//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 13377 SUBJECT: GRB 120624B: Fermi GBM detection DATE: 12/06/25 09:39:54 GMT FROM: David Gruber at MPE D. Gruber (MPE), J. M. Burgess (UAH) and V. Connaughton (UAH) report on behalf of the Fermi GBM Team: "At 22:23:54.92 UT on 24 June 2012, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 120624B (trigger 362269436 / 120624933). The on-ground calculated location, using the GBM trigger data, is RA = 172.9, DEC = 6.5 (J2000 degrees, equivalent to 11 h 31 m 36 s, 06 d 30 '), with an uncertainty of 1 degree (radius, 1-sigma containment, statistical only; there is additionally a systematic error which is currently estimated to be 2 to 3 degrees). The angle from the Fermi LAT boresight is 71 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 3 bright, highly variable pulses starting ~ 250 s prior to the GBM trigger. The first pulse lasted ~100 s, the second pulse lasted ~120 s and the final pulse, which triggered GBM, lasted ~50 s. The event duration (T90) is about 271 s (50-300 keV). GBM triggered on the third episode because the first and second episode occurred during the brief part of the Fermi orbit at high geomagnetic latitude where triggering is currently disabled owing to particle activity and ensuing false triggers. The time-averaged spectrum from T0-270 s to T0+22.5 s is best fit by a Band function with Epeak = 566 +/- 20 keV, alpha = -0.85 +/- 0.01, and beta = -2.36 +/- 0.08. The event fluence (10-1000 keV) in this time interval is (8.980 +/- 0.007)E-03 erg/cm^2. The 1-sec peak photon flux measured starting from T0+11.4 s in the 10-1000 keV band is 846 +/- 17 ph/s/cm^2. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog." //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 13379 SUBJECT: GRB 120624B: Fermi-LAT Detection DATE: 12/06/25 10:18:47 GMT FROM: Giacomo Vianello at SLAC Giacomo Vianello (CIFS/SLAC), Daniel Kocevski (Stanford Univ.) report on behalf of the Fermi LAT Team: Fermi-LAT has detected high energy emission from the long, hard and bright GRB 120624B in ground analysis. The GRB was triggered on by the GBM on June 24, 2012 at 22:23:54.93 UTC, although the emission started ~250 seconds earlier (trigger 362269436, GCN 13377). The best GBM position was \~70 deg off-axis for the whole duration of the prompt emission (~270 seconds), outside of the Fermi/LAT nominal field of view for the standard data analysis. Using a non-standard data selection most sensitive in the tens-of-MeV energy range and with a broader acceptance, we significantly detected the burst between ~T0-250s and ~T0+20 s. The significance of the excess corresponds to 10 sigma. The light curve shows 3 peaks, with a total duration of \~270 s. This burst was bright enough to result in a Fermi spacecraft autonomous rapid repoint (ARR) maneuver, starting 100 s after the GBM trigger. Thus, the GBM position entered the LAT field of view at \~T0+100 s. A preliminary maximum-likelihood analysis of the E>100MeV P7TRANSIENT_V6 LAT data generated during the interval T0+100, T0+1.3 ks (until the GRB became occulted by the Earth) revealed a very significant transient source, with a spectrum well described by a power law of index -2.4 +/- 0.1 (68% c.l. statistical only). Using this analysis, we obtained the best LAT on-ground localization of: RA(J2000) = 170.73 deg Dec(J2000) = 9.48 deg with an error radius 0.45 deg (90% containment, statistical error only), which is 3.6 deg from the best GBM localization. The Zenith angle for this source was ~30 deg at the time of the trigger, thus very far from the Earth Limb. A Swift/ToO request has been submitted. The Fermi-LAT point of contact for this burst is Daniel Kocevski (kocevski@stanford.edu) //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 13381 SUBJECT: GRB 120624B: Swift detection of a burst DATE: 12/06/25 15:35:04 GMT FROM: Scott Barthelmy at NASA/GSFC S. D. Barthelmy (GSFC), J. Kennea (PSU), J. Racusin (GSFC) report on behalf of the Swift Team: At 22:19:51 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 120624B (trigger=525068) (also detected by Fermi-GBM, Circ 13377 and Fermi-LAT, Circ 13379). There were no real-time notices for this event because it occurred during a TDRSS outage (22:07 to 22:46), so none of the normal sequence of real-time notices were available. There was no automated slew to this BAT trigger because of a Moon constraint. The BAT on-board calculated location is RA, Dec 170.94, 8.93 (J2000), with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). We are in the process of getting the full data set downlinked, and will produce the nomal "refined" circular when it becomes available. [GCN OPS NOTE905jul12): Per author's request, the Trigger Time has been changed from 22:19:51 to 22:19:33.66 UT. We apologize for the mistake. We thank Frank Marshall for bring the mistake to our attention.] //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 13382 SUBJECT: Konus-Wind observation of GRB 120624B DATE: 12/06/25 17:39:20 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 intense hard GRB 120624B (GBM trigger 362269436: Gruber et al., GCN 13377; Fermi/LAT detection: Vianello & Kocevski, GCN 13379) triggered Konus-Wind at T0=80406.904s UT (22:20:06.904) The light curve shows multiple pulses grouped to three main episodes. A total duration of the burst is ~300 s. We note a quasi-periodic light curve structure (with T~3.6s) which is observed during the second bursting episode (from ~T0+120s to ~T0+150s). The emission is seen up to ~10 MeV. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB120624_T80406/ As observed by Konus-Wind the burst had a fluence of 2.75(-0.1,+0.1)x10-4 erg/cm2, and a 2.944-ms peak flux, measured from T0+235.28 s, of 3.0(-0.6,+0.7)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+253.952 s) is best fitted in the 20 keV - 10 MeV range with the GRB (Band) model, for which: the low-energy photon index alpha = -1.02 (-0.10, +0.12), the high energy photon index beta = -2.6 (-2.0, +0.4), the peak energy Ep = 530(-80, +90) keV, chi2 = 82.7/86 dof. The spectrum at the maximum count rate (measured from T0+229.634 to T0+237.824 s) is best fitted in the 20 keV - 10 MeV range with the GRB (Band) model, for which: the low-energy photon index alpha = -1.12 (-0.13, +0.21), the high energy photon index beta = -2.3 (<-1.8), the peak energy Ep = 1000(-450, +620) keV, chi2 = 77.8/86 dof. All the quoted results are preliminary. All the quoted errors are at the 90% confidence level. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 13383 SUBJECT: GRB 120624B: Fermi GBM fluence and peak photon flux correction DATE: 12/06/25 19:38:51 GMT FROM: David Gruber at MPE D. Gruber (MPE) reports on behalf of the Fermi GBM Team: "The peak flux and fluence values reported for GRB 120624B in GCN 13380 were erroneously calculated. The correct numbers are as follows: The fluence in the 10-1000 keV energy range is (1.916 +/- 0.002)E-04 erg/cm^2. This is consistent with the values reported by Konus-Wind (Golenetskii et al. GCN 13382). The 1-sec peak photon flux measured in the 10-1000 keV band is 17.7 +/- 0.3 ph/s/cm^2. We apologize for any inconvenience this has caused." //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 13384 SUBJECT: GRB 120624B, Swift-BAT refined analysis DATE: 12/06/25 20:53:53 GMT FROM: Takanori Sakamoto at NASA/GSFC T. Sakamoto (GSFC/UMBC), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC), E. E. Fenimore (LANL), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), D. M. Palmer (LANL), A. M. Parsons (GSFC), G. Sato (ISAS), M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (GWU) (i.e. the Swift-BAT team): Using the data set from T-60 to T+243 sec from recent telemetry downlinks, we report further analysis of BAT GRB 120624B (trigger #525068) (Vianello, et al., GCN Circ. 13379; Barthelmy, et al., GCN Circ. 13381). The BAT ground-calculated position is RA, Dec = 170.886, 8.933 deg which is RA(J2000) = 11h 23m 32.6s Dec(J2000) = +08d 56' 00.4" with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment). The partial coding was 86%. The mask-weighted light curve shows multiple overlapping episodes starting from T-25 sec. There are two main episodes going from T-10 to T+70 sec with a peak around T+35 sec, and the second episode starts T+120 sec and appears to end around T+200 sec, with peaks at T+140 sec and T+170 sec. But the data ends due to observing constraint and slewing to a pre-planned target. T90 (15-350 keV) is greater than 192 sec due to the end of the mask-weighted light curve when the source location left the field of view. The time-averaged spectrum from T-15.1 to T+192.8 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.17 +- 0.03. The fluence in the 15-150 keV band is 2.83 +- 0.04 x 10^-5 erg/cm2. The 1-sec peak photon flux measured from T+138.06 sec in the 15-150 keV band is 5.5 +- 0.2 ph/cm2/sec. All the quoted errors are at the 90% confidence level. The results of the batgrbproduct analysis are available at http://gcn.gsfc.nasa.gov/notices_s/525068/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 13385 SUBJECT: GRB 120624B: optical observations DATE: 12/06/25 22:47:56 GMT FROM: Alberto Castro-Tirado at Inst.de Astro. de Andalucia A. Sánchez-Caso (Gualba Observatory, Barcelona) and A. J. Castro-Tirado (IAA-CSIC Granada), on behalf of a larger collaboration, report: “Following the detection of GRB 120624B by Fermi/GBM, Fermi/LAT, Konus/Wind and Swift/BAT (GCNC 13377, 13378, 13379 and 13381 respectively), we have imaged the field with the 0.36m f/7 telescope at Gualba Observatory in Barcelona (Spain) starting on June 25 at 20:30 UT (i.e. about 22 hr post-burst). Within the Swift/BAT 3’ radius error box no optical afterglow candidate is identified for GRB 120624B. The limiting magnitude in the 300-s unfiltered image (with the crescent moon only 9 deg away) is 18.5.” This message can be quoted. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 13387 SUBJECT: GRB 120624B: NOT optical upper limit DATE: 12/06/25 23:32:09 GMT FROM: Dong Xu at Weizmann Inst D. Xu (WIS), A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), D. Malesani (DARK/NBI), D. Gandolfi (ESTEC/ESA), G. Leloudas (OKC, Stockholm) report on behalf of a larger collaboration: We observed the Swift/BAT field of GRB 120624B (Gruber et al., GCN 13377; Vianello& Kocevski, GCN 13379; Sakamoto et al., GCN 13384) using the 2.5m Nordic Optical Telescope (NOT) equipped with the ALFOSC camera, at La Palma, Canary Islands. Observations started at 21:26 UT on 2012-06-25 (i.e., 23.05 hr after the Fermi trigger) and a series of SDSS r-band frames with a total exposure time of 1250s were obtained, but were affected by the dusty calima from the Sahara desert. No new optical source was detected within the refined BAT error circle down to a 3-sigma limit of r(AB)~21.0. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 13389 SUBJECT: GRB 120624B: Discussion of Fermi and Swift measurements and future Swift observations DATE: 12/06/26 01:42:50 GMT FROM: Massimiliano de Pasquale at MSSL-UCL M. De Pasquale (UNLV), D. Gruber (MPE), J. M. Burgess (UAH), J. McEnery (NASA/GSFC), S. T. Holland (STSCI), S. Razzaque (GMU/NRL) and J. L. Racusin (NASA/GSFC), on behalf of the Swift, Fermi-GBM, and the Fermi-LAT teams: GRB 120624B, detected by Fermi-GBM (GCN 13377), Fermi-LAT (GCN 13379), Swift-BAT (GCN 13381), and Konus-Wind (GCN 13382) has very high fluence (1.9e-04 erg cm-2) and peak flux. The fluence of GRB 120624B in among the top 1.5% of bursts detected by Swift-BAT and the top 0.55% detected by Fermi-GBM. The GRB position is unfortunately within the Swift Moon constraint. Swift-XRT/-UVOT follow-up observations are planned when if comes out of Moon constraint on June 27.4. The refined BAT localization (GCN 13384) has an error radius of 1 arcmin (90% containment). There are 13 SDSS galaxies with r>24 within the BAT error circle. Analysis of the prompt emission suggests that the redshift of this event is z > ~0.3 if this burst obeys the Amati relation, with E_iso > ~4e+52 erg. We strongly encourage follow-up observations of GRB 120624B. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 13391 SUBJECT: GRB 120624B: NIR counterpart candidate from HAWKI DATE: 12/06/27 19:33:15 GMT FROM: Antonio de Ugarte Postigo at IAA-CSIC P. D'Avanzo (OaB/INAF), A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), S. Campana (OaB/INAF), J. Gorosabel (IAA-CSIC), S. Covino (OaB/INAF), J.P.U. Fynbo (DARK/NBI), and C.C. Thoene (IAA-CSIC) report on behalf of a larger collaboration, We observed the field of the very intense GRB 120426B detected by Fermi, Swift and Konus-Wind (Gruber et al., GCN 13377, Barthelmy et al. GCN 13381, Golenetskii et al. GCN 13382) with HAWKI at ESO's VLT (Paranal, Chile). Observations consisted of two epochs of 600s of integration in K-band covering the entire BAT error box (Sakamoto et al. GCN 13384). In the first epoch obtained 24.7 hr after the burst, we detect a faint source with a preliminary photometry K~20.8 compared to the 2MASS catalogue. This source is no longer visible in a second epoch 48.7 hr after the burst, where we estimate a 3-sigma limiting magnitude of K~21.6. The coordinates of the candidate nIR counterpart are (J2000 +/- 0.3"): R.A.: 11:23:29.67 Dec.: +08:55:28.7 We note that this source falls North East of a galaxy at a projected distance of ~1.7" from the center of the galaxy. We acknowledge excellent support from the Paranal staff, in particular Emanuela Pompei. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 13393 SUBJECT: GRB 120624B: GROND upper limits DATE: 12/06/28 09:14:58 GMT FROM: Patricia Schady at MPE/Swift P. Schady (MPE Garching), A. Nicuesa Guelbenzu, S. Klose, D. A. Kann (TLS Tautenburg), M. Nardini (Universita' degli Studi Milano-Bicocca), and J. Greiner (MPE Garching) report on behalf of the GROND team: We observed the field of the bright GRB 120624B (Fermi/GBM trigger 362269436/120624933, Gruber et al., GCN 13377, 13383; Konus-Wind detection, Golenetskii et al., GCN 13382; Swift trigger 525068, Sakamoto et al., GCN 13384) 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 at 23:17 UT on 2012-06-25, about 23 hrs after the GRB trigger and lasted for about 2 hrs. At the time of our observations, the angular distance of the source position to the Moon (last quarter) was just 10 degrees, significantly increasing the background in our optical images. In stacked images of the first 20min in the g'-band, of the first hour in r', i' and z' and the whole 2 hr period of J, H and K observations, we do not detect any new source at the position of the NIR afterglow candidate (D'Avanzo et al., GCN 13391), nor within the BAT error circle (Sakamoto et al., GCN 13384). The 3sigma limiting AB magnitudes are as follows g' > 23.3 r' > 24.0 i' > 23.5 z' > 23.4 J > 21.7 H > 21.1 K > 20.0 The galaxy close to the NIR afterglow candidate position mentioned in D'Avanzo et al. (GCN 13391) is clearly detected in our J and H-band images, with AB magnitudes J=20.9+/-0.2 and H=20.4+/-0.2. The above limits are derived based on calibrating the optical and NIR images against GROND zeropoints and 2MASS field stars respectively, and are not corrected for the Galactic foreground extinction corresponding to a reddening of E(B-V)=0.06 mag in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 13394 SUBJECT: GRB 120624B: Swift-XRT observations DATE: 12/06/28 10:24:28 GMT FROM: Owen Littlejohns at U of Leicester O.M. Littlejohns, P.A. Evans, K.L. Page (U. Leicester), A. Melandri, P. D'Avanzo (INAF-OAB) and J.Racusin (GSFC) reports on behalf of the Swift-XRT team: We have analysed 10 ks of XRT data for GRB 120624B (Barthelmy et al. GCN Circ. 13381), from 218.7 ks to 260.9 ks after the BAT trigger. The data are entirely in Photon Counting (PC) mode. Inside the BAT refined error circle (Sakamoto et al. GCN Circ. 13384) we find an uncatalogued X-ray source (S1) at RA, Dec = 170.8845, +8.9283 which is equivalent to: RA (J2000): 11 23 32.28 Dec(J2000): +08 55 42.0 with an uncertainty of 4.3 arcsec (radius, 90% confidence). This source lies 40 arcsec from the NIR object reported by D'Avanzo et al. (GCN Circ. 13391). We cannot determine at the present time whether the source is fading, the count-rate is approximately 2e-3 ct/sec in XRT. There is a second source (S2) at RA, Dec = 170.8670, +8.9319 which is equivalent to: RA (J2000): 11 23 28.07 Dec(J2000): +08 55 54.8 with an uncertainty of 4.2 arcsec (radius, 90% confidence). This source is 70 arcsec away from the BAT refined position, just outside the error circle. This source is 35 arcsec from the NIR counterpart. This source has a count-rate of approximately 1e-3 ct/sec, and again we cannot measure variability at this time. An image of the XRT field, with the two XRT sources, BAT error circle and NIR source marked, is available at http://www.swift.ac.uk/products/GRB120624B.png Further observations are planned. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 13395 SUBJECT: GRB 120624B: Further analysis of the HAWKI observations DATE: 12/06/28 10:50:37 GMT FROM: Antonio de Ugarte Postigo at IAA-CSIC A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), P. D'Avanzo (OaB/INAF), S. Campana (OaB/INAF), J. Gorosabel (IAA-CSIC), S. Covino (OaB/INAF), J.P.U. Fynbo (DARK/NBI), and C.C. Thoene (IAA-CSIC) report on behalf of a larger collaboration, In light of the recent XRT observation (Littlejohns et al., GCN13394) we have performed further analysis of the HAWKI data reported by D'Avanzo et al. (GCN 13391). Within the error circle of the XRT source we detect a point-like source and a galaxy at the following coordinates (J2000 +/- 0.3"): Galaxy 1A (RA, Dec): 11:23:32.08, +08:55:44.7 Point-like 1B (RA, Dec): 11:23:32.30, +08:55:42.5 We have performed image subtraction between our two K-band observations and we detect no variability of any of these sources between the two epochs. We also note that the galaxy is well detected in the SDSS with r=21.46 and a has a photometric redshift of 0.57+/-0.07. Our observations also cover the second XRT source that lies slightly outside the BAT error circle. Within this region we detect 2 extended sources, with coordinates (J2000 +/- 0.3"): Galaxy 2 (RA, Dec): 11:23:28.17, +08:55:57.6 Galaxy 3 (RA, Dec): 11:23:28.07, +08:55:56.8 Again, no variability is found within the second XRT position. These are detected as a single source in SDSS at r=21.55 and a photometric redshift of 0.43+/-0.07. [GCN OPS NOTE(28jun12): Per author's request, the "120426B" in the Subject-line was changed to "120624B:.] //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 13397 SUBJECT: GRB 120624B: Swift/UVOT Upper Limits DATE: 12/06/28 13:17:00 GMT FROM: Alice Breeveld at MSSL-UCL A. A. Breeveld (MSSL/UCL), F. E. Marshall (NASA/GSFC) and J.Racusin (GSFC) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 120624B 60hours 45mins after the BAT trigger (Barthelmy et al., GCN Circ. 13381). No optical afterglow is found at either of the XRT positions (Littlejohns et al. GCN 13394) nor the HAWKI position reported by D'Avanzo et al. (GCN 13391) in the initial UVOT exposures. Preliminary 3-sigma upper limits using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first finding chart (FC) exposure and subsequent summed exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag white_FC 218726 218864 136 >20.9 white 218865 260947 7027 >23.1 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.06 in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 13398 SUBJECT: GRB 120624B Further Swift-XRT analysis DATE: 12/06/28 20:30:51 GMT FROM: Owen Littlejohns at U of Leicester O.M. Littlejohns, P.T. O'Brien, P.A. Evans, K. Page (UL) and J.Racusin (GSFC) reports on behalf of the Swift-XRT team: Following the XRT observations of the BAT error circle for GRB 120624B reported in Littlejohns et al. (GCN Circ. 13394), we have compared the measured XRT flux of source S1 at 240 ks to that of bursts with similar or greater measured BAT fluence. Measurements of the XRT flux at approximately 240 ks for these bursts show that GRB 120624B lies at the faint end of the distribution of such bursts, should S1 prove to be the X-ray counterpart to GRB 120624B. Further XRT observations are planned for Tuesday the 3rd July (2012), with a total exposure time of 10 ks, to check if either source S1 or S2 has faded. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 13400 SUBJECT: GRB120624B: Chandra observations and afterglow detection DATE: 12/07/01 19:04:24 GMT FROM: Sergio Campana at INAF-OAB S. Campana (INAF-OAB), A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), A. J. Levan (U. Warwick) on behalf of a larger collaboration report: we imaged for 10 ks the field of GRB 120624B (Gruber et al. 2012, GCN 13377) with the Chandra ACIS-S starting on June 30, 2012 8:56:22 UT. Within the Swift/BAT 1 arcmin error circle (Barthelmy et al. 2012, GCN 13381) we detect two sources, already reported by Swift/XRT (Littlejohns et al. 2012, GCN 13394). S1 source is detected with wavdetect at a (preliminary) position: RA(J2000): 11 23 32.31 Dec(J2000):+08 55 42.8 The nominal positional error (90% c.l.) is 0.3 arcsec (not including any statistical error). The source is detected with 25 counts. S2 source is detected with wavdetect at a (preliminary) position: RA(J2000): 11 23 28.09 Dec(J2000):+08 55 57.0 The nominal positional error (90% c.l.) is 0.2 arcsec (not including any statistical error). The source is detected with 49 counts. We do not detect any X-ray source at the position of the NIR afterglow candidate (D'Avanzo et al. 2012, GCN13391). We note that S1 is brighter than S2 in Swift/XRT observations. The contrary occurs in the Chandra observation. We extrapolate the Swift XRT rates based on the Swift/XRT spectrum (Galactic column density of 3.6e20 cm-2, intrinsic column density of 2.4e21 cm-2 at redshift zero and a power law photon index of 2.52). Assuming this spectrum for both sources, we predict 78 counts for S1 and 59 counts for S2, with large uncertainties due to spectral modeling and statistics. Despite this, the disagreement between Swift/XRT predictions (78 counts) and Chandra observation (25 counts), likely indicate that S1 is the afterglow of GRB120624B. We thank Chandra director (H. Tananbaum) for granting this observation under the DDT program. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 13413 SUBJECT: GRB 120624B Suzaku WAM observation of the prompt emission DATE: 12/07/04 08:26:22 GMT FROM: Makoto Tashiro at Saitama U/Swift A. Sakamoto, M. Tashiro, Y. Terada, W. Iwakiri, T. Yasuda, K. Takahara, M. Asahina, S. Kobayashi, H. Ueno (Saitama U.), M. Akiyama, N. Ohmori, M. Yamauchi (Univ. of Miyazaki), K. Yamaoka, Y. E. Nakagawa (Waseda U.), Y. Hanabata, T. Kawano, K. Takaki, Y.Tanaka, R. Nakamura, M. Ohno, Y. Fukazawa (Hiroshima U.), S. Sugita (Nagoya U.), M. Kokubun, T. Takahashi (ISAS/JAXA),　Y. Urata, P. Tsai (NCU), K. Nakazawa, K. Makishima (Univ. of Tokyo),　on behalf of the Suzaku WAM team, report: The long GRB 120624B (Fermi/GRM; Gruber et al., GCN 13377,Fermi/LAT; Vianello et al., GCN 13379,Konus-Wind; Golenetskii et al., GCN 13382,Swift/BAT; Sakamoto et al., GCN 13384)　was detected by the Suzaku Wide-band All-sky Monitor (WAM) which covers an energy range of 50 keV - 5 MeV at 22:19:30.985 UT (=T0). The observed light curve shows a multi-peaked structure starting at T0+5 s, ending at T0+279 s, with a duration (T90) of about 274 seconds. The fluence in　100 - 1000 keV was 1.22(-0.06 +0.02) x 10^-4 erg/cm^2. The 1-s peak flux measured from T0+274.5s was 6.88(-2.11 +0.27) photons/cm^2/s in the same energy range. Preliminary result shows that the time-averaged spectrum from T0-20s to T0+285s is well fitted by a GRB Band model: the low-energy photon index alpha: -1.03(-0.16 +0.20), beta : -2.61 (-0.33, +0.20) and the peak energy Epeak: 628(-73 +84) keV (chi^2/d.o.f = 72.1/50). All the quoted errors are at statistical 90% confidence level, in which the systematic uncertainties are not included. ---- The light curves for this burst will be available at: http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/untrig/grb_table.html //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 13421 SUBJECT: GRB 120624B: mm detection at PdBI DATE: 12/07/06 06:34:59 GMT FROM: Alberto Castro-Tirado at Inst.de Astro. de Andalucia M. Bremer, J. M. Winters, S. König (IRAM Grenoble), A. de Ugarte Postigo and A. J. Castro-Tirado (IAA-CSIC Granada) on behalf of a larger collaboration, report: "Following the detection of the intense GRB 120624B by different spacecraft (GCNC 13379, 13381,13382), we have conducted follow-up observations at 3 mm with the PdBI on June 28 and July 2. Consistent with the position of the proposed X-ray afterglow (GCNC 13394, 13400) we detect a 1 mJy source (6 sigma). Observations are ongoing". This message can be quoted. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 13474 SUBJECT: GRB 120624B: VLA Observations DATE: 12/07/15 03:50:18 GMT FROM: S. Bradley Cenko at Caltech C. Bathurst (U. South Florida), D. A. Frail (NRAO) and S. B. Cenko (UC Berkeley) report on behalf of a larger collaboration: We have observed the field of the potential X-ray afterglow (GCN 13400, 13394) of the Fermi GBM (GCN 13377) and LAT (GCN 13379) GRB 120624B with the VLA. In observations taken on 2012 July 10.00 UT, at center frequencies of 5 GHz and 14 GHz, we find an unresolved radio source coincident with the position of the claimed X-ray afterglow (GCN 13400). The radio source is detected at 5-6 sigma significance and it has a rising spectrum consistent with the extrapolation of the 3mm PdBI detection (GCN 14321). Further 5 GHz observations were also made on June 26, June 29 and July 11. The 5 GHz flux density of the radio source shows no evidence for variability through these 4 epochs. Further observations are planned.