GRB140508A

This page lists all entries on GRB140508A in GRBweb

Summary Fermi GBM IPN GCN 16224 GCN 16225 GCN 16226 GCN 16227 GCN 16228 GCN 16229 GCN 16231 GCN 16232 GCN 16234 GCN 16235 GCN 16236 GCN 16243 GCN 16244 GCN 16246 GCN 16254 GCN 16259 GCN 16260 GCN 16266

Summary table
Variable Value Source
GRB_name_Fermi GRB140508128
T0 3:03:54.598 UTC Fermi_GBM
ra 255.6292° IPN
decl 46.7500° IPN
pos_error 1.50e+00° IPN
T90 44.288 s Fermi_GBM
T90_error 0.231 s Fermi_GBM
T90_start 3:03:57.414 UTC Fermi_GBM
fluence 6.14e-05 erg/cm² Fermi_GBM
fluence_error 1.21e-07 erg/cm² Fermi_GBM
redshift 1.0285
T100 47.104 s
GBM_located False
mjd 56785.12771525463 Fermi_GBM
Fermi GBM table
GRB_name_Fermi GRB140508128
trigger_name bn140508128
ra 255.4671°
decl 46.7803°
pos_error 2.58e+00°
datum 2014-05-08
t_trigger 3:03:54.598 UTC
T90 44.288 s
T90_error 0.231 s
T90_start 3:03:57.414 UTC
fluence 6.14e-05 erg/cm²
fluence_error 1.21e-07 erg/cm²
flux_1024 6.68e+01 erg/cm²/s
flux_1024_error 9.60e-01 erg/cm²/s
flux_1024_time 4.48e+00 erg/cm²/s
flux_64 8.81e+01 erg/cm²/s
flux_64_error 4.32e+00 erg/cm²/s
IPN table
GRB_name GRB140508A
ra 255.6292°
decl 46.7500°
pos_error 1.50e+00°
redshift 1.0270
GCN 16224 table
GRB_name GRB140508A
GCN_number 16224
Detection_method Fermi GBM Det
t_trigger 3:03:54.600 UTC
ra 250.1000°
decl 44.4000°
Circular_text TITLE: GCN CIRCULAR NUMBER: 16224 SUBJECT: GRB 140508A: Fermi GBM detection DATE: 14/05/08 14:51:43 GMT FROM: Hoi-Fung Yu at MPE Hoi-Fung Yu (MPE) and Adam Goldstein (ORAU/NASA MSFC) report on behalf of the Fermi GBM Team: "At 03:03:54.60 UT on 08 May 2014, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 140508A (trigger 421211037 / 140508128). The trigger resulted in an Autonomous Repoint Request (ARR) that was accepted and the spacecraft slewed to the GBM in-flight location. The on-ground calculated location, using the GBM trigger data, is RA = 250.1, Dec = 44.4 (J2000 degrees, equivalent to 16h 40m, 44d 24'), with an uncertainty of 1.0 degrees (radius, 1-sigma containment, statistical only; there is additionally a systematic error which is currently estimated to be 2 to 3 degrees). The initial angle from the Fermi LAT boresight is 112 degrees. This burst was also independently detected by INTEGRAL SPI-ACS. The GBM light curve consists of several pulses with decaying peak flux with a duration (T90) of about 44.3 s (50-300 keV). The time-averaged spectrum from T0-0.512 s to T0+51.712 s is well fit by a Band function with Epeak = 256.2 +/- 11.8 keV, alpha = -1.07 +/- 0.02, and beta = -2.38 +/- 0.09. The event fluence (10-1000 keV) in this time interval is (6.24 +/- 0.07)E-05 erg/cm^2. The 1.024-sec peak photon flux measured starting from T0+4.480 s in the 10-1000 keV band is 66.8 +/- 1.0 ph/s/cm^2. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog."
GCN 16225 table
GRB_name GRB140508A
GCN_number 16225
Detection_method IPN Triangulation
t_trigger 3:03:55 UTC
ra 255.6310°
decl 46.7470°
Circular_text TITLE: GCN CIRCULAR NUMBER: 16225 SUBJECT: IPN triangulation of GRB 140508A DATE: 14/05/08 19:05:02 GMT FROM: Valentin Pal'shin at Ioffe Inst 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, V. Connaughton, M. S. Briggs, C. Meegan, and V. Pelassa, on behalf of the Fermi GBM 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 140508A (Yu and Goldstein, GCN Circ. 16224) has been observed by Fermi (GBM), Konus-Wind, INTEGRAL (SPI-ACS), Swift (BAT), and MESSENGER (GRNS) so far, at about 11035 s UT (03:03:55). 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: 255.631 (17h 02m 31s) +46.747 (+46d 44' 51") Corners: 254.602 (16h 58m 24s) +47.063 (+47d 03' 48") 256.275 (17h 05m 06s) +46.717 (+46d 43' 00") 256.649 (17h 06m 36s) +46.418 (+46d 25' 06") 254.988 (16h 59m 57s) +46.773 (+46d 46' 23") --------------------------------------------- The error box area is 882 sq. arcmin, and its maximum dimension is 1.5 deg (the minimum one is 12 arcmin). The Sun distance was about 110 deg. This box can be improved. A triangulation map will be posted at ssl.berkeley.edu/ipn3/140508/140508.png Details of the K-W observation will be given in a forthcoming GCN Circular
GCN 16226 table
GRB_name GRB140508A
GCN_number 16226
Detection_method Optical
ra 255.4665°
decl 46.7804°
Circular_text TITLE: GCN CIRCULAR NUMBER: 16226 SUBJECT: GRB 140508A: iPTF optical transient candidate DATE: 14/05/08 19:30:09 GMT FROM: Leo Singer at CIT/PTF L. P. Singer (Caltech), S. B. Cenko (NASA/GSFC), M. M. Kasliwal (Carnegie Observatories/Princeton), Christoffer Fremling (Stockholm University), and Yifat Dzigan (Weizmann) report on behalf of the intermediate Palomar Transient Factory (iPTF) collaboration: We have searched for an optical counterpart of GRB 140508A (Yu and Goldstein, GCN 16224), Fermi/GBM trigger 421211037 (2014-05-08 03:03:54.60), using the Palomar 48-inch Oschin telescope (P48). Based on the final Fermi GBM localization, we observed 10 fields covering 73 deg2, with an estimated 67% chance of containing the true location of the event. Due to weather at Palomar early in the night, observations started at 09:48 UTC, 6.7 hours after the trigger. Also detected by Konus-Wind, INTEGRAL, Swift BAT (outside FoV), and MESSENGER, the IPN error box (Hurley et al., GCN 16225) was mostly contained within two CCDs in one of our fields. Sifting through candidate variable sources using image subtraction and standard iPTF vetting procedures, we detected several optical transients. Only is located within the IPN error box: iPTF14aue, at the coordinates: RA(J2000) = 17h 01m 51.95s (255.466450 deg) Dec(J2000) = +46d 46' 49.5" (+46.780417 deg) The source was detected at r = 17.89 +/- 0.01 mag and appeared to fade. A power-law fit to the first two observations, relative to the time of the GBM trigger, gives a decay index of alpha = 1.12 +/- 0.1. There is no source coincident with this location in our reference images or in SDSS DR10. This position is also consistent with the IPN triangulation (Hurley et al., GCN 16225), and is 7' from the center of the error box. Given the spatial coincidence with the IPN localization, the lack of archival detections, and the source fading, iPTF14aue is likely associated with the GRB. We are submitting a Swift XRT target of opportunity. Further observations are encouraged to confirm the association and the nature of the candidate. The diagram http://www.its.caltech.edu/~lsinger/iptf/Fermi421211037.pdf shows the ten P48 fields in relation to the Fermi GBM 1- and 2-sigma statistical+systematic contours, and the IPN error box. We thank the Fermi-GBM and IPN teams for sharing their localizations with us.
GCN 16227 table
GRB_name GRB140508A
GCN_number 16227
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 16227 SUBJECT: GRB 140508A: 1.23m CAHA BVRI-band observations DATE: 14/05/08 23:02:30 GMT FROM: Javier Gorosabel at IAA-CSIC J. Gorosabel (UPV-EHU/IAA-CSIC), A. Sanchez-Lavega (UPV/EHU), S. Perez-Hoyos (UPV/EHU), R. Hueso (UPV/EHU), J. Ugarte (UPV/EHU), I. Ordonez (UPV/EHU), E. Arandia (UPV/EHU), I. Perez de Nanclares (UPV/EHU), on behalf of the BEGIRA project: "We observed the field of GRB140508A (GCN Cir. 16224,16225) starting on May 8.93559 UT. The optical transient detected by Singer et al. (GCN Cir. 16226) is clearly detected in our images with an approximate Vega magnitude of R=18.8 with respect to the USNO B1.0."
GCN 16228 table
GRB_name GRB140508A
GCN_number 16228
Detection_method IPN Triangulation
Circular_text TITLE: GCN CIRCULAR NUMBER: 16228 SUBJECT: GRB 140508A: SAO RAS and MASTER photometric and spectroscopic observations DATE: 14/05/09 01:15:15 GMT FROM: Vladimir Sokolov at SAO RAS A. S. Moskvitin, D. I. Makarov, A. F. Valeev, V. V. Sokolov (SAO-RAS, Russia), A. J. Castro-Tirado, J. Gorosabel (IAA-CSIC, Spain), E. S. Gorbovskoy, D. V. Denisenko, V. M.Lipunov (MASTER-team, Russia), on behalf of a larger collaboration, report: "Following the detection of GRB 140508A by Fermi (Yu et al. GCNC 16224) and the IPN (Hurley et al. GCNC 16225), we have conducted BVRc imaging and spectroscopy of the iPTF optical candidate (Singer et al. GCNC 16226) with the 6m BTA telescope in Zelenchukskaia, starting at 19:47:56 UT (i.e. 16.7 hr after the trigger). The 20 minutes (noisy) spectrum, covering the range 3800-7200 A, displays no clear absorption features, i.e. a conservative upper limit of z < 2.1 is derived. The GRB OT magnitude was measured to have R = 18.7 +/- 0.05 during the BTA observations spanning more than 1 hr. OT magnitudes calibrated against the USNO-B1 star 1367-0290781 with R2 = 16.48. MASTER II robotic telescope (MASTER-Net: http://observ.pereplet.ru) located in Kislovodsk also pointed to the GRB140508A (Yu et. al GCNC 16224, Hurley et. al. GCN 16224) ~17.5 h after trigger time at 2014-05-08 20:31:01.484 UT directly after sunset and weather conditions became satisfactory. On the first (180s exposure) unfiltred image the iPTF optical transient preliminary photometry is given below: T_start T-T_trig FILTER Mag Err.Mag Exptime 2014-05-08 20:31:01 17h 28m C 18.7 0.3 180 s 2014-05-08 20:48:33 17h 45m R 18.7 0.3 180 s 2014-05-08 20:48:33 17h 45m V <19.0 0.3 180 s upper limit 2014-05-08 21:20:36 18h 17m R 18.9 0.3 540 s 2014-05-08 21:20:36 18h 17m V 19.9 0.4 540 s "C" is unfiltred 0.8R+0.2B magnitude. This message can be quoted."
GCN 16229 table
GRB_name GRB140508A
GCN_number 16229
Detection_method Optical
redshift 1.0300
Circular_text TITLE: GCN CIRCULAR NUMBER: 16229 SUBJECT: GRB 140508A: NOT photometry and spectroscopy DATE: 14/05/09 02:30:41 GMT FROM: Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst D. Malesani, D. Xu (DARK/NBI), P. D'Avanzo (INAF/OAB), E. Palazzi (INAF/IASF Bologna), D. Perna (Obs. Paris) report on behalf of a larger collaboration: We observed the optical afterglow candidate of GRB 140508A (Yu & Goldstein GCN 16224; Hurley et al., GCN 16225; Singer et al., GCN 16226) with the Nordic Optical Telescope (NOT) equipped with ALFOSC. The observation consisted of a 1800 s spectrum covering the wavelength range between 3200 and 9100 AA, carried out at a mean time of 20.63 hr after the GRB. The afterglow is detected in the acquisition image (20.13 hr after the GRB) with r = 19.07+-0.03 (AB) calibrated against SDSS stars. Compared with the measurement by Singer et al. (GCN 16226), our measurement yields a power-law decay slope alpha ~ 1, consistent with the value reported by these authors. We detect several absorption features which we intepret as due to Fe II 2600 and Mg II 2796, 2803 at a common redshift of z = 1.03. This can be considered as a firm lower limit to the GRB redshift, and is consistent with the constraint by Moskvitin et al. (GCN 16228).
GCN 16231 table
GRB_name GRB140508A
GCN_number 16231
Detection_method Other
redshift 1.0270
Circular_text TITLE: GCN CIRCULAR NUMBER: 16231 SUBJECT: GRB 140508A: WHT spectroscopy DATE: 14/05/09 03:06:22 GMT FROM: Klaas Wiersema at U Leicester K. Wiersema (Leicester), N. Tanvir (Leicester), A. Levan (Warwick), R. Karjalainen (ING) report: We observed the afterglow candidate of GRB 140508A (Singer et al. GCN 16226) with the 4.2m William Herschel Telescope using the ACAM instrument. We acquired 3x600s spectroscopic exposures, with midpoint 23:02 UT on 8 May 2014. We find absorption lines of Mg II and Fe II at a common redshift of z=1.027, though we caution this redshift is based on archival wavelength calibrations. This is consistent with the redshift reported by Malesani et al. (GCN 16229).
GCN 16232 table
GRB_name GRB140508A
GCN_number 16232
Detection_method Swift-XRT Other
ra 255.4665°
decl 46.7803°
Circular_text TITLE: GCN CIRCULAR NUMBER: 16232 SUBJECT: GRB 140508A: Swift-XRT observations DATE: 14/05/09 06:26:12 GMT FROM: Alex Amaral-Rogers at U.of Leicester reports on behalf of the Swift-XRT team: We have analysed 3.0 ks of XRT data for the Fermi/GBM-detected burst: GRB 140508A, from 69.0 ks to 75.2 ks after the Fermi/GBM trigger. The data are entirely in Photon Counting (PC) mode. An X-ray source is detected within the Fermi/GBM error circle. Using 2973 s of PC mode data and 3 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 = 255.46650, +46.78033 which is equivalent to: RA (J2000): 17h 01m 51.96s Dec(J2000): +46d 46' 49.2" with an uncertainty of 1.8 arcsec (radius, 90% confidence). This position is 0.3 arcsec from the iPTF optical transient candidate (GCN Circ. 16226). The late-time light curve (from T0+69.0 ks) is consistent with a constant source of mean count rate 2.0e-01 ct/sec. A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 2.01 (+0.25, -0.23). The best-fitting absorption column is 7.8 (+5.9, -5.1) x 10^20 cm^-2, in excess of the Galactic value of 2.1 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 3.3 x 10^-11 (3.9 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 7.8 (+5.9, -5.1) x 10^20 cm^-2 Galactic foreground: 2.1 x 10^20 cm^-2 Excess significance: 1.8 sigma Photon index: 2.01 (+0.25, -0.23) The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00020376. This circular is an official product of the Swift-XRT team.
GCN 16234 table
GRB_name GRB140508A
GCN_number 16234
Detection_method Konus-Wind Det
t_trigger 3:03:58.423 UTC
redshift 1.0300
Circular_text TITLE: GCN CIRCULAR NUMBER: 16234 SUBJECT: Konus-Wind observation of GRB 140508A DATE: 14/05/09 11:20:08 GMT FROM: Dmitry Frederiks 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: The long-duration, very intense GRB 140508A (Fermi-GBM detection: Yu and Goldstein, GCN 16224; IPN triangulation: Hurley et al., GCN 16225) triggered Konus-Wind at T0=11038.423 s UT (03:03:58.423). The light curve shows multiple emission episodes with decaying peak intensity. A total duration of the burst is ~80 s. The emission is seen up to ~9 MeV. A hint of an extended emission in softer energy channels can be traced to at least 250 s after the trigger; however, its attribution to GRB 140508A is unclear due to the variable solar particle background. As observed by Konus-Wind, the burst had a fluence of 7.4(-0.7,+0.8)x10^-5 erg/cm2, and a 64-ms peak flux, measured from T0+2.576 s, of 3.0(-0.2,+0.2)x10^-5 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+72.448 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 = -1.11 (-0.08,+0.09), the high energy photon index beta = -2.5 (-0.4,+0.2), the peak energy Ep = 213 (-20,+23) keV, chi2 = 70/86 dof. The spectrum near the peak count rate (measured from T0 to T0+4.864 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 = -1.0 (-0.1,+0.1), the high energy photon index beta = -2.4 (-0.2,+0.1), the peak energy Ep = 345 (-47,+59) keV, chi2 = 65/64 dof. Assuming the redshift z=1.03 (Malesani et al., GCN 16229; Wiersema et al., GCN 16231) and a standard cosmology model with H_0 = 70 km/s/Mpc, Omega_M = 0.27, and Omega_Lambda = 0.73, we estimate the following rest-frame parameters: the isotropic energy release E_iso is ~2.1x10^53 erg, the peak luminosity L_iso is ~1.8x10^53 erg/s, and the rest-frame peak energy, Ep,i, is ~430 keV. The Konus-Wind light curve of this GRB is available at http://www.ioffe.ru/LEA/GRBs/GRB140508_T11038/ All the quoted errors are at the 90% sigma confidence level. All the quoted values are preliminary.
GCN 16235 table
GRB_name GRB140508A
GCN_number 16235
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 16235 SUBJECT: GRB 140508A: Optical Observations via Virtual Telescope DATE: 14/05/09 11:40:39 GMT FROM: Gianluca Masi at Bellatrix Astronomical Obs G. Masi (Ceccano, Italy) reports: On May 09.06569 2014 UT (22.5 hours after the burst), we imaged the field around GRB 140508A (Singer et al. GCN 16226) remotely using the the 0.43m-f/6.8 robotic unit part of the Virtual Telescope robotic facility in Italy. The source is visible on 300 seconds unfiltered CCD images at the following coordinates (J2000): R.A. = 17 01 51.94 Decl. +46 46 49.2 We also performed photometry, assuming R-mags from UCAC-4 for the stars in the field, getting an estimate for the magnitude of 19.3CR). This message can be cited.
GCN 16236 table
GRB_name GRB140508A
GCN_number 16236
Detection_method Swift-BAT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 16236 SUBJECT: GRB 140508A: RATIR Optical and NIR Observations DATE: 14/05/09 14:34:57 GMT FROM: Nat Butler at Az State U 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), Owen Littlejohns (ASU), 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 140508A (Yu, et al., GCN 16224) 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 2014/05 9.19 to 2014/05 9.46 UTC (25.61 to 32.04 hours after the BAT trigger), obtaining a total of 4.27 hours exposure in the r and i bands and 1.79 hours exposure in the Z, Y, J, and H bands. For a source positionally coincident with the iPTF optical transient (Singer, et al. , GCN 16226), in comparison with the SDSS DR9 and 2MASS, we obtain the following detections: r 19.65 +/- 0.02 i 19.52 +/- 0.02 Z 19.36 +/- 0.03 Y 19.20 +/- 0.03 J 19.18 +/- 0.03 H 18.98 +/- 0.03 These magnitudes are in the AB system and are not corrected for Galactic extinction in the direction of the GRB. The source fades in time approximately as t^(-1.5) in all bands during our observation. We thank the staff of the Observatorio Astronómico Nacional in San Pedro Mártir.
GCN 16243 table
GRB_name GRB140508A
GCN_number 16243
Detection_method Swift-UVOT Det
ra 255.4665°
decl 46.7804°
Circular_text TITLE: GCN CIRCULAR NUMBER: 16243 SUBJECT: GRB 140508A: Swift/UVOT Detection DATE: 14/05/09 19:03:14 GMT FROM: Frank Marshall at GSFC F.E. Marshall (NASA/GSFC) and A. Amarel-Rogers (U. of Leicester) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 140508A 68965 s after the GBM trigger (Yu and Goldstein, GCN Circ. 16224). A source consistent with the optical position (Singer et al., GCN Circ. 16226) and the X-ray position (Amarel-Rogers, GCN Circ. 16232) is detected in the initial UVOT exposures. The preliminary UVOT position is: RA (J2000) = 17:01:51.95 = 255.46647 (deg.) Dec (J2000) = +46:46:49.5 = 46.78043 (deg.) with an estimated uncertainty of 0.46 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 v 68965 69792 814 19.38 +/- 0.10 b 70632 71427 782 19.59 +/- 0.06 u 69799 70626 814 18.81 +/- 0.05 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.031 in the direction of the burst (Schlegel et al. 1998).
GCN 16244 table
GRB_name GRB140508A
GCN_number 16244
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 16244 SUBJECT: GRB 140508A: ​HCT spectroscopy DATE: 14/05/10 16:45:53 GMT FROM: Varun Bhalerao at IUCAA V. Bhalerao, D. K. Sahu report: We obtained optical spectroscopy of the iPTF afterglow candidate of GRB140508A (Yu & Goldstein GCN 16224; Hurley et al., GCN 16225; Singer et al., GCN 16226) with the HFOSC instrument on the 2-m Himalayan Chandra Telescope (HCT). We obtained two spectra of 1800 sec each, spanning the wavelength range from 3800-8400A, at a mean time of 15.5 hours after the trigger. The spectrum shows weak absorption features, consistent with the Fe II and Mg II at redshift ~1.03, as identified by Malesani et al. (GCN 16229) and Wiersema et al. (GCN 16231).
GCN 16246 table
GRB_name GRB140508A
GCN_number 16246
Detection_method Swift-BAT Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 16246 SUBJECT: GRB 140508A: Continued RATIR Optical and NIR Observations DATE: 14/05/12 16:15:45 GMT FROM: Nat Butler at UC berkeley 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), Owen Littlejohns (ASU), 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 140508A (Yu, et al., GCN 16224) 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 2014/05 10.31 to 2014/05 10.48 UTC (52.29 to 56.42 hours after the BAT trigger), obtaining a total of 2.49 hours exposure in the r and i bands and 1.04 hours exposure in the Z, Y, J, and H bands and again from 2014/05 11.23 to 2014/05 11.48 UTC (74.56 to 80.45 hours after the BAT trigger), obtaining a total of 3.91 hours exposure in the r and i bands and 1.64 hours exposure in the Z, Y, J, and H bands. For a source positionally coincident with the iPTF optical transient (Singer, et al., GCN 16226), in comparison with the SDSS DR9 and 2MASS, we obtain the following detections: t+54.4 hrs t+77.5 hrs r 20.63 +/- 0.03 21.25 +/- 0.05 i 20.47 +/- 0.03 21.08 +/- 0.05 Z 20.29 +/- 0.05 21.04 +/- 0.08 Y 20.24 +/- 0.07 20.76 +/- 0.10 J 20.17 +/- 0.06 20.79 +/- 0.11 H 19.92 +/- 0.08 20.58 +/- 0.13 These magnitudes are in the AB system and are not corrected for Galactic extinction in the direction of the GRB. Including our initial set of observations (Butler, et al., GCN 16236), the source appears to have faded as t^(-1.5) in all bands. We thank the staff of the Observatorio Astronómico Nacional in San Pedro Mártir.
GCN 16254 table
GRB_name GRB140508A
GCN_number 16254
Detection_method Swift Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 16254 SUBJECT: Swift Observations of GRB 140508A DATE: 14/05/13 05:30:00 GMT FROM: Alex Amaral-Rogers at U.of Leicester Alex Amaral-Rogers reports on behalf of the Swift-XRT team: Swift has reobserved the field of GRB 140508A for a further 4.6 ks from 253.9 ks to 288.1 ks after the Fermi/GBM trigger. The source reported in GCN 16232 has been observed in the XRT to be fading; consistent with a power-law decay with an index of alpha = 1.48 (+0.15, -0.14). We now confirm the the source is the afterglow of GRB 140508A.
GCN 16259 table
GRB_name GRB140508A
GCN_number 16259
Detection_method MITSuME
Circular_text TITLE: GCN CIRCULAR NUMBER: 16259 SUBJECT: GRB 140508A: MITSuME Akeno Optical observation DATE: 14/05/13 13:52:06 GMT FROM: Taketoshi Yoshii at Tokyo Tech T. Fujiwara, T. Yoshii, Y. Saito, Y. Tachibana, H. Ohuchi, S. Kurita, Y.Ono , Y. Yatsu, and N. Kawai (Tokyo Tech) report on behalf of the MITSuME collaboration: We observed the field of GRB 140508A (H.Yu et al., GCN Circular #16224) with the optical three color (g, Rc, and Ic) CCD cameras attached to the MITSuME 50 cm telescope of Akeno Observatory, Yamanashi, Japan. The observation started on 2014-05-09 11:07:31 UT (32.1h after the burst). We detected the optical afterglow of GRB140508A in the g',Rc and Ic band. The measured magnitudes were listed below. T0+[h] T-EXP[sec] g' Rc Ic ---------------------------------------------------------------------------------------- 35.3 19800 20.16+/-0.22 19.74+/-0.24 18.85+/-0.17 ---------------------------------------------------------------------------------------- T0+ : Elapsed time after the burst T-EXP: Total Exposure time We used GSC2.3 catalog for flux calibration.
GCN 16260 table
GRB_name GRB140508A
GCN_number 16260
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 16260 SUBJECT: GRB 140508A: Mondy upper limit DATE: 14/05/13 14:17:02 GMT FROM: Alexei Pozanenko at IKI, Moscow A. Volnova (IKI), E. Klunko (ISTP), M. Eselevich (ISTP), I. Korobtsev (ISTP), A. Pozanenko (IKI) report on behalf of larger GRB follow-up collaboration: We observed the field of GRB 140508A (Yu et al., GCN 16224) with AZT-33IK telescope of of Sayan observatory (Mondy) starting on May, 12 (UT) 15:32:03. Within enhanced Swift-XRT error circle (Amarel-Rogers et al., GCN 16232) we do not detect the optical source reported by Singer et al. (GCN 16226). Details of the photometry are the following: date UT start t-T0 Exp. Filter UpperLimit (mid, days) (s) (3sigma) 2014-05-12 15:32:03 4.56124 60x120 R 22.9 The photometry is based on a reference star from SDSS-DR9, (R mag, transformation by Lupton 2005): SDSS_id R(Lupton) err J170144.75+464707.7 18.272 0.018
GCN 16266 table
GRB_name GRB140508A
GCN_number 16266
Detection_method VLA Det
Circular_text TITLE: GCN CIRCULAR NUMBER: 16266 SUBJECT: GRB 140508A: VLA detection DATE: 14/05/14 21:23:46 GMT FROM: Assaf Horesh at Caltech A. Horesh (Weizmann Institute), L. P. Singer (Caltech), S. B. Cenko (NASA/GSFC), M. M. Kasliwal (Carnegie Observatories/Princeton), and D. Perley (Caltech) report on behalf of a larger collaboration: We observed iPTF14aue, the afterglow candidate of GRB140508A (Yu & Goldstein, GCN 16224; Hurley et al., GCN 16225; Singer et al., GCN 16226) with the Jansky Very Large Array (VLA). The observations were undertaken on 2014 May 13 UT, 5.2 days after the Fermi trigger. We detected the source at 6.1 GHz (C-band) with a flux of 127 +/- 9 micro Jy. The source was also detected at 22 GHz (K-band). We thank the VLA staff for scheduling this target of opportunity.