- GCN/BACODINE POSITION NOTICE
TITLE: GCN/SWIFT NOTICE
NOTICE_DATE: Fri 17 Nov 23 03:03:41 UT
NOTICE_TYPE: Swift-BAT GRB Position
TRIGGER_NUM: 1197027, Seg_Num: 0
GRB_RA: 332.409d {+22h 09m 38s} (J2000),
332.701d {+22h 10m 48s} (current),
331.800d {+22h 07m 12s} (1950)
GRB_DEC: +13.514d {+13d 30' 49"} (J2000),
+13.632d {+13d 37' 54"} (current),
+13.268d {+13d 16' 03"} (1950)
GRB_ERROR: 3.00 [arcmin radius, statistical only]
GRB_INTEN: 8892 [cnts] Image_Peak=1824 [image_cnts]
TRIGGER_DUR: 0.128 [sec]
TRIGGER_INDEX: 122 E_range: 25-100 keV
BKG_INTEN: 15265 [cnts]
BKG_TIME: 10983.61 SOD {03:03:03.61} UT
BKG_DUR: 8 [sec]
GRB_DATE: 20265 TJD; 321 DOY; 23/11/17
GRB_TIME: 10999.68 SOD {03:03:19.68} UT
GRB_PHI: -178.22 [deg]
GRB_THETA: 28.79 [deg]
SOLN_STATUS: 0x20000003
RATE_SIGNIF: 255.99 [sigma]
IMAGE_SIGNIF: 24.19 [sigma]
MERIT_PARAMS: +1 +0 +0 -3 +2 +8 +0 +0 +24 +0
SUN_POSTN: 232.13d {+15h 28m 31s} -18.89d {-18d 53' 25"}
SUN_DIST: 104.18 [deg] Sun_angle= -6.7 [hr] (East of Sun)
MOON_POSTN: 282.62d {+18h 50m 29s} -28.01d {-28d 00' 37"}
MOON_DIST: 63.90 [deg]
MOON_ILLUM: 16 [%]
GAL_COORDS: 73.78,-33.50 [deg] galactic lon,lat of the burst (or transient)
ECL_COORDS: 339.62, 23.17 [deg] ecliptic lon,lat of the burst (or transient)
COMMENTS: SWIFT-BAT GRB Coordinates.
COMMENTS: This is a rate trigger.
COMMENTS: A point_source was found.
COMMENTS: This does not match any source in the on-board catalog.
COMMENTS: This does not match any source in the ground catalog.
COMMENTS: This is a GRB.
COMMENTS: This trigger occurred at longitude,latitude = 204.36,15.16 [deg].
COMMENTS:
COMMENTS: NOTE: This BAT event is temporally(0.0<100sec) coincident with the CALET_GBM event (trignum=1384225326).
- red DSS finding chart
ps-file
- GCN NOTICE
TITLE: GCN/SWIFT NOTICE
NOTICE_DATE: Fri 17 Nov 23 03:05:09 UT
NOTICE_TYPE: Swift-XRT Nack-Position
TRIGGER_NUM: 1197027, Seg_Num: 0
POINT_RA: 332.419d {+22h 09m 41s} (J2000)
POINT_DEC: +13.506d {+13d 30' 20"} (J2000)
IMG_START_DATE: 20265 TJD; 321 DOY; 23/11/17
IMG_START_TIME: 11101.52 SOD {03:05:01.52} UT, 101.8 [sec] since BAT Trigger Time
COUNTS: 5 Min_needed= 20
STD_DEV: 0.00 Max_StdDev_for_Good=28.44 [arcsec]
PH2_ITER: 1 Max_iter_allowed= 4
ERROR_CODE: 1
COMMENTS: SWIFT-XRT Nack Position.
COMMENTS: No source found in the image.
- GCN NOTICE
TITLE: GCN/SWIFT NOTICE
NOTICE_DATE: Fri 17 Nov 23 03:06:57 UT
NOTICE_TYPE: Swift-BAT GRB Lightcurve
TRIGGER_NUM: 1197027, Seg_Num: 0
GRB_RA: 332.409d {+22h 09m 38s} (J2000),
332.701d {+22h 10m 48s} (current),
331.800d {+22h 07m 12s} (1950)
GRB_DEC: +13.514d {+13d 30' 49"} (J2000),
+13.632d {+13d 37' 54"} (current),
+13.268d {+13d 16' 03"} (1950)
GRB_DATE: 20265 TJD; 321 DOY; 23/11/17
GRB_TIME: 10999.68 SOD {03:03:19.68} UT
TRIGGER_INDEX: 122
GRB_PHI: -178.22 [deg]
GRB_THETA: 28.79 [deg]
DELTA_TIME: -5.00 [sec]
TRIGGER_DUR: 0.128 [sec]
SOLN_STATUS: 0x3
RATE_SIGNIF: 255.99 [sigma]
IMAGE_SIGNIF: 24.19 [sigma]
LC_URL: sw01197027000msb.lc
SUN_POSTN: 232.13d {+15h 28m 32s} -18.89d {-18d 53' 27"}
SUN_DIST: 104.18 [deg] Sun_angle= -6.7 [hr] (East of Sun)
MOON_POSTN: 282.66d {+18h 50m 38s} -28.01d {-28d 00' 30"}
MOON_DIST: 63.87 [deg]
MOON_ILLUM: 16 [%]
GAL_COORDS: 73.78,-33.50 [deg] galactic lon,lat of the burst (or transient)
ECL_COORDS: 339.62, 23.17 [deg] ecliptic lon,lat of the burst (or transient)
COMMENTS: SWIFT-BAT GRB Lightcurve.
COMMENTS:
COMMENTS: The next comments were copied from the BAT_POS Notice:
COMMENTS: This is a rate trigger.
COMMENTS: A point_source was found.
COMMENTS: This does not match any source in the on-board catalog.
COMMENTS: This does not match any source in the ground catalog.
COMMENTS: This is a GRB.
COMMENTS: This trigger occurred at longitude,latitude = 204.36,15.16 [deg].
- GCN NOTICE
TITLE: GCN/SWIFT NOTICE
NOTICE_DATE: Fri 17 Nov 23 03:08:00 UT
NOTICE_TYPE: Swift-UVOT Source List
TRIGGER_NUM: 1197027, Seg_Num: 0
POINT_RA: 332.418d {+22h 09m 40s} (J2000)
POINT_DEC: +13.506d {+13d 30' 21"} (J2000)
POINT_ROLL: 253.537d
IMG_START_DATE: 20265 TJD; 321 DOY; 23/11/17
IMG_START_TIME: 11105.63 SOD {03:05:05.63} UT, 105.9 [sec] since BAT Trigger Time
FILTER: 10, White
BKG_MEAN: 2.142
N_STARS: 34
X_OFFSET: 548 [pixels]
Y_OFFSET: 587 [pixels]
X_MAX: 1507 [pixels]
Y_MAX: 1546 [pixels]
DET_THRESH: 12
PHOTO_THRESH: 6
SL_URL: sw01197027000msufc0105.fits
SUN_POSTN: 232.13d {+15h 28m 32s} -18.89d {-18d 53' 28"}
SUN_DIST: 104.18 [deg] Sun_angle= -6.7 [hr] (East of Sun)
MOON_POSTN: 282.67d {+18h 50m 41s} -28.01d {-28d 00' 27"}
MOON_DIST: 63.87 [deg]
MOON_ILLUM: 16 [%]
GAL_COORDS: 73.78,-33.51 [deg] galactic lon,lat of the pointing direction
ECL_COORDS: 339.62, 23.16 [deg] ecliptic lon,lat of the pointing direction
COMMENTS: SWIFT-UVOT Source List.
- GCN NOTICE
TITLE: GCN/SWIFT NOTICE
NOTICE_DATE: Fri 17 Nov 23 03:08:14 UT
NOTICE_TYPE: Swift-UVOT Processed Source List
TRIGGER_NUM: 1197027, Seg_Num: 0
POINT_RA: 332.418d {+22h 09m 40s} (J2000)
POINT_DEC: +13.506d {+13d 30' 21"} (J2000)
POINT_ROLL: 253.537d
IMG_START_DATE: 20265 TJD; 321 DOY; 23/11/17
IMG_START_TIME: 11105.63 SOD {03:05:05.63} UT, 105.9 [sec] since BAT Trigger Time
FILTER: 10, White
BKG_MEAN: 2.142
N_STARS: 34
X_OFFSET: 548 [pixels]
Y_OFFSET: 587 [pixels]
X_MAX: 1507 [pixels]
Y_MAX: 1546 [pixels]
DET_THRESH: 12
PHOTO_THRESH: 6
SL_URL: sw01197027000msufc0105.fits
SUN_POSTN: 232.13d {+15h 28m 32s} -18.89d {-18d 53' 28"}
SUN_DIST: 104.18 [deg] Sun_angle= -6.7 [hr] (East of Sun)
MOON_POSTN: 282.67d {+18h 50m 41s} -28.01d {-28d 00' 27"}
MOON_DIST: 63.86 [deg]
MOON_ILLUM: 16 [%]
GAL_COORDS: 73.78,-33.51 [deg] galactic lon,lat of the pointing direction
ECL_COORDS: 339.62, 23.16 [deg] ecliptic lon,lat of the pointing direction
COMMENTS: SWIFT-UVOT Processed Source List.
COMMENTS: If you have elected to receive attachments:
COMMENTS: The uvot_catalog_srclist.fits.gz file does not exist; skipping the attachment.
- GCN NOTICE
TITLE: GCN/SWIFT NOTICE
NOTICE_DATE: Fri 17 Nov 23 03:10:00 UT
NOTICE_TYPE: Swift-UVOT Image
TRIGGER_NUM: 1197027, Seg_Num: 0
POINT_RA: 332.418d {+22h 09m 40s} (J2000)
POINT_DEC: +13.506d {+13d 30' 21"} (J2000)
ROLL: 253.537d
IMG_START_DATE: 20265 TJD; 321 DOY; 23/11/17
IMG_START_TIME: 11105.63 SOD {03:05:05.63} UT, 105.9 [sec] since BAT Trigger Time
FILTER: 10, White
EXPOSURE_ID: 721883138
X_OFFSET: 867 [pixels]
Y_OFFSET: 906 [pixels]
WIDTH: 160 [pixels]
HEIGHT: 160 [pixels]
X_GRB_POS: 1027
Y_GRB_POS: 1066
BINNING_INDEX: 1
IM_URL: sw01197027000msuni0138.fits
SUN_POSTN: 232.14d {+15h 28m 32s} -18.89d {-18d 53' 29"}
SUN_DIST: 104.18 [deg] Sun_angle= -6.7 [hr] (East of Sun)
MOON_POSTN: 282.69d {+18h 50m 46s} -28.01d {-28d 00' 23"}
MOON_DIST: 63.85 [deg]
MOON_ILLUM: 16 [%]
GAL_COORDS: 73.78,-33.51 [deg] galactic lon,lat of the pointing direction
ECL_COORDS: 339.62, 23.16 [deg] ecliptic lon,lat of the pointing direction
COMMENTS: SWIFT-UVOT Image.
COMMENTS: The GRB Position came from the Window Position in the Mode Command.
COMMENTS: The image has 2x2 binning (compression).
COMMENTS: This notice was forced out after watchdog timer expiring -- most likely due to missing packet(s);
COMMENTS: as a consequence some of the fields may be incoorect (eg TRIGGER_NUM,RA,DEC).
- GCN NOTICE
TITLE: GCN/SWIFT NOTICE
NOTICE_DATE: Fri 17 Nov 23 03:10:14 UT
NOTICE_TYPE: Swift-UVOT Processed Image
TRIGGER_NUM: 1197027, Seg_Num: 0
POINT_RA: 332.418d {+22h 09m 40s} (J2000)
POINT_DEC: +13.506d {+13d 30' 21"} (J2000)
ROLL: 253.537d
IMG_START_DATE: 20265 TJD; 321 DOY; 23/11/17
IMG_START_TIME: 11105.63 SOD {03:05:05.63} UT, 105.9 [sec] since BAT Trigger Time
FILTER: 10, White
EXPOSURE_ID: 721883138
X_OFFSET: 867 [pixels]
Y_OFFSET: 906 [pixels]
WIDTH: 160 [pixels]
HEIGHT: 160 [pixels]
X_GRB_POS: 1027
Y_GRB_POS: 1066
BINNING_INDEX: 1
IM_URL: sw01197027000msuni0138.fits
SUN_POSTN: 232.14d {+15h 28m 33s} -18.89d {-18d 53' 29"}
SUN_DIST: 104.18 [deg] Sun_angle= -6.7 [hr] (East of Sun)
MOON_POSTN: 282.69d {+18h 50m 46s} -28.01d {-28d 00' 22"}
MOON_DIST: 63.85 [deg]
MOON_ILLUM: 16 [%]
GAL_COORDS: 73.78,-33.51 [deg] galactic lon,lat of the pointing direction
ECL_COORDS: 339.62, 23.16 [deg] ecliptic lon,lat of the pointing direction
COMMENTS: SWIFT-UVOT Processed Image.
COMMENTS: The GRB Position came from the Window Position in the Mode Command.
COMMENTS: The image has 2x2 binning (compression).
COMMENTS: If you have elected to receive attachments:
COMMENTS: The uvot_catalog_image.fits.gz file does not exist; skipping the attachment.
COMMENTS: This notice was forced out after watchdog timer expiring -- most likely due to missing packet(s);
COMMENTS: as a consequence some of the fields may be incoorect (eg TRIGGER_NUM,RA,DEC).
- GCN NOTICE
TITLE: GCN/SWIFT NOTICE
NOTICE_DATE: Fri 17 Nov 23 03:09:51 UT
NOTICE_TYPE: Swift-XRT Position
TRIGGER_NUM: 1197027, Seg_Num: 0
GRB_RA: 332.3914d {+22h 09m 33.93s} (J2000),
332.6825d {+22h 10m 43.80s} (current),
331.7819d {+22h 07m 07.66s} (1950)
GRB_DEC: +13.5232d {+13d 31' 23.5"} (J2000),
+13.6411d {+13d 38' 28.1"} (current),
+13.2772d {+13d 16' 37.8"} (1950)
GRB_ERROR: 4.3 [arcsec radius, statistical plus systematic, 90% containment]
GRB_INTEN: 1.00e-10 [erg/cm2/sec]
GRB_SIGNIF: 10.00 [sigma]
IMG_START_DATE: 20265 TJD; 321 DOY; 23/11/17
IMG_START_TIME: 11111.00 SOD {03:05:11.00} UT, 111.3 [sec] since BAT Trigger Time
TAM[0-3]: 100.00 100.00 100.00 100.00
AMPLIFIER: 1
WAVEFORM: 31
SUN_POSTN: 232.14d {+15h 28m 32s} -18.89d {-18d 53' 29"}
SUN_DIST: 104.16 [deg] Sun_angle= -6.7 [hr] (East of Sun)
MOON_POSTN: 282.69d {+18h 50m 45s} -28.01d {-28d 00' 23"}
MOON_DIST: 63.84 [deg]
MOON_ILLUM: 16 [%]
GAL_COORDS: 73.77,-33.48 [deg] galactic lon,lat of the burst
ECL_COORDS: 339.60, 23.19 [deg] ecliptic lon,lat of the burst
COMMENTS: SWIFT-XRT Coordinates.
COMMENTS: This Notice was ground-generated -- not flight-generated.
COMMENTS: TAM values, flux and significance fields are not valid.
COMMENTS: This position was automatically generated on the ground using
COMMENTS: Photon Counting data telemetered via TDRSS (SPER data).
COMMENTS: See http://www.swift.ac.uk/sper/docs.php for details.
COMMENTS: The probability that this is a serendipitous source in the
COMMENTS: SPER window is 0.58% < P(seren) < 1.1%.
- GCN Circular #35071
S. Laha (GSFC/UMBC), C. Gronwall (PSU), J.D. Gropp (PSU),
N. J. Klingler (GSFC/UMBC/CRESSTII), D. M. Palmer (LANL),
T. M. Parsotan (GSFC/UMBC/CRESSTII), C. Salvaggio (INAF-OAB) and
A. Tohuvavohu (U Toronto) report on behalf of the Neil Gehrels Swift
Observatory Team:
At 03:03:19 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 231117A (trigger=1197027). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 332.409, +13.514 which is
RA(J2000) = 22h 09m 38s
Dec(J2000) = +13d 30' 49"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve showed a single bright
peak structure with a duration of about 1.5 sec. The peak count rate
was ~80,000 counts/sec (15-350 keV), at ~0 sec after the trigger.
The XRT began observing the field at 03:05:01.5 UT, 101.8 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 332.39146, 13.52328 which is equivalent
to:
RA(J2000) = 22h 09m 33.95s
Dec(J2000) = +13d 31' 23.8"
with an uncertainty of 4.3 arcseconds (radius, 90% containment). This
location is 69 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. 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.
UVOT took a finding chart exposure of 150 seconds with the White filter
starting 105 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image processing
FAILED because of no aspect solution. Results from the list of sources
generated on-board are not available at this time. No correction has been made
for the expected extinction corresponding to E(B-V) of 0.071.
Burst Advocate for this burst is S. Laha (sib.laha AT gmail.com).
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 NOTICE
TITLE: GCN/SWIFT NOTICE
NOTICE_DATE: Fri 17 Nov 23 03:46:16 UT
NOTICE_TYPE: Swift-XRT Position UPDATE
TRIGGER_NUM: 1197027, Seg_Num: 0
GRB_RA: 332.3910d {+22h 09m 33.84s} (J2000),
332.6821d {+22h 10m 43.70s} (current),
331.7815d {+22h 07m 07.56s} (1950)
GRB_DEC: +13.5226d {+13d 31' 21.3"} (J2000),
+13.6405d {+13d 38' 25.9"} (current),
+13.2766d {+13d 16' 35.7"} (1950)
GRB_ERROR: 3.5 [arcsec radius, statistical plus systematic, 90% containment]
GRB_INTEN: 1.00e-10 [erg/cm2/sec]
GRB_SIGNIF: 10.00 [sigma]
IMG_START_DATE: 20265 TJD; 321 DOY; 23/11/17
IMG_START_TIME: 11111.00 SOD {03:05:11.00} UT, 111.3 [sec] since BAT Trigger Time
TAM[0-3]: 100.00 100.00 100.00 100.00
AMPLIFIER: 1
WAVEFORM: 31
SUN_POSTN: 232.16d {+15h 28m 39s} -18.90d {-18d 53' 52"}
SUN_DIST: 104.14 [deg] Sun_angle= -6.7 [hr] (East of Sun)
MOON_POSTN: 283.08d {+18h 52m 20s} -27.98d {-27d 59' 00"}
MOON_DIST: 63.54 [deg]
MOON_ILLUM: 16 [%]
GAL_COORDS: 73.77,-33.48 [deg] galactic lon,lat of the burst
ECL_COORDS: 339.60, 23.19 [deg] ecliptic lon,lat of the burst
COMMENTS: SWIFT-XRT Coordinates.
COMMENTS: This Notice was ground-generated -- not flight-generated.
COMMENTS: This is an Update Notice -- the RA,Dec values herein supersede the previous XRT_POS Notice.
COMMENTS: TAM values, flux and significance fields are not valid.
COMMENTS: This position was automatically generated on the ground using
COMMENTS: Photon Counting data telemetered via TDRSS (SPER data).
COMMENTS: See http://www.swift.ac.uk/sper/docs.php for details.
COMMENTS: The probability that this is a serendipitous source in the
COMMENTS: SPER window is 0.58% < P(seren) < 1.1%.
- GCN Circular #35072
P. K. Navaneeth (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 bright short duration GRB 231117A which was also detected by Swift-BAT (Laha et al., GCN Circ. 35071), and CALET (Trigger 1384225326).
The source was clearly detected in the CZT detectors in the 20-200 keV energy range. The light curve peaks at 2023-11-17 03:03:19.74 UTC. The measured peak count rate associated with the burst is 8467 (+1562, -767) counts/s above the background in the combined data of all quadrants, with a total of 1375 (+86, -77) counts. The local mean background count rate was 335 (+15, -38) counts/s. Using cumulative rates, we measure a T90 of 0.42 (+0.04, -0.06) s.
The source was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range. The light curve peaks at 2023-11-17 03:03:18.82 UTC. The measured peak count rate associated with the burst is 1496 (+86, -96) counts/s above the background in the combined data of all quadrants, with a total of 1883 (+307, -334) counts. The local mean background count rate was 1497 (+6, -7) counts/s. Due to the intrinsic 1 s binning of Veto data, we cannot reliably estimate a T90 from it.
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 #35073
B. Godson, K. Ackley, B. P. Gompertz, J. Lyman, M. Dyer, D. Steeghs, A. Kum=
ar, A. J. Levan, R. Starling, F. Jim=C3=A9nez-Ibarra, K. Ulaczyk, D. Gallow=
ay, V. Dhillon, P. O'Brien, G. Ramsay, K. Noysena, R. Kotak, R. Breton, L. =
Nuttall, E. Pall=C3=A9, D. Pollacco, T. Killestein and D. O'Neill report on=
behalf of the GOTO collaboration:
The Gravitational-wave Optical Transient Observer (GOTO, Steeghs et al. 202=
2) performed a targeted observation in response to GRB 231117A (Laha et al.=
, GCN 35071; Navaneeth et al, GCN 35072) at 10:00:02 UT on 2023-11-17, star=
ting approximately 7 hours after trigger. The observation consisted of a 4x=
90s exposure in the GOTO L-band (400-700 nm).
Images were processed immediately after acquisition using the GOTO pipeline.
No optical counterpart to the X-ray afterglow detected by Swift/XRT (Laha
et al., GCN 35071) is seen to a 3-sigma limit of L > 20.4 magnitudes (AB).
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 prin=
cipally 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 #35074
A.P. Beardmore, P.A. Evans, M.R. Goad and J.P. Osborne (U. Leicester)
report on behalf of the Swift-XRT team.
Using 2459 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 231117A, 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 = 332.38988, +13.52255 which is equivalent
to:
RA (J2000): 22h 09m 33.57s
Dec (J2000): +13d 31' 21.2"
with an uncertainty of 2.0 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 #35075
P.W. Cattaneo (INFN Pavia), F. Verrecchia (SSDC, and INAF/OAR),=C2=A0
F. Longo (Univ. Trieste, and INFN Trieste), C. Pittori (SSDC, and INAF/OAR),=C2=A0
C. Casentini (INAF/IAPS), M. Tavani (INAF/IAPS, and Univ. Roma Tor Vergata),
A. Argan, M. Cardillo, Y. Evangelista, L. Foffano, G. Piano (INAF/IAPS),
A. Addis, L. Baroncelli, A. Bulgarelli, A. Ciabattoni, A. Di Piano, V. Fior=
etti=C2=A0
(INAF/OAS-Bologna), G. Panebianco (Univ. Bologna - INAF/OAS Bologna),=C2=A0
N. Parmiggiani (INAF/OAS-Bologna), F. Lucarelli (SSDC, and INAF/OAR),
M. Marisaldi (INAF/OAS-Bologna, and Bergen University), M. Pilia, A. Trois
(INAF/OA-Cagliari), A. Ursi (ASI and INAF/IAPS), I. Donnarumma, E. Menegoni=C2=A0
(ASI), A. Giuliani (INAF/IASF-Mi), F. Cutrona (Univ. Milano Bicocca) and P.=C2=A0
Tempesta (TeleSpazio) report on behalf of the AGILE Team:
The AGILE satellite detected the short GRB 231117A at T0 =3D 2023-11-17
03:03:20.50 (UT) , reported by Swift (GCN #35071) and AstroSat (GCN #35072).
A preliminary analysis of the AGILE minicalorimeter (MCAL) triggered data
found a=C2=A0 burst at T_mcal =3D 2023-11-17 03:03:20 +/- 0.01 s (UTC).
The event lasted about 0.16 s and released a total number of 222 counts
in the detector (in the 0.4-100 MeV energy range), above an average
background rate of 364 counts/s.
The light curve can be found at:
http://www.agilescienceapp.it/notices/086277-086279_GRB_MCAL_627274999.673711.png.
The AGILE-MCAL detector is a CsI detector with a 4 pi FoV, sensitive in
the energy range 0.4-100 MeV. Additional analysis of AGILE data is in progress.
- GCN Circular #35076
H. Takei, N. Higuchi, I. Takahashi, M. Sasada, M. Niwano, S. Sato, S. Hayatsu, H. Seki, Y. Yatsu and N. Kawai (Tokyo Tech) report on behalf of the MITSuME collaboration:
We observed the field of GRB 231117A (Laha et al. GCN Circular #35071) with the optical three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm telescope Akeno.
The observation started at 2023-11-17 08:14:35 UT (5.19 hours after the Swift/BAT trigger). We stacked the images with good conditions. We did not detect any uncatalogued sources within the enhanced Swift/XRT error region (Beardmore et al. GCN Circular #35074). We obtained the 5-sigma limits of the stacked images as follows.
T0+[hour] | MID-UT | T-EXP[sec] | 5-sigma limits
------------------------------------------------------------------------------------------------
6.38 | 2023-11-17 09:25:57 | 5160 | g'>19.9, Rc>19.9, Ic>19.3
------------------------------------------------------------------------------------------------
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, Vol.73, Issue 1, Pages 4-24; https://github.com/MNiwano/Eclaire).
- GCN Circular #35079
D. Svinkin, D. Frederiks, A. Lysenko, A. Ridnaia,
Yu. Temiraev, A. Tsvetkova, M. Ulanov, and T. Cline,
on behalf of the Konus-Wind team, report:
The bright, short-duration GRB 231117A
(Swift-BAT detection: Laha et al., GCN Circ. 35071;
AstroSat-CZTI detection: Navaneeth et al., GCN Circ. 35072;
AGILE-MCAL detection: Cattaneo et al., GCN Circ. 35075)
triggered Konus-Wind at T0=10998.926 s UT (03:03:18.926).
The burst light curve shows a single pulse
which starts at ~T0 and has a total duration of ~0.7 s.
The emission is seen up to ~10 MeV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB231117_T10998/
As observed by Konus-Wind, the burst
had a fluence of 9.10(-0.94,+0.97)x10^-6 erg/cm2,
and a 16-ms peak flux, measured from T0+0.052 s,
of 5.88(-1.01,+1.03)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+0.256 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 = -1.15(-0.11,+0.13),
the high energy photon index beta = -2.81(-7.19,+0.43),
the peak energy Ep = 400(-82,+89) keV
(chi2 = 45/51 dof).
All the quoted errors are at the 90% confidence level.
All the quoted values are preliminary.
- GCN Circular #35080
J. H. Gillanders (Oxford), S. J. Smartt, S. Srivastav (Oxford/QUB), M. D. Fulton, K. W. Smith, A. Aamer, C. R. Angus, M. McCollum, T. Moore, M. Nicholl, X. Sheng, J. Weston, D. R. Young (QUB), P. Ramsden (QUB/Birmingham), L. Shingles (GSI/QUB), A. Andersson, S. Ramaiya, L. Rhodes, H. Stevance (Oxford), J. Sommer (LMU/QUB), L. Denneau, J. Tonry, H. Weiland, A. Lawrence, R. Siverd (IfA, University of Hawaii), N. Erasmus, W. Koorts (South African Astronomical Observatory), A. Jordan, V. Suc (UAI, Obstech), A. Rest (STScI), T.-W. Chen (NCU), C. Stubbs (Harvard).
Here we report optical observations in the field of the Swift-BAT discovered GRB 231117A (Laha et al. GCN Circ. 35071), obtained during normal survey operations with ATLAS.
ATLAS is a quadruple 0.5-m telescope system with two units in Hawaii, one in Chile and one in South Africa (see Tonry et al. 2018, PASP, 130:064505), routinely surveying the visible sky on a daily basis. We promptly process all data with our transient science server (Smith et al. 2020, PASP, 132:085002).
The ATLAS system observed the field of the GRB 231117A in normal survey mode 3.3-hr after the GRB trigger date of MJD 60265.127 (=2023-11-17 03:03:19 UT, hereafter T0). We obtained forced photometry at the enhanced Swift-XRT X-ray source coordinates of RA = 332.38988, Dec = +13.52255 (Beardmore et al. GCN Circ. 35074). We found no historical detections of any excess optical flux at this position, or at any location within the XRT and BAT error regions.
Forced photometry at those coordinates results in the following most recent non-detection in the ATLAS c-band. These measurements are not corrected for any Galactic dust extinction.
Exp. time (s) = 120 (4 x 30)
MJD = 60265.310 (T0 + 3.3-hr)
Flux (uJy) < 19 (3-sigma)
Mag (AB) > 20.7 (3-sigma)
- GCN Circular #35081
C.C. Cheung, M. Kerr, J. E. Grove, R. Woolf (NRL), A. Goldstein (USRA), C.A.
Wilson-Hodge (MSFC), and M.S. Briggs (UAH) report:
The Glowbug gamma-ray telescope [1,2], operating on the International Space=
Station, reports the detection of the short burst, GRB 231117A, which was =
also detected by Swift/BAT, AstroSat/CZTI, AGILE, and Konus/Wind (GCN 35071=
, 35072, 35075, 35079).=20
Using an adaptive window with a resolution of 32-ms, the burst onset is det=
ermined to be 2023-11-17 03:03:18.592 with a duration of 1.024 s and a tota=
l significance of about 124.0 sigma. The light curve comprises a single FRE=
D-shaped pulse.
Using a standard power-law function with an exponential high-energy cutoff =
[3] to model the emission over this duration results in a photon index dN/d=
E~E^x of x=3D0.2 and a cutoff energy ("Epeak") of 461 keV. The modeled 10-=
10000 keV fluence is 5.1e-06 erg/cm^2.
The analysis results presented here are preliminary and use a response func=
tion that lacks a detailed characterization of the surrounding passive stru=
cture of the ISS.
Glowbug is a NASA-funded technology demonstrator for sensitive, low-cost ga=
mma-ray transient telescopes developed, built, and operated by the U.S. Nav=
al Research Laboratory (NRL) with support from the University of Alabama in=
Huntsville, USRA, and NASA MSFC. It was launched on 2023 March 15 aboard =
the Department of Defense Space Test Program=E2=80=99s STP-H9 to the ISS. =
The detector comprises 12 large-area (15 cm x 15 cm) CsI:Tl panels covering=
the surface of a half cube, and two hexagonal (5-cm diameter, 10-cm length=
) CLLB scintillators, giving it a large field of view (instantaneous FoV ~2=
/3 sky) over a wide energy band of 50 keV to >2 MeV.
[1] Grove, J.E. et al. 2020, Proc. Yamada Conf. LXXI, arXiv:2009.11959
[2] Woolf, R.S. et al. 2022, Proc. SPIE, 12181, id. 121811O
[3] Goldstein, A. et al. 2020, ApJ 895, 40, arXiv :1909.03006
Distribution Statement A: Approved for public release. Distribution is unl=
imited.
- GCN Circular #35082
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-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 231117A ( S. Laha et al., GCN 35071) errorbox 44404 sec after notice time and 44429 sec after trigger time at 2023-11-17 15:23:48 UT, with upper limit up to 19.2 mag. The observations began at zenith distance = 29 deg. The sun altitude is -17.8 deg.
The galactic latitude b = -34 deg., longitude l = 74 deg.
Real time updated cover map and OT discovered available here:
https://master.sai.msu.ru/site/master2/observ.php?id=2307518
We obtain a following upper limits.
Tmid-T0 | Site |Filt.| Expt. | Limit| Comment
_________|_____________________|_____|_______|______|________
44519 | MASTER-Kislovodsk | C | 180 | 18.0 |
44519 | MASTER-Kislovodsk | C | 180 | 17.9 |
44920 | MASTER-Kislovodsk | C | 180 | 18.5 |
44920 | MASTER-Kislovodsk | C | 180 | 19.2 |
Filter C is a clear (unfiltred) band.
The observation and reduction will continue.
The message may be cited.
- GCN Circular #35083
S. Yang (HNAS), T.-W. Chen, C.-S. Lin, C.-C. Ngeow (NCUIA), Z.-N. Wang (HNA=
S), S. Smartt (Oxford/QUB), M. Fraser (UCD), J. Gillanders (Oxford), M.-H. =
Lee, Y.-C. Pan, H.-Y. Hsiao, W.-J. Hou, J.-K. Guo (NCUIA), M. Fulton, S. Sr=
ivastav, T. Moore, C. Angus, and A. Aamer (QUB) report:
We observed the field of GRB 231117A, a bright, short GRB discovered by the=
Swift BAT (Laha et al., GCN 35071). This burst is also detected by AstroSa=
t (Navaneeth et al., GCN 35072), AGILE (Cattaneo et al., GCN 35075), Konus-=
Wind (Svinkin et al., GCN 35079), and Glowbug (Cheung et al., GCN 35081).
We used the 40cm SLT at Lulin Observatory, Taiwan to obtain r-band images o=
f the field of GRB 231117A, as part of the Kinder collaboration (Chen et al=
., AstroNote 2021-92). The first SLT epoch of observations started at 10:26=
UT on 17 of November 2023 (MJD =3D 60265.435), 7.39 hours after the Swift =
trigger. The images were combined from 14 frames with a 300-second exposure=
time for the r band, taken under seeing conditions of an average of 1".93 =
and at a median airmass of 1.02. We then used the Lulin One-meter Telescope=
(LOT) to obtain g, r, i, and z-band images of this field starting on MJD =
=3D 60265.520, under seeing conditions of an average of 1".39 and at a medi=
an airmass of 1.21.
We found a GRB afterglow candidate at the position:
RA (J2000): 22h 09m 33.37s
Dec (J2000): +13d 31' 20.2=E2=80=9D
which is about 3" away from the enhanced Swift-XRT position (Beardmore et a=
l., GCN 35074). This afterglow condidate is right on the top of the faint g=
alaxy, SDSS J220933.34+133119.5, with a petroMag_r =3D 21.32 +/- 0.22 mag. =
The likely host galaxy has a SDSS photo-z of 0.481 +/- 0.103 and a Legacy S=
urvey photo-z of 0.342 +/- 0.131.
We used the Kinder pipeline (Yang et al. A&A 646, A22) to measure the PSF photometry of this afterglow candidate after template subtraction using the
SDSS images. We obtained the following magnitudes (in the AB system):
SLT r =3D 20.94 +/- 0.10 mag (exposure time of 300sec*14)
LOT g =3D 20.90 +/- 0.10 mag (300sec*1),
LOT r =3D 20.77 +/- 0.07 mag (300sec*7),
LOT i =3D 20.52 +/- 0.11 mag (300sec*1) and,
LOT z =3D 20.00 +/- 0.18 mag (SNR=3D2; 300sec*1).
The given limit is derived based on calibrating against SDSS field stars an=
d is not corrected for the expected Galactic foreground extinction correspo=
nding to a reddening of E_(B-V) =3D 0.06 mag in the direction of the burst =
(Schlafly & Finkbeiner 2011).
Our detection magnitudes are deeper than those non-detection reports from t=
he GOTO (Godson et al., GCN 35073), MITSuME (Takei et al., GCN 35076) and A=
TLAS (Gillanders et al., GCN 35080).
- GCN Circular #35084
M. Odeh (Al-Khatim Observatory, AKO, operated by the International
Astronomical Center in Abu Dhabi, UAE) and N. Guessoum and D. Akl (American
University of Sharjah, UAE) report:
We observed the field of GRB 231117A, which was detected by Swift/BAT,
AstroSat/CZTI, AGILE, and Konus/Wind (GCN 35071, 35072, 35075, 35079) with
our 0.36m f/7.7 robotic telescope on November 17 starting at: 14:46:29 UT
(corresponding to 11.72 hours from the GRB trigger time) using an (Ic)
filter. We obtained 33x180 second images.
We do not detect a source within the Swift-XRT error region around the
candidate X-ray source (Laha et al., GCN 35071). The following 5-sigma
upper limit is calculated using the ATLAS catalog as a reference:
Ic = 20.2.
We should note, however, that a star of Imag = 21.5 (AB) was barely
detected and is located at the position R.A. (2000) = 22 09 33.34, Dec.
(2000) = +13 31 19.44, that is about 2 arcseconds from the location of GRB
231117A, as per Pan-STARRS (PS1, ID = 124223323889577032).
- GCN Circular #35085
C. Casentini (INAF/IAPS), F. Verrecchia (SSDC, and INAF/OAR), P.W. Cattaneo (INFN Pavia), F. Longo (Univ. Trieste, and INFN Trieste), C. Pittori (SSDC, and INAF/OAR), M. Tavani (INAF/IAPS, and Univ. Roma Tor Vergata), A. Argan, M. Cardillo, Y. Evangelista, L. Foffano, G. Piano (INAF/IAPS), L. Baroncelli, A. Bulgarelli, A. Ciabattoni, A. Di Piano, V. Fioretti (INAF/OAS-Bologna), G. Panebianco (Univ. Bologna - INAF/OAS Bologna), N. Parmiggiani (INAF/OAS-Bologna), F. Lucarelli (SSDC, and INAF/OAR), M. Marisaldi (INAF/OAS-Bologna, and Bergen University), M. Pilia, A. Trois (INAF/OA-Cagliari), A. Ursi (ASI and INAF/IAPS), I. Donnarumma, E. Menegoni (ASI), A. Giuliani (INAF/IASF-Mi), F. Cutrona (Univ. Milano Bicocca) and P. Tempesta (TeleSpazio) report on behalf of the AGILE Team:
We carried out further analysis of the AGILE/MCAL data of GRB 231117A (GCNs #35071, #35072, #35073, #35074, #35075, #35076, #35079, #35080, #35081, #35082, #35083, #35084).
The burst released 415 counts in the detector in 0.14s, above a background rate of 532 Hz.
The spectral analysis shows a clear component up to 5 MeV.
The time-integrated spectrum of the burst can be fitted in the energy range 0.4-2.0 MeV with a power-law model with alpha = -2.3 (+/-0.2). The fit results in a reduced chi-squared of 1.204 (21 d.o.f.) and a fluence of 2.4e-06 erg/cm^2, in the energy range 0.4-10 MeV.
Additional analysis of AGILE data is in progress. Automatic MCAL GRB alert Notices can be found at:
https://gcn.gsfc.nasa.gov/agile_mcal.html.
- GCN Circular #35086
M.Ferro, R. Brivio, P. D'Avanzo, S. Covino, D. Fugazza (INAF-OAB) on behalf of the REM team, report:
We observed the field of GRB 231117A (Laha et al., GCN 35071) with the REM 60cm robotic telescope located at the ESO observatory of La Silla (Chile). The observations were carried in the g, r, i, z, J, H, K bands, starting on 2023 November 17 at 03:04:27 UT (i.e. 68 seconds after the burst) at airmass ~ 3, and lasting for about 2 hours.
From a preliminary analysis, we find no source at the enhanced XRT position (Beardmore et al., GCN 35074) at a mid time of t-t0 = 5.6 min, down to the following 3sigma magnitude upper limits:
r > 18.6
i > 17.9
z > 16.7
(AB; calibrated against the Pan-STARRS catalogue).
- GCN Circular #35087
J. C. Rastinejad, W. Fong, H. Sears (Northwestern), R. Chornock, W. Jacobso=
n-Galan (UC Berkeley), C. D. Kilpatrick (Northwestern), R. Margutti (UC Ber=
keley), G. Schroeder (Northwestern) et al. report:
''We observed the location of the bright short-duration GRB 231117A (Laha e=
t al., GCN 35071, Navaneeth et al., GCN 35072, Cattaneo et al., GCN 35075, =
Svinkin et al., GCN 35079, Cheung et al., GCN 35081) with the Low Resolutio=
n Imaging Spectrometer (LRIS) mounted on the Keck I 10-meter telescope on M=
auna Kea, Hawaii (PI Margutti). We obtain 6x150s of imaging in the g- and I=
-bands starting at 2023 Nov 17.096 UT (2.3 hr post-burst) at an airmass of =
1.02 in 0.8'' seeing and thin clouds.
We detect the archival source (SDSS J220933.34+133119.5, photo-z =3D 0.34-0=
.48) first noted by Yang et al. (GCN 35083). This source is on the outskirt=
s of the latest XRT position (Beardmore et al., GCN 35074). Calibrated to P=
an-STARRS, we measure g =3D 20.3 +/- 0.1 mag and I =3D 19.8 +/- 0.1 mag (AB=
system and not corrected for Galactic extinction). These magnitudes are ~1=
.3.-1.5 mag brighter than the Pan-STARRS catalog magnitudes for this source=
across both filters. Although visual inspection does not indicate a clear =
physical separation between an afterglow and the center of the host, we att=
ribute the clear brightening in flux to the optical afterglow, supporting t=
he afterglow candidate discovered by Yang et al., and an origin for this sh=
ort GRB at z~0.3-0.5.
Performing differential photometry relative to the Pan-STARRS catalog magni=
tudes results in an afterglow brightness of g~20.7 mag and I~20.1 mag at th=
e time of our Keck observations. At z=3D0.4, this translates to an optical =
luminosity of ~7e43 erg/s, consistent with optical afterglow luminosities a=
t similar rest-frame times. Taken at face value, our observations also indi=
cate a slow decline rate (Fopt ~ t^-0.2 - t^-0.3) compared to the Lulin Obs=
ervatory observations at 7.5 hr, although we caution that our preliminary a=
nalysis is only based on differential photometry and not image subtraction.
We encourage follow-up to determine the source=E2=80=99s redshift and confi=
rm the fading of the optical afterglow candidate."
- GCN Circular #35088
B. P. Gompertz (U. Birmingham) and K. Ackley (U. Warwick) report:
We observed the field of the short GRB 231117A (Laha et al., GCN 35071; Navaneeth et al., GCN 35072; Cattaneo et al., GCN 35075; Svinkin et al., GCN 35079; Cheung et al., GCN 35081) with the IO:O camera on the 2m robotic Liverpool Telescope. Observations began at 19:18:59 UT on 2023-11-17, ~16.3 hours after trigger, and consisted of 20x120s exposures in each of the SDSS r and i filters.
At the position of the optical counterpart reported by Yang et al. (GCN 35083) we detect a source with preliminary AB magnitudes of:
i = 20.10 +/- 0.03
r = 20.24 +/- 0.02
While these magnitudes include the contribution from the underlying galaxy, a comparison to the Keck observations taken ~14 hours prior (Rastinejad et al., GCN 35087) indicates fading at around the 3-sigma level. Combined with the significant excess above archival magnitudes, this supports the presence of the optical afterglow of GRB 231117A.
Analysis is ongoing. Reported magnitudes are not corrected for Galactic foreground extinction.
- GCN Circular #35089
R. Kumar, A. Salgundi, V. Swain, V. Bhalerao (IIT Bombay), G. C. Anupama, S. Barway (IIA), R. Norboo (IAO)
We observed the field of GRB 231117A detected by Swift (S. Laha et al., GCN 35071) with 0.7m GROWTH-India Telescope (GIT). We started the observation at 2023-11-17 13:36:59 UT, i.e., 10.56 hours after the Swift trigger. We obtained the multiple images of 300s each in the r' and g' band. We did not detect any source within the uncertainty radius of Swift-XRT position reported by A.P. Beardmore et al., GCN 35074 upto a limiting magnitude of 22.38 in r' band. We do detect the candidate optical afterglow in our subtracted image at the position reported by Yang et al. (GCN 35083). The photometry values are given below:
------------------------------------------------------------------------
| JD (mid) | t-t0 (days) | Filter | Exposure (s) | Magnitude (5 sigma) |
------------------------------------------------------------------------
| 2460266.072780335 | 0.445 | r' | 3 x 300 | 20.80 +/- 0.06 |
| 2460266.087725621 | 0.460 | r' | 3 x 300 | 21.18 +/- 0.08 |
| 2460266.098941961 | 0.471 | r' | 3 x 300 | 20.88 +/- 0.07 |
| 2460266.203419748 | 0.576 | r' | 3 x 300 | 20.84 +/- 0.07 |
| 2460266.253062681 | 0.625 | g' | 2 x 300 | 20.88 +/- 0.07 |
------------------------------------------------------------------------
Our data shows slight variability in the source, but no clear decay. The results are comparable to the values reported by B. P. Gompertz et al., GCN 35088; J. C. Rastinejad et al., GCN 35087; Yang et al., GCN 35083; and consistent with the upper limits given by M.Ferro et al., GCN 35086; M. Odeh et al., GCN 35084; J. H. Gillanders et al., GCN 35080; H. Takei., GCN 35076; B. Godson et al., GCN 35073. Based on these measurements, we conclude that this source is unlikely to be the afterglow. The magnitudes are calibrated against PanSTARRS DR1 (Chambers et al., 2016) and not corrected for Galactic extinction.
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 #35093
Tomas Ahumada, Yashvi Sharma(Caltech) on behalf of a larger collaboration:
We report optical spectroscopic observations of the candidate counterpart of the short GRB 231117A (GCN 35083, 35071) with the Low Resolution Imaging Spectrometer (LRIS, Oke et al. 95) at the Keck I Observatory (C358, PI: Kasliwal). Observations started 2023-11-18 05:19:00 (~1.1 days after the burst), and consisted of 2x900 exposures with the 400/3400 grism and 400/8500 grating.
The spectrum shows narrow galaxy lines at redshift of z = 0.257 (H, [O II], [O III], N II). We also see narrow absorption lines consistent with MgII(2796,2803) doublet at this redshift. We note the spectrum shows a blue continuum.
We thank Michael Lundquist and the Keck team for their support during this Target of Opportunity trigger.
The data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California and the National Aeronautics and Space Administration. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.
- GCN Circular #35095
M. Dafcikova, J. Ripa (Masaryk U.), A. Pal (Konkoly Observatory), N. Werner=
(Masaryk U.), M. Ohno, H. Takahashi (Hiroshima U.), L. Meszaros, B. Csak (=
Konkoly Observatory), N. Husarikova, F. Munz , M. Topinka, M. Kolar, J.-P. =
Breuer, F. Hroch (Masaryk U.), T. Urbanec, M. Kasal, A. Povalac (Brno U. o=
f Technology), J. Hudec, J. Kapus, M. Frajt (Spacemanic s.r.o), R. Laszlo, =
M. Koleda (Needronix s.r.o), M. Smelko, P. Hanak, P. Lipovsky (Technical U.=
of Kosice), G. Galgoczi (Wigner Research Center/Eotvos U.), Y. Uchida, H. =
Poon, H. Matake (Hiroshima U.), N. Uchida (ISAS/JAXA), T. Bozoki (Eotvos U.=
), G. Dalya (Eotvos U.), yyT. Enoto (Kyoto U.), Zs. Frei (Eotvos U.), G. Fr=
iss (Eotvos U.), Y. Fukazawa, K. Hirose (Hiroshima U.), S. Hisadomi (Nagoya=
U.), Y. Ichinohe (Rikkyo U.), K. Kapas (Eotvos U.), L. L. Kiss (Konkoly Ob=
servatory), T. Mizuno (Hiroshima U.), K. Nakazawa (Nagoya U.), H. Odaka (U=
niv of Tokyo), J. Takatsy (Eotvos U.), K. Torigoe (Hiroshima U.), N. Kogiso=
, M. Yoneyama (Osaka Metropolitan U.), M. Moritaki (U. Tokyo), T. Kano (U. =
Michigan) -- the GRBAlpha collaboration.
The short-duration GRB 231106B (Swift/BAT detection: GCN 35071; AstroSat de=
tection: GCN 35072; AGILE/MCAL detection: GCN 35075; Konus/Wind detection: =
GCN 35079; Glowbug detection: GCN 35081; CALET/CGBM detection: trigger no. =
1384225326) was observed by the GRBAlpha 1U CubeSat (Pal et al. 2023, A&A, =
677, 40; arXiv:2302.10048).
The detection was confirmed at the peak time 2023-11-17 03:03:19 UTC. The T=
90 duration measured by GRBAlpha is 1 s and the overall significance during=
T90 reaches 14 sigma.
The light curve obtained by GRBAlpha is available here: https://grbalpha.ko=
nkoly.hu/static/share/GRB231117A_GCN.pdf
All GRBAlpha detections are listed at: https://monoceros.physics.muni.cz/he=
a/GRBAlpha/=20
GRBAlpha, launched on 2021 March 22, is a demonstration mission for a futur=
e CubeSat constellation (Werner et al. Proc. SPIE 2018). The detector of GR=
BAlpha consists of a 75 x 75 x 5 mm3 CsI scintillator read out by a SiPM ar=
ray, covering the energy range from ~50 keV to ~1000 keV. To increase the d=
uty cycle and the downlink rate, the upgrade of the on-board data acquisiti=
on software stack is in progress. The ground segment is also supported by t=
he radio amateur community and it takes advantage of the SatNOGS network fo=
r increased data downlink volume.
- GCN Circular #35097
L. Rhodes (Oxford), G. E. Anderson (Curtin), A. J. van der Horst (GWU),J. K. Leung (UofT/HUJI), S. D. Ryder (Macquarie), A. Gulati (USyd), S. Chastain (UNM) on behalf of the PanRadio GRB collaboration
The Australia Telescope Compact Array (ATCA) observed short GRB 231117A (Laha et al., GCN 35071) as part of the Large ATCA "PanRadio GRB" follow-up programme C3542 (PI. Anderson) starting at 2023-11-17 04:00UT for 11hours.
We detect a radio source with a flux density of ~210uJy/beam at 9GHz at coordinates consistent with both those given by the XRT and the Lulin Observatory (A.P. Beardmore et al., GCN 35074; S. Yang et al., GCN 35083).
Further observations are planned.
We thank the CSIRO Space and Astronomy staff for supporting these observations.
We acknowledge the Gomeroi people as the traditional owners of the Observatory site. The Australia Telescope Compact Array is part of the Australia Telescope National Facility (https://ror.org/05qajvd42) which is funded by the Australian Government for operation as a National Facility managed by CSIRO.
- GCN Circular #35098
M. Gonzalez-Ba=C3=B1uelos, M. Kopsacheili (ICE), P. D'Avanzo (INAF-OAB), D.=
B. Malesani (DAWN/NBI and Radboud univ.), L. Galbany, T. M=C3=BCller-Bravo=
(ICE), C. Gutierrez (IEEC/ICE-CSIC), M. Dennefeld (IAP), A. Gkini (Stockh=
olm), N. Ihanec (Warsaw and ING), J. Anderson (ESO), T.-W. Chen (NCU), M. G=
romadzki (Warsaw), C. Inserra (Cardiff), E. Kankare (Turku), M. Nicholl (QU=
B), O. Yaron (Weizmann), D. Young (QUB), report on behalf of the ePESSTO+ c=
ollaboration:
We observed the candidate counterpart of the short GRB 231117A (Laha et al.=
, GCN Circ. 35071; Navaneeth et al., GCN Circ. 35072; Cattaneo et al., GCN =
Circ. 35075; Svinkin et al., Gin Circ. 35079; Cheung et al. GCN Circ. 35081=
; Dafcikova et al. GCN Circ. 35095) under the advanced Public ESO Spectrosc=
opic Survey for Transient Objects (ePESSTO+; see Smartt et al. 2015, A&A, 5=
79, 40; http://www.pessto.org). The observations were performed with the ES=
O New Technology Telescope (NTT) at La Silla equipped with the EFOSC2 instr=
ument in spectroscopic mode, starting on 2023 Nov 18 at 00:22:34 UT (i.e. 2=
1.3 hr after the burst) and using grism 13 (covering the wavelength range 3=
985-9315 AA).=20
The 1.5" slit was oriented in order to cover both the optical afterglow and=
the host galaxy candidate positions (Yang et al., GCN Circ. 35083; Rastine=
jad et al., GCN 35087; Gompertz & Ackley, GCN 35088). However, the observat=
ions were carried out under poor seeing conditions (1.7") and in the acquis=
ition image the two objects cannot be distinguished.
The spectrum shows prominebt emission features, which we identify as [O II], [O III] and Halpha at a common redshift z =3D 0.257, in agreement with the findings of Ahumada et al. (GCN Circ. 35093). No clear absorption features are detected.
- GCN Circular #35099
I. Andreoni (JSI/UMD/NASA-GSFC), G. Srinivasaragavan (UMD), B. O'Connor (CMU), T. Ahumada (Caltech), S. B. Cenko (NASA-GSFC), J. Durbak (UMD), E. Hammerstein (UMD), N. Klingler (UMBC/NASA-GSFC), A. Kutyrev (NASA-GSFC), L. Singer (NASA-GSFC), S. Veilleux (UMD):
We report target of opportunity follow-up observations of GRB 231117A (Laha et al., GCN 35071; Navaneeth et al., GCN 35072; Beardmore et al., GCN3574; Cattaneo et al., GCN 35075; Svinkin et al., GCN 35079; Cheung et al., GCN 35081, Dafcikova et al., GCN 53095) with the Large Monolithic Imager (LMI) mounted at the Lowell Discovery Telescope (LDT) located in Flagstaff, AZ, under program M01 (PI: Andreoni).
Observations started on 2023-11-18 at 01:46 UT (~22.7 hr after the GRB trigger). We obtained sets of 4x150s exposures for each g-r-i-z filter. The candidate afterglow identified by Yang et al.; GCN 35083 (also detected by Rastinejad et al., GCN 35087; Gompertz et al., GCN 35088; Kumar et al., GCN 35089, Ahumada et al., GCN 35093; Rhodes et al., GCN 35097) is well detected. Preliminary photometry of the images, with contribution from the host galaxy included and not corrected for Galactic extinction, was measured as follows in the AB magnitude system:
g = 20.55 +/- 0.04 mag
r = 20.20 +/- 0.04 mag
i = 20.05 +/- 0.04 mag
z = 19.98 +/- 0.03 mag
We thank Ben Shafransky and the Lowell Observatory staff for their support.
- GCN Circular #35102
C. D. Kilpatrick (Northwestern), L. Santana (CBPF), R. Salinas (ULS), C. Br=
ice=C3=B1o (NOIRLab/CTIO), C. Fuentes (PUC), C. Bom, A. Santos (CBPF) repor=
t on behalf of a larger collaboration:
=E2=80=9CWe observed the putative host galaxy of GRB 231117A (Laha et al., =
GCN 30571, Navaneeth et al., GCN 35072, Cattaneo et al., GCN 35075, Svinkin=
et al., GCN 35079, Cheung et al., GCN 35081, Odeh et al., GCN 35084, D'Ava=
nzo et al., GCN 35086, Rastinejad et al., GCN 35087, Gompertz et al., GCN 3=
5088) with the Goodman High-Throughput Spectrograph mounted on the SOAR 4m =
telescope on Cerro Pachon, Chile. We obtained 5x200s of imaging in r-band =
starting at 2023 Nov 18.03.
We detect a r=3D20.4+/-0.1 mag counterpart at the location of SDSS J220933.=
34+133119.5, consistent with the reported afterglow position reported by Ya=
ng et al. (GCN 35083) and subsequent detections of the putative afterglow (=
Rastinejad et al., GCN 35087, Gompertz & Ackley, GCN 35088, Kumar et al., G=
CN 35089, Andreoni et al., GCN 35099). These data are on the AB magnitude =
system and not corrected for Galactic extinction, however we caution that t=
hese data are preliminary and there is uncertain contribution from the host=
galaxy in our aperture. Additional SOAR follow up is planned.=E2=80=9D
- GCN Circular #35105
T.-W. Chen (NCUIA), S. Yang (HNAS), C.-S. Lin (NCUIA), S. Smartt (Oxford/QU=
B), M. Fraser (UCD), A.J. Levan (Radboud), M.-H. Lee, C.-C. Ngeow, Y.-C. Pa=
n, H.-Y. Hsiao, W.-J. Hou, J.-K. Guo (NCUIA), Z.-N. Wang (HNAS), J. Gilland=
ers (Oxford), M. Fulton, S. Srivastav, T. Moore, C. Angus, A. Aamer (QUB), =
and N. Tanvir (Leicester) report:
We observed the field of GRB 231117A (Laha et al., GCN 35071; Navaneeth et =
al., GCN 35072; Beardmore et al., GCN 35074; Cattaneo et al., GCN 35075; Sv=
inkin et al., GCN 35079; Cheung et al., GCN 35081; Dafcikova et al. GCN 350=
95).
The afterglow candidate was initially identified in our previous report (Ya=
ng et al., GCN 35083) . Since it is a real astrophysical transient, but not=
yet confirmed as the afterglow, we registered it as AT2023yba (Chen et al.=
, TNS 194096).
We used the 40cm SLT at Lulin Observatory, Taiwan to obtain r-band images o=
f the field of GRB 231117A, as part of the Kinder collaboration (Chen et al=
., AstroNote 2021-92). The first SLT epoch of observations started at 10:51=
UT on 18 of November 2023 (MJD =3D 60266.452), 1.32 days after the Swift t=
rigger. The r-band images were combined from 21 frames with a 300-second ex=
posure time for the r band, taken under seeing conditions of an average of =
1".87 and at a median airmass of 1.16. Then we continuously conducted obser=
vations of i, g, and z-band images, commencing from MJD =3D 60266.552, unde=
r seeing conditions of an average of 1".94 and at a median airmass of 1.83.
We used the Kinder pipeline (Yang et al. A&A 646, A22) to measure the PSF p=
hotometry of AT 2023yba after template subtraction using the SDSS images. W=
e obtained the following magnitudes and a 3-sigma detection limit (in the A=
B system):
r =3D 20.86 +/- 0.13 mag (exposure time of 300sec*21),
i =3D 20.94 +/- 0.17 mag (300sec*6),
g =3D 21.37 +/- 0.13 mag (300sec*6) and
z > 20.02 mag (300sec*6).
The given magnitudes derived based on calibrating against SDSS field stars =
and is not corrected for the expected Galactic foreground extinction corres=
ponding to a reddening of E_(B-V) =3D 0.06 mag in the direction of the burs=
t (Schlafly & Finkbeiner 2011).
Since the various GCNs on this source have heterogeneous methods, we focus =
on comparing our own nightly template subtracted measurements. By comparing=
these data with measurements on MJD =3D 60265.435 (at the epoch of 7.39 ho=
urs after the Swift trigger), we found AT 2023yba has faded by more than 0.=
4 mag in g and i bands in one day, but no fading in the r band. No fading i=
n r band was also noticed in Kumar et al. (GCN 35089) at the epoch of 10.56=
hours. The redshift of the host galaxy, SDSS J220933.34+133119.5, has been=
spectroscopically confirmed at z =3D 0.257 (Ahumada et al., GCN 35093; Gon=
zalez-Ba=C3=B1uelos et al., GCN 35098), placing this transient at absolute =
magnitude M_r =3D -19.6 mag.
- GCN Circular #35114
G. Schroeder (Northwestern), W. Fong, T. Laskar (Utah) report:
"We observed the position of the short GRB 231117A (Laha et al., GCN 35071,
Navaneeth et al., GCN 35072, Cattaneo et al., GCN 35075, Svinkin et al.,
GCN 35079, Cheung et al., GCN 35081) with the Karl G. Jansky Very Large
Array (VLA) under program 23A-296 (PI: Schroeder) beginning on 2023 Nov.
17.98 UT (0.85 days post-burst) for 0.75 hours at a mean frequency of 10
GHz.
We confirm the presence of a radio source consistent with the location of
the putative optical afterglow and host galaxy (Yang et al. GCN 35083,
Rastinejad et al., GCN 35087, Gompertz & Ackley, GCN 35088, Kumar et al.,
GCN 35089, Andreoni et al., GCN 35099, Kilpatrick et al., GCN 35102, Chen
et al. 35105). We measure a flux density of ~190 uJy, resulting in a radio
luminosity of ~4e29 erg/s/Hz, consistent with typical radio luminosities of
SGRB radio afterglows (Laskar et al. 2022).
Our measured flux density is somewhat fainter than the 9 GHz flux with ATCA
reported by Rhodes et al. (GCN 35097). While the ATCA observations occurred
at a slightly earlier mid-time of 0.54 days than our VLA observations, we
cannot make a strong statistically significant claim regarding fading
between the two observations at this time.
We thank the VLA staff for quickly approving and executing these
observations. Further observations are planned to assess the nature of the
radio source."
- GCN Circular #35117
Wang-Chen Xue, Shao-Lin Xiong and Chen-Wei Wang
report on behalf of the GECAM team:
GECAM-C was triggered on ground by a short burst, GRB 231117A at
2023-11-17T03:03:19.210 UTC (denoted as T0), which has been
detected by Swift (GCN 35071), AstroSat (GCN 35072), AGILE (GCN 35075),
Konus-Wind (GCN 35079), Glowbug (GCN 35081), and GRBalpha (GCN 35095).
According to the ground data of GECAM-C, this burst mainly consists
of a short pulse with a duration (T90) of 0.59 +/- 0.04 sec (15-4000 keV).
The GECAM-C localization is consistent with the Swift/BAT localization
(GCN 35074) within the error.
The time-averaged spectrum of GECAM-C data from T0 to T0+1.3 s could be
adequately fit by a cut-off power-law with photon index alpha of -1.52 (-0.07, +0.09),
and peak energy Ep of 437 (-174, +556) keV. The corresponding burst fluence is
8.40 (-1.64, +2.70) * 10^-6 erg/cm^2 in 15-4000 keV.
We note that these results are preliminary and refined analysis will be reported later.
Gravitational wave high-energy Electromagnetic Counterpart All-sky Monitor
(GECAM) mission originally consists of two micro-satellites (GECAM-A and GECAM-B)
launched in Dec. 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).
- GCN Circular #35118
M. Odeh (Al-Khatim Observatory, AKO, operated by the International
Astronomical Center in Abu Dhabi, UAE) and N. Guessoum, D. Akl and I. Abdi
(American University of Sharjah, UAE) report:
As a follow-up to our first observation of GRB 231117A, performed on Nov.
17, 2023 (GCN 35084 <https://gcn.nasa.gov/circulars/35084>), we again
observed the field with our 0.36m f/7.7 robotic telescope, on Nov. 18,
starting at 15:50 UT using an (Ic) filter.
We again detected a faint object at the same location of the source SDSS
J220933.34+133119.5 (PS1 ID =3D 124223323889577032), which is listed in the
Pan-STARRS catalogue with imag =3D 21.5, and in the SDSS catalogue with ima=
g
=3D 20.9. The coordinates of the detected object are: R.A. (2000) =3D
22:09:33.36, Dec. (2000) =3D +13:31:20.1, which is consistent with the
coordinates of the candidate optical source reported by Yang et al. (GCN
35083 <https://gcn.nasa.gov/circulars/35083>).
The following table summarizes the results of both nights using the Atlas
catalogue as a reference:
---------------------------------------------------------------------------
ObsTime (mid), T(Mid)=E2=80=93T(0), Exposure, Filter, Mag, RMS, Limiting Magnitude
---------------------------------------------------------------------------
2023-11-17 15:37:30Z, 12.6 h, 33x180s (stacked), Ic, 19.85, 0.20, 20.2
2023-11-18 15:50:06Z, 1.53 d, 40x180s (stacked), Ic, 19.78, 0.21, 20.4
---------------------------------------------------------------------------
The magnitudes are not corrected for galactic extinction.
- GCN Circular #35119
Lim, Gu (PNU); Park, Junyeong (PNU); Kim, Dohyeong (PNU); Paek, Gregory S. H. (SNU); Im, Myungshin (SNU); Park, Keunhong (MAAO); Choi, Changmin (MAAO); and GECKO Collaboration
We searched for the optical afterglow of GRB 231117A (S. Laha et al., GCN 35071) with a 0.7m telescope at Miryang Arirang Astronomical Observatory (MAAO), one of the facilities of the GW EM-Counterpart Korean Observatory (GECKO). We started the observation at 2023-11-17 10:04:30 UT and obtained 30 images of each 120s with I-band after 6.9 hours after the Swift detection (GCN 35071). No significant source is found within the updated Swift-XRT position (Beardmore et al. GCN 35074). The photometry is performed using a 2xFWHM diameter aperture. The flux is calibrated using the PanStarrs DR1 photometric catalog (AB system) as a reference. The depth is the limiting magnitude for a point source without the galactic extinction correction.
T0 = 2023-11-17T03:03:19 UT (Laha et al., GCN 35071)
Filter Mean_Date-obs(UT) exptime(s) T-T0(d) FWHM(") Depth_3sigma(AB) Depth_5sigma(AB) zp zper
--------------------------------------------------------------------------------------------------------------------------------------------------
I 2023-11-17T10:38:14 120x30 +0.32 3.41 >20.34 >19.78 25.99 0.02
Our detection limit is deeper than the report from MITSuME (Takei et al., GCN 35076).
Gravitational-wave EM Counterpart Korean Observatory (GECKO) is a network of 10+ 0.4m to 1m class telescopes worldwide.
- GCN Circular #35121
M. D. Fulton (QUB), S. Srivastav, S. J. Smartt (Oxford/QUB), J. H. Gillanders (Oxford), K. C. Chambers, M. E. Huber, A. S. B. Schultz (IfA, Hawaii), K. W. Smith, D. R. Young, M. Nicholl, M. McCollum, T. Moore, S. Sim, J. Weston, A. Aamer, C. R. Angus, X. Sheng (QUB), P. Ramsden (QUB/Birmingham), L. Shingles (GSI/QUB), J. Sommer (LMU/QUB), H. Stevance, L. Rhodes, S. Ramaiya, A. Andersson (Oxford), T. de Boer, J. Herman, J. Fairlamb, H. Gao, C. C. Lin, T. Lowe, E. Magnier, P. Minguez, I. A. Smith, R. J. Wainscoat (IfA, Univ. Hawaii), T.-W. Chen (NCU), A. Rest (STScI), C. Stubbs (Harvard) report:
We observed the field of GRB 231117A (Laha et al., GCN 35071; Navaneeth et al., GCN 35072; Beardmore et al., GCN 35074; Cattaneo et al., GCN 35075; Svinkin et al., GCN 35079; Cheung et al., GCN 35081; Dafcikova et al., GCN 35095) with Pan-STARRS1 (Chambers et al., 2016) on two nights in the grizy filters, with the exposures beginning on MJDs 60266.255617 and 60267.271553.
We apply the Pan-STARRS1 reference frames for image subtraction and in all exposures, the afterglow candidate identified by Yang et al. (GCN 35083) as AT2023yba is well detected in griz and marginally in y. We confirm a clear and significant fading in all bands in a comparison between the two nights of:
delta-g = 1.5 +/- 0.2
delta-r = 1.3 +/- 0.2
delta-i = 1.2 +/- 0.2
delta-z = 1.1 +/- 0.2
The latest r-band magnitude at 60267.282458 is r = 22.0 +/- 0.2. This confirms the fast-fading nature of the optical transient AT2023yba, indicating this optical source, discovered by Yang et al. (GCN 35083), is very likely the afterglow of GRB 231117A.
Operation of the Pan-STARRS1 and Pan-STARRS2 telescopes is primarily supported by the National Aeronautics and Space Administration under Grant No. NNX12AR65G and Grant No. NNX14AM74G issued through the SSO Near-Earth Object Observations Program. Data are processed at Queen's University Belfast enabled through the STFC grants ST/P000312/1 and ST/T000198/1.
- GCN Circular #35124
B. Schneider (MIT), C. Adami (LAM/Pytheas/AMU), D. Turpin (CEA Paris-Saclay=
), S. Basa (Pytheas/OHP/LAM), Jean Balcaen (Pytheas/OHP), E. Le Floc'h, F. =
Sch=C3=BCssler (CEA Paris-Saclay), report on behalf of a larger collaborati=
on:
We observed the field of the short GRB 231117A (Laha et al., GCN 35071; Nav=
aneeth et al. GCN 35072; Cattaneo et al., GCN 35075; Svinkin et al., GCN 35=
079; Cheung et al., GCN 35081) and its afterglow candidate (Yang et al. GCN=
35083; Rastinejad et al., GCN 35087; Gompertz et al., GCN 35088; Kumar et =
al., GCN 35089; Ahumada et al., GCN 35093; =E2=80=8B=E2=80=8BRhodes et al.,=
GCN 35097; Andreoni et al., GCN 35099; Kilpatrick et al., GCN 35102) using=
the T120cm telescope at Observatoire de Haute-Provence (France). A total o=
f 11 exposures of 900 seconds were obtained in the r band at 19:52:31.680 U=
T on 2023-11-17, ~16.82h after the trigger.
In the combined frame, we measured a flux excess at the position of SDSS J2=
20933.34+133119.5 compared to archive values. After subtracting the SDSS J2=
20933.34+133119.5 galaxy using the Legacy Survey image, we clearly detect a=
source consistent with the afterglow candidate reported by Yang et al., GC=
N 35083.
The preliminary magnitude derived for that source is
r = 21.0 =C2=B1 0.1 mag (AB)
The photometric calibration was performed using nearby stars from the PanST=
ARRS catalog and magnitudes are not corrected for Galactic extinction.
We acknowledge the Observatoire de Haute Provence staff for their excellent=
support.
- GCN Circular #35128
A. Melandri (INAF-OAR), T. Sbarrato (INAF-OAB), J.A. Kennea (PSU), A.
Tohuvavohu (U. Toronto), D.N. Burrows (PSU), A.P. Beardmore (U.
Leicester), J.P. Osborne (U. Leicester), P. D'Avanzo (INAF-OAB) and
P.A. Evans report on behalf of the Swift-XRT team:
We have analysed 8.8 ks of XRT data for GRB 231117A, from 85 s to 223.3
ks after the BAT trigger. The data comprise 9 s in Windowed Timing
(WT) mode (taken while Swift was slewing), with the remainder in Photon
Counting (PC) mode.
The light curve can be modelled with a power-law decay with a decay
index of alpha=0.65 (+0.07, -0.06).
A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.81 (+0.17, -0.13). The
best-fitting absorption column is consistent with the Galactic value
of 6.1 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 3.6 x 10^-11 (4.1 x 10^-11) erg cm^-2 count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 6.1 (+/-3.8) x 10^20 cm^-2
Galactic foreground: 6.1 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index: 1.81 (+0.17, -0.13)
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/01197027.
This circular is an official product of the Swift-XRT team.
- GCN Circular #35133
I. Takahashi, H. Takei, N. Higuchi, M. Sasada, M. Niwano, S. Sato, S. Hayatsu, H. Seki, Y. Yatsu and N. Kawai (Tokyo Tech) report on behalf of the MITSuME collaboration:
After our previous report (Takei et al., GCN 35076), we reanalyzed all of the GRB 231117A field data observed by the MITSuME 50 cm telescope Akeno on Nov. 17th, and the point source was presumably detected at the afterglow candidate position reported by Yang et al. (GCN 35083). Here we report the Rc-band magnitudes and the 3-sigma limits of the stacked images as follows.
T0+[hour] | MID-UT | T-EXP[sec] | magnitudes of forced-photometry | 3-sigma limits
--------------------------------------------------------------------------------------
6.38 | 2023-11-17 09:25:57 | 5160 | Rc=20.7+/-0.3 | g'>20.5, Rc>20.4, Ic>19.8
7.59 | 2023-11-17 10:38:29 | 10320 | Rc=20.7+/-0.2 | g'>20.8, Rc>20.7, Ic>20.1
--------------------------------------------------------------------------------------
T0+ : Elapsed time after the trigger
T-EXP: Total Exposure time
These magnitudes include the contribution from the underlying host galaxy.
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, Vol.73, Issue 1, Pages 4-24; https://github.com/MNiwano/Eclaire).
- GCN Circular #35134
N.P.M. Kuin (MSSL/UCL) and S. L. Laha (GSFC/UMBC) report
on behalf of the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 231117A
106 s after the BAT trigger (Laha et al., GCN Circ. 35071).
A source consistent with the XRT position (Beardmore et al.,
GCN Circ. 35074 is detected in the initial UVOT exposures.
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 106 1713 392 21.21 +/- 0.27
v 648 1418 78 >18.8
b 574 1688 78 >19.3
u 318 741 265 >19.9
The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.071 in the direction of the burst
(Schlegel et al. 1998).
- GCN Circular #35136
K. Yamaoka (Nagoya U), A. Yoshida, T. Sakamoto, S. Sugita (AGU),
Y. Kawakubo (LSU), S. Nakahira (JAXA), Y. Asaoka (ICRR),
S. Torii, Y. Akaike, K. Kobayashi (Waseda U),
Y. Shimizu, T. Tamura (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 short GRB 231117A (Swift detection: Laha et al., GCN Circ. 35071;
AstroSat CZTI detection: Navaneeth et al., GCN Circ. 35072; AGILE
detection: Cattaneo et al., GCN Circ. 35075; Konus-Wind detection:
Svinkin et al., GCN Circ. 35079; Glowbug gamma-ray detection:
Cheung et al., GCN Circ. 35081; AGILE/MCAL analysis: Casentini
et al., GCN Circ. 35085; GRBAlpha detection: Dafcikova et al., GCN
Circ. 35095; GECAM-C detection: Wang-Chen et al., GCN Circ. 35117)
triggered the CALET Gamma-ray Burst Monitor (CGBM) at 03:03:19.31
UTC on 17 November 2023
(http://cgbm.calet.jp/cgbm_trigger/flight/1384225326/).
The burst signal was seen by all CGBM detectors.
The burst light curve shows a single pulse that starts
at T+0.35 sec, peaks at T+0.68 sec, and ends at T+1.02 sec.
The T90 and T50 durations measured by the SGM data are 0.45
+/- 0.08 sec and 0.15 +/- 0.02 sec (40-1000 keV), respectively.
The ground-processed light curve is available at
http://cgbm.calet.jp/cgbm_trigger/ground/1384225326/
The CALET data used in this analysis are provided by
the Waseda CALET Operation Center located at Waseda University.
- GCN Circular #35138
Malte Busman (LMU), Daniel Gruen (LMU), Brendan O=E2=80=99Connor (CMU), Antonella Palmese (CMU), Lei Hu (CMU), Arno Riffeser (LMU/MPE), Ananya Shankar (LMU) report:
We observed GRB 231117A (Laha et al., GCN 35071; Navaneeth et al., GCN 35072; Beardmore et al., GCN3574; Cattaneo et al., GCN 35075; Svinkin et al., GCN 35079; Cheung et al., GCN 35081, Dafcikova et al., GCN 53095) with the 2m Fraunhofer telescope at Wendelstein Observatory, Germany. Observations were obtained using the 3kk imager in the r, i, and J bands simultaneously. The data were obtained starting at 2023-11-19 18:11:39 UT (~2.6 d after the
GRB) under ~2=E2=80=9D seeing.
At the location of the optical transient (Yang et al., GCN 35083; Rastinejad et al., GCN 35087; Gompertz et al., GCN 35088; Kumar et al., GCN 35089, Ahumada et al., GCN 35093; Andreoni et al., GCN 35099; Kilpatrick et al., GCN 35102; Chen et al., GCN 35105; Odeh et al., GCN 35118; Takahashi et al.,
GCN 35133; Schneider et al., GCN 35124) we measure an optical brightness of
r =3D 21.1 +/- 0.1 AB mag
i =3D 21.2 +/- 0.2 AB mag
Image subtraction has not yet been performed and these magnitudes encompass
both the transient and host galaxy flux. These measurements are consistent
with the archival host galaxy magnitudes, and confirm fading of the optical transient as reported by Fulton et al. (GCN 35121), solidifying the connection to the GRB.
The magnitudes are not corrected for Milky Way extinction and the photometry was calibrated against nearby stars in the PS1 catalog.=20
We thank the staff of the Wendelstein Observatory for obtaining these observations.
- GCN Circular #35139
B. O'Connor (CMU), I. Andreoni (JSI/UMD/NASA-GSFC), G. Srinivasaragavan (UMD), T. Ahumada (Caltech), S. B. Cenko (NASA-GSFC), J. Durbak (UMD), E. Hammerstein (UMD), N. Klingler (UMBC/NASA-GSFC), A. Kutyrev (NASA-GSFC), L. Singer (NASA-GSFC), S. Veilleux (UMD):
We performed additional observations of GRB 231117A (Laha et al., GCN 35071; Navaneeth et al., GCN 35072; Beardmore et al., GCN3574; Cattaneo et al., GCN 35075; Svinkin et al., GCN 35079; Cheung et al., GCN 35081, Dafcikova et al., GCN 53095) with the Large Monolithic Imager (LMI) mounted at the 4-m Lowell Discovery Telescope (LDT) located in Flagstaff, AZ, under program M01 (PI: Andreoni). The observations began on 2023-11-20 02:50:02 UT (~3 d after the GRB) under seeing of ~2.2". We performed observations in the riz bands with 750 s exposure in each band.
At the location of the optical afterglow (Yang et al., GCN 35083; Rastinejad et al., GCN 35087; Gompertz et al., GCN 35088; Kumar et al., GCN 35089, Ahumada et al., GCN 35093; Andreoni et al., GCN 35099; Kilpatrick et al., GCN 35102; Chen et al., GCN 35105; Odeh et al., GCN 35118; Takahashi et al., GCN 35133; Schneider et al., GCN 35124; Busman et al., GCN 35138), we clearly detect a source.
Preliminary photometry (including some contribution from the host) suggests fading by ~0.85 magnitudes in i-band from our previous observations obtained 2.0 days before (Andreoni et al., GCN 35099). Our observations confirm the fading of the optical afterglow candidate, as first reported by Fulton et al. (GCN 35121) and later by Busman et al. (GCN 35138).
We thank the staff of the Lowell Observatory for their support during the observations.
- GCN Circular #35142
Lauren Rhodes, Rob Fender (Oxford), Dave Green, Dave Titterington (Cambridge) report:
We observed the field of the afterglow candidate GRB 231117A (GCN 35071) with the Arcminute Microkelvin Imager Large-Array (AMI-LA) at 15.5 GHz beginning at UT 15:30:45 on 17-Nov-2023 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 J2232+1143 was used as an interleaved complex gain calibrator.
We do not detect any radio emission at the position of the afterglow candidate as reported in GCN 35083 with a 3-sigma upper limit of 230uJy/beam.
We thank the staff at the Mullard Radio Astronomy Observatory for carrying out these observations and operating the AMI-LA.
- GCN Circular #35152
C. B. Markwardt (GSFC), S. D. Barthelmy (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/UMBC),
T. Sakamoto (AGU), M. Stamatikos (OSU)
(i.e. the Swift-BAT team):
Using the data set from T-60 to T+243 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 231117A (trigger #1197027)
(Laha, et al., GCN Circ. 35071). The BAT ground-calculated position is
RA, Dec =3D 332.404, 13.516 deg which is
RA(J2000) =3D 22h 09m 37.0s
Dec(J2000) =3D +13d 30' 58.1"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 83%.
The mask-weighted light curve shows a very strong fast rise exponential decay profile
with potential precursor emission prior to the main pulse.
T90 (15-350 keV) is 0.67 +- 0.07 sec (estimated error including systematics).
The time-averaged spectrum from T-0.42 to T+1.30 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
1.55 +- 0.04. The fluence in the 15-150 keV band is 2.3 +- 0.1 x 10^-06 erg/cm2.
The 1-sec peak photon flux measured from T-0.05 sec in the 15-150 keV band
is 28.9 +- 0.7 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/1197027/BA/
- GCN Circular #35153
Alan M. Watson (UNAM), Simone Dichiara (PSU), Eleonora Troja
(Universit=C3=A0 di Roma Tor Vergata), Brendan O=E2=80=99Connor (CMU), Rosa L.
Becerra (UNAM), Nathaniel R. Butler (ASU), Nissim Fraija (UNAM),
William Lee (UNAM), Oc=C3=A9lotl L=C3=B3pez (UNAM), and Margarita Pereyra (UNAM)
report:
We observed the field of GRB 231117A (Laha et al., GCN 35071;
Navaneeth et al., GCN 35072; Beardmore et al., GCN3574; Cattaneo et
al., GCN 35075; Svinkin et al., GCN 35079; Cheung et al., GCN 35081;
Dafcikova et al., GCN 53095; Busman et al. GCN 35138; O'Connor et al.,
GCN 35139) with the EMIR instrument on the GTC telescope from
2023-11-19 19:33 to 19:57 UTC (64.5 to 64.9 hours after the trigger).
We obtained total integrations of 420 in J and 252 in Ks with a seeing
of about 0.8 arcsec.
From our preliminary analysis, the source is detected in all filters
with brightness J =3D 20.9 +/- 0.1 AB, with an uncertain contribution
from the host galaxy. This value is not corrected for Galactic
extinction.
Further observations are planned.
We thank the staff of the GTC, including Riccardo Scarpa and Antonio
Cabrera, for their help with these observations.
- GCN Circular #35154
N.P.M. Kuin (MSSL/UCL) and S. L. Laha (GSFC/UMBC)
report on behalf of the Swift/UVOT team:
The initial Swift/UVOT observations of the field of GRB 231117A
(Laha et al., GCN Circ. 35071) have been reported by Kuin and
Laha (GCN Circ. 35134) based on the enhanced XRT position (Beardmore
et al. GCN Circ. 35074). A refined position was published by
Yang et al. (GCN Circ. 35083) which we use for the current
circular.
We report here exposures taken over the specified period and summed for
better S/N. We also report here in AB magnitudes (Breeveld et al. 2011,
AIP Conf. Proc. 1358, 373):
Filter T_start(s) T_stop(s) Exp(s) AB-Mag
white 106 1713 392 22.3 +/- 0.5
u 5863 18,406 917 20.9 +/- 0.2
white 67,725 68,529 675 21.7 +/- 0.2
white 210,209 223,742 4848 22.4 +/- 0.4
Considering that these are AB magnitudes, we can compare the white and u
values to see a likely peak around the time of the u magnitude with a
subsequent decay.
The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.071 in the direction of the burst
(Schlegel et al. 1998).
- GCN Circular #35160
Simone Dichiara (PSU), Alan M. Watson (UNAM), Nathaniel R. Butler (ASU), El=
eonora Troja (Universit=C3=A0 di Roma Tor Vergata), Brendan O=E2=80=99Conno=
r (CMU), Rosa L. Becerra (UNAM), Nissim Fraija (UNAM), William Lee (UNAM), =
Kin L=C3=B3pez (UNAM), and Margarita Pereyra (UNAM) report:
We observed the field of GRB 231117A (Laha et al., GCN 35071; Navaneeth et =
al., GCN 35072; Beardmore et al., GCN3574; Cattaneo et al., GCN 35075; Svin=
kin et al., GCN 35079; Cheung et al., GCN 35081; Dafcikova et al., GCN 5309=
5; Busman et al. GCN 35138; O'Connor et al., GCN 35139; Watson et al., GCN =
35153, Kuin et al., GCN 35154) with the OSIRIS instrument on the GTC telesc=
ope from 2023-11-21 20:34 to 21:16 UTC (113.5 to 114.2 hours after the trig=
ger). We obtained total integrations of 480 s in r and 960 s in z with a s=
eeing of about 0.9 arcsec.
We detect the source in both bands but, even with our good seeing, reliable
photometry will require image subtraction. We measure r =3D 21.8 +/- 0.1 AB,
with an uncertain contribution from the host galaxy. This value is not corrected for Galactic extinction.
Further observations are planned.
We thank the staff of the GTC, especially David Garc=C3=ADa =C3=81lvarez and
Antonio Cabrera, for their help with these observations.
- GCN Circular #35163
W. Fong, T. Eftekhari, G. Schroeder (Northwestern), A. Rouco Escorial (ESA/ESAC) report:
"The Chandra X-ray Observatory observed the position of the short-duration GRB 231117A (Laha et al., GCN 35071, Navaneeth et al., GCN 35072, Cattaneo et al., GCN 35075, Svinkin et al., GCN 35079, Cheung et al., GCN 35081) starting on 2023 November 21 at 06:22:13 UT. We obtained an ACIS-S observation under Proposal 24400307 (PI: Fong), with an effective exposure time of ~27 ksec, for a mid-time of 4.3 days post-burst.
The X-ray afterglow is clearly detected at high significance. The source is spatially coincident with the optical (e.g., Yang et al., GCN 35083, Rastinejad et al., GCN 35087, Gompertz et al., GCN 35088) and radio (Rhodes et al., GCN 35097, Schroeder et al., GCN 35114) afterglows at the position:
RA (J2000) = 22:09:33.37
Dec (J2000) = 13:31:20.0
We note that, similar to the reported optical positions, the Chandra source is just outside the 90% confidence region of the latest XRT position. We measure a 0.3-10 keV flux for the Chandra afterglow of FX ~ 2e-13 erg/s/cm^2. We find that the XRT light curve beyond ~300 seconds post-burst can be modeled with a single power-law with FX ~ t^-0.6, and that the Chandra observation is fully consistent with this power law.
We thank the Chandra staff for rapid approval and planning of these observations."
- GCN Circular #35172
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 231117A (Laha et al., GCN 35071; Navaneeth et al., GCN 35072; Beardmore et al., GCN3574; Cattaneo et al., GCN 35075; Svinkin et al., GCN 35079; Cheung et al., GCN 35081; Dafcikova et al., GCN 53095; Busman et al. GCN 35138; O'Connor et al., GCN 35139; Watson et al., GCN 35153, Kuin et al., GCN 35154; Dichiara et al., GCN 35160; Fong et al., GCN 35163) with AZT-33IK telescope of Mondy observatory in R-filter on 2023-11-17, 2023-11-18 and 2023-11-20. Using image subtraction and the image on 2023-11-20 as a template we obtained preliminary photometry of the optical transient
Date UT start t-T0 Exp. Filter OT Err.
(mid, days) (s)
2023-11-17 11:45:33 0.38349 30x120 R 21.00 0.16
2023-11-18 12:09:46 1.41142 46x120 R 21.59 0.16
The photometry is based on nearby USNO-B1.0 R2 stars. The index of power law (t-T0)^-alpha between the two epochs is alpha = 0.8 (+0.13 -0.2).
However, photometry may be biased due to the template contamination by a still decaying optical transient, so we caution against using this index for any physical assessments.
- GCN Circular #35201
L. Rhodes (Oxford), G. Schroeder (Northwestern), G. Anderson (Curtin), W. Fong (Northwestern), S. Chastain (UNM), A. Gulati (USyd), A. van der Horst(GWU), C. Kilpatrick (Northwestern), N. Klinger (NASA/GSFC), T. Laskar (Utah), J. K. Leung (UofT/HUJI), A. Nugent (Northwestern), J. Rastinejad (Northwestern), S. D. Ryder (Macquarie) on behalf of a larger collaboration.
We observed GRB 231117A (GCN 35071) with the MeerKAT radio telescope at 1.3GHz for a total of 2 hours starting on 26 November 2023 at 12:47 UTC. The observations used J1939-6342 and J2232+1143 as flux and phase calibrators, respectively. Using the SARAO SDP image we find an unresolved source at the position of the afterglow candidate (GCN 35083) with a flux density of ~100uJy/beam. The rms noise in the field is 7uJy/beam. We note that the measured flux density may have a substantial contribution from the host galaxy reported in GCN 35083 but said contribution cannot be quantified until the afterglow has faded.
We thank the staff at the South African Radio Astronomy Observatory for scheduling these observations.
Previous IAU Circulars 