//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 15656 SUBJECT: GRB 140103A: Swift detection of a burst DATE: 14/01/03 00:55:31 GMT FROM: Scott Barthelmy at NASA/GSFC V. Mangano (PSU), S. D. Barthelmy (GSFC), D. Grupe (PSU), S. T. Holland (STScI), J. A. Kennea (PSU), D. M. Palmer (LANL), T. Sakamoto (AGU), B. Sbarufatti (INAF-OAB/PSU), C. A. Swenson (PSU) and T. N. Ukwatta (MSU) report on behalf of the Swift Team: At 00:30:43 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 140103A (trigger=582773). Swift slewed after 100 sec to the burst. The BAT on-board calculated location is RA, Dec 232.131, +37.749 which is RA(J2000) = 15h 28m 31s Dec(J2000) = +37d 44' 58" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve shows a single peak with a duration of about 15 sec. The peak count rate was ~1400 counts/sec (15-350 keV), at ~1 sec after the trigger. The XRT began observing the field at 00:33:31.6 UT, 168.3 seconds after the BAT trigger. No source was detected in the 2.5-s promptly available image. We are waiting for the full dataset to detect and localise the XRT counterpart. UVOT took a finding chart exposure of 150 seconds with the White filter starting 171 seconds after the BAT trigger. No credible afterglow candidate has been found in the initial data products. The 2.7'x2.7' sub-image covers 25% of the BAT error circle. The typical 3-sigma upper limit has been about 19.6 mag. The 8'x8' region for the list of sources generated on-board covers 100% of the BAT error circle. The list of sources is typically complete to about 18 mag. No correction has been made for the expected extinction corresponding to E(B-V) of 0.01. Burst Advocate for this burst is V. Mangano (vxm22 AT 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: 15660 SUBJECT: GRB 140103A: MASTER-Net optical observations DATE: 14/01/03 12:05:21 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs E. Gorbovskoy, V. Lipunov, D.Denisenko, V.Kornilov, D.Kuvshinov, N.Tyurina, P.Balanutsa, A.Kuznetsov Sternberg Astronomical Institute, Moscow State University A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Sennik Kislovodsk Solar Station of the Pulkovo Observatory V.Yurkov, Yu.Sergienko, D.Varda, E.Sinyakov Blagoveschensk Educational State University, Blagoveschensk K.Ivanov, S.Yazev, N.M.Budnev, O.Gres, O.Chuvalaev, V.A.Poleshchuk Irkutsk State University 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 Kislovodsk was pointed to the GRB140103A 22 sec after notice time and 303 sec after trigger time at 00:35:54 UT. On our first (60s exposure) set we haven`t found optical transient within SWIFT error-box (V. Mangano et. al. GCN 15656). The 5-sigma upper limit has been about 18.5 mag on first image and 21.2 mag on coadd of 20 images with total exposure 3600 sec and avagare time 01:18:38 UT i.e. 2890 sec after trigger. The message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 15664 SUBJECT: GRB 140103A, Swift-BAT refined analysis DATE: 14/01/03 14:14:10 GMT FROM: Takanori Sakamoto at AGU W. H. Baumgartner (GSFC/UMBC), S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/UMBC), V. Mangano (PSU), C. B. Markwardt (GSFC), D. M. Palmer (LANL), 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 140103A (trigger #582773) (Mangano, et al., GCN Circ. 15656). The BAT ground-calculated position is RA, Dec = 232.114, 37.752 deg which is RA(J2000) = 15h 28m 27.2s Dec(J2000) = +37d 45' 08.4" with an uncertainty of 1.7 arcmin, (radius, sys+stat, 90% containment). The partial coding was 48%. The mask-weighted light curve shows two peaks. The first weak peak starts at ~T-13 sec, peaks at ~T-11 sec and ends at ~T-6 sec. The second peak starts at ~T-4 sec, peaks at ~T+1 sec and ends at ~T+9 sec. T90 (15-350 keV) is 17.3 +- 1.9 sec (estimated error including systematics). The time-averaged spectrum from T-12.52 to T+6.94 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 6.0 +- 0.7 x 10^-7 erg/cm2. The 1-sec peak photon flux measured from T+0.39 sec in the 15-150 keV band is 2.1 +- 0.3 ph/cm2/sec. All the quoted errors are at the 90% confidence level. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 15666 SUBJECT: GRB 140103A: Swift-XRT refined analysis DATE: 14/01/03 15:17:05 GMT FROM: Vanessa Mangano at PSU V. Mangano (PSU) reports on behalf of the Swift-XRT team: We have analysed 5.1 ks of XRT data for GRB 140103A (Mangano et al. GCN Circ. 15656), from 172 s to 8.5 ks after the BAT trigger. The data comprise 2.6 ks in Windowed Timing (WT) mode with the remainder in Photon Counting (PC) mode. A faint X-ray source at the level of 0.05 counts/s is detected during PC mode observation. The refined XRT position is RA, Dec = 232.08747, +37.75917 which is equivalent to: RA (J2000): 15 28 20.99 Dec(J2000): +37 45 33.0 with an uncertainty of 3.6 arcsec (radius, 90% confidence). The 2.5 ks PC observation show a small scale flare and WT mode data are background dominated due to bright earth contamination and highly scattered. At present time we cannot asses if the source is fading. Further observations have been scheduled. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 15671 SUBJECT: GRB 140103A: Swift/UVOT Upper Limits DATE: 14/01/03 18:13:02 GMT FROM: Mike Siegel at PSU/Swift MOC M. H. Siegel and V. Mangano (PSU) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 140103A 172 s after the BAT trigger (Mangano et al., GCN Circ. 15656). No optical afterglow consistent with the XRT position (Mangano et al., GCN Circ 15666) 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 white_FC 172 321 147 >20.8 white 172 2581 361 >21.5 v 406 2631 252 >19.1 b 506 2557 233 >19.9 u 480 2704 252 >19.5 w1 456 2680 252 >19.6 m2 6760 8396 393 >20.0 w2 382 2607 252 >19.9 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.01 in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 15675 SUBJECT: GRB 140103A: P60 Observations DATE: 14/01/03 23:46:00 GMT FROM: S. Bradley Cenko at NASA/GSFC S. B. Cenko (NASA/GSFC) and D. A. Perley (Caltech) report on behalf of a larger collaboration: We imaged the field of GRB140103A (Mangano et al., GCN 15656) with the robotic Palomar 60 inch telescope. Observations were obtained in the i’ filter at a median time of 11:40 UT on 2014 January 3 (11.15 hr after the Swift trigger time). We do not detect any sources within the XRT localization (Mangano, GCN 15666). Using several nearby point sources from SDSS for reference, we calculate an upper limit of i’ > 22.9 mag at this time. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 15682 SUBJECT: GRB 140103A: Lulin Optical r-band Observations DATE: 14/01/05 01:37:12 GMT FROM: Yuji Urata at Nat. Central U. K.Y. Huang (NTNU), Y. Urata (NCU) on behalf of EAFON report: We observed the field of GRB 140103A (Mangano et al., GCN 15656) with r filter using the Lulin One-meter Telescope (LOT). The observation was started at 2014-01-03T20:48 and ended at 21:37 (20.7 hr after the trigger at the mid). We do not detect any sources within the XRT localization (Mangano et al., GCN 15666) brighter than 22.5. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 15693 SUBJECT: GRB 140103A: Swift XRT afterglow confirmation DATE: 14/01/06 19:17:38 GMT FROM: Vanessa Mangano at PSU V. Mangano (PSU) reports on behalf of the Swift-XRT team: We have analysed 6.9 ks of XRT data for GRB 140103A (Mangano et al. GCN Circ. 15656), from 153 s to 59.7 ks after the BAT trigger. The data comprise 2.6 ks in Windowed Timing (WT) mode (the first 7 s were taken while Swift was slewing) with the remainder in Photon Counting (PC) mode. We confirm that the X-ray source reported in Mangano et al. GCN Circ. 15666 is the afterglow of GRB 140103A. Its light curve can now be modelled with an initial power-law decay with an index of alpha=0.18 (+0.17, -0.19), followed by a break at T+3221 s to an alpha of 1.18 (+0.51, -0.28). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 2.6 (+0.5, -0.4). The best-fitting absorption column is 2.5 (+1.9, -1.3) x 10^21 cm^-2, in excess of the Galactic value of 1.3 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 2.7 x 10^-11 (6.1 x 10^-11) erg cm^-2 count^-1. A summary of the WT-mode spectrum is thus: Total column: 2.5 (+1.9, -1.3) x 10^21 cm^-2 Galactic foreground: 1.3 x 10^20 cm^-2 Excess significance: 3.0 sigma Photon index: 2.6 (+0.5, -0.4) The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00582773. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 15735 SUBJECT: GRB 140103A: AAO optical afterglow candidate DATE: 14/01/14 20:23:50 GMT FROM: Alexei Pozanenko at IKI, Moscow A. Volnova (IKI), R. Inasaridze (AAO), G. Inasaridze (AAO), V. Zhuzhunadze (AAO), Yu. Krugly (IA KhNU), I. Molotov (KIAM), A. Pozanenko (IKI) report on behalf of larger GRB follow-up collaboration: We observed the optical counterpart of the Swift GRB 140103A (Mangano et al., GCN 15656) with AS-32 (0.7m) telescope of Abastumani Observatory on Jan. 3 and 4. We obtained several unfiltered images of 120 s exposure during each observational set. In the refined XRT position (Mangano, GCN 15666) we do not detect any object in stacked images. However we found a fading object which is not present in SDSS catalog. The coordinates of the obsjet is (J2000) RA=15 28 20.73, Dec = +37 45 28.8 with uncertainity of 0.3" in each coordinate. The position of the fading object is 5.2" from the refined XRT position (Mangano, GCN 15666). Due to fading nature of the new object we suggest it as an afterglow of the GRB 140103A. Details of the photometry is following: Date T_start t-t0, Filter Exp., OT err. (UT) mid, d s 2014-01-03 01:21:18 0.03953 None 5*120 21.14 0.12 2014-01-03 01:34:40 0.05345 None 10*120 21.35 0.12 2014-01-03 02:01:21 0.07662 None 15*120 21.41 0.11 2014-01-04 01:47:48 1.08483 None 34*120 >22.3 (3 sigma) The photometry is based on SDSS DR9 stars and gri -> R transformations (Lupton): N SDSS_id R(Lupton) 1 J152814.09+374706.3 18.20 2 J152819.83+374538.8 15.61 Finding chart and a light curve of the afterglow can be found in http://grb.rssi.ru/GRB140103A/grb140103A_chart.png and http://grb.rssi.ru/GRB140103A/grb140103A_lc.PNG //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 15745 SUBJECT: GRB 140103A: optical upper limit DATE: 14/01/16 07:41:19 GMT FROM: Alina Volnova at SAI MSU A. Volnova (IKI), A. Ivanov (KubSU), V. Ivanov (KubSU), V. Lysenko (KubSU), I. Molotov (KIAM), A. Pozanenko (IKI) report on behalf of GRB follow-up collaboration: We observed the field of the Swift GRB 140103A (Mangano et al., GCN 15656) with 0.51-m f/8 telescope of Kuban State University Astrophysical Observatory on Jan. 3, starting 12 minutes after GRB trigger. We obtained several images of 30 s exposure in R-band. In the refined XRT position (Mangano, GCN 15666) we do not detect any object in stacked image. In particular we do not detected the optical afterglow candidate reported by Volnova et al. (GCN 15735). Details of the photometry are following: Date T_start t-t0, Filter Exp., OT (UT) mid, d s 2014-01-03 00:42:05 0.02314 R 80*30. >17.2 (3 sigma) //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 15746 SUBJECT: GRB 140103A: MASTER-Net early OT detection DATE: 14/01/16 15:20:24 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs E. Gorbovskoy, V. Lipunov, D.Denisenko, V.Kornilov, D.Kuvshinov, N.Tyurina, P.Balanutsa, A.Kuznetsov Lomonosov Moscow State University, Sternberg Astronomical Institute A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Sennik Kislovodsk Solar Station of the Pulkovo Observatory V.Yurkov, Yu.Sergienko, D.Varda, E.Sinyakov Blagoveschensk Educational State University, Blagoveschensk K.Ivanov, S.Yazev, N.M.Budnev, O.Gres, O.Chuvalaev, V.A.Poleshchuk Irkutsk State University 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 Kislovodsk was pointed to the SWIFT GRB 140103A (V. Mangano et. al. GCN 15656) 22 sec after notice time and 303 sec after trigger time at 00:35:54 UT (Gorbovskoy et al., GCN 15660). We finaly processed our data and found faint optical afterglow on ours coadd images starting from t_0 + 303 sec (exp=240 sec) the position reported by Volnova et. al. ( GCN 15744). The afterglow have a local maximum near 1560 sec after the burst, which, in the principle, can be result of long plato-like X-ray activity. Out photometry data available at table below. t_start t_mid t_finish t-t0 Exp. Mag. S/N coadd --------+----------+---------+------+-----+-------+---+----- 00:35:45 00:36:45 00:37:59 458 240 19.4 3.6 3 00:35:45 00:36:45 00:41:50 689 670 20.2 2.6 6 00:40:24 00:42:24 00:44:09 828 430 <20.7 --- 3 00:38:33 00:40:13 00:44:50 869 710 20.3 3.0 5 00:51:29 00:54:29 00:56:23 1562 540 19.8 4.3 3 00:48:06 00:51:06 00:58:08 1667 1080 20.2 3.8 6 01:08:39 01:11:39 02:11:41 6080 6660 22.0 2.5 37 The light curve available here http://master.sai.msu.ru/static/GRB/GRB140103A.png The message may be cited.