GRB 170607A
GCN Circular 21275
Subject
GRB 170607A: 15 GHz upper limits from AMI
Date
2017-06-27T15:37:54Z (9 years ago)
From
Kunal Mooley at Oxford U <kunal.mooley@physics.ox.ac.uk>
K. P. Mooley (Hintze Fellow, Oxford), 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
170607A (D'Ai et al., GCN 21214) 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 Jun 08.12, Jun 10.29, Jun
12.28 and Jun 16.24 (UT) do not reveal any radio source at the XRT
location (Beardmore et al., GCN 21215), with 3sigma upper limits of 318
uJy, 108 uJy, 117 uJy and 117 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 21259
Subject
GRB 170607A CALET Gamma-Ray Burst Monitor detection
Date
2017-06-20T00:40:51Z (9 years ago)
From
Takanori Sakamoto at AGU <tsakamoto@phys.aoyama.ac.jp>
S. Nakahira (RIKEN), A. Yoshida, T. Sakamoto, Y. Kawakubo,
M. Moriyama, Y. Yamada, A. Tezuka, S. Matsukawa (AGU),
K. Yamaoka (Nagoya U), I. Takahashi (IPMU), Y. Asaoka, S. Ozawa,
S. Torii (Waseda U), Y. Shimizu, T. Tamura (Kanagawa U), W. Ishizaki (ICRR),
M. L. Cherry (LSU), S. Ricciarini (U of Florence),
A. V. Penacchioni, P. S. Marrocchesi (U of Siena)
and the CALET collaboration:
The long-duration GRB 170607A (D'Ai et al., GCN Circ. 21214;
Hamburg et al., GCN Circ. 21218; INTEGRAL SPI-ACS trigger #7864)
triggered the CALET Gamma-ray Burst Monitor (CGBM) at 23:17:56.98
on 7 June 2017. The burst signal was seen only by the SGM instrument.
The light curve of the SGM shows two distinct peaks. The first
peak starts at T+2 sec, peaks at T+4 sec and ends at T+8 sec.
The second peak starts at T+210 sec, peaks at T+215 sec and
ends at T+230 sec. The T90 durations of the first peak and the
second peak measured by the SGM data separately are 4.0 +- 0.5 sec
and 10.5 +- 0.8 sec (40-1000 keV).
The light curve is available at
http://cgbm.calet.jp/cgbm_trigger/flight/1180912206/
The CALET data used in this analysis are provided by the Waseda
CALET Operation Center located at the Waseda University.
GCN Circular 21240
Subject
GRB 170607A: Redshift from GTC/OSIRIS
Date
2017-06-10T07:33:46Z (9 years ago)
From
Antonio de Ugarte Postigo at IAA-CSIC <deugarte@iaa.es>
A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), L. Izzo (IAA-CSIC),
C.C. Thoene (IAA-CSIC), Z. Cano (IAA-CSIC), D. A. Kann (IAA-CSIC),
R. Scarpa (GTC), and V. Herrera (GTC) report on behalf of a larger
collaboration:
We observed the afterglow of GRB 170607A (D���Ai et al. GCN 21214,
Heintz et al. GCN 21217, Lipunov et al. GCN 21219, Volnova et al.
GCN 21237) using OSIRIS at the 10.4m GTC telescope. Observation
consisted of 3x900s using grism R1000R, which covers the range
between 5100 and 10100 ��, at a mean epoch of 10.1955 June 2017
UT (2.2222 days after the GRB).
The acquisition image still shows a bright afterglow at r(AB) = 20.70
+/- 0.05 mag, as compared to SDSS field stars. In spite of the strong
contribution from the afterglow, no clear absorption features can be
detected in this spectral range. However, there are strong emission
lines due to [OII], [OIII], and H-beta at a common redshift of 0.557,
which we identify as the redshift of the GRB.
GCN Circular 21237
Subject
GRB 170607A: ISON/Terskol optical observations
Date
2017-06-09T18:33:32Z (9 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
A. Volnova (IKI), A. Pozanenko (IKI), V. Agletdinov (KIAM), E. Mazaeva
(IKI), A. Mokhnatkin (KIAM), I. Molotov (KIAM) report on behalf of
larger GRB follow-up collaboration:
We observed the field of GRB 170607A (D���Ai et al., GCN 21214) with K-800
(0.8m) telescope of ISON/Terskol observatory starting on June, 08
(UT) 23:23:04, about 1 day after the burst onset. We obtained several
unfiltered images of 20 s exposure. The optical afterglow (D���Ai et al.,
GCN 21214; Heintz et al., GCN 21217; Lipunov et al., GCN 21220) is
still bright and clearly visible in a combined image. Preliminary
photometry of the afterglow is following
Date UT start t-T0 Filter Exp. OT Err. UL
(mid, days) (s)
2017-06-08 22:21:31 1.01959 CR 128*20 18.50 0.28 18.90
Photometry is based on nearby SDSS DR9 stars
SDSS id R_Lupton
J002930.50+091415.3 16.314
J002920.28+091527.1 15.963
J002925.73+091637.7 14.803
GCN Circular 21230
Subject
GRB 170607A: Swift-BAT refined analysis
Date
2017-06-09T03:15:15Z (9 years ago)
From
Amy Lien at GSFC <amy.y.lien@nasa.gov>
T. N. Ukwatta (LANL), S. D. Barthelmy (GSFC),
J. R. Cummings (CPI), A. D'Ai (INAF-IASFPA),
H. A. Krimm (NSF/USRA), A. Y. Lien (GSFC/UMBC),
C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (AGU), M. Stamatikos (OSU),
(i.e. the Swift-BAT team):
Using the data set from T-240 to T+962 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 170607A (trigger #756284)
(D'Ai et al., GCN Circ. 21214). The BAT ground-calculated position is
RA, Dec = 7.358, 9.225 deg which is
RA(J2000) = 00h 29m 26.0s
Dec(J2000) = +09d 13' 30.8"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 57%.
The mask-weighted light curve show two prominent pulses. The first pulse
starts before it came into the BAT FOV at T0-217.9 s during a preplanned
spacecraft slew. It peaks at ~T0-210 s and ends at ~T0-190 s. The second
pulse starts at ~T0-10 s, peaks at T0, and ends at ~T0+40 s, with a tail
lasting till ~T0+140 s.
The time-averaged spectrum from T0-207.896 to T0+144.104 s is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
1.61 +- 0.07. The fluence in the 15-150 keV band is 7.5 +- 0.3 x 10^-6 erg/cm2.
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/756284/BA/
GCN Circular 21225
Subject
GRB 170607A: Correction on the possible host galaxy identification
Date
2017-06-08T17:54:18Z (9 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), A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), and S. Schulze (Weizmann Institute) report on behalf of a larger collaboration,
In our previous GCN (Heintz et al., GCN 21217) we reported a possible SDSS host galaxy at z=0.632. We note, however, that this identification was incorrect, as this galaxy lies a few arcseconds away from the GRB afterglow. However, further analysis of SDSS and Pan-STARRS images do show a possible host galaxy lying just 0.���8 of the afterglow position as measured by UVOT, with a faintness around the Pan-STARRS r-band detection limit.
GCN Circular 21220
Subject
GRB 170607A: Swift/UVOT Detection
Date
2017-06-08T12:56:36Z (9 years ago)
From
Sam Emery at MSSL-UCL <samuel.emery.15@ucl.ac.uk>
S.W.K. Emery (UCL-MSSL) and A. D'Ai (INAF-IASFPA)
report on behalf of the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 170607A
84 s after the BAT trigger (D'Ai et al., GCN Circ. 21214).
GRB 170607A was also triggered by Fermi GBM
(Hamburg and Meegan GCN Circ. 21218)
We detect a fading afterglow consistent with the position given by XRT
(Beardmore et al., GCN Circ. 21215) and ground-based optical detections
(Heintz et al., GCN Circ. 21217; Lipunov et al., GCN Circ. 21219).
The preliminary UVOT position is:
RA (J2000) = 00:29:27.82 = 7.36591 (deg.)
Dec (J2000) = +09:14:36.0 = 9.24334 (deg.)
with an estimated uncertainty of 0.42 arc sec. (radius, 90% confidence).
Preliminary detections using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and subsequent exposures are:
Filter T_start(s) T_stop(s) Exp(s) Mag
white_FC 84 233 147 15.76 +/- 0.02
white 575 5285 461 17.11 +/- 0.03
white 6895 7065 197 17.50 +/- 0.04
v 625 5696 313 17.51 +/- 0.11
b 551 1859 132 17.63 +/- 0.09
u_FC 295 545 246 16.14 +/- 0.04
u 699 6205 210 16.80 +/- 0.06
u 6454 29372 1601 17.68 +/- 0.04
uvw1 847 6105 313 16.87 +/- 0.06
uvm2 5700 5900 197 16.86 +/- 0.09
uvw2 1720 5491 216 17.04 +/- 0.07
The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.04 in the direction of the burst
(Schlegel et al. 1998).
GCN Circular 21219
Subject
GRB 170607A: MASTER-Tavrida early OT observations
Date
2017-06-08T11:05:09Z (9 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <lipunov@xray.sai.msu.ru>
V. Lipunov, N.Tyurina, V.Kornilov, E.Gorbovskoy, A.Kuznetsov,
V.Vladimirov, I.Gorbunov, D.Kuvshinov, A.V.Krylov, P.Balanutsa, V.V.Chazov, D. Vlasenko
Lomonosov Moscow State University, Sternberg Astronomical Institut of MSU
A. Tlatov, V.Senik, A.V. Parhomenko, D. Dormidontov
Kislovodsk Solar Station of the Pulkovo Observatory
N.M.Budnev, O.Gres, O. Ershova
Irkutsk State University
A.Gabovich, V.Yurkov, Yu.Sergienko
Blagoveschensk Educational State University, Blagoveschensk
D.Buckley, S. Potter, A.Kniazev, M.Kotze
South African Astronomical Observatory
R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres
The Instituto de Astrofisica de Canarias
R.Podesta, C.Lopez, F. Podesta Observatorio Astronomico Felix Aguilar (OAFA),
National University of San Juan, Argentina
H. Levato, C. Saffe
Instituto de Ciencias Astronomicas,de la Tierra y del Espacio (ICATE),
San Juan, Argentina
MASTER-Tavrida robotic telescope (MASTER-Net: http://observ.pereplet.ru)
located in Crimea Astronomical station of Lomonosov Moscow State
University pointed to the FERMI GRB 170607A error-box (ra=00 37 55
dec=+07 46 10 r=1.53, see Hamburg and Meegan GCN #21218) 25 sec after
Fermi GBM notice time and 63 sec after Fermi GBM trigger time at
2017-06-08 23:19:03 UT. This was 150 sec before Swift trigger (D'Ai et
al., GCN #21214).
MASTER-Tavrida robotic telescope repointed to Swift BAT error box (D'Ai et
al., GCN #21214) 25 sec after Swift Notice Time and 42 sec after Swift
trigger at 2017-06-07 23:22:15 UT . We see OT at first image with 10 sec
exposition. We have OT light curve starting before maximum (UT_max = ~
23h 24m) up to 2017-06-08 00:40:52 UT:
UT_max = 23:23:45 +/- 10sec
OT unfiltered magnitude (max) = 16.4 +- 0.1
RA,DEC = 00h 29m 27s.8 + 9d 14m 35s.8
Error = 0.5 arcsec
Position is coincide with UVOT position (D'Ai et al., GCN #21214).
We see rebrighting or plato starting at 2017-06-07 23:52:43 UT (~30 min
after Swift trigger).
The message may be cited.
GCN Circular 21218
Subject
GRB 170607A: Fermi GBM observation
Date
2017-06-08T09:02:25Z (9 years ago)
From
Elisabetta Bissaldi at U.Innsbruk/IAPP <Elisabetta.Bissaldi@uibk.ac.at>
R. Hamburg (UAH) and C. Meegan (UAH)
report on behalf of the Fermi GBM Team:
"At 23:17:59.57 UT on 07 June 2017, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 170607A (trigger 518570284 / 170607971),
which was also detected by the Swift/BAT (D'Ai et al. 2017, GCN 21214).
The GBM on-ground location is consistent with the Swift position.
The angle from the Fermi LAT boresight at the GBM trigger time is 100 degrees.
The GBM light curve consists of a sharp peak
with a duration (T90) of about 23 s (50-300 keV).
The time-averaged spectrum from T0-2.4 s to T0+14.0 s is
adequately fit by a power law function with an exponential
high-energy cutoff. The power law index is -1.40 +/- 0.04 and
the cutoff energy, parameterized as Epeak, is 154 +/- 13 keV.
The event fluence (10-1000 keV) in this time interval is
(9.6 +/- 0.3)E-06 erg/cm^2. The 1-sec peak photon flux measured
starting from T0+2.1 s in the 10-1000 keV band
is 15.5 +/- 0.6 ph/s/cm^2.
The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."
GCN Circular 21217
Subject
GRB 170607A: NOT optical afterglow detection
Date
2017-06-08T08:39:04Z (9 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), A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), and J. Claesen (NOT) report on behalf of a larger collaboration,
We have observed the field of GRB 170607A (D���Ai et al., GCN 21214) with the 2.5m Nordic Optical Telescope at La Palma, Spain. The observations consisted of 3x180s in the Sloan g-, r- and i-bands and were carried out at a mid-time of 04:23:59 UT (i.e. 5.03 hr after the burst). The bright afterglow is well detected in all the individual frames. From the reduced and combined images we measure magnitudes of:
g(AB) = 18.57 +/- 0.08 mag
r(AB) = 18.36 +/- 0.06 mag
i(AB) = 18.22 +/- 0.05 mag
calibrated against nearby SDSS field stars.
We also note the presence of a galaxy at a photometric redshift of 0.632 in the SDSS images, close to the location of the burst, which we identify as a host galaxy candidate.
GCN Circular 21216
Subject
GRB 170607A: Swift-XRT refined Analysis
Date
2017-06-08T07:07:40Z (9 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
D.N. Burrows (PSU), A. Cholden-Brown (PSU), A.P. Beardmore (U.
Leicester), P.A. Evans (U. Leicester), S.L. Gibson (U. Leicester), A.
Melandri (INAF-OAB), P. D'Avanzo (INAF-OAB), S. J. LaPorte (PSU) and A.
D'Ai report on behalf of the Swift-XRT team:
We have analysed 7.5 ks of XRT data for GRB 170607A (D'Ai et al. GCN
Circ. 21214), from 63 s to 19.1 ks after the BAT trigger. The data
comprise 395 s in Windowed Timing (WT) mode (the first 8 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Beardmore
et al. (GCN Circ. 21215).
The late-time light curve (from T0+5.1 ks) can be modelled with a
power-law decay with a decay index of alpha=0.54 (+/-0.09).
A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 2.003 (+0.038, -0.019). The
best-fitting absorption column is consistent with the Galactic value
of 4.4 x 10^20 cm^-2 (Willingale et al. 2013). The PC mode spectrum has
a photon index of 1.92 (+/-0.08) and a best-fitting absorption column
of 7.1 (+1.9, -1.8) x 10^20 cm^-2. The counts to observed (unabsorbed)
0.3-10 keV flux conversion factor deduced from this spectrum is 3.4 x
10^-11 (3.9 x 10^-11) erg cm^-2 count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 7.1 (+1.9, -1.8) x 10^20 cm^-2
Galactic foreground: 4.4 x 10^20 cm^-2
Excess significance: 2.5 sigma
Photon index: 1.92 (+/-0.08)
If the light curve continues to decay with a power-law decay index of
0.54, the count rate at T+24 hours will be 0.13 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 4.3 x
10^-12 (5.0 x 10^-12) erg cm^-2 s^-1.
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00756284.
This circular is an official product of the Swift-XRT team.
GCN Circular 21215
Subject
GRB 170607A: Enhanced Swift-XRT position
Date
2017-06-08T02:43:48Z (9 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
A.P. Beardmore, P.A. Evans, M.R. Goad and J.P. Osborne (U. Leicester)
report on behalf of the Swift-XRT team.
Using 1379 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 170607A, 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 = 7.36612, +9.24329 which is equivalent
to:
RA (J2000): 00h 29m 27.87s
Dec (J2000): +09d 14' 35.8"
with an uncertainty of 1.7 arcsec (radius, 90% confidence).
This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, A&A, 476, 1401) and Evans
et al. (2009, MNRAS, 397, 1177).
This circular was automatically generated, and is an official product of the
Swift-XRT team.
GCN Circular 21214
Subject
GRB 170607A: Swift detection of a burst with a bright optical counterpart
Date
2017-06-07T23:32:47Z (9 years ago)
From
David Palmer at LANL <palmer@lanl.gov>
A. D'Ai (INAF-IASFPA), D. N. Burrows (PSU), A. Cholden-Brown (PSU),
V. D'Elia (ASDC), J. A. Kennea (PSU), N. P. M. Kuin (UCL-MSSL),
F. E. Marshall (NASA/GSFC), D. M. Palmer (LANL),
B. Sbarufatti (INAF-OAB/PSU) and M. H. Siegel (PSU) report on behalf
of the Swift Team:
At 23:21:33 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 170607A (trigger=756284). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 7.343, +9.238 which is
RA(J2000) = 00h 29m 22s
Dec(J2000) = +09d 14' 16"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve showed a single FRED
structure with a duration of about 40 sec. The peak count rate
was ~4000 counts/sec (15-350 keV), at ~1 sec after the trigger.
The XRT began observing the field at 23:22:47.1 UT, 73.4 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 7.3655, 9.2425 which is equivalent to:
RA(J2000) = +00h 29m 27.72s
Dec(J2000) = +09d 14' 33.0"
with an uncertainty of 4.8 arcseconds (radius, 90% containment). This
location is 81 arcseconds from the BAT onboard position, within the BAT
error circle. No event data are yet available to determine the column
density using X-ray spectroscopy.
The initial flux in the 2.5 s image was 5.32e-09 erg cm^-2 s^-1 (0.2-10
keV).
UVOT took a finding chart exposure of 150 seconds with the White filter
starting 83 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
RA(J2000) = 00:29:27.80 = 7.36582
DEC(J2000) = +09:14:36.2 = 9.24339
with a 90%-confidence error radius of about 0.61 arc sec. This position is 3.4
arc sec. from the center of the XRT error circle. The estimated magnitude is
15.90 with a 1-sigma error of about 0.14. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.04.
Burst Advocate for this burst is A. D'Ai (antonino.dai AT ifc.inaf.it).
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.)