GRB 211129A
GCN Circular 31136
Subject
GRB 211129A: Swift detection of a burst
Date
2021-11-29T10:11:32Z (4 years ago)
From
Phil Evans at U of Leicester <pae9@star.le.ac.uk>
J.D. Gropp (PSU), S. D. Barthelmy (GSFC), P. A. Evans (U Leicester),
N. J. Klingler (GSFC/UMBC/CRESSTII), K. L. Page (U Leicester) and
B. Sbarufatti (PSU) report on behalf of the Neil Gehrels Swift
Observatory Team:
At 09:51:06 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 211129A (trigger=1085430). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 274.557, +31.776 which is
RA(J2000) = 18h 18m 14s
Dec(J2000) = +31d 46' 33"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve shows 3 major peaks
with a duration of about 200 sec. The peak count rate was ~1400 counts/sec
(15-350 keV),
at ~3 sec after the trigger.
The XRT began observing the field at 09:52:19.7 UT, 73.5 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 274.58129, 31.78820 which
is equivalent to:
RA(J2000) = 18h 18m 19.51s
Dec(J2000) = +31d 47' 17.5"
with an uncertainty of 4.0 arcseconds (radius, 90% containment). This
location is 86 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/1085430.
We cannot determine whether the source is fading at the present time. No
spectrum from the promptly downlinked event data is yet available to
determine the column density.
The initial flux in the 2.5 s image was 1.41e-09 erg cm^-2 s^-1 (0.2-10
keV).
UVOT took a finding chart exposure of 150 seconds with the White filter
starting 83 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
0.082.
Burst Advocate for this burst is J.D. Gropp (jdg44 AT psu.edu).
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 31137
Subject
GRB 211129A: MITSuME Akeno optical upper limits
Date
2021-11-29T10:36:23Z (4 years ago)
From
Ryohei Hosokawa at Tokyo Institute of Technology <hosokawa@hp.phys.titech.ac.jp>
R. Yamaguchi, R. Hosokawa, Y. Imai, K. L. Murata, M. Niwano, Y.
Takamatsu, N. Ito, R. Noto, S. Sato, M. Takaku, Y. Yatsu, and N. Kawai
(TokyoTech) report on behalf of the MITSuME collaboration:
We observed the field of GRB 211129A(J.D. Gropp et al. GCN Circular
#31136) 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 10 sec exposures started at 2021-11-29 09:52:06 UT (60
seconds after Swift trigger). We stacked the images with good
conditions. We did not detect any uncatalogued sources within the XRT
error region (J.D. Gropp et al. GCN Circular #31136). We obtained the
5-sigma limits of the stacked images as follows.
T0+[sec] MID-UT T-EXP[sec] 5-sigma limits
------------------------------------------------------------------------------------------------
159 2021-11-29 09:53:45 70 g'>17.0, Rc>17.3, Ic>16.4
------------------------------------------------------------------------------------------------
T0+ : Elapsed time after the burst
T-EXP: Total Exposure time
We used PS1 catalog for flux calibration.
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, Vol.73, Issue 1, Pages
4-24; https://github.com/MNiwano/Eclaire).
GCN Circular 31139
Subject
GRB 211129A: Enhanced Swift-XRT position
Date
2021-11-29T14:07:46Z (4 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
M.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester)
report on behalf of the Swift-XRT team.
Using 1213 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 211129A, 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 = 274.58031, +31.78886 which is equivalent
to:
RA (J2000): 18h 18m 19.27s
Dec (J2000): +31d 47' 19.9"
with an uncertainty of 2.1 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 31140
Subject
GRB 211129A: Nanshan/NEXT optical upper limit
Date
2021-11-29T14:24:12Z (4 years ago)
From
Dong Xu at NAOC/CAS <dxu@nao.cas.cn>
Z.P. Zhu (NAOC, HUST), X. Liu, S.Y. Fu, S.Q. Jiang, D. Xu (NAOC), X. Gao
(Urumqi No.1 Senior High School), J.Z. Liu (XAO) report:
We observed the field of Swift GRB 211129A (Gropp et al. GCN Circ.
31136) using the NEXT-0.6m telescope located at Nanshan, Xinjiang,
China. We obtained 18x120 s frames in the Sloan r-band, starting at
12:38:57 UT on 2021-11-29, i.e., 2.8 hr after the BAT trigger.
No optical source is detected at the Enhanced Swift/XRT position (Goad
et al. GCN Circ. 31139) in our stacked image, down to a limiting
magnitude of r~21.2, calibrated with the nearby PanSTARRS field.
GCN Circular 31141
Subject
Swift GRB 211129A: Global MASTER-Net observations report
Date
2021-11-29T14:48:10Z (4 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>
V. Lipunov, V.Kornilov, E.Gorbovskoy, K.Zhirkov, N.Tyurina, P.Balanutsa, A.Kuznetsov,
D. Vlasenko, G.Antipov, D.Zimnukhov, V.Senik, T.Pogrosheva, E.Minkina,
A.Chasovnikov, V.Topolev, V.Grinshpun, D.Kuvshinov, D. Cheryasov
(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. Gres, N.M. Budnev
(Irkutsk State University, API),
A. Tlatov, D. Dormidontov
(Kislovodsk Solar Station of the Pulkovo Observatory),
A. Gabovich, V.Yurkov
(Blagoveschensk Educational State University)
MASTER-Kislovodsk robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory) was pointed to the Swift GRB 211129A ( J.D. Gropp et al., GCN 31136) errorbox 17290 sec after notice time and 17308 sec after trigger time at 2021-11-29 14:39:34 UT, with upper limit up to 16.0 mag. Observations started at twilight. The observations began at zenith distance = 45 deg. The sun altitude is -11.1 deg.
The galactic latitude b = 20 deg., longitude l = 59 deg.
Real time updated cover map and OT discovered available here:
https://master.sai.msu.ru/site/master2/observ.php?id=1799491
We obtain a following upper limits.
Tmid-T0 | Site |Filt.| Expt. | Limit| Comment
_________|_____________________|_____|_______|______|________
17399 | MASTER-Kislovodsk | C | 180 | 16.0 |
17399 | MASTER-Kislovodsk | C | 180 | 12.8 |
Filter C is a clear (unfiltred) band.
The observation and reduction will continue.
The message may be cited.
GCN Circular 31142
Subject
GRB 211129A: Fermi GBM observation
Date
2021-11-29T16:53:17Z (4 years ago)
From
Elisabetta Bissaldi at INFN,Bari <elisabetta.bissaldi@ba.infn.it>
E. Bissaldi (Politecnico and INFN Bari)
reports on behalf of the Fermi GBM Team:
"At 09:51:06.36 UT on 29 November 2021, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 211129A (trigger 659872271 / 211129410),
which was also detected by the Swift/BAT (Gropp et al. 2021, GCN 31136).
The GBM on-ground location is consistent with the Swift position.
The angle from the Fermi LAT boresight at the GBM trigger time is 22 degrees.
The GBM light curve consists of multiple peaks
with a duration (T90) of about 111 s (50-300 keV).
The time-averaged spectrum from T0-8 s to T0+41 s is
adequately fit by a power law function with an exponential
high-energy cutoff. The power law index is -1.54 +/- 0.09 and
the cutoff energy, parameterized as Epeak, is 220 +/- 90 keV.
The event fluence (10-1000 keV) in this time interval is
(4.3 +/- 0.4)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+27 s in the 10-1000 keV band
is 2.81 +/- 0.22 ph/s/cm^2.
The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog:
https://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html
For Fermi GBM data and info, please visit the official Fermi GBM Support Page:
https://fermi.gsfc.nasa.gov/ssc/data/access/gbm/"
GCN Circular 31147
Subject
GRB 211129A: Swift/UVOT Upper Limits
Date
2021-11-29T23:54:11Z (4 years ago)
From
Alexander Belles at PSU/Swift <aub1461@psu.edu>
A. Belles (PSU) and J. D. Gropp (PSU)
report on behalf of the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 211129A
84 s after the BAT trigger (Gropp et al., GCN Circ. 31136).
No optical afterglow consistent with the XRT position
(Goad et al. GCN Circ. 31139)
is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and subsequent exposures are:
Filter T_start(s) T_stop(s) Exp(s) Mag
white_FC 84 234 147 >20.7
u_FC 297 547 246 >20.4
white 84 769 186 >20.9
v 626 818 39 >18.8
b 552 744 39 >19.6
u 297 719 265 >20.5
w1 675 695 19 >19.6
m2 651 831 28 >19.2
w2 602 794 39 >20.1
The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.081 in the direction of the burst
(Schlegel et al. 1998).
GCN Circular 31148
Subject
GRB 211129A: Swift-XRT refined Analysis
Date
2021-11-30T01:32:32Z (4 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
J.A. Kennea (PSU), A. Tohuvavohu (U. Toronto), K.L. Page (U.
Leicester), A.P. Beardmore (U. Leicester), P.A. Evans (U. Leicester),
T. Sbarrato (INAF-OAB), P. D'Avanzo (INAF-OAB), M.G. Bernardini
(INAF-OAB), B. Sbarufatti (PSU) and J.D. Gropp report on behalf of the
Swift-XRT team:
We have analysed 6.2 ks of XRT data for GRB 211129A (Gropp et al. GCN
Circ. 31136), from 62 s to 50.9 ks after the BAT trigger. The data
comprise 325 s in Windowed Timing (WT) mode (the first 9 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Goad et al.
(GCN Circ. 31139).
The late-time light curve (from T0+4.5 ks) can be modelled with a
power-law decay with a decay index of alpha=1.02 (+/-0.08).
A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.63 (+/-0.05). The
best-fitting absorption column is 4.8 (+/-0.3) x 10^21 cm^-2, in
excess of the Galactic value of 8.8 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 2.30 (+0.16, -0.15)
and a best-fitting absorption column of 5.9 (+0.9, -0.8) x 10^21 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum is 3.6 x 10^-11 (7.5 x 10^-11) erg cm^-2
count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 5.9 (+0.9, -0.8) x 10^21 cm^-2
Galactic foreground: 8.8 x 10^20 cm^-2
Excess significance: 10.1 sigma
Photon index: 2.30 (+0.16, -0.15)
If the light curve continues to decay with a power-law decay index of
1.02, the count rate at T+24 hours will be 0.038 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.4 x
10^-12 (2.9 x 10^-12) erg cm^-2 s^-1.
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/01085430.
This circular is an official product of the Swift-XRT team.
GCN Circular 31149
Subject
GRB 211129A: Swift-BAT refined analysis
Date
2021-11-30T03:22:44Z (4 years ago)
From
Amy Lien at GSFC <amy.y.lien@nasa.gov>
D. M. Palmer (LANL), S. D. Barthelmy (GSFC),
J. D. Gropp (PSU), H. A. Krimm (NSF),
S. Laha (GSFC/UMBC), A. Y. Lien (U Tampa),
C. B. Markwardt (GSFC), T. Parsotan (GSFC/UMBC),
T. Sakamoto (AGU), M. Stamatikos (OSU) (i.e. the Swift-BAT team):
Using the data set from T-239 to T+800 sec from the recent telemetry
downlink, we report further analysis of BAT GRB 211129A (trigger #1085430)
(Gropp et al., GCN Circ. 31136). The BAT ground-calculated position is
RA, Dec = 274.565, 31.781 deg which is
RA(J2000) = 18h 18m 15.6s
Dec(J2000) = +31d 46' 51.5"
with an uncertainty of 1.5 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 83%.
The mask-weighted light curve shows a multi-peaked structure that starts
at ~T-2 s and ends at ~T+120 s. The three main peaks occur at ~T+1 s,
~T+29 s, and ~T+91 s, respectively. T90 (15-350 keV) is 113.01 +- 9.14 sec
(estimated error including systematics).
The time-averaged spectrum from T-1.80 to T+124.11 sec is best fit by
a simple power-law model. The power law index of the time-averaged
spectrum is 1.75 +- 0.13. The fluence in the 15-150 keV band
is 2.3 +- 0.2 x 10^-6 erg/cm2. The 1-sec peak photon flux measured
from T+0.99 sec in the 15-150 keV band is 1.5 +- 0.2 ph/cm2/sec.
All the quoted errors are at the 90% confidence level.
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/1085430/BA/