GRB190613A

This page lists all entries on GRB190613A in GRBweb

Summary Fermi GBM IPN Swift GCN 24798 GCN 24799 GCN 24800 GCN 24801 GCN 24803 GCN 24809 GCN 24810 GCN 24815 GCN 24816 GCN 24819 GCN 24822 GCN 24835 GCN 24838 GCN 24850

Summary table
Variable Value Source
GRB_name_Fermi GRB190613172
T0 4:07:18 UTC GCN_circulars,Fermi GBM final loc
ra 182.5292° Swift
decl 67.2353° Swift
pos_error 5.57e-05° Swift
T90 17.149 s Fermi_GBM
T90_error 1.493 s Fermi_GBM
T90_start 4:07:18.237 UTC Fermi_GBM
fluence 3.20e-06 erg/cm² Fermi_GBM
fluence_error 5.46e-08 erg/cm² Fermi_GBM
T100 17.6 s
GBM_located False
mjd 58647.17173611111 GCN_circulars,Fermi GBM final loc
Fermi GBM table
GRB_name_Fermi GRB190613172
trigger_name bn190613172
ra 182.5592°
decl 67.2331°
pos_error 3.10e+00°
datum 2019-06-13
t_trigger 4:07:18.234 UTC
T90 17.149 s
T90_error 1.493 s
T90_start 4:07:18.237 UTC
fluence 3.20e-06 erg/cm²
fluence_error 5.46e-08 erg/cm²
flux_1024 2.73e+00 erg/cm²/s
flux_1024_error 2.80e-01 erg/cm²/s
flux_1024_time 9.79e+00 erg/cm²/s
flux_64 4.36e+00 erg/cm²/s
flux_64_error 1.42e+00 erg/cm²/s
IPN table
GRB_name GRB190613A
ra 182.5583°
decl 67.2333°
pos_error 5.00e-02°
Swift table
GRB_name GRB190613A
t_trigger 4:07:18 UTC
ra 182.5292°
decl 67.2353°
pos_error 5.57e-05°
T90 17.6 s
fluence 1.70e-06 erg/cm²
GCN 24798 table
GRB_name GRB190613A
GCN_number 24798
Detection_method Swift Det
t_trigger 4:07:18 UTC
ra 182.5590°
decl 67.2330°
Circular_text TITLE: GCN CIRCULAR NUMBER: 24798 SUBJECT: GRB 190613A: Swift detection of a burst with an optical counterpart DATE: 19/06/13 04:18:46 GMT FROM: David Palmer at LANL E. Ambrosi (INAF-IASFPA), A. D'Ai (INAF-IASFPA), V. D'Elia (SSDC), J.D. Gropp (PSU), N. J. Klingler (PSU), A. Y. Lien (GSFC/UMBC), F. E. Marshall (NASA/GSFC), D. M. Palmer (LANL), M. H. Siegel (PSU) and A. Tohuvavohu (PSU) report on behalf of the Neil Gehrels Swift Observatory Team: At 04:07:18 UT, the Swift Burst Alert Telescope (BAT) triggered and located GRB 190613A (trigger=908288). Swift slewed immediately to the burst. The BAT on-board calculated location is RA, Dec 182.559, +67.233 which is RA(J2000) = 12h 10m 14s Dec(J2000) = +67d 13' 58" with an uncertainty of 3 arcmin (radius, 90% containment, including systematic uncertainty). The BAT light curve showed a single peak structure with a duration of about 30 sec. The peak count rate was ~500 counts/sec (15-350 keV), at ~10 sec after the trigger. The XRT began observing the field at 04:09:34.8 UT, 136.5 seconds after the BAT trigger. Using promptly downlinked data we find a bright, uncatalogued X-ray source located at RA, Dec 182.53286, 67.23489 which is equivalent to: RA(J2000) = 12h 10m 07.89s Dec(J2000) = +67d 14' 05.6" with an uncertainty of 4.0 arcseconds (radius, 90% containment). This location is 37 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. No spectrum from the promptly downlinked event data is yet available to determine the column density. The initial flux in the 2.5 s image was 1.18e-09 erg cm^-2 s^-1 (0.2-10 keV). UVOT took a finding chart exposure of 150 seconds with the White filter starting 144 seconds after the BAT trigger. There is a candidate afterglow in the list of sources generated on-board at RA(J2000) = 12:10:07.01 = 182.52919 DEC(J2000) = +67:14:07.0 = 67.23528 with a 90%-confidence error radius of about 1.10 arc sec. This position is 9.9 arc sec. from the center of the XRT error circle. The estimated magnitude is 18.28. No correction has been made for the expected extinction corresponding to E(B-V) of 0.02. Burst Advocate for this burst is E. Ambrosi (elena.ambrosi AT 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/)
GCN 24799 table
GRB_name GRB190613A
GCN_number 24799
Detection_method Fermi GBM final loc
t_trigger 4:07:18 UTC
ra 176.4000°
decl 64.8000°
Circular_text TITLE: GCN CIRCULAR NUMBER: 24799 SUBJECT: GRB 190613A: Fermi GBM Final Real-time Localization DATE: 19/06/13 04:19:01 GMT FROM: Fermi GBM Team at MSFC/Fermi-GBM The Fermi GBM team reports the detection of a likely LONG GRB At 04:07:18 UT on 13 Jun 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190613A (trigger 582091643.234478 / 190613172). The on-ground calculated location, using the Fermi GBM trigger data, is RA = 176.4, Dec = 64.8 (J2000 degrees, equivalent to J2000 11h 45m, 64d 47'), with a statistical uncertainty of 3.0 degrees. The angle from the Fermi LAT boresight is 11.0 degrees. The skymap can be found here: http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190613172/quicklook/glg_skymap_all_bn190613172.png The HEALPix FITS file, including the estimated localization systematic, can be found here: http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190613172/quicklook/glg_healpix_all_bn190613172.fit The GBM light curve can be found here: http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190613172/quicklook/glg_lc_medres34_bn190613172.gif
GCN 24800 table
GRB_name GRB190613A
GCN_number 24800
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 24800 SUBJECT: GRB 190613A: BALROG localization (Fermi Trigger 582091643 / GRB 190613172) DATE: 19/06/13 04:32:11 GMT FROM: Jochen Greiner at MPE,Garching J. Burgess, B. Biltzinger, F. Kunzweiler, F. Berlato, & J. Greiner (all MPE Garching) report: The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger 582091643 at 04:07:18 on 13 June 2019 were automatically fitted for spectrum and sky location with BALROG (Burgess et al. 2018, MNRAS 476, 1427; Berlato et al. 2019, ApJ 873, 60). The best-fit position (1 sigma statistical errors) is: RA(2000.0) = 200.2+/-13.8 deg Decl.(2000.0) = 66.4+/-3.8 deg We estimate an additional systematic error of 2 deg. Further details are available at: https://grb.mpe.mpg.de/grb/GRB190613172/ The Healpix map can be downloaded from: https://grb.mpe.mpg.de/grb/GRB190613172/healpix The location parameters are available as JSON at: https://grb.mpe.mpg.de/grb/GRB190613172/json
GCN 24801 table
GRB_name GRB190613A
GCN_number 24801
Detection_method Swift-UVOT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 24801 SUBJECT: GRB 190613A: KAIT Optical Afterglow Confirmation DATE: 19/06/13 05:02:42 GMT FROM: Weikang Zheng at UC Berkeley WeiKang Zheng and Alexei V. Filippenko (UC Berkeley) report on behalf of the KAIT GRB team: The 0.76-m Katzman Automatic Imaging Telescope (KAIT), located at Lick Observatory, responded to the Swift GRB 190613A (Ambrosi et al., GCN 24798) starting at 734s after the burst. Observations were performed with a sequence in the clear (roughly R), V, and I filters, and the exposure time was 60 s per image. We detected a fading source at the Swift/UVOT reported afterglow position (Ambrosi et al., GCN 24798) in all the filters. We estimate the clear band magnitude to be ~18.2 at 764s after the burst and faded to ~19.0 at 1290s after the burst. Observation are on going, multi-band follow-ups are encouraged. [GCN OPS NOTE(14jun19): The typo in Swift's name was corrected.]
GCN 24803 table
GRB_name GRB190613A
GCN_number 24803
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 24803 SUBJECT: GRB 190613A: MASTER OT detection DATE: 19/06/13 07:48:54 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs V. Lipunov, E.Gorbovskoy, V.Kornilov, N.Tiurina, A.Kuznetsov, I.Gorbunov, V.Vladimirov, P.Balanutsa, D.Vlasenko, D.Zimnukhov, F.Balakin,A. Chasovnikov, V.Topolev, V.Senik, D.Kuvshinov(Lomonosov Moscow State University, SAI, Physics Department), R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres (The Instituto de Astrofisica de Canarias), D. Buckley (South African Astronomical Observatory), R. Podesta, C. Lopez, C.Francile, F. Podesta (Observatorio Astronomico Felix Aguilar OAFA, San Juan National University), H.Levato (Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE, SJNU) O. Gress, N.M. Budnev, O.Ershova, S.Yazev (Applied Physics Institute, Irkutsk State University), V. Yurkov, A. Gabovich, Yu. Sergienko, D. Kobcev (Blagoveschensk Educational State University), A. Tlatov, D.Dormidontov, A.V. Parhomenko (Kislovodsk Solar Station of the Pulkovo Observatory), MASTER-IAC robotic telescope (MASTER Global Robotic Net: Lipunov et al., 2010, Advances in Astronomy,vol.2010, 30L (http://observ.pereplet.ru) located in Spain (IAC Teide Observatory) was pointed to the GRB 190613A (Swift alert, Ambrosi et al. GCN 24798, Fermi localization GCN 24799, BALROG localization Burgess et al. GCN 24800) 38 sec after notice time (104 sec after trigger time) at 2019-06-13 04:09:09 UT (Lipunov et al. GCN 24802). On our first (20s exposure) set MASTER auto-detection system found 1 optical transient within Swift error-box (ra=182.558 dec=67.2325 r=0.05) brighter than 16.4. T-Tmid Date Time Expt. Ra Dec Mag ---------|---------------------|-------|-----------------|-----------------|------- 114 2019-06-13 04:09:09 20 ( 12h 10m 07.08s , +67d 14m 06.5s) 15.96 this OT, discovered by Swift and also confirmed by KAIT(Ambrosi et al. GCN 24798, WeiKang Zheng et al. GCN 24801) The 5-sigma upper limit has been about 16.4mag
GCN 24809 table
GRB_name GRB190613A
GCN_number 24809
Detection_method Swift-XRT Det
ra 182.5296°
decl 67.2353°
Circular_text TITLE: GCN CIRCULAR NUMBER: 24809 SUBJECT: GRB 190613A: Enhanced Swift-XRT position DATE: 19/06/13 11:26:22 GMT FROM: Phil Evans at U of Leicester J.P. Osborne, A.P. Beardmore, P.A. Evans and M.R. Goad (U. Leicester) report on behalf of the Swift-XRT team. Using 3378 s of XRT Photon Counting mode data and 4 UVOT images for GRB 190613A, 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 = 182.52964, +67.23535 which is equivalent to: RA (J2000): 12h 10m 7.11s Dec (J2000): +67d 14' 07.3" 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.
GCN 24810 table
GRB_name GRB190613A
GCN_number 24810
Detection_method Swift-XRT Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 24810 SUBJECT: GRB 190613A: Swift-XRT refined Analysis DATE: 19/06/13 12:51:45 GMT FROM: Phil Evans at U of Leicester D.N. Burrows (PSU), J.P. Osborne (U. Leicester), K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester), V. D'Elia (ASDC), A. D'Ai (INAF-IASFPA), A. Melandri (INAF-OAB), A. Tohuvavohu (PSU), S. J. LaPorte (PSU) and report on behalf of the Swift-XRT team: report on behalf of the Swift-XRT team: We have analysed 8.1 ks of XRT data for GRB 190613A, from 142 s to 18.3 ks after the BAT trigger. The data comprise 127 s in Windowed Timing (WT) mode with the remainder in Photon Counting (PC) mode. The enhanced XRT position for this burst was given by Osborne et al. (GCN Circ. 24809). The light curve can be modelled with a series of power-law decays. The initial decay index is alpha=5.1 (+1.1, -0.9). At T+174 s the decay flattens to an alpha of -1.500000 (+0.905300, -0.000007). The light curve breaks again at T+207 s to a decay with alpha=5.0 (+0.7, -0.6), and again at T+372 s s to alpha=1.44 (+0.18, -0.15), before a final break at T+7345 s s after which the decay index is -1.5 (+0.0, -1.4). A spectrum formed from the WT mode data can be fitted with an absorbed power-law with a photon spectral index of 2.01 (+/-0.12). The best-fitting absorption column is 5.1 (+2.8, -2.6) x 10^20 cm^-2, in excess of the Galactic value of 1.5 x 10^20 cm^-2 (Willingale et al. 2013). The PC mode spectrum has a photon index of 1.75 (+0.22, -0.15) and a best-fitting absorption column of 2.0 (+4.9, -0.5) x 10^20 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor deduced from this spectrum is 3.7 x 10^-11 (3.8 x 10^-11) erg cm^-2 count^-1. A summary of the PC-mode spectrum is thus: Total column: 2.0 (+4.9, -0.5) x 10^20 cm^-2 Galactic foreground: 1.5 x 10^20 cm^-2 Excess significance: <1.6 sigma Photon index: 1.75 (+0.22, -0.15) If the light curve continues to decay with a power-law decay index of -1.5, the count rate at T+24 hours will be 0.41 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.5 x 10^-11 (1.6 x 10^-11) erg cm^-2 s^-1. The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00908288. This circular is an official product of the Swift-XRT team.
GCN 24815 table
GRB_name GRB190613A
GCN_number 24815
Detection_method Swift-UVOT Det
ra 182.5292°
decl 67.2353°
Circular_text TITLE: GCN CIRCULAR NUMBER: 24815 SUBJECT: GRB 190613A: Swift/UVOT Detection DATE: 19/06/13 17:36:46 GMT FROM: Frank Marshall at Swift/UVOT F. E. Marshall (NASA/GSFC) and E. Ambrosi (INAF-IASFPA) report on behalf of the Swift/UVOT team: The Swift/UVOT began settled observations of the field of GRB 190613A 145 s after the BAT trigger (Ambrosi et al., GCN Circ. 24798). A source consistent with the enhanced XRT position (Osborne et al. GCN Circ. 24809) is detected in the initial UVOT exposures. The preliminary UVOT position is: RA (J2000) = 12:10:07.01 = 182.52920 (deg.) Dec (J2000) = +67:14:07.0 = 67.23529 (deg.) with an estimated uncertainty of 0.43 arc sec. (radius, 90% confidence). Preliminary detections and 3-sigma upper limits 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 145 295 147 17.88 +/- 0.04 v 634 1061 58 18.63 +/- 0.29 b 560 753 39 18.93 +/- 0.21 u 303 553 246 18.88 +/- 0.11 w1 685 11118 1121 >20.1 m2 5323 6859 296 >20.8 w2 4913 6548 393 >21.5 The magnitudes in the table are not corrected for the Galactic extinction due to the reddening of E(B-V) = 0.02 in the direction of the burst (Schlegel et al. 1998).
GCN 24816 table
GRB_name GRB190613A
GCN_number 24816
Detection_method Fermi GBM Det
t_trigger 4:07:18.230 UTC
Circular_text TITLE: GCN CIRCULAR NUMBER: 24816 SUBJECT: GRB 190613A: Fermi GBM detection DATE: 19/06/13 17:38:42 GMT FROM: Suraj Poolakkil at UAH S. Poolakkil (UAH) and C. Meegan (UAH) report on behalf of the Fermi GBM Team: "At 04:07:18.23 UT on 13 June 2019, the Fermi Gamma-Ray Burst Monitor triggered and located GRB 190613A (trigger 582091643/ 190613172), which was also detected by the Swift/BAT (Ambrosi et al. 2019, GCN 24798). The GBM on-ground location is consistent with the Swift position. The angle from the Fermi LAT boresight at the GBM trigger time is 9 degrees. The GBM light curve shows a single peak with a duration (T90) of about 18 s (50-300 keV). The time-averaged spectrum from T0-1.0 s to T0+19.4 s is best fit by a power law function with an exponential high-energy cutoff. The power law index is 0.06 +/- 0.18 and the cutoff energy, parameterized as Epeak, is 108 +/- 5 keV. The event fluence (10-1000 keV) in this time interval is (3.092 +/- 0.129)E-06 erg/cm^2. The 1-sec peak photon flux measured starting from T+11.9 s in the 10-1000 keV band is 2.3 +/- 0.2 ph/s/cm^2. The spectral analysis results presented above are preliminary; final results will be published in the GBM GRB Catalog: https://heasarc.gsfc.nasa.gov/W3Browse/fermi/fermigbrst.html For Fermi GBM data and info, please visit the official Fermi GBM Support Page: https://fermi.gsfc.nasa.gov/ssc/data/access/gbm/"
GCN 24819 table
GRB_name GRB190613A
GCN_number 24819
Detection_method Swift-BAT Det
ra 182.5520°
decl 67.2440°
Circular_text TITLE: GCN CIRCULAR NUMBER: 24819 SUBJECT: GRB 190613A, Swift-BAT refined analysis DATE: 19/06/13 19:46:50 GMT FROM: Amy Lien at GSFC M. Stamatikos (OSU), E. Ambrosi (INAF-IASFPA) S. D. Barthelmy (GSFC), J. R. Cummings (CPI), H. A. Krimm (NSF), A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU), T. N. Ukwatta (LANL) (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 190613A (trigger #908288) (Ambrosi et al., GCN Circ. 24798). The BAT ground-calculated position is RA, Dec = 182.552, 67.244 deg which is RA(J2000) = 12h 10m 12.5s Dec(J2000) = +67d 14' 39.7" with an uncertainty of 2.2 arcmin, (radius, sys+stat, 90% containment). The partial coding was 9%. The mask-weighted light curve shows a weak pulse that starts at ~T0, peaks at ~T+7 s, and ends at ~T+20 s. T90 (15-350 keV) is 17.6 +- 3.1 sec (estimated error including systematics). The time-averaged spectrum from T+0.6 to T+20.3 sec is best fit by a simple power-law model. The power law index of the time-averaged spectrum is 1.22 +- 0.26. The fluence in the 15-150 keV band is 1.7 +- 0.3 x 10^-6 erg/cm2. The 1-sec peak photon flux measured from T+6.88 sec in the 15-150 keV band is 1.5 +- 0.7 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/908288/BA/ [GCN OPS NOTE(13jun19): Per author's request, in the 3rd line "GCN Circ. 908288" was corrected to read "GCN Circ. 24798".
GCN 24822 table
GRB_name GRB190613A
GCN_number 24822
Detection_method Other
Circular_text TITLE: GCN CIRCULAR NUMBER: 24822 SUBJECT: GRB 190613A: FRAM-ORM afterglow detection DATE: 19/06/13 20:37:13 GMT FROM: Martin Jelinek at Astro.Inst-AVCR,Ondrejov Martin Jelinek, Jan Strobl (ASU CAS Ondrejov, CZ), Martin Masek, Petr Janecek, Sergey Karpov, Jakub Jurysek, Jan Ebr, Ronan Cunniffe, Petr Travnicek and Michael Prouza (Institute of Physics, Prague, CZ) report: The 25cm robotic telescope FRAM-ORM at La Palma (Spain) reacted robotically to the alert of GRB190613A (Ambrosi et al, GCNC 24798), starting with a series of 20 s unfiltered images at 04:10:11 UT, i.e. 3 min post trigger. We clearly detect the source reported by (Ambrosi et al, GCN 24798; Zheng & Filipenko, GCN 24801 and Lipunov et al, GCN 24803), decaying at a rate of alpha ~ 1.51. The brightnes of the object was R = 18.2 +- 0.2 at an image centered at 04:25:15 UT, i.e. 18 min post burst. [GCN OPS Note(15jun19): Per OPS, the extra "Subject:" was removed from the Subject line.]
GCN 24835 table
GRB_name GRB190613A
GCN_number 24835
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 24835 SUBJECT: GRB 190613A: SEDM Observations DATE: 19/06/15 01:26:58 GMT FROM: Virginia Cunningham at U of MD V. Cunningham (U of Maryland), J. D. Neill (Caltech), S. B. Cenko (NASA GSFC), and R. Walters (Caltech) report on behalf of the SEDM team: We observed the optical counterpart to GRB 190613A (Ambrosi et al., GCN 24798) with the Spectral Energy Distribution Machine (SEDM) on the 60 inch telescope at Palomar Observatory. The SEDM is a low resolution (R ~ 100) integral field unit spectrometer with a multi-band (ugri) rainbow camera imager (see Blagorodnova et al. 2018, PASP, 130, 035003, and Rigault et al. 2019, astro-ph/1902.08526). The SEDM began observing the optical counterpart at 04:18:22 UTC (8.75 minutes after the burst trigger time). We performed an 1800 s exposure over the wavelength range 3800-9200 A. The continuum emission is well-fit by a power law spectrum with index alpha = 0.56 (f_nu ~ nu^-alpha). We detect an absorption line at an observed wavelength of ~ 4597 A. We tentatively identify this line as due to Lyman alpha at z = 2.78 - however due to the lack of corroborating features we consider this redshift tentative currently. [GCN OPS NOTE(07sep19): Per author's request, in the last paragraph, the "alpha = 0.56" was changed to "alpha = 1.4".]
GCN 24838 table
GRB_name GRB190613A
GCN_number 24838
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 24838 SUBJECT: GRB 190613A: Kitab and AbAO optical upper limit DATE: 19/06/15 09:38:38 GMT FROM: Alexei Pozanenko at IKI, Moscow S. Belkin (IKI), A. Novichonok (KIAM), A. Zhornichenko (KIAM), R. Ya. Inasaridze (AbAO), V.R. Ayvazian (AbAO), A. Pozanenko (IKI), E. Mazaeva (IKI), A. Volnova (IKI), I. Molotov (KIAM), Sh. Ehgamberdiev (UBAI) report on behalf of larger IKI GRB FuN collaboration: We observed the field of the GRB 190613A (Ambrosi et al., GCN 24798) with RC-36 telescope of Kitab Observatory and AS-32 of Abastumani observatory . We do not detect the optical afterglow (Ambrosi et al., GCN 24798; Zheng et al., GCN 24801; Lipunov et al., GCN 24803). Preliminary photometry of the field is following. Date UT start t-T0 Filter Exp. OT Err. UL(3sigma) Telescope (mid, days) (s) 2019-06-13 16:26:41 0.54575 CR 5500 n/d n/d 20.6 RC-36 2019-06-13 21:33:40 0.73706 R 1800 n/d n/d 21.0 AS-32 The photometry is based on the nearby USNO-B1 (R2) stars USNO-B1.0_id R2 1572-0165015 13.62 1572-0164999 14.91 1572-0164916 14.28 [GCN OPS NOTE(15jun19): Per OPS, the typo in the Subject-line "1906013A" was changed to "190613A".]
GCN 24850 table
GRB_name GRB190613A
GCN_number 24850
Detection_method Optical
Circular_text TITLE: GCN CIRCULAR NUMBER: 24850 SUBJECT: GRB 190613A: SEDM Observations DATE: 19/06/19 14:01:11 GMT FROM: Virginia Cunningham at U of MD V. Cunningham (U of Maryland), J. D. Neill (Caltech), S. B. Cenko (NASA GSFC), and R. Walters (Caltech) report on behalf of the SEDM team: We observed the optical counterpart to GRB 190613A (Ambrosi et al., GCN 24798) with the Spectral Energy Distribution Machine (SEDM) on the 60 inch telescope at Palomar Observatory. The SEDM is a low resolution (R ~ 100) integral field unit spectrometer with a multi-band (ugri) rainbow camera imager (see Blagorodnova et al. 2018, PASP, 130, 035003, and Rigault et al. 2019, astro-ph/1902.08526). The SEDM began observing the optical counterpart at 04:18:22 UTC (8.75 minutes after the burst trigger time). We performed an 1800 s exposure over the wavelength range 3800-9200 A. The continuum emission is well-fit by a power law spectrum with index alpha = 0.56 (f_nu ~ nu^-alpha). We detect an absorption line at an observed wavelength of ~ 4597 A. We tentatively identify this line as due to Lyman alpha at z = 2.78 - however due to the lack of corroborating features we consider this redshift tentative currently.