GRB 221110A
GCN Circular 32925
Subject
GRB 221110A: Swift detection of a burst with an optical counterpart
Date
2022-11-10T02:57:59Z (3 years ago)
From
David Palmer at LANL <palmer@lanl.gov>
M. A. Williams (PSU), S. Dichiara (PSU), J. A. Kennea (PSU),
S. Laha (GSFC/UMBC), D. M. Palmer (LANL) and A. Tohuvavohu (U Toronto)
report on behalf of the Neil Gehrels Swift Observatory Team:
At 02:28:17 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 221110A (trigger=1136936). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 29.119, -27.314 which is
RA(J2000) = 01h 56m 29s
Dec(J2000) = -27d 18' 50"
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 about 10 sec. The peak count rate
was ~1400 counts/sec (15-350 keV), at ~0 sec after the trigger.
The XRT began observing the field at 02:29:32.8 UT, 75.3 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 29.09928, -27.29435 which
is equivalent to:
RA(J2000) = 01h 56m 23.83s
Dec(J2000) = -27d 17' 39.7"
with an uncertainty of 3.5 arcseconds (radius, 90% containment). This
location is 94 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 (1.46 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 4.2
(+3.14/-2.70) x 10^21 cm^-2 (90% confidence).
UVOT took a finding chart exposure of 150 seconds with the White filter
starting 80 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
RA(J2000) = 01:56:23.90 = 29.09958
DEC(J2000) = -27:17:36.9 = -27.29355
with a 90%-confidence error radius of about 0.5 arc sec. This position is 3.0
arc sec. from the center of the XRT error circle. The estimated magnitude is
18.62 with a 1-sigma error of about 0.07.
Burst Advocate for this burst is M. A. Williams (mjw6837 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 32926
Subject
GRB 221110A: LCOGT Optical Afterglow Detection
Date
2022-11-10T04:44:32Z (3 years ago)
From
Robert Strausbaugh at University of Minnesota <rstrausb@umn.edu>
R. Strausbaugh (University of Minnesota), A. Cucchiara (NASA) report on
behalf of a larger collaboration:
We observed the GRB 221110A (Williams et al., GCN 32925) field with the
LCOGT 1-meter Sinistro instrument at the Cerro Tololo Interamerican
Observatory, Chile site, on November 10, from 03:12 to 03:40 (corresponding
to 0.73 to 1.20 hours from the GRB trigger time) with the SDSS r and i
filters.
We performed a series of 3x300s exposures in each band. We detect an
uncataloged source in the Swift error region, in both bands, consistent
with the optical counterpart candidate (Lipunov et al., GCN 32924).
The following magnitudes are calculated using the Pan-STARRS catalog as
reference:
r = 19.45 +/- 0.06
i = 18.19 +/- 0.08
These magnitudes are not corrected for galactic extinction. Imaging and
spectroscopic follow-up has been conducted with Gemini and analysis is
ongoing.
GCN Circular 32927
Subject
GRB 221110A: COATLI Afterglow detection
Date
2022-11-10T04:49:36Z (3 years ago)
From
Emma Margarita Pereyra Talamantes at IA-UNAM Ensenada <mpereyra@astro.unam.mx>
*Margarita Pereyra (UNAM), Alan M. Watson (UNAM), Nat Butler (ASU), Rosa
Becerra (UNAM), Simone Dichiara (PSU), Tzveti Dimitrova (ASU), Oc��lotl
L��pez (UNAM), Diego Gonz��lez (UNAM), Alexander Kutyrev (GSFC), William H.
Lee (UNAM), Eleonora Troja (UTV/ASU) and report:We observed the field of
the GRB 221110A (Williams et al., GCN Circ. 32925) with the COATLI 50-cm
telescope and HUITZI f/8 imager at the Observatorio Astron��mico Nacional on
the Sierra de San Pedro M��rtir (http://coatli.astroscu.unam.mx
<http://coatli.astroscu.unam.mx/>) from 2022-11-10 03:26 UTC to 03:59 UTC
(0.96hrs to 1.5 hours after the trigger), obtaining a total of 29 minutes
of exposure in the r filter.At the position of the UVOT afterglow (Williams
et al., GCN Circ. 32925), we detect a source with the following magnitude
and 1-sigma uncertainty:r = 19.7 +/- 0.15Our photometry is calibrated
against the Pan-STARRS1 catalog, is on an approximate AB system, and is not
corrected for Galactic extinction in the direction of the GRB.Observations
and reductions will continue. Further observations are planned.We thank the
COATLI/HUITZI technical team and the staff of the Observatorio Astron��mico
Nacional.*
--
*Dr. Margarita Pereyra *
*FFTF, Schlumberger Foundation Alumnae*
----------------------------------------------------------------------------------------------------------------
*Catedr��tica Conacyt*
*Instituto de Astronom��a de la UNAM,*
*Km. 107 Carretera Tijua**na-Ensenada, *
*Ensenada Baja California, M��xico. C.P. 22860*
Oficina: 405
Skype: margarita-pereyra
GCN Circular 32928
Subject
GRB 221110A: VLT/X-shooter redshift
Date
2022-11-10T05:18:41Z (3 years ago)
From
Daniele B Malesani at Radboud U <d.malesani@astro.ru.nl>
L. Izzo (DARK/NBI), D. B. Malesani (Radboud Univ. and DAWN/NBI), S.
Vejlgaard Nielsen (DAWN/NBI), N. R. Tanvir (Univ. Leicester), J. P. U.
Fynbo (DAWN/NBI), D. Xu (NAOC) report on behalf of the Stargate
collabaration:
We observed the optical afterglow of GRB 221110A (Williams et al., GCN
32925; Lipunov et al., GCN 32924; Strausbaugh & Cucchiara, GCN 32926;
Pereyra et al., GCN 32927) using the ESO VLT UT3 (Melipal) equipped with
the X-shooter spectrograph. Our spectra cover the wavelength range
3000-25000 AA, and consist of 2 exposures by 600 s each. The observation
mid time was 2022 Nov 10.158 UT (1.33 hr after the GRB).
We clearly detect continuum over the wavelength range 6200-25000 AA. A
sharp break is visible around 6200 AA, which we identify as due to H I.
From detection of multiple absorption features, which we interpret as
due to Si IV, C IV, Fe II, O I, Si II, Al II, Al III, and many others,
we infer a redshift of z = 4.06. An intervening system is also detected
from Fe II and Mg II at z = 2.724.
We acknowledge excellent support from the ESO observing staff in
Paranal, in particular Michael Marsset and Florian Rodler.
GCN Circular 32929
Subject
GRB 221110A: Enhanced Swift-XRT position
Date
2022-11-10T06:08:06Z (3 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
P.A. Evans, M.R. Goad, J.P. Osborne and A.P. Beardmore (U. Leicester)
report on behalf of the Swift-XRT team.
Using 1662 s of XRT Photon Counting mode data and 4 UVOT
images for GRB 221110A, 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 = 29.09871, -27.29519 which is equivalent
to:
RA (J2000): 01h 56m 23.69s
Dec (J2000): -27d 17' 42.7"
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 32930
Subject
GRB 221110A: Swift-XRT refined Analysis
Date
2022-11-10T16:24:22Z (3 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
J. D. Gropp (PSU), S. Dichiara (PSU), J.A. Kennea (PSU), J.P. Osborne
(U. Leicester), K.L. Page (U. Leicester), A.P. Beardmore (U.
Leicester), B. Sbarufatti (INAF-OAB), A. D'Ai (INAF-IASFPA), A.
Melandri (INAF-OAB) and M.A. Williams report on behalf of the Swift-XRT
team:
We have analysed 6.4 ks of XRT data for GRB 221110A (Williams et al.
GCN Circ. 32925), from 64 s to 40.0 ks after the BAT trigger. The data
comprise 55 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 Evans et
al. (GCN Circ. 32929).
The light curve can be modelled with a power-law decay with a decay
index of alpha=0.971 (+0.028, -0.027).
A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.88 (+/-0.15). The
best-fitting absorption column is 8 (+14, -8) x 10^21 cm^-2, at a
redshift of 4.06, in addition to the Galactic value of 1.5 x 10^20
cm^-2 (Willingale et al. 2013). The counts to observed (unabsorbed)
0.3-10 keV flux conversion factor deduced from this spectrum is 3.4 x
10^-11 (3.6 x 10^-11) erg cm^-2 count^-1.
A summary of the PC-mode spectrum is thus:
Galactic foreground: 1.5 x 10^20 cm^-2
Intrinsic column: 8 (+14, -8) x 10^21 cm^-2 at z=4.06
Photon index: 1.88 (+/-0.15)
If the light curve continues to decay with a power-law decay index of
0.971, the count rate at T+24 hours will be 9.2 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.1 x
10^-13 (3.3 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/01136936.
This circular is an official product of the Swift-XRT team.
GCN Circular 32931
Subject
GRB 221110A: Swift-BAT refined analysis
Date
2022-11-10T18:59:32Z (3 years ago)
From
Amy Lien at GSFC <amy.y.lien@nasa.gov>
T. Parsotan (GSFC/UMBC), S. D. Barthelmy (GSFC),
H. A. Krimm (NSF), S. Laha (GSFC/UMBC),
A. Y. Lien (U Tampa), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (AGU),
M. Stamatikos (OSU), M. A. Williams (PSU)
(i.e. the Swift-BAT team):
Using the data set from T-240 to T+600 sec from the recent telemetry
downlink, we report further analysis of BAT GRB 221110A (trigger #1136936)
(Williams et al., GCN Circ. 32925). The BAT ground-calculated position is
RA, Dec = 29.106, -27.298 deg which is
RA(J2000) = 01h 56m 25.5s
Dec(J2000) = -27d 17' 51.4"
with an uncertainty of 1.5 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 75%.
The mask-weighted light curve shows a single-pulse structure
that starts at ~T0, peaks at ~T+1 s, and ends at ~T+10 s.
T90 (15-350 keV) is 8.98 +- 2.11 sec (estimated error including
systematics).
The time-averaged spectrum from T-0.41 to T+9.74 sec is best fit
by a simple power-law model. The power law index of the time-averaged
spectrum is 1.41 +- 0.16. The fluence in the 15-150 keV band
is 5.1 +- 0.5 x 10^-7 erg/cm2. The 1-sec peak photon flux measured
from T+0.52 sec in the 15-150 keV band is 1.1 +- 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/1136936/BA/
GCN Circular 32932
Subject
GRB 221110A: Swift/UVOT Detection and Corrected UVOT Position
Date
2022-11-11T04:27:28Z (3 years ago)
From
Sam LaPorte at PSU <sjl5346@psu.edu>
GRB 221110A: Swift/UVOT Detection and Corrected UVOT Position
S. J. LaPorte (PSU) and M. Williams (PSU)
report on behalf of the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 221110A
83 s after the BAT trigger (Williams et al., GCN Circ. 32925).
A fading source is detected at
RA (J2000) = 01:56:23.72 = 29.09882
Dec (J2000): = -27:17:45.09 = -27.29586
which is consistent with the XRT position (Evans et al. GCN Circ. 32929).
The UVOT position reported in the initial detection circular
(Williams et al., GCN Circ. 32925)
was incorrect, and differs from the updated position presented here by 8.45
arcsec.
We apologize for any inconvenience this discrepancy may cause.
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
b 3773 3973 196 >19.91
m2 4593 4793 196 >19.35
u 326 439 110 >19.33
v 4357 4557 197 >19.5
w1 4798 4998 196 >19.48
w2 4184 4383 196 >19.55
white_FC 114 264 147 18.68+-0.08
white 3978 4178 196 >20.66
The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.013 in the direction of the burst
(Schlegel et al. 1998).
GCN Circular 32933
Subject
GRB 221110A: GMG upper limit
Date
2022-11-11T11:22:24Z (3 years ago)
From
Jirong Mao at Yunnan Obs <jirongmao_obs@ynao.ac.cn>
J. Mao, J.-J. Zhang, and J.-M. Bai (YNAO) report:We observed the field of GRB 221110A (Williams et al. GCN 32925) by the GMG telescope in Yunnan observatories.The observation began from UT 17:06:28 Nov 10, 2022, about 15 hours from the trigger. We could not observe the opticalafterglow down to a magnitude limit of r~20.8.
GCN Circular 32935
Subject
GRB 221110A: COATLI Second-Epoch Upper Limits
Date
2022-11-11T21:03:17Z (3 years ago)
From
Alan M Watson at UNAM <alan@astro.unam.mx>
Alan M. Watson (UNAM), Nat Butler (ASU), Rosa Becerra (UNAM), Simone
Dichiara (PSU), Tzveti Dimitrova (ASU), Oc��lotl L��pez (UNAM), Diego
Gonz��lez (UNAM), Alexander Kutyrev (GSFC), William H. Lee (UNAM), Margarita
Pereyra (UNAM), and Eleonora Troja (UTV/ASU) report:
We observed the field of the GRB 221110A (Williams et al., GCN Circ. 32925)
with the COATLI 50-cm telescope and HUITZI f/8 imager at the Observatorio
Astron��mico Nacional on the Sierra de San Pedro M��rtir (
http://coatli.astroscu.unam.mx) from 2022-11-11 03:28 UTC to 09:01 UTC
(25.0 to 30.6 hours after the trigger), obtaining a total of 270 minutes of
exposure in the r filter.
The source detected in our earlier observations (Pereyra et al., GCN Circ.
32927 has now faded and is not detected to a 3-sigma limit of
r > 22.6
Our photometry is calibrated against the Pan-STARRS1 catalog, is on an
approximate AB system, and is not corrected for Galactic extinction in the
direction of the GRB.
We thank the COATLI/HUITZI technical team and the staff of the Observatorio
Astron��mico Nacional.
GCN Circular 32939
Subject
GRB 221110A: GRANDMA observations
Date
2022-11-15T13:57:43Z (3 years ago)
From
Iara Tosta e Melo at INFN <tostaemelo@lns.infn.it>
Content:
M. Coughlin (UMN), E. Gurbanov (ShAO), F. Navarete (SOAR/NOIRLab),
N. Kochiashvili (AbAO), M. Masek (FZU), Y. Rajabov (UBAI),
T. Sadibekova (AIM-CEA), M. Freeberg (KNC), A. Klotz (OMP/IRAP),
M. Boer, A. de Ugarte Postigo, S. Antier (OCA/Artemis), D. Turpin (CEA),
R.W. Kiendrebeogo (OCA/Artemis, LPCE/UJKZ), I. Tosta e Melo (INFN-LNS),
M. Lamoureux, K. Kruiswijk (UCLouvain), J.-G. Ducoin (IAP),
C. Rinner, Z. Benkhaldoun (OUCA), J. Ali, A. Kaouech (OUCA/KNC),
A. M. Fouad, A. Takey, A. Hamed, M. Abdel-Sabour, A. Shokry,
M. Soliman (NRIAG), X. F. Wang (THU/BJP), J. Zhu (BJP), X. Y. Zeng
(CGTU),
L. T. Wang, A. Iskandar (XAO), K. Smith (UVI), P. Gokuldass (Florida
Tech)
N. Orange (OrangeWave Innovative Science, LLC), T. Hussenot (IJCLab),
A. M. Fouad (NRIAG), A. Takey(NRIAG), H. A. Ismail, M. Abdel-Sabour
(NRIAG),
D. A. Kann (Goethe Univ.) report on behalf of the GRANDMA collaboration:
The GRANDMA telescope network responded to the Swift-BAT alert of
GRB 221110A (M. A. Williams et al., GCN 32925, P.A. Evans et al. GCN
32929)
detected at 02:28:17.62 UT. An afterglow was immediately detected by
UVOT with
the estimated magnitude of 18.62 with a 1-sigma error of ~0.07 at XRT
(not refined) position RA, Dec: 29.09928, -27.29435. The VLT/X-shooter
spectroscopic observations (L. Izzo et al., GCN 32928) reported a high-z
candidate at z=4.06.
The first GRANDMA observations started 40 s after the BAT trigger time
with TCH telescope at La Silla, Chile.
Below, we report selected observations. We also report our 5-sigma upper
limits. Magnitudes are given in the AB system.
T-T0(hr)| MJD | Obser. | Exposure | Filter | Mag +/- err|Upp.Lim
_______________________________________________________________________________
0.06 |59893.105660| TCH | 5x30s | clear | 15.9+/-0.1 | 17.2
3.3 |59893.242788| SOAR | 1x300s | sdssr | 21.7+/-0.2 | -
3.3 |59893.246601| SOAR | 1x300s | sdssi | 19.8+/-0.1 | -
3.3 |59893.238496| SOAR | 1x300s | sdssz | 19.4+/-0.2 | -
8.1 |59893.440510| KNC-SSO | 5x300s | Ic | - | 19.0
17.6 |59893.835694| KAO | 10x250s | sdssz | - | 19.9
18.7 |59893.881065| KNC-HAO | 20x180s | R | - | 19.8
19.3 |59893.905405| MOSS | 60x60s | clear | - | 20.4
25.1 |59894.149306| VIRT | 400x10s | R | - | 20.1
These observations are consistent with previous reports by LCOGT
(R. Strausbaugh et al GCN 32926) and COATLI (M. Pereyra et al. GCN
32927).
TCH and MOSS data have been calibrated using nearby
stars from the Pan-STARRS catalogue in sdss-r measured with
STDpipe (Karpov 2022).
KNC-HAO data have been calibrated with respect to
field stars from the Pan-STARRS and APASS catalogues, using the MUPHOTEN
pipeline (Duverne et al. 2022).
The upper limit derived for KAO data was defined with the faintest
detected
star in the field and the images were processed with IRAF.
SOAR used the "Goodman Spectroscopic Pipeline" for imaging processing
and IRAF for getting the astrometric solution. The photometric
calibration
was done by comparison with SkyMapper sources in the field in SDSS.
The images of iTelescope 32 (Siding Spring Observatory, Australia)
have been processed using the STDpipe and photometry was performed
using field stars from the PanSTARRS1-i catalogue as a reference.
VIRT data was processed with the in-house pipeline which uses the
USNO.B1 catalogue.
The nearly full Moon contaminated the observations.
GRANDMA is a worldwide telescope network (grandma.ijclab.in2p3.fr)
devoted to the observation of transients in the context of
multi-messenger
astrophysics (Antier et al. 2020 MNRAS 497, 5518). Kilonova-Catcher
(KNC) is
the citizen science program of GRANDMA
(http://kilonovacatcher.in2p3.fr/).