GRB 191019A
GCN Circular 26098
Subject
GRB 191019A: Zadko Telescope optical observations
Date
2019-10-30T05:46:27Z (7 years ago)
From
Bruce Gendre at UVI <bruce.gendre@gmail.com>
B. Gendre (OzGrav-UWA), H. Crisp (OzGrav-UWA), D. Coward (OzGrav-UWA),
J. Zadko (Claire Energy), J. A. Moore (OzGrav-UWA), A. Burrell
(OzGrav-UWA), A. Klotz (IRAP-OMP-UPS), P. Thierry (Auragne Observatory),
E.J. Howell (OzGrav-UWA), A. Verveer (ASA), J. Kennewell (UWA, ASA)
report:
We observed GRB 191019A (Simpson et al., GCN 26031) with the Zadko
Telescope (Coward et al. 2017), starting at 2019 October the 19th at
15:20:23 UT (7 minutes 50 seconds after the trigger) under fair conditions.
The object reported by Reva et al. (GCN 26036) is clearly visible in our
images. However, we measure an R magnitude of 18.92 at the time reported
by the GCN. Observations stopped one hour twenty three minutes after the
burst, and during that time we do not see any variation on the light
curve, similar to other teams (Perley et al., GCN 26039; Fynbo et al.,
GCN 26041; and Zhu et al., GCN 26059). At that position, the USNO
catalog reports a source of magnitude R = 19.0, consistent with our
findings. We conclude that this object is not the afterglow of GRB
191019A, but the host galaxy, as reported by Perley et al. (GCN 26062).
The Zadko Telescope has been under refurbishment during the last year,
and is still in recommissioning mode. This message can be cited.
--
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GCN Circular 26062
Subject
GRB 191019A: NOT optical afterglow and host association confirmation
Date
2019-10-23T21:55:37Z (7 years ago)
From
Daniel Perley at Liverpool JMU <d.a.perley@ljmu.ac.uk>
D. A. Perley (LJMU), D. B. Malesani (DTU Space), A. J. Levan (Radboud
Univ.), J. P. U. Fynbo (DAWN/NBI), and A. A. Djupvik (NOT) report on
behalf of a larger collaboration:
We obtained additional observations of the optical counterpart (Reva et
al., GCN 26036; LaPorte & Simpson, GCN 26053; Zhu et al., GCN 26059) of
GRB 191019A (Simpson et al., GCN 26031), using the Nordic Optical
Telescope (NOT) equipped with the ALFOSC camera. A total of 25 minutes
exposure was secured with mid time Oct 22.875 UT (77.8 hr after the GRB).
The archival object consistent with the XRT error circle is well
detected, with a magnitude of i = 18.71 +/- 0.02 AB, consistent with the
Pan-STARRS tabulated value of i = 18.71 +/- 0.01 and slightly fainter
than our earlier observation (Perley et al., GCN 26039), for which the
mid time was 4.60 hr after the GRB.
Digital image subtraction was carried out with ISIS (Alard 2000, A&AS,
144, 363) between the two epochs. A clear point-like residual is
detected, for which we measure a magnitude i = 21.78 +/- 0.05 AB
(assuming no residual flux in our second epoch). Its position calibrated
against the Gaia catalog is:
RA(J2000) = 22:40:05.89
Dec(J2000) = -17:19:42.6
(+/- 0.3")
An image showing the subtraction result is available here:
http://outer.space.dtu.dk/~dmales/GRB/191019A/subtraction.jpg
The transient location is 0.07" east of the galaxy nucleus,
strengthening the case for a physical association between the two
objects. The offset is within the margin of error, although the NOT
spectroscopy (Fynbo et al., GCN 26041) does not suggest that the source
is an AGN.
Our observations thus confirm the presence of a transient optical source
at a position consistent with the X-ray afterglow, located to within the
errors on top of the nucleus of the candidate host. The lack of any
non-obscured star formation makes this system unique among long-duration
GRBs.
We encourage observations of this puzzling source at all wavelengths.
DisclaimerNone
GCN Circular 26059
Subject
GRB 191019A: Nanshan-0.6m optical observations
Date
2019-10-22T13:58:53Z (7 years ago)
From
Dong Xu at NAOC/CAS <dxu@nao.cas.cn>
Z.P. Zhu, B.Y. Yu, D. Xu (NAOC), X. Gao (Urumqi No.1 Senior High School)
report:
We observed the field of GRB 191019A (Simpson et al., GCN 26031) using
the 0.6m NEXT telescope located at Nanshan, Xinjiang, China.
Observations started at 15:34:01 UT (i.e., 21.5 min after the BAT
trigger) and ended at 18:22:51 UT on 2019-10-19, and a series of 60 s,
200 s, 300 s Sloan r-band frames were obtain in a high airmass.
A source is detected in our images at the XRT position (Osborne et al.,
GCN 26043), which is already present in Pan-STARRS with m(r) = 19.12 +/-
0.01. The source had m(r) = 18.96 +/- 0.10 at the beginning and decayed
to m(r) = 19.19 +/- 0.10 in about an hour. Because the flux difference
is small and observations were carried out in high airmass, it's not
clear if there is a GRB afterglow contribution. Our measurements are in
agreement with that by NOT (Perley et al., GCN 26039; Fynbo et al., GCN
26041) and GROND (Guelbenzu et al., GCN 26042).
GCN Circular 26053
Subject
GRB 191019A: Swift/UVOT Detection
Date
2019-10-21T22:05:22Z (7 years ago)
From
Sam LaPorte at PSU <sjl5346@psu.edu>
GRB 191019A: Swift/UVOT Detection
S. J. LaPorte (PSU) and K. K. Simpson (PSU)
report on behalf of the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 191019A
3294 s after the BAT trigger (Simpson et al., GCN Circ. 26031).
A fading source consistent with the XRT position
(Evans et al. GCN Circ. 26034)
is detected in the initial UVOT exposures.
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
b 4541 4741 196
19.55+-0.30
uvm2 5361 5561 196 >19.20
u 4336 4536 196 >19.43
v 5156 5356 196 >18.75
uvw1 4131 4331 196 >19.13
uvw2 4952 5151 196 >19.28
white 4746 4946 196 19.66+-0.20
white 27982 28668 668 20.27+-0.18
The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.04 in the direction of the burst
(Schlegel et al. 1998). Additionally, these magnitudes likely include a
contribution
from the probable host-galaxy, as reported by TSHAO (Reva et al., GCN Circ.
26036),
NOT (Fynbo et al., GCN Circ. 26041), and GROND (Guelbenzu et al. GCN Circ.
26042).
GCN Circular 26048
Subject
GRB 191019A: Swift-XRT updated analysis
Date
2019-10-20T20:12:27Z (7 years ago)
From
Boris Sbarufatti at PSU <bxs60@psu.edu>
B. Sbarufatti (PSU), P.A. Evans (U. Leicester), J.P. Osborne (U. Leicester)
and K.K. Simpson (PSU) report on behalf of the Swift-XRT team:
We have analyzed 8.5 ks of XRT data for GRB 191019a (Simpson et al. GCN Circ. 26031), from 3.3 ks to 32.4 ks after the BAT trigger.
The data are entirely in Photon Counting (PC) mode. The enhanced XRT position for this burst was given by Osborne et al. (GCN Circ. 26043).
The light curve can be modeled with a power-law decay with a decay index of alpha=1.0 (+/-0.2).
A spectrum formed from the PC mode data can be fitted with an absorbed power-law with a photon spectral index of 2.0 (+/- 0.40). The
best-fitting absorption column is consistent with the Galactic value of 3.3 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 3.4 x 10^-11 (4.1 x 10^-11) erg cm^-2 count^-1.
A summary of the PC-mode spectrum is thus:
Total intrinsic column: < 2.23 x 10^21 cm^-2
Galactic foreground: 3.3 x 10^20 cm^-2
Photon index: 2.0 (+/- 0.4)
If the light curve continues to decay with a power-law decay index of 1.0, the count rate at T+48 hours will be 1.2 x 10^-3 count s^-1, corresponding to an observed (unabsorbed) 0.3-10 keV flux of 4.1 x 10^-14 (4.9 x 10^-14) erg cm^-2 s^-1.
The results of the XRT-team automatic analysis are available at http://www.swift.ac.uk/xrt_products/00930285/.
This circular is an official product of the Swift-XRT team.
GCN Circular 26046
Subject
GRB 191019A: Swift-BAT refined analysis
Date
2019-10-20T16:54:32Z (7 years ago)
From
Amy Lien at GSFC <amy.y.lien@nasa.gov>
H. A. Krimm (NSF), S. D. Barthelmy (GSFC),
J. R. Cummings (CPI), S. Laha (GSFC/UMBC),
A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (AGU),
K. K. Simpson (PSU), M. Stamatikos (OSU),
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 191019A (trigger #930285)
(Simpson et al., GCN Circ. 26031). The BAT ground-calculated position is
RA, Dec = 340.035, -17.340 deg which is
RA(J2000) = 22h 40m 08.3s
Dec(J2000) = -17d 20' 23.9"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 46%.
The mask-weighted light curve shows a complex structure with many
overlapping
pulses that starts at ~T0 and ends at ~T+90 s. The burst went out of the
BAT FOV at ~T+400 s. T90 (15-350 keV) is 64.35 +- 4.45 sec (estimated error
including systematics).
The time-averaged spectrum from T-0.83 to T+84.28 sec is best fit by a
simple
power-law model. The power law index of the time-averaged spectrum is
2.25 +- 0.05. The fluence in the 15-150 keV band is 1.0 +- 0.03 x 10^-5
erg/cm2.
The 1-sec peak photon flux measured from T-0.14 sec in the 15-150 keV band
is 5.7 +- 0.4 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/930285/BA/
GCN Circular 26045
Subject
GRB 191019A: Swift-XRT refined Analysis
Date
2019-10-20T15:32:57Z (7 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
A. D'Ai (INAF-IASFPA), A. Melandri (INAF-OAB), P. D'Avanzo (INAF-OAB),
J. D. Gropp (PSU), A. Tohuvavohu (U. Toronto), J.A. Kennea (PSU), P.A.
Evans (U. Leicester), J.P. Osborne (U. Leicester), K.L. Page (U.
Leicester) and K.K. Simpson report on behalf of the Swift-XRT team:
We have analysed 3.9 ks of XRT data for GRB 191019A (Simpson et al. GCN
Circ. 26031), from 3.3 ks to 17.2 ks after the BAT trigger. The data
are entirely in Photon Counting (PC) mode. The enhanced XRT position
for this burst was given by Osborne et al. (GCN Circ. 26043). The
results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00930285.
This circular is an official product of the Swift-XRT team.
GCN Circular 26043
Subject
GRB 191019A: Enhanced Swift-XRT position
Date
2019-10-20T15:06:57Z (7 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
J.P. Osborne, A.P. Beardmore, P.A. Evans and M.R. Goad (U. Leicester)
report on behalf of the Swift-XRT team.
Using 616 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 191019A, 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 = 340.02470, -17.32803 which is equivalent
to:
RA (J2000): 22h 40m 5.93s
Dec (J2000): -17d 19' 40.9"
with an uncertainty of 2.4 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 26042
Subject
GRB 191019A: GROND observations
Date
2019-10-20T13:43:49Z (7 years ago)
From
Ana Nicuesa at TLS Tautenburg <ana@tls-tautenburg.de>
A. Nicuesa Guelbenzu (TLS Tautenburg) reports:
GROND (Greiner et al. 2008, PASP 120, 405) performed a first visit of
the field of GRB 191019A (Swift trigger 930285; Simpson et al., GCN 26031)
at 01:35 UT on 2019-10-20, about 10.3 hours after the burst.
Observations were performed at an airmass of 1.02 and a seeing of 2.0
arcsec. Second-epoch observations started at 05:10 UT on the same night
(airmass 1.75, seeing 1.7 arcsec).
The potential afterglow plus host-galaxy complex is clearly detected.
Between the 1st and the 2nd-epoch observations there is no evidence for
fading in any band (g'r'i'z' as well as in JHKs). The GROND
r'(AB = 19.14 +/- 0.01) and i' (AB = 18.73 +/- 0.01) magnitudes are in
agreement with the NOT observations and the Pan-STARRS catalog (Perley et
al., GCN 26039; Fynbo et al., GCN 26041).
I acknowledge the excellent support from Sam Kim on La Silla in acquiring
these observations
GCN Circular 26041
Subject
GRB 191019A: NOT optical spectroscopy of candidate counterpart
Date
2019-10-19T23:47:11Z (7 years ago)
From
Daniele B Malesani at DTU Space <malesani@space.dtu.dk>
J. P. U. Fynbo (DAWN/NBI), D. A. Perley (LJMU), A. de Ugarte Postigo
(HETH/IAA-CSIC; DARK/NBI), D. B. Malesani (DTU Space), N. E. Jannsen
(NOT), report on behalf of a larger collaboration:
Spectroscopy was secured of the optical counterpart (Reva et al., GCN
26036; Perley et al., GCN 26039) of GRB 191019A (Simpson et al., GCN
26031), using the ALFOSC instrument mounted on the Nordic Optical
Telescope (NOT). Observations started on 2019 Oct 19.873 UT (5.74 hr
after the GRB), for a total of 2x1800 s exposure.
Our spectrum, secured with grism #4, covers the approximate wavelength
range 3500-9400 AA. The continuum is well detected. No prominent
emission lines are visible. However, several absorption features can be
identified, including Ca H & K, Na I D, Hdelta, Hgamma, Hbeta, G band,
all at a common redshift z = 0.248. The 4000 AA break is also present.
The spectrum is typical of an old stellar population, and is unlike that
of long-duration GRB host galaxies. The association of this object with
GRB 191019A is therefore unclear.
Using the formula by Bloom et al. (2002, AJ, 123, 1111), the chance
association probability for a source with magnitude r = 19.14 AB (from
the Pan-STARRS catalog) and an error circle radius of 3.1" (Evans et
al., GCN 26034) is approximately 3*10^-3.
GCN Circular 26039
Subject
GRB 191019A: NOT optical observations
Date
2019-10-19T21:30:22Z (7 years ago)
From
Daniel Perley at Liverpool JMU <d.a.perley@ljmu.ac.uk>
D. A. Perley (LJMU), D. B. Malesani (DTU Space), A. de Ugarte Postigo
(HETH, IAA/CSIC; DARK/NBI), D. Xu (NAO/CAS), J. P. U. Fynbo (DAWN/NBI),
K. E. Heintz (Univ. Iceland), and N. E. Jannsen (NOT) report on behalf
of a larger collaboration:
We observed the field of GRB 191019A (Simpson et al., GCN 26031) with
the Nordic Optical Telescope (NOT) equipped with the ALFOSC imaging
camera. Observations started on 2019 Oct 19.822 UT (4.52 hr after the
trigger).
In a single 120 s image taken in the SDSS i band, we detect the object
mentioned by Reva et al. (GCN 26036), which is also visible in the
Pan-STARRS archival images and is consistent with the X-ray position
(Evans et al., GCN 26034). The target is clearly extended (FWHM 1.4"
with a seeing of 1.1").
The object centroid has coordinates (J2000, calibrated against the Gaia
catalog):
RA = 22:40:05.89
Dec = -17:19:42.7
Measuring its magnitude over an aperture of 1.7" radius, we obtain i =
18.66 +/- 0.01 AB (statistical error), compared to i = 18.71 +/- 0.01
from the Pan-STARRS catalog (Chambers et al. 2015, arXiv:1612.05560),
confirmed by our own measurement on the i-band Pan-STARRS image. The
small flux difference may be due to calibration, color effects, or
variable aperture correction, so we do not claim any afterglow
detection. A conservative limit on the afterglow magnitude at the time
of our observation would be i > 21.
We note the elevated column density measured in a preliminary analysis
of the X-ray spectra (Evans et al., GCN 26034). This may suggest a
dust-obscured event.
DisclaimerNone
GCN Circular 26036
Subject
GRB 191019A: TSHAO optical observations, probable afterglow and host galaxy
Date
2019-10-19T18:55:20Z (7 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
I. Reva (FAPHI), A. Pozanenko (IKI), M. Krugov (FAPHI), S. Belkin (IKI),
E. Mazaeva (IKI), A. Volnova (IKI) report on behalf of IKI-GRB-FuN:
We observed the field of GRB 191019A (Simpson et al. GCN 26031) with
Zeiss-1000 1-m telescope of Tien Shan Astronomical Observatory starting
on Oct. 19 (UT) 15:26:32, i.e. 14 minutes after GRB trigger. Within
XRT error circle (Evans et al., GCN 26034) we found only one source
which is presented in catalogs. Preliminary photometry of the source
is following.
Date UT start t-T0 Filter Exp. OT Err.
(mid, days) (s)
2019-10-19 15:26:32 0.013877 R 720 18.37 0.03
The photometry is based nearby USNO-B1.0 stars.
The brightness of the catalogued source is R2(USNO-B1.0 340.024514480) =
19.36 and r'(Pan-STARRS 0726-1153339) = 19.30. The source is probably a
host galaxy of GRB 191019A and we suggest the afterglow of the source
on a top of the host galaxy.
GCN Circular 26034
Subject
GRB 191019A: Swift-XRT observations
Date
2019-10-19T16:22:58Z (7 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
P.A. Evans (U. Leicester), J.P. Osborne (U. Leicester), D.N. Burrows
(PSU), J.A. Kennea (PSU), S. Campana (INAF-OAB) and G. Cusumano
(INAF-IASF PA) report on behalf of the Swift-XRT team:
The XRT began observing the field of GRB 191019A at 16:06:04.5 UT,
3210.9 seconds after the BAT trigger. Using promptly downlinked data we
find an uncatalogued X-ray source with an enhanced position: RA, Dec
340.0244, -17.3286 which is equivalent to:
RA(J2000) = 22h 40m 05.86s
Dec(J2000) = -17d 19' 42.9"
with an uncertainty of 3.1 arcseconds (radius, 90% containment). This
location is 49 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.
A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (3.28 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 3.5
(+2.44/-3.29) x 10^22 cm^-2 (90% confidence).
GCN Circular 26032
Subject
GRB 191019A: MASTER optical observation
Date
2019-10-19T15:46:07Z (7 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>
V. Lipunov, N.Tiurina, E. Gorbovskoy, V.Kornilov, F.Balakin,P.Balanutsa,A.Kuznetsov, V.Vladimirov, D. Vlasenko, I.Gorbunov,
D.Zimnukhov,V.Senik, T.Pogrosheva, K.Pozdnyakov,A.Chasovnikov, V.Topolev, D.Kuvshinov(Lomonosov Moscow State University, SAI,Physics Department),
R. Podesta, C.Lopez, F. Podesta, C.Francile(Observatorio Astronomico FelixAguilar OAFA),
H.Levato(Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE),
R. Rebolo, M. Serra(The Instituto de Astrofisica de Canarias),
D. Buckley(South African Astronomical Observatory),
O.A. Gres, N.M. Budnev, O.Ershova(Irkutsk State University, API),
A. Tlatov, D. Dormidontov(Kislovodsk Solar Station of the Pulkovo Observatory),
V. Yurkov, A. Gabovich, Yu. Sergienko(Blagoveschensk Educational StateUniversity)
MASTER-Kislovodsk robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, v.2010, 30L)
started Swift GRB191019A (Simpson et al. GCN26031 , BAT, RA,Dec= RA(J2000) = 22h 40m 09s, -17d 19' 59")
observations at 2019-10-19 15:13:14Ut with exp. 10s, but sun altitude=-10.
The first image with mlim=15.0 made at 2019-10-19 15:23:59UT.
Real time updated cover map and possibly OT, that can be discovered,
will be available here:
https://master.sai.msu.ru/site/master2/event.php?id=1171578
The observation and reduction will be continued.
The message may be cited.
GCN Circular 26031
Subject
GRB 191019A: Swift detection of a burst
Date
2019-10-19T15:21:47Z (7 years ago)
From
David Palmer at LANL <palmer@lanl.gov>
K. K. Simpson (PSU), S. D. Barthelmy (GSFC), J.D. Gropp (PSU),
A. Y. Lien (GSFC/UMBC), K. L. Page (U Leicester), D. M. Palmer (LANL)
and A. Tohuvavohu (Toronto) report on behalf of the Neil Gehrels Swift
Observatory Team:
At 15:12:33 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 191019A (trigger=930285). Swift did not slew due to an observing
constraint. The BAT on-board calculated location is
RA, Dec 340.038, -17.333, which is
RA(J2000) = 22h 40m 09s
Dec(J2000) = -17d 19' 59"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve shows multiple peaks in a FRED
envelope with a total duration of about 80 sec. The peak count rate
was ~4500 counts/sec (15-350 keV), at ~4 sec after the trigger.
Due to an observing constraint, Swift will not slew until T0+51.6
minutes. There will be no XRT or UVOT data until this time.
Burst Advocate for this burst is K. K. Simpson (kira.simpson1984 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/)