GRB130216A

This page lists all entries on GRB130216A in GRBweb

Summary Fermi GBM IPN Swift GCN 14223 GCN 14224 GCN 14228 GCN 14229 GCN 14230 GCN 14233 GCN 14234 GCN 14236 GCN 14238 GCN 14240 GCN 14241 GCN 14247 GCN 14248 GCN 14254

Summary table
Variable Value Source
GRB_name_Fermi GRB130216927
T0 22:15:21.227 UTC Fermi_GBM
ra 67.9010° Swift
decl 14.6700° Swift
pos_error 7.77e-03° Swift
T90 6.592 s Fermi_GBM
T90_error 0.345 s Fermi_GBM
T90_start 22:15:21.227 UTC Fermi_GBM
fluence 5.92e-06 erg/cm² Fermi_GBM
fluence_error 6.06e-08 erg/cm² Fermi_GBM
T100 9.273 s
GBM_located False
mjd 56339.9273290162 Fermi_GBM
Fermi GBM table
GRB_name_Fermi GRB130216927
trigger_name bn130216927
ra 67.9000°
decl 14.6700°
pos_error 2.64e+00°
datum 2013-02-16
t_trigger 22:15:21.419 UTC
T90 6.592 s
T90_error 0.345 s
T90_start 22:15:21.227 UTC
fluence 5.92e-06 erg/cm²
fluence_error 6.06e-08 erg/cm²
flux_1024 9.20e+00 erg/cm²/s
flux_1024_error 2.90e-01 erg/cm²/s
flux_1024_time 4.48e+00 erg/cm²/s
flux_64 1.26e+01 erg/cm²/s
flux_64_error 1.25e+00 erg/cm²/s
IPN table
GRB_name GRB130216A
ra 67.9000°
decl 14.6667°
pos_error 5.00e-02°
Swift table
GRB_name GRB130216A
t_trigger 22:15:24 UTC
ra 67.9010°
decl 14.6700°
pos_error 7.77e-03°
T90 6.5 s
fluence 3.00e-06 erg/cm²
GCN 14223 table
GRB_name GRB130216A
GCN_number 14223
Detection_method Swift Det
t_trigger 22:15:24 UTC
ra 67.8980°
decl 14.6650°
Circular_text TITLE: GCN CIRCULAR NUMBER: 14223 SUBJECT: GRB 130216A: Swift detection of a burst DATE: 13/02/16 22:33:11 GMT FROM: Scott Barthelmy at NASA/GSFC A. Melandri (INAF-OAB), S. D. Barthelmy (GSFC), D. N. Burrows (PSU), J. R. Cummings (NASA/UMBC), P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC), J. A. Kennea (PSU), B. Sbarufatti (INAF-OAB/PSU) and C. A. Swenson (PSU) report on behalf of the Swift Team: At 22:15:24 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 130216A (trigger=548927). Swift did not slew because of the Moon observing constraint. The BAT on-board calculated location is RA, Dec 67.898, +14.665 which is RA(J2000) = 04h 31m 36s Dec(J2000) = +14d 39' 53" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve shows a small precursor peak at T-6 sec, and then the main peak at T+2 sec with a total duration of about 20 sec. The peak count rate was ~10,000 counts/sec (15-350 keV), at ~2 sec after the trigger. Due to a Moon observing constraint, Swift cannot slew to the BAT position until 13:16 UT on 2013 February 20. There will thus be no XRT or UVOT data for this trigger before this time. Burst Advocate for this burst is A. Melandri (andrea.melandri AT brera.inaf.it). Please contact the BA by email if you require additional information regarding Swift followup of this burst. In extremely urgent cases, after trying the Burst Advocate, you can contact the Swift PI by phone (see Swift TOO web site for information: http://www.swift.psu.edu/too.html.)
GCN 14224 table
GRB_name GRB130216A
GCN_number 14224
Detection_method Swift-BAT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 14224 SUBJECT: GRB 130216A: OSN I-band observations DATE: 13/02/16 23:56:39 GMT FROM: Alberto Castro-Tirado at Inst.de Astro. de Andalucia A. Sota (OSN, IAA-CSIC) and A. J. Castro-Tirado (IAA-CSIC), on behalf of a larger collaboration, report: "Following the detection of GRB 130216A by Swift (Melandri et al. GCN Circ. 14223), we are carrying out I-band observations with the 1.5m OSN telescope at Sierra Nevada Observatory starting 32 min post burst. We do not find any new or varying optical source within the 3 radius Swift/BAT error cirle down to I about 20. Observations are ongoing. This message can be quoted.
GCN 14228 table
GRB_name GRB130216A
GCN_number 14228
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 14228 SUBJECT: GRB 130216A: TAROT La Silla observatory optical observations DATE: 13/02/17 13:53:05 GMT FROM: Bruce Gendre at ASDC Gendre B. (ARTEMIS/IRAP), Klotz A. (IRAP-CNRS-OMP), Boer M. (CNRS-ARTEMIS), Atteia J.L. (IRAP-CNRS-OMP) report: We imaged the field of GRB 130216A detected by SWIFT (trigger 548927, Melandri et al., GCN 14223) with the TAROT robotic telescope (D=25cm) located at the European Southern Observatory, La Silla observatory, Chile. The observations started 1.96h after the GRB trigger. The elevation of the field decreased from 44 degrees above horizon and weather conditions were good. The date of trigger : t0 = 2013-02-16T22:15:24.620 The first image is trailed with a duration of 180.0s (see the description in Klotz et al., 2006, A&A 451, L39). We do not detect any OT with a limiting magnitude of: t0+7048.3s to t0+7228.3s : R > 15.1 The second image is 180.0s exposure in tracking mode: t0+7238.9s to t0+7418.9s : R > 16.2 We co-added a series of exposures: t0+7238.9s to t0+8399.0s : R > 17.7 Magnitudes were estimated with the nearby USNO-B1 stars and are not corrected for galactic dust extinction. N.B. Galactic coordinates are lon=181.8416 lat=-22.2057 and the galactic extinction in R band is 0.3 magnitudes estimated from D. Schlegel et al. 1998ApJ...500..525S. This message may be cited.
GCN 14229 table
GRB_name GRB130216A
GCN_number 14229
Detection_method Swift-BAT Det
ra 67.9010°
decl 14.6700°
Circular_text TITLE: GCN CIRCULAR NUMBER: 14229 SUBJECT: GRB 130216A: Swift-BAT refined analysis DATE: 13/02/17 13:55:37 GMT FROM: Scott Barthelmy at NASA/GSFC S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (GSFC), A. Melandri (INAF-OAB), D. M. Palmer (LANL), T. Sakamoto (AGU), G. Sato (ISAS), M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU) (i.e. the Swift-BAT team): Using the data set from T-240 to T+962 sec from recent telemetry downlinks, we report further analysis of BAT GRB 130216A (trigger #548927) (Melandri, et al., GCN Circ. 14223). The BAT ground-calculated position is RA, Dec = 67.901, 14.670 deg, which is RA(J2000) = 04h 31m 36.2s Dec(J2000) = +14d 40' 10.4" with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment). The partial coding was 54%. The mask-weighted light curve shows two peaks. There is an initial small peak centered on ~T-6 sec with a duration of about 4 sec. The second peak starts at ~T-3 sec, peaks at ~T+2 sec, and ends at ~T+10 sec. T90 (15-350 keV) is 6.5 +- 1.1 sec (estimated error including systematics). The time-averaged spectrum from T-6.16 to T+4.31 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.35 +- 0.04. The fluence in the 15-150 keV band is 3.1 +- 0.1 x 10^-6 erg/cm2. The 1-sec peak photon flux measured from T+1.11 sec in the 15-150 keV band is 6.5 +- 0.3 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/548927/BA/
GCN 14230 table
GRB_name GRB130216A
GCN_number 14230
Detection_method Swift-BAT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 14230 SUBJECT: GRB 130216A: P200 NIR Observations DATE: 13/02/17 14:01:31 GMT FROM: Daniel Perley at Caltech D. A. Perley (Caltech) and S. B. Cenko (UC Berkeley) report: We imaged the BAT position of GRB 130216A (Melandri et al., GCN 14223; Barthelmy et al., GCN 14299) on 2013-02-17 (UT) in Ks-band at two different epochs: 9 one-minute exposures between 02:56 and 03:08 followed by 18 one-minute exposures between 05:46 and 06:13. The FOV covers the entire BAT error circle. No new sources are seen in the field relative to the 2MASS catalog. Digital image subtraction of the two epochs gives a limit on variability of Ks >~ 18.7 mag (5 sigma) between 4.77 and 7.74 hours after the BAT trigger.
GCN 14233 table
GRB_name GRB130216A
GCN_number 14233
Detection_method MITSuME
Circular_text TITLE: GCN CIRCULAR NUMBER: 14233 SUBJECT: GRB 130216A: MITSuME Ishigakijima upper limits DATE: 13/02/18 01:13:02 GMT FROM: Daisuke Kuroda at OAO/NAOJ D. Kuroda (OAO, NAOJ), H. Hanayama, T. Miyaji, J. Watanabe (IAO, NAOJ), K. Yanagisawa (OAO, NAOJ), S.Nagayama (NAOJ), M. Yoshida (Hiroshima), K. Ohta (Kyoto) and N. Kawai(Tokyo Tech) report on behalf of the MITSuME collaboration: We observed the field of GRB 130216A (Melandri et al., GCNC 14223) with the optical three color (g', Rc and Ic) CCD camera attached to the Murikabushi 1m telescope of Ishigakijima Astronomical Observatory. The observation started on 22013-02-17 14:30:07 UT (~16.2 h after the burst). We did not find any new point source within the refined BAT error circle (Barthelmy et al., GCNC 14229) in all the three bands. Three sigma upper limits of the OT are listed below. We used GSC2.3 catalog for flux calibration. T0+[day] MID-UT T-EXP[sec] g' Rc Ic ------------------------------------------------------ 0.69477 14:55:52 1560.0 >20.1 >19.7 >18.9 ------------------------------------------------------ T0+ : Elapsed time after the burst [day] T-EXP: Total Exposure time [sec]
GCN 14234 table
GRB_name GRB130216A
GCN_number 14234
Detection_method Swift-BAT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 14234 SUBJECT: GRB 130216A: possible early detection at 15 GHz DATE: 13/02/18 01:44:14 GMT FROM: Alexander van der Horst at U of Amsterdam T.D. Staley, R.P. Fender (Univ. of Southampton), A.J. van der Horst, A. Rowlinson (Univ. of Amsterdam), D.J. Titterington, K.J.B. Grainge (MRAO) report on behalf of the 4 Pi Sky / AMI team: "We observed the BAT position of GRB 130216A (Melandri et al., GCN 14223; Barthelmy et al., GCN 14229) with the AMI Large Array at 15 GHz on February 16, for one hour starting at 22:28 UT, i.e. 13 minutes after the burst. The beam FWHM covers the entire BAT error circle. We detect a source at >10 sigma significance consistent with the location of the BAT trigger. Further observations are planned to confirm if this is indeed very early radio emission from GRB 130216A. These observations were triggered via the system described in Staley et. al (2013, MNRAS, 428, 3114)."
GCN 14236 table
GRB_name GRB130216A
GCN_number 14236
Detection_method Fermi GBM Det
t_trigger 22:15:21.420 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 14236 SUBJECT: GRB 130216A: Fermi GBM observation DATE: 13/02/18 04:18:14 GMT FROM: Vandiver Chaplin at UAH/Fermi-GBM V.Chaplin (UAH) reports on behalf of the Fermi GBM Team: "At 22:15:21.42 UT on 16 Feb 2013, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 130216A (trigger 382745724 / 130216927), which was also detected by the Swift/BAT (Melandri et al. 2013, GCN 14223). The GBM on-ground location is consistent with the Swift position. The angle from the Fermi LAT boresight is 71 degrees. The GBM light curve consists of two peaks at T0 and T0+4 s, with a duration (T90) of about 7 s (50-300 keV). The time-averaged spectrum from T0-0 s to T0+6.7 s is best fit by a Band function with Epeak = 152 +/- 13 keV, alpha = -0.7 +/- 0.1, and beta = -2.6 +/- 0.3. The event fluence (10-1000 keV) in this time interval is (6.231 +/- 0.255)E-06 erg/cm^2. The 1-sec peak photon flux measured starting from T0+4.5 s in the 10-1000 keV band is 9.2 +/- 0.3 ph/s/cm^2. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog."
GCN 14238 table
GRB_name GRB130216A
GCN_number 14238
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 14238 SUBJECT: GRB 130216A: MASTER-Net early observations DATE: 13/02/18 11:19:43 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs E. Gorbovskoy, V. Lipunov, V.Kornilov, D.Kuvshinov, A.Belinski, N.Tyurina, N.Shatskiy, P.Balanutsa, D.Zimnukhov, A.Kuznetsov, V.V.Chazov, D.Denisenko, A.Sankovich Sternberg Astronomical Institute, Moscow State University A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Sennik Kislovodsk Solar Station of the Pulkovo Observatory V.Yurkov, Yu.Sergienko, D.Varda, E.Sinyakov Blagoveschensk Educational State University, Blagoveschensk K.Ivanov, S.Yazev, N.M.Budnev, O.Gres, O.Chuvalaev, V.A.Poleshchuk Irkutsk State University V.Krushinski, I.Zalozhnih, A. Popov Ural Federal University, Kourovka Hugo Levato and Carlos Saffe Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE) Claudio Mallamaci, Carlos Lopez and Federico Podest Observatorio Astronomico Felix Aguilar (OAFA) MASTER-VWF robotic telescope (MASTER-Net: http://observ.pereplet.ru) in Kislovodsk was pointed to the GRB130216A 15 sec after notice time and 31 sec after GRB time at 2013-02-16 22:15:52.273 UT using FERMI coordinates (V.Chaplin et. al. GCN14236). We observ SWIFT error-box by very wide field cameras (FOV=400 sq. deg. d=8.2 cm) and haven't found optical transient on images with 5-sigma upper limit has been about 8 mag. MASTER II robotic telescope located in Kislovodsk was pointed to the GRB130216A 23 sec after notice time and 582 sec after GRB time at 2013-02-16 22:25:06.231 UT. On our first (120s exposure) set we haven't found optical transient within SWIFT error-box (A. Melandri et. al. GCN14223). The 5-sigma upper limit has been about 14.0 mag All bservations were made on high (z>85 deg.) zenith distances and in bad weather condition . The message may be cited.
GCN 14240 table
GRB_name GRB130216A
GCN_number 14240
Detection_method Swift-BAT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 14240 SUBJECT: GRB 130216A: Further Swift-BAT refined analysis DATE: 13/02/18 14:57:39 GMT FROM: Takanori Sakamoto at AGU T. Sakamoto (AGU) and S. D. Barthelmy (GSFC) reports on behalf of the Swift-BAT team: Due to a issue in our automatic pipeline analysis script of the BAT data, we only reported the result based on a simple power-law fit at the spectral analysis section of the BAT refined circular (GCN Circ. 14229). However, this GRB had an enough signal-to-noise ratio in the spectrum to obtain Epeak by the BAT data alone. Therefore, we would like to update the spectral analysis part of the circular to: "The time-averaged spectrum from T-6.16 to T+4.31 sec is best fit by a power law with an exponential cutoff. This fit gives a photon index 0.80 +- 0.20, and Epeak of 123.7 +- 27.1 keV (chi squared 47.17 for 56 d.o.f.). For this model the total fluence in the 15-150 keV band is 3.0 +- 0.1 x 10^-06 erg/cm2 and the 1-sec peak flux measured from T+1.11 sec in the 15-150 keV band is 6.5 +- 0.3 ph/cm2/sec. A fit to a simple power law gives a photon index of 1.35 +- 0.04 (chi squared 72.98 for 57 d.o.f.). All the quoted errors are at the 90% confidence level. " We want to thank Alex Kann for pointing this out.
GCN 14241 table
GRB_name GRB130216A
GCN_number 14241
Detection_method Swift-BAT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 14241 SUBJECT: GRB 130216A: Further Swift-BAT refined analysis DATE: 13/02/19 03:08:35 GMT FROM: Takanori Sakamoto at AGU T. Sakamoto (AGU) and S. D. Barthelmy (GSFC) reports on behalf of the Swift-BAT team: Due to a issue in our automatic pipeline analysis script of the BAT data, we only reported the result based on a simple power-law fit at the spectral analysis section of the BAT refined circular (GCN Circ. 14229). However, this GRB had an enough signal-to-noise ratio in the spectrum to obtain Epeak by the BAT data alone. Therefore, we would like to update the spectral analysis part of the circular to: "The time-averaged spectrum from T-6.16 to T+4.31 sec is best fit by a power law with an exponential cutoff. This fit gives a photon index 0.80 +- 0.20, and Epeak of 123.7 +- 27.1 keV (chi squared 47.17 for 56 d.o.f.). For this model the total fluence in the 15-150 keV band is 3.0 +- 0.1 x 10^-06 erg/cm2 and the 1-sec peak flux measured from T+1.11 sec in the 15-150 keV band is 6.5 +- 0.3 ph/cm2/sec. A fit to a simple power law gives a photon index of 1.35 +- 0.04 (chi squared 72.98 for 57 d.o.f.). All the quoted errors are at the 90% confidence level. " We want to thank Alex Kann for pointing this out.
GCN 14247 table
GRB_name GRB130216A
GCN_number 14247
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 14247 SUBJECT: GRB 130216A: Swift/XRT observations DATE: 13/02/21 18:03:58 GMT FROM: Andrea Melandri at INAF-OAB A. Melandri (INAF-OAB) reports on behalf of the Swift team: We have analysed 8 ks of XRT data for GRB 130216A (Melandri et al., GCN Circ. 14223), from 317.7 ks to 347.4 ks after the BAT trigger. The data are all in Photon Counting (PC) mode. No X-ray afterglow is detected inside the refined BAT error circle (Sakamoto & Berthelmy, GCN Circ. 14240). The 3sigma upper limit is of 4.7 x 10^-3 cts/s. This corresponds to an observed 0.3-10 keV flux of 1.8 x 10^-13 erg/ cm2/s (assuming a typical GRB spectrum with photon spectral index of 2). If we consider the Galactic absorption in this direction (1.5 x 10^21 cm^-2; Kalberla et al. 2005) this corresponds to an unabsorbed flux of 2.4 x 10^-13 erg/cm2/s.
GCN 14248 table
GRB_name GRB130216A
GCN_number 14248
Detection_method Swift-BAT Det
ra 67.8917°
decl 14.6600°
Circular_text TITLE: GCN CIRCULAR NUMBER: 14248 SUBJECT: GRB 130216A: possible radio counterpart is steady field source DATE: 13/02/21 20:15:01 GMT FROM: Alexander van der Horst at U of Amsterdam A.J. van der Horst (U. of Amsterdam), R.D.E. Saunders (MRAO), K.J.B. Grainge (U. of Manchester), R.P. Fender, T.D. Staley (U. of Southampton), A. Rowlinson, R.A.M.J. Wijers (U. of Amsterdam) report on behalf of a large collaboration: "We have observed the Swift/BAT error circle of GRB 130216A (GCN 14229) at multiple epochs with the AMI Large Array and the Westerbork Synthesis Radio Telescope, at 15 and 4.8 GHz respectively. The radio source we reported in GCN 14234 was clearly detected at all epochs at this position: RA, Dec (J2000) = 04:31:34, +14:39:36 (+/- 2 arcsec). Our flux density measurements are given in the table below. Epoch Delta T Freq. Flux density ============== ======== ======= ============ Feb 16.94-16.98 0.03 days 15 GHz 0.78 +/- 0.08 mJy Feb 18.55-19.01 1.86 days 15 GHz 0.80 +/- 0.04 mJy Feb 19.51-19.59 2.62 days 4.8 GHz 1.11 +/- 0.09 mJy Feb 19.86-19.99 3.00 days 4.8 GHz 1.15 +/- 0.06 mJy Feb 20.50-20.64 3.64 days 4.8 GHz 0.92 +/- 0.07 mJy Feb 20.91-20.99 4.02 days 4.8 GHz 1.09 +/- 0.08 mJy The source is constant in flux between our observing epochs and also within the 11-hour AMI observation. The spectral index between 4.8 and 15 GHz is -0.3. There is no significant polarization detected in the combined Westerbork data, with a 3-sigma upper limit of 15%. From these observations we conclude that this source is not the counterpart of GRB 130216A, but possibly a radio galaxy or AGN. Based on the combined 9C and 10C Surveys of Radio Sources (see, e.g., Davies et al. 2011, MNRAS, 415, 2708), we estimate that the probability for a source as bright or brighter than the one we detect to occur by chance inside the Swift/BAT error circle is 2%. We would like to thank the AMI and WSRT staff for scheduling and obtaining these observations."
GCN 14254 table
GRB_name GRB130216A
GCN_number 14254
Detection_method Swift-UVOT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 14254 SUBJECT: GRB 130216A: Swift/UVOT Upper Limit DATE: 13/03/01 22:02:14 GMT FROM: Frank Marshall at GSFC F. E. Marshall (NASA/GSFC) and A. Melandri (INAF-OAB) report on behalf of the Swift/UVOT team: The Swift/UVOT began observations of the field of GRB 130216A 3.67 days after the BAT trigger (Melandri et al., GCN Circ. 14223). The observations were delayed because of an observing constraint due to the Moon. No new source is seen inside the refined BAT error circle (Barthelmy et al. GCN Circ. 14229). The preliminary 3-sigma upper limit using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag w1 317224 346946 7959 >22.2 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.49 in the direction of the burst (Schlegel et al. 1998).