GRB 170519A
GCN Circular 21211
Subject
GRB 170519A: 15 GHz upper limits from AMI
Date
2017-06-07T22:36:01Z (9 years ago)
From
Kunal Mooley at Oxford U <kunal.mooley@physics.ox.ac.uk>
K. P. Mooley (Hintze Fellow, Oxford), T. D. Staley, R. P. Fender
(Oxford), G. E. Anderson (Curtin), T. Cantwell (Manchester), D.
Titterington, S. H. Carey, J. Hickish, Y. C. Perrott, N. Razavi-Ghods,
P. Scott (Cambridge), K. Grainge, A. Scaife (Manchester)
The AMI Large Array robotically triggered on the Swift alert for GRB
170519A (Ukwatta et al., GCN 21106) as part of the 4pisky program, and
subsequent follow up observations were obtained up to 10 days
post-burst. Our observations at 15 GHz on 2016 May 19.61, May 20.84, May
23.74 and May 27.78 (UT) do not reveal any radio source at the XRT
location (Beardmore et al., GCN 21107), with 3sigma upper limits of 228
uJy, 190 uJy, 150 uJy, and 100 uJy respectively.
We thank the AMI staff for scheduling these observations. The AMI-GRB
database is a log of all GRB follow up observations with the AMI, and is
available at http://4pisky.org/ami-grb/.
GCN Circular 21208
Subject
GRB 170519A: TShAO and AbAO optical observations
Date
2017-06-05T19:41:04Z (9 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
E. Mazaeva (IKI), A. Pozanenko (IKI), A. Kusakin (Fesenkov Astrophysical
Institute), R. Inasaridze (AbAO), I. Reva (Fesenkov Astrophysical
Institute), A. Volnova (IKI), V. Ayvazian (AbAO), O. Kvaratskhelia
(AbAO), G. Inasaridze (AbAO), I. Molotov (KIAM) report on behalf of
larger GRB follow-up collaboration:
We observed the field of GRB 170519A (Ukwatta et al., GCN 21106) with
Zeiss-1000 1-m telescope of Tien Shan Astronomical Observatory
starting on May 20 (UT) 18:42:38. We took several images in R-filter
with exposures of 120 s during this night and 2 subsequent nights.
The optical afterglow (Ukwatta et al., GCN 21106; Izzo, et al.,
GCN 21108) is visible in stacked images.
We also observed this field with AS-32 (0.7m) telescope of Abastumani
Observatory on May 21 (UT) 17:22:33. We took several unfiltered frames
with 60 s exposure. In the enhanced XRT error circle (Beardmore et al.,
GCN 21107) we do not detect the afterglow.
Preliminary photometry of the afterglow is following:
Date UT start t-T0 Filter Exp. OT Err. UL Telescope
(mid, days) (s) (3 sigma)
2017-05-20 18:42:38 1.58414 R 24*120 20.06 0.06 21.4 Zeiss-1000
2017-05-21 15:58:25 2.48340 R 39*120 20.95 0.14 21.6 Zeiss-1000
2017-05-22 15:27:05 3.46168 R 39*120 22.20 0.40 21.9 Zeiss-1000
2017-05-21 17:22:33 2.52050 CR 20*60 n/d n/d 20.8 AS-32
The photometry is based on nearby SDSS stars, reported by
Mazaeva et al. (GCN 21169).
The light curve of the GRB 170519A afterglow based on our observations
(GCNs 21162, 21169, 21206) can be found at
http://grb.rssi.ru/GRB170519A/GRB170519A_lc.png
GCN Circular 21206
Subject
GRB 170519A: Mondy optical observations
Date
2017-06-05T19:07:17Z (9 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
E. Mazaeva (IKI), A. Pozanenko (IKI), E. Klunko (ISTP), A. Volnova (IKI)
report on behalf of larger GRB follow-up collaboration:
We observed the field of GRB 170519A (Ukwatta et al., GCN 21106) with
AZT-33IK telescope of Sayan observatory (Mondy) starting on May 20 (UT)
16:27:01. We took several images in R-filter with exposures of 120 s.
The optical afterglow (Ukwatta et al., GCN 21106; Izzo, et al., GCN
21108) is clearly visible in single images.
We continued our observations on May 27 (UT) 16:28:02, i.e., ~8.5 days
after the BAT trigger. We took several R-filtered images. We do not
detect the optical counterpart in the enhanced XRT error circle
(Beardmore et al., GCN 21107).
Preliminary photometry of the afterglow is following:
Date UT start t-T0 Filter Exp. OT Err. UL
(mid, days) (s)
(3 sigma)
2017-05-20 16:27:01 1.47708 R 10*120 19.99 0.03 22.8
2017-05-20 17:07:02 1.50487 R 10*120 19.99 0.03 22.6
2017-05-27 16:28:02 8.49905 R 39*120 n/d n/d 22.6
The photometry is based on nearby SDSS stars reported by
Mazaeva et al. (GCN 21169).
GCN Circular 21169
Subject
GRB 170519A: CrAO optical observations
Date
2017-05-30T20:33:55Z (9 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
E. Mazaeva (IKI), K. Antonyuk (CrAO), I. Nikolenko (CrAO), V. Rumyantsev
(CrAO), A. Volnova (IKI), A. Pozanenko (IKI) report on behalf of larger
GRB follow-up collaboration:
We observed the field of the GRB 170519A (Ukwatta et al., GCN 21106)
with AZT-11 telescope of CrAO observatory starting on May 19 (UT)
19:07:44, and with Zeiss-1000/Koshka telescope of Simeiz branch of CrAO
observatory starting on May 19 (UT) 19:28:57. We took several images in
filter R with exposures of 180 s. We clearly detect the afterglow
(Ukwatta et al., GCN 21106; Izzo et al., GCN 21108) in combined images.
Preliminary photometry of the combined images is following
UT start t-T0 Filter Exp. OT err UL Telescope
(mid, days) (s) (3sigma)
19:07:44 0.58810 R 6*180 19.17 0.11 20.9 AZT-11
19:26:08 0.59878 R 4*180 19.23 0.12 20.7 AZT-11
19:41:28 0.61473 R 9*180 19.58 0.12 21.1 AZT-11
19:28:57 0.59751 R 1*180 19.05 0.10 20.4 Zeiss-1000
19:31:58 0.60066 R 2*180 19.12 0.10 21.1 Zeiss-1000
19:38:02 0.60592 R 3*180 19.52 0.14 20.3 Zeiss-1000
19:47:08 0.61224 R 3*180 19.52 0.16 20.3 Zeiss-1000
19:56:13 0.62065 R 5*180 19.64 0.14 21.3 Zeiss-1000
The photometry is based on nearby SDSS stars:
SDSS-DR9_id R(Lupton)
J105339.53+252259.9 17.32
J105332.97+252127.3 16.22
J105348.21+252041.2 17.03
J105341.14+252534.0 16.18
J105353.70+252400.0 15.30
GCN Circular 21162
Subject
GRB 170519A: ISON/Multa optical observations
Date
2017-05-29T18:41:18Z (9 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
E. Mazaeva (IKI), A. Krylov (KIAM), Yu. Krylova (KIAM), S. Schmalz
(KIAM), A. Volnova (IKI), A. Pozanenko (IKI) report on behalf of larger
GRB follow-up collaboration:
We observed the field of GRB 170519A (Ukwatta et al., GCN 21106) with
22cm SSS-220 telescope of ISON/Multa observatory(* starting on May 19
(UT) 16:02:54. We took 120 unfiltered frames with 60 s exposure. The
optical transient (Ukwatta et al., GCN 21106; Izzo, et al., GCN 21108)
is clearly detected in a combined image.
Preliminary photometry of the combined image is following
Date UT start t-T0 Filter Exp. OT err UL
(mid, days) (s) (3sigma)
2017-05-19 16:02:54 0.53936 CR 120*60 18.92 0.28 19.0
The photometry is based on nearby SDSS stars:
SDSS-DR9_id R(Lupton)
J105316.02+252545.1 16.75
J105332.97+252127.3 16.22
J105336.13+251707.2 15.46
J105322.03+251651.0 15.91
J105339.27+251620.6 16.66
J105338.87+252621.2 16.00
*) The ISON/Multa observatory is located in Altai, N 50d 10��� 07��� E 85d
57��� 25���. The SSS-220 telescope (22 cm, f/2.3) is equipped with CCD
camera ML 11002.
GCN Circular 21124
Subject
GRB 170519A: MITSuME Akeno Optical Observation
Date
2017-05-22T06:07:27Z (9 years ago)
From
Taketoshi Yoshii at Tokyo Tech <yoshii.t.ac@m.titech.ac.jp>
K. Morita, Y. Saito, R. Itoh, T. Yoshii, Y. Tachibana, S. Harita, Y. Muraki,
T. Ozawa, K. Shiraishi, H. Mamiya, Y. Yatsu, and N. Kawai
(Tokyo Tech)
report on behalf of the MITSuME collaboration:
We searched for the optical counterpart of GRB 170519A (T. N. Ukwatta et al., GCN Circular #21106)
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 2017-05-19 11:03:14 UT (21192 sec after the burst).
We detected the optical counterpart (T. N. Ukwatta et al., GCN Circular #21106) in g', Rc and Ic band.
The measured magnitudes were listed as follows.
T0+[hour] MID-UT T-EXP[sec] g' Rc Ic
----------------------------------------------------------------------------
~5.9 11:34:54 4278 $B!!!!(B19.14+/-0.15 18.48+/-0.11 18.13+/-0.13
----------------------------------------------------------------------------
T0+ : Elapsed time after the burst
T-EXP: Total Exposure time
We used GSC2.3 catalog for flux calibration.
GCN Circular 21123
Subject
GRB 170519A: Watcher optical observations
Date
2017-05-20T18:31:58Z (9 years ago)
From
Antonio Martin-Carrillo at UCD,Space Science Group <antonio.martin-carrillo@ucd.ie>
A. Martin-Carrillo (UCD), D. Murphy (UCD), L. Hanlon (UCD), H. J. van Heerden (UFS), B. van Soelen (UFS) and P. J. Meintjes (UFS)
We observed the field of GRB 170519A (Ukwatta, et al., GCN 21106 using the 40cm UCD Watcher telescope at Boyden Observatory in South Africa.
Observations started on May 19th at 16:30 UT (T0+11.5h) and consisted of a series of 20s exposures in SDSS r��� filter for a total monitoring time of 3 hours. Based on combined images with mid-time at 17:00 UT, we derive a preliminary magnitude of r���=19.3 +/- 0.3 (AB system).
Magnitudes were calibrated using 2 nearby APASS stars. No correction for Galactic extinction in the direction of the GRB has been applied.
GCN Circular 21122
Subject
GRB 170519A: Continued RATIR Optical and NIR Observations
Date
2017-05-20T14:32:57Z (9 years ago)
From
Nat Butler at Az State U <natbutler@asu.edu>
Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William
H. Lee (UNAM), Michael G. Richer (UNAM), Ori Fox (STScI), J. Xavier
Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (UVI), Eleonora
Troja (GSFC), Owen Littlejohns (ASU), Enrico Ramirez-Ruiz (UCSC), Jes��s
Gonz��lez (UNAM), Carlos Rom��n-Z����iga (UNAM), Harvey Moseley (GSFC), John
Capone (UMD), V. Zach Golkhou (ASU), and Vicki Toy (UMD) report:
We observed the field of GRB 170519A (Ukwatta,, et al., GCN 21106) with the
Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the
1.5m Harold Johnson Telescope at the Observatorio Astron��mico Nacional on
Sierra San Pedro M��rtir from 2017/05 20.16 to 2017/05 20.32 UTC (22.66 to
26.62 hours after the BAT trigger), obtaining a total of 2.49 hours
exposure in the r and i bands and 0.97 hours exposure in the Z, Y, J, and H
bands.
In comparison with the SDSS DR9 and 2MASS catalogs, we obtain the following
detections of the optical transient:
r = 20.57 +/- 0.01
i = 20.39 +/- 0.01
Z = 20.05 +/- 0.04
Y = 20.15 +/- 0.05
J = 20.02 +/- 0.06
H = 19.72 +/- 0.07
These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB.
We thank the staff of the Observatorio Astron��mico Nacional in San Pedro
Martir.
GCN Circular 21121
Subject
GRB 170519A: MITSuME Okayama Optical Observation
Date
2017-05-20T05:01:54Z (9 years ago)
From
Daisuke Kuroda at OAO/NAOJ <dikuroda@oao.nao.ac.jp>
D. Kuroda, K. Yanagisawa, Y. Shimizu, H. Toda (OAO, NAOJ),
S. Nagayama (NAOJ), M. Yoshida (Subaru, NAOJ), K. Ohta (Kyoto)
and N. Kawai(Tokyo Tech)
report on behalf of the MITSuME and OISTER collaboration:
We observed the field of GRB 170519A (Ukwatta et al., GCNC 21106)
with the optical three color (g', Rc and Ic) CCD camera attached
to the MITSuME 50cm telescope of Okayama Astrophysical Observatory.
The observation started on 2017-05-19 11:03:26 UT (~5.9 h after
the burst). We detected the previously reported afterglow (Ukwatta
et al., GCNC 21106; Izzo et al., GCNC 21108) in all the three bands.
Photometric results of the OT are listed below. We used SDSS-DR8
catalog for flux calibration.
#T0+[day] MID-UT T-EXP[sec] g' g'_err Rc Rc_err Ic Ic_err
------------------------------------------------------------------
0.26646 11:33:44 3120.0 19.1 0.2 18.7 0.2 18.1 0.2
------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]
GCN Circular 21120
Subject
GRB 170519A: NOT optical observations
Date
2017-05-19T23:53:45Z (9 years ago)
From
Antonio de Ugarte Postigo at IAA-CSIC <deugarte@iaa.es>
A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), D. Xu (NAOC),
D. Malesani (DARK/NBI), K.E. Heintz (DARK/NBI),
D. Gandolfi (Univ. Turin), and J. Telting (NOT) report on behalf
of a larger collaboration,
We have observed the field of GRB 170519A (Ukwatta et al.,
GCN 21106) with the 2.5m Nordic Optical Telescope at La
Palma (Spain). The observations consisted of 3x120s in V-band
and 5x120s in Sloan i-band. The GRB afterglow is well detected in
all the individual frames. On an image starting at 21:51 UT (16.68 hr
after the burst) we detect the optical afterglow at i(AB) = 19.7 mag,
as compared to SDSS field stars. This confirms the t^(-0.8) decay
reported by Butler et al. (GCN 21109) and by Zheng et al.
(GCN 21115) that started 900 s after the GRB trigger.
GCN Circular 21119
Subject
GRB 170519A: Redshift from GTC/OSIRIS
Date
2017-05-19T23:43:59Z (9 years ago)
From
Luca Izzo at IAA-CSIC <Luca.Izzo@ICRA.it>
L. Izzo (IAA-CSIC), A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), D.A. Kann (IAA-CSIC), C.C. Thoene (IAA-CSIC), P. Pessev (GTC, IAC) and A. Tejero (GTC) report on behalf of a larger collaboration:
We observed the afterglow of the GRB 170519A (Ukwatta et al., GCN 21106) using OSIRIS on the 10.4m GTC at the Roque de los Muchachos observatory (La Palma, Spain). The observation consisted of 3x1200s exposures using the R1000B grism, covering the range between 3700 and 7800 AA. The first spectrum started at 21:23 UT (16.22 hr after the burst).
We detect clear absorption features due to Mg II, Mg I, Fe II, Fe II* and Ca II H&K lines at the common redshift of z = 0.818, which we identify as the redshift of the GRB.
GCN Circular 21118
Subject
GRB170519A, Swift-UVOT Detection
Date
2017-05-19T23:24:09Z (9 years ago)
From
Sam LaPorte at PSU <sjl5346@psu.edu>
GRB 170519A: Swift/UVOT Detection
S. J. LaPorte (PSU) and T. N. Ukwatta (LANL)
report on behalf of the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 170519A
93 s after the BAT trigger (Ukwatta et al., GCN Circ. 21106).
A fading source consistent with the XRT position
(Beardmore et al. GCN Circ. 21107)
is detected in all initial UVOT exposures.
The preliminary UVOT position is:
RA (J2000) = 10:53:42.45 = 163.42688 (deg.)
Dec (J2000) = +25:22:27.5 = 25.37431 (deg.)
with an estimated uncertainty of 0.42 arc sec. (radius, 90% confidence).
Preliminary detections using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the early exposures are:
Filter T_start(s) T_stop(s) Exp(s) Mag
white 5315 5515 196 17.22+-0.03
white 582 773 38 16.25+-0.04
white 89 239 147 16.91+-0.03
v 68 5926 421 17.46+-0.08
b 557 6594 282 17.66+-0.05
u 302 552 245 16.00+-0.04
uvw1 680 6337 412 16.76+-0.05
uvm2 5932 6131 196 17.13+-0.11
uvw2 607 627 19 16.45+-0.20
The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.03 in the direction of the burst
GCN Circular 21117
Subject
GRB 170519A: BOOTES-5/JGT early optical detection
Date
2017-05-19T22:58:31Z (9 years ago)
From
Alberto Castro-Tirado at Inst.de Astro. de Andalucia <ajct@iaa.es>
A. J. Castro-Tirado (IAA-CSIC & ISA-UMA), J. C. Tello, R. Cunniffe,
B.-B. Zhang, Y. Hu and A. Gonzalez-Rodriguez (IAA-CSIC), A. Castellon
(Univ. de Malaga), D. Hiriart, W. H. Lee (UNAM), S. Jeong and I. H. Park (SKKU)
and P. Kubanek (Inst. of Physics, CZ) on behalf of a larger collaboration, report:
The 60 cm BOOTES-5/Javier Gorosabel Telescope at Observatorio
Astron��mico Nacional in San Pedro M��rtir (M��xico) automatically
responded to the Swift trigger of GRB 170519A (Ukwatta et al., GCN
21106). The first unfiltered images (60 s exposures) were obtained at
05:15:08.9 UT (5 min after the burst). At the position of the Swift
X-ray afterglow, we confirm the optical afterglow detected by UVOT, at a
magnitude of 16.6+/-0.1 when compared to the GSC2.3 catalog, and fading
during the late-time BOOTES-5/JGT observation.
We thank the staff at Observatorio Astron��mico Nacional in San Pedro
M��rtir for its excellent support.
[GCN OPS NOTE(19may17), At the request of the author, the last 3 authors
were added.]
GCN Circular 21115
Subject
GRB 170519A: KAIT Optical Observations
Date
2017-05-19T18:44:38Z (9 years ago)
From
Weikang Zheng at UC Berkeley <weikang@berkeley.edu>
WeiKang Zheng, Max Genecov, and Alex Filippenko (UC Berkeley) report on
behalf of the KAIT GRB team:
The 0.76-m Katzman Automatic Imaging Telescope (KAIT) at
Lick Observatory responded to Swift GRB 170519A (Ukwatta et al.,
GCN 21106) starting at 05:14:24 UT, 262s after the burst.
Observations were performed with an automatic sequence in the
V, I, and clear (roughly R) filters, and the exposure time was
20 s per image, observations lasted about 2 hours.
The optical afterglow (Ukwatta et al., GCN 21106; Izzo et al.,
GCN 21108; Butler et al., GCN 21109; Guidorzi et al., GCN 21110;
Xu et al., GCN 21111; Hentunen & Nissinen, GCN 21113) was well
detected in our V, I and clear filter images. A preliminary
analysis shows that the afterglow rises at early time and peaked
around 1 ks. After 3 ks after the burst, the light curve can be
fitted by a power law with index of -0.83.
A preliminary light curve is posted at:
http://astro.berkeley.edu/~zwk/grb/GRB170519A/GRB170519A_kait.png
GCN Circular 21114
Subject
GRB 170519A: Swift-XRT refined Analysis
Date
2017-05-19T16:20:48Z (9 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
S. J. LaPorte (PSU), K.L. Page (U. Leicester), B. Mingo (U. Leicester),
A.P. Beardmore (U. Leicester), A. D'Ai (INAF-IASFPA), A. Melandri
(INAF-OAB), P. D'Avanzo (INAF-OAB), J.A. Kennea (PSU), B. Sbarufatti
(INAF-OAB/PSU) and T.N. Ukwatta report on behalf of the Swift-XRT team:
We have analysed 9.5 ks of XRT data for GRB 170519A (Ukwatta et al. GCN
Circ. 21106), from 73 s to 23.1 ks after the BAT trigger. The data
comprise 291 s in Windowed Timing (WT) mode (the first 6 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Beardmore
et al. (GCN Circ. 21107).
The late-time light curve (from T0+4.1 ks) can be modelled with a
power-law decay with a decay index of alpha=0.94 (+/-0.08).
A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.62 (+/-0.05). The
best-fitting absorption column is 1.78 (+0.12, -0.11) x 10^21 cm^-2,
in excess of the Galactic value of 2.4 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 1.98 (+/-0.10) and a
best-fitting absorption column of 1.20 (+0.29, -0.27) x 10^21 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum is 3.4 x 10^-11 (4.3 x 10^-11) erg cm^-2
count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 1.20 (+0.29, -0.27) x 10^21 cm^-2
Galactic foreground: 2.4 x 10^20 cm^-2
Excess significance: 5.8 sigma
Photon index: 1.98 (+/-0.10)
If the light curve continues to decay with a power-law decay index of
0.94, the count rate at T+24 hours will be 0.030 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.0 x
10^-12 (1.3 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/00753445.
This circular is an official product of the Swift-XRT team.
GCN Circular 21113
Subject
GRB 170519A: iTelescope T11 optical observations
Date
2017-05-19T15:42:57Z (9 years ago)
From
Veli-Pekka Hentunen at Taurus Hill Obs,A95 <veli-pekka.hentunen@kassiopeia.net>
Veli-Pekka Hentunen and Markku Nissinen (Taurus Hill Observatory (A95),
Varkaus, Finland) report:
We have detected GRB 170519A optical afterglow at iTelescope observatory
T11 (Mayhill, New Mexico) using 0.51-m/6.8 Planewave CDK telescope and
FLI ProLine PL11002M CCD camera. The observations were started at
2017-05-19 05:25:24 (UT). Eleven unfiltered images and seven photometric
R filter images with 120 sec exposure time were taken.
The optical afterglow was detected at the position RA 10:53:42.46
and DEC +25:22:27.4.
The following magnitudes were obtained from the observations using
NOMAD1 1153-0183949 (R = 12.650) as a comparison star:
Tmid(s)+T0 Filter Exp. time Mag Mag err.
1119 unfiltered 3x120 15.52CR 0.03
1452 unfiltered 2x120 15.63CR 0.03
1906 R 3x120 15.98R 0.10
2324 R 2x120 16.08R 0.11
2806 unfiltered 4x120 16.07CR 0.05
3327 unfiltered 2x120 16.17CR 0.05
3795 R 2x120 16.50R 0.16
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GCN Circular 21112
Subject
GRB 170519A: Swift-BAT refined analysis
Date
2017-05-19T15:26:19Z (9 years ago)
From
Hans Krimm at NSF/NASA-GSFC <hkrimm@nsf.gov>
H. A. Krimm (NSF/USRA), S. D. Barthelmy (GSFC), J. R. Cummings (CPI),
A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (AGU), M. Stamatikos (OSU), T. N. Ukwatta (LANL)
(i.e. the Swift-BAT team):
Using the data set from T-240 to T+630 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 170519A (trigger #753445)
(Ukwatta, et al., GCN Circ. 21106). The BAT ground-calculated position is
RA, Dec = 163.429, 25.374 deg which is
RA(J2000) = 10h 53m 42.9s
Dec(J2000) = +25d 22' 26.6"
with an uncertainty of 1.5 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.
The mask-weighted light curve shows an initial peak starting around T-30 s, peaking
at T+0 s, and decaying by T+15 s. Then there is a second, weaker peak from about
T+180 s to T+220 s. T90 (15-350 keV) is 216.4 +- 49.4 sec (estimated error including
systematics).
The time-averaged spectrum from T-28.5 to T+255.6 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
1.94 +- 0.26. The fluence in the 15-150 keV band is 1.1 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+0.84 sec in the 15-150 keV band
is 0.7 +- 0.1 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/753445/BA/
GCN Circular 21111
Subject
GRB 170519A: Weihai optical observations
Date
2017-05-19T14:41:03Z (9 years ago)
From
Dong Xu at NAOC/CAS <dxu@nao.cas.cn>
D. Xu, Z.P. Zhu, H.X. Feng (NAOC), C.M. Zhang, S.M. Hu (SDU), Y.D. Hu
(IAA-CSIC), Y. Qin (Geneva Observatory) report:
We observed the field of GRB 170519A (Ukwatta et al., GCN 21106) using
the 1-m telescope located at Weihai, Shandong, China. We obtained 4x360s
frames in the Sloan r-filter, starting at 11:52:54 UT on 2017-05-19,
i.e., 6.71 hr after the burst.
The optical afterglow (Ukwatta et al., GCN 21106; Izzo et al., GCN
21108) is clearly detected in our stacked image, and it has decayed to
m(r) = 18.92 +/- 0.06 at 6.94 hr post-burst, calibrated with nearby SDSS
stars.
GCN Circular 21109
Subject
GRB 170519A: RATIR Optical and NIR Observations
Date
2017-05-19T13:08:22Z (9 years ago)
From
Nat Butler at UC berkeley <natxbutler@gmail.com>
Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William
H. Lee (UNAM), Michael G. Richer (UNAM), Ori Fox (STScI), J. Xavier
Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (UVI), Eleonora
Troja (GSFC), Owen Littlejohns (ASU), Enrico Ramirez-Ruiz (UCSC), Jes��s
Gonz��lez (UNAM), Carlos Rom��n-Z����iga (UNAM), Harvey Moseley (GSFC), John
Capone (UMD), V. Zach Golkhou (ASU), and Vicki Toy (UMD) report:
We observed the field of GRB 170519A (Ukwatta, et al., GCN 21106) with the
Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the
1.5m Harold Johnson Telescope at the Observatorio Astron��mico Nacional on
Sierra San Pedro M��rtir from 2017/05 19.22 to 2017/05 19.32 UTC (1.8
minutes to 2.44 hours after the BAT trigger), obtaining a total of 1.41
hours exposure in the r and i bands and 0.60 hours exposure in the Z, Y, J,
and H bands.
The optical transient (GCN 21106; Izzo, et al., GCN 21108) is clearly
detected. In comparison with the SDSS DR9 and 2MASS catalogs, we obtain:
r 16.72 +/- 0.01
i 16.50 +/- 0.01
Z 16.34 +/- 0.01
Y 16.25 +/- 0.01
J 16.15 +/- 0.01
H 15.87 +/- 0.01
These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB. The lightcurve rises in all bands
initially, peaking at i~16 at about 15 minutes after the GRB trigger, then
fading as t^(-0.8).
We thank the staff of the Observatorio Astron��mico Nacional in San Pedro
M��rtir.
GCN Circular 21108
Subject
GRB 170519A: optical observations
Date
2017-05-19T10:10:58Z (9 years ago)
From
Luca Izzo at IAA-CSIC <Luca.Izzo@ICRA.it>
L. Izzo, A. de Ugarte Postigo, Z. Cano, D.A. Kann (IAA-CSIC) report on behalf of a larger collaboration,
We observed the field of GRB 170519A (Ukwatta et al., GCN 21106) with the T24 (Plane Wave CDK 0.61m) of the iTelescope.Net (http://www.itelescope.net) located at Auberry, CA.
A single image of 300 s was taken in the V filter, starting at 07:18:04 UT, 2.13 hr after the GRB trigger. The GRB optical afterglow is clearly detected with a preliminary photometry estimate of V ~ 18, as compared to field stars of the GSC2.3 catalog.
An image of the field can be seen at http://goo.gl/GScY4H
GCN Circular 21107
Subject
GRB 170519A: Enhanced Swift-XRT position
Date
2017-05-19T08:49:25Z (9 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
A.P. Beardmore, P.A. Evans, M.R. Goad and J.P. Osborne (U. Leicester)
report on behalf of the Swift-XRT team.
Using 2439 s of XRT Photon Counting mode data and 5 UVOT
images for GRB 170519A, 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 = 163.42699, +25.37417 which is equivalent
to:
RA (J2000): 10h 53m 42.48s
Dec (J2000): +25d 22' 27.0"
with an uncertainty of 1.7 arcsec (radius, 90% confidence).
This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).
This circular was automatically generated, and is an official product of the
Swift-XRT team.
GCN Circular 21106
Subject
GRB 170519A: Swift detection of a burst with an optical counterpart
Date
2017-05-19T05:24:17Z (9 years ago)
From
Kim Page at U.of Leicester <klp5@leicester.ac.uk>
T. N. Ukwatta (LANL), H. A. Krimm (NSF/USRA), A. Y. Lien (GSFC/UMBC)
and K. L. Page (U Leicester) report on behalf of the Swift Team:
At 05:10:02 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 170519A (trigger=753445). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 163.450, +25.378 which is
RA(J2000) = 10h 53m 48s
Dec(J2000) = +25d 22' 41"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve showed a single-peaked
structure with a duration of about 10 sec. The peak count rate
was ~1500 counts/sec (15-350 keV), at ~3 sec after the trigger.
The XRT began observing the field at 05:11:23.2 UT, 80.4 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 163.42823, 25.37377 which
is equivalent to:
RA(J2000) = 10h 53m 42.78s
Dec(J2000) = +25d 22' 25.6"
with an uncertainty of 4.8 arcseconds (radius, 90% containment). This
location is 72 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 3.58e-09 erg cm^-2 s^-1 (0.2-10
keV).
UVOT took a finding chart exposure of 150 seconds with the White filter
starting 91 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
RA(J2000) = 10:53:42.46 = 163.42693
DEC(J2000) = +25:22:27.4 = 25.37429
with a 90%-confidence error radius of about 0.75 arc sec. This position is 1.4
arc sec. from the center of the XRT error circle. The estimated magnitude is
17.07 with a 1-sigma error of about 0.14. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.03.
Burst Advocate for this burst is T. N. Ukwatta (tilan.ukwatta AT gmail.com).
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.)