//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16248 SUBJECT: GRB 140512A: MASTER optical observations DATE: 14/05/12 19:49:04 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, V.Kornilov, D.Kuvshinov, A.Belinski, N.Tyurina, N.Shatskiy, P.Balanutsa, D.Zimnukhov, A.Kuznetsov, V.V.Chazov, D.Denisenko, A.Sankovich Lomonosov Moscow State University, Sternberg Astronomical Institute, Moscow State University 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.Krushinsky, I.Zalozhnih, A. Popov Ural Federal University, Yekaterinburg, 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 Tunka was pointed to the GRB140512A 171 sec after trigger time at 2014-05-12 19:34:40.212 UT. On our first (30s exposure) set we haven`t found optical transient within SWIFT error-box (ra=19 17 28 dec=-15 06 00 r=0.050000). The 5-sigma upper limit has been about 16.2 mag Observations were made in twilight. The message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16249 SUBJECT: GRB 140512A: Swift detection of a burst with an optical counterpart DATE: 14/05/12 19:56:20 GMT FROM: Scott Barthelmy at NASA/GSFC C. Pagani (U Leicester), S. D. Barthelmy (GSFC), D. N. Burrows (PSU), J. R. Cummings (NASA/UMBC), N. Gehrels (NASA/GSFC), J. A. Kennea (PSU), V. Mangano (PSU), C. J. Mountford (U Leicester), K. L. Page (U Leicester), B. Sbarufatti (INAF-OAB/PSU), M. H. Siegel (PSU), C. A. Swenson (PSU) and T. N. Ukwatta (MSU) report on behalf of the Swift Team: At 19:31:49 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 140512A (trigger=598819). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 289.371, -15.100 which is RA(J2000) = 19h 17m 29s Dec(J2000) = -15d 05' 59" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve shows a multi-peak event with a total duration of about 170 sec. The peak count rate was ~8000 counts/sec (15-350 keV), at ~122 sec after the trigger. The XRT began observing the field at 19:33:27.5 UT, 98.4 seconds after the BAT trigger. The position determined from promptly downlinked data differs significantly from the on-board position, suggesting that the XRT may have centroided on a cosmic ray; the initial XRT position notice should be treated with caution. Using promptly downlinked data we find an uncatalogued X-ray source located at RA, Dec 289.36925, -15.09492 which is equivalent to: RA(J2000) = 19h 17m 28.62s Dec(J2000) = -15d 05' 41.7" with an uncertainty of 3.6 arcseconds (radius, 90% containment). This location is 19 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. No spectrum from the promptly downlinked event data is yet available to determine the column density. UVOT took a finding chart exposure of 150 seconds with the White filter starting 106 seconds after the BAT trigger. There is a candidate afterglow in the rapidly available 2.7'x2.7' sub-image at RA(J2000) = 19:17:28.78 = 289.36991 DEC(J2000) = -15:05:39.2 = -15.09423 with a 90%-confidence error radius of about 0.61 arc sec. This position is 3.4 arc sec. from the center of the XRT error circle. The estimated magnitude is 15.01 with a 1-sigma error of about 0.14. No correction has been made for the expected extinction corresponding to E(B-V) of 0.16. Burst Advocate for this burst is C. Pagani (cp232 AT star.le.ac.uk). 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: 16250 SUBJECT: GRB 140512A: MASTER OT decay and early light curve DATE: 14/05/12 20:44:05 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs E. Gorbovskoy, V. Lipunov, V.Kornilov, D.Kuvshinov, A.Belinski, N.Tyurina, N.Shatskiy, P.Balanutsa, D.Zimnukhov, A.Kuznetsov, V.V.Chazov, D.Denisenko, A.Sankovich Lomonosov Moscow State University, Sternberg Astronomical Institute, Moscow State University 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 A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Sennik Kislovodsk Solar Station of the Pulkovo Observatory V.Krushinsky, I.Zalozhnih, A. Popov Ural Federal University, Yekaterinburg, 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 Tunka was pointed to the GRB140512A 171 sec after trigger time at 2014-05-12 19:34:40.212 UT in two polarizations. We definetly see OT (Pagani et. al. GCN 16249) on our images in bosh polarizations. The preliminary automatic light curve available at Tab.1 and here: http://master.sai.msu.ru/static/GRB/GRB140512A_lc.png Table 1. GRB140512B early automatic light curve. T_start T-T_trig mag 2014-05-12 19:34:44.3 175 sec 13.5 2014-05-12 19:36:36.3 287 sec 13.9 2014-05-12 19:38:21.9 392 sec 14.5 2014-05-12 19:39:43.7 474 sec 14.8 2014-05-12 19:41:05.3 556 sec 15.1 2014-05-12 19:42:26.3 637 sec 15.2 2014-05-12 19:43:47.3 718 sec 15.5 2014-05-12 19:45:56.8 847 sec 16.2 Our unfiltered magnitude is well described by a parity 0.8R + 0.2B (USNO-B1) The power low index alpha from 175 to 847 seconds after the trigger is 1.5 +- 0.1 (F ~ t-apha). We erraticly reported (Ivanov et. al. GCN 16248) that we don't see object earlier because of the wrong identification. We are sorry for it. The message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16251 SUBJECT: GRB 140512A: Mondy optical detection DATE: 14/05/12 20:47:05 GMT FROM: Alexei Pozanenko at IKI, Moscow E. Klunko (ISTP), A. Volnova (IKI), M. Eselevich (ISTP), I. Korobtsev (ISTP), A. Pozanenko (IKI) report on behalf of larger GRB follow-up collaboration: We observed the field of GRB 140512A (Pagani et al., GCN 16249) with AZT-33IK telescope of Sayan observatory (Mondy). We took several images in R-filter of 60 s exposure starting on May, 12 (UT) 19:56:58. We clearly detect a fading optical transient in the position reported early (Pagani et al., GCN 16249). A brightness of the OT in the first image is about R=16.7 (at (UT) 19:57:28, mid time). Observation is continuing. The finding chart can be found in http://grb.rssi.ru/GRB140512A/GRB140512A_AZT33IK_R_fc.png //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16253 SUBJECT: GRB 140512A: Optical observations from the 2.5 m NOT DATE: 14/05/13 03:16:22 GMT FROM: Antonio de Ugarte Postigo at IAA-CSIC A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), J. Gorosabel (IAA-CSIC, UPV-EHU), D. Xu (DARK/NBI), T. Kruehler (ESO), A.A. Djupvik (NOT), E. Gafton (OKC, Stockholm Univ.) and T. Libbrecht (Stockholm Univ.) report on behalf of a larger collaboration: We have observed the field of GRB 140512A (Pagani et al. GCN 16249) with the AlFOSC instrument on the 2.5 m Nordic Optical Telescope (La Palma, Spain), as part of the Stockholm remote observing school. Observations consisted of 3x300s imaging in R, starting at 02:10 UT (6.65 hrs after the burst). Observations were performed under variable seeing conditions of 2.0-2.5". Preliminary photometry, based on the USNO-B1.0 catalogue yields R~19.5 mag. Spectroscopic observations are ongoing. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16256 SUBJECT: GRB 140512A: Swift-XRT refined Analysis DATE: 14/05/13 07:56:04 GMT FROM: Phil Evans at U of Leicester P.A. Evans (U. Leicester), B.P. Gompertz (U. Leicester), V. D'Elia (ASDC), M. de Pasquale (INAF-IASFPA), A. Maselli (INAF-IASFPA), V. Mangano (PSU), M.C. Stroh (PSU), D.N. Burrows (PSU), J.P. Osborne (U. Leicester) and C. Pagani report on behalf of the Swift-XRT team: We have analysed 6.1 ks of XRT data for GRB 140512A (Pagani et al. GCN Circ. 16249), from 87 s to 12.6 ks after the BAT trigger. The data comprise 841 s in Windowed Timing (WT) mode (the first 9 s were taken while Swift was slewing) with the remainder in Photon Counting (PC) mode. The late-time light curve (from T0+4.6 ks) can be modelled with a power-law decay with a decay index of alpha=1.06 (+/-0.09). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 1.460 (+0.029, -0.016). The best-fitting absorption column is consistent with the Galactic value of 1.5 x 10^21 cm^-2 (Willingale et al. 2013). The PC mode spectrum has a photon index of 1.80 (+/-0.07) and a best-fitting absorption column of 2.02 (+0.28, -0.26) x 10^21 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 4.0 x 10^-11 (5.1 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 2.02 (+0.28, -0.26) x 10^21 cm^-2 Galactic foreground: 1.5 x 10^21 cm^-2 Excess significance: 3.4 sigma Photon index: 1.80 (+/-0.07) If the light curve continues to decay with a power-law decay index of 1.06, the count rate at T+24 hours will be 0.15 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 5.8 x 10^-12 (7.4 x 10^-12) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00598819. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16257 SUBJECT: GRB140512A : GROND observations DATE: 14/05/13 09:52:24 GMT FROM: Karla Varela at MPE J. Graham, K. Varela, C. Delvaux and J. Greiner (all MPE Garching) report on behalf of the GROND team: We observed the field of GRB 140512A (Pagani et al., GCN 16249) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120, 405) mounted at the 2.2m MPG telescope at La Silla Observatory (Chile). Observations started at 03:36 UT on May 13, about 8.0 hrs after the GRB trigger. They were performed at an average seeing of 1.7" and at an average airmass of 2.3. The afterglow discovered by Gorbovskoy et al. (GCN 16250) is detected in all optical bands and the JH bands. At a mean time of 04:02 UT, with a 264 s exposure in g’r’i’z’ bands and 240 s in JHK, we measure the following preliminary AB magnitudes: g'= 20.3 +/- 0.1 mag, r'= 19.7 +/- 0.1 mag, i'= 19.5 +/- 0.1 mag, z'= 19.3 +/- 0.1 mag, J = 19.0 +/- 0.1 mag, H = 18.6 +/- 0.1 mag, and K > 18.2 mag. The given optical and NIR magnitudes are calibrated against GROND zeropoints and 2MASS field stars in g'r'i'z and JHK respectively, and are not corrected for the Galactic foreground extinction corresponding to a reddening of E(B-V)=0.16 in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16255 SUBJECT: GRB 140512A: Enhanced Swift-XRT position DATE: 14/05/13 06:52:43 GMT FROM: Phil Evans at U of Leicester P.A. Evans, M.R. Goad, J.P. Osborne and A.P. Beardmore (U. Leicester) report on behalf of the Swift-XRT team. Using 5222 s of XRT Photon Counting mode data and 10 UVOT images for GRB 140512A, 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 = 289.37006, -15.09430 which is equivalent to: RA (J2000): 19h 17m 28.81s Dec (J2000): -15d 05' 39.5" with an uncertainty of 1.5 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: 16258 SUBJECT: GRB 140512A: Swift-BAT refined analysis DATE: 14/05/13 13:34:16 GMT FROM: Hans Krimm at NASA-GSFC T. Sakamoto (AGU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/UMBC), C. B. Markwardt (GSFC), C. Pagani (U Leicester), D. M. Palmer (LANL), 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 140512A (trigger #598819) (Pagani, et al., GCN Circ. 16249). The BAT ground-calculated position is RA, Dec = 289.366, -15.087 deg which is RA(J2000) = 19h 17m 27.9s Dec(J2000) = -15d 05' 14.8" with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment). The partial coding was 35%. The mask-weighted light curve shows a complex structure. The first group of multiple peaks begins at ~T-15 sec, reaches maximum at T+0 sec, and returns to background by ~T+40 sec. Then a second longer, brighter group of multiple peaks begins at ~T+85 sec, reaches maximum at T+120 sec and falls to background by T+170 sec. T90 (15-350 keV) is 154.8 +- 4.88 sec (estimated error including systematics). The time-averaged spectrum from T-22.84 to T+186.29 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.45 +- 0.04. The fluence in the 15-150 keV band is 1.4 +- 0.03 x 10^-5 erg/cm2. The 1-sec peak photon flux measured from T+121.96 sec in the 15-150 keV band is 6.8 +- 0.3 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/598819/BA/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16261 SUBJECT: GRB 140512A: Xinglong TNT optical observation DATE: 14/05/13 16:25:20 GMT FROM: L.P. Xin at NAOC L. P. Xin, X. F. Wang, J. Y. Wei, Y. L. Qiu, J. S. Deng, J. Wang, X. H. Han and C. Wu on behalf of EAFON report: We began to observe GRB 140512A (Pagani et al., GCN 16429) with Xinglong 0.8-m TNT telescope at 19:33:54 (UT) , 126 sec after the burst. The optical counterpart (Pagani et al., GCN 16429) was clearly detected in our white and R band images. A preliminary analysis shows that the brightness of the OT was fading from 13.0 mag to 17.0 mag, calibrated by nearby USNO B1.0 R2mag, during our observation epoch, with an index of 1.54 after fitting by a single power law. The message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16262 SUBJECT: GRB 140512A: Fermi GBM detection DATE: 14/05/13 18:01:19 GMT FROM: Matthew Stanbro at UAH/Fermi Matthew Stanbro (UAH) reports on behalf of the Fermi GBM Team: "At 19:31:42.50 UT on 12 May 2014, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 140512A (trigger 421615905 / 140512814) which was also detected by Swift (C. Pagani et al. 2014, GCN 16249). The GBM on-ground location, using the Fermi GBM trigger data, is consistent with the Swift/BAT location. The GBM light curve shows a complex structure, consisting of two main separated episodes with a total duration (T90) of about 148.0 s (50-300 keV). The time-averaged spectrum from T0-10.240 s to T0+152.578 s is well fit by a power law function with an exponential high-energy cutoff. The power law index is -1.33 +/- 0.03 and the cutoff energy, parameterized as Epeak, is 588 +/- 84 keV. The event fluence (10-1000 keV) in this time interval is (4.30 +/- 0.10)E-05 erg/cm^2. The 1.024-sec peak photon flux measured starting from T0+128.70 s in the 10-1000 keV band is 11.0 +/- 0.3 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: 16263 SUBJECT: GRB 140512A: Continued UVOT Observations DATE: 14/05/13 20:08:32 GMT FROM: Mike Siegel at PSU/Swift MOC B. Porterfield (PSU) and C. Pagani (U Leicester) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 140512A 106 s after the BAT trigger (Pagani et al., GCN Circ. 16249). We can confirm the detection of a fading source with the UVOT position RA(J2000) = 19:17:28.78 = 289.36991 DEC(J2000) = -15:05:39.2 = -15.09423 Preliminary detections and 3-sigma upper limits using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the finding chart (FC) exposures and subsequent exposures are: Filter T_start(s) T_stop(s) Exp(s) Mag white (fc) 106 256 293 14.91 +/- 0.07 white 106 1022 186 16.99 +/- 0.07 white 1175 6197 412 19.07 +/- 0.08 v 88 1072 68 15.97 +/- 0.09 v 4973 6608 393 18.68 +/- 0.15 b 574 1344 76 16.84 +/- 0.08 b 5793 5992 196 19.56 +/- 0.19 u (fc) 319 568 491 15.37 +/- 0.07 u 5587 7102 275 19.08 +/- 0.18 uvw1 697 1295 58 17.52 +/- 0.19 uvw1 5383 7018 393 20.10 +/- 0.34 uvm2 672 1270 77 >18.71 uvm2 5177 6812 393 >20.17 uvw2 624 1220 77 >19.05 uvw2 4769 6403 393 >20.47 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.162 in the direction of the burst (Schlegel et al. 1998). //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16265 SUBJECT: Konus-Wind observation of GRB 140512A DATE: 14/05/14 15:26:32 GMT FROM: Dmitry Svinkin at Ioffe Institute S. Golenetskii, R.Aptekar, D. Frederiks, V. Pal'shin, P. Oleynik, M. Ulanov, D. Svinkin, A. Tsvetkova, A.Lyssenko, and T. Cline on behalf of the Konus-Wind team, report: A long-duration GRB 140512A (Swift-BAT trigger 598819: Pagani et al., GCN 16249; Sakamoto et al., GCN 16258; Fermi-GBM detection: Stanbro, GCN 16262) triggered Konus-Wind at T0=70310.769 s UT (19:31:50.769). The light curve shows two separated multipeaked episodes: the first from ~T0-21 s to ~T0+12 s and the second longer and brighter from ~T0+88 s to ~T0+158 s. A total duration of the burst is ~179 s. As observed by Konus-Wind, the burst had a fluence of 4.8(-0.8,+2.0)x10^-5 erg/cm2, and a 256-ms peak flux, measured from T0+121.856 s, of 3.7(-1.2,+1.3)x10^-6 erg/cm2/s (both in the 20 keV - 10 MeV energy range). The time-averaged spectrum of the first bursting episode (measured from T0 to T0+8.448 s) is best fit in the 20 keV - 1.2 MeV range by a power law with exponential cutoff model: dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep) with alpha = -0.85 (-0.47,+0.61) and Ep = 279 (-69,+148) keV (chi2 = 62/60 dof). Fitting by a GRB (Band) model yields the same alpha and Ep, and an upper limit on the high energy photon index: beta < -2.1 (chi2 = 62/59 dof). The time-averaged spectrum of the second bursting episode (measured from T0+90.368 to T0+155.904 s) is best fit in the 20 keV - 6 MeV range by a power law with exponential cutoff model with the following parameters: alpha = -1.30 (-0.18,+0.21) and Ep = 466 (-124, +287) keV (chi2 = 79/79 dof). Fitting by a GRB (Band) model yields the same alpha and Ep, and an upper limit on the high energy photon index: beta < -1.9 (chi2 = 78/78 dof). The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB140512_T70310/ All the quoted errors are at the 90% confidence level. All the quoted values are preliminary. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16307 SUBJECT: GRB 140512A: MASTER prompt and afterglow optical observations DATE: 14/05/19 05:47:51 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs E. Gorbovskoy, V. Lipunov, V.Kornilov, D.Kuvshinov, A.Belinski, N.Tyurina, N.Shatskiy, P.Balanutsa, D.Zimnukhov, A.Kuznetsov, V.V.Chazov, D.Denisenko, A.Sankovich Lomonosov Moscow State University, 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 Tunka began observations of GRB140512A (Pagani et. al. GCN 16249) from pointing on several FERMI alerts. During the second set of observations by FERMI coordinates the GRB140512A error box was covered by our very wide field cameras MASTER VWF (FOV=2x384 square degrees, D=72mm, f/1.2, 1 pix = 22 arcsec) which installed on MASTER-II telescope. So we have 5 images with 5 second exptime without time gap since 2014-05-12 19:32:38 i.e. 29 sec. after the trigger and 49 sec. after the burst. We did not see optical transient (Pagani et. al. GCN 16249) at GRB140512A place. The 5-sigma upper limit on coadd of 5 MASTER-VWF images since 49 sec. till 74 sec. after the burst has been about 12.3 mag. The prompt images available here http://master.sai.msu.ru/static/GRB/GRB140512A.png . After several repointing by FERMI alerts MASTER II was pointed to the GRB140512A 171 sec after trigger time at 2014-05-12 19:34:40.212 UT in two polarizations by Swift coordinates. We definitely see OT on our images in both polarizations. Out final light curve is available in Tab. 1 Start time Exptime T-T_mid P/ eP/ P\ eP\ 2014-05-12T19:34:40.212 30 186 14,45 0,04 14,37 0,03 2014-05-12T19:36:37.643 60 318 14,72 0,05 14,74 0,04 2014-05-12T19:38:24.484 60 425 15,60 0,12 15,35 0,06 2014-05-12T19:39:47.447 60 508 15,41 0,10 15,65 0,07 2014-05-12T19:41:10.651 60 591 15,75 0,13 15,75 0,08 2014-05-12T19:42:32.663 60 673 15,98 0,16 15,94 0,09 2014-05-12T19:43:54.083 60 754 16,46 0,22 16,42 0,12 2014-05-12T19:45:56.002 170 931 16,37 0,20 16,79 0,15 2014-05-12T19:50:30.564 180 1211 17,50 0,39 16,84 0,15 2014-05-12T19:56:11.667 180 1552 16,82 0,27 17,57 0,22 P/ and P\ is a polarization filter which are oriented at an angle 45 and 135 degrees to RA axis respectivel. eP/ and eP\ is a error of P/ and P\ values. T is a GRB trigger time. The dimensionless Stokes parameter averaged over 5 first expositions is estimated to be less than observational error which equals to 2.9% (i.e. q = 0.3 +- 2.9%). So big error is connected to observation in a morning twilight (sun altitude ~ 12 d) and high object zenith distance (z ~ 70 d). Our unfiltered magnitude is well described by a parity 0.8R + 0.2B (USNO-B1) The message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16310 SUBJECT: GRB 140512A: Redshift from NOT DATE: 14/05/19 21:17:34 GMT FROM: Antonio de Ugarte Postigo at IAA-CSIC A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), J. Gorosabel (IAA-CSIC,UPV-EHU), D. Xu (DARK/NBI), D. Malesani (DARK/NBI), G. Leloudas (DARK/NBI),P. Jakobsson (U. Iceland), T. Kruehler (ESO), A.A. Djupvik (NOT), E. Gafton (OKC, Stockholm Univ.) and T. Libbrecht (Stockholm Univ.) report on behalf of a larger collaboration: Following the photometric observations of the counterpart of GRB 140512A (Pagani et al. GCN 16249) from the 2.5 m NOT (+ALFOSC) reported by de Ugarte Postigo et al. (GCN 16253) we obtained spectroscopic data. Observations consisted in 2x1800s exposures using Grism #4, which covers the range from 3800 to 9100. The mean observing epoch was May 13, 3:18:50 UT (7.78 hrs after the burst). The spectrum presents absorption features consistent with FeII and MgII at a common redshift of z=0.725, which we consider the most probable redshift for this event.