GRB230217A

This page lists all entries on GRB230217A in GRBweb

Summary Fermi GBM IPN Swift GCN 33338 GCN 33339 GCN 33343 GCN 33348 GCN 33349 GCN 33353 GCN 33356 GCN 33358 GCN 33360 GCN 33361 GCN 33363 GCN 33365 GCN 33368 GCN 33370 GCN 33374 GCN 33433

Summary table
Variable Value Source
GRB_name_Fermi GRB230217912
T0 21:53:06.119 UTC GCN_circulars,Konus-Wind Det
ra 280.7700° Swift
decl -28.8374° Swift
pos_error 6.08e-04° Swift
T90 0.896 s Fermi_GBM
T90_error 0.143 s Fermi_GBM
T90_start 21:53:10.785 UTC Fermi_GBM
fluence 1.73e-05 erg/cm² Fermi_GBM
fluence_error 7.63e-08 erg/cm² Fermi_GBM
T100 5.562 s
GBM_located False
mjd 59992.911876377315 GCN_circulars,Konus-Wind Det
Fermi GBM table
GRB_name_Fermi GRB230217912
trigger_name bn230217912
ra 280.7708°
decl -28.8561°
pos_error 2.69e+00°
datum 2023-02-17
t_trigger 21:53:10.689 UTC
T90 0.896 s
T90_error 0.143 s
T90_start 21:53:10.785 UTC
fluence 1.73e-05 erg/cm²
fluence_error 7.63e-08 erg/cm²
flux_1024 4.38e+01 erg/cm²/s
flux_1024_error 5.26e-01 erg/cm²/s
flux_1024_time -9.60e-02 erg/cm²/s
flux_64 9.31e+01 erg/cm²/s
flux_64_error 2.77e+00 erg/cm²/s
IPN table
GRB_name GRB230217A
ra 280.7708°
decl -28.8500°
pos_error 5.00e-02°
Swift table
GRB_name GRB230217A
t_trigger 21:53:10 UTC
ra 280.7700°
decl -28.8374°
pos_error 6.08e-04°
T90 1.3 s
fluence 2.30e-06 erg/cm²
GCN 33338 table
GRB_name GRB230217A
GCN_number 33338
Detection_method Fermi GBM final loc
t_trigger 21:53:10 UTC
ra 278.8000°
decl -27.4000°
Circular_text TITLE: GCN CIRCULAR NUMBER: 33338 SUBJECT: GRB 230217A: Fermi GBM Final Real-time Localization DATE: 23/02/17 22:04:27 GMT FROM: Fermi GBM Team at MSFC/Fermi-GBM The Fermi GBM team reports the detection of a likely LONG GRB At 21:53:10 UT on 17 Feb 2023, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 230217A (trigger 698363595.689472 / 230217912). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 278.8, Dec = -27.4 (J2000 degrees, equivalent to J2000 18h 35m, -27d 23'), with a statistical uncertainty of 1.0 degrees. The angle from the Fermi LAT boresight is 56.0 degrees. The skymap can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230217912/quicklook/glg_skymap_all_bn230217912.png The HEALPix FITS file, including the estimated localization systematic, can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230217912/quicklook/glg_healpix_all_bn230217912.fit The GBM light curve can be found here: https://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2023/bn230217912/quicklook/glg_lc_medres34_bn230217912.gif
GCN 33339 table
GRB_name GRB230217A
GCN_number 33339
Detection_method Swift Det
t_trigger 21:53:10 UTC
ra 280.7710°
decl -28.8560°
Circular_text TITLE: GCN CIRCULAR NUMBER: 33339 SUBJECT: GRB 230217A: Swift detection of a short burst DATE: 23/02/17 22:07:41 GMT FROM: Kim Page at U.of Leicester M. J. Moss (GWU), R. A. J. Eyles-Ferris (U Leicester), J.D. Gropp (PSU), H. A. Krimm (NSF), F. E. Marshall (NASA/GSFC), K. L. Page (U Leicester), B. Sbarufatti (INAF-OAB) and M. A. Williams (PSU) report on behalf of the Neil Gehrels Swift Observatory Team: At 21:53:10 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 230217A (trigger=1154967). Swift did not slew to the burst due to an observing constraint. The BAT on-board calculated location is RA, Dec 280.771, -28.856 which is RA(J2000) = 18h 43m 05s Dec(J2000) = -28d 51' 19" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a single short peak with a duration of about 1 sec. The peak count rate was ~15000 counts/sec (15-350 keV), at ~0 sec after the trigger. Due to a Moon observing constraint, Swift cannot slew to the BAT position until 10:09 UT on 2023 February 18. There will thus be no XRT or UVOT data for this trigger before this time. Burst Advocate for this burst is M. J. Moss (mikejmoss3 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 33343 table
GRB_name GRB230217A
GCN_number 33343
Detection_method Swift-BAT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 33343 SUBJECT: GRB 230217A: AGILE/MCAL detection DATE: 23/02/18 10:41:34 GMT FROM: Claudio Casentini at INAF-IAPS C. Casentini (INAF/IAPS), F. Verrecchia (SSDC, and INAF/OAR), F. Longo (Uni. Trieste, INFN Trieste) M. Tavani (INAF/IAPS, and Univ. Roma Tor Vergata), C. Pittori, F. Lucarelli, A. Argan, M. Cardillo, Y. Evangelista, L. Foffano, G. Piano (INAF/IAPS), A. Addis, L. Baroncelli, A. Bulgarelli, A. Di Piano, V. Fioretti, G. Panebianco, N. Parmiggiani (INAF/OAS-Bologna), M. Romani (INAF/OA-Brera), M. Marisaldi (INAF/OAS-Bologna, Bergen University), M. Pilia, A. Trois (INAF/OA Cagliari), I. Donnarumma, E. Menegoni, A.Ursi (ASI), A. Giuliani (INAF/IASF-Mi) and P. Tempesta (TeleSpazio), report on behalf of the AGILE Team: The AGILE satellite detected the short GRB 230217A at T0 = 2023-02-17 21:53:10.87 (UTC), reported by Fermi/GBM (GCN #33338) and Swift BAT (GCN #33339). The burst is clearly visible in the AGILE scientific ratemeters of the MiniCALorimeter (MCAL; 0.4-100 MeV), and in all the panels of the AntiCoincidence detectors (AC Top, 50-200 keV; AC Lat, 80-200 keV). The event lasted about 2 s and it released a total number of 7554 counts in the MCAL detector (above a background rate of 529 Hz), and 38605 counts in the AC Top detector (above a background rate of 3530 Hz). The AGILE ratemeters light curves can be found at: http://www.agilescienceapp.it/notices/GRB230217A_AGILE_RM_ND.png . The event also triggered a high-time resolution MCAL data acquisition, from T0-0.7 s to T0+5.8 s (UTC), and released 2515 counts in the detector, above a background rate of 776 Hz. The MCAL light curve can be found at: http://www.agilescienceapp.it/notices/GRB230217A_082311_603755590.000000.png . The time-integrated spectrum of the burst between T0-1s and T0+1s, fitted in the energy range 0.4-10 MeV with a p.l. with ph. ind. = -2.12 (+/-0.08) resulting in a reduced chi-squared of 0.92 (48 d.o.f.) and a fluence of 4.05e-06 ergs/cm^2 (90% confidence level), in the same energy range. At the T0, the event was 59 deg off-axis. 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 33348 table
GRB_name GRB230217A
GCN_number 33348
Detection_method Swift-XRT Other
ra 280.7700°
decl -28.8374°
Circular_text TITLE: GCN CIRCULAR NUMBER: 33348 SUBJECT: GRB 230217A: Swift-XRT observations DATE: 23/02/19 07:48:15 GMT FROM: Phil Evans at U of Leicester M. Capalbi (INAF-IASFPA), J.A. Kennea (PSU), A. Tohuvavohu (U. Toronto), D.N. Burrows (PSU), K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester), M. Perri (SSDC & INAF-OAR), V. D'Elia (SSDC & INAF-OAR) and M. J. Moss (GWU) report on behalf of the Swift-XRT team: We have analysed 4.8 ks of Photon Counting (PC) mode XRT data for the Swift-BAT-detected burst GRB 230217A (Moss et al. GCN Circ. 33339), collected between T0+45.8 ks and T0+84.4 ks. Two uncatalogued X-ray sources have been detected consistent with being within 296 arcsec of the Swift-BAT position, however none of them is above the RASS limit or shows definitive signs of fading. Therefore, at the present time we cannot identify which, if any, is the afterglow. Details of these sources are given below: Source 3: RA (J2000): 280.7700 = 18:43:4.80 Dec (J2000): -28.8374 = -28:50:14.6 Error: 4.7 arcsec (radius, 90% conf. [Enhanced position]) Count-rate: 0.0144 [+0.0022, -0.0021] ct s^-1 Distance: 67 arcsec from Swift-BAT position. Flux: (6.48 [+0.98, -0.94])e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV) Source 5: RA (J2000): 280.7763 = 18:43:6.30 Dec (J2000): -28.7796 = -28:46:46.7 Error: 6.4 arcsec (radius, 90% conf.) Count-rate: (1.43 [+0.85, -0.64])e-3 ct s^-1 Distance: 275 arcsec from Swift-BAT position. Six uncatalogued sources were also detected too far from the GRB position to be likely afterglow candidates. The results of the XRT-team automatic analysis of the XRT observations, including a position-specific upper limit calculator, are available at https://www.swift.ac.uk/ToO_GRBs/01154967. This circular is an official product of the Swift-XRT team.
GCN 33349 table
GRB_name GRB230217A
GCN_number 33349
Detection_method Konus-Wind Det
t_trigger 21:53:06.119 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 33349 SUBJECT: Konus-Wind detection of GRB 230217A DATE: 23/02/19 12:10:55 GMT FROM: Dmitry Svinkin at Ioffe Institute D. Svinkin, D. Frederiks, M. Ulanov, A. Tsvetkova, A. Lysenko, A. Ridnaia, and T. Cline on behalf of the Konus-Wind team, report: The short-duration GRB 230217A (Fermi-GBM detectin: The Fermi-GBM team, GCN Circ. 33338; Swift-BAT detection: Moss et al., GCN Circ. 33339; CALET-GBM detection: Torii et al., GCN Circ. 33342; AGILE-MCAL detection: Casentini et al., GCN Circ. 33343) triggered Konus-Wind at T0=78786.119 s UT (21:53:06.119). The burst light curve shows a multi-peaked structure which starts at ~T0-0.2 s and has a total duration of ~0.9 s. The emission is seen up to ~6 MeV. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB230217_T78786/ As observed by Konus-Wind, the burst had a fluence of 2.74(-0.35,+0.39)x10^-5 erg/cm2, and a 16-ms peak flux, measured from T0+0.128 s, of 9.45(-1.84,+1.94)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+8.448 s) is best fit in the 20 keV - 10 MeV range by a power law with exponential cutoff model: dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep) with alpha = -0.81(-0.13,+0.14) and Ep = 1367(-240,+309) keV (chi2 = 105/98 dof). Fitting by a GRB (Band) model yields the same alpha and Ep, and an upper limit on the high energy photon index: beta <-2.7 (chi2 = 105/97 dof). All the quoted errors are at the 90% confidence level. All the quoted values are preliminary.
GCN 33353 table
GRB_name GRB230217A
GCN_number 33353
Detection_method Fermi GBM Det
t_trigger 21:53:10.690 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 33353 SUBJECT: GRB 230217A: Fermi GBM observation DATE: 23/02/20 14:57:16 GMT FROM: Peter Veres at UAH P. Veres (UAH) reports on behalf of the Fermi GBM Team: "At 21:53:10.69 UT on 17 February 2023, the Fermi Gamma-Ray Burst Monitor (GBM) triggered and located GRB 230217A (trigger 698363595 / 230217912). which was also detected by the Swift/BAT (Moss et al., GCN 33339), AGILE (Casentini et al., GCN 33343), CALET-GBM (Torii et al., GCN 33342) and Konus-Wind (Svinkin et al., GCN 33349). The GBM on-ground location is consistent with the Swift position. The angle from the Fermi LAT boresight at the GBM trigger time is 58 degrees. The GBM light curve consists of a single pulse with a duration (T90) of about 0.90 s (50-300 keV). The time-averaged spectrum from T0s to T0+1.4 s is best fit by a power law function with an exponential high-energy cutoff. The power law index is -0.74 +/- 0.02 and the cutoff energy, parameterized as Epeak, is 1497 +/- 63 keV. The event fluence (10-1000 keV) in this time interval is (1.81 +/- 0.02)E-5 erg/cm^2. The 64 ms peak photon flux measured starting from T0+0.22 s in the 10-1000 keV band is 93.1 +/- 2.8 ph/s/cm^2. A Band function fits the spectrum equally well with Epeak= 1476 +/- 79 keV, alpha = -0.74 +/- 0.02 and beta = 3.07+/-0.82. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog: https://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html For Fermi GBM data and info, please visit the official Fermi GBM Support Page: https://fermi.gsfc.nasa.gov/ssc/data/access/gbm/"
GCN 33356 table
GRB_name GRB230217A
GCN_number 33356
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 33356 SUBJECT: GRB 230217A: Gemini-South Optical Observation DATE: 23/02/20 18:26:01 GMT FROM: Brendan O'Connor at UMD B. O'Connor (UMD, GWU) and E. Troja (UTV, ASU), report on behalf of a larger collaboration: We carried out optical observations with the 8.1m Gemini-South Telescope in Cerro Pachon, Chile targeting the location of the short GRB 230217A (Moss et al. GCN 33339). We observed the position of X-ray Source 3 reported by Capalbi et al. (GCN 33348) at 09:24:47 UT on 2023-02-20, corresponding to ~2.5 d after the GRB trigger (Moss et al. GCN 33339, Svinkin et al. GCN 33349, Veres et al. GCN 33353). The target was observed during twilight for 300 s in i-band. Within the source localization, we do not find any obvious counterpart when compared to the PS1 catalog to depth i>22.8 AB mag (not corrected for Galactic extinction along the line of sight). However, objects fainter than the PS1 limits are resolved in our observation and will require image subtraction to establish fading. Further observations are planned. We thank the staff of the Gemini Observatory for assistance in rapidly obtaining these observations.
GCN 33358 table
GRB_name GRB230217A
GCN_number 33358
Detection_method VLA Det
ra 280.7706°
decl -28.8379°
Circular_text TITLE: GCN CIRCULAR NUMBER: 33358 SUBJECT: GRB 230217A: 6 GHz VLA observations DATE: 23/02/20 22:04:09 GMT FROM: Genevieve Schroeder at Northwestern University G. Schroeder, W. Fong (Northwestern), E. Berger (Harvard), T. Laskar (Utah) report: "We observed the short GRB 230217A (Moss et al., GCN 33339; Casentini et al., GCN 33343; Torii et al., GCN 33342; Svinkin et al., GCN 33349) with the Karl G. Jansky Very Large Array (VLA) under program 23A-296 (PI: Schroeder) beginning on 2023 February 18.67 UT (0.76 days post-burst) at a mean frequency of 6 GHz. The VLA has a primary beam of ~7 arcmin at 6 GHz, covering the entirety of the Swift/BAT position (Moss et al., GCN 33339). We searched for radio sources near the two X-ray sources coincident with the Swift/BAT localization found by Swift/XRT (Source 3 and Source 5, Capalbi et. al GCN 33348), though neither X-ray source has been definitively determined the X-ray afterglow. We detect radio sources coincident with both XRT sources. Our preliminary results are as follows: Source 3: flux of ~65 microJy (~9 sigma) at the position: RA(J2000) = 18:43:04.948 Dec(J2000) = -28:50:16.60 with an uncertainty of ~0.3" in each coordinate. Source 5: flux of ~20 microJy (~3 sigma) at the position: RA(J2000) = 18:43:06.762 Dec(J2000) = -28:46:48.06 with an uncertainty of ~0.6" in each coordinate. We thank the VLA staff for quickly approving and executing these observations."
GCN 33360 table
GRB_name GRB230217A
GCN_number 33360
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 33360 SUBJECT: GRB 230217A: Gemini South optical upper limits DATE: 23/02/21 07:27:44 GMT FROM: Eleonora Troja at GSFC E. Troja (UTV) and B. O’Connor (GWU) report: We inspected the GMOS-S observations of the short GRB 230217A reported in O’Connor et al. (GCN Circ. 33356). At the position of the radio source (Schroeder et al., GCN Circ 33358) coincident with the X-ray source #3 (Capalbi et al. GCN Circ. 33348), no optical counterpart is detected down to i>23 AB mag, not corrected for Galactic extinction. The lack of optical detection does not rule out an afterglow origin for the X-ray source and remains consistent with a power-law spectrum with slope beta_OX < 0.6. Further observations are encouraged to establish variability. Our images do not cover the position of the X-ray/radio source #5, which lies just outside the BAT error circle. We thank the staff of the Gemini Observatory for assistance in rapidly obtaining these observations.
GCN 33361 table
GRB_name GRB230217A
GCN_number 33361
Detection_method AstroSat CZTI
Circular_text TITLE: GCN CIRCULAR NUMBER: 33361 SUBJECT: GRB 230217A: AstroSat CZTI detection DATE: 23/02/21 08:14:53 GMT FROM: Gaurav Waratkar at IIT,Bombay P K. Navaneeth (IUCAA), R. Gopalakrishnan (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 short GRB230217A which was also detected by Fermi-GBM (Fermi GBM team, GCN Circ. 33338), Swift-BAT (Moss et al., GCN Circ. 33339), AGILE/MCAL (Casentini et al., GCN Circ. 33343), Swift-XRT (Capalbi et al., GCN Circ. 33348) and Konus-Wind (Svinkin et al., GCN Circ. 33349). The source was clearly detected in the 20-200 keV energy range. The light curve peaks at 2023-02-17 21:53:10.9 UTC. The measured peak count rate associated with the burst is 6691 (+436, -444) counts/s above the background in the combined data of all quadrants, with a total of 3487 (+142, -172) counts. The local mean background count rate was 454 (+9, -10) counts/s. Using cumulative rates, we measure a T90 of 0.77 (+0.19, -0.07) s. It was also detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range. CZTI GRB detections are reported regularly on the payload site at http://astrosat.iucaa.in/czti/?q=grb. 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.
GCN 33363 table
GRB_name GRB230217A
GCN_number 33363
Detection_method Swift-BAT Det
ra 280.7590°
decl -28.8400°
Circular_text TITLE: GCN CIRCULAR NUMBER: 33363 SUBJECT: GRB 230217A: Swift-BAT refined analysis DATE: 23/02/21 18:54:55 GMT FROM: Hans Krimm at NSF/NASA-GSFC S. D. Barthelmy (GSFC), H. A. Krimm (NSF), S. Laha (GSFC/UMBC), A. Y. Lien (U Tampa), C. B. Markwardt (GSFC), M. J. Moss (GWU), 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-240 to T+962 sec from the recent telemetry downlink, we report further analysis of BAT GRB 230217A (trigger #1154967) (Moss, et al., GCN Circ. 33339). The BAT ground-calculated position is RA, Dec = 280.759, -28.840 deg which is RA(J2000) = 18h 43m 02.2s Dec(J2000) = -28d 50' 23.0" with an uncertainty of 1.3 arcmin, (radius, sys+stat, 90% containment). The partial coding was 21%. The mask-weighted light curve shows a double-peaked event running from T -0.2 sec to about T+1.2 sec. T90 (15-350 keV) is 1.30 +- 0.45 sec. (estimated error including systematics). The T90 vs. hardness diagram shows the burst well within the short-hard burst region. The time-averaged spectrum from T-0.26 to T+1.75 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 0.99 +- 0.12. The fluence in the 15-150 keV band is 2.3 +- 0.2 x 10^-6 erg/cm2. The 1-sec peak photon flux measured from T-0.24 sec in the 15-150 keV band is 20.2 +- 1.5 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/1154967/BA/
GCN 33365 table
GRB_name GRB230217A
GCN_number 33365
Detection_method Swift-XRT Other
ra 280.7700°
decl -28.8374°
Circular_text TITLE: GCN CIRCULAR NUMBER: 33365 SUBJECT: GRB 230217A: Swift-XRT afterglow detection DATE: 23/02/22 08:59:54 GMT FROM: Phil Evans at U of Leicester M. Capalbi (INAF-IASFPA), J.A. Kennea (PSU), A. Tohuvavohu (U. Toronto), D.N. Burrows (PSU), K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester), M. Perri (SSDC & INAF-OAR), V. D'Elia (SSDC & INAF-OAR) and P.A. Evans (U. Leicester) report on behalf of the Swift-XRT team: Swift-XRT has conducted further observations of the field of the Swift-BAT-detected burst GRB 230217A (Barthelmy et al. GCN Circ. 33363). The observations now extend from T0+45.9 ks to T0+342.9 ks. Of the sources reported by Capalbi et al. (GCN Circ. 33348), "Source 3" is fading with >3-sigma significance, and is therefore likely the GRB afterglow. Using 874 s of PC mode data and 1 UVOT image, we find an enhanced XRT position (using the XRT-UVOT alignment and matching UVOT field sources to the USNO-B1 catalogue): RA, Dec = 280.77002, -28.83740 which is equivalent to: RA (J2000): 18h 43m 04.80s Dec(J2000): -28d 50' 14.6" with an uncertainty of 4.7 arcsec (radius, 90% confidence). This position is 67 arcsec from the Swift-BAT position. The light curve can be modelled with a power-law decay with a decay index of alpha=1.1 (+0.6, -0.4). A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 1.6 (+0.8, -0.4). The best-fitting absorption column is consistent with the Galactic value of 1.6 x 10^21 cm^-2 (Willingale et al. 2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 4.4 x 10^-11 (5.1 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 1.6 (+/-4.1) x 10^21 cm^-2 Galactic foreground: 1.6 x 10^21 cm^-2 Excess significance: <1.6 sigma Photon index: 1.6 (+0.8, -0.4) The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/01154967. The results of the full analysis of the XRT observations are available at https://www.swift.ac.uk/ToO_GRBs/01154967. This circular is an official product of the Swift-XRT team.
GCN 33368 table
GRB_name GRB230217A
GCN_number 33368
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 33368 SUBJECT: GRB 230217A: Continued Gemini Observations DATE: 23/02/22 16:50:07 GMT FROM: James Gillanders at University of Rome Tor Vergata J. Gillanders (UTV), B. O'Connor (UMD, GWU) and E. Troja (UTV) report: We performed further follow-up of the short GRB 230217A (Moss et al. GCN 33339, Svinkin et al. GCN 33349, Veres et al. GCN 33353) using the GMOS instrument at Gemini-South. Observations were carried out in the i-band and began at 08:55:27 on 2023-02-21, corresponding to ~3.5 d after the GRB trigger. Following recent XRT observations, X-ray source 3 has been confirmed to fade with >3-sigma significance, and thus is likely the GRB afterglow (Capalbi et al. GCN 33365). By performing image subtraction between the two Gemini observations (see also O’Connor et al. GCN 33356, Troja et al. GCN 33360) we find no sign of variability and place a limit of i>23 AB mag over the entire XRT error circle. At the position of the radio source #3 (Schroeder et al. GCN 33358), we set an upper limit of i>24.3 AB mag at 3.5 d post-burst. This value is not corrected for Galactic extinction. We thank the staff of the Gemini Observatory for executing these observations.
GCN 33370 table
GRB_name GRB230217A
GCN_number 33370
Detection_method Swift-UVOT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 33370 SUBJECT: GRB 230217A: Swift/UVOT Upper Limits DATE: 23/02/22 21:02:57 GMT FROM: Alexander Belles at PSU/Swift The Swift/UVOT began settled observations of the field of GRB 230217A 45.8 ks after the Swift/BAT trigger (Moss et al., GCN Circ. 33339). No optical afterglow consistent with the XRT position (Capalbi et al., GCN Circ. 33365) is detected in the initial UVOT exposures. Preliminary 3-sigma upper limits using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the initial exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag wh 45886 84347 2643 >21.37 u 329962 342875 4884 >20.78 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.15 in the direction of the burst (Schlegel et al. 1998).
GCN 33374 table
GRB_name GRB230217A
GCN_number 33374
Detection_method Optical
ra 280.7707°
decl -28.8379°
Circular_text TITLE: GCN CIRCULAR NUMBER: 33374 SUBJECT: GRB 230217A: VLT/FORS2 optical observations and candidate counterpart DATE: 23/02/24 15:50:32 GMT FROM: Paolo D'Avanzo at INAF-OAB P. D'Avanzo, A. Rossi (INAF-OAS), R. Brivio (INAF-OAB), D. B. Malesani (Radboud Univ.and DAWN/NBI), A. Saccardi (GEPI, Observatoire de Paris), S. Campana (INAF-OAB), B. Gompertz (Univ. Birmingham), D. Hartmann (Clemson Univ.), D. A. Kann (Goethe Univ). A. J. Levan (Radboud Univ.), G. Tagliaferri (INAF-OAB), N. R. Tanvir (Univ. Leicester) report on behalf of the Stargate consortium: We observed the field of the short GRB 230217A (Moss et al. GCN Circ. 33339) with the ESO/VLT equipped with the FORS2 instrument. A series of optical images has been obtained with the I filter on 2023 February 20 (i.e. about 2.5 days after the burst) and on 2023 February 23 (i.e. about 5.5 days after the burst). Image subtraction carried out between the two epochs shows a residual at the following position: RA (J2000) = 18:43:04.97 Dec (J2000) = -28:50:16.4 +/- 0.3". This position lies inside the XRT error circle of the X-ray afterglow position (Capalbi et al., GCN Circ. 33365) and is consistent with the position of the radio source reported by Schroeder et al. (GCN Circ. 33358). From preliminary photometry, we measure for this source a magnitude of I ~ 24.5 (AB) at t-t0 = 2.5 days. We propose this source as a candidate optical counterpart of GRB 230217A. Further observations are planned. We acknowledge excellent support from the ESO observing staff in Paranal, in particular Julia Seidel, Konrad Tristram and Thomas Rivinius.
GCN 33433 table
GRB_name GRB230217A
GCN_number 33433
Detection_method Swift-BAT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 33433 SUBJECT: GRB 230217A: ATCA rapid-response radio detection DATE: 23/03/09 07:49:56 GMT FROM: Gemma Anderson at Curtin U G. E. Anderson (Curtin), J. Stevens (CSIRO), M. E. Bell (UNewcastle), T. D. Russell (INAF), P. J. Hancock (Curtin), J. C. A. Miller-Jones (Curtin), A. Bahramian (Curtin), A. J. van der Horst (GWU), S. D. Ryder (Macquarie), A. Rowlinson (UvA, ASTRON), R. A. M. J. Wijers (UvA) The Australia Telescope Compact Array (ATCA) automatically triggered on the Swift-BAT detection of the short GRB 230217A (Moss et al., GCN 33339) at 5.5 and 9 GHz using the rapid-response mode under program C3204 (PI: Anderson). ATCA was on target observing GRB 230217A at 22:20:19.9 UT, just 27 minutes post-burst (Moss et al., GCN 33339) and observed for 7 hours. At the position of the proposed X-ray (Capalbi et al., GCN 33348, GCN 33365), radio (Schroeder et al., GCN 33358) and optical (D’Avanzo et al., GCN 33374) counterpart, we detected a source at both 5.5 GHz and 9 GHz with flux densities of 170 +/- 30 and 150 +/- 20 microJy/beam, respectively. Further observations have been taken. We thank the ATCA and the CSIRO Space and Astronomy staff for supporting and maintaining the ATCA rapid-response observing mode.