GRB120711A

This page lists all entries on GRB120711A in GRBweb

Summary Fermi GBM IPN Fermi LAT GCN 13430 GCN 13432 GCN 13433 GCN 13434 GCN 13435 GCN 13436 GCN 13437 GCN 13438 GCN 13439 GCN 13441 GCN 13442 GCN 13443 GCN 13444 GCN 13446 GCN 13448 GCN 13451 GCN 13452 GCN 13463 GCN 13468 GCN 13485 GCN 13513

Summary table
Variable Value Source
GRB_name_Fermi GRB120711115
T0 2:44:48 UTC GCN_circulars,INTEGRAL
ra 94.6785° Fermi_LAT
decl -70.9991° Fermi_LAT
pos_error 0.00e+00° Fermi_LAT
T90 44.033 s Fermi_GBM
T90_error 0.724 s Fermi_GBM
T90_start 2:45:55.759 UTC Fermi_GBM
fluence 1.94e-04 erg/cm² Fermi_GBM
fluence_error 2.28e-07 erg/cm² Fermi_GBM
redshift 1.8037
T100 111.792 s
GBM_located False
mjd 56119.11444444444 GCN_circulars,INTEGRAL
Fermi GBM table
GRB_name_Fermi GRB120711115
trigger_name bn120711115
ra 94.6900°
decl -71.0000°
pos_error 3.53e+00°
datum 2012-07-11
t_trigger 2:44:53.294 UTC
T90 44.033 s
T90_error 0.724 s
T90_start 2:45:55.759 UTC
fluence 1.94e-04 erg/cm²
fluence_error 2.28e-07 erg/cm²
flux_1024 2.67e+01 erg/cm²/s
flux_1024_error 5.82e-01 erg/cm²/s
flux_1024_time 9.49e+01 erg/cm²/s
flux_64 4.47e+01 erg/cm²/s
flux_64_error 2.81e+00 erg/cm²/s
IPN table
GRB_name GRB120711A
ra 94.7042°
decl -71.0167°
pos_error 5.00e-02°
redshift 1.4050
Fermi LAT table
GRB_name_Fermi GRB120711115
GRB_name GRB120711A
MET 363667496.0
datum 2012-07-11
t_trigger 2:44:53 UTC
ra 94.6785°
decl -70.9991°
pos_error 0.00e+00°
GCN 13430 table
GRB_name GRB120711A
GCN_number 13430
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 13430 SUBJECT: Skynet/PROMPT Observations of GRB120711A DATE: 12/07/11 03:23:16 GMT FROM: Aaron LaCluyze at U.North Carolina A. Lacluyze, J. Haislip, K. Ivarsen, D. Reichart, J. Moore, H. T. Cromartie, R. Egger, A. Foster, N. Frank, M. Nysewander, A. Oza, E. Speckhard, A.Trotter, and J. A. Crain report: Skynet observed the field of GRB12711 (INTEGRAL trigger 6599) in B, V, and R starting 37 seconds after the burst. Although no afterglow was detected in the initial exposures, a transient source was detected at 06:18:42.839 -70:59:56.78 (J2000). The source rapidly brightened, peaking at roughly 112 seconds after the trigger. Preliminary peak magnitudes, calibrated to ~5 UNSO B1.0 stars are as follows: Time Tel Filt Mag 1sigERR 112 P4 R 12.117 0.008 113 P1 V 12.593 0.014 116 P3 B 14.061 0.014 The post-peak temporal index is estimated to be -2.1, suggesting a reverse shock. Further observations are ongoing.
GCN 13432 table
GRB_name GRB120711A
GCN_number 13432
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 13432 SUBJECT: GRB 120711A: ROTSE-III confirm of Optical Counterpart DATE: 12/07/11 03:43:34 GMT FROM: Weikang Zheng at U.of Michigan W. Zheng (U Mich), report on behalf of the ROTSE collaboration: ROTSE-IIIc, located at the H.E.S.S. site at Mt. Gamsberg, Namibia, responded to GRB 120711A (Integral trigger 6599). The first image was at 02:45:54.4 UT, 59.1 s after the burst (5.4 s after the GCN notice time). We also detected the suggested optical afterglow found by Skynet/PROMPT (Lacluyze et al., GCN 13430). The afterglow is detected in our first co-add image with Mag ~14.2 (mean time of ~60s) and decayed fainter than 15.8 mag in the second co-add (mean time of 460s). The unfiltered images are calibrated relative to USNO A2.0. Continuing observations are in progress.
GCN 13433 table
GRB_name GRB120711A
GCN_number 13433
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 13433 SUBJECT: Continued Skynet/PROMPT observations of GRB120711A DATE: 12/07/11 04:14:24 GMT FROM: Aaron LaCluyze at U.North Carolina A. Lacluyze, J. Haislip, K. Ivarsen, D. Reichart, J. Moore, H. T. Cromartie, R. Egger, A. Foster, N. Frank, M. Nysewander, A. Oza, E. Speckhard, A.Trotter, and J. A. Crain report: Skynet continued to observe the field of GRB120711A (INTEGRAL trigger 6599, GCN 13430 and 13432.) A preliminary light curve in B, V, and R, calibrated to ~5 USNO B1.0 stars can be found at: http://skynet.unc.edu/grb/grb120711a.png
GCN 13434 table
GRB_name GRB120711A
GCN_number 13434
Detection_method INTEGRAL
t_trigger 2:44:48 UTC
ra 94.7030°
decl -71.0010°
Circular_text TITLE: GCN CIRCULAR NUMBER: 13434 SUBJECT: GRB 120711A: an bright long GRB detected with INTEGRAL DATE: 12/07/11 04:28:05 GMT FROM: Diego Gotz at CEA D. Gotz (CEA-Saclay), S. Mereghetti (IASF Milano), E. Bozzo, C. Ferrigno, L. Gibaud (ISDC, Versoix), and J. Borkowski (CAMK, Torun) on behalf of the IBAS Localization Team report: a long and bright GRB has been detected by IBAS in the IBIS/ISGRI data at 02:44:48 UT on July 11th 2012. The GRB lasts approximately 135 s and its refined coordinates are RA: 94.703 [degrees] DEC: -71.001 [degrees] with an uncertainty of 1.1 arc min (90% c.l.). A preliminary spectral analysis yields a fluence of 1.6e-5 erg/cmsq in the 20-200 keV energy band and a peak flux over 1 s of 10 photons/cmsq/s in the same energy band. Please note that due to telemetry saturation at satellite levels there values are only lower limits. We note that our position is consistent with the optical transient reported by Lacluyze et al. (CGN 13430). A plot of the light curve has been posted at http://ibas.iasf-milano.inaf.it/IBAS_Results.html This message can be cited.
GCN 13435 table
GRB_name GRB120711A
GCN_number 13435
Detection_method IBAS
Circular_text TITLE: GCN CIRCULAR NUMBER: 13435 SUBJECT: GRB 120711A: a possible X-ray transient DATE: 12/07/11 09:59:40 GMT FROM: Diego Gotz at CEA E. Bozzo (ISDC, Versoix), D. Gotz (CEA-Saclay), S. Mereghetti (IASF Milano), C. Ferrigno, L. Gibaud (ISDC, Versoix), and J. Borkowski (CAMK, Torun) on behalf of the IBAS Localization Team report: A refined analysis of a larger IBIS/ISGRI dataset corresponding to the GRB120711A (GCN 13434), revealed a faint emission, lasting for at least ~1000s, after the main outburst. Being this duration unusual for a GRB, we are at present unable to rule out a different nature for this event (e.g. a bright transient in the direction of the LMC). The event has been detected also using the SPI Anti Coincidence System (ACS) on board of INTEGRAL which is not saturated and shows a highly structured light-curve at the peak http://www.isdc.unige.ch/~bozzo/lightcurve.dat . Further observations are encouraged. [GCN OPS NOTE(11jul12): Per author's request, the 13432 reference was changed to 13434.]
GCN 13436 table
GRB_name GRB120711A
GCN_number 13436
Detection_method MAXI Det
t_trigger 2:45:12 UTC
ra 94.0400°
decl -71.0900°
Circular_text TITLE: GCN CIRCULAR NUMBER: 13436 SUBJECT: GRB 120711A: MAXI/GSC detection DATE: 12/07/11 10:14:08 GMT FROM: Mikio Morii at Tokyo Inst Tech M. Serino (RIKEN), M. Morii(Tokyo Tech), S. Nakahira (JAXA), N. Kawai, R. Usui, K. Ishikawa, T. Yoshii (Tokyo Tech), S. Ueno, H. Tomida, M. Ishikawa (JAXA), T. Mihara, M. Sugizaki, T. Yamamoto, J. Sugimoto, M. Matsuoka (RIKEN), A. Yoshida (AGU), H. Tsunemi, M. Kimura (Osaka U.), H. Negoro, M. Nakajima, M. Asada, H. Sakakibara, N. Serita (Nihon U.), Y. Ueda, K. Hiroi, M. Shidatsu, R. Sato (Kyoto U.), Y. Tsuboi, M. Higa (Chuo U.) M. Yamauchi, Y. Nishimura, T. Hanayama, K. Yoshidome (Miyazaki U.), K. Yamaoka (Waseda U.) report on behalf of the MAXI team: MAXI/GSC triggered at 2012-07-11T02:45:12 UT on a bright uncatalogued X-ray transient source. The transient emission lasted at least 50 seconds within the 67 second long triangular transit response of MAXI/GSC. Assuming that the source flux was constant over the transit, we obtain the source position at (R.A., Dec) = (94.04 deg, -71.09 deg) = (06 16 10,$B!!(B-71 05 37)(J2000) with a 90% C.L. statistical error of 12 arcmin and an additional systematic uncertainty of 0.1 deg (90% containment radius). Without assuming the source constancy, we obtain a rectangular error box (90%C.L.) with the following corners: (R.A., Dec) = (+94.86 deg, -70.99 deg) = (06 19 29, -70 59 26)(J2000) (R.A., Dec) = (+94.93 deg, -71.21 deg) = (06 19 44, -71 12 23)(J2000) (R.A., Dec) = (+91.53 deg, -71.22 deg) = (06 06 06, -71 13 27)(J2000) (R.A., Dec) = (+91.52 deg, -71.01 deg) = (06 06 05, -71 00 26)(J2000) This error region includes the position of GRB 120711A reported by Lacluyze et al. (GCN #13430) and Gotz et al. (GCN #13434). Fixing the source position to that of GRB 120711A, we obtained the light curve corrected with the transit response within the GSC scan. It was variable within the scan, and the peak flux was 610 +- 130 (mCrab, 2-20 keV) on 2012-07-11 02:44:54 UT.
GCN 13437 table
GRB_name GRB120711A
GCN_number 13437
Detection_method Fermi GBM Det
t_trigger 2:44:53.290 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 13437 SUBJECT: GRB 120711A: Fermi GBM observation DATE: 12/07/11 10:18:39 GMT FROM: David Gruber at MPE David Gruber (MPE) and Vronique Pelassa (UAH) report on behalf of the Fermi GBM Team: "At 02:44:53.29 UT on 11 July 2012, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 120711A (trigger 363667496 / 120711115). which was also detected by the INTEGRAL/IBAS (Gotz et al. 2012, GCN 13434). The GBM on-ground location is consistent with the INTEGRAL position. The angle from the Fermi LAT boresight is 140 degrees. Moreover, this burst was bright enough to result in a Fermi spacecraft autonomous rapid repoint (ARR) maneuver. This burst was also independently detected by INTEGRAL SPI-ACS. The GBM light curve consists of a precursor which is followed by a hard, main emission after ~ 50 s, lasting for another ~ 50 s. The T90 is about 44 s (50-300 keV). The time-averaged spectrum from T0-1 s to T0+131 s is best fit by a Band function with Epeak = 973 +/- 35 keV, alpha = -0.94 +/- 0.01, and beta = -2.40 +/- 0.04. This spectrum is typical of a bright, hard GRB, and would be highly unusual for an X-ray transient (Bozzo et al. 2012, GCN 13435). The event fluence (10-1000 keV) in this time interval is (1.942 +/- 0.002)E-04 erg/cm^2. The 1-sec peak photon flux measured starting from T0+95 s in the 10-1000 keV band is 26.7 +/- 0.6 ph/s/cm^2. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog."
GCN 13438 table
GRB_name GRB120711A
GCN_number 13438
Detection_method correction
redshift 3.0000
Circular_text TITLE: GCN CIRCULAR NUMBER: 13438 SUBJECT: GRB 120711A: GROND photometric redshift DATE: 12/07/11 11:11:49 GMT FROM: Sylvio Klose at TLS Tautenburg J. Elliott (MPE Garching), S. Klose (TLS Tautenburg), and J. Greiner (MPE Garching) report on behalf of the GROND team: We observed the field of GRB 120711A (INTEGRAL trigger 6599: Gotz et al., GCN 13434; Bozzo et al., GCN 13435; MAXI/GSC detection: Serino et al., GCN 13436; Fermi/GBM trigger 363667496 / 120711115: Gruber & Pelassa, GCN 13427) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120, 405) mounted at the 2.2m MPG/ESO telescope at La Silla Observatory (Chile). Observations started on July 11, 08:34 UT, 5.8 hrs after the trigger as soon the location became visible at La Silla. The afterglow (Lacluyze et al., GCN 13430, 13433; Zheng, GCN 13432) is clearly detected in all bands. For an exposure of 8 min in JHK and 7.66 min in g'r'i'z', at an average airmass of 2.5 and an average seeing of 2".0, we measure the following preliminary AB magnitudes g' = 20.9 +/- 0.1 r' = 20.2 +/- 0.1 i' = 19.6 +/- 0.1 z' = 19.4 +/- 0.1 J = 18.6 +/- 0.1 H = 18.2 +/- 0.1 K = 18.0 +/- 0.1 The SED, after correction for Galactic reddening along the line of sight (E(B-V)=0.09 mag; Schlegel et al. 1998), can be described by a power law (beta ~ 1.4) with a reduced flux in the g-band, suggesting a photometric redshift of about 3. We note that also the PROMPT afterglow light curve (http://skynet.unc.edu/grb/grb120711a.png) supports a drop-out in the blue bands. Magnitudes are derived based on GROND zeropoints (g'r'i'z') and 2MASS stars (JHK).
GCN 13439 table
GRB_name GRB120711A
GCN_number 13439
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 13439 SUBJECT: GRB 120711A: REM NIR early time detection DATE: 12/07/11 11:31:46 GMT FROM: Stefano Covino at Brera Astronomical Observatory D. Fugazza, S. Covino, A. Rossi on behalf of the REM team report: We imaged the field of GRB120711A (Gotz et al., GCN 13434 and Bozzo et al., GCN 13435) with the NIR camera (the optical camera is at present under maintenance) of the REM 60cm telescope located at La Silla. The bright optical counterpart reported in GCN 13430 (Lacluyze et al.), GCN 13432 (Zheng et al.) and GCN 13438 (Elliot et al.) is well detected in the NIR at a peak magnitude of H = 11.90 + 0.05 between 2-4 minutes after the burst. The source was then fading rapidly remaining approximately at the same magnitude, H~13, for several more minutes. Data have been calibrated by isolated not-saturated 2MASS stars in the field.
GCN 13441 table
GRB_name GRB120711A
GCN_number 13441
Detection_method Other
redshift 2.2025
Circular_text TITLE: GCN CIRCULAR NUMBER: 13441 SUBJECT: GRB 120711A Gemini-S likely redshift DATE: 12/07/11 12:46:35 GMT FROM: Nial Tanvir at U.Leicester N. R. Tanvir, K. Wiersema (U. Leicester), A. J. Levan (U. Warwick), D. Fox (Penn State), A. Fruchter (STScI) and D. Krogsrud (Gemini) report on behalf of a larger collaboration: We observed the afterglow of GRB 120711A (Gotz et al. GCN 12434; Lacluyze et al. GCN 12430) using the GMOS-S spectrograph on Gemini-South. Observations began at 2012-7-11 10:08 UT, about 7.5 hr post-burst. The data were obtained at high air-mass and on the boundary of twilight, so the signal-to-noise is rather poor. Nevertheless, in the spectrum we identify lines of MgII (2797/2804A) and FeII (2374/2383/2587/2600A) at a common redshift of z=1.405. This therefore provides a robust lower-limit to the redshift of the GRB. Furthermore, given the lack of other absorption features, in particular any matching a redshift z~3 (Elliott et al. GCN 13438), we tentatively identify z=1.405 as the most likely GRB redshift.
GCN 13442 table
GRB_name GRB120711A
GCN_number 13442
Detection_method Swift-XRT Other
ra 94.6783°
decl -70.9990°
Circular_text TITLE: GCN CIRCULAR NUMBER: 13442 SUBJECT: GRB 120711A: Swift-XRT observations DATE: 12/07/11 13:00:00 GMT FROM: Andy Beardmore at U Leicester A.P. Beardmore and P.A. Evans (U. Leicester) report on behalf of the Swift-XRT team: We have analysed 657 s of XRT data for the INTEGRAL-detected burst: GRB 120711A (Gotz et al. GCN Circ. 13434), from 8.3 ks to 20.0 ks after the INTEGRAL trigger. The data comprise 269 s in Windowed Timing (WT) mode with the remainder in Photon Counting (PC) mode. An X-ray source is detected within the INTEGRAL error circle. Using 336 s of PC mode data and 1 UVOT images, we find an enhanced XRT position (using the XRT-UVOT alignment and matching UVOT field sources to the USNO-B1 catalogue): RA, Dec = 94.67830, -70.99905 which is equivalent to: RA (J2000): 06h 18m 42.79s Dec(J2000): -70d 59' 56.6" with an uncertainty of 1.7 arcsec (radius, 90% confidence). This position is 29 arcsec from the INTEGRAL position and 0.3 arcsec from the Skynet/PROMPT position (LaCluyze et al. GCN Circ. 13430). The light curve can be modelled with a power-law decay with a decay index of alpha=1.59 (+0.16, -0.15). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 2.15 (+/-0.11). The best-fitting absorption column is 3.6 (+/-0.4) x 10^21 cm^-2, in excess of the Galactic value of 7.9 x 10^20 cm^-2 (Kalberla et al. 2005). The PC mode spectrum has a photon index of 1.80 (+0.25, -0.23) and a best-fitting absorption column of 2.4 (+0.9, -0.8) x 10^21 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 4.5 x 10^-11 (6.2 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 2.4 (+0.9, -0.8) x 10^21 cm^-2 Galactic foreground: 7.9 x 10^20 cm^-2 Excess significance: 3.2 sigma Photon index: 1.80 (+0.25, -0.23) The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00020223. This circular is an official product of the Swift-XRT team.
GCN 13443 table
GRB_name GRB120711A
GCN_number 13443
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 13443 SUBJECT: GRB 120711A: MASTER early OT detection DATE: 12/07/11 15:51:48 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs H. Levato and C. Saffe Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE) C. Mallamaci, C. Lopez and F. Podest Observatorio Astronomico Felix Aguilar (OAFA) D. Denisenko, A. Kuznetsov, V. Lipunov, E. Gorbovskoy, V. Kornilov, D. Kuvshinov, A. Belinski, N. Tyurina, N. Shatskiy, P. Balanutsa, D. Zimnukhov, V.V. Chazov Lomonosov Moscow State University, Sternberg Astronomical Institute A. Tlatov, A.V. Parhomenko, D. Dormidontov, V. Sennik Kislovodsk Solar Station of the Pulkovo Observatory K. Ivanov, S. Yazev, N.M. Budnev, O. Gres, O. Chuvalaev, V.A. Poleshchuk Irkutsk State University V. Yurkov, Yu. Sergienko, D. Varda, E. Sinyakov Blagoveschensk Educational State University, Blagoveschensk V. Krushinski, I. Zalozhnich, A. Popov, A. Bourdanov, A. Punanova Ural Federal University MASTER-ICATE robotic very wide field cameras (FOV=2x384 square degrees, D=72mm, f/1.2, 1 pix = 22 arcsec, http://observ.pereplet.ru) located in Argentina (Observatorio Astronomico Felix Aguilar, http://93.180.27.230:8080/) were pointed to the INTEGRAL TRIGGER_NUM 6599 = Fermi TRIGGER_NUM: 363667496 60 sec after INTEGRAL trigger Time (Gotz et al., GCN 13434, Gruber and Pelassa, GCN 13437) on 2012-07-11 at 02:45:54.107 UT. Our cameras are continuously imaging the sky with 5 sec exposures. On our first unfiltered image (5 sec exposure) we have not found any OT. We see OT (Lacluyze et al., GCN 13430, Zheng et al., GCN 13432, Elliot et al., GCN 13438, Fugazza et al., GCN 13439 and Tanvir et al., GCN 13441) on the sum of 4 images obtained between T0+121s and T0+141s with the unfiltered magnitude 12.5. Nothing is visible at the OT position on the individual (m_lim = 12.0) and combined (m_lim=13.0) images obtained before T0+121s and after T0+141s. This message can be cited.
GCN 13444 table
GRB_name GRB120711A
GCN_number 13444
Detection_method Fermi LAT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 13444 SUBJECT: GRB 120711A: Fermi LAT detection DATE: 12/07/11 17:29:37 GMT FROM: Thomas P.H. Tam at Nat.Tsing Hua U. P.H.T. Tam, K.L. Li and A.K.H. Kong (NTHU) report: We report on the Fermi Large Area Telescope (LAT) detection of >100 MeV gamma-ray emission from the direction of the bright GRB 120711A, which triggered INTEGRAL (Gotz et al., GCN 13434), MAXI/GSC (Serino et al., GCN 13436), and Fermi/GBM (Gruber et al., GCN 13437). The GRB position was outside the LAT field of view at the GRB onset (c.f. GCN 13437). However, gamma-ray emission up to around 2 GeV was detected from the GRB direction from 0.8 ks to ~7 ks after the burst. Such duration is one of the longest ever observed for a GRB in GeV domain. Using the data obtained from the above period, an unbinned likelihood analysis resulted in a detection significance of ~7 sigma, and a photon spectral index of -1.8+-0.3. We localized the LAT emission to be at RA, DEC (J2000 deg) = 94.58, -70.93, with a statistical error of ~0.17 deg (68% CL), which is compatible with the Swift/XRT position (Beardmore et al., GCN 13442).
GCN 13446 table
GRB_name GRB120711A
GCN_number 13446
Detection_method Konus-Wind Det
t_trigger 2:45:55.810 UTC
redshift 1.4050
Circular_text TITLE: GCN CIRCULAR NUMBER: 13446 SUBJECT: Konus-Wind observation of GRB 120711A DATE: 12/07/11 18:35:12 GMT FROM: Dmitry Frederiks at Ioffe Institute S. Golenetskii, R.Aptekar, D. Frederiks, E. Mazets, V. Pal'shin, P. Oleynik, M. Ulanov, D. Svinkin, and T. Cline on behalf of the Konus-Wind team, report: The long hard intense GRB 120711A (detected by the INTEGRAL/IBAS Gotz et al., GCN 13434; MAXI/GSC detection: Serino et al., GCN 13436; Fermi/GBM trigger 363667496/120711115: Gruber & Palassa, GCN 13437; Fermi/LAT detection: Tam, Li & Kong, GCN 13444) triggered Konus-Wind at T0=09955.810s UT (02:45:55.810) The light curve starts with a precursor at ~T0-65s followed by a strong hard double pulse lasting from ~T0-3 s to ~T0+50 s. Several short (100 - 200 ms) bright spikes are well detected over the general burst light curve in the ~T0+30 s to ~T0+40 s time interval. A a weak decaying emission tail in the soft energy channel G1(25-90 keV) is detectable till at least ~T0+400s. The emission during the main phase of the event is seen up to ~10 MeV. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB120711_T09955/ As observed by Konus-Wind the burst had a fluence of 3.8(-0.2,+0.2)x10-4 erg/cm2, and a 64-ms peak flux, measured from T0+32.576 s, of 3.6(-0.4,+0.4)x10-5 erg/cm2/s (both in the 20 keV - 10 MeV energy range). The time-integrated spectrum of the burst (measured from T0 to T0+46.336 s) is best fit in the 20 keV - 10 MeV range with the GRB (Band) model, for which: the low-energy photon index alpha = -0.97 (-0.02, +0.02), the high energy photon index beta = -2.7 (-0.3, +0.2), the peak energy Ep = 1060(-60, +60) keV, chi2 = 95.7/87 dof. The spectrum at the maximum count rate (measured from T0+30.208 to T0+34.560 s) is best fit in the 20 keV - 10 MeV range with the GRB (Band) model, for which: the low-energy photon index alpha = -0.93 (-0.04, +0.04), the high energy photon index beta = -2.5 (-0.5, +0.3), the peak energy Ep = 1400(-160, +170) keV, chi2 = 85.5/87 dof. Assuming the likely GRB redshift of z=1.405 (Tanvir et al., GCN 13441) and a standard cosmology model with H_0 = 71 km/s/Mpc, Omega_M = 0.27, Omega_Lambda = 0.73: the isotropic energy release E_iso is (1.95 0.1)x10^54 erg, the isotropic peak luminosity L_iso_max is (4.5 0.5)x10^53 erg/s, and Ep_rest is (2550 150) keV. All the quoted results are preliminary. All the quoted errors are at the 90% confidence level.
GCN 13448 table
GRB_name GRB120711A
GCN_number 13448
Detection_method Swift-UVOT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 13448 SUBJECT: GRB 120711A: Swift/UVOT Observations DATE: 12/07/11 21:55:34 GMT FROM: Alice Breeveld at MSSL-UCL A. A. Breeveld (MSSL-UCL) and M. J. Page (MSSL-UCL) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 120711A 8216 s after the INTEGRAL trigger (Gotz et al., GCN Circ. 13434). No significant optical afterglow consistent with the position given in Lacluyze et al. (GCN_Circ. 13430) is detected in the initial UVOT exposures. However, in the U filter, the source may be detected at this position with a significance of 2 sigma. The possible detection is included in the table. 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 b 8464 8480 16 >18.7 u 8380 8459 79 >19.4 w1 8216 8375 157 >19.8 u 8380 8459 79 19.6 0.5 (2sig) The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.08 in the direction of the burst (Schlegel et al. 1998).
GCN 13451 table
GRB_name GRB120711A
GCN_number 13451
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 13451 SUBJECT: GRB 120711A: ATCA 34GHz upper limit DATE: 12/07/12 01:53:15 GMT FROM: Paul Hancock at U of Sydney P. Hancock, T. Murphy, B. Gaensler, M. Bell, D. Burlon (University of Sydney/CAASTRO), A. de Ugarte Postigo (Dark Cosmology / IAA) We observed GRB120711A (GCN 13434) with the Australia Telescope Compact Array at 34GHz for 26 minutes centered on 21:37UT Jul 11 2012 (T0+18.9hours) in stormy weather. We detect no radio source at the location of the GRB (GCN 13430) and place an upper limit of 3.6mJy on the flux of an afterglow. Further observations are planned. These observations were obtained as part of ATCA project C2689. We thank the observatory staff for their support and scheduling the observations. The Australia Telescope is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO.
GCN 13452 table
GRB_name GRB120711A
GCN_number 13452
Detection_method Fermi LAT Det
t_trigger 2:44:53.290 UTC
ra 94.7000°
decl -70.9000°
Circular_text TITLE: GCN CIRCULAR NUMBER: 13452 SUBJECT: GRB 120711A: Fermi LAT Detection DATE: 12/07/12 02:03:05 GMT FROM: Daniel Kocevski at SLAC Daniel Kocevski (Stanford Univ.) and Giacomo Vianello (CIFS/SLAC), Nicola Omodei (Stanford Univ.), and Seth Digel (SLAC) report on behalf of the Fermi LAT Team: Fermi-LAT has detected high energy emission from the bright GRB 120711A in ground analysis. The GRB triggered the Fermi-GBM on July 11th, 2012 at 02:44:53.29 UTC (trigger 363667496/120711115, Gruber et al. GCN 13437) and was bright enough to result in a spacecraft autonomous repoint. At the time of the GBM trigger, the angle between the GRB position and the LAT bore-sight was 134.4 degrees for the duration of the prompt emission, and remained outside the Fermi-LAT nominal field of view for an additional ~600 seconds. A preliminary maximum-likelihood analysis of the E>75MeV P7TRANSIENT_V6 LAT data centered on the XRT position reported by Beardmore et al. (GCN 13442) generated for the interval T0+600s to T0+1100s revealed a significant transient source, with a spectrum well described by a power law of index -2.0 +/ 0.3 (68% C.L. statistical only). These results are in agreement with those found by Tam et al. (GCN 13444). Using the data covering T0+600s to T0+1100s, we obtained the best LAT on-ground localization of: RA(J2000) = 94.7 deg Dec(J2000) = -70.9 deg with an error radius of 0.16 deg (90% containment, statistical error only), which is 0.09 deg from the XRT position, and 0.07 deg from the position reported by Tam et al. (GCN 13444). We note that this position is ~1.4 degrees away from the known variable gamma-ray source 2FGL J0601.1-7037, which has been associated with the blazar PKS 0601-70. In order to understand if the observed excess can be due to a brightening of the blazar we considered two nested models for our data, one including just the blazar, and one including both the blazar and a new source (the GRB). Our data favor the latter model, with the fit converging to a solution with a negligible contribution from the blazar, as expected from the mean flux reported in the Fermi 2FGL catalog (Nolan et al., 2012). An analysis using E>75MeV P7TRANSIENT_V6 data covering an interval before the burst (T0-6000s to T0-2000 s) shows no significant emission at the location of the blazar. Thus, 2FGL J0601.1-7037 is unlikely to be the source of the excess. We caution against the use of data after ~T0+2600 s, because of a large Zenith angle of the GRB, potentially resulting in a strong contamination from terrestrial gamma-rays originating from charged particle interactions with Earth's atmosphere. The Fermi-LAT point of contact for this burst is Daniel Kocevski (kocevski@stanford.edu)
GCN 13463 table
GRB_name GRB120711A
GCN_number 13463
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 13463 SUBJECT: GRB 120711A: ATCA 34GHz further observations (upper limit) DATE: 12/07/14 01:29:01 GMT FROM: Paul Hancock at U of Sydney P. Hancock, T. Murphy, B. Gaensler, M. Bell, D. Burlon (University of Sydney/CAASTRO), A. de Ugarte Postigo (IAA-CSIC, DARK/NBI) We observed GRB120711A (GCN 13434) with the Australia Telescope Compact Array at 34GHz for 60 minutes centered on 23:18UT Jul 13 2012 (T0+2.85days). We detect no radio source at the location of the GRB (GCN 13430) and place a 3sigma upper limit of 230uJy on the flux of an afterglow. Further observations are planned. These observations were obtained as part of ATCA project C2689. We thank the observatory staff for their support and scheduling the observations. The Australia Telescope is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO.
GCN 13468 table
GRB_name GRB120711A
GCN_number 13468
Detection_method INTEGRAL
t_trigger 2:44:48 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 13468 SUBJECT: GRB 120711A: INTEGRAL/SPI observations DATE: 12/07/14 12:08:26 GMT FROM: Andreas von Kienlin at MPE L. Hanlon (UCD), A. Martin-Carrillo (UCD), X.-L. Zhang (MPE) and A. von Kienlin (MPE) report: "The bright and long GRB detected by IBAS in the INTEGRAL IBIS/ISGRI data at 02:44:48 UT on July 11th 2012 (Gotz et al., GCN 13434 ) was also observed by the Spectrometer SPI onboard INTEGRAL, in addition to the detection by its anticoincidence shield (SPI-ACS). The event was located in the field of view of SPI, which allows spectral analysis of this event. The light curve from SPI events starts with a precursor at 02:44:50 UT followed by a bright double peaked main emission phase at 02:45:55 UT with a duration of about 50 sec. The emission during the main peak is seen up to ~3 MeV. We searched for the faint and soft emission after the main outburst reported by E. Bozzo et al. (GCN 13435) and S. Golenetskii et al. (GCN 13446). We find a weak tail in the 20 to 100 keV energy range, lasting for about 800 s after the main emission phase . The time-integrated spectrum of the main emission phase is well fitted (in the 20 keV - 3 MeV range) by an exponential cutoff powerlaw model, with photon index = 1.00+/-0.03 and an high energy cutoff at 1200 +/- 200 keV. The fluence during the 50 seconds main emission phase in the 20-1000 keV range is (2.26 +/- 0.04)E-4 erg/cm^2. The spectral analysis results presented above are preliminary."
GCN 13485 table
GRB_name GRB120711A
GCN_number 13485
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 13485 SUBJECT: GRB 120711A: ATCA 34GHz final observations (upper limit) DATE: 12/07/17 01:19:37 GMT FROM: Paul Hancock at U of Sydney P. Hancock, T. Murphy, B. Gaensler, M. Bell, D. Burlon (University of Sydney/CAASTRO), A. de Ugarte Postigo (IAA-CSIC, DARK/NBI) We observed GRB120711A (GCN 13434) with the Australia Telescope Compact Array at 34GHz for 64 minutes centered on 21:42UT Jul 16 2012 (T0+3.78days) in clear weather. We detect no radio source at the location of the GRB (GCN 13430) and place a 3sigma upper limit of 96uJy on the flux of an afterglow. No further observations are planned. These observations were obtained as part of ATCA project C2689. We thank the observatory staff for their support and scheduling the observations. The Australia Telescope is funded by the Commonwealth of Australia for operation as a National Facility managed by CSIRO.
GCN 13513 table
GRB_name GRB120711A
GCN_number 13513
Detection_method Other
ra 94.6783°
decl -70.9991°
Circular_text TITLE: GCN CIRCULAR NUMBER: 13513 SUBJECT: GRB120711A: Planned XMM-Newton observation DATE: 12/07/24 15:22:35 GMT FROM: Norbert Schartel at XMM-Newton/ESA XMM-Newton will observe GRB120711A at location (RA=06h 18m 42.79s, DEC=-70d 59' 56.6", J2000), starting at 20:01:44 UT, on July 28, 2012, for an exposure of 28000 seconds. XMM-Newton SOC This message and any attachments are intended for the use of the addressee or addressees only. The unauthorised disclosure, use, dissemination or copying (either in whole or in part) of its content is not permitted. If you received this message in error, please notify the sender and delete it from your system. Emails can be altered and their integrity cannot be guaranteed by the sender. Please consider the environment before printing this email.