GRB 100925A
GCN Circular 11314
Subject
GRB 100925A / MAXI J1659-152: MASTER optical observations
Date
2010-09-29T16:00:26Z (15 years ago)
From
Vladimir Lipunov at Moscow State U/Krylov Obs <gcncirc@observ.inetcomm.ru>
E. Gorbovskoy, V.Kornilov, V. Lipunov, A.Belinski,
N.Shatskiy, N.Tyurina, P.Balanutsa, V.V.Chazov, D.Kuvshinov, ,
A.Kuznetsov, D.Zimnukhov, M. Kornilov, A.Sankovich
Sternberg Astronomical Institute, Moscow State University
K.Ivanov, O.Chuvalaev, V.Poleschuk, E.Konstantinov, V.Lenok, O.Gres,
S.Yazev, N.M.Budnev,
Irkutsk State University
A. Tlatov, A.V. Parhomenko, D. Dormidontov, V.Sennik
Kislovodsk Solar Station of the Pulkovo Observatory
V.Yurkov, Yu.Sergienko, D.Varda, I.Kudelina
Blagoveschensk Educational State University, Blagoveschensk
V.Krushinski, I.Zalozhnich, T.Kopytova, A. Popov
Ural State University, Kourovka
We observed GRB 100925A / MAXI J1659-152 (Mangano et al., GCN
11296; Barthelmy et al., GCN 11300; Marshall et al. GCN 11298;
Negoro et al.ATEL 2873) in automatic regime after sunset
at Tunka and Kislovodsk (MASTER-Net: http://observ.pereplet.ru, Lipunov
et al., 2010, Advances in Astronomy, vol. 2010, pp. 1-7).
The elevation of the source was about 15 degrees at Tunka and about 22
degrees at Kislovodsk.
The results of the R photometry are:
Date JD T-T_trigger [day] R[mag] [+-] Site
2010-09-25 12:09:27 2455465.00657 0.098 16.08 0.25 Tunka
2010-09-26 02:54:12 2455465.62098 0.274 16.14 0.20 Tunka
2010-09-26 16:25:36 2455466.18445 1.276 16.20 0.10 Kislo
This photometry calibrated by USNOB1 stars.
The message may be cited.
mailto: lipunov@sai.msu.ru
GCN Circular 11309
Subject
GRB 100925A / MAXI J1659-152: WSRT Radio and Polarization Detection
Date
2010-09-27T01:15:56Z (15 years ago)
From
Alexander van der Horst at NASA/MSFC <Alexander.J.VanDerHorst@nasa.gov>
A.J. van der Horst (NASA/MSFC/ORAU), J. Granot (U of Hertfordshire),
Z. Paragi (JIVE), C. Kouveliotou (NASA/MSFC), R.A.M.J. Wijers (U of
Amsterdam) and E. Ramirez-Ruiz (UC Santa Cruz) report:
"We observed the position of the hard X-ray transient GRB 100925A /
MAXI J1659-152 (GCN 11296, ATel #2873, GCN 11307) with the Westerbork
Synthesis Radio Telescope at 4.8 GHz, at September 26 14.27 to 19.75 UT,
i.e. 1.37 days after the Swift/BAT trigger (GCN 11296) and 1.60 days
after the start of the source brightening in MAXI/GSC (ATel #2873).
We detect a radio source at the Swift/UVOT position of the transient
(GCN 11298), with a flux density of 4.92 +/- 0.04 mJy. The source is
linearly polarized at a level of 23 +/- 2 %, but there is no circular
polarization detected, with a 3-sigma upper limit of 2 %.
We would like to thank the WSRT staff for rapidly scheduling and
obtaining these observations."
GCN Circular 11308
Subject
GRB 100925A / MAXI J1659-152: Optical observation with the Kottamia 188cm telescope
Date
2010-09-26T19:37:50Z (15 years ago)
From
Michitoshi Yoshida at HASC,Hiroshima U <yoshidam@hiroshima-u.ac.jp>
M. Yoshida, K. S. Kawabata (HASC, Hiroshima U.), Gamal B. Ali,
A. Haroon, A. Essam, I. Zead, A. Nakhlawy, and M. Ismail (NRIAG,
Egypt) report:
We observed GRB 100925A / MAXI J1659-152 (Mangano et al., GCN
11296;Barthelmy et al., GCN 11300; Marshall et al. GCN 11298;
Negoro et al.ATEL 2873) with the Newtonian CCD camera attached to
the 188 cm telescope of Kottamia Astronomical Observatory in Egypt
on September 26 2010. We measured the brightness of this possible
X-ray binary (Ugarte Postigo et al. GCN 11307) in B, V, R and I
bands. Results of the photometry are listed below. We used a
nearby USNO B1.0 star (USNO 0747-0361593) for photometric
calibration.
band START-UT T-EXP[sec] mag.(Vega) error(*)
-------------------------------------------------------------
B 2010-09-26 18:11:24 300.0 16.64 0.08
V($) 2010-09-26 18:17:05 180.0 16.33 0.06
R 2010-09-26 17:59:24 120.0 16.11 0.05
I 2010-09-26 18:01:59 120.0 15.87 0.04
-------------------------------------------------------------
(*) Poisson noise error only.
($) We interpolated the B2 and the R2 magnitudes of the
comparison star to estimate the V band magnitude of the star.
GCN Circular 11307
Subject
GRB100925A/MAXI J1659-152: X-shooter identification as an X-ray binary
Date
2010-09-26T09:25:09Z (15 years ago)
From
Antonio Deugarte at IAA-CSIC <deugarte@iaa.es>
A. de Ugarte Postigo (DARK/NBI), H. Flores (Paris Obs.), K. Wiersema (U.
Leicester), C.C. Thoene (NBIA), J.P.U. Fynbo (DARK/NBI), P. Goldoni
(APC/Univ. Paris 7 and SAp/CEA) report on behalf of the X-shooter GRB
collaboration:
We have observed the optical source related to GRB 100925A/MAXI J1659-152
(Mangano et al. GCN Circ. 11296, Marshall et al. GCN Circ. 11298) using
the X-shooter spectrograph mounted at the Kueyen telescope of ESO's VLT
(Paranal Observatory, Chile). The spectrum consists of a combined exposure
of 2x600s and was started at 23:40 UT on September 25. The spectrum covers
the complete range from 3000 to 24800 angstroms. In a preliminary analysis
we identify broad emission lines from the Balmer series of hydrogen and
HeII as well as CaII and Na I absorption from the ISM of the MW, all at
redshift zero. The emission lines have a width of about 2000 km/s showing
a double peak profile. The spectrum is consistent with that of an X-ray
binary and we hence confirm that GRB 100925A/MAXI J1659-152 is a Galactic
source (Kann GCN Circ. 11299, Negoro et al. ATEL 2873).
We thank the Paranal staff for excellent support, in particular Claudio Melo.
GCN Circular 11306
Subject
GRB100925A/MAXI J1659-152 MITSuME Ishigakijima and Okayama Optical Observation
Date
2010-09-26T08:20:38Z (15 years ago)
From
Daisuke Kuroda at OAO/NAOJ <dikuroda@oao.nao.ac.jp>
D. Kuroda (OAO, NAOJ), H. Hanayama (IAO, NAOJ), K. Yanagisawa, Y. Shimizu,
H. Toda (OAO, NAOJ), S. Nagayama, T. Miyaji, J. Watanabe (NAOJ),
M. Yoshida (Hiroshima), K. Ohta (Kyoto) and N. Kawai(Tokyo Tech) report on
behalf of the MITSuME collaboration:
We observed the field of GRB 100925A / MAXI J1659-152 (Mangano et al.,
GCN 11296; Barthelmy et al., GCN 11300) with the optical three color
(g', Rc and Ic) CCD camera attached to the MITSuME 50cm telescope of
Okayama Astrophysical Observatory and the Murikabushi 1m telescope of
Ishigakijima Astronomical Observatory.
We detected the previously reported source at the UVOT position
(Marshall, GCN 11298) in all the three bands.
Photometric results of the OT are listed below. We used GSC2.3 catalog
for flux calibration.
Okayama Astrophysical Observatory:
The observation started on 2010-09-25 09:58:43 UT (~ 1.9 h after the
trigger).
#T0+[day] MID-UT T-EXP[sec] g' g'_err Rc Rc_err Ic Ic_err
----------------------------------------------------------------------
0.08949 10:13:57 1560.0 17.13 0.06 16.46 0.03 16.45 0.16
0.11081 10:44:39 1500.0 17.08 0.08 16.61 0.04 16.32 0.19
0.13201 11:15:11 1560.0 17.15 0.09 16.46 0.05 15.98 0.15
Ishigakijima Astronomical Observatory:
The observation started on 2010-09-25 10:53:50 UT (~ 2.8 h after the
trigger).
#T0+[day] MID-UT T-EXP[sec] g' g'_err Rc Rc_err Ic Ic_err
----------------------------------------------------------------------
0.12082 10:59:03 480.0 16.97 0.04 16.48 0.02 16.24 0.03
0.12818 11:09:40 540.0 17.05 0.03 16.52 0.02 16.32 0.03
0.13556 11:20:17 540.0 17.02 0.04 16.52 0.02 16.30 0.02
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]
GCN Circular 11305
Subject
GRB 100925A / MAXI J1659-152: SARA-S Observations
Date
2010-09-26T04:03:03Z (15 years ago)
From
Adria C. Updike at Clemson U <aupdike@clemson.edu>
Adria C. Updike and Dieter H. Hartmann (Clemson University) report:
We observed the field of GRB 100925A / MAXI J1659-152 (Mangano et
al., GCN 11296) using the SARA-South 0.6m telescope located at CTIO
beginning 15 hours after the trigger and continuing for 3 hours in the
BVRI Bessel filters under good conditions. We clearly detect the
source (Marshall, GCN 11298) in each image.
Filter Exp Time Magnitude
---------------------------------
B 120s 16.8 +/- 0.1
V 120s 16.3 +/- 0.1
R 120s 16.3 +/- 0.1
I 120s 16.1 +/- 0.1
Magnitudes are given relative to field stars in the USNO B1.0 and
NOMAD catalogs. This message may be cited.
GCN Circular 11304
Subject
GRB 100925A/MAXI J1659-152: Submm observations from APEX
Date
2010-09-26T01:51:55Z (15 years ago)
From
Antonio Deugarte at IAA-CSIC <deugarte@iaa.es>
A. de Ugarte Postigo (Dark/NBI), A. Lundrgren (ESO), F. Wyrowski (MPIfR),
C.C. Thoene (NBIA), A. J. Castro-Tirado, J. Gorosabel, M. Jelinek
(IAA-CSIC) report on behalf of a larger collaboration:
"We observed the field of GRB 100925A/MAXI J1659-152 (Mangano et al. GCNC
11296, Negoro et al. ATel 2873, Barthelmy et al. GCNC 11300), a burst with
possible Galactic origin (Kann GCNC 11299, Xu GCNC 11303), using
LABOCA/APEX at Chajnantor (Chile) in the 870 micrometer band. Observations
began on September 25th at 23:30 UT (15.5 hours after the burst onset). In
a preliminary analysis we detect emission at the position of the optical
afterglow (Marshall et al., GCNC 11298, Jelinek et al., GCNC 11301, De Cia
et al. GCNC 11302) at a flux of 12.6+/-2.4 mJy."
GCN Circular 11303
Subject
GRB100925A/MAXI J1659-152: Galactic origin from SED analysis
Date
2010-09-26T00:44:23Z (15 years ago)
From
Dong Xu at Weizmann Inst <dong@astro.ku.dk>
Dong Xu (Weizmann Institute) reported on a larger collaboration:
GRB100925A happened in the error circle of MAXI J1659-152 (Negoro et
al., ATel 2873; Magano et al., GCN 11296). Spectroscopy or a broadband
SED is critical to pin down its origin. The Swift UVOT and XRT data
were analyzed, covering 2000-1x10^4 s since the BAT trigger.
Generally, UVOT light curves are rather flat as the X-ray does.
The flux densities in the six UVOT filters without Galactic extinction
correction are rather low compared with the X-ray flux density. The
UVW2 flux density is almost comparable to that of the X-ray. Assuming
the source being extragalactic and correction of E(B-V)~0.61 (Magano
et al., GCN 11296) applied, then UVOT flux densities are too high
compared with the downward extrapolation of the X-ray, if interpreted
with synchrotron radiation mechanism. Additionally, the UVOT spectral
index has \beta~2 (F_\nu \propto \nu^\beta) in this case, which is
unusual for GRB afterglows. To make UVOT-XRT SED explained by one
single mechanism, a moderate extinction is required. We found
E(B-V)~0.35 would naturally give rise to a good SED modeling: the
synchrotron radiation lies in the slow cooling phase with the minimum
frequency ~3x10^15 Hz, above which X-ray has \beta_X~-(p-1)/2~0.7
(i.e., p~2.4) and below which UVOT has \beta_opt~1/3. Therefore, we
suggest this source is of Galactic origin.
If the above synchrotron mechanism governs the broadband SED from
radio to X-ray, then MAXI J1659-152 is likely not detectable at radio,
especially when the synchrotron-self absorption frequency is above the
radio band. Therefore, radio follow-up is encouraged.
[GCN OPS NOTE(28sep10): Per auther's request, "100525A" was changed
to "100925A" in both the Subject line and text.]
GCN Circular 11302
Subject
GRB 100925A/MAXI J1659-152 - NOT optical observations
Date
2010-09-26T00:08:46Z (15 years ago)
From
Annalisa De Cia at U of Reykjavik,Science Inst. <annalisa@raunvis.hi.is>
A. De Cia (U. of Iceland), D. Malesani (DARK/NBI), Remy Avila
(UNAM), Graham Cox (NOT), Vik Dhillon (U. of Sheffield), James
Osborn, Richard Wilson (U. of Durham), P.M. Vreeswijk and P.
Jakobsson (U. of Iceland) report on behalf of a larger
collaboration:
We observed the field of GRB 100925A/MAXI J1659-152 (Marshall et
al., GCN 11298, Negoro et al., ATEL 2873) with the Nordic Optical
Telescope (NOT) on La Palma, equipped with StanCam, in poor
weather conditions.
We detect the source reported by Marshall et al., estimating a
magnitude R = 16.4 +/- 0.3 at 21:28 UT (13.4 hours after the BAT
trigger), calibrated against USNO B1 stars.
We thank the Nordic Optical Telescope Scientific Association for
the use of NOT facilities.
GCN Circular 11301
Subject
GRB 100925A / MAXI J1659-152: BOOTES-2/TELMA and IAC80 optical observations
Date
2010-09-25T22:09:39Z (15 years ago)
From
Alberto Castro-Tirado at Inst.de Astro. de Andalucia <ajct@iaa.es>
M. Jel�nek (IAA-CSIC Granada), C. Zurita, M. Vis�s (IAC Tenerife),
P. Papics (Katholieke Universiteit Leuven), P. Kub�nek (IPL, Univ.
de Valencia), L. Sabau-Graziati (INTA), A, de Ugarte Postigo (DARK/NBI),
R. Cunniffe, J. Gorosabel and A. J. Castro-Tirado (IAA-CSIC), report on
behalf of a larger collaboration:
"Following the detection of MAXI J1659-152 (Negoro et al. ATEL
2873) by Swift (GRB 100925A, Magano et al. GCNC 11296), we
have obtained further observations at the position of the
optical counterpart reported by Marshall et al. (GCNC 11298)
with the 0.6m TELMA robotic telescope at the BOOTES-2 station
in M�laga and the 0.8m IAC telescope at Observatorio del Teide
in Tenerife (Spain). TELMA observations started on 25 Sep 20.1
UT in the R-band filter. IAC80 observations were carried out
in BVRI with dense monitoring in the R-band. For a combined
image (120 x 20s) Preliminary analysis yields R = 16.6 +/- 0.1
(based on USNO B-1.0 magnitude for a 15.5 star 1 arcmin north
of the target), thus supporting a Galactic transient (Kann, GCNC 11299),
either a hard outburst of a new compact binary, or a magnetar candidate
similarly to GRB 070610/SWIFT J195509+261406 (Castro-Tirado et
al. 2008, Nat 405, 556; Stefanescu et al. 2008, Nat 405, 503).
Spectroscopic observations are most essential to discern its
nature."
This message can be quoted.
[GCN OPS NOTE(26sep10): Per author's request, the Kann citation
was added and 071006 was changed to 070610.]
GCN Circular 11299
Subject
GRB 100925A: Nearby DSS Source - SN-GRB or new Galactic transient?
Date
2010-09-25T13:55:24Z (15 years ago)
From
Alexander Kann at TLS Tautenburg <kann@tls-tautenburg.de>
D. A. Kann (TLS Tautenburg) speculates:
GRB 100925A (Mangano et al., GCN 11296) is a very peculiar event. It was
an extremely long image trigger (1592 seconds), yet, after slewing to it,
Swift discovered that the X-ray afterglow is still bright. Furthermore,
looking at the Swift XRT repository page (Evans et al. 2007, 2009)
(http://www.swift.ac.uk/xrt_curves/00434928/) the source remains
constantly bright over almost 9000 seconds (two orbits).
Inspection of the DSS images of this field, using the position of the
bright UVOT transient (Marshall, GCN 11298), shows that there is what
seems to be an extended source a few arcseconds to the west (R.A.:
16:59:01.501; Dec.: -15:15:28.76 according to the native DSS WCS system).
It is clearly detected in the red frame, and more marginally in the IR
frame (DSS blue or SDSS are not available for this field). There are also
some stars nearby, but at much larger separation (> 10 arcsec). There is
no source directly beneath the UVOT position.
While the initial properties are reminiscent of two local XRFs associated
with broadlined Type Ic SNe, namely XRF 060218 (Campana et al. 2006) and
XRF 100316D (Starling et al. 2010) (the nearby DSS source being the host
galaxy), the continuing strong X-ray emission as well as the position near
the Galactic bulge (Galactic longitude 5.52, Galactic latitude 16.56) may
also point to a new Galactic source.
Spectroscopic follow-up is encouraged.
This message may be cited.
GCN Circular 11298
Subject
GRB100925A UVOT afterglow
Date
2010-09-25T12:23:06Z (15 years ago)
From
Phil Evans at U of Leicester <pae9@star.le.ac.uk>
F. E. Marshall (NASA/GSFC) reports on behalf of the Swift team:
In response to GRB100925 (Swift/BAT trigger 434928), UVOT took a finding chart
exposure of 150 seconds with the White filter starting 1882 seconds after the
BAT trigger. There is a candidate afterglow in the rapidly available 2.7'x2.7'
sub-image at
RA(J2000) = 16:59:01.68 = 254.75702
DEC(J2000) = -15:15:28.4 = -15.25789
with a 90%-confidence error radius of about 0.61 arc sec.
This position is 11" from the center of the XRT error circle (Mangano et al. GCN
Circ. 11296). The estimated magnitude is 16.83 with a 1-sigma error of about
0.14. No correction has been made for the expected extinction corresponding to
E(B-V) of 0.61.
GCN Circular 11296
Subject
GRB 100925A: Swift detection of a burst
Date
2010-09-25T08:45:18Z (15 years ago)
From
Vanessa Mangano at INAF-IASFPA <vanessa@ifc.inaf.it>
V. Mangano (INAF-IASFPA), E. A. Hoversten (PSU),
C. B. Markwardt (NASA/GSFC), B. Sbarufatti (INAF-OAB/IASFPA),
R. L. C. Starling (U Leicester) and T. N. Ukwatta (GSFC/GWU) report on
behalf of the Swift Team:
At 08:05:05 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 100925A (trigger=434928). Swift slewed immediately to the burst.
The BAT on-board calculated location is RA, Dec 254.736, -15.236 which is
RA(J2000) = 16h 58m 57s
Dec(J2000) = -15d 14' 07"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). This is an image trigger with on-board significance
of 8.1 sigma. As is typical for image triggers, there is no obvious structure
in the raw light curve.
The XRT began observing the field at 08:36:18.0 UT, 1872.2 seconds
after the BAT trigger. XRT found a bright, uncatalogued X-ray source
located at RA, Dec 254.7603, -15.2576 which is equivalent to:
RA(J2000) = 16h 59m 02.47s
Dec(J2000) = -15d 15' 27.3"
with an uncertainty of 5.3 arcseconds (radius, 90% containment). This
location is 115 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 1882 seconds after the BAT trigger. No credible afterglow candidate
has been found in the initial data products. Data from the 2.7'x2.7' sub-image
are not available at this time. The 8'x8' region for the list of sources
generated on-board covers 100% of the XRT error circle. The list of sources is
typically complete to about 18 mag. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.61.
Burst Advocate for this burst is V. Mangano (vanessa 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.)