# GCN_circulars

GRB_name: GRB190103A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23646
SUBJECT: IPN triangulation of GRB 190103A (long)
DATE:    19/01/09 11:34:55 GMT
FROM:    Anna Kozlova at Ioffe Institute  <ann_kozlova@mail.ioffe.ru>

K. Hurley, on behalf of the IPN,

I. G. Mitrofanov, D. Golovin, M. L. Litvak, and A. B. Sanin,
on behalf of the HEND-Odyssey GRB team,

A. Kozlova, S. Golenetskii, R. Aptekar, D. Frederiks, D. Svinkin,
and T. Cline on behalf of the Konus-Wind team,

A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo,
and C. Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team,

S. Barthelmy, J. Cummings, H. Krimm, and D. Palmer,
on behalf of the Swift-BAT team,

and

W. Boynton, C. Fellows, K. Harshman, H. Enos, and R. Starr,
on behalf of the GRS-Odyssey GRB team, report:

The long-duration GRB 190103A (AGILE (MCAL) detection:
Ursi et al., GCN Circ. 23600; AstroSat (CZTI) detection:
Khanam et al., GCN Circ. 23609) was detected by Konus-Wind,
INTEGRAL (SPI-ACS), Mars-Odyssey (HEND), AGILE (MCAL),
AstroSat (CZTI), and Swift (BAT) at about 60113 s UT (16:41:53).
The burst was outside the coded field of view of the BAT.

We have triangulated it to a preliminary, 3-sigma error box
whose coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   251.409 (16h 45m 38s) +17.382 (+17d 22' 54")
  Corners:
   251.079 (16h 44m 19s) +18.134 (+18d 08' 01")
   251.470 (16h 45m 53s) +18.711 (+18d 42' 41")
   251.734 (16h 46m 56s) +16.622 (+16d 37' 21")
   251.342 (16h 45m 22s) +16.027 (+16d 01' 37")
  ---------------------------------------------
The error box area is about 0.93 sq. deg, and its maximum
dimension is 2.69 deg (the minimum one is 26.4 arcmin).
The Sun distance was about 51 deg.

This box may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB190103_T60113/IPN/

The Konus-Wind time history and spectrum will be given in a forthcoming
GCN Circular.


GRB_name: GRB190109B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23648
SUBJECT: GRB 190109B: Swift detection of a burst
DATE:    19/01/09 12:18:35 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

B. Sbarufatti (PSU), S. D. Barthelmy (GSFC), J.D. Gropp (PSU),
J. A. Kennea (PSU) and K. L. Page (U Leicester) report on behalf of
the Neil Gehrels Swift Observatory Team:

At 11:56:09 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 190109B (trigger=882809).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 55.595, +63.578, which is 
   RA(J2000)  =  03h 42m 23s
   Dec(J2000) = +63d 34' 40"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a single peak
with a duration of about 10 sec.  The peak count rate
was ~1700 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 11:57:36.3 UT, 87.1 seconds after
the BAT trigger. No source was detected in the 2.5-s promptly available
image. We are waiting for the full dataset to detect and localise the
XRT counterpart. 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 90 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 25% of
the BAT 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
BAT 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
0.70. 

Even without an XRT detection, we believe this event to be a real GRB
given an 8.6 sigma detection in BAT and that there is a temporal coincidence
with a Fermi-GBM event.  However there still is a possibility that this
is not real.  We will have to wait for the full data set to be downlinked. 

Burst Advocate for this burst is B. Sbarufatti (bxs60 AT psu.edu). 
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.)


GRB_name: GRB190109A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23649
SUBJECT: GRB190109A: MITSuME Akeno optical upper limits
DATE:    19/01/09 12:34:19 GMT
FROM:    Motoki Oeda at Tokyo Inst. of Tech.  <oeda@hp.phys.titech.ac.jp>

M. Oeda, R. Adachi, K. L. Murata, R. Itoh, Y. Tachibana, S. Harita, K.
Morita, K.Shiraishi, K. Iida, M. Niwano,  Y. Yatsu, and N. Kawai (TokyoTech)
report on behalf of the MITSuME collaboration:

We searched for the optical counterpart of GRB 190109A (M. J. Moss  et
al.,GCN Circular #23642) with the optical three color (g', Rc, and Ic)
CCD cameras attached to the MITSuME 50 cm telescope of Akeno
Observatory,Yamanashi, Japan.

The observation started on 08:18:30.05 UT. We did not find any new
point source within the enhanced XRT circle (P.A. Evans et al., GCN
Circular #23643) in all three bands. We obtained following 3 sigma limits
for the magnitudes.

T0+[hour]    MID-UT      T-EXP[sec]    g'       Rc        Ic
-------------------------------------------------------------------------------------------------------
3.097       8:42:32.91          1140      >16.23     >15.42     >15.34
-------------------------------------------------------------------------------------------------------
T0+ : Elapsed time after the burst
T-EXP: Total Exposure time
We used GSC2.3 catalog for flux calibration.


GRB_name: GRB190109B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23651
SUBJECT: GRB 190109B: Swift-XRT observations
DATE:    19/01/09 13:21:11 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

D.N. Burrows (PSU), J.A. Kennea (PSU), S. Campana (INAF-OAB), G.
Cusumano (INAF-IASF PA), P.A. Evans (U. Leicester) and J.P. Osborne (U.
Leicester) report on behalf of the Swift-XRT team:

The XRT began observing the field of GRB 190109B at 11:57:36.3 UT, 87.1
seconds after the BAT trigger. Using promptly downlinked data we find a
fading, uncatalogued X-ray source with an enhanced position: RA, Dec
55.4870, 63.5920 which is equivalent to:
   RA(J2000)  = 03h 41m 56.88s
   Dec(J2000) = +63d 35' 31.2"
with an uncertainty of 2.1 arcseconds (radius, 90% containment). This
location is 180 arcseconds from the BAT onboard position, outside 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 consistent with the Galactic value of 4.56
x 10^21 cm^-2 (Willingale et al. 2013). 


GRB_name: GRB190109B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23652
SUBJECT: GRB 190109B: Enhanced Swift-XRT position
DATE:    19/01/09 14:22:21 GMT
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 649 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 190109B, 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 = 55.48723, +63.59203 which is equivalent
to:

RA (J2000): 03h 41m 56.94s
Dec (J2000): +63d 35' 31.3"

with an uncertainty of 1.8 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.


GRB_name: GRB190109A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23653
SUBJECT: GRB 190109A: Swift-BAT refined analysis
DATE:    19/01/09 15:23:32 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

T. Sakamoto (AGU), S. D. Barthelmy (GSFC), J. R. Cummings (CPI),
J. D. Gropp (PSU), H. A. Krimm (NSF/USRA), A. Y. Lien (GSFC/UMBC),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), 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 190109A (trigger #882747)
(Gropp, et al., GCN Circ. 23642).  The BAT ground-calculated position is
RA, Dec = 33.213, 38.111 deg, which is 
   RA(J2000)  =  02h 12m 51.2s 
   Dec(J2000) = +38d 06' 39.5" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 28%.
 
The mask-weighted light curve shows several overlapping peaks starting at ~T+1 sec,
peaking at ~T+40 sec, and returning to baseline at ~T+200 sec.
T90 (15-350 keV) is 115.0 +- 33.5 sec (estimated error including systematics).
 
The time-averaged spectrum from T+5.86 to T+205.36 sec (with a 1.03 sec gap
in the data at T+111.97 sec) is best fit by a power law with an exponential cutoff.
This fit gives a photon index 0.36 +- 0.47, and Epeak of 49.7 +- 4.0 keV
(chi squared 46.05 for 56 d.o.f.).  For this model the total fluence
in the 15-150 keV band is 5.5 +- 0.3 x 10^-6 erg/cm2 and the 1-sec peak flux
measured from T+38.82 sec in the 15-150 keV band is 1.9 +- 0.3 ph/cm2/sec.
A fit to a simple power law gives a photon index of 1.86 +- 0.08
(chi squared 87.76 for 57 d.o.f.).  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/882747/BA/


GRB_name: GRB190109B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23654
SUBJECT: GRB 190109B: Mondy optical upper limit
DATE:    19/01/09 15:29:40 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

S. Belkin (IKI), E. Klunko (ISTP), A. Pozanenko (IKI), E. Mazaeva (IKI), 
A. Volnova (IKI) report   on behalf of IKI-FuN:

We observed the field of the GRB 190109B (Sbarufatti et al., GCN 23648) 
with AZT-33IK telescope of Sayan observatory (Mondy).  We obtained 
several images in R-filter starting on Jan. 09 (UT) 12:17:03, i.e. 21 
minutes after the burst trigger.  We do not detect any object within 
enhanced Swift-XRT position  (Beardmore et al., GCN 23652). Preliminary 
photometry of the field is following.

Date        UT start  t-T0      Filter Exp.   OT      Err.  UL(3sigma)
                       (mid, days)      (s)

2019-01-09  12:17:03  0.02463    R     1900   n/d     n/d   22.6

The photometry is based on several nearby USNO-B1.0 stars.

[GCN OPS NOTE(09jan19):  Using information from Circ# 23657, the SUBJECT-line
and first sentence has been changed from 190109A to 190109B.]


GRB_name: GRB190109B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23655
SUBJECT: GRB 190109B: BOOTES-5/JGT optical observations
DATE:    19/01/09 15:44:19 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

X.-Y.Li, Y.-D. Hu, I. Carrasco, E. Fernandez-Garcia 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) followed-up GRB 190109B 
(Sbarufatti et al., GCNC 23648) starting at 13:30 UT (~1.6 hr after 
trigger). Within the enhanced Swift/XRT position (Beardmore et al., GCNC 
23652), no optical afterglow is found down to 20.4 mag in the r-band on 
the co-added image, in agreement with the UVOT upper limit (Sbarufatti 
et al., GCNC 23648).

We thank the staff at Observatorio Astronomico Nacional in San Pedro 
Martir for its excellent support.


GRB_name: GRB190109B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23656
SUBJECT: GRB 190109B: COATLI Optical Observations
DATE:    19/01/09 16:11:22 GMT
FROM:    Alan M. Watson at Instituto de Astronomia UNAM  <alan@astro.unam.mx>

Eleonora Troja (GSFC), Alan M. Watson (UNAM), Nat Butler (ASU), Rosa L.
Becerra (UNAM), William H. Lee (UNAM), Margarita Pereyra (UNAM), Carlos
RomÃ¡n-ZÃºÃ±iga (UNAM), and Alexander Kutyrev (GSFC) report:

We observed the field of GRB 190109B (Sbarufatti et al., GCN Circ.
23642) with the COATLI 50-cm telescope and interim imager at the
Observatorio AstronÃ³mico Nacional on the Sierra de San Pedro MÃ¡rtir
(http://coatli.astroscu.unam.mx) from 2019-01-09 11:57:47.6 to
13:27:45.2 (from 98.5 seconds to 1.53 hours after the trigger) at air
masses above 3, obtaining a total of 59.1 minutes of exposure in the w
filter.

We do not detect an optical source within the enhanced XRT position
region (Beardmore et al., GCN Circ. 23652) to a 5-sigma limiting
magnitude of w = 20.3.

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
AstronÃ³mico Nacional.


GRB_name: GRB190109B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23657
SUBJECT: Correction to the GCN circ. 23654 / GRB 190109B: Mondy optical upper limit
DATE:    19/01/09 16:43:11 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Pozanenko (IKI) report on behalf of IKI-FuN:

The title and text of the GCN circ. 23654 refers to the GRB 190109B, not 
GRB 190109A.

We apologize for possible inconvenience.


GRB_name: GRB190109A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23658
SUBJECT: GRB 190109A: Fermi GBM observation
DATE:    19/01/09 16:56:02 GMT
FROM:    Andreas von Kienlin at MPE  <azk@mpe.mpg.de>

A. von Kienlin (MPE) reports on behalf of the Fermi GBM Team:

"At 05:12:49.45 UT on 09 January 2019, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 190109A (trigger 568703574 / 190109217), which was
also detected by the Swift/BAT (Gropp et al. 2019, GCN 23642)
The GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight at the GBM trigger time is 65 degrees.

The GBM light curve shows a structured emission
with a duration (T90) of about 120 s (50-300 keV).
The time-averaged spectrum from T0-4.096 s to T0+114.690 s is
best fit by a Band function with Epeak = 46.8 +/- 2.2 keV, alpha = 1.3 +/- 0.3, 
and beta = -2.71 +/- 0.13 

The event fluence (10-1000 keV) in this time interval is
(7.6 +/-  0.4)E-06 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+30.91 s in the 10-1000 keV band
is 2.6 +/- 0.2 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB190109B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23659
SUBJECT: GRB 190109B: Swift-BAT refined analysis
DATE:    19/01/09 17:11:22 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

M. Stamatikos (OSU), S. D. Barthelmy (GSFC), J. R. Cummings (CPI),
H. A. Krimm (NSF/USRA), A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (AGU), B. Sbarufatti (PSU),
T. N. Ukwatta (LANL)   (i.e. the Swift-BAT team):
 
Using the data set from T-60 to T+243 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 190109B (trigger #882809)
(Sbarufatti, et al., GCN Circ. 23648).  The BAT ground-calculated position is
RA, Dec = 55.563, 63.592 deg, which is 
   RA(J2000)  =  03h 42m 15.1s 
   Dec(J2000) = +63d 35' 31.7" 
with an uncertainty of 1.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 60%.
 
The mask-weighted light curve shows a couple overlapping peaks starting at
~T-4sec, peaking at ~T+1 sec, and a shallow tail out to ~T+40 sec.
T90 (15-350 keV) is 5.92 +- 0.78 sec (estimated error including systematics).
 
The time-averaged spectrum from T-4.24 to T+3.31 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.58 +- 0.16.  The fluence in the 15-150 keV band is 4.8 +- 0.5 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T-0.12 sec in the 15-150 keV band
is 1.7 +- 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/882809/BA/


GRB_name: GRB190106A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23660
SUBJECT: GRB 190106A: Liverpool Telescope observations
DATE:    19/01/09 18:23:02 GMT
FROM:    Luca Izzo at IAA-CSIC  <luca.izzo@gmail.com>

L. Izzo, D. A. Kann (HETH-IAA/CSIC) A. de Ugarte Postigo (DARK/NBI & HETH-IAA/CSIC), M. Blazek, C. C. Thoene (HETH-IAA/CSIC) report:

We observed the field of GRB 190106A (Sonbas et al. GCN 23615) with the 2-m Liverpool Telescope located in La Palma, Spain. Observations started on January 6th at 21:10:35 UT (8.0 hours after the GRB trigger) and we obtained a series of 5x60s images in the g, r and i filters.

We clearly detect the optical afterglow (Lipunov  et al. GCN 23616, Itoh et al. GCN 23617, Mao et al. GCN 23618, Reva et al., GCN 23620, Xin et al. GCN 23622, Quadri et al. GCN 23624, Hu et al. GCN 23627, Noschese et al. GCN 23628) for which we measure the following magnitudes:

g = 19.47 +- 0.03
r = 18.90 +- 0.09
i = 18.49 +- 0.26

The calibration was performed using nearby SDSS stars.

[GCN OPS NOTE(09jan19): Per author's request, the first citation was changed from
"Deich et al.; GCN Circ. 22710" to "Sonbas et al. GCN 23615".]


GRB_name: GRB190106A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23661
SUBJECT: GRB 190106A: optical observations, possible jet break detection
DATE:    19/01/09 18:42:15 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

S. Belkin (IKI),  A. Pozanenko (IKI), P. Minaev (IKI), E. Klunko (ISTP), 
I. Reva (FAPI), M. Krugov (FAPI), V. Rumyantsev (CrAO), R. Ya. 
Inasaridze (AbAO), E. Mazaeva (IKI), A. Volnova (IKI)   report   on 
behalf of IKI-FuN:

We continue observations the optical afterglow (e.g. Lipunov  et al. 
GCN 23616, Itoh et al. GCN 23617, Mao et al. GCN 23618, Reva et al., GCN 
23620, Xin et al. GCN 23622, Quadri et al. GCN 23624, Hu et al. GCN 
23627)  of  the GRB 190106A (Sonbas et al., GCN 23615)  with AZT-33IK 
telescope of Sayan observatory (Mondy), Zeiss-1000 1-m telescope of Tien 
Shan Astronomical Observatory, and  AS-32 (0.7m) telescope of Abastumani 
Observatory.  Preliminary photometry of the afterglow is following.

Date       UT start t-T0    Filter Exp.   OT    Err. Observatory
                    (mid, days) (s)

2019-01-07 17:27:12 1.19251 R      63*60  20.27 0.08  AbAO
2019-01-08 11:07:16 1.91774 R      30*120 21.11 0.13  Mondy
2019-01-08 15:53:23 2.09628 R      12*120 21.1  0.3   CrAO


The photometry is based on nearby SDSS  stars
SDSS-DR12_id              R(Lupton)
J015920.22+235150.7 16.475
J015929.35+235237.5 15.774

Based on our previous results (GCNs 23620, 23638, 23640) and photometry 
above we plot a light curve  ( 
http://grb.rssi.ru/GRB190106A/GRB190106A_LC_R_fit.png ). We could 
suggest the jet break at 1.5 +/- 0.5 days.


GRB_name: GRB190109B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23662
SUBJECT: GRB 190109B: Swift-XRT refined Analysis
DATE:    19/01/09 19:58:19 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P.A. Evans (U. Leicester), A. Melandri (INAF-OAB), P. D'Avanzo
(INAF-OAB), V. D'Elia (ASDC), S. J. LaPorte (PSU), J.A. Kennea (PSU),
J.P. Osborne (U. Leicester), K.L. Page (U. Leicester) and B. Sbarufatti
report on behalf of the Swift-XRT team:

We have analysed 6.5 ks of XRT data for GRB 190109B (Sbarufatti et al.
GCN Circ. 23648), from 96 s to 18.3 ks after the  BAT trigger. The data
are entirely in Photon Counting (PC) mode. The enhanced XRT position
for this burst was given by Beardmore et al. (GCN Circ. 23652).

The light curve can be modelled with a power-law decay with a decay
index of alpha=0.97 (+/-0.06).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.04 (+0.27, -0.21). The
best-fitting absorption column is  5.1 (+1.6, -0.5) x 10^21 cm^-2,
consistent with the Galactic value of 4.6 x 10^21 cm^-2 (Willingale et
al. 2013). The counts to observed (unabsorbed) 0.3-10 keV flux
conversion factor deduced from this spectrum  is 4.0 x 10^-11 (6.7 x
10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      5.1 (+1.6, -0.5) x 10^21 cm^-2
Galactic foreground: 4.6 x 10^21 cm^-2
Excess significance: <1.6 sigma
Photon index:      2.04 (+0.27, -0.21)

If the light curve continues to decay with a power-law decay index of
0.97, the count rate at T+24 hours will be 2.2 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 8.7 x
10^-14 (1.5 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/00882809.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB190109A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23663
SUBJECT: GRB 190109A: Swift/UVOT Upper Limits
DATE:    19/01/09 20:36:24 GMT
FROM:    Kira Simpson at PSU  <kira.simpson1984@gmail.com>

GRB 190109A: Swift/UVOT Upper Limits

K. K. Simpson (PSU) and J. D. Gropp (PSU)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 190109A
181 s after the BAT trigger (Gropp et al., GCN Circ. 23642).
No optical afterglow consistent with the XRT position
(Osborne et al. GCN Circ. 23644)
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           181          331          147         >99.0
u_FC               340          590          246         >17.3
white              181        12997         1291         >99.0
v                  670         6867          490         >16.8
b                  596        18739         1727         >18.6
u                  340        24226         2551         >17.5
w1                 720        23954         2223         >17.4
m2                 695        23048         1357         >18.1
w2                 646         6662          491         >17.9

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.05 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB190109B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23664
SUBJECT: GRB 190109B: Swift/UVOT Upper Limits
DATE:    19/01/09 20:37:32 GMT
FROM:    Kira Simpson at PSU  <kira.simpson1984@gmail.com>

GRB 190109B: Swift/UVOT Upper Limits

K. K. Simpson (PSU) and B. Sbarufatti (PSU)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 190109B
91 s after the BAT trigger (Sbarufatti et al., GCN Circ. 23648).
No optical afterglow consistent with the XRT position
(Beardmore et al. GCN Circ. 23652)
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            91          241          147         >20.7
u_FC               303          553          246         >20.7
white               91         6461          727         >22.1
v                  634         6860          441         >20.4
b                  559         6256          432         >20.9
u                  303         6050          470         >21.0
w1                 683         5845          236         >20.2
m2                5440         5640          197         >20.8
w2                5030         6666          393         >20.2

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.72 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB190106A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23665
SUBJECT: GRB 190106A: OSN Afterglow Observations
DATE:    19/01/09 20:55:41 GMT
FROM:    Alexander Kann at IAA-CSIC  <kann@iaa.es>

M. Blazek, D. A. Kann (both HETH/IAA-CSIC), A. de Ugarte Postigo 
(HETH/IAA-CSIC and DARK/NBI), L. Izzo, and K. Bensch (all HETH/IAA-CSIC) 
report:

We observed the optical afterglow of GRB 190106A (e.g., Yurkov et al., 
GCN #23614), detected by Swift (Sonbas et al., GCN #23615), with with 
the T150 telescope of the Sierra Nevada Observatory (OSN). We obtained 
18 x 300 s images in the Ic band from 5.02 to 6.47 hours after the GRB. 
The afterglow is well-detected in each single image. We find it decays 
between the beginning and end of our observing run.

Days Ic mag error

0.2091 18.54 0.05
0.2696 18.73 0.06

Magnitudes are given in the AB system. They were measured vs. four SDSS 
comparison stars, using the transformation equations of Lupton (2005), 
and transformed back into AB mags.


GRB_name: GRB190109B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23666
SUBJECT: GRB 190109B: Fermi GBM observation
DATE:    19/01/09 23:30:49 GMT
FROM:    Cori Fletcher at USRA/NASA  <corinne.l.fletcher@nasa.gov>

C. Fletcher (USRA) and C. Meegan (UAH)
report on behalf of the Fermi GBM Team:

"At 11:56:10.76 UT on 09 January 2019, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 190109B (trigger 568727775 / 190109497)
which was also detected by the Swift (Sbarufatti et al. 2019, GCN 23648).
The GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight at the GBM trigger time is 46 degrees.

The GBM light curve consists of a single peak
with a duration (T90) of about 8 s (50-300 keV).
The time-averaged spectrum from T0-6.1 s to T0+3.1 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.85 +/- 0.25 and
the cutoff energy, parameterized as Epeak, is 92 +/- 14 keV.

The event fluence (10-1000 keV) in this time interval is
(6.76 +/- 0.67)E-7 erg/cm^2. The 1-sec peak photon flux measured
starting from T0-1.6 s in the 10-1000 keV band
is 2.8 +/- 0.2 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB190106A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23668
SUBJECT: GRB 190106A: GMG continued observation
DATE:    19/01/10 07:19:51 GMT
FROM:    Jirong Mao at Yunnan Obs  <jirongmao_obs@ynao.ac.cn>

J. Mao, X.-L. Zhang, J.-M. Bai (YNAO) report:


We still monitor the afterglow of GRB 190106A with the 2.4-meter optical telescope at Gao-Mei-Gu (GMG) station of Yunnan Observatories. The observation began at UT 13:57:39, 9th, Jan, 2019, about 72.2 hours after the trigger. We marginally detected the source. A very preliminary measurement provided a magnitude of R~21.2.


GRB_name: GRB181228A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23669
SUBJECT: GRB 181228A: FRAM-ORM optical limit
DATE:    19/01/10 07:26:40 GMT
FROM:    Martin Jelinek at Astro.Inst-AVCR,Ondrejov  <martin.jelinek@asu.cas.cz>

Martin Jelinek and 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 25cm robotic telescope FRAM-ORM at La Palma (Spain)
reacted robotically to the alert of GRB181228A (Moss et
al, GCNC 23570), obtaining a series of 20s R-band images
starting at 02:53:51.1UT, i.e. 34s post trigger.

We do not detect any new source in comparison to USNO-B1.0
catalog neither in single images (3-sigma limit R>~17.1)
nor in a combined 20x20s frame (mean exp time 269s post
trigger, 3-sigma limit R>~18.7).


Martin JelÃ­nek, +420602105255, +34617840945, lascaux.asu.cas.cz/mates
       AstronomickÃ½ Ãºstav AVÄŒR, OndÅ™ejov


GRB_name: GRB190110A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23670
SUBJECT: GRB 190110A: Swift detection of a burst
DATE:    19/01/10 17:34:23 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@milkyway.gsfc.nasa.gov>

B. Sbarufatti (PSU), S. D. Barthelmy (GSFC), J.D. Gropp (PSU),
J. A. Kennea (PSU), N. J. Klingler (PSU),
M. J. Moss (George Washington University), K. L. Page (U Leicester),
D. M. Palmer (LANL), M. H. Siegel (PSU) and A. Tohuvavohu (PSU) report
on behalf of the Neil Gehrels Swift Observatory Team:

At 17:24:48 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 190110A (trigger=883012).  Swift did not slew due to an observing
constraint.  The BAT on-board calculated location is 
RA, Dec 276.882, -53.676, which is 
   RA(J2000)  =  18h 27m 32s
   Dec(J2000) = -53d 40' 34"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows several peaks
with a total duration of about 15 sec.  The peak count rate
was ~7000 counts/sec (15-350 keV), at ~5 sec after the trigger. 

Due to a Sun observing constraint, Swift cannot slew to the BAT
position until 16:10 UT on 2019 February 01. There will thus be no XRT
or UVOT data for this trigger before this time. 

Burst Advocate for this burst is B. Sbarufatti (bxs60 AT psu.edu). 
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.)


GRB_name: GRB190110A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23671
SUBJECT: GRB 190110A: Fermi GBM detection
DATE:    19/01/11 05:34:52 GMT
FROM:    Suraj Poolakkil at UAH  <sp0076@uah.edu>

S.Poolakkil(UAH) and C. Meegan (UAH)
report on behalf of the Fermi GBM Team:

"At 17:24:49.21 UT on 10 January 2019, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 190110A(trigger 568833894/ 190110726),
which was also detected by the Swift/BAT (Sbarufatti et al. 2019, GCN
23670).
The GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight
at the GBM trigger time is 50 degrees.

The GBM light curve consists of a single bright peak
with a duration (T90) of about 9 s (50-300 keV).
The time-averaged spectrum from T0-2.04 s to T0+10.24 s is
best fit by a Band function with Epeak = 73 +/- 8 keV,
alpha = -0.44 +/- 0.20 and beta = -2.12 +/- 0.08.

The event fluence (10-1000 keV) in this time interval is
(5.331 +/- 0.209)E-06 erg/cm^2. The 1-sec peak photon flux
measured starting from T0+3.71 s in the 10-1000 keV band
is 14.7 +/- 0.3 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB190103A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23672
SUBJECT: Konus-Wind observation of GRB 190103A
DATE:    19/01/11 09:40:36 GMT
FROM:    Anastasia Tsvetkova at Ioffe Institute  <tsvetkova@mail.ioffe.ru>

A. Tsvetkova, S. Golenetskii, R.Aptekar, D. Frederiks,
M. Ulanov, D. Svinkin, A. Lysenko, A. Kozlova and T. Cline
on behalf of the Konus-Wind team, report:

The long-duration, intense GRB 190103A
(AGILE/MCAL detection: Ursi et al., GCN 23600;
AstroSat CZTI detection: Khanam et al., GCN 23609;
IPN triangulation: Hurley et al., GCN 23646)
triggered Konus-Wind at T0=60113.215 s UT (16:41:53.215).

The burst light curve shows two emission episodes
with a total duration of ~33 s.
The emission is seen up to ~16 MeV.

As observed by Konus-Wind, the burst
had a fluence of 7.14(-0.65,+0.68)x10^-5 erg/cm2,
and a 64-ms peak energy flux, measured from T0+21.648 s,
of 2.00(-0.30,+0.32)x10^-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum of the burst
(measured from T0 to T0+32.512 s)
is best fit in the 20 keV - 16 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.90(-0.07,+0.07),
the high energy photon index beta = -2.41(-0.24,+0.16),
the peak energy Ep = 304(-26,+28) keV,
chi2 = 85/97 dof.

The spectrum near the peak count rate
(measured from T0+21.504 to T0+24.320 s)
is best fit in the 20 keV - 3 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.76(-0.08,+0.09),
the high energy photon index beta = -2.39(-0.31,+0.20),
the peak energy Ep = 396(-46,+50) keV,
chi2 = 49/62 dof.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB190103_T60113/

All the quoted errors are at the 90% confidence level.
All the quoted values are preliminary.


GRB_name: GRB190109A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23673
SUBJECT: Correction to GCN Circular 23663: GRB 190109A: Swift UVOT Upper Limits
DATE:    19/01/11 15:01:41 GMT
FROM:    Kira Simpson at PSU  <kira.simpson1984@gmail.com>

The values for magnitude UVOT's white filter were listed as 99th magnitude
in the previous circular and have been corrected here.

GRB 190109A: Swift/UVOT Upper Limits

K. K. Simpson (PSU) and J. D. Gropp (PSU)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 190109A
181 s after the BAT trigger (Gropp et al., GCN Circ. 23642).
No optical afterglow consistent with the XRT position
(Osborne et al. GCN Circ. 23644)
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           181          331          147         >21.60
white              181        12997         1291         >20.27
v                  670         6867          490         >16.8
b                  596        18739         1727         >18.6
u                  340        24226         2551         >17.5
w1                 720        23954         2223         >17.4
m2                 695        23048         1357         >18.1
w2                 646         6662          491         >17.9

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.05 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB190110A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23674
SUBJECT: GRB 190110A, Swift-BAT refined analysis
DATE:    19/01/11 20:23:05 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

T. N. Ukwatta (LANL), S. D. Barthelmy (GSFC),
J. R. Cummings (CPI), H. A. Krimm (NSF/USRA),
A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (AGU),
B. Sbarufatti (PSU), M. Stamatikos (OSU)
(i.e. the Swift-BAT team):

Using the data set from T-240 to T+180 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 190110A (trigger #883012)
(Sbarufatti et al., GCN Circ. 23670).  The BAT ground-calculated position is
RA, Dec = 276.939, -53.643 deg which is
  RA(J2000)  =  18h 27m 45.3s
  Dec(J2000) = -53d 38' 34.3"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 43%.

The mask-weighted light curve shows several overlapping peaks that starts at
~ T-1 s and ends at ~ T+11 s. The main peak occurs at ~T+5 s. T90 (15-350 keV)
is 9.3 +- 0.8 sec (estimated error including systematics).

The time-averaged spectrum from T-0.8 to T+11.0 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.66 +- 0.07.  The fluence in the 15-150 keV band is 2.5 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+4.66 sec in the 15-150 keV band
is 9.0 +- 0.5 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/883012/BA/


GRB_name: GRB190110A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23675
SUBJECT: Konus-Wind observation of GRB 190110A
DATE:    19/01/12 21:29:13 GMT
FROM:    Anna Kozlova at Ioffe Institute  <ann_kozlova@mail.ioffe.ru>

A. Kozlova, S. Golenetskii, R. Aptekar, D. Frederiks,
M. Ulanov, D. Svinkin, A. Tsvetkova, A. Lysenko, and T. Cline
on behalf of the Konus-Wind team, report:

The long-duration GRB 190110A
(Swift-BAT detection and analysis: Sbarufatti et al., GCN Circ. 23670;
Ukwatta et al., GCN Circ. 23674;
Fermi-GBM detection: Poolakkil & Meegan, GCN Circ. 23671)
triggered Konus-Wind at T0=62689.767 s UT (17:24:49.767).

The burst light curve shows a single pulse
started at ~T0-3.5 s with a total duration of ~5 s.
The emission is seen up to ~8 MeV.

As observed by Konus-Wind, the burst
had a fluence of 3.39(-0.51,+0.88)x10^-6 erg/cm2,
and a 64-ms peak flux, measured from T0+0.158 s,
of 2.21(-0.93,+1.71)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 - 8 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = -1.44(-0.46,+0.58)
and Ep = 132(-60,+111) keV (chi2 = 62/81 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.4
(chi2 = 62/80 dof).

The spectrum near the maximum count rate
(measured from T0+0.128 to T0+0.256 s)
is best fit in the 20 keV - 8 MeV range
by a power law with exponential cutoff model
with  alpha = -0.87(-0.82,+1.27)
and Ep = 165(-53,+382) keV (chi2 = 12/18 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.0
(chi2 = 12/17 dof).

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB190110_T62689/

All the quoted errors are at the 90% confidence level.
All the quoted values are preliminary.


GRB_name: GRB190114A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23677
SUBJECT: GRB 190114A: Swift detection of a burst
DATE:    19/01/14 03:25:02 GMT
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.)


GRB_name: GRB190114A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23678
SUBJECT: GRB 190114A: Possible UVOT Detection
DATE:    19/01/14 03:41:48 GMT
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. 


GRB_name: GRB190114A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23679
SUBJECT: GRB 190114A: Prompt enhanced Swift-XRT position
DATE:    19/01/14 03:52:27 GMT
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.


GRB_name: GRB190114A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23680
SUBJECT: GRB 190114A: VLT/X-shooter redshift
DATE:    19/01/14 06:26:51 GMT
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.


GRB_name: GRB190114A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23681
SUBJECT: GRB 190114A: Enhanced Swift-XRT position
DATE:    19/01/14 07:24:20 GMT
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.


GRB_name: GRB190114A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23682
SUBJECT: GRB 190114A: GROND detection of the afterglow
DATE:    19/01/14 09:21:12 GMT
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) = 4:22:10.58
DEC (J2000) = +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).


GRB_name: GRB190114A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23683
SUBJECT: GRB 190114A: Swift-XRT refined Analysis
DATE:    19/01/14 11:21:34 GMT
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.


GRB_name: GRB190103B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23684
SUBJECT: GRB 190103B: Swift/UVOT Upper Limits
DATE:    19/01/14 15:53:58 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

A. A. Breeveld (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 190103B
103 s after the BAT trigger (Lien et al., GCN Circ. 23602).
No optical afterglow consistent with the XRT position (Evans et al. GCN
Circ. 23603) 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           103          253          147         >20.5
u_FC               316          565          246         >19.5
white              103        23827         1860         >21.8
v                  646        40393         2202         >20.6
b                  571        46547         2987         >21.5
u                  316        46101         3922         >21.3
w1                4776        45188         3715         >21.2
m2                4570        41036         2792         >21.1
w2                4161        39480         1904         >21.0

The magnitudes in the table are not corrected for the Galactic
extinction due to the reddening of E(B-V) = 0.01 in the direction of the
burst (Schlegel et al. 1998).


GRB_name: GRB190114A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23685
SUBJECT: GRB 190114A: Swift-BAT refined analysis
DATE:    19/01/14 18:36:28 GMT
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/


GRB_name: GRB190114B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23686
SUBJECT: GRB 190114B: Swift detection of a burst
DATE:    19/01/14 19:48:11 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

M. H. Siegel (PSU), D. N. Burrows (PSU), J.D. Gropp (PSU),
J. A. Kennea (PSU), N. J. Klingler (PSU), H. A. Krimm (NSF/USRA),
N. P. M. Kuin (UCL-MSSL), S. J. LaPorte (PSU), A. Y. Lien (GSFC/UMBC),
M. J. Moss (George Washington University), K. L. Page (U Leicester),
B. Sbarufatti (PSU) and A. Tohuvavohu (PSU) report on behalf of the
Neil Gehrels Swift Observatory Team:

At 19:31:12 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 190114B (trigger=883818).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 174.883, +18.877 which is 
   RA(J2000) = 11h 39m 32s
   Dec(J2000) = +18d 52' 36"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a weak pulse
with a duration of about 20 sec. Also, there is a possible precursor
at ~T-75 s. The peak count rate was ~800 counts/sec (15-350 keV), 
at ~4 sec after the trigger. 

The XRT began observing the field at 19:33:49.6 UT, 157.5 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source located at RA, Dec 174.87349, 18.89230 which
is equivalent to:
   RA(J2000)  = 11h 39m 29.64s
   Dec(J2000) = +18d 53' 32.3"
with an uncertainty of 3.7 arcseconds (radius, 90% containment). This
location is 63 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 consistent with the Galactic value of 1.75
x 10^20 cm^-2 (Willingale et al. 2013). 

UVOT took a finding chart exposure of 250 seconds with the U filter starting
157 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 19.2 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 18.0 mag. No
correction has been made for the expected extinction corresponding to E(B-V) of
0.02. 

Burst Advocate for this burst is M. H. Siegel (siegel AT swift.psu.edu). 
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.)


GRB_name: GRB190114A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23687
SUBJECT: GRB 190114A: OSN Detection
DATE:    19/01/14 20:48:52 GMT
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.


GRB_name: GRB190114C
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23688
SUBJECT: GRB 190114C: Swift detection of a very bright burst with a bright optical counterpart
DATE:    19/01/14 21:17:08 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

J.D. Gropp (PSU), J. A. Kennea (PSU), N. J. Klingler (PSU),
H. A. Krimm (NSF/USRA), S. J. LaPorte (PSU), A. Y. Lien (GSFC/UMBC),
M. J. Moss (George Washington University), D. M. Palmer (LANL),
B. Sbarufatti (PSU) and M. H. Siegel (PSU) report on behalf of the
Neil Gehrels Swift Observatory Team:

At 20:57:03 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 190114C (trigger=883832).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 54.510, -26.939 which is 
   RA(J2000) = 03h 38m 02s
   Dec(J2000) = -26d 56' 18"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a very bright
multi-peaked structure with a total duration of about 25 sec.  The
peak count rate was ~200000 counts/sec (15-350 keV), at ~2 sec after the trigger. 

The XRT began observing the field at 20:58:07.1 UT, 64.0 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 54.5068, -26.9467 which is equivalent to:
   RA(J2000)  = 03h 38m 1.63s
   Dec(J2000) = -26d 56' 48.1"
with an uncertainty of 5.0 arcseconds (radius, 90% containment). This
location is 29 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 0.1 s image was 7.39e-08 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White
filter  starting 73 seconds after the BAT trigger. There is a
candidate afterglow in  the rapidly available 2.7'x2.7' sub-image. We
can not provide a refined position due to a failed aspect correction. 
The estimated magnitude is 15.60 with a 1-sigma error of about  0.02. 
No correction has been made for the expected extinction corresponding
to E(B-V) of 0.01. 

Burst Advocate for this burst is J.D. Gropp (jdg44 AT psu.edu). 
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.)


GRB_name: GRB190114C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23690
SUBJECT: GRB 190114C: MASTER afterglow  Detection
DATE:    19/01/14 21:39:56 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

N.Tyurina, V. Lipunov, A.Kuznetsov, E. Gorbovskoy, V.Kornilov, 
D.Kuvshinov, P.Balanutsa,D. Vlasenko
Lomonosov Moscow State University,
Sternberg Astronomical Institute, Moscow State University


V. Yurkov, A. Gabovich, Yu. Sergienko, D. Kobcev
Blagoveschensk Educational State University, Blagoveschensk

A. Tlatov, V.Senik, A.V. Parhomenko, D. Dormidontov
Kislovodsk Solar Station of the Pulkovo Observatory

K. Ivanov, O. Gres, N.M. Budnev, S. Yazev, O. Chuvalaev, V. Poleshchuk
Irkutsk State University

R. Podesta, Carlos Lopez and F. Podesta
Observatorio Astronomico Felix Aguilar (OAFA)

Hugo Levato and Carlos Saffe
Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE)

R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres
The Instituto de Astrofisica de Canarias

D. Buckley, S. Potter, A. Kniazev, M. Kotze
South African Astronomical Observatory

MASTER-IAC robotic telescope (Global MASTER-Net: 
http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, 
vol. 2010, 30L) located in Spain (IAC Teide Observatory) was pointed to 
the  GRB190114.87 25 sec after notice time and 47 sec after trigger time 
at 2019-01-14 20:57:51 UT. On our first (10s exposure)  set we  found 1 
optical transient within SWIFT error-box (ra=54.5042 dec=-26.9383 r=0.05) 
brighter than 16.54.


  T-Tmid      Date      Time       Expt.        Ra                Dec 
Mag
---------|---------------------|-------|-----------------|-----------------|-------
       52   2019-01-14 20:57:51      10   (  3h 38m 01.17s , -26d 56m 46.73s)    11.21

The 5-sigma upper limit has been about 16.54mag
The message may be cited.


GRB_name: GRB190114B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23691
SUBJECT: GRB 190114B: Enhanced Swift-XRT position
DATE:    19/01/14 21:53:07 GMT
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 1925 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 190114B, 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 = 174.87422, +18.89079 which is equivalent
to:

RA (J2000): 11h 39m 29.81s
Dec (J2000): +18d 53' 26.9"

with an uncertainty of 2.3 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.


GRB_name: GRB190114C
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23692
SUBJECT: GRB 190114C: Possible host galaxy in Pan-STARRS
DATE:    19/01/14 21:59:08 GMT
FROM:    Alexander Kann at IAA-CSIC  <kann@iaa.es>

A. de Ugarte Postigo (HETH/IAA-CSIC and DARK/NBI), D. A. Kann, C. C. 
Thoene, and L. Izzo (both HETH/IAA-CSIC) report:

At the position of the ultra-bright GRB 190114C (Gropp et al., GCN 
#23688, Tyurana et al., GCN #23690), we detect a source in Pan-STARRS 
archival imaging with:

r' = 21.229 +/- 0.156 mag,
i' = 21.574 +/- 0.198 mag,
z' = 20.994 +/- 0.179 mag.

We suggest this source is the host galaxy of GRB 190114C, and that it is 
at low-z. We note this GRB is similar to GRB 130427A, being about half 
as bright in INTEGRAL SPI-ACS counts.


GRB_name: GRB190114C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23693
SUBJECT: GRB 190114C: MASTER 4-polarizations filters OT detection
DATE:    19/01/14 22:14:54 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, N.Tyurina, A.Kuznetsov, E. Gorbovskoy, V.Kornilov, 
D.Kuvshinov, P.Balanutsa,D. Vlasenko, V.Vladimirov, A.Kuznetsov,
A. Chasovnikov
Lomonosov Moscow State University,
Sternberg Astronomical Institute, Moscow State University

R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres
The Instituto de Astrofisica de Canarias

D. Buckley, S. Potter, 
South African Astronomical Observatory

V. Yurkov, A. Gabovich, Yu. Sergienko, D. Kobcev
Blagoveschensk Educational State University, Blagoveschensk

A. Tlatov, V.Senik, A.V. Parhomenko, D. Dormidontov
Kislovodsk Solar Station of the Pulkovo Observatory

O. Gres, N.M. Budnev, S. Yazev, O. Chuvalaev, V. Poleshchuk
Irkutsk State University

R. Podesta, C. Lopez, C.Francile, F. Podesta
Observatorio Astronomico Felix Aguilar (OAFA)

Hugo Levato 
Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE)


MASTER-SAAO robotic telescope (Global MASTER-Net: 
http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, 
vol. 2010, 30L) located in South Africa (South African Astronomical 
Observatory) was pointed to the  GRB190114C  (Gropp et al., GCN 23688) 
24 sec after notice time and 45 sec after trigger time
at 2019-01-14 20:57:48 UT. On our first (10s 
exposure in two polarization)  set we  found 1 optical transient (Tiurina 
et al., GCN 23690) within SWIFT error-box (ra=54.5042 dec=-26.9383 r=0.05)
brighter than 17.3 .


  T-Tmid      Date      Time       Expt.        Ra                Dec           Mag
--------|--------------------|-------|-----------------|-----------------|-------
     50    2019-01-14 20:57:48    10   (03h 38m 01.15s , -26d 56m 47.07s)    11.10

The 5-sigma upper limit has been about 17.32mag

Taking into account the observations on the MASTER-IAC at Canaries 
(Tiurina et al., GCN 23690) , we have a polarization photometry  in 4-position angles!

The message may be cited.


====================================================================


The galactic latitude b = -53 deg., longitude l = 222 deg.
The observations made on zenit distance = 31 deg.The moon (56 % bright 
part) is 22 deg. above the horizon. The distance between  moon and  object 
is 41
The sun  altitude  is -30.6 deg.
The object can be observed till 2019-01-15 01:56:12
.


The 5-sigma upper limit has been about 16.54mag
The message may be cited.


GRB_name: GRB190114B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23694
SUBJECT: GRB 190114B: BOOTES-4/MET optical afterglow detection
DATE:    19/01/14 22:31:44 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

E. Fernandez-Garcia, Y.-D. Hu, X.-Y.Li, , A. Ayala, A. J. Castro-Tirado 
(IAA-CSIC), C. Perez del Pulgar, A. Castellon, I. Carrasco (Univ. de 
Malaga),  and D. Xiong, Y. Fan, X. Zhao, J. Bai, C. Wang, Y. Xin (Yunnan 
Nacional Astronomical Observatory) on behalf of a larger collaboration, 
report:

"Following the detection of GRB 190114B by Swift/BAT (Siegel et al. GCNC 
23686), the 0.6m BOOTES-4/MET robotic telescope at Lijiang Astronomical 
Observatory (China) obtained follow-up  observations starting at 
19:53:24 UT (~0.37 hr after trigger). Within the enhaced Swift/XRT 
position (Goad et al. GCNC 23691) an optical source with a preliminary 
magnitude of 20.3 mag (clear filter) is detected, fading in brightness 
in the late-time images, which we suggest as the optical afterglow to 
GRB 190114B at coordinates (J2000) RA = 11:39:29.81, Dec =+18:53:28.1 
(+/- 1"). Observations are ongoing."


GRB_name: GRB190114C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23695
SUBJECT: GRB 190114C: NOT optical counterpart and redshift
DATE:    19/01/14 22:45:48 GMT
FROM:    Jonatan Selsing at DARK/NBI  <jselsing@dark-cosmology.dk>

J. Selsing (DAWN/NBI and DAWN/DTU), J.P.U. Fynbo (DAWN/NBI and
DAWN/DTU), K.E. Heintz (Univ. of Iceland), D. Watson (DAWN/NBI and
DAWN/DTU), and S. Dyrbye (NOT), report on behalf of a larger
collaboration:

We observed the optical afterglow of GRB 190114C (Gropp et al., GCN
23688; Tyurina et al., GCN 23690, de Ugarte Postigo et al., GCN 23692,
Lipunov et al. GCN 23693) with the 2.5-m Nordic Optical Telescope (NOT)
equipped with the Alfosc instument. We have carried out a series of 300s
griz observations, starting at 21:26:28 UT, January 14th - 29 minutes
after the BAT trigger. The optical counterpart is very clearly detected.

We have calibrated the photometric zeropoint against the Pan-STARRS
catalog and derive the following magnitudes for the afterglow:

g = 17.72 +- 0.11 AB mag 
r = 16.90 +- 0.04 AB mag 
i = 16.40 +- 0.02 AB mag 
z = 16.25 +- 0.12 AB mag

We immediately followed up with spectroscopic observations using the
Alfosc instrument, in which the afterglow is very clearly detected. From
the detection of strong absorption lines from Ca H & K along with Na ID
in the afterglow spectrum, we derive a redshift of z = 0.42, which we
suggest is the redshift of the GRB.

[GCN OPS NOTE(15jan19): Per author's request, Dyrbye was moved from the
last paragraph to the author list.]


GRB_name: GRB190114B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23696
SUBJECT: GRB 190114B: Mondy optical afterglow detection
DATE:    19/01/14 22:46:53 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Pozanenko (IKI), E. Klunko (ISTP), E. Mazaeva (IKI), A. Volnova (IKI), S. 
Belkin (IKI)  report   on behalf of IKI-FuN:

We observed the field of  the GRB  190114B (Siegel et al., GCN 23686)  with 
AZT-33IK telescope of Sayan observatory (Mondy).   We started observations 
on Jan. 14 (UT) 20:28:30, i.e. 57 minutes   after burst trigger.   Within 
the enhanced XRT position (Goad et al., GCN 23691) we detect the object 
which is absent in SDSS catalog. Coordinates of the object are (J2000) 
11:39:29.84 +18:53:27.8 with uncertainty 0.5 arcsec in both coordinates. The 
brightens of the object is R ~ 20.1m at (UT) 20:28:30. We suggest the object 
is the afterglow of GRB  190114B. The photometry is based on nearby SDSS 
DR12 stars, Lupton transformation.
. 


GRB_name: GRB190114A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23697
SUBJECT: GRB 190114A: NOT optical observations
DATE:    19/01/15 00:24:42 GMT
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.]


GRB_name: GRB150114C
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23698
SUBJECT: GRB 150114C#: Planned XMM-Newton observation
DATE:    19/01/15 00:56:14 GMT
FROM:    Norbert Schartel at XMM-Newton/ESA  <too@xmm.esac.esa.int>

XMM-Newton will observe GRB 150114C at location

RA=03h 38m 01.6s, DEC=-26d 56' 48", J2000

starting at 04:45 UT, on January 15, 2019,
for an exposure of 55000 seconds.




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protected content. Any unauthorised disclosure, use, retention or dissemination is prohibited. If you have received
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GRB_name: GRB190114C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23699
SUBJECT: GRB 190114C: OASDG optical observations
DATE:    19/01/15 01:01:57 GMT
FROM:    Luca Izzo at IAA-CSIC  <luca.izzo@gmail.com>

L. Izzo (HETH/IAA-CSIC), A. Noschese, L. Dâ€™Avino and M. Mollica (AC-OASDG) report:

We observed the field of GRB 190114C (Gropp et al. GCN 23688) with the 0.5m telescope of the Osservatorio Astronomico S. Di Giacomo located in Agerola, Italy ( https://goo.gl/Dqvqhf ). Observations were carried out under bad weather conditions and with the GRB position initially at 15 degrees above the horizon.

We obtained a series of 180 s images in the Rc filter, starting at 21:29:23 UT, ~ 0.54 hrs after the GRB detection. The GRB is clearly detected in the first image at the position of the observed optical counterpart (Tyurina et al. GCN 23690, Lipunov et al. GCN 23693, Selsing et al GCN 23695), but it is rapidly fading in the following images. We have stacked our set of images in groups of two images each, measuring the following magnitudes (AB):

Time   Rc          dRc
(hrs)   (mag)     (mag)

0.54   16.86      0.07
0.65   17.06      0.07
0.74   17.21      0.08
0.86   17.27      0.08
0.97   17.47      0.09
1.07   17.69      0.10

The calibration was performed using nearby stars in the Pan-STARRS PS1 catalog and using transformation equations to Rc magnitudes.


GRB_name: GRB190114C
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23700
SUBJECT: CORRECTED TARGET NAME: GRB 190114C: Planned XMM-Newton observation
DATE:    19/01/15 01:08:23 GMT
FROM:    Norbert Schartel at XMM-Newton/ESA  <too@xmm.esac.esa.int>

XMM-Newton will observe GRB 190114C at location
(RA=03h 38m 01.2s, DEC=-26d 56' 47", J2000),
starting at 04:45 UT, on January 15 2019,
for an exposure of 55000 seconds.




This message is intended only for the recipient(s) named above. It may contain proprietary information and/or
protected content. Any unauthorised disclosure, use, retention or dissemination is prohibited. If you have received
this e-mail in error, please notify the sender immediately. ESA applies appropriate organisational measures to protect
personal data, in case of data privacy queries, please contact the ESA Data Protection Officer (dpo@esa.int).


GRB_name: GRB190114C
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23701
SUBJECT: MAGIC detects the GRB 190114C in the TeV energy domain
DATE:    19/01/15 01:56:36 GMT
FROM:    Razmik Mirzoyan at MPI/MAGIC  <Razmik.Mirzoyan@mpp.mpg.de>

R. Mirzoyan (MPP Munich), K. Noda (ICRR University of Tokyo), 

E. Moretti (IFAE Barcelona), A. Berti (University and INFN Torino), 

C. Nigro (DESY Zeuthen), J. Hoang (UCM Madrid), S. Micanovic 

(University of Rijeka), M. Takahashi (ICRR University of Tokyo), 

Y. Chai (MPP Munich), A. Moralejo (IFAE Barcelona) and the MAGIC

Collaboration report:

 

On January 14, 2019, the MAGIC telescopes located at the Observatorio 

Roque de los Muchachos on the Canary island of La Palma, detected 

very-high-energy gamma-ray emission from GRB 190114C (Gropp et al., 

GCN 23688; Tyurina et al., GCN 23690, de Ugarte Postigo et al., GCN 

23692, Lipunov et al. GCN 23693, J. Selsing et al. GCN 23695). 
The observation was triggered by the Swift-BAT alert and it started about 

50s after the Swift T0: 20:57:03.19. 

The GRB data of MAGIC shows a clear excess of gamma-ray events with the 

significance >20 sigma in the first 20 min (starting at T0+50s) for energies


>300GeV. The relatively high detection threshold is due to the large zenith 

angle of observations (~60 deg.) and the presence of partial moon. After 

the first bright flash the source is quickly fading.

The MAGIC point of contact for this burst is R. Mirzoyan
(Razmik.Mirzoyan@mpp.mpg.de). 

Burst Advocate for this burst is K. Noda ( <mailto:nodak@icrr.u-tokyo.ac.jp>
nodak@icrr.u-tokyo.ac.jp)

 

 


GRB_name: GRB190114C
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23702
SUBJECT: GRB 190114C: GROND detection of the afterglow
DATE:    19/01/15 01:58:25 GMT
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 190114C (Swift trigger 883832; Gropp et al., GCN #23688) 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 the ESO
La Silla Observatory (Chile).

Observations started at 00:48 UT on 15th January, around 3.8 hours after the GRB trigger. They were performed
at an average seeing of 1.0" and at an average airmass of 1.0. 

We found a source consistent with the one reported by Selsing et al., GCN #23695.

Based on the first 5.8 min of exposure in g'r'i'z', and 8.0 min in JHK, we report the
following preliminary AB magnitudes:  

g =  19.00 +/- 0.09 mag
r = 18.17 +/-  0.03  mag
i =  17.66 +/- 0.05 mag
z = 17.15 +/-  0.04 mag
J = 16.76 +/- 0.05 mag
H = 16.30 +/- 0.05 mag
K = 16.08 +/- 0.07 mag

The above magnitudes are calibrated against PanSTARRS and 2MASS and are not corrected for the expected
Galactic foreground extinction corresponding to a reddening of E_(B-V)=0.01 in the direction
of the burst (Schlafly & Finkbeiner 2011).


GRB_name: GRB190114B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23703
SUBJECT: GRB 190114B: GWAC-F60B upper limit
DATE:    19/01/15 03:15:45 GMT
FROM:    L.P. Xin at NAOC  <xlp@nao.cas.cn>

L. P. Xin,  Y. J. Xiao, P. P. Zhang, R. S. Zhang,  J. Wang,   J. Y. Wei,   
E. W. Liang,  X. G. Wang,    Y. G. Yang,  X. M. Lu,  L. Huang,    H. B. Cai,   
Y. L. Qiu,  Y. Xu, Y.  J. Xiao, Y. T. Zheng,  C. Wu,   J. S. Deng,  D. W. Xu, 
D. TURPIN, H. L. Li, and W. L. Dong, report:

We  started to observe  GRB 190114B  ( Siegel et al., GCN 23686 )  
with  GWAC-F60B 60cm optical telescope  at 19:46:26 UT, 
Jan. 14th  2019,  about 14  min after the burst. 

The afterglow reported by ( Goad et al., GCN 23691;  Fernandez-Garcia et al., GCN 23694; 
Pozanenko et al., GCN 23696) was not detected  in R band images.  
The upper limit is estimated to be about 18.3 mag  calibrated by nearby USNO-B1.0 stars.

GWAC-F60B is operated by Guangxi university and NAOC, CAS, at Xinglong observatory, China.

The message may be cited.


GRB_name: GRB190114C
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23704
SUBJECT: GRB 190114C: Enhanced Swift-XRT position
DATE:    19/01/15 05:31:58 GMT
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 4709 s of XRT Photon Counting mode data and 12 UVOT
images for GRB 190114C, 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 = 54.50499, -26.94657 which is equivalent
to:

RA (J2000): 03h 38m 1.20s
Dec (J2000): -26d 56' 47.6"

with an uncertainty of 1.4 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.


GRB_name: GRB190114B
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23705
SUBJECT: GRB 190114B: MITSuME Akeno optical upper limits
DATE:    19/01/15 05:48:16 GMT
FROM:    Ryosuke Itoh at Tokyo Institute of Tech.  <itoh@hp.phys.titech.ac.jp>

R. Itoh, K. L. Murata, Y. Tachibana, S. Harita, K. Morita,
K. Shiraishi, K. Iida, M. Niwano, R. Adachi, M. Oeda,  Y. Yatsu,
and N. Kawai (Tokyo Tech) report on behalf of the MITSuME collaboration

We searched for the optical counterpart of
GRB 190114B (M. Siegel et al., GCN #23686)
with the optical three color (g', Rc, and Ic)
CCD cameras attached to the MITSuME 50 cm telescope at Akeno
Observatory,Yamanashi, Japan.

The observation started on 19:33:01 UT which corresponds to 109 sec
after the trigger.
We did not find any new point source within the enhanced XRT circle
(Goad et al., GCN #23691;  Fernandez-Garcia et al., GCN #23694;
Pozanenko et al., GCN #23696; Xin et al., GCN #23703) in all three bands.
We obtained following 5 sigma limits for the magnitudes.

T0+[sec]    MID-UT      T-EXP[sec]    g'       Rc        Ic
-------------------------------------------------------------------------------------------------------
109  19:37:35    480    >19.4     >18.7     >18.2
-------------------------------------------------------------------------------------------------------
T0+ : Elapsed time after the burst
T-EXP: Total Exposure time
We used UCAC-4 catalog for flux calibration.


GRB_name: GRB190114C
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23706
SUBJECT: GRB 190114C: Swift-XRT refined Analysis
DATE:    19/01/15 05:58:56 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

V. D'Elia (ASDC), A. D'Ai (INAF-IASFPA), B. Sbarufatti (INAF-OAB/PSU),
D.N. Burrows (PSU), A. Tohuvavohu (PSU), K.L. Page (U. Leicester), A.P.
Beardmore (U. Leicester), P.A. Evans (U. Leicester), A. Melandri
(INAF-OAB) and J.D. Gropp report on behalf of the Swift-XRT team:

We have analysed 7.3 ks of XRT data for GRB 190114C (Gropp et al. GCN
Circ. 23688), from 67 s to 23.2 ks after the  BAT trigger. The data
comprise 1.1 ks in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The enhanced XRT position for this burst was
given by Osborne et al. (GCN Circ. 23704).

The late-time light curve (from T0+3.8 ks) can be modelled with a
power-law decay with a decay index of alpha=2.7 (+1.1, -2.2).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index  of 1.66 (+/-0.04). The
best-fitting absorption column is  8.19 (+0.24, -0.23) x 10^22 cm^-2,
at a redshift of 0.42, in addition to the Galactic value of 7.5 x 10^19
cm^-2 (Willingale et al. 2013). The PC mode spectrum has a photon index
of 1.84 (+0.14, -0.13) and a best-fitting absorption column of 8.1
(+0.8, -0.7) x 10^22 cm^-2. The counts to observed (unabsorbed) 0.3-10
keV flux conversion factor deduced from this spectrum  is 7.6 x 10^-11
(1.6 x 10^-10) erg cm^-2 count^-1.

A summary of the PC-mode spectrum is thus:
Galactic foreground: 7.5 x 10^19 cm^-2
Intrinsic column:    8.1 (+0.8, -0.7) x 10^22 cm^-2 at z=0.42
Photon index:        1.84 (+0.14, -0.13)

If the light curve continues to decay with a power-law decay index of
2.7, the count rate at T+24 hours will be 1.4 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.1 x
10^-13 (2.4 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/00883832.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB190114C
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23707
SUBJECT: GRB 190114C: Fermi GBM detection
DATE:    19/01/15 05:59:42 GMT
FROM:    Rachel Hamburg at UAH  <rkh0007@uah.edu>

R. Hamburg (UAH), P. Veres (UAH), C. Meegan (UAH), E. Burns (GSFC),
V. Connaughton (USRA), A. Goldstein (USRA), D. Kocevski, and O.J. Roberts
(USRA)
report on behalf of the Fermi GBM Team:

"At 20:57:02.63 UT on 14 January 2019, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 190114C (trigger 569192227 / 190114873)
which was also detected by the Swift/BAT (Gropp et al. 2019, GCN 23688),
MASTER (Tyurina et al. 2019, GCN 23690; Lipunov et al. 2019, GCN 23693),
Pan-STARRS (de Ugarte Postigo et al. 2019, GCN 23692), NOT
(Selsing et al. 2019, GCN 23695), OASDG (Izzo et al. 2019, GCN 23699),
and GROND (Bolmer et al. 2019, GCN 23702) optical telescopes, and at
Very High Energy (VHE) by the MAGIC telescope (Mirzoyan et al. 2019,
GCN 23701). The GBM on-ground location is consistent with the Swift/BAT
position.

The angle from the Fermi LAT boresight at the GBM trigger time is 68
degrees.

The GBM light curve shows a very bright, multi-peaked pulse starting from
about T0+0 s to T0+15 s and is followed by a weaker pulse occurring at
approximately T0+15 s to T0+25 s. There is also evidence of fainter
emission
lasting to about T0+200 s. The calculated duration (T90) is about
116 s (50-300 keV). The time-averaged spectrum from T0-0.00 s to
T0+38.59 s can be fit by a Band function with Epeak = 998.6 +/- 11.9 keV,
alpha = -1.058 +/- 0.003, and beta = -3.18 +/- 0.07. The event fluence
(10-1000 keV) in this time interval is (3.99E-04 +/- 8.10E-07) erg/cm^2.
The 1-sec peak photon flux measured starting from T0+3.84 s in the 10-1000
keV band is 246.86 +/- 0.86 ph/s/cm^2.

Using the Band spectral fit and the distance measure of
z = 0.42 (Selsing et al. 2019), we calculate the energetics of GRB 190114C.
We estimate that the isotropic energy release in gamma-rays Eiso = 3E53
erg,
and the isotropic peak luminosity Liso = 1E53 erg/s,
in the 1 keV â€“ 10 MeV energy band.

Preliminary spectral analysis shows a strong statistical preference for an
extra power-law component, previously seen in some bright bursts.
The TeV observations by MAGIC and the optical polarization observations by
MASTER begin at about T0+50 s. This is well after the main peaks observed
in GBM, but significant GBM emission is evident out to about 200 s,
covering
the start of these observations.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB190114C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23708
SUBJECT: GRB 190114C: refined redshift by the 10.4m GTC
DATE:    19/01/15 06:38:04 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

A. J. Castro-Tirado. Y. Hu, E. Fernandez-Garcia (IAA-CSIC), A. Valeev, 
V. Sokolov (SAO-RAS), S. Guziy (Univ. of Nikolaev), S. Oates (U. 
Warwick) S. Jeong (SKKU), S. B. Pandey (ARIES), I. Carrasco (Univ. de 
MÃ¡laga) and D. Reverte-Paya (GRANTECAN, IAC, ULL), on behalf of a larger 
collaboration, report:

"Following the detection of the ultra-bright GRB 190114C (Gropp et al. 
GCN 23688, Hamburg et al. GCN 23707), also recorded at very-high 
gamma-ray energies (Mirzoyan et al. GCN 23701), optical spectroscopy of 
the reported optical afterglow (Gropp et al., GCN 23688; Tyurina et al. 
GCN 23690; Lipunov et al. GCN 23693; Selsing et al., GCN 23695; Izzo et 
al., GCN 23699; Bolmer et al., GCN 23702) has been undertaken at the 
10.4m GTC telescope (+OSIRIS) at the Spanish island of La Palma starting 
on Jan 14, 23:32 UT (2.6 hr post-burst). The two spectra (600s each, at 
high airmass) covered the range 3,700-9.600 A and the detection of Ca H 
& K lines and the Na I doublet (as well as other Fraunhofer lines) 
confirms the redshift value reported by Selsing et al. (GCN 23695) which 
we refine to z = 0.4245 +/- 0.0005, supporting the association with the 
galaxy detected in the Pan-STARRS archival data (de Ugarte Postigo et 
al. GCN 23692).

We acknowledge the excellent support of the GTC staff."


GRB_name: GRB190114C
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23709
SUBJECT: GRB 190114C: Fermi-LAT detection
DATE:    19/01/15 07:23:42 GMT
FROM:    Magnus Axelsson at Stockholm U.  <magaxe@kth.se>

D. Kocevski, N. Omodei (Stanford U.), M. Axelsson (KTH & Stockholm Univ.), E. Burns (NASA/GSFC), G. Vianello (Stanford U.), E. Bissaldi (Politecnico & INFN Bari) and F. Longo (University and INFN Trieste) report on behalf of the Fermi-LAT team:

On January, 14, 2019, Fermi-LAT detected high-energy emission from GRB 190114C, which was also detected by the Fermi GBM (Hamburg et al. 2019, GCN 23707), Swift/BAT (Gropp et al. 2019, GCN 23688), and at Very High Energy by the MAGIC telescope (Mirzoyan et al. 2019, GCN 23701).

The best LAT on-ground location is found to be

RA, Dec = 54.57, -26.99 (degrees, J2000)

with an error radius of 0.05 deg (90% containment, statistical error only). This position is consistent with the Swift/BAT localization. The LAT position was 68 deg from the LAT boresight at the time of the GBM trigger time (20:57:02.63 UT) and remained in the LAT field of view for 150 seconds.

The data from the Fermi-LAT show a significant increase in the event rate that is spatially correlated with the GBM trigger with high significance. The highest-energy photon is a 22.9 GeV event which is observed 15 s after the GBM trigger.

The estimated photon index above 100 MeV is -1.98 +/- 0.06, with an estimated photon and energy flux of 2.69e-03 +/- 1.86e-04 ph/cm2/s and 2.06e-06 +/- 1.42e-07 erg/cm2/s, respectively.

The Fermi-LAT point of contact for this burst is Daniel Kocevski (kocevski@slac.stanford.edu<http://slac.stanford.edu>).

The Fermi-LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.


GRB_name: GRB190114C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23710
SUBJECT: GRB 190114C: X-shooter observations of a highly extinguished afterglow
DATE:    19/01/15 09:41:05 GMT
FROM:    Alexander Kann at IAA-CSIC  <kann@iaa.es>

D. A. Kann, C. C. Thoene (both HETH/IAA-CSIC), J. Selsing 
(DAWN/NBI/DTU), L. Izzo (HETH/IAA-CSIC), A. de Ugarte Postigo 
(HETH/IAA-CSIC and DARK/NBI), G. Pugliese (API, Univ. Amsterdam), B. 
Sbarufatti (PSU), K. E. Heintz (Univ. Iceland), V. D'Elia (ASI/SSDC, 
INAF/OAR), S. Covino (INAF-OAB), K. Wiersema (Univ. Warwick), D. A. 
Perley (LJMU), S. Vergani (GEPI/Obs. Paris), J. P. U. Fynbo 
(DAWN/NBI/DTU), D. Watson (DAWN/NBI), N. R. Tanvir (Univ. Leicester), D. 
Hartmann (Clemson Univ.), D. Xu (NAOC), S. Schulze (WIS), and J. Bolmer 
(MPE) report on behalf of the Stargate Consortium:

We observed the optical counterpart of GRB 190114C (Gropp et al., GCN 
#23688; Tyurina et al., GCN #23690; Lipunov et al., GCN #23693; Selsing 
et al., GCN #23695; Izzo et al., GCN #23699; Bolmer & Schady, GCN 
#23702), the first-ever TeV-detected GRB (Mirzoyan et al., GCN #23701), 
with the ESO-VLT UT2 (Kueyen) equipped with the X-shooter spectrograph, 
covering the wavelength range 3000-21000 AA. We acquired four 600 second 
spectra on 2019-01-15 between 01:42UT and 02:32UT, approximately 4.75 
hours after the GRB. In the acquisition image we measure r' = 18.2 +/- 
0.4 (AB), calibrated against several nearby Pan-STARRS comparison stars.

We detect several strong absorption features, namely Ca H&K, Na ID, Mg 
II and Mg I, at a common redshift z = 0.4250, consistent with the values 
reported by Selsing et al. (GCN #23695) and Castro-Tirado et al. (GCN 
#2370, and in agreement with the existence of a likely host galaxy in 
archival observations (de Ugarte Postigo et al., GCN #23692). 
Furthermore, the spectrum shows OII, Hbeta, OIII and Halpha in emission 
at the same redshift, fully confirming it.

The line-of-sight is highly extinguished, which is in agreement with the 
large column density seen in Swift XRT observations (Evans et al., GCN 
#23706) as well as the red GROND colors (Bolmer & Schady, GCN #23702).

We acknowledge Bin Yang, Elizabeth Bartlett, Trystyn Berg, and Juan 
Carlos Olivares at Paranal for their excellent help in obtaining these 
observations.


GRB_name: GRB190109B
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23711
SUBJECT: GRB190109B: MITSuME Akeno optical upper limits
DATE:    19/01/15 11:15:43 GMT
FROM:    Motoki Oeda at Tokyo Inst. of Tech.  <oeda@hp.phys.titech.ac.jp>

M. Oeda,  K. L. Murata, R. Itoh, Y. Tachibana, S. Harita, K. Morita,
K.Shiraishi, K. Iida, M. Niwano, R. Adachi, Y. Yatsu, and N. Kawai
(TokyoTech)
report on behalf of the MITSuME collaboration:

We searched for the optical counterpart of GRB 190109B (B. Sbarufatti
et al.,GCN Circular #23648) with the optical three color (g', Rc, and
Ic) CCD cameras attached to the MITSuME 50 cm telescope of Akeno
Observatory,Yamanashi, Japan.

The observation started on 11:57:03.81 UT. We did not find any new
point source within the enhanced XRT circle (A.P. Beardmore et al.,
GCN Circular #23652) in all three bands. We obtained following 5 sigma
limits for the magnitudes.

T0+[min]    MID-UT      T-EXP[sec]    g'       Rc        Ic
-------------------------------------------------------------------------------------------------------
0.913      11:57:33.81           60        >17.54     >17.26     >16.72
0.913       12:31:59.3          3660      >19.29     >17.67     >17.12
-------------------------------------------------------------------------------------------------------
T0+ : Elapsed time after the burst
T-EXP: Total Exposure time
We used UCAC-4 catalog for flux calibration.


GRB_name: GRB190114C
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23712
SUBJECT: GRB 190114C: AGILE/MCAL detection
DATE:    19/01/15 12:13:44 GMT
FROM:    Alessandro Ursi at INAF/IAPS  <alessandro.ursi@gmail.com>

A. Ursi (INAF/IAPS), M. Tavani (INAF/IAPS, and Univ. Roma Tor Vergata), M.
Marisaldi (INAF/OAS-Bologna, and Bergen University), N. Parmiggiani
(INAF/OAS-Bologna), F. Longo (Univ. Trieste and INFN Trieste), A. Argan, M.
Cardillo, C. Casentini, Y. Evangelista, G. Piano (INAF/IAPS), F. Lucarelli,
C. Pittori, F. Verrecchia (SSDC, and INAF/OAR), A. Bulgarelli, V. Fioretti,
F. Fuschino (INAF/OAS-Bologna), M. Pilia, A. Trois (INAF/OA-Cagliari), I.
Donnarumma (ASI), A. Giuliani (INAF/IASF-Mi), report on behalf of the AGILE
Team:

The AGILE Mini-CALorimeter (MCAL) detected the GRB 190114C at T0 =
2019-01-14 20:57:02.26 +/- 0.01 s (UTC), which was also detected by
Swift/BAT-XRT (Gropp et al., GCN #23688), MASTER (Tyurina et al., GCN
#23690), Pan-STARRS (de Ugarte Postigo et al., GCN #23692), NOT (Selsing et
al., GCN #23695), OASDG (Izzo et al., GCN #23699), GROND (Bolmer et al.,
GCN #23702), Fermi/GBM (Hamburg et al., GCN #23707), Fermi/LAT (Kocevski et
al., GCN #23709), X-shooter (Kann et al., GCN #23710), and representing the
first GRB ever detected by ground-based Cherenkov telescopes (MAGIC,
Mirzoyan et al., GCN #23701).

In the 0.4-100 MeV energy band, the event lasted T90=6.2 s and released a
total number of ~32600 counts in the detector, above an average background
rate of about 700 Hz. The light curve shows several peaks, which can be
grouped in three episodes, characterized by different energy profiles: the
first and third episodes are mostly constituted of counts with energies <
1.4 MeV, whereas the second central episode exhibits a substantial fraction
of high-energy counts with energies > 1.4 MeV. The AGILE/MCAL light curve
can be viewed at:
http://www.agilescienceapp.it/results/wp-content/uploads/2019/01/GRB190114C_MCAL-1.png
.

The time-integrated spectrum of the first episode (from T0 to T0+2.5 s) can
be fitted in the energy range [0.4-2 MeV] with a simple power law with
ph.ind.=2.55 -0.07/+0.08, resulting in a reduced chi-square of 1.56 (21
d.o.f.). The burst fluence in the same energy range and time interval is
2.11e-05 erg/cm^2 (90% confidence level).

The time-integrated spectrum of the second episode (from T0+2.5 s to T0+4.8
s) can be fitted in the energy range [0.4-60 MeV] with a broken power law
with alpha=1.46 -0.35/+0.41, beta=2.53 -0.05/+0.07, and a break energy of
750 +56/-110 keV, resulting in a reduced chi-square of 1.44 (46 d.o.f.).
This episode is possibly made by several spectral components. The burst
fluence in the same energy range and time interval is 1.31e-4 erg/cm^2 (90%
confidence level).

The time-integrated spectrum of the third episode (from T0+4.8 s to T0+6.2
s) can be fitted in the energy range [0.4-2 MeV] with a simple power law
with ph.ind.=2.95 -0.09/+0.10, resulting in a reduced chi-square of 1.11
(21 d.o.f.). The burst fluence in the same energy range and time interval
is 1.11e-05 erg/cm^2 (90% confidence level).

The GRB is clearly detected also by the AGILE scientific ratemeters: in
particular, by the Super-AGILE (20-60 keV), Anti-Coincidence (50-200 keV),
and MCAL (0.4-100 MeV) ratemeters.

Further analysis is still in progress.

The AGILE-MCAL detector has a full solid angle acceptance, and is
operational in the range 0.4 - 100 MeV.


GRB_name: GRB190114B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23713
SUBJECT: GRB 190114B: NOT optical counterpart
DATE:    19/01/15 12:53:20 GMT
FROM:    Jonatan Selsing at DARK/NBI  <jselsing@dark-cosmology.dk>

J. Selsing (DAWN/NBI and DAWN/DTU), A. de Ugarte Postigo (HETH/IAA-CSIC
and DARK/NBI), and S. Dyrbye (NOT), report on behalf of a larger
collaboration:

We have observed the optical afterglow of GRB GRB190114B (Siegel et al.,
GCN 23686; Goad et al., GCN 23691) at the 2.5-m Nordic Optical Telescope
(NOT). We have obtained an griz-band imaging sequence using the ALFOSC
instrument, with 3x300s exposure in gri-band and 5x200s in z-band.
Observations began at 01:51:42 UT, on the night of the 14th of January,
6.3 hr after the BAT trigger. 

In the images we confirm the detection of the optical counterpart in
Fernandez-Garcia et al. (GCN 23694) and Pozanenko et al. (GCN 23696) and
report further fading. The source is located at:

RA (J2000) = 11:39:29.823
DEC (J2000) = +18:53:28.19

with the astrometric solution calibrated against the 2MASS catalog. 

We calibrate the photometric zeropoints against the Pan-STARRS catalog
and calculate the following magnitudes for the optical counterpart:

g = 21.61 +- 0.13 AB mag 
r = 21.15 +- 0.09 AB mag 
i = 20.96 +- 0.04 AB mag 
z = 20.59 +- 0.08 AB mag


GRB_name: GRB190114C
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23714
SUBJECT: GRB 190114C: SPI-ACS/INTEGRAL extended emission detection
DATE:    19/01/15 13:12:17 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

P. Minaev (IKI), A. Pozanenko (IKI) report:

We analyzed the publicly available SPI-ACS data (>~ 80 keV) of INTEGRAL 
observatory covering trigger time (UT) 20:57:02 of the GRB 190114C 
(Gropp et al. 2019, GCN 23688; Hamburg et al. 2019, GCN 23707).

We found statistically significant extended emission up to ~ 5000 sec 
after the trigger. The extended emission can be approximated by power 
law model with the index of 0.99 +/- 0.05.

We do not detect any significant emission from possible precursor on 
time scales 0.05 â€“ 10 sec within (-500, 0) sec time interval before the 
trigger.

The SPI-ACS/INTEGRAL light curve can be found at:
http://grb.rssi.ru/GRB190114C/GRB190114C_SPI-ACS_LC.png


GRB_name: GRB190114C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23715
SUBJECT: GRB 190114C: A type 1 BdHN with TeV emission
DATE:    19/01/15 15:29:54 GMT
FROM:    Remo Rufinni at ICRA  <ruffini@icra.it>

R. Ruffini, R. Moradi, Y. Aimuratov, U. Barres de Almeida, V.A. Belinski,
C. L. Bianco, Y. C. Chen, C. Cherubini, S. Filippi,  D. M. Fuksman, M.
Karlica, Liang Li, D. Primorac, J.A. Rueda, N. Sahakyan, Y. Wang, S.S. Xue
on behalf of the ICRANet team, report:


GRB 190114C with T90=116 s (50-300 keV), Epeak = 998.6 +/- 11.9 keV,
isotropic energy release in gamma-rays Eiso = 3 E53
erg, and the isotropic peak luminosity Liso = 1 E53 erg/s (R. Hamburg et
al., CGN 23707) presents the typical characteristics of type I
binary-driven hypernova (BdHN) (Y. Wang et al., submitted to Astrophysical
Journal arXiv:1811.05433v2). The most significant ever Fermi-LAT GeV
emission (D. Kocevski et al., GCN 23709) with test statistic value TS>2500
implies that this GRB is seen from the normal to the orbital plane of the
progenitor binary system composed of a carbon-oxygen core and a neutron
star companion (R. Ruffini et al., submitted to Astrophysical Journal
arXiv:1803.05476). The TeV emission (R. Mirzoyan et al., GCN 23701), a
first in GRBs, has been recently predicted, as originating from the Wald
solution, within the new inner engine approach of the long GRBs recently
introduced in Ruffini et al (submitted to Physical Review Letter:
arXiv:1811.01839) and Ruffini et al (submitted to Astrophysical Journal:
arXiv:1812.00354). Most interesting this system being at z=0.4245 (A. J.
Castro-Tirado et al., GCN 23708), can give a strong support to our BdHN
approach by observing a supernova. Using the averaged appearance time of
the SNe associated to GRBs (Cano et al., 2016), and considering the
redshift z=0.42 (J. Selsing  et al., GCN 23695, A. J. Castro-Tirado et al.,
GCN 23708), a bright optical signal will peak at 18.8 +/- 3.7 days after
the trigger (February 2nd 2019, uncertainty from  January 30th 2019 to
February 6th 2019) at the location of RA 54.510 and DEC -26.939, with an
uncertainty 3 arcmin (J.D. Gropp et al., GCN 23688). The follow-up
observations, especially the optical bands for the SN, are recommended.


GRB_name: GRB190114C
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23716
SUBJECT: GRB 190114C:Insight-HXMT/HE detection
DATE:    19/01/15 15:49:09 GMT
FROM:    Shuo Xiao at IHEP  <xiaoshuo@ihep.ac.cn>

S. Xiao, 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, J. L. Zhao,
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 2019-01-14T20:57:02.63 (T0), the Insight-HXMT/HE detected 
GRB 190114C (trigger ID: HEB190114872) in a routine search of the data, 
which was also triggered by Swift/BAT (Gropp et al., GCN23688), 
MAGIC (Mirzoyan et al., GCN23701), Fermi/GBM (Hamburg et al., GCN23707), 
AGILE/MCAL (Ursi et al., GCN23712), INTEGRAL/SPI-ACS (Minaev et al., 
GCN23714) and Fermi/LAT (Kocevski et al., GCN23709).

The Insight-HXMT/HE light curve mainly consists of multiple 
pulses with a duration (T90) of 15.68 s measured from T0+0.12 s. 
The 1-s peak rate, measured from T0-0.01 s, is 10860.9 cnts/s. 
The total counts from this burst is 61531.1 counts. 
URL_LC: http://www.hxmt.org/images/GRB/HEB190114872_lc.jpg 

All measurements above are made with the CsI detectors operating in the 
GRB mode with the energy range of about 200-3000 keV (record 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 could be found at: http://www.hxmt.org.


GRB_name: GRB190114C
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23717
SUBJECT: GRB 190114C: Optical observations
DATE:    19/01/15 15:50:04 GMT
FROM:    Myungshin Im at Seoul Nat U  <mim@astro.snu.ac.kr>

Myungshin Im, Gregory S. Paek, Sophia Kim, Gu Lim, Changsu Choi (CEOU/SNU),
on behalf of a larger collaboration

We observed the afterglow of GRB 190114C (Gropp et al., GCN 23688; Tyurina
et al., GCN 23690, de Ugarte Postigo et al., GCN 23692, Lipunov et al. GCN
23693, Selsing et al. GCN 23695, Izzo et al. GCN 23699, Bolmer et al. GCN
23702, Castro-Tirado et al. GCN 23708, Kann et al. GCN 23710) with the 0.8m
and 0.25m telescopes at the McDonald Observatory, and the 1.0m telescope at
the SNU Astronomical Observatory. The observation at the McDonald
observatory started at about 6.1 hours after the initial alert, and used B,
V, R filters.

We identify the afterglow in the McDonald observatory's data, and
preliminary photometry shows R = 18.9 +- 0.1 mag at 6.1 hours post-burst.

Further observations and analysis are being carried out.


GRB_name: GRB190114A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23718
SUBJECT: GRB 190114A: Mondy optical afterglow detectio
DATE:    19/01/15 16:08:15 GMT
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


GRB_name: GRB190114A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23719
SUBJECT: GRB 190114A: Swift/UVOT Observations
DATE:    19/01/15 16:52:55 GMT
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).


GRB_name: GRB190114B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23720
SUBJECT: GRB 190114B: Swift/UVOT Upper Limits
DATE:    19/01/15 16:53:38 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <mhs18@psu.edu>

M. H. Siegel (PSU) reports on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 190114B
158 s after the BAT trigger (Siegel et al., GCN Circ. 23686).
No optical afterglow consistent with the enhanced XRT position
(Goad et al. GCN Circ. 23691) or the position of the faint
optical counterpart (Fernandez-Garcia et al., GCN Circ. 23694; 
Pozanenko et al., GCN Circ. 23696, Selsing et al. GCN Circ. 23713)
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

u_FC               158          408          246         >20.2
v                  464         1976          175         >18.5
b                  414         2075          214         >19.9
u                  158         2050          568         >20.4
w1                 513         2025          194         >19.7
m2                 786         2000          117         >18.9
w2                 440         2100          194         >19.8

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.02 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB190114B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23721
SUBJECT: GRB 190114B, Swift-BAT refined analysis
DATE:    19/01/15 16:59:37 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

J. R. Cummings (CPI), S. D. Barthelmy (GSFC),
H. A. Krimm (NSF/USRA), A. Y. Lien (GSFC/UMBC),
C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (AGU), M. H. Siegel (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 190114B (trigger #883818)
(Siegel et al., GCN Circ. 23686).  The BAT ground-calculated position is
RA, Dec = 174.868, 18.882 deg which is
  RA(J2000)  =  11h 39m 28.3s
  Dec(J2000) = +18d 52' 53.5"
with an uncertainty of 2.3 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 63%.

The mask-weighted light curve shows a weak pulse that starts at ~T0 and ends
at ~T+30 s. The possible precursor seen at ~T-75 s (Siegel et al., GCN Circ. 23686)
turns out to be purely instrumental and is not related to this GRB.
T90 (15-350 keV) is 26.5 +- 6.7 sec (estimated error including systematics).

The time-averaged spectrum from T-1.2 to T+27.9 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.98 +- 0.28.  The fluence in the 15-150 keV band is 5.1 +- 1.0 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+3.62 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/883818/BA/


GRB_name: GRB190114B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23722
SUBJECT: GRB 190114B: optical afterglow observations in Mondy and Abastumani observatories
DATE:    19/01/15 17:32:45 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (IKI), A. Pozanenko (IKI),  E. Mazaeva (IKI),  E. Klunko 
(ISTP), S. Belkin (IKI),  R. Ya. Inasaridze (AbAO), V.R. Ayvazian 
(AbAO),  G. V.  Kapanadze (AbAO),    report   on behalf of IKI-FuN:

We observed the field of  the GRB  190114B (Siegel et al., GCN 23686) 
with AZT-33IK telescope of Sayan observatory (Mondy),   and  AS-32 
(0.7m) telescope of Abastumani Observatory.  The optical afterglow 
(Fernandez-Garcia et al., GCN 23694;  Pozanenko et al., GCN 23696; 
Selsing et al., GCN 23713) is detected in stacked images. Preliminary 
photometry is following.

Date       UT start t-T0    Filter Exp.   OT    Err. Observatory
                    (mid, days) (s)

2019-01-14 20:28:30 0.10233 R      30*120 19.87 0.06  Mondy
2019-01-15 01:04:51 0.24212 R      18*60  20.40 0.25  AbAO

The photometry is based on nearby SDSS  stars
SDSS id             R_Lupton
J113927.36+185157.2 17.094 0.014
J113940.10+185315.3 17.015 0.015
J113939.20+185354.8 17.954 0.018

The photometry might be affected by a nearby galaxy (r'=20.534, z_ph = 
0.32813+/-0.08585) at a distance of 5.6 arc seconds.


GRB_name: GRB190114B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23723
SUBJECT: GRB 190114B: Liverpool Telescope near-IR observations
DATE:    19/01/15 18:31:09 GMT
FROM:    Luca Izzo at IAA-CSIC  <luca.izzo@gmail.com>

M. Blazek, L. Izzo (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 190114B (Siegel et al. GCN 23686) with the IO:I camera mounted on the 2-m Liverpool Telescope located in La Palma, Spain. Observations started on January 15th at 02:51:47 UT (7.34 hours after the GRB trigger) and we obtained a series of 10x60s images in the H filter.

We detect the faint optical afterglow (Fernandez-Garcia et al. GCN 23694, Pozanenko et al. GCN 23696, Selsing et al. GCN 23713, Volnova et al., GCN 23722) for which we measure the following magnitude:

H(AB) = 20.35 +- 0.34 mag

The calibration was performed using four nearby 2MASS stars.


GRB_name: GRB190114C
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23724
SUBJECT: GRB 190114C: Swift-BAT refined analysis
DATE:    19/01/15 19:51:20 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

H. A. Krimm (NSF/USRA), S. D. Barthelmy (GSFC),
J. R. Cummings (CPI), J. D. Gropp (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 190114C (trigger #883832)
(Gropp et al., GCN Circ. 23688).  The BAT ground-calculated position is
RA, Dec = 54.503, -26.938 deg which is
  RA(J2000)  =  03h 38m 00.7s
  Dec(J2000) = -26d 56' 17.5"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.

The mask-weighted light curve shows a multi-peaked structure that starts at
~T-7 s. The brightest emission contains two complex pulses and ends at ~T+50 s.
Afterwards, the emission appeared to decay exponentially out to beyond ~T+720 s,
when the burst went out of the BAT field of view. The burst did not come back into the
BAT field of view until ~T+3800, and nothing significant was detected at that time.
T90 (15-350 keV) estimated using data before the burst went out of the BAT field of view
 is 361.5 +- 11.7 sec (estimated error including systematics). Please note that this
T90 might be an underestimate.

The time-averaged spectrum from -6.604 to 703.192 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.43 +- 0.02.  The fluence in the 15-150 keV band is 8.3 +- 0.1 x 10^-5 erg/cm2.
The 1-sec peak photon flux measured from T+0.23 sec in the 15-150 keV band
is 101.0 +- 1.5 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/883832/BA/


GRB_name: GRB190114C
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23725
SUBJECT: GRB 190114C: Swift/UVOT Detection
DATE:    19/01/15 19:59:02 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <mhs18@psu.edu>

M. H. Siegel (PSU) and J. D. Gropp (PSU)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 190114C
74 s after the BAT trigger (Gropp et al., GCN Circ. 23688).
A source consistent with the XRT position
(Osborne et al. GCN Circ. 23704) and previously reported optical 
detections (Tyurina et al., GCN Circ. 23690, Selsing et al., GCN Circ. 23695,
Izzy et al., GCN Circ. 23699, Bolmer & Schady, GCN Circ. 23702, Im et al.,
GCN Circ. 23717) is detected in the initial UVOT exposures.

The preliminary UVOT position is:
   RA  (J2000) =  03:38:01.16 =  54.50484 (deg.)
   Dec (J2000) = -26:56:46.9  = -26.94637 (deg.)
with an estimated uncertainty of 0.42 arc sec. (radius, 90% confidence).

The data of the first few orbits shows the afterglow to fade rapidly, particularly
in the NUV filters, which could be consistent with the heavy extinction reported by
Kann et al. (GCN Circ. 23710).

Preliminary detections 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)          74          224          147      14.89+/-0.02
white              566          586           19      16.90+/-0.07
white             5851         6050          196      19.19+/-0.09
white            21950        22857          885      20.22+/-0.09
v                  616          627           10      16.28+/-0.19
v                16295        17136          820      18.97+/-0.13
v                26775        27682          885      19.41+/-0.24
v                39149        57221         1694      19.92+/-0.20
b                  542          561           19      17.38+/-0.14
b                 5646         5845          196      19.38+/-0.16
b                21038        46521         1591      20.83+/-0.26
u (fc)             286          536          245      17.58+/-0.07
u                33738        34038          295            >20.28
uvw1              4044        51522         3671      21.05+/-0.31
uvm2              3839        50615         3251      21.00+/-0.30
uvw2              6056        56384         3552            >21.33

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.01 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB190114C
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23726
SUBJECT: GRB 190114C: VLA Detection
DATE:    19/01/15 20:25:00 GMT
FROM:    Kate Alexander at Northwestern U  <kate.alexander@northwestern.edu>

K. D. Alexander (Northwestern), T. Laskar (University of Bath), E. Berger
(Harvard), C. G. Mundell (University of Bath), and R. Margutti
(Northwestern), report on behalf of a larger collaboration:

We observed GRB 190114C (Gropp et al., GCN 23688) with the Karl G.
Jansky Very Large Array (VLA) beginning on 2019 January 15.05 UT (4.2 hours
after the burst). At a mean frequency of 33.5 GHz, we detect a radio source
with a preliminary flux density of 3.1 mJy at the position

RA (J2000) = 03:38:01.191 +/- 0.04 arcsec
Dec (J2000) = -26:56:46.73 +/- 0.02 arcsec

consistent with the position of the optical afterglow (Tyurina et al., GCN
23690; Lipunov et al., GCN 23693; Selsing et al., GCN 23695)
and the XRT afterglow (Osborne et al. GCN 23704). Follow-up observations are
planned.

We thank the VLA staff for rapidly executing these observations.


GRB_name: GRB190114C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23727
SUBJECT: GRB 190114C: Mondy optical observations
DATE:    19/01/15 23:01:32 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

E. Mazaeva (IKI),   E. Klunko (ISTP),  A. Pozanenko (IKI), A. Volnova (IKI), 
S. Belkin (IKI)  report   on behalf of IKI-FuN:

We observed the field of localization of  GRB 190114C  (Gropp   et al.  GCN 
23688)    with AZT-33IK telescope of Sayan observatory
(Mondy).   We started observations on Jan. 15 (UT) 12:35:00. We do not 
detect  the optical afterglow (Gropp et al., GCN 23688; Tyurina
et al., GCN 23690, de Ugarte Postigo et al., GCN 23692, Lipunov et al. GCN 
23693, Selsing et al. GCN 23695, Izzo et al. GCN 23699, Bolmer et al. GCN 
23702, Castro-Tirado et al. GCN 23708, Kann et al. GCN 23710; Im  et al. GCN 
23717; Siegel  et al. GCN  23725). Preliminary
photometry of the field is following.

Date               UT start      t-T0          Filter Exp.   OT     Err. 
UL(3sigma)
                                           (mid, days)      (s)

2019-01-15  12:35:00   1.39354     R      300      n/d     n/d   19.8

The photometry is based on nearby PanSTARRS  stars. 


GRB_name: GRB190114C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23728
SUBJECT: GRB 190114C: ALMA detection of a fading mm counterpart
DATE:    19/01/15 23:08:49 GMT
FROM:    Tanmoy Laskar at U of Bath  <tanmoylaskar@gmail.com>

T. Laskar (University of Bath), K. D. Alexander (Northwestern), E. Berger
(Harvard), W. Fong (Northwestern), R. Margutti (Northwestern), C. G.
Mundell (University of Bath), and P. Schady (University of Bath) report on
behalf of a larger collaboration:

"We observed GRB 190114C (Gropp et al. GCN 23688) with the Atacama Large
Millimeter/Submillimeter Array (ALMA) starting at 3.2 hr after the burst at
90 GHz. Preliminary analysis reveals a bright (S/N > 800), fading mm
counterpart at a location consistent with the X-ray position (Osborne et
al. GCN 23704) and optical position (Tyurina et al., GCN
23690; Lipunov et al., GCN 23693). Follow-up observations are planned.

We thank the JAO staff, AoD, and the ALMA team for their help with these
observations."


GRB_name: GRB190114C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23729
SUBJECT: GRB 190114C: REM optical/NIR detection
DATE:    19/01/15 23:15:59 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

P. D'Avanzo, S.Covino, D. Fugazza, A. Melandri (INAF-OAB), on behalf of the REM team, report:

We observed the field of GRB 190114C (Gropp et al., GCN 23688) with the REM 60cm robotic telescope located 
at the ESO premise of La Silla (Chile). The observations were performed starting on 2019 January 15 at 00:47:35 UT 
(i.e. about 3.8 hours after the burst) and were carried in the g, r, i, z, J, H and K bands. 

From preliminary photometry, for the optical/NIR afterglow (Tyurina et al., GCN 23690; Lipunov et al. GCN 23693; 
Selsing et al., GCN 23695; Izzo et al. GCN 23699; Bolmer et al. GCN 23702; Castro-Tirado et al., GCN 23708; 
Kann et al. GCN 23710; Im et al., GCN 23717; Siegel et al. GCN 23725) we estimate the following magnitudes:

r = 18.6 +/- 0.2
H = 16.7 +/- 0.1

(AB; calibrated against the pan-STARRS and the 2MASS catalogues), at a mean time of about 4.3 hours after the GRB.


GRB_name: GRB190114B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23730
SUBJECT: GRB 190114B: Swift-XRT refined Analysis
DATE:    19/01/16 02:09:21 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

A. D'Ai (INAF-IASFPA), D.N. Burrows (PSU), A. Tohuvavohu (PSU), S. J.
LaPorte (PSU), A.P. Beardmore (U. Leicester), P.A. Evans (U.
Leicester), J.P. Osborne (U. Leicester), A. Melandri (INAF-OAB), P.
D'Avanzo (INAF-OAB) and M.H. Siegel report on behalf of the Swift-XRT
team:

We have analysed 2.4 ks of XRT data for GRB 190114B (Siegel et al. GCN
Circ. 23686), from 165 s to 104.3 ks after the BAT trigger. The data
are entirely in Photon Counting (PC) mode. The enhanced XRT position
for this burst was given by Goad et al. (GCN Circ. 23691).

The light curve can be modelled with a power-law decay with a decay
index of alpha=2.1 (+/-0.4).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.99 (+0.34, -0.14). The
best-fitting absorption column is  consistent with the Galactic value
of 1.7 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 3.2 x 10^-11 (3.4 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.7 (+/-4.8) x 10^20 cm^-2
Galactic foreground: 1.7 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:      1.99 (+0.34, -0.14)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00883818.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB190114A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23731
SUBJECT: GRB 190114A: DOAO/LOAO optical observation
DATE:    19/01/16 03:11:54 GMT
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.]


GRB_name: GRB190114C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23732
SUBJECT: GRB 190114C: LSGT optical observation
DATE:    19/01/16 03:30:37 GMT
FROM:    Joonho Kim at Seoul National U.  <joonho@astro.snu.ac.kr>

Joonho Kim, Myungshin Im, (CEOU/SNU),

report on behalf of a larger collaboration


We observed the optical afterglow of GRB 190114C Gropp et al., GCN 23688,

Tyurina et al., GCN 23690, de Ugarte Postigo et al., GCN 23692, Lipunov et
al.

GCN  23693, Selsing et al. GCN 23695, Izzo et al. GCN 23699, Bolmer et al.

GCN  23702, Castro-Tirado et al. GCN 23708, Kann et al. GCN 23710, Im et al.

GCN 23717; Siegel  et al. GCN  23725, Mazaeva et al. GCN 23727, D'Avanzo

et al. GCN 23729) with the Lee Sang Gak Telescope (LSGT; 0.42m) at the

Siding Spring Observatory. The observation started at about 14.7 hours after

the initial alert, and used g, r, i, z filters with 540 sec of exposure in
each filter.


Preliminary photometry is following based on nearby Pan-STARRS stars.


Filter    Date    UT-Start    Mag

g    2019-01-15    10:41:00    20.2 +/- 0.3

r    2019-01-15    10:50:57    19.7 +/- 0.3

i    2019-01-15    11:00:42    18.6 +/- 0.3

z    2019-01-15    11:10:23    18.4 +/- 0.4


Further observations and analysis are being carried out.


GRB_name: GRB190114C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23733
SUBJECT: GRB190114C: GRowth-India detection of optical afterglow
DATE:    19/01/16 07:33:37 GMT
FROM:    Varun Bhalerao at Indian Inst of Tech  <varunb@iitb.ac.in>

Harsh Kumar (IITB), Shubham Srivastav (IITB), Viraj karambelkar (IITB), Gaurav Waratkar(IITB), Tsewang Stanzin (IAO, IIA), Varun Bhalerao (IITB), G.C. Anupama (IIA) report on behalf of the GROWTH-India collaboration:

We observed the optical afterglow of GRB190114C (Gropp et al., GCN 23688) with the 0.7m robotic GROWTH-India telescope at the Indian Astronomical Observatory. Observation were started about 16.36 hrs after the initial alert. We observed the field using g,r,i filters with 600sec exposure in each filter. We clearly detected a faint afterglow source. Magnitudes were calibrated using PanSTARRs reference stars in the same field. The measured magnitudes are:

t-t0â€ƒ       MJD        Filt  Magnitude 
16.36hrs    58498.55    g    19.92 +- 0.24
16.68hrs    58498.56    r    19.29 +- 0.14
17.00hrs    58498.58    i    18.78 +- 0.19

Source has faded significantly as compared to its early time optical detection (Gropp et al., GCN 23688, Izzo et al. GCN 23699). Based on our data combined with other r band measurements (Selsing et al., GCN 23695; Bolmer et al., GCN 23702; Dâ€™Avanzo et al., GCN 23729; Kim et al., GCN 23732), we see that the source flux is fading approximately as a power law t^-alpha, with alpha = 0.7 +- 0.1.

GROWTH India telescope is a 70-cm telescope with a 0.7 degree field of view, set up by the Indian Institute of Astrophysics and the Indian Institute of Technology Bombay with support from the Indo-US Science and Technology Forum (IUSSTF) and the Science and Engineering Research Board (SERB) of the Department of Science and Technology (DST), Government of India (https://sites.google.com/view/growthindia/). It is located at the Indian Astronomical Observatory (Hanle), operated by the Indian Institute of Astrophysics (IIA).


GRB_name: GRB190114C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23734
SUBJECT: GRB 190114C: KMTNet optical observation
DATE:    19/01/16 09:44:40 GMT
FROM:    Joonho Kim at Seoul National U.  <joonho@astro.snu.ac.kr>

Joonho Kim, Myungshin Im, (CEOU/SNU), Chung-Uk Lee, Seung-Lee Kim (KASI)

report on behalf of a larger collaboration


We observed the optical afterglow of GRB 190114C Gropp et al., GCN 23688,
Tyurina et al., GCN 23690, de Ugarte Postigo et al., GCN 23692, Lipunov et
al. GCN 23693, Selsing et al. GCN 23695, Izzo et al. GCN 23699, Bolmer et
al. GCN 23702, Castro-Tirado et al. GCN 23708, Kann et al. GCN 23710, Im et
al. GCN 23717; Siegel et al. GCN 23725, Mazaeva et al. GCN 23727, D'Avanzo et
al. GCN 23729, Peak et al. GCN 23731, Kim et al. GCN 23732, Kumar et al.
GCN 23733) with KMTnet 1.6m telescope at the South African Astronomical
Observatory. The observation started at about 22.1 hours after the initial
alert, and used R, I filters with 600 sec of exposure in each filter.


Preliminary photometry is following based on nearby Pan-STARRS stars.

Filter Date UT-Start Mag

R 2019-01-15 18:49:42    19.45 +/- 0.05

I 2019-01-15 18:52:39    18.45 +/- 0.04

Further observations and analysis are being carried out.


GRB_name: GRB190114C
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23735
SUBJECT: GRB190114C, Long follow up urged 
DATE:    19/01/16 11:14:09 GMT
FROM:    Arnon Dar at Technion-Israel Inst. of Tech  <arnon@physics.technion.ac.il>

S. Dado and A. Dar report:

A long follow up of the afterglow of the very bright GRB190114C (Groop
et al. GCN 23688; Hamburg et al. GCN 23707) like that of GRB130427A
(De Pasquale et al. MNRAS 462 (2016) 1111) may provide another critical
test of GRB theories. In the Cannonball (CB) model, the X-ray afterglow
of very bright SN-GRBs is expected to decay like a single power-law in
time and in frequency, Fnu ~ t^{-alpha} nu^{-beta}, where for a constant 
density ISM the temporal and spectral indices satisfy alpha=beta+1/2 and 
the "missing break" is hidden under the prompt emission (Dado & Dar, PRD 
94 (2016) 3007). The current values alpha=1.34+/-0.01 and beta=0.82+/-0.12,
reported for GRB190114C in the Swift XRT light curve repository (Evans et 
al. 2009) seem to satisfy well the above CB model closure relation, which 
suggests an SN-GRB association similar to SN2013cq-GRB130427A.


GRB_name: GRB190114C
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23736
SUBJECT: The Swift-XRT WT mode spectrum of GRB190114C
DATE:    19/01/16 11:57:45 GMT
FROM:    Andy Beardmore at U Leicester  <ab271@leicester.ac.uk>

A. P. Beardmore (U. Leicester) reports on behalf of the Swift-XRT Team:

The Swift-XRT Windowed Timing (WT) mode spectrum of GRB 190114C shows
an apparent strong excess of emission below ~0.8 keV when compared to
a simple absorbed powerlaw model. The excess is not thought to be
intrinsic to the GRB (e.g. an additional spectral component), but is
instead caused by a well-known instrumental effect whereby charge from
deep charge traps (formed by radiation damage to the CCD) is released
on a timescale comparable to the WT readout time (1.78ms). The
released charge is subsequently detected in trailing readout rows
as additional low energy events, causing excess emission to be seen at
low energies (see http://www.swift.ac.uk/analysis/xrt/digest_cal.php#trail).
The excess is more apparent in strongly absorbed sources such as this.

The XRT Team is developing software to identify and remove occurences
of such trailing charge from WT data. In the meantime, the WT spectra
can be reliably modelled above ~0.8 keV.


GRB_name: GRB190114C
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23737
SUBJECT: Konus-Wind observation of GRB 190114C
DATE:    19/01/16 13:01:40 GMT
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, very bright GRB 190114C
(Swift-BAT detection: Gropp et al., GCN 23688;
MAGIC detection: Mirzoyan et al., GCN 23701;
Fermi-GBM detection: Hamburg et al., GCN 23707;
Fermi-LAT detection: Kocevski et al., GCN 23709;
AGILE/MCAL detection: Ursi et al., GCN 23712;
Insight-HXMT/HE detection: Xiao et al., GCN 23712)
triggered Konus-Wind (KW) at T0=75422.341 s UT (20:57:02.341).

The main part of the burst light curve shows a hard-spectrum,
multi-peaked pulse, which started at ~T0 and lasting for ~6 s, followed 
by a weaker and softer pulse at ~T0+16 s.
The decaying emission tail is seen in the KW data until the end of the
trigger record at ~T0+320 s.
The emission in the main pulse is seen up to ~20 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB190114_T75422/

As observed by Konus-Wind, the main part of the burst had
a fluence of (4.83 Â± 0.10)x10^-4 erg/cm2 and
a 64-ms peak energy flux, measured from T0+3.872,
of (2.40 Â± 0.08)x10^-4 erg/cm2 (both in the 20 keV - 10 MeV
energy range).

The time-integrated spectrum (measured from T0 to T0+21.248 s)
is best fit in the 30 keV - 20 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.73 (-0.02,+0.02),
the high energy photon index beta = -3.17 (-0.20,+0.16),
the peak energy Ep = 646 (-16,+16) keV,
chi2 = 122/95 dof.

The spectrum near the peak count rate (measured from T0+3.584 s
to T0+4.096 s) is best fit in the 30 keV - 20 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.01 (-0.07,+0.07),
the high energy photon index beta = -2.98 (-0.22,+0.17),
the peak energy Ep = 695 (-36,+38) keV,
chi2 = 61/62 dof.

The spectrum of the extended emission (measured from T0+21 s
to T0+220 s) is best fit in the 30 keV - 20 MeV range
by a simple power law with the photon index of 2.13 (-0.11,+0.12),
chi2 = 67/99 dof.

Assuming the redshift z=0.4245 (Selsing et al., GCN 23965;
Castro-Tirado et al., GCN 23708)
and a standard cosmology with H_0 = 67.3 km/s/Mpc, Omega_M = 0.315,
and Omega_Lambda = 0.685 (Planck Collaboration, 2014),
we estimate the following rest-frame parameters:
the isotropic energy release E_iso is (2.4 Â± 0.05)x10^53 erg,
the peak luminosity L_iso is (1.67 Â± 0.05)x10^53 erg/s
(both in the 1-10000 keV rest-frame band).
With these values, GRB 190114C is within 68% prediction bands
for both 'Amati' and 'Yonetoku' relations built for the sample
of 138 long KW GRBs with known redshifts (Tsvetkova et al., ApJ 850 161, 
2017), see http://www.ioffe.ru/LEA/GRBs/GRB190114_T75422/GRB190114C.pdf

All the quoted errors are estimated at the 90% confidence level.
All the presented results are preliminary.


GRB_name: GRB190114A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23739
SUBJECT: GRB 190114A: NOEMA detection of the mm afterglow
DATE:    19/01/16 14:51:27 GMT
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


GRB_name: GRB190114C
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23740
SUBJECT: GRB 190114C: UKIRT JHK observation
DATE:    19/01/16 15:08:40 GMT
FROM:    Myungshin Im at Seoul Nat U  <mim@astro.snu.ac.kr>

Myungshin Im, Gregory S. H. Paek, Changsu Choi (CEOU/SNU), on behalf of a
larger collaboration

We observed the afterglow of GRB 190114C (Gropp et al., GCN 23688; Tyurina
et al., GCN 23690, de Ugarte Postigo et al., GCN 23692, Lipunov et al. GCN
23693, Selsing et al. GCN 23695, Izzo et al. GCN 23699, Bolmer et al. GCN
23702, Castro-Tirado et al. GCN 23708, Kann et al. GCN 23710, Im et al. GCN
23717; Siegel et al. GCN 23725, Mazaeva et al. GCN 23727, D'Avanzo et al.
GCN 23729, Peak et al. GCN 23731, Kim et al. GCN 23732, Kumar et al.
GCN 23733) with the United Kingdom Infrared Telescope (UKIRT). The
observation started at 2019-01-16 05:06 UT or about 1.33 days after the
initial alert.

The afterglow is clearly detected in all J, H, K bands, and preliminary
magnitudes are derived from quick-look data, using nearby 2MASS stars as
photometry references.

Filter Date UT-start Vega_Mag (AB mag)
K   2019-01-16 05:06:05.011    15.5 +/- 0.1   (17.7 AB)
H   2019-01-16 05:26:45.974    16.5 +/- 0.1   (18.1 AB)
J    2019-01-16 05:47:58.042    17.5 +/- 0.1   (18.7 AB)

This shows an H-band fading of 1.4 mag with respect to the value reported
by D'Avanzo et al. (GCN 23729) which give an H-band fading rate of 1.2
mag/day.

Further observations are planned.
We thank the staffs at UKIRT for carrying out the observation.


GRB_name: GRB190114C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23741
SUBJECT: GRB 190114C: CHILESCOPE optical observations
DATE:    19/01/16 16:09:52 GMT
FROM:    Elena Mazaeva at IKI, Moscow  <30.v@mail.ru>

E. Mazaeva (IKI), A. Pozanenko (IKI), A. Volnova (IKI), S. Belkin (IKI), M. Krugov (FAPHI) report on behalf of IKI-GRB-FuN:

We observed the field of GRB 190114C (Gropp et al., GCN 23688) with RC-1000 telescope of CHILESCOPE observatory. Observations started on Jan. 16 (UT) 01:34:52 in r'-filter. We detected optical afterglow (Tyurina et al., GCN 23690; de Ugarte Postigo et al., GCN 23692; Lipunov et al. GCN 23693; Selsing et al. GCN 23695; Izzo et al. GCN 23699; 
Bolmer et al. GCN 23702; Castro-Tirado et al. GCN 23708; Kann et al. GCN 23710; Im  et al. GCN 23717; Siegel  et al. GCN  23725; Mazaeva et al., GCN  23727; D'Avanzo et al., GCN 23729; Kim et al., GCNs 23732,23734).
Preliminary photometry of a stacked image is following.

Date       UT start t-T0   Filter Exp.   OT    Err. UL(3sigma)
                     (mid, days)   (s)
2019-01-16 01:34:52 1.94457 r'    10*180 20.09 0.05 22.1

The photometry is based on several nearby PanSTARRS stars.
PanSTARRS_id        r
75670544556329552   16.117
75640544615203120   18.270
75620545839473520   16.802
75610545901287840   14.901
75690546042320496   14.750


GRB_name: GRB190114C
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23742
SUBJECT: GRB 190114C: Optical detection from HCT
DATE:    19/01/16 17:00:44 GMT
FROM:    Brajesh Kumar at Indian Inst. of Astrophysics  <brajesh.kumar@iiap.res.in>

Brajesh Kumar (IIA), S. B. Pandey (ARIES), Avinash Singh (IIA), D. K. 
Sahu (IIA), G. C. Anupama (IIA) and Piyali Saha (IIA)

We observed the afterglow of GRB 190114C (Gropp et al., GCN 23688) with 
the 2-m Himalayan Chandra Telescope (HCT) located at the Indian 
Astronomical Observatory, Hanle, India. The observations started on 
2019-01-15 (14:51:32 UT) and two Bessell R-band images were obtained in 
a gap of about 1.3 hr. The exposure time was 200 sec for each frame. The 
OT candidate (Lipunov et al., GCN 23693; Selsing et al., GCN 23695; 
Bolmer et GCN 23702; D'Avanzo et al., GCN 23729; Kim et al., GCN 23732, 
23734; Kumar et al., GCN 23733) is clearly detected in our frames with 
the following magnitudes:

UT-mid                   JD               Mag
-------------------    ----------    --------------
2019-01-15 14:53:13    2458499.12    19.70 +/- 0.10
2019-01-15 16:13:33    2458499.18    19.81 +/- 0.09

These magnitudes were calibrated using the magnitudes of field stars 
from the USNO-B1.0 catalogue.

We thank the observing staff at IAO and CREST for helping with the 
observations.


GRB_name: GRB190114B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23743
SUBJECT: GRB 190114B: continued optical observations in Mondy
DATE:    19/01/16 17:06:37 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova (IKI), A. Pozanenko (IKI),  E. Mazaeva (IKI),  E. Klunko 
(ISTP), S. Belkin (IKI) report   on behalf of IKI-GRB-FuN:

We observed the field of  the GRB  190114B (Siegel et al., GCN 23686) 
with AZT-33IK telescope of Sayan observatory (Mondy) starting on Jan. 15 
(UT) 21:06:04. The optical afterglow (e.g. Fernandez-Garcia et al., GCN 
23694;  Pozanenko et al., GCN 23696; Selsing et al., GCN 23713) is 
marginally detected in a stacked image. Preliminary photometry is following.

Date       UT start t-T0    Filter Exp.   OT    Err.
                    (mid, days) (s)

2019-01-15 21:06:04 1.08672 R      30*120 22.2 0.35

The photometry is based on nearby SDSS  stars
SDSS id             R_Lupton
J113927.36+185157.2 17.094 0.014
J113940.10+185315.3 17.015 0.015
J113939.20+185354.8 17.954 0.018


GRB_name: GRB190106A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23744
SUBJECT: GRB 190106A: Discovery Channel Telescope observations
DATE:    19/01/16 22:09:39 GMT
FROM:    Simone Dichiara at UMCP/NASA/GSFC  <dichiara@umd.edu>

S.Dichiara (UMD, NASA-GSFC), P. Gatkine (UMD), J.M. Durbak (UMD),
E. Troja (UMD, NASA-GSFC), A. Kutyrev (UMD, NASA-GSFC), S. Veilleux (UMD),
report on behalf of a larger collaboration:

We observed at the optical counterpart of GRB 190106A (Sonbas et al. GCN
23615) using the Large Monolithic Imager (LMI) on the 4.3m Discovery
Channel Telescope (DCT) at Happy Jack, AZ. Observations start on January
 08, 06:36:53 UT (about 41 hours after the Swift trigger) with SDSS r,
 i and z filters.
We measured the following magnitudes:

Start Time         Exposure       Filter    Magnitude
(hs from trigger)    (s)
--------------------------------------------------------------------
41.036               3x120          r'    20.77 +- 0.03
41.157               3x120          i'    20.60 +- 0.05
41.279               3x120          z'    20.70 +- 0.15
---------------------------------------------------------------------

Magnitudes are calibrated against SDSS nearby stars:
J015939.43+235056.5 25.7308, J015938.69+235101.6, J015933.94+235145.7 and
J015923.06+235109.1.
We thank the staff of the Discovery Channel Telescope for assistance with
these observations.


GRB_name: GRB190114C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23745
SUBJECT: GRB190114C: ATCA detection of the radio afterglow
DATE:    19/01/17 09:16:12 GMT
FROM:    Steve Schulze at U of Iceland  <sts30@hi.is>

S. Schulze (WIS), G. Anderson (ICRAR-Curtin), A. Moin (UAEU), E. Troja
(UMD & NASA/GSFC), M. Wieringa (CSIRO), J. Stevens (CSIRO), S. Klose (TLS
Tautenburg),  M. Bell (UTS), A. de Ugarte Postigo (HETH/IAA-CSIC and
DARK/NBI), S. Dichiara (UMD & NASA/GSFC),  L. Izzo (HETH/IAA-CSIC) D. A.
Kann (HETH/IAA-CSIC), M. Michalowski (AOI-AMU), J. Miller-Jones
(ICRAR-Curtin), K. Misra (ARIES), S. Nasri (UAEU), D. A. Perley (LJMU), L.
Piro (INAF IAPS Rome),  L. Resmi (IIST), R. Ricci (IRA Bologna),  and C.
C. Thoene (HETH/IAA-CSIC) report:

On 16 January 2019, we observed the field of GRB 190114C (Gropp et al. GCN
23688, Hamburg et al. GCN 23707) with the Australia Telescope Compact
Array (ATCA) at the central frequencies of 5.5, 9, 17 and 19 GHz each with
bandwidth of 2 GHz. The first data were obtained at 7:08 UTC.

At the position of the optical counterpart (Gropp et al., GCN 23688;
Tyurina et al. GCN 23690; Lipunov et al. GCN 23693; Selsing et al., GCN
23695; Izzo et al., GCN 23699; Bolmer et al., GCN 23702), we detect a
radio source with a brightness of approximately 2 mJy.

Further observations are planned.

We thank the CSIRO staff for approving and executing these observations.


GRB_name: GRB190114C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23746
SUBJECT: GRB 190114C: continued CHILESCOPE optical obs
DATE:    19/01/17 12:39:39 GMT
FROM:    Elena Mazaeva at IKI, Moscow  <30.v@mail.ru>

E. Mazaeva (IKI), A. Pozanenko (IKI), A. Volnova (IKI), S. Belkin (IKI), M. Krugov (FAPHI) report on behalf of IKI-GRB-FuN:

We observed the field of GRB 190114C (Gropp et al., GCN 23688) with RC-1000 telescope of CHILESCOPE observatory. Observations started on Jan. 17 (UT) 01:19:05 in r'-filter. We detected optical afterglow (Tyurina et al., GCN 23690; de Ugarte Postigo et al., GCN 23692; Lipunov et al. GCN 23693; Selsing et al. GCN 23695; Izzo et al. GCN 23699; Bolmer et al. GCN 23702; Castro-Tirado et al. GCN 23708; Kann et al. GCN 23710; Im et al. GCN 23717; Siegel et al. GCN 23725; Mazaeva et al., GCNs 23727, 23741; D'Avanzo et al., GCN 23729; Kim et al., GCNs 23732, 23734; Kumar et al., GCN 23742).
Preliminary photometry of a stacked image is following.

Date UT start t-T0 Filter Exp. OT Err. UL(3sigma)
                     (mid, days) (s)
2019-01-17 01:19:05 2.93361 r' 10*180 20.64 0.09 21.9

The photometry is based on several nearby PanSTARRS stars.
PanSTARRS_id r
75670544556329552 16.117
75640544615203120 18.270
75620545839473520 16.802
75610545901287840 14.901
75690546042320496 14.750


GRB_name: GRB190114C
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23747
SUBJECT: GRB 190114C: Continued UKIRT JHK observation
DATE:    19/01/17 14:35:59 GMT
FROM:    Myungshin Im at Seoul Nat U  <mim@astro.snu.ac.kr>

Myungshin Im, Gregory S. H. Paek, Changsu Choi (CEOU/SNU), on behalf of a
larger collaboration

We observed again the afterglow of GRB 190114C (Gropp et al., GCN 23688;
Tyurina et al., GCN 23690, de Ugarte Postigo et al., GCN 23692, Lipunov et
al. GCN 23693, Selsing et al. GCN 23695, Izzo et al. GCN 23699, Bolmer et
al. GCN 23702, Castro-Tirado et al. GCN 23708, Kann et al. GCN 23710, Im et
al. GCN 23717, 23741; Siegel et al. GCN 23725, Mazaeva et al. GCN 23727,
D'Avanzo et al. GCN 23729, Peak et al. GCN 23731, Kim et al. GCN 23732,
Kumar et al. GCN 23733, Mazaeva et al. GCN 23741, 23746, Kumar et al. GCN
23742) with the United Kingdom Infrared Telescope (UKIRT). The observation
started at 2019-01-17 05:06 UT or about 2.33 days after the initial alert.

Preliminary magnitudes are derived from quick-look data, using nearby 2MASS
stars as photometry references. The afterglow faded by about 0.5 magnitude
in all of the JHK bands with the J-band magnitude given below.

Filter Date UT-start Vega_Mag (AB mag)
J    2019-01-16 05:47:58.042    18.0 +/- 0.1   (19.2 AB)

The result implies that the current fading of NIR afterglow (0.5 mag/day)
is slower  than what we reported in a previous circular (1.2 mag/day) based
on earlier data (Im et al. GCN 23740).

Further observations are planned.
We thank the staffs at UKIRT for carrying out the observation.


GRB_name: GRB190114C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23748
SUBJECT: GRB 190114C: ePESSTO NTT optical observations
DATE:    19/01/17 15:24:40 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

F. Ragosta (U. Federico II/OACN), F. Olivares (MAS/U. de Chile), P. D'Avanzo (INAF-OAB), S. Campana, (INAF-OAB), M. De Pasquale (Istanbul Univ.), 
A. Melandri (INAF-OAB), E. Palazzi (INAF-OAS), S. Piranomonte (INAF-OAR), A. Rossi (INAF-OAS), O. Rodriguez (UNAB/MAS), G. Pignata (UNAB/MAS), 
Cristina Barbarino (Stockholm), Stefan Taubenberger (MPA-Garching), C. Inserra (Cardiff), E. Kankare (Turku), K. Maguire (QUB), S. J. Smartt (QUB), 
O. Yaron (Weizmann), D. R. Young (QUB), I. Manulis (Weizmann) report:


We observed the optical counterpart of GRB 190114C (Gropp et al., GCN Circ. 23688) under the extended Public ESO Spectroscopic Survey for Transient Objects 
(ePESSTO; see Smartt et al. 2015, A&A, 579, 40; http://www.pessto.org <http://www.pessto.org/>). The observations were performed on the ESO New Technology Telescope at La Silla with 
the EFOSC2 instrument in imaging mode starting at 04:36:53 UT on 2019-01-16 (i.e. about 1.32 days from the burst) and they were carried out with the g, r, i, z gunn 
filters. 

The optical afterglow is clearly detected in all bands. From preliminary photometry, we find a magnitude of r = 19.84 +/- 0.05 (AB, calibrated against the Pan-STARRS 
catalogue).


GRB_name: GRB190114C
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23749
SUBJECT: GRB 190114C: COATLI Optical Detection
DATE:    19/01/17 17:53:43 GMT
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
GonzÃ¡lez (UNAM), William H. Lee (UNAM), Margarita Pereyra (UNAM), Carlos
RomÃ¡n-ZÃºÃ±iga (UNAM), Alexander Kutyrev (GSFC), and Eleonora Troja
(GSFC) report:

We observed the field of GRB 190114C (Gropp et al., GCN Circ. 23688)
with the COATLI 50-cm telescope and interim imager at the Observatorio
AstronÃ³mico Nacional on the Sierra de San Pedro MÃ¡rtir
(http://coatli.astroscu.unam.mx) from 2019-01-17 02:25 to 2019-01-17
07:56 (from 53.7 to 59.2 hours after the trigger), obtaining a total of
2.93 hours of exposure in the w filter.

We detect a source coincident with the enhanced XRT position (Osborne et
al., GCN Circ. 23704) and possible host galaxy (de Ugarte Postigo et
al., GCN Circ. 23692) with w = 20.32 +/- 0.07.

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 (Fernando Ãngeles, Oscar Chapa,
Salvador Cuevas, Alejandro Farah, Jorge Fuentes, RosalÃ­a Langarica,
Fernando QuirÃ³s, and Carlos Tejada) and the staff of the Observatorio
AstronÃ³mico Nacional.


GRB_name: GRB190114C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23750
SUBJECT: GRB 190114C: RT-22 detection at 36.8 GHz
DATE:    19/01/17 17:57:30 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A.E. Volvach (CrAO), L.N. Volvach (CrAO), A. Pozanenko (IKI) report on 
behalf of IKI-GRB-FuN report:

We observed the field of GRB 190114C (Gropp et al., GCN 23688) with 
RT-22 telescope at 36.8 GHz on Jan. 15 and Jan. 16.
At the position of the optical afterglow (Tyurina et al., GCN
23690; Lipunov et al., GCN 23693; Selsing et al., GCN 23695)
and the XRT afterglow (Osborne et al. GCN 23704) we detected a source. 
Preliminary results of the observations are following.

Date       UT-start UT-stop  Flux   Err.
                              mJy    mJy

2019-01-15  16:02   18:11    3.9    0.9
2019-01-16  15:53   18:24    4.2    0.9


GRB_name: GRB190114C
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23751
SUBJECT: GRB 190114C: RATIR Optical and NIR Detections 
DATE:    19/01/17 18:07:47 GMT
FROM:    Alan M. Watson at Instituto de Astronomia UNAM  <alan@astro.unam.mx>

Alan M. Watson (UNAM), Nat Butler (ASU), Alexander Kutyrev (GSFC),
William H. Lee (UNAM), Michael G. Richer (UNAM), Ori Fox (STScI), J.
Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (UVI),
Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico Ramirez-Ruiz
(UCSC), JesÃºs GonzÃ¡lez (UNAM), Carlos RomÃ¡n-ZÃºÃ±iga (UNAM), Harvey
Moseley (GSFC), John Capone (UMD), V. Zach Golkhou (U. Wash.), and Vicki
Toy (UMD) report:

We observed the field of GRB 190114C (Gropp et al., GCN Circ. 23688)
with the Reionization and Transients Infrared Camera (RATIR;
www.ratir.org) on the 1.5m Harold Johnson Telescope at the Observatorio
AstronÃ³mico Nacional on Sierra San Pedro MÃ¡rtir from 2019/01 17.09 to
2019/01 17.29 UTC (53.26 to 58.02 hours after the BAT trigger),
obtaining a total of 0.88 hours of exposure in the g and r bands, 1.76
hours exposure i band, and 1.01 hours exposure in the Z, Y, J, and H
bands.

We detect a source coincident with the enhanced XRT position (Osborne et
al., GCN Circ. 23704) and possible host galaxy (de Ugarte Postigo et
al., GCN Circ. 23692) with the following magnitudes:

  r = 20.24 +/- 0.10
  i = 19.65 +/- 0.06
  Z = 19.48 +/- 0.05
  Y = 19.22 +/- 0.03
  J = 18.60 +/- 0.04
  H = 18.23 +/- 0.06

These magnitudes are in the AB system, in comparison with the USNO-B1
and 2MASS catalogs, and are not corrected for Galactic extinction in the
direction of the GRB.

The source is still considerably brighter in riz than the Pan-STARRs
photometry reported by de Ugarte Postigo et al. (GCN Circ. 23692).
Further observations are planned.

We thank the staff of the Observatorio AstronÃ³mico Nacional in San Pedro
MÃ¡rtir.


GRB_name: GRB190117A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23752
SUBJECT: GRB 190117A: AGILE/MCAL detection of a burst
DATE:    19/01/17 19:01:06 GMT
FROM:    Alessandro Ursi at INAF/IAPS  <alessandro.ursi@gmail.com>

A.Ursi (INAF/IAPS), C. Pittori (SSDC, and INAF/OAR), M. Tavani (INAF/IAPS,
and Univ. Roma Tor Vergata), A. Argan, M. Cardillo, C. Casentini, Y.
Evangelista, G. Piano (INAF/IAPS), F. Lucarelli, F. Verrecchia (SSDC, and
INAF/OAR), A. Bulgarelli, V. Fioretti, F. Fuschino, N. Parmiggiani
(INAF/OAS-Bologna), M. Marisaldi (INAF/OAS-Bologna, and Bergen University),
M. Pilia, A. Trois (INAF/OA-Cagliari), I. Donnarumma (ASI), F. Longo (Univ.
Trieste and INFN Trieste), A. Giuliani (INAF/IASF-Mi), report on behalf of
the AGILE Team:

The AGILE Mini-CALorimeter (MCAL) detected a burst at T0 = 2019-01-17
14:36:49.01 +/- 0.01 s (UTC).

In the 0.4-100 MeV energy range, the event lasted about 0.6 s and released
a total number of ~530 counts in the detector, above an average background
rate of 540 counts / s.

The GRB is clearly detected also by the AGILE scientific ratemeters: in
particular, by the Super-AGILE (20-60 keV), Anti-Coincidence (50-200 keV),
and MCAL (0.4-100 MeV) ratemeters.

Further analysis is still in progress.

The AGILE-MCAL detector has a full solid angle acceptance, and is
operational in the range 0.4 - 100 MeV.


GRB_name: GRB190114C
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23753
SUBJECT: GRB 190114C: Sardinia Radio Telescope observations
DATE:    19/01/18 09:45:52 GMT
FROM:    Marco Marongiu at Ferrara U  <marco.marongiu@unife.it>

M. Marongiu (U. Ferrara), G. Carboni, A. Melis, A. Pellizzoni 
(INAF/OAC), and Sara Loru (INAF/OACT), report on behalf of a larger 
collaboration:

We observed GRB 190114C (Gropp et al., GCN 23688) with the Sardinia 
Radio Telescope (SRT, www.srt.inaf.it) through single-dish imaging in 
C-band (central frequency 6.9 GHz, bandwidth 1.5 GHz) in the time 
interval 16:30-22:00 UTC on January 18, 2019 (2.8-3.1 days after the burst).

At the position of the radio afterglow (Alexander et al. GCN 23726), we 
did not detect any significant signal with a 2-sigma upper limit of 3 mJy.

We acknowledge the TAC, the scheduler and the SRT staff for approving 
and executing these observations.


GRB_name: GRB190114C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23754
SUBJECT: GRB 190114C: REM optical/NIR detection (CORRECTION) 
DATE:    19/01/18 10:30:16 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

P. D'Avanzo (INAF-OAB), on behalf of the REM team, report:

We noticed a typo in our GCN Circular 23729 (D'Avanzo et al.), reporting about REM observations of GRB 190114C. 
In that GCN Circular we reported a H-band magnitude, while the filter used to measure the NIR afterglow magnitude was J.

So, the magnitudes we measure in the REM images of GRB 190114C are:

r = 18.6 +/- 0.2
J = 16.7 +/- 0.1

(AB; calibrated against the pan-STARRS and the 2MASS catalogues), at a mean time of about 4.3 hours after the GRB. 

We apologize for any confusion this may have caused.


GRB_name: GRB190114C
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23755
SUBJECT: GRB 190114C: Sardinia Radio Telescope observations (CORRECTION)
DATE:    19/01/18 11:38:45 GMT
FROM:    Marco Marongiu at Ferrara U  <marco.marongiu@unife.it>

M. Marongiu (U. Ferrara), on behalf of our collaboration, report:

We noticed a typo in our GCN Circular 23753 (Marongiu et al.), reporting 
SRT observations.
The correct date is Jan 17 (2.8-3.1 days after the burst) instead of 18 
as reported.

We apologise for any confusion this may have caused.


GRB_name: GRB190114C
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23756
SUBJECT: GRB 190114C: UKIRT JHK observation continuation - steady fading?
DATE:    19/01/18 13:20:06 GMT
FROM:    Myungshin Im at Seoul Nat U  <mim@astro.snu.ac.kr>

Myungshin Im, Gregory S. H. Paek, Changsu Choi (CEOU/SNU), on behalf of a
larger collaboration

We continued the observation of the NIR afterglow of GRB 190114C (Gropp et
al., GCN 23688, D'Avanzo et al. GCN 23729, 23754, Im et al. GCN 23740,
23747, Watson et al. GCN 2375 ) with the United Kingdom Infrared Telescope
(UKIRT). Our 3rd epoch UKIRT observation started at 2019-01-18 05:04 UT or
about 3.33 days after the initial alert.

Preliminary magnitudes are derived from quick-look data, using nearby 2MASS
stars as photometry references. The afterglow faded by about 0.3 magnitude
in all of the JHK bands with the J-band magnitude given below, consistent
with the ~0.5 mag/day fading rate reported earlier (Im et al. GCN 23747).

Filter Date UT-start Vega_Mag (AB mag)
J      2019-01-18 08:30:12.989 18.3 +- 0.12 (19.2 AB)

In view of the recent correction report by D'Avanzo et al. (GCN 23754),
J-band fading rate is now 0.6 mag/day from 2019-01-15 to 2019-01-16, which
is consistent with the fading rate of ~0.5/day derived from the later epoch
data. However, the most recent result indicates that GRB may be fading a
bit slower as time goes on.
Note that host galaxy light is not subtracted.

Further observations are planned.
We thank the staffs at UKIRT for carrying out the observation.


GRB_name: GRB190114C
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23757
SUBJECT: GRB 190114C: UKIRT JHK observation (CORRECTIONS)
DATE:    19/01/18 13:36:07 GMT
FROM:    Myungshin Im at Seoul Nat U  <mim@astro.snu.ac.kr>

Myungshin Im, Gregory S. H. Paek, Changsu Choi (CEOU/SNU), on behalf of a
larger collaboration

The reported AB magnitudes in our earlier reports of UKIRT observations (Im
et al. GCN 23740, 23747) had errors in AB corrections, and hence the AB
magnitudes were reported to be a bit fainter than real. The Vega magnitudes
are correct. Also, the reported UT time in the table and the text of Im et
al. (GCN 23747, 23756) had errors. Below is a summary of our reported
photometry with corrections to the AB mag.

Filter Date UT-start Vega_Mag (AB mag)
K   2019-01-16 05:06:05.011    15.5 +/- 0.1   (17.4 AB)
H   2019-01-16 05:26:45.974    16.5 +/- 0.1   (17.9 AB)
J    2019-01-16 05:47:58.042   17.5 +/- 0.1    (18.4 AB)
J    2019-01-17 05:31:27.984   18.0 +/- 0.1    (18.9 AB)
J    2019-01-18 08:30:12.989   18.3 +- 0.12    (19.2 AB)

We apologize for any confusion that this might have caused.


GRB_name: GRB190117A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23759
SUBJECT: GRB 190117A: Insight-HXMT/HE detection
DATE:    19/01/19 09:26:21 GMT
FROM:    Shuo Xiao at IHEP  <xiaoshuo@ihep.ac.cn>

S. Xiao, 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, J. L. Zhao,
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 2019-01-17T14:36:47.000 (T0), the Insight-HXMT/HE detected 
GRB 190117A (trigger ID: HEB190117608) in a routine search of the data, 
which was also triggered by Konus-Wind and INTEGRAL/SPI-ACS.

The Insight-HXMT/HE light curve mainly consists of multiple 
pulses with a duration (T90) of 23.29 s measured from T0+0.13 s. 
The 1-s peak rate, measured from T0+1.97 s, is 5013.1 cnts/s. 
The total counts from this burst is 21613.5 counts. 
URL_LC: http://www.hxmt.org/images/GRB/HEB190117608_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 (record 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 could be found at: http://www.hxmt.org.


GRB_name: GRB190114C
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23760
SUBJECT: GRB 190114C: MeerKAT radio observation
DATE:    19/01/19 21:03:10 GMT
FROM:    Alexander van der Horst at George Washington U  <ajvanderhorst@gwu.edu>

L. Tremou (CEA-Saclay), I. Heywood (Oxford/Rhodes), A.J. van der Horst
(GWU), S.D. Vergani (GEPI), P.A. Woudt (UCT), R.P. Fender (Oxford/UCT),
A. Horesh (HUJI), S. Passmoor and S. Goedhart (SARAO) report on behalf
of the ThunderKAT collaboration:

We observed the position of the GRB 190114C afterglow at 1.3 GHz with
the new MeerKAT radio telescope on January 15, from 18.25 to 20.74 UT,
i.e. 0.94 days after the burst (GCN 23688). We detect a radio source at
the position of the afterglow. The afterglow flux is uncertain due to
emission from the host galaxy, detected in a pre-GRB observation of the
field (MIGHTEE collaboration, private comm.). However, the flux level
indicates significant synchrotron self-absorption in the GHz range (GCN
23745). The two emission components will be disentangled with further
analysis and follow-up observations.

We would like to thank the staff at the South African Radio Astronomy
Observatory (SARAO) for scheduling and obtaining these observations.


GRB_name: GRB190114C
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23762
SUBJECT: GRB 190114C: GMRT detection at 1.26GHz
DATE:    19/01/20 19:57:03 GMT
FROM:    Kuntal Misra at ARIES,India  <kuntal@aries.res.in>

S. V. Cherukuri (IIST), V. Jaiswal (IIST), K. Misra (ARIES),  L. Resmi (IIST), S. Schulze (WIS) and A. de Ugarte Postigo (HETH/IAA-CSIC and DARK/NBI) report on behalf of a larger collaboration :

We observed the field of GRB 190114C (Gropp et al. GCN 23688, Hamburg et al. GCN 23707) with the Giant Meterwave Radio Telescope (GMRT) at a mean frequency of 1.26GHz on 17th Jan 2019 13.44 UT (2.8 days after burst).  At the position of the JVLA radio afterglow (Alexander et al., GCN 23726), we report a weak detection of 73+/-17 micro Jy.  The measurement is not corrected for host which is detected in the pre-explosion images obtained with MeerKAT (Tremou et al.  GCN 23760).  The data were reduced using the customised CASA pipeline presented in Ishwara-Chandra et al. (2019).  Further observations are planned.  

We thank the staff of the GMRT for making these observations possible. GMRT is run by the National Centre for Radio Astrophysics of the Tata Institute of Fundamental Research.


GRB_name: GRB190117A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23764
SUBJECT: IPN Triangulation of GRB 190117A (long)
DATE:    19/01/21 16:44:34 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

K. Hurley, on behalf of the IPN,

I. G. Mitrofanov, D. Golovin, M. L. Litvak, and A. B. Sanin,
on behalf of the HEND-Odyssey GRB team,

D. Svinkin, S. Golenetskii, R. Aptekar, D. Frederiks, A. Kozlova
and T. Cline on behalf of the Konus-Wind team,

A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo,
and C. Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team,

S. Barthelmy, J. Cummings, H. Krimm, and D. Palmer,
on behalf of the Swift-BAT team,

S. Xiao, C. K. Li, X. B. Li, Y. Huang, and S. L. Xiong
on behalf of the Insight-HXMT GRB team,

and

W. Boynton, C. Fellows, K. Harshman, H. Enos, and R. Starr,
on behalf of the GRS-Odyssey GRB team, report:

The long-duration GRB 190117A was detected by
AGILE (MCAL; Ursi, et al., GCN Circ. 23752),
Insight (HXMT/HE; Xiao et al., GCN Circ. 23759),
Konus-Wind, INTEGRAL (SPI-ACS), and Swift (BAT),
at about 52607 s UT (14:36:47).
The burst was outside the coded field of view of the BAT.

We have triangulated it to a preliminary, 3 sigma error box
whose coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   113.864 (07h 35m 27s)  +6.519 ( +6d 31' 10")
  Corners:
   113.942 (07h 35m 46s)  +8.247 ( +8d 14' 49")
   113.615 (07h 34m 28s)  +5.249 ( +5d 14' 56")
   113.807 (07h 35m 14s)  +4.881 ( +4d 52' 52")
   114.126 (07h 36m 30s)  +7.833 ( +7d 49' 58")
  ---------------------------------------------
The error box area is about 2453 sq. arcmin, and its maximum
dimension is 3.369 deg (the minimum one is 13.68 arcmin).
The Sun distance was about 163 deg.

This box may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB190117_T52611/IPN

The Konus-Wind time history and spectrum will be given in a forthcoming
GCN Circular.


GRB_name: GRB190118A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23765
SUBJECT: IPN Triangulation of GRB 190118A (long)
DATE:    19/01/21 16:59:08 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

D. Svinkin, S. Golenetskii, R. Aptekar, D. Frederiks, A. Kozlova,
and T. Cline on behalf of the Konus-Wind team,

K. Hurley, on behalf of the IPN,

A. Goldstein, M. S. Briggs, and C. Wilson-Hodge
on behalf of the Fermi GBM team,

A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo,
and C. Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team,

and

S. Barthelmy, J. Cummings, H. Krimm, and D. Palmer,
on behalf of the Swift-BAT team, report:

The long-duration GRB 190118A was detected by
Fermi (GBM; trigger 569543394), INTEGRAL (SPI-ACS),
Konus-Wind, and Swift (BAT), at about 80990 s UT (22:29:50).
The burst was outside the coded field of view of the BAT.

We have triangulated it to a preliminary, 3 sigma error box
whose coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   232.423 (15h 29m 42s) +74.202 (+74d 12' 06")
  Corners:
   220.973 (14h 43m 54s) +89.312 (+89d 18' 44")
   263.843 (17h 35m 22s) +88.731 (+88d 43' 51")
   230.052 (15h 20m 13s) +55.646 (+55d 38' 46")
   228.831 (15h 15m 19s) +56.984 (+56d 59' 01")
  ---------------------------------------------
The error box area is 26.0 sq. deg, and its maximum
dimension is 33.7 deg (the minimum one is 47.5 arcmin).
The Sun distance was 96 deg.

This box may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB190118_T80991/IPN/

The time history and spectrum will be given in forthcoming
GCN Circulars.


GRB_name: GRB190114C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23766
SUBJECT: GRB 190114C: RTT150 optical observations
DATE:    19/01/21 20:05:18 GMT
FROM:    Rodion Burenin at IKI, Moscow  <rodion@hea.iki.rssi.ru>

I. Bikmaev, E. Irtuganov, N. Sakhibullin (KFU/AST),
R. Burenin, M. Pavlinsky, R. Sunyaev (IKI),
I. Khamitov, S. Ozdemir (TUG), E. Gogus (Sabanci Uni.)

report:

We observed the field of GRB 190114C (Gropp et al., GCN 23688)
with the Russian-Turkish 1.5-m optical telescope (RTT150, Bakirlitepe,
TUBITAK National Observatory, Turkey) using the TFOSC instrument.

We obtained series of Rc exposures in January 17, 2019 (6 frames x 300
sec, UT = 17:42 - 18:28), ~ 69 hours after the burst. In the combined
image we detected the optical transient observed earlier by many
groups (Tyurina et al., GCN 23690; de Ugarte Postigo et al., GCN
23692; Lipunov et al. GCN 23693; Selsing et al. GCN 23695; Izzo et
al. GCN 23699; Bolmer et al. GCN 23702; Castro-Tirado et al. GCN
23708; Kann et al. GCN 23710; Im et al. GCN 23717; Siegel et al. GCN
23725; Mazaeva et al., GCNs 23727, 23741; D'Avanzo et al., GCN 23729;
Kim et al., GCNs 23732, 23734; Kumar et al., GCN 23742, Mazaeva et
al., GCN 23746, Ragosta et al., GCN 23748, Watson at al., GCN 23749,
Watson et al., GCN 23751).

Using the observations of Landolt standard stars we estimated the
brightness of the optical object in the combined image as
Rc=20.7+-0.1. Taking into account host galaxy brightness, r'=21.23,
measured from Pan-STARRS archival imaging by de Ugarte Postigo et al
(GCN 23692) we can conclude that OT brighness should be around
21.8+-0.1.


GRB_name: GRB190122A
Detection_method: Fermi LAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23767
SUBJECT: GRB 190122A: Fermi-LAT detection
DATE:    19/01/22 16:32:13 GMT
FROM:    Magnus Axelsson at Stockholm U.  <magaxe@kth.se>

F. Longo (University and INFN Trieste), E. Bissaldi (Politecnico & INFN Bari), M. Axelsson (KTH & Stockholm Univ.), M. Arimoto (Kanazawa Univ.), F. Piron (CNRS/IN2P3/LUPM) and N. Omodei (Stanford Univ.) report on behalf of the Fermi-LAT team:

On January, 22, 2019, Fermi-LAT detected high-energy emission from GRB 190122A, which was also detected by the Fermi GBM (trigger 569834352 / 190122305).

The best LAT on-ground location is found to be

RA, Dec =  258.71, 48.12 (degrees, J2000)

with an error radius of 0.91 deg (90% containment, statistical error only).

The LAT position was 26 deg from the LAT boresight at the time of the GBM trigger time (07:19:07.57 UT) and remained in the LAT field of view for ~1000 seconds, and then re-entered the FoV ~3800s after the trigger.

The data from the Fermi-LAT show a significant increase in the event rate above 100 MeV during the interval 0 4000s that is spatially correlated with the GBM trigger. The spectrum of the GRB appears to be soft, and the highest-energy photon is a 310 MeV event, which is observed ~820 seconds after the GBM trigger.

GRB190122A is also detected with high significance in the LAT Low Energy events (LLE), with a time profile which is temporally coincident with the GBM light curve.

Further analysis will be performed as more data become available.



The Fermi-LAT point of contact for this burst is Francesco Longo (francesco.longo@ts.infn.it<mailto:francesco.longo@ts.infn.it>).

The Fermi-LAT is a pair conversion telescope designed to cover the energy band from 20 MeV to greater than 300 GeV. It is the product of an international collaboration between NASA and DOE in the U.S. and many scientific institutions across France, Italy, Japan and Sweden.


GRB_name: GRB190122A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23768
SUBJECT: GRB 190122A: Fermi GBM observation
DATE:    19/01/22 22:01:37 GMT
FROM:    Peter Veres at UAH  <veresp@gmail.com>

E. Bissaldi (Politecnico & INFN Bari), C. Meegan (UAH) and P. Veres (UAH)
report on behalf of the Fermi GBM Team:


"At 07:19:07.57 UT on 22 January 2019, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 190122A (trigger 569834352 / 190122305),
which was also detected by the Fermi/LAT (Longo et al. 2019, GCN 23767).
The GBM on-ground location is consistent with the LAT position.

The angle from the Fermi LAT boresight at the GBM trigger time is 26
degrees.

The GBM light curve consists of a single FRED-like pulse
with a duration (T90) of about 54 s (50-300 keV).
The time-averaged spectrum from T0+0.8 s to T0+22.3 s is
adequately fit by a simple power law function with index -1.59 +/- 0.01.

The event fluence (10-1000 keV) in this time interval is
(3.95 +/- 0.10)E-7 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+5.6 s in the 10-1000 keV band
is 6.3 +/- 0.3 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB190123A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23769
SUBJECT: GRB 190123A: Swift detection of a burst
DATE:    19/01/23 12:32:59 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

A. D'Ai (INAF-IASFPA), D. N. Burrows (PSU), J.D. Gropp (PSU),
N. P. M. Kuin (UCL-MSSL), K. L. Page (U Leicester) and
M. H. Siegel (PSU) report on behalf of the Neil Gehrels Swift
Observatory Team:

At 12:19:13 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 190123A (trigger=885314).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 53.229, +45.484 which is 
   RA(J2000) = 03h 32m 55s
   Dec(J2000) = +45d 29' 02"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single-peaked
structure with a duration of about 20 sec.  The peak count rate
was ~1400 counts/sec (15-350 keV), at ~4 sec after the trigger. 

The XRT began observing the field at 12:21:10.4 UT, 117.3 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 53.22071, 45.52425 which
is equivalent to:
   RA(J2000)  = 03h 32m 52.97s
   Dec(J2000) = +45d 31' 27.3"
with an uncertainty of 4.0 arcseconds (radius, 90% containment). This
location is 146 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. No spectrum from the promptly downlinked
event data is yet available to determine the column density. 

The initial flux in the 2.5 s image was 7.12e-10 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 125 seconds with the White filter
starting 124 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 extinction. 

Burst Advocate for this burst is A. D'Ai (antonino.dai 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.)


GRB_name: GRB190123A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23770
SUBJECT: GRB 190123A: MASTER Global Robotic Net optical observation
DATE:    19/01/23 13:27:41 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <lipunov@xray.sai.msu.ru>

V. Lipunov, V.Kornilov, E. Gorbovskoy, N.Tiurina, P.Balanutsa, D.Vlasenko, V.Vladimirov, A.Kuznetsov,  D.Kuvshinov, A.Chasovnikov
(Lomonosov Moscow State University,SAI, Physics Department),

O. Gres, N.M. Budnev, 
(Applied Physics Institute of Irkutsk State University)

V. Yurkov, A. Gabovich, Yu. Sergienko, D. Kobcev
(Blagoveschensk Educational State University)

R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres
(The Instituto de Astrofisica de Canarias)

D. Buckley (South African Astronomical Observatory)

A. Tlatov, V.Senik, D. Dormidontov
(Kislovodsk Solar Station of the Pulkovo Observatory)


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-Tunka robotic telescope (MASTER Global Robotic Net http://observ.pereplet.ru,
Lipunov et al., 2010, Advances in Astronomy, v.2010, 30L)
  located in Russia (Applied Physics Institute, Irkutsk State University)
was pointed to the  GRB190123A 17 sec after notice time (66 sec after trigger time)
at 2019-01-23 12:20:25 UT.
On our first (10s exposure) image we don't find  optical transient  within 
SWIFT-XRT error-box ( A. D'Ai et al. GCN 23769 RA,Dec(2000)=03h 32m 52.97s +45d 31' 27.3" r=4")
up to 16.7 unfiltered magnitude limit (5-sigma)

The galactic latitude b = -8 deg., longitude l = 151 deg.
The observations made on zenit distance =  7 deg.
The Moon altitude is -1 deg. (92 % bright part)
The sun  altitude  is -24.7 deg.


MASTER-Amur robotic telescope ocated in Russia (Blagoveshchensk State Pedagogical University)
was pointed to the  GRB190123A 27 sec after notice time (77 sec after trigger time)
  at 2019-01-23 12:20:35 UT.
On our first (10s exposure, mlim=16.3 (5-sigma)) image we don't find optical transient
within SWIFT-XRT error-box.

The observations made on zenit distance = 15 deg.
The moon (92 % bright part) is 14 deg. above the horizon.
The sun  altitude  is -40.1 deg.

The message may be cited.


GRB_name: GRB190123A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23771
SUBJECT: GRB 190123A: Enhanced Swift-XRT position
DATE:    19/01/23 14:07:26 GMT
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 80 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 190123A, 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 = 53.22060, +45.52531 which is equivalent
to:

RA (J2000): 03h 32m 52.94s
Dec (J2000): +45d 31' 31.1"

with an uncertainty of 2.3 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.


GRB_name: GRB190123A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23772
SUBJECT: GRB 190123A: BOOTES-4/MET optical limit
DATE:    19/01/23 14:11:37 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

Y.-D. Hu, X.-Y.Li, E. Fernandez-Garcia, A. Ayala, A. J. Castro-Tirado 
(IAA-CSIC), C. Perez del Pulgar, A. Castellon, I. Carrasco (Univ. de 
Malaga),  S. Guziy (Univ. of Nikolaev) and D. Xiong, Y. Fan, X. Zhao, J. 
Bai, C. Wang, Y. Xin (Yunnan Nacional Astronomical Observatory) on 
behalf of a larger collaboration, report:

"Following the detection of GRB 190123A by Swift (D'Ai et al. GCNC 
23769), the 0.6m BOOTES-4/MET robotic telescope at Lijiang Astronomical 
Observatory (China) gathered images starting at 12:36 UT (~0.29 hr after 
trigger). No optical afterglow is found down to 20.9 mag (unfiltered 
images) within the Swift/XRT error box, consistent with the 
non-detections by Swift/UVOT (D'Ai et al. GCNC 23769) or MASTER (Lipunov 
et al. GCNC 23770). Observations are ongoing."


GRB_name: GRB190123A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23773
SUBJECT: GRB 190123A: Fermi GBM observation
DATE:    19/01/23 17:30:47 GMT
FROM:    Elisabetta Bissaldi at INFN,Bari  <elisabetta.bissaldi@ba.infn.it>

E. Bissaldi (Politecnico & INFN Bari)
reports on behalf of the Fermi GBM Team:


"At 12:19:18.22 UT on 23 January 2019, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 190123A (trigger 569938763 / 190123513),
which was also detected by the Swift/BAT (D'Ai et al. 2019, GCN 23769).
The GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight at the GBM trigger time is 42 degrees.

The GBM light curve consists of a multipeaked emission episode
with a duration (T90) of about 17 s (50-300 keV).
The time-averaged spectrum from T0-5.1 s to T0+10.8 s is
adequately fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.68 +/- 0.25 and
the cutoff energy, parameterized as Epeak, is 310 +/- 100 keV.

The event fluence (10-1000 keV) in this time interval is
(2.07 +/- 0.04)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+7.1 s in the 10-1000 keV band
is 1.8 +/- 0.2 ph/s/cm^2.


The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB190123A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23774
SUBJECT: GRB 190123A: GOTO optical limit
DATE:    19/01/23 22:41:39 GMT
FROM:    Danny Steeghs at U.of Warwick/GOTO  <dsteeghs@gmail.com>

D.Steeghs, J.Lyman, K.Ulaczyk (U. Warwick), G.Ramsay (Armagh O.),
M.Dyer (U. Sheffield), A.Obradovic, K. Ackley, D.K. Galloway, E.Rol
(Monash U.), K. Wiersema, B.Gompertz, A.Levan, R.Cutter  (U. Warwick),
V.Dhillon (U. Sheffield), P.O'Brien, R.Starling (U. Leicester),
S.Poshyachinda
(NARIT), D.Pollacco (U. Warwick), E.Thrane (Monash U.), E.Palle (IAC)

report on behalf of the GOTO collaboration:

In response to GRB 190123A (D'Ai et al. GCN Circ. 23769), the
Gravitational-wave Optical Transient Observer (GOTO) observed the
field covering the Swift BAT/XRT positions.

Observations started at 2019-01-23T19:51:53 (7.54 hours post burst)
consisting of a set of 5x120s exposures in our wide L filter
(400-700nm). In line with other reports (Hu et al. GCN 23772;
Lipunov et al. GCN 23770), no optical source g<21.0 is visible
at the updated XRT position (Beardmore et al. GCN 23771),
based on PS1 and SDSS calibrators.

GOTO is operated at the La Palma observing facilities of the
University of Warwick on behalf of a consortium including the
University of Warwick, Monash University, Armagh Observatory, the
University of Leicester, the University of Sheffield, the National
Astronomical Research Institute of Thailand (NARIT) and the Instituto
de Astrofisica de Canarias (IAC) (https://goto-observatory.org/)


GRB_name: GRB190123A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23775
SUBJECT: GRB 190123A: Swift-XRT refined Analysis
DATE:    19/01/24 01:25:27 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

A. Tohuvavohu (PSU), S. J. LaPorte (PSU), J.A. Kennea (PSU), P.A. Evans
(U. Leicester), J.P. Osborne (U. Leicester), K.L. Page (U. Leicester),
A. Melandri (INAF-OAB), P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC) and A.
D'Ai report on behalf of the Swift-XRT team:

We have analysed 8.3 ks of XRT data for GRB 190123A (D'Ai et al. GCN
Circ. 23769), from 123 s to 33.3 ks after the  BAT trigger. The data
comprise 41 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. 23771).

The light curve can be modelled with a power-law decay with a decay
index of alpha=1.28 (+0.06, -0.05).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.8 (+0.5, -0.4). The
best-fitting absorption column is  2.3 (+0.9, -0.7) x 10^22 cm^-2, in
excess of the Galactic value of 4.4 x 10^21 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 7.0 x 10^-11 (1.3 x 10^-10) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      2.3 (+0.9, -0.7) x 10^22 cm^-2
Galactic foreground: 4.4 x 10^21 cm^-2
Excess significance: 4.3 sigma
Photon index:      1.8 (+0.5, -0.4)

If the light curve continues to decay with a power-law decay index of
1.28, the count rate at T+24 hours will be 1.2 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 8.6 x
10^-14 (1.6 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/00885314.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB190123A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23777
SUBJECT: GRB 190123A: GMG observational limit
DATE:    19/01/24 05:53:15 GMT
FROM:    Jirong Mao at Yunnan Obs  <jirongmao_obs@ynao.ac.cn>

J. Mao, L.-F. Xing, M. Xiao, J.-M. Bai (YNAO) report: 


We observed the field of GRB 190123A (D'Ai et al. GCN Circ. 23769) with the 2.4-meter optical telescope at Gao-Mei-Gu (GMG) station of Yunnan Observatories. The observation began at UT 13:15:51, 23, Jan, 2019, about 1 hour after the trigger. We did not detect any source within the Swift-XRT error circle down to a magnitude of R~22.7.


GRB_name: GRB190123A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23778
SUBJECT: GRB190123A: MITSuME Akeno optical upper limits
DATE:    19/01/24 10:11:22 GMT
FROM:    Kazuki Shiraishi at Tokyo Institute of Technology  <shiraishi@hp.phys.titech.ac.jp>

K. Shiraishi, K. L. Murata, R. Itoh, Y. Tachibana, S. Harita,

K. Morita, K. Iida, M. Niwano, R. Adachi, M. Oeda,  Y. Yatsu,

and N. Kawai (Tokyo Tech) report on behalf of the MITSuME collaboration



We searched for the optical counterpart of

GRB 190123A (A. D'Ai et al., GCN #23769)

with the optical three color (g', Rc, and Ic)

CCD cameras attached to the MITSuME 50 cm telescope at Akeno

Observatory,Yamanashi, Japan.



The observation started on 12:20:56 UT which corresponds to 103 sec

after the trigger.

We did not find any new point source within the enhanced XRT circle

Dâ€™Ai et al., GCN #23769;  A.P. Beardmore et al., GCN #23771) in all three bands.

We obtained following 5 sigma limits for the magnitudes.



T0+[sec]    MID-UT      T-EXP[sec]    g'       Rc        Ic

-------------------------------------------------------------------------------------------------------

103  12:25:31    540    >18.2     >17.8     >17.0

723  12:35:51    540    >17.9     >17.7     >17.6

1,764  14:21:35    10,800    >18.4     >18.2     >17.4

-------------------------------------------------------------------------------------------------------

T0+ : Elapsed time after the burst

T-EXP: Total Exposure time

We used UCAC-4 catalog for flux calibration.


GRB_name: GRB190121A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23779
SUBJECT: GRB 190121A: CALET Gamma-Ray Burst Monitor detection of a short burst
DATE:    19/01/24 12:08:28 GMT
FROM:    Valentin Pal'shin at AGU  <val@phys.aoyama.ac.jp>

S. Matsukawa, A. Yoshida, T. Sakamoto, V. Pal'shin, S. Sugita (AGU),
Y. Kawakubo (LSU), A. Tezuka, H. Onozawa, T. Ito, H. Morita, Y. Sone (AGU),
K. Yamaoka (Nagoya U), S. Nakahira (RIKEN), I. Takahashi (IPMU),
Y. Asaoka, S. Ozawa, S. Torii (Waseda U),
Y. Shimizu, T. Tamura (Kanagawa U),
W. Ishizaki (ICRR), M. L. Cherry (LSU),
S. Ricciarini (U of Florence),
A. V. Penacchioni, P. S. Marrocchesi (U of Siena),
and the CALET collaboration:

At 12:55:17.284 UTC on 21 January 2019, the CALET Gamma-ray Burst 
Monitor (CGBM)
triggered on GRB 190121A.
The burst signal was detected only by the SGM detector.
Because of a problem in one of the ground alert processing scripts,
the GCN notice was not distributed automatically for this event.

This GRB is also clearly seen by the publicly available
INTEGRAL SPI-ACS light curve.

The burst light curve shows a short pulse which
starts at T-0.224 sec and ends at T+0.096 sec.
The T90 and the T50 durations measured by the SGM data are
0.288 s +- 0.091 sec and 0.128 +- 0.101 sec (40-1000 keV), respectively.

The ground processed light curve is available at

http://cgbm.calet.jp/cgbm_trigger/ground/1232110402/

The CALET data used in this analysis are provided by
the Waseda CALET Operation Center located at the Waseda University.


GRB_name: GRB190123A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23780
SUBJECT: GRB 190123A: Swift-BAT refined analysis
DATE:    19/01/24 12:20:11 GMT
FROM:    Hans Krimm at NSF/NASA-GSFC  <hkrimm@nsf.gov>

A. Y. Lien (GSFC/UMBC), S. D. Barthelmy (GSFC),  J. R. Cummings (CPI),
A. D'Ai (INAF-IASFPA), H. A. Krimm (NSF/USRA), 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 190123A (trigger #885314)
(D'Ai, et al., GCN Circ. 23769).  The BAT ground-calculated position is
RA, Dec = 53.175, 45.505 deg, which is
   RA(J2000)  =  03h 32m 42.0s
   Dec(J2000) = +45d 30' 16.3"
with an uncertainty of 1.7 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 64%.

The mask-weighted light curve shows a single FRED-shaped peak from about
T-5 to T+20 sec, with a peak around T+3 sec.   Observations were discontinued
due to an observing constraint at ~T+325 sec.  T90 (15-350 keV) is
24.4 +- 4.3 sec (estimated error including systematics).

The time-averaged spectrum from T-1.22 to T+28.06 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.13 +- 0.23.  The fluence in the 15-150 keV band is 8.4 +- 1.1 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+4.82 sec in the 15-150 keV band
is 1.0 +- 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/885314/BA/


GRB_name: GRB190123A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23781
SUBJECT: GRB 190123A: COATLI Optical Observations 
DATE:    19/01/24 12:51:10 GMT
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
GonzÃ¡lez (UNAM), William H. Lee (UNAM), Margarita Pereyra (UNAM), Carlos
RomÃ¡n-ZÃºÃ±iga (UNAM), Alexander Kutyrev (GSFC), and Eleonora Troja (GSFC)
report:

We observed the field of GRB 190123A (D'Ai et al., GCN Circ. 23769) with
the COATLI 50-cm telescope and interim imager at the Observatorio
AstronÃ³mico Nacional on the Sierra de San Pedro MÃ¡rtir
(http://coatli.astroscu.unam.mx) from 2019-01-24 02:30 to 2019-01-23
10:56 (from 14.2 to 22.6 hours after the trigger), obtaining a total of
6.7 hours of exposure in the w filter.

We do not detect a source at the enhanced XRT position (Beardmore et
al., GCN Circ. 23771) to a 5-sigma upper limit of w > 22.9.

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.

Our deeper non-detection follows non-detections reported by Lipunov et
al. (GCN Circ. 23770), Hu et al. (GCN Circ. 23772), Steeghs et al. (GCN
Circ. 23774), and Shiraishi et al.(GCN Circ. 23778).

We thank the COATLI technical team and the staff of the Observatorio
AstronÃ³mico Nacional.


GRB_name: GRB190117A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23782
SUBJECT: Konus-Wind of observation of GRB 190117A
DATE:    19/01/24 14:12:03 GMT
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 190117A (Agile/MCAL detection: Ursi et al., GCN 23752;
Insight-HXMT/HE detection: Xiao et al., GCN 23759,
IPN triangulation: Hurley et al., GCN 23764)
triggered Konus-Wind (KW) at T0=52611.684 s UT (14:36:51.684).

The burst light curve shows a weak emission pulse at ~T0-10 s and
three bright pulses in the interval from ~T0 to ~T0+30 s.
A total duration of the burst (T100) is ~36.3 s.
The emission is seen up to ~15 MeV.

As observed by Konus-Wind, the burst had a fluence of
(4.1 Â± 0.3)x10^-5 erg/cm2 and a 64-ms peak energy flux,
measured from T0+1.984, of (1.66 Â± 0.13)x10^-5 erg/cm2
(both in the 20 keV - 10 MeV energy range).

The time-integrated spectrum (measured from T0 to T0+33.024 s)
is best fit in the 20 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -1.19 (-0.08,+0.07),
the high energy photon index beta = -2.67 (-0.60,+0.27),
the peak energy Ep = 190 (-17,+18) keV
(chi2 = 90/97 dof).

The spectrum near the peak count rate (measured from T0
to T0+8.448 s) is best fit in the 20 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
alpha = -1.04 (-0.08,+0.07),
beta = -2.68 (-0.44,+0.23),
Ep = 208 (-18,+20) keV
(chi2 = 74/97 dof).

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB190117_T52611/

All the quoted errors are estimated at the 68% confidence level.
All the presented results are preliminary.


GRB_name: GRB190122A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23783
SUBJECT: Konus-Wind observation of GRB 190122A
DATE:    19/01/24 14:34:28 GMT
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 190122A
(Fermi-LAT detection: Longo et al., GCN Circ. 23767;
Fermi-GBM detection: Bissaldi et al., GCN Circ. 23768)
triggered Konus-Wind at T0=26347.426 s UT (07:19:07.426).

The burst light curve shows a FRED-like pulse
which starts at ~T0-0.4 s and has a total duration of ~67 s.
The emission is seen up to ~6 MeV.

As observed by Konus-Wind, the burst
had a fluence of 3.52(-0.74,+0.85)x10^-5 erg/cm2,
and a 64-ms peak flux, measured from T0-0.046 s,
of 3.77(-1.47,+3.90)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+73.984 s)
is best fit in the 20 keV - 15 MeV range
by a simple power-law function with the
photon index = -1.58(-0.08,+0.08), chi2 = 80/99 dof.
Fitting by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
yields alpha = -1.48(-0.12,+0.16)
and only an upper limit on Ep: Ep > 560 keV
(chi2 = 76/98 dof).

The spectrum near the maximum count rate
(measured from T0 to T0+8.448 s)
is best fit in the 20 keV - 15 MeV range
by a power law with exponential cutoff model:
with  alpha = -1.43(-0.16,+0.17)
and Ep = 718(-337,+7104) keV (chi2 = 99/98 dof).

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB190122_T26347/

All the quoted errors are at the 90% confidence level.
All the quoted values are preliminary.


GRB_name: GRB190123A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23784
SUBJECT: GRB 190123A: Swift/UVOT Upper Limits
DATE:    19/01/24 14:44:09 GMT
FROM:    Mike Siegel at PSU/Swift MOC  <mhs18@psu.edu>

M. H. Siegel (PSU) 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 190123A
124 s after the BAT trigger (D'Ai et al., GCN Circ. 23769).
No optical afterglow consistent with the XRT position
(Beardmore et al. GCN Circ. 23771)
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           124          250          123         >20.3
white              124        10248         1258         >22.0
v                 3470        11721          947         >20.3
b                 4290         5926          393         >21.1
u                 4085         5721          393         >21.0
w1                3880         5516          393         >20.1
m2                3675         5310          393         >19.9
w2                4701        11151         1079         >21.1

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.44 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB190123A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23786
SUBJECT: GRB 190123A: AROMA-N Optical Observation
DATE:    19/01/24 14:59:31 GMT
FROM:    Takanori Sakamoto at AGU  <tsakamoto@phys.aoyama.ac.jp>

M. Nakamura, T. Sakamoto (AGU)

We observed the field of GRB 190123A detected by Swift
(D'Ai et al., GCN Circ. 23769) with the 14-inch AGU Robotic
Optical Monitor for Astrophysical object - Narrow (AROMA-N)
located at the Sagamihara campus of Aoyama Gakuin University.

30 images of 60 sec exposures were taken in the R filter
starting from January 23 12:21:49 (UT) about 156 seconds
after the trigger and stopped on January 23 12:58:25 (UT).
We do not detect the optical afterglow both in the individual
images and the stacked image.  The estimated five sigma
upper limit of the combined image (total exposure of 1800 sec)
is ~17.7 mag using the USNO-B1 catalog.


GRB_name: GRB190114C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23787
SUBJECT: GRB 190114C: CHILESCOPE optical observations
DATE:    19/01/24 17:10:35 GMT
FROM:    Elena Mazaeva at IKI, Moscow  <30.v@mail.ru>

E. Mazaeva (IKI), A. Pozanenko (IKI), A. Volnova (IKI), S. Belkin (IKI), M. Krugov (FAPHI) report on behalf of IKI-GRB-FuN:

We observed the field of GRB 190114C (Gropp et al., GCN 23688) with RC-1000 telescope of CHILESCOPE observatory. Observations started on Jan. 24 (UT) 01:11:25. We obtained several images in r'-filter with FWHM of 1.0 arcsec. We detected optical afterglow (Tyurina et al., GCN 23690; Lipunov et al. GCN 23693; Selsing et al. GCN 23695; Izzo et al. GCN 23699; Bolmer et al. GCN 23702; Castro-Tirado et al. GCN 23708; Kann et al. GCN 23710; Im et al. GCNs 23717, 23747, 23757; Siegel et al. GCN 23725; Mazaeva et al., GCNs 23727, 23741, 23746; D'Avanzo et al., GCNs 23729, 23754; Kim et al., GCNs 23732, 23734; Kumar et al., GCN 23742; Ragosta et al. GCN 23748; Watson et al. GCNs 23749, 23751; Bikmaev et al. GCN 23766).
Preliminary PSF photometry of a stacked image is following.

Date UT start t-T0 Filter Exp. OT Err. UL(3sigma)
                      (mid, days) (s)
2019-01-24 01:11:25 9.93326 r' 14*180 21.56 0.09 23.2

We detected a source that is located northwest of the center of the host galaxy (de Ugarte Postigo et al., GCN 23692),  aperture photometry of the galaxy + OT is r'= 21.29 +/- 0.08.

The photometry is based on several nearby PanSTARRS stars used in (Mazaeva et al., GCN 23741).


GRB_name: GRB190123A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23788
SUBJECT: GRB 190123A: NEXT-0.6m optical limit
DATE:    19/01/24 17:11:59 GMT
FROM:    Dong Xu at NAOC/CAS  <dxu@nao.cas.cn>

D. Xu, Z.P. Zhu (NAOC) report on behalf of a larger collaboration

We observed the field of GRB 190123A (D'Ai et al., GCN Circ. 23769) with 
the robotic NEXT-0.6m telescope located at Nanshan, Xinjiang, China. We 
obtained 3x40s, 4x60s, 3x90s R-band frames, starting at 12:20:56 UT on 
2019-01-23, i.e., 103 sec after the BAT trigger.

No optical afterglow consistent with the XRT position (Beardmore et al. 
GCN Circ. 23771) is detected in the stacked image, download a limiting 
magnitude of R~19.5, calibrated with the USNO-B1 catalog.


GRB_name: GRB190123A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23789
SUBJECT: GRB 190123A: IKI-GRB-FuN optical upper limit
DATE:    19/01/24 17:24:58 GMT
FROM:    Alina Volnova at SAI MSU  <alinusss@gmail.com>

A. Volnova (IKI), A. Pozanenko (IKI),  E. Mazaeva (IKI),  E. Klunko
(ISTP), A. Kusakin (FAPHI), I. Reva  (FAPHI), R. Inasaridze (AAO),
A. Ivanov (KubSU), S. Belkin (IKI)  report on behalf of IKI-GRB-FuN:

We observed the field of GRB 190123A (D'Ai et al., GCN 23769)
on Jan., 23 with Zeiss-1000 1-m telescope of Tien Shan Astronomical
Observatory starting on 13:38:38, with MC 0.25-meter telescope of
Kuban State University Astrophysical observatory starting on 15:09:35
UT, with AS-32 (0.7m) telescope of Abastumani Observatory starting on
16:12:18 UT, and with AZT-33IK telescope of Sayan observatory (Mondy)
starting on 18:24:05 UT. We took several frames in R band with every
listed telescope.

We do not detect any source at the enhanced XRT position (Beardmore et
al., GCN 23771) in stacked images of each observatory.

Preliminary photometry of AZT-33IKI observations is based on several
nearby USNO-B1.0 stars:

Date            UT_start   t-T0            Filter    Exp.   OT   UL(3sigma)
                                    (mid, days)             (s)
2019-01-23 18:24:05   0.28248      R         4980  n/d   22.5

Our non-detection is consistent with non-detections reported by Lipunov
et al. (GCN 23770), Hu et al. (GCN 23772), Steeghs et al. (GCN 23774),
Shiraishi et al.(GCN 23778), Watson et al. (GCN 23781), Siegel et al.
(GCN 23784), and Nakamura & Sakamoto (GCN 23786).


GRB_name: GRB190122B
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23791
SUBJECT: GRB 190122B: AstroSat CZTI detection
DATE:    19/01/25 03:50:21 GMT
FROM:    Tanazza Khanam at IUCAA  <tanazza@iucaa.in>

T. Khanam, V. Sharma, D. Bhattacharya 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 190122B.

The source was clearly detected in the 20-200 keV energy range. The light curve shows strongest peak of emission at 16:57:02.5 UT. The measured peak count rate is 266 cts/s above the background in combined data of four quadrants, with a total of 801 cts. The local mean background count rate was 559 cts/s. Using cumulative rates, we measure a T90 of 4.18 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.


GRB_name: GRB190117A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23792
SUBJECT: GRB 190117A: AstroSat CZTI detection
DATE:    19/01/25 03:59:06 GMT
FROM:    Tanazza Khanam at IUCAA  <tanazza@iucaa.in>

T. Khanam, V. Sharma, D. Bhattacharya 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 190117A, which was also detected by AGILE (MCAL; Ursi, et al., GCN Circ. 23752), Insight (HXMT/HE; Xiao et al., GCN Circ. 23759), Konus-Wind, INTEGRAL (Frederiks D. et al., GCN Circ 23782),  IPN Triangulation (Hurley K. et al., GCN Circ. 23764) and Swift (BAT).

The source was clearly detected in the 40-200 keV energy range. The light curve shows multiple peaks of emission with strongest peak at 14:36:49.5 UT. The measured peak count rate is 2356 cts/s above the background in combined data of four quadrants, with a total of 11729 cts. The local mean background count rate was 524 cts/s. Using cumulative rates, we measure a T90 of 22.75 s. In preliminary analysis, we find that 862 Compton events are associated with this event.

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.


GRB_name: GRB190114C
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23798
SUBJECT: GRB 190114C: Optical follow-up from HCT
DATE:    19/01/27 11:12:34 GMT
FROM:    Brajesh Kumar at Indian Inst. of Astrophysics  <brajesh.kumar@iiap.res.in>

Avinash Singh (IIA), Brajesh Kumar (IIA), D. K. Sahu (IIA), G. C. 
Anupama (IIA), S. B. Pandey (ARIES) and Varun Bhalerao (IITB)

We followed-up the optical afterglow of GRB 190114C (Gropp et al., GCN 
23688) with the 2-m Himalayan Chandra Telescope (HCT)
located at the Indian Astronomical Observatory, Hanle, India. The 
observations were carried out in the Bessell R-band on
2019-01-24 15:02:44.59 UT (MJD 58507.627). The OT candidate (Lipunov et 
al., GCN 23693; Selsing et al., GCN 23695; Bolmer
et al., GCN 23702; D'Avanzo et al., GCN 23729; Kim et al., GCN 23732, 
23734; Kumar et al., GCN 23733, Kumar et al., GCN 23742,
Mazaeva et al., GCN 23746, Ragosta et al., GCN 23748, Watson et al., GCN 
23749, 23751) is detected in a stacked R-band image
comprising of 4 images, each with an exposure of 300s. The magnitude, 
calibrated using the magnitudes of field stars from the
USNO-B1.0 catalogue is estimated as 21.38+/-0.16 including host 
contamination.

We corrected the host contamination using the magnitudes reported for 
the source and source + galaxy by Mazaeva et al., GCN 23787.
The GRB OT magnitude after correction for the host galaxy is:

         UT-mid             Delta T(d)         JD          Exposure       
     Mag(AB)
  ----------------------   ------------    -----------    -------------   
  ---------------
  2019-01-24 15:02:44.59      9.754        2458508.127    1200s (4X300)   
  21.68 +/- 0.16

Using the reported magnitudes of GRB 190114C spanning almost 10 days in 
the SDSS-r and Bessell-R band filters, we estimated that
the source flux (F_lambda) is declining with a power law exponent of 
0.77+/-0.05, in agreement with the values inferred earlier
(Kumar et al. GCN 23733, Dado S. & Dar A. GCN 23735).

We thank the observing staff at IAO and CREST for their support during 
the observations.


GRB_name: GRB190129A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23806
SUBJECT: GRB 190129A: MAXI/GSC detection
DATE:    19/01/29 13:21:11 GMT
FROM:    Satoshi Sugita at Aoyama Gakuin U.  <sugita@phys.aoyama.ac.jp>

S. Nakahira (RIKEN), S. Sugita (AGU),
H. Negoro, M. Nakajima, A. Sakamaki, W. Maruyama, M. Aoki, K.
Kobayashi (Nihon U.),
T. Mihara, F. Yatabe, Y. Takao, M. Matsuoka (RIKEN),
T. Sakamoto, M. Serino, Y. Kawakubo, T. Hashimoto, A. Yoshida (AGU),
N. Kawai, M. Sugizaki, Y. Tachibana, K. Morita (Tokyo Tech),
S. Ueno, H. Tomida, M. Ishikawa, Y. Sugawara, N. Isobe, R. Shimomukai,
T. Midooka (JAXA),
Y. Ueda, A. Tanimoto, T. Morita, S. Yamada, S. Ogawa (Kyoto U.),
Y. Tsuboi, W. Iwakiri, R. Sasaki, H. Kawai, T. Sato (Chuo U.),
H. Tsunemi, T. Yoneyama, K. Asakura, S. Ide (Osaka U.),
M. Yamauchi, K. Hidaka, S. Iwahori (Miyazaki U.),
T. Kawamuro (NAOJ),
K. Yamaoka (Nagoya U.),
M. Shidatsu (Ehime U.),
Y. Kawakubo (LSU)
report on behalf of the MAXI team:
The MAXI/GSC nova alert system triggered a bright uncatalogued X-ray
transient source at 12:21:40 UT on January 29, 2019.
Assuming that the source flux was constant over the transit,
we obtain the source position at
(R.A., Dec) = (11.459 deg, -31.887 deg) = (00 45 50, -31 53 13) (J2000)
with a statistical 90% C.L. elliptical error region
with long and short radii of 0.16 deg and 0.15 deg, respectively.
The roll angle of long axis from the north direction is 40.0 deg
counterclockwise.
There is an additional systematic uncertainty of 0.1 deg (90%
containment radius).
The X-ray flux averaged over the scan was 306 +- 37 mCrab
(4.0-10.0keV, 1 sigma error).
Without assumptions on the source constancy,we obtain a rectangular error
box for the transient source with the following corners:
(R.A., Dec) = (10.934, -32.736) deg = (00 43 44, -32 44 09) (J2000)
(R.A., Dec) = (11.230, -32.814) deg = (00 44 55, -32 48 50) (J2000)
(R.A., Dec) = (11.935, -30.870) deg = (00 47 44, -30 52 12) (J2000)
(R.A., Dec) = (11.645, -30.793) deg = (00 46 34, -30 47 34) (J2000)
There was no significant excess flux in the previous transit at UT 10:49
with an upper limit of 20 mCrab.


GRB_name: GRB190129B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23808
SUBJECT: IPN Triangulation of GRB 190129B (long/extremely bright)
DATE:    19/01/29 18:28:09 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

K. Hurley, on behalf of the IPN,

I. G. Mitrofanov, D. Golovin, M. L. Litvak, and A. B. Sanin,
on behalf of the HEND-Odyssey GRB team,

D. Svinkin, S. Golenetskii, R. Aptekar, D. Frederiks, A. Kozlova
and T. Cline on behalf of the Konus-Wind team,

A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo,
and C. Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team,

and

W. Boynton, C. Fellows, K. Harshman, H. Enos, and R. Starr,
on behalf of the GRS-Odyssey GRB team, report:

The extremely bright, long-duration GRB 190129B
was detected by Konus-Wind, INTEGRAL (SPI-ACS), and
Mars-Odyssey (HEND) at about 44134 s UT (12:15:34).

We have triangulated it to a preliminary, 3 sigma error box
whose coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   117.285 (07h 49m 08s)  +1.257 ( +1d 15' 24")
  Corners:
   117.253 (07h 49m 01s)  +0.258 ( +0d 15' 28")
   117.088 (07h 48m 21s)  +0.627 ( +0d 37' 38")
   117.326 (07h 49m 18s)  +2.291 ( +2d 17' 26")
   117.485 (07h 49m 56s)  +1.896 ( +1d 53' 45")
  ---------------------------------------------
The error box area is about 1284 sq. arcmin, and its maximum
dimension is 2.034 deg (the minimum one is 12.84 arcmin).
The Sun distance was about 157 deg.

This box may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB190129_T44134/IPN

The time history and spectrum will be given in forthcoming
GCN Circulars.


GRB_name: GRB190129B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23809
SUBJECT: Konus-Wind observation of extremely bright GRB 190129B
DATE:    19/01/29 18:31:05 GMT
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 extremely bright, long GRB 190129B
(IPN triangulation: Hurley et al., GCN 23808)
triggered Konus-Wind (KW) at T0=44134.335 s UT (12:15:34.335).

The light curve of the burst shows a multi-peaked pulse,
which started at ~T0-10 s and had a duration of ~ 60s,
which was followed by a weaker and softer pulse around ~T0+130 s.
The emission is seen up to ~20 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB190129_T44134/

As observed by Konus-Wind, the burst had
a fluence of (5.59 Â± 0.40)x10^-4 erg/cm2 and
a 64-ms peak energy flux, measured from T0+17.344,
of (1.19 Â± 0.04)x10^-4 erg/cm2 (both in the 20 keV - 10 MeV
energy range).

The time-integrated spectrum (measured from T0 to T0+152.832 s)
is best fit in the 20 keV - 20 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.85 (-0.06,+0.06),
the high energy photon index beta = -2.18 (-0.16,+0.11),
the peak energy Ep = 561 (-53,+56) keV,
chi2 = 107/97 dof.

The spectrum near the peak count rate (measured from T0+17.152 s
to T0+18.432 s) is best fit in the 20 keV - 20 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.64 (-0.06,+0.06),
the high energy photon index beta = -2.13 (-0.08,+0.07),
the peak energy Ep = 717 (-62,+66) keV,
chi2 = 89/77 dof.

All the quoted errors are estimated at the 90% confidence level.
All the presented results are preliminary.


GRB_name: GRB190129A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23810
SUBJECT: GRB 190129A: Fermi GBM detection
DATE:    19/01/29 21:36:58 GMT
FROM:    Bagrat Mailyan at UAH  <bm0054@uah.edu>

E. Bissaldi (Politecnico & INFN Bari), B. Mailyan (UAH) and C. Meegan (UAH)
report on behalf of the Fermi GBM Team:

"At 12:21:41.87 UT on 29 January 2019, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 190129A (trigger 570457306 / 190129515),
which was also detected by MAXI/GSC (Nakahira et al. 2019, GCN 23806).
The GBM on-ground location is consistent with the MAXI/GSC position.

The angle from the Fermi LAT boresight at the GBM trigger time is 118
degrees.

The GBM light curve shows/consists of a single peak
with a duration (T90) of about 8.7 s (50-300 keV).
The time-averaged spectrum from T0-1 s to T0+4 s is
adequately fit by
a power law function with an exponential
high-energy cutoff.  The power law index is -1.37 +/- 0.23  and
the cutoff energy, parameterized as Epeak, is 78 +/- 19 keV.

The event fluence (10-1000 keV) in this time interval is
(9 +/- 1)E-07 erg/cm^2. The 1-sec peak photon flux measured
starting from T0-0.38 s in the 10-1000 keV band
is 3.7 +/- 0.3 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB190129B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23812
SUBJECT: GRB 190129B: Tiled Swift observations
DATE:    19/01/29 22:45:45 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P. A. Evans (U. Leicester) reports on behalf of the Swift team:

Swift has initiated a series of observations, tiled on the sky, of the
IPN GRB 190129B. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00076

Any uncatalogued X-ray sources detected in this analysis will be
reported on this website and via GCN COUNTERPART notices. The probability of finding
serendipitous sources, unrelated to the IPN event is high: any X-ray source
considered to be a probable afterglow candidate will be reported via a GCN Circular
after manual consideration.

Details of the XRT automated analysis methods are detailed in Evans et
al. (2007, A&A, 469, 379; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8).

This circular is an official product of the Swift-XRT team.


GRB_name: GRB190129B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23813
SUBJECT: GRB 190129B: Swift-XRT candidate afterglow detection
DATE:    19/01/30 09:11:11 GMT
FROM:    Andrea Melandri at INAF-OAB  <andrea.melandri@brera.inaf.it>

S. J. LaPorte (PSU), J.A. Kennea (PSU), J.P. Osborne (U. Leicester),
K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester), P. D'Avanzo
(INAF-OAB), V. D'Elia (ASDC), A. D'Ai (INAF-IASFPA), B. Sbarufatti
(INAF-OAB/PSU) and P.A. Evans (U. Leicester) report on behalf of the
Swift-XRT team:

Swift-XRT has performed follow-up observations of the IPN-detected
burst GRB 190129B in a series of observations tiled on the sky. The
total exposure time is 6.3 ks, distributed over 14 tiles; the maximum
exposure at a single sky location was 1.1 ks. The data were collected
between T0+45.0 ks and T0+60.4 ks, and are entirely in Photon Counting
(PC) mode. 

An uncatalogued X-ray source is detected and is above the RASS limit,
and is therefore likely the GRB afterglow. Using 42 s of PC mode data
and 1 UVOT image, we find an enhanced XRT position (using the XRT-UVOT
alignment and matching UVOT field sources to the USNO-B1 catalogue):
RA, Dec = 117.46104, +0.93484 which is equivalent to:

RA (J2000): 07h 49m 50.65s
Dec(J2000): +00d 56' 05.4"

with an uncertainty of 3.0 arcsec (radius, 90% confidence). This
position is about 7 arcmin from the edge of the IPN 3 sigma error box
(Hurley et al., GCN Circ 23808).  The light curve is consistent with a
constant source of mean count rate 4.4e-01 ct/sec. A power-law fit
gives an index of 1.2 (+1.6, -2.1).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.8 (+/-0.4). The
best-fitting absorption column is  4.7 (+2.8, -2.1) x 10^21 cm^-2, in
excess of the Galactic value of 7.3 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 4.4 x 10^-11 (6.3 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      4.7 (+2.8, -2.1) x 10^21 cm^-2
Galactic foreground: 7.3 x 10^20 cm^-2
Excess significance: 3.1 sigma
Photon index:      1.8 (+/-0.4)

The results of the XRT-team automatic analysis of the likely afterglow
are at http://www.swift.ac.uk/xrt_products/TILED_GRB00076/Source1.php.
The results of the full analysis of the tiled XRT observations are
available at http://www.swift.ac.uk/xrt_products/TILED_GRB00076.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB190129B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23814
SUBJECT: GRB 190129B: GROND possible host candidate
DATE:    19/01/30 09:30:29 GMT
FROM:    Jan Bolmer at MPE/Garching  <jan@bolmer.de>

J. Bolmer (MPE, Garching) and H. Steinle report:

We observed the field of the extremely bright GRB 190129B (detected by Konus-Wind, INTEGRAL,
and Mars-Odyssey; Hurley et al., GCN #23808) 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 the ESO
La Silla Observatory (Chile).

Observations started at 07:38 UT on 30th January, around 19.5 hours after the GRB trigger.
They were performed at an average seeing of 1.8" and at an average airmass of 2.1. 

We found a faint source at the edge of the XRT error circle reported by LaPorte et al.
(GCN #23813) at:

RA (J2000) = 07:49:50.81
DEC (J2000) = +00:56:03.8

with an uncertainty of 1.5" in each coordinate.

This source is already visible in the the PanSTARRS images and might
therefore be the host or an unrelated foreground galaxy.

Based on 7.7 min of exposure in g'r'i'z', and 8.0 min in JHK, we report the
following preliminary AB magnitudes:  

g < 23.0 mag
r = 22.7 +/- 0.3 mag
i = 21.8 +/- 0.3 mag
z = 21.7 +/- 0.4 mag
J = 20.4 +/- 0.4 mag
H = 19.1 +/- 0.2 mag
K = 19.0 +/- 0.4 mag

The above magnitudes are calibrated against SDSS and 2MASS and are not corrected
for the expected Galactic foreground extinction corresponding to a reddening
of E_(B-V)=0.08 in the direction of the burst (Schlafly & Finkbeiner 2011).


GRB_name: GRB190129A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23815
SUBJECT: GRB 190129A: CALET Gamma-Ray Burst Monitor detection
DATE:    19/01/30 12:12:35 GMT
FROM:    Valentin Pal'shin at AGU  <val@phys.aoyama.ac.jp>

H. Onozawa, A. Yoshida, T. Sakamoto, V. Pal'shin, S. Sugita (AGU),
Y. Kawakubo (LSU), A. Tezuka, S. Matsukawa, T. Ito, H. Morita, Y. Sone 
(AGU),
K. Yamaoka (Nagoya U), S. Nakahira (RIKEN), I. Takahashi (IPMU),
Y. Asaoka, S. Ozawa, S. Torii (Waseda U),
Y. Shimizu, T. Tamura (Kanagawa U),
W. Ishizaki (ICRR), M. L. Cherry (LSU),
S. Ricciarini (U of Florence),
A. V. Penacchioni, P. S. Marrocchesi (U of Siena),
and the CALET collaboration:

The long GRB 190129A (MAXI/GSC detection: Nakahira et al., GCN Circ. 23806;
Fermi GBM detection: Bissaldi, Mailyan & Meegan, GCN Circ. 23810)
triggered the CALET Gamma-ray Burst Monitor (CGBM) at 12:55:43.519 UTC
on 29 January 2019. The burst signal was seen by the HXM2 and SGM 
detectors.

The burst light curve shows a weak pulse which starts at T-2.2 sec and
ends at T+4.8 sec. The T90 and T50 durations measured by the SGM data
are 6.0 +- 2.2 sec and 3.0 +- 2.2 sec (40-1000 keV), respectively.

The ground processed light curve is available at

http://cgbm.calet.jp/cgbm_trigger/ground/1232801614/

The CALET data used in this analysis are provided by
the Waseda CALET Operation Center located at the Waseda University.


GRB_name: GRB190129B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23816
SUBJECT: GRB 190129B: MASTER Global Robotic Net optical observation
DATE:    19/01/30 12:25:05 GMT
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.Ishmuhametov (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-Kislovodsk robotic telescope (Global MASTER-Net: http://observ.pereplet.ru, Lipunov et al., 2010, Advances in Astronomy, vol. 2010, 30L)
was pointed to Konus-Wind GRB190129B  (Hurley et al. GCN23808, Frederiks et al. GCN 23809; Ttrig=2019-01-29 12:15:34.335 UT)
at 2019-01-29 17:21:59UT.
There is no OT at GROND (Bolmer et al. GCN23814) position inside Swift-XRT error-box (LaPorte et al. GCN 23813) RA,Dec=117.46104,+0.93484; +-3arcsec)
with 5-sigma upper limit mlim=20.0 (MASTER unfiltered W=0.2B+0.8R calibrated by USNO-B1 field stars)

Observations started when error-box altitude was 30.95deg.
The sun  altitude  was -33.77 deg.


MASTER-SAAO robotic telescope, located in South  African Astronomical Observatory,
was pointed to GRB190129B at 2019-01-29 19:09:22 UT.
There is no OT inside Swift-XRT error-box and at GROND position with unfiltered mlim=21m (5-sigma upper limit 1080s exp.)

Observations started when error-box altitude was 39.29.
The sun  altitude  was -17.36.


MASTER-Tavrida robotic telescope, located in Lomonosov MSU SAI Crimean astronomical station,
was pointed to GRB190129B at 2019-01-29 2019-01-29 19:11:21UT.
There is no OT inside Swift-XRT error-box and at GROND position with mlim=20.4 (5-sigma upper limit on 1080s exp.)

Observations started when error-box altitude was 40.18
The sun  altitude  was -46.51


MASTER-IAC robotic telescope, located in Teide observatory (Tenerife, Canarias islands, Spain, IAC),
was pointed to GRB190129B at 2019-01-29 20:57:26UT.
There is no OT inside Swift-XRT error-box and at GROND position with mlim=20.3 (5-sigma upper limit on 540s exp.)

Observations started when error-box altitude was 34.38
The sun  altitude  was -29.88.


The message may be cited.


GRB_name: GRB190129B
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23817
SUBJECT: GRB 190129B: AstroSat CZTI detection
DATE:    19/01/30 14:42:38 GMT
FROM:    Tanazza Khanam at IUCAA  <tanazza@iucaa.in>

T. Khanam, V. Sharma, D. Bhattacharya 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 190129B, which was also detected by IPN Triangulation (Hurley K. et al., GCN Circ. 23808), Konus-Wind (Frederiks D. et al., GCN Circ 23809), Swift (Evans P. A. et al., GCN Circ 23812 and LaPorte S. J. et al., GCN Circ 23813) and GROND (Bolmer J. et al,. GCN Circ 23814).

The source was clearly detected in the 40-200 keV energy range. The light curve shows multiple peaks of emission with strongest peak at 12:15;45.5 UT. The measured peak count rate is 3638 cts/s above the background in combined data of four quadrants, with a total of 29852 cts. The local mean background count rate was 601 cts/s. Using cumulative rates, we measure a T90 of 15.83 s. In preliminary analysis, we find that 2588 Compton events are associated with this event.

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.


GRB_name: GRB190129B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23818
SUBJECT: GRB 190129B: ePESSTO NTT optical observations
DATE:    19/01/30 16:53:05 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

S. Piranomonte (INAF-OAR), R. Carini (INAF-OAR), P. D'Avanzo (INAF-OAB), D. Malesani (DAWN/NBI and DARK/NBI), J. Bolmer (MPE, Garching), A. Melandri (INAF-OAB), T.-W. Chen (MPE), M. Nicholl (Univ. Edinburgh), S. C. Williams (Univ. Lancaster), S. Benetti (INAF-OAPd), L. Tomasella (INAF-OAPd), A. Fiore (Univ. Padova and INAF-OAPd), C. Inserra (Cardiff), E. Kankare (Turku), K. Maguire (QUB), S. J. Smartt (QUB), O. Yaron (Weizmann), D. R. Young (QUB), I. Manulis (Weizmann) report:

We observed the location of the candidate X-ray afterglow (LaPorte et al., GCN 23813) of the IPN-detected GRB 190129B (Hurley et al., GNC 23808; Frederiks et al., GCN 23809), under the extended Public ESO Spectroscopic Survey for Transient Objects (ePESSTO; see Smartt et al. 2015, A&A, 579, 40; http://www.pessto.org <http://www.pessto.org/>). The observations were performed on the ESO New Technology Telescope (NTT) at La Silla with the EFOSC2 instrument, starting on 2019 Jan 30 at 07:12:54 UT (i.e. 18.9 hr after the burst). Two images were acquired in the r band, by 120 and 240 s, respectively. The seeing conditions were unfortunately poor (~2â€).

We confirm a low-S/N detection of the object visible in the Pan-STARRS images, as reported by Bolmer & Steinle (GCN 23814).

Astrometry and photometry of this object are unfortunately affected by the presence of a nearby source ~2" to the SE, which is most likely a ghost from an 11-th magnitude star in the field of view. As this object is not seen in nearly-simultaneous GROND images of comparable depth (J. Bolmer, priv. comm.), we conclude that it is likely an artefact.


GRB_name: GRB190129B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23819
SUBJECT: GRB 190129B: Swift/UVOT Upper Limits
DATE:    19/01/30 19:55:48 GMT
FROM:    Paul Kuin at MSSL  <npkuin@gmail.com>

S.W.K. Emery (UCL-MSSL)
reports on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 190129B
44980 s after the IPN-detected burst (Hurley et al. GCN Circ. 23808).
No optical afterglow consistent with either the XRT position of the
uncatalogued X-ray source, source 1 (LaPorte et al. GCN Circ. 23813)
or the position of the GROND candidate (Bolmer et al. GCN Circ. 23814)
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
exposures at the position of source 1 are:

Filter      T_start(s)   T_stop(s)      Exp(s)         Mag

u             44980         60425         208         > 20.2


The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.10 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB190129B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23820
SUBJECT: GRB 190129B: DDOTI Detection of the Possible Afterglow and Suggestion of Fading 
DATE:    19/01/30 20:32:24 GMT
FROM:    Alan M. Watson at Instituto de Astronomia UNAM  <alan@astro.unam.mx>

Nat Butler (ASU), Alan M. Watson (UNAM), Rosa L. Becerra (UNAM), Diego
GonzÃ¡lez (UNAM), William H. Lee (UNAM), Margarita Pereyra (UNAM),
Alexander Kutyrev (GSFC), Eleonora Troja (GSFC), and Tanner Wolfram (ASU)
report:

We observed the entire IPN error box of GRB 190129B (Hurley et al., GCN
Circ. 23808) with the DDOTI/OAN wide-field imager at the Observatorio
AstronÃ³mico Nacional on Sierra San Pedro MÃ¡rtir
(http://ddoti.astroscu.unam.mx) from 2019-01-30 02:15 UTC to 12:48 UTC
(14.0 to 24.5 hours after burst) obtaining a total of 4.4 hours exposure
in the w filter.

If we split our exposures roughly in two, in the first half from 02:15
to 05:40 UTC we clearly detect a faint source close to the error region
for the candidate XRT afterglow (LaPorte et al., GCN Circ. 23813) at

  07:49:50.82 +00:56:06.1 J2000 (+/- 0.5 arcsec). 

In the second half from 05:41 to 12:48 UTC, this source is not visible.

The presence of a nearby bright star complicates photometry. However, in
the difference image we measure a magnitude and 1-sigma error of

  w = 22.7 +/- 1.0.

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 assume this source corresponds to the sources reported previously by
Bolmer & Steinle (GCN Circ. 23814) and Piranomonte et al. (GCN Circ.
23818) at a similar position and magnitude. However, our observations
are the first to suggest fading, albeit at low significance.

We thank the DDOTI technical team and the staff of the Observatorio
AstronÃ³mico Nacional.


GRB_name: GRB190129B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23821
SUBJECT: GRB 190129B: GOTO optical observations
DATE:    19/01/30 22:22:59 GMT
FROM:    Danny Steeghs at U.of Warwick/GOTO  <dsteeghs@gmail.com>

D.Steeghs, A.Levan, K.Ulaczyk (U. Warwick), G.Ramsay (Armagh O.),
M.Dyer (U. Sheffield), A.Obradovic, K. Ackley, D.K. Galloway, E.Rol
(Monash U.), K. Wiersema, B.Gompertz, J.Lyman, R.Cutter  (U. Warwick),
V.Dhillon (U. Sheffield), P.O'Brien, R.Starling (U. Leicester),
S.Poshyachinda (NARIT), D.Pollacco (U. Warwick), E.Thrane (Monash U.),
E.Palle (IAC)

report on behalf of the GOTO collaboration:

The Gravitational-wave Optical Transient Observer (GOTO) observed the
IPN region of GRB 190129B (Hurley et al., GCN Circ. 23808), between
 2019-01-29T21:07:31 and 2019-01-30T02:41:31 with several sets of 5x120s
exposures in our wide L filter (400-700nm).

No viable counterpart is detected within or near the 3-sigma error region
of Hurley et al. down to a 5-sigma detection limit of g=20.9. Our limits
are consistent with those reported in Lupinov et al. (GCN 23816) at around
the same delta since the burst.

We see no evidence for the source candidates reported by Bolmer et al.
(GCN 23814), Piranomonto et al. (GCN 23818) and Butler et al. (GCN 23820).


GOTO is operated at the La Palma observing facilities of the
University of Warwick on behalf of a consortium including the
University of Warwick, Monash University, Armagh Observatory, the
University of Leicester, the University of Sheffield, the National
Astronomical Research Institute of Thailand (NARIT) and the Instituto
de Astrofisica de Canarias (IAC) (https://goto-observatory.org/)


GRB_name: GRB190129B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23822
SUBJECT: Improved IPN error box for GRB 190129B
DATE:    19/01/30 22:42:18 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

K. Hurley, on behalf of the IPN,

I. G. Mitrofanov, D. Golovin, M. L. Litvak, and A. B. Sanin,
on behalf of the HEND-Odyssey GRB team,

D. Svinkin, S. Golenetskii, R. Aptekar, D. Frederiks, A. Kozlova
and T. Cline on behalf of the Konus-Wind team,

A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo,
and C. Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team,

and

W. Boynton, C. Fellows, K. Harshman, H. Enos, and R. Starr,
on behalf of the GRS-Odyssey GRB team, report:

Using the updated Mars-Odyssey (HEND) data we have
triangulated this GRB to an improved, but still preliminary,
3 sigma error box whose coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   117.441 (07h 49m 46s)  +0.895 ( +0d 53' 42")
  Corners:
   117.395 (07h 49m 35s)  -0.055 ( +0d 03' 17")
   117.262 (07h 49m 03s)  +0.238 ( +0d 14' 18")
   117.494 (07h 49m 58s)  +1.875 ( +1d 52' 31")
   117.623 (07h 50m 30s)  +1.563 ( +1d 33' 46")
  ---------------------------------------------
The error box area is about 1022 sq. arcmin, and its maximum
dimension is 1.932 deg (the minimum one is 10.3 arcmin).
The Sun distance was about 157 deg.

This error box doesn't overlap the initial error box (Hurley et al., GCN 
Circ. 23808), the distance between box centers is 23.65 arcmin.
The distance between the improved box center and the
Swift-XRT candidate afterglow (LaPorte et al., GCN Circ. 23813)
is 2.68 arcmin, supporting the association of the transient and the GRB.

This box may be further improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB190129_T44134/IPN

We apologize for any inconvenience caused.


GRB_name: GRB190114C
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23823
SUBJECT: GRB 190114C: JCMT SCUBA-2 sub-mm observations
DATE:    19/01/31 00:43:08 GMT
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 GRB 190114C (Gropp et al., GCN Circ. 23688)
using the SCUBA-2 sub-millimeter continuum camera on the James 
Clerk Maxwell Telescope in very good weather conditions on 
UT 2019-01-15, 2019-01-16, and 2019-01-18.  The source was not 
detected in the separate nights, or in the combination of all
the data.  The RMS background noise in the combined image was
0.95 mJy/beam at 850 microns and 5.4 mJy/beam at 450 microns.

We thank Mark Rawlings, Kevin Silva, Sheona Urquart, and the 
JCMT staff for the prompt support of these observations that 
were taken under project M18BP040.


GRB_name: GRB190129B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23824
SUBJECT: GRB 190129B: Insight-HXMT/HE detection
DATE:    19/01/31 11:28:42 GMT
FROM:    QiBin Yi at IHEP, HXMT  <yiqb@ihep.ac.cn>

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, J. L. Zhao,
A. M. Zhang, Y. F. Zhang, C. L. Zou (IHEP), Y. J. Jin, 
Z. Zhang (THU), T. P. Li (IHEP/THU), L. M. Song, 
M. Wu, Y. P. Xu, S. N. Zhang (IHEP), 
report on behalf of the Insight-HXMT team: 

At 2019-01-29T12:15:31.000 (T0), the Insight-HXMT/HE detected 
GRB 190129B (trigger ID: HEB190129510) in a routine search of the data, 
which was also triggered by IPN  (Hurley et al., GCN 23808) 
and Konus-Wind (Frederiks et al., GCN 23809)

The Insight-HXMT/HE light curve mainly consists of multiple 
pulses with a duration (T90) of 10.1 s measured from T0+8.10 s. 
The 1-s peak rate, measured from T0+14.07 s, is 18437.6 cnts/s. 
The total counts from this burst is 126004.0 counts. 
URL_LC: http://www.hxmt.org/images/GRB/HEB190129510_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 (record 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 
fundedjointly by the China National Space Administration (CNSA) and 
the Chinese Academy of Sciences (CAS). 
More information could be found at: http://www.hxmt.org.


GRB_name: GRB190126A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23826
SUBJECT: GRB 190126A: AstroSat CZTI detection
DATE:    19/02/01 11:31:18 GMT
FROM:    Tanazza Khanam at IUCAA  <tanazza@iucaa.in>

T. Khanam, V. Sharma, D. Bhattacharya 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 190126A.

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 05:14:42.3 UT. The measured peak count rate is 467 cts/s above the background in the combined data of four quadrants, with a total of 2407 cts. The local mean background count rate was 522 cts/s. Using cumulative rates, we measure a T90 of 9.2 s.

It was also 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.


GRB_name: GRB190131A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23827
SUBJECT: GRB 190131A: AstroSat CZTI detection
DATE:    19/02/01 13:39:46 GMT
FROM:    Tanazza Khanam at IUCAA  <tanazza@iucaa.in>

T. Khanam, V. Sharma, D. Bhattacharya 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 190131A.

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 23:08:38.5 UT. The measured peak count rate is 216 cts/s above the background in the combined data of four quadrants, with a total of 2804 cts. The local mean background count rate was 518 cts/s. Using cumulative rates, we measure a T90 of 17.6 s.

It was also 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.


GRB_name: GRB190131A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23828
SUBJECT: GRB 190131A: Insight-HXMT/HE detection
DATE:    19/02/01 14:48:23 GMT
FROM:    Ce Cai at IHEP  <caice@ihep.ac.cn>

C. Cai, 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, A. M. Zhang, 
Y. F. Zhang, X. F. Lu, 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 2019-01-31T23:08:35.000 (T0), the Insight-HXMT/HE detected 
GRB 190131A (trigger ID: HEB190131964) in a routine search of the data, 
which was also triggered by Fermi/GBM (trigger number 570668920);
AstroSAT (T. Khanam et al., GCN 23827); 

The Insight-HXMT/HE light curve mainly consists of multiple 
pulses with a duration (T90) of 23.40 s measured from T0+0.98 s. 
The 1-s peak rate, measured from T0+2.04 s, is 1371.5 cnts/s. 
The total counts from this burst is 15799.2 counts. 
URL_LC: http://www.hxmt.org/images/GRB/HEB190131964_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 (record 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 
fundedjointly by the China National Space Administration (CNSA) and 
the Chinese Academy of Sciences (CAS). 
More information could be found at: http://www.hxmt.org.


GRB_name: GRB190202A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23830
SUBJECT: GRB 190202A: Swift detection of a burst with an optical counterpart
DATE:    19/02/02 01:58:11 GMT
FROM:    Aaron Tohuvavohu at PSU/Swift  <aaronb@swift.psu.edu>

A. Y. Lien (GSFC/UMBC), P. D'Avanzo (INAF-OAB), J.D. Gropp (PSU),
N. J. Klingler (PSU), N. P. M. Kuin (UCL-MSSL),
F. E. Marshall (NASA/GSFC), D. M. Palmer (LANL), M. H. Siegel (PSU)
and A. Tohuvavohu (PSU) report on behalf of the Neil Gehrels Swift
Observatory Team:

At 01:39:30 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 190202A (trigger=887217).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 166.512, +9.388 which is 
   RA(J2000) = 11h 06m 03s
   Dec(J2000) = +09d 23' 17"
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 30 sec.  The peak count rate
was ~4500 counts/sec (15-350 keV), at ~5 sec after the trigger. 

The XRT began observing the field at 01:42:13.5 UT, 163.2 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 166.5026, 9.3779 which is equivalent to:
   RA(J2000)  = 11h 06m 0.62s
   Dec(J2000) = +09d 22' 40.4"
with an uncertainty of 5.9 arcseconds (radius, 90% containment). This
location is 49 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. 

UVOT took a finding chart exposure of 126 seconds with the White filter
starting 172 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 11:06:00.63 = 166.50262
  DEC(J2000) = +09:22:36.6  = 9.37683
with a 90%-confidence error radius of about 0.74 arc sec. This position is 3.9
arc sec. from the center of the XRT error circle. The estimated magnitude is
16.01 with a 1-sigma error of about  0.14. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.02. 

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.)


GRB_name: GRB190202A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23831
SUBJECT: GRB 190202A: Koshka Zeiss-1000 optical observations
DATE:    19/02/02 03:29:43 GMT
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 190202A (Lien , et al., GCN  23830)   with 
Zeiss-1000 1-m telescope of Koshka Observatory starting on Feb. 02  (UT) 
02:40:34 in  R-filter.   We detect the optical afterglow  (Lien , et al., 
GCN  23830) in coordinates (J2000) 11:06:00.60  +09:22:36.2 (uncertainiies 
in both coordinates of 0.5 arcsec) coinciding with reported  in GCN 23830. 
Preliminary photometry of the afterglow at 2019-02-02 02:49:35 is R=17.8 +/- 
0.15.

The photometry is based on several nearby USNO-B1.0 stars.
 


GRB_name: GRB190202A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23832
SUBJECT: GRB 190202A: Enhanced Swift-XRT position
DATE:    19/02/02 09:28:31 GMT
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 348 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 190202A, 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 = 166.50234, +9.37689 which is equivalent
to:

RA (J2000): 11h 06m 0.56s
Dec (J2000): +09d 22' 36.8"

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.


GRB_name: GRB190202A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23833
SUBJECT: GRB 190202A: GOTO optical observations
DATE:    19/02/02 12:48:07 GMT
FROM:    Danny Steeghs at U.of Warwick/GOTO  <dsteeghs@gmail.com>

D.Steeghs (U.Warwick), Y.-L.Mong (Monash U.), G.Ramsay (Armagh O.),
M.Dyer (U. Sheffield), J.Lyman, K.Ulaczyk (U. Warwick),
A.Obradovic, K. Ackley, D.K. Galloway, E.Rol (Monash U.),
K. Wiersema, B.Gompertz, A.Levan, R.Cutter  (U. Warwick),
V.Dhillon (U. Sheffield), P.O'Brien, R.Starling (U. Leicester),
S.Poshyachindav(NARIT), D.Pollacco (U. Warwick), E.Thrane (Monash U.),
E.Palle (IAC)

report on behalf of the GOTO collaboration:

In response to Swift BAT trigger 887217 (GRB190202A; Lien et al.
GCN 23830), the Gravitational-wave Optical Transient Observer (GOTO)
observed the survey field covering the Swift BAT/XRT positions.

Due to adverse weather, observations started at 2019-02-02T03:51:41
(2.2 hours post burst) consisting of a set of 5x120s exposures in our
wide L filter (400-700nm).

We detect the optical counterpart coincident with the revised XRT
position reported in Evans et al. (GCN 23832) at a S/N of 18.
Preliminary pipeline photometry based off a PS1 zeropoint provides
g=19.1 +/- 0.2, with the  uncertainty including a systematic error
component due to the calibration uncertainty. This has not been
corrected for galactic extinction.


GOTO is operated at the La Palma observing facilities of the
University of Warwick on behalf of a consortium including the
University of Warwick, Monash University, Armagh Observatory, the
University of Leicester, the University of Sheffield, the National
Astronomical Research Institute of Thailand (NARIT) and the Instituto
de Astrofisica de Canarias (IAC) (https://goto-observatory.org/)


GRB_name: GRB190202A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23834
SUBJECT: GRB 190202A: Swift/UVOT Detection
DATE:    19/02/02 13:00:54 GMT
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 190202A
173 s after the BAT trigger (Lien et al., GCN Circ. 23830). The source
was also observed in R (Novichonok et al., GCN Circ. 23831). A source
consistent with the XRT position  (Evans et al. GCN Circ. 23832)
is detected in the initial UVOT exposures.

The preliminary UVOT position is:
    RA  (J2000) =  11:06:00.63 = 166.50261 (deg.)
    Dec (J2000) = +09:22:36.7  =   9.37687 (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              173          299          124         16.02 +/- 0.03
v                 1613         2153           78         17.94 +/- 0.18
b                 1711         1903           39         18.38 +/- 0.16
u                 1686         2054           58         18.20 +/- 0.17
w1                1662         2376           97        >18.5

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.02 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB190202A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23835
SUBJECT: GRB 190202A: AGILE ratemeters detection
DATE:    19/02/02 13:29:32 GMT
FROM:    Francesco Verrecchia at ASDC  <francesco.verrecchia@ssdc.asi.it>

 F. Verrecchia (SSDC, and INAF/OAR), A. Ursi (INAF/IAPS), M. Tavani
(INAF/IAPS, and Univ. Roma Tor Vergata), M. Cardillo, Y. Evangelista, G.
Piano (INAF/IAPS), C. Pittori,  F. Lucarelli, (SSDC, and INAF/OAR), F.
Longo
(Univ. Trieste and INFN Trieste), A. Bulgarelli, V. Fioretti, F. Fuschino
(INAF/OAS-Bologna), A. Argan (INAF/IAPS), A. Giuliani (INAF/IASF-Mi), M.
Marisaldi (INAF/OAS, and Bergen University), M. Pilia, A. Trois
(INAF/OA-Cagliari), I. Donnarumma (ASI), report on behalf of the AGILE Team:

AGILE detected the long GRB 190202A first reported by Swift in Lien et al.,
GCN 23830, in the scientific ratemeters of the Anti-Coincidence (50-200
keV),
Super-AGILE (SA; 18-60 keV) and Mini-Caloremeter (MCAL; 0.4-100 MeV)
detectors.
The event position was not exposed by the AGILE Gamma-Ray Imaging Detector.

The low significance event lasted about 15s in the three light curves with
the
SA one starting about 8 s before the trigger time and the MCAL one about 10
s before.

Further analyses are still in progress.


GRB_name: GRB190202A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23836
SUBJECT: GRB 190202A, Swift-BAT refined analysis
DATE:    19/02/02 19:42:08 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

C. B. Markwardt (GSFC), S. D. Barthelmy (GSFC),
J. R. Cummings (CPI), H. A. Krimm (NSF/USRA),
A. Y. Lien (GSFC/UMBC), 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-240 to T+400 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 190202A (trigger #887217)
(Lien et al., GCN Circ. 23830).  The BAT ground-calculated position is
RA, Dec = 166.506, 9.393 deg which is
  RA(J2000)  =  11h 06m 01.4s
  Dec(J2000) = +09d 23' 33.9"
with an uncertainty of 1.9 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 4%.

The mask-weighted light curve shows two overlapping pulses that start
at ~T0 and end at ~T+25 s. The two peaks occur at ~T0 and ~T+5 s, respectively,
Note that the burst location came into the BAT field of view at ~T-69 s, and Swift
went into SAA at ~T+210 s. T90 (15-350 keV) is 19.4 +- 6.9 sec (estimated
error including systematics).

The time-averaged spectrum from T-0.90 to T+26.52 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.32 +- 0.13.  The fluence in the 15-150 keV band is 6.0 +- 0.5 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+4.68 sec in the 15-150 keV band
is 7.8 +- 1.5 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/887217/BA/


GRB_name: GRB190202A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23838
SUBJECT: GRB 190202A: Fermi GBM observation
DATE:    19/02/02 21:12:16 GMT
FROM:    Peter Veres at UAH  <veresp@gmail.com>

P. Veres  and C. Meegan (both UAH)
report on behalf of the Fermi GBM Team:

"At 01:39:26.21 UT on 02 February 2019, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 190202A (trigger 570764371 / 190202069) which was
also detected by the Swift/BAT (Lien et al., GCN 23830). The GBM on-ground
location is consistent with the Swift position.

The angle from the Fermi LAT boresight at the GBM trigger time is 76
degrees.

The GBM light curve shows a dominant pulse with some structure
with a duration (T90) of about 18.4 s (50-300 keV).
The time-averaged spectrum from T0-0.4 s to T0+12.8 s is
best fit by a  Band function with Epeak = 287 +/- 18 keV,
alpha = -0.74 +/- 0.04, and beta = -2.22 +/- 0.12.

The event fluence (10-1000 keV) in this time interval is
(1.81 +/- 0.03)E-5 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+5.4 s in the 10-1000 keV band
is 13.6 +/- 0.3 ph/s/cm^2.


The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB190202A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23839
SUBJECT: GRB 190202A: LCO-CTIO optical observations
DATE:    19/02/02 21:34:03 GMT
FROM:    Antonino Cucchiara at UVI  <antonino.cucchiara@uvi.edu>

A. Cucchiara (U. of the Virgin Islands) reports on
behalf of a larger collaboration:

We observed Swift GRB 190202A (Tohuvavohu et al. GCN 23803) with
the LCO 1-m units at CTIO on January 2, from 06:49 to 07:40 UT
(corresponding to 0.2 to 0.25 hours from the GRB trigger time)
with the SDSS r' and i' filters.

We performed a series of 10x120s in both filters and we clearly
detect the optical afterglow (Novichonok et al. GCN 23831) with
the following  magnitudes:

r' = 19.57 +-  0.04
i' = 19.19 +- 0.05

These magnitude are calibrated against several SDSS objects
near the GRB location and are not corrected for Galactic Extinction.

These observations were possible thanks to the USVI NASA-EPSCoR
Research Infrastructure Development (RID) grant NNX16AL44A.


GRB_name: GRB190202A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23840
SUBJECT: GRB 190202A: Swift-XRT refined Analysis
DATE:    19/02/02 23:24:29 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

A. Y. Lien (GSFC/UMBC) reports on behalf of the Swift-XRT team:

We have analysed 3.6 ks of XRT data for GRB 190202A (Lien et al. GCN
Circ. 23830), from 152 s to 65.6 ks after the  BAT trigger. The data
comprise 819 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. 23832).

The light curve can be modelled with an initial power-law decay with an
index of alpha=0.592 (+0.021, -0.077), followed by a break at T+1879 s
to an alpha of 1.47 (+0.05, -0.04).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.89 (+/-0.05). The
best-fitting absorption column is  consistent with the Galactic value
of 2.4 x 10^20 cm^-2 (Willingale et al. 2013). The PC mode spectrum has
a photon index of 1.82 (+0.13, -0.12) and a best-fitting absorption
column of 6.8 (+3.2, -2.9) x 10^20 cm^-2. The counts to observed
(unabsorbed) 0.3-10 keV flux conversion factor deduced from this
spectrum  is 3.6 x 10^-11 (4.1 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      6.8 (+3.2, -2.9) x 10^20 cm^-2
Galactic foreground: 2.4 x 10^20 cm^-2
Excess significance: 2.5 sigma
Photon index:      1.82 (+0.13, -0.12)

If the light curve continues to decay with a power-law decay index of
1.47, the count rate at T+24 hours will be 0.027 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 9.8 x
10^-13 (1.1 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/00887217.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB190202A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23841
SUBJECT: GRB 190202A: McDonald 0.8-m telescope optical observation
DATE:    19/02/03 05:22:41 GMT
FROM:    Gregory SungHak Paek at SNU  <shpaek@astro.snu.ac.kr>

Gregory S. H. Paek, Myungshin Im, Lim Gu, on behalf of a larger
collaboration

 We observed the afterglow of GRB 190202A (Lien et al., GCN 23830;
Novichonok et al., GCN 23831; Evans et al., GCN 23832; Steeghs et al., GCN
23833; Kuin et al., GCN 23834; Verrecchia et al., GCN 23835; Markwardt et
al., GCN 23836; Veres et al., GCN 23838; Cucchiara et al., GCN 23839; Lien
et al., GCN 23840) with the 0.8-m telescope at the McDonald observatory.
The observation started at 2019-02-02 08:02 UT or about 6.3 hours after the
initial alert.

 The afterglow is detected in R bands, and preliminary magnitudes are
derived, using nearby Pan-STARRS stars as photometry references.

Filter Date UT-start exptime[sec] AB_mag
R    2019-02-02 08:02:05        180*3    19.72 +/- 0.15


GRB_name: GRB190202A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23842
SUBJECT: GRB 190202A: NOT optical observations
DATE:    19/02/03 08:45:29 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@dark-cosmology.dk>

D. Malesani (DAWN/NBI and DARK/NBI), A. de Ugarte Postigo (HETH/IAA-CSIC, DARK/NBI), and H. J. Deeg (IAC) report on behalf of a larger collaboration:

We observed the optical afterglow of GRB 190202A (Lien et al., GCN 23830) using the Nordic Optical Telescope (NOT) equipped with the StanCam imager. Observations were carried out starting on 2019 Feb 3.06 UT (0.99 days after the GRB). A total of 3x600 s in the SDSS g band was acquired.

Calibrating against nearby reference stars from the SDSS catalog, we measure for the afterglow a preliminary magnitude of g = 21.72 +- 0.03 (AB).


GRB_name: GRB190202A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23843
SUBJECT: GRB 190202A: TSHAO optical observations
DATE:    19/02/03 11:14:49 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

S. Belkin (IKI), I. Reva (FAPHI), A. Pozanenko (IKI), E. Mazaeva (IKI), 
A. Volnova (IKI), A. Kusakin (FAPHI), M. Krugov (FAPHI) report on behalf 
of IKI-GRB-FuN collaboration:

We observed the afterglow of GRB 190202A (Lien et al., GCN 23830; 
Novichonok et al., GCN 23831; Evans et al., GCN 23832; Steeghs et al., 
GCN 23833; Kuin et al., GCN 23834; Verrecchia et al., GCN 23835; 
Markwardt et al., GCN 23836; Veres et al., GCN 23838; Cucchiara et al., 
GCN 23839; Lien et al., GCN 23840; Paek  et al., GCN 23841; Malesani et 
al., GCN 23842) with Zeiss-1000 1-m telescope of Tien Shan Astronomical 
Observatory starting on Feb. 02 (UT) 21:04:32.   Preliminary photometry 
of the field is following.

Date       UT start t-T0    Filter Exp.   OT    Err.  UL
                     (mid, days) (s)

2019-02-02 21:04:32 0.82502 R      21*120 20.43 0.11  21.6

The photometry is based on nearby USNO-B1.0 stars


GRB_name: GRB190202A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23844
SUBJECT: GRB 190202A: SAO RAS optical observations
DATE:    19/02/03 14:23:55 GMT
FROM:    Moskvitin Alexander at SAO RAS  <mosk@sao.ru>

A. S. Moskvitin and O. I. Spiridonova (SAO RAS)
report on behalf of larger collaboration.

We observed the field of the GRB 190202A (Lien et al., GCNC #23830)
with the Zeiss-1000 telescope of SAO RAS (+ CCD photometer)
on February, 3, 2:21:17--3:13:27 UT (mid.date 2:47:22).
The observations were carried out in Rc band.

We detected the OT (Novichonok et al., GCNC #23831; Steeghs et al.,
GCNC #23833; Paul Kuin & A. Y. Lien, GCNC #23834; Cucchiara,
GCNC #23839; Paek et al., GCNC #23841; Malesani et al., GCNC #23842;
Belkin et al., 23843) in the stacked 9 x 300 sec image.

Preliminary brightness of OT is R = 21.45 +/- 0.15 (T-T0 = 1.047 d).
The calibrations is based on nearby SDSS stars, magnitudes converted
with the Lupton 2005 equations.


GRB_name: GRB190203A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23845
SUBJECT: GRB 190203A: Swift detection of a burst with an optical counterpart
DATE:    19/02/03 15:57:07 GMT
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.)


GRB_name: GRB190203A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23846
SUBJECT: GRB 190203A: Koshka Zeiss-1000 optical upper limit
DATE:    19/02/03 16:51:04 GMT
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".]


GRB_name: GRB190203A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23847
SUBJECT: GRB 190203A: SAO RAS optical observations, afterglow fading
DATE:    19/02/03 18:43:44 GMT
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.


GRB_name: GRB190203A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23848
SUBJECT: GRB 190203A: Enhanced Swift-XRT position
DATE:    19/02/03 19:51:46 GMT
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.


GRB_name: GRB190203A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23850
SUBJECT: GRB 190203A: MASTER OT detection
DATE:    19/02/03 23:55:04 GMT
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.


GRB_name: GRB190204A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23852
SUBJECT: GRB 190204A: Swift detection of a burst with a possible optical counterpart
DATE:    19/02/04 06:12:47 GMT
FROM:    Aaron Tohuvavohu at PSU/Swift  <aaronb@swift.psu.edu>

A. Y. Lien (GSFC/UMBC), M. G. Bernardini (INAF-OAB),
P. D'Avanzo (INAF-OAB), N. J. Klingler (PSU), A. Melandri (INAF-OAB),
D. M. Palmer (LANL) and A. Tohuvavohu (PSU) report on behalf of the
Neil Gehrels Swift Observatory Team:

At 05:46:01 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 190204A (trigger=887579 and 887580). 
Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 351.514, +54.878 which is 
   RA(J2000) = 23h 26m 03s
   Dec(J2000) = +54d 52' 42"
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 20 sec.  The peak count rate
was ~28000 counts/sec (15-350 keV), at ~5 sec after the trigger. 

The XRT began observing the field at 05:47:15.7 UT, 75.0 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 351.47755, 54.87623 which
is equivalent to:
   RA(J2000)  = 23h 25m 54.61s
   Dec(J2000) = +54d 52' 34.4"
with an uncertainty of 3.6 arcseconds (radius, 90% containment). This
location is 119 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 consistent with the Galactic value of 4.36
x 10^21 cm^-2 (Willingale et al. 2013). 

The initial flux in the 2.5 s image was 5.72e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 250 seconds with the U filter starting
295 seconds after the BAT trigger. There is a candidate afterglow in the
rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 23:25:54.58 = 351.47742
  DEC(J2000) = +54:52:34.9  =  54.87637
with a 90%-confidence error radius of about 0.63 arc sec. This position is 4.2
arc sec. from the center of the XRT error circle. The estimated magnitude is
17.76 with a 1-sigma error of about  0.15. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.38. 

This GRB resulted in two BAT triggers in the on-board processing (#887579 at 05:46:01 and #887580 at 05:46:06).  
We adopt the first trigger number and time as T0. 

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.)


GRB_name: GRB190202A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23853
SUBJECT: GRB 190202A: R and I band observation from HCT
DATE:    19/02/04 07:09:08 GMT
FROM:    Brajesh Kumar at Indian Inst. of Astrophysics  <brajesh.kumar@iiap.res.in>

Brajesh Kumar (IIA), Avinash Singh (IIA), Ashish Raj (IIA), S. B. Pandey 
(ARIES), D. K. Sahu (IIA) and G. C. Anupama (IIA)

We observed the field of GRB 190202A (Lien et al., GCNC 23830) with the 
2-m Himalayan Chandra Telescope (HCT) located at the Indian Astronomical 
Observatory, Hanle, India on 2019-02-02 (21:32:29 UT). Two frames in 
Bessell R and I-bands with an exposure time of 300 sec each were 
obtained. The OT candidate (Novichonok et al., GCNC 23831; Steeghs et 
al., GCNC 23833; Cucchiara, GCNC 23839; Paek et al., GCNC 23841; 
Malesani et al., GCNC 23842; Belkin et al., 23843; Moskvitin & 
Spiridonova, GCNC 23844) is clearly detected in both frames at the Swift 
UVOT coordinates (Kuin & Lien, GCNC 23834). The preliminary magnitudes 
calibrated against the USNO-B1.0 catalogue are following:

       UT-mid          Band           Mag
-------------------  ------    --------------
2019-02-02 21:34:59    R       20.66 +/- 0.17
2019-02-02 21:40:56    I       20.08 +/- 0.20

We thank the observing staff at IAO and CREST for helping with the 
observations.


GRB_name: GRB190204A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23854
SUBJECT: GRB 190204A: MAXI/GSC detection
DATE:    19/02/04 07:23:51 GMT
FROM:    Satoshi Nakahira at RIKEN  <nakahira@crab.riken.jp>

T. Oeda (Tokyo Tech), M. Nakajima (Nihon U.), S. Nakahira (RIKEN),
H. Negoro, A. Sakamaki, W. Maruyama, M. Aoki, K. Kobayashi (Nihon U.), 
T. Mihara, F. Yatabe, Y. Takao, M. Matsuoka (RIKEN),
T. Sakamoto, M. Serino, S. Sugita, T. Hashimoto, A. Yoshida (AGU), 
N. Kawai, M. Sugizaki, Y. Tachibana, K. Morita (Tokyo Tech), 
S. Ueno, H. Tomida, M. Ishikawa, Y. Sugawara, N. Isobe, R. Shimomukai, T. Midooka (JAXA), 
Y. Ueda, A. Tanimoto, T. Morita, S. Yamada, S. Ogawa (Kyoto U.), 
Y. Tsuboi, W. Iwakiri, R. Sasaki, H. Kawai, T. Sato (Chuo U.), 
H. Tsunemi, T. Yoneyama, K. Asakura, S. Ide (Osaka U.), 
M. Yamauchi, K. Hidaka, S. Iwahori (Miyazaki U.), 
T. Kawamuro (NAOJ), 
K. Yamaoka (Nagoya U.),
M. Shidatsu (Ehime U.),
Y. Kawakubo (LSU) 
report on behalf of the MAXI team:
The MAXI/GSC nova alert system triggered a bright X-ray transient at 05:45:55 UT on February 4, 2019.
Assuming that the source flux was constant over the transit,
we obtain the source position at
(R.A., Dec) = (351.341 deg, 54.761 deg) = (23 25 21, +54 45 38) (J2000)
with a 90% C.L. statistical error of 0.10 deg and an additional systematic uncertainty of 0.1 deg (90% containment radius).
The X-ray flux averaged over the scan was 2286 +- 126 mCrab
(4.0-10.0keV, 1 sigma error).
Without assumptions on the source constancy,we obtain a rectangular error
box for the transient source with the following corners:
(R.A., Dec) = (350.693, 54.635) deg = (23 22 46, +54 38 05) (J2000)
(R.A., Dec) = (350.828, 54.512) deg = (23 23 18, +54 30 43) (J2000)
(R.A., Dec) = (352.146, 54.985) deg = (23 28 35, +54 59 05) (J2000)
(R.A., Dec) = (352.013, 55.110) deg = (23 28 03, +55 06 35) (J2000).

The trigger time and position was consistent with that of GRB 190204A detected 
by Swift (Lien et al. 2019, GCN 23852).


GRB_name: GRB190204A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23856
SUBJECT: GRB 190204A: AstroSat CZTI detection
DATE:    19/02/04 11:43:22 GMT
FROM:    Vidushi Sharma at IUCAA  <vidushi@iucaa.in>

T. Khanam, V. Sharma, D. Bhattacharya 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 190204A, which was also detected by Swift (Lien A. Y. et al., GCN Circ 23852) and MAXI/GSC (Oeda T. et al., GCN Circ 23854).

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 05:46:06.5 UT. The measured peak count rate is 1455 cts/s above the background in the combined data of four quadrants, with a total of 5579 cts. The local mean background count rate was 569 cts/s. Using cumulative rates, we measure a T90 of 11.9 s. In preliminary analysis, we find that 578 Compton events are associated with this event.

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.


GRB_name: GRB190204A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23857
SUBJECT: GRB 190204A: Swift-XRT refined Analysis
DATE:    19/02/04 11:45:54 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

J.A. Kennea (PSU), K.L. Page (U. Leicester), A.P. Beardmore (U.
Leicester), P.A. Evans (U. Leicester), V. D'Elia (ASDC), A. D'Ai
(INAF-IASFPA), A. Melandri (INAF-OAB), B. Sbarufatti (INAF-OAB/PSU),
D.N. Burrows (PSU) and A.Y. Lien report on behalf of the Swift-XRT
team:

We have analysed 6.4 ks of XRT data for GRB 190204A (Lien et al. GCN
Circ. 23852), from 81 s to 13.0 ks after the  BAT trigger. The data
comprise 926 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The refined XRT position is RA, Dec =
351.4775, +54.8766 which is equivalent to:

RA (J2000): 23 25 54.59
Dec(J2000): +54 52 35.7

with an uncertainty of 3.6 arcsec (radius, 90% confidence).

The late-time light curve (from T0+4.8 ks) can be modelled with a
power-law decay with a decay index of alpha=1.36 (+/-0.16).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.740 (+0.022, -0.018). The
best-fitting absorption column is  consistent with the Galactic value
of 4.4 x 10^21 cm^-2 (Willingale et al. 2013). The PC mode spectrum has
a photon index of 1.83 (+0.12, -0.11) and a best-fitting absorption
column of 5.4 (+0.8, -0.7) x 10^21 cm^-2. The counts to observed
(unabsorbed) 0.3-10 keV flux conversion factor deduced from this
spectrum  is 4.6 x 10^-11 (6.8 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      5.4 (+0.8, -0.7) x 10^21 cm^-2
Galactic foreground: 4.4 x 10^21 cm^-2
Excess significance: 2.4 sigma
Photon index:      1.83 (+0.12, -0.11)

If the light curve continues to decay with a power-law decay index of
1.36, the count rate at T+24 hours will be 9.9 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 4.5 x
10^-13 (6.8 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/00887579.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB190203A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23858
SUBJECT: GRB 190203A: Swift-XRT refined Analysis
DATE:    19/02/04 12:09:15 GMT
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.


GRB_name: GRB190203A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23859
SUBJECT: Konus-Wind observation of GRB 190203A
DATE:    19/02/04 12:23:45 GMT
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 Â± 0.5)x10^-5 erg/cm2 and a 64-ms peak energy flux,
measured from T0+20.352, of (3.5 Â± 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.


GRB_name: GRB190203A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23860
SUBJECT: GRB 190203A: Liverpool Telescope near-IR observations
DATE:    19/02/04 12:30:13 GMT
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.


GRB_name: GRB190204A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23861
SUBJECT: GRB 190204A: COATLI Optical Detection of the Fading Afterglow 
DATE:    19/02/04 12:54:35 GMT
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
GonzÃ¡lez (UNAM), William H. Lee (UNAM), Margarita Pereyra (UNAM), Carlos
RomÃ¡n-ZÃºÃ±iga (UNAM), Alexander Kutyrev (GSFC), and Eleonora Troja (GSFC)
report:

We observed the field of GRB 190204A (Lien et al., GCN Circ. 23852) with
the COATLI 50-cm telescope and interim imager at the Observatorio
AstronÃ³mico Nacional on the Sierra de San Pedro MÃ¡rtir
(http://coatli.astroscu.unam.mx) from 2019-02-04 05:46:35 to 2019-02-04
05:57:30 (from 34 to 689 seconds after the trigger), obtaining a total
of 345 seconds of exposure in the w filter.

At the position of the UVOT afterglow candidate (Lien et al., GCN Circ.
23852), we detect a source that fades from w = 13.5 to w = 17.5 over the
course of our observations. A power-law fit suggest a temporal index of
-1.44 +/- 0.03.

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
AstronÃ³mico Nacional.


GRB_name: GRB190204A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23862
SUBJECT: GRB 190204A: Enhanced Swift-XRT position
DATE:    19/02/04 13:35:49 GMT
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 2532 s of XRT Photon Counting mode data and 6 UVOT
images for GRB 190204A, 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 = 351.47820, +54.87637 which is equivalent
to:

RA (J2000): 23h 25m 54.77s
Dec (J2000): +54d 52' 34.9"

with an uncertainty of 1.5 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.


GRB_name: GRB190204A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23863
SUBJECT: GRB 190204A: Swift/UVOT Detection
DATE:    19/02/04 13:47:25 GMT
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 190204A
84 s after the BAT trigger (Lien et al., GCN Circ. 23852).
The updated UVOT position is:

The preliminary UVOT position is:
    RA  (J2000) =  23:25:54.58 = 351.47744 (deg.)
    Dec (J2000) = +54:52:35.1  =  54.87642 (deg.)
with an estimated uncertainty of 0.4 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               84          233          147         16.84 +/- 0.07
white              576          596           20         18.66 +/- 0.20
v                  626         1247           78         18.30 +/- 0.23
b                  551         1507           85         19.29 +/- 0.21
u                  296          546          246         17.85 +/- 0.10
w1                 676         1470           97        >18.3
m2                 651         1444           97        >19.5
w2                 602         1395           97        >18.7

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.38 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB190203A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23864
SUBJECT: GRB 190203A: COATLI Optical Observations 
DATE:    19/02/04 14:21:01 GMT
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
GonzÃ¡lez (UNAM), William H. Lee (UNAM), Margarita Pereyra (UNAM), Carlos
RomÃ¡n-ZÃºÃ±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
AstronÃ³mico Nacional on the Sierra de San Pedro MÃ¡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
AstronÃ³mico Nacional.


GRB_name: GRB190203A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23865
SUBJECT: GRB190203A: UVOT analysis
DATE:    19/02/04 17:01:34 GMT
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).


GRB_name: GRB190203A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23866
SUBJECT: GRB 190203A: AstroSat CZTI detection
DATE:    19/02/04 18:38:24 GMT
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.


GRB_name: GRB190204A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23867
SUBJECT: GRB 190204A: Mondy optical upper limit
DATE:    19/02/04 18:55:55 GMT
FROM:    Alina Volnova at SAI MSU  <alinusss@gmail.com>

A. Volnova (IKI),  A. Pozanenko (IKI),  E. Klunko (ISTP), R. Inasaridze
(AbAO), E. Mazaeva (IKI), S. Belkin (IKI)  report   on behalf of
IKI-GRB-FuN:

We observed the field of localization of  GRB 190204A   (Lien et al. GCN
23852)    with AZT-33IK telescope of Sayan observatory (Mondy).   We
started observations on Feb. 04 (UT) 13:10:12 in R-filter. We do not
detect  the optical afterglow (Lien et al.  GCN 23852; Watson et al.,
GCN  23861;  Kuin et al., GCN  23863). Preliminary photometry of the
field is following.

Date               UT start      t-T0          Filter Exp.   OT     Err.
  UL
                                         (mid, days)        (s)
                (3 sigma)

2019-02-04  13:10:12  0.32583     R      25*120      n/d     n/d   20.3

The photometry is based on nearby SDSS stars:
SDSS_id                         R_Lupton
J232549.70+545348.8 16.978 0.014
J232550.46+545253.5 17.052 0.014
J232544.33+545253.6 16.085 0.013


Our observation confirm rapid initial decay of the afterglow detected by
UVOT (Kuin et al., GCN  23863).


GRB_name: GRB190204A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23868
SUBJECT: GRB 190204A: SAO RAS optical observations
DATE:    19/02/04 19:02:35 GMT
FROM:    Moskvitin Alexander at SAO RAS  <mosk@sao.ru>

A. S. Moskvitin (SAO RAS)
report on behalf of larger GRB follow-up team.

We observed the field of the GRB 190204A (Lien et al., GCNC #23852)
with the Zeiss-1000 telescope of SAO RAS (+ CCD photometer)
on February, 4, 15:36:17--16:44:07 UT (mid. time 16:10:12).
The observations were carried out in Rc band.

We detected the OT (Lien et al., GCNC #23852; Watson et al.,
GCNC #23861; Kuin & Lien, GCNC #23863)
in the stacked 12 x 300 sec. image.

Preliminary brightness of OT is R = 21.9 +/- 0.1 (T-T0 = 0.4335 d).
The calibrations is based on nearby SDSS stars (Volnova et al.,
GCNC #23867), magnitudes converted with the Lupton 2005 equations.


GRB_name: GRB190204A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23869
SUBJECT: Konus-Wind observation of GRB 190204A
DATE:    19/02/04 19:23:03 GMT
FROM:    Anna Kozlova at Ioffe Institute  <ann_kozlova@mail.ioffe.ru>

A. Kozlova, S. Golenetskii, R. Aptekar, D. Frederiks,
M. Ulanov, D. Svinkin, A. Tsvetkova, A. Lysenko, and T. Cline
on behalf of the Konus-Wind team, report:

The long-duration GRB 190204A
(Swift detection: Lien et al., GCN Circ. 23852;
MAXI/GSC detection: Oeda et al., GCN Circ. 23854;
AstroSat CZTI detection: Khanam et al., GCN Circ. 23856)
triggered Konus-Wind at T0=20755.832 s UT (05:45:55.832).

The burst light curve shows a multipeaked structure
started at ~T0-1 s with a total duration of ~49 s.
The emission is seen up to ~10 MeV.

As observed by Konus-Wind, the burst
had a fluence of 5.31(-0.51,+0.53)x10^-5 erg/cm2,
and a 64-ms peak flux, measured from T0+8.288 s,
of 2.17(-0.28,+0.29)x10^-5 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum of the burst
(measured from T0 to T0+17.408 s)
is best fit in the 20 keV - 10 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.88(-0.07,+0.08),
the high energy photon index beta = -2.43(-0.30,+0.18),
the peak energy Ep = 308(-30,+33) keV
(chi2 = 76/98 dof).

The spectrum near the maximum count rate
(measured from T0+7.680 to T0+9.472 s)
is best fit in the 20 keV - 10 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.85(-0.07,+0.08),
the high energy photon index beta = -2.70(-0.58,+0.25),
the peak energy Ep = 387(-39,+46) keV
(chi2 = 69/66 dof).

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB190204_T20755/

All the quoted errors are at the 90% confidence level.
All the quoted values are preliminary.


GRB_name: GRB190202A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23870
SUBJECT: GRB 190202A: SAO RAS further optical observations
DATE:    19/02/04 19:53:15 GMT
FROM:    Moskvitin Alexander at SAO RAS  <mosk@sao.ru>

A. S. Moskvitin, O. I. Spiridonova, O. A. Maslennikova (SAO RAS),
and A. A. Volnova (IKI RAS) report on behalf of larger collaboration.

We observed the field of the GRB 190202A (Lien et al., GCNC #23830)
with the Zeiss-1000 telescope of SAO RAS (+ CCD photometer)
on February, 3, 21:15:42--22:45:25 UT (mid. time 22:00:33).
The observations were carried out in Rc band.

We detected the OT (Novichonok et al., GCNC #23831; Steeghs et al.,
GCNC #23833; Paul Kuin & A. Y. Lien, GCNC #23834; Cucchiara,
GCNC #23839; Paek et al., GCNC #23841; Malesani et al., GCNC #23842;
Belkin et al., 23843; Moskvitin & Spiridonova, GCNC #23844;
Brajesh Kumar et al., GCNC #23853) in the stacked 15 x 300 sec image.

Preliminary brightness of OT is R = 21.9 +/- 0.1 (T-T0 = 1.848 d).
The calibrations is based on nearby SDSS stars, magnitudes converted
with the Lupton 2005 equations.


GRB_name: GRB190202A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23871
SUBJECT: GRB 190202A: Xinglong-2.16m optical observations
DATE:    19/02/05 01:35:49 GMT
FROM:    Dong Xu at NAOC/CAS  <dxu@nao.cas.cn>

D. Xu, Z.P. Zhu, B.J. Xi, B.Y. Yu, F. Xiao, H.J. Wang (NAOC), J.H. Liu, 
X. Zhang (XAO) report on behalf of a larger collaboration:

We observed the field of GRB 190202A (Lien et al., GCN 23830) using the 
Xinglong-2.16m equipped with the BFOSC camera. Observations were carried 
out starting at 17:26:32 UT on 2019-02-03, and 6x600s R-band frames were 
obtained.

The previously reported afterglow (e.g., Lien et al., GCN 23830; 
Novichonok et al., GCN 23833, Cucchiara, GCN 23839; Paek et al., GCN 
23841; Malesani et al., GCN 23842; Belkin et al., 23843; Moskvitin & 
Spiridonova, GCN 23844; Kumar et al., GCN 23853; Moskvitin et al., GCN 
23870) is very weakly detected in our stacked image, with R=22.0 +/- 0.4 
mag (at Tmid-T0 = 1.679 days post-burst), calibrated with nearby SDSS stars.


GRB_name: GRB190204A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23872
SUBJECT: GRB 190204A: Swift-BAT refined analysis
DATE:    19/02/05 03:33:29 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

T. Sakamoto (AGU), S. D. Barthelmy (GSFC),
J. R. Cummings (CPI), H. A. Krimm (NSF/USRA),
A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), M. Stamatikos (OSU),
T. N. Ukwatta (LANL) (i.e. the Swift-BAT team):

Using the data set from T-234 to T+968 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 190204A (trigger #887579 and #887580)
(Lien et al., GCN Circ. 23852). In this circular, we adopted the trigger time
from the first trigger (#887579), 2019-02-04 05:46:01 UT, to be consistent
with the T0 quoted in other circulars.
The BAT ground-calculated position is
RA, Dec = 351.491, 54.884 deg which is
   RA(J2000)  =  23h 25m 57.8s
   Dec(J2000) = +54d 53' 02.4"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 48%.

The mask-weighted light curve shows several overlapping pulses that starts
at ~T-7 s and ends at ~T+55 s. The main peak occurs at ~T+5 s.
T90 (15-350 keV) is 26.4 +- 7.5 sec (estimated error including systematics).

The time-averaged spectrum from T-6.93 to T+53.82 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.30 +- 0.04.  The fluence in the 15-150 keV band is 1.3 +- 0.03 x 10^-5 erg/cm2.
The 1-sec peak photon flux measured from T+4.55 sec in the 15-150 keV band
is 30.5 +- 0.9 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/887580/BA/
(Please note that this page shows the automatic analysis from the 2nd trigger #887580,
because BAT associated most of the data with this trigger ID. Thus, the T0 displayed in
the webpage is 4.995 sec later than the trigger time referenced in this circular.)


GRB_name: GRB190203A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23873
SUBJECT: GRB 190203A: Swift-BAT refined analysis
DATE:    19/02/05 03:40:35 GMT
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/


GRB_name: GRB190202A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23874
SUBJECT: GRB190202A: GROWTH-India detection of optical afterglow
DATE:    19/02/05 04:35:21 GMT
FROM:    Varun Bhalerao at Indian Inst of Tech  <varunb@iitb.ac.in>

Harsh Kumar (IITB), Shubham Srivastav (IITB), Viraj karambelkar (IITB), Gaurav Waratkar(IITB), Tsewang Stanzin (IAO, IIA), Varun Bhalerao (IITB), G.C. Anupama (IIA) report on behalf of the GROWTH-India collaboration:

We observed the optical afterglow of GRB190202A (Lien , et al., GCN  23830, Novichonok et al. GCN 23831, Kuin P, et al. GCN 23834, Cucchiara A, et al. GCN 23839) with the 0.7m robotic GROWTH-India telescope at the Indian Astronomical Observatory.Observation were started at 2019-02-02 19:25:26.704. We observed the field using r filter with 600sec exposure.. We clearly detected a faint afterglow source at coordinates specified in (Kuin P, et al. GCN 23834). Magnitudes were calibrated using PanSTARRs reference stars in the same field from the PS1 catalog. The measured magnitude in r filter image is 20.58 +/- 0.1 (AB magnitude)

GROWTH India telescope is a 70-cm telescope with a 0.7 degree field of view, set up by the Indian Institute of Astrophysics and the Indian Institute of Technology Bombay with support from the Indo-US Science and Technology Forum (IUSSTF) and the Science and Engineering Research Board (SERB) of the Department of Science and Technology (DST), Government of India (https://sites.google.com/view/growthindia/). It is located at the Indian Astronomical Observatory (Hanle), operated by the Indian Institute of Astrophysics (IIA).

[GCN OPS NOTE(05feb19):  The Operator has added the "A" to the GRB name in the SUBJECT-line and in the body of the circular.]


GRB_name: GRB190202A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23875
SUBJECT: GRB 190202A: AstroSat CZTI detection
DATE:    19/02/05 06:45:51 GMT
FROM:    Vidushi Sharma at IUCAA  <vidushi@iucaa.in>

V. Sharma, T. Khanam 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 190202A, which was also detected by Swift (Lien A. Y. et al., GCN Circ 23830), AGILE ratemeters (Verrecchia F. et al., GCN Circ 23835) and Fermi GBM (Veres P. et al., GCN Circ 23838).

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 01:39:31.5 UT. The measured peak count rate is 453 cts/s above the background in the combined data of four quadrants, with a total of 3173 cts. The local mean background count rate was 471 cts/s. Using cumulative rates, we measure a T90 of 14.8 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.


GRB_name: GRB190204A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23877
SUBJECT: GRB 190204A: CALET Gamma-Ray Burst Monitor detection
DATE:    19/02/06 14:36:42 GMT
FROM:    Valentin Pal'shin at AGU  <val@phys.aoyama.ac.jp>

T. Ito, A. Yoshida, T. Sakamoto, V. Pal'shin, S. Sugita (AGU),
Y. Kawakubo (LSU), A. Tezuka, S. Matsukawa, H. Onozawa, H. Morita,
Y. Sone (AGU), K. Yamaoka (Nagoya U), S. Nakahira (RIKEN),
I. Takahashi (IPMU), Y. Asaoka, S. Ozawa, S. Torii (Waseda U),
Y. Shimizu, T. Tamura (Kanagawa U),
W. Ishizaki (ICRR), M. L. Cherry (LSU),
S. Ricciarini (U of Florence),
A. V. Penacchioni, P. S. Marrocchesi (U of Siena),
and the CALET collaboration:

The long GRB 190204A (Swift-BAT triggers #887579 and #887580:
Lien et al., GCN Circ. 23852, Sakamoto et al., GCN Circ.23872;
MAXI/GSC detection: Oeda et al., GCN Circ. 23854;
AstroSat CZTI detection: Khanam et al., GCN Circ. 23856;
Konus-Wind observation: Kozlova et al., GCN Circ. 23869)
triggered the CALET Gamma-ray Burst Monitor (CGBM)
at 05:46:05.075 UTC on 4 February 2019.
No real-time CGBM GCN notice was distributed about this trigger
because the real-time communication from the ISS was off (loss of signal).
The burst signal was seen by all CGBM detectors.

The burst light curve shows a single pulse which starts at T-7.7 sec,
peaks at 1.1 sec and ends at T+5.8 sec.
The T90 and T50 durations measured by the SGM data are
11.0 +- 2.0 sec and 2.2 +- 0.5 sec (40-1000 keV), respectively.
The ground processed light curve is available at

http://cgbm.calet.jp/cgbm_trigger/ground/1233294225/

The CALET data used in this analysis are provided by
the Waseda CALET Operation Center located at the Waseda University.


GRB_name: GRB190203A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23878
SUBJECT: GRB 190203A: Mondy optical observations
DATE:    19/02/06 18:09:10 GMT
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.


GRB_name: GRB190206A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23879
SUBJECT: IPN Triangulation of GRB 190206A (short/extremely bright)
DATE:    19/02/06 18:25:20 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

D. Svinkin, S. Golenetskii, R. Aptekar, D. Frederiks,
A. Kozlova, and T. Cline on behalf of the Konus-Wind team,

K. Hurley, on behalf of the IPN,

and

S. Barthelmy, J. Cummings, H. Krimm, and D. Palmer,
on behalf of the Swift-BAT team, report:

The extremely bright, short-duration GRB 190206A
has been detected by Konus-Wind and Swift (BAT),
so far, at about 13759 s UT (03:49:19).
The burst was outside the coded field of view of the BAT.

We have triangulated it to two preliminary, 3 sigma error boxes
whose coordinates are:

Box 1:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   313.330 (20h 53m 19s) -30.510 (-30d 30' 35")
  Corners:
   324.521 (21h 38m 05s) -35.854 (-35d 51' 16")
   323.780 (21h 35m 07s) -36.074 (-36d 04' 27")
   307.665 (20h 30m 40s) -23.586 (-23d 35' 08")
   308.080 (20h 32m 19s) -23.489 (-23d 29' 22")
  ---------------------------------------------

Box 2:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
   357.837 (23h 51m 21s) -14.585 (-14d 35' 07")
  Corners:
   354.375 (23h 37m 30s) -24.856 (-24d 51' 20")
   355.013 (23h 40m 03s) -24.585 (-24d 35' 08")
   357.410 (23h 49m 38s)  -6.031 ( -6d 01' 53")
   357.048 (23h 48m 12s)  -6.188 ( -6d 11' 16")
  ---------------------------------------------
The error box area is about 7.4 sq. deg, and their maximum
dimension is 19.05 deg (the minimum one is 23.2 arcmin).
The Sun distances were about 13 (Box 1) and 34 deg (Box 2).

This localization may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB190206_T13763/IPN/

The time history and spectrum will be given in forthcoming
GCN Circulars.


GRB_name: GRB190206A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23880
SUBJECT: Konus-Wind observation of GRB 190206A
DATE:    19/02/06 18:33:33 GMT
FROM:    Anna Kozlova at Ioffe Institute  <ann_kozlova@mail.ioffe.ru>

A. Kozlova, S. Golenetskii, R. Aptekar, D. Frederiks,
M. Ulanov,  D. Svinkin, A. Tsvetkova, A. Lysenko, and T. Cline
on behalf of the Konus-Wind team, report:

The extremely bright, short-duration, hard-spectrum
GRB 190206A (IPN triangulation: Svinkin et al., GCN Circ. 23879)
triggered Konus-Wind at T0=13763.926 s UT (03:49:23.926).

The burst light curve shows a single smooth pulse
which starts at ~T0 s and has a total duration of ~0.1 s.
There is no evidence of an extended emission following the burst.
The emission is seen up to ~10 MeV.

As observed by Konus-Wind, the burst
had a fluence of 1.64(-0.17,+0.17)x10^-5 erg/cm2,
and a 16-ms peak flux, measured from T0+0.004 s,
of 6.44(-0.75,+0.76)x10^-4 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum of the burst
(measured from T0 to T0+0.064 s)
is best fit in the 20 keV - 10 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = -0.58(-0.10,+0.12)
and Ep = 1600(-223,+248) keV (chi2 = 31/30 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.3
(chi2 = 30/29 dof).

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB190206_T13763/

The spectrum of the burst is typical of short-hard GRBs.
Assuming the measured fluxes, GRB 190206A is the third-brightest
short GRB detected by KW since November, 1994 in terms of peak flux,
and among the dozen brightest short GRBs, in terms of the fluence
(Svinkin et al. 2016, ApJS 224 10).

Although the redshift of GRB 190206A is not available (yet),
a comparison of the provisional track of the burst in the Ep,z-Eiso
and Ep,z-Liso planes with the KW sample of GRBs with known redshifts
(Tsvetkova et al., 2017, ApJ 850 161) suggests z < 0.5
(see http://www.ioffe.ru/LEA/GRBs/GRB190206_T13763/GRB190206A_z.pdf).

All the quoted errors are at the 90% confidence level.
All the quoted values are preliminary.


GRB_name: GRB190202A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23881
SUBJECT: GRB 190202A: Terskol 2-m optical observations
DATE:    19/02/07 21:13:59 GMT
FROM:    Moskvitin Alexander at SAO RAS  <mosk@sao.ru>

I. V. Sokolov (Terskol Peak Observatory), A. V. Sergeev (Terskol Peak
Observatory), A. S. Moskvitin (SAO RAS), V. B. Petkov (BNO INR RAS)
report on behalf of larger collaboration.

We observed the field of the GRB 190202A (Lien et al., GCNC #23830)
with the Zeiss-2000 telescope of Terskol Peak Observatory
on February, 3, 21:14:49--22:52:52 UT.

We detected the OT (Novichonok et al., GCNC #23831; Steeghs et al.,
GCNC #23833; Paul Kuin & A. Y. Lien, GCNC #23834; Cucchiara,
GCNC #23839; Paek et al., GCNC #23841; Malesani et al., GCNC #23842; Belkin
et al., 23843; Moskvitin & Spiridonova, GCNC #23844;
Brajesh Kumar et al., GCNC #23853; Moskvitin et al., GCNC #23870;
Xu et al., GCNC #23871) in the stacked 16 x 180 sec. R band image.

Preliminary brightness of OT is R = 21.92 +/- 0.17 (T-T0 = 1.850 d).
The calibrations is based on nearby SDSS stars, magnitudes converted
with the Lupton 2005 equations.


GRB_name: GRB190211A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23883
SUBJECT: GRB 190211A: Swift detection of a burst
DATE:    19/02/11 17:13:07 GMT
FROM:    Jamie A. Kennea at PSU/Swift-XRT  <kennea@swift.psu.edu>

F. E. Marshall (NASA/GSFC), P. A. Evans (U Leicester),
J.D. Gropp (PSU), J. A. Kennea (PSU), N. J. Klingler (PSU),
H. A. Krimm (NSF/USRA), K. L. Page (U Leicester), D. M. Palmer (LANL),
B. Sbarufatti (PSU), M. H. Siegel (PSU), A. Tohuvavohu (PSU) and
S. F. Tooke (U Leicester) report on behalf of the Neil Gehrels Swift
Observatory Team:

At 16:54:44 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 190211A (trigger=888648).  Swift slewed after a short delay 
to the burst. 
The BAT on-board calculated location is 
RA, Dec 196.675, +41.966 which is 
   RA(J2000) = 13h 06m 42s
   Dec(J2000) = +41d 57' 58"
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 3 sec.  The peak count rate
was ~1300 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 16:58:01.1 UT, 196.4 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source located at RA, Dec 196.65896, 41.96717 which is equivalent
to:
   RA(J2000)  = 13h 06m 38.15s
   Dec(J2000) = +41d 58' 01.8"
with an uncertainty of 3.6 arcseconds (radius, 90% containment). This
location is 43 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 (1.72 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 3.8
(+2.01/-1.78) x 10^21 cm^-2 (90% confidence). 

UVOT data are not available at this time. 

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: /too.html.)


GRB_name: GRB190211A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23884
SUBJECT: GRB 190211A: NEXT-0.6m optical afterglow detection
DATE:    19/02/11 18:00:56 GMT
FROM:    Dong Xu at NAOC/CAS  <dxu@nao.cas.cn>

D. Xu, B.Y. Yu (NAOC), J.H. Liu (XAO), Z.P. Zhu, B.J. Xi (NAOC), X. Gao 
(Urumqi No.1 Senior High School) report on behalf of a larger collaboration:

We observed the field of GRB 190211A (Marshall et al., GCN 23883) using 
the robotic NEXT-0.6m telescope located at Nanshan, Xinjiang, China. 
Observations started at 16:56:38 UT on 2019-02-11, i.e., 114 s after the 
BAT trigger. A series of 40 s, 60 s, 90 s, and 300 s R-band exposures 
were obtained and observations are ongoing.

An uncatalogued and fading optical source is detected at coordinates

R.A. (J2000) = 13:06:38.47
Dec. (J2000) = +41:58:04.93

with an error of the radius ~ 0.3 arcsec, being consistent with the XRT 
position (Marshall et al., GCN 23883). The source has m(R)~17.8 mag from 
our first 40s exposure. We thus conclude this source is the optical 
afterglow of the burst.


GRB_name: GRB190211A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23885
SUBJECT: GRB190211A: MASTER Global Robotic Net optical observation 
DATE:    19/02/11 18:21:54 GMT
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),

O. Gress, N.M. Budnev, O.Ershova, Yu.Ishmuhametova (Applied Physics Institute, Irkutsk State University),

V. Yurkov, A. Gabovich, Yu. Sergienko, D. Kobcev (Blagoveschensk Educational State University),

R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres (The Instituto de Astrofisica de Canarias),

D. Buckley (South African Astronomical Observatory),

A. Tlatov, V.Senik, A.V. Parhomenko, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory),

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)
  located in Russia (Blagoveshchensk State Pedagogical University)
was pointed to the  GRB190211A (Marshall et al. GCN 23883)
8 sec after notice time (46 sec after trigger time) at 2019-02-11 16:55:30 UT.

On our first (10s exposure)  set there is no  optical transient  within SWIFT 
error-box (ra=196.675 dec=41.9658 r=0.05) with 16.4m (5-sigma) upper limit 
(NEXT-0.6,  Xu et al. GCN 23884 with RA,Dec=13:06:38.47 +41:58:04.93).

The galactic latitude b = 75 deg., longitude l = 110 deg.
The observations started when error box altitude was 65 deg.
The moon (38 % bright part) altitude was -14 deg.
The sun  altitude was -50.9 deg.


MASTER-Tunka robotic telescope located in Russia (Applied Physics Institute, Irkutsk State University)
was pointed to the  GRB190211A 38 sec after notice time (76 sec after triggertime)
at 2019-02-11 16:56:00 UT.

On our first (10s exposure)  set we didn't find optical transient  within SWIFT 
error-box with  5-sigma upper limit 16.4m

The observations started when error-box altitde was  50 deg.
The sun  altitude  was -51.9 deg.


The message may be cited.


GRB_name: GRB190211A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23886
SUBJECT: GRB 190211A: BOOTES-4/MET optical afterglow confirmation
DATE:    19/02/11 19:23:23 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

Y.-D. Hu, X.-Y.Li, E. Fernandez-Garcia, A. Ayala, A. J. Castro-Tirado 
(IAA-CSIC), C. Perez del Pulgar, A. Castellon, I. Carrasco (Univ. de 
Malaga),Ã‚  S. Guziy (Univ. of Nikolaev) and D. Xiong, Y. Fan, X. Zhao, 
J. Bai, C. Wang, Y. Xin (Yunnan Nacional Astronomical Observatory), on 
behalf of a larger collaboration, report:

"Following the detection of GRB 190211A by Swift/BAT (Marshall et al. 
GCNC 23883), the 0.6m BOOTES-4/MET robotic telescope at Lijiang 
Astronomical Observatory (China) obtained follow-up  observations 
starting at 17:10 UT (~0.26 hr after trigger). The optical afterglow is 
detected within the Swift/XRT error box with a preliminary magnitude of 
19.1 mag (clear filter), thus confirming the fading in brightness of the 
optical source earlier reported by Xu et al. (GCNC 23884). Observations 
are ongoing."


GRB_name: GRB190211A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23887
SUBJECT: GRB 190211A: Swift-BAT refined analysis
DATE:    19/02/11 22:39:44 GMT
FROM:    Hans Krimm at NSF/NASA-GSFC  <hkrimm@nsf.gov>

M. Stamatikos (OSU), S. D. Barthelmy (GSFC),  J. R. Cummings (CPI),
H. A. Krimm (NSF/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 190211A (trigger #888648)
(Marshall, et al., GCN Circ. 23883).  The BAT ground-calculated position is
RA, Dec = 196.652, 41.976 deg which is 
   RA(J2000)  =  13h 06m 36.5s 
   Dec(J2000) = +41d 58' 32.1" 
with an uncertainty of 2.3 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 26%.

The mask-weighted light curve shows a a pair of peaks, the first from T-12 to T-5 sec,
and the second from T-4 to T+2 sec. T90 (15-350 keV) is 12.48 +- 1.46 sec (estimated 
error including systematics).

The time-averaged spectrum from T-11.49 to T+1.66 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.51 +- 0.33.  The fluence in the 15-150 keV band is 6.5 +- 1.2 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+0.56 sec in the 15-150 keV band
is 1.9 +- 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/888648/BA/


GRB_name: GRB190211A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23888
SUBJECT: GRB 190211A: Swift-XRT refined Analysis
DATE:    19/02/12 04:12:55 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P.A. Evans (U. Leicester), J.P. Osborne (U. Leicester), A. Melandri
(INAF-OAB), P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC), D.N. Burrows
(PSU), A. Tohuvavohu (PSU), S. J. LaPorte (PSU), K.L. Page (U.
Leicester) and F.E. Marshall report on behalf of the Swift-XRT team:

We have analysed 9.4 ks of XRT data for GRB 190211A (Marshall et al.
GCN Circ. 23883), from 205 s to 24.2 ks after the  BAT trigger. The
data are entirely in Photon Counting (PC) mode. The refined XRT
position is RA, Dec = 196.6588, +41.9671 which is equivalent to:

RA (J2000): 13 06 38.10
Dec(J2000): +41 58 01.5

with an uncertainty of 3.5 arcsec (radius, 90% confidence).

The light curve can be modelled with an initial power-law decay with an
index of alpha=0.15 (+0.16, -0.21), followed by a break at T+1088 s to
an alpha of 1.11 (+0.05, -0.06).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.94 (+0.11, -0.10). The
best-fitting absorption column is  7.1 (+2.6, -2.4) x 10^20 cm^-2, in
excess of the Galactic value of 1.7 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 (3.9 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      7.1 (+2.6, -2.4) x 10^20 cm^-2
Galactic foreground: 1.7 x 10^20 cm^-2
Excess significance: 3.7 sigma
Photon index:      1.94 (+0.11, -0.10)

If the light curve continues to decay with a power-law decay index of
1.11, the count rate at T+24 hours will be 9.4 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.2 x
10^-13 (3.7 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/00888648.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB180703A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23889
SUBJECT: GRB 180703A: VLT/MUSE host galaxy redshift measurement
DATE:    19/02/12 08:58:39 GMT
FROM:    Luca Izzo at IAA-CSIC  <luca.izzo@gmail.com>

L. Izzo (HETH/IAA-CSIC), A. de Ugarte Postigo (HETH/IAA-CSIC and DARK/NBI), P. Schady (U. Bath), D. B. Malesani (DAWN/NBI and DARK/NBI), D. A. Kann (HETH/IAA-CSIC), C. Kouveliotou (GWU), V. Dâ€™Elia (SSDC) and N. R. Tanvir (U. Leicester) report on behalf of the Stargate collaboration:

We have analysed the data obtained using the MUSE instrument, mounted on the ESO VLT UT4 (Yepun) telescope in Paranal, of the Fermi GRB 180703A (Racusin et al., GCN #22883; Poolakkil &  Meegan, GCN #22896). MUSE is an integral-field-unit spectrograph which covers a field of view of up to ~1 arcmin**2. Our observations started on 2018 July 04 at 07:53:56 UT, 10.92 hr after the GRB detection, and consisted of four exposures of 250 s each.

When we integrate the data cube along the full MUSE wavelength range, we detect a source within the uncertainty of the Swift/XRT afterglow position (Gibson et al., GCN #22891), and consistent with the position of the reported optical counterpart (Guidorzi et al., GCN #22892, #22944). We extracted a spectrum of this source within the wavelength range 4750-9350 AA. The spectrum is noisy, and we cannot confirm continuum afterglow emission. However, we identify three strong emission lines which can be consistently interpreted as [O III] 4960,5008 AA and [O II] 3727/29 AA at a common redshift of z = 0.6678. Given the spatial coincidence with the optical counterpart, we propose that these features come from the GRB host galaxy and we conclude that this is the redshift of GRB 180703A.

We acknowledge support from the ESO observing staff in Paranal, in particular Andrea Mehner.


GRB_name: GRB190211A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23890
SUBJECT: GRB 190211A: NOT optical observations
DATE:    19/02/12 09:23:10 GMT
FROM:    Dong Xu at NAOC/CAS  <dxu@nao.cas.cn>

K.E. Heintz (Univ. of Iceland), D. Xu (NAOC), D.B. Malesani (DAWN/NBI 
and DARK/NBI), S. Moran (NOT), report on behalf of a larger collaboration:

We observed the field of GRB 190211A (Marshall et al., GCN 23883) using 
the 2.56-m Nordic Optical Telescope (NOT) equipped with the ALFOSC 
camera. We obtained 3x200 s SDSS r-band and 3x300 s SDSS z-band frames, 
starting at 02:23:58 UT on 2019-02-12, i.e., 9.487 hr after the BAT trigger.

The previously reported optical afterglow (e.g., Xu et al., GCN 23884; 
Hu et al., GCN 23886) is clearly detected in our stacked images. The 
afterglow faded to m(r)=22.7  0.1 mag at 9.578 hr post-burst and m(z) = 
22.0  0.2 mag at 9.815 hr post-burst, calibrated with nearby SDSS stars.


GRB_name: GRB190211A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23891
SUBJECT: GRB190211A: MITSuME Akeno optical observation
DATE:    19/02/12 11:18:29 GMT
FROM:    Motoki Oeda at Tokyo Inst. of Tech.  <oeda@hp.phys.titech.ac.jp>

M. Oeda, R. Itoh, K. L. Murata, Y. Tachibana, S. Harita, K. Morita,
K. Shiraishi, K. Iida, M. Niwano, R. Adachi, Y. Yatsu,
and N. Kawai (Tokyo Tech) report on behalf of the MITSuME collaboration

We searched for the optical counterpart of GRB 190211A (F. E. Marshall et
al., GCN
Circular #23883) with the optical three color (g', Rc, and Ic) CCD cameras
attached to the MITSuME 50cm telescope of Akeno Observatory, Yamanashi,
Japan.

The observation started on 16:55:48.41 UT which corresponds to
64 sec after the trigger.
We detected the point source at the position consistent with the robotic
NEXT-0.6m telescope
observation (D. Xu et al., GCN Circular #23884).
The measured magnitudes are listed as follows.

T0+[sec]    MID-UT      T-EXP[sec]        g'       Rc        Ic
-------------------------------------------------------------------------------------------------------
~64      16:56:48.41          120              ~18.3      ~17.7     ~17.0
-------------------------------------------------------------------------------------------------------
T0+ : Elapsed time after the burst
T-EXP: Total Exposure time
We used GSC2.3 catalog for flux calibration.
The magnitudes are expressed in the Vega system.


GRB_name: GRB190206A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23892
SUBJECT: GRB 190206A: AstroSat CZTI detection
DATE:    19/02/12 13:47:25 GMT
FROM:    Vidushi Sharma at IUCAA  <vidushi@iucaa.in>

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 short bright GRB 190206A, which was also detected by Konus-Wind (Kozlova A. et al., GCN # 23880).

The source was clearly detected in the 40-200 keV energy range. The light curve shows single pulse of emission with peak at 03:49:28.5 UT, about 4.6 s after the Konus-Wind trigger time, consistent with possible propagation delay. We do not see any activity around 03:49:19 UT, the reference time quoted by IPN  (Svinkin D. et al., GCN # 23879). The measured peak count rate associated with the burst is 396 cts/s above the background in the combined data of four quadrants, with a total of 413 cts. The local mean background count rate was 515 cts/s. Using cumulative rates, we measure a T90 of 0.94 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.


GRB_name: GRB190211A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23893
SUBJECT: GRB 190211A: DOAO optical observation
DATE:    19/02/12 14:47:34 GMT
FROM:    Gregory SungHak Paek at SNU  <shpaek@astro.snu.ac.kr>

Gregory S.H. Paek, Myungshin Im (CEOU/SNU), Taewoo Kim, and Wonseok Kang
(DOAO) on behalf of a larger collaboration

We observed the afterglow of GRB 190211A(Marshall et al., GCN 23883; Xu et
al., GCN 23884; Lipunov et al., GCN 23885; Hu et al., GCN 23886; Stamatikos
et al., GCN 23887; Evans et al., GCN 23888) with the 1.0-m telescope at the
Deokheung Optical Astronomy Observatory.
The observation started at 2019-02-11 18:28 UT or about 1.5 hours after the
initial alert.
The afterglow is detected in R bands, and preliminary magnitudes are
derived, using nearby Pan-STARRS stars as photometry references.

Filter Date UT-start exptime[sec] AB_mag
R    2019-02-11 18:28:45        300*3    21.27 +/- 0.2


GRB_name: GRB190211A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23894
SUBJECT: GRB 190211A: Swift/UVOT Detection
DATE:    19/02/12 18:05:47 GMT
FROM:    Frank Marshall at Swift/UVOT  <marshall@milkyway.gsfc.nasa.gov>

F. E. Marshall (NASA/GSFC) reports on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 190211A
203 s after the BAT trigger (Marshall et al., GCN Circ. 23883).
A source consistent with the optical position
(Xu et al. GCN Circ. 23884) and just outside the
90% confidence XRT position (Evans et al. GCN Circ. 23888)
is detected in the only UVOT exposure.

The preliminary UVOT position is:
     RA  (J2000) =  13:06:38.45 =  196.66019 (deg.)
     Dec (J2000) = +41:58:04.9  =  41.96803 (deg.)
with an estimated uncertainty of 0.53 arc sec. (radius, 90% confidence).

The preliminary detection using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the early
exposures is:
Filter         T_start(s)   T_stop(s)      Exp(s)           Mag

white              203          351          146         19.73 +/- 0.11

The magnitude in the table is not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.02 in the direction of the burst
(Schlegel et al. 1998).


GRB_name: GRB190211A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23895
SUBJECT: GRB 190211A: Tautenburg observations
DATE:    19/02/14 09:49:17 GMT
FROM:    Sylvio Klose at TLS Tautenburg  <klose@tls-tautenburg.de>

B. Stecklum, S. Klose, and U. Laux report:

We observed the field of GRB 190211A (Marshall et al., GCN 23883) with the 
Tautenburg Schmidt telescope equipped with the Taukam 6k x 6k CCD camera. 
Observations were performed under modest seeing conditions 3.5 hr after 
the burst.

In a 5-min exposure we detect the GRB afterglow (Xu et al., GCN 23884; Hu 
et al., GCN 23886; Heintz et al., GCN 23890; Oeda et al., GCN 23891; Peak 
et al., GCN 23893; Marshall et al., GCN 23894) with V=20.75 +/- 0.10 (Vega 
mag), calibrated against the nearby star NOMAD1 1319-0272410 which has 
V=14.89.


GRB_name: GRB190211A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23896
SUBJECT: GRB190211A: GROWTH-India detection of optical afterglow
DATE:    19/02/15 01:45:15 GMT
FROM:    Varun Bhalerao at Indian Inst of Tech  <varunb@iitb.ac.in>

Harsh Kumar (IITB), Viraj karambelkar (IITB), Gaurav Waratkar(IITB), Shubham Srivastav (IITB), Tsewang Stanzin (IAO, IIAP), Varun Bhalerao (IITB), G.C. Anupama (IIAP) report on behalf of the GROWTH-India collaboration:

We observed the optical afterglow of GRB190211A (Marshall et al., GCN 23883; Xu et al. GCN 23884; Hu et al., GCN 23886; Stamatikos et al., GCN 23887; Evans et al., GCN 23888; K.E. Heintz et al., GCN 23890;  M. Oeda et al.,GCN 23891; Gregory S.H.P. et al., GCN 23893) with the 0.7m robotic GROWTH-India telescope at the Indian Astronomical Observatory. We obtained 600 s exposures in two bands, starting at UT 2019-02-11 18:16:55.961 for r filter and at UT 2019-02-11 18:28:07.536 in i filter. The afterglow is clearly detected in both images. Magnitudes were calibrated using PanSTARRs reference stars in the same field. The measured magnitude in r filter image is 21.37+/- 0.2 and in i filter is 20.28+/- 0.3.  

Based on our data combined with other r band measurements (Xu et al. GCN 23884; Hu et al., GCN 23886; M. Oeda et al.,GCN 23891; Heintz et al., GCN 23890), we see that the source flux is fading approximately as a power law t^-alpha, with alpha = 0.69 +/- 0.08.

GROWTH India telescope is a 70-cm telescope with a 0.7 degree field of view, set up by the Indian Institute of Astrophysics and the Indian Institute of Technology Bombay with support from the Indo-US Science and Technology Forum (IUSSTF) and the Science and Engineering Research Board (SERB) of the Department of Science and Technology (DST), Government of India (https://sites.google.com/view/growthindia/). It is located at the Indian Astronomical Observatory (Hanle), operated by the Indian Institute of Astrophysics (IIA).

[GCN OPS NOTE(14feb19):  The GRB ID has been corrected by adding an "A".]


GRB_name: GRB190212A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23897
SUBJECT: GRB 190212A: Insight-HXMT/HE detection
DATE:    19/02/15 03:23:44 GMT
FROM:    Qi Luo at IHEP  <luoqi@ihep.ac.cn>

Q. Luo, 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 2019-02-12T03:06:06.12 (T0), the Insight-HXMT/HE detected
GRB 190212A(trigger ID: HEB190212129) in a routine search of the data,
which was also triggered by CALET/CGBM(trigger_num:1233975813).

The Insight-HXMT/HE light curve mainly consists of two 
pulses with a duration (T90) of 0.063 s measured from T0-0.03 s.
The 1-ms peak rate, measured from T0+0.004 s, is 8211.5 cnts/sec.
The total counts from this burst is 218.8 counts.
URL_LC: http://www.hxmt.org/images/GRB/HEB190212129_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 (record 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
fundedjointly 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.


GRB_name: GRB190215A
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23898
SUBJECT: GRB 190215A: Fermi GBM detection
DATE:    19/02/16 01:00:56 GMT
FROM:    Bagrat Mailyan at UAH  <bm0054@uah.edu>

B. Mailyan (UAH) and C. Meegan (UAH)
 report on behalf of the Fermi GBM Team:

"At 18:31:22.48 UT on 15 February 2019, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 190215A (trigger 571948287 / 190215772).
The on-ground calculated location, using the GBM trigger data, is

RA, Dec = 340.4, +37.5 (J2000 degrees)

with an uncertainty of 1.0 degree (radius, 1-sigma containment,
statistical only; there is additionally a systematic
error which we have characterized as a core-plus-tail model, with 90% of
GRBs having a 3.7 deg error and a small tail suffering a larger than 10 deg
systematic error. [Connaughton et al. 2015, ApJS, 216, 32]).

The initial angle from the Fermi LAT boresight to
the best location is 25 degrees.

The GBM light curve consists of a bright FRED-like peak with multiple
pulses within it,
with a duration (T90) of about 23 s (50-300 keV).
The time-averaged spectrum from T0+0 s to T0+23 s is
best fit by a power law function with an exponential
high-energy cutoff.  The power law index is -0.18 +/- 0.03 and
the cutoff energy, parameterized as Epeak, is 204 +/- 4 keV.

The event fluence (10-1000 keV) in this time interval is
(2.0 +/- 0.3)E-05  erg/cm^2. The 1s peak photon flux measured
starting from T0+5.8 s in the 10-1000 keV band
is 8.7 +/- 0.3 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB190215A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23899
SUBJECT: GRB 190215A: Insight-HXMT/HE detection
DATE:    19/02/17 13:59:59 GMT
FROM:    QiBin Yi at IHEP, HXMT  <yiqb@ihep.ac.cn>

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 2019-02-15T18:31:22.000 (T0), the Insight-HXMT/HE detected
GRB 190215A(trigger ID: HEB190215771) in a routine search of the data,
which was also triggered by Fermi/GBM (B. Mailyan et al., GCN 23898).

The Insight-HXMT/HE light curve mainly consists of two 
pulses with a duration (T90) of 14.80 s measured from T0+1.22 s.
The 1-ms peak rate, measured from T0+6.155 s, is 3193.6 cnts/sec.
The total counts from this burst is 28093.7 counts.
URL_LC: http://www.hxmt.org/images/GRB/HEB190215771_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 (record 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
fundedjointly 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.



_______________________________________________
Hxmt-ba mailing list
Hxmt-ba@maillist.ihep.ac.cn
http://maillist.ihep.ac.cn/mailman/listinfo/hxmt-ba


GRB_name: GRB190215A
Detection_method: AstroSat CZTI
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23901
SUBJECT: GRB 190215A: AstroSat CZTI detection
DATE:    19/02/18 21:00:01 GMT
FROM:    Vidushi Sharma at IUCAA  <vidushi@iucaa.in>

V. Sharma, T. Khanam, D. Bhattacharya 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 190215A, which was also detected by Fermi/GBM (Mailyan B. et al., GCN # 23898) and Insight-HXMT/HE (Yi Q. B. et al., GCN # 23899).

The source was clearly detected in the 40-200 keV energy range. The light curve shows multiple pulses of emission with strongest peak at 18:31:29.5 UT, about 7 s after the Fermi/GBM trigger time. The measured peak count rate associated with the burst is 273 cts/s above the background in the combined data of four quadrants, with a total of 2683 cts. The local mean background count rate was 506 cts/s. Using cumulative rates, we measure a T90 of 23 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.


GRB_name: GRB190219A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23902
SUBJECT: GRB 190219A: Swift detection of a burst
DATE:    19/02/19 19:53:25 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

A. P. Beardmore (U Leicester), J. A. Kennea (PSU),
N. J. Klingler (PSU), A. Y. Lien (GSFC/UMBC),
F. E. Marshall (NASA/GSFC), M. J. Moss (George Washington University),
K. L. Page (U Leicester), D. M. Palmer (LANL) and A. Tohuvavohu (PSU)
report on behalf of the Neil Gehrels Swift Observatory Team:

At 19:38:58 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 190219A (trigger=889748).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 189.757, +76.614 which is 
   RA(J2000) = 12h 39m 02s
   Dec(J2000) = +76d 36' 50"
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 100 sec.  The peak count rate
was ~1300 counts/sec (15-350 keV), at ~70 sec after the trigger. 

The XRT began observing the field at 19:40:38.9 UT, 100.9 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source located at RA, Dec 189.62442,
76.61186 which is equivalent to:
   RA(J2000)  = 12h 38m 29.86s
   Dec(J2000) = +76d 36' 42.7"
with an uncertainty of 3.8 arcseconds (radius, 90% containment). This
location is 110 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. No spectrum from the promptly downlinked
event data is yet available to determine the column density. 

The initial flux in the 0.1 s image was 1.38e-08 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 109 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 A. P. Beardmore (apb AT star.le.ac.uk). 
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/)


GRB_name: GRB190219A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23903
SUBJECT: GRB 190219A: Prompt enhanced Swift-XRT position
DATE:    19/02/19 20:19:17 GMT
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 190219A, we find an
enhanced XRT position of the afterglow: RA, Dec: 189.6264, 76.6128
which is equivalent to:
   RA (J2000)  = 12 38 30.33
   Dec (J2000) = +76 36 46.2
with an uncertainty of 2.1 arcseconds (radius, 90% confidence).
Analysis of the promptly available data is online at
http://www.swift.ac.uk/sper/889748.

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.


GRB_name: GRB190219A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23904
SUBJECT: GRB 190219A: BOOTES-1 optical limits
DATE:    19/02/19 21:47:58 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

C. Perez del Pulgar (Univ. de Malaga), Y.-D. Hu, X.-Y.Li, E. 
Fernandez-Garcia, A. Ayala, A. J. Castro-Tirado (IAA-CSIC),  A. 
Castellon, I. Carrasco (Univ. de Malaga) on behalf of a
larger collaboration, report:

"Following the detection of GRB 190219A by Swift/BAT (Beardmore et al. 
GCNC 23902), the 0.3m BOOTES-1B robotic telescope in Mazagon (Huelva), 
southern Spain, responded automatically starting at 19:40:59 UT (121s 
after trigger; 82s after the alert). No optical afterglow is found down 
to 19 mag (unfiltered) on the co-added (50x10s) frames within the 
Swift/XRT error box (Evans et al. GCNC 23903), consistent with the 
non-detection by Swift/UVOT (Beardmore et al. GCNC 23902). Observations 
are ongoing".


GRB_name: GRB190219A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23905
SUBJECT: GRB190219A: MASTER Global Robotic Net optical observation 
DATE:    19/02/19 21:53:13 GMT
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),

O. Gress, N.M. Budnev, O.Ershova, Yu.Ishmuhametova (Applied Physics Institute, Irkutsk State University),

V. Yurkov, A. Gabovich, Yu. Sergienko, D. Kobcev (Blagoveschensk Educational State University),

R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres (The Instituto de Astrofisica de Canarias),

D. Buckley (South African Astronomical Observatory),

A. Tlatov, V.Senik, A.V. Parhomenko, D. Dormidontov (Kislovodsk Solar Station of the Pulkovo Observatory),

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, vol. 2010, 30L) located in Russia (Blagoveshchensk State Pedagogical University)
  was pointed to the  GRB190219A (Beardmore et al. GCN 23902  Ttrig=19:38:58 UT)
  16 sec after notice time (55 sec after trigger time) at 2019-02-19 19:39:53 UT.

On our first (10s exposure)  set we don't find optical transient  within 
SWIFT error-box (Evans et al. GCN 23903 12 38 30.33 +76 36 46.2   +-2.1arcsec).
The 5-sigma upper limit has been about 16.2mag at 10-s first exposition, 
16.7m on the 30-sec.exp., started at 2019-02-19 19:41:28UT.

The galactic latitude b = 41 deg., longitude l = 124 deg.
The observations started on zenit distance = 28 deg.
The moon (100 % bright part) altitude was 32 deg.The distance between  moon and  object is 66deg.
The sun  altitude  was -28.1 deg.


MASTER-Kislovodsk robotic telescope  located in Russia (Lomonosov MSU, Kislovodsk Solar Station of Pulkovo observatory)
was pointed to the  GRB190219.82 21 sec after notice time (60 sec after trigger time)
at 2019-02-19 19:39:58 UT.
On our first (10s exposure) there is no new OT inside Swift XRT error box 
brighter than 16.5.

The observations started on zenit distance = 41 deg.
The sun  altitude  was -50.7 deg.


MASTER-Tavrida robotic telescope  located in Russia (Lomonosov MSU, SAI Crimea astronomical station)
was pointed to the  GRB190219.82 18 sec after notice time (57 sec after trigger time)
  at 2019-02-19 19:39:55 UT.
On our first (10s exposure)  there is no  optical transient  within SWIFT error-box .
with the 5-sigma upper limit  about 17.44mag

The observations started on zenit distance = 42 deg.
The sun  altitude  was -45.5 deg.


MASTER-IAC robotic telescope located in Spain (IAC Teide Observatory) was 
pointed to the  GRB190219.82 20 sec after notice time  (59 sec after trigger time)
  at 2019-02-19 19:39:57 UT.
On our first (10s exposure)  set there is no optical transient  within SWIFT error-box 
with the 5-sigma upper limit  about 15.5

The observation started when error box altitude was 21deg.
Observations started at twilight.
The sun  altitude  was -9.9 deg.


MASTER-Tunka robotic telescope ocated in Russia (Applied Physics Institute, Irkutsk State University)
was pointed to the  GRB190219.82 29 sec after notice time (71 sec after trigger time)
at 2019-02-19 19:40:09 UT.

On our first (10s exposure) there is no optical transient  within SWIFT error-box
with the 5-sigma upper limit 15mag
The observations made on zenit distance = 25 deg.
The sun  altitude  is -40.6 deg.


GRB_name: GRB190219A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23906
SUBJECT: GRB 190219A: CAHA 2.2m observations
DATE:    19/02/19 21:55:37 GMT
FROM:    Alexander Kann at IAA-CSIC  <kann@iaa.es>

D. A. Kann (HETH/IAA-CSIC), A. de Ugarte Postigo (HETH/IAA-CSIC, 
DARK/NBI), M. Blazek, L. Izzo (both HETH/IAA-CSIC), A. Guijarro Roman, 
A. Fernandez Martin (both CAHA), C. C. Thoene, K. Bensch (both 
HETH/IAA-CSIC), report:

We observed the enhanced XRT position (Evans et al., GCN #23903) of 
Swift GRB 190219A (Beardmore et al., GCN #23902) with the 2.2m telescope 
of CAHA equipped with CAFOS. We obtained 3 x 180 s images in the Ic band 
under inclement weather conditions and the influence of the full Moon.

At the XRT position, we do not detect any source down to Ic > 21.5 mag 
(AB mag) at 0.038627 days after the GRB trigger, calibrated against 
nearby PanSTARRS objects. No source is visible at this position in 
PanSTARRS imaging either. This non-detection is in agreement with 
Beardmore et al. (GCN #23902) and Perez del Pulgar et al. (GCN #23904).


GRB_name: GRB190219A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23907
SUBJECT: GRB 190219A: Enhanced Swift-XRT position
DATE:    19/02/20 03:09:13 GMT
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 1531 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 190219A, 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 = 189.62654, +76.61261 which is equivalent
to:

RA (J2000): 12h 38m 30.37s
Dec (J2000): +76d 36' 45.4"

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.


GRB_name: GRB190220A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23908
SUBJECT: GRB 190220A: Swift detection of a burst with an optical counterpart
DATE:    19/02/20 03:14:43 GMT
FROM:    Kim Page at U.of Leicester  <klp5@leicester.ac.uk>

K. L. Page (U Leicester), N. J. Klingler (PSU),
F. E. Marshall (NASA/GSFC), D. M. Palmer (LANL), M. H. Siegel (PSU)
and A. Tohuvavohu (PSU) report on behalf of the Neil Gehrels Swift
Observatory Team:

At 02:59:34 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 190220A (trigger=889785).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 330.142, -76.691 which is 
   RA(J2000) = 22h 00m 34s
   Dec(J2000) = -76d 41' 27"
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 10 sec.  The peak count rate
was ~1700 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 03:00:55.5 UT, 80.8 seconds after
the BAT trigger. The position determined from promptly downlinked data
differs significantly from the on-board position, suggesting that the
XRT may have centroided on a cosmic ray; the initial XRT position
notice should be treated with caution. Using promptly downlinked data
we find an uncatalogued, fading X-ray source located at RA, Dec 330.16325,
-76.68047 which is equivalent to:
   RA(J2000)  = 22h 00m 39.18s
   Dec(J2000) = -76d 40' 49.7"
with an uncertainty of 3.7 arcseconds (radius, 90% containment). This
location is 41 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 (1.10 x
10^21 cm^-2, Willingale et al. 2013), with an excess column of 4.9
(+3.65/-3.07) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 86 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 22:00:39.14 = 330.16309
  DEC(J2000) = -76:40:50.4  = -76.68067
with a 90%-confidence error radius of about 0.66 arc sec. This position is 3.1
arc sec. from the center of the XRT error circle. The estimated magnitude is
19.29 with a 1-sigma error of about  0.16. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.13. 

Burst Advocate for this burst is K. L. Page (klp5 AT leicester.ac.uk). 
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/)


GRB_name: GRB190219A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23909
SUBJECT: GRB 190219A: Swift-XRT refined Analysis
DATE:    19/02/20 06:15:02 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

J.P. Osborne (U. Leicester), P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC),
A. D'Ai (INAF-IASFPA), A. Tohuvavohu (PSU), S. J. LaPorte (PSU), J.A.
Kennea (PSU), K.L. Page (U. Leicester) and A.P. Beardmore report on
behalf of the Swift-XRT team:

We have analysed 6.2 ks of XRT data for GRB 190219A (Beardmore et al.
GCN Circ. 23902), from 104 s to 13.3 ks after the  BAT trigger. The
data comprise 168 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. 23903).

The light curve can be modelled with a series of power-law decays. The
initial decay index is alpha=1.7 (+0.6, -0.9). At T+130 s  the decay
steepens to an alpha of 5.27 (+0.11, -0.12) before breaking again at
T+554 s to a final decay with index alpha=0.13 (+0.08, -0.09).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.63 (+0.07, -0.06). The
best-fitting absorption column is  1.92 (+0.17, -0.16) x 10^21 cm^-2,
in excess of the Galactic value of 3.5 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 2.14 (+0.21, -0.19)
and a best-fitting absorption column of 1.6 (+0.6, -0.5) x 10^21 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.2 x 10^-11 (4.4 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      1.6 (+0.6, -0.5) x 10^21 cm^-2
Galactic foreground: 3.5 x 10^20 cm^-2
Excess significance: 3.8 sigma
Photon index:      2.14 (+0.21, -0.19)

If the light curve continues to decay with a power-law decay index of
0.13, the count rate at T+24 hours will be 0.064 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 2.0 x
10^-12 (2.8 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/00889748.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB190219A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23910
SUBJECT: GRB 190219A: NEXT-0.6m optical upper limit
DATE:    19/02/20 07:41:53 GMT
FROM:    Dong Xu at NAOC/CAS  <dxu@nao.cas.cn>

Z.P. Zhu, D. Xu, B.Y. Yu (NAOC), J.H. Liu (XAO) report:

We observed the field of GRB 190219A (Beardmore et al., GCN 23902) using 
the NEXT-0.6m telescope located at Nanshan, Xinjiang, China. We obtained 
10x90s frames in the R filter, started at 19:57:52 UT on 2019-02-19, 
i.e., 18.43 min after the burst.

No optical source is detected at the XRT position (Beardmore et al., GCN 
23902 & 23907) in our stacked image, down to a 3 sigma limiting 
magnitude of R~17.5.


GRB_name: GRB190219A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23911
SUBJECT: GRB 190219A: NOT optical afterglow candidate
DATE:    19/02/20 11:16:15 GMT
FROM:    Dong Xu at NAOC/CAS  <dxu@nao.cas.cn>

D. Xu (NAOC), K.E. Heintz (Univ. of Iceland), D.B. Malesani 
(DAWN/NBI/DTU and DARK/NBI), Z.P. Zhu (NAOC), P. Galindo (NOT), J. Viuho 
(NOT), report on behalf of a larger collaboration:

We observed the field of GRB 190219A (Beardmore et al., GCN 23902) using 
the 2.56-m Nordic Optical Telescope (NOT) equipped with the ALFOSC 
camera. Observations started at 01:13:50 UT on 2019-02-20, i.e., 5.58 hr 
after the burst, and we obtained 6x300 s Sloan r-band and 10x200 s 
z-band frames. The weather conditions of the night were bad, with thick 
clouds (which accounts for the large delay of our observations).

Among our data, the z-band images are deeper, and a source is detected 
in the stacked observations, at coordinates (J2000):

R.A. (J2000) = 12:38:30.32
Dec. (J2000) = +76:36:46.62

with a radius uncertainty of ~ 0.2 arcsec, within the enhanced Swift-XRT 
error circle (Beardmore et al., GCN 23907). We measure m(z) = 22.8  0.4 
AB at 6.32 hr post-burst, calibrated against nearby Pan-STARRS stars. 
The source is not detected in the stacked r-band image, down to a 
limiting magnitude of m(r) > 22.5 AB. We note that the detected 
magnitude is fainter than the Pan-STARRS survey limit, and as we lack 
temporal information we cannot comment on variability. We propose this 
object as a candidate counterpart for GRB 191202A, but further 
observations are required to establish variability.


GRB_name: GRB190220A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23912
SUBJECT: GRB 190220A: Enhanced Swift-XRT position
DATE:    19/02/20 15:13:27 GMT
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 749 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 190220A, 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 = 330.16376, -76.68124 which is equivalent
to:

RA (J2000): 22h 00m 39.30s
Dec (J2000): -76d 40' 52.5"

with an uncertainty of 1.5 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.


GRB_name: GRB190219A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23913
SUBJECT: GRB 190219A: Swift-BAT refined analysis
DATE:    19/02/20 17:57:57 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

T. N. Ukwatta (LANL), S. D. Barthelmy (GSFC),
A. P. Beardmore (U Leicester), J. R. Cummings (CPI),
H. A. Krimm (NSF/USRA), 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 190219A (trigger #889748)
(Beardmore et al., GCN Circ. 23902).  The BAT ground-calculated position is
RA, Dec = 189.686, 76.606 deg which is
  RA(J2000)  =  12h 38m 44.7s
  Dec(J2000) = +76d 36' 21.6"
with an uncertainty of 1.6 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 76%.

The mask-weighted light curve shows a multi-peaked structure that starts
at ~ T-110 s and ends at ~T+100 s. The first major pulse starts at ~T-5 s,
peaks at ~T+5 s, and end at ~T+40 s. It is followed by the second major pulse
that peaks at ~T+65 s and ends at ~T+90 s. T90 (15-350 keV) is 167.8 +- 12.8 sec
(estimated error including systematics).

The time-averaged spectrum from T-106.20 to T+88.68 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.24 +- 0.10.  The fluence in the 15-150 keV band is 3.9 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+65.52 sec in the 15-150 keV band
is 1.9 +- 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/889748/BA/


GRB_name: GRB190220A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23914
SUBJECT: GRB 190220A: Swift-BAT refined analysis
DATE:    19/02/20 17:59:59 GMT
FROM:    Amy Lien at GSFC  <amy.y.lien@nasa.gov>

S. D. Barthelmy (GSFC), J. R. Cummings (CPI),
H. A. Krimm (NSF/USRA), A. Y. Lien (GSFC/UMBC),
C. B. Markwardt (GSFC), D. M. Palmer (LANL),
K. L. Page (U Leicester), 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 190220A (trigger #889785)
(Page et al., GCN Circ. 23908).  The BAT ground-calculated position is
RA, Dec = 330.128, -76.669 deg which is
  RA(J2000)  =  22h 00m 30.7s
  Dec(J2000) = -76d 40' 10.1"
with an uncertainty of 1.3 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 46%.

The mask-weighted light curve shows a single-pulse structure that starts
at ~T0, peaks at ~T+2 s, and ends at ~T+12 s. T90 (15-350 keV)
is 10.0 +- 2.0 sec (estimated error including systematics).

The time-averaged spectrum from T-0.12 to T+11.88 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 0.79 +- 0.77,
and Epeak of 40.3 +- 6.7 keV (chi squared 60.03 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 8.9 +- 1.0 x 10^-7 erg/cm2
and the 1-sec peak flux measured from T+1.88 sec in the 15-150 keV band is
2.6 +- 0.4 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 2.03 +- 0.13 (chi squared 70.39 for 57 d.o.f.).  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/889785/BA/


GRB_name: GRB190220B
Detection_method: IBAS
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23915
SUBJECT: GRB 190220B: a long GRB detected by IBAS
DATE:    19/02/20 22:01:11 GMT
FROM:    Diego Gotz at CEA  <diego.gotz@cea.fr>

D.Gotz (CEA, Saclay), S.Mereghetti (INAF, IASF-Milano), C.Ferrigno,
E.Bozzo, V.Savchenko (ISDC, Versoix), L.Ducci (IAAT, Germany and ISDC,
Versoix) and J.Borkowski (CAMK, Torun) report:

a gamma ray burst lasting about 200 s with a multi-peaked structure has been detected by IBAS in the
IBIS/ISGRI data at 20:12:43  UT of February 20, 2019.

The refined coordinates (J2000) are:

R.A.= 242.4512 deg
DEC.= -21.1314 deg

with an uncertainty of  2.0   arcmin (90% c.l.).

The burst had a peak flux of 0.2  counts/cm2/s (20-200 keV, 1-s integration  time) and a fluence in the same energy range of about 3.6e-6
erg/cmsq.

A plot of the light curve will  be posted at
http://ibas.iasf-milano.inaf.it/IBAS_Results.html


GRB_name: GRB190220B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23916
SUBJECT: GRB 190220B: BOOTES-4 optical observation
DATE:    19/02/20 23:05:52 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

Y.-D. Hu, X.-Y.Li, E. Fernandez-Garcia, A. Ayala, A. J. Castro-Tirado 
(IAA-CSIC), C. Perez del Pulgar, A. Castellon, I. Carrasco (Univ. de 
Malaga),  S. Guziy (Univ. of Nikolaev) and D. Xiong, Y. Fan, X. Zhao, J. 
Bai, C. Wang, Y. Xin (Yunnan Nacional Astronomical Observatory) on 
behalf of a larger collaboration, report:

"Following the detection of GRB 190220B by INTEGRAL (Gotz et al. GCNC 
23915), the 0.6m BOOTES-4/MET robotic telescope at Lijiang Astronomical 
Observatory (China) responded to the the burst gathering images starting 
at 20:17:12 UT (89 s after trigger, 84 s after notice). No optical 
afterglow candidate is found down to 18 mag (g'-band) in the co-added 
(5x10s) image within the reported INTEGRAL 2 arcmin radius error box. 
Observations are ongoing."


GRB_name: GRB190220A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23917
SUBJECT: GRB 190220A: Swift-XRT refined Analysis
DATE:    19/02/21 02:51:09 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

V. D'Elia (ASDC), A. D'Ai (INAF-IASFPA), A. Melandri (INAF-OAB), S. J.
LaPorte (PSU), J.A. Kennea (PSU), B. Sbarufatti (INAF-OAB/PSU), A.P.
Beardmore (U. Leicester), P.A. Evans (U. Leicester) and K.L. Page
report on behalf of the Swift-XRT team:

We have analysed 6.9 ks of XRT data for GRB 190220A (Page et al. GCN
Circ. 23908), from 68 s to 80.7 ks after the  BAT trigger. The data
comprise 67 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 Evans et
al. (GCN Circ. 23912).

The light curve can be modelled with an initial power-law decay with an
index of alpha=2.4 (+0.3, -0.4), followed by a break at T+173 s to an
alpha of 1.10 (+/-0.08).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.69 (+0.25, -0.23). The
best-fitting absorption column is  3.9 (+1.5, -1.2) x 10^21 cm^-2, in
excess of the Galactic value of 1.1 x 10^21 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 4.7 x 10^-11 (6.2 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      3.9 (+1.5, -1.2) x 10^21 cm^-2
Galactic foreground: 1.1 x 10^21 cm^-2
Excess significance: 3.7 sigma
Photon index:      1.69 (+0.25, -0.23)

If the light curve continues to decay with a power-law decay index of
1.10, the count rate at T+24 hours will be 1.9 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 9.1 x
10^-14 (1.2 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/00889785.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB190220B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23919
SUBJECT: GRB 190220B: Kitab Observatory optical upper limit
DATE:    19/02/21 14:58:34 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

S. Belkin (IKI), A. Novichonok (KIAM), A. Pozanenko (IKI), E. Mazaeva 
(IKI), A. Volnova (IKI), I. Molotov (KIAM) report on behalf of larger 
GRB follow-up collaboration:

We observed the field of INTEGRAL GRB 190220B (Gotz et al., GCN  23915) 
  with RC-36 0.36-m telescope of Kitab Observatory starting on Feb. 20 
(UT) 23:20:25 in  Clear filter.   We do not find any optical afterglow 
candidate in the INTEGRAL  GRB 190220B localization error circle (Gotz, 
et al., GCN  23915) with is in agreement with earlier non detection by 
BOOTES-4 (Hu et al., GCN  23916). Preliminary photometry of the field is 
following.

Date       UT start   t-T0       Filter Exp.    OT     Err.   UL(3sigma)
                       (mid, days)        (s)

2019-02-20 23:20:25   0.14972    CR     48*60   19.0   n/d    n/d

The photometry is based on the nearby USNO-B1 (R2) stars.
  .


GRB_name: GRB190219A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23920
SUBJECT: GRB 190219A: CrAO and AbAO optical upper limit
DATE:    19/02/21 18:44:49 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

A. Volnova  (IKI),  S. Nazarov (CrAO), S. Schmalz (KIAM), R. Ya. 
Inasaridze (AbAO),  A. Pozanenko (IKI),  S. Belkin (IKI), E. Mazaeva 
(IKI),  I. Molotov (KIAM) report on behalf of  IKI-GRB-FuN  collaboration:

We observed the field of GRB 190219A (Beardmore et al., GCN 23902) with 
AZT-8 of CrAO,  AS-32 (0.7m) telescope of Abastumani Observatory and 
ORI-22 telescope of ISON-Castelgrande Observatory, first observation 
starting on Feb. 19 (UT) 19:48:14.  We do not detect any object within 
enhanced XRT error circle (Beardmore et al., GCN 23907). In particular 
we do not detect the afterglow candidate (Xu et al., GCN 23911). 
Preliminary photometry of the field is following.

date       UT start    t-T0    Filter   Exp. UL         Obs./Tel.
                      (mid, d)           (s) (3 sigma)
2019-02-19 20:14:14  0.02991   R   780      20.3        CrAO/AZT-8
2019-02-20 00:39:36  0.28998   R    95*60   20.8        AbAO/AS-32

The photometry is based on nearby USNO-B1.0 stars.


GRB_name: GRB190220B
Detection_method: Fermi GBM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23921
SUBJECT: GRB 190220B: Fermi GBM observation
DATE:    19/02/21 19:49:45 GMT
FROM:    Cori Fletcher at USRA/NASA  <corinne.l.fletcher@nasa.gov>

C. Fletcher (USRA) and C. Meegan (UAH)
report on behalf of the Fermi GBM Team:

"At 20:15:31.49 UT on 20 February 2019, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 190220B (trigger 572386536 / 190220844).

which was also detected by INTEGRAL (Gotz et al. 2019, GCN 23915).
The GBM on-ground location is consistent with the INTEGRAL position.

The angle from the Fermi LAT boresight at the GBM trigger time is 23 degrees.

The GBM light curve consists of multiple peaks
with a duration (T90) of about 109 s (50-300 keV).
The time-averaged spectrum from T0-51.201 s to T0+59.393 s is
well fit by a power law function with an exponential
high-energy cutoff.  The power law index is -1.4 +/- 0.1 and
the cutoff energy, parameterized as Epeak, is 83 +/- 8 keV

The event fluence (10-1000 keV) in this time interval is
(7.2 +/- 0.6)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+38.72 s in the 10-1000 keV band
is 2.5 +/- 0.2 ph/s/cm^2.

A Band function fits the spectrum equally well
with Epeak= 73 +/- 13 keV, alpha = -1.3 +/- 0.2 and beta = -2.5 +/- 0.4.


The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."


GRB_name: GRB190226A
Detection_method: Fermi GBM Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23929
SUBJECT: GRB 190226A: Insight-HXMT/HE detection
DATE:    19/02/27 14:29:19 GMT
FROM:    Shuo Xiao at IHEP  <xiaoshuo@ihep.ac.cn>

S. Xiao, 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 2019-02-26T12:21:45.500 (T0), the Insight-HXMT/HE detected 
GRB 190226A (trigger ID: HEB190226515) in a routine search of the data, 
which was also triggered by Fermi/GBM.

The Insight-HXMT/HE light curve mainly consists of single 
pulse with a duration (T90) of 0.12 s measured from T0+0.13 s. 
The 1-s peak rate, measured from T0+0.14 s, is 3602.6 cnts/s. 
The total counts from this burst is 357.0 counts. 
URL_LC: http://www.hxmt.org/images/GRB/HEB190226515_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 (record 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 could be found at: http://www.hxmt.org.
GRB 190117A:Insight-HXMT/HE detection


GRB_name: GRB190305A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23930
SUBJECT: GRB 190305A: AGILE/MCAL detection of a burst
DATE:    19/03/05 14:39:05 GMT
FROM:    Alessandro Ursi at INAF/IAPS  <alessandro.ursi@gmail.com>

A. Ursi (INAF/IAPS), M. Cardillo, C. Casentini (INAF/IAPS), C. Pittori
(SSDC, and INAF/OAR), A. Bulgarelli, N. Parmiggiani (INAF/OAS-Bologna), M.
Tavani (INAF/IAPS, and Univ. Roma Tor Vergata), A. Argan, M. Cardillo, Y.
Evangelista, G. Piano (INAF/IAPS), F. Lucarelli, F. Verrecchia (SSDC, and
INAF/OAR), V. Fioretti, F. Fuschino (INAF/OAS-Bologna), M. Marisaldi
(INAF/OAS-Bologna, and Bergen University), M. Pilia, A. Trois
(INAF/OA-Cagliari), I. Donnarumma (ASI), F. Longo (Univ. Trieste and INFN
Trieste), A. Giuliani (INAF/IASF-Mi), report on behalf of the AGILE Team:

The AGILE Mini-CALorimeter (MCAL) detected a burst at T0 = 2019-03-05
13:05:19.34 +/- 0.01 s (UTC).

The event lasted about 1.8 s and released a total number of ~8040 counts in
the detector (in the 0.4-100 MeV energy range), above an average background
rate of 620 counts / s. The burst is also clearly visible in the scientific
ratemeters of the Anti-Coincidence (AC, 50-200 keV), SuperAGILE (SA, 18-60
keV) and MiniCALorimeter (MCAL, 0.4-100 MeV) detectors.

Further analysis is still in progress.

The AGILE-MCAL detector has a full solid angle acceptance, and is
operational in the range 0.4 - 100 MeV.


GRB_name: GRB190305A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23931
SUBJECT: GRB 190305A: Tiled Swift observations
DATE:    19/03/05 21:58:17 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P. A. Evans (U. Leicester) reports on behalf of the Swift team:

Swift has initiated a series of observations, tiled on the sky, of the
AGILE GRB 190305A. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00077

Any uncatalogued X-ray sources detected in this analysis will be
reported on this website and via GCN COUNTERPART notices. The probability of finding
serendipitous sources, unrelated to the AGILE event is high: any X-ray source
considered to be a probable afterglow candidate will be reported via a GCN Circular
after manual consideration.

Details of the XRT automated analysis methods are detailed in Evans et
al. (2007, A&A, 469, 379; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8).

This circular is an official product of the Swift-XRT team.


GRB_name: GRB190305A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23933
SUBJECT: GRB 190305A: MAXI/GSC detection
DATE:    19/03/06 05:10:26 GMT
FROM:    Satoshi Nakahira at RIKEN  <nakahira@crab.riken.jp>

S. Nakahira (RIKEN), S. Sugita (AGU), W. Iwakiri(Chuo U.), 
T. Mihara, F. Yatabe, Y. Takao, M. Matsuoka (RIKEN),
H. Negoro, M. Nakajima, A. Sakamaki, W. Maruyama, M. Aoki, K. Kobayashi (Nihon U.), 
T. Sakamoto, M. Serino, T. Hashimoto, A. Yoshida (AGU), 
N. Kawai, M. Sugizaki, Y. Tachibana, K. Morita (Tokyo Tech), 
S. Ueno, H. Tomida, M. Ishikawa, Y. Sugawara, N. Isobe, R. Shimomukai, T. Midooka (JAXA), 
Y. Ueda, A. Tanimoto, T. Morita, S. Yamada, S. Ogawa (Kyoto U.), 
Y. Tsuboi, W. Iwakiri, R. Sasaki, H. Kawai, T. Sato (Chuo U.), 
H. Tsunemi, T. Yoneyama, K. Asakura, S. Ide (Osaka U.), 
M. Yamauchi, K. Hidaka, S. Iwahori (Miyazaki U.), 
T. Kawamuro (NAOJ), 
K. Yamaoka (Nagoya U.),
M. Shidatsu (Ehime U.),
Y. Kawakubo (LSU) 
report on behalf of the MAXI team:
Using the MAXI/GSC count rate monitor data collected at one second intervals,
we have detected GRB 190305A reported by AGILE (Ursi et al., GCN23930) and CALET 
CGBM (Trigger ID 1235826131) with a duration of 1-2 sec.
Because this event is considered to be coming from outside of field of view, 
no localization was given.

Then, about two minutes after the first event, MAXI/GSC nova alert system triggered 
an uncatalogued X-ray transient source at 2019/03/05 13:07:43 UT.
Assuming that the source flux was constant over the transit,
we obtain the source position at
(R.A., Dec) = (11.326 deg, -50.122 deg) = (00 45 18, -50 07 19) (J2000) 
with a statistical 90% C.L. elliptical error region 
with long and short radii of 0.39 deg and 0.34 deg, respectively. 
The roll angle of long axis from the north direction is 68.0 deg counterclockwise. 
There is an additional systematic uncertainty of 0.1 deg (90% containment radius).
The X-ray flux averaged over the scan was 101 +- 22 mCrab
(4.0-10.0keV, 1 sigma error).
There was no significant excess flux in the previous transit at UT 11:35 
and in the next transit at 14:40 UT with an upper limit of 20 mCrab for each.

The second event is possibly an extended mission of GRB 190305A.
However, we cannot distinguish whether these two events are the same origin for now.
Further analysis is still in progress.


GRB_name: GRB190305A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23934
SUBJECT: GRB 190305A: Insight-HXMT/HE detection
DATE:    19/03/06 14:59:08 GMT
FROM:    Shuo Xiao at IHEP  <xiaoshuo@ihep.ac.cn>

S. Xiao, 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 2019-03-05T13:05:19.000 (T0), the Insight-HXMT/HE detected 
GRB 190305A (trigger ID: HEB190305545) in a routine search of the data, 
which was also triggered by AGILE/MCAL (Ursi et al., GCN23930), 
CALET/CGBM and MAXI/GSC (Nakahira et al., GCN23933). 

The Insight-HXMT/HE light curve mainly consists of multiple 
pulses with a duration (T90) of 1.35 s measured from T0+0.45 s. 
The 1-s peak rate, measured from T0+1.51 s, is 22 cnts/ms. 
The total counts from this burst is 23194 counts. 
URL_LC: http://www.hxmt.org/images/GRB/HEB190305545_lc.jpg 

This light curve has not been corrected for the data loss, 
which was caused by the extreme brightness of this burst.

All measurements above are made with the CsI detectors operating in the 
regular mode with the energy range of about 80-800 keV (record 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 could be found at: http://www.hxmt.org.


GRB_name: GRB190305A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23935
SUBJECT: GRB 190305A: Swift-XRT observations
DATE:    19/03/06 15:43:43 GMT
FROM:    Valerio D'Elia at ASDC  <valerio.delia@ssdc.asi.it>

A. D'Ai (INAF-IASFPA), A. Melandri (INAF-OAB), J.A. Kennea (PSU), B.
Sbarufatti (INAF-OAB/PSU), D.N. Burrows (PSU), A.P. Beardmore (U.
Leicester), J.P. Osborne (U. Leicester), P. D'Avanzo (INAF-OAB) and
P.A. Evans (U. Leicester) report on behalf of the Swift-XRT team:

Swift-XRT has performed follow-up observations of the AGILE and MAXI
detected burst GRB 190305A (Ursi et al. GCN Circ. 23930, Nakahira et
al. GCN Circ.23933) in a series of observations tiled on the sky. The
total exposure time is 4.4 ks, distributed over 7 tiles; the maximum
exposure at a single sky location was 1.4 ks. The data were collected
between T0+31.9 ks and T0+43.5 ks, and are entirely in Photon Counting
(PC) mode. 

Six uncatalogued X-ray sources have been detected.  Source 1 is
significantly brighter than the other candidates and  it is marginally
above the RASS limit, although,  at the moment, we cannot assess if it
is fading.

Details of these sources are given below:

Source 1:
  RA (J2000):  11.62657  =  00:46:30.38
  Dec (J2000): -50.34865  =  -50:20:55.1
  Error: 2.5 arcsec (radius, 90% conf. [Enhanced position])
  Count-rate: 0.100 +/- 0.014 ct s^-1 
  Distance: 1069 arcsec from MAXI position.
  Flux: (4.79 +/- 0.67)e-12 erg cm^-2 s^-1 (observed, 0.3-10 keV)

Source 2:
  RA (J2000):  10.5180  =  00:42:4.32
  Dec (J2000): -50.1058  =  -50:06:20.9
  Error: 6.9 arcsec (radius, 90% conf.)
  Count-rate: 0.0109 [+0.0066, -0.0047] ct s^-1   
  Distance: 1875 arcsec from MAXI position.

Source 3:
  RA (J2000):  11.5149  =  00:46:3.57
  Dec (J2000): -49.9843  =  -49:59:03.4
  Error: 6.5 arcsec (radius, 90% conf.)
  Count-rate: 0.0172 [+0.0055, -0.0045] ct s^-1   
  Distance: 649 arcsec from MAXI position.
  Flux: (1.07 [+0.34, -0.28])e-12 erg cm^-2 s^-1 (observed, 0.3-10 keV)


Source 4:
  RA (J2000):  10.8580  =  00:43:25.92
  Dec (J2000): -50.1848  =  -50:11:05.2
  Error: 7.7 arcsec (radius, 90% conf.)
  Count-rate: 0.0208 [+0.0085, -0.0067] ct s^-1   
  Distance: 1113 arcsec from MAXI position.
  Flux: (7.6 [+3.1, -2.5])e-12 erg cm^-2 s^-1 (observed, 0.3-10 keV)

Source 5:
  RA (J2000):  11.1918  =  00:44:46.04
  Dec (J2000): -49.9995  =  -49:59:58.1
  Error: 9.8 arcsec (radius, 90% conf.)
  Count-rate: (5.5 [+4.0, -2.7])e-3 ct s^-1   
  Distance: 538 arcsec from MAXI position.

Source 6:
  RA (J2000):  10.7329  =  00:42:55.89
  Dec (J2000): -49.9464  =  -49:56:47.0
  Error: 12.4 arcsec (radius, 90% conf.)
  Count-rate: (9.5 [+5.8, -4.2])e-3 ct s^-1   
  Distance: 1515 arcsec from MAXI position.

The results of the XRT-team automatic analysis of the tiled XRT
observations, including a position-specific upper limit calculator, are
available at http://www.swift.ac.uk/xrt_products/TILED_GRB00077.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB190305A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23936
SUBJECT: IPN Triangulation of GRB 190305A
DATE:    19/03/06 21:09:01 GMT
FROM:    Dmitry Svinkin at Ioffe Institute  <svinkin@mail.ioffe.ru>

D. Svinkin, S. Golenetskii, R. Aptekar, D. Frederiks, A. Kozlova,
and T. Cline on behalf of the Konus-Wind team,

K. Hurley, on behalf of the IPN,

S. Barthelmy, J. Cummings, H. Krimm, and D. Palmer,
on behalf of the Swift-BAT team, and

A. von Kienlin, X. Zhang, A. Rau, V. Savchenko, E. Bozzo,
and C. Ferrigno, on behalf of the INTEGRAL SPI-ACS GRB team,
report:

The very bright, long-duration GRB 190305A was detected by
AGILE (MCAL; Ursi et al., GCN Circ. 23930),
MAXI (GSC; Nakahira et al., GCN Circ. 23933),
CALET (GBM trigger 1235826131), Konus-Wind, INTEGRAL (SPI-ACS),
Swift (BAT), and Insight (HXMT/HE; Xiao et al., GCN Circ. 23934)
at about 47118 s UT (13:05:18).
The burst was outside the coded field of view of the BAT.

We have triangulated this GRB to a Konus-INTEGRAL annulus centered at
RA(2000)=340.399 deg (22h 41m 36s) Dec(2000)=-10.588 deg (-10d 35' 17"), 
whose radius is 47.461 +/- 0.110 deg (3 sigma), and
to a Konus-BAT annulus centered at
RA(2000)=337.304 deg (22h 29m 13s) Dec(2000)=-7.381 deg (-7d 22' 51"), 
whose radius is 51.552 +/- 0.132 deg (3 sigma).

The position of the XRT source #1 (D'Ai et al., GCN Circ. 23935)
lies 0.019 deg from the center line of the Konus-BAT annulus
and 0.136 deg from the center line of the Konus-INTEGRAL annulus,
supporting the conclusion that this source is the GRB counterpart.

This localization may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB190305_T47118/IPN/

The Konus-Wind time history and spectrum will be given in a forthcoming 
GCN Circular.


GRB_name: GRB190306A
Detection_method: MAXI Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23937
SUBJECT: GRB 190306A: MAXI/GSC detection
DATE:    19/03/07 02:09:26 GMT
FROM:    H. Negoro at Nihon U.  <negoro@phys.cst.nihon-u.ac.jp>

M. Shidatsu (Ehime U.), H. Negoro (Nihon U.), M. Serino (AGU),
M. Nakajima, A. Sakamaki, W. Maruyama, M. Aoki, K. Kobayashi (Nihon U.),
T. Mihara, S. Nakahira, F. Yatabe, Y. Takao, M. Matsuoka (RIKEN),
T. Sakamoto, S. Sugita, T. Hashimoto, A. Yoshida (AGU), N. Kawai, 
M. Sugizaki, Y. Tachibana, K. Morita (Tokyo Tech), S. Ueno, H. Tomida, 
M. Ishikawa, Y. Sugawara, N. Isobe, R. Shimomukai, T. Midooka (JAXA),
Y. Ueda, A. Tanimoto, T. Morita, S. Yamada, S. Ogawa (Kyoto U.),
Y. Tsuboi, W. Iwakiri, R. Sasaki, H. Kawai, T. Sato (Chuo U.),
H. Tsunemi, T. Yoneyama, K. Asakura, S. Ide (Osaka U.), M. Yamauchi, 
K. Hidaka, S. Iwahori (Miyazaki U.), T. Kawamuro (NAOJ), 
K. Yamaoka (Nagoya U.), Y. Kawakubo (LSU)
report on behalf of the MAXI team:

The MAXI/GSC nova alert system triggered on a bright uncatalogued X-ray
transient source at 2019 March 06 UT 20:51:59.
Assuming that the source flux was constant over the transit,
we obtain the source position at
(R.A., Dec) = (222.563 deg, 30.944 deg) = (14 50 15, +30 56 38) (J2000)
with a statistical 90% C.L. elliptical error region 
with long and short radii of 0.34 deg and 0.33 deg, respectively.
The roll angle of long axis from the north direction is 142.0 deg
counterclockwise. There is an additional systematic uncertainty of 
0.1 deg (90% containment radius). The X-ray flux averaged over the scan 
was 81 +- 16 mCrab (4.0-10.0keV, 1 sigma error).
There was no significant excess flux in the previous transit at UT 19:19
and in the next transit at UT 22:24 with an upper limit of 20 mCrab for each.


GRB_name: GRB190306A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23938
SUBJECT: GRB 190306A: Tiled Swift observations
DATE:    19/03/07 03:43:22 GMT
FROM:    Phil Evans at U of Leicester  <pae9@leicester.ac.uk>

P. A. Evans (U. Leicester) reports on behalf of the Swift team:

Swift has initiated a series of observations, tiled on the sky, of the
MAXI GRB 190306A. Automated analysis of the XRT data will
be presented online at http://www.swift.ac.uk/xrt_products/TILED_GRB00078

Any uncatalogued X-ray sources detected in this analysis will be
reported on this website and via GCN COUNTERPART notices. The probability of finding
serendipitous sources, unrelated to the MAXI event is high: any X-ray source
considered to be a probable afterglow candidate will be reported via a GCN Circular
after manual consideration.

Details of the XRT automated analysis methods are detailed in Evans et
al. (2007, A&A, 469, 379; 2009, MNRAS, 397, 1177 and 2014, ApJS, 210, 8).

This circular is an official product of the Swift-XRT team.


GRB_name: GRB190305A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23939
SUBJECT: Konus-Wind observation of GRB 190305A
DATE:    19/03/07 10:21:16 GMT
FROM:    Anna Kozlova at Ioffe Institute  <ann_kozlova@mail.ioffe.ru>

A. Kozlova, S. Golenetskii, R. Aptekar, D. Frederiks,
M. Ulanov, D. Svinkin, A. Tsvetkova, A. Lysenko, and T. Cline
on behalf of the Konus-Wind team, report:

The long-duration GRB 190305A
(AGILE/MCAL detection: Ursi et al., GCN Circ. 23930;
MAXI/GSC detection: Nakahira et al., GCN Circ. 23933;
Insight-HXMT/HE detection: Xiao et al., GCN Circ. 23934;
IPN Triangulation: Svinkin et al., GCN Circ. 23936)
triggered Konus-Wind at T0=47115.9 s UT (13:05:15.900).

The burst light curve shows a single pulse
started at ~T0-0.1 s with a total duration of ~11 s.
The emission is seen up to ~10 MeV.

As observed by Konus-Wind, the burst
had a fluence of 1.47(-0.04,+0.04)x10^-4 erg/cm2,
and a 64-ms peak flux, measured from T0+1.024 s,
of 2.00(-0.08,+0.08)x10^-4 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum of the burst
(measured from T0 to T0+2.560 s)
is best fit in the 20 keV - 10 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.44(-0.04,+0.05),
the high energy photon index beta = -2.82(-0.11,+0.10),
the peak energy Ep = 387(-15,+16) keV
(chi2 = 130/74 dof).

The spectrum near the maximum count rate
(measured from T0+0.768 to T0+1.280 s)
is best fit in the 20 keV - 10 MeV range
by the GRB (Band) model with the following parameters:
the low-energy photon index alpha = -0.15(-0.07,+0.07),
the high energy photon index beta = -2.96(-0.15,+0.12),
the peak energy Ep = 422(-20,+20) keV
(chi2 = 87/59 dof).

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB190305_T47118/

All the quoted errors are at the 90% confidence level.
All the quoted values are preliminary.


GRB_name: GRB190306B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23940
SUBJECT: GRB 190306B: Insight-HXMT/HE detection
DATE:    19/03/07 13:10:41 GMT
FROM:    Shuo Xiao at IHEP  <xiaoshuo@ihep.ac.cn>

S. Xiao, 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 2019-03-06T11:13:27.950 (T0), the Insight-HXMT/HE detected 
GRB 190306B (trigger ID: HEB190306467) in a routine search of the data. 

The Insight-HXMT/HE light curve mainly consists of multiple 
pulses with a duration (T90) of 49.28 s measured from T0-3.18 s. 
The 1-ms peak rate, measured from T0-0.022 s, is 871 cnts/s. 
The total counts from this burst is 7360 counts. 
URL_LC: http://www.hxmt.org/images/GRB/HEB190306467_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 could be found at: http://www.hxmt.org.


GRB_name: GRB190306A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23941
SUBJECT: GRB 190306A: Swift-XRT observations
DATE:    19/03/07 17:38:55 GMT
FROM:    Valerio D'Elia at ASDC  <valerio.delia@ssdc.asi.it>

D.N. Burrows (PSU), A. Tohuvavohu (PSU), S. J. LaPorte (PSU), J.P.
Osborne (U. Leicester), K.L. Page (U. Leicester), A.P. Beardmore (U.
Leicester), P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC), A. D'Ai
(INAF-IASFPA) and P.A. Evans (U. Leicester) report on behalf of the
Swift-XRT team:

Swift-XRT has performed follow-up observations of the MAXI-detected
burst GRB 190306A (Shidatsu et al. GCN Circ. 23937) in a series of
observations tiled on the sky. The total exposure time is 1.2 ks,
distributed over 7 tiles; the maximum exposure at a single sky location
was 379 s. The data were collected between T0+24.2 ks and T0+25.6 ks,
and are entirely in Photon Counting (PC) mode. 

No uncatalogued X-ray sources have been detected. The 3-sigma upper
limit in the field (not including the regions where the tiles overlap)
ranges from ~0.05 to ~0.15 ct s^-1, corresponding to a 0.3-10 keV
observed flux of 1.8e-12 to 6.1e-12 erg cm^-2 s^-1 (assuming a typical
GRB spectrum).

A previously-catalogued X-ray source has been detected, however because
it is a catalogued object it is unlikely to be the afterglow.

The results of the XRT-team automatic analysis of the tiled XRT
observations, including a position-specific upper limit calculator, are
available at http://www.swift.ac.uk/xrt_products/TILED_GRB00078.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB190304A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23942
SUBJECT: IPN Triangulation of GRB 190304A (long)
DATE:    19/03/07 21:36:04 GMT
FROM:    Anna Kozlova at Ioffe Institute  <ann_kozlova@mail.ioffe.ru>

K. Hurley, on behalf of the IPN,

I. G. Mitrofanov, D. Golovin, M. L. Litvak, and A. B. Sanin,
on behalf of the HEND-Odyssey GRB team,

A. Kozlova, S. Golenetskii, R. Aptekar, D. Frederiks, D. Svinkin,
and T. Cline on behalf of the Konus-Wind team,

A. Goldstein, M. S. Briggs, and C. Wilson-Hodge
on behalf of the Fermi GBM team,

S. Barthelmy, J. Cummings, H. Krimm, and D. Palmer,
on behalf of the Swift-BAT team,

and

W. Boynton, C. Fellows, K. Harshman, H. Enos, and R. Starr,
on behalf of the GRS-Odyssey GRB team, report:

A long-duration GRB 190304A was detected by Fermi (GBM;
trigger 573421048), Konus-Wind, Mars-Odyssey (HEND),
and Swift (BAT), at about 70642 s UT (19:37:22).
The burst was outside the coded field of view of the BAT.

We have triangulated it to a preliminary, 3 sigma error box
whose coordinates are:
  ---------------------------------------------
   RA(2000), deg                 Dec(2000), deg
  ---------------------------------------------
  Center:
    16.909 (01h 07m 38s) -80.695 (-80d 41' 41")
  Corners:
    14.558 (00h 58m 14s) -80.443 (-80d 26' 35")
    20.223 (01h 20m 54s) -80.804 (-80d 48' 14")
    19.382 (01h 17m 32s) -80.930 (-80d 55' 49")
    13.675 (00h 54m 42s) -80.556 (-80d 33' 21")
  ---------------------------------------------
The error box area is about 581 sq. arcmin, and its maximum
dimension is 1.09 deg (the minimum one is 9.7 arcmin).
The Sun distance was about 76 deg.

This box may be improved.

A triangulation map is posted at
http://www.ioffe.ru/LEA/GRBs/GRB190304_T70641/IPN/

The time history and spectrum will be given in forthcoming
GCN Circulars.


GRB_name: GRB190304A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23943
SUBJECT: Konus-Wind observation of GRB 190304A
DATE:    19/03/09 21:24:57 GMT
FROM:    Anna Kozlova at Ioffe Institute  <ann_kozlova@mail.ioffe.ru>

A. Kozlova, S. Golenetskii, R. Aptekar, D. Frederiks,
M. Ulanov, D. Svinkin, A. Tsvetkova, A. Lysenko, and T. Cline
on behalf of the Konus-Wind team, report:

The long-duration GRB 190304A
(IPN Triangulation: Hurley et al., GCN Circ. 23942)
triggered Konus-Wind at T0=70641.622 s UT (19:37:21.622).

The burst light curve shows a double-peaked structure
started at ~T0-1.6 s with a total duration of ~3.3 s.
The emission is seen up to ~1 MeV.

As observed by Konus-Wind, the burst
had a fluence of 2.48(-0.35,+0.38)x10^-6 erg/cm2,
and a 64-ms peak flux, measured from T0-0.028 s,
of 4.70(-1.01,+1.03)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 - 1 MeV range
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with  alpha = -0.61(-0.56,+0.69)
and Ep = 97(-15,+22) keV (chi2 = 84/60 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.4
(chi2 = 84/59 dof).

The spectrum near the maximum count rate
(measured from T0 to T0+0.256 s)
is best fit in the 20 keV - 1 MeV range
by a power law with exponential cutoff model
with  alpha = -0.15(-0.43,+0.49)
and Ep = 153(-19,+25) keV (chi2 = 22/22 dof).
Fitting by a GRB (Band) model yields the same alpha and Ep,
and an upper limit on the high energy photon index: beta < -2.6
(chi2 = 21/21 dof).

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB190304_T70641/

All the quoted errors are at the 90% confidence level.
All the quoted values are preliminary.


GRB_name: GRB190305A
Detection_method: CALET
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23944
SUBJECT: GRB 190305A: CALET Gamma-Ray Burst Monitor detection
DATE:    19/03/11 04:48:56 GMT
FROM:    Valentin Pal'shin at AGU  <val@phys.aoyama.ac.jp>

H. Morita, A. Yoshida, T. Sakamoto, V. Pal'shin, S. Sugita (AGU),
Y. Kawakubo (LSU), A. Tezuka, S. Matsukawa, H. Onozawa, T. Ito,
Y. Sone (AGU), K. Yamaoka (Nagoya U), S. Nakahira (RIKEN),
I. Takahashi (IPMU), Y. Asaoka, S. Ozawa, S. Torii (Waseda U),
Y. Shimizu, T. Tamura (Kanagawa U),
W. Ishizaki (ICRR), M. L. Cherry (LSU),
S. Ricciarini (U of Florence),
A. V. Penacchioni, P. S. Marrocchesi (U of Siena),
and the CALET collaboration:

The bright GRB 190305A (AGILE/MCAL detection: Ursi et al., GCN Circ.23930;
MAXI/GSC detection: Nakahira et al., GCN Circ. 23933;
Insight-HXMT/HE detection: Xiao et al., GCN Circ. 23934;
IPN Triangulation: Svinkin et al., GCN Circ. 23936;
Konus-Wind observation: Kozlova et al., GCN Circ. 23939)
triggered the CALET Gamma-ray Burst Monitor (CGBM) at 13:05:18.648 UTC
on 5 March 2019. The burst signal was seen by all CGBM detectors.

The burst light curve shows a single pulse which starts at T=0.6 sec,
peaks at 1.6 sec and ends at T+3.7 sec. The T90 and T50 durations
measured by the SGM data are 1.4 +- 0.1 sec and
0.5 +- 0.1 sec (40-1000 keV), respectively.
The ground processed light curve is available at

http://cgbm.calet.jp/cgbm_trigger/ground/1235826131/

The CALET data used in this analysis are provided by
the Waseda CALET Operation Center located at the Waseda University.


GRB_name: GRB190305A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  23945
SUBJECT: GRB 190305A: Swift-XRT afterglow detection
DATE:    19/03/11 13:16:34 GMT
FROM:    Antonino D'Ai at IASF-PA  <antonino.dai@ifc.inaf.it>

A. D'Ai (INAF-IASFPA), A. Melandri (INAF-OAB), J.A. Kennea (PSU), B.
Sbarufatti (INAF-OAB/PSU), D.N. Burrows (PSU), A.P. Beardmore (U.
Leicester), J.P. Osborne (U. Leicester), P. D'Avanzo (INAF-OAB) and
P.A. Evans (U. Leicester) report on behalf of the Swift-XRT team:

Swift-XRT has conducted further observations of the field of the AGILE
and MAXI detected burst GRB 190305A (Ursi et al. GCN Circ. 23930,
Nakahira et al. GCN Circ.23933). The observations now extend from
T0+32.7 ks to T0+143 ks. 

Of the sources reported by D'Ai et al. (GCN Circ. 23935), "Source 1" is
fading with 3-sigma significance, and is therefore likely the GRB
afterglow. Using 668 s of PC mode data and 2 UVOT images, we find an
enhanced XRT position (using the XRT-UVOT alignment and matching UVOT
field sources to the USNO-B1 catalogue): RA, Dec = 11.62657, -50.34865
which is equivalent to:

RA (J2000): 00h 46m 30.38s
Dec(J2000): -50d 20' 55.1"

with an uncertainty of 2.5 arcsec (radius, 90% confidence). This
position is 17.8 arcmin from the MAXI position. 

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.6 (+0.7, -0.6). The
best-fitting absorption column is  3.7 (+4.3, -2.9) x 10^21 cm^-2, in
excess of the Galactic value of 2.3 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 5.1 x 10^-11 (6.5 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:      3.7 (+4.3, -2.9) x 10^21 cm^-2
Galactic foreground: 2.3 x 10^20 cm^-2
Excess significance: 2.0 sigma
Photon index:      1.6 (+0.7, -0.6)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00020869.
The results of the full analysis of the tiled XRT observations are
available at http://www.swift.ac.uk/xrt_products/TILED_GRB00077.

This circular is an official product of the Swift-XRT team.


