GRB 160119A
GCN Circular 18893
Subject
GRB 160119A: Swift detection of a burst
Date
2016-01-19T03:18:51Z (9 years ago)
From
David Palmer at LANL <palmer@lanl.gov>
F. E. Marshall (NASA/GSFC), D. N. Burrows (PSU), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), K. L. Page (U Leicester) and
D. M. Palmer (LANL) report on behalf of the Swift Team:
At 03:06:08 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 160119A (trigger=671014). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 211.893, +20.474 which is
RA(J2000) = 14h 07m 34s
Dec(J2000) = +20d 28' 28"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve shows low level variability
followed by a peak from T+120 to T+180. The peak count rate
was ~3000 counts/sec (15-350 keV), at ~142 sec after the trigger.
The XRT began observing the field at 03:08:48.0 UT, 159.8 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source located at RA, Dec 211.92111,
20.46161 which is equivalent to:
RA(J2000) = 14h 07m 41.07s
Dec(J2000) = +20d 27' 41.8"
with an uncertainty of 3.8 arcseconds (radius, 90% containment). This
location is 104 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.
A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (3.08 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 3.4
(+2.60/-1.22) x 10^21 cm^-2 (90% confidence).
The initial flux in the 0.1 s image was 2.75e-08 erg cm^-2 s^-1 (0.2-10
keV).
UVOT took a finding chart exposure of 150 seconds with the White filter
starting 168 seconds after the BAT trigger. No credible afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 19.6 mag.
The 8'x8' region for the list of sources generated on-board covers 100% of the
XRT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.03.
Burst Advocate for this burst is F. E. Marshall (marshall AT milkyway.gsfc.nasa.gov).
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.)
GCN Circular 18895
Subject
GRB 160119A: NOT and GTC afterglow candidate
Date
2016-01-19T05:06:13Z (9 years ago)
From
Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst <malesani@dark-cosmology.dk>
D. Malesani (DARK/NBI), A. de Ugarte Postigo (IAA-CSIC and DARK/NBI), D.
Xu (NAO/CAS), C.E. Martinez-Vazquez (IAC-ULL), A. Tejero (GTC), S. Geier
(GTC), C.C. Thoene (IAA-CSIC), P. Jakobsson (Univ. Iceland) report on
behalf of a larger collaboration.
We observed the field of GRB 160119A (Marshall et al., GCN 18893) with
the Nordic Optical Telescope (NOT) equipped with the ALFOSC camera.
Observations were carried out in the SDSS r and i bands, starting on
2015 Jan 19.151 UT (31 min after the GRB trigger).
We also observed the same field using the Gran Telescopio Canarias
(GTC), equipped with OSIRIS, starting on Jan 19.164 UT (50 min after the
GRB trigger), also in the r and i bands.
Compatible with the current XRT localization (3.6" radius, SPER-based;
http://www.swift.ac.uk/xrt_positions/), we detect a single, faint
optical source, at coordinates (J2000):
RA = 14:07:41.35
Dec = +20:27:40.1
with an uncertainty of <0.5".
Using nearby stars from the SDSS catalog, we measure from the NOT image
a magnitude r = 22.75 +- 0.15 (AB). This magnitude measurement is
affected by the extended glare of a nearby bright star, making
background subtraction less accurate than normal. This object is also
seen, faintly, in the short GTC images (30-60 s exposure).
The object seems marginally brighter than the SDSS detection limit.
However, despite ~20 min time difference between the NOT and GTC data,
we do not measure obvious variability between the two epochs, as it is
common among GRB afterglows close to the trigger. Further observations
will be necessary to ascertain the relation of this object with the GRB.
GCN Circular 18896
Subject
GRB 160119A: Enhanced Swift-XRT position
Date
2016-01-19T08:13:37Z (9 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
M.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester)
report on behalf of the Swift-XRT team.
Using 1310 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 160119A, 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 = 211.92183, +20.46094 which is equivalent
to:
RA (J2000): 14h 07m 41.24s
Dec (J2000): +20d 27' 39.4"
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 18897
Subject
GRB 160119A: Swift-XRT refined Analysis
Date
2016-01-19T11:13:02Z (9 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
A. Melandri (INAF-OAB), P. D'Avanzo (INAF-OAB), D.N. Burrows (PSU),
T.G.R. Roegiers (PSU), L.M. McCauley (PSU), J.P. Osborne (U.
Leicester), K.L. Page (U. Leicester), C. Pagani (U. Leicester), V.
D'Elia (ASDC) and F.E. Marshall report on behalf of the Swift-XRT team:
We have analysed 8.4 ks of XRT data for GRB 160119A (Marshall et al.
GCN Circ. 18893), from 149 s to 18.2 ks after the BAT trigger. The
data comprise 456 s in Windowed Timing (WT) mode (the first 9 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 Goad
et al. (GCN Circ. 18896).
The late-time light curve (from T0+4.9 ks) can be modelled with a
power-law decay with a decay index of alpha=0.59 (+/-0.11).
A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.86 (+/-0.05). The
best-fitting absorption column is 2.57 (+0.23, -0.22) x 10^21 cm^-2,
in excess of the Galactic value of 3.1 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 2.11 (+/-0.11) and a
best-fitting absorption column of 1.9 (+/-0.3) x 10^21 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum is 3.3 x 10^-11 (4.7 x 10^-11) erg cm^-2
count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 1.9 (+/-0.3) x 10^21 cm^-2
Galactic foreground: 3.1 x 10^20 cm^-2
Excess significance: 8.0 sigma
Photon index: 2.11 (+/-0.11)
If the light curve continues to decay with a power-law decay index of
0.59, the count rate at T+24 hours will be 0.056 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.8 x
10^-12 (2.6 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/00671014.
This circular is an official product of the Swift-XRT team.
GCN Circular 18899
Subject
GRB 160119A: Swift-BAT refined analysis
Date
2016-01-19T15:29:16Z (9 years ago)
From
Hans Krimm at NASA-GSFC <hans.a.krimm@nasa.gov>
M. Stamatikos (OSU), S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), A. Y. Lien (GSFC/UMBC),
C. B. Markwardt (GSFC), F. E. Marshall (NASA/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 160119A (trigger #671014)
(Marshall, et al., GCN Circ. 18893). The BAT ground-calculated position is
RA, Dec = 211.916, 20.453 deg which is
RA(J2000) = 14h 07m 39.8s
Dec(J2000) = +20d 27' 09.1"
with an uncertainty of 2.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 77%.
The mask-weighted light curve shows some low-level activity from about T+20 sec
to T+100 sec. This is followed by a single main peak starting at T+110 sec,
with a broad peak from T+140 to T+155 sec, and a slow decay out to T+200 sec.
T90 (15-350 keV) is 116 +- 14 sec (estimated error including systematics).
The time-averaged spectrum from T+32.62 to T+190.39 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
1.68 +- 0.05. The fluence in the 15-150 keV band is 7.1 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+146.06 sec in the 15-150 keV band
is 2.9 +- 0.2 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/671014/BA/
GCN Circular 18901
Subject
GRB 160119A: RATIR Optical and NIR Observations
Date
2016-01-19T16:20:11Z (9 years ago)
From
Antonino Cucchiara at NASA/GSFC <antonino.cucchiara@nasa.gov>
Antonino Cucchiara (GSFC/STScI),Nat Butler (ASU), Alan M. Watson (UNAM),
Alexander Kutyrev (GSFC),William H. Lee (UNAM), Michael G. Richer (UNAM),
Ori Fox (UCB), J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Eleonora
Troja (GSFC), Owen Littlejohns (ASU), Enrico Ramirez-Ruiz (UCSC), Jos��
A. de Diego (UNAM), Leonid Georgiev (UNAM), Jes��s Gonz��lez (UNAM),
Carlos Rom��n-Z����iga (UNAM), Neil Gehrels (GSFC), Harvey Moseley (GSFC),
John Capone (UMD), V. Zach Golkhou (ASU), and Vicki Toy (UMD) report:
We observed the field of GRB 160119A (Marshall, et al., GCN 18893) 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 2016/01 19.36 to 2016/01 19.54 UTC (5.61 to 9.76 hours after
the BAT trigger), obtaining a total of 3.20 hours exposure in the r, i, and z bands.
We identified the source reported by Malesani et al., GCN 18895.
In comparison with the SDSS DR9 and 2MASS catalogs, we obtain the
following detections and upper limits (3-sigma):
r 23.78 +/- 0.28
i 23.26 +/- 0.17
z > 20.78
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 M��rtir.
GCN Circular 18902
Subject
GRB 160119A: GROND optical/NIR afterglow observations
Date
2016-01-19T18:52:32Z (9 years ago)
From
Ting-Wan Chen at MPE <jchen@mpe.mpg.de>
T.-W. Chen, T. Kruehler, F. Knust, J. Greiner (all MPE Garching), and D. A. Kann (TLS Tautenburg) report on behalf of the GROND team:
We observed the field of GRB 160119A (Swift trigger 671014; Marshall et al., GCN #18893) 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 07:53 UT on 2016-01-19, about 4.8 hours after the GRB trigger.
Our images were performed at an average seeing of 1.8" and at an average airmass of 2.0. Based on 19 min of total exposure in g'r'i'z' and 16 min in JHK at a midtime of 08:38 UT on 2016-01-19, we estimate the detection and upper-limit magnitudes (all in the AB system):
g' > 23.9 mag,
r' = 23.6 +- 0.2 mag,
i' = 22.9 +- 0.2 mag,
z' = 22.5 +- 0.2 mag,
J > 20.5 mag,
H > 20.2 mag, and
K > 19.1 mag.
Our observation was about 4.8 hours later than the NOT followup observed by Malesani et al. (GCN #18895), and about 0.2 hours earlier than the RATIR observation by Cucchiara et al. (GCN #18901).
The fading of r'-band magnitudes between NOT and GROND is about 0.85 mag, and within the uncertainties between GROND and RATIR. The decline rate is about 0.18 mag/hr, which confirms the afterglow nature.
The given magnitudes are derived based on calibrating the images against SDSS and 2MASS field stars and are not corrected for the Galactic foreground extinction corresponding to a reddening of E(B-V)= 0.03 mag in the direction of the burst (Schlafly & Finkbeiner 2011).
GCN Circular 18904
Subject
GRB 160119A: Swift/UVOT Upper Limits
Date
2016-01-20T13:46:13Z (9 years ago)
From
Marissa McCaule at PSU <marissamc@swift.psu.edu>
L. M. McCauley (PSU) and F. E. Marshall (NASA/GSFC)
report on behalf of the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 160119A
169 s after the BAT trigger (Marshall et al., GCN Circ. 18893).
No optical afterglow consistent with the optical position
(Malesani et al. GCN Circ. 18895)
is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and subsequent exposures are:
Filter T_start(s) T_stop(s) Exp(s) Mag
white_FC 169 319 147 >21.04
white 607 7398 478 >21.06
v 657 34548 4935 >20.99
b 755 7355 471 >20.19
u 327 7150 716 >20.26
uvw1 1460 30371 3157 >21.07
uvm2 6540 29669 3739 >21.45
uvw2 6130 6330 196 >19.89
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).
GCN Circular 18905
Subject
GRB160119A: BOOTES-2/TELMA Early Upper Limits
Date
2016-01-20T14:59:20Z (9 years ago)
From
Juan Carlos Tello at IAA-CSIC <jtello@iaa.es>
J. C. Tello, S. R. Oates (IAA-CSIC), Martin Jelinek (Astronomical Institute
ASU-AVCR Ondrejov) and A. J.Castro-Tirado (IAA-CSIC & ISA-UMA), on behalf
of a larger collaboration, report:
"The 60 cm BOOTES-2/TELMA robotic telescope (Malaga, Spain) automatically
responded to the Swift trigger of GRB 160119A (Marshall et al., GCN 18893).
The first unfiltered images where obtained at 03:07:59 (111 seconds after
the burst, 9.44 seconds after receiving the GCN alert).
No credible source is found when combining the first 40 unfiltered images
of 3 seconds exposure. The combined image ranges from 03:07:59 UT -
03:10:28 UT (1.85-4.33 minutes after the burst) and results in a limiting
magnitude of 19.5 when compared to SDSS-R6 r filter catalog.
We also observed the field using the i filter, no credible source is found
either when combining 6x60s exposures. The combined image ranges from
03:16:54 UT - 03:40:01 UT (10.7-33.9 minutes after the burst) and results
in a limiting magnitude of 18.5 when compared to SDDS-R6 catalog."
GCN Circular 18906
Subject
GRB 160119A: afterglow confirmation from the NOT
Date
2016-01-20T16:36:39Z (9 years ago)
From
Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst <malesani@dark-cosmology.dk>
D. Malesani (DARK/NBI), D. Xu (NAOC/CAS), P. Jakobsson (Univ. Iceland),
C.E. Martinez-Vazquez (IAC-ULL), S. Murabito (IAC-ULL) report on behalf
of a larger collaboration:
We observed again the field of GRB 160119A (Marshall et al., GCN 18893)
with the Nordic Optical Telescope (NOT) equipped with the AlFOSC camera.
Observations start on January 20.14 UT (1.01 days after the GRB) and
consisted of 3x600 s in the SDSS r band.
No object is detected at the position of the candidate afterglow
(Malesani et al., GCN 18895; Cucchiara et al., GCN 18901; Chen et al.,
GCN 18902), down to a limiting magnitude r > 23.8 AB (3 sigma),
calibrated against nearby SDSS stars.
Compared to our previous observation (Malesani et al., GCN 18895), the
new measurement conclusively establishes fading, thus confirming that
this source is the afterglow of GRB 160119A, as already suggested by
Chen et al. (GCN 18902).
GCN Circular 18909
Subject
GRB 160119A: VLA Detection
Date
2016-01-21T01:55:34Z (9 years ago)
From
Kate Alexander at Harvard <kalexander@cfa.harvard.edu>
K. D. Alexander (Harvard), T. Laskar (NRAO / UC Berkeley), and E. Berger
(Harvard) report on behalf of a larger collaboration:
We observed GRB 160119A (Marshall et al, GCN 18893) at multiple frequencies
with the Karl G. Jansky Very Large Array (VLA) beginning 2016 January 20.44
UT (1.31 days after the burst). At a mean frequency of 21.8 GHz, we detect
a radio source with a preliminary flux density of ~ 0.13 mJy at
RA = 14:07:41.295 +/- 0.36���
Dec = +20:27:40.04 +/- 0.11���
consistent with the enhanced Swift/XRT position (Goad et al., GCN 18896)
and the optical position (Malesani et al,. GCN 18895). Follow-up
observations are planned.
We thank the VLA staff for rapidly executing these observations.
GCN Circular 18911
Subject
Konus-Wind observation of GRB 160119A
Date
2016-01-21T12:57:45Z (9 years ago)
From
Anna Kozlova at Ioffe Institute <ann_kozlova@mail.ioffe.ru>
A. Kozlova, S. Golenetskii, R. Aptekar, D. Frederiks, P. Oleynik,
M. Ulanov, D. Svinkin, A. Tsvetkova, A.Lysenko, and T. Cline,
on behalf of the Konus-Wind team, report:
The long-duration GRB 160119A (Swift-BAT trigger #671014:
Marshall, et al., GCN Circ. 18893, Stamatikos, et al.,
GCN Circ. 18899) was detected by Konus-Wind in the waiting mode.
The burst light curve shows a weak count rate increase
starting from ~T0(BAT)+9 s. The main phase of the event
consists of a single peak from ~T0(BAT)+120 s to ~T0(BAT)+175 s.
As calculated from the Bayesian block division,
the total duration of the burst is ~215 s.
The K-W light curve of this burst is available at
http://www.ioffe.rssi.ru/LEA/GRBs/GRB160119A/
As observed by Konus-Wind, the burst had a fluence of
1.68(-0.18,+0.19)x10^-5 erg/cm2 and a 2.944-s peak flux,
measured from ~T0(BAT)+144.3 s, of 6.39(-0.85,+0.89)x10^-7 erg/cm2/s
(both in the 20 - 1200 keV energy range).
Modelling the K-W 3-channel time-integrated spectrum
(measured from ~T0(BAT)+8.9 s to ~T0(BAT)+223.8 s)
by the cutoff power law yields the following model parameters:
the photon index alpha = -1.73(-0.12,+0.15),
and the peak energy Ep = 189(-53,+231) keV.
Modelling the 3-channel spectrum near the peak count rate
(from ~T0(BAT)+138.4 s to ~T0(BAT)+150.2 s)
by the cutoff power law yields the following model parameters:
the photon index alpha = -1.16(-0.13,+0.15),
and the peak energy Ep = 187(-25,+34) keV.
All the quoted errors are estimated at the 1 sigma confidence level.
All the presented results are preliminary.