.03(-0.06,+0.05)x10^-4 erg/cm2,
and a 64-ms peak flux, measured from T0+10.960 s,
of 3.02(-0.33,+0.34)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+29.440 s)
is best fit in the 20 keV - 10 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.94(-0.05,+0.05),
the high energy photon index beta = -2.92(-0.42,+0.22),
the peak energy Ep = 248(-13,+13) keV
(chi2 = 111/98 dof).
The spectrum near the maximum count rate
(measured from T0+10.752 to T0+11.264 s)
is best fit in the 20 keV - 10 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.21(-0.18,+0.19),
the high energy photon index beta = -2.77(-0.37,+0.20),
the peak energy Ep = 249(-24,+31) keV
(chi2 = 54/46 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/36659.
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TITLE: GCN CIRCULAR
NUMBER: 36657
SUBJECT: EXO 0748-676: Swift-BAT refined analysis
DATE: 24/06/10 22:17:46 GMT
FROM: Tyler Parsotan at NASA GSFC <tyler.parsotan(a)nasa.gov>
M. J. Moss (GSFC), S. D. Barthelmy (GSFC),
R. Gupta (GSFC), H. A. Krimm (NSF),
S. Laha (GSFC/UMBC), A. Y. Lien (U Tampa),
C. B. Markwardt (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 EXO 0748-676 (trigger #1236151)
(D’Elia, et al., GCN Circ. 36653). The BAT ground-calculated position is
RA, Dec = 117.083, -67.777 deg which is
RA(J2000) = 07h 48m 20.0s
Dec(J2000) = -67d 46' 35.5"
with an uncertainty of 2.7 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 92%.
The mask-weighted lightcurve shows a fast rise exponential decay profile in the
15-25 keV energy range.
T90 (15-350 keV) is 8.06 +- 2.52 sec (estimated error including systematics).
The time-averaged spectrum from T-1.45 to T+7.90 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
5.07 +- 0.86. The fluence in the 15-150 keV band is 7.4 +- 1.7 x 10^-08 erg/cm2.
The 1-sec peak photon flux measured from T+0.90 sec in the 15-150 keV band
is 0.3 +- 0.1 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/1236151
View this GCN Circular online at https://gcn.nasa.gov/circulars/36657.
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TITLE: GCN CIRCULAR
NUMBER: 36656
SUBJECT: GRB240529A: 3.6m TNG NIR detection 8d after the burst
DATE: 24/06/10 17:25:40 GMT
FROM: Youdong HU at INAF-OAB <huyoudong072(a)hotmail.com>
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).
View this GCN Circular online at https://gcn.nasa.gov/circulars/36656.
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TITLE: GCN CIRCULAR
NUMBER: 36655
SUBJECT: GRB 240529A: LBT optical detection and late temporal decay
DATE: 24/06/10 13:22:57 GMT
FROM: Andrea Rossi at INAF <andrea.rossi(a)inaf.it>
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.
View this GCN Circular online at https://gcn.nasa.gov/circulars/36655.
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TITLE: GCN CIRCULAR
NUMBER: 36654
SUBJECT: GRB 240529A : MITSuME Akeno optical afterglow detection
DATE: 24/06/10 11:17:09 GMT
FROM: Masafumi Niwano at Tokyo Institute of Technology <niwano(a)hp.phys.titech.ac.jp>
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).
View this GCN Circular online at https://gcn.nasa.gov/circulars/36654.
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TITLE: GCN CIRCULAR
NUMBER: 36653
SUBJECT: Trigger 1236151: Swift detection of EXO 0748-676
DATE: 24/06/10 08:04:47 GMT
FROM: K.L. Page at U Leicester <klp5(a)leicester.ac.uk>
V. D'Elia (SSDC & INAF-OAR), J. A. Kennea (PSU),
K. L. Page (U Leicester) and T. M. Parsotan (GSFC) report on behalf of
the Neil Gehrels Swift Observatory Team:
At 07:36:36 UT, the Swift Burst Alert Telescope (BAT) triggered and
located EXO 0748-676 (trigger=1236151). Swift slewed immediately to the source.
The BAT on-board calculated location is
RA, Dec 117.175, -67.804 which is
RA(J2000) = 07h 48m 42s
Dec(J2000) = -67d 48' 13"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve showed a complex
structure with a duration of about 25 sec. The peak count rate
was ~500 counts/sec (15-350 keV), at ~5 sec after the trigger.
The XRT began observing the field at 07:37:56.0 UT, 79.7 seconds after
the BAT trigger. Using promptly downlinked data we find a bright X-ray
source with an enhanced position: RA, Dec 117.13960, -67.75271 which is
equivalent to:
RA(J2000) = 07h 48m 33.50s
Dec(J2000) = -67d 45' 09.7"
with an uncertainty of 1.9 arcseconds (radius, 90% containment). This
location is 190 arcseconds from the BAT onboard position, outside 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. This position is 2.7 arcseconds from a
known X-ray source: LSXPS J074833.8-674507. This source is in the Swift
XRT LSXPS catalogue with a mean 0.3-10 keV count-rate of 0.07018 +/-
0.00060 ct/sec; see https://www.swift.ac.uk/LSXPS
/LSXPS%20J074833.8-674507 for details of these previous observations.
A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of 1.50
x 10^21 cm^-2 (Willingale et al. 2013).
The initial flux in the 2.5 s image was 6.37e-10 erg cm^-2 s^-1 (0.2-10
keV).
UVOT took a finding chart exposure of 150 seconds with the White filter
starting 879 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag.
The 8'x8' region for the list of sources generated on-board covers 100% of the
XRT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.126.
View this GCN Circular online at https://gcn.nasa.gov/circulars/36653.
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