GRB141207A

This page lists all entries on GRB141207A in GRBweb

Summary Fermi GBM IPN Fermi LAT GCN 17146 GCN 17147 GCN 17149 GCN 17150 GCN 17151 GCN 17152 GCN 17155 GCN 17157 GCN 17193 GCN 17194

Summary table
Variable Value Source
GRB_name_Fermi GRB141207800
T0 19:11:21.100 UTC GCN_circulars,Fermi GBM Det
ra 159.8547° Fermi_LAT
decl 3.7114° Fermi_LAT
pos_error 1.36e-03° Fermi_LAT
T90 20.992 s Fermi_GBM
T90_error 0.572 s Fermi_GBM
T90_start 19:11:22.385 UTC Fermi_GBM
fluence 3.42e-05 erg/cm² Fermi_GBM
fluence_error 1.16e-07 erg/cm² Fermi_GBM
T100 22.277 s
GBM_located False
mjd 56998.79954976852 GCN_circulars,Fermi GBM Det
Fermi GBM table
GRB_name_Fermi GRB141207800
trigger_name bn141207800
ra 159.9900°
decl 3.9100°
pos_error 2.80e+00°
datum 2014-12-07
t_trigger 19:11:21.105 UTC
T90 20.992 s
T90_error 0.572 s
T90_start 19:11:22.385 UTC
fluence 3.42e-05 erg/cm²
fluence_error 1.16e-07 erg/cm²
flux_1024 8.67e+00 erg/cm²/s
flux_1024_error 2.62e-01 erg/cm²/s
flux_1024_time 7.55e+00 erg/cm²/s
flux_64 1.27e+01 erg/cm²/s
flux_64_error 1.20e+00 erg/cm²/s
IPN table
GRB_name GRB141207A
ra 159.9917°
decl 3.9167°
pos_error 2.17e-01°
Fermi LAT table
GRB_name_Fermi GRB141207800
GRB_name GRB141207A
MET 439672293.64
datum 2014-12-07
t_trigger 19:11:30.640 UTC
ra 159.8547°
decl 3.7114°
pos_error 1.36e-03°
GCN 17146 table
GRB_name GRB141207A
GCN_number 17146
Detection_method Fermi LAT Det
t_trigger 19:11:21.100 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 17146 SUBJECT: GRB 141207A: Fermi-LAT Detection DATE: 14/12/08 06:29:49 GMT FROM: Daniel Kocevski at GSFC M. Arimoto (Tokyo Tech), D. Kocevski (NASA/GSFC), R. Desiante (INFN Trieste & Udine University), and M. Axelsson (KTH Royal Institute of Technology, Sweden) report on behalf of the Fermi-LAT team: At 19:11:21.10 on December 7, 2014, Fermi-LAT detected high-energy emission from GRB 141207A, which was also detected by Fermi-GBM (trigger 439672284/141207800). The best LAT on-ground location is found to be (RA, Dec.) = 159.99, +3.91 deg with an error radius of 0.215 deg (90% containment, statistical error only). This position was 59 deg from the LAT boresight at the time of the trigger. The data from the Fermi-LAT show a significant increase in the event rate within 2 degree of the GBM location after the GBM trigger that is spatially and temporally correlated with the GBM emission with high significance. More than 27 photons above 100 MeV and more than 6 photons above 1 GeV are observed within 100 seconds. The highest-energy photon is a ~5 GeV event which is observed ~750 seconds after the GBM trigger. A Swift ToO has been requested for this burst. The Fermi-LAT point of contact for this burst is Makoto Arimoto (arimoto@hp.phys.titech.ac.jp). The Fermi-LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.
GCN 17147 table
GRB_name GRB141207A
GCN_number 17147
Detection_method Swift Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 17147 SUBJECT: GRB 141207A Tiled Swift observations DATE: 14/12/08 08:00:11 GMT FROM: Phil Evans at U of Leicester P. A. Evans (U. Leicester) reports on behalf of the Swift team: Swift has initiated a series of observations, tiled on the sky, of the Fermi/LAT GRB 141207A. Automated analysis of the XRT data will be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00034 Any uncatalogued X-ray sources detected in this analysis will be reported on this website and via GCN COUNTERPART notices. The probability of finding serendipitous sources, unrelated to the Fermi/LAT event is high: any X-ray source considered to be a probable afterglow candidate will be reported via a GCN Circular after manual consideration. Details of the XRT automated analysis methods are detailed in Evans et al. (2007, A&A, 469, 379; and 2009, MNRAS, 397, 1177). This circular is an official product of the Swift-XRT team.
GCN 17149 table
GRB_name GRB141207A
GCN_number 17149
Detection_method Swift-XRT Other
ra 160.0639°
decl 3.8933°
Circular_text TITLE: GCN CIRCULAR NUMBER: 17149 SUBJECT: GRB 141207A: Swift-XRT observations DATE: 14/12/08 15:45:31 GMT FROM: Alex Amaral-Rogers at U.of Leicester A. Amaral-Rogers & P.A. Evans (U. Leicester) report on behalf of the Swift-XRT team: We have observed the area around the Fermi-LAT GRB 141207A (Arimoto et al., GCN Circ. 17146), in 4 XRT fields starting at 07:59:28 UT, 12 hours and 48 minutes after Fermi/LAT detection. With 1.3-1.7 ks per field, we find an uncatalogued X-ray source at a position of RA,Dec=160.0639, 3.8933, which is equivalent to: RA (J2000) = 10h 40m 15.34s Dec (J2000) = +03d 53' 35.9" with an uncertainty of 5.2" (radius, 90% confidence). Although this source is uncatalogued, it is a factor of 3 below the ROSAT limit at this location, with a 0.3-10 keV flux of 1.7e-13 erg/cm^2/s. We expect ~0.9 sources at this flux to be serendipitously present in our XRT observations, therefore we caution that this may not be the afterglow. We cannot currently tell whether the source is fading, but follow-up observations are planned. There is a second uncatalogued X-ray source present in the data, at RA,Dec=159.8172, 4.0930 with an uncertainty of 6.5"; however this source is coincident with the object [VV2006] J103916.6+040536 which SIMBAD classifies as a quasar, thus it is unlikely to be the GRB afterglow. This circular is an official product of the Swift-XRT team.
GCN 17150 table
GRB_name GRB141207A
GCN_number 17150
Detection_method Fermi GBM Det
t_trigger 19:11:21.100 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 17150 SUBJECT: GRB 141207A: Fermi GBM detection DATE: 14/12/08 17:01:18 GMT FROM: Eric Burns at U of Alabama Eric Burns (UAH) report on behalf of the Fermi GBM Team: "At 19:11:21.10 UT on 07 December 2014, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 141207A (trigger 439672284 / 141207800) which was also detected by Fermi LAT (Arimoto et al. 2014, GCN 17146) and observed by Swift (Evans 2014, GCN 17147). The GBM on-ground location is consistent with the LAT/Swift positions. The angle from the Fermi LAT boresight is 59 degrees. The GBM light curve consists of a single pulse with multiple spikes, with a duration (T90) of about 20 s (50-300 keV). The time-averaged spectrum from T0-0.768 s to T0+24.83 s is adequately fit by a power law function with an exponential high-energy cutoff. The power law index is -0.70 +/- 0.02 and the cutoff energy, parameterized as Epeak, is 1080 +/- 56 keV. The event fluence (10-1000 keV) in this time interval is (3.58 +/- 0.04)E-05 erg/cm^2. The 1.024-sec peak photon flux measured starting from T0+7.55 s in the 10-1000 keV band is 8.6 +/- 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 17151 table
GRB_name GRB141207A
GCN_number 17151
Detection_method Swift-UVOT Det
ra 160.0644°
decl 3.8948°
Circular_text TITLE: GCN CIRCULAR NUMBER: 17151 SUBJECT: GRB 141207A: Swift-UVOT Observations DATE: 14/12/08 22:35:11 GMT FROM: Mike Siegel at PSU/Swift MOC GRB 141207A: Swift-UVOT Observations M. H. Siegel (PSU) and A. Amaral-Rogers (U. Leicester) report on behalf of the Swift-UVOT team: We have observed the area around the Fermi-LAT GRB 141207A (Arimoto et al., GCN Circ. 17146), in 4 UVOT fields starting at 07:59:28 UT, 12 hours and 48 minutes after Fermi/LAT detection. There is an optical source at a position of RA,Dec=160.06441, 3.89477, which is equivalent to: RA (J2000) = 10h 40m 15.46s Dec (J2000) = +03d 53' 41.2 with an uncertainty of 0.1 (radius, 90% confidence). This source is 5.6 from the position of the XRT source (Amaral-Rogers and Evans, GCN Circ. 17149) and shows up as a marginal detection in the DSS. It is possibly unrelated to the burst. Follow-up observations will be needed to confirm its nature. The preliminary u magnitude using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) is 19.91+-0.17.
GCN 17152 table
GRB_name GRB141207A
GCN_number 17152
Detection_method Fermi LAT Other
ra 160.0639°
decl 3.8933°
Circular_text TITLE: GCN CIRCULAR NUMBER: 17152 SUBJECT: GRB141207A: Discovery Channel Telescope Optical Observations DATE: 14/12/09 01:41:06 GMT FROM: Vicki Toy at UMD V. Toy (UMD), J. Capone (UMD), E. Troja (NASA-GSFC), S.B. Cenko (NASA-GSFC), A. Cucchiara (NASA-GSFC), A. Kutyrev (NASA-GSFC), and S. Veilleux (UMD) report on behalf of a larger collaboration: We observed the field of the Fermi-LAT GRB141207A (Fermi-GBM trigger 439672284/141207800, Arimoto et al., GCN 17146; Burns et al., GCN 17150) with the Large Monolithic Imager (LMI) on the 4.3m Discovery Channel Telescope (DCT) at Happy Jack, AZ from 2014/12/08 11:08 to 2014/12/08 12:30 UTC (starting 16.0 hours after the Fermi trigger). We imaged 5 fields covering the entire 90% LAT error region. No source is detected at the positions of the two X-ray sources reported by Amaral-Rogers and Evans (GCN 17149). We estimate a 3-sigma upper limit of r > 23.2 (RA,Dec=160.0639,3.8933) and r > 21.3 (RA,Dec=159.8172, 4.0930). We detect the source reported by Siegel and Amaral-Rogers (GCN 17151) with r'=20.09+/-0.04. We note that this coincides with a galactic SDSS source, J104015.45+035341.0. These magnitudes are reported in AB magnitude and are not corrected for Galactic extinction in the direction of the GRB. We thank the staff of the Discovery Channel Telescope for assistance with these observations.
GCN 17155 table
GRB_name GRB141207A
GCN_number 17155
Detection_method Konus-Wind Det
t_trigger 19:11:21.298 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 17155 SUBJECT: Konus-Wind observation of GRB 141207A DATE: 14/12/09 15:28:39 GMT FROM: Valentin Pal'shin at Ioffe Inst S. Golenetskii, R. Aptekar, D. Frederiks, V. Pal'shin, P. Oleynik, M. Ulanov, D. Svinkin, A. Tsvetkova, A. Lysenko, and T. Cline on behalf of the Konus-Wind team, report: The long-duration, hard-spectrum GRB 141207A (Fermi-LAT detection: Arimoto et al., GCN 17146; Fermi-GBM detection: Burns, GCN Circ. 17150) triggered Konus-Wind at T0=69081.298 s UT (19:11:21.298). The burst light curve shows two pulses started at ~T0-2.3 s with a total duration of ~25 s. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB141207_T69081/ As observed by Konus-Wind, the burst had a fluence of 4.87(-0.34,+0.38)x10^-5 erg/cm2, and a 64-ms peak flux, measured from T0+6.224 s, of 9.62(-2.26,+2.27)x10^-6 erg/cm2/s (both in the 20 keV - 10 MeV energy range). The time-integrated spectrum of the burst (measured from T0 to T0+24.832 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 = -0.50 (-0.13,+0.14) and Ep = 723(-72,+87) 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 < -2.6 (chi2 = 104/97 dof) All the quoted errors are at the 90% confidence level. All the quoted values are preliminary.
GCN 17157 table
GRB_name GRB141207A
GCN_number 17157
Detection_method Swift-XRT Other
ra 159.8547°
decl 3.7114°
Circular_text TITLE: GCN CIRCULAR NUMBER: 17157 SUBJECT: GRB 141207A: Swift-XRT afterglow candidate detection DATE: 14/12/10 20:56:07 GMT FROM: Phil Evans at U of Leicester P.A. Evans, K.L. Page & A. Amaral-Rogers (U. Leicester) report on behalf of the Swift-XRT team: Swift has continued to observe the field of the Fermi-LAT GRB 141207A (Arimoto et al., GCN Circ. 17146). The uncatalogued X-ray source reported by Amaral-Rogers & Evans (GCN. Circ 17149) shows no evidence of fading. An additional uncatalogued X-ray source has also been detected at RA,Dec=159.8547, 3.71139 degrees, which is equivalent to: RA (J2000) = 10h 39m 25.13s Dec (J2000) = +03d 42' 41.0" with an uncertainty of 4.9 arcsec (radius, 90% confidence). This source was initially detected with a count-rate of 0.012 +/- 0.003 ct/sec. In a second observation, from T0+191 ks to T0+231 s, the source has faded to a count-rate of 1.0 (+/-0.5) x 10^-3 ct/sec. We therefore suggest that this is likely the afterglow of GRB 141207A. The PC mode spectrum of this source can be fitted with an absorbed power-law with a photon index of 2.1 (+1.5, -0.7). The best-fitting absorption column is 5.2 (+18, -4.8) x 10^21 cm^-2, consistent with the Galactic value of 0.4 x 10^21 cm^-2 (Willingale et al. 2013). A summary of the PC-mode spectrum is thus: Total column: 5.2 (+18, -4.8) x 10^21 cm^-2 Galactic foreground: 3.7 x 10^20 cm^-2 Excess significance: <1.6 sigma Photon index: 2.1 (+1,5, -0.7) This circular is an official product of the Swift-XRT team.
GCN 17193 table
GRB_name GRB141207A
GCN_number 17193
Detection_method Suzaku WAM Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 17193 SUBJECT: GRB 141207A: Suzaku WAM observation of the prompt emission DATE: 14/12/19 04:58:51 GMT FROM: Makoto Tashiro at Saitama U/Swift T. Fujinuma, M. Tashiro, Y. Terada, T. Yasuda, S. Koyama, S. Takeda, T. Nagayoshi, J. Enomoto, S. Nakaya, S. Matsuoka (Saitama U.), M. Yamauchi, N. Ohmori, R. Kinoshita (Univ. of Miyazaki), W. Iwakiri (RIKEN), K. Yamaoka (Nagoya U.), S. Sugita (Ehime U.), Y. Hanabata (ICRR), M. Ohno, T. Kawano, S. Furui, Y. Fukazawa (Hiroshima U.), Y. E. Nakagawa, M. Kokubun, T. Takahashi (ISAS/JAXA), Y. Urata (NCU), K. Nakazawa, K. Makishima (Univ. of Tokyo) on behalf of the Suzaku WAM team, report: The long GRB 141207A(Fermi-LAT Detection: Kocevski et al.,GCN 17146; Swift-XRT observation:Amaral-Rogers et al.,GCN 17149;Fermi GBM dection: Burns et al.,GCN 17150) triggered the Suzaku Wide-band All-sky Monitor (WAM) which covers an energy range of 50 keV - 5 MeV at 19:11:22.452 UT (=T0). The observed light curve shows a multi-peaked structure starting at T0-1s, ending at T0+22s with a duration(T90) of about 20 seconds. The fluence in 100 - 1000 keV was 1.94(+0.10/-0.19)x10^-5 erg/cm^2.The 1-s peak flux measured from T0+6s was 4.74(+0.37/-1.32) photons/cm^2/s in the same energy range. Preliminary result shows that the time-averaged spectrum from T0-1s to T0+22s is well fitted by a power-law with exponential cutoff model: dN/dE ~ E^{-alpha} * exp(-(2-alpha)*E/Epeak) with alpha 1.11(+0.40/-0.48), and Epeak 579(+126/-92) keV (chi^2/d.o.f. = 28.2/25). Due to the brightness of this burst, a 3% systematic error was added for low energy channels. There might be uncertainty since the response for the incident angle of GRB photons to WAM is not reliable. All the quoted errors are at statistical 90% confidence level. The light curves for this burst will be available at: http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html
GCN 17194 table
GRB_name GRB141207A
GCN_number 17194
Detection_method IPN Triangulation
ra 73.6580°
decl 4.9106°
Circular_text TITLE: GCN CIRCULAR NUMBER: 17194 SUBJECT: IPN Triangulation of GRB 141207A DATE: 14/12/19 22:01:24 GMT FROM: Kevin Hurley at UCBerkeley/SSL K. Hurley, on behalf of the IPN, S. Golenetskii, R. Aptekar, V. Pal'shin, D. Frederiks, D. Svinkin, and T. Cline on behalf of the Konus-Wind team, D. M. Smith, J. McTiernan, R. Schwartz, W. Hajdas, and A. Zehnder, on behalf of the RHESSI GRB team, A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo, and C. Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team, K. Yamaoka, M. Ohno, Y. Hanabata, Y. Fukazawa, T. Takahashi, M. Tashiro, Y. Terada, T. Murakami, and K. Makishima on behalf of the Suzaku WAM team, S. Barthelmy, J. Cummings, N. Gehrels, H. Krimm, and D. Palmer, on behalf of the Swift-BAT team, J. Goldsten, on behalf of the MESSENGER NS GRB team, and V. Connaughton, M. S. Briggs, C. Meegan, V. Pelassa, and A. Goldstein, on behalf of the Fermi GBM team, report: GRB 141207A, initially reported by the Fermi LAT and GBM teams (GCN 17146, 17150), was also observed by Konus-Wind, INTEGRAL SPI-ACS, Swift BAT (outside the coded FoV), MESSENGER GRNS, RHESSI, and Suzaku WAM. We have triangulated it to a preliminary, 3 sigma annulus centered at RA(2000), Dec(2000) = 73.658 deg (04h 54m 38s), +23.585 deg (+23d 35'04"), whose radius is 85.031 +/- 0.100 deg. The XRT source reported in Evans, Page, & Amaral-Rogers, GCN 17157, lies 0.003 degrees from the center line of this annulus, supporting the conclusion that this source is the GRB counterpart.