//////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 15864 SUBJECT: IPN Triangulation of extremely bright long GRB 140219A DATE: 14/02/20 13:42:33 GMT FROM: Dmitry Svinkin at Ioffe Institute K. Hurley and J. Goldsten, on behalf of the MESSENGER NS GRB team, I. G. Mitrofanov, D. Golovin, M. L. Litvak, and A. B. Sanin, on behalf of the HEND-Odyssey 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, K. Yamaoka, M. Ohno, Y. Hanabata, Y. Fukazawa, T. Takahashi, M. Tashiro, Y. Terada, T. Murakami, and K. Makishima, on behalf of the Suzaku WAM team, and V. Connaughton, M. S. Briggs, C. Meegan, V. Pelassa, and A. Goldstein, on behalf of the Fermi GBM team, report: The extremely bright long 140219A has been observed by Fermi/GBM (trigger 414531995), INTEGRAL (SPI-ACS), Suzaku (WAM), Mars Odyssey (HEND) and MESSENGER (GRNS), so far, at about 71192 s UT (19:46:32). We have triangulated it to a preliminary, 3 sigma error box whose coordinates are: --------------------------------------------- idx RA(2000),deg Dec(2000),deg --------------------------------------------- Center: 156.44 7.46 Corners: 1 157.06 10.06 2 156.56 7.30 3 155.51 4.70 4 156.31 7.66 --------------------------------------------- The error box area is 0.644 sq. deg, and its maximum dimension is 5.57 deg (the minimum one is 0.36 deg). This box can be improved. A triangulation map is posted at http://www.ioffe.ru/LEA/GRBs/GRB140219_T71192/IPN/ //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 15865 SUBJECT: GRB 140219A Tiled Swift observations DATE: 14/02/20 15:16:24 GMT FROM: Phil Evans at U of Leicester P. A. Evans (U. Leicester) reports on behalf of the Swift team: Swift has initiated a series of observations, tiled on the sky, of the IPN GRB 140219A. Automated analysis of the XRT data will be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00024 Any uncatalogued X-ray sources detected in this analysis will be reported on this website and via GCN COUNTERPART notices. The probability of finding serendipitous sources, unrelated to the IPN event is high: 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; and 2009, MNRAS, 397, 1177). This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 15866 SUBJECT: GRB 140219A: Fermi GBM Detection DATE: 14/02/20 19:08:45 GMT FROM: Binbin Zhang at UAH Bin-Bin Zhang (UAH) reports on behalf of the Fermi GBM Team: “At 19:46:32.24 UT on February 19 2014, the Fermi Gamma-Ray Burst Monitor triggered and located an extremely bright long GRB 140219A (trigger 414531995/140219824), which was also detected by INTEGRAL (SPI-ACS), Suzaku (WAM), Mars Odyssey (HEND) and MESSENGER (GRNS) (Holland et al., GCN 15825). The GBM on-ground location is consistent with IPN error box. The GRB position was occulted by the Earth during the brightest period of emission and only the weaker tail emission was observed by GBM. Using the available data we find that the GBM light curve consists of a multiple-peak structure with a duration of about 80 s (50-300 keV). The time-averaged spectrum from T0-2 s to T0+78 s is well fit with a power law function with an exponential high energy cutoff, which is parameterized as Epeak = 194 +/- 61 keV, alpha = -1.3 +/- 0.1. The event fluence (10-1000 keV) in this time interval is (4.9 +/- 0.6)E-06 erg/cm^2. The 1.0-sec peak photon flux measured starting from T0-0.9 s in the 10-1000 keV band is 3.2 +/- 0.2 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: 15867 SUBJECT: GRB 140219A: Fermi-LAT detection of a burst DATE: 14/02/20 20:47:28 GMT FROM: Sylvain Guiriec at UAH S. Guiriec (GSFC/CRESST/UMD), J. Racusin (GSFC), G. Vianello (Stanford) and E. Bissaldi (University & INFN Trieste), report on behalf of the Fermi-LAT team: At 19:46:32.2 on February 19, 2014, Fermi LAT detected high-energy emission from GRB 140219A, which was also detected by Fermi-GBM (trigger 414531995 - Zhang et al., GCN 15866) and located by IPN (Hurley et al., GCN 15864). GRB 140219A was not observable by LAT until ~T0+500 s due to Earth occultation and it remained in the LAT field of view from ~T0+500 s until T0+2300 s. An analysis of the LAT data over a period covering ~T0+500 s to ~T0+2300 s reveals a marginal detection with a TS of about 25 using the center of the IPN error box. The best LAT on-ground location is RA, Dec 158.2, 7.2 (J2000). The 90% containment region (statistical error only) is asymmetrical with a width of 2.75 deg and a height of 1.65 deg compatible with the IPN contour (see http://fermigrb.stanford.edu/GRB140219A_tsmap.jpg). The highest energy photon with a probability of being associated with the GRB > 90% is a 1.6 GeV photon at T0+1350 s. The Fermi LAT point of contact for this burst is Sylvain Guiriec (sylvain.guiriec*@nasa.gov *). The Fermi LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 15870 SUBJECT: Konus-Wind observation of exceptionally bright GRB 140219A DATE: 14/02/21 11:42:29 GMT FROM: Valentin Pal'shin at Ioffe Inst S. Golenetskii, R.Aptekar, D. Frederiks, V. Pal'shin, P. Oleynik, M. Ulanov, D. Svinkin, and T. Cline on behalf of the Konus-Wind team, report: The long-duration, exceptionally bright and hard GRB 140219A (localized by IPN: Hurley et al., GCN 15864; GBM detection: Zhang, GCN 15866; LAT detection: Guiriec et al., GCN 15867) triggered Konus-Wind at T0=71162.611 s UT (19:46:02.611). The burst light curve shows an extremely bright multi-peaked pulse with a duration of ~2.5 s followed by a less intense multi-peaked emission episodes until ~T0+26 s and a very weak tail until ~T0+35 s. The emission is seen up to ~18 MeV. As observed by Konus-Wind, the burst had a fluence of (1.14 ± 0.02)x10^-3 erg/cm2, and a 16-ms peak flux, measured from T0+0.240 s, of (1.44 ± 0.12)x10^-3 erg/cm2/s (both in the 20 keV - 10 MeV energy range). The time-integrated spectrum (measured from T0 to T0+38.912 s) is best fit (in the 26 keV - 18 MeV range) by a GRB (Band) model with the following model parameters: the low-energy photon index alpha = -1.07 ± 0.01, the high energy photon index beta = -3.26(-0.88,+0.38), the peak energy Ep = 2777 ± 70 keV, chi2 = 112.7/96 dof. The spectrum of the main pulse (measured from T0 to T0+2.304 s) is best fit (in the 26 keV - 18 MeV range) by a GRB (Band) model with the following model parameters: the low-energy photon index alpha = -0.65 ± 0.04, the high energy photon index beta = -3.28(-0.89,+0.39), the peak energy Ep = 3363 ± 141 keV, chi2 = 47.9/77 dof. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB140219_T71162/ All the quoted errors are at the 90% confidence level. All the quoted results are preliminary. The derived peak flux and Epeak are the highest ever measured for GRBs with Konus-Wind during almost 20 years of its continuous observations: the peak flux is ~50% higher than the previous record holder, GRB 110918A, with the measured peak flux of ~0.9x10^-3 erg/cm2/s (Frederiks et al. ApJ, 779, 151 (2013)). Follow-up observations are strongly encouraged. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 15871 SUBJECT: GRB 140219A: MASTER before and after GRB observational arguments of the exceptionally Dark GRB DATE: 14/02/21 15:42:34 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs E. Gorbovskoy, V. Lipunov, 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 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 VWF robotic very wide field cameras (FOV=2x384 square degrees, D=72mm, f/1.2, 1 pix = 22 arcsec) installed on MASTER-II robotic telescope in Tunka covered full IPN error box (Hurley et. al. GCN15864) for very short time before and after the trigger. Fortunatelly we have set of 26 continous 5 seconds exposure images since 19:43:16 to 19:45:21 UT i.e. since 196 s to 71 s before the trigger and set of continous 5 seconds exposure images since 19:47:01 to 19:58:31 UT i.e. 3 sec after Notice Time and 29 s after the trigger. We haven`t found credible optical transient with 3-sigma upper limit 10.5m on single and about 12.0 m on coadd (20 x 5 sec = 100 sec) images. The Very Wide Field Cameras observation schedule with respect to GRB light curve (S. Golenetskii, R.Aptekar, D. Frederiks, V. Pal'shin et al., GCN 15870) is available at http://master.sai.msu.ru/static/GRB/GRB140219A_schedule.png The first images movie available here http://master.sai.msu.ru/static/GRB/GRB140219A_IPN_single.gif The coadd images move available here http://master.sai.msu.ru/static/GRB/GRB140219A_IPN_coadd1.gif http://master.sai.msu.ru/static/GRB/GRB140219A_IPN_coadd2.gif The same MASTER VWF robotic very wide field cameras installed on MASTER-II robotic telescope in Blagoveschensk also made the observations of IPN error box after the trigger. However the upper limit on them on 1.5m worse than in Tunka due to adverse weather conditions. MASTER II robotic telescope (MASTER-Net: http://observ.pereplet.ru) located in Tunka was pointed to the GRB140219A 78 sec after trigger time at 2014-02-19 19:47:50.943 UT by FERMI GBM trigger N414531995 in two polarizations. On our first (10s exposure) set we haven`t found optical transient within 4 sq. degree center part of FERMI-GBM first error-box (ra=10 11 55 dec=+12 14 00 radius = 32, Zhang et. al. GCN 15866) . The 5-sigma upper limit has been about 15.1 mag. MASTER II robotic telescope (MASTER-Net: http://observ.pereplet.ru) located in Blagoveschensk was pointed to the GRB140219A 30 sec after notice time and 57 sec after trigger time at 2014-02-19 19:47:29.9 UT by FERMI GBM trigger .414531995 in two polarizations. On our first (10s exposure) set we haven`t found optical transient within 4 sq. degree center part of FERMI-GBM first error-box (ra=10 11 55 dec=+12 14 00 radius = 32 ). The 5-sigma upper limit has been about 14.9 mag. After IPN notice (Hurley et. al. GCN15864) we cover full IPN and LAT (Guiriec et. al GCN 15867) error boxes in survey mode using 3 fields on two MASTER II telescope in Tunka and Blagoveschensk. The first images was obtained 18h 22m after trigger time at 2014-02-20 14:08:49 with upper limit 19.5 m in Tunka and 18.0 m in Blagoveschensk. We also haven`t found credible optical transient up to 20.5 m here. The obseravtions argue that GRB 140219A is extremely dark GRB with low Optical to Gamma Emission Ratio: F_opt/F_gamma <~ 1 : 130 000 On the figure ( http://master.sai.msu.ru/static/GRB/GRB140219A_schedule.png ) you can find the Gamma-Optic diagramm for the prompt fluence of GRBs observed by MASTER (Gorbovskoy et. al Astronomy Reports, Volume 57, Issue 4, pp.233-286). The message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 15872 SUBJECT: GRB 140219A: results from Swift XRT and UVOT tiled observations DATE: 14/02/21 17:19:26 GMT FROM: Vanessa Mangano at PSU V. Mangano (PSU), P. A. Evans (U. Leicester), F. E. Marshall (NASA/GSFC) report on behalf of the Swift Team: Swift-XRT has observed the central part of the error region of the IPN GRB 140219A in a series of observations tiled on the sky. The total exposure time is 5.9 ks spread over 3 fields; the maximum exposure within the sky observed was 3.9 ks. The observations started 70.3 ks after the IPN trigger. Within these data there are 2 objects which are not catalogued in X-rays. At the present time we cannot be sure which, if either, of these is the afterglow. Source details: Source 1 RA: 156.49768 = 10h 25m 59.44s (J2000) Dec: 7.52128 = +07d 31' 16.6" (J2000) Err: 10.0 (radius, 90% confidence) Exposure time: 2.2 ks Online products: http://www.swift.ac.uk/xrt_products/TILED_GRB00024/index_1.php Source 2 RA: 156.44031 = 10h 25m 45.67s (J2000) Dec: 7.96378 = +07d 57' 49.6" (J2000) Err: 10.0 (radius, 90% confidence) Exposure time: 1.5 ks Online products: http://www.swift.ac.uk/xrt_products/TILED_GRB00024/index_2.php UVOT observed both of the XRT source regions. In the region for XRT Source 1, UVOT finds a bright optical source that we identify with the star SDSS J102559.46+073114.1. UVOT finds no optical counterpart to XRT Source 2 in a 803-second exposure with the white filter starting 82.3 ks after the trigger. The preliminary 3-sigma upper limit using the UVOT photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) is 21.7 mag. No correction has been made for Galactic extinction due to the reddening of E(B-V) of 0.03 in the direction of the source (Schlegel et al. 1998). This circular is an official product of the Swift team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 15873 SUBJECT: GRB 140219A: Xuyi and Nanshan upper limits DATE: 14/02/21 17:51:56 GMT FROM: Dong Xu at DARK/NBI D. Xu (DARK/NBI), D.-M. Wei, H.-B. Zhao, Y. Xia (PMO), C.-H. Bai, X. Zhang, H.-B. Niu, A. Esamdin, L. Ma (XAO), Y. Osorio (NOT) report on behalf of a large collaboration: We observed the whole IPN field and its surrounding region of GRB 140219A (Hurley et al., GCN 15864). The first epoch was done at ~15:40 UT on 2014-02-20 using the 1m telescope located at Xuyi, Jiangsu, China, equipped with a 3x3 deg^2 CCD camera. The second epoch was done at ~17:50 UT on 2014-02-20 using the 1m telescope located at Nanshan, Xinjiang, China, equipped with a 1.2x1.2 deg^2 CCD camera. For both epochs, a series of R-band 120s exposures were obtained. The depths of the images of the two epochs are largely comparable and it has R~19 mag. Within the IPN field, we found two relatively bright sources, but they can be ruled out to be an afterglow by cross checking the Xuyi, Nanshan, and DSS images. A third epoch was done at the 2.5m Nordic Optical Telescope (NOT) and the NOT images confirm the above ruling-out. Therefore, assuming GRB 140219A is a conventional cosmological burst happening within the IPN field, its afterglow would be fainter than R~19 mag at T~20 hrs post-burst, which is a possible case according to previous GRB follow-ups. Inspection of some surrounding region of the IPN field also leads to no credible afterglow candidate detection. For the reported two Swift/XRT sources in the central part of the IPN field (Mangano et al., GCN 15872), S2 is not present in the Xuyi and Nanshan images as well, while S1 is a known source. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 15875 SUBJECT: GRB 140219A: XRT afterglow candidate DATE: 14/02/22 18:03:46 GMT FROM: Vanessa Mangano at PSU V. Mangano (PSU) and P. A. Evans (U. Leicester) report on behalf of the Switf-XRT team Swift-XRT has observed the error circle of the IPN GRB 140219A in a series of observations tiled on the sky. The total exposure time is 9.9 ks spread over 5 fields; the maximum exposure within the sky observed was 3.9 ks. The observations started 70.3 ks after the IPN trigger. Within these data we detect a fading, uncatalogued X-ray source at RA, Dec= 156.02772, 6.49399 which is equivalent to: RA (J2000.0) = 10h 24m 6.65s Dec (J2000.0) = +06d 29' 38.4" with an uncertainty of 7.9 arcsec (radius, 90% confidence). The exposure at this location was 3.0 ks. This previously uncatalogued source is fading, and we thus consider it the likely GRB afterglow. The results of the automatic processing for this source are available athttp://www.swift.ac.uk/xrt_products/TILED_GRB00024/index_5.php This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 15876 SUBJECT: GRB 140219A: optical observations of XRT source #5 DATE: 14/02/22 19:50:38 GMT FROM: Alexei Pozanenko at IKI, Moscow A. Pozanenko (IKI), E. Klunko (ISTP), A.Volnova (IKI), M. Eselevich (ISTP), report on behalf of larger GRB follow-up collaboration: We observed the field of XRT afterglow candidate (Mangano et al., GCN 15875) of the GRB 140219A (Hurley et al., GCN 15864, Zhang GCN 15866, Guiriec et al.,GCN 15867, Golenetskii et al. GCN 15870) with AZT-33IK telescope of Mondy observatory starting on Feb. 22 (UT) 14:45. We obtained 60 images in R-filter. In the initial images within XRT error circle (Mangano et al., GCN 15875) we detected two objects which are present in SDSS DR9. One of them is a galaxy (SDSS 3015-301-3-0280-0458) and other one is a star (SDSS 3015-301-3-0280-0457). No new objects were detected. Upper limit of the initial image of 60-s exposure is R=20.8. A finding chart can be found in http://grb.rssi.ru/GRB140219A/GRB140219A_XRT_5_fc.png //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 15878 SUBJECT: GRB 140219A: iPTF optical observations DATE: 14/02/23 02:36:37 GMT FROM: Leo Singer at CIT/PTF L. P. Singer (Caltech), M. M. Kasliwal (Carnegie Observatories/Princeton), and S. B. Cenko (NASA/GSFC) report on behalf of the intermediate Palomar Transient Factory (iPTF) collaboration: We have searched for optical counterparts of GRB 140219A using the Palomar 48-inch Oschin telescope (P48). We observed 9 fields covering an area of 67.8 deg2 intersecting the Fermi GBM 1-sigma contour (Fermi trigger 414531995, Zhang et al., GCN 15866) and a preliminary MESSENGER-Suzaku IPN annulus (K. Hurley, personal communication) that was available when the GBM localization was first observable from Palomar. We observed all 9 fields for several epochs, with the first epoch extending from 7.0 to 8.1 hours after the burst. Sifting through candidate variable sources using image subtraction and standard iPTF vetting procedures, we found no compelling optical afterglow candidates to an average limiting magnitude of r=21.1 mag. About 80% of the published IPN error box (Hurley et al., GCN 15864) was contained in these 9 fields, with most of the remaining 20% falling on a disabled CCD on the P48. To fill the gap in the IPN error box, we observed two additional fields starting 33.7 hours after the burst. The deepest epoch of observations of these two fields had a limiting magnitude of r=20.7 mag. Since we lacked reference images for these two offset fields, we performed a catalog comparison search, examining any source that was detected in our two deepest epochs but was not coincident with a stellar object in SDSS. Of 342 sources meeting this criterion, all were known galaxies and none were compelling optical afterglow candidates. XRT source 1 (http://www.swift.ac.uk/xrt_products/TILED_GRB00024/index_1.php, Mangano et al., GCN 15872) is contained in our nine early fields, and we associate a coincident optical detection with the star SDSS J102559.46+073114.1. XRT source 2 (http://www.swift.ac.uk/xrt_products/TILED_GRB00024/index_2.php, Mangano et al., GCN 15872) is contained in our two late fields, and we detect no coincident optical source to a limiting magnitude of r=20.5 mag at 35.7 hours after the burst. XRT source 4 (http://www.swift.ac.uk/xrt_products/TILED_GRB00024/index_4.php) is contained in our nine early fields, and we find no coincident optical source to a limiting magnitude of r=20.2 mag at 8.1 hours after the burst. XRT source 5 (http://www.swift.ac.uk/xrt_products/TILED_GRB00024/index_5.php, Mangano et al., GCN 15875), the most plausible afterglow candidate due to its observed fading, is also contained in our two late fields. We detect two optical sources within the XRT error circle: the star SDSS J102406.41+062937.6, and the galaxy SDSS J102406.58+062945.7. These were also the sources detected by Pozanenko et al. (GCN 15876). For the star, we report r=20.0+/-0.1, which is about 0.5 mag brighter than the value given by SDSS DR10. We find no additional sources inside the XRT error circle to a limiting magnitude of r=21.0. The diagram http://www.its.caltech.edu/~lsinger/iptf/Fermi414531995.pdf shows the footprints of the nine early P48 fields in relation to the Fermi GBM 1-, 2-, and 3-sigma statistical+systematic contours (black) and the IPN INTEGRAL-MESSENGER and WAM-HEND annuli (blue). The INTEGRAL-MESSENGER annulus is comparable to the initial MESSENGER-Suzaku localization on which we based these observations. The diagram http://www.its.caltech.edu/~lsinger/iptf/Fermi414531995_inset_1.pdf shows the early P48 fields in relation to a six-sided IPN polygon and the XRT candidates. The diagram http://www.its.caltech.edu/~lsinger/iptf/Fermi414531995_inset_2.pdf shows the late P48 fields. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 15879 SUBJECT: GRB 140219A: MASTER optical brightening inside XRT-5 error box detection DATE: 14/02/23 15:59:55 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V. Lipunov, M. Pruzhinskaya, E. Gorbovskoy, 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 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) We refined our reduction of images started 18h 22m after trigger time (Gorbovskoy et al., GCN 15871). We found the 3-sigma OT on several (at least 4) best unfiltered images with limit ~ 20 mag inside XRT error box (Mangano and Evans, GCN 15875) at automatic position: 2014-02-20 14:08:50.873 10h 24m 06.46s , +06d 29m 40s.8 with 2 arcsec error (2 arcsec = 1 pix). The unfiltered magnitude is about 19. Fortunately we have archive images of this area at the same telescope with slightly better limit(MASTER II, Tunka,2011-02-06 16:34:55 180) without any optical source. The OT is brighter at least 1 magnitude at 18.5 hours after trigger. The OT position does not coincide with SDSS J102406.58+062945.7 galaxy (Singer, iPTF GCN 15878, source XRT 5), closer to SDSS star J102406.41+062937.6 . The detection and reference images are available at http://master.sai.msu.ru/static/GRB/GRB140219A_OT.png We do not see any OT at alert Very Wide Field images at this place (Gorbovskoy et al., GCN 15871). The message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 15880 SUBJECT: GRB 140219A: Retraction of X-ray afterglow DATE: 14/02/24 09:34:59 GMT FROM: Phil Evans at U of Leicester P.A. Evans (U. Leicester) reports on behalf of the Swift-XRT team: Further analysis of the XRT afterglow candidate of GRB 140219A (GCN Circ. 15875) reveals that the light curve of this object had been contaminated by the presence of a nearby, bright, catalogued X-ray source. Refined analysis of the previously-announced afterglow candidate reveals it to be approximately constant, with a count rate of ~5e-3 ct/sec, thus it is probably not the afterglow. This circular is an official product of the Swift-XRT team. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 15881 SUBJECT: GRB 140219A: the confirmation of the brightening SDSS J102406.41+062937.6 star DATE: 14/02/24 11:11:24 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V. Lipunov, M. Pruzhinskaya, E. Gorbovskoy, 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 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) We present the reduction of the best coadded image started 2014-02-20 14:42:07, i.e. 18.92 hour after trigger time with total exposition 3960 s (Gorbovskoy et al., GCN 15871) with unfiltered 21.0 mag limit. We found the optical source inside XRT-5 error box (Mangano and Evans, GCN 15875) at automatic position: T_start = 2014-02-20 14:42:07.5 (T_start-T_trig = 18.92 h) T_mid = 2014-02-20 16:14:23.7 (T_start-T_mid = 20.45 h) T_fin = 2014-02-20 17:46:40.0 (T_start-T_fin = 22.01 h) RA 10h 24m 06.45s Dec +6d 29m 37.86s (156.021889 6.420445) with 0.7 arcsec error. Unfiltered magnitude: Mag = 19.7+/-0.3 This source coincides with SDSS J102406.41+062937.6 star. This star must be visible at archive image of this area at the same telescope (MASTER II, Tunka,2011-02-06 16:34:55 180, Lipunov et all., GCN 15879) on 4 sigma level. The absence of the SDSS J102406.41+062937.6 star confirms its brightening ~0.7 mag. But the absence of the X-ray variation of XRT-5 source (P.F. Evans, GCN15880) argues that brightening may be usual variable star and does not connect with GRB 140219A. All our limits published earlier are still valid (GCN 15871, GCN 15879 ) The coadded image is available at http://observ.pereplet.ru/images/10240645+062937.jpg The message may be cited. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 15882 SUBJECT: GRB 140219A: MAXI/GSC detection DATE: 14/02/26 03:08:11 GMT FROM: Motoko Suzuki at RIKEN M. Serino (RIKEN), S. Ueno, H. Tomida, S. Nakahira, M. Kimura, M. Ishikawa, Y. E. Nakagawa (JAXA), T. Mihara, M. Sugizaki, M. Morii, J. Sugimoto, T. Takagi, A. Yoshikawa, M. Matsuoka (RIKEN), N. Kawai, R. Usui, T. Yoshii, Y. Tachibana (Tokyo Tech), A. Yoshida, T. Sakamoto, Y. Nakano, Y. Kawakubo, H. Ohtsuki (AGU), H. Tsunemi, M. Sasaki (Osaka U.), H. Negoro, M. Nakajima, K. Fukushima, T. Onodera, K. Suzuki (Nihon U.), Y. Ueda, M. Shidatsu, T. Kawamuro, T. Hori (Kyoto U.), Y. Tsuboi, M. Higa (Chuo U.), M. Yamauchi, K. Yoshidome, Y. Ogawa, H. Yamada (Miyazaki U.), K. Yamaoka (Nagoya U.) report on behalf of the MAXI team: The MAXI/GSC detected a rapid increase of the count rate in all six working counters at 2014-02-19T19:45:58.15 UT. The time is consistent with GRB 140219A (Hurley et al., GCN 15864; Zhang, GCN 15866; Guiriec et al., GCN 15867; Golenetskii et al., GCN 15870). The IPN postion of GRB 140219A was not in the field of view of any of the MAXI Gas Slit Cameras, implying that the detected counts are produced by the hard X-rays that penetrated the Ti counter walls with Pb shiled, or the phosphor bronze collimator with Al housing of GSC, or by the Compton-scattered electrons induced by the gamma-rays. It suggests that this GRB was exceptionally bright and hard. The light curve shows an intense spike with a duration of ~0.2 s followed by a bright emission until T0+~2.5 s. A weak emission lasts until T0+~20 s. The peak count rate is ~2000 c/s per counter (GSC_3). The MAXI/GSC light curve of this GRB is available at http://maxi.riken.jp/news/en/?p=1101 . There was no significant excess flux in the transits before and after the GRB at UT 19:40 and 21:13 with an upper limit of 20 mCrab (4-10 keV, 1 sigma) for each. -- Motoko SERINO //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 15885 SUBJECT: GRB 140219A: Suzaku WAM observation of the prompt emission DATE: 14/02/27 11:42:27 GMT FROM: Tetsuya Yasuda at Saitama U W. Iwakiri(RIKEN), M. Tashiro, Y. Terada, T. Yasuda, 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.), Y. E. Nakagawa, M. Kokubun, T. Takahashi (ISAS/JAXA), Y. Hanabata (ICRR), Y. Urata (NCU), K. Nakazawa, K. Makishima (Univ. of Tokyo) on behalf of the Suzaku WAM team, report: The extremely bright and long-duration GRB 140219A (localized by IPN: Hurley et al., GCN 15864; Fermi-GBM detection: Zhang, GCN 15866; Fermi-LAT detection: Guiriec et al., GCN 15867; Konus-Wind detection: Golenetskii et al., GCN15870; MAXI/GSC detection: Serino et al., GCN15882) triggered the Suzaku Wide-band All-sky Monitor (WAM) which covers an energy range of 50 keV - 5 MeV at 19:45:57.754 UT (=T0). The observed light curve shows a strong multi-peaked structure lasting from T0 s to T0+3 s, followed by a weaker multi-peaked emissions seen up to T0+27 s with a total duration (T90) of about 17 seconds.　 The fluence in 100 - 1000 keV was 1.73 (+0.06,-0.08)x10^-5 erg/cm^2. The 1-s peak flux measured from T0+1.5 s was 83.6 (+6.5,-6.4) photons/cm^2/s in the same energy range. Preliminary result shows that the time-averaged spectrum from T0 s to T0+27 s is fitted by a GRB Band model as follows. the low-energy photon index alpha: -1.00 (+0.06,-0.11), the high-energy photon index beta: -2.68 (+0.08,-0.11), and the peak energy Epeak: 1930(+176,-79) keV (chi^2/d.o.f = 71.9/47). There might be some calibration uncertainties in spectral parameters since the GRB photons came through the X-ray micro-calorimeter (XRS) dewar. All the quoted errors are at 90% confidence level. The light curves for this burst are available at: http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 15890 SUBJECT: GRB 140219A: Mondy optical observations of XRT source #5 DATE: 14/02/28 14:57:36 GMT FROM: Alexei Pozanenko at IKI, Moscow A.Volnova (IKI), A. Pozanenko (IKI), I. Korobtsev (ISTP), E. Klunko (ISTP), M. Eselevich (ISTP), report on behalf of larger GRB follow-up collaboration: We observed the field of possible XRT afterglow candidate (Mangano et al., GCN 15875) of the GRB 140219A (Hurley et al., GCN 15864, Zhang GCN 15866, Guiriec et al.,GCN 15867, Golenetskii et al. GCN 15870, Serino et al. GCN 15882) with AZT-33IK telescope of Mondy observatory on Feb. 22 (UT) 14:45-15:45 (Pozanenko et al., GCN 15876) and Feb. 27 (UT) 15:18-16:18. We obtained several images with exposure of 60 seconds in R-filter during each observational set. In the stacked images within XRT error circle (Mangano et al., GCN 15875) we clearly detect two objects which are present in SDSS plates and SDSS DR9. One of them is a galaxy (refereed below as G5), SDSS J102406.58+062945.8, and other one is a star (X5), SDSS J102406.41+062937.6, both objects mentioned earlier (Pozanenko et al., GCN 15876, Singer et al., GCN 15878). No new objects were detected. The photometry of the two sources is following: date UT start t-T0 Exp. Filter G5 X5 (mid, days) (s) 2014-02-22 14:45:44 2.81197 51*60 R 20.77+/-0.12 19.74+/-0.05 2014-02-27 15:18:29 7.81388 60*60 R 20.51+/-0.09 19.59+/-0.06 The photometry is based on reference stars SDSS-DR9, (R mag, transformation by Lupton 2005): N SDSS_id R(Lupton) err 1 J102410.32+062923.9 17.391 0.017 2 J102410.04+062943.6 18.163 0.023 3 J102404.63+062938.7 18.962 0.025 The known star X5 is ~0.5m brighter than assumed R mag from SDSS DR9, i.e. R = 20.24 +/- 0.06, in accordance with Singer et al. (GCN 15878). We also may suspect, that known galaxy G5 might be brighter in our second epoch (Feb. 27) than on first epoch (Feb. 22). We encourage further observation of the galaxy G5 to confirm re-brightening, and if so the galaxy might be a host of GRB 140219A. Also we report a redshift of G5 galaxy z= 0.12 +/- 0.12 obtained photometrically using SDSS DR9 catalog. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 16067 SUBJECT: GRB 140219A: Correction to GCN 15885 (Suzaku-WAM fluence) DATE: 14/04/01 12:03:07 GMT FROM: Kazutaka Yamaoka at Nagoya U W. Iwakiri (RIKEN), M. Tashiro, Y. Terada, T. Yasuda, 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.), 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 quoted fluence in GCN 15885 was incorrect. The correct value is 1.73 (+0.06,-0.08)x10^-4 erg/cm^2 in the 100-1000 keV range. We apologize for any inconvenience. //////////////////////////////////////////////////////////////////////// TITLE: GCN CIRCULAR NUMBER: 17842 SUBJECT: GRB 140219A: Swift ToO observations DATE: 15/05/21 18:04:23 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 IPN GRB 140219A. Automated analysis of the XRT data will be presented online at http://www.swift.ac.uk/ToO_GRBs/00020368 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 IPN 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.