GRB 190114C
GCN Circular 23688
Subject
GRB 190114C: Swift detection of a very bright burst with a bright optical counterpart
Date
2019-01-14T21:17:08Z (6 years ago)
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.)
GCN Circular 23690
Subject
GRB 190114C: MASTER afterglow Detection
Date
2019-01-14T21:39:56Z (6 years ago)
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.
GCN Circular 23692
Subject
GRB 190114C: Possible host galaxy in Pan-STARRS
Date
2019-01-14T21:59:08Z (6 years ago)
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.
GCN Circular 23693
Subject
GRB 190114C: MASTER 4-polarizations filters OT detection
Date
2019-01-14T22:14:54Z (6 years ago)
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.
GCN Circular 23695
Subject
GRB 190114C: NOT optical counterpart and redshift
Date
2019-01-14T22:45:48Z (6 years ago)
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.]
GCN Circular 23699
Subject
GRB 190114C: OASDG optical observations
Date
2019-01-15T01:01:57Z (6 years ago)
From
Luca Izzo at IAA-CSIC <luca.izzo@gmail.com>
L. Izzo (HETH/IAA-CSIC), A. Noschese, L. D���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.
GCN Circular 23700
Subject
CORRECTED TARGET NAME: GRB 190114C: Planned XMM-Newton observation
Date
2019-01-15T01:08:23Z (6 years ago)
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).
GCN Circular 23701
Subject
MAGIC detects the GRB 190114C in the TeV energy domain
Date
2019-01-15T01:56:36Z (6 years ago)
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)
GCN Circular 23702
Subject
GRB 190114C: GROND detection of the afterglow
Date
2019-01-15T01:58:25Z (6 years ago)
From
Jan Bolmer at MPE/Garching <jan@bolmer.de>
J. Bolmer (MPE, Garching) and P. Schady (Univ. of Bath) report:
We observed the field of GRB 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).
GCN Circular 23704
Subject
GRB 190114C: Enhanced Swift-XRT position
Date
2019-01-15T05:31:58Z (6 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
J.P. Osborne, A.P. Beardmore, P.A. Evans and M.R. Goad (U. Leicester)
report on behalf of the Swift-XRT team.
Using 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.
GCN Circular 23706
Subject
GRB 190114C: Swift-XRT refined Analysis
Date
2019-01-15T05:58:56Z (6 years ago)
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.
GCN Circular 23707
Subject
GRB 190114C: Fermi GBM detection
Date
2019-01-15T05:59:42Z (6 years ago)
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 ��� 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."
GCN Circular 23708
Subject
GRB 190114C: refined redshift by the 10.4m GTC
Date
2019-01-15T06:38:04Z (6 years ago)
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
M��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."
GCN Circular 23709
Subject
GRB 190114C: Fermi-LAT detection
Date
2019-01-15T07:23:42Z (6 years ago)
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.
GCN Circular 23710
Subject
GRB 190114C: X-shooter observations of a highly extinguished afterglow
Date
2019-01-15T09:41:05Z (6 years ago)
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.
GCN Circular 23712
Subject
GRB 190114C: AGILE/MCAL detection
Date
2019-01-15T12:13:44Z (6 years ago)
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.
GCN Circular 23714
Subject
GRB 190114C: SPI-ACS/INTEGRAL extended emission detection
Date
2019-01-15T13:12:17Z (6 years ago)
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 ��� 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
GCN Circular 23715
Subject
GRB 190114C: A type 1 BdHN with TeV emission
Date
2019-01-15T15:29:54Z (6 years ago)
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.
GCN Circular 23716
Subject
GRB 190114C:Insight-HXMT/HE detection
Date
2019-01-15T15:49:09Z (6 years ago)
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.
GCN Circular 23717
Subject
GRB 190114C: Optical observations
Date
2019-01-15T15:50:04Z (6 years ago)
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.
GCN Circular 23724
Subject
GRB 190114C: Swift-BAT refined analysis
Date
2019-01-15T19:51:20Z (6 years ago)
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/
GCN Circular 23725
Subject
GRB 190114C: Swift/UVOT Detection
Date
2019-01-15T19:59:02Z (6 years ago)
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).
GCN Circular 23726
Subject
GRB 190114C: VLA Detection
Date
2019-01-15T20:25:00Z (6 years ago)
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.
GCN Circular 23727
Subject
GRB 190114C: Mondy optical observations
Date
2019-01-15T23:01:32Z (6 years ago)
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.
GCN Circular 23728
Subject
GRB 190114C: ALMA detection of a fading mm counterpart
Date
2019-01-15T23:08:49Z (6 years ago)
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."
GCN Circular 23729
Subject
GRB 190114C: REM optical/NIR detection
Date
2019-01-15T23:15:59Z (6 years ago)
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.
GCN Circular 23732
Subject
GRB 190114C: LSGT optical observation
Date
2019-01-16T03:30:37Z (6 years ago)
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.
GCN Circular 23733
Subject
GRB190114C: GRowth-India detection of optical afterglow
Date
2019-01-16T07:33:37Z (6 years ago)
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-t0��� 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; D���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).
GCN Circular 23734
Subject
GRB 190114C: KMTNet optical observation
Date
2019-01-16T09:44:40Z (6 years ago)
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.
GCN Circular 23735
Subject
GRB190114C, Long follow up urged
Date
2019-01-16T11:14:09Z (6 years ago)
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.
GCN Circular 23736
Subject
The Swift-XRT WT mode spectrum of GRB190114C
Date
2019-01-16T11:57:45Z (6 years ago)
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.
GCN Circular 23737
Subject
Konus-Wind observation of GRB 190114C
Date
2019-01-16T13:01:40Z (6 years ago)
From
Dmitry Frederiks at Ioffe Institute <fred@mail.ioffe.ru>
D. Frederiks, S. Golenetskii, R.Aptekar, A. Kozlova,
A.Lysenko, D. Svinkin, A. Tsvetkova, M. Ulanov, and T. Cline,
on behalf of the Konus-Wind team, report:
The long, 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 �� 0.10)x10^-4 erg/cm2 and
a 64-ms peak energy flux, measured from T0+3.872,
of (2.40 �� 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 �� 0.05)x10^53 erg,
the peak luminosity L_iso is (1.67 �� 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.
GCN Circular 23740
Subject
GRB 190114C: UKIRT JHK observation
Date
2019-01-16T15:08:40Z (6 years ago)
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.
GCN Circular 23741
Subject
GRB 190114C: CHILESCOPE optical observations
Date
2019-01-16T16:09:52Z (6 years ago)
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
GCN Circular 23742
Subject
GRB 190114C: Optical detection from HCT
Date
2019-01-16T17:00:44Z (6 years ago)
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.
GCN Circular 23745
Subject
GRB190114C: ATCA detection of the radio afterglow
Date
2019-01-17T09:16:12Z (6 years ago)
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.
GCN Circular 23746
Subject
GRB 190114C: continued CHILESCOPE optical obs
Date
2019-01-17T12:39:39Z (6 years ago)
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
GCN Circular 23747
Subject
GRB 190114C: Continued UKIRT JHK observation
Date
2019-01-17T14:35:59Z (6 years ago)
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.
GCN Circular 23748
Subject
GRB 190114C: ePESSTO NTT optical observations
Date
2019-01-17T15:24:40Z (6 years ago)
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).
GCN Circular 23749
Subject
GRB 190114C: COATLI Optical Detection
Date
2019-01-17T17:53:43Z (6 years ago)
From
Alan M. Watson at Instituto de Astronomia UNAM <alan@astro.unam.mx>
Alan M. Watson (UNAM), Nat Butler (ASU), Rosa L. Becerra (UNAM), Diego
Gonz��lez (UNAM), William H. Lee (UNAM), Margarita Pereyra (UNAM), Carlos
Rom��n-Z����iga (UNAM), Alexander Kutyrev (GSFC), and Eleonora Troja
(GSFC) report:
We observed the field of GRB 190114C (Gropp et al., GCN Circ. 23688)
with the COATLI 50-cm telescope and interim imager at the Observatorio
Astron��mico Nacional on the Sierra de San Pedro M��rtir
(http://coatli.astroscu.unam.mx) from 2019-01-17 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 ��ngeles, Oscar Chapa,
Salvador Cuevas, Alejandro Farah, Jorge Fuentes, Rosal��a Langarica,
Fernando Quir��s, and Carlos Tejada) and the staff of the Observatorio
Astron��mico Nacional.
GCN Circular 23750
Subject
GRB 190114C: RT-22 detection at 36.8 GHz
Date
2019-01-17T17:57:30Z (6 years ago)
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
GCN Circular 23751
Subject
GRB 190114C: RATIR Optical and NIR Detections
Date
2019-01-17T18:07:47Z (6 years ago)
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), Jes��s Gonz��lez (UNAM), Carlos Rom��n-Z����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
Astron��mico Nacional on Sierra San Pedro M��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 Astron��mico Nacional in San Pedro
M��rtir.
GCN Circular 23753
Subject
GRB 190114C: Sardinia Radio Telescope observations
Date
2019-01-18T09:45:52Z (6 years ago)
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.
GCN Circular 23754
Subject
GRB 190114C: REM optical/NIR detection (CORRECTION)
Date
2019-01-18T10:30:16Z (6 years ago)
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.
GCN Circular 23755
Subject
GRB 190114C: Sardinia Radio Telescope observations (CORRECTION)
Date
2019-01-18T11:38:45Z (6 years ago)
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.
GCN Circular 23756
Subject
GRB 190114C: UKIRT JHK observation continuation - steady fading?
Date
2019-01-18T13:20:06Z (6 years ago)
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.
GCN Circular 23757
Subject
GRB 190114C: UKIRT JHK observation (CORRECTIONS)
Date
2019-01-18T13:36:07Z (6 years ago)
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.
GCN Circular 23760
Subject
GRB 190114C: MeerKAT radio observation
Date
2019-01-19T21:03:10Z (6 years ago)
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.
GCN Circular 23762
Subject
GRB 190114C: GMRT detection at 1.26GHz
Date
2019-01-20T19:57:03Z (6 years ago)
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.
GCN Circular 23766
Subject
GRB 190114C: RTT150 optical observations
Date
2019-01-21T20:05:18Z (6 years ago)
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.
GCN Circular 23787
Subject
GRB 190114C: CHILESCOPE optical observations
Date
2019-01-24T17:10:35Z (6 years ago)
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).
GCN Circular 23798
Subject
GRB 190114C: Optical follow-up from HCT
Date
2019-01-27T11:12:34Z (6 years ago)
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.
GCN Circular 23823
Subject
GRB 190114C: JCMT SCUBA-2 sub-mm observations
Date
2019-01-31T00:43:08Z (6 years ago)
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.
GCN Circular 23983
Subject
GRB 190114C: photometric detection of a SN component
Date
2019-03-20T21:25:17Z (6 years ago)
From
Andrea Melandri at INAF-OAB <andrea.melandri@brera.inaf.it>
A. Melandri (INAF-OAB), L. Izzo (HETH/IAA-CSIC), P. D'Avanzo (INAF-OAB), D. Malesani (DAWN/NBI and DARK/NBI), M. Della Valle (INAF-OAC), E. Pian (INAF-OAS), N. R. Tanvir (U. of Leicester), F. Ragosta (U. Federico II/OAC), F. Olivares (MAS/U. de Chile), R. Carini (INAF-OAR), E. Palazzi (INAF-OAS), S. Piranomonte (INAF-OAR), P. Jonker (SRON), A. Rossi (INAF-OAS), D. A. Kann (HETH/IAA-CSIC), D. Hartmann (Clemson U.), C. Inserra (Cardiff), E. Kankare (Turku), K. Maguire (QUB), S. J. Smartt (QUB), O. Yaron (Weizmann), D. R. Young (QUB), I. Manulis (Weizmann) on behalf of a larger collaboration
We report the discovery of the supernova associated with the gamma-ray burst GRB 190114C (Gropp et al., GCN 23688) at z=0.42 (Selsing et al., GCN 23695; Castro-Tirado et al., GCN 23708; Kann et al., GCN 23710). An observational campaign lasting about 50 days has been carried out with the VLT+FORS2, the NTT+EFOSC2 and the REM+ROS2 at the European Southern Observatory (Chile), the TNG+DOLORES, the LBT+MODS2 located at Mount Graham (Arizona), and the WHT+ACAM located at the Roque de los Muchachos Observatory (Canary Islands). These observations show, at about 15 days after the burst, an apparent flattening of the afterglow light curves, in the i and z filters, in excess of the host galaxy flux, as measured in our latest epochs. This is the consistent with the emergence of a SN associated with GRB 190114C, as observed in several previous events.
By modelling the overall light curve between 0.01 and 15 days after the burst trigger (including also data from GCN circulars) with a broken power-law (afterglow contribution) + constant (host galaxy contribution), the residual fluxes in the observed i and z bands show a peak of brightness of ~23.9 and ~23.5 mag (AB), respectively. With these values we derive an estimate for the rest frame visual absolute magnitude of the SN associated with GRB 190114C of about -18 mag. This value is about 1 mag fainter than SN 1998bw (Patat et al. 2001, ApJ, 555, 900). However, the two SNe could have a comparable brightness considering the significant extinction, yet to be quantified, suffered by this event (see e.g. Kann et al., GCN 23710).
We caution that the reported values for the SN peak brightness strongly depend on the modelling of the temporal behaviour of the overall light curve. Further photometric and spectroscopic analysis is on going.
We thank the VLT, TNG, LBT and WHT staffs for executing these observations. Part of these data have been obtained 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/>).
GCN Circular 24766
Subject
GRB 190114C: East Asia VLBI Network observations
Date
2019-06-06T20:51:25Z (6 years ago)
From
Marcello Giroletti at INAF Euro VLBI <marcello.giroletti@inaf.it>
M. Giroletti, M. Orienti (INAF-IRA), G. Ghirlanda, G. Ghisellini,
L. Nava, M. Ravasio, O. Salafia (INAF-OABrera), T. An (SHAO),
K. Hada (NAOJ), B. W. Sohn (KASI), G. Giovannini (Univ. Bologna),
Y. Zhang (UCAS)
We observed GRB 190114C (Gropp et al., GCN 23688) within the DDT project
a19mg01 using the East Asia VLBI Network (EAVN) at 22 GHz on three
epochs: 7, 16, and 33 days after the burst, respectively. We report in
the table below the observing dates and times, with the resulting
3-sigma upper limits on the source flux density (assuming the source is
unresolved at the few milliarcsecond angular resolution of the instrument):
Date Time (UT) 3-sigma u.l. (mJy)
2019-01-21 08:30-14:30 2.8
2019-01-30 08:00-14:00 1.8
2019-02-16 08:00-14:05 0.84
We acknowledge the EAVN Directors, the scheduler, and the staff at
the stations and at the KJCC for approving, executing, and correlating
these observations.