This file contains both GRBs: 070714A and 070714B /////////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 6619 SUBJECT: Swift detection of a possible burst (Trigger 284850) DATE: 07/07/14 04:20:07 GMT FROM: Scott Barthelmy at NASA/GSFC D. Grupe (PSU), S. D. Barthelmy (GSFC), D. N. Burrows (PSU), M. M. Chester (PSU) and N. Gehrels (NASA/GSFC) report on behalf of the Swift Team: At approximately 03:18 +/-5min UT BAT triggered on a possible GRB (trigger 284850). Swift automatically slewed to the location RA=43.94 Dec=+30.24 (J2000). The uncertainty is 6 arcmin. We are uncertain about both the time and the location at this time because the trigger occurred during a TDRSS outage, so most of the regular TDRSS Notices were lost. We are also in the middle of the computer downtime as announced earlier today, so analysis of the full Malindi downlink data will have to wait until late Saturday UT. We wish to thank J. Knavel of the Swift Operations Team for notifying the science team that Swift had slewed to a GRB. Burst Advocate for this burst is D. Grupe (grupe AT astro.psu.edu). 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.) /////////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 6620 SUBJECT: GRB 070714: Swift detection of a bright burst, possibly short DATE: 07/07/14 05:28:15 GMT FROM: Scott Barthelmy at NASA/GSFC J. L. Racusin (PSU), S. D. Barthelmy (GSFC), D. N. Burrows (PSU), M. M. Chester (PSU), N. Gehrels (NASA/GSFC), H. A. Krimm (GSFC/USRA), D. M. Palmer (LANL) and T. Sakamoto (NASA/ORAU) report on behalf of the Swift Team: At 04:59:29 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 070714 (trigger=284856). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 57.854, +28.295 which is RA(J2000) = 03h 51m 25s Dec(J2000) = +28d 17' 43" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve shows a duration of 3 seconds with a spike to a peak of 20000 counts/s (15-350 keV) at T+0.2 s. The XRT began observing the field at 05:00:30 UT, 61 seconds after the BAT trigger. Using ground processed data, XRT found a bright, fading, uncatalogued X-ray source located at RA, Dec 57.8423, +28.2978 which is RA(J2000) = 03h 51m 22.1s Dec(J2000) = 28d 17' 52.0" with an uncertainty of 3.9 arcseconds (radius, 90% containment). This location is 39 arcseconds from the BAT on-board position, within the BAT error circle. The initial flux in the 2.5s image was 2.4e-09 erg/cm2/s (0.2-10 keV). The UVOT began observing the field at 05:00:40.05 UT, 70.4 s after the BAT trigger. No counterpart is apparent in the 2.7' x 2.7' subimage, based on visual comparison with the DSS. Additional processing is underway. Burst Advocate for this burst is J. L. Racusin (racusin AT astro.psu.edu). 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.) /////////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 6621 SUBJECT: GRB 070714 : Liverpool Telescope optical counterpart ? DATE: 07/07/14 07:07:04 GMT FROM: Andrea Melandri at Liverpool John Moores U A. Melandri (Liverpool JMU) on behalf of the Liverpool GRB team report: On 2007 Jul 14 at 05:10:56 UT the 2-m Liverpool Telescope automatically observed the field of GRB 070714 (trigger=284856, Racusin et al. GCN 6620). Due to the incoming dawn the automatic observation sequence stopped after ~15 minutes, after the acquisition of only 9 frames. Inside the XRT error circle (Racusin et al. GCN 6620) we find a single source at the position (error of 0.5 arcsec) RA = 03:51:22.2 Dec = +28:17:51.4 It is not a catalog source but presently it's not clear yet whether the object is fading. /////////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 6622 SUBJECT: GRB 070714A, Swift-BAT refined analysis DATE: 07/07/14 19:38:35 GMT FROM: Scott Barthelmy at NASA/GSFC S.D. Barthelmy (GSFC), L. Barbier (GSFC), J. Cummings (GSFC/UMBC), E. Fenimore (LANL), N. Gehrels (GSFC), D. Grupe (PSU), H. Krimm (GSFC/USRA), C. Markwardt (GSFC/UMD), D. Palmer (LANL), A. Parsons (GSFC), T. Sakamoto (GSFC/ORAU), G. Sato (GSFC/ISAS), M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC), T. Ukwatta (GWU) (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 070714A (trigger #284850) (Grupe, et al., GCN Circ. 6619). The BAT ground-calculated position is RA, Dec = 42.933, 30.241 deg which is RA(J2000) = 2h 51m 43.8s Dec(J2000) = 30d 14' 28" with an uncertainty of 1.3 arcmin, (radius, sys+stat, 90% containment). The partial coding was 96%. The mask-weight lightcurve shows a single peak starting at T+0, peaking at T+0.7, and ending at T+2 sec, where the rise time is a little faster than the decay. T90 (15-350 keV) is 2.0 +- 0.3 sec (estimated error including systematics). The time-averaged spectrum from T-0.7 to T+2.3 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 2.6 +- 0.2. The fluence in the 15-150 keV band is 1.5 +- 0.2 x 10^-7 erg/cm2. The 1-sec peak photon flux measured from T+0.30 sec in the 15-150 keV band is 1.8 +- 0.2 ph/cm2/sec. All the quoted errors are at the 90% confidence level. We note that the fluence ratio in a simple power-law fit between the 25-50 keV band and the 50-100 keV band is 1.52. This fluence ratio is larger than 1.32, which can be achieved in the Band function of alpha=-1.0, beta=-2.5, and Epeak=30 keV. Thus, preliminary analysis shows that Epeak of the burst is very likely around or below 30 keV. Therefore the burst can be classified as an X-ray flash. /////////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 6623 SUBJECT: GRB 070714B, Swift-BAT refined analysis of the short hard burst DATE: 07/07/14 21:47:27 GMT FROM: Takanori Sakamoto at NASA/GSFC L. Barbier (GSFC), S. D. Barthelmy (GSFC), J. Cummings (GSFC/UMBC), E. Fenimore (LANL), N. Gehrels (GSFC), H. Krimm (GSFC/USRA), C. Markwardt (GSFC/UMD), D. Palmer (LANL), A. Parsons (GSFC), J. Racusin (PSU), T. Sakamoto (GSFC/ORAU), G. Sato (GSFC/ISAS), M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC), T. Ukwatta (GWU) (i.e. the Swift-BAT team): Using the data set from T-120 to T+182 sec from recent telemetry downlinks, we report further analysis of BAT GRB 070714B (trigger #284856) (Racusin, et al., GCN Circ. 6620). The BAT ground-calculated position is RA, Dec = 57.853, 28.294 deg which is RA(J2000) = 3h 51m 24.8s Dec(J2000) = 28d 17' 37" with an uncertainty of 1.4 arcmin, (radius, sys+stat, 90% containment). The partial coding was 93%. The BAT mask-weighted light curve shows multiple short spikes starting from T-0.8 sec with a duration of 3 sec. There is extended softer emission from T+20 sec to T+70 (and possibly T+100) sec. T90 (15-350 keV) is 64 +- 5 sec (estimated error including systematics). The light curve looks similar to previous short bursts such as GRB 050724 with a short-hard initial episode followed by a softer extended episode, so we think it is likely that this burst is in the short category. The time-averaged spectrum from T-0.8 to T+65.6 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.36 +- 0.19. The fluence in the 15-150 keV band is 7.2 +- 0.9 x 10^-7 erg/cm2. The 1-sec peak photon flux measured from T-0.39 sec in the 15-150 keV band is 2.7 +- 0.2 ph/cm2/sec. Separating out the initial "spike" of emission (from T-0.8 to T+2 sec), the photon index in a simple power-law fit is 0.99 +- 0.08. The fluence in the 15-150 keV band of this part is 5.1 +-0.3 x 10^-7 erg/cm2. All the quoted errors are at the 90% confidence level. /////////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 6624 SUBJECT: GRB 070714 ("Bastille"): Optical Pre-Imaging DATE: 07/07/14 22:47:19 GMT FROM: Josh Bloom at UC Berkeley P. Nugent (LBL) and J. S. Bloom (UC Berkeley) report: We have created a stacked image through the co-addition of 8 unfiltered images taken by the NEAT collaboration and 51 images in the RG610 filter taken by the Palomar-Quest Consortium at the Palomar Oschin Schmidt telescope (obtained from 2002-2006), of what is being called a short-hard burst (SHB) 070714A (Barbier et al.; GCN #6622). The stacked image is significantly deeper than the DSS (3 sigma limit of R~22.7 mag). There is no source at the position of the proposed counterpart (Melandri et al. GCN #6621). Since this Liverpool Telescope source was detected in twilight, it was likely seen near the DSS limit (or brighter) and thus, while we cannot say for sure (since no magnitude was given in GCN #6621), the absence of a similarly bright source in our image suggests that the Melandri et al. source was indeed the afterglow. Note that the source @ position RA = 03:51:21.24, DEC = +28:17:45.5 is in the 2MASS catalog and is blue (J - K = 0.5 mag). This message may be cited. /////////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 6625 SUBJECT: GRB 070714b ("Bastille"): Optical Pre-Imaging (Clarification) DATE: 07/07/14 23:25:42 GMT FROM: Josh Bloom at UC Berkeley J. S. Bloom notes: "We clarify that the imaging information reported in the circular GCN 6624 (Nugent & Bloom) refers to GRB 070714b (short-hard burst; Barbier et al. 6623; trigger #284856) and not GRB 070714a (short and XRF-like; Barthelmy et al. 6622; trigger #284850). We apologize for any confusion and thank S. Barthlemy for alerting us to the citation error in the previous circular. The corrected circular should read: GRB 070714b ("Bastille"): Optical Pre-Imaging P. Nugent (LBL) and J. S. Bloom (UC Berkeley) report: "We have created a stacked image through the co-addition of 8 unfiltered images taken by the NEAT collaboration and 51 images in the RG610 filter taken by the Palomar-Quest Consortium at the Palomar Oschin Schmidt telescope (obtained from 2002-2006), of what is being called a short-hard burst (SHB) 070714B (Barbier et al.; GCN #6623). The stacked image is significantly deeper than the DSS (3 sigma limit of R~22.7 mag). There is no source at the position of the proposed counterpart (Melandri et al. GCN #6621). Since this Liverpool Telescope source was detected in twilight, it was likely seen near the DSS limit (or brighter) and thus, while we cannot say for sure (since no magnitude was given in GCN #6621), the absence of a similarly bright source in our image suggests that the Melandri et al. source was indeed the afterglow. Note that the source @ position RA = 03:51:21.24, DEC = +28:17:45.5 is in the 2MASS catalog and is blue (J - K = 0.5 mag). This message may be cited." /////////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 6627 SUBJECT: GRB070714B: Swift-XRT refined analysis DATE: 07/07/15 03:33:26 GMT FROM: Judith Racusin at PSU J. Racusin, J. Kennea, C. Pagani, L. Vetere (PSU), and P. Evans (U. Leicester) report on behalf of the Swift/XRT team: We have analyzed the first 15 ks of Swift XRT PC and WT data from GRB 070714B (Racusin et al., GCN 6620). Using 770 s of overlapping XRT Photon Counting mode and UVOT V-band data, we find an astrometrically corrected X-ray position (using the XRT-UVOT alignment and matching UVOT field sources to the USNO-B1 catalogue): RA, Dec = 57.84287, 28.29782 which is equivalent to: RA (J2000): 03h 51m 22.29s Dec (J2000): +28d 17' 52.2" with an uncertainty of 1.8 arcsec (90% confidence, radius). This is 35 arcsec from the refined BAT position (Barbier et al., GCN 6623), and 1.4 arcsec from the Liverpool optical afterglow candidate (Melandri et al., GCN 6621). The XRT light curve shows a fading behavior with super-imposed small flaring. The light curve can be fit with a power-law beginning with a steep decay with a slope of 2.49 +/- 0.18 followed by a plateau beginning at 413s +/- 50s with a slope of 0.60 +/- 0.29 until another break at 1187 +/- 270s with a decay of 1.73 +/- 0.11. The X-ray PC and WT spectrum is well fit by an absorbed power law with a photon index for 1.2 +/- 0.1 and a column density of 13 +/- 3 e20 cm^-2 in excess of the galactic value (6.4e20 cm-2). The absorbed (unabsorbed) 0.3-10.0 keV flux of the WT spectrum is 9.2e-10 (1.0e-9) erg cm^-2s^-1 and the flux of the PC spectrum is 3.4e-12 (3.7e-12) ergs cm^-2 s^-1. Assuming the source continues to decay at the same rate, we predict an XRT count rate of 2.7e-4 counts/s at T0+24 hours, which corresponds to an observed (unabsorbed) flux of 1.8e-13 (2.0e-13) ergs cm^-2 s^-1. This circular is an official product of the Swift XRT team. /////////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 6628 SUBJECT: GRB 070714A: Swift XRT refined analysis DATE: 07/07/15 04:57:42 GMT FROM: Dirk Grupe at PSU/Swift-XRT D.Grupe (PSU) reports on behalf of the Swift/XRT team: I analyzed the first (and only) orbit of X-ray data of GRB 070714A (BAT trigger 284850; Grupe et al. GCN 6619) with a total exposure time of 2.3 ks. The XRT began observing the field of GRB 070714A at 2007-07-14 03:21:25 UT, 54.4 seconds after the BAT trigger. Using 799 s of overlapping XRT Photon Counting (PC) mode and UVOT V-band data, we find an astrometrically corrected X-ray position (using the XRT-UVOT alignment and matching UVOT field sources to the USNO-B1 catalogue): RA, Dec = 42.93073, 30.24339 which is equivalent to: RA (J2000): 02 51 43.37 Dec (J2000): +30 14 36.2 with an uncertainty of 2.0" (90% confidence radius). The XRT PC mode light curve shows a fading afterglow with a decay slope of 1.02+\-0.29. The predicted count rate (flux) 24 hours after the burst is 1.5e-3 counts s-1 (1.4e-13 ergs s-1 cm-2) and 7.3e-4 counts s-1 (6.8e-14 ergs s-1 cm-2) at 48 hours after the trigger. The X-ray spectrum can be fitted by a single absorbed power law with the absorption column density in agreement with the Galactic value (NH=9.24e20 cm-2; Dickey & Lockman 1990) and a Photon spectra index Gamma = 1.68+\-0.23. This circular is an official product of the Swift XRT team. /////////////////////////////////////////////////////////////////////////// TO: All people interested in the GCN Website 15 July 07 RE: Website off-line until Monday The power upgrade and outage Friday evening through Saturday day has been completed. As expected the GCN Notices and Circulars continued to work during that interval. And they continue to work normally since them. However, the disks for the hold the GCN website pages suffered a failure during power-up. So the GCN website (and all Goddard Building 2 websites) are off-line. And while I am sending out this annoncement, I'll take the opportunity to explain why there were no GCN Notices for GRB 070714A (Swift Trigger 284850). This burst occurred during the portion of the Swift orbit covered by the TDRSS_275 satellite which was experiencing problems at the time. Hense all the messages transmitted by Swift for that burst were not received by the TDRSS satellite and therefore nothing was transmitted down to the ground to GCN. So there were no Notices to send out. TDRSS_275 was restored to normal operations a couple orbits later. Sincereely, Scott Barthelmy PRE POWER OUTAGE ANNOUNCEMENT: 13 Jul 07 > A power outage is planned for tonight and tomorrow that will take > the Swift Data Center off-line (including access to Swift quick look data), > prevent access to HEASARC web pages (including access to Swift data), > prevent access to GCN web pages, > and interrupt normal e-mail service to most of the Swift science team at GSFC. > > The GCN Notices will continue to be distributed. The GCN computer and routers > are on a separate power circuit. > > However, the GCN Circulars will have some difficulties. Reviewing the traceroutes > of recent Circular submissions shows about 1/3 of them went though a machine > that will be in the power-shutdown (2/3 went straight to the GCN computer). > (I could not determine why there was a difference between the two groups of > submissions.) So please note that if you submit, you might be in the 1/3 group. > For this 20-hour interval, if you submit and do not receive back the usual > success/problem preport email, do not submit it again. The lack of a return > probably means you are in the 1/3-group. If you send in a second submission, > they will both queue up, and ten when power is restored both copies will be distributed. > > These systems should start going off line at 22:00 UT July 13th (today), > and should begin to be restored tomorrow July 14th at about 17:00 UT. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 6630 SUBJECT: GRB 070714B: confirmation of optical afterglow DATE: 07/07/15 21:42:36 GMT FROM: Andrew Levan at U.of Leicester A.J. Levan (Warwick), N.R. Tanvir (Leicester), D Bonfield (Oxford), Alejo Martinez-Sansigre (MPI Heidelberg), J. Graham, A. Fruchter (STScI) report on behalf of a larger collaboration: We imaged the field of GRB 070714B (Racusin et al. GCNC 6620) with the William Herschel Telescope (WHT), obtaining at total of 2700s of observations in the R-band, beginning on July 15 04:17 UT. At the position of the afterglow candidate of Melandri (GCNC 6621), we detect an object with a magnitude of R~23.5 (relative to two USNO stars within the field). The observed fading confirms the association with GRB 070714B. Further observations will be necessary to determine if the current magnitude is significantly contaminated by an underlying host galaxy. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 6631 SUBJECT: GRB 070714B: Swift-BAT spectral lag for the SHB DATE: 07/07/16 18:48:06 GMT FROM: Scott Barthelmy at NASA/GSFC J. Norris (Stanford U), S.D. Barthelmy (GSFC), T. Ukwatta (GWU) on behalf of the Swift-BAT team: Using the event-by-event data from Swift-BAT, the spectral lag for GRB 070714B (Racusin, et al., 6620; Barbier, et al., 6623) is: 9 ms +- 4 ms (100-350 to 25-50 keV) 14 ms +- 7 ms ( 50-100 to 15-25 KeV) using 4-msec binning (for the 2.9-sec interval covering the initial spike). This is consistent with "zero lag" for short hard bursts. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 6632 SUBJECT: GRB 070714B: Swift/UVOT Upper Limits DATE: 07/07/16 19:59:10 GMT FROM: Wayne Landsman at GSFC/SSAI W. Landsman (NASA/GSFC) and J. Racusin (PSU) report on behalf of the Swift/UVOT team: The Swift/UVOT observed the field of GRB 070714B starting 70 s after the BAT trigger (Racusin et al. GCN Circ.6620). We do not find any source, in any of the UVOT observations, inside the refined XRT error circle (Racusin et al., GCN Circ. 6627), or at the location of the Liverpool source (Melandri et al., GCN Circ. 6621). The 3-sigma upper limits for detecting a source inside the refined XRT error circle are: Filter T_start T_end Exp(s) Mag (3-sigma upper limit) White 70 170 98.2 > 20.4 v 177 577 393.4 > 19.6 b 657 1637 58.1 > 19.2 u 632 1766 89.2 > 19.2 uvw1 607 1750 97.3 > 19.1 uvw2 687 1676 77.8 > 19.2 The values quoted above are not corrected for the expected Galactic extinction corresponding to a reddening of E_{B-V} = 0.14 mag in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 6633 SUBJECT: GRB 070714A: Swift/UVOT Upper limits DATE: 07/07/16 20:38:18 GMT FROM: Margaret Chester at PSU M.M. Chester (PSU) and D. Grupe (PSU) report on the behalf of the Swift UVOT team: The Swift/UVOT observed the field of GRB070714A (trigger=284850) starting 2007-195-03:21:15, 44 s after the BAT trigger (Grupe et al. 2007, GCN Circ. 6619). We do not find any new source in any of the UVOT observations inside the refined XRT error circle (Grupe 2007, GCN Circ. 6628). The 3-sigma upper limits for detecting a source inside the XRT error circle in the first finding chart (FC) exposure and the co-added frames (including the finding chart) are: Filter Tstart Tstop Exp Magnitude (s) (s) (s) (3-sigma UL) White FC 61 161 98.2 20.19 White 61 1641 235 20.63 v 44 1690 855 19.69 b 647 5955 138 19.55 u 622 5868 274 19.71 uvw1 598 5664 274 19.03 uvm2 5258 5458 197 18.96 uvw2 677 1666 77.8 18.49 The values quoted above are not corrected for the expected Galactic extinction corresponding to a reddening of E_{B-V} = 0.186 mag in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 6635 SUBJECT: GRB070714B: TNG NIR observations DATE: 07/07/17 12:34:16 GMT FROM: Stefano Covino at Brera Astronomical Observatory S. Covino, S. Piranomonte, P. D'Avanzo, L.A. Antonelli, F. de Luise, M. Pedani, N. Pinilla Alfonso report, on behalf of the CIBO collaboration: We observed the field of the short/hard GRB070714B (Racusin et al., GCN 6620; Barbier et al., GCN 6623) on July 15 2007 at about 5 UT with the TNG equipped with NICS in the J and K bands. The observations were performed at high airmass (higher than 2). We only marginally detected the afterglow identified by Melandri et al. (GCN 6621) and Levan et al. (GCN 6630) in the K band at approximately K~21. In the J band we could only derive a mild 3sigma upper limit, J > 20.7. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 6636 SUBJECT: GRB 070714A: Swift-BAT T_zero DATE: 07/07/17 13:29:12 GMT FROM: Scott Barthelmy at NASA/GSFC S.D. Barthelmy (GSFC) on behalf of the Swift-BAT team: It has been noted by several people (D. Grupe, M. Chester, and F. Marshall) that the T_zero trigger time for GRB 070714A (Grupe, et al., 6619; Barthelmy et al., 6622) is missing from the standard set of communications on this burst. Normally T_zero is published in the Notices and the "first Swift Circular" on the burst. But because all the TDRSS messages were lost due to a TDRSS outage, we dropped the ball on this in the later circular. The trigger time for GRB 070714A (trigger 284850) is 03:20:30.618 UT. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 6637 SUBJECT: GRB 070714B : Suzaku WAM observation of the prompt emission DATE: 07/07/19 13:37:25 GMT FROM: Makoto Tashiro at Saitama U/Swift N. Kodaka, M. Tashiro, Y. Urata, A. Endo, K. Onda, M. Suzuki, K. Morigami (Saitama U.),Y. Terada, T. Tamagawa (RIKEN), M. Ohno, T. Uehara, T. Takahashi, Y. Fukazawa, C. Kira (Hiroshima U.), K. Yamaoka, Y. E. Nakagawa, S. Sugita (Aoyama Gakuin U.), T. Enoto, R. Miyawaki, K. Nakawaza, K. Makishima (Univ. of Tokyo), E. Sonoda, M.Yamauchi, S. Maeno, H. Tanaka, R. Hara (Univ. of Miyazaki), M. Kokubun, M. Suzuki, T. Takahashi (ISAS/JAXA), S. Hong (Nihon U.), on behalf of the Suzaku WAM team, report: The short GRB 070714B (Swift/BAT trigger #284856; Racusin et al., GCN 6620; Barbier et al., GCN 6623) triggered the Suzaku Wide-band All-sky Monitor (WAM) which covers an energy range of 50 keV - 5 MeV at 04:59:29.247 UT (=T0). The observed light curve with 1/64 sec resolution shows a multi-peaked structure with a sharp strong peak at ~T0+0.45 sec. The duration (T90) was about 2.0 sec. The fluence in 100 - 1000 keV was (2.3 ± 0.2)x10^-6 erg/cm^2, while the 1-s peak flux measured from T0+0 to T0+1 sec was 2.8 ± 0.3 photons/cm^2/s in the same energy range. Preliminary result shows that the time-averaged spectrum from T0+0 to T0+2 sec is well fitted by a single power-law with a photon index of 1.3 ± 0.2 (chi^2 / d.o.f. = 22/20). All the quoted errors are at statistical 90% confidence level, in which the systematic uncertainties are not included. The light curve data for this burst is available at: http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 6638 SUBJECT: GRB 070714B: Swift/BAT and Suzaku/WAM joint spectral analysis DATE: 07/07/19 13:55:47 GMT FROM: Takanori Sakamoto at NASA/GSFC M. Ohno, T. Uehara, T. Takahashi, Y. Fukazawa, C. Kira (Hiroshima U.), K. Yamaoka, Y. E. Nakagawa, S. Sugita (Aoyama Gakuin U.), Y. Terada, T. Tamagawa (RIKEN), K. Morigami, N. Kodaka, K. Onda, M. Tashiro, M. Suzuki, Y. Urata, A. Endo (Saitama U.), T. Enoto, R. Miyawaki, K. Nakawaza, K. Makishima (Univ. of Tokyo), E. Sonoda, M.Yamauchi, S. Maeno, H. Tanaka, R. Hara (Univ. of Miyazaki), M. Kokubun, M. Suzuki, T. Takahashi (ISAS/JAXA), S. Hong (Nihon U.), on behalf of the Suzaku-WAM team, T. Sakamoto (GSFC/ORAU), L. Barbier (GSFC), S. D. Barthelmy (GSFC), J. Cummings (GSFC/UMBC), E. Fenimore (LANL), N. Gehrels (GSFC), H. Krimm (GSFC/USRA), C. Markwardt (GSFC/UMD), D. Palmer (LANL), A. Parsons (GSFC), G. Sato (GSFC/ISAS), M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC), T. Ukwatta (GWU) on behalf of the Swift-BAT team, report: We performed the Swift/BAT, and Suzaku/WAM joint fit spectral analysis of GRB 070714B (Swift-BAT trigger #284856; Racusin, et al., GCN Circ. 6620). The time interval of the spectral data for each instrument is chosen from T0(WAM) to T0(WAM)+2 sec where T0(WAM) is the trigger time of WAM at 04:59:29.247 UTC. The energy ranges which we used in the joint spectral analysis are 14-150 keV and 100-2000 keV for Swift/BAT and Suzaku/WAM respectively. The spectral data of two instruments are fit with the spectral model multiplied by the constant factor to take into account the systematic uncertainties in the response matrices of each instrument. The spectrum is well fit with a power-law with exponential cutoff model (dN/dE ~ E^{alpha} * exp(-(2+alpha)*E/Epeak)). The constant factors of each instrument agree within 10%. No systematic residual from the best fit model is seen in the spectral data of each instrument. The best fit spectral parameters are: alpha = -0.86 +- 0.10 and Epeak = 1120 (-380/+780) keV (chi2/dof = 64/69). The energy fluence in the 15-2000 keV band calculated by a power-law with exponential cutoff model for this two-second interval is 3.7 (-0.6/+1.3) x 10^-6 erg/cm2 (assuming the constant factor of the BAT is fixed to 1). All the quoted errors are at the 90% confidence level. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 6652 SUBJECT: GRB 070714B: Keck observations DATE: 07/07/22 20:15:47 GMT FROM: Daniel Perley at U.C. Berkeley GRB 070714B: Keck late-time observations D. A. Perley, J. S. Bloom (UC Berkeley), C. Thoene (DARK, UCB), and N. R. Butler (UC Berkeley) report: On the night of 2007 July 18 (UT) we observed the field of GRB 070714B with the 10m Keck I Telescope (+LRIS) for 780 seconds in R and 920 seconds in g', starting at 14:30 UT. We detect a single, very faint source consistent with the position reported by Melandri et al. (GCN 6621) and inside the refined (GCN 6627) and improved [1] XRT error circles, in both filters. The location of this source is: RA = 03:51:22.23 Dec = +28:17:50.8 (+/- 0.4") The object has an approximate magnitude of R~25.5, calibrating relative to the USNO-B2.0 star at (03:51:21.5973, +28:18:55.810). It does not appear visibly extended in our imaging. This rules out the presence of a bright host galaxy and, comparing to the magnitude reported by Levan et al. (GCN 6630) suggests a rapid late-time afterglow decay rate of the afterglow. [1] http://astro.berkeley.edu/~nat/swift/xrt_pos.html //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 6657 SUBJECT: Short-Hard GRB070714B: PROMPT Observations DATE: 07/07/24 15:35:26 GMT FROM: Christine Weaver at FUNGRB/PROMPT C. Weaver, T. Brennan, M. Schubel, J. Styblova, J. Haislip, D. Reichart, M. Nysewander, A. LaCluyze, K. Ivarsen, J. A. Crain, A. Foster, and A. Trotter report: Skynet observed the localization of short-hard GRB 070714B (Racusin et al., GCN 6620) with two of the 16" PROMPT telescopes at CTIO beginning 4.5 hours after the burst in UBV. We do not detect the afterglow (Melandri et al., GCN 6621) to 3-sigma limiting magnitudes of B = 19.9 mag at a mean time of 4.9 hours after the burst (13 x 80 sec, calibrated to 14 USNO B1.0 stars) and V = 19.8 mag at a mean time of 5.5 hours after the burst (20 x 80 sec, calibrated to 13 NOMAD stars. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 6685 SUBJECT: VLA upper limit on short hard burst GRB 070714B DATE: 07/07/29 20:09:34 GMT FROM: Poonam Chandra at U Virginia/NRAO Poonam Chandra (NRAO/UVA) and Dale A. Frail (NRAO) report on behalf of the Caltech-NRAO-Carnegie GRB Collaboration: "We used the Very Large Array to observe the field of view toward GRB 070714B (GCN 6620), which was classified as short hard burst (GCN 6623), at a frequency of 8.46 GHz on 2007 July 29th at 17.47 UT. The radio afterglow of the GRB is undetected. The flux density of the GRB at the SWIFT-XRT afterglow position (GCN 6627) is -42 +/- 45 uJy. The National Radio Astronomy Observatory is a facility of the National Science Foundation operated under cooperative agreement by Associated Universities, Inc." //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 6689 SUBJECT: Swift/UVOT detection of GRB070714B DATE: 07/07/30 21:17:07 GMT FROM: Wayne Landsman at GSFC/SSAI W. Landsman (NASA/GSFC), F.E. Marshall (NASA/GSFC), and J. Racusin (PSU) report on behalf of the Swift/UVOT team: The Swift/UVOT observed the field of the short-hard burst GRB 070714B starting 70 s after the BAT trigger (Racusin et al. GCN Circ. 6620). Upper limits on individual exposures were reported by Landsman & Racusin (GCN Circ. 6632). We now combine all data obtained within the first 7350s and find detections in the white (4.5 sigma) and v (3.3 sigma) filters at the position of the source first reported by Melandri et al. (GCN Circ. 6621). The source is detected in each of the three UV filters at the ~2.9 sigma level. Presuming the detection in the UVW2 (2100 A) filter is real, an upper limit of ~1.3 can be set on the redshift. Filter Tstart Tstop Exp Mag (s) (s) (s) White 70 7143 628 20.95 ± 0.23 v 177 6117 1435 20.36 ± 0.32 7355 87569 4321 >20.9 (3 sigma) uvw1 607 6528 294 20.14 ± 0.38 11649 99315 9741 >22.1 (3 sigma) uvm2 583 6321 294 20.02 ± 0.37 10742 98409 8750 >22.3 (3 sigma) uvw2 687 7350 471 20.55 ± 0.37 16463 104208 5313 >22.1 (3 sigma) //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 6836 SUBJECT: GRB 070714B: host galaxy spectroscopic redshift DATE: 07/10/02 00:36:25 GMT FROM: John Graham at STScI J. F. Graham (STScI/JHU), A. S. Fruchter (STScI), A. J. Levan (U. Warwick), M. Nysewander (STScI), N. R. Tanvir (U. Leicester), T. Dahlen (STScI), D. Bersier (Liverpool John Moores U.), A. Pe'er (STScI) report on behalf of a larger collaboration: Gemini Nod & Shuffle spectroscopy on the host of GRB 070714B shows a single emission line at 7165 A. A photometric redshift based on Gemini grizJHK observations with GMOS and NIRI strongly implies that this is the 3727 A [O II] line. This places the host at a redshift of z=.92 The Swift BAT discovery data show the burst to have had a short, hard main component of three seconds duration followed by a soft, longer duration tail (Sakamoto et al. GCN 6623). The main component also shows a small spectral lag (Norris et al. GCN 6631). Both of these observations are consistent with GRB 070714B being a short GRB. This then would be the highest spectroscopically confirmed redshift of a short burst. The observed fluence of 7.2 x 10^-7 erg/cm^2 (Barbier et al. GCN 6638) at a redshift of z=.92 corresponds to an isotropic energy release of Eiso = 1.6 x 10^51 erg.