GRB 150910A
GCN Circular 18556
Subject
GRB 150910A: CrAO optical observations
Date
2015-11-03T19:13:53Z (10 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
V. Rumyantsev (CrAO), E. Mazaeva (IKI), A. Volnova (IKI), A. Pozanenko
(IKI) report on behalf of larger GRB follow-up collaboration:
We observed the field of the Swift GRB 150910A (Pagani et al., GCN
18264) with ZTSh telescope of CrAO observatory on Sep. 11 and Sep. 12.
We took several images in R,B-filters of 120 s exposure under good
weather conditions on Sep. 11 and non-optimal weather conditions (mean
seeing of 4") on Sep. 12.
The photometry of the afterglow (Pagani et al., GCN 18264; Zheng &
Filippenko, GCN 18265) is following
Date UT start, t-t0 Filter Exp. OT OT_err UL(3sigma)
(mid, days) (s)
2015-09-11 17:56:37 1.3762 R 10*120 21.69 0.12 22.9
2015-09-11 18:18:31 1.4022 B 20*120 22.48 0.15 23.5
2015-09-11 18:39:47 1.4244 R 10*120 21.82 0.10 23.2
2015-09-11 19:22:17 1.4436 B 16*120 22.09 0.10 23.5
2015-09-12 18:04:32 2.3801 R 10*120 n/d n/a 22.3
The photometry is based on SDSS stars used in GCN 18281 (Mazaeva et al.)
GCN Circular 18327
Subject
GRB 150910A: AAO optical observations
Date
2015-09-17T07:27:12Z (10 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
E. Mazaeva (IKI), R. Inasaridze (AAO), O. Kvaratskhelia(AAO), I. Molotov
(KIAM), A. Pozanenko (IKI) report on behalf of larger GRB follow-up
collaboration:
We observed the field of GRB 150910A (Pagani et al., GCN 18264) with
AS-32 (0.7m) telescope of Abastumani Observatory starting on Sep. 11
(UT) 20:32:45. We obtained several unfiltered images. The afterglow
(Pagani et al., GCN 18264; Zheng & Filippenko, GCN 18265) is clearly
visible in a combined image. The photometry of the combined image is
following
Date UT start t-T0 Filter Exp. OT Err
(mid, days) (s)
2015-09-11 20:32:45 1.46327 none 49*120 21.55 +/- 0.08
The photometry is based on SDSS stars used in GCN 18281 (Mazaeva et
al.), R magnitude deduced from Lupton's transformations.
GCN Circular 18320
Subject
GRB 150910A: Mt. Terskol observatory optical observations
Date
2015-09-16T11:45:10Z (10 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
A. Volnova (IKI), A. Sergeev (Terskol Branch of INASAN), M. Andreev
(Terskol Branch of INASAN), E. Mazaeva (IKI), A. Pozanenko (IKI) report
on behalf of larger GRB follow-up collaboration:
We observed the field of GRB 150910A (Pagani et al., GCN 18264) with
Zeiss-2000 telescope of Mt. Terskol observatory in R-filter starting on
Sep. 11 (UT) 00:40:58. The afterglow (Pagani et al., GCN 18264; Zheng &
Filippenko, GCN 18265) is clearly detected in a each image. The
photometry of a combined image is following
Date UT start t-T0 Filter Exp. OT Err
(mid, days) (s)
2015-09-11 00:40:58 0.67083 R 13*120 20.90 0.07
The photometry is based on SDSS stars used in GCN 18281 (Mazaeva et al.)
GCN Circular 18319
Subject
GRB 150910A: TSHAO optical observations
Date
2015-09-16T11:35:17Z (10 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
A. Volnova (IKI), I. Reva (Fesenkov Astrophysical Institute), A. Kusakin
(Fesenkov Astrophysical Institute), E. Mazaeva (IKI), A. Pozanenko
(IKI) report on behalf of larger GRB follow-up collaboration:
We observed the field of GRB 150910A (Pagani et al., GCN 18264) with
Zeiss-1000 (East) 1-m telescope of Tien Shan Astronomical Observatory on
Sep. 11 and Sep. 12. We obtained several images in R filter. The
afterglow (Pagani et al., GCN 18264; Zheng & Filippenko, GCN 18265) is
clearly visible in a combined image on Sep. 11 and on Sep. 12 we
obtained upper limit. The photometry of the combined images are following
Date UT start t-T0 Filter Exp. OT Err
(mid, days) (s)
2015-09-11 18:39:41 1.38753 R 16*300 21.87 0.10
2015-09-12 19:03:44 2.39553 R 21*300 >22.3 (3 sigma)
The photometry is based on SDSS stars used in GCN 18281 (Mazaeva et al.)
GCN Circular 18314
Subject
GRB 150910A: T100 observations
Date
2015-09-15T08:24:52Z (10 years ago)
From
Eda Sonbas at NASA/GSFC <edasonbas@gmail.com>
E. Sonbas (Adiyaman Univ.), O. Basturk (Ankara Univ.), T. Guver (Istanbul
Univ.), E. Gogus (Sabanci Univ.), S. Eryilmaz, O. Erece, H. Kirbiyik (TUG)
report on behalf of a larger collaboration
We observed the field of Swift GRB 150910A (Pagani et al., GCN#18264) with
the 1.0 meter T100 telescope (Bakirlitepe, TUBITAK National Observatory,
Turkey), starting September, 10, 20:08:16 UT (~ 11 hours after the
trigger). Observations were carried out in the R filter. The afterglow is
detected in the R band images with an exposure time of 300 s.
Using USNO-B1 star USNO-B1 1234-0008068 (R.A.=5.65, Dec=+33.45) in the
field, the magnitudes of the OT were estimated as follows;
t-t0 (hr) exp.(s) filt mag err (+/-)
10.97 300 R 20.09 0.23
11.06 300 R 20.18 0.25
Analysis of further observations with the same filter is ongoing.
We thank to TUBITAK National Observatory for a partial support in using
T100 telescope with project number 10CT100-95 and technical support.
GCN Circular 18312
Subject
GRB 150910A: Continued RATIR Observations
Date
2015-09-14T17:25:20Z (10 years ago)
From
Nat Butler at UC berkeley <natxbutler@gmail.com>
Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William H. Lee (UNAM), Michael G. Richer (UNAM), Ori Fox (UCB), J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (GSFC/STScI), 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), V. Zach Golkhou (ASU), and Vicki Toy (UMD) report:
We observed the field of GRB 150910A (Pagani et al., GCN 18264) 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 2015/09 14.17 to 2015/09 14.46 UTC (90.88 to 98.01 hours after the BAT trigger), obtaining a total of 1.71 hours exposure in the r, i, and z bands.
The optical afterglow (Pagani et al.; Zheng and Filippenko, GCN 18265) is well detected. In comparison with the SDSS DR9 catalog, we obtain:
r = 22.23 +/- 0.09
i = 22.44 +/- 0.10
z > 19.89 (3-sigma)
These magnitudes are in the AB system and are not corrected for Galactic extinction in the direction of the GRB. Compared to our previous night of observations (Butler et al., GCN 18302), the source flux is consistent with remaining constant at the ~1-sigma level. Also, the source appears to be extended in our images, suggesting that the flux may be dominated by the GRB host galaxy.
We thank the staff of the Observatorio Astron�mico Nacional in San Pedro
M�rtir.
GCN Circular 18306
Subject
GRB 150910A: Mt. Terskol observatory optical observation
Date
2015-09-14T07:16:41Z (10 years ago)
From
Alexei Pozanenko at IKI <alex@grb.rssi.ru>
M. Andreev (Terskol Branch of INASAN), E. Mazaeva (IKI), A. Sergeev (Terskol Branch of INASAN), A. Volnova (IKI), A. Pozanenko (IKI) report on behalf of larger GRB follow-up collaboration:
We observed the field of GRB 150910A (Pagani et al., GCN 18264) with Zeiss-600 telescope of Mt. Terskol observatory in R-filter starting on Sep. 10 (UT) 20:45:05. We obtained several unfiltered images. The afterglow (Pagani et al., GCN 18264; Zheng & Filippenko, GCN 18265) is clearly detected in a combined image. The photometry of the combined image is following
Date UT start t-T0 Filter Exp. OT Err
(mid, days) (s)
2015-09-10 20:45:05 0.51974 R 46*120 20.46 +/- 0.07
The photometry is based on SDSS stars used in GCN 18281 (Mazaeva et al.)
GCN Circular 18302
Subject
GRB 150910A: RATIR Observations
Date
2015-09-13T16:22:24Z (10 years ago)
From
Nat Butler at UC berkeley <natxbutler@gmail.com>
Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William H. Lee (UNAM), Michael G. Richer (UNAM), Ori Fox (UCB), J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara (GSFC/STScI), 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), V. Zach Golkhou (ASU), and Vicki Toy (UMD) report:
We observed the field of GRB 150910A (Pagani et al., GCN 18264) 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 2015/09 13.15 to 2015/09 13.26 UTC (66.44 to 69.21 hours after the BAT trigger), obtaining a total of 0.99 hours exposure in the r, i, and z bands.
The optical afterglow (Pagani et al.; Zheng and Filippenko, GCN 18265) is well detected. In comparison with the SDSS DR9 catalog, we obtain:
r 22.44 +/- 0.13
i 22.31 +/- 0.11
z > 20.29 (3-sigma)
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 18301
Subject
GRB 150910A: MITSuME Ishigakijima Optical Observation after 2 days
Date
2015-09-13T00:03:14Z (10 years ago)
From
Daisuke Kuroda at OAO/NAOJ <dikuroda@oao.nao.ac.jp>
D. Kuroda (OAO, NAOJ), H. Hanayama, T. Miyaji, J. Watanabe (IAO, NAOJ),
K. Yanagisawa (OAO, NAOJ), S.Nagayama (NAOJ), M. Yoshida (Hiroshima),
K. Ohta (Kyoto) and N. Kawai(Tokyo Tech)
report on behalf of the MITSuME and OISTER collaboration:
We observed the field of GRB 150910A (Pagani et al., GCNC 18264)
with the optical three color (g', Rc and Ic) CCD camera attached
to the Murikabushi 1m telescope of Ishigakijima Astronomical
Observatory.
The observation started on 2015-09-12 13:59:26 UT (~2.2 days after
the burst). We detected the previously reported afterglow (Pagani
et al., GCNC 18264; Zheng and Filippenko, GCNC 18265; Dichiara
et al., GCNC 18266; Kuroda et al., GCNC 18267) in Rc band.
Photometric results and three sigma upper limit of the OT are listed below.
We used GSC2.3 catalog for flux calibration.
#T0+[day] MID-UT T-EXP[sec] g' Rc Rc_err Ic
-----------------------------------------------------------------------
2.22658 14:31:04 3240.0 >22.4 22.3 0.4 >20.73
-----------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]
GCN Circular 18295
Subject
GRB150910A: P60 Observations
Date
2015-09-12T16:15:10Z (10 years ago)
From
Daniel Perley at Caltech <dperley@astro.caltech.edu>
D. A. Perley (DARK) and S. B. Cenko (NASA/GSFC) report:
We observed the location of GRB 150910A (Pagani et al., GCN 18264) using
the robotic Palomar 60-inch telescope on two epochs during the night of
2015-09-11 UT, and an additional epoch during the night of 2015-09-12
UT. During each epoch we acquired 3x180s of imaging in each of the g',
r', and i' filters.
The optical afterglow (Pagani et al.; Zheng and Filippenko, GCN 18265)
is detected in each observation. Preliminary photometry relative to
SDSS yields:
t_start(d) filt mag emag
0.973 i = 21.24 +/- 0.12
0.980 g = 21.54 +/- 0.06
0.989 r = 21.35 +/- 0.08
1.067 i = 21.28 +/- 0.07
1.074 g = 21.85 +/- 0.06
1.081 r = 21.50 +/- 0.06
2.060 i = 22.21 +/- 0.17
2.067 g = 22.66 +/- 0.14
2.074 r = 23.03 +/- 0.26
GCN Circular 18289
Subject
GRB 150910A: AAO optical observations
Date
2015-09-12T03:14:23Z (10 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
E. Mazaeva (IKI), R. Inasaridze (AAO), V. Zhuzhunadze (AAO), I. Molotov
(KIAM), A. Pozanenko (IKI) report on behalf of larger GRB follow-up
collaboration:
We observed the field of GRB 150910A (Pagani et al., GCN 18264) with
with AS-32 (0.7m) telescope of Abastumani Observatory starting on Sep.
10 (UT) 18:53:54. We obtained several unfiltered images. The afterglow
(Pagani et al., GCN 18264; Zheng & Filippenko, GCN 18265) is clearly
visible in a combined image. The photometry of the combined image is
following
Date UT start t-T0 Filter Exp. OT Err
(mid, days) (s)
2015-09-10 18:53:54 0.45834 none 50*120 20.16 +/- 0.06
The photometry is based on SDSS stars used in GCN 18281 (Mazaeva et al.)
GCN Circular 18288
Subject
GRB 150910A: MITSuME Ishigakijima Optical Observation after 1 day
Date
2015-09-12T02:51:13Z (10 years ago)
From
Daisuke Kuroda at OAO/NAOJ <dikuroda@oao.nao.ac.jp>
D. Kuroda (OAO, NAOJ), H. Hanayama, T. Miyaji, J. Watanabe (IAO, NAOJ),
K. Yanagisawa (OAO, NAOJ), S.Nagayama (NAOJ), M. Yoshida (Hiroshima),
K. Ohta (Kyoto) and N. Kawai(Tokyo Tech)
report on behalf of the MITSuME and OISTER collaboration:
We observed the field of GRB 150910A (Pagani et al., GCNC 18264)
with the optical three color (g', Rc and Ic) CCD camera attached
to the Murikabushi 1m telescope of Ishigakijima Astronomical
Observatory.
The observation started on 2015-09-11 12:29:42 UT (~1.14 days after
the burst). We detected the previously reported afterglow (Pagani
et al., GCNC 18264; Zheng and Filippenko, GCNC 18265; Dichiara
et al., GCNC 18266; Kuroda et al., GCNC 18267) in g' and Rc bands.
Photometric results and three sigma upper limit of the OT are listed below.
We used GSC2.3 catalog for flux calibration.
#T0+[day] MID-UT T-EXP[sec] g' g'_err Rc Rc_err Ic Ic_err
-----------------------------------------------------------------------
1.21526 14:14:46 4800.0 21.8 0.2 21.2 0.2 >20.8
-----------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]
GCN Circular 18287
Subject
GRB 150910A: Chuguev observatory optical observations
Date
2015-09-12T02:51:11Z (10 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
Yu. Krugly (IA KhNU), E. Mazaeva (IKI), V. Shevchenko (IA KhNU), T.
Gromakina (IA KhNU), I. Molotov (KIAM), A. Pozanenko (IKI) report on
behalf of larger GRB follow-up collaboration:
We observed the field of GRB 150910A (Pagani et al., GCN 18264) with
0.7m telescope of Institute of Astronomy, Kharkiv National University
starting on Sep. 10 (UT) 21:41:15. We obtained several images in R B
filter. The afterglow (Pagani et al., GCN 18264; Zheng & Filippenko,
GCN 18265) is clearly visible in a combined image. The photometry of the
combined image is following
Date UT start t-T0 Filter Exp. OT Err
(mid, days) (s)
2015-09-10 21:41:15 0.52235 R 11*180 20.25 +/-0.14
The photometry is based on SDSS stars used in GCN 18281 (Mazaeva et al.)
GCN Circular 18285
Subject
GRB 150910A: VLA Detection
Date
2015-09-11T22:54:59Z (10 years ago)
From
Kate Alexander at Harvard <kalexander@cfa.harvard.edu>
K. Alexander (Harvard), T. Laskar (NRAO / UC Berkeley), and E. Berger
(Harvard) report on behalf of a larger collaboration:
We observed GRB 150910A (Pagani et al; GCN 18264) at multiple frequencies
with the Karl G. Jansky Very Large Array (VLA) beginning 2015 September
11.10 UT (0.72 days after the burst). At a mean frequency of 9.8 GHz, we
detect a radio source with a preliminary flux density of ~ 0.1 mJy at
RA = 00:22:40.120 +/- 0.021
Dec = +33:28:21.750 +/- 0.036
consistent with the UVOT optical position (McCauley et al; GCN 18270) and
the enhanced Swift/XRT position (Evans et al.; GCN 18271). Follow-up
observations are planned.
GCN Circular 18284
Subject
GRB 150910A: continued SAO RAS optical observations
Date
2015-09-11T22:20:23Z (10 years ago)
From
Moskvitin Alexander at SAO RAS <mosk@sao.ru>
A. S. Moskvitin (SAO RAS), report on behalf of larger GRB follow-up team:
The field of the GRB 150910A (Pagani et al., GCN #18264) was observed
with the Zeiss-1000 telescope of SAO RAS (Russia) in Rc band
on September, 11.791 (T_mid-T0 = 1.413 days), 17:55:54--20:01:44 UT.
20 x 300 seconds frames were obtained. The OT is still clearly visible
in the stacked image. The brightness of the object R = 22.2 +/- 0.10
(based on the same SDSS stars as in previous circular GCN #18275).
GCN Circular 18281
Subject
GRB 150910A: TSHAO optical observations
Date
2015-09-11T19:27:21Z (10 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
E. Mazaeva (IKI), I. Reva (Fesenkov Astrophysical Institute), A.
Kusakin (Fesenkov Astrophysical Institute), A. Volnova (IKI), A.
Pozanenko (IKI) report on behalf of larger GRB follow-up collaboration:
We observed the field of GRB 150910A (Pagani et al., GCN 18264) with
Zeiss-1000 (East) 1-m telescope of Tien Shan Astronomical Observatory on
Sep. 10 (UT) 18:02:59 -- 20:37:38. We obtained several images in R and
B filters. In both filters the afterglow (Pagani et al., GCN 18264;
Zheng & Filippenko, GCN 18265) is clearly visible. Within 2.5 hours of
observations we do not detect significant fading of the afterglow. The
photometry of combined images are following
Date UT start t-T0 Filter Exp. OT Err
(mid, days) (s)
2015-09-10 18:08:20 0.42807 R 11*300 20.18 +/- 0.05
2015-09-10 18:02:59 0.42436 B 12*300 20.85 +/- 0.08
The photometry is based on nearby SDSS stars
SDSS_id R(Lupton)
J002232.47+332751.3 16.29
J002236.24+332854.2 15.92
J002241.61+332836.1 16.23
J002248.33+332723.4 16.76
J002231.90+333004.8 16.93
J002225.39+332809.6 16.12
J002246.76+332716.9 17.63
Our photometry in R-filter is in agreement with in subsequent
observations (Moskvitin & Goranskij, GCN 18275).
GCN Circular 18279
Subject
GRB 150910A: NOT observations of the afterglow
Date
2015-09-11T13:06:31Z (10 years ago)
From
Zach Cano at U of Iceland <zewcano@gmail.com>
Z. Cano (U. Iceland), D. Malesani (DARK/NBI), A. de Ugarte Postigo
(IAA-CSIC, DARK/NBI), D. Xu (NAOC/CAS), J. Saario (NOT, U. Turku) and P.
Jakobsson (U. Iceland) report on behalf of a larger collaboration:
We observed the field of GRB 150910A (Pagani et al., GCN Circ. 18264) with
the 2.5-m Nordic Optical Telescope (NOT) equipped with MOSCA in two epochs
on the morning of 11-Sept-2015, at 01:10 and 04:45 UT, respectively. In
SDSS filters r (epoch 1) and ugrz (epoch 2) we clearly detect the optical
afterglow (e.g. Zheng & Filippenko, GCN Circ. 18265).
A summary of our photometry is as follows:
-------------------------------------------------------
filter (SDSS) t-t0 (hr) mag +- merr
-------------------------------------------------------
r 16.27 20.85 +- 0.18
r 20.18 21.24 +- 0.21
u 20.05 21.82 +- 0.24
g 20.24 21.49 +- 0.22
z 19.84 20.78 +- 0.24
These magnitudes are calibrated to SDSS and are not corrected for
foreground extinction. We note that these magnitudes are in good agreement
with those obtained by GROND (Schmidl et al., GCN Circ. 18277) at a
contemporaneous post-explosion epoch. Compared with other datasets, e.g.
Xu et al. (GCN Circ. 18269), our second epoch of r-band observations
implies a power-law like decay in time, e.g. f(t)=t^-alpha, with a decay
slope of alpha=1.
���1.
GCN Circular 18278
Subject
GRB 150910A: MITSuME Okayama Ks-band Observation
Date
2015-09-11T09:07:35Z (10 years ago)
From
Kenshi Yanagisawa at OAO/NAOJ <yanagi@oao.nao.ac.jp>
Kenshi Yanagisawa, Daisuke Kuroda, Yasuhiro Shimizu, Hideyuki
Izumiura (OAO/NAOJ), Michitoshi Yoshida (Hiroshima-U),
Kouji Ohta(Kyoto-U), and Nobuyuki Kawai(Tokyo Tech.) report
on behalf of the MITSuME collaboration:
We observed the field of GRB150910A (Pagani et al., GCNC 18264)
in Ks-band with a wide-field NIR camera at Okayama Astrophysical
Observatory (Japan). The camera has an effective aperture of 0.91m.
Observations started from 10:03 UT on 10th September, 59 min after
the BAT trigger, to 11:14 UT. The total exposure of 26 min was
successfully obtained.
In our co-add image, we found a single point source at
R.A.(J2000) = 00:22:39.84
DEC (J2000) = +33:28:20.5
with an uncertainty of of about 2 arcsec.
We estimate the magnitude Ks = 14.85 +/- 0.13 (Vega).
The calibration was made against 2MASS field stars.
T0+[min] MID-UT T-EXP[min] Ks
------------------------------------------------------------
+94 10:38 26 14.85 +/- 0.13 (Vega)
------------------------------------------------------------
T0+ : Elapsed time after the burst [min]
T-EXP: Total Exposure time [min]
GCN Circular 18277
Subject
GRB 150910A: GROND observation of the afterglow
Date
2015-09-11T08:30:45Z (10 years ago)
From
Sebastian Schmidl at TLS Tautenburg <schmidl@tls-tautenburg.de>
S. Schmidl (TLS Tautenburg), F. Knust, and J. Greiner (both MPE Garching)
report on behalf of the GROND team:
We observed the field of GRB 150910A (SWIFT trigger 655097; Pagani et al,
GCN 18264) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008,
PASP 120, 405) mounted at the 2.2m MPG telescope at ESO La Silla
Observatory (Chile).
Observations started on September 11, 2015, at 05:08 UT, 20.1 hrs after the
GRB trigger. They were performed at an average seeing of 2.8" and at an
average airmass of 2.2.
We clearly detect the optical afterglow reported by Pagani et al. (GCN
18264), Zheng & Filippenko (GCN 18265), Dichiara et al. (GCN 18266),
Kuroda et al. (GCN 18267), Xu et al. (GCN 18269), de Ugarte Postigo et al.
(GCN 18274) and Moskvitin et al (GCN 18275).
Based on total exposures of 7.7 minutes in g'r'i'z'and 4.0 minutes in
JHK, at a midtime of 20.8 hrs after the burst, we measure the following
preliminary magnitudes (AB magnitude system):
g' = 21.5 +/- 0.2 mag,
r' = 21.2 +/- 0.2 mag,
i' = 21.0 +/- 0.2 mag,
z' = 20.8 +/- 0.2 mag,
J > 19.8 mag,
H > 19.3 mag, and
K > 18.1 mag.
Given magnitudes and upper limits are calibrated against SDSS as well as
2MASS field stars and are not corrected for the expected Galactic
foreground extinction corresponding to a reddening of E_(B-V) = 0.05 mag
in the direction of the burst (Schlegel et al. 1998).
GCN Circular 18276
Subject
GRB 150910A: MITSuME Ishigakijima Optical Observation
Date
2015-09-11T04:46:31Z (10 years ago)
From
Daisuke Kuroda at OAO/NAOJ <dikuroda@oao.nao.ac.jp>
D. Kuroda (OAO, NAOJ), H. Hanayama, T. Miyaji, J. Watanabe (IAO, NAOJ),
K. Yanagisawa (OAO, NAOJ), S.Nagayama (NAOJ), M. Yoshida (Hiroshima),
K. Ohta (Kyoto) and N. Kawai(Tokyo Tech)
report on behalf of the MITSuME and OISTER collaboration:
We observed the field of GRB 150910A (Pagani et al., GCNC 18264)
with the optical three color (g', Rc and Ic) CCD camera attached
to the Murikabushi 1m telescope of Ishigakijima Astronomical
Observatory.
The observation started on 2015-09-10 12:21:44 UT (~3.3 h after
the burst). We detected the previously reported afterglow (Pagani
et al., GCNC 18264; Zheng and Filippenko, GCNC 18265; Dichiara
et al., GCNC 18266; Kuroda et al., GCNC 18267) in all the three
bands.
Photometric results of the OT are listed below.
We used GSC2.3 catalog for flux calibration.
#T0+[day] MID-UT T-EXP[sec] g' g'_err Rc Rc_err Ic Ic_err
-----------------------------------------------------------------------
0.14010 12:26:33 540.0 19.1 0.1 18.8 0.1 18.4 0.1
-----------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]
GCN Circular 18275
Subject
GRB 150910A: SAO RAS optical photometry
Date
2015-09-11T02:06:57Z (10 years ago)
From
Moskvitin Alexander at SAO RAS <mosk@sao.ru>
A.S.Moskvitin (SAO RAS), V.P.Goranskij (SAI, Moscow State University),
report on behalf of larger GRB follow-up team:
We observed the field of the GRB 150910A (Pagani et al., GCN #18264)
with the Zeiss-1000, 1-meter telescope of SAO RAS (Russia),
equipped with the broadband filters UBVRcIc and EEV 42-40 CCD.
The observations started since 10.85 hours after the trigger.
We obtained sets of 6 x 300-sec. frames in Rc band three times per
September, 10/11 night. The OT (reported by Pagani et al., GCN #18264;
Zheng & Filippenko, GCN #18265; Dichiara et al., GCN #18266;
Kuroda et al., GCN #18267; Xu et al., GCN #18269; McCauley & Pagani,
GCN #18270; Zheng et al., GCN #18273; de Ugarte Postigo et al.,
GCN #18274) is clearly visible even in single frames.
The results of observations are as following.
# (T_mid-T0),h exp.,s R_mag time, UT
1. 11.035 6 x 300 20.20 +/- 0.05 19:56:03--20:17:48
2. 13.448 6 x 300 20.57 +/- 0.05 22:15:17--22:48:09
3. 15.739 6 x 300 20.78 +/- 0.05 00:32:30--01:05:46
Photometry is based on nearby SDSS stars (their magnitudes
were converted with the Lupon 2005 equations).
GCN Circular 18274
Subject
GRB 150910A: Redshift from 10.4m GTC+OSIRIS
Date
2015-09-11T00:17:10Z (10 years ago)
From
Antonio de Ugarte Postigo at IAA-CSIC <deugarte@iaa.es>
Antonio de Ugarte Postigo (IAA-CSIC, DARK/NBI), Christina Thoene (IAA-CSIC),
Gianluca Lombardi (IAC, ULL, GRANTECAN), and Alberto Perez (GRANTECAN)
report on behalf of a larger collaboration:
We have observed the afterglow of GRB 150910A (Pagani et al., GCN 18264)
using the 10.4 m GTC telescope equipped with OSIRIS. Our observation began
at 23:11 UT (14.1 hr after the burst) and consisted of 3x900s exposures using the
R1000B grism. The spectrum covers the wavelength range between 3700 and
7800 AA.
The acquisition image shows the afterglow at a magnitude of r=20.65+/-0.07 as
compared to SDSS stars.
The first spectrum shows a continuum throughout the full spectral range, with
several absorption features that correspond to AlII, AlIII, FeII, MgII and MgI at a
common redshift of 1.360, which we interpret as the redshift of the GRB.
GCN Circular 18273
Subject
GRB 150910A: Kast spectroscopy from 3m Shane telescope
Date
2015-09-11T00:05:09Z (10 years ago)
From
Weikang Zheng at UC Berkeley <weikang@berkeley.edu>
WeiKang Zheng, Alexei V. Filippenko and Heechan Yuk (UC Berkeley),
Yinan Zhu (NAOC) and Daniel A. Perley (Dark Cosmology Center)
report on behalf of the KAIT GRB team:
We observed the optical afterglow of GRB 150910A (Pagani et al.,
GCN 18264; Zheng & Filippenko, GCN 18265) with the Kast spectrograph
on the 3m Shane telescope at Lick Observatory, started at 10:08 UT
(about 1.1 hours after the burst), covering the 3500 - 10000 A
wavelength range. A 1200-second and a 2400-second exposures
were acquired.
The spectrum shows blue continuum flux across the entire spectral
range. We detect absorption lines from Mg II (2796,2803) and Fe II
(2344,2374,2383) at a common redshift of z=1.359, as well as additional
lines further to the blue. We suggest this as the likely redshift of
the GRB.
GCN Circular 18272
Subject
GRB 150910A: Swift-XRT refined Analysis
Date
2015-09-10T22:26:03Z (10 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
K.L. Page (U. Leicester), A.P. Beardmore (U. Leicester), A. Melandri
(INAF-OAB), P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC), D.N. Burrows
(PSU), T.G.R. Roegiers (PSU), L.M. McCauley (PSU) and C. Pagani report
on behalf of the Swift-XRT team:
We have analysed 8.0 ks of XRT data for GRB 150910A (Pagani et al. GCN
Circ. 18264), from 136 s to 35.1 ks after the BAT trigger. The data
comprise 938 s in Windowed Timing (WT) mode (the first 7 s were taken
while Swift was slewing) with the remainder in Photon Counting (PC)
mode. The enhanced XRT position for this burst was given by Evans et
al. (GCN Circ. 18271).
The late-time light curve (from T0+6.4 ks) can be modelled with a
series of power-law decays. The initial decay index is alpha=0.67
(+0.23, -0.21). At T+10.9 ks the decay steepens to an alpha of 3.17
(+0.86, -0.30) before breaking again at T+20.3 ks to a final decay with
index alpha=1.3 (+/-0.4).
A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.56 (+/-0.04). The
best-fitting absorption column is 1.30 (+0.16, -0.15) x 10^21 cm^-2,
in excess of the Galactic value of 5.4 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 1.77 (+0.09, -0.08)
and a best-fitting absorption column of 7.1 (+2.3, -1.7) x 10^20 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum is 3.7 x 10^-11 (4.2 x 10^-11) erg cm^-2
count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 7.1 (+2.3, -1.7) x 10^20 cm^-2
Galactic foreground: 5.4 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index: 1.77 (+0.09, -0.08)
If the light curve continues to decay with a power-law decay index of
1.3, the count rate at T+24 hours will be 0.033 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.2 x
10^-12 (1.4 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/00655097.
This circular is an official product of the Swift-XRT team.
GCN Circular 18271
Subject
GRB 150910A: Enhanced Swift-XRT position
Date
2015-09-10T19:10:24Z (10 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
P.A. Evans, M.R. Goad, J.P. Osborne and A.P. Beardmore (U. Leicester)
report on behalf of the Swift-XRT team.
Using 1428 s of XRT Photon Counting mode data and 5 UVOT
images for GRB 150910A, 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 = 5.66723, +33.47278 which is equivalent
to:
RA (J2000): 00h 22m 40.14s
Dec (J2000): +33d 28' 22.0"
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 18270
Subject
GRB 150910A: Swift/UVOT Detection of a Brightening Afterglow
Date
2015-09-10T16:11:49Z (10 years ago)
From
Marissa McCaule at PSU <marissamc@swift.psu.edu>
L. M. McCauley (PSU) and C. Pagani (U Leicester)
report on behalf of the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 150910A
154 s after the BAT trigger (Pagani et al., GCN Circ. 18264).
A source consistent with the XRT position
(Pagani et al. GCN Circ. 18264)
is detected in the initial UVOT exposures.
The preliminary UVOT position is:
RA (J2000) = 00:22:40.11 = 5.66713 (deg.)
Dec (J2000) = +33:28:21.9 = 33.47274 (deg.)
with an estimated uncertainty of 0.58 arc sec. (radius, 90% confidence).
Preliminary detections using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) show a very rapid and steep
rise in the luminosity of the afterglow over the first 1 ks of observation.
Further investigation is strongly encouraged.
Preliminary detections for the early exposures are:
Filter T_start(s) T_stop(s) Exp(s) Mag
white 153 303 147 19.90
white 156 303 144 19.93
white 592 612 19 17.09
white 765 785 19 16.67
white 866 1016 147 16.30
v 135 145 9 >17.23
v 642 662 19 16.64
v 815 835 19 16.91
v 1046 1066 19 16.11
b 568 588 19 17.56
b 741 761 19 16.87
u 312 561 245 18.03
u 312 561 245 18.02
u 716 736 19 16.14
uvw1 692 712 19 16.76
uvw2 1022 1041 19 >17.97
The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.05 in the direction of the burst
(Schlegel et al. 1998).
GCN Circular 18269
Subject
GRB 150910A: Nanshan optical observations
Date
2015-09-10T14:50:26Z (10 years ago)
From
Dong Xu at NAOC/CAS <dong.dark@gmail.com>
D. Xu (NAOC/CAS), Y. Qin (Geneva Observatory), Y.-D. Hu (IAA-CSIC),
Y.-H. Han (NAOC/CAS, HUST), X. Zhang, A. Esamdin, L. Ma (XAO) report:
We observed the field of GRB 150910A (Pagani et al., GCN 18264) using
the 1m telescope located at Nanshan, Xinjiang, China. We obtained
3x600s R-band frames with some floating clouds in the sky.
The afterglow (Pagani et al., GCN 18264; Zheng & Filippenko, GCN
18265) is detected in each of the frames. Preliminary results are as
follows
Mid Time Exposure Mag MagErr
(hr) (s)
4.91 600 19.40 0.20
5.14 600 19.55 0.20
5.31 600 19.30 0.20
and calibrated with the nearby SDSS field.
GCN Circular 18268
Subject
GRB 150910A: Swift-BAT refined analysis
Date
2015-09-10T13:19:46Z (10 years ago)
From
Scott Barthelmy at NASA/GSFC <scott@lheamail.gsfc.nasa.gov>
A. Y. Lien (GSFC/UMBC), S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC),
C. Pagani (U Leicester), 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 downlinks,
we report further analysis of BAT GRB 150910A (trigger #655097)
(Pagani, et al., GCN Circ. 18264). The BAT ground-calculated position is
RA, Dec = 5.677, 33.466 deg, which is
RA(J2000) = 00h 22m 42.5s
Dec(J2000) = +33d 27' 56.8"
with an uncertainty of 2.3 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 14%.
The mask-weighted light curve shows the burst definitely starting at ~T-150 sec
(and posibly before T-240 when we start having data), peaking at ~T+83 sec,
and ending at ~T+450 sec. T90 (15-350 keV) is 112.2 +- 38.3 sec
(estimated error including systematics).
The time-averaged spectrum from T-5.00 to T+149.75 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
1.42 +- 0.12. The fluence in the 15-150 keV band is 4.8 +- 0.4 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+82.89 sec in the 15-150 keV band
is 1.1 +- 0.4 ph/cm2/sec. All the quoted errors are at the 90% confidence
level.
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/655097/BA/
GCN Circular 18267
Subject
GRB 150910A: MITSuME Okayama Optical Observation
Date
2015-09-10T11:41:03Z (10 years ago)
From
Daisuke Kuroda at OAO/NAOJ <dikuroda@oao.nao.ac.jp>
D. Kuroda, K. Yanagisawa, Y. Shimizu, H. Toda (OAO, NAOJ),
S. Nagayama (NAOJ), M. Yoshida (Hiroshima), K. Ohta (Kyoto)
and N. Kawai(Tokyo Tech)
report on behalf of the MITSuME and OISTER collaboration:
We observed the field of GRB 150910A (Pagani et al., GCNC 18264)
with the optical three color (g', Rc and Ic) CCD camera attached
to the MITSuME 50cm telescope of Okayama Astrophysical Observatory.
The observation started on 2015-09-10 10:20:44 UT (~1.3 h after
the burst). We detected the previously reported afterglow (Pagani
et al., GCNC 18264; Zheng and Filippenko, GCNC 18265; Dichiara
et al., GCNC 18266) in all the three bands.
Photometric results of the OT are listed below.
We used SDSS-DR7 catalog for flux calibration.
#T0+[day] MID-UT T-EXP[sec] g' g'_err Rc Rc_err Ic Ic_err
-----------------------------------------------------------------------
0.05630 10:25:52 540.0 17.6 0.2 18.4 0.2 17.0 0.1
------------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]
GCN Circular 18266
Subject
GRB 150910A: LCOGT FTN afterglow observations
Date
2015-09-10T11:05:14Z (10 years ago)
From
Cristiano Guidorzi at Ferrara U,Italy <guidorzi@fe.infn.it>
S. Dichiara, C. Guidorzi (U. Ferrara), S. Kobayashi (LJMU), A. Gomboc
(U. Ljubljana), C. Mundell (U. Bath) on behalf of a larger collaboration
report:
The 2-m LCOGT Faulkes Telescope North in Hawaii began observing Swift
GRB 150910A (Pagani et al. GCN 18264) on September 10, 09:33:19 UT (28
minutes after the burst trigger) with SDSS r and i filters. We clearly
detect the optical afterglow (Pagani et al. GCN 18264; Zheng et al. GCN
18265) with the following magnitudes:
Mid Time Exposure Filter Magnitude
(min) (s)
-------------------------------------------------------
29.0 60 r' 16.60 +- 0.02
35.6 60 i' 16.42 +- 0.02
-------------------------------------------------------
Calibration is done against SDSS magnitudes of nearby stars.
GCN Circular 18265
Subject
GRB 150910A: KAIT Optical Afterglow Detection
Date
2015-09-10T10:00:52Z (10 years ago)
From
Weikang Zheng at UC Berkeley <weikang@berkeley.edu>
WeiKang Zheng and Alexei V. Filippenko (UC Berkeley) report on
behalf of the KAIT GRB team:
The 0.76-m Katzman Automatic Imaging Telescope (KAIT), located at
Lick Observatory, responded to Swift GRB 150910A (Pagani
et al., GCN 18264) starting at 09:34:20 UT, ~30 minutes after
the burst. Observations were performed with an automatic sequence
in the clear (roughly R), V, and I filters, and the exposure time was
20 s per image. The UVOT afterglow reported by Pagani et al. (GCN 18264)
was clearly detected in all filters. The brightness is about R~16.2 mag
at ~30 minutes after the burst, and is decreasing.
Follow-up observations are encouraged.
GCN Circular 18264
Subject
GRB 150910A: Swift detection of a burst with an optical afterglow
Date
2015-09-10T09:26:53Z (10 years ago)
From
Kim Page at U.of Leicester <klp5@leicester.ac.uk>
C. Pagani (U Leicester), A. P. Beardmore (U Leicester),
A. A. Breeveld (UCL-MSSL), K. L. Page (U Leicester),
P. Romano (INAF-IASFPA) and T. N. Ukwatta (LANL) report on behalf of
the Swift Team:
At 09:04:48 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 150910A (trigger=655097). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 5.675, +33.499 which is
RA(J2000) = 00h 22m 42s
Dec(J2000) = +33d 29' 55"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). As is typical for image triggers, the real-time
light curve does not show anything significant.
The XRT began observing the field at 09:07:14.1 UT, 145.3 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 5.6669, 33.4717 which is equivalent to:
RA(J2000) = +00h 22m 40.06s
Dec(J2000) = +33d 28' 18.1"
with an uncertainty of 5.1 arcseconds (radius, 90% containment). This
location is 101 arcseconds from the BAT onboard position, within the
BAT error circle. No event data are yet available to determine the
column density using X-ray spectroscopy.
UVOT took a finding chart exposure of 150 seconds with the White filter
starting 153 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
RA(J2000) = 00:22:40.14 = 5.66723
DEC(J2000) = +33:28:21.9 = 33.47275
with a 90%-confidence error radius of about 0.71 arc sec. This position is 3.9
arc sec. from the center of the XRT error circle. The estimated magnitude is
20.27 with a 1-sigma error of about 0.18. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.05.
Burst Advocate for this burst is C. Pagani (cp232 AT star.le.ac.uk).
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)