GRB 161014A
GCN Circular 20115
Subject
GRB 161014A: 15 GHz upper limits from AMI
Date
2016-10-27T21:35:51Z (10 years ago)
From
Kunal Mooley at Oxford U <kunal.mooley@physics.ox.ac.uk>
K. P. Mooley, T. D. Staley, R. P. Fender (Oxford), G. E. Anderson
(Curtin), T. Cantwell (Manchester), D. Titterington, S. H. Carey, J.
Hickish, Y. C. Perrott, N. Razavi-Ghods, P. Scott (Cambridge), K.
Grainge, A. Scaife (Manchester)
The AMI Large Array robotically triggered on the Swift alert for GRB
161014A (Racusin et al., GCN 20035) as part of the 4pisky program, and
subsequent follow up observations were obtained up to 10 days
post-burst. Our observations at 15 GHz on 2016 Oct 14.67, Oct 15.85, Oct
17.85, and Oct 20.85 (UT) do not reveal any radio source at the XRT
location (Mingo et al., GCN 20050), with 3sigma upper limits of 225 uJy,
285 uJy, 129 uJy, and 228 uJy respectively.
We thank the AMI staff for scheduling these observations. The AMI-GRB
database is a log of all GRB follow up observations with the AMI, and is
available at http://4pisky.org/ami-grb/.
GCN Circular 20066
Subject
GRB 161014A: Continued RATIR Optical and NIR Observations
Date
2016-10-17T23:23:29Z (10 years ago)
From
V. Zach Golkhou at ASU/RATIR <golkhou@gmail.com>
V. Zach Golkhou (ASU), Nat Butler (ASU), Alan M. Watson (UNAM), 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), Jos�� A. de Diego (UNAM), Leonid Georgiev (UNAM), Jes��s Gonz��lez
(UNAM), Carlos Rom��n-Z����iga (UNAM), Neil Gehrels (GSFC), Harvey Moseley
(GSFC), John Capone (UMD), and Vicki Toy (UMD) report:
We observed the field of GRB 161014A (Racusin, et al., GCN 20035) with
the Reionization
and Transients Infrared Camera (RATIR; www.ratir.org) on the 1.5m Harold
Johnson Telescope at the Observatorio Astron��mico Nacional on Sierra San
Pedro M��rtir from 2016/10 16.16 to 2016/10 16.26 UTC (39.29 to 41.69 hours
after the BAT trigger), obtaining a total of 1.78 hours exposure in the r
and i bands and 0.75 hours exposure in the Z, Y, J, and H bands.
For a source within the Swift-XRT error circle (Mingo, et al., GCN 20050)
and reported in Golkhou, et al. (GCN 20052), in comparison with the SDSS
DR9 and 2MASS catalogs, we obtain the following detection and upper limits
(3-sigma):
r > 23.79
i 23.57 +/- 0.32
Z > 22.72
Y > 22.57
J > 22.20
H > 21.91
These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB.
We thank the staff of the Observatorio Astron��mico Nacional in San Pedro
M��rtir.
GCN Circular 20061
Subject
GRB 161014A: VLT/X-shooter redshift confirmation
Date
2016-10-17T12:23:39Z (10 years ago)
From
Jonatan Selsing at DARK/NBI <jselsing@dark-cosmology.dk>
J. Selsing (DARK/NBI), K. E. Heintz (Univ. of Iceland and DARK/NBI), D. Malesani
(DARK/NBI and DTU Space), D. Xu (NAOC), A. de Ugarte Postigo (IAA-CSIC and
DARK/NBI), N. R. Tanvir (Univ. Leicester), K. Wiersema (Univ. Leicester) and
J. P. U. Fynbo (DARK/NBI) report on behalf of a larger collaboration:
We have observed the optical afterglow of GRB 161014A (Racusin et al., GCN
20035; Morita et al. GCN 20036; Guidorzi et al., GCN 20037; D'Avanzo et al., GCN
20040), with the cross-dispersed echelle spectrograph, X-shooter, mounted at
VLT/UT2. Observations started 11.6 hours after the BAT trigger and consist of 4
x 1200 s integration time in the three spectral arms of X-shooter, covering 3000
- 21000 AA.
The afterglow continuum is detected in all arms at high significance. A broad
absorption trough from Lyman alpha is visible at 4650 AA, along with a number of
absorption lines spread across the rest of the afterglow continuum, among which
we identity absorption features due to Mg II, Si II, C II, C IV, Al II, Al III,
Fe II, all at a consistent redshift of z = 2.823, confirming the redshift
reported by de Ugarte Postigo et al. (GCN 20043).
We acknowledge excellent support from the ESO observing staff in Paranal, in
particular Jonathan Smoker, Thomas Rivinius, Marcela Espinoza and Dimitri Gadotti
GCN Circular 20059
Subject
Konus-Wind observation of GRB 161014A
Date
2016-10-16T18:14:06Z (10 years ago)
From
Dmitry Frederiks at Ioffe Institute <fred@mail.ioffe.ru>
D. Frederiks, S. Golenetskii, R.Aptekar, P. Oleynik, M. Ulanov,
D. Svinkin, A. Tsvetkova, A.Lysenko, A. Kozlova, and T. Cline,
on behalf of the Konus-Wind team, report:
The long GRB 161014A (Swift/BAT observation:
Racusin et al., GCN 20035; Barthelmy et al., GCN 20049;
Fermi GBM observation: Bissaldi, GCN 20051)
triggered Konus-Wind at T0=45088.321 s UT (12:31:28.321).
The light curve shows a multi-peaked pulse with a duration
of ~25 s. A weak, soft pulse is also seen in the burst light
curve around ~T0+95 s, which KW ecliptic latitude response is
consistent with the position of GRB 161014A.
The emission is seen up to ~3 MeV.
As observed by Konus-Wind, the burst had a fluence of
(4.7 �� 0.7)x10^-6 erg/cm2 and a 64-ms peak energy flux,
measured from T0-0.032, of (1.3 �� 0.4)x10^-6 erg/cm2
(both in the 20 keV - 10 MeV energy range).
The time-integrated spectrum (measured from T0 to T0+16.640 s)
is best fit in the 20 keV - 5 MeV range by a cutoff power-law
(CPL) function with the following model parameters:
the photon index alpha = -1.15(-0.48,+0.73),
and the peak energy Ep = 226(-79,+267) keV,
chi2 = 92/78 dof.
Fitting this spectrum with the GRB (Band) function yields
the same alpha and Ep with only an upper limit on beta of -1.8,
chi2 = 92/71 dof.
Assuming the redshift z=2.823 (de Ugarte Postigo et al., GCN 20043)
and a standard cosmology model with H_0 = 70 km/s/Mpc,
Omega_M = 0.3, and Omega_Lambda = 0.7,
we estimate the following rest-frame parameters:
the isotropic energy release E_iso is ~8.2x10^52 erg,
the peak luminosity L_iso is ~8.7x10^52 erg/s,
and the rest-frame peak energy of the time-integrated spectrum,
Ep,i, is ~860 keV.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB161014_T45088/
All the quoted errors are estimated at the 90% confidence level.
All the presented results are preliminary.
GCN Circular 20058
Subject
GRB 161014A: refined analysis of TSHAO optical observations
Date
2016-10-16T15:59:49Z (10 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
E. Mazaeva (IKI), A. Kusakin (Fesenkov Astrophysical Institute), I.
Reva (Fesenkov Astrophysical Institute), A. Volnova (IKI), A. Pozanenko
(IKI) report on behalf of larger GRB follow-up collaboration:
We observed the field of GRB 161014A (Racusin et al., GCN 20035) with
Zeiss-1000 (East) 1-m telescope of Tien Shan Astronomical Observatory.
We obtained several images in R filter starting on Oct. 14 (UT)
13:48:35. Preliminary light curve of the afterglow (Morita et al., GCN
20036; Guidorzi et al., GCN 20037; Xin et al., GCN 20038; Nakaoka et
al., GCN 20039; Mazaeva et al., GCN 20042; Heintz et al., GCN 20044) can
be found at http://grb.rssi.ru/GRB161014A/GRB161014A_TSHAO_LC.png
Photometry is based on nearby SDSS-DR9 stars used in GCN 20042 (Mazaeva
et al.)
GCN Circular 20052
Subject
GRB 161014A: RATIR Optical and NIR Observations
Date
2016-10-15T23:51:01Z (10 years ago)
From
V. Zach Golkhou at ASU/RATIR <golkhou@gmail.com>
V. Zach Golkhou (ASU), Nat Butler (ASU), Alan M. Watson (UNAM), 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), Jos�� A. de Diego (UNAM), Leonid Georgiev (UNAM), Jes��s Gonz��lez
(UNAM), Carlos Rom��n-Z����iga (UNAM), Neil Gehrels (GSFC), Harvey Moseley
(GSFC), John Capone (UMD), and Vicki Toy (UMD) report:
We observed the field of GRB 161014A (Racusin, et al., GCN 20035) with the
Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the
1.5m Harold Johnson Telescope at the Observatorio Astron��mico Nacional on
Sierra San Pedro M��rtir from 2016/10 15.20 to 2016/10 15.39 UTC (16.17 to
20.80 hours after the BAT trigger), obtaining a total of 2.72 hours
exposure in the r and i bands and 1.22 hours exposure in the Z, Y, J, and H
bands.
For a source within the Swift-XRT error circle (Mingo, et al., GCN 20050),
in comparison with the SDSS DR9 and 2MASS catalogs, we obtain the following
detections and upper limits (3-sigma):
r 22.89 +/- 0.12
i 22.24 +/- 0.10
Z 22.01 +/- 0.15
Y > 21.60
J 21.19 +/- 0.15
H > 20.48
This source is consistent with the source reported in Morita et al., (GCNs
20036, 20046), Guidorzi et al., (GCN 20037), Xin et al., (GCN
20038), Nakaoka et al., (GCN 20039), Mazaeva et al., (GCN
20042), and Melandri et al., (GCN 20048). These magnitudes are in the AB
system and are not corrected for Galactic extinction in the direction of
the GRB.
We thank the staff of the Observatorio Astron��mico Nacional in San Pedro
M��rtir.
GCN Circular 20051
Subject
GRB 161014A: Fermi GBM observation
Date
2016-10-15T16:16:43Z (10 years ago)
From
Elisabetta Bissaldi at U.Innsbruk/IAPP <Elisabetta.Bissaldi@uibk.ac.at>
E. Bissaldi (Politecnico & INFN Bari)
reports on behalf of the Fermi GBM Team:
"At 12:31:15.91 UT on 14 October 2016, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 161014A (trigger 498141079 / 161014522),
which was also detected by the Swift/BAT (Racusin et al. 2016, GCN 20035).
The GBM on-ground location is consistent with the Swift position.
The angle from the Fermi LAT boresight at the GBM trigger time is 69 degrees.
The GBM light curve shows multiple peaks with a duration (T90) of
about 37 s (50-300 keV).
The time-averaged spectrum from T0-6 s to T0+23 s is
adequately fit by a power law function with an exponential
high-energy cutoff. The power law index is -0.74 +/- 0.09 and
the cutoff energy, parameterized as Epeak, is 167 +/- 15 keV.
The event fluence (10-1000 keV) in this time interval is
(5.4 +/- 0.3)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+7 s in the 10-1000 keV band
is 5.7 +/- 0.3 ph/s/cm^2.
The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."
GCN Circular 20050
Subject
GRB 161014A: Swift-XRT refined Analysis
Date
2016-10-15T14:31:20Z (10 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
B. Mingo (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), T.G.R.
Roegiers (PSU) and J.L. Racusin report on behalf of the Swift-XRT team:
We have analysed 5.5 ks of XRT data for GRB 161014A (Racusin et al. GCN
Circ. 20035), from 108 s to 34.8 ks after the BAT trigger. The data
comprise 48 s in Windowed Timing (WT) mode (the first 7 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. Using 5612 s of PC mode data and 8 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 = 332.64760, +7.46873
which is equivalent to:
RA (J2000): 22h 10m 35.42s
Dec(J2000): +07d 28' 07.4"
with an uncertainty of 1.4 arcsec (radius, 90% confidence).
The light curve can be modelled with an initial power-law decay with an
index of alpha=0.45 (+/-0.12), followed by a break at T+1757 s to an
alpha of 1.59 (+0.14, -0.13).
A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.83 (+0.11, -0.10). The
best-fitting absorption column is 1.5 (+0.9, -0.8) x 10^22 cm^-2, at a
redshift of 2.823, in addition to the Galactic value of 7.5 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 3.7 x
10^-11 (4.5 x 10^-11) erg cm^-2 count^-1.
A summary of the PC-mode spectrum is thus:
Galactic foreground: 7.5 x 10^20 cm^-2
Intrinsic column: 1.5 (+0.9, -0.8) x 10^22 cm^-2 at z=2.823
Photon index: 1.83 (+0.11, -0.10)
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00717500.
This circular is an official product of the Swift-XRT team.
GCN Circular 20049
Subject
GRB 161014A: Swift-BAT refined analysis
Date
2016-10-15T14:04:09Z (10 years ago)
From
Takanori Sakamoto at AGU <tsakamoto@phys.aoyama.ac.jp>
S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), A. Y. Lien (GSFC/UMBC), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), J. L. Racusin (NASA/GSFC), 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+962 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 161014A (trigger #717500)
(Racusin, et al., GCN Circ. 20035). The BAT ground-calculated position is
RA, Dec = 332.626, 7.467 deg which is
RA(J2000) = 22h 10m 30.1s
Dec(J2000) = +07d 28' 01.9"
with an uncertainty of 1.5 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 13%.
The mask-weighted light curve shows a complex structure starting at T-10 sec
and ending at T+15 sec. T90 (15-350 keV) is 18.3 +- 2.8 sec (estimated error
including systematics).
The time-averaged spectrum from T-9.1 to T+12.5 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
1.47 +- 0.15. The fluence in the 15-150 keV band is 1.9 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+0.10 sec in the 15-150 keV band
is 2.9 +- 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/717500/BA/
GCN Circular 20048
Subject
GRB 161014A: TNG optical observations
Date
2016-10-15T12:08:09Z (10 years ago)
From
Andrea Melandri at INAF-OAB <andrea.melandri@brera.inaf.it>
A. Melandri, P. D'Avanzo (INAF-OAB), V. D'Elia (INAF/OAR & ASI/ASDC), W. Boschin, D. Carosati (INAF-TNG) report on behalf of the CIBO collaboration:
We observed the field of GRB 161014A (Racusin et al., GCN 20035) with the 3.6m Telescopio Nazionale Galileo (TNG) equipped with DOLoRes. Observations were carried out in the r-sdss filter. Observations started on Oct 15 at 00:19:03 UT (~11.8 hours after the burst) and consist in a single image lasting 120 seconds.
The optical afterglow (Morita et al., GCN 20036 and GCN 20046; Guidorzi et al., GCN 20037; Xin et al., GCN 20038; Nakaoka et al., GCN 20039; Mazaeva et al., GCN 20042; Heintz et al. GCN 20044; Kitaoka et al., GCN 20047) is detected with a magnitude r(AB) = 21.5 +/- 0.3 (calibrated against nearby SDSS stars).
GCN Circular 20047
Subject
GRB 161014A: AROMA-N Optical Observation
Date
2016-10-15T11:38:58Z (10 years ago)
From
Takanori Sakamoto at AGU <tsakamoto@phys.aoyama.ac.jp>
Y. Kitaoka, T. Sakamoto, A. Yoshida (AGU)
We observed the field of GRB 161014A detected by Swift
(Racusin et al., GCN Circ. 20035) with the 12-inch AGU Robotic
Optical Monitor for Astrophysical object - Narrow (AROMA-N)
located at the Sagamihara campus of Aoyama Gakuin University.
20 images of 60 sec exposures were taken in the R filter starting
from October 14 12:47:48 (UT) about 1200 seconds after the trigger
and stopped on October 14 13:13:14 (UT). We do not detect the optical
afterglow (Morita et al., GCN Circ. 20036; Guidorzi et al., GCN Circ. 20037;
Xin et al., GCN Circ. 20038; Nakaoka et al., GCN Circ. 20039;
D'Avanzo et al., GCN Circ. 20040; Mazaeva et al., GCN Circ. 20042;
de Ugarte Postigo et al., GCN CIrc. 20043) both in the individual
images and the stacked image. The estimated five sigma upper limit
of the combined image (total exposure of 1200 sec) is ~15.9 mag
using the USNO-B1 catalog.
GCN Circular 20046
Subject
GRB 161014A: Continued MITSuME Akeno Optical Observation
Date
2016-10-15T11:33:51Z (10 years ago)
From
Taketoshi Yoshii at Tokyo Tech <yoshii.t.ac@m.titech.ac.jp>
K.Morita, T.Fujiwara, Y. Saito, Y. Ono, T. Yoshii, H. Ohuchi, Y.Tachibana, Y. Yano, S. Harita, Y.Muraki, K.Saisho, T.Ozawa, Y. Yatsu, and N. Kawai (Tokyo Tech)
report on behalf of the MITSuME collaboration:
We have been observing the optical counterpart of GRB 161014A (J. L. Racusin et al., GCN
Circular #20035) 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 2016-10-14 12:32:08 UT (46 sec after the burst) and
we detected the optical counterpart in all three bands.
The measured magnitudes were listed as follows.
We obtained following results for the magnitudes.
T0+[sec] MID-UT T-EXP[sec] g' Rc Ic
-------------------------------------------------------------------------------------------------------
46 12:34:48 270 16.67 +/- 0.13 15.69 +/- 0.08 15.40 +/- 0.07
376 13:03:53 1380 > 18.57 17.59 +/- 0.17 17.86 +/- 0.25
-------------------------------------------------------------------------------------------------------
T0+ : Elapsed time after the burst
T-EXP: Total Exposure time
We used GSC2.3 catalog for flux calibration.
GCN Circular 20045
Subject
GRB 161014A: Swift/UVOT Detection
Date
2016-10-15T10:59:41Z (10 years ago)
From
Samantha Oates at MSSL <sro@mssl.ucl.ac.uk>
S. R. Oates (U. of Warwick) and J. L. Racusin (NASA/GSFC)
report on behalf of the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 161014A
4 ks after the BAT trigger (Racusin et al., GCN Circ. 20035).
A source consistent with the optical position reported by MITSuME (Morita et al GCN Circ 20036)
and LCOGT-FTS (Guidorzi et al., GCN Circ. 20037) is detected in the
initial UVOT exposures. The lack of detection in the u and UV bands
is consistent with the redshift of 2.823 reported by GTC
(de Ugarte Postigo et al., GCN Circ. 20043).
The preliminary UVOT position is:
RA (J2000) = 22:10:35.46 = 332.64775 (deg.)
Dec (J2000) = 7:28:07.3 = 7.46869 (deg.)
with an estimated uncertainty of about 0.9 arc sec. (radius, 90% confidence).
Preliminary magnitudes using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) are:
Filter T_start(s) T_stop(s) Exp(s) Mag
wh 4491 4690 197 20.4 +/- 0.3
wh 5929 6129 197 > 20.85
v 4903 5103 197 19.1 +/- 0.4
b 4286 5924 393 20.3 +/- 0.3
u 4081 23870 1630 > 20.9
w1 5314 23503 1968 > 21.0
m2 5109 18128 1163 > 20.8
w2 4698 6335 393 > 20.2
The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.08 in the direction of the burst
(Schlegel et al. 1998).
GCN Circular 20044
Subject
GRB161014A: NOT optical observations
Date
2016-10-15T00:35:17Z (10 years ago)
From
Kasper Elm Heintz at Univ. of Iceland and DARK/NBI <heintz@dark-cosmology.dk>
K. E. Heintz (Univ. of Iceland and DARK/NBI), D. Xu (NAOC), D. Malesani (DARK/NBI and DTU Space), E. Poretti (INAF/OABr), J. Telting (NOT), A. de Ugarte Postigo (IAA-CSIC and DARK/NBI) and J. P. U. Fynbo (DARK/NBI) report on behalf of a larger collaboration:
We observed the field of GRB 161014A (Racusin et al., GCN 20035) using the ALFOSC camera mounted at the 2.56m Nordic Optical Telescope (NOT). Observations started at 21:22:59 UT on 2016-10-14 (i.e., 8.85 hr after the trigger) and SDSS g-/r-/i-filter frames were obtained with 4x300 s in each filter in a cloudy weather.
In the stacked r- and i-bands we clearly detect the optical afterglow of the burst (Morita et al., GCN 20036, Guidorzi et al., GCN 20037, Xin et al., GCN 20038, Nakaoka et al., GCN 20039 and Mazaeva et al., GCN 20042).
We measure a magnitude of m(r) = 21.60 +/- 0.06 AB mag at a median time of 9.44 hr post-burst, calibrated with nearby SDSS stars.
GCN Circular 20043
Subject
GRB 161014A: GTC spectroscopy
Date
2016-10-15T00:26:17Z (10 years ago)
From
Antonio de Ugarte Postigo at IAA-CSIC <deugarte@iaa.es>
A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), C. Thoene (IAA-CSIC),
L. Izzo (IAA-CSIC), D.A. Kann (TLS Tautenburg), P. Pessev
(IAC, ULL, GRANTECAN), A. Tejero (GRANTECAN) report on behalf
of a larger collaboration:
We observed the afterglow of GRB 161014A (Racusin et al., GCN 20035,
Morita et al. GCN 20036, Guidorzi et al. GCN 20037, Xin et al.
GCN 20038, Nakaoka et al. GCN 20039, D���Avanzo et al. GCN 20040,
Mazaeva et al. GCN 20042) with OSIRIS at the 10.4m GTC telescope on
La Palma (Spain). The observations started at 20:52 UT (with an average
epoch at 8.8 hr after the burst) and consisted of 3 x 900 s spectra using
grism R1000B, which covers the spectral region between 3700 and 7800 AA
at a resolution of R ~ 1000.
The spectrum has a low signal to noise ratio, but the preliminary reduction
with archive calibrations still reveals prominent features due to Ly-alpha,
SiII, CII, SiIV, CIV, AlII, and AlIII at a common redshift of z=2.823, which
we identify as the redshift of the GRB.
GCN Circular 20042
Subject
GRB 161014A: TSHAO optical observations
Date
2016-10-15T00:07:46Z (10 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
E. Mazaeva (IKI), A. Kusakin (Fesenkov Astrophysical Institute), I.
Reva (Fesenkov Astrophysical Institute), A. Volnova (IKI), A. Pozanenko
(IKI) report on behalf of larger GRB follow-up collaboration:
We observed the field of GRB 161014A (Racusin et al., GCN 20035) with
Zeiss-1000 (East) 1-m telescope of Tien Shan Astronomical Observatory.
We obtained several images in R filter starting on Oct. 14 (UT)
13:48:35. We detected the afterglow of GRB 161014A (Morita et al., GCN
20036; Guidorzi et al., GCN 20037; Xin et al., GCN 20038). Preliminary
photometry of of combined the first observational set is following
Date UT start t-T0 Filter Exp. OT Err. UL
(mid, days) (s)
2016-10-14 13:48:35 0.07046 R 21*120 19.0 0.10 20.6
Photometry is based on nearby SDSS-DR9 stars (Lupton transformations):
SDSS-DR9_id R(Lupton)
J221053.78+072643.3 14.88
J221018.77+072726.4 14.05
J221023.66+073006.3 15.49
J221024.28+072335.5 15.75
J221050.55+072341.7 17.10
GCN Circular 20040
Subject
GRB 161014A: Swift-XRT and UVOT afterglow detection
Date
2016-10-14T19:04:03Z (10 years ago)
From
Andrea Melandri at INAF-OAB <andrea.melandri@brera.inaf.it>
P. D'Avanzo, S. R. Oates (U. of Warwick), A. Melandri (INAF-OAB), P. A. Evans (U. Leicester), F. E. Marshall (NASA/GSFC), J. L. Racusin (NASA/GSFC) report on behalf of the Swift team:
We have analysed 1.9 ks of XRT data for GRB 161014A (Racusin et al. GCN Circ. 20035), from 108 s to 5.8 ks after the BAT trigger. The data comprise 48 s in Windowed Timing (WT) mode (the first 7 s were taken while Swift was slewing) with the remainder in Photon Counting (PC) mode. Using 1696 s of PC mode data and 4 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 = 332.64764, +7.46858 which is equivalent to:
RA (J2000): 22h 10m 35.43s
Dec(J2000): +07d 28' 06.9"
with an uncertainty of 1.7 arcsec (radius, 90% confidence).
UVOT took a settling exposure of 9.8 seconds with the v filter starting 109 seconds after the BAT trigger. We find a source consistent with the position of the afterglow reported by MITSuME (Morita et al GCN Circ 20036) and LCOGT FTS (Guidorzi et al., GCN Circ. 20037). The estimated magnitude is 16.52. No correction has been made for the expected extinction corresponding to E(B-V) of 0.08 in the direction of the burst (Schlegel et al. 1998).
GCN Circular 20039
Subject
GRB 161014A: Kanata optical observation
Date
2016-10-14T16:56:59Z (10 years ago)
From
Michitoshi Yoshida at HASC,Hiroshima U <yoshidam@hiroshima-u.ac.jp>
Nakaoka, T., Kawahara, N., Yang, C., Nagashima, H, Yoshida, M.,
Kawabata, K. (Hiroshima Univ.) on behalf of the OISTER collaboration
We performed R band imaging observations around the error circle of
GRB 161014A (Racusin et al., GCN 20035) with the optical imager HOWPol
attached to Kanata telescope of Hiroshima University. The observation
was made at 2016-10-14 12:32:48 UT (mid time of the observation). We
detected the optical transient reported by Morita et al. (GCN 20036),
Guidorzi et al. (GCN 20037) and Xin et al. (GCN 20038) in our R-band
image. The detected magnitude and five sigma upper limit (in Vega
magnitude) of the OT are listed below.
# T0+ MID-UT T-EXP R mag. R err R limit
-------------------------------------------------------
86 12:32:48 30 15.1 0.2 17.0
-------------------------------------------------------
T0+ : Elapsed time after the burst [sec]
T-EXP: Total Exposure time [sec]
GCN Circular 20038
Subject
GRB 161014A : Xinglong TNT optical observation
Date
2016-10-14T15:18:07Z (10 years ago)
From
L.P. Xin at NAOC <xlp@nao.cas.cn>
L. P. Xin, M. Zhai, J. Y. Wei, Y. L. Qiu, J. S. Deng,
J. Wang, X. H. Han, L. H. Li and C. Wu on behalf of EAFON report:
We began to observe GRB 161014A (Racusin et al., GCN 20035)
with Xinglong 0.8-m TNT telescope at 2016-10-14, 12:33:03(UT),
about 100 sec after the Swift trigger time.
The new source reported by Morita et al., (GCN 20036) and
Guidorzi et al., (GCN 20037) was clearly detected in the white images.
Preliminary analysis shows that the brightness of the optical afterglow
in R band is about 15.02 mag, calibrated by a nearby USNO B1.0 object
(22:10:31.5, +07:28:47, J2000, R=13.78mag),
at the mid time of 110 sec after the burst.
This message could be cited.
We thank the excellent support of the Xinglong 80cm TNT staff, particularly S. Liu
GCN Circular 20037
Subject
GRB161014A: optical afterglow candidate with the LCOGT-FTS
Date
2016-10-14T13:20:55Z (10 years ago)
From
Cristiano Guidorzi at Ferrara U,Italy <guidorzi@fe.infn.it>
C. Guidorzi (U. Ferrara), S. Kobayashi, I.A. Steele (LJMU), C.G. Mundell
(U. Bath), A. Gomboc (U. Nova Gorica) on behalf of a large collaboration
report:
The 2-m LCOGT Faulkes Telescope South began observing Swift GRB161014A
(Racusin et al., GCN 20035) in the SDSS r and i filters on October 14,
12:44:15 UT (~13 minutes since trigger). Within the BAT error circle we
find an uncatalogued object at the following position:
RA(J2000)= 22:10:35.47
Dec(J2000)= +07:28:07.3
with a 1 arcsec error radius and a magnitude of i~18 as calibrated
against nearby SDSS stars.
GCN Circular 20036
Subject
GRB 161014A: MITSuME-Akeno optical observation
Date
2016-10-14T13:14:41Z (10 years ago)
From
Yoichi Yatsu at Tokyo Tech. <yatsu@hp.phys.titech.ac.jp>
K.Morita, Y. Saito, Y. Ono, T. Yoshii, H. Ohuchi, Y.Tachibana, Y. Yano,
T.Fujiwara, S. Harita, Y.Muraki, K.Saisho, T.Ozawa, Y. Yatsu, and N. Kawai
(Tokyo Tech)
report on behalf of the MITSuME collaboration:
We searched for the optical counterpart of GRB 161014A (J. L. Racusin et
al., GCN Circular #20035) 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 2016-10-14 12:32:08 UT (46 sec after the burst).
We found a candidate afterglow in the BAT error circle (J. L. Racusin,
GCNCircular
#20035), at
RA(J2000) = 22:10:35.47
Dec(J2000) = +07:28:07.6
with an uncertainty of ~0.4 arcsec.
We obtained the following magnitude in Rc band.
T0+[sec] MID-UT T-EXP[sec] Rc Rc_err
���������������������������������������������������������������������������������������������
46 12:32:23 30 ~14.52 0.06
���������������������������������������������������������������������������������������������
T0+ : Elapsed time after the burst
T-EXP: Total Exposure time
We used GSC2.3 catalog for flux calibration.
GCN Circular 20035
Subject
GRB 161014A: Swift detection of a burst
Date
2016-10-14T12:49:21Z (10 years ago)
From
Scott Barthelmy at NASA/GSFC <scott@milkyway.gsfc.nasa.gov>
J. L. Racusin (NASA/GSFC), S. D. Barthelmy (GSFC),
D. N. Burrows (PSU), P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC),
N. Gehrels (NASA/GSFC), J. A. Kennea (PSU), N. P. M. Kuin (UCL-MSSL),
A. Melandri (INAF-OAB), B. Mingo (U Leicester),
K. L. Page (U Leicester), T. Sakamoto (AGU) and
B. Sbarufatti (INAF-OAB/PSU) report on behalf of the Swift Team:
At 12:31:22 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 161014A (trigger=717500). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 332.628, +7.486 which is
RA(J2000) = 22h 10m 31s
Dec(J2000) = +07d 29' 09"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve shows any short peaks
with a total duration of about 35 sec. The peak count rate
was ~3200 counts/sec (15-350 keV), at ~1 sec after the trigger.
The XRT began observing the field at 12:33:24.5 UT, 121.8 seconds after
the BAT trigger. No source was detected in 574 s of promptly downlinked
data, which covered 0% of the BAT error circle. We are waiting for the
full dataset to detect and localise the XRT counterpart.
No UVOT data is available at this time.
We note that this BAT trigger time is within 7 sec of a Fermi-GBM trigger
(trigger= 498141079).
Burst Advocate for this burst is J. L. Racusin (judith.racusin 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: http://www.swift.psu.edu/too.html.)