GRB 190114A
GCN Circular 23739
Subject
GRB 190114A: NOEMA detection of the mm afterglow
Date
2019-01-16T14:51:27Z (8 years ago)
From
Antonio de Ugarte Postigo at IAA-CSIC <deugarte@iaa.es>
A. de Ugarte Postigo (HETH/IAA-CSIC and DARK/NBI), M. Bremer,
O. Feher (both IRAM), S. Schulze (Weizmann), C. C. Thoene,
L. Izzo, D. A. Kann, M. Blazek, K. Bensch (all HETH/IAA-CSIC),
D. A. Perley (LJMU), S. Martin (ALMA), I. de Gregorio-Monsalvo
(ESO), M. Michalowski (AOI-AMU), D. B. Malesani (DARK/NBI,
DAWN/NBI) R. Sanchez-Ramirez (INAF-IAPS) report:
We observed the afterglow of GRB 190114A (LaPorte et al.,
GCN 23677, Siegel et al. GCN 23678), at a redshift of z = 3.3765
(de Ugarte Postigo et al. GCN 23680) with NOEMA at 76, 92, 136
and 152 GHz. Observations started at 21:02 UT on 15 January,
42 hrs after the GRB. The afterglow is well detected at all
frequencies and had a flux density of 0.9 mJy at 92 GHz.
We derive the following refined coordinates for the afterglow:
R.A.(J2000): 04:22:10.58
Dec.(J2000): +02:11:28.4
with an error of +/- 0.1"
Further follow-up observations are encouraged
GCN Circular 23738
Subject
GRB 190114A:DOAO/LOAO optical observation
Date
2019-01-16T14:21:00Z (8 years ago)
From
Gregory SungHak Paek at SNU <shpaek@astro.snu.ac.kr>
Gregory S.H. Paek, Myungshin Im, Changsu Choi, Sophia Kim (CEOU/SNU),
Hyun-Il Sung (KASI), and Yuji Urata (NCU) on behalf of a larger
collaboration
This report is an errata version for GCN 23731.
The time duration between the initial alert and observing time at Deokheung
Optical Astronomy Observatory was changed from '0.2 hours' to '12.3 hours.'
We observed the afterglow of GRB 190114A(LaPorte et al., GCN 23677; Siegel
et al., GCN 23678; Evans et al., GCN 23679; de Ugarte Postigo et al., GCN
23680; Evans et al., 23681; Bolmer et al., GCN 23682; D'Avanzo et al., GCN
23683; Barthelmy et al., GCN 23685; de Ugarte Postigo et al., GCN 23687;
Selsing et al. GCN 23697) with the 1.0m telescope at the Deokheung Optical
Astronomy Observatory and the 1.0m telescope at the Lemonsan Optical
Astronomical Observatory.
The observation at the Deokheung Optical Astronomy Observatory started at
about 12.3 hours after the initial alert and the observation at the
Lemonsan Optical Astronomy Observatory started at about 24.7 hours after
the initial alert.
We did not find any positive signal at both observations and obtained
following preliminary 3 sigma upper limits.
obs mjd filter exptime[sec] ul[AB magtnitude]
DOAO 58497.642 R 60*10 >17.1
LOAO 58498.660 R 120*15 >20.3
The photometry is based on nearby APASS stars, Blaton transformation
(Blaton et al. 2007).
Further observations and analysis are being carried out
GCN Circular 23731
Subject
GRB 190114A: DOAO/LOAO optical observation
Date
2019-01-16T03:11:54Z (8 years ago)
From
Gregory SungHak Paek at SNU <shpaek@astro.snu.ac.kr>
Gregory S.H. Paek, Myungshin Im, Changsu Choi, Sophia Kim (CEOU/SNU),
Hyun-Il Sung (KASI), and Yuji Urata (NCU) on behalf of a larger
collaboration
We observed the afterglow of GRB 190114A(LaPorte et al., GCN 23677; Siegel
et al., GCN 23678; Evans et al., GCN 23679; de Ugarte Postigo et al., GCN
23680; Evans et al., 23681; Bolmer et al., GCN 23682; D'Avanzo et al., GCN
23683; Barthelmy et al., GCN 23685; de Ugarte Postigo et al., GCN 23687;
Selsing et al. GCN 23697) with the 1.0m telescope at the Deokheung Optical
Astronomy Observatory and the 1.0m telescope at the Lemonsan Optical
Astronomical Observatory.
The observation at the Deokheung Optical Astronomy Observatory started at
about 0.2 hours after the initial alert and the observation at the Lemonsan
Optical Astronomy Observatory started at about 24.7 hours after the initial
alert.
We did not find any positive signal at both observations and obtained
following preliminary 3 sigma upper limits.
obs mjd filter exptime[sec] ul[AB magtnitude]
DOAO 58497.642 R 60*10 >17.1
LOAO 58498.660 R 120*15 >20.3
The photometry is based on nearby APASS stars, Blaton transformation
(Blaton et al. 2007).
Further observations and analysis are being carried out.
[GCN OPS NOTE(15jan19): The authors have corrected a mistake in the time delay
value; it should have been 12.3 hrs. Please see Circ# 23738.]
GCN Circular 23719
Subject
GRB 190114A: Swift/UVOT Observations
Date
2019-01-15T16:52:55Z (8 years ago)
From
Mike Siegel at PSU/Swift MOC <mhs18@psu.edu>
M. H. Siegel (PSU) and S. J. LaPorte (PSU)
report on behalf of the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 190114A
258 s after the BAT trigger (LaPorte et al., GCN Circ. 23677).
We confirm a source consistent with the XRT position (Evans et al. GCN
Circ. 23681) as initially reported in UVOT (Siegel \& LaPorte, GCN Circ. 23678)
and later detected by GROND (Bolmer \& Schady, GCN Circ. 23682), OSN (de Ugarte
Postigo et al., GCN Circ. 23687) and NOT (Selsing et al., GCN Circ. 23697).
Notably, the optical counterpart was not seen in the initial finding chart and
had faded beyond detectability by the second orbit. The lack of detection in any
of the NUV filters would be consistent with the redshift of 3.4 reported by
de Ugarte Postigo et al. (GCN Circ. 23680).
The preliminary UVOT position is:
RA (J2000) = 04:22:10.55 = 65.54397 (deg.)
Dec (J2000) = +02:11:29.6 = 2.19157 (deg.)
with an estimated uncertainty of 0.42 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 (fc) 258 408 147 >20.58
white 514 1701 264 19.69+/-0.13
v 564 1752 136 18.33+/-0.22
b 490 1676 136 19.57+/-0.27
u 465 1825 155 >19.64
uvw1 440 1801 155 >19.17
uvm2 5866 7502 393 >19.66
uvw2 540 1726 136 >19.12
The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.22 in the direction of the burst
(Schlegel et al. 1998).
GCN Circular 23718
Subject
GRB 190114A: Mondy optical afterglow detectio
Date
2019-01-15T16:08:15Z (8 years ago)
From
Elena Mazaeva at IKI, Moscow <30.v@mail.ru>
E. Mazaeva (IKI), A. Pozanenko (IKI), E. Klunko (ISTP), A. Volnova (IKI), S. Belkin (IKI) report on behalf of of larger GRB follow-up collaboration:
We observed the field of GRB 190114A (LaPorte et al., GCN 23677) with AZT-33IK telescope of Sayan observatory (Mondy). We obtained several images in R-filter starting on Jan. 14 (UT) 11:43:08, i.e. ~ 9 hours after the BAT trigger. The afterglow (Siegel et al., GCN 23678; de Ugarte Postigo et al., GCN 23680; Bolmer et al., GCN 23682; de Ugarte Postigo et al., GCN 23687; Selsing et al., GCN 23697) is clearly detected in a stacked image.
Preliminary photometry is following.
Date UT start t-T0 Filter Exp. OT Err. UL
������������������������������������������(mid, days) (s)
2019-01-14 11:43:08 0.37663 R 60*60 20.10 0.09 21.8
The photometry is based on nearby PanSTARRS stars.
PanSTARRS_id R(applied Lupton' transformation)
110620655351961024 16.89
110610655260315104 17.67
110600655358532464 17.05
110580655437279536 17.37
GCN Circular 23697
Subject
GRB 190114A: NOT optical observations
Date
2019-01-15T00:24:42Z (8 years ago)
From
Jonatan Selsing at DARK/NBI <jselsing@dark-cosmology.dk>
Jonatan Selsing (DAWN/NBI and DAWN/DTU), A. de Ugarte Postigo
(HETH/IAA-CSIC and DARK/NBI), Kasper E. Heintz (Univ. of Iceland),
and S. Dyrbye (NOT), report on behalf of a larger collaboration:
We observed the optical afterglow of GRB 190114A (LaPorte et al., GCN
23677; Siegel et al., GCN 23678; de Ugarte Postigo et al., GCN 23680:
Bolmer et al., GCN 23682: D'Avanzo et al., GCN 23683) with the 2.5-m
Nordic Optical Telescope (NOT) equipped with the ALFOSC instrument.
We have carried out a three r-band imaging integrations each lasting
300s. The observations started in twilight on 2019.01.14 at 19:54:06 UT,
~16.5 hours after the BAT trigger. The afterglow is still well detected.��
Calibrating the photometric zeropoint against the Pan-STARRS catalog we
derive��
r = 21.24 +- 0.08 AB mag.
We do not detect any counterpart to the intervening system at z=2.6232
reported by de Ugarte Postigo et al. (GCN 23680) down to a 3-simga
limiting magnitude of r > 22.44.
[GCN OPS NOTE(15jan19): Per author's request, Dyrbye was moved from the
last paragraph to the author list.]
GCN Circular 23687
Subject
GRB 190114A: OSN Detection
Date
2019-01-14T20:48:52Z (8 years ago)
From
Alexander Kann at IAA-CSIC <kann@iaa.es>
A. de Ugarte Postigo (HETH/IAA-CSIC and DARK/NBI), D. A. Kann, L. Izzo,
C. C. Thoene, M. Blazek, K. Bensch (all HETH/IAA-CSIC), and F. Aceituno
(IAA-CSIC) report:
We observed the optical afterglow of GRB 190114A (Siegel & LaPorte, GCN
#23678), detected by Swift (LaPorte et al., GCN #23677), with the T150
telescope of the Sierra Nevada Observatory (OSN). We obtained 5 x 360 s
images in the Ic band at 16.98 hours after the GRB. The afterglow is
well-detected in each single image.
Days Ic mag error
0.7075 20.41 0.10
Magnitudes are given in the AB system. They were measured vs. four
Pan-STARRS comparison stars, using the transformation equations of
Lupton (2005), and transformed back into AB mags.
GCN Circular 23685
Subject
GRB 190114A: Swift-BAT refined analysis
Date
2019-01-14T18:36:28Z (8 years ago)
From
Amy Lien at GSFC <amy.y.lien@nasa.gov>
S. D. Barthelmy (GSFC), J. R. Cummings (CPI),
H. A. Krimm (NSF/USRA), S. J. LaPorte (PSU),
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-239 to T+963 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 190114A (trigger #883600)
(LaPorte et al., GCN Circ. 23677). The BAT ground-calculated position is
RA, Dec = 65.543, 2.196 deg which is
RA(J2000) = 04h 22m 10.2s
Dec(J2000) = +02d 11' 45.8"
with an uncertainty of 1.7 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 78%.
The mask-weighted light curve shows some weak-overlapping pulses that start
at ~T+125 s and end at ~T+200 s. T90 (15-350 keV) is 66.6 +- 10.2 sec
(estimated error including systematics).
The time-averaged spectrum from T+126.40 to T+199.22 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
2.06 +- 0.22. The fluence in the 15-150 keV band is 8.0 +- 1.2 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+151.08 sec in the 15-150 keV band
is 0.5 +- 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/883600/BA/
GCN Circular 23683
Subject
GRB 190114A: Swift-XRT refined Analysis
Date
2019-01-14T11:21:34Z (8 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC), A. D'Ai (INAF-IASFPA), J.A.
Kennea (PSU), B. Sbarufatti (INAF-OAB/PSU), D.N. Burrows (PSU), J.P.
Osborne (U. Leicester), K.L. Page (U. Leicester), A.P. Beardmore (U.
Leicester) and S.J. LaPorte report on behalf of the Swift-XRT team:
We have analysed 6.8 ks of XRT data for GRB 190114A (LaPorte et al. GCN
Circ. 23677), from 235 s to 19.0 ks after the BAT trigger. The data
comprise 64 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 Evans et
al. (GCN Circ. 23679).
The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=7.87 (+0.13, -0.43). At T+403 s the decay
flattens to an alpha of 0.01 (+0.20, -0.17) before breaking again at
T+2398 s to a final decay with index alpha=1.16 (+/-0.14).
A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.38 (+0.17, -0.12). The
best-fitting absorption column is 1 (+13, -1) x 10^21 cm^-2, at a
redshift of 3.3765, in addition to the Galactic value of 1.6 x 10^21
cm^-2 (Willingale et al. 2013). The PC mode spectrum has a photon index
of 1.80 (+0.09, -0.08) and a best-fitting absorption column of 2 (+10,
-2) x 10^21 cm^-2. The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum is 3.9 x 10^-11 (4.8 x
10^-11) erg cm^-2 count^-1.
A summary of the PC-mode spectrum is thus:
Galactic foreground: 1.6 x 10^21 cm^-2
Intrinsic column: 2 (+10, -2) x 10^21 cm^-2 at z=3.3765
Photon index: 1.80 (+0.09, -0.08)
If the light curve continues to decay with a power-law decay index of
1.16, the count rate at T+24 hours will be 0.013 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 5.0 x
10^-13 (6.2 x 10^-13) erg cm^-2 s^-1.
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00883600.
This circular is an official product of the Swift-XRT team.
GCN Circular 23682
Subject
GRB 190114A: GROND detection of the afterglow
Date
2019-01-14T09:21:12Z (8 years ago)
From
Jan Bolmer at MPE/Garching <jan@bolmer.de>
J. Bolmer (MPE, Garching) and P. Schady (Univ. of Bath) report:
We observed the field of GRB 190114A (Swift trigger 883600; LaPorte et al., GCN #23677) 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 03:16 UT on 14th January, around 5 minutes after the GRB trigger. They were performed
at an average seeing of 1.4" and at an average airmass of 1.3.
We found a faint source within the 1.7 arcsec Swift-XRT error circle reported by Evans et al. (GCN #23681) at
RA (J2000.0) = 4:22:10.58
DEC (J2000.0) = +2:11:28.32
with an uncertainty of 0.25" in each coordinate.
Based on the first 6.5 min of exposure, we report the following preliminary JHK magnitudes:
J = 16.41 +/- 0.05 mag
H = 15.88 +/- 0.05 mag
K = 15.53 +/- 0.07 mag
The above magnitudes are calibrated against 2MASS and are not corrected for the expected
Galactic foreground extinction corresponding to a reddening of E_(B-V)=0.19 in the direction
of theburst (Schlafly & Finkbeiner 2011).
GCN Circular 23681
Subject
GRB 190114A: Enhanced Swift-XRT position
Date
2019-01-14T07:24:20Z (8 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
P.A. Evans, M.R. Goad, J.P. Osborne and A.P. Beardmore (U. Leicester)
report on behalf of the Swift-XRT team.
Using 1511 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 190114A, 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 = 65.54389, +2.19150 which is equivalent
to:
RA (J2000): 04h 22m 10.53s
Dec (J2000): +02d 11' 29.4"
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 23680
Subject
GRB 190114A: VLT/X-shooter redshift
Date
2019-01-14T06:26:51Z (8 years ago)
From
Antonio de Ugarte Postigo at IAA-CSIC <deugarte@iaa.es>
A. de Ugarte Postigo (HETH/IAA-CSIC and DARK/NBI),
N. R. Tanvir (U. Leicester), D. Xu (NAOC), JPU.Fynbo
(DAWN/NBI and DAWN/DTU) report on behalf of the
STARGATE Consortium:
We observed the optical counterpart of the Swift GRB 190114A
(LaPorte et al. GCN 23677, Siegel et al. GCN 23678) with the
ESO Very Large Telescope UT 2 (Kueyen) equipped with the
X-shooter spectrograph, covering the wavelength range
3500-24000 AA. Observations started on 2019 Jan 14 03:25 UT
(approx 15 min after the GRB).
The spectrum exhibits many absorption features, including
Lya, SII, OI, OI*, SiII, SiII*, CII, CII*, NiII, SiIV, CIV, FeII, FeII*,
AlII, AlIII, ZnII, MgII, MgI, and CaII at a common redshift of
z=3.3765. We conclude that this is the redshift of the GRB. We also
identify an intervening system at a redshift of z=2.6232, characterised
by strong features due to MgII, FeII and AlII.
We acknowledge the expert support from the ESO observing
staff, in particular Elizabeth Bartlett, Trystyn Berg and Juan Carlos
Olivares, and the visiting astronomer, Boris Gaensicke.
GCN Circular 23679
Subject
GRB 190114A: Prompt enhanced Swift-XRT position
Date
2019-01-14T03:52:27Z (8 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
P.A. Evans (U. Leicester) reports on behalf of the Swift-XRT team:
Using promptly downlinked XRT event data for GRB 190114A, we find an
enhanced XRT position of the afterglow: RA, Dec: 65.5439, 2.1913 which
is equivalent to:
RA (J2000) = 04 22 10.54
Dec (J2000) = +02 11 28.6
with an uncertainty of 2.0 arcseconds (radius, 90% confidence).
Analysis of the promptly available data is online at
http://www.swift.ac.uk/sper/883600.
Position enhancement is is described by Goad et al. (2007, A&A, 476,
1401) and Evans et al. (2009, MNRAS, 397, 1177).
This circular is an official product of the Swift-XRT team.
GCN Circular 23678
Subject
GRB 190114A: Possible UVOT Detection
Date
2019-01-14T03:41:48Z (8 years ago)
From
Mike Siegel at PSU/Swift MOC <mhs18@psu.edu>
M. H. Siegel (PSU) and S. J. LaPorte (PSU) report on behalf of the Swift/UVOT team.
UVOT took a finding chart exposure of 150 seconds with the White filter
starting 859 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
RA(J2000) = 04:22:10.57 = 65.54403
DEC(J2000) = +02:11:29.3 = 2.19146
with a 90%-confidence error radius of about 0.79 arc sec. This position is 1.7
arc sec. from the center of the XRT error circle. The estimated magnitude is
19.52 with a 1-sigma error of about 0.17. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.22.
GCN Circular 23677
Subject
GRB 190114A: Swift detection of a burst
Date
2019-01-14T03:25:02Z (8 years ago)
From
David Palmer at LANL <palmer@lanl.gov>
S. J. LaPorte (PSU), J. A. Kennea (PSU), N. J. Klingler (PSU),
A. Y. Lien (GSFC/UMBC), D. M. Palmer (LANL) and M. H. Siegel (PSU)
report on behalf of the Neil Gehrels Swift Observatory Team:
At 03:10:49 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 190114A (trigger=883600). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 65.544, +2.170 which is
RA(J2000) = 04h 22m 11s
Dec(J2000) = +02d 10' 11"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). Due to a telemetry gap, the BAT lightcurve
is not available.
The XRT began observing the field at 03:14:56.4 UT, 246.6 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source located at RA, Dec 65.54341, 2.19058
which is equivalent to:
RA(J2000) = 04h 22m 10.42s
Dec(J2000) = +02d 11' 26.1"
with an uncertainty of 3.6 arcseconds (radius, 90% containment). This
location is 74 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 (1.62 x
10^21 cm^-2, Willingale et al. 2013), with an excess column of 4.1
(+2.51/-2.16) x 10^21 cm^-2 (90% confidence).
The initial flux in the 2.5 s image was 1.18e-09 erg cm^-2 s^-1 (0.2-10
keV).
UVOT took a finding chart exposure of 150 seconds with the White filter
starting 257 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
0.22.
Burst Advocate for this burst is S. J. LaPorte (extragsam 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.)