GRB141220A

This page lists all entries on GRB141220A in GRBweb

Summary Fermi GBM IPN Swift GCN 17196 GCN 17197 GCN 17198 GCN 17199 GCN 17200 GCN 17201 GCN 17202 GCN 17203 GCN 17204 GCN 17205 GCN 17207 GCN 17215 GCN 17653

Summary table
Variable Value Source
GRB_name_Fermi GRB141220252
T0 6:02:51.590 UTC Fermi_GBM
ra 195.0657° Swift
decl 32.1464° Swift
pos_error 5.82e-05° Swift
T90 7.616 s Fermi_GBM
T90_error 0.923 s Fermi_GBM
T90_start 6:02:51.590 UTC Fermi_GBM
fluence 5.34e-06 erg/cm² Fermi_GBM
fluence_error 3.51e-08 erg/cm² Fermi_GBM
redshift 1.3195 GCN_circulars,Other
T100 7.62 s
GBM_located False
mjd 57011.25198599537 Fermi_GBM
Fermi GBM table
GRB_name_Fermi GRB141220252
trigger_name bn141220252
ra 195.0671°
decl 32.1336°
pos_error 2.92e+00°
datum 2014-12-20
t_trigger 6:02:52.486 UTC
T90 7.616 s
T90_error 0.923 s
T90_start 6:02:51.590 UTC
fluence 5.34e-06 erg/cm²
fluence_error 3.51e-08 erg/cm²
flux_1024 1.20e+01 erg/cm²/s
flux_1024_error 3.03e-01 erg/cm²/s
flux_1024_time 1.28e-01 erg/cm²/s
flux_64 1.61e+01 erg/cm²/s
flux_64_error 1.48e+00 erg/cm²/s
IPN table
GRB_name GRB141220A
ra 195.0500°
decl 32.1500°
pos_error 5.00e-02°
redshift 1.3195
Swift table
GRB_name GRB141220A
t_trigger 6:02:52 UTC
ra 195.0657°
decl 32.1464°
pos_error 5.82e-05°
T90 7.21 s
fluence 2.60e-06 erg/cm²
redshift 1.3195
GCN 17196 table
GRB_name GRB141220A
GCN_number 17196
Detection_method Swift Det
t_trigger 6:02:52 UTC
ra 195.0500°
decl 32.1440°
Circular_text TITLE: GCN CIRCULAR NUMBER: 17196 SUBJECT: GRB 141220A: Swift detection of a burst with an optical afterglow DATE: 14/12/20 06:23:27 GMT FROM: David Palmer at LANL J. R. Cummings (NASA/UMBC), V. D'Elia (ASDC), N. Gehrels (NASA/GSFC), A. Y. Lien (GSFC/UMBC), D. M. Palmer (LANL), B. Sbarufatti (INAF-OAB/PSU) and M. H. Siegel (PSU) report on behalf of the Swift Team: At 06:02:52 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 141220A (trigger=621915). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 195.050, +32.144 which is RA(J2000) = 13h 00m 12s Dec(J2000) = +32d 08' 37" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a double-peaked structure with a duration of about 10 sec. The peak count rate was ~5000 counts/sec (15-350 keV), at ~0 sec after the trigger. The XRT began observing the field at 06:04:31.8 UT, 99.2 seconds after the BAT trigger. The position determined from promptly downlinked data differs significantly from the on-board position, suggesting that the XRT may have centroided on a cosmic ray; the initial XRT position notice should be treated with caution. Using promptly downlinked data we find a fading, uncatalogued X-ray source located at RA, Dec 195.06735, 32.13361 which is equivalent to: RA(J2000) = 13h 00m 16.16s Dec(J2000) = +32d 08' 01.0" with an uncertainty of 3.7 arcseconds (radius, 90% containment). This location is 64 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 http://www.swift.ac.uk/sper. A power-law fit to a spectrum formed from promptly downlinked event data gives a column density consistent with the Galactic value of 1.33 x 10^20 cm^-2 (Willingale et al. 2013). UVOT took a finding chart exposure of 150 seconds with the White filter starting 105 seconds after the BAT trigger. The 2.7'x2.7' sub-image shows a likely optical afterglow near the XRT position. We are unable to confirm or measure a magnitude due to the loss of star tracker lock. We note that the XRT position may have an additional error of order 10 arcseconds due to star tracker lock. A more accurate location will be generated when the full dataset is available. Burst Advocate for this burst is J. R. Cummings (jayc AT milkyway.gsfc.nasa.gov). 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 17197 table
GRB_name GRB141220A
GCN_number 17197
Detection_method Swift Other
ra 195.0657°
decl 32.1461°
Circular_text TITLE: GCN CIRCULAR NUMBER: 17197 SUBJECT: GRB141220A: 1.23m CAHA I-band observations DATE: 14/12/20 07:52:06 GMT FROM: Javier Gorosabel at IAA-CSIC J. Gorosabel (IAA-CSIC/UPV-EHU), S. Hellmich (DLR), A. de Ugarte Postigo (IAA-CSIC), S. Mottola (DLR), C. Thoene (IAA-CSIC), report on behalf of a larger collaboration: We observed the field of GRB 141220A with the 1.23m CAHA in the I-band starting ~8 min post burst. A bright afterglow is detected at RA(J2000)=13:00:15.76, DEC(J2000)=32:08:46:4 (+/-0.8"). We note an important discrepancy with the initial position reported by Swift.
GCN 17198 table
GRB_name GRB141220A
GCN_number 17198
Detection_method Other
redshift 1.3195
Circular_text TITLE: GCN CIRCULAR NUMBER: 17198 SUBJECT: GRB 141220A: Redshift from OSIRIS at the 10.4m GTC DATE: 14/12/20 07:53:28 GMT FROM: Antonio de Ugarte Postigo at IAA-CSIC A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), C.C. Thoene (IAA-CSIC), J. Gorosabel (UPV, IAA-CSIC), N. Tanvir (U. Leicester), J.P.U. Fynbo (DARK/NBI), P. Pesev (GRANTECAN), G. Gomez Velarde (GRANTECAN), and D. Perez Valladares (GRANTECAN) report on behalf of a larger collaboration We observed the afterglow of GRB141220A (Cummings et al. GCN 17196, Gorosabel et al. GCN 17197) with OSIRIS at the 10.4m GTC. Observations began at 6:45 UT (50 min after the burst). In a first 600 s spectrum obtained with grism R1000B covering from 3750 to 7800 A we detect absorption features of AlII, FeII, MgII, MgI, at a redshift of 1.3195, including several absorptions of FeII* which make it very likely the redshift of the GRB. We also detect two MgII intervening systems at redshifts of 1.280 and 0.527.
GCN 17199 table
GRB_name GRB141220A
GCN_number 17199
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 17199 SUBJECT: GRB 141220A: LT optical afterglow observations DATE: 14/12/20 08:32:50 GMT FROM: Cristiano Guidorzi at Ferrara U,Italy C. Guidorzi (U. Ferrara), A. Gomboc (U. Ljubljana) on behalf of a larger collaboration report: The 2-m Liverpool Telescope automatically began observing Swift GRB 141220A (Cummings et al. GCN 17196) on Dec 20 at 06:04:57 UT (125 sec after the burst trigger). The robotic LT-TRAP pipeline identified the optical afterglow at the position reported by Gorosabel et al. (GCN 17197) with r=18.6 +- 0.1 mag at 34 minutes after the GRB, calibrated against nearby SDSS-R stars.
GCN 17200 table
GRB_name GRB141220A
GCN_number 17200
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 17200 SUBJECT: GRB 141220A: Photometry from OSIRIS/GTC DATE: 14/12/20 11:08:46 GMT FROM: Antonio de Ugarte Postigo at IAA-CSIC A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), C.C. Thoene (IAA-CSIC), J. Gorosabel (IAA-CSIC, UPV-EHU), N.R. Tanvir (U. Leicester), J.P.U. Fynbo (DARK/NBI), P. Pesev (GRANTECAN), G. Gomez Velarde (GRANTECAN), and D. Perez Valladares (GRANTECAN) report on behalf of a larger collaboration: Photometric observations of the afterglow of GRB 141220A (Cummings et al. GCN 17196, Gorosabel et al. GCN 17197, de Ugarte Postigo et al. GCN 17198) were obtained by OSIRIS/GTC starting 20.6 min after the GRB onset. The afterglow was detected at r' = 18.11+/-0.05 mag in the first image and had decayed by 0.6+/-0.1 mag 38.7 min after the burst. Using our photometric data we derive a decay slope of alpha=0.96+/-0.11 (where F_nu ~ t^-alpha). These results are consistent with the observations reported by Guidorzi et al. (GCN 17199). Our photometry was performed using SDSS stars as reference. We encourage further observations and in particular spectroscopy of the afterglow, in particular to check for possible variability of the FeII* features between 5400 and 6100 A.
GCN 17201 table
GRB_name GRB141220A
GCN_number 17201
Detection_method Swift-UVOT Det
ra 195.0657°
decl 32.1464°
Circular_text TITLE: GCN CIRCULAR NUMBER: 17201 SUBJECT: GRB 141220A: Swift/UVOT Detection DATE: 14/12/20 16:08:45 GMT FROM: Frank Marshall at GSFC F. E. Marshall (NASA/GSFC) and J. R. Cummings (NASA/UMBC) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 141220A 597 s after the BAT trigger (Cummings et al., GCN Circ. 17196). There were also other exposures when the spacecraft attitude was not stable. A source consistent with the optical position Gorosabel et al. (GCN Circ. 17197) is detected in the initial UVOT exposures. The preliminary UVOT position is: RA (J2000) = 13:00:15.76 = 195.06565 (deg.) Dec (J2000) = +32:08:47.0 = 32.14639 (deg.) with an estimated uncertainty of 0.45 arc sec. (radius, 90% confidence). Preliminary detections 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 597 617 19 17.30 0.07 v 647 839 39 17.65 0.16 b 573 593 20 17.58 0.13 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.01 in the direction of the burst (Schlegel et al. 1998).
GCN 17202 table
GRB_name GRB141220A
GCN_number 17202
Detection_method Swift-BAT Det
ra 195.0580°
decl 32.1460°
Circular_text TITLE: GCN CIRCULAR NUMBER: 17202 SUBJECT: GRB 141220A: Swift-BAT refined analysis DATE: 14/12/20 16:48:39 GMT FROM: Jay R. Cummings at NASA/GSFC/Swift M. Stamatikos (OSU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings, N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU), J. Tueller (GSFC), T. N. Ukwatta (LANL) (i.e. the Swift-BAT team): Using the data set from T-61 to T+243 sec from the recent telemetry downlink, we report further analysis of BAT GRB 141220A (trigger #621915) (Cummings, et al., GCN Circ. 17196). The BAT ground-calculated position is RA, Dec = 195.058, 32.146 deg which is: RA(J2000) = 13h 00m 14.0s Dec(J2000) = +32d 08' 46.4" with an uncertainty of 1.2 arcmin, (radius, sys+stat, 90% containment). The partial coding was 19%. The mask-weighted light curve shows two peaks at about T+1 and T+3 seconds, with an exponential decline noticeable out to ~T+20 seconds. T90 (15-350 keV) is 7.21 +- 0.48 sec (estimated error including systematics). The time-averaged spectrum from T-0.91 to T+7.30 sec is best fit by a power law with an exponential cutoff. This fit gives a photon index 0.62 +- 0.38, and Epeak of 117.4 +- 45.1 keV (chi squared 56.50 for 56 d.o.f.). For this model the total fluence in the 15-150 keV band is 2.6 +- 0.1 x 10^-06 erg/cm2 and the 1-sec peak flux measured from T-0.13 sec in the 15-150 keV band is 8.9 +- 0.7 ph/cm2/sec. A fit to a simple power law gives a photon index of 1.30 +- 0.08 (chi squared 67.35 for 57 d.o.f.). 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/621915/BA/
GCN 17203 table
GRB_name GRB141220A
GCN_number 17203
Detection_method Swift-XRT Other
ra 195.0653°
decl 32.1466°
Circular_text TITLE: GCN CIRCULAR NUMBER: 17203 SUBJECT: GRB 141220A: Swift-XRT refined Analysis DATE: 14/12/20 20:23:04 GMT FROM: Phil Evans at U of Leicester B.P. Gompertz (U. Leicester), M. de Pasquale (INAF-IASFPA), A. Maselli (INAF-IASFPA), A. Melandri (INAF-OAB), M.C. Stroh (PSU), D.N. Burrows (PSU), J.A. Kennea (PSU), J.P. Osborne (U. Leicester), K.L. Page (U. Leicester) and J.R. Cummings report on behalf of the Swift-XRT team: We have analysed 6.8 ks of XRT data for GRB 141220A (Cummings et al. GCN Circ. 17196), from 87 s to 36.3 ks after the BAT trigger. The data comprise 42 s in Windowed Timing (WT) mode (the first 8 s were taken while Swift was slewing) with the remainder in Photon Counting (PC) mode. The refined XRT position is RA, Dec = 195.0653, +32.1466 which is equivalent to: RA (J2000): 13 00 15.66 Dec(J2000): +32 08 47.9 with an uncertainty of 3.6 arcsec (radius, 90% confidence). The late-time light curve (from T0+5.6 ks) can be modelled with a power-law decay with a decay index of alpha=1.38 (+0.26, -0.23). A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 1.81 (+0.21, -0.20). The best-fitting absorption column is 8.3 (+5.9, -5.1) x 10^20 cm^-2, in excess of the Galactic value of 1.3 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 3.7 x 10^-11 (4.2 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 8.3 (+5.9, -5.1) x 10^20 cm^-2 Galactic foreground: 1.3 x 10^20 cm^-2 Excess significance: 2.3 sigma Photon index: 1.81 (+0.21, -0.20) If the light curve continues to decay with a power-law decay index of 1.38, the count rate at T+24 hours will be 2.6 x 10^-3 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 9.5 x 10^-14 (1.1 x 10^-13) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00621915. This circular is an official product of the Swift-XRT team.
GCN 17204 table
GRB_name GRB141220A
GCN_number 17204
Detection_method MITSuME
Circular_text TITLE: GCN CIRCULAR NUMBER: 17204 SUBJECT: GRB 141220A: MITSuME Okayama upper limits DATE: 14/12/20 23:57:05 GMT FROM: Daisuke Kuroda at OAO/NAOJ D. Kuroda, K. Yanagisawa, Y. Shimizu, H. Toda (OAO, NAOJ), S. Nagayama (NAOJ), M. Yoshida (Hiroshima), K. Ohta (Kyoto) and N. Kawai(Tokyo Tech) report on behalf of MITSuME and OISTER collaboration: We observed the field of GRB 141220A (Cummings et al., GCNC 17196) with the optical three color (g', Rc and Ic) CCD camera attached to the MITSuME 50cm telescope of Okayama Astrophysical Observatory. The observation started on 2014-12-20 16:27:31 UT (~10.4 h after the burst) We could not detect the previously reported afterglow (Cummings et al., GCNC 17196; Gorosabel et al., GCNC 17197; de Ugarte Postigo et al., GCNC 17198) in all the three bands. Three sigma upper limits of the OT are listed below. We used SDSS-DR7 catalog for flux calibration. #T0+[day] MID-UT T-EXP[sec] g' Rc Ic ----------------------------------------------------- 0.47547 17:27:32 5940.0 >19.8 >19.9 >19.0 ----------------------------------------------------- T0+ : Elapsed time after the burst [day] T-EXP: Total Exposure time [sec]
GCN 17205 table
GRB_name GRB141220A
GCN_number 17205
Detection_method Fermi GBM Det
t_trigger 6:02:52.490 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 17205 SUBJECT: GRB 141220A: Fermi GBM observation DATE: 14/12/21 04:24:48 GMT FROM: Hoi-Fung Yu at MPE H.-F. Yu (MPE) reports on behalf of the Fermi GBM Team: "At 06:02:52.49 UT on 20 Dec 2014, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 141220A (trigger 141220252/ 141220252), which was also detected by Swift (Cummings et al. 2014, GCN 17196). The GBM on-ground location, using the Fermi GBM trigger data, is consistent with the Swift location. The trigger resulted in an Autonomous Repoint Request (ARR) that was accepted and the spacecraft slewed to the GBM in-flight location. The angle from the Fermi LAT boresight is about 47 degrees. The GBM light curve consists of two main pulses with a duration (T90) of about 7.6 s (50-300 keV). The time-averaged spectrum from T0-1.920 s to T0+8.320 s is best fit by a power law function with an exponential high-energy cutoff. The power law index is -0.80 +/- 0.05 and the cutoff energy, parameterized as Epeak, is 180 +/- 9 keV. The event fluence (8-1000 keV) in this time interval is (5.23 +/- 0.15)E-06 erg/cm^2. The 1.024-sec peak photon flux measured starting from T0+0.128 s in the 8-1000 keV band is 12.0 +/- 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 17207 table
GRB_name GRB141220A
GCN_number 17207
Detection_method Konus-Wind Det
t_trigger 6:02:51.666 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 17207 SUBJECT: Konus-Wind observation of GRB 141220A DATE: 14/12/21 12:57:37 GMT FROM: Dmitry Frederiks at Ioffe Institute S. Golenetskii, R.Aptekar, D. Frederiks, V. Pal'shin, P. Oleynik, M. Ulanov, D. Svinkin, A. Tsvetkova, A.Lyssenko, and T. Cline on behalf of the Konus-Wind team, report: The long-duration GRB 141220A (Swift-BAT trigger #621915: Cummings et al., GCN 17196; Stamatikos et al., GCN 17202; Fermi-GBM observation: Yu, GCN 17205) triggered Konus-Wind at T0=21771.666 s UT (06:02:51.666). The KW light curve shows a single emission episode lasting from ~T0-0.5 s to ~T0+7.5 s. The emission in this episode is visible up to ~4 MeV. As observed by Konus-Wind, the burst had a fluence of 4.7(-0.4,+0.5)x10^-6 erg/cm2, and a 64-ms peak flux, measured from T0, of 2.2(-0.4,+0.5)x10^-6 erg/cm2/s (both in the 20 keV - 10 MeV energy range). The time-averaged spectrum (measured from T0 to T0+8.448 s) is best fit in the 20 keV - 15 MeV range by the cutoff power law with the following model parameters: the photon index alpha = -0.55(-0.26,+0.30), and the peak energy Ep = 139(-14,+18) keV, chi2 = 83/98 dof. Fitting this spectrum with the Band model yields the same values of alpha and Ep and an upper limit on beta of -2.0 The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB141220_T21771/ All the quoted errors are at the 90% confidence level. All the quoted values are preliminary.
GCN 17215 table
GRB_name GRB141220A
GCN_number 17215
Detection_method MITSuME
Circular_text TITLE: GCN CIRCULAR NUMBER: 17215 SUBJECT: GRB 141220A: MITSuME Akeno upper limits DATE: 14/12/22 07:06:48 GMT FROM: Taketoshi Yoshii at Tokyo Tech Y. Yano, T. Yoshii, Y. Saito, Y. Tachibana, H. Ohuchi, S. Kurita, Y. Ono, T. Fujiwara, Y. Yatsu, and N. Kawai (Tokyo Tech) report on behalf of the MITSuME collaboration: We observed the field of GRB 141220A (J. R. Cummings et al., GCN Circular #17196) with the optical three color (g', Rc, and Ic) CCD cameras attached to the MITSuME 50 cm telescope of Akeno Observatory, Yamanashi, Japan. The observation started on 2014-12-20 15:16:22 UT (~9.2 h after the burst). We did not find any new point source within the refined XRT error circle (B. P. Gompertz., GCN Circular #17203) in all the three bands. The measured magnitudes are listed below. T0+[sec] MID-UT T-EXP[sec] g' Rc Ic ----------------------------------------------------------------------------- 36707 18:07:29 8460 >21.4 >20.8 >20.4 ----------------------------------------------------------------------------- T0+ : Elapsed time after the burst T-EXP: Total Exposure time We used GSC2.3 catalog for flux calibration.
GCN 17653 table
GRB_name GRB141220A
GCN_number 17653
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 17653 SUBJECT: GRB 141220A: GMG observation limit DATE: 15/03/29 11:09:44 GMT FROM: Jirong Mao at Yunnan Obs J. Mao, B. Lun and J.-M. Bai (YNAO) report: We observed the field of GRB 141220A (Cummings et al., GCN 17196) with the 2.4-meter optical telescope at Gao-Mei-Gu (GMG) station of Yunnan Observatory. Observations began from UT 22:28:38.1 20, Dec., 2014 (about 18.4 hours after the trigger). We did not detect the optical counterpart down to a limit of r'~21.0. We thank Dr. A., de Ugarte Postigo for his kind suggestion and disucssion. J. Mao apologizes for this very later GCN circular submission.