GRB 060105
GCN Circular 4429
Subject
GRB060105: Swift detection of a bright long burst
Date
2006-01-05T07:56:10Z (19 years ago)
From
David Burrows at PSU/Swift <dxb15@psu.edu>
H. Ziaeepour (UCL-MSSL), A. Blustin (UCL-MSSL), D. Burrows (PSU),
J. Cummings (GSFC/ORAU), N. Gehrels (GSFC), O. Godet (U. Leicester),
J. Kennea (PSU), C. Markwardt (GSFC/UMd), K. Page (U. Leicester), and
D. Palmer (LANL)
on behalf of the Swift team:
At 06:49:28 UT, Swift-BAT triggered and located GRB 060105
(trigger=175942). The spacecraft slewed immediately. The BAT
on-board calculated location is RA,Dec 297.474d, +46.362d
{19h 49m 54s, +46d 21' 45"} (J2000), with an uncertainty of
3 arcmin (radius, 90% containment, stat+sys). The BAT light curve
shows a multi-peaked structure with a total
duration of 60 sec, beginning around T-20s. The peak count
rate is ~20000 counts/sec (15-350 keV), at ~10 seconds after
the trigger.
XRT began observing the field at 06:50:55.3 UT, 87 sec after the BAT
trigger. Onboard centroiding found a bright fading uncatalogued X-ray
source in the field of view at the following coordinates:
RA(J2000): 19h 50m 01.1s
Dec(J2000): +46d 21' 01.0"
We estimate the uncertainty of this position to be 7 arcsec (radius,
90% containment). This uncertainty includes a systematic error of
about 5 arcseconds in the on-board calculated positions due to
the XRT boresight offset. This position is 87 arcsec from the BAT
position above. The initial source flux is 6.8e-9 erg/cm2/sec.
We note that the automated GCN notice identified this as a
probable cosmic ray. The XRT image at the position given above is
definitely a bright celestial source, not a cosmic ray.
UVOT took a finding chart exposure of 200 seconds with the V filter
starting 91 seconds after the BAT trigger. The 2.7'x2.7' sub-image
covers 100% of the XRT error circle. The 8'x8' region for the list
of sources generated on-board covers 100% of the XRT error circle.
No unambiguous afterglow candidate has been found in the initial
data products, although there is a potential low-significance UVOT
counterpart on the edge of the XRT error circle, at
RA=19h 50m 01s DEC=+46d 20m 56s, with a V magnitude of ~19.
The typical 3-sigma upper limit has been about 18th mag.
No correction has been made for the expected visual
extinction of about 0.6 magnitudes. The XRT position is very close
to a bright (B mag ~ 12.8) star.
We are currently in the portion of the orbits where the spacecraft
does not pass over the Malindi downlink station. Therefore, it will
be ~8 hours before we have access to the full data set for the
refined analyses.
GCN Circular 4430
Subject
GRB060105 : Kiso optical observation
Date
2006-01-05T12:33:38Z (19 years ago)
From
Yuji Urata at RIKEN <urata@crab.riken.go.jp>
GRB060105 : Kiso optical observation
H. Izumiura (NAOJ), H. Mito(Tokyo U.), Y. Urata (RIKEN), K.Y. Huang,
W.H. Ip (NCU), Y. Qiu (BAO) on behalf of EAFON report:
" We started R band imaging observation for GRB 060105 (Ziaeepour et
al. # 4429) using Kiso observatory's 1.05-m Schmidt telescope at 09:39
UT (2.82 hour after the burst). There are no new sources down to the
R=20.2 (S/N=3). Since we could not find the UVOT candidate with the
limiting magnitude, the source has potential to be an afterglow of GRB
060105.
Further analysis is in progress."
This message may be cited.
GCN Circular 4431
Subject
GRB060105, optical observation
Date
2006-01-05T14:56:33Z (19 years ago)
From
Shouta Maeno at U.of Miyazaki <shouta@astro.miyazaki-u.ac.jp>
S.Maeno,E.Sonoda,S.Masuda,Y.Nakamura,M.Yamauchi
(University of Miyazaki)
"We have observed the field covering the error circle of
GRB 060105 (GCN 4429) with the unfiltered CCD camera on
the 30-cm telescope at University of Miyazaki.
The observation was started 09:13:18 UT on Jan.05.
After co-adding a set of 15 images (09:13:18 - 09:31:05 UT)
of 30 sec exposures, we have compared with the USNO A2.0 catalog.
Preliminary analysis shows there is no new source brighter
than 16.1mag."
GCN Circular 4432
Subject
GRB060105: Suzaku-XIS and -HXD observation plan
Date
2006-01-05T15:02:18Z (19 years ago)
From
Kazutaka Yamaoka at Aoyama Gakuin U <yamaoka@phys.aoyama.ac.jp>
Kazuhisa Mitsuda on behalf of Suzaku team
We started observation of GRB 060105 (GCN 4429: H. Ziaeepour et
al.) at location (RA=19h 50m 01s, DEC=+46d 21' 01", J2000), with the
Suzaku narrow field instruments (the XIS and HXD).
It started around 12:10 UT, on January 05, 2006, and
will continue until 12:00 UT January 06, 2006.
GCN Circular 4433
Subject
GRB 060105: XRT refined analysis
Date
2006-01-05T18:51:52Z (19 years ago)
From
Olivier Godet at U.of Leicester <og19@star.le.ac.uk>
O. Godet, K. Page, A. Bearmore, J. Osborne (U. Leicester), D. N. Burrows
(PSU), D. Grupe (PSU), H. Ziaeepour (UCL-MSSL), P. Boyd (GSFC-UMBC), L.
Angelini (GSFC-JHU) report on behalf of the Swift XRT team:
We analyzed the first 5 orbits of XRT data from GRB 060105. A 10.2ks
photon counting (PC) mode image provides a refined XRT position:
RA(J2000) = 19h 50m 00.6s
Dec(J2000) = +46d 20' 58.3''
with an uncertainty of 3.2 arcsecs (90% containment). This position is
4.5 arcsecs away from the on-board XRT position quoted in Ziaeepour et
al. (GCN 4429) and includes the latest XRT boresight correction. This
position is 83 arcseconds from the BAT position (Ziaeepour et al., GCN
4429).
The X-ray light curve can be fit with a double broken power-law with an
initial decay slope of alpha1 = -1.16+/-0.14, a break at t1-T = 196 +
23/-29s, and a shallower post-break slope of alpha2 = -0.80+/-0.02,
followed by another break at t2-T = 3306+/-200s and a steeper decay
slope of alpha3 = -2.30+/-0.08.
An absorbed power-law fit of the WT data (first orbit) from T+187s to
T+1287s gave a photon index of 2.06+/-0.03 and an excess absorption
value of (2.4+/-0.2)e21 cm**-2. The error bars are given at a 90%
confidence level. The Galactic hydrogen column density in the direction
of the burst is 1.8e21 cm**-2. The spectrum of the PC data (4 orbits)
can be fit by an absorbed power-law with Gamma=2.17+/-0.16 and excess
absorption of (2.8+/-0.8)e21 cm**-2.
If the burst continues decaying at the current rate (alpha3) we estimate
an XRT count rate of 0.0029 counts/s at T + 24hr, which corresponds to
an observed 0.5-10.keV flux of 6.26e-13 ergs cm**-2 s**-1 and an
unabsorbed flux of 9.82e-13 ergs cm**-2 s**-1.
GCN Circular 4435
Subject
GRB 060105: BAT refined analysis
Date
2006-01-05T20:45:09Z (19 years ago)
From
Hans Krimm at NASA-GSFC <krimm@milkyway.gsfc.nasa.gov>
C. Markwardt (GSFC/UMD), L. Angelini (GSFC/JHU), L. Barbier (GSFC),
S. Barthelmy (GSFC), J. Cummings (GSFC/ORAU), E. Fenimore (LANL),
N. Gehrels (GSFC), J. Greiner (MPE), D. Hullinger (UMD),
H. Krimm (GSFC/USRA), D. Palmer (LANL), A. Parsons (GSFC),
T. Sakamoto (GSFC/NRC), G. Sato (ISAS), J. Tueller (GSFC),
on behalf of the Swift-BAT team:
Using the data set from T-120 to T+300 sec from the recent
telemetry downlink, we report further analysis of BAT GRB 060105
(trigger #175942) (Ziaeepour, et al., GCN 4429). The BAT ground-
calculated position is
(RA,Dec) = 297.488, 46.359 {19h 49m 57.1s, 46d 21' 32.4"} [deg; J2000]
+- 0.9 arcmin, (radius, sys+stat, 90% containment). This is 36 arcsec
from the BAT onboard position and 52 arcsec from the Swift XRT onboard
position (Ziaeepour et al, GCN #4429). The partial coding was 28.5%.
The BAT mask-weighted light curve has 3 main peaks, each with multiple
sub-peaks, an overall flat-topped shape, and similar spectra. The
first is T-22 to T-15 sec, the second from T-3 to T+11 sec, and the
third from T+23 to T+36 sec. There is softer, weaker emission in the
15-50 keV band out to at least T+150. T90 (15-350 keV) is (55 +- 5)
sec (estimated error including systematics).
The power law index of the time-averaged spectrum is 1.11 +- 0.03.
The fluence in the 15-150 keV band is (1.82 +- 0.04) x 10^-05 erg/cm2.
The 1-sec peak photon flux measured from T+30.42 sec in the 15-150 keV
band is (7.5 +- 0.4) ph/cm2/sec. All the quoted errors are at the 90%
confidence level. This GRB is among the brightest bursts seen by BAT.
GCN Circular 4436
Subject
GRB 060105: Mitsume optical observations
Date
2006-01-05T21:33:51Z (19 years ago)
From
Nobuyuki Kawai at Tokyo Tech <nkawai@hp.phys.titech.ac.jp>
K. Yanagisawa (OAO/NAOJ), Y. Yatsu, and N. Kawai (Tokyo Tech) report
on behalf of the Mitsume collaboration:
"We have observed the field of GRB 060105 (Ziaeepour et al. GCN 4429)
with the three-color Mitsume 50 cm telescopes at Okayama and Akeno,
Japan starting at 9:14 UT (2.4 hours after the burst).
The summary of the observations is following:
Telescope bands time (UT) exposure
--------- ---------- ---------------- ------------
Okayama g', Rc, Ic 09:14 - 09:41 UT 60 s x 20
Akeno V, Rc, Ic 09:32 - 11:20 UT 30 s x 158
--------- ---------- ---------------- ------------
Comparison with the DSS-2R image does not reveal an OT at the position
of the XRT error circle.
The 10-sigma upper limit magnitudes for the Okayama images are
g': 17.1
Rc: 17.3
Ic: 17.5
The images obtained at Okayama can be viewed at
http://bragi.oao.nao.ac.jp/support/telescope/grb50/images/GRB060105A.pdf."
GCN Circular 4437
Subject
GRB 060105: Swift/UVOT upper limits
Date
2006-01-05T23:31:06Z (19 years ago)
From
Patricia Schady at MSSL/Swift <ps@mssl.ucl.ac.uk>
P. Schady (UCL-MSSL/PSU), M. Page (UCL-MSSL), A. Cucchiara (PSU),
F. Marshall (GSFC), N. Gehrels (GSFC) on behalf of the Swift/UVOT
team report:
The Swift/UVOT began observing the field of GRB 060105 at 06:50:59
UT on 2006-01-05, 91 s after the BAT trigger (Ziaeepour et al., GCN
4429). No source was observed in any of the UVOT filters at the XRT position
and the potential candidate mentioned in GCN 4429 is most likely contamination
from a bright, nearby star. The 3-sigma upper limits in summed images from each
of the filters are listed below (not corrected for extinction; E(B-V) = 0.171).
Filter T_range(s) Exp(s) 3sigUL(mag)
V 91-29544 29453 20.4
B 457-5533 5076 20.1
U 403-23780 23377 20.8
W1 349-22873 22524 20.3
M2 295-30329 30034 20.6
W2 565-28638 28073 21.0
White 511-889 378 19.9
_______________________________________________
Uvot_cal mailing list
Uvot_cal@phoenix.astro.psu.edu
https://phoenix.astro.psu.edu/mailman/listinfo/uvot_cal
GCN Circular 4438
Subject
GRB 060105: ISAS observations and near IR upper limit
Date
2006-01-06T03:16:15Z (19 years ago)
From
Daisuke Yonetoku at Kanazawa U <yonetoku@astro.s.kanazawa-u.ac.jp>
D. Yonetoku, T. Murakami, H. Kodaira, S. Okuno, S. Yoshinari,
T. Kidamura (Kanazawa Univ.) and Y. Kobayashi (NAOJ)
on behalf of the Kanazawa team report:
We have observed the field of GRB 060105 (Ziaeepour et al. GCN #4429)
with J, H, Ks-bands using the 1.3m telescope on the roof top of
ISAS, Japan. The observation was started at 08:37 UT (1.8 hours after
the burst) in poor condition and low elevation.
Comparison with the 2MASS catalogue does not reveal any new source
within the position of the XRT error circle. The 5-sigma upper limit
magnitudes are Ks: 13.8, H: 14.2, J: 15.7, respectively.
GCN Circular 4439
Subject
Konus-Wind observation of GRB 060105
Date
2006-01-06T13:10:21Z (19 years ago)
From
Valentin Pal'shin at Ioffe Inst <val@mail.ioffe.ru>
S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, and
T. Cline on behalf of the Konus-Wind team report:
The GRB 060105 (Swift-BAT trigger #175942;
Ziaeepour et al., GCN 4429; Markwardt et al., GCN 4435)
triggered Konus-Wind at T0=24544.371 s UT (06:49:04.371).
The Konus-Wind light curve consists of three main
multipeaked pulses with a total duration of ~60 sec.
As observed by Konus-Wind the burst had
a fluence of 7.86(-0.37,+0.19)x10^-5 erg/cm2 and
peak flux on 256 msec time scale 6.55(-0.45,+0.19)x10^-6 erg/cm2/sec
(both in the 20 keV - 2 MeV energy range).
The time-integrated spectrum of the GRB (from T0 to T0+58.880 sec)
is well fitted (in the 20 keV - 2 MeV range)
by a power law with exponential cutoff model:
dN/dE ~ E^(-alpha) * exp(-E*(2-alpha)/Ep)
with alpha = 0.827(-0.044,+0.042)
and Ep = 424(-22, +25) keV (chi2 = 63/62dof).
It can also be fitted by GRBM (Band) model for which:
the low-energy photon index is alpha = -0.790 (-0.052,+0.067),
the high energy photon index beta = -2.70(-0.73, +0.35),
the break energy E0 = 327 (-46, +40) keV (chi2 = 58/61dof).
The spectrum integrated over the most intense part of the GRB
(from T0+16.64 to T0+29.184 sec) is well fitted
(in the 20 keV - 2 MeV range)
by a power law with exponential cutoff model:
dN/dE ~ E^(-alpha) * exp(-E*(2-alpha)/Ep)
with alpha = 0.571(-0.060,+0.057)
and Ep = 549(-31, +34) keV (chi2 = 73/62dof).
All the quoted errors are at the 90% confidence level.
GCN Circular 4440
Subject
GRB 060105: MDM Observation
Date
2006-01-06T13:18:06Z (19 years ago)
From
Jules Halpern at Columbia U. <jules@astro.columbia.edu>
N. Zimmerman, S. Tyagi, & J. P. Halpern (Columbia U.) report:
"Using the MDM 2.4m outfitted with RETROCAM, we have obtained an upper
limit on the SDSS r-band magnitude of GRB 060105 as of Jan. 6 02:00 UT, or
19 hours after the burst. The sum of eight 5-minute exposures reveals no
new source within the refined XRT error circle (Godet et al,. GCN 4433) to
a limit of r = 21.0, as calibrated with Sloan standard stars."
GCN Circular 4441
Subject
GRB 060105: Radio observations
Date
2006-01-06T15:40:31Z (19 years ago)
From
Dale A. Frail at NRAO <dfrail@nrao.edu>
Dale A. Frail (NRAO) reports on behalf of a larger collaboration:
"We used the Very Large Array to observe the Swift burst GRB060105
(GCN 4435; GCN 4429) at a frequency of 8.46 GHz on 2006 January 6.10
UT. No radio emission is detected within the XRT error circle (GCN
4433) with a peak flux density of 49 +/- 47 uJy.
No further observations are planned.
The National Radio Astronomy Observatory is a facility of the National
Science Foundation operated under cooperative agreement by Associated
Universities, Inc."
GCN Circular 4442
Subject
GRB 060105: pseudo-z from spectral parameters of the prompt emission
Date
2006-01-06T17:02:38Z (19 years ago)
From
Jean-Luc Atteia at Lab d Astrophys.,OMP,Toulouse <atteia@ast.obs-mip.fr>
A. Pelangeon & J-L. Atteia (LATT-OMP) report:
We have used the spectral parameters of the most intense part
of GRB 060105 provided by Golenetskii et al. (GCNC 4439) to
compute the spectral pseudo-redshift of this GRB, assuming that
the most intense part of the burst contains half of the total fluence.
We find a pseudo-redshift pz= 4.0 +/- 1.3
GCN Circular 4449
Subject
GRB 060105: quick look analysis of the Suzaku/XIS afterglow observation
Date
2006-01-09T01:40:38Z (19 years ago)
From
Makoto Tashiro at Saitama U/Swift <tashiro@phy.saitama-u.ac.jp>
K. Mitsuda, R. Fujimoto, T. Inui, T. Murakami and the
Suzaku GRB-ToO team reports:
The Suzaku narrow field instruments: XIS and HXD started observation
of GRB060105 from 12:10 UT on 2006-01-05 (Mitsuda et al. GCN 4432),
at 5.4 hours after the Swift BAT detection (Ziaeepour et al. GCN 4429).
Preliminary analysis shows a fading X-ray source at the reported XRT
position (Godet et al. GCN4433). The intensity decreased to 1/3 of
the initial at the end of observation, 12:00 UT on 2006-01-06.
The averaged flux during the observation is approximately
7x10^-13 erg/s/cm2 (2-10 keV). Detail analysis is in progress.
GCN Circular 4606
Subject
GRB060105: refined analysis of the Suzaku observation
Date
2006-01-27T14:52:24Z (19 years ago)
From
Kazuhiro Nakazawa at ISAS/JAXA <nakazawa@astro.isas.jaxa.jp>
K. Nakazawa (ISAS/JAXA), K. Yamaoka , Y. Nakagawa (AGU),
M. Yamauchi, E. Sonoda, S. Maeno (Univ. of Miyazaki),
T. Murakami, D. Yonetoku (Kanazawa U.),
M. Tashiro, K. Abe, K. Onda (Saitama U.),
N. Ishikawa, A. Yoshida (AGU),
N. Yamasaki, Y. Terashima, H. Murakami (ISAS/JAXA),
K. Torii (Osaka U.), Y. Ichikawa, S. Murasawa,
R. Fujimoto (ISAS/JAXA), Tatsuya Inui (Kyoto U.),
on behalf of Suzaku GRB ToO team report:
We have carried out refined analysis on the data from the Suzaku
TOO observation of GRB060105 (Ziaeepour et al. GCN4429).
The Suzaku observation started on 2006,
January 5 at 12:10 UT, 5 hours 20 minutes after the GRB,
and ended on January 6, at 12:00 UT.
A good exposure of 35 ks was obtained in total.
As reported by Mitsuda et al (GCN4449), the afterglow of
GRB060105 is clearly detected in the XIS images and
its position is fully consistent with the refined Swift/XRT one
(Godet et al., GCN4433).
Suzaku XIS spectra ranging 0.5-8 keV are well described
with an absorbed power law model. The derived best fit photon
index and column density are Gamma = 2.1+/- 0.1 and
NH = (3.0 +/- 0.6) x 10^21 cm^-2, respectively.
No signature of spectral variability is detected during the observation.
The flux fades along the Suzaku observation
from (1.9 +/- 0.3) x 10^-12 erg/s/cm2 (T_burst + 5.7-7.0 hours)
to (1.5 +/- 0.5) x 10^-13 erg/s/cm2 (T_burst + 26-28 hours)
in the 2-10 keV energy band. Decay index was found to be -1.3 +/- 0.2.
Note that a possible 10% systematic calibration error is not included
in the errors quoted above.
These results are generally consistent with those obtained by analyzing
the Swift/XRT data.
GCN Circular 4754
Subject
GRB060105: optical observations
Date
2006-02-13T15:07:19Z (19 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
D. Sharapov (MAO, and NOT La Palma), M. Ibrahimov, (MAO), A. Pozanenko
(IKI) and V. Rumyantsev (CrAO) on behalf of larger GRB follow up
collaboration report:
We observed error box of GRB060105 (Ziaeepour et al., GCN 4429) with 1.5m
telescope of Maidanak Astronomical Observatory in R-band on Jan. 06 between
(UT) XX and YY. Within refined XRT error circle (Godet et al., GCN 4433) we
do not detect new optical objects. Limiting magnitude is based on USNO B1.0
is following:
Obs. time, Exp., Mag.(UL), Seeing
(UT) (s)
Jan. 06 13:35-13:57 7x180 20.8 ~2.3"
GCN Circular 5278
Subject
GRB 060105: Upper limit on Host Galaxy
Date
2006-06-27T18:49:53Z (19 years ago)
From
Alexander Kann at TLS Tautenburg <kann@tls-tautenburg.de>
D. A. Kann (Thueringer Landessternwarte Tautenburg) and S. Manohar (USC,
Los Angeles), report:
We observed the field of GRB 060105 (Ziaeepour et al., GCN 4429) with the
Tautenburg 1.34m Schmidt telescope under good observing conditions. We
obtained 6 x 600 sec images in the Rc filter for a total integration time
of 60 minutes. The mean observation time was June 27.9288 UT, which is
172.7 days after the burst. We determine the zero point of the image in
comparison with nine unsaturated and isolated stars of the USNOB1.0
catalog. Astrometry is also performed against the USNOB1.0 catalog.
At the refined position of the X-ray afterglow (Godet et al., GCN 4433),
we do not detect any sources. The 2 sigma limiting magnitude of the image
is Rc=23, but the position of the afterglow is affected by the PSF of
several nearby bright stars. We set a limiting magnitude of Rc=22.5 for
any source at this position. This magnitude is not corrected for the
moderate foreground extinction, E(B-V)=0.171.
This message may be cited.