//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16000 SUBJECT: GRB 140320A: Swift detection of a burst DATE: 14/03/20 02:42:04 GMT FROM: David Palmer at LANL J. K. Cannizzo (NASA/UMBC), J. A. Kennea (PSU), A. Y. Lien (NASA/GSFC/ORAU), C. J. Mountford (U Leicester), D. M. Palmer (LANL) and B. Sbarufatti (INAF-OAB/PSU) report on behalf of the Swift Team: At 02:12:45 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 140320A (trigger=592544). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 281.857, -11.173 which is RA(J2000) = 18h 47m 26s Dec(J2000) = -11d 10' 21" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a double-peaked structure with two peaks separated by ~140 sec and a total duration of about 150 sec. The peak count rate was ~3700 counts/sec (15-350 keV), at ~0 sec after the trigger. No source was detected in 57 s of promptly downlinked data. We are waiting for the full dataset to detect and localise the XRT counterpart. Due to partial real-time telemetry, no further information is available at this time. However the burst was also detected by the Fermi-GBM instrument, verifying its reality. More details will be available following the next ground pass telemetry dump. Burst Advocate for this burst is J. K. Cannizzo (cannizzo AT milkyway.gsfc.nasa.gov). Please contact the BA by email if you require additional information regarding Swift followup of this burst. In extremely urgent cases, after trying the Burst Advocate, you can contact the Swift PI by phone (see Swift TOO web site for information: http://www.swift.psu.edu/too.html.) //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16001 SUBJECT: GRB 140320A: Fermi GBM observations suggest a short GRB DATE: 14/03/20 04:55:01 GMT FROM: George A. Younes at USRA/NASA/MSFC G. Younes (USRA/MSFC) and V. Connaughton (UAH) report on behalf of the Fermi GBM Team: "At 02:12:46.11 UT on 19 March 2014, the Fermi Gamma-Ray Burst Monitor Triggered and located GRB 140320A (trigger 416974369/140320092), which was also detected by Swift (Cannizzo et al. 2014, GCN 16000). The double peaked structure seen with BAT, with ~150 s separation, and reported by Cannizzo et al. is also visible with FERMI/GBM, however, a location analysis with GBM shows that the two peaks are unrelated. The first peak (trigger peak) is most likely due to a short/hard GRB located at RA~284.6 DEC~-5.0 deg, consistent with the BAT location. The second peak, 150 s after the trigger, is much softer and locates at RA~265.0 DEC~-28.0, the location of the bursting pulsar GRO J1744-28, which is currently active. Hence, we encourage multi-wavelength follow-up observations of this candidate short/hard GRB.” //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16003 SUBJECT: GRB 140320B: FTN optical afterglow candidate DATE: 14/03/20 10:18:18 GMT FROM: Cristiano Guidorzi at Ferrara U,Italy C. Guidorzi (U. Ferrara), A. Melandri (INAF-OAB), D. Kopac, A. Gomboc (U. Ljubljana), C.G. Mundell, F. Virgili (LJMU) on behalf of a larger collaboration report: The 2-m Faulkes Telescope North automatically began observing INTEGRAL GRB 140320B on March 20 at 09:31:27 UT (~4.6 min after the burst trigger). We find a fading uncatalogued object at coordinates RA(2000.0)= 09:42:14.17 Dec(2000.0)= +60:16:05.7 (error 1.0") with i=19.7 +- 0.1 mag at 16 minutes after the GRB, calibrated against nearby SDSS-I stars. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16004 SUBJECT: GRB 140320B: A long GRB detected by INTEGRAL DATE: 14/03/20 10:20:11 GMT FROM: Sandro Mereghetti at IASF/CNR S.Mereghetti (IASF-Milano), D.Gotz (CEA, Saclay), C.Ferrigno, E.Bozzo, E.Filippova (ISDC, Versoix), and J.Borkowski (CAMK, Torun) on behalf of the IBAS Localization Team report: a gamma ray burst lasting about 100 s has been detected by IBAS in the IBIS/ISGRI data at 09:26:00 UT of March 20. The refined coordinates (J2000) are: R.A.= 145.5409 deg DEC.= +60.2794 deg with an uncertainty of 2 arcmin (90% c.l.). A preliminary analysis gives a peak flux of 0.2 counts/cm2/s (20-200 keV, 1-s integration time) and a fluence in the same energy range of about 5e-7 erg/cmq. A plot of the light curve will be posted at http://ibas.iasf-milano.inaf.it/IBAS_Results.html //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16005 SUBJECT: GRB 140320B: ISON-NM optical observations DATE: 14/03/20 11:15:24 GMT FROM: Alexei Pozanenko at IKI, Moscow L. Elenin (KIAM), A. Volnova (IKI), I. Molotov (KIAM), A. Pozanenko (IKI) report on behalf of larger GRB follow-up collaboration: We observed of the field of the INTEGRAL GRB 140320B (Mereghetti et al., GCN 16004) with 0.4-m telescope of ISON-NM observatory starting on Mar., 20 (UT) 09:35:41. We took unfiltered images of 30 s exposures. We detect a fading optical afterglow of GRB 140320B (Guidorzi et al., GCN 16003) in a stacked image of total exposure 300 s and do not detect it in the next stacked image of the same exposure. Coordinates of the optical afterglow (J2000) 09 42 13.96 +60 16 05.9 (uncertainties of 1 arcsec) coincide with OT coordinates (Guidorzi et al., GCN 16003). Preliminary photometry of first stacked images is based on nearby USNO-B1.0 stars: UT mid, T0+ Filter Exposure, OT, err OT mid s 09:38:39 0.00878 none 10Ñ…30 19.1 0.2 09:44:40 0.03102 none 10Ñ…30 > 19.3 UpperlLimit //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16006 SUBJECT: GRB 140320B: Xinglong TNT upper limit DATE: 14/03/20 14:05:01 GMT FROM: L.P. Xin at NAOC L. P. Xin, J. Y. Wei, T. M. Zhang, Y. L. Qiu, J. S. Deng, J. Wang, X. H. Han and C. Wu on behalf of EAFON report: We began to observe GRB 140320B (Mereghetti et al., GCN 16004) with Xinglong 0.8-m TNT telescope at 12:15:47(UT) , 2.83 hrs after the burst. We do not detect the reported afterglow counterpart (Guidorzi et al., GCN 16003,Elenin et al., GCN 16005). in our combined images down to the upper limit of 21.8 mag in R band, calibrated by nearby USNO B1.0 R2 mag, at the mean time of 3.22 hrs after the burst. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16007 SUBJECT: GRB 140320C: A long GRB detected by INTEGRAL DATE: 14/03/20 14:48:47 GMT FROM: Sandro Mereghetti at IASF/CNR S.Mereghetti (IASF-Milano), D.Gotz (CEA, Saclay), C.Ferrigno, E.Bozzo, E.Filippova (ISDC, Versoix), and J.Borkowski (CAMK, Torun) on behalf of the IBAS Localization Team report: a gamma ray burst lasting about 30 s has been detected by IBAS in the IBIS/ISGRI data at 13:17:20 UT of March 20, 2014. The refined coordinates (J2000) are: R.A.= 134.4175 deg DEC.= +71.2002 deg with an uncertainty of 3 arcmin (90% c.l.). A preliminary analysis gives a peak flux of about 0.15 counts/cm2/s (20-200 keV, 1-s integration time) and a fluence in the same energy range of about 2e-7 erg/cmq. A plot of the light curve will be posted at http://ibas.iasf-milano.inaf.it/IBAS_Results.html //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16008 SUBJECT: GRB 140320C: FTN optical observations DATE: 14/03/20 15:10:15 GMT FROM: Andrea Melandri at INAF-OAB A. Melandri (INAF-OAB), C. Guidorzi (U. Ferrara), A. Gomboc (U. Ljubljana) and C. G. Mundell (LJMU) on behalf of a larger collaboration report: The 2-m Faulkes Telescope North automatically began observing INTEGRAL GRB 140320C (Mereghetti et al. GCN 16007) on March 20 at 13:21:39.3 UT (~4.3 min after the burst trigger). We do not find any fading candidate in our first 10s image within the entire INTEGRAL error circle down to a limiting magnitude or R>19.5 (5 sigma upper limit). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16009 SUBJECT: GRB 140320C: MASTER optical observations DATE: 14/03/20 15:12:11 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V.Yurkov, Yu.Sergienko, D.Varda, E.Sinyakov Blagoveschensk Educational State University, Blagoveschensk E. Gorbovskoy, V. Lipunov, M. Pruzhinskaya, D.Denisenko, V.Kornilov, N.Tyurina, P.Balanutsa, A.Kuznetsov, V.V.Chazov, D.Kuvshinov Lomonosov Moscow State University, Sternberg Astronomical Institute K.Ivanov, S.Yazev, N.M.Budnev, O.Gres, O.Chuvalaev, V.A.Poleshchuk Irkutsk State University A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Sennik Kislovodsk Solar Station of the Pulkovo Observatory V.Krushinski, I.Zalozhnih, A. Popov Ural Federal University, Kourovka Hugo Levato and Carlos Saffe Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE) Claudio Mallamaci, Carlos Lopez and Federico Podest Observatorio Astronomico Felix Aguilar (OAFA) MASTER II robotic telescope (MASTER-Net: http://observ.pereplet.ru) located in Blagoveschensk was pointed to the GRB140320C (Mereghetti et. al GCN 16007) 25 sec after notice time and 33 sec after trigger time at 2014-03-20 13:18:13 UT in two polarizations. We haven`t found optical transient within INTEGRAL error-box on single and coadd images. The 5-sigma upper limit has been about 16.8 mag on first single 10 sec image. On coadd of 11 first images with different exposures and total exosure time 610 sec the 5-sigma upper limit has been about 20.0 mag in bosh polarization. The message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16010 SUBJECT: GRB 140320A: Swift-XRT detection of an afterglow candidate DATE: 14/03/20 19:36:01 GMT FROM: Kim Page at U.of Leicester K.L. Page, C. Pagani (U. Leicester) and J.K. Cannizzo (NASA/UMBC) report on behalf of the Swift-XRT team: We have analysed 5 ks of XRT data for GRB 140320A (Cannizzo et al. GCN Circ. 16000), from 93 s to 11.8 ks after the BAT trigger. The data are entirely in Photon Counting (PC) mode. We detect a faint, uncatalogued X-ray source with a mean count rate of (5.9 +/- 1.3) x 10^-3 count s^-1, at a position of RA, Dec = 281.85583, -11.19333, which is equivalent to RA(J2000) = 18 47 25.4 Dec(J2000) = -11 11 36.9 with an uncertainty of 5.3 arcsec (radius, 90% confidence). This is 73 arcsec from the initial BAT position, within the BAT error circle. We cannot determine at this time whether the source is fading. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16011 SUBJECT: GRB 140320A: Enhanced Swift-XRT position DATE: 14/03/20 20:29:53 GMT FROM: Kim Page at U.of Leicester K.L. Page, C. Pagani, P.A. Evans and M.R. Goad (U. Leicester) report on behalf of the Swift-XRT team: Using 715 s of XRT Photon Counting mode data and 1 UVOT images, 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 = 281.85530, -11.19412 which is equivalent to: RA (J2000): 18 47 25.27 Dec (J2000): -11 11 38.8 with an uncertainty of 4.9 arcsec (radius, 90% confidence). This position may be improved as more data are received. The latest position can be viewed at http://www.swift.ac.uk/xrt_positions. Position enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans et al. (2009, MNRAS, 397, 1177). This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16012 SUBJECT: GRB 140320C: Mondy optical observations DATE: 14/03/20 20:31:29 GMT FROM: Alexei Pozanenko at IKI, Moscow A.Volnova (IKI), E. Klunko (ISTP), I. Korobtsev (ISTP), M. Eselevich (ISTP), A. Pozanenko (IKI) report on behalf of larger GRB follow-up collaboration: We observed the field of GRB 140320C (Mereghetti et al., GCN 16007) with AZT-33IK telescope of Mondy observatory starting on Mar. 20 (UT) 15:12:44. We obtained several images of 120 s exposure in R-filter. Within entire INTEGRAL error circle we identified sources which are not presented in the DSS2(R) image: N RA(J2000) Dec. (J2000) 1. 08 57 55.04 +71 13 36.5 2. 08 57 16.68 +71 10 10.6 3. 08 57 34.11 +71 11 55.0 (Uncertainty of all coordinates are 1 arcsec.) However, our images are more deep than DSS2(R), down to a limiting magnitude R~21, and at present time we cannot determine whether the sources are fading. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16013 SUBJECT: GRB 140320B: Swift-XRT detection of the afterglow DATE: 14/03/20 21:57:31 GMT FROM: Claudio Pagani at U of Leicester C. Pagani, K.L. Page, R.L.C. Starling, (U. Leicester) report on behalf of the Swift-XRT team: We have analysed 4 ks of XRT data for the INTEGRAL detected GRB 140320B (Mereghetti et al. GCN Circ. 16004), from 11.6 s to 23.1 ks after the trigger. The data are entirely in Photon Counting (PC) mode. An uncatalogued, fading X-ray source is detected inside the INTEGRAL error circle. Using 3683 s of XRT PC data and 4 UVOT images, 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 = 145.55932, 60.26822 which is equivalent to: RA (J2000): 09 42 14.24 Dec (J2000): +60 16 05.6 with an uncertainty of 1.7 arcsec (radius, 90% confidence). This is consistent with the optical position reported by Guidorzi et al. (GCN 16003) and Elenin et al. (GCN 16005). The light curve can be modelled with a power-law decay with an index of alpha=1.12 (+1.21, -0.05). A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 2.3 (+0.4, -0.3). The best-fitting absorption column is 6 (+8, -6) x 10^20 cm^-2, consistent with the Galactic value of 2.4 x 10^20 cm^-2 (Kalberla et al. 2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 2.8 x 10^-11 (3.0 x 10^-11) erg cm^-2 count^-1. If the light curve continues to decay with a power-law decay index of 1.12, the count rate at T+24 hours will be 7.8 x 10^-3 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.2 x 10^-14 (2.3 x 10^-14) erg cm^-2 s^-1. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16014 SUBJECT: GRB 140320A: Fermi GBM detection DATE: 14/03/20 22:12:14 GMT FROM: George A. Younes at USRA/NASA/MSFC G. Younes (USRA/MSFC), V. Connaughton (UAH), C. Meegan (UAH), and A. von Kienlin (MPE) report on behalf of the Fermi GBM Team: "At 02:12:46.11 UT on 20 March 2014, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 140320A (trigger 416974369/140320092), which was also detected by Swift (Cannizzo et al. 2014, GCN 16000). The GBM on-ground location, using the Fermi GBM trigger data, is consistent with the Swift/BAT location. The angle to the Fermi LAT boresight is 24 deg. using the Swift location. The GBM light curve consists of a single pulse with a duration (T90) of 1 s (50-300 keV). The time-averaged spectrum from T0-0.32 to T0+0.704 s is well fit by a simple power law function with index of -1.5 +/- 0.1. The event fluence (10-1000 keV) in this time interval is (4.0 +/- 0.5) E-07 erg/cm^2. The 0.064-sec peak photon flux measured starting from T0-0.128 s in the 10-1000 keV band is 5.0 +/- 1.0 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: 16015 SUBJECT: GRB 140320C: Swift-XRT detection of the X-ray afterglow DATE: 14/03/21 07:10:35 GMT FROM: Kim Page at U.of Leicester C. Pagani and K.L. Page (U. Leicester) report on behalf of the Swift-XRT team: We have analysed 4 ks of XRT data for the INTEGRAL detected GRB 140320C (Mereghetti et al. GCN Circ. 16007), from 19.5 s to 37.2 ks after the trigger. The data are entirely in Photon Counting (PC) mode. We detect an uncatalogued X-ray source. Using 1552 s of XRT Photon Counting mode data astrometrically corrected X-ray position (using the XRT-UVOT alignment and matching UVOT field sources to the USNO-B1 catalogue): RA, Dec = 134.39401, 71.19829, which is equivalent to: RA(J2000) =  08 57 34.56 Dec(J2000) = 71 11 53.9 with an uncertainty of 2.6 arcsec (radius, 90% confidence). This is 28 arcsec from the initial INTEGRAL position, within the INTEGRAL error circle. This is consistent with the optical source N3 from Volnova et al. (GCN 16012). The source has faded from a count rate of 0.013 (+/- 0.003) at 20.5 ks after the INTEGRAL trigger to 0.003 (+0.002,-0.001) by 33.9 ks, so we confirm it as the X-ray afterglow. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16016 SUBJECT: GRB 140320A: Confirmation of a fading X-ray afterglow DATE: 14/03/21 10:08:11 GMT FROM: Kim Page at U.of Leicester K.L. Page, C. Pagani, P.A. Evans (U. Leicester) & J.K. Cannizzo (NASA/UMBC) report on behalf of the Swift-XRT team: We have now analysed 9.8 ks of Swift-XRT data for GRB 140320A, between 93 s and 33.5 ks after the trigger. The X-ray source given by Page, Pagani & Cannizzo in GCN Circ. 16010 has now faded, with a 3-sigma upper limit on the count rate centred at 27 ks after the trigger of 1.2 x 10^-3 count s^-1. We therefore confirm this source as the X-ray afterglow of GRB 140320A. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16017 SUBJECT: GRB 140320C: Swift-XRT observations DATE: 14/03/21 10:34:38 GMT FROM: Claudio Pagani at U of Leicester C. Pagani, K.L. Page and P.A. Evans report on behalf of the Swift-XRT team: We have analysed 4.0 ks of XRT data for the INTEGRAL-detected burst: GRB 140320C, from 19.5 ks to 37.3 ks after the INTEGRAL trigger. The data are entirely in Photon Counting (PC) mode. An X-ray source is detected within the INTEGRAL error circle. Using 1552 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 = 134.39421, +71.19839 which is equivalent to: RA (J2000): 08h 57m 34.61s Dec(J2000): +71d 11' 54.2" with an uncertainty of 2.6 arcsec (radius, 90% confidence). This position is 27 arcsec from the INTEGRAL position. The light curve can be modelled with a power-law decay with a decay index of alpha=2.8 (+1.0, -1.7). A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 1.3 (+0.9, -0.3) and an absorption column consistent with the Galactic value of 3.6 x 10^20 cm^-2 (Willingale et al. 2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 5 x 10^-11 (5 x 10^-11) erg cm^-2 count^-1. If the light curve continues to decay with a power-law decay index of 2.8, the count rate at T+24 hours will be 2.4 x 10^-4 count s^-1 The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00020371. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16018 SUBJECT: GRB 140320A: Swift/UVOT Upper Limits DATE: 14/03/21 11:18:38 GMT FROM: Samantha Oates at MSSL S. R. Oates (UCL-MSSL) and J. K. Cannizzo (NASA/UMBC) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 140320A 3723 s after the BAT trigger (Cannizzo et al., GCN Circ. 16000). No optical afterglow consistent with the enhanced XRT position (Page et al., GCN Circ 16011) is detected 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 exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag v 3723 5358 393 >19.2 b 4543 10186 1149 >20.8 u 4338 5973 393 >19.7 w1 4133 5768 393 >19.8 m2 3928 5563 393 >20.0 w2 3518 5153 393 >20.2 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.51 in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16019 SUBJECT: GRB 140320B: Swift/UVOT Upper Limits DATE: 14/03/21 13:02:09 GMT FROM: Samantha Oates at MSSL S. R. Oates (UCL-MSSL) and R. L. C. Starling, (U. Leicester) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 140320B 11975 s after the INTEGRAL trigger (Mereghetti et al., GCN Circ. 16004). No optical afterglow consistent with the XRT position (Pagani et al., GCN Circ. 16013) and the FTN optical position (Guidorzi et al., GCN Circ. 16003) is detected 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 initial exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag white 11975 29408 5864 >23.1 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.02 in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16020 SUBJECT: GRB 140320A: Swift-BAT refined analysis DATE: 14/03/21 13:04:45 GMT FROM: Amy Lien at GSFC D. M. Palmer (LANL), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. K. Cannizzo (NASA/UMBC), J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/UMBC), C. B. Markwardt (GSFC), T. Sakamoto (AGU), M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU) (i.e. the Swift-BAT team): Using the data set from T-240 to T+962 sec from the recent telemetry downlink, we report further analysis of BAT GRB 140320A (trigger #592544) (Cannizzo, et al., GCN Circ. 16000). The BAT ground-calculated position is RA, Dec = 281.843, -11.188 deg which is RA(J2000) = 18h 47m 22.4s Dec(J2000) = -11d 11' 18.5" with an uncertainty of 2.4 arcmin, (radius, sys+stat, 90% containment). The partial coding was 88%. The mask-weighted light curve shows a double short-peaked structure starts at ~T-0.1 s. The second peak starts immediately at the end of the first peak at ~T+0.3 s, and ends at ~T+0.4 s. T90 (15-350 keV) is 0.45 +- 0.07 sec (estimated error including systematics). The time-averaged spectrum from T-0.08 to T+0.44 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.24 +- 0.36. The fluence in the 15-150 keV band is 4.9 +- 1.0 x 10^-8 erg/cm2. The 1-sec peak photon flux measured from T-0.32 sec in the 15-150 keV band is 0.6 +- 0.2 ph/cm2/sec. All the quoted errors are at the 90% confidence level. As noted in the Fermi/GBM circular (Younes et al.; GCN Circ. 16001), the pulse at ~T+140 s initially reported in Cannizzo, et al. (GCN Circ. 16000) is originated from a different source, the bursting pulsar GROJ1744-28. Therefore, GRB 140320A is a short burst. The results of the batgrbproduct analysis are available at http://gcn.gsfc.nasa.gov/notices_s/592544/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16021 SUBJECT: GRB 140320C: Swift/UVOT Upper Limits DATE: 14/03/21 13:05:13 GMT FROM: Samantha Oates at MSSL S. R. Oates (UCL-MSSL) and J. K. Cannizzo (NASA/UMBC) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 140320C 19435 s after the INTEGRAL trigger (Mereghetti et al., GCN Circ. 16007). No optical afterglow consistent with the XRT position (Pagani et al., GCN Circ. 16015; 16017) is detected 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 initial exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag white 20211 32984 1056 >22.1 v 20986 33302 1087 >20.5 u 19435 37277 1741 >21.4 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.07 in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16022 SUBJECT: GRB 140320C: Mini-GWAC prompt observation DATE: 14/03/21 14:03:44 GMT FROM: L.P. Xin at NAOC J. Y. Wei, L. P. Xin, Y. L. Qiu, J. S. Deng, J. Wang, X. H. Han, C. Wu, H. L. Huang, X. M. Meng, Y. F. Xuan and Y. Xu on behalf of EAFON report: Mini-GWAC system is located at Xinglong observatory, National Astronomical Observatories, China, including 6 mounts and 12 Canon 85/f1.2 cameras. Each mount is equipped with 2 cameras. For each camera, the Apogee U9000X CCD was used, which gives about 400 square degree of FOV. The total field of view of this system is about 5000 sq.deg. The field of INTERGRAL GRB 140320C (Mereghetti et al. GCN 16007) was monitored by Mini-GWAC system continuously during about 2 hrs before and 4 hrs after the burst. The exposure time for each frame is 10 sec. No any new optical counterpart in single frame was detected down to the 5 sigma upper limit of 13.1 mag calibrated by nearby USNO B1.0 R2 mag, at the epoch of prompt emission phase. Combining 5 frames after the burst trigger initially with total exposure time of 50 sec gives a 5 sigma upper limit of 13.7 mag. This message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16023 SUBJECT: IPN Triangulation of very intense GRB 140320D DATE: 14/03/21 16:28:50 GMT FROM: Dmitry Svinkin at Ioffe Institute K. Hurley and J. Goldsten, on behalf of the MESSENGER NS GRB team, S. Golenetskii, R. Aptekar, V. Pal'shin, D. Frederiks, D. Svinkin, and T. Cline, on behalf of the Konus-Wind team, A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo, and C. Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team, and S. Barthelmy, J. Cummings, N. Gehrels, H. Krimm, and D. Palmer, on behalf of the Swift-BAT team, report: The long-duration very intense GRB 140320D has been observed by Konus-Wind, INTEGRAL (SPI-ACS), Swift (BAT), and MESSENGER (GRNS), so far, at about 73297 s UT (20:21:37). The burst was outside the coded field of view of the BAT. We have triangulated it to a preliminary, 3 sigma error box whose coordinates are: --------------------------------------------- RA(2000), deg Dec(2000), deg --------------------------------------------- Center: 87.893 (05h 51m 34s) +85.429 (+85d 25' 46") Corners: 98.997 (06h 35m 59s) +86.721 (+86d 43' 15") 98.219 (06h 32m 53s) +87.023 (+87d 01' 23") 81.849 (05h 27m 24s) +84.026 (+84d 01' 35") 83.033 (05h 32m 08s) +83.741 (+83d 44' 28") --------------------------------------------- The error box area is 0.635 sq. deg, and its maximum dimension is 3.474 deg (the minimum one is 0.196 deg). This box may be improved. A triangulation map is posted at http://www.ioffe.ru/LEA/GRBs/GRB140320_T73298/IPN/ The time history and spectrum will be given in a forthcoming GCN Circular. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16024 SUBJECT: GRB 140320B: P60 detection of a very red afterglow DATE: 14/03/21 16:39:00 GMT FROM: Daniel Perley at Caltech D. A. Perley (Caltech) and S. B. Cenko (NASA-GSFC) report: The Palomar 60-inch telescope automatically responded to the INTEGRAL trigger for GRB 130420B (Mereghetti et al. GCN 16004) and began taking a series of 60-second exposures in the r, i, and z filters starting at 2014-03-20 09:31:41.744 (7.12 minutes after the trigger). The afterglow candidate reported by Guidorzi et al. (GCN 16003) is well-detected in the initial z-band exposure, weakly detected in the initial i-band exposure, and not detected in the initial r-band exposure. However, a weak r-band detection is recovered by stacking several images. The light curve (in the i- and z-band filters) shows a rise to a peak at around 15 minutes post-trigger, followed by a decline up until the end of our sequence at 1.3 hours after the GRB. Stacking the first 7 exposures in each filter, we estimate magnitudes of: r = 21.29 +/- 0.24 i = 20.07 +/- 0.09 z = 17.97 +/- 0.03 At a mid-UT time of approximately 09:46 in each filter (20 minutes after the trigger). The redder apparent color in i-z compared to r-i may suggest a highly reddened afterglow with host contribution to the r-band, or a reddened afterglow with a very strong 2175 dust feature at z~2.5, or a Lyman break in the i-band with some Lyman-alpha forest blueward (z~5). We encourage further observations, particularly in the NIR. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16025 SUBJECT: Konus-Wind observation of GRB 140320D DATE: 14/03/21 17:15:12 GMT FROM: Dmitry Svinkin at Ioffe Institute S. Golenetskii, R.Aptekar, D. Frederiks, V. Pal'shin, P. Oleynik, M. Ulanov, D. Svinkin, A. Tsvetkova, and T. Cline on behalf of the Konus-Wind team, report: A very intense, long-duration, hard-spectrum GRB 140320D (IPN triangulation: K. Hurley et al., GCN 16023) triggered Konus-Wind at T0=73298.804 s UT (20:21:38.804). The burst light curve shows a bright, double-peaked pulse with a total duration of ~50 s. The emission is seen up to ~10 MeV. As observed by Konus-Wind, the burst had a fluence of (2.1 +/- 0.1)x10^-4 erg/cm2, and a 64-ms peak flux, measured from T0+15.456 s, of (6.7 +/- 0.7)x10^-5 erg/cm2/s (both in the 20 keV - 10 MeV energy range). The time-averaged spectrum (measured from T0 to T0+45.568 s) is best fit in the 20 keV - 10 MeV range by the GRB (Band) function with the following model parameters: the low-energy photon index alpha = -0.83 (-0.03,+0.03), the high energy photon index beta = -2.75 (-0.32,+0.20), the peak energy Ep = 575 (-30,+32) keV, chi2 = 100/87 dof. The spectrum near the maximum count rate (measured from T0+15.360 to T0+15.872 s) is best fit in the 20 keV - 10 MeV range by the GRB (Band) function with the following model parameters: the low-energy photon index alpha = -0.30 (-0.11,+0.13), the high energy photon index beta = -2.59 (-0.62,+0.30), the peak energy Ep = 655 (-89,+102) keV, chi2 = 82/56 dof. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB140320_T73298/ All the quoted errors are at the 90% confidence level. All the quoted values are preliminary. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16026 SUBJECT: GRB 140320A: RATIR Optical and NIR Observations DATE: 14/03/21 23:44:39 GMT FROM: Owen Littlejohns at Az State U Owen Littlejohns (ASU), Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori Fox (UCB), J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (ORAU/GSFC), Eleonora Troja (GSFC), Enrico Ramirez-Ruiz (UCSC), José A. de Diego (UNAM), Leonid Georgiev (UNAM), Jesús González (UNAM), Carlos Román-Zúñiga (UNAM), Neil Gehrels (GSFC), and Harvey Moseley (GSFC) report: We observed the field of GRB 140320A (Cannizzo, et al., GCN 16000) with the Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the 1.5m Harold Johnson Telescope at the Observatorio Astronómico Nacional on Sierra San Pedro Mártir from 2014/03 21.42 to 2014/03 21.51 UTC (31.77 to 33.94 hours after the BAT trigger), obtaining a total of 1.40 hours exposure in the r and i bands and 0.56 hours exposure in the Z, Y, J, and H bands. For a source within the Swift-XRT error circle, in comparison with 2MASS, we obtain the following upper limits (3-sigma): r > 22.70 i > 22.38 Z > 21.23 Y > 21.27 J > 20.82 H > 20.24 These magnitudes are in the AB system and are not corrected for Galactic extinction in the direction of the GRB. We thank the staff of the Observatorio Astronómico Nacional in San Pedro Mártir. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16036 SUBJECT: GRB 140320C: Mondy optical observations and afterglow confirmation DATE: 14/03/25 12:03:24 GMT FROM: Alexei Pozanenko at IKI, Moscow A.Volnova (IKI), E. Klunko (ISTP), I. Korobtsev (ISTP), M. Eselevich (ISTP), A. Pozanenko (IKI) report on behalf of larger GRB follow-up collaboration: We observed the field of GRB 140320C (Mereghetti et al., GCN 16007) with AZT-33IK telescope of Mondy observatory starting on Mar. 20 (UT) 15:12:44 and Mar. 23 (UT) 15:37:46. Several images of 120 s exposure in R-filter ere obtained in both epochs. After receiving all data sets we refined our measurements of the optical source N3 reported early as one of a possible afterglow candidate (Volnova et al., GCN 16012). Enhanced position of the source is (J2000) 08 57 34.40 +71 11 54.7 (uncertainty of 0.35" is each coordinate) is within XRT error circle and apart 1.1" of the center of XRT localization (Pagani et al., GCN 16017). A photometry of the source: date UT start t-T0 Exp. Filter OT err (mid, days) (s) 2014-03-20 15:12:44 0.08918 1560 R 22.63 0.24 2014-03-20 15:38:46 0.12147 3840 R 23.14 0.28 2014-03-23 15:37:46 3.13782 6960 R 23.5 (3 sigma upper limit) is based on two USNO-B1.0 stars (R2 mags) N Id RA Dec. R 1 1612-0081687 08:57:32.78 +71:12:43.9 18.9 3 1611-0081293 08:57:55.56 +71:10:05.6 18.8 Based on our photometry we confirm the source N3 (Volnova et al., GCN 16012) is the afterglow of GRB 140320C. Finding chart can be found at http://grb.rssi.ru/GRB140320C/140320C_AZT33IK_fc.png //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16040 SUBJECT: GRB 140320D: Suzaku WAM observation of the prompt emission DATE: 14/03/29 03:42:36 GMT FROM: Tetsuya Yasuda at Saitama U T. Yasuda, M. Tashiro, Y. Terada, Y. Ishida, H. Ueno, S. Sugimoto S. Koyama, S. Takeda, T. Nagayoshi (Saitama U.), M. Yamauchi, N. Ohmori, M. Akiyama, R. Kinoshita (Univ. of Miyazaki), M. Ohno, K. Takaki, T. Kawano, R. Nakamura, S. Furui, Y. Fukazawa (Hiroshima U.), K. Yamaoka (Nagoya U.), S. Sugita (Ehime U.), W. Iwakiri(RIKEN), Y. Hanabata (ICRR), 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 bright, long, and IPN localized GRB 140320D (Hurley et al., GCN 16023; Golenetskii et al., GCN 16025) triggered the Suzaku Wide-band All-sky Monitor (WAM) which covers an energy range of 50 keV - 5 MeV at 20:21:38.309 UT (=T0). The observed light curve shows a multi-peaked structure lasting from T0-5 s to T0+50 s with a duration (T90) of about 22 seconds. The fluence in 100 - 1000 keV was 1.14 (+0.03, -0.04) x10^-4 erg/cm^2. The 1-s peak flux measured from T0+17 s was 35.4 (+0.8, -0.9) photons/cm^2/s in the same energy range. Preliminary result shows that the time-averaged spectrum from T0-10.5 s to T0+49.5 s is well fitted in 200 keV to 5 MeV by a power-law with exponential cutoff model: dN/dE ~ E^{-alpha} * exp(-(2-alpha)*E/Epeak) with alpha 0.99 (+0.12, -0.13), and Epeak 746 (+33, -31) keV (chi^2/d.o.f. = 72.1/48). Fitting by a GRB Band model yields the following parameters: the low-energy photon index alpha: -0.97 (+0.14, -0.13), the high-energy photon index beta: <-3.62, and the peak energy Epeak: 742 (+34, -22) keV (chi^2/d.o.f = 71.4/47). Due to the brightness of this burst, a 3% systematic error was added for low energy channels. 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 //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16043 SUBJECT: GRB 140320D: MASTER optical observations DATE: 14/03/30 08:42:43 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs K.Ivanov, S.Yazev, N.M.Budnev, O.Gres, O.Chuvalaev, V.A.Poleshchuk Irkutsk State University E. Gorbovskoy, V. Lipunov, M. Pruzhinskaya, D.Denisenko, V.Kornilov, N.Tyurina, P.Balanutsa, A.Kuznetsov, V.V.Chazov, D.Kuvshinov Lomonosov Moscow State University, Sternberg Astronomical Institute V.Yurkov, Yu.Sergienko, D.Varda, E.Sinyakov Blagoveschensk Educational State University, Blagoveschensk A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Sennik Kislovodsk Solar Station of the Pulkovo Observatory V.Krushinski, I.Zalozhnih, A. Popov Ural Federal University, Kourovka Hugo Levato and Carlos Saffe Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE) Claudio Mallamaci, Carlos Lopez and Federico Podest Observatorio Astronomico Felix Aguilar (OAFA) MASTER II robotic telescope located in Tunka (MASTER-Net: http://observ.pereplet.ru) have done a survey of the large area around IPN error box (Hurley et. al. GCN16023). The survey was started 2014-03-21 13:15:06 i.e. 16h 53m after the burst and proceeded during 5 hours. The 5 sigma unfiltered upper limit was ~17.5 m on single 180 image and ~18.8 m on coadd of 5 images with total exposure 900 s. We haven`t found credible optical afterglow candidate within IPN error box. The covarege map is available at http://master.sai.msu.ru/static/GRB/GRB140320D_map.png The message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 17845 SUBJECT: GRB 140320C: Swift ToO observations DATE: 15/05/21 18:04:32 GMT FROM: Phil Evans at U of Leicester P. A. Evans (U. Leicester) reports on behalf of the Swift team: Swift has initiated a ToO observation of the INTEGRAL GRB 140320C. Automated analysis of the XRT data will be presented online at http://www.swift.ac.uk/ToO_GRBs/00020371 Any uncatalogued X-ray sources detected in this analysis will be reported on this website and via GCN COUNTERPART notices. These are not necessarily related to the INTEGRAL event. 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; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8). This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 29371 SUBJECT: GRB 140320B: Swift-XRT refined Analysis DATE: 21/01/29 14:52:13 GMT FROM: Phil Evans at U of Leicester V. D'Elia (SSDC & INAF-OAR), A. D'Ai (INAF-IASFPA), J.A. Kennea (PSU), A. Tohuvavohu (U. Toronto), B. Sbarufatti (PSU), A.P. Beardmore (U. Leicester), P.A. Evans (U. Leicester), J.P. Osborne (U. Leicester), A. Melandri (INAF-OAB) and C. Pagani report on behalf of the Swift-XRT team: report on behalf of the Swift-XRT team: We have analysed 6.0 ks of XRT data for the INTEGRAL-detected burst GRB 140320B (Pagani et al. GCN Circ. 16013), from 12.0 ks to 29.4 ks after the INTEGRAL trigger. The data are entirely in Photon Counting (PC) mode. The refined XRT position is RA, Dec = 145.5611, +60.2690 which is equivalent to: RA (J2000): 09 42 14.66 Dec(J2000): +60 16 08.3 with an uncertainty of 3.6 arcsec (radius, 90% confidence). This position is 51 arcsec from the INTEGRAL position. We cannot determine at the present time whether the source is fading. A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 2.4 (+0.4, -0.3). The best-fitting absorption column is 7.2 (+7.1, -4.8) x 10^20 cm^-2, consistent with the Galactic value of 2.4 x 10^20 cm^-2 (Willingale et al. 2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 2.8 x 10^-11 (3.8 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 7.2 (+7.1, -4.8) x 10^20 cm^-2 Galactic foreground: 2.4 x 10^20 cm^-2 Excess significance: <1.6 sigma Photon index: 2.4 (+0.4, -0.3) The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00020370. This circular is an official product of the Swift-XRT team.