GRB 220711B
GCN Circular 32416
Subject
GRB 220711B: CALET Gamma-Ray Burst Monitor detection
Date
2022-07-19T14:35:42Z (3 years ago)
From
Yuta Kawakubo at Louisiana State U./CALET <kawakubo1@lsu.edu>
Y. Shimizu, (Kanagawa U) A. Yoshida, T. Sakamoto, S. Sugita (AGU),
Y. Kawakubo (LSU), K. Yamaoka (Nagoya U), S. Nakahira (RIKEN),
Y. Asaoka (ICRR), S. Torii, Y. Akaike, K. Kobayashi (Waseda U),
Y. Shimizu (Kanagawa U), N. Cannady (GSFC/UMBC),
M. L. Cherry (LSU), S. Ricciarini (U of Florence),
P. S. Marrocchesi (U of Siena),
and the CALET collaboration:
The long GRB 220711B (Fermi GBM Final Real-time Localization: Fermi GBM team,
GCN Circ. 32365; Fermi GBM Detection: Lesage et al., GCN Circ 32369;
Swift detection: D'Ai et al., GCN Circ 32366, Swift-BAT refined analysis:
Krimm et al., GCN Circ 32374) triggered the CALET Gamma-ray
Burst Monitor (CGBM) at 18:16:31.192 UTC on 11 July 2022
(http://cgbm.calet.jp/cgbm_trigger/flight/1341598587/index.html).
The burst signal was seen by all CGBM detectors. No real-time CGBM GCN
notice was distributed about this trigger because the real-time communication
from the ISS was off (loss of signal).
The burst light curve shows a multi-peaked structure which starts
at T-39.5 sec, peaks at T-2.4 sec, and ends at T+93.7 sec.
The T90 and T50 durations measured by the SGM data are 82.7 +/- 3.8 sec
and 15.7 +/- 4.0 sec (40-1000 keV), respectively.
The ground processed light curve is available at
http://cgbm.calet.jp/cgbm_trigger/ground/1341598587/
The CALET data used in this analysis are provided by
the Waseda CALET Operation Center located at the Waseda University.
GCN Circular 32388
Subject
Retraction of GRB 220711B: 10.4 m GTC(+EMIR) observations (GCN 32387)
Date
2022-07-13T21:19:03Z (3 years ago)
From
Youdong HU at IAA-CSIC <huyoudong072@hotmail.com>
Y.-D. Hu report:
GCNC 32387 is a repeated submittion of GCNC 32386 by mistake. Please ignore it and pay attention to GCNC 32386. Sorry for this mistake and I apologize for any confusion this mistake may have caused.
GCN Circular 32387
Subject
GRB 220711B: 10.4 m GTC(+EMIR) observations
Date
2022-07-13T18:43:53Z (3 years ago)
From
Youdong HU at IAA-CSIC <huyoudong072@hotmail.com>
R. Sanchez-Ramirez, Y.-D. Hu, I. Perez-Garcia, M.D. Caballero-Garcia, A.J. Castro-Tirado (IAA-CSIC) report on behalf of a larger collaboration:
We observed the field of GRB220711B (Fermi GBM team GCNC 32365, D'Ai et al. GCNC 32366) with the Espectrografo Multiobjeto Infra-Rojo (EMIR), mounted on the 10.4m Gran Telescopio de Canarias (GTC) in La Palma (Spain). Imaging observations started on Jul 12 at 00:32:14 (~4.3 hrs after the GRB) and were carried out in the J and Ks bands for a total exposure time of 1260s in each filter. The afterglow reported by Malesani et al. (GCNC 32368 and 32377) is clearly detected in a preliminary reduction of both filters, measuring J~21.3 AB.
A second epoch was obtained on Jul 12 at 23:31:10 in the J band, observing a decay of about 1 magnitude between both epochs. Further observations are planned.
We thank the excellent support from the GTC staff.
GCN Circular 32386
Subject
GRB 220711B: 10.4 m GTC(+EMIR) observations
Date
2022-07-13T18:24:32Z (3 years ago)
From
Rubén Sánchez-Ramírez at IAA-CSIC <ruben@iaa.es>
R. Sanchez-Ramirez, Y.-D. Hu, I. Perez-Garcia, M.D. Caballero-Garcia, A.J. Castro-Tirado (IAA-CSIC) report on behalf of a larger collaboration:
We observed the field of GRB220711B (Fermi GBM team GCNc 32365, D'Ai et al. GCNc 32366) with the Espectrografo Multiobjeto Infra-Rojo (EMIR), mounted on the 10.4m Gran Telescopio de Canarias (GTC) in La Palma (Spain).
Imaging observations started on Jul 12 at 00:32:14 (~4.3 hrs after the GRB) and were carried out in the J and Ks bands for a total exposure time of 1260s in each filter.
The afterglow reported by Malesani et al. (GCNc 32368 and 32377) is clearly detected in a preliminary reduction of both filters, measuring J~21.3 AB.
A second epoch was obtained on Jul 12 at 23:31:10 in the J band, observing a decay of about 1 magnitude between both epochs.
Further observations are planned.
We thank the excellent support from the GTC staff.
GCN Circular 32383
Subject
GRB 220711B, GROND observations
Date
2022-07-13T14:52:45Z (3 years ago)
From
Ana Nicuesa at TLS Tautenburg <ana@tls-tautenburg.de>
A. Nicuesa Guelbenzu, S. Klose (both TLS Tautenburg), and A. Rau (MPE
Garching) report:
We observed the field of GRB 220711B (D'Ai et al., GCN 32366;
Beardmore et al. GCN 32370) with GROND mounted at the 2.2m MPG
telescope at La Silla Observatory (Chile).
Observations started at 01:53 UT on July 13, 2022, about 32 hr after
the GRB trigger and were on target for 40 minutes. They were performed
at an average seeing of 1.0 arcsec and at an airmass of 1.7.
The fading source discovered by Malesani et al. (GCN 32377) is
detected in the combined JHK images. For the individual bands we can
only provide the following preliminary upper limits (midtime of 2:20
UT):
g' > 23.0,
r' > 23.5,
i' > 23.2,
z' > 19.8,
J > 21.7,
H > 21.1,
K > 20.1 (AB mag; 3 sigma).
The given limits are derived based on calibrating the optical images
against the SDSS catalog and the JHK data against 2MASS stars.
We thank Sam Kim and Regis Lachaume for excellent support and for
performing the observations.
GCN Circular 32381
Subject
GRB 220711B: NUTTelA-TAO / BSTI Early Optical Limits (Preliminary)
Date
2022-07-13T06:42:29Z (3 years ago)
From
Toktarkhan Komesh at Nazarbayev University <toktarkhan.komesh@nu.edu.kz>
T. Komesh (NU), B. Grossan (UCB, NU), Z. Maksut (NU), M. Krugov (FAI),
report on behalf of the Energetic Cosmos Laboratory: The Nazarbayev
University Transient Telescope at Assy-Turgen Astrophysical Observatory
(NUTTelA-TAO) observed the field of GRB 220711B on receipt of an
automated GCN / BAT position alert, observing in Sloan g', r' and i'
bands, with the Burst Simultaneous Three-Channel Imager (BSTI; Grossan,
Kumar & Smoot 2019, JHEA, 32, 14). We received the alert at UT
2022-07-11 18:16:50, 22 seconds after ��the BAT trigger time, and started
observations at UT 18:17:02, 12 s after receipt, 34 s after the BAT
trigger. Observations were made under partially cloudy conditions. No
new or changing sources consistent with the XRT position (Beardmore
2022, GCN 32370) were detected. The observations fully cover the
UVOT/XRT observation time interval and partly cover the prompt emission
time (D'Ai 2022, GCN 32366). Note that these observations provide
essentially full-time coverage, simultaneous in all three bands. We
report the following results: start time t-t0(s) end time UL g' UL r'
ULi' exposure_time (s) ------------ -------- ----------- ------ ------
----- ------ 18:17:02 34 18:18:02 18.3 18.1 17.7 60 18:18:17 109
18:23:17 19.2 18.9 18.7 300 start time is in UT. t-t0(s) gives the time
since trigger, in seconds. UL gives the 5 sigma upper limit sensitivity
in magnitudes, for images co-added to the given exposure time. The first
row in the table corresponds to co-adds of an initial short exposure
image sequence of 0.3 s (these sub-second exposures are read-noise
suppressed by our EMCCD cameras, with high gain electron multiplication
active; other images are taken in conventional CCD operation mode) for
g' and r', and 7.5 s for i'. The second row corresponds to co-adds from
a continuing series of 3 s exposures for g' and r', and 15 s exposures
for i'.�� Calibration was done with 4 bright Pan-STARRS catalog stars on
our images. We caution the reader that these are preliminary results,
without color or other corrections. Please also note that times are
approximate. ---------------------------------- NU = Nazarbayev
University, Nur-Sultan, Kazakhstan UCB = University of California,
Berkeley, USA HKUST = Hong Kong University of Science and Technology FAI
= Fesenkov Astrophysical Institute, Kazakhstan The NUTTelA-TAO Team
acknowledges the support of the staff of the Assy-Turgen Astrophysical
Observatory, Almaty, Kazakhstan, and the Fesenkov Astrophysical
Institute, Almaty, Kazkhstan.
GCN Circular 32380
Subject
GRB 220711B: GIT optical upper limits
Date
2022-07-13T02:48:45Z (3 years ago)
From
Varun Bhalerao at Indian Inst of Tech <varunb@iitb.ac.in>
V. Swain (IITB), H. Kumar (IITB), K. Angail (IAO), V. Bhalerao (IITB), G. C. Anupama (IIA), S. Barway (IIA) report on behalf of the GIT team:
We observed GRB 220711B detected by Fermi (Fermi GBM Team, GCN 32365; Lesage, GCN 32369), Swift (D'Ai et al., GCN 32366) and NOT optical (Malesani et al., GCN 32368), with the 0.7m GROWTH-India Telescope (GIT). The observations started at 18:22:15 UT on 2022-07-11, 5.78 mins after the Fermi trigger. We obtained multiple 300-sec exposures in the g', r' and i' filters. We did not detect any new source in our stacked images within the 2.1 arcsec radius circle around R.A.= 17h 28m 4.56s, Dec.= +24d 40' 51.5" (Beardmore et al. GCN #32370). The obtained upper limits follow as:
-------------------------------------------------------------------
JD (mid) | T_mid-T0(hrs) | Exposure (sec) | Filter | Lim_mag (5-sigma) |
-------------------------------------------------------------------
2459772.307085455 | 1.09 | 10 x 300 (stacked) | r' | > 21.03 |
2459772.313860030 | 1.25 | 5 x 300 (stacked) | g' | > 20.50 |
2459772.330168085 | 1.65 | 5 x 300 (stacked) | i' | > 20.34 |
-------------------------------------------------------------------
While the first image was observed within just 6 minutes of the burst, the observing conditions were suboptimal and the first r' image has a limiting magnitude of ~19. No source is detected in that single 300-s exposure either.
These upper limits are consistent with Strausbaugh et al.(GCN #32367), and Klingler et al.(GCN #32371), and with detection by Malesani et al (GCN #32368, 32377) given the high r-z colour they have inferred. The magnitudes are calibrated against PanSTARRS DR1 (Chambers et al., 2016) and not corrected for Galactic extinction.
The GROWTH India Telescope (GIT) 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 operations of the telescope. Telescope technical details are available at https://sites.google.com/view/growthindia/.
GCN Circular 32378
Subject
Fermi GRB 220711B: Global MASTER-Net observations report
Date
2022-07-13T00:30:23Z (3 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, E.Minkina, A.Chasovnikov, V.Topolev, D.Kuvshinov, D.Cheryasov, Ya.Kechin
(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),
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),
A. Gabovich, V.Yurkov
(Blagoveschensk Educational State University)
MASTER-SAAO robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L) located in South Africa (South African Astronomical Observatory) started inspect of the Fermi GRB 220711B ( Fermi GBM team, GCN 32365) errorbox 1 days 20192 sec after notice time and 1 days 20226 sec after trigger time at 2022-07-12 23:53:34 UT, with upper limit up to 17.0 mag. The observations began at zenith distance = 75 deg. The sun altitude is -71.6 deg.
The galactic latitude b = 25 deg., longitude l = 57 deg.
Real time updated cover map and OT discovered available here:
https://master.sai.msu.ru/site/master2/observ.php?id=2028449
We obtain a following upper limits.
Tmid-T0 | Date Time | Site | Coord (J2000) |Filt.| Expt. | Limit| Comment
_________|_____________________|_____________________|____________________________________|_____|_______|_______|________
9098 | 2022-07-11 20:47:36 | MASTER- | (17h 52m 34.45s , +31d 27m 32.4s) | C | 60 | 18.1 |
9173 | 2022-07-11 20:48:51 | MASTER- | (18h 02m 05.30s , +31d 27m 48.8s) | C | 60 | 18.0 |
9320 | 2022-07-11 20:51:18 | MASTER- | (17h 58m 24.11s , +29d 35m 23.4s) | C | 60 | 18.0 |
9395 | 2022-07-11 20:52:32 | MASTER- | (17h 57m 18.45s , +33d 21m 21.6s) | C | 60 | 18.3 |
9529 | 2022-07-11 20:54:47 | MASTER- | (18h 06m 54.95s , +33d 23m 15.9s) | C | 60 | 18.1 |
9603 | 2022-07-11 20:56:01 | MASTER- | (18h 06m 41.33s , +29d 33m 13.2s) | C | 60 | 17.9 |
9960 | 2022-07-11 21:01:58 | MASTER- | (18h 15m 59.80s , +29d 34m 09.9s) | C | 60 | 18.0 |
10371 | 2022-07-11 21:08:49 | MASTER- | (17h 52m 33.12s , +31d 28m 51.2s) | C | 60 | 18.1 |
10445 | 2022-07-11 21:10:03 | MASTER- | (18h 02m 02.64s , +31d 27m 49.2s) | C | 60 | 17.5 |
87628 | 2022-07-12 18:36:25 | MASTER- | (17h 44m 54.03s , +35d 17m 39.5s) | C | 60 | 17.1 |
87703 | 2022-07-12 18:37:40 | MASTER- | (17h 54m 49.30s , +35d 17m 32.4s) | C | 60 | 17.6 |
87835 | 2022-07-12 18:39:53 | MASTER- | (17h 34m 51.34s , +31d 31m 06.4s) | C | 60 | 17.6 |
87909 | 2022-07-12 18:41:06 | MASTER- | (17h 44m 09.20s , +31d 29m 54.8s) | C | 60 | 17.6 |
88045 | 2022-07-12 18:43:22 | MASTER- | (17h 39m 13.60s , +33d 24m 50.7s) | C | 60 | 17.8 |
88119 | 2022-07-12 18:44:36 | MASTER- | (17h 48m 43.86s , +33d 23m 37.4s) | C | 60 | 17.9 |
88258 | 2022-07-12 18:46:56 | MASTER- | (18h 04m 17.54s , +27d 42m 49.8s) | C | 60 | 17.6 |
88332 | 2022-07-12 18:48:10 | MASTER- | (18h 13m 13.60s , +27d 41m 39.0s) | C | 60 | 15.8 |
88469 | 2022-07-12 18:50:27 | MASTER- | (18h 03m 39.99s , +35d 18m 02.0s) | C | 60 | 18.1 |
88544 | 2022-07-12 18:51:41 | MASTER- | (18h 13m 29.75s , +35d 16m 52.5s) | C | 60 | 17.8 |
88680 | 2022-07-12 18:53:58 | MASTER- | (17h 44m 55.34s , +35d 19m 28.8s) | C | 60 | 17.9 |
88755 | 2022-07-12 18:55:13 | MASTER- | (17h 54m 50.22s , +35d 18m 15.6s) | C | 60 | 18.2 |
88893 | 2022-07-12 18:57:31 | MASTER- | (17h 34m 46.75s , +31d 31m 50.7s) | C | 60 | 18.0 |
88967 | 2022-07-12 18:58:45 | MASTER- | (17h 44m 15.51s , +31d 30m 40.0s) | C | 60 | 18.0 |
89105 | 2022-07-12 19:01:02 | MASTER- | (17h 39m 08.40s , +33d 25m 37.7s) | C | 60 | 18.0 |
89179 | 2022-07-12 19:02:17 | MASTER- | (17h 48m 51.01s , +33d 24m 26.3s) | C | 60 | 18.2 |
89255 | 2022-07-12 19:03:32 | MASTER- | (18h 04m 14.10s , +27d 41m 34.0s) | C | 60 | 17.8 |
89388 | 2022-07-12 19:05:45 | MASTER- | (18h 13m 15.43s , +27d 43m 22.9s) | C | 60 | 17.9 |
89464 | 2022-07-12 19:07:02 | MASTER- | (18h 03m 39.10s , +35d 17m 57.1s) | C | 60 | 18.3 |
89602 | 2022-07-12 19:09:20 | MASTER- | (18h 13m 29.70s , +35d 17m 42.4s) | C | 60 | 18.1 |
89678 | 2022-07-12 19:10:35 | MASTER- | (17h 44m 54.93s , +35d 17m 19.4s) | C | 60 | 18.2 |
89813 | 2022-07-12 19:12:51 | MASTER- | (17h 54m 44.11s , +35d 19m 07.0s) | C | 60 | 18.3 |
89888 | 2022-07-12 19:14:06 | MASTER- | (17h 34m 50.97s , +31d 30m 35.0s) | C | 60 | 18.1 |
90076 | 2022-07-12 19:17:14 | MASTER- | (17h 44m 10.26s , +31d 31m 24.1s) | C | 60 | 18.2 |
90150 | 2022-07-12 19:18:28 | MASTER- | (17h 39m 13.33s , +33d 24m 23.1s) | C | 60 | 18.1 |
90288 | 2022-07-12 19:20:46 | MASTER- | (17h 48m 44.63s , +33d 25m 12.3s) | C | 60 | 18.2 |
90364 | 2022-07-12 19:22:02 | MASTER- | (18h 04m 20.94s , +27d 42m 14.5s) | C | 60 | 17.8 |
90523 | 2022-07-12 19:24:41 | MASTER- | (18h 13m 17.06s , +27d 43m 04.0s) | C | 60 | 17.9 |
90600 | 2022-07-12 19:25:57 | MASTER- | (18h 03m 38.78s , +35d 17m 46.6s) | C | 60 | 18.3 |
90785 | 2022-07-12 19:29:02 | MASTER- | (18h 13m 21.62s , +35d 18m 32.9s) | C | 60 | 17.9 |
90860 | 2022-07-12 19:30:18 | MASTER- | (18h 10m 27.72s , +31d 28m 46.9s) | C | 60 | 18.0 |
91048 | 2022-07-12 19:33:26 | MASTER- | (18h 19m 51.93s , +31d 30m 34.1s) | C | 60 | 18.1 |
91123 | 2022-07-12 19:34:41 | MASTER- | (18h 15m 36.84s , +33d 22m 32.1s) | C | 60 | 12.4 |
91337 | 2022-07-12 19:38:14 | MASTER- | (17h 31m 41.85s , +29d 35m 08.8s) | C | 60 | 18.1 |
91524 | 2022-07-12 19:41:21 | MASTER- | (17h 40m 55.44s , +29d 36m 59.9s) | C | 60 | 18.1 |
91598 | 2022-07-12 19:42:36 | MASTER- | (17h 47m 05.69s , +27d 40m 57.4s) | C | 60 | 18.0 |
91785 | 2022-07-12 19:45:43 | MASTER- | (17h 56m 07.99s , +27d 42m 48.1s) | C | 60 | 17.9 |
91860 | 2022-07-12 19:46:58 | MASTER- | (18h 10m 33.38s , +31d 29m 29.1s) | C | 60 | 17.9 |
92048 | 2022-07-12 19:50:05 | MASTER- | (18h 19m 51.50s , +31d 30m 18.0s) | C | 60 | 18.0 |
92122 | 2022-07-12 19:51:20 | MASTER- | (18h 15m 41.53s , +33d 23m 16.4s) | C | 60 | 18.0 |
92335 | 2022-07-12 19:54:53 | MASTER- | (17h 31m 48.72s , +29d 35m 45.3s) | C | 60 | 18.0 |
92521 | 2022-07-12 19:57:58 | MASTER- | (17h 40m 53.67s , +29d 36m 37.9s) | C | 60 | 18.0 |
92595 | 2022-07-12 19:59:13 | MASTER- | (17h 47m 11.12s , +27d 41m 34.8s) | C | 60 | 17.8 |
92782 | 2022-07-12 20:02:20 | MASTER- | (17h 56m 07.69s , +27d 42m 26.6s) | C | 60 | 17.8 |
92856 | 2022-07-12 20:03:34 | MASTER- | (18h 10m 33.09s , +31d 29m 13.3s) | C | 60 | 17.0 |
106657 | 2022-07-12 23:53:34 | MASTER-SAAO | (17h 45m 25.60s , +31d 37m 42.4s) | C | 60 | 16.7 |
106737 | 2022-07-12 23:54:54 | MASTER-SAAO | (17h 54m 53.08s , +31d 37m 30.4s) | C | 60 | 16.8 |
106827 | 2022-07-12 23:56:24 | MASTER-SAAO | (17h 42m 12.38s , +29d 44m 25.4s) | C | 60 | 16.8 |
106906 | 2022-07-12 23:57:44 | MASTER-SAAO | (17h 51m 25.02s , +29d 45m 10.9s) | C | 60 | 16.9 |
106997 | 2022-07-12 23:59:15 | MASTER-SAAO | (17h 50m 05.59s , +33d 33m 46.5s) | C | 60 | 16.6 |
107087 | 2022-07-13 00:00:45 | MASTER-SAAO | (17h 59m 44.94s , +33d 32m 11.4s) | C | 60 | 16.8 |
107170 | 2022-07-13 00:02:07 | MASTER-SAAO | (17h 59m 41.66s , +29d 43m 34.7s) | C | 60 | 17.0 |
107260 | 2022-07-13 00:03:38 | MASTER-SAAO | (18h 08m 50.39s , +29d 44m 05.3s) | C | 60 | 17.0 |
107340 | 2022-07-13 00:04:57 | MASTER-SAAO | (17h 57m 22.60s , +27d 51m 15.7s) | C | 60 | 16.9 |
107432 | 2022-07-13 00:06:30 | MASTER-SAAO | (18h 06m 18.27s , +27d 49m 45.4s) | C | 60 | 17.0 |
107512 | 2022-07-13 00:07:50 | MASTER-SAAO | (17h 27m 56.18s , +31d 40m 35.1s) | C | 60 | 14.9 |
107814 | 2022-07-13 00:12:52 | MASTER-SAAO | (17h 37m 16.91s , +31d 39m 31.8s) | C | 60 | 15.8 |
107905 | 2022-07-13 00:14:23 | MASTER-SAAO | (17h 45m 37.78s , +31d 40m 12.6s) | C | 60 | 16.1 |
107996 | 2022-07-13 00:15:53 | MASTER-SAAO | (17h 54m 57.41s , +31d 38m 25.7s) | C | 60 | 16.3 |
108075 | 2022-07-13 00:17:13 | MASTER-SAAO | (17h 42m 25.20s , +29d 46m 22.8s) | C | 60 | 16.1 |
108166 | 2022-07-13 00:18:44 | MASTER-SAAO | (17h 51m 26.66s , +29d 45m 13.2s) | C | 60 | 16.3 |
108246 | 2022-07-13 00:20:03 | MASTER-SAAO | (17h 59m 51.64s , +33d 32m 54.3s) | C | 60 | 16.3 |
108336 | 2022-07-13 00:21:34 | MASTER-SAAO | (17h 59m 42.45s , +29d 43m 45.6s) | C | 60 | 16.4 |
108416 | 2022-07-13 00:22:54 | MASTER-SAAO | (18h 08m 57.21s , +29d 43m 34.7s) | C | 60 | 16.5 |
108507 | 2022-07-13 00:24:24 | MASTER-SAAO | (17h 57m 25.77s , +27d 51m 33.7s) | C | 60 | 16.4 |
108586 | 2022-07-13 00:25:44 | MASTER-SAAO | (18h 06m 25.29s , +27d 49m 33.4s) | C | 60 | 16.6 |
Filter C is a clear (unfiltred) band.
The observation and reduction will continue.
The message may be cited.
GCN Circular 32374
Subject
GRB 220711B: Swift-BAT refined analysis
Date
2022-07-12T16:35:07Z (3 years ago)
From
Amy Lien at GSFC <amy.y.lien@nasa.gov>
H. A. Krimm (NSF), S. D. Barthelmy (GSFC),
A. D'Ai (INAF-IASFPA), S. Laha (GSFC/UMBC),
A. Y. Lien (U Tampa), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), 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+963 sec from the recent telemetry
downlink, we report further analysis of BAT GRB 220711B (trigger #1115766)
(D'Ai et al., GCN Circ. 32366). The BAT ground-calculated position is
RA, Dec = 262.018, 24.674 deg which is
RA(J2000) = 17h 28m 04.3s
Dec(J2000) = +24d 40' 27.1"
with an uncertainty of 1.3 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 19%.
The mask-weighted light curve shows a multi-peaked structure that
starts at ~T-40 s and ends at ~T+100 s. The main peak occurs at ~T0.
T90 (15-350 keV) is 88.64 +- 19.96 sec (estimated error including
systematics).
The time-averaged spectrum from T-37.72 to T+98.89 sec is best fit
by a simple power-law model. The power law index of the time-averaged
spectrum is 1.75 +- 0.08. The fluence in the 15-150 keV band
is 6.0 +- 0.3 x 10^-6 erg/cm2. The 1-sec peak photon flux measured
from T-0.02 sec in the 15-150 keV band is 3.0 +- 0.4 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/1115766/BA/
GCN Circular 32372
Subject
GRB 220711B: Swift-XRT refined Analysis
Date
2022-07-12T12:14:06Z (3 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester), E. Ambrosi
(INAF-IASFPA) , M. Capalbi (INAF-IASFPA), M. Perri (SSDC & INAF-OAR),
D.N. Burrows (PSU), J. D. Gropp (PSU), J.A. Kennea (PSU), P.A. Evans
(U. Leicester) and A. D'Ai report on behalf of the Swift-XRT team:
We have analysed 6.3 ks of XRT data for GRB 220711B (D'Ai et al. GCN
Circ. 32366), from 93 s to 44.7 ks after the BAT trigger. The data
comprise 414 s in Windowed Timing (WT) mode (the first 8 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 Beardmore
et al. (GCN Circ. 32370).
The late-time light curve (from T0+4.2 ks) can be modelled with a
power-law decay with a decay index of alpha=0.91 (+/-0.11).
A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.94 (+/-0.04). The
best-fitting absorption column is 2.59 (+/-0.16) x 10^21 cm^-2, in
excess of the Galactic value of 7.4 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 2.08 (+/-0.18) and a
best-fitting absorption column of 2.3 (+0.7, -0.6) x 10^21 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum is 3.4 x 10^-11 (4.9 x 10^-11) erg cm^-2
count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 2.3 (+0.7, -0.6) x 10^21 cm^-2
Galactic foreground: 7.4 x 10^20 cm^-2
Excess significance: 4.4 sigma
Photon index: 2.08 (+/-0.18)
If the light curve continues to decay with a power-law decay index of
0.91, the count rate at T+24 hours will be 0.016 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 5.4 x
10^-13 (7.9 x 10^-13) erg cm^-2 s^-1.
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/01115766.
This circular is an official product of the Swift-XRT team.
GCN Circular 32371
Subject
GRB 220711B: Swift/UVOT Upper Limits
Date
2022-07-12T05:02:33Z (3 years ago)
From
Noel Klingler at NASA-GSFC / UMBC <njk5441@psu.edu>
N. J. Klingler (GSFC/UMBC/CRESTII) and A. D'Ai (INAF-IASFPA)
report on behalf of the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 220711B
114 s after the BAT trigger (D'Ai et al., GCN Circ. 32366).
No optical afterglow consistent with the XRT position
(Beardmore et al. GCN Circ. 32370)
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 114 264 147 >21.0
u_FC 326 576 246 >20.2
white 114 915 221 >21.0
v 655 4601 236 >19.7
b 581 773 39 >19.7
u 326 5120 368 >20.4
w1 704 5011 216 >20.5
m2 852 4806 216 >19.4
w2 631 4396 216 >20.4
The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.067 in the direction of the burst
(Schlegel et al. 1998).
GCN Circular 32370
Subject
GRB 220711B: Enhanced Swift-XRT position
Date
2022-07-12T02:09:51Z (3 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
A.P. Beardmore, P.A. Evans, M.R. Goad and J.P. Osborne (U. Leicester)
report on behalf of the Swift-XRT team.
Using 3094 s of XRT Photon Counting mode data and 7 UVOT
images for GRB 220711B, 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 = 262.01900, +24.68096 which is equivalent
to:
RA (J2000): 17h 28m 4.56s
Dec (J2000): +24d 40' 51.5"
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 32369
Subject
GRB 220711B: Fermi GBM Detection
Date
2022-07-12T00:49:33Z (3 years ago)
From
Stephen Lesage at Fermi-GBM Team <sjl0014@uah.edu>
S. Lesage (UAH) and C. Meegan (UAH) report on behalf of
the Fermi Gamma-ray Burst Monitor Team:
"At 18:16:28.06 UT on 11 July 2022, the Fermi Gamma-ray Burst Monitor (GBM)
triggered and located GRB 220711B (trigger 679256193/220711761)
which was also detected by Swift-BAT (A. D'Ai et al. 2022, GCN 32366).
The Fermi GBM Final Real-time Localization (GCN 32365) is consistent
with the Swift-BAT position.
The angle from the Fermi LAT boresight is 101 degrees.
The GBM light curve consists of a multipeaked emission episode with a
duration (T90)
of about 82 s (10-1000 keV). The time-averaged spectrum
from T0-40 to T0+61 s is best fit by
a power law function with an exponential high-energy cutoff.
The power law index is -1.39 +/- 0.07 and the cutoff energy,
parameterized as Epeak, is 81 +/- 6 keV.
The event fluence (10-1000 keV) in this time interval is
(1.02 +/- 0.04)E-05 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+0.4 s in the 10-1000 keV band is 6.0 +/- 0.4 ph/s/cm^2.
A Band function fits the spectrum equally well
with Epeak= 79 +/- 8 keV, alpha = -1.37 +/- 0.09 and beta = -2.93 +/- 0.71.
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 32368
Subject
GRB 220711B: NOT optical observations
Date
2022-07-11T23:20:15Z (3 years ago)
From
Daniele B Malesani at Radboud U <d.malesani@astro.ru.nl>
D. B. Malesani (Radboud Univ. and DAWN/NBI), D. Alexander Kann
(IAA/CSIC), S. D. Vergani (CNRS - Paris Obs./GEPI), L. Izzo (DARK/NBI),
O. Durfeldt Pedros (NOT and DTU Space), and T. Pursimo (NOT), report on
behalf of a larger collaboration:
We observed the field of GRB 220711B (D'Ai et al., GCN 32366) with the
Nordic Optical Telescope (NOT) equipped with the ALFOSC imager.
Observations started in twilight in the r band, so that the first images
are not especially deep. A further set of five 200-s z-band images
started on 2022 Jul 11.90 UT (3.23 hr after the trigger).
Close to the currently available XRT position, we see three sources in
the stack of the z-band images (astrometry and photometry are calibrated
against the Gaia and Pan-STARRS catalogs, respectively):
1)
RA = 17:28:04.49
Dec = +24:40:50.8
z = 21.78 +- 0.13 AB
2)
RA = 17:28:04.44
Dec = +24:40:46.7
z = 22.09 +- 0.15 AB
3)
RA = 17:28:04.97
Dec = +24:40:44.7
z = 22.60 +- 0.19 AB
Sources 2) and 3) are visible in archival images from the Pan-STARRS
survey, while source 1) is not, which makes it a viable afterglow
candidate. However, sources 1), and 2) are slightly outside (5.6" and
5.7" away) the currently available (unenhanced) XRT position (which has
a 3.6" 90% error radius).
Sources 2) and 3) are also detected in our NOT r-band images, while
source 1) is not.
The relation of these sources to GRB 220711B is still under
investigation. Further NOT observations are planned.
GCN Circular 32367
Subject
GRB 220711B: LCO Optical Upper Limits
Date
2022-07-11T22:19:28Z (3 years ago)
From
Robert Strausbaugh at U. of the Virgin Islands <robert.strausbaugh@uvi.edu>
R. Strausbaugh (U. of the Virgin Islands), A. Cucchiara (College of Marin) report on behalf of a larger collaboration:
We observed the Fermi/Swift GRB 220711B (Fermi GBM Team, GCN 32365; D'Ai et al., GCN 32366) field with the Teide Observatory, Tenerife site, on July 11, from 21:05 to 21:23 (corresponding to 2.82 to 3.12 hours from the GRB trigger time) with the SDSS r and i filters.
We performed a series of 2x335s exposures in i and r bands. We do not detect an optical counterpart within the XRT error region (D'Ai et al., GCN 32366) in either band.
The following upper limits are calculated using the PanSTARRS catalog as reference:
r>21.54
i>21.34
These magnitudes are not corrected for galactic extinction.
R.S. is funded by NSF AST grant #1831682
GCN Circular 32366
Subject
GRB 220711B: Swift detection of a burst
Date
2022-07-11T18:36:05Z (3 years ago)
From
Jamie Kennea at Penn State U <jak51@psu.edu>
A. D'Ai (INAF-IASFPA), E. Ambrosi (INAF-IASFPA),
V. D'Elia (SSDC & INAF-OAR), J.D. Gropp (PSU), J. A. Kennea (PSU),
N. J. Klingler (GSFC/UMBC/CRESSTII), N. P. M. Kuin (UCL-MSSL),
A. Y. Lien (U Tampa), F. E. Marshall (NASA/GSFC),
K. L. Page (U Leicester) and A. Tohuvavohu (U Toronto) report on
behalf of the Neil Gehrels Swift Observatory Team:
At 18:16:28 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 220711B (trigger=1115766). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 261.993, +24.669 which is
RA(J2000) = 17h 27m 58s
Dec(J2000) = +24d 40' 10"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve showed a multi-peaked
structure with a duration of about 100 sec. The peak count rate
was ~2000 counts/sec (15-350 keV), at ~0 sec after the trigger.
The XRT began observing the field at 18:18:12.3 UT, 103.7 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source located at RA, Dec 262.02020,
24.67997 which is equivalent to:
RA(J2000) = 17h 28m 04.85s
Dec(J2000) = +24d 40' 47.9"
with an uncertainty of 3.6 arcseconds (radius, 90% containment). This
location is 97 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 in excess of the Galactic value (7.40 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 2
(+2.26/-2.02) x 10^21 cm^-2 (90% confidence).
UVOT took a finding chart exposure of 150 seconds with the White filter
starting 113 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
0.067.
Burst Advocate for this burst is A. D'Ai (antonino.dai AT inaf.it).
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 32365
Subject
GRB 220711B: Fermi GBM Final Real-time Localization
Date
2022-07-11T18:27:45Z (3 years ago)
From
Fermi GBM Team at MSFC/Fermi-GBM <do_not_reply@GIOC.nsstc.nasa.gov>
The Fermi GBM team reports the detection of a likely LONG GRB
At 18:16:28 UT on 11 Jul 2022, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 220711B (trigger 679256193.06458 / 220711761).
The on-ground calculated location, using the Fermi GBM trigger data, is RA = 267.8, Dec = 31.5 (J2000 degrees, equivalent to J2000 17h 51m, 31d 30'), with a statistical uncertainty of 4.6 degrees.
The angle from the Fermi LAT boresight is 109.0 degrees.
The skymap can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220711761/quicklook/glg_skymap_all_bn220711761.png
The HEALPix FITS file, including the estimated localization systematic, can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220711761/quicklook/glg_healpix_all_bn220711761.fit
The GBM light curve can be found here:
https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2022/bn220711761/quicklook/glg_lc_medres34_bn220711761.gif