//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 15765 SUBJECT: GRB 140129B: Swift detection of a burst with an optical afterglow DATE: 14/01/29 13:07:18 GMT FROM: David Palmer at LANL M. G. Bernardini (INAF-OAB), P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC), P. A. Evans (U Leicester), J. A. Kennea (PSU), A. Y. Lien (NASA/GSFC/ORAU), F. E. Marshall (NASA/GSFC), A. Melandri (INAF-OAB), K. L. Page (U Leicester), D. M. Palmer (LANL), M. H. Siegel (PSU) and C. A. Swenson (PSU) report on behalf of the Swift Team: At 12:51:09 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 140129B (trigger=585149). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 326.763, +26.207 which is RA(J2000) = 21h 47m 03s Dec(J2000) = +26d 12' 24" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a single-peaked structure with a duration of about 2 sec. The peak count rate was ~1200 counts/sec (15-350 keV), at ~1 sec after the trigger. The XRT began observing the field at 12:52:16.5 UT, 67.1 seconds after the BAT trigger. Using promptly downlinked data we find an uncatalogued X-ray source with an enhanced position: RA, Dec 326.7574, 26.2065 which is equivalent to: RA(J2000) = 21h 47m 01.77s Dec(J2000) = +26d 12' 23.3" with an uncertainty of 2.1 arcseconds (radius, 90% containment). This location is 18 arcseconds from the BAT onboard position, within the BAT error circle. This position may be improved as more data are received; the latest position is available at http://www.swift.ac.uk/sper. We cannot determine whether the source is fading at the present time. A power-law fit to a spectrum formed from promptly downlinked event data gives a column density in excess of the Galactic value (5.58 x 10^20 cm^-2, Kalberla et al. 2005), with an excess column of 2.7 (+2.52/-2.09) x 10^21 cm^-2 (90% confidence). UVOT took a finding chart exposure of 150 seconds with the White filter starting 356 seconds after the BAT trigger. There is a candidate afterglow in the rapidly available 2.7'x2.7' sub-image at RA(J2000) = 21:47:01.67 = 326.75695 DEC(J2000) = +26:12:22.9 = 26.20637 with a 90%-confidence error radius of about 0.61 arc sec. This position is 1.5 arc sec. from the center of the XRT error circle. The estimated magnitude is 16.92 with a 1-sigma error of about 0.14. No correction has been made for the expected extinction corresponding to E(B-V) of 0.09. Burst Advocate for this burst is M. G. Bernardini (grazia.bernardini AT brera.inaf.it). 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: 15766 SUBJECT: GRB 140129B: MASTER OT confirmation DATE: 14/01/29 13:32:07 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 V.Yurkov, Yu.Sergienko, D.Varda, E.Sinyakov Blagoveschensk Educational State University, Blagoveschensk E. Gorbovskoy, V. Lipunov, D.Denisenko, V.Kornilov, D.Kuvshinov, N.Tyurina, N.Shatskiy, P.Balanutsa, D.Zimnukhov, A.Kuznetsov, V.V.Chazov Sternberg Astronomical Institute, Moscow State University V.Krushinski, I.Zalozhnih, A. Popov Ural Federal University, Kourovka A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Sennik Kislovodsk Solar Station of the Pulkovo Observatory 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 Tunka was pointed to the GRB140129B 106 sec after trigger time at 2014-01-29 12h 52m 55 s UT (expo time = 20 sec). On our first (20s exposure) set we found optical transient at the SWIFT optical transient position. The unfiltered magnitude is about ~ 14m. The message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 15770 SUBJECT: GRB 140129B: Enhanced Swift-XRT position DATE: 14/01/29 20:37:45 GMT FROM: Phil Evans at U of Leicester M.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester) report on behalf of the Swift-XRT team. Using 1682 s of XRT Photon Counting mode data and 5 UVOT images for GRB 140129B, 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 = 326.75708, +26.20648 which is equivalent to: RA (J2000): 21h 47m 1.70s Dec (J2000): +26d 12' 23.3" with an uncertainty of 1.7 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 was automatically generated, and is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 15774 SUBJECT: GRB 140129B, Swift-BAT refined analysis (probably not a short burst) DATE: 14/01/30 02:54:55 GMT FROM: Amy Lien at GSFC D. M. Palmer (LANL), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), M. G. Bernardini (INAF-OAB), 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-239 to T+963 sec from the recent telemetry downlink, we report further analysis of BAT GRB 140129B (trigger #585149) (Bernardini, et al., GCN Circ. 15765). The BAT ground-calculated position is RA, Dec = 326.764, 26.215 deg which is RA(J2000) = 21h 47m 03.3s Dec(J2000) = +26d 12' 53.1" with an uncertainty of 2.1 arcmin, (radius, sys+stat, 90% containment). The partial coding was 100%. The mask-weighted light curve shows a single short peak starts at ~T0, peaks at ~T+0.7 s, and ends at T+1.6 s. T90 (15-350 keV) is 1.36 +- 0.21 sec (estimated error including systematics). The time-averaged spectrum from T+0.08 to T+1.59 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 2.23 +- 0.33. The fluence in the 15-150 keV band is 7.1 +- 1.4 x 10^-8 erg/cm2. The 1-sec peak photon flux measured from T+0.17 sec in the 15-150 keV band is 0.9 +- 0.2 ph/cm2/sec. All the quoted errors are at the 90% confidence level. Although the T90 for this burst is shorter than 2 seconds, the power law index of the time-averaged spectrum is relatively soft for a short GRB. Therefore, we suspect that this burst might belong to the long-soft burst category with some burst emission missed due to background noise and detection limit. The results of the batgrbproduct analysis are available at http://gcn.gsfc.nasa.gov/notices_s/585149/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 15776 SUBJECT: GRB 140129B: MASTER OT early light curve DATE: 14/01/30 08:54:54 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V.A.Poleshchuk, O.Gres, K.Ivanov, S.Yazev, N.M.Budnev, O.Chuvalaev, Irkutsk State University D.Denisenko, E. Gorbovskoy, V. Lipunov, D.Kuvshinov, N.Tyurina, N.Shatskiy, P.Balanutsa, A.Kuznetsov, V.Kornilov, V.V.Chazov Lomonosov Moscow State University, Sternberg Astronomical Institute V.Yurkov, Yu.Sergienko, D.Varda, E.Sinyakov Blagoveschensk Educational State University, Blagoveschensk V.Krushinski, I.Zalozhnih, A. Popov Ural Federal University, Kourovka A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Sennik Kislovodsk Solar Station of the Pulkovo Observatory 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 Tunka was pointed to the GRB140129B 78 sec after notice time and 105 sec after trigger time at 2014-01-29 12:52:54 UT (Bernardini et al., GCN 15765). Such a long pointing time is due to internal mount pointing error under strong Siberian frost, which was automatically solved. A set of images with increasing exposures was obtained with the field at zenith distance 75 deg and setting. On our first (20s exposure) image we found optical transient at the SWIFT optical transient position. The unfiltered magnitude is about ~14m (Ivanov et al., GCN 15766). Our coordinates measured from the combination of 7 images are coincident with Swift UVOT position taking into account the error box reported by Bernardini et al., GCN 15765 and Swift-XRT position (Goad et al., GCN 15770): R.A. Dec. Err 21 47 01.71 +26 12 22.8 +/-0.5 arcsec The object is visible on 6 images, gradually fading below the detection limit on the 7th image. The results of our photometry are given in table below: T_start T-T_trig Tm-T_trig Exp,s Elevation Mag ---------------------------------------------------- 12:52:54 105 115 20 15.5 14.4 12:54:03 174 189 30 15.3 15.4 12:55:28 259 284 50 15.1 15.9 12:57:15 366 401 70 14.9 16.2 12:59:19 490 540 100 14.6 17.0 13:02:11 662 727 130 14.2 17.3 13:05:28 859 944 170 13.7 17.7 13:09:21 1091 1181 180 12.7 18.0 13:13:20 1330 1540 360 11.6 <18.4 # coadd 2 image In the table above 'T' is time of exposure beginning, 'Tm' is mid-exposure time. The power law slope is alpha = 1.42. The GRB140129B duration is small (T_90 < 2 sec, Palmer et al., GCN 15774), but spectrum is soft and this burst must be faint long GRB (Pal'shin, privet communication; Palmer et al., GCN 15774). Animation of seven frames by MASTER-Tunka is uploaded to http://master.sai.msu.ru/static/GRB/GRB140129B-MASTER-Tunka-anim.gif The light curve is available here: http://master.sai.msu.ru/static/GRB/GRB140129B_last.png Take the opportunity we would like to congratulate our first author from Siberia Vladimir Poleshchuk with the birth of the grandchild. The message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 15777 SUBJECT: GRB 140129B: Swift-XRT refined Analysis DATE: 14/01/30 10:57:45 GMT FROM: Maria Grazia Bernardini at INAF/Brera M. G. Bernardini (INAF-OAB) reports on behalf of the Swift-XRT team: We have analysed 1.8 ks of XRT data for GRB 140129B (Bernardini et al. GCN Circ. 15765), from 322 s to 6.9 ks after the BAT trigger. The data are entirely in Photon Counting (PC) mode. The enhanced XRT position for this burst was given by Goad et al. (GCN. Circ 15770). The light curve can be modelled with a power-law decay with a decay index of alpha=1.24 (+0.10, -0.09). A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 2.12 (+0.21, -0.20). The best-fitting absorption column is 1.1 (+0.5, -0.4) x 10^21 cm^-2, in excess of the Galactic value of 5.6 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 3.4 x 10^-11 (4.6 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 1.1 (+0.5, -0.4) x 10^21 cm^-2 Galactic foreground: 5.6 x 10^20 cm^-2 Excess significance: 1.9 sigma Photon index: 2.12 (+0.21, -0.20) If the light curve continues to decay with a power-law decay index of 1.24, the count rate at T+24 hours will be 1.8 x 10^-3 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 6.2 x 10^-14 (8.3 x 10^-14) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00585149. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 15780 SUBJECT: GRB 140129B: Swift/UVOT Detection DATE: 14/01/30 19:11:46 GMT FROM: Craig Swenson at PSU/Swift C. A. Swenson (PSU) and M. G. Bernardini (INAF-OAB) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 140129B 356 s after the BAT trigger (Bernardini et al., GCN Circ. 15765). A source consistent with the XRT position (Goad et al. GCN Circ. 15770) is detected in the initial UVOT exposures. The preliminary UVOT position is: RA (J2000) = 21:47:01.66 = 326.75691 (deg.) Dec (J2000) = +26:12:23.0 = 26.20638 (deg.) with an estimated uncertainty of 0.50 arc sec. (radius, 90% confidence). Preliminary detections using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the early exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag white 356 506 147 17.05 ± 0.03 v 663 5031 72 18.04 ± 0.20 b 588 608 20 17.90 ± 0.20 u 562 582 20 17.24 ± 0.17 w1 538 732 39 17.27 ± 0.16 m2 513 1089 58 17.57 ± 0.19 w2 638 1039 58 17.99 ± 0.19 The clear detection in all UVOT filters indicate this burst is at a redshift of z < ~1.5. The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.09 in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16055 SUBJECT: GRB 140129B: AAO optical upper limit DATE: 14/03/31 16:06:47 GMT FROM: Alina Volnova at SAI MSU GRB 140129B: AAO optical upper limit A. Volnova (IKI), R. 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 field of Swift GRB 140129B (Bernardini et al., GCN 15765) with AS-32 (0.7m) telescope of Abastumani Observatory starting on on Jan. 29 (UT) 15:23:49. We obtained several unfiltered frames with exposures of 120 s. Within the enhanced XRT circle (Goad et al., GCN 15770) we do not detect the afterglow (Bernardini et al., GCN 15765; Ivanov et al., GCN 15766). The details of the photometry are the following: UT start t-T0 Filter Exp. Uplim (mid, days) (s) (3 sigma) 15:23:49 0.10949 None 4*120 18.7 The photometry is based on SDSS stars, R mag (R mag obtained using ugriz transformations in BVRI (Lupton, 2005): SDSS id R J214659.19+261356.3 16.404 J214707.35+261127.0 15.825 J214657.00+261421.1 15.385