GRB 190203A
GCN Circular 23878
Subject
GRB 190203A: Mondy optical observations
Date
2019-02-06T18:09:10Z (7 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
A. Volnova (IKI), E. Klunko (ISTP), A. Pozanenko (IKI), E. Mazaeva
(IKI), S. Belkin (IKI) report on behalf of IKI-GRB-FuN:
We observed the field of GRB 190203A (Lien et al. GCN 23845) with
AZT-33IK telescope of Sayan observatory (Mondy) starting on Feb. 03 (UT)
16:23:21. We detected the optical afterglow (Lien et al. GCN
23845; Moskvitin et al., GCN 23847; Lipunov et al. GCN 23850).
Preliminary photometry of the afterglow is following.
Date UT start t-T0 Filter Exp. OT Err. UL(3sigma)
(mid, days) (s)
2019-02-03 16:23:21 0.04807 R 30*120 21.14 0.27 21.3
The photometry is based on the nearby USNO-B1 stars used in GCN 23847.
GCN Circular 23873
Subject
GRB 190203A: Swift-BAT refined analysis
Date
2019-02-05T03:40:35Z (7 years ago)
From
Amy Lien at GSFC <amy.y.lien@nasa.gov>
D. M. Palmer (LANL), S. D. Barthelmy (GSFC),
J. R. Cummings (CPI), H. A. Krimm (NSF/USRA),
A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC),
T. Sakamoto (AGU), M. Stamatikos (OSU),
T. N. Ukwatta (LANL) (i.e. the Swift-BAT team):
Using the data set from T-213 to T+456 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 190203A (trigger #887512)
(Lien et al., GCN Circ. 23845). The BAT ground-calculated position is
RA, Dec = 22.603, 55.736 deg which is
RA(J2000) = 01h 30m 24.7s
Dec(J2000) = +55d 44' 10.5"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 21%.
The mask-weighted light curve shows several overlapping pulses that starts ~ T-60 s
and ends at T+40 s. Note that there is a large data gap from T-117.652 s to T-60.784 s,
so it is possible that there is additional burst emission during this interval.
T90 (15-350 keV) is 96 +- 16 sec (estimated error including systematics).
The time-averaged spectrum from T-60.784 to T+ 43.216 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
1.06 +- 0.06. The fluence in the 15-150 keV band is 1.5 +- 0.05 x 10^-5 erg/cm2.
The 1-sec peak photon flux measured from T+2.72 sec in the 15-150 keV band
is 3.1 +- 0.6 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/887512/BA/
GCN Circular 23866
Subject
GRB 190203A: AstroSat CZTI detection
Date
2019-02-04T18:38:24Z (7 years ago)
From
Vidushi Sharma at IUCAA <vidushi@iucaa.in>
T. Khanam, V. Sharma and D. Bhattacharya (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 190203A, which was also detected by Swift (Lien A. Y. et al., GCN Circ 23845) and Konus-Wind (Frederiks D. et al., GCN Circ 23859).
The source was clearly detected in the 20-200 keV energy range. The light curve shows multiple peaks of emission with the strongest peak at 15:44:14.0 UT. The measured peak count rate is 314 cts/s above the background in the combined data of four quadrants, with a total of 387 cts. The local mean background count rate was 340 cts/s. Using cumulative rates, we measure a T90 of 46.45 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 23865
Subject
GRB190203A: UVOT analysis
Date
2019-02-04T17:01:34Z (7 years ago)
From
Paul Kuin at MSSL <npkuin@gmail.com>
Paul Kuin (UCL/MSSL) and A. Y. Lien (GSFC/UMBC)
report on behalf of the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 190203A
121 s after the BAT trigger (Lien et al., GCN Circ. 23845).
A source consistent with the XRT position
(Goad et al. GCN Circ. 23848)
is detected in the initial UVOT exposures.
The preliminary UVOT position is:
RA (J2000) = 01:30:23.21 = 22.59672 (deg.)
Dec (J2000) = +55:43:20.6 = 55.72240 (deg.)
with an estimated uncertainty of 0.46 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 121 271 147 18.66 +/- 0.06
v 609 5462 225 >19.2
b 535 4846 236 >20.5
u 279 5967 551 >21.0
w1 658 5872 413 >20.2
m2 634 5666 413 >21.0
w2 585 5257 236 >20.2
The short v image during settling, i.e., prior to the settled
images reported here, shows a 16.3 +/- 0.3 mag source as well.
Usually we have a detection in the other bands besides in the
early white filter. Either the GRB decayed so fast as to be
below u > 19.8 mag between To+278 and 529s or this burst is
of a high redshift. A rapid decay is consistent with Watson
et al. (GCN Circ. 23864).
The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.64 in the direction of the burst
(Schlegel et al. 1998).
GCN Circular 23864
Subject
GRB 190203A: COATLI Optical Observations
Date
2019-02-04T14:21:01Z (7 years ago)
From
Alan M. Watson at Instituto de Astronomia UNAM <alan@astro.unam.mx>
Alan M. Watson (UNAM), Nat Butler (ASU), Rosa L. Becerra (UNAM), Diego
Gonz��lez (UNAM), William H. Lee (UNAM), Margarita Pereyra (UNAM), Carlos
Rom��n-Z����iga (UNAM), Alexander Kutyrev (GSFC), and Eleonora Troja (GSFC)
report:
We observed the field of GRB 190203A (Lien et al., GCN Circ. 23845) with
the COATLI 50-cm telescope and interim imager at the Observatorio
Astron��mico Nacional on the Sierra de San Pedro M��rtir
(http://coatli.astroscu.unam.mx) from 2019-02-04 02:39 to 2019-02-04
09:19 (from 10.9 to 17.6 hours after the trigger), obtaining a total of
3.2 hours of exposure in the w filter.
At the position of the UVOT afterglow candidate (Lien et al., GCN Circ.
23852), we do not detect anything to a 5-sigma limit of w = 22.4.
Our non-detection is consistent with the rapid fading seen by Lien et
al. (GCN Circ. 23845), Novichonok et al. (GCN Circ. 23846), Moskvitin et
al. (GCN Circ. 23847), and Lipunov (GCN Circ. 23850).
Our w magnitudes are calibrated against the USNO-B1 catalog (adjusted to
an approximate AB system) and are not corrected for Galactic extinction
in the direction of the GRB.
We thank the COATLI technical team and the staff of the Observatorio
Astron��mico Nacional.
GCN Circular 23860
Subject
GRB 190203A: Liverpool Telescope near-IR observations
Date
2019-02-04T12:30:13Z (7 years ago)
From
Luca Izzo at IAA-CSIC <luca.izzo@gmail.com>
L. Izzo, M. Blazek (HETH-IAA/CSIC), A. de Ugarte Postigo (DARK/NBI & HETH-IAA/CSIC), D. A. Kann, C. C. Thoene (HETH-IAA/CSIC) report:
We observed the field of GRB 190203A (Lien et al. GCN 23845) with the IO:I camera mounted on the 2-m Liverpool Telescope located in La Palma, Spain. Observations started on February 3rd at 20:31:17 UT (4.72 hours after the GRB trigger) and we obtained a series of 10x60s images in the H filter.
In our stacked image, we find no source at the position of the observed counterpart (Moskvitin et al. GCN 23847, Lipunov et al. GCN 23850) down to a 3-sigma limit of H(AB) > 20.1 mag. The calibration was performed using four nearby 2MASS stars.
GCN Circular 23859
Subject
Konus-Wind observation of GRB 190203A
Date
2019-02-04T12:23:45Z (7 years ago)
From
Dmitry Frederiks at Ioffe Institute <fred@mail.ioffe.ru>
D. Frederiks, S. Golenetskii, R.Aptekar, A. Kozlova,
A.Lysenko, D. Svinkin, A. Tsvetkova, M. Ulanov, and T. Cline,
on behalf of the Konus-Wind team, report:
The long GRB 190203A (Swift/BAT detection: Lien et al., GCN 23845)
triggered Konus-Wind at T0=56630.443 s UT (15:43:50.443).
The KW light curve shows a multi-peaked structure in the interval
from T0-39 s to T0-58 s.
The emission is seen up to ~4 MeV.
As observed by Konus-Wind, the burst had a fluence of
(4.9 �� 0.5)x10^-5 erg/cm2 and a 64-ms peak energy flux,
measured from T0+20.352, of (3.5 �� 0.4)x10^-6 erg/cm2
(both in the 20 keV - 10 MeV energy range).
The time-integrated spectrum (measured from T0 to T0+57.344 s)
is best fit in the 20 keV - 15 MeV range by a cutoff power-law
(CPL) function with the following model parameters:
the photon index alpha = -0.45(-0.11,+0.12),
and the peak energy Ep = 314(-22,+25) keV,
chi2 = 98/98 dof.
Fitting this spectrum with the GRB (Band) function yields
the same alpha and Ep, and only an upper limit on beta (<-2.7).
The spectrum near the peak count rate (measured from T0+16.640
to T0+24.574 s) is best fit in the 20 keV - 15 MeV range by
the CPL function with the following model parameters:
the photon index alpha = -0.17(-0.16,+0.18),
and the peak energy Ep = 348(-29,+34) keV,
chi2 = 90/98 dof.
Fitting this spectrum with the GRB (Band) function yields
the same alpha and Ep, and only an upper limit on beta (<-2.5).
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB190203_T56630/
All the quoted errors are estimated at the 90% confidence level.
All the presented results are preliminary.
GCN Circular 23858
Subject
GRB 190203A: Swift-XRT refined Analysis
Date
2019-02-04T12:09:15Z (7 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
A.P. Beardmore (U. Leicester), P.A. Evans (U. Leicester), J.P. Osborne
(U. Leicester), A. D'Ai (INAF-IASFPA), A. Melandri (INAF-OAB), P.
D'Avanzo (INAF-OAB), B. Sbarufatti (INAF-OAB/PSU), D.N. Burrows (PSU),
A. Tohuvavohu (PSU) and A.Y. Lien report on behalf of the Swift-XRT
team:
We have analysed 6.5 ks of XRT data for GRB 190203A (Lien et al. GCN
Circ. 23845), from 103 s to 50.0 ks after the BAT trigger. The data
comprise 669 s in Windowed Timing (WT) mode (the first 8 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. 23848).
The late-time light curve (from T0+4.1 ks) can be modelled with a
power-law decay with a decay index of alpha=1.73 (+/-0.08).
A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.69 (+/-0.04). The
best-fitting absorption column is 7.2 (+/-0.5) x 10^21 cm^-2, in
excess of the Galactic value of 4.0 x 10^21 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 1.63 (+0.21, -0.20)
and a best-fitting absorption column of 6.9 (+2.0, -1.7) x 10^21 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum is 5.4 x 10^-11 (7.6 x 10^-11) erg cm^-2
count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 6.9 (+2.0, -1.7) x 10^21 cm^-2
Galactic foreground: 4.0 x 10^21 cm^-2
Excess significance: 2.8 sigma
Photon index: 1.63 (+0.21, -0.20)
If the light curve continues to decay with a power-law decay index of
1.73, the count rate at T+24 hours will be 0.012 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 6.4 x
10^-13 (8.9 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/00887512.
This circular is an official product of the Swift-XRT team.
GCN Circular 23850
Subject
GRB 190203A: MASTER OT detection
Date
2019-02-03T23:55:04Z (7 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>
V. Lipunov, E. Gorbovskoy, N.Tyurina, V.Kornilov, D.Vlasenko, V.Vladimirov,
D.Zimnukhov, A.Kuznetsov, P.Balanutsa, A. Chasovnikov, D.Kuvshinov (Lomonosov
Moscow State University, SAI, Physics Department),
R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres (The Instituto
de Astrofisica de Canarias),
D. Buckley (South African Astronomical Observatory),
V. Yurkov, A. Gabovich, Yu. Sergienko, D. Kobcev (Blagoveschensk Educational
State University),
A. Tlatov, V.Senik, A.V. Parhomenko, D. Dormidontov (Kislovodsk Solar Station
of the Pulkovo Observatory),
O. Gress, N.M. Budnev, O.Ershova, Yu.Ishmuhametova (Applied Physics
Institute, Irkutsk State University),
R. Podesta, C. Lopez, C.Francile, F. Podesta (Observatorio Astronomico Felix
Aguilar OAFA),
H.Levato (Instituto de Ciencias Astronomicas, de la Tierra y del Espacio ICATE)
MASTER-Amur robotic telescope (Global MASTER-Net http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, v.2010, 30L)
was pointed to Swift GRB190203B (Lien et al. GCN23845, Ttrig=2019-02-03 15:44:08 UT)
19 sec after notice time (63 sec after trigger time) at 2019-02-03 15:45:11 UT.
On our first (10s exposure) set we found 1 optical transient within SWIFT error-box:
T-Tmid Date Time Exp,s Ra Dec Mag
---------|---------------------|-------|-----------------|-----------------|-------
68 2019-02-03 15:45:11 10 (01h 30m 23.25s , +55d 43m 20.59s) 15.28
There is fast decay on the light curve.
The 5-sigma upper limit on the first 10s exposition was 16.3mag
The galactic latitude b = -6 deg., longitude l = 129 deg.
The observations started on zenit distance = 61 deg.
The sun altitude was -56.2 deg
The message may be cited.
GCN Circular 23848
Subject
GRB 190203A: Enhanced Swift-XRT position
Date
2019-02-03T19:51:46Z (7 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 77 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 190203A, 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 = 22.59659, +55.72219 which is equivalent
to:
RA (J2000): 01h 30m 23.18s
Dec (J2000): +55d 43' 19.9"
with an uncertainty of 2.7 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 23847
Subject
GRB 190203A: SAO RAS optical observations, afterglow fading
Date
2019-02-03T18:43:44Z (7 years ago)
From
Moskvitin Alexander at SAO RAS <mosk@sao.ru>
A. S. Moskvitin and O. I. Spiridonova (SAO RAS),
A. A. Volnova (IKI RAS), report on behalf of larger collaboration.
We observed the field of the GRB 190203A (Lien et al. GCNC #23845)
with the Zeiss-1000 telescope of SAO RAS (+ CCD photometer),
started on February, 3, 15:54:38 UT (10.5 min after the trigger).
We clearly detected the OT in the first few 300 sec. Rc band frames
(coordinates are consistent with the reported UVOT position).
Preliminary measurements of the OT brightness are as following:
T_start, UT T_end T_mid-T0, h exp., s R +/- R_err
15:54:38 16:11:51 0.318 3 x 300 19.34 +/- 0.08
16:12:54 16:30:11 0.624 3 x 300 20.46 +/- 0.12
16:30:54 17:19:23 1.183 8 x 300 21.23 +/- 0.14
OT is fading quickly with the slope about -1.3.
The photometry is based on the nearby USNO-B1 stars.
No correction has been made for the Galactic extinction.
GCN Circular 23846
Subject
GRB 190203A: Koshka Zeiss-1000 optical upper limit
Date
2019-02-03T16:51:04Z (7 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
A. Novichonok (KIAM), A. Pozanenko (IKI), E. Mazaeva (IKI), S. Belkin
(IKI), A. Volnova (IKI), I. Molotov (KIAM) report on behalf of larger
GRB follow-up collaboration:
We observed the field of GRB 190203A (Lien , et al., GCN 23845) with
Zeiss-1000 1-m telescope of Koshka Observatory starting on Feb. 03 (UT)
16:01:10 in R-filter under not optimal weather conditions. We do not
detect the optical afterglow candidate (Lien , et al., GCN 23830).
Preliminary photometry of the combined of first 4 images of 4*180
seconds started on 2019-02-03 16:01:10 is R=19.5. Observation is continuing.
The photometry is based on several nearby USNO-B1.0 stars.
[GCN OPS NOTE(03feb19): Per author's request, a typo in the first time
specification has been changed from "02:40:34" to "16:01:10".]
GCN Circular 23845
Subject
GRB 190203A: Swift detection of a burst with an optical counterpart
Date
2019-02-03T15:57:07Z (7 years ago)
From
Aaron Tohuvavohu at PSU/Swift <aaronb@swift.psu.edu>
A. Y. Lien (GSFC/UMBC), S. D. Barthelmy (GSFC),
P. D'Avanzo (INAF-OAB), J. A. Kennea (PSU), N. J. Klingler (PSU),
M. H. Siegel (PSU) and A. Tohuvavohu (PSU) report on behalf of the
Neil Gehrels Swift Observatory Team:
At 15:44:08 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 190203A (trigger=887512). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 22.577, +55.738 which is
RA(J2000) = 01h 30m 18s
Dec(J2000) = +55d 44' 18"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve showed a multi-peaked
structure with a duration of about 55 sec. The peak count rate
was ~2000 counts/sec (15-350 keV), at ~2 sec after the trigger.
The XRT began observing the field at 15:46:04.0 UT, 115.7 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 22.5984, 55.7211 which is equivalent to:
RA(J2000) = 01h 30m 23.62s
Dec(J2000) = +55d 43' 16.0"
with an uncertainty of 4.8 arcseconds (radius, 90% containment). This
location is 74 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 4.46e-09 erg cm^-2 s^-1 (0.2-10
keV).
UVOT took a finding chart exposure of 150 seconds with the White filter
starting 120 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
RA(J2000) = 01:30:23.19 = 22.59662
DEC(J2000) = +55:43:20.7 = 55.72241
with a 90%-confidence error radius of about 0.63 arc sec. This position is 5.9
arc sec. from the center of the XRT error circle. The estimated magnitude is
18.58 with a 1-sigma error of about 0.15. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.64.
Burst Advocate for this burst is A. Y. Lien (amy.y.lien AT 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: /too.html.)