GRB 190613B
GCN Circular 25081
Subject
GRB 190613B: FRAM-Auger afterglow detection
Date
2019-07-17T11:48:38Z (7 years ago)
From
Martin Jelinek at Astro.Inst-AVCR,Ondrejov <martin.jelinek@asu.cas.cz>
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 30cm robotic telescope FRAM-Auger in Malarg��e
(Argentina) reacted robotically to the Swift/BAT and
Fermi/GBM alert of GRB190613B (D'Ai et al., GCNC 24807;
Bissaldi et al., GCNC 24814), starting with a series of
20s unfiltered images at 10:47:33.45 UT, i.e. 31.4s
post trigger.
We detect the source reported by Marshall et al. (GCN
24817), Zheng & Filipenko (GCN 24818), Hu et al. (GCNC
24826), de Ugarte Postigo (GCNC 24825) and other teams
at a 5 x 20s combined image taken between 79s and 202s
after the initial trigger. The brightness of the object
was r'(AB) = 15.6 +- 0.2, as calibrated against APASS
Catalogue.
GCN Circular 24848
Subject
GRB 190613B: JCMT SCUBA-2 sub-mm observations
Date
2019-06-19T01:14:23Z (7 years ago)
From
Ian Smith at Rice U <iansmith@rice.edu>
I.A. Smith (Rice U.), D.A. Perley (LJMU), and N.R. Tanvir
(U. of Leicester) report:
We observed the location of GRB 190613B (D'Ai et al., GCN
Circ. 24807) using the SCUBA-2 sub-millimeter continuum camera
on the James Clerk Maxwell Telescope. The observation started
at 11:40 UT on 2019-06-13, corresponding to 53 minutes after
the burst trigger. Exposures totaling 1.0 hours were made in
very good weather conditions. No source was detected, with
the RMS background noise being 1.8 mJy/beam at 850 microns and
21.3 mJy/beam at 450 microns.
We thank Kevin Silva, Jan Wouterloot, Koji Sugitani, and the
JCMT staff for the prompt support of these observations that
were taken under project M19AP044.
GCN Circular 24846
Subject
GRB 190613B: AstroSat CZTI detection
Date
2019-06-18T05:55:40Z (7 years ago)
From
Prachee Ghumatkar at IUCAA/AstroSat <prachee@iucaa.in>
P. Ghumatkar, V. Sharma, D. Bhattacharya, T. Khanam and A. Vibhute (IUCAA), V. Bhalerao (IIT-B), A. R. Rao (TIFR) and S. Vadawale (PRL) report on behalf of the AstroSat CZTI collaboration:
Analysis of AstroSat CZTI data showed the detection of a long GRB 190613B, which was also detected by Fermi GBM (GCN #24806), Swift detection (D'Ai A. et al., GCN #24807), BALROG (Burgess J. et al., GCN #24808), Swift-XRT (Beardmore A.P. et al., GCN #24812), Swift-BAT (Ukwatta T.N. et al., GCN #24820), Insight-HXMT/HE (Luo Q. et al., GCN #24829) and Konus-Wind (Svinkin D. et al., GCN #24844).
The source was clearly detected in the 40-200 keV energy range. The light curve shows multiple pulses of emission with the strongest peak at 10:47:02.5 UT. The measured peak count rate associated with the burst is 439 cts/s above the background in the combined data of four quadrants, with a total of 1298 cts. The local mean background count rate was 654 cts/s. Using cumulative rates, we measure a T90 of 11.75 s.
It was also clearly detected in the CsI anticoincidence (Veto) detector in the 100-500 keV energy range.
CZTI GRB detections are reported regularly on the payload site at http://astrosat.iucaa.in/czti/?q=grb. CZTI is built by a TIFR-led consortium of institutes across India, including VSSC, ISAC, IUCAA, SAC and PRL. The Indian Space Research Organisation funded, managed and facilitated the project.
GCN Circular 24844
Subject
Konus-Wind observation of GRB 190613B
Date
2019-06-17T18:30:10Z (7 years ago)
From
Dmitry Svinkin at Ioffe Institute <svinkin@mail.ioffe.ru>
D. Svinkin, S. Golenetskii, R. Aptekar, D. Frederiks,
M. Ulanov, A. Tsvetkova, A. Lysenko, A. Kozlova, and T. Cline
on behalf of the Konus-Wind team, report:
The long-duration GRB 190613B
(Swift-BAT detection: D'Ai et al., GCN Circ. 24807;
Fermi-GBM observation: Bissaldi et al., GCN Circ. 24814;
Insight-HXMT/HE detection: Luo et al., GCN Circ. 24829)
triggered Konus-Wind at T0=38825.774 s UT (10:47:05.774).
The burst light curve shows a single pulse
which starts at ~T0-2.6 s and has a total duration of ~4 s.
The emission is seen up to ~3 MeV.
As observed by Konus-Wind, the burst
had a fluence of 3.48(-0.79,+1.29)x10^-6 erg/cm2,
and a 64-ms peak flux, measured from T0+0.544 s,
of 2.65(-1.10,+1.54)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).
The time-averaged spectrum of the burst
(measured from T0 to T0+8.448 s)
is best fit in the 20 keV - 4 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with alpha = -0.93(-0.53,+0.83)
and Ep = 277(-107,+331) keV (chi2 = 82/72 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -1.8
(chi2 = 82/71 dof).
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB190613_T38825/
All the quoted errors are at the 90% confidence level.
All the quoted values are preliminary.
GCN Circular 24841
Subject
GRB 190613B: Kitab observatory optical upper limit
Date
2019-06-16T14:10:05Z (7 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
S. Belkin (IKI), A. Novichonok (KIAM), A. Zhornichenko (KIAM), A. Pozanenko
(IKI), E. Mazaeva (IKI), A. Volnova (IKI), I. Molotov (KIAM), Sh.
Ehgamberdiev (UBAI) report on behalf of larger GRB IKI FuN collaboration:
We observed the field of the GRB 190613B (D'Aiet al., GCN 24807) with
RC-36 0.36-m telescope of Kitab Observatory starting on June 13 (UT)
22:26:32 in Clear filter. We do not detect the optical afterglow
(D'Aiet al., GCN 24807; Marshall al., GCN 24817; Zheng al., GCN 24818;
Ugarte Postigo al., GCN 24825; Hu al., GCN 24826).
Preliminary photometry of the field is following.
Date UT start t-T0 Filter Exp. OT Err. UL(3sigma)
(mid, days) (s)
2019-06-13 20:55:3 0.43001 CR 3600 n/d n/d 20.0
The photometry is based on the nearby USNO-B1 (R2) stars.
USNO-B1.0_id R2
0853-0556521 16.14
0853-0556781 16.31
GCN Circular 24836
Subject
GRB 190613B: SEDM Observations
Date
2019-06-15T01:26:59Z (7 years ago)
From
Virginia Cunningham at U of MD <vcunning@astro.umd.edu>
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 190613B (D'Ai et al. GCN 24807)
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 11:00:28 UTC (11.79
minutes after the burst trigger time). We performed an 1800 s exposure over
the wavelength range 3800-9200 A. We tentatively identify an absorption
feature at ~ 5385 A that is consistent with the Mg II 2796,2803 doublet at
z = 0.92. However, due to the relatively low significance of the feature and
the lack of corroborating lines, we cannot confirm this redshift currently.
The continuum emission is well-fit by a power law spectrum with index alpha = 1.8
(f_nu ~ nu^-alpha).
[GCN OPS NOTE(07sep19): Per author's request, In the last sentence,
the "alpha = 0.09" was changed to "alpha = 1.8".]
GCN Circular 24832
Subject
GRB 190613B: Optical observation from Asiago Schmidt
Date
2019-06-14T15:13:45Z (7 years ago)
From
Sheng Yang at OAPD, INAF <saberyoung@gmail.com>
S. Yang, L. Tomasella, E. Cappellaro (OAPD, INAF) and N. Khetan (GSSI, L'Aquila)
Using the 0.92m Asiago Schmidt telescope, we observed the field of GRB 190613B 11.954 h after the burst (D���Ai et al. GCN 24807) in g, r and i.
We detected a source consistent with the optical and X-ray afterglow (Burgess et al. GCN 24808, Beardmore et al. GCN 24812, Bissaldi et al. GCN 24814, Marshall et al. GCN 24817, Zheng & Filippenko GCN 24818, Ukwatta et al. GCN 24820, Page et al. GCN 24823) in g band images while we could only set upper limits in the other bands.
The measured magnitude and 2.5-sigma upper limits are listed below:
Filter T_start T_stop JD_avg Exp(s) Mag
g 2019-06-13T22:44:17 2019-06-13T23:02:00 58647.95239 180*5 21.40 +/- 0.30
r 2019-06-13T23:02:14 2019-06-13T23:20:00 58647.96488 180*5 > 20.1
i 2019-06-13T23:23:32 2019-06-13T23:34:38 58647.97735 180*5 > 20.4
GCN Circular 24831
Subject
GRB 190613B: GROND Detection of the Optical/NIR Afterglow
Date
2019-06-14T14:41:35Z (7 years ago)
From
Patricia Schady at Swift <p.schady@bath.ac.uk>
P. Schady (Uni. Bath) and J. Bolmer (MPE Garching) report:
We observed the field of GRB 190613B (Fermi trigger 582115625.049376/190613449; GCN #24806, Swift trigger 908329; D'Ai et al., GCN #24807) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120, 405) mounted at the 2.2 m MPG telescope at ESO La Silla Observatory (Chile).
Observations started at 09:18 UT on 14 June 2019, 22.4 hrs after the GRB trigger. They were performed at an average seeing of 1.4" and at an average airmass of 1.2.
We detect a single point source in our g'r'i'z'JH images consistent with the reported GRB optical and X-ray afterglow (Beardmore et al., GCN #24812, Marshall et al., GCN #24817). Based on a total 22 min exposure in g'r'i'z' and 22 min in JHK, we estimate the following preliminary magnitudes (all in Vega system):
g' = 22.79 +/- 0.05 mag
r' = 22.05 +/- 0.04 mag
i' = 21.56 +/- 0.05 mag
z' = 21.15 +/- 0.07 mag
J = 20.5 +/- 0.1 mag
H = 20.2 +/- 0.2 mag
K > 19.8 mag
Given magnitudes are calibrated against PanStarrs as well as 2MASS field stars and are not corrected for the expected Galactic foreground extinction corresponding to a reddening of E_(B-V)=0.06 mag in the direction of the burst (Schlafly & Finkbeiner 2011).
We thank the observer astronomer at the MPG 2.2m in La Silla for their help in obtaining these data.
GCN Circular 24829
Subject
GRB 190613B: Insight-HXMT/HE detection
Date
2019-06-14T14:23:15Z (7 years ago)
From
Qi Luo at IHEP <luoqi@ihep.ac.cn>
Q. Luo, S. Xiao, C. Cai, Q. B. Yi, C. K. Li,
X. B. Li, G. Li, J. Y. Liao, S. L. Xiong,
C. Z. Liu, X. F. Li, Z. W. Li, Z. Chang, X. F. Lu,
A. M. Zhang, Y. F. Zhang, C. L. Zou (IHEP), Y. J. Jin,
Z. Zhang (THU), T. P. Li (IHEP/THU), F. J. Lu, L. M. Song,
M. Wu, Y. P. Xu, S. N. Zhang (IHEP),
report on behalf of the Insight-HXMT team:
At 2019-06-13T10:47:00.00 (T0), Insight-HXMT/HE detected
GRB 190613B (trigger ID: HEB190613449) in a routine search of the data,
which was also triggered by Fermi/GBM (GCN #24806) and Swift/BAT
(D'Ai et al. 2019, GCN #24807).
The Insight-HXMT/HE light curve mainly consists of two
pulses with a duration (T90) of 3.59 s measured from T0-0.56 s.
The 1-ms peak rate, measured from T0+2.09 s, is 2847 cnts/sec.
The total counts from this burst is 6013 counts.
URL_LC: http://www.hxmt.org/images/GRB/HEB190613449_lc.jpg
All measurements above are made with the CsI detectors operating in the
regular mode with the energy range of about 80-800 keV (deposited energy).
Only gamma-rays with energy greater than about 200 keV can penetrate
the spacecraft and leave signals in the CsI detectors installed inside
of the telescope.
Insight-HXMT is the first Chinese space X-ray telescope, which was
funded jointly by the China National Space Administration (CNSA) and
the Chinese Academy of Sciences (CAS).
More information about it could be found at:
http://www.hxmt.org.
GCN Circular 24826
Subject
GRB 190613B: BOOTES-5/JGT early optical observations
Date
2019-06-14T05:04:33Z (7 years ago)
From
Alberto J. Castro-Tirado at IAA-CSIC <ajct@iaa.es>
Y.-D. Hu, X.-Y.Li, I. Carrasco, E. Fernandez-Garcia, A. Ayala and
A. J. Castro-Tirado (IAA-CSIC), D. Hiriart and W. H. Lee (UNAM),
S. Jeong and I. H. Park (SKKU) and M. D. Caballero-Garcia (ASU-CAS, CZ)
on behalf of a larger collaboration, report:
The 60cm BOOTES-5/JGT robotic telescope at Observatorio Astronomico
Nacional in San Pedro Martir (Mexico) automatically responded to the
Swift trigger of GRB 190613B (D'Ai et al., GCNC 24807). The first image
(1s exposure, clear-filter) was obtained at 10:48:04.16 UT (i.e. 62s
post-burst). We detect the optical afterglow at the position reported
by Swift (Beardmore et al. GCNC 24812, Marshall et al. GCNC 24817)
with R = 16.1. A sequence of images was obtained and the analysis is on
going. The magnitude is calibrated against the USNO-B1 catalog and is
not corrected for Galactic extinction in the direction of the GRB.
We thank the staff at Observatorio Astronomico Nacional in San Pedro
Martir for its excellent support.
GCN Circular 24825
Subject
GRB 190613B: Optical observations from NOT
Date
2019-06-14T04:57:01Z (7 years ago)
From
Antonio de Ugarte Postigo at IAA-CSIC <deugarte@iaa.es>
A. de Ugarte Postigo (HETH/IAA-CSIC, DARK/NBI), D.B. Malesani
(DTU Space), K.E. Heintz (U.Iceland), S. Moran (UTU, NOT) report
on behalf of a larger collaboration:
We observed the field of GRB 190613B (D���Ai et al. GCN 24807,
Burgess et al. GCN 24808, Beardmore et al. GCN 24812, Bissaldi et
al. GCN 24814, Marshall et al. GCN 24817, Zheng & Filippenko
GCN 24818, Ukwatta et al. GCN 24820, Page et al. GCN 24823)
using STANCAM, mounted on the 2.5m Nordic Optical Telescope, at
Roque de los Muchachos Observatory (La Palma, Spain). The
observations consisted of 3x300s imaging in R-band and 5x200s in
z-band. Observations started on 14 June at 2:50 UT (16.05 hr after
the burst). The optical counterpart is well detected in both bands at
an estimated R(Vega) = 21.8+/-0.2 mag, as compared to field stars
from the Nomad catalogue.
GCN Circular 24823
Subject
GRB 190613B: Swift-XRT refined Analysis
Date
2019-06-13T22:01:33Z (7 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester), P.A. Evans (U.
Leicester), A. Melandri (INAF-OAB), P. D'Avanzo (INAF-OAB), A.
Tohuvavohu (PSU), S. J. LaPorte (PSU), J.A. Kennea (PSU) and A. D'Ai
report on behalf of the Swift-XRT team:
We have analysed 6.3 ks of XRT data for GRB 190613B (D'Ai et al. GCN
Circ. 24807), from 103 s to 19.3 ks after the BAT trigger. The data
comprise 352 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The enhanced XRT position for this burst was
given by Beardmore et al. (GCN Circ. 24812).
The late-time light curve (from T0+5.3 ks) can be modelled with a
power-law decay with a decay index of alpha=0.52 (+/-0.11).
A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.93 (+/-0.05). The
best-fitting absorption column is 3.28 (+0.24, -0.23) x 10^21 cm^-2,
in excess of the Galactic value of 6.0 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 1.90 (+/-0.11) and a
best-fitting absorption column of 2.6 (+0.5, -0.4) x 10^21 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum is 3.8 x 10^-11 (5.2 x 10^-11) erg cm^-2
count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 2.6 (+0.5, -0.4) x 10^21 cm^-2
Galactic foreground: 6.0 x 10^20 cm^-2
Excess significance: 7.6 sigma
Photon index: 1.90 (+/-0.11)
If the light curve continues to decay with a power-law decay index of
0.52, the count rate at T+24 hours will be 0.091 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.5 x
10^-12 (4.8 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/00908329.
This circular is an official product of the Swift-XRT team.
GCN Circular 24820
Subject
GRB 190613B: Swift-BAT refined analysis
Date
2019-06-13T19:48:02Z (7 years ago)
From
Amy Lien at GSFC <amy.y.lien@nasa.gov>
T. N. Ukwatta (LANL), S. D. Barthelmy (GSFC),
J. R. Cummings (CPI), A. D'Ai (INAF-IASFPA),
H. A. Krimm (NSF), A. Y. Lien (GSFC/UMBC),
C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (AGU), M. Stamatikos (OSU),
(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 190613B (trigger #908329)
(D'Ai et al., GCN Circ. 24807). The BAT ground-calculated position is
RA, Dec = 305.434, -4.655 deg which is
RA(J2000) = 20h 21m 44.2s
Dec(J2000) = -04d 39' 17.0"
with an uncertainty of 1.9 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 18%.
The mask-weighted light curve shows a main pulse structure that starts
at ~T-3 s, peaks at ~T0, and ends at ~T+2 s. In addition, there are
some weak emissions that lasts until ~T+175 s. T90 (15-350 keV)
is 160.84 +- 16.83 sec (estimated error including systematics).
The time-averaged spectrum from T-2.85 to T+175.42 sec is best fit by a
simple
power-law model. The power law index of the time-averaged spectrum is
1.84 +- 0.24. The fluence in the 15-150 keV band is 2.3 +- 0.3 x 10^-6
erg/cm2.
The 1-sec peak photon flux measured from T+0.01 sec in the 15-150 keV band
is 5.7 +- 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/908329/BA/
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GCN Circular 24818
Subject
GRB 190613B: KAIT Optical Afterglow Confirmation
Date
2019-06-13T18:48:19Z (7 years ago)
From
Weikang Zheng at UC Berkeley <weikang@berkeley.edu>
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 190613B (D'Ai et al.
GCN 24807) starting at 2311s after the burst. Observations were
performed with a sequence in the clear (roughly R), V, and I filters,
and the exposure time was 20 s per image. We detected the optical
afterglow at the reported Swift/UVOT position (D'Ai et al., GCN 24798;
Marshall & D'Ai, GCN 24817) in clear band image. We estimate the
clear band magnitude to be ~19.3 at 2321s after the burst.
[GCN OPS NOTE(14jun19): The typo in Swift's name was corrected.]
GCN Circular 24817
Subject
GRB 190613B: Swift/UVOT Detection
Date
2019-06-13T17:39:39Z (7 years ago)
From
Frank Marshall at Swift/UVOT <marshall@milkyway.gsfc.nasa.gov>
F. E. Marshall (NASA/GSFC) and A. D'Ai (INAF-IASFPA)
report on behalf of the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 190613B
106 s after the BAT trigger (D'Ai et al., GCN Circ. 24807).
A source consistent with the enhanced XRT position
(Beardmore et al. GCN Circ. 24812)
is detected in the initial UVOT exposures.
The preliminary UVOT position is:
RA (J2000) = 20:21:43.66 = 305.43191 (deg.)
Dec (J2000) = -04:38:48.0 = -4.64666 (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 106 256 147 17.84 +/- 0.04
v 648 667 19 >18.0
b 574 594 19 >18.7
u 318 568 246 18.86 +/- 0.12
w1 697 717 19 >18.6
m2 672 692 19 >18.4
w2 624 643 19 >18.8
The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.07 in the direction of the burst
(Schlegel et al. 1998).
GCN Circular 24814
Subject
GRB 190613B: Fermi GBM observation
Date
2019-06-13T16:35:51Z (7 years ago)
From
Oliver J Roberts at USRA/NASA <oliver.roberts@nasa.gov>
E. Bissaldi (Politecnico & INFN Bari), O.J. Roberts (USRA/NASA) and C. Meegan (UAH)
report on behalf of the Fermi GBM Team:
"At 10:47:00.05 UT on 13 June 2019, the Fermi Gamma-Ray Burst Monitor (GBM)
triggered and located GRB 190613B (trigger 582115625 / 190613449),
which was also detected by the Swift/BAT (D'Ai et al. 2019, GCN 24807)
The GBM on-ground location is consistent with the Swift position.
The angle from the Fermi LAT boresight at the GBM trigger time using
the Swift-BAT position is 59 degrees.
The GBM light curve consists of single bright peak
with a duration (T90) of about 5 s (50-300 keV).
The time-averaged spectrum from T0-1 s to T0+4 s is
best fit by a power law function with an exponential
high-energy cutoff. The power law index is -0.96 +/- 0.05 and
the cutoff energy, parameterized as Epeak, is 334 +/- 35 keV.
The event fluence (10-1000 keV) in this time interval is
(4.4 +/- 0.2)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+2 s in the 10-1000 keV band
is 7.5 +/- 0.3 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 Circular 24812
Subject
GRB 190613B: Enhanced Swift-XRT position
Date
2019-06-13T14:19:40Z (7 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 2078 s of XRT Photon Counting mode data and 6 UVOT
images for GRB 190613B, 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 = 305.43206, -4.64686 which is equivalent
to:
RA (J2000): 20h 21m 43.69s
Dec (J2000): -04d 38' 48.7"
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 24808
Subject
GRB 190613B: BALROG localization (Fermi Trigger 582115625 / GRB 190613449)
Date
2019-06-13T11:13:48Z (7 years ago)
From
Jochen Greiner at MPE,Garching <jcg@mpe.mpg.de>
J. Burgess, F. Kunzweiler, B. Biltzinger, F. Berlato, & J. Greiner (all MPE Garching) report:
The public trigdat data of the Fermi Gamma-ray Burst Monitor (GBM) trigger
582115625 at 10:47:00 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) = 302.8+/-2.3 deg
Decl.(2000.0) = -8.2+/-2.7 deg
We estimate an additional systematic error of 1 deg.
Further details are available at:
https://grb.mpe.mpg.de/grb/GRB190613449/
The Healpix map can be downloaded from:
https://grb.mpe.mpg.de/grb/GRB190613449/healpix
The location parameters are available as JSON at:
https://grb.mpe.mpg.de/grb/GRB190613449/json
GCN Circular 24807
Subject
GRB 190613B: Swift detection of a burst with an optical counterpart
Date
2019-06-13T10:58:54Z (7 years ago)
From
David Palmer at LANL <palmer@lanl.gov>
A. D'Ai (INAF-IASFPA), E. Ambrosi (INAF-IASFPA), V. D'Elia (SSDC),
J.D. Gropp (PSU), N. J. Klingler (PSU), F. E. Marshall (NASA/GSFC),
D. M. Palmer (LANL) and M. H. Siegel (PSU) report on behalf of the
Neil Gehrels Swift Observatory Team:
At 10:47:02 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 190613B (trigger=908329). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 305.422, -4.664 which is
RA(J2000) = 20h 21m 41s
Dec(J2000) = -04d 39' 49"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve showed a complex
structure with a duration of about 15 sec. The peak count rate
was ~2500 counts/sec (15-350 keV), at ~1 sec after the trigger.
The XRT began observing the field at 10:48:39.5 UT, 97.5 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 305.4294, -4.6461 which is equivalent to:
RA(J2000) = 20h 21m 43.06s
Dec(J2000) = -04d 38' 46.0"
with an uncertainty of 4.8 arcseconds (radius, 90% containment). This
location is 69 arcseconds from the BAT onboard position, within the BAT
error circle. No event data are yet available to determine the column
density using X-ray spectroscopy.
The initial flux in the 2.5 s image was 4.90e-09 erg cm^-2 s^-1 (0.2-10
keV).
UVOT took a finding chart exposure of 150 seconds with the White filter
starting 105 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
RA(J2000) = 20:21:43.65 = 305.43189
DEC(J2000) = -04:38:47.9 = -4.64665
with a 90%-confidence error radius of about 0.62 arc sec. This position is 9.2
arc sec. from the center of the XRT error circle. The estimated magnitude is
17.76 with a 1-sigma error of about 0.14. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.07.
Burst Advocate for this burst is A. D'Ai (antonino.dai 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 Circular 24806
Subject
GRB 190613B: Fermi GBM Final Real-time Localization
Date
2019-06-13T10:58:04Z (7 years ago)
From
Fermi GBM Team at MSFC/Fermi-GBM <do_not_reply@GIOC.nsstc.nasa.gov>
The Fermi GBM team reports the detection of a likely LONG GRB
At 10:47:00 UT on 13 Jun 2019, the Fermi Gamma-ray Burst Monitor (GBM) triggered and located GRB 190613B (trigger 582115625.049376 / 190613449).
The on-ground calculated location, using the Fermi GBM trigger data, is RA = 305.4, Dec = -11.6 (J2000 degrees, equivalent to J2000 20h 21m, -11d 35'), with a statistical uncertainty of 3.2 degrees.
The angle from the Fermi LAT boresight is 60.0 degrees.
The skymap can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190613449/quicklook/glg_skymap_all_bn190613449.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/bn190613449/quicklook/glg_healpix_all_bn190613449.fit
The GBM light curve can be found here:
http://heasarc.gsfc.nasa.gov/FTP/fermi/data/gbm/triggers/2019/bn190613449/quicklook/glg_lc_medres34_bn190613449.gif