# GCN_circulars

GRB_name: GRB150702A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  1454
SUBJECT: IPN triangulation of GRB150702
DATE:    02/07/17 16:06:36 GMT
FROM:    Kevin Hurley at UCBerkeley/SSL  <khurley@sunspot.ssl.berkeley.edu>

K. Hurley and T. Cline, on behalf of the Ulysses, Mars Odyssey, 
and Konus-Wind GRB teams,

I. Mitrofanov, D. Anfimov, A. Kozyrev, M. Litvak and A. Sanin,  
on behalf of the HEND/Odyssey GRB team,

W. Boynton, C. Fellows, K. Harshman, C. Shinohara and R. Starr,
on behalf of the GRS/Odyssey GRB team, and

E. Mazets and S. Golenetskii, on behalf of the Konus-Wind GRB team, 
report:

Ulysses, Konus-Wind, and MO-HEND observed this burst at 69663 s.

As observed by Ulysses, it had a duration of approximately  10
seconds, a 25-100 keV fluence of approximately  1.3E-05 erg/cm2, and a
peak flux of approximately  3.0E-06 erg/cm2 s over 0.25 seconds.

We have triangulated it to two alternate preliminary 3 sigma error boxes whose
approximate areas are 140 sq. arcmin. each and whose coordinates are:

    RA(2000)                              DEC(2000)
 ERROR BOX CENTER:  13 h 50 m 12.66 s     61 o 50 '  43.79 " 
 ERROR BOX CORNER 1: 13 h 50 m 25.94 s     62 o 13 '  54.09 " 
 ERROR BOX CORNER 2: 13 h 50 m 25.32 s     61 o 29 '  58.72 " 
 ERROR BOX CORNER 3: 13 h 49 m 57.94 s     62 o 10 '  25.39 " 
 ERROR BOX CORNER 4: 13 h 49 m 57.26 s     61 o 25 '  42.46 " 

OR

 ERROR BOX CENTER:  13 h 44 m 44.28 s      54 o 40 ' 41.39 "
 ERROR BOX CORNER 5: 13 h 44 m 23.07 s      54 o 17 '  40.27 "  
 ERROR BOX CORNER 6: 13 h 45 m 23.41 s      55 o 00 '  43.10 "   
 ERROR BOX CORNER 7: 13 h 44 m 05.82 s      54 o 21 '  43.49 "  
 ERROR BOX CORNER 8: 13 h 45 m 06.47 s      55 o 05 '  34.50 " 

These error boxes may be improved considerably, and we are seeking
auxiliary data which may allow us to distinguish between these two
possibilities.  Maps will be posted shortly at
sunspot.ssl.berkeley.edu/ipn3/020715.


GRB_name: GRB200618A
Detection_method: Optical
Circular_text:
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  4836
SUBJECT: GRB200618: optical polarimetry and photometry
DATE:    06/02/26 15:25:13 GMT
FROM:    Valeri Larionov at NIAI SpBU  <vlar@crao.crimea.ua>

V. Larionov and L.Larionova from St.Petersburg University (Russia)
<vml@VL1104.spb.edu>, <vlar@nm.ru> report:

We imaged GRB20060218 with 70-cm telescope of Crimean Astrophysical
observatory (Ukraine) and ST-7 camera of St.Petersburg University
in photometric and polarimetric mode. Observations were made in R band from 
February 20.17 to February 23.18. The rate of brightening in this period was 
0.18 mag/day. The polarization reached maximum of 6% on February 21
and decreased to 3% on February 23. The positional angle remained 
practically unchanged, 110+\-5 deg. The high and variable polarization
gives evidence of strongly aspherical or non-thermal component in
GRB20060218/SN2006aj radiation.

This message is citeable.


GRB_name: GRB120706A
Detection_method: Optical
Circular_text:
TITLE:   GCN GRB OBSERVATION REPORT
NUMBER:  5302
SUBJECT: GRB120706: MASTER optical observation  
DATE:    06/07/12 21:56:37 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

V. Lipunov, V.Kornilov, D.Kuvshinov, N.Tyurina, A.Belinski, E.Gorbovskoy,
A.Krylov, G.Borisov, A.Sankovich, M.Sinitsin, P.Gritsyk

Sternberg Astronomical Institute, Moscow Union 'Optic'
MASTER  robotic system (http://observ.pereplet.ru) responded to GRBGRB120706 
(GRB_TIME is 2006-03-19 21:07:43.71) at high zenit distance jn the west 
at white night.

The first R image was at 2006-07-12 21:10:32 UT, 72 s after 
notice time and   212 s after the GRB time

The robot not find OT-candidate in error box brighter then  14.5 (s/n=3).

The reduction is continuing.
This work is supported by RFFI  04-02-16411 grant.
This message can be cited.
Mailto: lipunov@sai.msu.ru


GRB_name: GRB080120A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7194
SUBJECT: GRB 080120: a long GRB detected by INTEGRAL
DATE:    08/01/20 18:51:53 GMT
FROM:    Sandro Mereghetti at IASF/CNR  <sandro@iasf-milano.inaf.it>

S.Mereghetti, A.Paizis (IASF-Milano), D.Gotz (CEA-Saclay), A.Manousakis, 
V.Beckmann, M. Beck (ISDC, Versoix), and J. Borkowski (CAMK, Torun) 
on behalf of the IBAS Localization Team report:

A  GRB lasting about 20 s has been detected by IBAS in IBIS/ISGRI 
data at  17:28:30 UT of January 20.
The coordinates (J2000)  are:

RA = 225.2547
Dec= -10.8854

with an uncertainty of 2 arcmin (90% c.l.).

A preliminary analysis gives a peak flux in the 20-200 keV range of about 
3 ph/cmq/s (1-s integration time) and a fluence over the same energy range 
of 1.5e-6 erg/cmq.

A plot of the light curve will be posted at

http://ibas.iasf-milano.inaf.it/IBAS_Results.html

This message can be cited.


GRB_name: GRB080120A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7195
SUBJECT: GRB080120: Swift XRT position
DATE:    08/01/20 23:24:55 GMT
FROM:    Boris Sbarufatti at INAF-IASF-Pa  <sbarufatti@ifc.inaf.it>

B. Sbarufatti and V. Mangano (INAF-IASF PA) on behalf
of the Swift XRT team

Swift XRT started a ToO observation of the INTEGRAL burst
GRB080120 at 19:47 UT. The analysis of the initial 1.5 ks
of data of the first orbit shows a single bright uncatologued
X-ray source in the field at

  RA (J2000):  15h 01m 03.13s
Dec (J2000): -10d 52' 31.8"

with an uncertainty of 3.8 arcsec (radius, 90% confidence). This is
46 arcsec away from the GRB position given in Mereghetti et al., GCN
Circ. 7194. The source has a count rate of (2.1+-0.1)E-1 counts/s
and, assuming a Crab spectrum, a flux of 1E-10 erg/cm2/s. More
data are being collected that will be used to determine whether the
source is fading and to perform a spectral analysis.

This Circular is an official product of the Swift XRT Team.


GRB_name: GRB080120A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7196
SUBJECT: GRB 080120 : Planned XMM-Newton observation
DATE:    08/01/20 23:52:53 GMT
FROM:    Norbert Schartel at XMM-Newton/ESA  <too@xmm.vilspa.esa.es>

XMM-Newton will observe GRB 080120 at location
(RA=15h 01m 1.13s, DEC=-10 d 53' 7.4", J2000),
starting at 23:00:00 UT, on Jan 20, 2008,
for an exposure of about 20000 seconds.


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GRB_name: GRB080120A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7197
SUBJECT: GRB 080120: GROND detection
DATE:    08/01/21 08:13:12 GMT
FROM:    Jochen Greiner at MPI  <jcg@mpe.mpg.de>

T. Kruehler, J. Greiner, S. McBreen, S. Loew, A. Kuepcue-Yoldas, A. Yoldas 
(all MPE Garching) report for the GROND team:

We started observing GRB 080120 observed by INTEGRAL (Mereghetti et al. 2008,
GCN #7194) simultaneously in grizJHK with GROND, mounted at the 2.2m MPI/ESO 
telescope at La Silla (Chile), at 7:02 UT, about 13.5 hrs after the GRB. 
At this time, the GRB location was becoming visible at 20 degrees 
above horizon.

We find an optical/NIR source inside the 3.8 arcsec Swift/XRT error circle 
of the X-ray afterglow (Sbarufatti et al. 2008, GCN #7195). The object is
seen in all bands except K, implying a redshift smaller than 3.5.

The coordinates are (+-1 arcsec):
RA (2000.0) = 15h 01m 03.2s
Decl (2000.0) = -10d 52' 30"

We estimate rough magnitudes of g'=21.1, r'=20.5, i'=20.0, z'=19.8,
J=19.6, H=19.4, K>18.9, calibrated against USNO and 2MASS stars. 
Given the high airmass and humidity, these estimates may have large errors.

No statement about variability can be made at this point. Observations are 
continuing.


GRB_name: GRB080120A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7198
SUBJECT: UVOT detection of GRB080120
DATE:    08/01/21 11:50:51 GMT
FROM:    Patricia Schady at MSSL/Swift  <ps@mssl.ucl.ac.uk>

P. Schady (MSSL-UCL) and B. Sbarufatti (INAF-IASF PA) report on behalf of 
the Swift UVOT team:

Swift UVOT started a ToO observation of the INTEGRAL burst GRB080120 at 
2008-01-20T19:50 UT, ~2.4hrs after the INTEGRAL trigger (Mereghetti et 
al., GCN 7194). Observations were taken in the white and v-band only. A 
new source is detected within the XRT error circle (Sbarufatti & Mangano, 
GCN7195), in co-added images in both these filters at

RA: 15:01:03.276
DEC: -10:52:29.79

with an uncertainty of 0.6 arcsec (90% confidence). This is consistent 
with the position reported by Kruehler et al. (GCN 7197). The source is 
seen to decay in the white band and has the following magnitudes and 
3-sigma upper limits (in the UVOT photometric system,Breeveld et al., GCN 
Circ. 6614)

Filter    Tstart   Exp      Magnitude
            (s)     (s)
white     9257     401      21.45 +/- 0.39
white     14524    679      > 22.08
v         8490     746      20.45 +/- 0.41
v         13232    126      20.53 +/- 0.33

The values quoted above are not corrected for the expected non-negligible 
Galactic extinction corresponding to a reddening of E(B-V) = 0.10 mag in the 
direction of the burst (Schlegel et al. 1998).


GRB_name: GRB080120A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7199
SUBJECT: GRB 080120: Swift-XRT refined analysis
DATE:    08/01/21 14:14:40 GMT
FROM:    Boris Sbarufatti at INAF-IASF-Pa  <sbarufatti@ifc.inaf.it>

B. Sbarufatti, V. Mangano (INAF-IASF PA)
report on behalf of the Swift-XRT team:

We have analyzed the 3.9 ks of data of the ToO observation of GRB  
080120,
started on Jan 20 at 19:47 UT. The refined position of the X-ray  
source is

  Ra (J2000):  15h 01m 03.14s
Dec (J2000): -10d 52' 30.7"

with an uncertainty of 3.7 arcsec (radius, 90% confidence). This is
1.1 arcsec away from the first XRT position given in
Sbarufatti & Mangano (GCN Circ. 7195), 47.2 arcsec from
the initial INTEGRAL position of Mereghetti et al.  (GCN Circ. 7194),
and 2.2 arcsec from the  optical counterparts reported by Kruehler et  
al.
(GCN Circ, 7197) and by Schady & Sbarufatti (GCN Circ. 7198).

The light curve shows an initial flare between 8 and 9 ks from the
trigger, followed by a very steep decay (slope 2.9 +/- 0.4).
At this decay rate the source will be at a level of 3E-4 counts/s today
at 17:30 UT.

The average spectrum can be modeled by an absorbed powerlaw with
photon index 2.5 +/- 0.3 with a column density of (1.5 +/- 0.6)E21  
cm^-2,
sligthly in excess with respect to the Galactic value (7.7E20 cm^-2).
The observed (unabsorbed) 0.3-10 keV flux is
4.7E-12 (8.2E-12) ergs cm^-2 s^-1.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB080120A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7200
SUBJECT: VLA radio upper limit on GRB 080120
DATE:    08/01/21 19:57:53 GMT
FROM:    Poonam Chandra at U Virginia/NRAO  <pc8s@virginia.edu>

Poonam Chandra (NRAO/UVA) and Dale A. Frail (NRAO) report on
behalf of the Caltech-NRAO-Carnegie GRB Collaboration:


"We used the Very Large Array to observe the field of view toward GRB
080120 (GCN 7194) at a frequency of 8.46 GHz on 2008 January 8th at 
21.72 UT.
The GRB is undetected and the 2-sigma upper limit on the peak radio flux 
at the
SWIFT-XRT position (GCN 7199) is 100 uJy (rms 50 uJy).

 
The National Radio Astronomy Observatory is a facility of the National
Science Foundation operated under cooperative agreement by Associated
Universities, Inc."


GRB_name: GRB080120A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7202
SUBJECT: GRB 080120: GROND confirmation of the optical afterglow
DATE:    08/01/22 09:10:16 GMT
FROM:    Thomas Kruehler at MPE/MPI  <kruehler@mpe.mpg.de>

T. Kruehler, J. Greiner, S. McBreen, S. Loew, A. Kuepcue-Yoldas, C. Clemens, A. Yoldas 
(all MPE Garching) report on behalf of the GROND team:

We observed the field of the INTEGRAL burst GRB 080120 (Mereghetti et al. 2008, GCN #7194) with the 2.2 m MPI/ESO telescope equipped with the multi-channel imager GROND. 
Observations started at 07:04 UTC on the 22nd of January at an airmass of 2.5 and seeing around 1.0". 

The optical/NIR source (Kruehler et al. 2008, GCN #7197, P. Schady et al. 2008, GCN #7198) inside the XRT-error circle (Sbarufatti et al. 2008, GCN #7195) is still detected, and clearly fading. Fitting a power-law to the two epochs yields a slope around 1.5.

A finding chart will be posted at: www.mpe.mpg.de/~jcg/grb080120.html


GRB_name: GRB080123A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7203
SUBJECT: GRB 080123: Swift detection of a short burst
DATE:    08/01/23 04:43:57 GMT
FROM:    Jamie A. Kennea at PSU/Swift-XRT  <kennea@astro.psu.edu>

T. N. Ukwatta (GSFC/GWU), W. H. Baumgartner (GSFC/UMBC),
M. M. Chester (PSU), N. Gehrels (NASA/GSFC),
S. T. Holland (CRESST/USRA/GSFC), E. A. Hoversten (PSU),
S. Immler (CRESST/GSFC/UMD), J. A. Kennea (PSU),
V. Mangano (INAF-IASFPA), F. E. Marshall (NASA/GSFC),
D. M. Palmer (LANL), T. Sakamoto (NASA/UMBC),
B. Sbarufatti (INAF-IASFPA) and D. E. Vanden Berk (PSU) report on
behalf of the Swift Team:

At 04:21:57 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 080123 (trigger=301578).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 338.929, -64.890 which is 
   RA(J2000) = 22h 35m 43s
   Dec(J2000) = -64d 53' 23"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a double-peaked
structure with a duration of about 0.5 sec.  The peak count rate
was ~6000 counts/sec (15-350 keV), at ~0.1 sec after the trigger. 

The XRT began observing the field at 04:23:38 UT, 102 seconds after the
BAT trigger. Using prompt downlinked data, we find a bright, fading X-ray 
source located at RA, Dec 338.9446, -64.9011 which is
  RA(J2000)  = 22h 35m 46.71s
  Dec(J2000) = -64d 54' 04.0"
with an uncertainty of 1.6 arcsec (radius, 90% containment). 
This location is 46 arcseconds from the BAT on-board position,
outside the BAT error circle. 

UVOT took a finding chart exposure of nominal 100 seconds with the
White (160-650 nm) filter starting 111 seconds after the BAT trigger. 
No afterglow candidate has been found in the initial data products. 
Image catalog data are not available at this time. The 8'x8' region
for the list of sources generated on-board covers 100% of the BAT
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 0.03. 

Burst Advocate for this burst is T. N. Ukwatta (tilan.ukwatta AT gmail.com). 
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.)


GRB_name: GRB080123A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7204
SUBJECT: GRB 080123: Enhanced Swift-XRT position
DATE:    08/01/23 10:46:03 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

J.P. Osborne, A.P. Beardmore, P.A. Evans and M.R. Goad (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 390 s of overlapping XRT Photon Counting mode and UVOT
V-band data for GRB 080123, 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 = 338.94226, -64.90090 which is equivalent
to:

RA (J2000): 22h 35m 46.1s
Dec (J2000): -64d 54' 3.24"

with an uncertainty of 2.1 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, astro-ph/0708.0986
http://www.swift.ac.uk/xrt_positions/Goad.pdf).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB080123A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7205
SUBJECT: GRB 080123, Swift-BAT refined analysis
DATE:    08/01/23 14:54:48 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

J. Tueller (GSFC), S. D. Barthelmy (GSFC), J. Cummings (GSFC/UMBC),
E. Fenimore (LANL), N. Gehrels (GSFC), H. Krimm (GSFC/USRA),
C. Markwardt (GSFC/UMD), D. Palmer (LANL), T. Sakamoto (GSFC/UMBC),
G. Sato (GSFC/ISAS), M. Stamatikos (GSFC/ORAU), T. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using the data set from T-240 to T+962 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 080123 (trigger #301578)
(Ukwatta, et al., GCN Circ. 7203).  The BAT ground-calculated position is
RA, Dec = 338.974, -64.930 deg which is 
   RA(J2000)  =  22h 35m 53.8s 
   Dec(J2000) = -64d 55' 48" 
with an uncertainty of 4.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 20%.
 
The mask-weighted light curve shows two well-separated peaks.  The first
starts at ~T+0.3 sec and is no wider than 64 msec.  The second peak
starts at ~T+0.6 sec with a FRED-like shape and a duration of ~256 msec.
There is soft extended emission lasting ~120 sec.  T90 (15-350 keV) is
115 +- 30 sec (estimated error including systematics).
 
The time-averaged spectrum from T+0.3 to T+122.2 sec (SHB plus extended
emmission) is best fit by a simple power-law model.  The power law index
of the time-averaged spectrum is 2.15 +- 0.54.  The fluence in the
15-150 keV band is 5.7 +- 1.7 x 10^-7 erg/cm2.  The 1-sec peak photon flux
measured from T-0.05 sec in the 15-150 keV band is 1.8 +- 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/301578/BA/


GRB_name: GRB080123A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7207
SUBJECT: GRB 080123: Swift/UVOT refined analysis 
DATE:    08/01/23 16:09:43 GMT
FROM:    Antonino Cucchiara at PSU  <cucchiara@astro.psu.edu>

A. Cucchiara (PSU), T. N. Ukwatta (GSFC/GWU)
report on behalf of the Swift-UVOT team:

The Swift/UVOT observed the field of GRB080123 (trigger #301578)
starting 111 seconds after the BAT trigger (Ukwatta et al. 2008, GCN
Circ. 7203). We do not find any new source in any of the UVOT
single or coadded observations inside the XRT enhanced error
circle (Osborne et al., GCN Circ. 7204).
The XRT position is not covered by the V ,U and B
images.

The 3-sigma upper limits (in the UVOT photometric system,
Breeveld et al., GCN Circ. 6614) are listed:

Filter           Tstart   Tstop     Exp    Magnitude  
                   (s)     (s)      (s)   

white              112     211      100    >20.48
(finding chart)

uvw1               651    8022      577    >20.86
uvm2               626    7817      578    >20.70
uvw2               731   14026     1188    >21.56

The values quoted above are not corrected for the expected Galactic
extinction corresponding to a reddening of E_{B-V} = 0.03  mag in the
direction of the burst (Schlegel et al. 1998).


GRB_name: GRB080123A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7208
SUBJECT: GRB 080123: Swift-XRT refined analysis
DATE:    08/01/23 17:24:42 GMT
FROM:    Boris Sbarufatti at INAF-IASF-Pa  <sbarufatti@ifc.inaf.it>

V. Mangano, B. Sbarufatti (INAF-IASF PA), T. N. Ukwatta (GSFC/GWU),
and D. N. Burrows (PSU) report on behalf of the Swift XRT team:

We have analyzed the XRT data collected during the first three
orbits of observation of GRB 080123 (Ukwatta et al., GCN Circ. 7203).
We have 124 s of exposure in WT mode (from T+108 to T+224 s)
and 7.1 ks in PC mode.

The initial XRT on-board position was centered on a cosmic ray hit. 
This position was retracted.  The XRT position reported in GCN Circ. 
7203 was obtained from the first downlinked data, but we note that the 
error circle given in this circular erroneously  ignored the systematic 
component and was therefore much too small.  The new, refined position 
of the XRT afterglow is

22h 35m 46.6s, -64d 54' 03.8" (J2000)

with an error circle radius of 3.9" (90% confidence).
As reported by Osborne et al. (GCN Circ. 7204), the UVOT-enhanced
astrometric position is RA, Dec = 338.94226, -64.90090 which is
equivalent to:

RA (J2000):   22h 35m 46.1s
Dec (J2000): -64d 54' 03.24"

with an uncertainty of 2.1 arcsec (radius, 90% confidence).

The X-ray light curve of the source shows a doubly broken
power law behaviour, with an initial decay with slope 1.7 +/- 0.2,
a first break at T+203 +/- 10 s, a second decay phase with
slope 6.9 +/- 0.4, a second break at T+436 +/- 250 s
and a third decay phase with slope 1.2 +/- 0.3.
If decaying at this rate the source will be at the level of
9.0e-5 counts/s at T+24 hr.

The WT spectrum is well fitted by an absorbed power law with
photon index 1.64 +/- 0.09, while the PC spectrum can be
fitted by a power law with photon index of 2.1 +/- 0.2.
Both spectra are consistent with an absorption column
of (8.1 +/- 2.4)e20 cm^-2, in excess with respect to the
Galactic absorption along the line of sight (2e20 cm^-2,
Kalberla et al. 2005).
The observed (unabsorbed) flux in the 0.3-10 keV band
is 7.0e-10 (7.9e-10) erg cm^-2 s^-1 for the WT spectrum
and 1.1e-12 (1.4e-12) erg cm^-2 s^-1 for the PC spectrum.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB080121A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7209
SUBJECT: GRB 080121: Swift-BAT detection of a very weak, short burst
DATE:    08/01/23 20:39:09 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <jayc@milkyway.gsfc.nasa.gov>

J. R. Cummings and D. M. Palmer for the Swift-BAT team

At 21:29:55 on Jan 21, 2008, BAT detected a weak short GRB 
(trigger #301491) at a ground-calculated location 
RA, Dec 137.235, +41.841, error radius 3 arcmin (90% confidence),
which is:
RA(J2000)  = 09h 08m 56s
Dec(J2000) = +41d 50' 29"
 
The significance of the source in the detection image was just 
below the alert threshold, so Swift did not slew immediately to 
the burst. In addition, the source location was in Moon constraint, 
so no late observation was made.

As seen in BAT, the burst was a single peak with T90 0.7 +- 0.2
seconds. Because of the weakness of the burst, a power-law fit to 
the spectrum from T-0.4 to T+0.4 sec is not well constrained. The 
power-law index is 2.6 +- 0.8. The fluence was 
(3 +- 2) x 10^-8 erg/cm2/sec. Quoted uncertainties are 90%
confidence including estimated systematic error.


GRB_name: GRB080121A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7210
SUBJECT: GRB 080121: Nearby SDSS galaxies
DATE:    08/01/23 22:51:25 GMT
FROM:    Daniel Perley at U.C. Berkeley  <dperley@astro.berkeley.edu>

D. A. Perley, R. J. Foley, and J. S. Bloom (UC Berkeley) report:

Two SDSS spectroscopically-catalogued galaxies are present in NED* 
within the Swift-BAT error circle of GRB 080121 (Cummings et al., GCN 7209):

SDSS J090858.15+414926.5   09:08:58.1 +41:49:27 z=0.045322
SDSS J090904.12+415033.2   09:09:04.1 +41:50:33 z=0.046041

Several other, fainter extended sources are also present in the field, 
possibly indicating that this GRB may have occurred within a group or 
small cluster.  At a redshift of z=0.046, the isotropic energy release 
would be ~10^47 erg, several orders of magnitude less than typical 
short-hard bursts.

* The NASA/IPAC Extragalactic Database (NED) is operated by the Jet 
Propulsion Laboratory, California Institute of Technology, under 
contract with the National Aeronautics and Space Administration.


GRB_name: GRB080122A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7211
SUBJECT: IPN triangulation of GRB080122
DATE:    08/01/23 23:53:42 GMT
FROM:    Kevin Hurley at UCBerkeley/SSL  <khurley@ssl.berkeley.edu>

K. Hurley and T. Cline on behalf of the Mars Odyssey, Konus,
and MESSENGER GRB teams,

W. Boynton, C. Fellows, K. Harshman, C. Shinohara and R. Starr, on
behalf of the GRS-Odyssey GRB team,

I. G. Mitrofanov, D. Golovin, M. L. Litvak, and A. B. Sanin,
on behalf of the HEND-Odyssey GRB team,

S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks
on behalf of the Konus-Wind team,

J. Goldsten, on behalf of the MESSENGER GRNS GRB team,

K. Yamaoka, M. Ohno, Y. Fukazawa, T. Takahashi, M. Tashiro, Y. Terada,
T. Murakami, and K. Makishima on behalf of the Suzaku WAM team,

J. Cummings, S. Barthelmy, N. Gehrels, and H. Krimm, on behalf of
the Swift-BAT team,

E. Del Monte, Y. Evangelista, I. Lapshov, M. Rapisarda, A. Giuliani,
F. Fuschino, and M. Marisaldi, on behalf of the AGILE Team, and

A. von Kienlin, G. Lichti, and A. Rau, on behalf of the
INTEGRAL SPI-ACS GRB team, report:

Mars Odyssey (GRS), Konus-Wind, MESSENGER (GRNS), Suzaku-WAM,
Swift-BAT, AGILE-MCAL, and INTEGRAL SPI-ACS observed the long-duration
GRB 080122 at about 66764 s UT (18:32:44).  The burst was outside the
coded field of view of the BAT. The time history consists of several
multipeaked pulses with a total duration of ~150 sec.

We have triangulated it to the following, preliminary 3-sigma 
error box:
-----------------------------------------------
     RA(2000), deg            Dec(2000), deg
-----------------------------------------------
Center:
  191.352 (12h 45m 24s)   +27.014 (+27d 00' 49")
Corners:
  191.825 (12h 47m 18s)   +27.508 (+27d 30' 30")
  191.786 (12h 47m 09s)   +27.830 (+27d 49' 47")
  190.880 (12h 43m 31s)   +26.512 (+26d 30' 44")
  190.914 (12h 43m 39s)   +26.181 (+26d 10' 52")
-----------------------------------------------

The error box area is 1106 sq. arcmin.  Some improvement
is possible.

Preliminary analysis of the Konus-Wind data yields
a burst fluence of ~5x10^-5 erg/cm2 (in the 20 keV - 1 MeV range),
and an Epeak of the time-integrated spectrum of ~260 keV.

Detailed spectral parameters will be reported later.


GRB_name: GRB080121A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7214
SUBJECT: GRB 080121: Enhanced Swift-XRT position
DATE:    08/01/25 09:07:23 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.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 1003 s of overlapping XRT Photon Counting mode and UVOT
V-band data for GRB 080121, 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 = 137.15169, +41.84639 which is equivalent
to:

RA (J2000): 09h 08m 36.41s
Dec (J2000): +41d 50' 47.0"

with an uncertainty of 3.5 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, astro-ph/0708.0986
http://www.swift.ac.uk/xrt_positions/Goad.pdf).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB080121A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7215
SUBJECT: GRB 080121 position was incorrect
DATE:    08/01/25 09:22:19 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

P. A. Evans reports,

The enhanced XRT position for GRB 081021 just reported (GCN Circ. 7124)
was not the position of the GRB afterglow. This source is a serendipitous
source. We apologise for any confusion.

We are implementing further checks to ensure that circulars are only issued for
GRB afterglow candidates. Details of the XRT enhancement process are provided at
http://www.swift.ac.uk/team/xrt_positions/docs.php


GRB_name: GRB080121A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7217
SUBJECT: GRB 080121: Swift/UVOT upper limits
DATE:    08/01/25 14:06:29 GMT
FROM:    Antonino Cucchiara at PSU  <cucchiara@astro.psu.edu>

A. Cucchiara (PSU), P. Schady (MSSL)
report on behalf of the Swift-UVOT team:

The Swift/UVOT observed the field of GRB080121 (trigger #301491)
starting 2.3 days after the BAT detection (J. R. Cummings et
al. 2008, GCN Circ. 7209). We do not find any new source in any
of the UVOT coadded observations inside the BAT error circle.

The 3-sigma upper limits (in the UVOT photometric system,
Breeveld et al., GCN Circ. 6614) are listed.

Filter     Tstart        Exp    Magnitude  
                         (s)
white       2.3 days     2015    >22.25
v           2.3 days     2268    >20.73
uvm2        3.4 days     1491    >21.13

The values quoted above are not corrected for the expected Galactic
extinction corresponding to a reddening of E_{B-V} = 0.02  mag in the
direction of the burst (Schlegel et al. 1998).


GRB_name: GRB080122A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7218
SUBJECT: GRB 080122 : Suzaku WAM observation of the prompt emission
DATE:    08/01/25 14:54:47 GMT
FROM:    Takeshi Uehara at Hiroshima U  <uehara@hirax7.hepl.hiroshima-u.ac.jp>

T. Uehara, M. Ohno, T. Takahashi, Y. Fukazawa, C. Kira, Y. Hanabata (Hiroshima U.),
T. Tamagawa (RIKEN), K. Yamaoka, Y. E. Nakagawa,
S. Sugita (Aoyama Gakuin U.), M. Tashiro, Y. Terada, Y. Urata, A. Endo,
K. Onda, M. Suzuki, N. Kodaka, K. Morigami (Saitama U.),
T. Enoto, R. Miyawaki, K. Nakazawa, K. Makishima (Univ. of Tokyo),
E. Sonoda, M. Yamauchi, H. Tanaka, R. Hara (Univ. of Miyazaki),
M. Kokubun, M. Suzuki, T. Takahashi (ISAS/JAXA), S. Hong (Nihon U.),
on behalf of the Suzaku WAM team, report:



The IPN localized long GRB 080122 (Hurley et al., GCN 7211) 
triggered the Suzaku Wide-band  All-sky Monitor (WAM) 
which covers an energy range of 50 keV - 5 MeV at 2008-01-22 18:32:45 UT (=T0).

The observed light curve shows a multi-peaked structure 
starting at T0-2 s, ending at T+98 s,
with a duration (T90) of about 100 seconds.
The fluence in 100-1000 keV was 2.5 x 10^-5 erg/cm^2. 
The 1-s peak flux measured from T0+5 s was 5.2 photons/cm^2/s in the same energy range.

Preliminary result shows that the time-averaged spectrum from
T0-4 s to T0+119 s is well fit by a power-law with exponential cutoff model:
  dN/dE ~  E^{-alpha} * exp(-(2-alpha)*E/Epeak)
  alpha       1.28 (+0.43, -0.54), and
  Epeak       420  (+326, -192) keV (chi2/dof = 15.8/24).

All the quoted errors are at statistical 90% confidence level,
in which the systematic uncertainties are not included.

The light curve data for this burst is available at:
http://www.astro.isas.ac.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html


GRB_name: GRB080122A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7219
SUBJECT: Konus-Wind observation of GRB 080122
DATE:    08/01/25 15:53:50 GMT
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 long GRB 080122 (Hurley et al., GCN 7211) triggered
Konus-Wind at T0=66764.605 s UT (18:32:44.605).

The burst light curve shows three multipeaked pulses with a total 
duration of ~150 s.

As observed by Konus-Wind the burst
had a fluence of 6.35(-3.39, +3.50)x10^-5 erg/cm2,
and a 64-ms peak flux measured from T0+6.768 s
of (4.80 +/- 0.95)x10^-6 erg/cm2/s
(both in the 20 keV - 1 MeV energy range).

The time-integrated spectrum of the burst
(from T0 to T0+112.384 s) is well fitted (in the 20 keV - 1 MeV range)
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with alpha = -1.27 +/- 0.10
and Ep = 259(-33, +46) keV (chi2 = 58.1/60 dof).
Fitting by GRBM (Band) model yields:
the low-energy photon index is alpha = -1.21(-0.11, +0.12),
the high energy photon index beta = -2.36(-0.68, +0.24),
the peak energy Ep = 227(-33, +43) keV (chi2 = 54.2/59 dof).

The spectrum of the most intense part (from T0 to T0+14.080 s) is well 
fitted (in the same range)
by a power law with exponential cutoff model
with alpha =  -1.00 +/- 0.07
and Ep = 341(-29, +35) keV (chi2 = 46.8/60 dof).
Fitting by GRBM (Band) model yields only an upper limit
on the high energy photon index: beta < -2.27.
The fluence of this part is (2.42+/-0.10)x10^-5 erg/cm2.

All the quoted errors are at the 90% confidence level.

The Konus-Wind light curve of this GRB is available
at http://www.ioffe.rssi.ru/LEA/GRBs/GRB080122_T66764/


GRB_name: GRB080122A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7220
SUBJECT: GRB 080122: pseudo-z= 1.93 from prompt emission spectrum
DATE:    08/01/25 17:31:35 GMT
FROM:    Alexandre Pelangeon at LATT,OMP,Toulouse  <alexandre.pelangeon@ast.obs-mip.fr>

A. Pelangeon & J-L. Atteia (LATT-OMP) report:

We used the spectral parameters of the most intense
part of GRB 080122 provided by Golenetskii et al. (GCNC 7219)
to compute the spectral pseudo-redshift(**) of this burst
detected by the IPN (Hurley et al., GCNC 7211).

We find a pseudo-redshift pz= 1.93 +/- 0.25


(**) cf. http://www.ast.obs-mip.fr/grb/pz


GRB_name: GRB080123A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7223
SUBJECT: GRB 080123 : Suzaku WAM observation of the prompt emission
DATE:    08/01/28 13:12:19 GMT
FROM:    Takeshi Uehara at Hiroshima U  <uehara@hirax7.hepl.hiroshima-u.ac.jp>

T. Uehara, M. Ohno, T. Takahashi, Y. Fukazawa, C. Kira, Y. Hanabata (Hiroshima U.),
T. Tamagawa (RIKEN), K. Yamaoka, Y. E. Nakagawa,
S. Sugita (Aoyama Gakuin U.), M. Tashiro, Y. Terada, Y. Urata, A. Endo,
K. Onda, M. Suzuki, N. Kodaka, K. Morigami (Saitama U.),
T. Enoto, R. Miyawaki, K. Nakazawa, K. Makishima (Univ. of Tokyo),
E. Sonoda, M. Yamauchi, H. Tanaka, R. Hara (Univ. of Miyazaki),
M. Kokubun, M. Suzuki, T. Takahashi (ISAS/JAXA), S. Hong (Nihon U.),
on behalf of the Suzaku WAM team, report:

The short GRB 080123 (Swift/BAT trigger #301578 ; Ukwatta et al., GCN 7203)
triggered the Suzaku Wide-band  All-sky Monitor (WAM) which covers an
energy range of 50 keV - 5 MeV at 2008-01-22 04:21:57 UT (=T0).

The observed light curve shows a double-peaked structure 
starting at T0 s, ending at T0+0.4 s with a duration (T90) of about 0.40 seconds. 
The fluence in 100 - 1000 keV was 3.1 (+/- 0.5) x 10^-7 erg/cm^2.
The 1-s peak flux measured from T0 s was 1.2 (+/- 0.2) photons/cm^2/s 
in the same energy range.

Preliminary result shows that the time-averaged spectrum from T0 s to
T0+0.5 s is well fitted by a single power-law with a photon index
of 1.22 (+0.21, -0.52) (chi^2/d.o.f = 10/13).

All the quoted errors are at statistical 90% confidence level,
in which the systematic uncertainties are not included.
 
The light curves for this burst are available at:

 http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html


GRB_name: GRB080121A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7224
SUBJECT: GRB 080121: Upper limit on X-ray afterglow
DATE:    08/01/28 15:43:03 GMT
FROM:    Eleonora Troja at INAF-IASFPA  <nora@ifc.inaf.it>

E. Troja (INAF/IASFPA), and D. N. Burrows (PSU) report
on behalf of the Swift XRT team:

We have analysed 21 ks of XRT/PC data for the short GRB 080121 (trigger
301491; Cummings & Palmer, GCN 7209), starting 2.3 d after the burst.
No X-ray afterglow candidate is found within the BAT error circle
(GCN 7209). A faint source is detected within the BAT error circle at

RA(2000) = 09h 08m 46.36s,
Dec(J2000) = +41d 51' 21.1''

with an error radius 5 arcsec (90% containment). This source has a count
rate of ~2E-03 cts/s, and displays no fading behaviour.

We place a 3 sigma upper limit of 1E-03 cts/s on the X-ray afterglow count
rate, which corresponds to an unabsorbed flux of 3.7E-14 erg/cm^2/s (over
0.3-10 keV), assuming a Crab-like spectrum and a Galactic absorption of
1.23E+20 cm^-2 (Kalberla et al. 2005).

This circular is an official product of the Swift XRT Team.


GRB_name: GRB080129A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7226
SUBJECT: GRB 080129 (?): Swift detection of a possible burst
DATE:    08/01/29 06:31:10 GMT
FROM:    Stefan Immler at NASA/GSFC  <immler@milkyway.gsfc.nasa.gov>

S. Immler (CRESST/GSFC/UMD), D. N. Burrows (PSU), M. M. Chester (PSU),
N. Gehrels (NASA/GSFC), S. T. Holland (CRESST/USRA/GSFC),
E. A. Hoversten (PSU), K. L. Page (U Leicester), D. M. Palmer (LANL),
D. Perez (U Leicester), M. Perri (ASDC), M. Stamatikos (NASA/ORAU) and
G. Stratta (ASDC) report on behalf of the Swift Team:

At 06:06:45 UT, the Swift Burst Alert Telescope (BAT) triggered and
located a possible GRB 080129 (trigger=301981). The BAT on-board calculated 
location is RA, Dec 105.280, -7.827 which is 
   RA(J2000) = 07h 01m 07s
   Dec(J2000) = -07d 49' 35"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve for this event appears
to show a duration of about 80 sec with a peak of ~600 counts/sec 
(15-350 keV), at ~30 sec after the trigger although, as is usual
for image triggers, the TDRSS light curve is noisy. 
The location of the source, 1.4 degrees from the Galactic plane
raises the possibility that this is a Galactic transient. 
Further analysis will require the downlinked data from Malindi. 

Because of an Earth limb constraint, the spacecraft did not slew promptly
to the BAT position, and so there are no immediate XRT or UVOT data products
to analyze.  Swift will slew to this position at about T+3006 s, or 
about 06:56 UT. 

Burst Advocate for this burst is S. Immler (immler AT milkyway.gsfc.nasa.gov). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB080129A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7227
SUBJECT: GRB 080129 (?): UVOT Upper Limits
DATE:    08/01/29 07:15:34 GMT
FROM:    Stephen Holland at USRA/NASA/GSFC/SSC  <sholland@milkyway.gsfc.nasa.gov>

S. T. Holland (CRESST/USRA/GSFC) reports on behalf of the Swift Team:

      UVOT took a 100 s finding chart exposure of the field of the
possible GRB 080129 (Immler et al., GCN Circ. 7226) with the white
(160-650 nm) filter starting 3207 seconds after the BAT trigger.  No
afterglow candidate has been found in the initial data products.  The
2.7'x2.7' sub-image covers 25% of the BAT error circle.  The 3-sigma
upper limit at the centre of the BAT position is white ~= 18.5 on the
UVOT photometric system (Poole et al. 2008).  The 8'x8' region for the
list of sources generated on-board covers 100% of the BAT error circle
and contains no uncatalogued sources.  This list of sources is typically
complete to about 18 mag.  This field is 1.42 degrees from the
Galactic place, and no correction has been made for the expected
Galactic extinction corresponding to a reddening of E(B-V) = 1.02.


GRB_name: GRB080129A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7228
SUBJECT: GRB 080129: Swift XRT position
DATE:    08/01/29 07:22:11 GMT
FROM:    Matteo Perri at ISAC/ASDC  <perri@asdc.asi.it>

M. Perri (ASDC), G. Stratta (ASDC) and D.N. Burrows (PSU) report on
behalf of the Swift XRT team:

The Swift XRT began observing the possible GRB 080129 (trigger #301981,
Immler et al., GCN Circ. 7226) at 07:00:08 UT, about 53 min after the
BAT trigger.

Analysis of prompt downlinked data finds an uncataloged X-ray source
located at RA, Dec 105.2848, -7.8463 which is
   RA(J2000) = 07 01 8.35
   Dec(J2000) = -07 50 46.8
with an uncertainty of 3.3 arcsec (radius, 90% containment). This location
is 71 arcseconds from the BAT on-board position, within the BAT error
circle (Immler et al., GCN Circ 7226). Further analysis will be
reported in a subsequent circular.

This circular is an official product of the Swift XRT Team.


GRB_name: GRB080129A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7229
SUBJECT: GRB 080129: Gemini-South Imaging Observations 
DATE:    08/01/29 08:23:04 GMT
FROM:    Josh Bloom at UC Berkeley  <jbloom@astron.berkeley.edu>

J. S. Bloom (UC Berkeley) reports on behalf of the larger GRAASP  
collaboration:

"Automatically triggering off of the original GCN/SWIFT_BAT_POSITION  
notice for GRB 080129 (GCN 7226), we observed the field with Gemini  
South + GMOS in the r-band starting at 06:50:21.4 2008-01-29 in a  
series of 5 dithered exposures of 5 minutes apiece. Consistent with  
the position of the X-ray source (GCN 7228) we find a point-like  
object at:

     07:01:08.20  -07:50:46.3  (J2000)

(preliminary uncertainty of 300 mas rms relative to 2MASS). We suggest  
that this is the optical afterglow of GRB 080129 but cannot confirm  
variability at this time. More observations are encouraged."

We thank the Gemini Staff for conducting these observations.

This message may be cited.


GRB_name: GRB080129A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7230
SUBJECT: GRB 080129: Enhanced Swift-XRT position
DATE:    08/01/29 10:36:12 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

M.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 399 s of overlapping XRT Photon Counting mode and UVOT
V-band data for GRB 080129, 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 = 105.28406, -7.84705 which is equivalent
to:

RA (J2000): 07h 01m 8.17s
Dec (J2000): -07d 50' 49.4"

with an uncertainty of 2.7 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, astro-ph/0708.0986
http://www.swift.ac.uk/xrt_positions/Goad.pdf).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB080129A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7231
SUBJECT: GRB 080129: GROND detection of the optical/NIR afterglow, and fading
DATE:    08/01/29 11:10:18 GMT
FROM:    Jochen Greiner at MPI  <jcg@mpe.mpg.de>

T. Kruehler, S. Loew, J.Greiner, C.Clemens, A. Kuepcue Yoldas, A. Yoldas
(all MPE Garching) report on behalf of the GROND team:  

We observed the field of GRB 080129 observed by Swift (Immler et al.
2008, GCN#7226) simultaneously in grizJHK with GROND mounted at the 2.2m
MPI/ESO telescope at La Silla (Chile).
  
Observations started at 06:11 UT, about 4 min after the GRB.
  
We find a point source not present in the Digital Sky Survey images
inside the Swift/XRT error circle of the X-ray afterglow 
(Perri et al. 2008, GCN#7228; Goad et al. 2008, GCN#7230).  
  
The coordinates are (+- 0.5 arcsec error):
RA (2000.0) = 07h 01m 08.2s    
Decl. (2000.0) = -07d 50' 47'
consistent with the optical source reported by J. S. Bloom (GCN#7229).
  
We estimate magnitudes of 22.8 (r), 21.5 (i), 20.6 (z), 18.9 (J), 18.1
(H) and 17.0 (K) calibrated against USNO and 2MASS field stars. These
magnitudes are not corrected for galactic extinction.
  
The source is fading by about 0.5 mag during the first 90 min, suggesting 
it to be the optical/NIR afterglow of GRB 080129.


GRB_name: GRB080129A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7232
SUBJECT: GRB 080129: GROND detection in all bands, and fading
DATE:    08/01/29 11:19:56 GMT
FROM:    Jochen Greiner at MPI  <jcg@mpe.mpg.de>

T. Kruehler, S. Loew, J.Greiner, C.Clemens, A. Kuepcue Yoldas, A. Yoldas
(all MPE Garching) report on behalf of the GROND team:  

We observed the field of GRB 080129 observed by Swift (Immler et al.
2008, GCN#7226) simultaneously in grizJHK with GROND mounted at the 2.2m
MPI/ESO telescope at La Silla (Chile).
  
Observations started at 06:11 UT, about 4 min after the GRB.
  
We find a point source not present in the Digital Sky Survey images
inside the Swift/XRT error circle of the X-ray afterglow 
(Perri et al. 2008, GCN#7228; Goad et al. 2008, GCN#7230).  
  
The coordinates are (+- 0.5 arcsec error):
RA (2000.0) = 07h 01m 08.2s    
Decl. (2000.0) = -07d 50' 47'
consistent with the optical source reported by J. S. Bloom (GCN#7229).
  
We estimate magnitudes of 22.8 (r), 21.5 (i), 20.6 (z), 18.9 (J), 18.1
(H) and 17.0 (K) calibrated against USNO and 2MASS field stars. These
magnitudes are not corrected for galactic extinction.
  
The source is fading by about 0.5 mag during the first 90 min, suggesting 
it to be the optical/NIR afterglow of GRB 080129.


GRB_name: GRB080129A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7233
SUBJECT: GRB 080129: Gemini-South photometry
DATE:    08/01/29 11:48:14 GMT
FROM:    Daniel Perley at U.C. Berkeley  <dperley@astro.berkeley.edu>

D. A. Perley and J. S. Bloom (UC Berkeley) report on behalf of the 
GRAASP collaboration:

Preliminary photometry of our first series of r-band observations of the 
candidate afterglow of GRB 080129 (Immler et al., GCN 7226; Bloom, 7229) 
yields the following magnitudes, calibrated using three DSS stars*:

t=44 min: R = 22.93 +/- 0.06
t=50 min: R = 22.86 +/- 0.05
t=56 min: R = 22.78 +/- 0.04
t=62 min: R = 22.56 +/- 0.04
t=68 min: R = 22.87 +/- 0.05

As these magnitudes are approximately consistent with the value reported 
by Kruehler et al. (GCN 7231/7232) we do not confirm general fading 
behavior of this source over the interval of our observations. 
However, we note that the fourth exposure shows statistically 
significant evidence of a short-lived rebrightening.  While an 
instrumental cause has not been ruled out, given the location in the 
Galactic plane of the source and the very slow fading reported by 
Kruehler et al. (0.5 mag from 4 to ~94 minutes, atypical of extragalactic 
GRBs), it is possible that the GRB may be an analog of GRB 070610 / 
SWIFT J195509.6+261406 (Pagani et al., GCN 6489; Kasliwal et al. 2007, 
arXiv:0708.0226), which showed extensive short-time scale early-time 
variability above a nearly-constant baseline.  Further observations 
(including rapid-time-series optical observations), and further analysis 
of the X-ray afterglow, are encouraged to further investigate the nature 
of this source.

---

*Calibration stars are:

ra            dec            R2
07:01:10.5033 -07:50:24.020  17.130
07:01:07.7333 -07:51:24.620  17.040
07:01:04.7193 -07:50:46.690  17.310

[GCN OPS NOTE(29jan08): Per author's request, the "Greiner" citation was changed
to "Kruehler".]


GRB_name: GRB080129A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7234
SUBJECT: GRB 080129: TAROT La Silla observatory optical observations
DATE:    08/01/29 12:29:15 GMT
FROM:    Alain Klotz at CESR-CNRS  <Alain.Klotz@free.fr>

Klotz, A. (CESR-OMP), Boer M. (OHP), Atteia J.L. (LATT-OMP) report:

We imaged the field of GRB 080129 detected by SWIFT
(trigger 301981) with the TAROT robotic telescope (D=25cm)
located at the European Southern Observatory,
La Silla observatory, Chile.

The observations started 352.7s after the GRB trigger
(270.9s after the notice). The elevation of the field decreased from
from 42 degrees above horizon and weather conditions
were good.

The date of trigger : t0 = 2008-01-29T06:06:45.216

The fiirst image is 90.0s exposure in tracking mode.
We do not detect any OT with a limiting magnitude of:
t0+352.7s to t0+442.7s : R > 16.4

We co-added a series of exposures:
t0+448.5s to t0+1039.0s : R > 18.3

Magnitudes were estimated with the nearby USNO-B1 stars
and are not corrected for galactic dust extinction.

N.B. Galactic coordinates are lon=220.9983 lat= -1.4244
and the galactic extinction in R band is about 9 magnitudes
estimated from D. Schlegel et al. 1998ApJ...500..525S.

This message may be cited.


GRB_name: GRB080129A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7235
SUBJECT: GRB 080129, Swift-BAT refined analysis
DATE:    08/01/29 16:35:01 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), J. Cummings (GSFC/UMBC), E. Fenimore (LANL),
N. Gehrels (GSFC), S. Immler (CRESST/GSFC/UMD), H. Krimm (GSFC/USRA),
C. Markwardt (GSFC/UMD), D. Palmer (LANL), T. Sakamoto (GSFC/UMBC),
G. Sato (GSFC/ISAS), M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC),
T. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+963 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 080129 (trigger #301981)
(Immler, et al., GCN Circ. 7226).  The BAT ground-calculated position is
RA, Dec = 105.297, -7.840 deg which is 
   RA(J2000)  = 07h 01m 11.2s 
   Dec(J2000) = -7d 50' 24" 
with an uncertainty of 2.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 46%.
 
The mask-weighted light curve shows a single broad peak starting at ~T-20 sec,
peaking at ~T+20, and ending at ~T+50.  T90 (15-350 keV) is 48 +- 10 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-15.0 to T+49.0 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.34 +- 0.26.  The fluence in the 15-150 keV band is 8.9 +- 1.4 x 10^-07 erg/cm2.
The 1-sec peak photon flux measured from T+24.50 sec in the 15-150 keV band
is 0.2 +- 0.1 ph/cm2/sec.  All the quoted errors are at the 90% confidence
level. 

The majority of the indicators say this is a GRB, but at this time
we can not rule out a galactic source explanation for this trigger.
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/301981/BA/


GRB_name: GRB080129A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7236
SUBJECT: GRB 080129: optical limit by  Pi of the Sky
DATE:    08/01/29 21:04:53 GMT
FROM:    Grzegorz Wrochna at Soltan Inst.for Nuclear Studies  <wrochna@fuw.edu.pl>

M.Cwiok, W.Dominik, G.Kasprowicz, A.Majcher, A.Majczyna,
K.Malek, L.Mankiewicz, M.Molak, K.Nawrocki, L.W.Piotrowski,
D.Rybka, M.Sokolowski, J.Uzycki, G.Wrochna, A.F.Zarnecki
on behalf of "Pi of the Sky" collaboration http://grb.fuw.edu.pl

"Pi of the Sky" apparatus located at Las Campanas Observatory
imaged the region of GRB 080129 from 6:09:21 UT,
i.e. 155s after the GRB (74s after the trigger),
with 10s exposures (IR-cut filter only).
No new object has been detected within the XRT error box.

Limiting magnitude for 10s exposures is >11.8 mag.
The limit for 20 coadded images is >12.5 mag.


GRB_name: GRB080123A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7237
SUBJECT: GRB 080123: Early afterglow detection with BATSS (BAT Slew Survey)
DATE:    08/01/29 23:57:04 GMT
FROM:    Antonio Copete at Harvard U  <acopete@head.cfa.harvard.edu>

A. Copete, J. Grindlay, B. Allen, J. Hong (Harvard)
S. Barthelmy, C. Markwardt, N. Gehrels (GSFC)

We report the independent detection of early afterglow (or post prompt- 
emission flaring) emission from the short GRB 080123 (GCN#7203). The  
BATSS pipeline processed the BAT data from the initial automatic slew  
to the burst, which started at 04:22:09 UT (T+12sec), and was  
completed within 5 hours of the BAT trigger. A 6.2-sigma image
detection (from stacked 0.2sec slew images throughout the 68sec slew)  
in the 15-50 keV energy band yielded a position of:
  RA(J2000) = 22h 35m 08s
  Dec(J2000) = -64d 57' 24"
with an uncertainty of 6 arcmin (90% confidence radius), consistent  
with the XRT reported position of GRB080123 (GCN# 7208). Preliminary  
lightcurve analysis shows the BATSS image detection is due to an  
inital ~4sec duration flare at T+20, followed by two possible broader  
(~10-15sec) peaks at T+49 and T+72. The total estimated fluence is  
2.1E-7 erg/cm2  (15-50keV; derived for a PL model with photon index 2)  
over the 68.8sec duration of the slew. This fluence is a factor of  
0.36 times that reported in the 15-150keV band (GCN Report 111.1) for T 
+0.3 to T+122.2 and is likely dominated by the soft flare emission  
after the prompt hard emission of the short GRB.

BATSS pipeline processing is in the final stages of development  
following our first preliminary tests, which discovered GRB070326  
(GCN# 6653). Full BATSS results will begin to be available soon from a  
website
to be announced.


GRB_name: GRB080129A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7238
SUBJECT: GRB 080129: KAIT optical limits
DATE:    08/01/30 00:16:38 GMT
FROM:    Weidong Li at UC Berkeley KAIT/LOSS  <weidong@astron.berkeley.edu>

W. Li and A. V. Filippenko, University of California, Berkeley, on behalf
of the KAIT GRB team, report:

We imaged the field of GRB 080129 detected by Swift (trigger 301981;
Immler et al. GCN 7226) with the robotic 0.76-m Katzman Automatic Imaging
Telescope (KAIT) at Lick Observatory. The automatic sequence was not 
executed due to poor weather, but a manual sequence was observed remotely.
In total, 14 x 20 s  unfiltered observations were observed. Our first 20 s
image started at 6:11:31 UT, 286 s after the GRB trigger. We did not detect 
the optical/NIR afterglow candidate reported by Bloom (GCN 7229) and
Kruehler et al. (GCN 7231) to a limiting magnitude of 17.9 (calibrated to 
USNO B1). A 200 s co-added image with the middle exposure time at 643 s 
after the GRB trigger did not detect the afterglow candidate to a limiting
magnitude of 20.0. 

This message may be cited.


GRB_name: GRB080129A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7240
SUBJECT: GRB 080129: Swift-XRT refined analysis
DATE:    08/01/30 16:42:11 GMT
FROM:    Giulia Stratta at ASDC  <giulia.stratta@gmail.com>

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G. Stratta (ASDC), M. Perri (ASDC) and D. N. Burrows (PSU)
report on behalf of the Swift-XRT team:

The Swift-XRT began observing GRB 080129 (trigger=301981) on
2008-01-29 at 07:00:17 UT, 53 minutes after the BAT trigger
(Immler et al., GCN Circ. 7226).

Using 2045 s of overlapping XRT Photon Counting mode and UVOT
v-band data for GRB 080129, we find a refined astrometrically
corrected X-ray position (using the XRT-UVOT alignment and
matching UVOT field sources to the USNO-B1 catalogue):
RA, Dec =  105.284125, -7.846722 which is equivalent to:

RA (J2000): 07h 01m 8.19s
Dec (J2000): -07d 50' 48.2"

with an uncertainty of 2.0 arcsec (radius, 90% confidence).
This is 1.2 arcsec away from the previous position derived from the
XRT and UVOT data reported in Goad et al. (GCN Circ. 7230),
51 arcsec from the refined BAT position of Barthelmy et al.
(GCN Circ. 7235) and 1.9 arcsec from the Gemini South position
(GCN Circ. 7229).

The X-ray light curve from T + 3.2 ks to T + 85.8 ks can be
fitted by a broken power law model (chi2 of 39 for 28 degrees
of freedom) with a temporal break at about T + 15.5 ks and
decay indices alpha1 = 0.6 +/- 0.1 and alpha2 = 1.5 +/- 0.1
before and after the break, respectively.

The 0.3-10 keV spectrum from T + 3.2 ks to T + 32.2 ks
is well fit by an absorbed power law
(reduced chi2 of 1.02, with 20 degrees of freedom).
The best fit photon index is 2.0 +/- 0.1, with an hydrogen column
density of (2 +/- 1)e21 cm^-2, in addition to the Galactic column along
the line of sight of 6.3e21 cm^-2 (Kalberla et al. 2005).
The observed (unabsorbed) flux in the 0.3-10 keV band is
4.2e-12 (8.5e-12) erg cm^-2 s^-1.

The timing and spectral behaviors are completely consistent
with those of a typical GRB X-ray afterglow,
removing any uncertainty about the nature of this burst.

The predicted XRT count rate 48 hours after the trigger is 1.6e-3
count s^-1, which corresponds to an observed 0.3-10.0 keV flux of
1.3e-12 ergs cm^-2 s^-1.

This circular is an official product of the Swift-XRT team.

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G. Stratta (ASDC), M. Perri (ASDC) and D. N. Burrows (PSU) <br>report on behalf of the Swift-XRT team:<br>&nbsp;<br>The Swift-XRT began observing GRB 080129 (trigger=301981) on <br>2008-01-29 at 07:00:17 UT, 53 minutes after the BAT trigger&nbsp; <br>
(Immler et al., GCN Circ. 7226). <br><br>Using 2045 s of overlapping XRT Photon Counting mode and UVOT<br>v-band data for GRB 080129, we find a refined astrometrically <br>corrected X-ray position (using the XRT-UVOT alignment and <br>
matching UVOT field sources to the USNO-B1 catalogue): <br>RA, Dec =&nbsp; 105.284125, -7.846722 which is equivalent to:<br><br>RA (J2000): 07h 01m 8.19s<br>Dec (J2000): -07d 50&#39; 48.2&quot;<br><br>with an uncertainty of 2.0 arcsec (radius, 90% confidence).<br>
This is 1.2 arcsec away from the previous position derived from the <br>XRT and UVOT data reported in Goad et al. (GCN Circ. 7230),&nbsp; <br>51 arcsec from the refined BAT position of Barthelmy et al. <br>(GCN Circ. 7235) and 1.9 arcsec from the Gemini South position <br>
(GCN Circ. 7229).<br><br>The X-ray light curve from T + 3.2 ks to T + 85.8 ks can be <br>fitted by a broken power law model (chi2 of 39 for 28 degrees <br>of freedom) with a temporal break at about T + 15.5 ks and <br>decay indices alpha1 = 0.6 +/- 0.1 and alpha2 = 1.5 +/- 0.1 <br>
before and after the break, respectively. <br><br>The 0.3-10 keV spectrum from T + 3.2 ks to T + 32.2 ks <br>is well fit by an absorbed power law <br>(reduced chi2 of 1.02, with 20 degrees of freedom). <br>The best fit photon index is 2.0 +/- 0.1, with an hydrogen column <br>
density of (2 +/- 1)e21 cm^-2, in addition to the Galactic column along <br>the line of sight of 6.3e21 cm^-2 (Kalberla et al. 2005). <br>The observed (unabsorbed) flux in the 0.3-10 keV band is <br>4.2e-12 (8.5e-12) erg cm^-2 s^-1. <br>
<br>The timing and spectral behaviors are completely consistent <br>with those of a typical GRB X-ray afterglow, <br>removing any uncertainty about the nature of this burst.<br><br>The predicted XRT count rate 48 hours after the trigger is 1.6e-3 <br>
count s^-1, which corresponds to an observed 0.3-10.0 keV flux of <br>1.3e-12 ergs cm^-2 s^-1.<br><br>This circular is an official product of the Swift-XRT team.<br><br clear="all"><br><br>

------=_Part_8281_12864563.1201711331484--


GRB_name: GRB080129A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7241
SUBJECT: GRB 080129: Optical observations from OSN
DATE:    08/01/30 20:18:53 GMT
FROM:    Antonio Deugarte at IAA-CSIC  <deugarte@iaa.es>

A. de Ugarte Postigo (ESO, Santiago), D. Diaz Fraile, F. Aceituno, E. 
Rodrguez,
A.J. Castro-Tirado, J. Gorosabel, M. Jelinek (IAA-CSIC, Granada) and
A. Pozanenko (IKI, Moscow)
report on behalf of a larger collaboration:

We have observed GRB 080129 (Immler et al. GCN 7226) with the 1.5m OSN 
telescope
at Sierra Nevada Observatory (Granda, Spain). The observations consist 
of a series of
625x19s exposures in I-band, and range from 29.8614 Jan 2008 to 30.0166 
Jan 2008 UT
(0.607-0.762 days after the burst). We do not detect any source in the 
individual frames down
to an average limiting magnitude I < 20.3. However, the combined frame 
does show the
source identified by Bloom et al. (GCN 7229) at I ~ 22.1.
A finding chart can be seen at:
http://www.iaa.es/~deugarte/GRBs/080129/080129_OSN_fc.jpg

This message may be cited.

[GCN OPS NOTE(31jan08): Per author's request, M. Jelinek was added
to the author list.]


GRB_name: GRB080130A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7243
SUBJECT: GRB 080130(?): Swift XRT observation
DATE:    08/01/31 06:38:14 GMT
FROM:    Rhaana Starling at U of Leicester  <rlcs1@star.le.ac.uk>

R.L.C. Starling (U. Leicester) and M. Stamatikos (GSFC/ORAU) report on behalf
of the Swift XRT team:

Swift XRT observed the field of possible GRB 080130 (Copete et al., GCN 7242)
found in the BAT Slew Survey, approximately 11 hours after the burst. In
1.98ks of Photon Counting (PC) mode data starting 2008-01-30:22:21 and ending
2008-01-30:22:54 we find one possible X-ray source inside the BATSS error
circle, detected at the 3-sigma level at RA,Dec=261.61657,-53.18878 deg 
and equivalent to:

RA (J2000)= 17h 26m 27.98s
Dec(J2000)= -53d 11' 19.6"

with an uncertainty of 8.7 arcsec (radius, 90% confidence). This is 2.1 arcmin
from the reported BATSS position.
At this stage we cannot tell if the source is fading or not and we have no
spectral information.

This is an official product of the Swift XRT team.


GRB_name: GRB080130A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7244
SUBJECT: GRB 080130: REM NIR observations
DATE:    08/01/31 08:42:57 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

P. D'Avanzo, S. Covino, L.A. Antonelli, D. Fugazza, L. Calzoletti, S. 
Campana, G.  Chincarini, M.L. Conciatore, S. Cutini, V. D'Elia, F. 
Dalessio, F.  Fiore, P. Goldoni, D. Guetta,  C. Guidorzi, G.L. Israel, 
N. Masetti, A. Melandri, E. Meurs, L. Nicastro, E. Palazzi, E. Pian, S. 
Piranomonte, L. Stella, G.  Stratta, G. Tagliaferri, G. Tosti, V.Testa, 
S.D. Vergani,  F. Vitali   report on behalf of the REM team:

The robotic 60-cm REM telescope located at La Silla (Chile) observed the 
field of the GRB 080130 (Copete et al., GCN 7242). Observations were 
performed in the H-band on Jan 31.3041 (about 0.8 days after the burst ) .

We detect two objects inside the XRT error box (Starling & Stamatikos, 
GCN 7243), both present in the 2MASS catalogue, at the following 
coordinates (J2000):

A) R.A. = 17:26:27.71, Dec. = -53:11:20.3
B) R.A. = 17:26:29.22, Dec. = -53:11:20.3

with an uncertainty of 0.4". The magnitude of both objects seems to be 
consistent with the value reported in the 2MASS catalogue. We note that 
a third 2MASS object is present inside the XRT error box at the 
coordinates (J2000):

C) R.A. = 17:26:28.76, Dec. = -53:11:14.4

but it is below our detection limit. No other sources are visible within 
the XRT error box down to a limiting magnitude of H > 16.1 (3sigma c.l. 
, calibrated against the 2MASS catalogue).

Sources A, B and C are also visible in the DSS image catalogue and seem 
to have a stellar-like profile.


GRB_name: GRB080130A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7245
SUBJECT: Swift/UVOT observations of GRB080130
DATE:    08/01/31 12:06:00 GMT
FROM:    Patricia Schady at MSSL/Swift  <ps@mssl.ucl.ac.uk>

P. Schady (MSSL-UCL), M. Stamatikos (GSFC/ORAU) report on behalf of the 
Swift/UVOT team:

The Swift/UVOT observed the field of GRB080130 (Copete et al., GCN 7242) 
approximately 11hrs after the possible burst, in the v, u, uvw1, uvm2 and 
uvw2 filters. All three 2MASS sources mentioned by D'Avanzo et al. (GCN 
7244) are detected in the UVOT observations. No new source is detected 
within the XRT error circle (Starling et al., GCN 7243) in any of the UVOT 
observations down to the following 3-sigma upper limits:

Filter Tmid (s) Exp.(s)  3-sig UL
v      40760    424      > 19.31
u      41979    248      > 19.47
uvw1   41631    424      > 19.68
uvm2   41195    424      > 19.79
uvw2   40324    424      > 19.07

The values quoted above are not corrected for the expected Galactic 
extinction corresponding to a reddening of E(B-V)=0.19 mag in the 
direction of the burst (Schlegel et al. 1998).


GRB_name: GRB080129A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7246
SUBJECT: GRB 080129: Swift/UVOT Refined Upper Limits
DATE:    08/01/31 13:12:48 GMT
FROM:    Stephen Holland at USRA/NASA/GSFC/SSC  <sholland@milkyway.gsfc.nasa.gov>

S. T. Holland (CRESST/GSFC/USRA) and S. Immler (CRESST/UMCP/GSFC)
report on the behalf of the Swift UVOT team:

        The Swift/UVOT observed the field of GRB 080129 starting 3188 s
after the BAT trigger (Immler et al. 2007, GCN Circ. 7226).  We do not
find any source, in any of the UVOT observations, at the location of
the Gemini-South source (Bloom, 2007 GCN Circ. 7229).

        The 3-sigma upper limits for detecting a source at this
location in the co-added images are:


Filter    T_start   T_stop    Exp(s)    Mag (3-sigma upper limit)
-----------------------------------------------------------------
    v         3188   21,457      2023    21.3
    b         4134   28,152      2164    22.2
    u         3929   27,239      1278    21.5
  uvw1        3724   32,166      1182    21.3
  uvm2        3519   22,362      1279    21.2
  uvw2        4545   17,372      1920    21.7
white        3207   28,940      2856    23.1
-----------------------------------------------------------------

This burst occurred 1.43 degrees from the Galactic plane, so the
Galactic reddening along the line of sight is highly uncertain.  The
values quoted above are not corrected for Galactic extinction.  All
photometry is on the UVOT flight system described in Poole et al.  
(2008).


GRB_name: GRB080130A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7247
SUBJECT: GRB 080130: further Swift XRT observations confirm fading source
DATE:    08/02/01 14:16:33 GMT
FROM:    Rhaana Starling at U of Leicester  <rlcs1@star.le.ac.uk>

R.L.C. Starling, P.A. Evans, P.T. O'Brien (U. Leicester), C. Guidorzi 
(U. Bicocca/INAF-OAB) and M. Stamatikos (GSFC/ORAU) report on behalf of 
the Swift XRT team:

Swift XRT re-observed the field of possible ground-detected GRB 080130 
(Copete et al., GCN 7242), approximately 34 hours after the burst. In 
4.98ks of Photon Counting (PC) mode data starting 2008-01-31:16:01 and 
ending 2008-01-31:20:51 we still detect an X-ray source inside the BATSS 
error circle at the 3-sigma level (Starling and Stamatikos, GCN 7243). By 
combining both XRT datasets for this field totalling ~7 ks we refine the 
source position to RA,Dec=261.61484,-53.18742 deg, equivalent to:

RA (J2000)= 17h 26m 27.56s
Dec(J2000)= -53d 11' 14.7"

with an uncertainty of 5 arsec (radius, 90% confidence). This is 6.2 
arcsec from the previously reported XRT position, and 2.2 arcmin from the 
BATSS position.

The count rate of the source in this second observation is 0.004+/-0.001
counts/s. Compared to the earlier measured count rate of 0.010+/-0.002
counts/s we can confirm that the source has faded. We conclude that GRB 
080130 was a real GRB, and that the source reported here is its X-ray 
afterglow.

This is an official product of the Swift XRT team.


GRB_name: GRB080130A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7248
SUBJECT: GRB 080130: Swift-BAT refined analysis
DATE:    08/02/02 20:16:21 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

J. Cummings (GSFC/UMBC), A. Copete, J. Grindlay, B. Allen, J. Hong (Harvard)
S. D. Barthelmy, N. Gehrels (GSFC), M. Stamatikos (GSFC/ORAU)
report:

Using the data set from T-3 to T+107 sec from recent telemetry
downlinks, we report further analysis of BAT GRB 080130
(T_zero chosen as 11:13:59 UT) detected during a Swift slew maneuver
(Copete, et al., GCN Circ. 7242).  The BAT ground-calculated position
from postslew (after T+33 sec) data is RA, Dec = 261.632, -53.190 deg,
which is
   RA(J2000) =  17h 26m 31.6s
  Dec(J2000) = -53d 11' 24"
with an uncertainty of 2.8 arcmin, (radius, sys+stat, 90% containment).
The burst was in the fully coded field of view after the slew.

The mask-weighted light curve shows 3 peaks at about T+4, T+30, and
T+63 sec.  T90 (15-350 keV) is 65 +- 5 sec (estimated error including
systematics).

The time-averaged spectrum from T-1 to T+68.0 sec is best fit by a
simple power-law model.  The power law index of the time-averaged
spectrum is 1.21 +- 0.12.  The fluence in the 15-150 keV band is
(7.7 +- 2.8) x 10^-7  erg/cm2.  The 1-sec peak photon flux measured 
from T+36 sec in the 15-150 keV band is 0.2 +- 0.1 ph/cm2/sec.
All the quoted errors are at the 90% confidence level.


GRB_name: GRB080205A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7250
SUBJECT: GRB 080205: Swift detection of a burst
DATE:    08/02/05 08:21:36 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

C. B. Markwardt (CRESST/GSFC/UMD), M. M. Chester (PSU),
J. R. Cummings (NASA/UMBC), P. A. Evans (U Leicester),
A. D. Falcone (PSU), N. Gehrels (NASA/GSFC), C. Guidorzi (INAF-OAB),
S. T. Holland (CRESST/USRA/GSFC), S. D. Hunsberger (PSU),
J. A. Kennea (PSU), C. Pagani (PSU), K. L. Page (U Leicester),
D. M. Palmer (LANL), D. Perez (U Leicester), J. L. Racusin (PSU),
T. Sakamoto (NASA/UMBC), M. Stamatikos (NASA/ORAU),
R. L. C. Starling (U Leicester), T. N. Ukwatta (GSFC/GWU) and
L. Vetere (PSU) report on behalf of the Swift Team:

At 07:55:51 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 080205 (trigger=302506).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 98.219, +62.769 which is 
   RA(J2000) = 06h 32m 53s
   Dec(J2000) = +62d 46' 07"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows three roughly
equal-height peaks spanning approximately 120 seconds.  The peak 
count rate was ~1000 counts/sec (15-350 keV), at ~0 sec, ~70 sec, 
and ~95 sec after the trigger. 

XRT began observing at 07:57:32 UT, 101 s after the BAT trigger. 
Using prompt downlinked data, we find a bright, fading, uncatalogued
X-ray source located at RA, Dec 98.2561, 62.7913 deg which is
   RA(J2000)  = 06h 33m 1.46s
   Dec(J2000) = +62d 47' 30.1"
with an uncertainty of 3.0 arcsec (radius, 90% containment). 
This location is 100 arcseconds from the BAT on-board position,
within the BAT error circle. 

UVOT took a finding chart exposure of 100 seconds with the White (160-650 nm)
filter starting 112 seconds after the BAT trigger. No afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 100% of
the XRT error circle. The 3-sigma upper limit at the XRT position is 19.2 mag. 
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
0.09. 

Burst Advocate for this burst is C. B. Markwardt (craigm AT milkyway.gsfc.nasa.gov). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB080205A
Detection_method: KAIT
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7251
SUBJECT: GRB 080205: KAIT OA detection
DATE:    08/02/05 08:27:42 GMT
FROM:    Weidong Li at UC Berkeley KAIT/LOSS  <weidong@astron.berkeley.edu>

W. Li, D. Perley, R. J. Foley, A. V. Filippenko, and J. S. Bloom,
University of California, Berkeley, on behalf of the KAIT GRB team,
report:

The robotic 0.76-m Katzman Automatic Imaging Telescope (KAIT) at Lick
Observatory observed GRB 080205 detected with Swift (Trigger 302506)
The automatic sequence started at 07:56:56, 64.3 s after the burst.
The BAT location has been monitored in V, I, and clear filters, with
varying exposure times. Our image processing pipeline found a new
object within the BAT error circle, with the following position:

R. A. = 06:33:00.64
DEC.  = +62:47:32.0  (J2000)

The OA has magnitude of 17.0 (calibrated with USNO B1.0) in a 20s
unfiltered exposure started at 08:01:45 UT, and show apparent variability.
Further observations are on-going.

This message may be cited.


GRB_name: GRB080205A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7252
SUBJECT: GRB 080205: Enhanced Swift-XRT position
DATE:    08/02/05 13:16:25 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

J.P. Osborne, A.P. Beardmore, P.A. Evans and M.R. Goad (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 794 s of overlapping XRT Photon Counting mode and UVOT
V-band data for GRB 080205, 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 = 98.25223, +62.79186 which is equivalent
to:

RA (J2000): 06h 33m 0.54s
Dec (J2000): +62d 47' 30.7"

with an uncertainty of 2.0 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, astro-ph/0708.0986
http://www.swift.ac.uk/xrt_positions/Goad.pdf).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB080205A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7253
SUBJECT: GRB 080205: Swift/UVOT observations
DATE:    08/02/05 16:16:32 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S.R. Oates (MSSL-UCL) and C.B Markwardt (CRESST/GSFC/UMD) report
on behalf of the UVOT team.

The Swift/UVOT observed the field of GRB 080205 (trigger #302506)
starting 111 seconds after the BAT trigger (Markwardt et al., GCN
Circ. 7250). We detect the optical afterglow at the position:

RA  (J2000) = 06:33:00.62
Dec (J2000) =+62:47:31.98

with an error of about 0.5". This is consistent with the position
reported by Li et al.(GCN 7251) and lies within the revised
XRT error circle (Osborne et al., GCN 7252).

The optical afterglow initially brightens in the first few hundred seconds
after the trigger and then begins to decay at around ~T+1000s. The
afterglow is detected in the white and v filters only. The lack
of detection in the b, u and uv filters suggests that this GRB is
at a z ~ 4.0.

The magnitudes and 3-sigma upper limits are listed:

Filter    Tstart(s) Tstop(s) Exp    Magnitude
--------------------------------------------------------------
white       111     211       98   20.37 +/- 0.28 (3.7-sigma)
             864     964       98   19.76 +/- 0.17 (6.2-sigma)
             5436    5636     196   20.59 +/- 0.25 (4.2-sigma)
v           217     617      393   18.07 +/- 0.09 (11.4-sigma)
             970     1370     393   19.02 +/- 0.20 (5.4-sigma)
b           697     686      451   20.83   (3 sigma UL)
u           672     6664     471   20.45   (3 sigma UL)
uvw1        647     6458     286   20.13   (3 sigma UL)
uvm2        622     7525     329   20.03   (3 sigma UL)
uvw2        727     7279     452   20.39   (3 sigma UL)
--------------------------------------------------------------

The values quoted above are not corrected for the expected Galactic
extinction corresponding to a reddening of E_{B-V} = 0.091 mag in the
direction of the burst (Schlegel et al. 1998).


GRB_name: GRB080205A
Detection_method: KAIT
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7254
SUBJECT: GRB 080205: OA evolution from KAIT observations 
DATE:    08/02/05 16:25:04 GMT
FROM:    Alex Filippenko at UC Berkeley  <alex@astro.berkeley.edu>

W. Li, D. Perley, and  A. V. Filippenko, University of California, 
Berkeley, on behalf of the KAIT GRB team, report:

We report further analysis of the KAIT observations of GRB 080205
(Swift Trigger 302506; Markwardt et al. GCN 7250) announced by
Li et al. (GCN 7251).  Preliminary reduction of the unfiltered 
data shows that the optical afterglow (OA) has a nearly constant 
brightness of mag 18.1 from t = 65 s to 90 s, declines to mag 19.1 
by t = 171 s, rises to mag 16.9 by t = 537 s, and has a steep 
power-law decline (with index around -1.6) thereafter until
at least t = 50 min. The OA is also detected in multiple I-band 
and V-band images, suggesting that the redshift of the GRB is lower 
than roughly 4 or 5.  The overall behavior of the OA of GRB 080205 
is similar to that of GRB 060206 (Monfardini et al. 2006, ApJ, 
648, 1125).

This message may be cited.


GRB_name: GRB080205A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7255
SUBJECT: GRB 080205: Swift XRT refined analysis
DATE:    08/02/05 17:45:32 GMT
FROM:    Rhaana Starling at U of Leicester  <rlcs1@star.le.ac.uk>

R.L.C. Starling (U. Leicester) and C.B. Markwardt (CRESST/GSFC/UMD) report 
on behalf of the Swift XRT team:

Swift XRT observations of GRB 080205 (trigger=302506) began 101 seconds 
after the BAT trigger (Markwardt et al., GCN 7250) in Windowed Timing mode 
and continued in Photon Counting (PC) mode 208 s after the trigger. The 
enhanced XRT position is given in Osborne et al. GCN 7252.

The light curve out to 13.5 ks post-trigger can be fit with a power law 
with two breaks. The initial steep decay has a slope of alpha1 = 4.5+/-0.3 
breaking at Tbk1 = 203+20/-8 s to a plateau with slope alpha2 = 0.4+/-0.4. 
The plateau phase ends at Tbk2 = 570+170/-120 s and the decay continues 
with alpha3 = 1.8+/-0.1.

We fit the first orbit PC mode spectrum, totalling 1.5ks of data and 
covering T0+208s-T0+1728s, with an absorbed power law. We measure a photon 
index of Gamma = 1.8+/-0.2 and intrinsic absorption of N_H = (1.0+/-0.7)e21 
cm^-2 (at z=0), whilst fixing the Galactic absorption at 7.1e20 cm^-2 
(Kalberla et al. 2005). 
The 0.5-10 keV observed (unabsorbed) flux is 6e-11 (7.2e-11) erg/cm^2/s. 
The count rate to flux conversion is approximately 1 count/s = 4.7e-11 
erg/cm^2/s.

The predicted count rate at T+24h is 2e-4 counts/s, or 1e-14 erg/cm^2/s.

This is an official product of the Swift XRT team. 


GRB_name: GRB080204A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7256
SUBJECT: IPN localization of very hard GRB 080204
DATE:    08/02/05 17:57:16 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks
on behalf of the Konus-Wind team,

K. Hurley and T. Cline on behalf of the Mars Odyssey, Konus,
and MESSENGER GRB teams,

W. Boynton, C. Fellows, K. Harshman, C. Shinohara and R. Starr, on
behalf of the GRS-Odyssey GRB team,

I. G. Mitrofanov, D. Golovin, M. L. Litvak, and A. B. Sanin,
on behalf of the HEND-Odyssey GRB team,

K. Yamaoka, M. Ohno, Y. Fukazawa, T. Takahashi, M. Tashiro, Y. Terada,
T. Murakami, and K. Makishima on behalf of the Suzaku WAM team,

A. von Kienlin, G. Lichti, and A. Rau, on behalf of the
INTEGRAL SPI-ACS GRB team,

M. Marisaldi, F. Fuschino, M. Galli, C. Labanti,
E. Del Monte, F. Lazzarotto, L. Pacciani, P. Soffitta
on behalf of the AGILE team, and

J. Cummings, S. Barthelmy, N. Gehrels, and H. Krimm, on behalf of
the Swift-BAT team, report:

Mars Odyssey (GRS), Konus-Wind, Suzaku-WAM, INTEGRAL SPI-ACS,
AGILE-MCAL, SuperAGILE, and Swift-BAT observed the long-duration, hard 
spectrum GRB 080204 at about 50192 s UT (13:56:32). The burst was 
outside the coded field of view of the BAT and SuperAGILE.
The burst light curve shows a short precursor, followed in ~3 sec by a 
single multipeaked pulse with a duration of ~15 sec. There is a sign of 
extended emission seen up to T-T0~80 s in the Konus-Wind soft band.

We have triangulated the burst to the following, preliminary 3-sigma
error box:
-----------------------------------------------
    RA(2000), deg             Dec(2000), deg
-----------------------------------------------
Center:
  285.566 (19h 02m 16s)   -62.896 (-62d 53' 44")
Corners:
  287.728 (19h 10m 55s)   -62.334 (-62d 20' 01")
  283.813 (18h 55m 15s)   -63.453 (-63d 27' 12")
  283.277 (18h 53m 07s)   -63.402 (-63d 24' 08")
  287.212 (19h 08m 51s)   -62.305 (-62d 18' 18")
-----------------------------------------------

The error box area is 1212 sq. arcmin.
This error box may be improved

Preliminary analysis of the Konus-Wind data yields
a burst fluence of ~4x10^-5 erg/cm2 (in the 20 keV - 4 MeV range),
and a very hard energy spectrum with an Epeak of the main pulse
of ~1.4 MeV.

Detailed spectral parameters will be reported later.


GRB_name: GRB080205A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7257
SUBJECT: GRB 080205, Swift-BAT refined analysis
DATE:    08/02/05 18:38:21 GMT
FROM:    Takanori Sakamoto at NASA/GSFC  <Taka.Sakamoto@nasa.gov>

J. Cummings (GSFC/UMBC), S. D. Barthelmy (GSFC), E. Fenimore (LANL),
N. Gehrels (GSFC), H. Krimm (GSFC/USRA), C. Markwardt (GSFC/UMD),
D. Palmer (LANL), T. Sakamoto (GSFC/UMBC), G. Sato (GSFC/ISAS),
M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC), T. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+963 sec from the recent telemetry 
downlink, we report further analysis of BAT GRB 080205 (trigger #302506)
(Markwardt, et al., GCN Circ. 7250).  The BAT ground-calculated 
position is RA, Dec = 98.261, 62.782 deg which is 
   RA(J2000)  = 6h 33m 2.6s 
   Dec(J2000) = 62d 46' 56" 
with an uncertainty of 1.5 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 52%.
 
The mask-weighted light curve shows at least 3 peaks at about T+2, 
T+65, and T+93 sec.  T90 (15-350 keV) is 106.5 +- 5.0 sec (estimated 
error including systematics).
 
The time-averaged spectrum from T-10.1 to T+105.3 sec is best fit by a 
simple power-law model.  The power law index of the time-averaged 
spectrum is 2.08 +- 0.12.  The fluence in the 15-150 keV band is 
2.1 +- 0.1 x 10^-06 erg/cm2.  The 1-sec peak photon flux measured from 
T+0.22 sec in the 15-150 keV band is 1.4 +- 0.2 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/302506/BA/


GRB_name: GRB080205A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7258
SUBJECT: INT+WFC R-band observations of GRB 080205
DATE:    08/02/06 03:12:46 GMT
FROM:    Evert Rol at U.Leicester  <er45@star.le.ac.uk>

E. Rol (U. of Leicester) and J. Anderson (LJMU) report for a larger
collaboration:

We observed the position of GRB 080205 with the Isaac Newton Telescope 
equipped with the Wide Field Camera at Roque de Los Muchachos. 
Observations were carried out in R-band, for 30 minutes starting at 23:05 
UT.

We detect the afterglow with a magnitude of R = 23.50 +/- 0.11; our
photometry is calibrated to several USNO B1.0 R2 magnitudes.

Compared with the early (unfiltered) 17.0 magnitude KAIT measurement
(Li et al., GCN 7251), this indicates a slightly shallower powerlaw
decay than the initial -1.6 (Li et al, GCN 7254), suggestive of
underlying contamination by a host galaxy. At the source position,
however, there is no clear evidence for extended emission.


GRB_name: GRB080205A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7259
SUBJECT: VLA radio upper limit on GRB 080205
DATE:    08/02/06 12:41:08 GMT
FROM:    Poonam Chandra at U Virginia/NRAO  <pc8s@virginia.edu>

Poonam Chandra (NRAO/UVA) and Dale A. Frail (NRAO) report on
behalf of the Caltech-NRAO-Carnegie GRB Collaboration:

"We used the Very Large Array to observe the field of view toward GRB
080205 (GCN 7250) at a frequency of 8.46 GHz on 2008 February 6.13 UT. The
GRB is undetected and the peak radio flux at the SWIFT-XRT position (GCN
7252) is 30 +/- 41 uJy.

The National Radio Astronomy Observatory is a facility of the National
Science Foundation operated under cooperative agreement by Associated
Universities, Inc."


GRB_name: GRB080205A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7260
SUBJECT: GRB 080205: optical observation
DATE:    08/02/06 13:30:27 GMT
FROM:    Giuseppe Greco at U Bologna  <giuseppe.greco2@studio.unibo.it>

F. Terra, (Second University of Roma "Tor Vergata"), G. Greco,
C. Bartolini, A. Guarnieri, A. Piccioni (Bologna University),
D. Nanni(INAF/OAR and Second University of Roma "Tor Vergata"), 
G. Pizzichini (INAF/IASF Bologna), G. Gavazzi (Milano-Bicocca
University) and A. De Blasi (INAF Bologna) report:


We observed the field of GRB 080205  (Markwardt et al. GCN 7250)
with the 152 cm Loiano telescope under modest sky (cirrus)
and seeing (2.5") conditions.
Our observation was carried out in R-band, 
for 20 minutes starting on 2008 February 5, 22:28 UT.

We do not detect the OT reported by Li et al. (GCN 7251)
to a limiting magnitude of R ~ 20  based on the NOMAD catalog.


GRB_name: GRB080205A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7261
SUBJECT: GRB 080205: MASTER optical observation  
DATE:    08/02/06 14:37:12 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

D.Kuvshinov, V. Lipunov, V.Kornilov, E.Gorbovskoy, N.Tyurina, A.Belinski, 
A.Krylov, N.Shatskiy, A.Sankovich, V.Vladimirov,
  P.Gritsyk, V.Vibornov, A.Kuznetsov, P.Balanutsa
Sternberg Astronomical Institute, Moscow Union 'Optic'


MASTER  robotic system (http://observ.pereplet.ru) observed
GRB 080205  (GRB_TIME is 08:21:36 UT, Markwardt et al. GCN Circ 7250 ) in 
survey mode (the GRB was at day time for Moscow).
The weather was  good.
We have 31 images   from  16:22:35  to
17:24:46 (481 - 545 minutes   after the GRB time) with mean time:
16  54 UT (513 min  after GRB time).

The unfiltered image is calibrated relative to USNO A2.0 (0.8 R + 0.2 B).

The robot not find OT brighter then 19.5m  at KAIT's position (Li et 
al., GCN Circ 7251). 
Our limit is agreement with power low line between Li et al.,(GCN 
Circ 7254) and  Rol & Anderson (GCN CIRC 7258) observations.


This message can be cited.
Mailto: lipunov@sai.msu.ru


GRB_name: GRB080205A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7262
SUBJECT: GRB 080205 optical upper limit
DATE:    08/02/06 14:46:31 GMT
FROM:    AAVSO GRB Network at AAVSO  <matthewt@aavso.org>

Stefano Sposetti (Gnosca, Switzerland) reports to the AAVSO International 
High Energy Network the following optical observations of GRB080205 (GCN 
#7250, Markwardt et al.):

Stefano Sposetti reports an upper limit on the optical afterglow of 
GRB080205 reported by Li et al (GCN #7251).  The reported afterglow 
position was observed for a total of 7200 seconds using a 0.4-meter 
Newtonian with an SBIG ST8XE CCD and no filter.  Observations commenced on 
2008 February 05.74, approximately 9.5 hours after the Swift-BAT 
detection.  The afterglow was not detected, and an upper limit of CR=21.0 
was obtained with a S/N of 3, using USNO A2.0 magnitudes as comparisons. 
This upper limit is consistent with the R < 20 upper limit by Terra et al. 
(GCN #7260) at 2008 February 05.94, and the R = 23.5 detection at 2008 Feb 
05.96 by Rol et al. (GCN #7258).

A detailed report on these observations is available on the AAVSO website 
at ftp://ftp.aavso.org/grb/StefanoSposetti_GRB080205_2454502.86049_.txt

A fits image is available at
ftp://ftp.aavso.org/grb/StefanoSposetti_GRB080205_2454502.86049_.fits

The AAVSO thanks the Curry Foundation for their continued support of the
AAVSO International High Energy Network.


GRB_name: GRB080204A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7263
SUBJECT: Konus-Wind observation of GRB 080204
DATE:    08/02/06 17:11:20 GMT
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 long hard GRB 080204 (Golenetskii et al., GCN 7256)
triggered Konus-Wind at T0=50190.835 (13:56:30.835).

As observed by Konus-Wind the burst
had a fluence of 2.65(-0.47, +0.37)x10^-5 erg/cm2,
and a 64-ms peak flux measured from T0-0.032 s
of 9.52(-2.49, +2.25)x10^-6 erg/cm2/s
(both in the 20 keV - 6 MeV energy range).

The time-integrated spectrum of the burst
(not including the precursor; from T0 to T0+16.640 s)
is well fitted (in the 20 keV - 6 MeV range)
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with alpha = -1.35(-0.09, +0.06)
and Ep = 1279(-382, +469) keV (chi2 = 79.2/78 dof).

All the quoted errors are at the 90% confidence level.

The Konus-Wind light curve of this GRB is available
at http://www.ioffe.rssi.ru/LEA/GRBs/GRB080204_T50190/


GRB_name: GRB080207A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7264
SUBJECT: GRB 080207: Swift detection of a burst
DATE:    08/02/07 21:48:14 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

J. L. Racusin (PSU), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), P. J. Brown (PSU),
D. N. Burrows (PSU), J. R. Cummings (NASA/UMBC),
P. A. Evans (U Leicester), S. D. Hunsberger (PSU),
J. A. Kennea (PSU), C. B. Markwardt (CRESST/GSFC/UMD),
F. E. Marshall (NASA/GSFC), P. T. O'Brien (U Leicester),
D. M. Palmer (LANL), T. Sakamoto (NASA/UMBC),
R. L. C. Starling (U Leicester), M. C. Stroh (PSU) and
T. N. Ukwatta (GSFC/GWU) report on behalf of the Swift Team:

At 21:30:21 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 080207 (trigger=302728).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 207.513, +7.514 which is 
   RA(J2000)  = 13h 50m 03s
   Dec(J2000) = +07d 30' 50"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  This was an image-trigger, so the TDRSS
lightcurve show little activity. 

The XRT began observing the field at 21:32:25 UT, 124 seconds after the
BAT trigger. XRT found a bright, uncatalogued X-ray source
located at RA, Dec 207.5117, +7.5018 which is
   RA(J2000)  =  13h 50m 02.8s
   Dec(J2000) =  07d 30' 06.4"
with an uncertainty of 4.7 arcseconds (radius, 90% containment). 
This location is 44 arcseconds from the BAT on-board position,
within the BAT error circle. The initial flux in the 2.5s image
was 8.2e-09 erg/cm2/s (0.2-10 keV). 

 UVOT took a finding chart exposure of 55 seconds with the White
(160-650 nm) filter starting 140 seconds after the BAT trigger. No
afterglow candidate has been found in the initial data products. The
3 sigma upper limit at the XRT position is white > 20. No correction
has been made for the expected extinction corresponding to E(B-V) of
0.02. 

Burst Advocate for this burst is J. L. Racusin (racusin AT astro.psu.edu). 
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.)


GRB_name: GRB080207A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7265
SUBJECT: GRB 080207: Enhanced Swift-XRT position
DATE:    08/02/08 03:05:36 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.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 199 s of overlapping XRT Photon Counting mode and UVOT
V-band data for GRB 080207, 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 = 207.51253, +7.50245 which is equivalent
to:

RA (J2000): 13h 50m 3.01s
Dec (J2000): +07d 30' 08.8"

with an uncertainty of 2.9 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, astro-ph/0708.0986
http://www.swift.ac.uk/xrt_positions/Goad.pdf).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB080207A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7266
SUBJECT: GRB 080207: Swift-XRT Refined Analysis
DATE:    08/02/08 06:02:57 GMT
FROM:    Judith Racusin at PSU  <racusin@astro.psu.edu>

J. L. Racusin (PSU) reports on behalf of the Swift-XRT Team:

We have analysed the first 4 orbits of Swift-XRT data obtained for GRB
080207 (Racusin et al. GCN Circ. 7264), totaling 64 s of Windowed Timing
(WT) data and 5.7 ks of Photon Counting (PC) data.  The enhanced XRT
position is given in Beardmore et al. (GCN 7265).

The X-ray light-curve can be fit by a broken power-law with an initial
bright short flat phase with a a break at 205 +/- 73 sec followed by a
power-law with a decay slope of 1.5 +/- 0.1.

The WT data (133-197 seconds) can be modeled as an absorbed power-law with
photon index of 1.1 +/- 0.1 and a total absorbing column of NH = (85 +/-
10)e20 cm^-2.  The PC data (4.7-17.1 ks) can be modeled as an absorbed
power-law with photon index of 2.4 +/- 0.2 and a total absorbing column of
NH = (75 +/- 17)e20 cm^-2.  Both fits are in excess of the Galactic value
of 1.95e20 cm^-2. The 0.3-10 keV observed (unabsorbed) flux during this
time is 5.80e-9 (5.81e-9) erg cm^-2 s^-1 and 1.15e-11 (1.16e-11) erg cm^-2
s^-1 for WT and PC, respectively.

Assuming the source continues to decay with the same decay index of 1.5,
we predict an XRT count rate of 7.6e-3 counts/s at T+24 hours, which
corresponds to an 0.3-10.0 keV observed flux of 6.6e-13 ergs cm^-2 s^-1.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB080207A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7267
SUBJECT: GRB 080207: TAROT Calern observatory optical observations
DATE:    08/02/08 06:36:15 GMT
FROM:    Alain Klotz at CESR-CNRS  <Alain.Klotz@free.fr>

Klotz, A. (CESR-OMP), Boer M. (OHP), Atteia J.L. (LATT-OMP) report:

We imaged the field of GRB 080207 detected by SWIFT
(trigger 302728) with the TAROT robotic telescope (D=25cm)
located at the Calern observatory, France.

Although the notice was received 100s after the trigger,
the observations started 1075s later
because the field was not risen at Calern during the burst.
First images are two low in elevation.
Stars become detectable on images ~1500s after the trigger.
Weather conditions were excellents.

The date of trigger : t0 = 2008-02-07T21:30:21
No afterglow was found at position delivered by
Beardmore et al. (GCNC 7265):

t0+1563s to t0+1653s : R > 14.3 (elevation 2.5)
t0+1670s to t0+1760s : R > 14.9 (elevation 2.8)
t0+3388s to t0+3568s : R > 16.2 (elevation 8)
t0+3388s to t0+7526s : R > 19.0 (elevation 20)

Magnitudes were estimated with the nearby USNO-B1 stars
and are not corrected for galactic dust extinction.

This message may be cited.


GRB_name: GRB080207A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7268
SUBJECT: GRB080207: Swift/UVOT refined analysis
DATE:    08/02/08 07:18:30 GMT
FROM:    Antonino Cucchiara at PSU  <cucchiara@astro.psu.edu>

A. Cucchiara (PSU), J. Racusin (PSU)
report on behalf of the Swift-UVOT team:

The Swift/UVOT observed the field of GRB080207 (trigger #302728)
starting 55 sec days after the BAT detection (Racusin et
al. 2008, GCN Circ. 7264). We do not find any new source in any
of the UVOT coadded observations inside the XRT enhanced error
circle (Beardmore et al. 2008, GCN Circ. 7265).

The 3-sigma upper limits (in the UVOT photometric system,
Breeveld et al., GCN Circ. 6614) are listed.

Filter     Tstart   Tstop     Exp    Upper limit  
             (s)      (s)     (s)           
white        55      11428   1167      22.40
v          4733      13063   1097      20.50
b          5553      16909    983      21.53
u          5347       6982    393      20.57
uvw1       5143       6777    393      20.75
uvm2       4937       6572    393      20.58
uvw2       5963      12334   1082      21.62

The values quoted above are not corrected for the expected Galactic
extinction corresponding to a reddening of E_{B-V} = 0.02  mag in the
direction of the burst (Schlegel et al. 1998).


GRB_name: GRB080207A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7269
SUBJECT: GRB 080207: REM NIR observations
DATE:    08/02/08 09:19:43 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

P. D'Avanzo, L.A. Antonelli, S. Covino, D. Fugazza, L.  Calzoletti, S. 
Campana, G.  Chincarini, M.L. Conciatore, S. Cutini, V. D'Elia, F. 
Dalessio, F.  Fiore, P. Goldoni, D. Guetta,  C. Guidorzi, G.L. Israel, 
N. Masetti, A. Melandri, E. Meurs, L. Nicastro, E. Palazzi, E. Pian, S. 
Piranomonte, L.  Stella, G.  Stratta, G. Tagliaferri, G. Tosti, V.Testa, 
S.D. Vergani,  F. Vitali report on behalf of the REM team:

The robotic 60-cm REM telescope located at La Silla (Chile) observed 
automatically the field of the GRB 080207 (Racusin et al., GCN 7264). A 
preliminary analysis of the first set of JHK exposures does not reveal 
any optical afterglow candidate inside the XRT error box (Beardmore et 
al., GCN 7265)  We derive the following 3sigma upper limits (calibrated 
against the 2MASS catalog):

J > 16.7 (7.8 hours after the burst)
H > 15.9 (7.7 hours after the burst)
K > 13.9 (10.1 hours after the burst)


GRB_name: GRB080207A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7270
SUBJECT: GRB080207: RTT150 Optical Observations
DATE:    08/02/08 12:21:20 GMT
FROM:    Irek Khamitov at TUG  <irekk@tug.tug.tubitak.gov.tr>

I. Khamitov (TUG), O. Kose, K.Yakut (Ege Uni.),
Z. Eker (TUG), U. Kiziloglu (METU), E. Gogus (Sabanci Uni.)
I. Bikmaev, N. Sakhibullin (KSU/AST)
R. Burenin, M. Pavlinsky, R. Sunyaev (IKI),

report:

We have observed field of the GRB080207 (trigger=302728, GCN Circ. 7264) 
with Russian-Turkish 1.5-m telescope  (RTT150, Bakirlitepe, TUBITAK 
National Observatory, Turkey) 07 Feb between 22:04UT and 22:27UT, i.e. 
starting about 34 min after the burst, using ANDOR CCD.

Series of 20*30sec direct images in Rc band were taken. We found no 
afterglow candidate inside of XRT error circle. Using USNO-B1 stars we 
estimated limiting magnitude of the co-added frame as R~21.8 mag.

The finding chart can be found at:
http://hea.iki.rssi.ru/grb/080207/indexeng.html


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GRB_name: GRB080207A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7272
SUBJECT: GRB 080207, Swift-BAT refined analysis
DATE:    08/02/08 15:19:29 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

M. Stamatikos (GSFC/ORAU), S. D. Barthelmy (GSFC), J. Cummings (GSFC/UMBC),
E. Fenimore (LANL), N. Gehrels (GSFC), H. Krimm (GSFC/USRA),
C. Markwardt (GSFC/UMD), D. Palmer (LANL), J. L. Racusin (PSU),
T. Sakamoto (GSFC/UMBC), G. Sato (GSFC/ISAS), J. Tueller (GSFC),
T. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+963 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 080207 (trigger #302728)
(Racusin, et al., GCN Circ. 7264).  The BAT ground-calculated position is
RA, Dec = 207.514, 7.492 deg which is 
   RA(J2000)  = 13h 50m 3.3s 
   Dec(J2000) =  7d 29' 32" 
with an uncertainty of 1.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.
 
The mask-weighted light curve shows a long smooth rise starting at ~T-20 sec,
peaking around T+100 sec, then dropping to a minimum around T+200 sec,
then rising again out to T+320 sec at which point the location went out
of the BAT FOV when the spacecraft slewed to a new target.
T90 (15-350 keV) is >300 sec (estimated error including systematics).
 
The time-averaged spectrum from T+4.7 to T+332.9 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 1.17 +- 0.27, 
and Epeak of 107.8 +- 72.5 keV (chi squared 51.31 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 6.1 +- 0.2 x 10^-06 erg/cm2
and the 1-sec peak flux measured from T+330.34 sec in the 15-150 keV band is
1.0 +- 0.3 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.58 +- 0.06 (chi squared 57.73 for 57 d.o.f.).  All the quoted errors
are at the 90% confidence level. 

The BAT characteristics of this burst, particularly the long smooth 
lightcurve, suggest that it might be at high redshift, but the high 
absorption of the XRT spectrum (Racusin et al. GCN 7266) make it unlikely.
 
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/302728/BA/
 


GRB_name: GRB080207A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7273
SUBJECT: GRB 080207: Super-LOTIS observations
DATE:    08/02/08 15:28:43 GMT
FROM:    Adria C. Updike at Clemson U  <aupdike@clemson.edu>

A. C. Updike (Clemson University), P. A. Milne (U Arizona), G. G.
Williams (MMTO), and D. H. Hartmann (CU) report on behalf of the
Super-LOTIS team:

The 0.6m Super-LOTIS telescope began observations of the field of GRB
080207 (Racusin et al., GCN 7264) approximately 13 hours and 16 min
after the trigger. Observations consisted of 58x60 second exposures in
the R band, under decent weather conditions.

No afterglow was detected within the XRT refined error circle (Beardmore
et al., GCN 7265) down to a limiting magnitude of 20.8 (as derived from
USNO B1.0 R2 magnitudes upon comparison to field stars).

This message may be cited.


GRB_name: GRB080205A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7275
SUBJECT: GRB 080205: RTT150 optical observations
DATE:    08/02/08 21:02:03 GMT
FROM:    Rodion Burenin at IKI, Moscow  <rodion@hea.iki.rssi.ru>

R. Burenin, A. Tkachenko, M. Pavlinsky, R. Sunyaev (IKI),  
I. Khamitov, Z. Eker (TUG), U. Kiziloglu (METU), E. Gogus (Sabanci Uni.),
I. Bikmaev, N. Sakhibullin (KSU/AST)

report:

The optical counterpart of GRB 080205 (Li et al., GCN 7251) was observed
with Russian-Turkish 1.5-m telescope (RTT150, Bakirlitepe, TUBITAK National
Observatory, Turkey). We made two sets of BVRI images on Feb 05
approximately at 18:00 and 22:00 UT (10 and 14 hours after the burst). The
afterglow is detected near the limit of our images, i.e. near about R=23.5
(USNO B1.0 calibrated), in agreement with later INT observation (Rol and
Anderson, GCN 7258).


GRB_name: GRB080207A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7276
SUBJECT: GRB 080207:  Optical limits from Gemini-South 
DATE:    08/02/08 22:42:28 GMT
FROM:    Antonino Cucchiara at PSU  <cucchiara@astro.psu.edu>

A. Cucchiara and D. B. Fox (PSU) reports on behalf of a larger
collaboration:

"We have imaged the field of GRB 080207 (Racusin et al., GCN 7264)
with the Gemini South + GMOS in griz bandds starting at 0.41 days
after the trigger.

We took a sequence of 5x 180s images in each band (total exposure
900s).  Our co-added images do not reveal any source inside the XRT
refined error circle (Beardmore et al., GCN 7265).  Using three
objects from the SDSS catalog to establish photometric zero-points, we
calculate the following 2-sigma upper limits on the emission of any
optical afterglow + host galaxy: g > 24.1 mag, r > 24.5 mag, i > 24.2
mag, z > 25.0 mag."


GRB_name: GRB080207A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7277
SUBJECT: GRB 080207, Swift-BAT refined analysis
DATE:    08/02/09 00:55:04 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <jayc@milkyway.gsfc.nasa.gov>

M. Stamatikos (GSFC/ORAU), S. D. Barthelmy (GSFC),
J. Cummings (GSFC/UMBC), E. Fenimore (LANL), N. Gehrels (GSFC),
H. Krimm (GSFC/USRA), C. Markwardt (GSFC/UMD), D. Palmer (LANL),
J. L. Racusin (PSU), T. Sakamoto (GSFC/UMBC), G. Sato (GSFC/ISAS),
J. Tueller (GSFC), T. Ukwatta (GWU)
(i.e. the Swift-BAT team):

Using the data set from T-239 to T+963 sec from the recent telemetry
downlink, we report further analysis of BAT GRB 080207 (trigger #302728)
(Racusin, et al., GCN Circ. 7264).  The BAT ground-calculated position
is RA, Dec = 207.514, 7.492 deg which is
   RA(J2000)  = 13h 50m 3.3s
   Dec(J2000) =  7d 29' 32"
with an uncertainty of 1.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.

The mask-weighted light curve shows a long smooth rise starting at
~T-20 sec, peaking around T+100 sec, then dropping to a minimum around
T+200 sec, then rising again out to ~T+340 sec at which point the 
location went out of the BAT FOV when the spacecraft slewed to a new
target.  Based on the raw counting rates, which are somewhat sensitive
to photons through the side of the instrument, there was not significant
emission above about 50 keV after this time.  T90 (15-350 keV) is 
340 +- 20 sec (estimated error including systematics).

The time-averaged spectrum from T+4.7 to T+332.9 sec is best fit by a
power law with an exponential cutoff.  This fit gives a photon index
1.17 +- 0.27, and Epeak of 107.8 +- 72.5 keV (chi squared 51.31 for
56 d.o.f.).  For this model the total fluence in the 15-150 keV band is
6.1 +- 0.2 x 10^-06 erg/cm2 and the 1-sec peak flux measured from
T+330.34 sec in the 15-150 keV band is 1.0 +- 0.3 ph/cm2/sec.  A fit to
a simple power law gives a photon index of 1.58 +- 0.06 (chi squared
57.73 for 57 d.o.f.).  All the quoted errors are at the 90% confidence
level.

The BAT characteristics of this burst, particularly the long smooth
lightcurve, suggest that it might be at high redshift, but the high
absorption of the XRT spectrum (Racusin et al. GCN 7266) make it
unlikely.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/302728/BA/


GRB_name: GRB080205A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7278
SUBJECT: GRB 080205: GAO 150cm telescope Optical limit
DATE:    08/02/09 12:31:49 GMT
FROM:    Kenzo Kinugasa at Gunma Astro. Obs/Japan  <kinugasa@astron.pref.gunma.jp>

K. Kinugasa (Gunma Astronomical Observatory)  report:

 The field of GRB 080205 (Markwardt et al. GCN 7250) was observed
with the 150 cm telescope of the Gunma Astronomical Observatory.
Starting at 14:42 UT (6.35 hours after the burst), Rc, and Ic frames
were acquired for 15 and 18 minutes, respectively.

 We do not identify the optical counterpart reported by Li et al. (GCN 7251).
to limiting magnitudes of R~20 and I~18 relative to USNO-B1.0 magnitudes.


GRB_name: GRB080207A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7279
SUBJECT: GRB 080207: GROND upper limits
DATE:    08/02/09 22:48:33 GMT
FROM:    Jochen Greiner at MPI  <jcg@mpe.mpg.de>

A. Kuepcue Yoldas, A. Yoldas, J. Greiner, T. Kruehler (all MPE Garching),
S. Klose (Tautenburg Obs), G. Szokoly (Budapest Univ.) report for the
GROND team:

We observed the field of GRB 080207 detected by Swift/BAT (Racusin et al.
2008, GCN 7264)  simultaneously in grizJHK with GROND (Greiner et al. 2008,
astro-ph/0801.4801), mounted at the 2.2m MPI/ESO telescope at La Silla (Chile).
Observations started on Feb. 08, at 06:35 UT, about 9 hrs after the GRB,
under poor conditions (particularly high humidity and airmass of 1.7-1.34).

No source is detected within the 3-sigma XRT error circle (Beardmore et al.
2008, GCN 7265). Comparison of the co-added images (with 3440 sec effective
exposure time in griz and 2400 seconds in JHK) to the Digital Sky Survey 
and 2MASS yields the following 3-sigma upper limits:
g' > 23.9,  r' > 23.8,  i' > 23.5,  z' > 22.8,  J > 21.0,  H > 19.7,  K > 19.0.


GRB_name: GRB080210A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7280
SUBJECT: GRB 080210: TAROT La Silla observatory optical detection
DATE:    08/02/10 08:17:14 GMT
FROM:    Alain Klotz at CESR-CNRS  <Alain.Klotz@free.fr>

Klotz, A. (CESR-OMP), Boer M. (OHP), Atteia J.L. (LATT-OMP) report:

We imaged the field of GRB 080210 detected by SWIFT
(trigger 302888) with the TAROT robotic telescope (D=25cm)
located at the European Southern Observatory,
La Silla observatory, Chile.

The observations started 345.9s after the GRB trigger
(11.2s after the notice). The elevation of the field was at
from 15 degrees above horizon and weather conditions
were good.

We detect a new fading source in the error box given by SWIFT
We detected the candidate couterpart not present in the DSS
at the following position (+/- 1 arcsec):

RA(J2000) = 16h 45m 03.97s
DEC(J2000) +13d 49' 35"

OT was R~16.2 at 345.9s after GRB.

Magnitudes were estimated with the nearby USNO-B1 stars
and are not corrected for galactic dust extinction.

N.B. Galactic coordinates are lon= 31.6032 lat=+34.1725
and the galactic extinction in R band is 0.2 magnitudes
estimated from D. Schlegel et al. 1998ApJ...500..525S.

This message may be cited.


GRB_name: GRB080210A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7281
SUBJECT: GRB 080210: Swift detection of a burst with optical afterglow
DATE:    08/02/10 08:27:08 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

D. Grupe (PSU), W. H. Baumgartner (GSFC/UMBC), M. M. Chester (PSU),
N. Gehrels (NASA/GSFC), E. A. Hoversten (PSU),
C. B. Markwardt (CRESST/GSFC/UMD), D. M. Palmer (LANL),
A. M. Parsons (GSFC), M. Stamatikos (NASA/ORAU) and M. C. Stroh (PSU)
report on behalf of the Swift Team:

At 07:50:05 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 080210 (trigger=302888).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 251.270, +13.830 which is 
   RA(J2000) = 16h 45m 05s
   Dec(J2000) = +13d 49' 49"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single-peak
with substructure with a duration of about 35 sec.  The peak count rate
was ~2000 counts/sec (15-350 keV), at ~10 sec after the trigger.  This
was an image trigger, but with a clear light curve. 

The XRT began observing the field at 07:54:08 UT, 243 seconds after the
BAT trigger. XRT found a bright, uncatalogued X-ray source
located at RA, Dec 251.2679, +13.8254 which is
   RA(J2000)  =  16h 45m 04.3s
   Dec(J2000) =  13d 49' 31.4"
with an uncertainty of 4.6 arcseconds (radius, 90% containment). 
This location is 18.1 arcseconds from the BAT on-board position,
within the BAT error circle. 

UVOT took a finding chart exposure of 100 seconds with the White
(160-650 nm) filter starting 160 seconds after the BAT trigger, and
an exposure of 193 seconds with the v filter starting 266 seconds
after the trigger. There is a candidate afterglow in the rapidly
available 2.7'x2.7' sub-image at RA, Dec = 251.2667, +13.8267 (white)
which is   
     RA(J2000) = 16:45:04.01    
     DEC(J2000) = +13:49:36.1 
with a 1-sigma error radius of about 0.6 arc sec. This position 
is 6.3 arcseconds from the center of the XRT error circle. The 
estimated magnitude is 18.0 in white and 17.6 in v with 
1-sigma errors of about 0.5 mag. The positions agree in both 
white and v. No correction has been made for the expected 
extinction corresponding to E(B-V) of 0.08. 

Burst Advocate for this burst is D. Grupe (grupe AT astro.psu.edu). 
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.)


GRB_name: GRB080210A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7282
SUBJECT: GRB080210 - SDSS Pre-Burst Observations
DATE:    08/02/10 09:00:47 GMT
FROM:    Richard J. Cool at U.of AZ/Steward Obs  <rcool@as.arizona.edu>

Richard J. Cool (Arizona), Daniel J. Eisenstein (Arizona), David W. Hogg
(NYU), Michael R. Blanton (NYU), David J. Schlegel (LBNL), J. Brinkmann
(APO),
Donald Q. Lamb (Chicago), Donald P. Schneider (PSU), and Daniel E. Vanden
Berk
(PSU) report:

The Sloan Digital Sky Survey (SDSS) imaged the field of burst GRB080210
prior to the burst.  As these data should be useful as a pre-burst comparison
and for calibrating photometry, we are supplying the images and photometry
measurements for this GRB field to the community.

Data from the SDSS, including 5 FITS images, 3 JPGS, and
3 files of photometry and astrometry, are being placed at
http://mizar.as.arizona.edu/~grb/public/GRB080210

We supply FITS images in each of the 5 SDSS bands of a 8'x8' region centered
on the GRB position (ra=251.270 (16:45:04.8), dec=13.8300 (13:49:48.0);
Swift Trigger 302888), as well as 3 gri color-composite JPGs (with different
stretches). The units in the FITS images are nanomaggies per pixel.  A pixel
is 0.396 arcsec on a side. A nanomaggie is a flux-density unit equal to
10^-9 of a magnitude 0 source or, to the extent that SDSS is an AB system,
3.631e-6 Jy.  The FITS images have WCS astrometric information.

In the file GRB080210_sdss.calstar.dat, we report photometry and astrometry
of 722 bright stars (r<20.5) within 15' of the burst location.  The
magnitudes
presented in this file are asinh magnitudes as are standard in the SDSS
(Lupton
1999, AJ, 118, 1406). Beware that some of these stars are not well-detected
in the u-band; use the errors and object flags to monitor data quality.

In the files GRB080210_sdss.objects_flux.dat and
GRB080210_sdss.objects_magnitudes.dat, we report photometry of 1246
objects detected within 6' of the GRB position.  We have removed saturated
objects and objects with model magnitudes fainter than 23.0 in the r-band.
The fluxes listed in GRB080210_sdss.objects_flux.dat are in nanomaggies
while the magnitudes listed in GRB080210_sdss.objects_magnitudes.dat are
asinh magnitudes.

**Be aware that at least a portion of the photometry provided in this release
has been flagged as non-photometric. As photometry for objects with this
flag set may have non-optimal calibration, we do not recommend these objects
be used for photometric calibration.  Non-photometric imaging may still be
valuable as a pre-burst comparison and for astrometric calibration.

All quantities reported are standard SDSS photometry, meaning that they are
very close to AB zeropoints and magnitudes are quoted in asinh magnitudes.
Photometric zeropoints are known to about 2% rms.  None of the photometry
is corrected for dust extinction.  The Schlegel, Finkbeiner, and Davis
(1998) predictions for this region are A_U=0.401 mag, A_g=0.295 mag, A_r =
0.214 mag, A_i=0.162 mag, and A_z=0.115 mag.

There are currently no objects within 6 arcminutes of the GRB position in
the SDSS spectroscopic database.


SDSS astrometry is generally better than 0.1 arcsecond per coordinate.
Users requiring high precision astrometry should take note that the SDSS
astrometric system can differ from other systems such as those used in other
notices; we have not checked the offsets in this region.

More detailed information pertaining to our SDSS GRB releases can be found
in our initial data release paper (Cool et al. 2006, PASP 118, 733).  See the
SDSS DR4 documentation for more details: http://www.sdss.org/dr5.

These data have been reduced using a slightly different pipeline than that
used for SDSS public data releases.  We cannot guarantee that the values here
will exactly match those in the data release in which these data are
included.
In particular, we expect the photometric calibrations to differ by of order
0.01 mag.

This note may be cited, but please also cite the SDSS data release paper,
Adelman-McCarthy et al. (2007, ApJS, 172, 634), when using the data or
referring to the technical documentation.


GRB_name: GRB080210A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7283
SUBJECT: GRB 080210: GOND detection in all bands and redshift upper limit
DATE:    08/02/10 10:06:35 GMT
FROM:    Jochen Greiner at MPI  <jcg@mpe.mpg.de>

A. Kuepcue Yoldas, A. Yoldas, J. Greiner (all MPE Garching),
S. Klose (Tautenburg Obs), report for the GROND team:

We observed the field of GRB 080210 detected by Swift/BAT (Grupe et al.
2008, GCN 7281)  simultaneously in grizJHK with GROND (Greiner et al. 2008,
astro-ph/0801.4801), mounted at the 2.2m MPI/ESO telescope at La Silla (Chile).
Observations started on Feb. 10, at 09:00 UT (1 hr after the GRB),
when the GRB location was becoming visible at 20 degrees above horizon.

We detect the optical afterglow reported by Klotz et al. (2008, GCN 7280) 
and Grupe et al. (2008, GCN 7281) in all filters. At 9:02 UT we measure 
g'=20.97, r'=19.9, i'=19.61, z'=19.52, J=17.2, H=16.4 and K=15.6, with 
errors of +-0.04 in the g'r'i'z' bands, and 0.13 in JHK. The g'-r' color 
is consistent with the Ly-break being below the g'-band. Thus, the
redshift is smaller than 3.5, despite the possible expectation from the
long T90 duration of the GRB (and being an image trigger).

The afterglow has clearly faded since the TAROT and UVOT measurements, and
also continues to fade since the start of our observations.


GRB_name: GRB080210A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7284
SUBJECT: GRB 080210: Rapid PROMPT Detections
DATE:    08/02/10 10:21:04 GMT
FROM:    Thomas Summers Brennan at UNC/GRB Group  <bre@email.unc.edu>

T. Brennan, J. Haislip, D. Reichart, M. Nysewander, A. LaCluyze, K. 
Ivarsen, J. A. Crain, A. Foster, M. Schubel, J. Styblova, and A. Trotter 
report:

Skynet observed the localization of GRB 080210 (Grupe et al., GCN 7281) 
with two of the 16" PROMPT telescopes at CTIO beginning 362 seconds 
after the trigger (27 seconds after notification) in VRI.

We detect the afterglow (Klotz et al., GCN 7280) in all filters.  At 382 
seconds after the burst, we measure V ~ 17.4 mag (calibrated to 2 NOMAD 
stars).


GRB_name: GRB080210A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7285
SUBJECT: GRB 080210: Enhanced Swift-XRT position
DATE:    08/02/10 11:56:08 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.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 193 s of overlapping XRT Photon Counting mode and UVOT
V-band data for GRB 080210, 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 = 251.26693, +13.82656 which is equivalent
to:

RA (J2000): 16h 45m 4.06s
Dec (J2000): +13d 49' 35.6"

with an uncertainty of 2.5 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, astro-ph/0708.0986
http://www.swift.ac.uk/xrt_positions/Goad.pdf).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB080210A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7286
SUBJECT: GRB 080210: VLT redshift
DATE:    08/02/10 12:22:25 GMT
FROM:    Pall Jakobsson at U Hertfordshire  <P.Jakobsson@herts.ac.uk>

Pall Jakobsson (U. Hertfordshire), Paul M. Vreeswijk, Daniele Malesani
(DARK, NBI), Andreas O. Jaunsen (U. Oslo), Johan P. U. Fynbo, Jens
Hjorth (DARK, NBI) and Nial R. Tanvir (U. Leicester) report on behalf
of a larger collaboration:

Using FORS2 on the Very Large Telescope, we have obtained a 10 min
spectrum (grism 300V) of the optical afterglow of GRB 080210 (Grupe et
al., GCN 7281).

The acquisition image shows the UVOT optical afterglow candidate to
have R = 18.8 on Feb 10.351 UT (0.597 hours after the GRB) using
photometric zeropoints from the ESO webpages. We also obtained an
R-band image at 1.65 hours after the GRB indicating a decay index of
0.76 +/- 0.04.

The spectrum is rich in absorption features, including Ly-alpha, Si II, 
C II, Si IV, C IV, Fe II and Al II, corresponding to a redshift of
z = 2.641. This is consistent with the redshift upper limit (z < 3.5)
reported by GROND (Kuepcue Yoldas et al., GCN 7283). There is also a
tentative detection of Ly-alpha in emission superimposed on the DLA
trough.

We thank the Paranal staff for excellent support, especially Paul
Lynam.


GRB_name: GRB080210A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7287
SUBJECT: GRB 080210: Swift-XRT Refined Analysis 
DATE:    08/02/10 13:39:47 GMT
FROM:    Dirk Grupe at PSU/Swift-XRT  <grupe@astro.psu.edu>

D. Grupe (PSU) reports on behalf of the Swift-XRT Team:

We have analyzed the first 2 orbits of Swift-XRT data obtained for GRB
080210 (Grupe et al. GCN Circ. 7281), totaling 78 s of Windowed Timing
(WT) data and 668 s of Photon Counting (PC) data.  The enhanced XRT
position is given in Evans et al. (GCN 7285).

In correction to GCN 7281, XRT started observing the burst 153s after the
trigger.
The X-ray light-curve shows a bright flare at the beginning of the 
observations
with an initial decay slope of 7.5+/-0.9 followed by a plateau phase 
starting at
290+/-20s after the burst with a decay slope of 0.76+/-0.07.

The WT data (158-232 s after burst) can be modeled as an absorbed 
power-law with
photon index of 2.85  0.25 and a free-fit absorbing column of NH = 
(21.5 +4.8
-5.4)e20 cm^-2 which is in excess of the Galactic value (5.47e20 cm^-2, 
Dickey &
Lockman 1990). The PC mode data are consistent with this result.


Assuming the source continues to decay with the same decay index of 0.76,
we predict an XRT count rate of 0.03 counts/s at T+24 hours, which
corresponds to an 0.3-10.0 keV observed flux of 8.3e-13 ergs cm^-2 s^-1.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB080210A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7288
SUBJECT: GRB 080210: Super-LOTIS observations
DATE:    08/02/10 14:14:49 GMT
FROM:    Adria C. Updike at Clemson U  <aupdike@clemson.edu>

A. C. Updike (Clemson University), G. G. Williams (MMTO), P. A. Milne
(Steward Observatory), and D. H. Hartmann (CU) report on behalf of the
Super-LOTIS Collaboration:

The robotic 0.6-m Super-LOTIS telescope began observing the error box of
GRB 080210 (Swift Trigger 302888, Grupe et al. GCN 7281) at 11:33:46.1 UT,
3 hours and 44 minutes after the trigger.  Our observations consist of 57
x 60s exposures in the R-band under good weather conditions.

We detect the afterglow reported by Klotz et al. (GCN 7280) in our stacked
images.  Using 5 field stars from the USNO-B1.0 catalogue, we estimate the
following R-band magnitude for the OT:

t_start (UT) exp t (s) t_start-t_0 (s) R Mag
----------------------------------------------------------------
11:33:46.1  3420             11166   R = 21.6 +/- 0.2

Additional observations and analysis are ongoing.  This message may be cited.


GRB_name: GRB080210A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7289
SUBJECT: GRB 080210, Swift-BAT refined analysis
DATE:    08/02/10 17:34:35 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

T. Ukwatta (GWU) S. D. Barthelmy (GSFC), J. Cummings (GSFC/UMBC),
E. Fenimore (LANL), N. Gehrels (GSFC), D. Grupe (PSU),
H. Krimm (GSFC/USRA), C. Markwardt (GSFC/UMD), D. Palmer (LANL),
A. Parsons (GSFC), T. Sakamoto (GSFC/UMBC), G. Sato (GSFC/ISAS),
M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+963 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 080210 (trigger #302888)
(Grupe, et al., GCN Circ. 7281).  The BAT ground-calculated position is
RA, Dec = 251.259, 13.826 deg, which is 
   RA(J2000)  = 16h 45m 02.0s 
   Dec(J2000) = 13d 49' 35" 
with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 73%.
 
The mask-weighted light curve shows 3-4 overlapping peaks starting at ~T-16 sec,
peaking at ~T+5 sec, and ending at ~T+33 sec.
T90 (15-350 keV) is 45 +- 11 sec (estimated error including systematics).
 
The time-averaged spectrum from T-14.6 to T+47.7 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.77 +- 0.12.  The fluence in the 15-150 keV band is 1.8 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+4.50 sec in the 15-150 keV band
is 1.6 +- 0.2 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/302888/BA/

[GCN OPS NOTE(10feb08): Per request, AP was added to the author list.]


GRB_name: GRB080210A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7290
SUBJECT: GRB 080210: Hobby-Eberly Telescope Absorption Spectroscopy
DATE:    08/02/10 20:01:00 GMT
FROM:    Antonino Cucchiara at PSU  <cucchiara@astro.psu.edu>

A. Cucchiara and D. B. Fox (PSU) report on behalf of a larger
collaboration:

"Starting on 2008 Feb 10.49 UT we used the Marcario LRS spectrograph
on the Hobby-Eberly Telescope to obtain 2x 1200s spectra of the
optical afterglow (Klotz, Boer & Atteia, GCN 7280) of GRB 080210
(Grupe et al., GCN 7281).  The coadded spectrum covers the wavelength
range 4100 to 10,500 Ang.  We clearly detect a Ly-alpha absorption
feature as well as several metal features corresponding to FeII, SiII,
CIV, AlII, MnII, the MgII doublet, and MgI at a redshift of z=2.64. No
clear emission lines are evident in our spectrum.  Our observations
are consistent with the redshift and features reported by Jakobsson et
al. (GCN 7286).  We thank HET Resident Astronomer John Caldwell for
performing this observation."


GRB_name: GRB080207A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7291
SUBJECT: GRB 080207: optical observations.
DATE:    08/02/11 16:43:59 GMT
FROM:    Javier Gorosabel at IAA-CSIC  <jgu@dfe-d14.iaa.csic.es>

V. Muoz Marn, J. Sabater, A.J. Castro-Tirado, J. Gorosabel, M.
Jelnek (IAA-CSIC), A. de Ugarte Postigo (ESO, Santiago), report:

"We carried out BVRI-band observations of the GRB 080207 XRT enhanced
position of (Beardmore et al., GCN 7265) with the 2.5m NOT(+MOSCA) at
Roque de los Muchachos observatory. A preliminary analysis reveals no
optical source in the XRT error circle brighter than R~23.5 at Feb
8.26389-8.27778 UT (8.83 - 9.16 hours after the GRB)."


GRB_name: GRB080210A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7292
SUBJECT: GRB 080210: Swift/UVOT Refined Analysis
DATE:    08/02/11 22:57:46 GMT
FROM:    Frank Marshall at GSFC  <marshall@milkyway.gsfc.nasa.gov>

F.E. Marshall (NASA/GSFC) and D. Grupe (PSU)
report on behalf of the Swift team:

The Swift/UVOT observed the field of GRB 080210 (trigger 302888)
starting 160 seconds  after the BAT trigger 
(Grupe et al., GCN Circ. 7281), which occurred at 07:50:05 UT.
A bright afterglow was seen in the initial 
exposures with the White and V filters
at a position of RA (J2000) of 16h45m04.01s and Dec (J2000) of  
+13o49'35.9" (J2000) with an estimated 90% confidence error radius
of 0.6". This position is consistent with the optical
position reported by Klotz et al. (GCN Circ. 7280) and
the enhanced XRT position reported by Evans et al. (GCN Circ. 7285).
There was no 3-sigma detection of the afterglow in
any subsequent exposure in any of the UVOT filters.
The non-detections in the UV filters is consistent with
the redshift of 2.641 reported by Jakobsson et al. 
(GCN Circ. 7286). The lack of detection in the second
exposure with the White filter indicates a decay slope
of steeper than -0.7 assuming a power law decay model.

The detections and 3-sigma upper limits in the UVOT photometric
system (Poole et al. MNRAS 383, 627 (2008)) are summarized in
the following table:

Filter T_start(s) T_stop(s) Exposure(s)  Mag/3-sigma UL

white    160         260      98         18.2 +/- 0.1
white   6081        6244     161        >20.5
v        267         460     190         17.6 +/- 0.1
b       5877       64094    2625        >21.2
u       5671       69878    4779        >21.3
uvw1    3846       69140    5453        >22.3
uvm2    3639       68241    4447        >21.8
uvw2    9469       74958    4171        >22.3

The values quoted above are not corrected for the expected Galactic 
extinction corresponding to a reddening of E(B-V) = 0.08 mag 
in the direction of the burst (Schlegel et al. 1998). 


GRB_name: GRB080207A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7293
SUBJECT: GRB 080207: VLT NIR early upper limits 
DATE:    08/02/12 09:53:52 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

D. Fugazza (INAF-OAB), V. D'Elia (INAF-OAR), P. D'Avanzo, S. Covino and 
G. Tagliaferri (INAF-OAB) report, on behalf of the MISTICI collaboration:

We observed the field of GRB 080207 (Racusin et al., GCN 7264) with the 
Very Large Telescope equipped with the SINFONI near infrared camera in 
imaging mode. Observations have been carried out on Feb 08.3673, i.e. 
about 11.3 hours after the burst and about 2 hours after the REM 
(D'Avanzo et al., GCN 7269) and GROND (Kuepcue Yoldas et al. GCN 7279) 
NIR observations. We do not detect any afterglow candidate inside the 
XRT error box (Beardmore et al., GCN 7265).  We derive the following 
3sigma upper limits (calibrated against standard stars taken the same 
night):

J > 23.5
H > 22.8
K > 21.5

We acknowledge support from the ESO staff.


GRB_name: GRB080212A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7294
SUBJECT: GRB 080212:  DSS/2MASS Galaxy at XRT position
DATE:    08/02/12 17:46:35 GMT
FROM:    Edo Berger at Princton U  <eberger@astro.princeton.edu>

E. Berger (Princeton) reports:

"Inspection of DSS and 2MASS images reveals an extended object coincident 
with the XRT position of GRB 080212 (trigger 303105).  The coordinates are 
(J2000):

  RA = 15:24:35.19
  DEC= -22:44:29.0

This indicates that the burst is likely at low redshift."


GRB_name: GRB080211A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7295
SUBJECT: IPN localization of GRB 080211
DATE:    08/02/12 17:51:47 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

K. Hurley and T. Cline on behalf of the Mars Odyssey, Konus,
and MESSENGER GRB teams,

J. Goldsten, on behalf of the MESSENGER GRNS GRB team,

W. Boynton, C. Fellows, K. Harshman, C. Shinohara and R. Starr, on
behalf of the GRS-Odyssey GRB team,

I. G. Mitrofanov, D. Golovin, M. L. Litvak, and A. B. Sanin,
on behalf of the HEND-Odyssey GRB team,

S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks
on behalf of the Konus-Wind team,

D. M. Smith, R. P. Lin, J. McTiernan, R. Schwartz, C. Wigger, W.
Hajdas, and A. Zehnder, on behalf of the RHESSI GRB team,

K. Yamaoka, M. Ohno, Y. Fukazawa, T. Takahashi, M. Tashiro, Y. Terada,
T. Murakami, and K. Makishima on behalf of the Suzaku WAM team, report:

Mars Odyssey (GRS), MESSENGER (GRNS), Konus-Wind, RHESSI, and Suzaku-WAM 
observed the long-duration GRB 080211 at about 26620 s UT (07:23:40).
The burst light curve shows a multipeaked structure with a duration of 
~35 sec.

We have triangulated the burst to the following, preliminary 3-sigma
error box:
-----------------------------------------------
      RA(2000)                    Dec(2000)
-----------------------------------------------
Center:
   43.968 (02h 55m 52s)   +60.035 (+60d 02' 07")
Corners:
   43.862 (02h 55m 27s)   +59.463 (+59d 27' 46")
   43.747 (02h 54m 59s)   +59.921 (+59d 55' 17")
   44.081 (02h 56m 19s)   +60.600 (+60d 35' 59")
   44.191 (02h 56m 46s)   +60.148 (+60d 08' 54")
-------------------------------------------------

The error box area is 409 sq. arcmin.
This error box may be improved.

Preliminary analysis of the Konus-Wind data yields
a burst fluence of ~6x10^-5 erg/cm2 (in the 20 keV - 2 MeV range),
and an Epeak of the time-integrated spectrum of ~360 keV.

Detailed spectral parameters will be reported later.


GRB_name: GRB080212A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7296
SUBJECT: GRB 080212: Swift detection of a burst
DATE:    08/02/12 17:58:30 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

H. Ziaeepour (UCL-MSSL), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), A. P. Beardmore (U Leicester),
P. J. Brown (PSU), D. N. Burrows (PSU), M. M. Chester (PSU),
J. R. Cummings (NASA/UMBC), G. Cusumano (INAF-IASFPA),
M. De Pasquale (UCL-MSSL), O. Godet (U Leicester),
C. Guidorzi (INAF-OAB), J. A. Kennea (PSU), H. A. Krimm (GSFC/USRA),
V. Mangano (INAF-IASFPA), J. Mao (INAF-OAB),
C. B. Markwardt (CRESST/GSFC/UMD), F. E. Marshall (NASA/GSFC),
P. T. O'Brien (U Leicester), C. Pagani (PSU),
K. L. Page (U Leicester), D. M. Palmer (LANL),
D. Perez (U Leicester), P. Romano (INAF-IASFPA),
T. Sakamoto (NASA/UMBC), G. Sato (GSFC/ISAS),
B. Sbarufatti (INAF-IASFPA), M. Stamatikos (NASA/ORAU),
R. L. C. Starling (U Leicester), G. Tagliaferri (INAF-OAB),
E. Troja (U Leicester/INAF-IASFPa), D. E. Vanden Berk (PSU) and
L. Vetere (PSU) report on behalf of the Swift Team:

At 17:34:33 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 080212 (trigger=303105).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 231.107, -22.752 which is 
   RA(J2000) = 15h 24m 26s
   Dec(J2000) = -22d 45' 06"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single peak
with a duration of about 20 sec.  The peak count rate was ~1000 
counts/sec (15-350 keV), at ~0 sec after the trigger.  There may be a
precursor at T-60 sec. 

The XRT began observing the field at 17:36:19 UT, 106 seconds after the
BAT trigger. XRT found a bright, fading X-ray source
located at RA, Dec 231.1466, -22.7410 which is
   RA(J2000)  =  15h 24m 35.1s
   Dec(J2000) = -22d 44' 27.5"
with an uncertainty of 4.7 arcseconds (radius, 90% containment). 
This location is 137 arcseconds from the BAT on-board position,
within the BAT error circle. The initial flux in the 2.5s image
was 6.9e-09 erg/cm2/s (0.2-10 keV). 

UVOT took a finding chart exposure of 400 seconds with the V filter
starting 109 seconds after the BAT trigger. No afterglow candidate
has been found in the initial data products. There is a object in the
DSS image inside the XRT error circle which is also detected by UVOT
with a magnitude of 17.7. 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 correction has been
made for the expected extinction of about 0.5 magnitudes. 

Burst Advocate for this burst is H. Ziaeepour (hz AT mssl.ucl.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.)


GRB_name: GRB080210A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7297
SUBJECT: VLA non-detection of GRB 080210
DATE:    08/02/12 18:15:54 GMT
FROM:    Poonam Chandra at U Virginia/NRAO  <pc8s@virginia.edu>

Poonam Chandra (NRAO/UVA) and Dale A. Frail (NRAO) report on
behalf of the Caltech-NRAO-Carnegie GRB Collaboration:


"We used the Very Large Array to observe the field of view toward
GRB 080210 (GCN 7281) at a frequency of 8.46 GHz on 2008 February
12.53 UT. The radio afterglow of the GRB is undetected at the
Swift-XRT position (GCN 7285). The peak flux at Swift XRT position is
-10+/-43 uJy.


The National Radio Astronomy Observatory is a facility of the National
Science Foundation operated under cooperative agreement by Associated
Universities, Inc."


GRB_name: GRB080210A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7298
SUBJECT: GRB 080210: Keck photometry
DATE:    08/02/13 00:12:19 GMT
FROM:    Daniel Perley at U.C. Berkeley  <dperley@astro.berkeley.edu>

D. A. Perley, M. Modjaz, J. S. Bloom, D. Poznanski, A. Miller, and D. 
Kocevski (UC Berkeley) report:

On the night of 2008-02-12 (UT), we observed the field of GRB080210 
(Grupe et al., GCN 7281) using Keck I (+LRIS) for 600s (R) and 900s (g). 
  We detect the GRB afterglow at the position noted by Klotz et al. (GCN 
7280) and Grupe et al.

Calibrating relative to seven stars from the SDSS calibration table 
given in GCN 7282 (Cool et al.), we measure the following magnitudes (at 
UT = 15:32, 55.7 hours after the BAT trigger):

R = 24.03 +/- 0.06
g = 25.20 +/- 0.07

The quoted uncertainty is photometric only and does not include scatter 
in the field calibration relative to SDSS (which is significant.)

Compared to the photometry given by Updike et al. (GCN 7288) this 
suggests an unusually slow decay rate of alpha~0.85.  This may suggest 
the presence of an underlying host galaxy, but the source appears 
pointlike in our images and the redshift of z=2.1 (Jakobbson et al., GCN 
7286) would argue against a large host galaxy contribution.  The X-ray 
afterglow* also appears to be decaying slowly.

---

* http://astro.berkeley.edu/~nat/swift/00302888/bat_xrt.jpg.


GRB_name: GRB080212A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7299
SUBJECT: GRB 080212: Swift-XRT Team refined analysis 
DATE:    08/02/13 00:48:16 GMT
FROM:    Kim Page at U.of Leicester  <kpa@star.le.ac.uk>

K.L. Page, D. Perez (U Leicester) and H. Ziaeepour (UCL-MSSL) report on 
behalf of the Swift-XRT team:

We have analysed the first three orbits of data obtained for GRB 080212 
(Ziaeepour et al., GCN Circ. 7296). Most of the initial orbit of data were 
collected in Windowed Timing (WT mode), and show strong flaring activity. 
Using the second two orbits [Photon Counting (PC) mode data; 5.2 ks of 
exposure time], we obtained a refined position of RA, Dec (J2000) = 
231.1468, -22.7420, which is equivalent to

RA(J2000) =   15 24 35.24
Dec(J2000) = -22 44 31.0

with an estimated uncertainty of 3.6 arcsec. This is 3.7 arcsec from the 
onboard XRT position (GCN Circ. 7296).

Following the flares in the first orbit of data, the X-ray light-curve can 
be fitted with a power-law, with the decay slope, alpha = 0.8 +/- 0.1.

There is strong spectral evolution during the flaring WT data. A spectrum 
formed from the PC mode data can be modelled with an absorbed power-law, 
with Gamma = 2.3 +/- 0.2 and NH = (2.1 +/- 0.4)e21 cm^-2, significantly in 
excess of the Galactic value of 7.26e20 cm^-2. The 0.3-10 keV observed 
(unabsorbed) flux during this time (~3.5 - 12 ks after the trigger) is 
8.4e-12 (1.5e-11) erg cm^-2 s^-1.

If the light-curve continues to decay at this rate, the predicted count 
rate at 24 hours will be 0.024 count s^-1. Using the PC data, a counts to 
flux conversion of 4.0e-11 erg cm^-2 count^-1 can be estimated, implying 
the predicted flux at 24 hours would be 9.6e-13 erg cm^-2 s^-1.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB080212A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7300
SUBJECT: GRB 080212: Enhanced Swift-XRT position
DATE:    08/02/13 00:56:41 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

M.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 399 s of overlapping XRT Photon Counting mode and UVOT
V-band data for GRB 080212, 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 = 231.14749, -22.74154 which is equivalent
to:

RA (J2000): 15h 24m 35.40s
Dec (J2000): -22d 44' 29.5"

with an uncertainty of 2.0 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, astro-ph/0708.0986
http://www.swift.ac.uk/xrt_positions/Goad.pdf).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB080212A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7301
SUBJECT: GRB 080212: optical observations
DATE:    08/02/13 06:49:06 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

A. Snchez Caso (Gualba Obs., Barcelona), M. Jelnek, A. J.
Castro-Tirado, J. Gorosabel (IAA-CSIC, Granada) and D. Prez-Ramrez (U.
Leicester), on behalf of a larger collaboration, report:

"Following the detection of GRB 080212 by Swift/BAT (Ziaeepour et al.,
GCN Circ. 7296), we have obtained VRI-band images with the 0.4m Gualba
Obs. telescope under non-optimal conditions, starting on Feb 13.263 UT
(i.e. 13.0 hr after the trigger). At the Swift/XRT position given by
Page et al. (GCN Circ. 7299) we only see the DSS2 galaxy pointed out by
Berger (GCN Circ. 7294). The limiting magnitude of our images is R = 18.
Much deeper optical/nIR observations are encouraged."

This message can be quoted.


GRB_name: GRB080212A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7302
SUBJECT: GRB 080212: REM NIR afterglow?
DATE:    08/02/13 08:02:40 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

P. D'Avanzo, L.A. Antonelli, S. Covino, D. Fugazza, L.  Calzoletti, S. 
Campana, G.  Chincarini, M.L. Conciatore, S. Cutini, V. D'Elia, F. 
Dalessio, F.  Fiore, P. Goldoni, D. Guetta,  C. Guidorzi, G.L. Israel, 
N. Masetti, A. Melandri, E. Meurs, L. Nicastro, E. Palazzi, E. Pian, S. 
Piranomonte, L.  Stella, G.  Stratta, G. Tagliaferri, G. Tosti, V.Testa, 
S.D. Vergani,  F. Vitali report on behalf of the REM team:

The robotic 60-cm REM telescope located at La Silla (Chile) observed 
automatically the field of the GRB 080212 (Ziaeepour et al., GCN 7296). 
A preliminary analysis of the first set of H-band exposures does reveal 
the presence of an object with H ~ 15.2 inside the XRT error box (Goad 
et al., GCN 7300) at the following coordinates (J2000):

R.A. = 15:24:35.49
Dec. = -22:44:29.0

with an uncertainty of 0.3". This position lies about 3.2" (East 
direction) far from the position of the DSS galaxy (Berger, GCN 7294). 
This object could thus be the NIR afterglow of GRB 080212. The 3sigma 
upper limit of our image is H > 15.7 (calibrated  against the 2MASS 
catalog).

Further analysis is in progress.


GRB_name: GRB080212A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7303
SUBJECT: GRB 080212: GROND detects afterglow
DATE:    08/02/13 08:08:18 GMT
FROM:    Jochen Greiner at MPI  <jcg@mpe.mpg.de>

A. Kuepcue Yoldas, A. Yoldas, J. Greiner, T. Kruehler (all MPE Garching),
A. Rossi (Tautenburg Obs) report for the GROND team:

We observed the field of GRB 080212 (trigger 303105) detected by Swift/BAT 
(Ziaeepour et al. 2008, GCN 7296) simultaneously in grizJHK with GROND 
(Greiner et al. 2008, astro-ph/0801.4801), mounted at the 2.2m MPI/ESO 
telescope at La Silla (Chile). Observations started on Feb. 13, at 05:30 UT 
(12 hrs after the GRB), when the GRB location was becoming visible at 
20 degrees above horizon.

We detect a new source in all filters, suggesting the Ly-break being below the 
g'-band (and thus z<3.5). It is clearly separated from the galaxy mentioned by 
Berger et al. (2008, GCN 7294). The position is

  RA (2000.0) = 15:24:35.4 
  Decl (2000.0) = -22:44:30

At 6:36 UT we measure i'=22.6 mag. No statement about variability can be 
made at this stage. GROND observations are continuing.


GRB_name: GRB080212A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7304
SUBJECT: GRB 080212:  Gemini-South optical observations
DATE:    08/02/13 08:13:50 GMT
FROM:    Edo Berger at Princton U  <eberger@astro.princeton.edu>

E. Berger (Princeton) reports:

"A 900-sec spectrum obtained with Gemini-South/GMOS reveals that the 
object near the XRT position is a late-K star and not a galaxy as 
initially indicated in GCN 7294.

In a 60 sec r-band acquisition image we find a faint source coincident 
with the XRT position at:
  RA = 15:24:35.4
  DEC = -22:44:30 (J2000)

This object is consistent with the positions reoprted in GCNs 7302 and 
7303."


GRB_name: GRB080212A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7305
SUBJECT: GRB080212: Optical afterglow candidate observed by MITSuME Telescope
DATE:    08/02/13 11:50:53 GMT
FROM:    Michitoshi Yoshida at Okayama Astrophysical Obs  <yoshida@oao.nao.ac.jp>

M. Yoshida, K. Yanagisawa, Y. Shimizu, S. Nagayama (OAO, NAOJ)
and N. Kawai (Tokyo Tech) report on behalf of the MITSuME
collaboration:

We performed optical imaging observation (g', Rc, and Ic) of the
field of GRB 080212 (Ziaeepour et al. GCN 7296) with 50cm MITSuME
telescope at Okayama Astrophysical Observatory from UT 17:36:37
(124 sec after the trigger) to UT 20:30:38 on Feb 12 2008.

We found a 18 mag star in the vicinity of the XRT position (Goad
et al. GCN 7300). This is the late-K star reported by Berger (GCN
7304). Although we could not spatially resolve the faint source
close to this star reported by Berger (GCN7304), we found that
a fading component is overlaid on the star. This component is
a GRB afterglow candidate. We estimated the magnitudes of the
fading component by subtracting the flux of the star at 2 hours
after the trigger from the star magnitude at early time.

The estimated magnitudes of the fading component are summarized
below.

Observation date  2008-02-12 UT

mid-UT    exp-T         g'           Rc           Ic
---------------------------------------------------------
17:42:47   10min   19.46+-0.26  17.77+-0.15  17.98+-0.22
18:00:27   22min   > 21.0       18.77+-0.14  18.91+-0.21
18:19:08   52min   > 21.0       19.88+-0.10  > 20.5
18:58:37  113min   > 21.0       > 20.5       > 20.5
---------------------------------------------------------


GRB_name: GRB080212A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7306
SUBJECT: GRB 080212, Swift-BAT refined analysis
DATE:    08/02/13 13:41:24 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

K. McLean (GSFC/UMD), S. D. Barthelmy (GSFC), J. Cummings (GSFC/UMBC),
E. Fenimore (LANL), N. Gehrels (GSFC), H. Krimm (GSFC/USRA),
C. Markwardt (GSFC/UMD), D. Palmer (LANL), A. Parsons (GSFC),
T. Sakamoto (GSFC/UMBC), G. Sato (GSFC/ISAS), M. Stamatikos (GSFC/ORAU),
J. Tueller (GSFC), T. Ukwatta (GWU), H. Ziaeepour (UCL-MSSL)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+963 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 080212 (trigger #303105)
(Ziaeepour, et al., GCN Circ. 7296).  The BAT ground-calculated position is
RA, Dec = 231.145, -22.739 deg, which is 
   RA(J2000)  =  15h 24m 34.8s 
   Dec(J2000) = -22d 44' 19" 
with an uncertainty of 1.5 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 35%.
 
The mask-weighted light curve shows the main burst acivity starting
at about T-60 sec, the main peak at ~T+5 sec, and ending at about T+110 sec.
There is a weak peak at T+250 to T+350 sec, which matches a flare
in in the XRT lighcurve peaking at about T+250 sec.
T90 (15-350 keV) is 123 +- 13 sec (estimated error including systematics).
 
The time-averaged spectrum from T-60.5 to T+75.7 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 0.31 +- 0.64, 
and Epeak of 67.6 +- 13.1 keV (chi squared 52.75 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 2.9 +- 0.3 x 10^-06 erg/cm2
and the 1-sec peak flux measured from T+3.75 sec in the 15-150 keV band is
1.2 +- 0.3 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.59 +- 0.12 (chi squared 68.06 for 57 d.o.f.).  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/303105/BA/


GRB_name: GRB080212A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7307
SUBJECT: Swift/UVOT refined analysis of GRB080212
DATE:    08/02/13 13:55:09 GMT
FROM:    Massimiliano de Pasquale at MSSL-UCL  <mdp@mssl.ucl.ac.uk>

   M. De Pasquale and H. Ziaeepour (MSSL/UCL)
report on behalf of the Swift team:

The Swift/UVOT observed the field of GRB 080212 (trigger 303105)
starting 110 seconds  after the BAT trigger (Ziaeepour et al
GCN Circ. 7296), which occurred at 17:34:33 UT.
A source is detected in the enhanced XRT error circle reported
by Evans et al (GCN circ. 7300), blended with the K-type star
mentioned in GCN 7304 by Berger et al.
The detection is only in the early V band exposures. There was
no other 3-sigma detection of the afterglow in any exposure
in any of the UVOT filters.

  We do caution that photometry for this burst has been
carried out in very difficult conditions. Furthermore, no
correction has been made for the non-negligible Galactic
extinction towards the burtst, which amounts to E(B-V) = 0.16

The detections and 3-sigma upper limits in the UVOT photometric
system (Poole et al MNRAS 383, 627 (2008)) are summarized in
the following table:


   Filter  Tstart(s)  Tstop(s)  Exp(s)     Mag / Upper limit

   V          110       510      393        17.8 +/- 0.1

   V         4734      6166      393        19.3 +/- 0.3

   V        21968     22876      893            >20.3


   B         4323      4522      393            >20.7

   B        11320     40999     1774            >21.2


   U         4119      5548      393            >20.3

   U        10408     40703     3400            >21.5


   UW1       3919      5344      393            >20.0

   UW1       9502     50920     4309            >21.2


   UM2       3741      6300      323            >19.3

   UM2      15290     45066     3413            >20.6


   UW2      4529       5961      393            >19.4

   UW2     21062      21961      893            >20.7


GRB_name: GRB080212A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7308
SUBJECT: VLA radio upper limit on GRB 080212
DATE:    08/02/13 14:10:29 GMT
FROM:    Poonam Chandra at U Virginia/NRAO  <pc8s@virginia.edu>

Poonam Chandra (NRAO/UVA) and Dale A. Frail (NRAO) report on
behalf of the Caltech-NRAO-Carnegie GRB Collaboration:


"We used the Very Large Array to observe the field of view toward
GRB 080212 (GCN 7296) at a frequency of 8.46 GHz on 2008 February
13.53 UT. The radio afterglow of the GRB is undetected at the
Swift-XRT position (GCN 7300) or optical afterglow position (GCN 7303).
The peak flux density at the afterglow position is 83 +/- 51 uJy.


The National Radio Astronomy Observatory is a facility of the National
Science Foundation operated under cooperative agreement by Associated
Universities, Inc."


GRB_name: GRB080211A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7309
SUBJECT: Konus-Wind observation of GRB 080211
DATE:    08/02/13 15:23:54 GMT
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 long GRB 080211 (Hurley et al., GCN 7295)
triggered Konus-Wind at T0=26622.790 s UT (07:23:42.790).

As observed by Konus-Wind the burst
had a fluence of 4.66(-0.19, +0.20)x10^-5 erg/cm2,
and a 64-ms peak flux measured from T0+5.824 s
of (6.66 +/- 1.22)x10^-6 erg/cm2/s
(both in the 20 keV - 2 MeV energy range).

The time-integrated spectrum of the burst
(from T0 to T0+27.648 s) can be 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 = -0.85 +/- 0.06
and Ep = 356(-22, +25) keV (chi2 = 70.6/62 dof).

The spectrum of the most intense part (from T0 to T0+5.888 s)
is well fitted (in the same range)
by a power law with exponential cutoff model
with alpha =  -0.67 +/- 0.09
and Ep = 484(-40, +45) keV (chi2 = 53.2/62 dof).
Fitting by GRBM (Band) model yields:
the low-energy photon index is alpha = -0.61(-0.11, +0.13),
the high energy photon index beta = -2.62(-1.48, +0.40),
the peak energy Ep = 441(-61, +62) keV (chi2 = 50.0/61 dof).
The fluence of this part is (1.81 +/- 0.11)x10^-5 erg/cm2.

All the quoted errors are at the 90% confidence level.

The Konus-Wind light curve of this GRB is available
at http://www.ioffe.rssi.ru/LEA/GRBs/GRB080211_T26622/


GRB_name: GRB080212A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7310
SUBJECT: GRB 080212: REM refined analysis
DATE:    08/02/13 18:12:44 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

P. D'Avanzo, L.A. Antonelli, S. Covino, D. Fugazza, L.  Calzoletti, S. 
Campana, G.  Chincarini, M.L. Conciatore, S. Cutini, V. D'Elia, F. 
D'Alessio, F. Fiore, P. Goldoni, D. Guetta,  C. Guidorzi, G.L. Israel, 
E. Maiorano, D. Malesani, N. Masetti, A. Melandri, E.J.A. Meurs, L. 
Nicastro, E. Palazzi, E. Pian, S. Piranomonte, L.  Stella, G.  Stratta, 
G. Tagliaferri, G. Tosti, V. Testa, S.D. Vergani,  F. Vitali report on 
behalf of the REM team:

We performed a more careful analysis of the REM H-band images of GRB 
080212 (Ziaeepour et al. GCN 7296). We confirm the afterglow detection 
reported in D'Avanzo et al. (GCN  7302).The observations have been 
carried out on Feb 13.2063 UT (about 11.4 hours after the burst) and 
consist of three sets of images (lasting 10, 30 and 60 s respectively).

We confirm the presence of a H = 15.3  0.2 object (calibrated against 
the 2MASS catalogue) about 2.5" East of the K-type star (Berger, GCNs 
7294 & 7304). The object is visible in both the 30 s and 60 s images at 
the following coordinates (J2000):

R.A. = 15:24:35.42
Dec. = -22:44:28.8

with an uncertainty of 0.3" (the REM pixel size is 1.2"/pixel) .

When compared to the GROND optical detection (obtained about 1.7 hours 
later, Kuepcue Yoldas et al. GCN  7303), our H-band measurement implies 
a colour I-H ~ 7 mag, which is very red. A possible way out is to invoke 
remarkable flaring activity around the time of the REM observation. We 
note that the X-ray light curve (available at: 
http://www.swift.ac.uk/xrt_curves/00303105/) shows some evidence for 
rebrightening about 2 hr before the REM observation.

A finding chart, showing the detection at different H-band images can be 
found at the following URL:

 http://www.brera.inaf.it/utenti/davanzo/public/grb/GRB080212/GRB080212_REMIR_FC.jpg


GRB_name: GRB080212A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7311
SUBJECT: GRB 080212: VLT optical rapid decay
DATE:    08/02/14 19:37:21 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

P. D'Avanzo, D. Fugazza (INAF-OAB), L.A. Antonelli (INAF-OAR), S. 
Covino, G. Chincarini, C. Guidorzi, G. Tagliaferri (INAF-OAB), V. 
D'Elia, F. Fiore, S. Piranomonte, L. Stella (INAF-OAR), M. Della Valle 
(INAF-OAA), S. D. Vergani (DIAS-DCU) report on behalf of the MISTICI 
collaboration:

We observed the optical afterglow of GRB 080212 (Ziaeepour et al., GCN 
7296) with the ESO-VLT equipped with the FORS2 camera in imaging mode at 
three different epochs. Observations have been carried out in R-band on 
Feb 13.3101 UT, Feb 13.3682 UT and Feb 14.2838 UT (0.58, 0.64 and 1.55 
days after the burst, respectively).

We found that between the first two epochs the afterglow faded very 
rapidly, with a decay index of alpha ~ 5.5. Very likely, the afterglow 
underwent a remarkable increase of its optical/NIR flux, probably 
related to the brightening observed in the X-rays about 4 hours before 
our VLT observations (see D'Avanzo et al., GCN 7310).

Assuming the above decay index, we estimate R ~ 20.8 at the epoch of the 
REM detection (D'Avanzo et al., GCN 7302) with an implied colour R-H~5

The decay of the afterglow then slowed down between the last two epochs 
and we measure R~25 in our last observation.


GRB_name: GRB080211A
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7312
SUBJECT: Swift-XRT and UVOT observations of the IPN burst GRB 080211
DATE:    08/02/14 20:08:15 GMT
FROM:    Andy Beardmore at U Leicester  <apb@star.le.ac.uk>

A.P. Beardmore, K.L. Page (U. Leicester), H. Ziaeepour and M. de Pasquale
(MSSL/UCL) report on behalf of the Swift team:

At 2008-02-12 16:42:52UT the Swift-XRT started a TOO observation of the 
IPN burst GRB 080211 (Hurley et al., GCN Circ. 7295), some 33.3 hours 
after the trigger. The observation lasted only 656 s, at which point it 
was terminated by the Swift discovery of GRB 080212 (Ziaeepour et al., GCN 
Circ. 7296).

The photon counting mode image accumulated during this time shows no 
evidence for a source in the XRT field of view, though only ~3/4 of the 
IPN error box was sampled. The 3 sigma limiting count rate for a point 
source in the XRT image is 0.009 count s^-1, which corresponds to a 
0.3-10.0 keV flux limit of 5e-13 erg cm^-2 s^-1 (assuming a power-law 
spectrum of photon index 2 absorbed by the Galactic column density of 
7.8e21 cm^-2 in the direction of the burst).

The IPN field was also observed by the Swift-UVOT in the UW1 filter only, 
for an exposure of 646 s. The 3 sigma upper limit is UW1 > 20.3. We note 
that the background in this field is very noisy and the extinction is 
highly variable throughout the field due to the presence of gas and dust 
visible in DSS images.

This circular is an official product of the Swift-XRT and UVOT teams.


GRB_name: GRB080218A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7313
SUBJECT: GRB 080218: Swift detection of a burst
DATE:    08/02/18 20:18:57 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

H. Ziaeepour (UCL-MSSL), S. D. Barthelmy (GSFC),
J. R. Cummings (NASA/UMBC), P. A. Evans (U Leicester),
S. T. Holland (CRESST/USRA/GSFC), J. A. Kennea (PSU),
W. B. Landsman (NASA/GSFC), K. M. McLean (GSFC/UMD), C. Pagani (PSU),
D. M. Palmer (LANL), T. Sakamoto (NASA/UMBC), G. Sato (GSFC/ISAS),
M. Stamatikos (NASA/ORAU), D. E. Vanden Berk (PSU), L. Vetere (PSU)
and P. A. Ward (MSSL-UCL) report on behalf of the Swift Team:

At 20:08:42 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 080218 (trigger=303609).  Swift did not slew to the burst
location because of the Sun observing constraint (34 deg from the Sun). 
The BAT on-board calculated location is 
RA, Dec 355.922, +12.175 which is 
   RA(J2000)  =  23h 43m 41s
   Dec(J2000) = +12d 10' 29"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a weak peak around T_0. 
The peak count rate was ~400 counts/sec (15-350 keV). 

Because this burst is in the Sun constraint until May,
no XRT or UVOT data will be available. 

Burst Advocate for this burst is H. Ziaeepour (hz AT mssl.ucl.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.)


GRB_name: GRB080218B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7314
SUBJECT: GRB 080218B: Swift detection of a burst
DATE:    08/02/19 00:37:50 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

P. Schady (MSSL-UCL), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), A. P. Beardmore (U Leicester),
D. N. Burrows (PSU), J. R. Cummings (NASA/UMBC),
P. A. Evans (U Leicester), S. T. Holland (CRESST/USRA/GSFC),
J. A. Kennea (PSU), H. A. Krimm (GSFC/USRA),
F. E. Marshall (NASA/GSFC), C. Pagani (PSU),
K. L. Page (U Leicester), D. M. Palmer (LANL),
T. Sakamoto (NASA/UMBC), G. Sato (GSFC/ISAS),
M. Stamatikos (NASA/ORAU), R. L. C. Starling (U Leicester),
D. E. Vanden Berk (PSU) and P. A. Ward (MSSL-UCL) report on behalf of
the Swift Team:

At 23:57:47 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 080218B (trigger=303631).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 177.951, -53.100 which is 
   RA(J2000) = 11h 51m 48s
   Dec(J2000) = -53d 06' 00"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a complex
structure with a duration of at least 12 sec, up to an
interruption in the available data caused by a TDRSS gap. 
The peak count rate was  ~1300 counts/sec (15-350 keV), 
at ~0 sec after the trigger. 

Using prompt downlinked data starting 931 s after the BAT trigger,
we find a bright X-ray source located at RA, Dec 177.9560, -53.0960
which is
   RA(J2000)  = 11 51 49.44
   Dec(J2000) = -53 05 45.7
with an uncertainty of 3.0 arcsec (radius, 90% containment). 
This location is 18 arcseconds from the BAT on-board position,
within the BAT error circle. 

UVOT took a finding chart exposure of 99 seconds with the White
(160-650 nm) filter starting 551 seconds after the BAT trigger.  No
afterglow candidate has been found in the initial data products.  The
UVOT image covers 100% of the XRT error circle and has an estimated
3-sigma limiting magnitude of white = 20.6.  No correction has been
made for the expected extinction corresponding to a reddening of
E(B-V) = 0.17 mag. 

Burst Advocate for this burst is P. Schady (ps AT mssl.ucl.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.)


GRB_name: GRB080211A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7315
SUBJECT: GRB 080211: Suzaku WAM observation of the prompt emission 
DATE:    08/02/19 01:00:42 GMT
FROM:    Masanori Ohno at Hiroshima U  <ohno@hirax7.hepl.hiroshima-u.ac.jp>

M. Ohno, T. Uehara, T. Takahashi, Y. Fukazawa, 
C. Kira, Y. Hanabata (Hiroshima U.), 
K. Yamaoka, Y. E. Nakagawa, S. Sugita (Aoyama Gakuin U.), 
M. Tashiro, Y. Terada, Y. Urata, A. Endo,
K. Onda, M. Suzuki, N. Kodaka, K. Morigami (Saitama U.), 
T. Tamagawa (RIKEN),
T. Enoto, R. Miyawaki, K. Nakazawa, K. Makishima (Univ. of Tokyo),
E. Sonoda, M. Yamauchi, H. Tanaka, R. Hara (Univ. of Miyazaki),
M. Kokubun, M. Suzuki, T. Takahashi (ISAS/JAXA), 
S. Hong (Nihon U.),
on behalf of the Suzaku WAM team, report:

The bright, long, IPN localized GRB 080211 (Hurley et al., GCN 7295)
was detected by the the Suzaku Wide-band  All-sky Monitor (WAM) which
covers an energy range of 50 keV - 5 MeV at 07:23:39 UT (=T0).
The observed light curve shows a multi-peaked structure, starting at
T0-10 s, ending at T0+25 s with a duration (T90) of about 25 seconds.
The fluence in 100 - 1000 keV was 2.8(+0.1,-0.1) x 10^-5 erg/cm^2.
The 1-s peak flux measured from T0+6 s was 5.5(+0.4,-0.6)
photons/cm^2/s in the same  energy range.

Preliminary result shows that the time-averaged spectrum from
T0-10s to T0+25s is well fitted by a power-law with exponential cutoff
model:
 dN/dE ~  E^{-alpha} * exp(-(2-alpha)*E/Epeak) with
 alpha       1.1(+0.2,-0.2), and
 Epeak       483(+66,-46) keV (chi^2/d.o.f. = 38/21).

All the quoted errors are at statistical 90% confidence level,
in which the systematic uncertainties are not included.

The light curves with 1-sec time resolution for this burst will be
appeared at:

 http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/untrig/grb_table.html


GRB_name: GRB080218B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7316
SUBJECT: GRB080218B: Watcher prompt limit
DATE:    08/02/19 02:02:07 GMT
FROM:    Martin Jelinek at Inst.Astrophys.Andalucia,Granada  <mates@iaa.es>

J. French (UCD Dublin), 
M. Jelinek  and Petr Kubanek (IAA CSIC Granada) and 
Antonio de Ugarte Postigo (ESO Santiago)

on behalf of the Watcher collaboration report:

"The  0.4 m telecope  Watcher,  located  at  Boyden
observatory,  South Africa,  followed the Swift GRB
080218B (Schady et al. GCN 7314).

10s unfiltered (limmag = 16.0) images were obtained
starting 60.4s after the GRB (18.3s after receiving
the notification).

We  do  not detect  any  new source in  single  nor
combined images within the BAT or XRT errorbox."

This message may be cited.


GRB_name: GRB080218A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7317
SUBJECT: GRB 080218A, Swift-BAT refined analysis
DATE:    08/02/19 03:24:29 GMT
FROM:    Takanori Sakamoto at NASA/GSFC  <Taka.Sakamoto@nasa.gov>

E. Fenimore (LANL), S. D. Barthelmy (GSFC), J. Cummings (GSFC/UMBC),
N. Gehrels (GSFC), H. Krimm (GSFC/USRA), C. Markwardt (GSFC/UMD),
K. McLean (GSFC/UMD), D. Palmer (LANL), A. Parsons (GSFC), 
T. Sakamoto (GSFC/UMBC), G. Sato (GSFC/ISAS), M. Stamatikos (GSFC/ORAU),
J. Tueller (GSFC), T. Ukwatta (GWU), H. Ziaeepour (UCL-MSSL)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+303 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 080218A (trigger #303609)
(Ziaeepour, et al., GCN Circ. 7313).  The BAT ground-calculated position is 
RA, Dec = 355.941, 12.159 deg which is 
   RA(J2000)  = 23h 43m 45.8s 
   Dec(J2000) = 12d 9' 34" 
with an uncertainty of 2.5 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 21%.

The mask-weighted light curve shows three peaks at T-12 sec, T+0 sec, 
and T+9 sec.  T90 (15-350 keV) is 27.6 +- 5.9 sec (estimated 
error including systematics).
 
The time-averaged spectrum from T-12.8 to T+18.6 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.34 +- 0.35.  The fluence in the 15-150 keV band is 6.3 +- 1.4 x 10^-07 erg/cm2.
The 1-sec peak photon flux measured from T+1.22 sec in the 15-150 keV band
is 1.4 +- 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/303609/BA/


GRB_name: GRB080218B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7318
SUBJECT: GRB 080218b, SMARTS optical/IR limits
DATE:    08/02/19 03:55:24 GMT
FROM:    Bethany Cobb at Yale U  <cobb@astro.yale.edu>

B. E. Cobb, part of the larger SMARTS consortium, reports:

Using the ANDICAM instrument on the 1.3m telescope at CTIO, we
obtained optical/IR imaging of the error region of GRB 080218b
(Schady et al. GCN 7314) with a mid-exposure time of ~3.1 hours
post-burst (2008-02-19 03:03 UT).  Total summed exposure times amounted
to 18 minutes in I and 15 minutes in J.

No source is detected at the position of the X-ray
afterglow (Schady et al. GCN 7314) to approximate
limiting magnitudes of I > 21.1 and J > 18.7. Magnitudes
are calibrated using USNO-B1.0 values for I, and 2MASS
values for J.


GRB_name: GRB080218B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7319
SUBJECT: GRB 080218B: GROND upper limits
DATE:    08/02/19 04:15:59 GMT
FROM:    Jochen Greiner at MPI  <jcg@mpe.mpg.de>

A. Rossi (Tautenburg Obs.), J. Greiner, A. K"upc"u Yoldas, and A. Yoldas
(MPE Garching) report for the GROND team:

We observed the field of GRB 080218B, Swift trigger 303631 (Schady et al. 2008,
GCN Circ. 7314) simultaneously in grizJHK with GROND (Greiner et al. 2008,
astro-ph/0801.4801) mounted at the 2.2m MPI/ESO telescope at La Silla (Chile).
Observations started at 00:37, 379 min after the GRB. At this time, the GRB 
location was becoming visible at 20 degrees above horizon.

Through thin cirrus, we do not detect any source inside the XRT error.
We estimate the following limits: g'>24.2, r'>24.2, i'>23.7, z'>23.4,
J>21.6, H>20.6, K>19.5, calibrated against USNO-B and 2MASS stars.
These values are not corrected for the substantial foreground extinction.


GRB_name: GRB080218B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7320
SUBJECT: GRB 080218B: Enhanced Swift-XRT position
DATE:    08/02/19 06:16:07 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

J.P. Osborne, A.P. Beardmore, P.A. Evans and M.R. Goad (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 311 s of overlapping XRT Photon Counting mode and UVOT
V-band data for GRB 080218B, 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 = 177.95739, -53.09712 which is equivalent
to:

RA (J2000): 11h 51m 49.77s
Dec (J2000): -53d 05' 49.6"

with an uncertainty of 2.4 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
http://www.swift.ac.uk/xrt_positions/Goad.pdf).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB080212A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7321
SUBJECT: GRB 080212: Mount Abu NIR observations
DATE:    08/02/19 06:29:45 GMT
FROM:    Lokesh Kumar Dewangan at Phys Res Lab, Ahmedabad,India  <lokeshd@prl.res.in>

Lokesh, V. Venkat, J. Jain, S. Vadawale and B.G. Anandarao
Physical Research Laboratory, Ahmedabad, India.

We made infrared photometry in J band at Mt. Abu 1.2 m Cassegrain telescope
using NICMOS camera on the GRB 080212 (Ziaeepour et al. GCN 7296)
during 2008 Feb 13 under good sky conditions. The H band magnitude was
earlier reported by P. D'Avanzo et. al (GCN 7310).
The calibration was made on the bright star SAO 183333.
The overall integration time and the magnitude along with the associated
error are given below:
UT           Integration time J band magnitude+/-error
13.97  1080s  16.8+/-0.1


GRB_name: GRB080218B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7322
SUBJECT: GRB 080218B: REM NIR early upper limits
DATE:    08/02/19 07:39:08 GMT
FROM:    Stefano Covino at Brera Astronomical Observatory  <stefano.covino@gmail.com>

S. Covino, P. D'Avanzo, L.A. Antonelli, D. Fugazza, L.  Calzoletti,  
S. Campana, G.  Chincarini, M.L. Conciatore, S. Cutini, V. D'Elia, F.  
D'Alessio, F. Fiore, P. Goldoni, D. Guetta,  C. Guidorzi, G.L.  
Israel, E. Maiorano, N. Masetti, A. Melandri, E.J.A. Meurs, L.  
Nicastro, E. Palazzi, E. Pian, S. Piranomonte, L.  Stella, G.   
Stratta, G. Tagliaferri, G. Tosti, V. Testa, S.D. Vergani,  F. Vitali  
report on behalf of the REM team:

The robotic 60-cm REM telescope located at La Silla (Chile) observed  
automatically the field of the GRB 080218B (Schady et al., GCN 7314).  
A preliminary analysis of the first set of H and K-band exposures  
does not reveal any afterglow candidate inside the refined XRT error  
box (Osborne et al., GCN 7320). The 3sigma upper limits of our images  
are H > 13.7 about 2 minutes after the burst and K > 12.6 about 8  
minutes after the burst (calibrated against the 2MASS catalog).

Further analysis is in progress.


GRB_name: GRB080218B
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7323
SUBJECT: Swift/UVOT observations of GRB080218B
DATE:    08/02/19 08:25:39 GMT
FROM:    Patricia Schady at MSSL/Swift  <ps@mssl.ucl.ac.uk>

P. Schady (MSSL-UCL) reports on behalf of the Swift-UVOT team

The Swift-UVOT observed the field of GRB080218B starting 551 s after the 
BAT trigger (Schady et al., GCN 7314). No new source is detected within 
the refined XRT error circle (Osborne et al., GCN 7320) in any of the UVOT 
co-added observations down to the following 3-sigma upper limits:

Filter  Tmid (s) Exp (s)  Upper Limit
wh      4178     420        > 21.09
v       2955     494        > 19.87
b       4126     283        > 20.24
u       4098     294        > 19.98
uvw1    3984     294        > 19.77
uvm2    3868     313        > 19.67
uvw2    6056     281        > 19.91

where Tmid is the weighted mid time of the co-added observations. The 
values quoted above are not corrected for the expected Galactic extinction 
corresponding to a reddening of E(B-V)= 0.17 mag in the direction of the 
burst (Schlegel et al. 1998),


GRB_name: GRB080218B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7324
SUBJECT: GRB 080218B: Swift-XRT refined analysis
DATE:    08/02/19 09:51:14 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

P.A. Evans, K.L. Page, A.P. Beardmore, J.P. Osborne (U Leicester) and P.
Schady (MSSL-UCL) report on behalf of the Swift-XRT team:

We have analysed the first four orbits of XRT data obtained for GRB
080218B (Schady et al., GCN Circ. 7314), totalling 4.6 ks in Photon
Counting (PC) mode. Partly due to the proximity of Swift to the SAA, the
observations did not start until 930 s after the trigger.  The
UVOT-enhanced XRT position was given in Osborne et al. (GCN Circ.
7320).

The light curve shows a simple power-law decay, with an index of
alpha=0.92 (+0.13/-0.11). A spectrum formed from all available data can
be modelled with an absorbed power law, with gamma=2.46 (+0.53/-0.47)
and a column density nH=5.17(+0.24/-0.18)e21 cm^-2, significantly in
excess of the Galactic value of 1.35e21 cm^-2 (Kalberla et al. 2005).
Given the excess absorption, the relation given in Grupe et al (2007)
suggests that this burst lies at a redshift <3.3 (90% confidence). The
0.3-10 keV observed (unabsorbed) flux during the interval T0+1--25 ks is
5.72e-12 (1.48e-11) erg cm^-2 s^-1.

If the light curve continues to decay at alpha=0.92, the XRT count rate
at T0+24 hours will be 4.0e-3 count s^-1, which is equivalent to an
observed (unabsorbed) 0.3-10 keV flux of 2.29e-13 (5.92e-13) erg cm^-2
s^-1.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB080218B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7325
SUBJECT: GRB 080218B, Swift-BAT refined analysis
DATE:    08/02/19 15:41:08 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

H. Krimm (GSFC/USRA), S. D. Barthelmy (GSFC), J. Cummings (GSFC/UMBC),
E. Fenimore (LANL), N. Gehrels (GSFC), C. Markwardt (GSFC/UMD),
K. McLean (GSFC/UMD), D. Palmer (LANL), A. Parsons (GSFC),
T. Sakamoto (GSFC/UMBC), G. Sato (GSFC/ISAS), P. Schady (MSSL-UCL),
M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC), T. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using the data set from T-198 to T+962 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 080218 (trigger #303631)
(Schady, et al., GCN Circ. 7314).  The BAT ground-calculated position is
RA, Dec = 177.927, -53.086 deg, which is 
   RA(J2000)  =  11h 51m 42.4s 
   Dec(J2000) = -53d 05' 11" 
with an uncertainty of 2.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 10%.
 
The mask-weighted light curve shows a roughly triangular peak starting
at ~T-3 sec, peaking at T+1 sec, and ending at ~T+7 sec.
T90 (15-350 keV) is 6.2 +- 1.2 sec (estimated error including systematics).
 
The time-averaged spectrum from T-0.8 to T+6.6 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 0.11 +- 2.44, 
and Epeak of 23.6 +- 14.6 keV (chi squared 49.02 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 5.1 +- 1.0 x 10^-7 erg/cm2
and the 1-sec peak flux measured from T+0.28 sec in the 15-150 keV band is
3.1 +- 0.6 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 2.63 +- 0.29 (chi squared 55.36 for 57 d.o.f.).  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/303631/BA/
 
We note that the fluence ratio in a simple power-law fit between the
25-50 keV band and the 50-100 keV band is 1.55.  This fluence ratio is larger
than 1.32 which can be achieved in the Band function of alpha=-1.0, beta=-2.5,
and Epeak=30 keV.  Thus, preliminary analysis shows that Epeak of the burst
is very likely around or below 30 keV.  Therefore the burst can be classified
as an X-ray flash (e.g. Sakamoto et al. ApJ in press, arXiv:0801.4319).


GRB_name: GRB080204A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7326
SUBJECT: GRB 080204: Suzaku WAM observation of the prompt emission
DATE:    08/02/22 11:19:24 GMT
FROM:    Makoto Tashiro at Saitama U/Swift  <tashiro@phy.saitama-u.ac.jp>

Y. Terada, K. Onda, M. Tashiro, Y. Urata, A. Endo,
M. Suzuki, N. Kodaka, K. Morigami (Saitama U.),
M. Ohno, T. Uehara, T. Takahashi, Y. Fukazawa,
C. Kira, Y. Hanabata (Hiroshima U.), T. Tamagawa (RIKEN),
K. Yamaoka, Y. E. Nakagawa, S. Sugita (Aoyama Gakuin U.),
T. Enoto, R. Miyawaki, K. Nakazawa, K. Makishima (Univ. of Tokyo),
E. Sonoda, M.Yamauchi, H. Tanaka, R. Hara (Univ. of Miyazaki),
M. Kokubun, M. Suzuki, T. Takahashi (ISAS/JAXA), S. Hong (Nihon U.),
on behalf of the Suzaku WAM team, report:

The IPN localized GRB 080204 (Golenetskii et al., GCN 7256)
triggered the Suzaku Wide-band  All-sky Monitor (WAM) which covers
an energy range of 50 keV - 5 MeV at 13:56:32 UT (=T0).
The observed light curve shows a multi-peaked structure,
starting at T0-1s, ending at T0+10s, with a duration (T90) of about
4.8seconds. The fluence in 100 - 1000 keV was 1.0(+0.1,-0.1)x10^-5
erg/cm^2. The 1-s peak flux measured from T0+3s was
3.9(+0.2,-0.9)photons/cm2/s in the same energy range.

Preliminary result shows that the time-averaged spectrum from
T0+0s to T0+10s is well fitted by a power-law with exponential cutoff model:
    dN/dE ~  E^{-alpha} * exp(-(2-alpha)*E/Epeak) with
    alpha       0.8(+0.2,-0.3), and
    Epeak       990(+350,-205) keV (chi^2/d.o.f. = 25.0/24).

All the quoted errors are at statistical 90% confidence level,
in which the systematic uncertainties are not included.

The light curves for this burst are available at:
http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html


GRB_name: GRB080218B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7327
SUBJECT: ESO optical and NIR observations of GRB 080218B
DATE:    08/02/22 16:51:29 GMT
FROM:    Paul Vreeswijk at Dark Cosmology Centre,U.of Copenhagen  <pmv@dark-cosmology.dk>

Paul Vreeswijk, Johan Fynbo, Bo Milvang-Jensen, Daniele Malesani,
Jens Hjorth (DARK/NBI), Pall Jakobsson (U. Hertfordshire),
Andreas Jaunsen (U. Oslo), Nial Tanvir (U. Leicester) report
on behalf of a larger collaboration:

The Swift localization of GRB 080218B (Schady et al., GCN 7314) was
observed with FORS2 mounted at the VLT Antu telescope on Cerro Paranal
in Rapid-Response Mode, and with SOFI at the NTT on La Silla. Starting
at Feb 19, 1:03 UT (roughly 1 hour after the burst) VLT/FORS2
performed the imaging sequence R-I-z-V-B-R (30-150s per filter)
through thin cirrus, at an airmass of 2.5, and with an effective
seeing of 1.5". NTT/SOFI imaged the afterglow location at an airmass
of 1.3-1.5 and in 1.4" seeing conditions in Ks-J-H-Ks (10 min. per
filter), starting at Feb 19, 2:52 UT.

No object is detected within the enhanced XRT error circle (Osborne et
al., GCN 7320) down to the following limiting magnitudes (2 sigma):
B>22.1, V>22.7, R>22.9, I>22.6, J>20.6, H>20.1 and Ks>19.4.  The
corresponding upper limit on the optical to X-ray spectral slope,
beta_OX, is 0.24, rendering the burst dark according to the definition
proposed by Jakobsson et al. (2004, ApJ, 617, L21). A spectrum of an
object just outside the XRT error circle at R.A. 11:51:49.25,
decl. -53:05:50.1 (J2000), shows it to be a Galactic star of type M6V.

We acknowledge the excellent support of ESO's night astronomers at La
Silla Paranal Observatory, and in particular that of Linda
Schmidtobreick, Colin Snodgrass, Stephane Brillant and Lorenzo Monaco.


GRB_name: GRB080211A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7331
SUBJECT: GRB080211: optical observations
DATE:    08/02/26 16:52:08 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

M. Andreev (Terskol Branch of Institute of Astronomy) V. Petkov, A. Kurenya 
(BNO INR RAS), A. Pozanenko (IKI) on behalf of larger GRB follow up 
collaboration  report:

We observed the GRB080211 (Hurley et al. GCN 7295, Golenetskii et al. GCN 
7309) with Zeiss-600 of Mt.Terskol observatory on Feb. 12 between (UT) 
17:10-17:21 in R-filter under poor weather conditions. Our observation 
covered  central part of the IPN error-box. Within IPN error-box (Hurley et 
al. GCN 7295), we found one source not presented in any DSS2 plates. 
Coordinates of the source are RA(J2000) = 02h55m50.9s,  Dec.(J2000) = +60 
05' 43.6". Photometry against of USNO-B1.0 is following

T0+  ,        Exposure,   R_mag
(mid time)

1.41d        10x30 s      17.3

Further examination of XRT and UVOT observation (Beardmore et al. GCN 7312) 
and additional observations are necessary to confirm the nature of the found 
source.

Finding chart and combined image can be found in 
http://grb.rssi.ru/GRB080211

The message may be cited.


GRB_name: GRB080205A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7332
SUBJECT: GRB080205: optical observations
DATE:    08/02/26 17:05:10 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

V. Rumyantsev (CrAO), V. Biryukov (SAI, MSU), E. Klunko (ISTP), M. Andreev 
(Terskol Branch of Institute of Astronomy), A.J. Castro-Tirado (IAA-CSIC), 
A. Pozanenko (IKI) on behalf of larger GRB follow up collaboration  report:

We observed the afterglow (Li at al,  GCN 7251), of GRB080205 (Palmer  et 
al, GCN7250) with 1.5m telescope of Sayan observatory (Mondy) on Feb.05 in 
BR and Feb.06; with Zeiss-600 of Mt. Terskol observatory on Feb.05 in R; and 
with CrAO Shajn 2.6m telescope in BVRI on Feb.05, and on Feb.06.  In CrAO 
observations we detected afterglow in R, V and not detected in B, I on 
Feb.05. We do not detect afterglow in any observations on Feb.06.

T0+       Exposure  R_mag (err)   UL    Site     seeing
(mean)

0.226 d  40x60 s   n/d           21.1  Mondy    2.2"
0.379 d  30x60 s   22.26 (0.19)  23.0  CrAO     1.5"
0.409 d  20x90 s   n/d           20.3  Terskol  2.0"
0.548 d  34x60 s   22.26 (0.15)  23.3  CrAO     1.4"
0.772 d  40x60 s   n/d           22.4  CrAO     1.4"
1.530  d 123x60 s   n/d           23.8  CrAO     1.7"

Preliminary photometry reduction is based on USNO-B1.0 stars.

Taking together KAIT (Li at al. GCN 7254) and ING (Rol  et al. GCN 7258) 
observations one can suggest some episodes of a light curve of the GRB080205 
afterglow: the steep decline of light curve with power law index  about -1.6 
between 537 s - 50 m (Li at al. GCN 7254), the shallow decay with power law 
index of  -0.9 between T0+ 50m - 9h,  plateau (or rebrightening) between T0+ 
9h - 13h, and after then very steep decline. The data after ~50 m after 
burst onset is also compatible with a single power law with index  -1.1 and 
a bump between   9h - 13h. Since we do not detect afterglow on Feb.06 
(R>23.8) it is most probably that the previous phases of the light curve is 
not contaminated by a host galaxy.  Our non detection of the afterglow in 
B-filter confirms the redshift less than ~4 (Oates at al.  GCN 7253,  Perley 
at al.  GCN 7254).

The message may be cited. 


GRB_name: GRB080207A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7333
SUBJECT: GRB080207: optical observations
DATE:    08/02/26 17:13:18 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

M. Andreev (Terskol Branch of Institute of Astronomy) V. Petkov, A. Kurenya 
(BNO INR RAS), A. Pozanenko (IKI) on behalf of larger GRB follow up 
collaboration  report:

We observed the GRB080207 (Racusin et al. GCN 7264) with Zeiss-600 of 
Mt.Terskol observatory on Feb.07-08. Two series in R-filter were completed. 
We do not detect new sources within XRT error circle (Beardmore et al. GCN 
7265). The limiting magnitudes against USNO-B1.0 are following:

UT,              Exposure,   R_mag
(mid time)

Feb.7.958    20 x 60s    >20.3
Feb.8.102    40 x 90s    >21.0

The message may be cited.


GRB_name: GRB080229A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7335
SUBJECT: GRB 080229: Swift detection of a bright burst
DATE:    08/02/29 17:31:15 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

J. K. Cannizzo (NASA/UMBC), S. D. Barthelmy (GSFC),
A. P. Beardmore (U Leicester), J. R. Cummings (NASA/UMBC),
P. A. Evans (U Leicester), O. Godet (U Leicester), C. Gronwall (PSU),
S. T. Holland (CRESST/USRA/GSFC), E. A. Hoversten (PSU),
S. Immler (CRESST/GSFC/UMD), J. A. Kennea (PSU),
V. Mangano (INAF-IASFPA), C. B. Markwardt (CRESST/GSFC/UMD),
K. M. McLean (GSFC/UMD), A. Moretti (INAF-OAB),
P. T. O'Brien (U Leicester), J. P. Osborne (U Leicester),
C. Pagani (PSU), K. L. Page (U Leicester), D. M. Palmer (LANL),
A. M. Parsons (GSFC), T. Sakamoto (NASA/UMBC), G. Sato (GSFC/ISAS),
B. Sbarufatti (INAF-IASFPA), M. Stamatikos (NASA/ORAU),
R. L. C. Starling (U Leicester), G. Stratta (ASDC) and
E. Troja (U Leicester/INAF-IASFPa) report on behalf of the Swift
Team:

At 17:04:59 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 080229 (trigger=304379).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 228.217, -14.712 which is 
   RA(J2000)  =  15h 12m 52s
   Dec(J2000) = -14d 42' 43"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed three or four bright 
peaks with the brightest at ~T+40 sec with a duration of about 60 sec. 
The peak count rate was ~7000 counts/sec (15-350 keV), at ~40 sec
after the trigger. 

The XRT began observing the field at 17:06:29.9 UT, 90.3 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source with an enhanced position: RA, Dec 228.21888,
-14.70536 which is equivalent to:
   RA(J2000)  = 15h 12m 52.53s
   Dec(J2000) = -14d 42' 19.3"
with an uncertainty of 2.7 arcseconds (radius, 90% containment). This
location is 24 arcseconds from the BAT onboard position, within the BAT
error circle. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of
8.97e+20 cm^-2 (Kalberla et al. 2005), so we cannot constrain the
redshift at this time using the relation from Grupe et al. (2007). A
summary of the promptly downlinked data is given at
http://www.swift.ac.uk/sper/304379/. 

The initial flux in the 2.5 s image was 5.98e-09 erg cm^-2 s^-2 (0.2-10
keV). 

UVOT took a finding chart exposure of 100 seconds with the White
(160-650 nm) filter starting 100 seconds after the BAT trigger. A 400
second image in V band was also taken 207 seconds after the trigger. 
No afterglow candidate has been found in the either image. The
2.7'x2.7' sub-image covers 100% of the XRT error circle. The typical
3-sigma upper limit has been about 18.5 mag in white and 18.0 in V. 
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 0.15. There is a F0
star with R1~13.3 in the USNO catalog nearby the XRT position which
appears in DSS images. 

Burst Advocate for this burst is J. K. Cannizzo (cannizzo AT milkyway.gsfc.nasa.gov). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB080229A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7336
SUBJECT: GRB 080229A: ROTSE-III Optical Limits
DATE:    08/02/29 17:42:42 GMT
FROM:    Brad Schaefer at LSU  <schaefer@grb.phys.lsu.edu>

B. E. Schaefer (Louisiana State) and E.S. Rykoff (UCSB), report on behalf
of the ROTSE collaboration:

ROTSE-IIIa, located at Siding Spring Observatory, Australia, responded to
GRB 080229A (Swift trigger 304379; Cannizzo et al. 2008, GCN 7335),
producing images beginning 9.8 s after the GCN notice time. An automated
response took the first image at 17:05:31.8 UT, 32.3 s after the burst,
and during the gamma-ray emission, under excellent conditions. We took 10
5-sec, 10 20-sec and 20 60-sec exposures, with continuing exposures now
ongoing. These unfiltered images are calibrated relative to USNO A2.0 (R).

Comparison to the DSS (second epoch) reveals no new sources within the
3-sigma Swift/BAT error circle; the field is not crowded.  Unfortunately,
the XRT position is close to a star of moderate brightness, so the optical
transient could possibly be hidden by the light from this star.  We do not
see any indication that the image of the star is not that of the PSF, and
preliminary image subtractions do not reveal any extra sources.  
Individual images have limiting magnitudes ranging from 14.7-16.1; we set
the following specific limits.

start UT       end UT      t_exp(s)   mlim   t_start-tGRB(s)  Coadd?
--------------------------------------------------------------------
17:05:31.8   17:05:36.8         5     14.7           32.3       N


GRB_name: GRB080229A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7337
SUBJECT: GRB 080229: Faulkes Telescope South optical limit
DATE:    08/02/29 20:43:58 GMT
FROM:    James Smith at ARI,Liverpool John Moors U  <rjs@astro.livjm.ac.uk>

R.J. Smith, D.F. Bersier, S. Kobayashi, A. Monfardini, C.G. Mundell,
I. A. Steele (Liverpool JMU), A. Gomboc (U. Ljubljana),
C. Guidorzi (U. Bicocca & INAF-OAB)
P. O'Brien, E. Rol, N. Bannister (Leicester) report:

The 2-m Faulkes Telescope South (Siding Spring) robotically followed  
up GRB080229 (SWIFT trigger 304379) starting 4.6 min after the GRB  
trigger time. The automatic "detection mode" procedure did not find  
any afterglow. In manual inspection of later observations we do not  
find any optical candidate  corresponding to the XRT X-ray afterglow  
(Cannizzo et al., GCN 7335) to the following limiting magnitudes.  
Magnitude zero points are relative to the USNO measure of R=13.3 for  
the adjacent bright star.

-----------------------------------------------
Mid Time      Filter  Tot.Exposure   Lim. Mag.
since GRB

10.95 min       R        60s          18.7
28.10 min       R        180s         21.9
-----------------------------------------------

[GCN OPS NOTE(29feb08): Per editor's choice, the Subject-line
was changed from "071021" to "080229".]


GRB_name: GRB080229A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7338
SUBJECT: GRB 080229, Swift-BAT refined analysis
DATE:    08/03/01 00:15:19 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

C. Markwardt (GSFC/UMD), S. D. Barthelmy (GSFC), J. K. Cannizzo (NASA/UMBC),
J. Cummings (GSFC/UMBC), E. Fenimore (LANL), N. Gehrels (GSFC),
H. Krimm (GSFC/USRA), K. McLean (GSFC/UMD), D. Palmer (LANL),
A. Parsons (GSFC), T. Sakamoto (GSFC/UMBC), G. Sato (GSFC/ISAS),
M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC), T. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+303 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 080229 (trigger #304379)
(Cannizzo, et al., GCN Circ. 7335).  The BAT ground-calculated position is
RA, Dec = 228.220, -14.697 deg, which is 
   RA(J2000)  =  15h 12m 52.7s 
   Dec(J2000) = -14d 41' 50" 
with an uncertainty of 1.5 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 18%.
 
The mask-weighted light curve shows an initial small peak starting
at ~T-3 sec, peaking at T_zero, and ending at ~T+12 sec.  Then there are
two smaller peaks centered on T+18 and T+28 sec.  Then comes two overlapping
large peaks on T+35 and T+39 sec with the latter tailing out to ~T+85 sec.
T90 (15-350 keV) is 64 +- 16 sec (estimated error including systematics).
 
The time-averaged spectrum from T-15.1 to T+64.9 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.91 +- 0.06.  The fluence in the 15-150 keV band is 9.0 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+40.36 sec in the 15-150 keV band
is 5.7 +- 0.2 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/304379/BA/


GRB_name: GRB080229A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7339
SUBJECT: UVOT analysis for GRB080229
DATE:    08/03/01 00:34:09 GMT
FROM:    Paul Kuin at MSSL  <npkuin@googlemail.com>

N.P.M. Kuin (MSSL/UCL) and J. K. Cannizzo (NASA/UMBC) report on
behalf of the Swift-UVOT team:

The Swift/UVOT observed the field of GRB 080229 (trigger #304379),
Canizzo et al. GCN CIRC. 7335) starting 2008:02:29 at 17:06:22 UT
with a 9.4 s setling image followed at 17:06:41 UT with a finding
chart. No afterglow is detected at the position of the enhanced
XRT position in the finding chart, nor in the three subsequent
exposures.

The source is near a bright star and may be affected by it.
Therefore a small aperture was used and the background was determined
for a region at equal distance to the nearby star.

The following 3-sigma upper limits (in the UVOT photometric system,
Breeveld et al., GCN Circ. 6614) were determined at the XRT
position (RA=15:12:52.53, DEC= -14:42:19.3, J2000):

Filter  Tstart(s)  Tstop(s)  Exp(s)  Mag (3-sigma Upper Limits)

 wh      101       200        99.8   > 20.9
 v       208       608       400.0   > 19.9
 wh      856       956        99.8   > 20.9
 v       962      1362       400.0   > 19.9

The values quoted above are not corrected for the expected Galactic
extinction corresponding to a reddening of E_{B-V} = 0.15 mag in the
direction of the burst (Schlegel et al. 1998).


GRB_name: GRB080229B
Detection_method: superAGILE
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7340
SUBJECT: GRB 080229B: Gamma Ray Burst Localization by SuperAGILE
DATE:    08/03/01 02:48:00 GMT
FROM:    Marco Feroci at IASF/INAF  <feroci@iasf-roma.inaf.it>

Y. Evangelista, E. Del Monte, M. Feroci, E. Costa, I. Donnarumma, 
I. Lapshov, F. Lazzarotto, L. Pacciani, M. Rapisarda, P. Soffitta
(INAF/IASF Rome), A. Giuliani, S. Vercellone, A. Chen, S. Mereghetti, A. 
Pellizzoni, F. Perotti, F. Fornari, M. Fiorini, P. Caraveo, 
A. Zambra (INAF/IASF Milan), A. Bulgarelli, F. Gianotti, 
M. Trifoglio, G. Di Cocco, C. Labanti, F. Fuschino, M. Marisaldi, 
M. Galli, (INAF/IASF Bologna), M. Tavani, G. Pucella, F. D'Ammando, V. 
Vittorini, A. Argan, A. Trois (INAF/IASF Rome), G. Barbiellini, 
F. Longo (INFN Trieste), P. Picozza, A. Morselli (INFN Roma-2),  
M. Prest, E. Vallazza (Universita' dell'Insubria), P. Lipari, 
D. Zanello (INFN Roma-1), and  P. Giommi, C. Pittori, L. A. Antonelli 
(ASDC) and L. Salotti (ASI), on bhealf of the AGILE Team, report:

"SuperAGILE detected and localized a gamma ray burst 
on February 29th, at 23:33:01 UT. The event was approximately 
13 degrees off-axis. The observed duration in the 20-60 keV
energy range is above 100 seconds, with time structure.
The burst was triggered and localized during on ground data processing.  
The burst position was reconstructed as (RA, Dec) (199.221 deg, 
-64.878 deg), which is:

RA(J2000) = 13h 16m 53.13s
Dec(J2000) = -64d 52' 40.8"

with an uncertainty of 3' radius. The given uncertainty accounts 
for both the statistical and systematic errors. 

An analysis of the AGILE Gamma Ray Imager (GRID) data is in progress."

This message may be cited.


GRB_name: GRB080229A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7341
SUBJECT: GRB080229: Possible optical afterglow
DATE:    08/03/01 03:16:54 GMT
FROM:    Michitoshi Yoshida at Okayama Astrophysical Obs  <yoshida@oao.nao.ac.jp>

M. Yoshida, K. Yanagisawa, Y. Shimizu, S. Nagayama, H. Toda
 (OAO, NAOJ) and N. Kawai (Tokyo Tech) report on behalf of the
MITSuME collaboration:

We performed optical imaging observations (g', Rc, and Ic) of the
field of GRB 080229 (Cannizzo et al. GCN 7335) with 50cm MITSuME
telescope at Okayama Astrophysical Observatory from UT 17:06:55
(117sec after the trigger) to UT 17:24:40 on Feb 29 2008.

We found a faint fading source in the XRT error circle (Cannizzo
et al: GCN 7335) only in the Ic band. There was no source in the
g' and the Rc bands. Together with the UVOT results (Kuin and
Cannizzo GCN7339), this may suggest that this GRB is a high-
redshift one. Follow-up observations in infrared bands are
encouraged.

The magnitude of the fading source and 3-sigma upper limits are
summarized below.

Observation date  2008-02-29 UT

mid-UT    exp-T      g'      Rc       Ic
---------------------------------------------
17:09:40   5 min   >17.5   >17.8    17.1+-0.3
17:18:58  11 min   >17.6   >18.2    >18.0
---------------------------------------------

The values quoted above are not corrected for the Galactic
extinction.


GRB_name: GRB080229A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7342
SUBJECT: GRB 080229: REM NIR observations
DATE:    08/03/01 07:00:23 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

P. D'Avanzo, L.A. Antonelli, S. Covino, D. Fugazza, L.  Calzoletti, S. 
Campana, G.  Chincarini, M.L. Conciatore, S. Cutini, V. D'Elia, F. 
D'Alessio, F.  Fiore, P. Goldoni, D. Guetta,  C. Guidorzi, G.L. Israel, 
E. Maiorano, N. Masetti, A. Melandri, E. Meurs, L. Nicastro, E. Palazzi, 
E. Pian, S. Piranomonte, L.  Stella, G.  Stratta, G. Tagliaferri, G. 
Tosti, V.Testa, S.D. Vergani,  F. Vitali report on behalf of the REM team:

The robotic 60-cm REM telescope located at La Silla (Chile) observed 
automatically the field of the GRB 080229 (Cannizzo et al., GCN 7335) on 
March 01.154 UT (about 10.6 hours after the burst).

We do not detect any afterglow candidate inside the XRT error box down 
to the following limiting magnitudes (3sigma c.l., calibrated against 
the 2MASS catalog):

J > 16.3
H > 15.6
K > 14.4

Further analysis is in progress.


GRB_name: GRB080229A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7343
SUBJECT: GRB 080229: Enhanced Swift-XRT position
DATE:    08/03/01 07:18:20 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.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 1276 s of overlapping XRT Photon Counting mode and UVOT
V-band data for GRB 080229, 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 = 228.21828, -14.70467 which is equivalent
to:

RA (J2000): 15h 12m 52.39s
Dec (J2000): -14d 42' 16.8"

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
http://www.swift.ac.uk/xrt_positions/Goad.pdf).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB080229A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7344
SUBJECT: GRB 080229:  Deep Gemini/GMOS optical observations
DATE:    08/03/01 07:53:03 GMT
FROM:    Edo Berger at Princton U  <eberger@astro.princeton.edu>

E. Berger (Princeton/Carnegie) reports on behalf of a larger 
collaboration:

"We observed the refined BAT error circle of GRB 080229 (GCN #7338) with 
GMOS on the Gemini-South telescope starting on 2008 Mar 1.26 UT (13.1 
hours after the burst).  We obtained a total of 5x120 sec in g,r,i,z is 
0.8" seeing.  We do not detect any sources within the XRT error circle 
(GCN #7343) to the following 3-sigma magnitude limits: g>26.0, r>25.9, 
i>25.6, z>25.3."


GRB_name: GRB080229A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7345
SUBJECT: GRB 080229: TNG NIR observations
DATE:    08/03/01 08:00:00 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

P. D'Avanzo, C. Guidorzi (INAF-OAB) on behalf of the CIBO collaboration 
and G. Andreuzzi and Noemi Pinilla Alonso (FGG-INAF, TNG) report:

We observed the field of the GRB 080229 (Cannizzo et al., GCN 7335) with 
the Italian 3.6m TNG telescope located at Canary Islands on March 01.259 
UT (about 13.1 hours after the burst). Observations have been carried 
out with the NICS NIR camera in imaging mode under good (1.1") seeing 
conditions.

We do not detect any afterglow candidate inside the enhanced XRT error 
box (Beardmore et al., GCN 7343) down to the following limiting 
magnitudes (3sigma c.l., calibrated against the 2MASS catalog):

J > 20.9
H > 20.1
K > 19.5


GRB_name: GRB080229A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7346
SUBJECT: GRB080229: Swift XRT refined analysis
DATE:    08/03/01 12:39:34 GMT
FROM:    Jirong Mao at INAF-OAB  <jirong.mao@brera.inaf.it>

GRB080229: Swift XRT refined analysis

J.Mao, (INAF-OAB), A. Moretti (INAF-OAB), J. Canizzo (NASA/UMBC), C. 
Guidorzi
(Univ. Bicocca & INAF-OAB), A, Beardmore (U Leicester)
P. Evans (U Leicester) report on behalf of the Swift-XRT team:

We have analysed the first 2 orbits of Swift-XRT data obtained for
BAT GRB 080229 (trigger #304379, Cannizzo, et al., GCN Circ. 7335).

The data consist of 149 s in Windowed Timing (WT) mode, starting 90 s
after the BAT trigger and 8.34 ks in Photon Counting (PC) mode.
The astrometrically corrected X-ray position is given  in Beardomre et 
al. GCN 7324.

The XRT light-curve shows a flare peaking few seconds after the beginning
of the observation (103+/-2 s). The descending part of the flare can be 
fit by a power law with
a slope of alpha1=4.45+/-0.09 up to a break at t1=192.4+/- 2.5 s, which is
followed by a flat decay with a slope of alpha2=0.18+/-0.01.
A second break is present at 2700+/-1000 s with alpha3=0.8+/-0.5

The spectrum formed from all the WT data can be modeled with a
power-law of photon index Gamma = 2.88  0.09, with an absorbing
column of NH = (3.1  0.2)e21 cm^-2 (in excess with respect to the
Galactic value of 8.97e20 cm^-2). The spectrum formed from the PC data
can be modeled with a power-law of photon index Gamma = 1.99 
0.07, with an absorbing column of NH = (3.1  0.2)e21 cm^-2, which
is in agreement with the WT one.

If the light-curve continues to decay with a slope of 0.8, the
afterglow at 24 hour will be still bright with an expected count
rate of 0.3 count s^-1. This corresponds to an observed (unabsorbed) flux
of 1.41E-11(2.2e-11) erg cm-2 s-1.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB080229A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7347
SUBJECT: GRB 080229: VLT NIR observations
DATE:    08/03/01 18:28:34 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

P. D'Avanzo and G. Tagliaferri (INAF-OAB) on behalf of the MISTICI 
collaboration report:

We observed the field of the GRB 080229 (Cannizzo et al., GCN 7335) with 
the ESO-VLT on March 01.411 UT (about 16.8 hours after the burst). 
Observations have been carried out in J-band with the ISAAC NIR camera 
in imaging mode under very good (0.7") seeing conditions.

We do not detect any afterglow candidate inside the enhanced XRT error 
box (Beardmore et al., GCN 7343) down to J > 21.6 (3sigma c.l., 
calibrated against the 2MASS catalog).

We acknowledge support from the ESO staff, in particular Thomas Szeifert.


GRB_name: GRB080229A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7348
SUBJECT: GRB 080229: I-band observations from OSN
DATE:    08/03/01 18:54:39 GMT
FROM:    Antonio Deugarte at IAA-CSIC  <deugarte@iaa.es>

A. de Ugarte Postigo (ESO, Chile), F. Aceituno,
A.J. Castro-Tirado (IAA-CSIC, Spain) on behalf
of a larger colaboration report,

We have observed the field of GRB 080229 (Cannizzo et al. GCN 7335)
with the 1.5m telescope at Sierra Nevada Observatory (OSN, Granada).
The observations were obtained in I-band and range between March
1.1681 and March 1.2638 UT (mean exposure 0.5042 days after the burst).
We do not detect any new source in the error box of Swift/XRT
(Beardmore et al. GCN 7343) down to a 3-sigma limiting magnitude of
I~22.0.

This message can be cited.


GRB_name: GRB080303A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7349
SUBJECT: GRB 080303A: ROTSE-III Optical Limits
DATE:    08/03/03 09:38:13 GMT
FROM:    Brad Schaefer at LSU  <schaefer@grb.phys.lsu.edu>

B. E. Schaefer (Louisiana State) and W. Rujopakarn (Steward), report on 
behalf of the ROTSE collaboration:

ROTSE-IIIa, located at Siding Spring Observatory, Australia, responded to 
GRB 080303A (Swift trigger 304549), producing images beginning 8.4 s after 
the GCN notice time. An automated response took the first image at 
09:10:55.3 UT, 20.0 s after the burst, and during the gamma-ray emission, 
under twilight conditions. We took 10 5-sec, 10 20-sec and 10 60-sec 
exposures. These unfiltered images are calibrated relative to USNO A2.0 
(R). Imaging is on going.

Comparison to the DSS (second epoch) reveals no new sources within the 
3-sigma Swift/BAT error circle or the XRT error circle, for both single 
images and coadding into sets of 10; the field is not crowded. Individual 
images have limiting magnitudes ranging from 13.3-15.8, with the poor 
limits at the start due to the bright twilight that was rapidly fading.  
We set the following specific limits.

start UT       end UT      t_exp(s)   mlim   t_start-tGRB(s)  Coadd?
--------------------------------------------------------------------
09:10:55.4   09:11:00.4         5     13.3           20.1       N
09:10:55.4   09:13:06.9       131     14.1           20.1       Y
09:21:35.1   09:29:30.1       475     16.2          659.8       Y


GRB_name: GRB080303A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7350
SUBJECT: GRB 080303: REM NIR afterglow candidate
DATE:    08/03/03 09:39:13 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

P. D'Avanzo, D. Fugazza, L.A. Antonelli, S. Covino, L.  Calzoletti, S. 
Campana, G.  Chincarini, M.L. Conciatore, S. Cutini, V. D'Elia, F. 
D'Alessio, F.  Fiore, P. Goldoni, D. Guetta,  C. Guidorzi, G.L. Israel, 
E. Maiorano, N. Masetti, A. Melandri, E. Meurs, L. Nicastro, E. Palazzi, 
E. Pian, S. Piranomonte, L.  Stella, G.  Stratta, G. Tagliaferri, G. 
Tosti, V.Testa, S.D. Vergani,  F. Vitali report on behalf of the REM team:

The robotic 60-cm REM telescope located at La Silla (Chile) observed 
automatically the field of the GRB 080303  on March 03 09:13:30 UT 
(about 180 seconds after the burst).

We detect an afterglow candidate inside the XRT error box down at the 
following coordinates (J2000):

R.A.= 07:28:13.91
Dec.: -70:14:00.3

with an uncertainty of 0.4". The object has H~15.9.

Further analysis is in progress.


GRB_name: GRB080303A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7351
SUBJECT: GRB 080303: Swift detection of a burst with optical afterglow
DATE:    08/03/03 09:41:42 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

T. Sakamoto (NASA/UMBC), W. H. Baumgartner (GSFC/UMBC),
A. P. Beardmore (U Leicester), G. Cusumano (INAF-IASFPA),
P. A. Evans (U Leicester), N. Gehrels (NASA/GSFC), C. Gronwall (PSU),
E. A. Hoversten (PSU), N. P. M. Kuin (MSSL), J. Mao (INAF-OAB),
A. Moretti (INAF-OAB), P. T. O'Brien (U Leicester),
S. R. Oates (UCL-MSSL), J. P. Osborne (U Leicester),
K. L. Page (U Leicester), D. M. Palmer (LANL),
D. Perez (U Leicester), P. Romano (INAF-IASFPA),
M. Stamatikos (NASA/ORAU), R. L. C. Starling (U Leicester),
G. Stratta (ASDC), G. Tagliaferri (INAF-OAB),
E. Troja (U Leicester/INAF-IASFPa) and H. Ziaeepour (UCL-MSSL) report
on behalf of the Swift Team:

At 09:10:35 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 080303 (trigger=304549).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 112.073, -70.240 which is 
   RA(J2000) = 07h 28m 18s
   Dec(J2000) = -70d 14' 23"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a FRED-like 
structure with a duration of about 30 sec.  The peak count rate
was ~2600 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 09:11:47.7 UT, 72.4 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source with an enhanced position: RA, Dec
112.05892, -70.23448 which is equivalent to:
   RA(J2000)  = 07h 28m 14.14s
   Dec(J2000) = -70d 14' 04.1"
with an uncertainty of 2.6 arcseconds (radius, 90% containment). This
location is 26 arcseconds from the BAT onboard position, within the BAT
error circle. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of
1.26e+21 cm^-2 (Kalberla et al. 2005), so we cannot constrain the
redshift at this time using the relation from Grupe et al. (2007). A
summary of the promptly downlinked data is given at
http://www.swift.ac.uk/sper/304549/. 

The initial flux in the 2.5 s image was 4.53e-10 erg cm^-2 s^-2 (0.2-10
keV). 

UVOT took a finding chart exposure of 100 seconds with the White
(160-650 nm) filter starting 80 seconds after the BAT trigger. There
is a candidate afterglow in the rapidly available 2.7'x2.7' sub-image
at
    RA(J2000) = 07:28:14.14 = 112.0589  
    DEC(J2000) = -70:14:01.7 = -70.2338 
with a 1-sigma error radius of about 0.6 arc sec. This
position is 2.4 arc sec. from the center of the XRT error circle. The
estimated magnitude is 18.4 with a 1-sigma error of about 0.5 mag. A
400s V band image was taken beginning 186 s after the burst. The
estimated magnitude is 18.3 with a 1 sigma error of 0.5 magnitudes. 
At 986 s after the burst the source is undetected in a 108 s V band
exposure. The typical limiting magnitude is 18.0 magnitudes in an
exposure of this length. No correction has been made for the expected
extinction corresponding to E(B-V) of 0.19. 

Burst Advocate for this burst is T. Sakamoto (Taka.Sakamoto AT nasa.gov). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB080303A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7352
SUBJECT: GRB 080303
DATE:    08/03/03 11:01:48 GMT
FROM:    Alan Gilmore at U of Canterbury,Mt John Obs  <alan.gilmore@canterbury.ac.nz>

A.C. Gilmore and P.M. Kilmartin (University of Canterbury's Mt John Observatory 
report:

We observed a fading source inside the XRT error box at coordinates (2000.0) 
R.A. = 07:28:14.10
Dec.: -70:14:01.4
Uncertainty ~0.5" in poor seeing.

Unfiltered R magnitudes from comparison with USNO A2.0 stars
 U.T.   R
09:28  18.1
09:40  18.5
09:48  19.0
10:02  19.2
10:13  19.4
10:28  19.9 

Observations with Mt John's 1.0-metre f/8 McLellan reflector.

This message may be cited.


GRB_name: GRB080303A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7353
SUBJECT: GRB 080303A: Faulkes Telescope South optical afterglow observations
DATE:    08/03/03 11:19:42 GMT
FROM:    Andreja Gomboc at LT,ARI,Liverpool JMU  <ag@astro.livjm.ac.uk>

A. Gomboc (U. Ljubljana), R.J. Smith, D.F. Bersier, S. Kobayashi, A. 
Melandri, A. Monfardini, C.G. Mundell, I.A. Steele (Liverpool JMU), C. 
Guidorzi (U. Bicocca & INAF-OAB), P. O'Brien, E. Rol, N. Bannister 
(Leicester) report:

The 2-m Faulkes Telescope South (Siding Spring) robotically followed up 
GRB 080303A (SWIFT trigger 304549) starting 3.3 min after the GRB trigger 
time. We detect an optical afterglow candidate in R, B, and i' filters at 
the position consistent with the UVOT (Sakamoto et al, GCN 7351),
REM (D'Avanzo et al., GCN 7350) and Mt. John (Gilmore & Kilmartin, GCN 
7352) optical afterglow candidate.

The magnitude of the source was R~17.4+-0.3 and 19.7+-0.3 at 8 min and 50 
min after the trigger time, respectively.


GRB_name: GRB080229B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7354
SUBJECT: GRB080229B: Swift XRT afterglow observation
DATE:    08/03/03 11:53:47 GMT
FROM:    Alberto Moretti at Obs Brera Merate  <alberto.moretti@brera.inaf.it>

A. Moretti (INAF-OAB), J. Mao (INAF-OAB), C. Guidorzi
(Univ. Bicocca & INAF-OAB) report on behalf of the Swift-XRT team:

We have analysed the Swift-XRT observation of GRB 080229B detected by
SuperAgile (Evangelista et al. GCN Circ).  The data consist of 13.4 ks
in Photon Counting (PC) mode starting 27 hours after the SuperAGILE
trigger and ending at 48 hours.

We found a fading, uncatalogued X-ray source at the position: RA:199.25169
Dec:-64.86239 which is equivalent to:

   RA(J2000)  = 13h 17m 00.40s
   Dec(J2000) = -64d 51' 44.6"

with an uncertainty of 3.9 arcseconds (radius, 90% containment). This
location is 73 arcseconds from the SuperAGILE position.

The afterglow is decaying with a power-law slope of 0.9+/-0.5.  

The spectral parameters are poorly constrained due to the paucity of
the statistics (~100 photons).  The spectrum can be modelled with a
power-law of photon index Gamma = 2.8 +/- 1.0, with an absorbing
column of NH = (1.4 +/- 0.7)e22 cm^-2 (consistent with the
Galactic value of 8.9e21 cm^-2).

If the light-curve continues to decay with a slope of 0.9, the
afterglow at 3 days (March 4th) will have an expected count rate of
0.0085 count s-1. This corresponds to an observed (unabsorbed)
flux of 5.8E-13 (2.2e-12) ergs cm-2 s-1.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB080229B
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7355
SUBJECT: Swift UVOT observations of GRB080229B
DATE:    08/03/03 13:45:48 GMT
FROM:    Massimiliano de Pasquale at MSSL-UCL  <mdp@mssl.ucl.ac.uk>

M. De Pasquale (MSSL/UCL) and J. K. Cannizzo (NASA/UMBC) report
on behalf of the Swift-UVOT team:

The Swift/UVOT observed the field of 080229B, detected by
SuperAgile (Evangelista et al. GCN CIRC 7340), starting 76.3 Ks
after the trigger. Exposures were taken in the v band.
No optical afterglow is detected at the position of the refined
XRT position (Moretti et al. GCN CIRC 7354) in the first 5
summed exposures.

  The following 3-sigma upper limit (in the UVOT photometric
system, Breeveld et al., GCN Circ. 6614) was determined at the
XRT position (RA=13:17:00.4 DEC= -64:51:44.6 J2000):

  Filter  Tstart(Ks)  Tstop(Ks)  Exp(s)   Mag

    v        76.27     104.73     816    >19.8


  We note that this field is very crowded and it suffers from a
high Galactic reddening E(B-V) = 1.9.


GRB_name: GRB080303A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7356
SUBJECT: GRB 080303: Enhanced Swift-XRT position
DATE:    08/03/03 15:12:21 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.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 1194 s of overlapping XRT Photon Counting mode and UVOT
data for GRB 080303, 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 = 112.05899, -70.23431 which is equivalent
to:

RA (J2000): 07h 28m 14.16s
Dec (J2000): -70d 14' 03.5"

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
http://www.swift.ac.uk/xrt_positions/Goad.pdf).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB080303A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7357
SUBJECT: GRB080303: Swift XRT refined analysis
DATE:    08/03/03 16:49:21 GMT
FROM:    Jirong Mao at INAF-OAB  <jirong.mao@brera.inaf.it>

GRB080303: Swift XRT refined analysis

J. Mao (INAF-OAB), A. Moretti (INAF-OAB), T. Sakamoto (NASA/UMBC),
C. Guidorzi (Univ. Bicocca & INAF-OAB) report on behalf of the Swift-XRT 
team:

We have analysed the Swift-XRT data obtained for
BAT GRB 080303 (trigger #304549, Sakamoto, et al., GCN Circ. 7351).
The data consist of 105 s in Windowed Timing (WT) mode, starting 80 s
after the BAT trigger and 206 s in Photon Counting (PC) mode.
The UVOT-enhanced XRT position was given in Evans et al. (GCN Circ. 7356).

The light-curve shows a simple power-law with a slope of alpha=1.65  0.05.

The spectrum formed from all the WT data can be modeled with a power-law 
of photon index
Gamma = 1.88  0.12, with an absorbing column of NH = (1.32  0.03)e21 
cm^-2 (in excess
with respect to the Galactic value of 8.97e20 cm^-2). The spectrum 
formed from the PC data
can be modeled with a power-law of photon index Gamma = 1.81  0.17, 
with an absorbing
column of NH = (5.72  4.77)e20 cm^-2.

If the light-curve continues to decay with a slope of 1.65, the 
afterglow at 24 hour will be with
an expected count rate of 1.5e-4 count s^-1. This corresponds to an 
observed (unabsorbed) flux
of 7E-15(9e-15) erg cm-2 s-1.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB080303A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7358
SUBJECT: GRB 080303: Rapid PROMPT Detections
DATE:    08/03/03 22:16:57 GMT
FROM:    Mark Schubel at UNC/PROMPT  <mschubel@physics.unc.edu>

M. Schubel, T. Brennan, D. Reichart, M. Nysewander, A. LaCluyze, K. Ivarsen, J. A. Crain, A. Foster, J. Haislip, J. Styblova, and A. Trotter report:

Skynet observed the localization of GRB 080303 (Sakamoto et al., GCN 7351) with two of the 16" PROMPT telescopes at CTIO beginning 45 seconds after the burst (30 seconds after notification) in VRI.

We detect the afterglow (D'Avanzo et al., GCN 7350) in R and I.  At 182 seconds after the burst we measure I ~ 16.2 mag, and at 242 seconds we measure R ~ 17.0 mag (calibrated to 5 USNO B1 stars).


GRB_name: GRB080303A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7359
SUBJECT: GRB 080303, Swift-BAT refined analysis
DATE:    08/03/03 23:05:07 GMT
FROM:    Takanori Sakamoto at NASA/GSFC  <Taka.Sakamoto@nasa.gov>

T. Sakamoto (GSFC/UMBC), S. D. Barthelmy (GSFC), J. Cummings (GSFC/UMBC),
E. Fenimore (LANL), N. Gehrels (GSFC), H. Krimm (GSFC/USRA), 
C. Markwardt (GSFC/UMD), K. McLean (GSFC/UMD), D. Palmer (LANL),
A. Parsons (GSFC), G. Sato (GSFC/ISAS), M. Stamatikos (GSFC/ORAU),
J. Tueller (GSFC), T. Ukwatta (GWU)
(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 080303 (trigger #304549)
(Sakamoto, et al., GCN Circ. 7351).  The BAT ground-calculated position is
RA, Dec = 112.019, -70.231 deg which is 
   RA(J2000)  = 7h 28m 4.6s 
   Dec(J2000) = -70d 13' 53" 
with an uncertainty of 1.6 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 80%.
 
The mask-weighted light curve shows a FRED-like peak T-1 sec, peaking at 
T+0.5 sec, and ending at T+20 sec.  There is also an extended emission until 
T+~90 sec.  T90 (15-350 keV) is 67 +- 20 sec (estimated error including systematics).
 
The time-averaged spectrum from T-0.2 to T+73.2 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.54 +- 0.25.  The fluence in the 15-150 keV band is 6.6 +- 1.0 x 10^-7 erg/cm2.  
The 1-sec peak photon flux measured from T+0.06 sec in the 15-150 keV band
is 1.4 +- 0.2 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/304549/BA/


GRB_name: GRB080303A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7360
SUBJECT: GRB 080303: Swift/UVOT follow-up of afterglow detection
DATE:    08/03/03 23:18:28 GMT
FROM:    Alice Breeveld at MSSL-UCL  <aad@mssl.ucl.ac.uk>

A.A. Breeevld (MSSL/UCL) and T. Sakamoto (GSFC/UMBC) report on behalf 
of the Swift UVOT team:

The Swift/UVOT observed the burst GRB080303 (Sakamoto et al. GCN circ 
7351) starting with the finding chart exposure in white, 81s after the 
BAT trigger. The afterglow is detected at the enhanced XRT position 
(Evans et al. GCN circ 7356) in all filters except uvm2. In white it is 
detectable until at least 6600s after the trigger. The brightness 
increases until about 700s after the burst, then fades with an 
estimated temporal slope in the v filter of alpha= 0.9

The initial UVOT magnitudes (in the UVOT photometric system; Breeveld 
et al. GCN circ 6614) and 3 sigma upper limts from single exposures are 
as follows:

Filter    Tstart(s)    Tstop(s)    Exp(s)   Mag      error(mags)
white    81            180             99.8      18.48    0.08
              682           691             9.8        18.19    0.19
              836           845             9.8        18.46    0.24
              880           979             99.8      18.88    0.11
             5195          5394          199.8    20.79    0.38
             6632           6831         199.8    20.72    0.35
v         187             586             399.8    18.03   0.08
             722             741            19.8       17.74   0.3
             987            1095           108.1    19.06    0.3
             5607          5806           199.8    19.76   0.38
b           667           676               9.8       18.59   0.36
               821           830              9.7         >18.74  (UL)
             4991          5190           199.8      >20.86  (UL)
             6427          6626           199.8     20.26   0.27
u           642             661             19.8     18.23    0.32
               797           816              19.8     17.99    0.26
             4785          4984            199.8    19.4     0.22
             6221          6420            199.8    20.33    0.41
uvw1    618            637             19.8        >18.1  (UL)
               771            790             19.7      17.83    0.38
              4581          4780            199.8   19.84    0.43
              6016          6215             199.8      >20.18 (UL)
uvm2    593            612               19.8        >17.58 (UL)
               746            765               19.8         >17.61 (UL)
               4375          4574            199.8       > 19.69 (UL)
                5811         6010            199.8      >19.76  (UL)
uvw2     698              717             19.8       >18.01 (UL)
                 851            870              19.8       17.82   0.37
               5401          5600            199.7       19.76 0.33
               6838          6875              37.6        >18.7  (UL)

The values quoted above are not corrected for the expected Galactic 
extinction corresponding to a reddening of E(B-V)=0.192 mag in the 
direction of the burst (Schlegel et al. 1998).


GRB_name: GRB080229A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7361
SUBJECT: VLA possible radio detection of GRB 080229 
DATE:    08/03/04 13:46:24 GMT
FROM:    Poonam Chandra at U Virginia/NRAO  <pc8s@virginia.edu>

Poonam Chandra (NRAO/UVA) and Dale A. Frail (NRAO) report on
behalf of the Caltech-NRAO-Carnegie GRB Collaboration:


"We used the Very Large Array to observe the field of view toward
GRB 080229 (GCN 7335) at a frequency of 8.46 GHz on 2008 March
01.50 UT. We detect a radio source of flux density of 635 +/- 44
uJy at a position of
RA(J2000) 15 12 52.21984, DEC(J2000) -14 42 15.3000.
This is 2.82" away from the X-ray afterglow position determined by
Swift-XRT (GCN 7343).

The National Radio Astronomy Observatory is a facility of the National
Science Foundation operated under cooperative agreement by Associated
Universities, Inc."


GRB_name: GRB080307A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7362
SUBJECT: GRB 080307: Swift detection of a burst
DATE:    08/03/07 12:01:53 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

S. T. Holland (CRESST/USRA/GSFC), S. D. Barthelmy (GSFC),
D. N. Burrows (PSU), J. R. Cummings (NASA/UMBC),
G. Cusumano (INAF-IASFPA), P. A. Evans (U Leicester),
N. Gehrels (NASA/GSFC), O. Godet (U Leicester),
C. Guidorzi (INAF-OAB), S. D. Hunsberger (PSU), J. A. Kennea (PSU),
V. Mangano (INAF-IASFPA), C. B. Markwardt (CRESST/GSFC/UMD),
A. Moretti (INAF-OAB), P. T. O'Brien (U Leicester),
J. P. Osborne (U Leicester), C. Pagani (PSU),
K. L. Page (U Leicester), D. M. Palmer (LANL),
D. Perez (U Leicester), P. Romano (INAF-IASFPA), G. Sato (GSFC/ISAS),
M. Stamatikos (NASA/ORAU), R. L. C. Starling (U Leicester) and
E. Troja (U Leicester/INAF-IASFPA) report on behalf of the Swift
Team:

At 11:23:30 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 080307 (trigger=305011).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 136.633, +35.168 which is 
   RA(J2000) = 09h 06m 32s
   Dec(J2000) = +35d 10' 06"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a FRED
structure with a duration of at least 30 sec.  The peak count rate
was ~600 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 11:25:10.1 UT, 99.3 seconds after
the BAT trigger. Using promptly downlinked data we find a bright, fading
uncatalogued X-ray source with an enhanced position: RA, Dec 136.62833,
35.13866 which is equivalent to:
   RA(J2000)  = 09h 06m 30.80s
   Dec(J2000) = +35d 08' 19.2"
with an uncertainty of 2.6 arcseconds (radius, 90% containment). This
location is 106 arcseconds from the BAT onboard position, within the
BAT error circle. No prompt spectrum is yet available to assess possible
redshift constraints using X-ray spectroscopy and the nH-z relation
from Grupe et al. (2007). 

The initial flux in the 2.5 s image was 7.63e-10 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 100 seconds with the White (160-650 nm)
filter starting 105 seconds after the BAT trigger. A possible fading source
that is not present in the DSS has been found in the initial data products at

    RA(J2000) =  09:06:25.5
   Dec(J2000) = +35:08:39

with an estimated uncertainty of 0.6 arcsec (radius, 90% confidence).  This
source is approximately 1 arcminute from the XRT position, which is too far
away to be consistent with the X-ray source.  The estimated white magnitude
 is 19.6 +/- 0.1.  No correction has been made for the expected
extinction corresponding to E(B-V) of 0.03 mag. 

Burst Advocate for this burst is S. T. Holland (sholland AT milkyway.gsfc.nasa.gov). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB080307A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7363
SUBJECT: GRB 080307: Optical observation with DMC/KANATA
DATE:    08/03/07 12:33:44 GMT
FROM:    Makoto Uemura at Hiroshima U  <uemuram@hiroshima-u.ac.jp>

M. Doi, S. Sako, J. Hayano, Y. Ihara, N. Takanashi, 
H. Kuncarayakti (The Univresity of Tokyo), D. Kuroda (NAOJ), 
K. S. Kawabata, and M. Uemura (Hiroshima Univ.)
report on behalf of the DMC team:

  We took optical CCD images of the field of GRB 080307 (GCNC 7362)
with Dichroic Mirror Camera (DMC; http://www.ioa.s.u-tokyo.ac.jp/dmc/)
attached to the 1.5-m KANATA telescope.  
DMC enables us to simultenaously obtain 15 band images in the 
optical range (typical delta lambda = 35 nm). 
We started observations at 11:31:18 (UT) 7 March 2008, 
467 s after the burst.  The exposure time was 60 s.  

No candidate of its optical afterglow brighther than 
r=17.13 mag (USNO B1.0 1251-0170228; RA=09:06:33.62, Dec=+35:08:44.1)
was found in our all images.

YYYYDDMM(UT)    limit mag.   center of wavelengths   
20080307.4804    17.13 r     641nm (chanel 07 of DMC) 


GRB_name: GRB080307A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7364
SUBJECT: GRB 080307 : BOAO optical afterglow observation
DATE:    08/03/07 13:35:23 GMT
FROM:    Yuji Urata at Saitama U  <urata@asiaa.sinica.edu.tw>

M. Im, I. Lee, W.K. Zheng, K.Y. Huang, Y. Urata
on behalf of EAFON report:

"We have been imaging the GRB 080307 optical afterglow (Holland et
al. #7362) using the 1.8 m telescope of the Bohyunsan Optical
Astronomy Observatory, Korea. The optical afterglow brightness at 
67 min after the burst is R~20.3 mag. 
Further deeper imaging are encouraged."

We thank J. Seo, and Y. Jeon for their assistance with the BOAO observation.
This message may be cited.


GRB_name: GRB080307A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7365
SUBJECT: GRB 080307, Preliminary Swift-BAT refined analysis
DATE:    08/03/07 13:52:56 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

D. Palmer (LANL), S. D. Barthelmy (GSFC), J. Cummings (GSFC/UMBC),
E. Fenimore (LANL), N. Gehrels (GSFC), S. T. Holland (CRESST/USRA/GSFC),
H. Krimm (GSFC/USRA), C. Markwardt (GSFC/UMD), K. McLean (GSFC/UMD),
T. Sakamoto (GSFC/UMBC), G. Sato (GSFC/ISAS), M. Stamatikos (GSFC/ORAU),
J. Tueller (GSFC), T. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using only a small amount of data set from the first telemetry downlink
(from T-119 to T+183 sec), we report preliminary analysis of BAT GRB 080307
(trigger #305011) (Holland, et al., GCN Circ. 7362).
The BAT ground-calculated position is RA, Dec = 136.626, 35.156 deg, which is 
   RA(J2000)  = 09h 6m 30.2s 
   Dec(J2000) = 35d 9' 20" 
with an uncertainty of 1.7 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 81%.
 
The mask-weighted light curve shows an initial FRED-like peak
starting at T+0 sec, and ending around T+80 sec.  There is evidence
for emission out to T+135 sec (and the end of the downlinked data ends
at T+183 sec).  T90 (15-350 keV) is 64 +- 22 sec (estimated error
including systematics).
 
Using this partial data set, the time-averaged spectrum from T-7.4 to T+56.6 sec
is best fit by a simple power-law model.  The power law index of the time-averaged
spectrum is 1.41 +- 0.19.  The fluence in the 15-150 keV band is
7.3 +- 0.9 x 10^-7 erg/cm2.  The 1-sec peak photon flux measured from T+16.06 sec
in the 15-150 keV band is 0.2 +- 0.0 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/305011/BA/
 
This burst satisfies Sakamoto/Ukwatta Swift-BAT possible high-z criteria
(Ukwatta et al. arXiv:0802.3815):
1) The power law photon index (= 1.41) is less than 2,
2) The 1-s peak photon flux (= 0.19) is less than 1.0 ph/cm2/s,
3) The light curve variance (= 2.11e-05 is less than 0.0001,
4) The T90/Peak_photon_flux (= 336) is greater than 100.
Based on a limited sample of bursts, these criteria yield
an 85% chance it has a redshift greater than 3.5. 
We must stress however, that we have downlinked data out to only T+180 sec
and there is evidence of continued emissin out to T+135 sec.  So if there
is further activity in this burst past T+180 sec, then the spectral and
temporal values used in this hi-z indicator test may change
and no longer fit the hi-z criteria.  We are publishing this preliminary
refined circular on that chance the hi-z indicator is correct
and follow-up observsers can choose to make observations sooner.

We will issue the regular 'refined' circular when the full data set
becomes available.


GRB_name: GRB080307A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7366
SUBJECT: GRB 080307: Enhanced Swift-XRT position
DATE:    08/03/07 14:19:41 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

M.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 161 s of overlapping XRT Photon Counting mode and UVOT
data for GRB 080307, 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 = 136.62799, +35.13896 which is equivalent
to:

RA (J2000): 09h 06m 30.72s
Dec (J2000): +35d 08' 20.3"

with an uncertainty of 1.8 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
http://www.swift.ac.uk/xrt_positions/Goad.pdf).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB080307A
Detection_method: retraction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7367
SUBJECT: GRB 080307: retraction of UVOT candidate
DATE:    08/03/07 14:44:30 GMT
FROM:    Patricia Schady at MSSL/Swift  <ps@mssl.ucl.ac.uk>

P. Schady (MSSL/UCL) and S. T. Holland (CRESST/USRA/GSFC) report on 
behalf of the Swift UVOT team:

There was a typo in the position for the optical afterglow candidate 
for GRB 080307 reported by Holland et al., (GCN 7362), and this should, 
in fact, be

    RA(J2000) =  09:06:25.5
    Dec(J2000) = +35:08:29

with an estimated uncertainty of 1 arcsec. However, we note that the 
new UVOT position is 0.2" from a known source, and is therefore 
unlikely to be the optical afterglow of GRB 080307.


GRB_name: GRB080307A
Detection_method: retraction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7368
SUBJECT: GRB 080307: BOAO imaging - retraction and new limit
DATE:    08/03/07 14:56:48 GMT
FROM:    Myungshin Im at Seoul Nat U  <mim@astro.snu.ac.kr>

M. Im, I. Lee, W.K. Zheng, K.Y. Huang, Y. Urata
on behalf of EAFON team.

  Earlier, we reported the detection of the after glow of GRB080307
  (GCN Circular, #7364). Our reported afterglow at the UVOT position
  turned out to be a known star, and we retract our earlier report.
  We do not detect the GRB afterglow at the enhanced XRT position
  (GCN Circular #7366), and we place the limit of R > 21.2 at 3 sigma.
  Further analysis is ongoing.

  This message may be cited.


GRB_name: GRB080307A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7369
SUBJECT: GRB 080307: Gemini-N i-band observations - candidate afterglow
DATE:    08/03/07 15:05:05 GMT
FROM:    Nial Tanvir at IofA U.Cambridge  <nrt@ast.cam.ac.uk>

N. R. Tanvir (U. Leicester) reports on behalf of a larger collaboration.

We observed the field of GRB 080307 with Gemini-N/GMOS, beginning
at 12:50 (UT), approximately 85 minutes post-burst.  We detect a
point source in the i-band image within the XRT error circle (GCN 7366)
with (J2000) coordinates:

 09 06 30.78  +35 08 20.0

Provisional photometry relative to field SDSS stars gives a magnitude
of i=22.4 at this time.

We thank the Gemini staff, particularly Ricardo Schiavon, for
support in obtaining these observations.


GRB_name: GRB080307A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7370
SUBJECT: GRB080307: Optical upper limits
DATE:    08/03/07 15:59:54 GMT
FROM:    Michitoshi Yoshida at Okayama Astrophysical Obs  <yoshida@oao.nao.ac.jp>

M. Yoshida, K. Yanagisawa, Y. Shimizu, S. Nagayama, H. Toda
(OAO, NAOJ) and N. Kawai (Tokyo Tech) report on behalf of the
MITSuME collaboration:

We performed optical imaging observations (g', Rc, and Ic) of
the field of GRB 080307 (Holland et al. GCN 7362) with the
50cm MITSuME telescope at Okayama Astrophysical Observatory
from UT 11:25:50 to UT 12:47:00 on March 7 2008.

Flux calibration was made using USNO B1.0 catalog. We could
not identify any new source at the XRT position (Holland et al.
GCN 7362) or the UVOT positions (Schady et al. GCN 7367).
Three sigma upper limits are listed below.

mid-UT                exp.time     g'     Rc      Ic
-------------------------------------------------------
2008-03-07 11:31:20    10 min.   >19.6   >19.3   >18.7
2008-03-07 12:12:00    57 min.   >20.5   >20.3   >19.5
-------------------------------------------------------


GRB_name: GRB080307A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7371
SUBJECT: GRB 080307: TNT optical observation
DATE:    08/03/07 16:49:51 GMT
FROM:    W.K. Zheng at NAOC  <zwk@bao.ac.cn>

L.P. Xin, X.M. Meng, M. Zhai, J.S. Deng,
Y.L. Qiu, J.Y. Wei, J.Y. Hu, J. Wang, W.K. Zheng
Y. Urata, M. Im, I. Lee, K.Y. Huang, Y.
on behalf of EAFON report:

We have imaged the field of GRB080307 (Holland et al., GCN 7362) 
using the TNT 0.8 telescope at Xinglong observatory under good
condition. A set of White and R band images were obtained.
Preliminary result shows we margianally detected the afterglow
candidate (Tanvir, GCN 7369) in our combined images. By performing
PSF photometry, we have the following magnitude calibrated to the
USNO B1.0 R2 mag:

T_mid(min)  Mag    Band  Exp   Merr
-------------------------------------
15.71       20.9   W    10*20s  0.3
24.50       21.3   R    10*60s  0.3
70.28       22.1   R    8*300s  0.3

The source faded during our observation epoch, we confirm this
is the afterglow of GRB 080307.

This message may be cited. For more information about Xinglong
GRBs Follow-up observations, please visit the website:
http://www.xinglong-naoc.org/grb/


GRB_name: GRB080307A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7372
SUBJECT: GRB080307 - SDSS Pre-Burst Observations
DATE:    08/03/07 17:47:58 GMT
FROM:    Richard J. Cool at U.of AZ/Steward Obs  <rcool@as.arizona.edu>

Richard J. Cool (Arizona), Daniel J. Eisenstein (Arizona),
David W. Hogg (NYU), Michael R. Blanton (NYU), David J. Schlegel
(LBNL), J. Brinkmann (APO), Donald Q. Lamb (Chicago), Donald
P. Schneider (PSU), and Daniel E. Vanden Berk (PSU) report:

The Sloan Digital Sky Survey (SDSS) imaged the field of burst
GRB080307 prior to the burst.  As these data should be useful
as a pre-burst comparison and for calibrating photometry,
we are supplying the images and photometry measurements for
this GRB field to the community.

Data from the SDSS, including 5 FITS images, 3 JPGS, and
3 files of photometry and astrometry, are being placed at
http://mizar.as.arizona.edu/~grb/public/GRB080307

We supply FITS images in each of the 5 SDSS bands of a 8'x8'
region centered on the GRB position (ra=136.633 (09:06:31.9),
dec=35.1680 (35:10:04.8); Swift-BAT TRIGGER 305011), as well
as 3 gri color-composite JPGs (with different stretches). The
units in the FITS images are nanomaggies per pixel.  A pixel
is 0.396 arcsec on a side. A nanomaggie is a flux-density unit
equal to 10^-9 of a magnitude 0 source or, to the extent that
SDSS is an AB system, 3.631e-6 Jy.  The FITS images have WCS
astrometric information.

In the file GRB080307_sdss.calstar.dat, we report photometry
and astrometry of 301 bright stars (r<20.5) within 15' of the
burst location.  The magnitudes presented in this file are asinh
magnitudes as are standard in the SDSS (Lupton 1999, AJ, 118,
1406). Beware that some of these stars are not well-detected
in the u-band; use the errors and object flags to monitor
data quality.

In the files GRB080307_sdss.objects_flux.dat and
GRB080307_sdss.objects_magnitudes.dat, we report photometry
of 1032 objects detected within 6' of the GRB position.
We have removed saturated objects and objects with model
magnitudes fainter than 23.0 in the r-band.  The fluxes listed
in GRB080307_sdss.objects_flux.dat are in nanomaggies while
the magnitudes listed in GRB080307_sdss.objects_magnitudes.dat
are asinh magnitudes.

**Be aware that at least a portion of the photometry provided in
this release has been flagged as non-photometric. As photometry
for objects with this flag set may have non-optimal calibration,
we do not recommend these objects be used for photometric
calibration.  Non-photometric imaging may still be valuable
as a pre-burst comparison and for astrometric calibration.

All quantities reported are standard SDSS photometry, meaning
that they are very close to AB zeropoints and magnitudes are
quoted in asinh magnitudes.  Photometric zeropoints are known
to about 2% rms.  None of the photometry is corrected for
dust extinction.  The Schlegel, Finkbeiner, and Davis (1998)
predictions for this region are A_U=0.137 mag, A_g=0.101 mag,
A_r = 0.073 mag, A_i=0.055 mag, and A_z=0.039 mag.

The file GRB080307_sdss.spectro.dat contains a list of the
2 objects with SDSS spectroscopy within 6 arcminutes of the
GRB position.  In addition to the redshift and 1-sigma error
for each object, this file also lists the object spectroscopic
classification.


SDSS astrometry is generally better than 0.1 arcsecond per
coordinate.  Users requiring high precision astrometry should
take note that the SDSS astrometric system can differ from
other systems such as those used in other notices; we have
not checked the offsets in this region.

More detailed information pertaining to our SDSS GRB releases
can be found in our initial data release paper (Cool et
al. 2006, PASP 118, 733).  See the SDSS DR4 documentation for
more details: http://www.sdss.org/dr5.

These data have been reduced using a slightly different
pipeline than that used for SDSS public data releases.
We cannot guarantee that the values here will exactly match
those in the data release in which these data are included.
In particular, we expect the photometric calibrations to differ
by of order 0.01 mag.

This note may be cited, but please also cite the SDSS data
release paper, Adelman-McCarthy et al. (2007, ApJS, 172, 634),
when using the data or referring to the technical documentation.


GRB_name: GRB080307A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7373
SUBJECT: GRB 080307, Swift-BAT refined analysis
DATE:    08/03/07 18:47:06 GMT
FROM:    Goro Sato at GSFC  <gsato@milkyway.gsfc.nasa.gov>

G. Sato (GSFC/ISAS), S. D. Barthelmy (GSFC), J. Cummings (GSFC/UMBC),
E. Fenimore (LANL), N. Gehrels (GSFC), S. T. Holland (CRESST/USRA/GSFC),
H. Krimm (GSFC/USRA), C. Markwardt (GSFC/UMD), K. McLean (GSFC/UMD),
D. Palmer (LANL), A. Parsons (GSFC), T. Sakamoto (GSFC/UMBC),
M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC), T. Ukwatta (GWU)
(i.e. the Swift-BAT team):

Using the data set from T-239 to T+963 sec from the recent telemetry
downlink, we report further analysis of BAT GRB 080307 (trigger #305011)
(Holland, et al., GCN Circ. 7362, and Palmer, et al., GCN Circ. 7365).
The BAT ground-calculated position is RA, Dec = 136.629, 35.151 deg
which is
    RA(J2000)  = 9h 6m 31.0s
    Dec(J2000) = 35d 9' 4"
with an uncertainty of 1.6 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 81%.

The mask-weighted light curve shows an initial FRED-like peak
starting at T+0 sec, and ending around T+140 sec.  A strong spectral
evolution can be seen in the BAT four energy band light curves.
T90 (15-350 keV) is 125.9 +- 24.6 sec (estimated error including
systematics).

The time-averaged spectrum from T+1.7 to T+146.1 sec is best fit by a
simple power-law model.  The power law index of the time-averaged
spectrum is 1.78 +- 0.21.  The fluence in the 15-150 keV band is
8.7 +- 1.2 x 10^-07 erg/cm2.  The 1-sec peak photon flux measured from
T+1.90 sec in the 15-150 keV band is 0.4 +- 0.1 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/305011/BA/

This burst satisfies Sakamoto/Ukwatta Swift-BAT possible high-z criteria
(Ukwatta et al. arXiv:0802.3815):
1) The power law photon index (= 1.78) is less than 2,
2) The 1-s peak photon flux (= 0.4) is less than 1.0 ph/cm2/s,
3) The light curve variance (= 9.4e-06) is less than 0.0001,
4) The T90/Peak_photon_flux (= 350) is greater than 100.
Based on a limited sample of bursts, these criteria yield
an 85% chance it has a redshift greater than 3.5.


GRB_name: GRB080307A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7374
SUBJECT: GRB 080307: Early RAPTOR Limits
DATE:    08/03/07 18:59:18 GMT
FROM:    James Wren at LANL  <jwren@nis.lanl.gov>

J. Wren, W.T. Vestrand, P.R. Wozniak, H. Davis
of Los Alamos National Laboratory report:

Our Raptor telescopes responded to Swift trigger 305011
(Holland et al., GCN 7362) at 11:24:30.8 UTC, 60.0 seconds
after the trigger and 7.3 seconds after receipt of the GCN
packet.  We detect no new optical source at the Swift XRT
position.  Five sigma limiting magnitudes are given for
three of our unfiltered response images in the table below.
Calibration was performed using the USNO B1.0 R-band
magnitudes.

T-start (UTC)           T-exp (s)    mag limit
-------------------------------------------------
2008-03-07 11:24:30.81    5            16.9
2008-03-07 11:25:53.96    10           17.3
2008-03-07 11:30:12.01    30           18.0


GRB_name: GRB080307A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7375
SUBJECT: GRB 080307: Swift/UVOT Upper Limits 
DATE:    08/03/07 20:20:40 GMT
FROM:    Stephen Holland at USRA/NASA/GSFC/SSC  <sholland@milkyway.gsfc.nasa.gov>

S. T. Holland (CRESST/GSFC/USRA) reports on the behalf of the Swift
UVOT team:

        The Swift/UVOT observed the field of GRB 080307 starting 105 s
after the BAT trigger (Holland et al. 2008, GCN Circ. 7362).  We do not
find any source, in any of the UVOT observations, at the location of
the Gemini-North source (Tanvir, 2008 GCN Circ. 7369).

        The 3-sigma upper limits for detecting a source at this
location in the co-added images are:


Filter    T_start   T_stop    Exp(s)    Mag (3-sigma upper limit)
-----------------------------------------------------------------
   v         212      5754       676     >20.7
   b         691      6574       412     >21.4
   u         666      6369       432     >21.1
  uvw1       642      6164       432     >20.9
  uvm2       618      5959       413     >20.6
  uvw2       721      6816       245     >20.7
white       105      6779       599     >22.3
-----------------------------------------------------------------

The quoted upper limits have not been corrected for the expected
Galactic extinction along the line of sight corresponding to a
reddening of E_{B-V} = 0.03 mag.  All photometry is on the UVOT flight
system described in Poole et al. (2008, MNRAS, 383, 627).


GRB_name: GRB080307A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7376
SUBJECT: GRB 080307: Swift-XRT Team refined analysis
DATE:    08/03/07 21:37:34 GMT
FROM:    Kim Page at U.of Leicester  <kpa@star.le.ac.uk>

K.L. Page, J.P. Osborne (U. Leicester) & S.T. Holland (CRESST/GSFC/USRA) 
report on behalf of the Swift-XRT team:

We have analysed the first four orbits of data obtained for GRB 080307
(Holland et al., GCN Circ. 7362), which includes 509 seconds in Windowed 
Timing (WT) mode and 7.9 ks in Photon Counting (PC mode).

The UVOT-enhanced XRT position has been given by Goad et al. in GCN Circ 
7366.

In the first orbit of the XRT data, the emission rises slowly, peaking 
around 200-300 seconds after the BAT trigger, after which the decay can be 
modelled with a single power-law with alpha = 1.83 +/- 0.08. The shape of 
the early light-curve is reminiscent of GRB 060218 (Campana, S. et al, 
2006, Nature, 442, 1008).

As the X-ray emission rises, it also softens; the hardness ratio then 
becomes close to constant as the light-curve decay sets in. The PC data at 
the end of the first orbit can be fitted with an absorbed power-law, with 
Gamma = 1.74 +0.23/-0.21 and NH = (1.5 +0.8/-0.6)e21 cm^-2, which is in 
excess of the Galactic value of 2.37e20 cm^-2.  From the relation in Grupe 
et al. (2007, AJ, 133, 2216), this indicates a redshift of less than 4.0. 

The mean observed (unabsorbed) flux for the PC data at the end of the 
first orbit (615-1030 seconds) is 7.86e-11 (9.83e-11)  erg cm^-2 s^-1. The 
corresponding counts to (observed) flux conversion is 1 count s^-1 = 
4.9e-11 erg cm-2 s^-1.

If the light-curve continues to decay following a power-law of 1.83, the 
count rate at 24 hours is predicted to be 3.6e-4 count s^-1 (an observed 
flux of 1.8e-14 erg cm^-2 s^-1).

This circular is an official product of the Swift-XRT team.


GRB_name: GRB080229A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7377
SUBJECT: GRB080229, optical upper limit
DATE:    08/03/08 07:30:06 GMT
FROM:    Ryuuji Hara at U of Miyazaki  <ryuu55@astro.miyazaki-u.ac.jp>

R. Hara, H.hayasi, N.Ohmori, K.Kono H. Tanaka, M.Yamauchi, E.Sonoda,
(University of Miyazaki)

We have observed the field covering the error circle of
GRB080229 (GCN 7338, C. Markwardt et al.) with
the unfiltered CCD camera on the 30-cm telescope at
University of Miyazaki.
The observation was started 17:05:03 UT, ~225 min
after the Swift trigger time.

We have compared our data of 30 sec exposures
with the USNO-A2.0 catalog,there is no new source
at the reported position.

the upper limits are as follows:
--------------------------------------------------------------
Start(UT) End(UT) Num. of frames  Limit (mag.)
--------------------------------------------------------------
19:33:57 19:34:27  1   ~16.06
19:33:57 20:39:37  20   ~16.79
---------------------------------------------------------------


GRB_name: GRB080307A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7378
SUBJECT: GRB080307 BOAO optical afterglow observation - detection of a possible OT
DATE:    08/03/08 08:12:01 GMT
FROM:    Myungshin Im at Seoul Nat U  <mim@astro.snu.ac.kr>

  M. Im, I. Lee, Y. Urata, W.K. Zheng, K.Y. Huang,
on behalf of EAFON team.

   We re-analyzed the I-band images taken with the 1.8m telescope
  of the Bohyunsan Optical Astronomy Observatory, Korea.
  The I-band observation started at 76.1 min after the burst (Holland
  et al. #7362), and continued for 2100 secs.
  Our reanalysis of the stacked image show the detection of a possible
  optial transient within the error circle of the XRT position (Goad et al.
  #7366), and the reported Gemini-N i-band position (Tanvir et al.7369).
  The brightness of the OT, calibrated against USNO-B1 star at
  (09:06:31.6,+35:08,06.4), is I ~ 21.9 +- 0.3 mag with the error arising
  mostly from the uncertainty associated with the subtraction of
  the fringe pattern.
  Further deeper imaging is encouraged.

  We thank J. Seo and Yeon-Bom Jeon for their assistance with
  the BOAO observation.
  This message may be cited.


GRB_name: GRB080307A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7379
SUBJECT: GRB080307, optical upper limit
DATE:    08/03/10 06:59:51 GMT
FROM:    Hiroki Tanaka at U of Miyazaki  <hiro0218@astro.miyazaki-u.ac.jp>

H. Tanaka, R. Hara, K.Kono, N.Ohmori, H.hayasi, M.Yamauchi, E.Sonoda
(University of Miyazaki)


We have observed the field covering the error circle of
GRB080307 (GCN 7366, M.R. Goad et al.) with
the unfiltered CCD camera on the 30-cm telescope at
University of Miyazaki.
The observation was started 11:25:17 UT,
but it was cloudy then,so we got first image at 13:44:43 UT, ~141 min
after the Swift trigger time.

We have compared our data of 30 sec exposures
with the USNO-A2.0 catalog,there is no new source
at the reported position (GCN 7369, N. R. Tanvir)


the upper limits are as follows:
--------------------------------------------------------------
Start(UT) End(UT) Num. of frames  Limit (mag.)
--------------------------------------------------------------
14:01:59 14:02:29  1   ~16.36
14:01:59 17:26:12  20   ~16.99
---------------------------------------------------------------


GRB_name: GRB080229A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7380
SUBJECT: GRB080229, optical upper limit (Correction)
DATE:    08/03/10 08:25:57 GMT
FROM:    Ryuuji Hara at U of Miyazaki  <ryuu55@astro.miyazaki-u.ac.jp>

R.Hara notes:

I stated in GCN7337$B!!(Bas
"The observation was started 17:05:03 UT, ~225 min
after the Swift trigger time."

but the correct one is
"The observation was started 19:30:40 UT, about 146 min
after the Swift trigger time."

We apologize for any inconvenience this may have caused.


GRB_name: GRB080310A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7381
SUBJECT: GRB 080310 afterglow candidate
DATE:    08/03/10 08:53:18 GMT
FROM:    Ryan Chornock at UC Berkeley  <chornock@astro.berkeley.edu>

R. Chornock, R. J. Foley, W. Li, and A. V. Filippenko report that:

The Katzman Automatic Imaging Telescope at Lick Observatory slewed to the 
position of GRB 080310 and found a new source not present in the DSS:

14:40:13.81  -00:10:30.6

at about magnitude 17.  The new object is detected in V, I, and unfiltered 
images starting at 14:40:20.04 UT.  We suggest it may be the afterglow of GRB 
080310.


GRB_name: GRB080310A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7382
SUBJECT: GRB 080310: Swift detection of a burst with optical afterglow
DATE:    08/03/10 08:58:27 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <jayc@milkyway.gsfc.nasa.gov>

J. R. Cummings (NASA/UMBC), W. H. Baumgartner (GSFC/UMBC),
A. P. Beardmore (U Leicester), S. Campana (INAF-OAB),
P. A. Evans (U Leicester), E. A. Hoversten (PSU),
S. D. Hunsberger (PSU), C. B. Markwardt (CRESST/GSFC/UMD),
P. T. O'Brien (U Leicester), K. L. Page (U Leicester),
D. M. Palmer (LANL), R. L. C. Starling (U Leicester),
G. Tagliaferri (INAF-OAB) and T. N. Ukwatta (GSFC/GWU) report on
behalf of the Swift Team:

At 08:37:58 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 080310 (trigger=305288).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 220.081, -0.166 which is 
   RA(J2000) = 14h 40m 19s
   Dec(J2000) = -00d 09' 55"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a precursor at
T-24 seconds and multiple peaks from T-10 to T+6 seconds. The peak count 
rate was ~2000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 08:39:27.9 UT, 89.2 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 220.0566, -0.1756 which is equivalent to:
   RA(J2000)  = 14h 40m 13.5s
   Dec(J2000) = -00d 10' 32.1"
with an uncertainty of 5.0 arcseconds (radius, 90% containment). This
location is 94 arcseconds from the BAT onboard position, within the BAT
error circle. No event data are yet available to assess possible
redshift constraints using X-ray spectroscopy and the nH-z relation
from Grupe et al. (2007). 

UVOT took a finding chart exposure of nominal 100 seconds with the White
(160-650 nm) filter starting 99 seconds after the BAT trigger. There is a
candidate afterglow in the list of sources generated on-board at
  RA(J2000)  = 14:40:13.80 = 220.0575
  DEC(J2000) = -00:10:29.6  =  -0.1749
with a 1-sigma error radius of about 0.6 arc sec. This position is 4.1 arc sec. 
from the center of the XRT error circle. The estimated magnitude is 18.8 with a
1-sigma error of about 0.5 mag. No correction has been made for the expected
extinction corresponding to E(B-V) of 0.04. 

Burst Advocate for this burst is J. R. Cummings (jayc AT milkyway.gsfc.nasa.gov). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)


GRB_name: GRB080310A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7383
SUBJECT: GRB 080310 afterglow candidate (correction to UT time)
DATE:    08/03/10 09:01:26 GMT
FROM:    Ryan Chornock at UC Berkeley  <chornock@astro.berkeley.edu>

[corrected UT time]

R. Chornock, R. J. Foley, W. Li, and A. V. Filippenko (UC Berkeley) report that:

The Katzman Automatic Imaging Telescope at Lick Observatory slewed to the
position of GRB 080310 and found a new source not present in the DSS:

14:40:13.81  -00:10:30.6

at about magnitude 17.  The new object is detected in V, I, and unfiltered
images starting at 08:40:01 UT.  We suggest it may be the afterglow of GRB
080310.


GRB_name: GRB080310A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7384
SUBJECT: GRB 080310:  Magellan redshift
DATE:    08/03/10 09:16:48 GMT
FROM:    Edo Berger at Princton U  <eberger@astro.princeton.edu>

E. Berger (Carnegie/Princeton) and M. Rauch (Carnegie) report:

"We obtained a spectrum of the optical afterglow of GRB 080310 (GCNs 7381, 
7382) using the MagE spectrograph on the Magellan/Clay 6.5-m telescope. 
From preliminary analysis we determine a redshift of about 1.7 based on 
broad Ly-alpha absorption at ~3300A.  Further observations and analysis 
are on-going."


GRB_name: GRB080310A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7385
SUBJECT: GRB 080310: REM observations
DATE:    08/03/10 09:23:53 GMT
FROM:    Stefano Covino at Brera Astronomical Observatory  <stefano.covino@brera.inaf.it>

S. Covino, P. D'Avanzo, D. Fugazza, L.A. Antonelli, L.  Calzoletti,  
S. Campana, G.  Chincarini, M.L. Conciatore, S. Cutini, V. D'Elia, F.
D'Alessio, F.  Fiore, P. Goldoni, D. Guetta,  C. Guidorzi, G.L.  
Israel, E. Maiorano, N. Masetti, A. Melandri, E. Meurs, L. Nicastro,  
E. Palazzi,
E. Pian, S. Piranomonte, L.  Stella, G.  Stratta, G. Tagliaferri, G.  
Tosti, V.Testa, S.D. Vergani,  F. Vitali report on behalf of the REM  
team:

The robotic 60-cm REM telescope located at La Silla (Chile) observed  
automatically the field of the GRB 080310  on March 10 08:40:27 UT
(about 150 seconds after the burst).

We detect the afterglow reported in GCN 7381 and 8383 (Chornock et  
al.) and GCN 7382 (Cummings et al.).

The object has H~14.5 at about 5 min from the burst time.

Further analyses and observations are in progress.


GRB_name: GRB080310A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7386
SUBJECT: GRB 080310, SMARTS optical/IR afterglow observations
DATE:    08/03/10 09:48:46 GMT
FROM:    Bethany Cobb at Yale U  <cobb@astro.yale.edu>

B. E. Cobb, part of the larger SMARTS consortium, reports:

Using the ANDICAM instrument on the 1.3m telescope at CTIO, we
obtained optical/IR imaging of the error region of GRB 080310
(GCN 7382, Cummings et al.) beginning 20 minutes post-burst
(2008-03-10 08:58 UT).  Total summed exposure times amounted
to 180s in BRIYJK and 120s in H and V.

The afterglow of GRB 080310 (GCN 7382, Cummings et al. & GCN 7383,
Chornock et al.) is detected in our images.  Preliminary comparison to
USNO-B1.0 stars in I and 2MASS stars in J indicates the following
afterglow magnitudes:

time post-burst         I mag           J mag
~25 minutes             16.3+/-0.2      15.9+/-0.2

The afterglow fades by ~0.4 magnitudes in I between 25 and 45 minutes
post-burst.  This source is therefore confirmed to
be the afterglow of GRB 080310, with a decay rate of alpha ~ -0.6.


GRB_name: GRB080310A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7387
SUBJECT: GRB080310: Super-LOTIS suggestion of brightening
DATE:    08/03/10 10:09:06 GMT
FROM:    Peter A. Milne at Super-LOTIS  <pmilne@as.arizona.edu>

P.A. Milne and G.G. Williams (U Arizona) report on behalf of the
Super-LOTIS team:

The 0.6m Super-LOTIS telescope began R-band observations of the error
region of GRB080310 (Swift trigger 305288) at 08:38:43 UT, 44 seconds
after the start of the burst.  The OT detected by Chornock et al.
(GCN 7381) and confirmed by Cummings et al. (GCN 7382) is not
apparent in the initial images, but is clearly visible in
subsequent images. A stack of the initial 3x10s exposures does not
detect the GRB, while subsequent single 20sec exposures do, suggesting
that the GRB brightened during the first two minutes.

We used the USNO-B star at RA=14:40:11.3, Dec==00:10:40.6 (0898-0239265) to
derive the R magnitude.

The R-band magnitude of the afterglow in the first image is:
UT Start   UT End ExpTime  R mag  error
Single
08:40:29  08:41:09 1x20s  17.97 +/- 0.18
08:41:03  08:41:23 1x20s  16.81 +/- 0.08
Stack
08:40:29  08:42:37 5x20s  16.91 +/- 0.04
08:43:24  08:54:27 10x60s 16.98 +/- 0.02

Observations are continuing.  This message can be cited.


GRB_name: GRB080310A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7388
SUBJECT: GRB 080310: Lick/Kast Spectroscopy
DATE:    08/03/10 10:13:12 GMT
FROM:    Jason Prochaska at UCO/Lick Obs  <xavier@ucolick.org>

J.X. Prochaska (UCSC), M. Murphy (Swinburne),
A.L. Malec (Swinburne), K. Miller (Lick)
report on behalf of GRAASP:

"We observed the afterglow of GRB 080310 with the Kast
dual spectrometer for a series of 900s exposures starting
at UT 09:06 under good conditions.  Analysis of the red side
reveals a series of strong absorption features (SiIV, CIV,
AlII 1670) consistent with the redshift z=2.4266.  At
present we consider this to be the redshift of GRB 080310.

Further analysis is in progress."


This GCN may be cited.

----------------------------------------------
Jason X. Prochaska
UCO/Lick Observatory
UC Santa Cruz
Santa Cruz, CA 95064

xavier@ucolick.org
http://www.ucolick.org/~xavier/
831-459-2135 (Direct)
831-459-2991 (UCO/Lick Main)
831-459-5244 (Fax)


GRB_name: GRB080310A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7389
SUBJECT: GRB 080310:  Magellan redshift revision
DATE:    08/03/10 10:15:09 GMT
FROM:    Edo Berger at Princton U  <eberger@astro.princeton.edu>

E. Berger (Carnegie/Princeton) and M. Rauch (Carnegie) report:

"The redshift of 1.7 previously quoted in GCN 7384 was due to 
mis-identification of the line.  Based on the detection of Ly-alpha, SII, 
CIV, SiIV, etc.  the correct redshift is z=2.42."


GRB_name: GRB080310A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7390
SUBJECT: GRB080310, optical observations with LBT
DATE:    08/03/10 10:18:39 GMT
FROM:    Peter Garnavich at U of Notre Dame  <pgarnavi@nd.edu>

P. Garnavich (Notre Dame), J. L. Prieto, R. Pogge (OSU) report:

We observed the position of GRB 080310 (Chornock et al. GCN 7381;
Cummings et al., GCN 7382) with the Large Binocular Telescope and
LBC red and blue cameras starting at 9:04 (UT) (0.44 hours
after the burst) and ending 1 hour after the burst. Observations
were obtained approximately every minute. The initial pair of
observations showed no significant decay, but then declined
rapidly into a power-law with a decay index of 0.65
(see Cobb et al., GCN 7386).

This message may be cited.


GRB_name: GRB080310A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7391
SUBJECT: GRB 080310: VLT/UVES spectroscopy
DATE:    08/03/10 10:47:31 GMT
FROM:    Paul Vreeswijk at Dark Cosmology Centre,U.of Copenhagen  <pmv@dark-cosmology.dk>

P.M. Vreeswijk (DARK), P. Jakobsson (U. Hertfordshire), A.O. Jaunsen
(U. Oslo) and C. Ledoux (ESO) report on behalf of a larger
collaboration:

We observed the optical afterglow (Chornock et al., GCN 7381) of GRB
080310 (Cummings et al., GCN 7382) with the Ultraviolet and Visual
Echelle Spectrograph (UVES) mounted at ESO's VLT Kueyen. Observations
were triggered automatically in rapid-response mode starting on 2008
March 10 at 08:51 UT (13 min after the Swift trigger). We secured two
epochs over the full UVES wavelength range before morning twilight.

Most absorption lines can be explained by three systems at redshifts
z=2.43, z=2.28, and z=1.67, confirming the probable redshift of
GRB080310 first reported by Prochaska et al. (GCN 7388).

We acknowledge excellent support from the observing staff at Paranal,
in particular Dominique Naef and Claudio Melo.


GRB_name: GRB080310A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7392
SUBJECT: GRB080310, detection of break in optical
DATE:    08/03/10 11:05:03 GMT
FROM:    Peter Garnavich at U of Notre Dame  <pgarnavi@nd.edu>

J. L. Prieto (OSU), P. Garnavich (Notre Dame), R. Pogge (OSU) report:

We continue to observe the afterglow of GRB 080310 (Garnavich et al.,
GCN 7390) with the LBT and LBC blue/red cameras. Data taken
between 1.7 and 2.1 hours after the burst show a steepening
decay rate. The power-law decay index over this period
was 1.01 suggesting a break in the light curve is underway.

This message may be cited.


GRB_name: GRB080310A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7393
SUBJECT: GRB 080310: RRM optical photometry with the VLT
DATE:    08/03/10 11:28:50 GMT
FROM:    Stefano Covino at Brera Astronomical Observatory  <stefano.covino@brera.inaf.it>

S. Covino, G. Tagliaferri, D. Fugazza, G. Chincarini, on behalf of  
the MISTICI collaboration report:

We observed the field of GRB 080310 (GCN 7382, Cummings et al.) with  
the VLT equipped with FORS2 with the Rapid Response Mode starting  
from 2008-03-20 at 08:42:59 UT  (about 5 minutes from the burst) for  
almost one hour of continuous observations. The optical afterglow  
(GCN 7381, Chornock et al.) is well detected and it was brighter than  
R~17 (compared to USNO stars) already in the first frame.

A complete analysis is in progress.

[GCN OPS NOTE(10mar08): Per author's request, the "VBLT" in the 
Subject-line was changed to "VLT".]


GRB_name: GRB080310A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7394
SUBJECT: GRB 080310: Enhanced Swift-XRT position
DATE:    08/03/10 11:40:54 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

J.P. Osborne, A.P. Beardmore, P.A. Evans and M.R. Goad (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 99 s of overlapping XRT Photon Counting mode and UVOT
data for GRB 080310, 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 = 220.05801, -0.17496 which is equivalent
to:

RA (J2000): 14h 40m 13.92s
Dec (J2000): -00d 10' 29.9"

with an uncertainty of 1.8 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
http://www.swift.ac.uk/xrt_positions/Goad.pdf).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB080310A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7395
SUBJECT: GRB080310 : Lulin optical observation
DATE:    08/03/10 16:29:02 GMT
FROM:    Yuji Urata at Saitama U  <urata@asiaa.sinica.edu.tw>

T.W. Chen, L.C. Huang, K.Y. Huang and Y. Urata 
on behalf of EAFON report:

"We have been monitoring the optical afterglow of GRB080310 
(GCN #7381, 7382) using Lulin 1m telescope. The brightness 
in R-band at 15:40 (~7hrs after the burst) is ~20 mag. 
Continuous optical monitoring is encouraged."

Further observation and analysis are in progress."


GRB_name: GRB080310A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7396
SUBJECT: GRB 080310 - SDSS Pre-Burst Observations
DATE:    08/03/10 16:55:44 GMT
FROM:    Richard J. Cool at U.of AZ/Steward Obs  <rcool@as.arizona.edu>

Richard J. Cool (Arizona), Daniel J. Eisenstein (Arizona),
David W. Hogg (NYU), Michael R. Blanton (NYU), David J. Schlegel
(LBNL), J. Brinkmann (APO), Donald Q. Lamb (Chicago), Donald
P. Schneider (PSU), and Daniel E. Vanden Berk (PSU) report:

The Sloan Digital Sky Survey (SDSS) imaged the field of burst
GRB080310 prior to the burst.  As these data should be useful
as a pre-burst comparison and for calibrating photometry,
we are supplying the images and photometry measurements for
this GRB field to the community.

Data from the SDSS, including 5 FITS images, 3 JPGS, and
3 files of photometry and astrometry, are being placed at
http://mizar.as.arizona.edu/~grb/public/GRB080310

We supply FITS images in each of the 5 SDSS bands of a 8'x8'
region centered on the GRB position (ra=220.081 (14:40:19.4),
dec=-0.166000 (-00:09:57.6); Swift-BAT TRIGGER 305288), as well
as 3 gri color-composite JPGs (with different stretches). The
units in the FITS images are nanomaggies per pixel.  A pixel
is 0.396 arcsec on a side. A nanomaggie is a flux-density unit
equal to 10^-9 of a magnitude 0 source or, to the extent that
SDSS is an AB system, 3.631e-6 Jy.  The FITS images have WCS
astrometric information.

In the file GRB080310_sdss.calstar.dat, we report photometry
and astrometry of 486 bright stars (r<20.5) within 15' of the
burst location.  The magnitudes presented in this file are asinh
magnitudes as are standard in the SDSS (Lupton 1999, AJ, 118,
1406). Beware that some of these stars are not well-detected
in the u-band; use the errors and object flags to monitor
data quality.

In the files GRB080310_sdss.objects_flux.dat and
GRB080310_sdss.objects_magnitudes.dat, we report photometry
of 818 objects detected within 6' of the GRB position.
We have removed saturated objects and objects with model
magnitudes fainter than 23.0 in the r-band.  The fluxes listed
in GRB080310_sdss.objects_flux.dat are in nanomaggies while
the magnitudes listed in GRB080310_sdss.objects_magnitudes.dat
are asinh magnitudes.

All quantities reported are standard SDSS photometry, meaning
that they are very close to AB zeropoints and magnitudes are
quoted in asinh magnitudes.  Photometric zeropoints are known
to about 2% rms.  None of the photometry is corrected for
dust extinction.  The Schlegel, Finkbeiner, and Davis (1998)
predictions for this region are A_U=0.202 mag, A_g=0.149 mag,
A_r = 0.108 mag, A_i=0.082 mag, and A_z=0.058 mag.

The file GRB080310_sdss.spectro.dat contains a list of the
3 objects with SDSS spectroscopy within 6 arcminutes of the
GRB position.  In addition to the redshift and 1-sigma error
for each object, this file also lists the object spectroscopic
classification.


SDSS astrometry is generally better than 0.1 arcsecond per
coordinate.  Users requiring high precision astrometry should
take note that the SDSS astrometric system can differ from
other systems such as those used in other notices; we have
not checked the offsets in this region.

More detailed information pertaining to our SDSS GRB releases
can be found in our initial data release paper (Cool et
al. 2006, PASP 118, 733).  See the SDSS DR4 documentation for
more details: http://www.sdss.org/dr5.

These data have been reduced using a slightly different
pipeline than that used for SDSS public data releases.
We cannot guarantee that the values here will exactly match
those in the data release in which these data are included.
In particular, we expect the photometric calibrations to differ
by of order 0.01 mag.

This note may be cited, but please also cite the SDSS data
release paper, Adelman-McCarthy et al. (2007, ApJS, 172, 634),
when using the data or referring to the technical documentation.


GRB_name: GRB080310A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7397
SUBJECT: GRB 080310: Redshift from Keck/DEIMOS Spectra
DATE:    08/03/10 17:20:17 GMT
FROM:    Jason Prochaska at UCO/Lick Obs  <xavier@ucolick.org>

J.X. Prochaska (UCSC), R.J. Foley (UCB), B. Holden (UCCS),
D. Magee (UCSC),  M. Cooper (Arizona) and A. Dutton (UCSC)
report on behalf of GRAASP:

"We observed the afterglow of GRB 080310 (Chornock, #7381)
with the Keck/DEIMOS spectrometer for a series of 900s exposures
starting ~2hr after the burst under good conditions.  Analysis of the
data confirms the three absorption systems reported by
Prochaska et al. (#7388) and Vreeswijk et al. (#7391).
We identify modest strength FeII and MgII resonance lines associated
with the absorber at z=2.4266 and also weaker FeII* absorption.  The  
latter observation
establishes this gas as the ISM surrounding GRB 080310.

Further analysis is in progress."


This GCN may be cited.


GRB_name: GRB080310A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7398
SUBJECT: GRB 080310: Swift/UVOT Refined Analysis
DATE:    08/03/10 18:15:23 GMT
FROM:    Erik Hoversten at Swift/Penn State  <hoversten@astro.psu.edu>

E. A. Hoversten (PSU) and J. R. Cummings (NASA/UMBC) report on behalf  
of the Swift UVOT team:

    The Swift/UVOT observed the field of GRB 080310 (trigger 305288)  
starting 99 seconds after the BAT trigger (Cummings, et al., GCN  
Circ. 7382) starting with a 100s finding chart exposure in the white  
filter.  A bright afterglow was clearly detected in the initial white  
and V band exposures.

Further analysis shows that a fading source is detected at the XRT  
position in the U, B, V, and white filter images.  The source is  
still detectable in these filters around 7000 seconds after the  
burst.  The white and U band images show a brightening of the source  
reaching a peak after 1 ks after the burst before fading smoothly.   
The B and V images show a more smooth decay.

The afterglow is not detected in the UVW1 and UVM2 filters and is  
weakly detected in the UVW1 filter.  This is consistent with the  
measured redshift of 2.42 (Prochaska, et al., GCN Circ. 7388).

The detections and 3-sigma upper limits in the UVOT photometric  
system (Poole, et al. 2008, MNRAS 383, 627) are given in the  
following table.  The white and optical magnitudes are individual  
exposures while the UV magnitudes are from co-added images.

Filter T_start(s) T_stop(s) Exposure(s)  Mag

white     99        197       98         18.50 +/- 0.06
white    868        967       98         17.95 +/- 0.05
white   6788       6985      197         18.99 +/- 0.07

v        208        602      393         17.38 +/- 0.05
v       7199       7334      135         18.5  +/- 0.3

b        685        695       10         17.7  +/- 0.2
b       6584       6780      197         18.9  +/- 0.1

u        660        680       19         17.8  +/- 0.2
u       1430       1450       19         17.3  +/- 0.2
u       6379       6575      197         18.3  +/- 0.1

uvw1     638       6373      452         20.3 +/- 0.3
uvm2     613       6168      197        >19.8
uvw2     716       7194      432        >20.8


No correction has been made for the expected Galactic extinction of E 
(B-V) of 0.04 mag in the direction of the burst (Schlegel, et al. 1998).


GRB_name: GRB080310A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7399
SUBJECT: GRB 080310: Swift-XRT refined analysis
DATE:    08/03/10 18:49:54 GMT
FROM:    Andy Beardmore at U Leicester  <apb@star.le.ac.uk>

A.P. Beardmore, J.P. Osborne, R.L.C. Starling, K.L. Page, P.A. Evans 
(U. Leicester) and J.R. Cummings (NASA/UMBC) report on behalf of 
the Swift-XRT team:

The Swift-XRT started observing GRB 080310 (trigger no. 305288,
Cummings et al. GCN 7382) at 2008-03-10 08:39:27.85 UT, 89s after the
trigger. The observation so far spans 3 snapshots, with Windowed Timing
mode data from T+95s to T+799s, and Photon Counting mode thereafter.

The best XRT position is the UVOT-enhanced position from Osborne et al.
(GCN 7394).

At first, the 0.3-10keV X-ray light curve decays from 39 count s^-1 at
T+95s to 18 count s^-1 at T+130s but then shows strong flaring
activity. An initial rebrightening occurs from about T+135s to T+420s,
reaching ~135 count s^-1 at approximate times of 200s, 250s, 280s and
350s after the trigger.  This is followed by a second flare from T+500
to T+620s, where it reaches a maximum of ~115 count s^-1 at T+565s.
Following the flaring activity, the X-ray light curve, thus far, shows
a slow decline out to the end of the third snapshot (T+1.0ks to
T+18.7ks), where it reaches a count rate of 0.1 count s^-1 with an
underlying decay slope of alpha~0.5.

The X-ray data also show strong spectral evolution during the flaring
intervals.  A 1.5-10keV/0.3-1.5keV hardness ratio reveals the X-ray
emission initially hardens from T+135s to T+200s as the light curve
rebrightens, at which point it remains approximately constant until
T+360s, before softening as the light curve decays.  Similarly, the
source hardens again during the second flare from T+500s to T+565s,
then softens as this flare declines.

A spectrum of the WT data from T+200s to T+360s, where the hardness
ratio is approximately constant, can be well fit by an absorbed
powerlaw with photon index 1.45 +/- 0.02 and column density of (7.0
+/- 1.0)e21 cm^-2 at the redshift of the burst (z=2.43, Prochaska et
al. GCN 7388; Berger and Rauch GCN 7389; Vreeswijk et al. GCN 7391),
in addition to the Galactic column density of 3.3e20 cm^2 in this
direction. The observed 0.3-10keV flux is (6.1 +/- 0.1)e-9 erg cm^-2 s^-1,
which corresponds to an unabsorbed flux of 6.8e-9 erg cm^-2 s^-1. 
The counts to observed flux conversion factor at the time of
this spectrum is 4.9e-11 erg cm^-2 count^-1.

The PC mode data from the second snapshot (T+5.1ks to T+7.3ks) show a 
softer spectrum, with a photon index of 1.9 +/- 0.2 and column density 
consistent with the value determined above. The observed 0.3-10keV flux at 
this time is (1.1 +/- 0.1) e-11 erg cm^-2 s^-1, and corresponds to a flux 
conversion factor of 4.7e-11 erg cm^-2 count^-1.

If the underlying powerlaw decay continues as is, we predict an XRT count 
rate of 0.05 count s^-1 at T+24hr, which corresponds to an observed 
0.3-10keV flux of 2.5e-12 erg cm^-2 s^-1.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB080307A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7400
SUBJECT: GRB080307: optical upper limit
DATE:    08/03/10 19:17:24 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

G. Kornienko, A. Erofeeva (UAFO), A. Pozanenko (IKI) on behalf of larger GRB 
follow up collaboration report:

We observed the error box of  GRB080307 (Holland  et al. GCN 7362) on March 
05 with SR-22 telescope of UAFO observatory. A set of 20 unfiltered images 
of 60 s exposure was obtained starting (UT) 11:36:55, i.e. 13.5 minutes 
after burst onset. No new object is detected within enhanced XRT error 
circle (Goad et al. GCN 7366). Based on USNO-A2.0 (R) we estimated upper 
limit as following

T0+           Exposure     UL
(mid)
23.5 m        10x60 s      18.8

The message may be cited. 


GRB_name: GRB080210A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7401
SUBJECT: GRB080210: optical observations
DATE:    08/03/10 19:25:26 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

E. Klunko (ISTP), A. Pozanenko (IKI) on behalf of larger GRB follow up 
collaboration  report:

We observed afterglow (Klotz et al. GCN 7280) of GRB080210  (Grupe et al. 
GCN 7281)  with 1.5m telescope of Sayan observatory (Mondy) on Feb.10 
between (UT) 21:36:37 - 22:49:36. The afterglow is marginally detected 
(SNR=1.8) in coordinates R.A.(J2000) = 16 45 03.98 Dec.(J2000) = +13 49 
35.8. A photometry against USNO-B1.0 is following:

T0+       Exposure  R_mag
(mid)

0.594 d  47x60 s   21.8

The afterglow at 0.594d appears ~1 magnitude brighter than expected from  a 
slow decay rate of alpha ~0.85 (Perley et al. GCN 7298).

The message may be cited. 


GRB_name: GRB080310A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7402
SUBJECT: GRB 080310, Swift-BAT refined analysis
DATE:    08/03/10 21:21:53 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <jayc@milkyway.gsfc.nasa.gov>

J. Tueller (GSFC),
S. D. Barthelmy (GSFC),
J. Cummings (GSFC/UMBC),
E. Fenimore (LANL),
N. Gehrels (GSFC),
H. Krimm (GSFC/USRA),
C. Markwardt (GSFC/UMD),
K. McLean (GSFC/UMD),
D. Palmer (LANL),
A. Parsons (GSFC),
T. Sakamoto (GSFC/UMBC),
G. Sato (GSFC/ISAS),
M. Stamatikos (GSFC/ORAU),
T. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+963 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 080310 (trigger #305288)
(Cummings, et al., GCN Circ. 7382).  The BAT ground-calculated position is
RA, Dec = 220.040, -0.164 deg which is
   RA(J2000)  = 14h 40m 9.6s
   Dec(J2000) = -0d 9' 49"
with an uncertainty of 1.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 68%.
 
The mask-weighted lightcurve shows many peaks starting at ~T-60 sec.  The
main peak extends from ~T-12 to T+7 sec, then there is a period with no
detectable emission, then a broad, weaker peak from T+180 to T+360 sec.
The later peak corresponds to the first strong flare seen in the XRT (Beardmore
et al., GCN circ. 7399).  BAT sees no emission at the time of the second flare
seen in the XRT, even though in the XRT energy range it was of similar intensity
at the peak to the first flare.

The location of the burst entered the BAT field of view at about T-80 sec during
a preplanned slew.  It is possible that some very weak emission preceded that
time, but the BAT raw lightcurve, which is partially sensitive to photons from
outside the FOV rules out strong emission. T90 (15-350 keV) is 365 +- 20 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-71.8 to T+318.7 sec is best fit by a simple
power-law model.  The burst does not appear to have significant emission above
about 150 keV however.  The power law index of the time-averaged spectrum is
2.32 +- 0.16.  The fluence in the 15-150 keV band is 2.3 +- 0.2 x 10^-06 erg/cm2.
The 1-sec peak photon flux measured from T+1.27 sec in the 15-150 keV band
is 1.3 +- 0.2 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/305288/BA/

[GCN OPS NOTE(10mar08): Per author's request, the missing minus sign
on the Dec specification was added (-0d 9' 49").]


GRB_name: GRB080310A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7403
SUBJECT: GRB 080310: early RAPTOR multicolor observations
DATE:    08/03/10 22:05:02 GMT
FROM:    Przemyslaw R. Wozniak at LANL  <wozniak@lanl.gov>

P. Wozniak, W.T. Vestrand, J. Wren, and H. Davis
(Los Alamos National Laboratory)

Our RAPTOR-S and RAPTOR-T telescopes began simultaneous multicolor
(clear, V, R, I) imaging of GRB 080310 at UT 08:38:27.14, 28.5 seconds
after the trigger, 6.7 seconds after receiving the trigger.

The counterpart identified by Chornok et al. (GCN 7381) brightened
from below 17 mag to about 16.8 mag at ~200 seconds (clear band
calibrated to USNO B1.0 R2 magnitudes) and dimmed to about 17.3 mag at
400 seconds. We clearly detect the OT simultaneously in all filters
and follow its flux evolution for 1.5 hours.
We observe a broad plateau between 400 and 1100 seconds
with slight rebrightening towards the end of this time interval,
folowed by rapid decay.


GRB_name: GRB080229A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7404
SUBJECT: GRB 080229: NIR upper limit
DATE:    08/03/11 03:23:10 GMT
FROM:    Takeo Minezaki at U.of Tokyo/Astro  <minezaki@mtk.ioa.s.u-tokyo.ac.jp>

T. Minezaki (IoA, Tokyo), P.A. Price (IfA, Hawaii), Y. Yoshii (IoA,
Tokyo), L. Cowie (IfA, Hawaii) and Y. Kakazu (IfA, Hawaii) report:

We observed the localisation of GRB 080229 with the MAGNUM telescope +
MIP dual-beam imager. We do not find any afterglow in the RIYJHK images
within the XRT error circle (GCN #7343). We estimated the upper limits
in JHK based on flux calibration with a nearby 2MASS star as follows:

  Filter   t - t_GRB (hour)    Limit (mag)
  J        +19.8               20.5
  H        +20.7               20.0
  K        +20.4               19.4

This message may be cited.


GRB_name: GRB080307A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7405
SUBJECT: GRB 080307: NIR upper limit
DATE:    08/03/11 03:24:43 GMT
FROM:    Takeo Minezaki at U.of Tokyo/Astro  <minezaki@mtk.ioa.s.u-tokyo.ac.jp>

T. Minezaki (IoA, Tokyo), P.A. Price (IfA, Hawaii), Y. Yoshii (IoA,
Tokyo), L. Cowie (IfA, Hawaii) and Y. Kakazu (IfA, Hawaii) report:

We observed the localisation of GRB 080307 with the MAGNUM telescope +
MIP dual-beam imager. We do not find any afterglow in the RIYJHK images
within the XRT error circle (GCN #7366), and at the Gemini-N i-band
candidate position (GCN #7369). We estimated the upper limits in JHK
based on flux calibration with a nearby 2MASS star as follows:

  Filter   t - t_GRB (hour)    Limit (mag)
  J        +18.9               20.8
  H        +19.8               20.1
  K        +19.5               19.2

This message may be cited.


GRB_name: GRB080310A
Detection_method: KAIT
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7406
SUBJECT: GRB 080310: PAIRITEL detection and PAIRITEL+KAIT+UVOT SED
DATE:    08/03/11 09:20:24 GMT
FROM:    Daniel Perley at U.C. Berkeley  <dperley@astro.berkeley.edu>

D. A. Perley, J. S. Bloom, and W. Li (UC Berkeley) report:

PAIRITEL responded to GRB 080310 and began taking data at UT 2008-03-10 
  09:04:58 in J, H, and K filters simultaneously.  The afterglow 
(Chornock et al., GCN 7381) is well-detected in all three filters.  We 
report the following magnitudes:

t_mid(s)  exp(s)  magnitude
1833      259     J = 15.63 +/- 0.03
1833      259     H = 14.94 +/- 0.03
1833      259     K = 14.29 +/- 0.03

Combining PAIRITEL data with 347 KAIT observations (calibrated to SDSS 
DR6) and the UVOT magnitudes reported by Hoversten et al. (GCN 7398), we 
generate a UV-through-IR spectral energy distribution interpolated to 
the midpoint of the PAIRITEL observations.  The SED is well-fit by an 
intrinsic power-law spectral index of beta ~ 0.6 with a small amount 
(A_V = 0.10 +/- 0.05) of SMC-like host-galaxy extinction:

http://lyra.berkeley.edu/~dperley/080310/080310sed.png

Additional, late-time follow-up is planned.


GRB_name: GRB080229A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7407
SUBJECT: GRB 080229A: GAO 150cm telescope Optical Observation
DATE:    08/03/11 11:18:46 GMT
FROM:    Kenzo Kinugasa at Gunma Astro. Obs/Japan  <kinugasa@astron.pref.gunma.jp>

K. Kinugasa (Gunma Astronomical Observatory)  report:

 The field of GRB 080229A (Cannizzo et al. GCN 7335) was observed
with the 150 cm telescope of the Gunma Astronomical Observatory.
Starting at 18:19 UT (1.25 hours after the burst), Rc, and Ic frames
were acquired for 5 x 3-min exposures  under a poor seeing (~3.5arcsec)
condition.

 The enhaunced XRT position (Beardmore et al. GCN 7343) is close to 
a bright star, so the field are strongly contaminated  with the light 
from this star. We do not identify the optical counterpart reported
by Yoshida et al. (GCN 7341) to 3-sigma limiting magnitudes of Rc=19.3
and Ic=18.7 relative to USNO-B1.0 magnitudes.


GRB_name: GRB080307A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7408
SUBJECT: GRB 080307: GAO 150cm telescope Optical Observation
DATE:    08/03/11 11:21:49 GMT
FROM:    Kenzo Kinugasa at Gunma Astro. Obs/Japan  <kinugasa@astron.pref.gunma.jp>

K. Kinugasa, S.Honda, O.Hashimoto, H.Taguchi (Gunma Astronomical
Observatory)  report:

 The field of GRB 080307 (Holland et al. GCN 7362) was observed
with the 150 cm telescope of the Gunma Astronomical Observatory.
Starting at 13:06 UT (1.67 hours after the burst), Rc, Ic, and
V frames were acquired for 3 x 5-min, 6 x 5-min, and 2 x 5-min
exposures, respectively.

 We do not identified the optical counterpart reported by
Tanvir et al. (GCN 7369) to 3-sigma limiting magnitudes of
Rc=21.5 and Ic=21.0 relative to USNO-B1.0 magnitudes.


GRB_name: GRB080310A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7409
SUBJECT: GRB080310, optical observations with the LBT
DATE:    08/03/11 14:23:35 GMT
FROM:    Peter Garnavich at U of Notre Dame  <pgarnavi@nd.edu>

P. Garnavich (Notre Dame), J. L. Prieto, R. Pogge (OSU) report:

We observed the position of GRB 080310 (Chornock et al. GCN 7381;
Cummings et al., GCN 7382) with the Large Binocular Telescope and
LBC red and blue cameras on March 11 starting at 11:30 (UT) or 26.8
hours after the burst. On the red camera the images were taken
through a Sloan-r filter and calibrating with the SDSS catalog
(Cool et al.; GCN 7396) we find the brightness to be r=21.38+/-0.05 mag.

Extrapolating the decay from LBT observations of March 10 (Prieto
et al., GCN 7392) with an index of 1.15, the afterglow is about
0.2 mag brighter than expected. This could be due to host galaxy
light or deviations from a single power-law decay.

The LBT is an international collaboration among institutions in the
United States, Italy and Germany. The LBT Corporation partners are:
*  The University of Arizona on behalf of the Arizona university system
*  Istituto Nazionale di Astrofisica, Italy
*  LBT Beteiligungsgesellschaft, Germany, representing the Max Planck
Society, the Astrophysical Institute Potsdam, and Heidelberg University
*  The Ohio State University
*  The Research Corporation, on behalf of The University of Notre Dame,
University of Minnesota and University of Virginia

This message may be cited.


GRB_name: GRB080310A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7410
SUBJECT: GRB080310: Optical observation by MITSuME telescope
DATE:    08/03/11 15:55:27 GMT
FROM:    Michitoshi Yoshida at Okayama Astrophysical Obs  <yoshida@oao.nao.ac.jp>

M. Yoshida, K. Yanagisawa, Y. Shimizu, S. Nagayama, H. Toda (OAO,
NAOJ) and N. Kawai (Tokyo Tech) report on behalf of the MITSuME
collaboration:

We detected the optical afterglow of GRB 080310 (Cummings, et al.,
GCN 7382) in the error circle of the XRT position (Osborne et al.
GCN 7394) with the 50cm MITSuME Telescope at Okayama Astrophysical
Observatory on March 10 UT. Photometric calibration was done using
USNO-B1.0 catalog. The light curve shows a plateau at around 19:00 -
20:00 UT (about 11 hours after the trigger).
The photometric results are summarized below.

Observation date: 2008-03-10 UT

mid-UT     exp-T         g'            Rc            Ic
------------------------------------------------------------
15:09:46   60min     20.0+-0.2     19.7+-0.3     19.1+-0.2
16:24:47   60min     20.4+-0.2     20.2+-0.2     19.5+-0.2
17:39:46   60min     20.6+-0.1     20.4+-0.2     19.8+-0.2
18:54:44   60min     20.6+-0.2     20.5+-0.1     20.2+-0.3
19:57:05   42min     20.6+-0.2     20.3+-0.1     20.0+-0.2
------------------------------------------------------------


GRB_name: GRB080310A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7411
SUBJECT: GRB 080310: ROTSE-III Observations of Optical Counterpart 
DATE:    08/03/12 03:32:31 GMT
FROM:    Fang Yuan at ROTSE  <yuanfang@umich.edu>

F. Yuan (U Mich), R. Quimby (Caltech), H. Swan (U Mich), C. Akerlof (U 
Mich), report on behalf of the ROTSE collaboration:

ROTSE-IIIb, located at McDonald Observatory, Texas, responded to GRB 
080310 (Swift trigger 305288; Cummings et al., GCN 7382) and began 
imaging at UT 08:38:25.7 (5.7 sec after the GCN notice time) under 
cloudy conditions. The first usable image with a detection of the OT 
(Chornock et al. GCN 7381) starts at UT 09:03:03.4. Observations 
continued in fluctuating weather conditions until about 3 hours after 
the trigger.
 
The OT is slightly blended with the two nearby stars in ROTSE images. To 
reduce the contamination, we tried two different methods to obtain the 
OT magnitudes, first by subtracting the scaled PSF of the two nearby 
stars, and, second, by subtracting a reference image constructed from 
images taken on Mar. 11  between UT 05:26:28.5 and 06:00:53.6 (when the 
OT has dropped below our detection threshold). The two methods yield 
similar results. From 0.42 to 1.72 hour after the burst, the OT is 
observed to decay with a power-law index 0.6+/-0.1, consistent with the 
observation by the LBT (Garnavich et al., GCN 7390). The later images 
have degraded seeing and don't constrain the time dependence of the OT 
very well. The magnitudes reported below are unfiltered calibrated to 
SDSS r using standard stars in the pre-burst SDSS observations (Cool et 
al., GCN 7396).

Start_UT     End_UT      mag    magerror    mlim(of image)
---------------------------------------------------------------
09:03:03.4  09:07:31.2   17.2    0.1         18.4
09:56:17.5  10:09:49.8   18.0    0.1         19.4


GRB_name: GRB080310A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7412
SUBJECT: GRB080310 : Optical observations by LOAO and Lulin
DATE:    08/03/12 09:45:58 GMT
FROM:    Yuji Urata at Saitama U  <urata@asiaa.sinica.edu.tw>

Y. Urata, M. Im. I. Lee, K.Y. Huang, T.W. Chen, L.C. Huang
on behalf of EAFON report:

"We have monitored the optical afterglow of GRB080310 (Cummings et al
GCN 7382) on the night of March 10th using the Mt. Lemmon 1m and the
Lulin 1m telescopes. These time coverage are 09:26 -- 12:54 UT
(Mt. Lemmon) and 15:52--21:16 UT (Lulin), respectively. All of images
taken with 300 sec exposure in V and R band show the afterglow clearly.

Based on our preliminary results calibrated using USNO-B1.0 catalog,
we confirmed the decaying light curve with a power-law index 0.7+/0.1
between 0.8 and 2.1 hours after the burst. This result is consistent
with the observations by the LBT (Garnavich et al., GCN 7390) and the
ROTSE-III (Yuan et al., GCN 7411).  The light curve between 7.3 and
12.2 hrs after the burst is well described by single power-law with
index 0.8+/-0.1 in R-band. The extrapolation of this power-law is also
consistent with the observation by the LBT (Garnavich et al. 7409).
We could not confirm the plateau phase reported by the MITSuME (Yoshida
et al., GCN 7410)."

This message may be cited.


GRB_name: GRB080310A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7413
SUBJECT: GRB 080310: GAO 150cm telescope Optical Observation
DATE:    08/03/12 14:09:55 GMT
FROM:    Kenzo Kinugasa at Gunma Astro. Obs/Japan  <kinugasa@astron.pref.gunma.jp>

K. Kinugasa (Gunma Astronomical Observatory)  report:

 The position of GRB 080310 (Chornock et al. GCN 7381;
Cummings et al., GCN 7382)  was observed with the 150 cm
telescope of Gunma Astronomical Observatory.
Starting at 15:09 and 18:01 UT (6.5 and 9.4 hours after
the burst), Rc and Ic frames were acquired for sets of
5 x 3-min and  5 x 3-min exposures.

 We clearly detected the optical counterpart in all frames.
We estimated the R magnitute below and confirmed the fading
trend. The decay index of single power-law is consistent
with the result reported by Urata et al. (GCN 7412).


mid-UT     exp           Rc
-----------------------------------
15:18:50   5 x 3-min     20.1+-0.1
18:09:42   5 x 3-min     20.5+-0.1
-----------------------------------


GRB_name: GRB080310A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7414
SUBJECT: GRB080310, unusual slow decay in the optical
DATE:    08/03/12 14:17:59 GMT
FROM:    Peter Garnavich at U of Notre Dame  <pgarnavi@nd.edu>

P. Garnavich (Notre Dame), J. L. Prieto, R. Pogge (OSU) report:

Beginning March 12.48 (UT), we again observed the position of
GRB 080310 (Chornock et al. GCN 7381; Cummings et al., GCN 7382)
with the Large Binocular Telescope and LBC red and blue cameras.
The seeing was 0.7 arcsec in the r-Sloan filter.

The brightness of the afterglow 2.12 days after the burst is measured
to be r=21.67+/-0.05 mag, or only 0.3 mag fainter than the previous
night. This corresponds to a power-law decay index of only 0.42
and confirms the slowing in the decay rate noted in GCN 7409.

It is unlikely that the slow fade is due to contamination from
a host galaxy or a galaxy along the line of sight. To explain the
observed decay rate, a galaxy would have to contribute at a
magnitude near r=22.5, but nothing at this brightness is detected
in the SDSS at the position of the afterglow. Also, the afterglow is
consistent with a point source in the LBT images obtained in good seeing.

We conclude that the shallow decay rate is intrinsic to the afterglow
and this suggests either a continuing energy input or that the shock has
encountered a change in density of the ambient medium. (We must note
another possibility: the afterglow is being gravitationally
microlensed.)

The LBT is an international collaboration among institutions in the
United States, Italy and Germany. The LBT Corporation partners are:
*  The University of Arizona on behalf of the Arizona university system
*  Istituto Nazionale di Astrofisica, Italy
*  LBT Beteiligungsgesellschaft, Germany, representing the Max Planck
Society, the Astrophysical Institute Potsdam, and Heidelberg University
*  The Ohio State University
*  The Research Corporation, on behalf of The University of Notre Dame,
University of Minnesota and University of Virginia

This message may be cited.


GRB_name: GRB080310A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7415
SUBJECT: GRB080310 : Lulin Optical observations
DATE:    08/03/12 18:54:46 GMT
FROM:    Yuji Urata at Saitama U  <urata@asiaa.sinica.edu.tw>

Y. Urata, T.W. Chen, K.Y. Huang, L.C. Huang, M. Im, I. Lee
on behalf of EAFON report:

"We have made R-band images for the optical afterglow of GRB 080310
(Chornock et al. GCN 7381; Cummings et al., GCN 7382) using the Lulin
1m telescope. According to USNO-B1.0 calibration, the afterglow at
1.44 days after the burst is R=21.3+/-0.1. This observation confirm
the plateau or bump reported by Garnavich et al., (GCN 7414). The
R-band lightcuve made from our observations (T.W. Chen et al., GCN
7395; Urata et al., GCN 7412) and the LBT points (Garnavich et al.,
GCN 7409, 7414) is resemble to that of GRB030329 (e.g. Lipkin et al
2004)."

This message may be cited.


GRB_name: GRB080315A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7416
SUBJECT: GRB 080315: Swift detection of a possible burst
DATE:    08/03/15 02:46:19 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

K. L. Page (U Leicester), W. H. Baumgartner (GSFC/UMBC),
A. P. Beardmore (U Leicester), D. N. Burrows (PSU),
M. M. Chester (PSU), N. Gehrels (NASA/GSFC),
S. T. Holland (CRESST/USRA/GSFC), J. A. Kennea (PSU),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (CRESST/GSFC/UMD),
F. E. Marshall (NASA/GSFC), D. M. Palmer (LANL),
M. Stamatikos (NASA/ORAU), E. Troja (U Leicester/INAF-IASFPA) and
T. N. Ukwatta (GSFC/GWU) report on behalf of the Swift Team:

At 02:25:01 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 080315 (trigger=306323).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 155.182, +41.729 which is 
   RA(J2000) = 10h 20m 44s
   Dec(J2000) = +41d 43' 44"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  As is usual for a 64-second image trigger,
the TDRSS light curve shows no obvious variation.  Further BAT analysis
will rely on the Malindi-downlinked data. 

The XRT began observing the field at 02:27:07.3 UT, 125.9 seconds after
the BAT trigger. No source was detected in the promptly available XRT
data. We are waiting for the full dataset to detect and localise the
XRT counterpart. 


UVOT took a finding chart exposure of 400 seconds with the V filter starting
125 seconds after the BAT trigger. No afterglow candidate has been found in the
initial data products. The 2.7'x2.7' sub-image covers 25% of the BAT error
circle. The typical 3-sigma upper limit has been about 18.5 mag. The 8'x8'
region for the list of sources generated on-board covers 100% of the BAT error
circle. The list of sources is typically complete to about 18.0 mag. No
correction has been made for the expected extinction of about 0.04 magnitudes. 




Burst Advocate for this burst is K. L. Page (kpa 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.)


GRB_name: GRB080315A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7417
SUBJECT: GRB 080315: TAROT Calern observatory optical observations
DATE:    08/03/15 03:08:37 GMT
FROM:    Alain Klotz at CESR-CNRS  <Alain.Klotz@free.fr>

Klotz, A. (CESR-OMP), Boer M. (OHP), Atteia J.L. (LATT-OMP) report:

We imaged the field of GRB 080315 detected by SWIFT
(trigger 306323) with the TAROT robotic telescope (D=25cm)
located at the Calern observatory, France.

The observations started 85.0s after the GRB trigger
(9.4s after the notice). The elevation of the field decreased from
from 45 degrees above horizon and weather conditions
were excellents.

The date of trigger : t0 = 2008-03-15T02:25:01.3

The first image is trailed with a duration of 60.0s
(see the description in Klotz et al., 2006, A&A 451, L39).
We do not detect any OT with a limiting magnitude of:
t0+85.0s to t0+145.0s : R > 16.8

The second image is 30.0s exposure in tracking mode:
t0+152.1s to t0+182.1s : R > 18.3

We co-added a series of exposures:
t0+152.1s to t0+436.0s : R > 19.7

These images are unfiltered.

Magnitudes were estimated with the nearby USNO-B1 stars
and are not corrected for galactic dust extinction.

N.B. Galactic coordinates are lon=177.6257 lat=+56.0163
and the galactic extinction in R band less than 0.1 magnitude
estimated from D. Schlegel et al. 1998ApJ...500..525S.

This message may be cited.


GRB_name: GRB080315A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7418
SUBJECT: GRB 080315: Optical observations
DATE:    08/03/15 05:28:20 GMT
FROM:    Antonio Deugarte at IAA-CSIC  <deugarte@iaa.es>

A. de Ugarte Postigo (ESO, Chile), Virginie Chantry (U. Liege, Belgium),
A.J. Castro-Tirado, M. Jelinek, J. Gorosabel (IAA-CSIC, Spain),
C. Melo, A. Smette (ESO, Chile) report:

We have observed the field of GRB 080315 (Page et al., GCN 7416) with the
1.3m Mercator telescope at La Palma starting at 02:55 UT (30 min after
the burst).
The observation consisted on a series of 24x60s I-band exposures. The
combined
exposure, with mean time 3:26 UT (61.3 minutes after the burst), does not
show
any new source inside the 3 arcmin BAT error box down to a limiting
magnitude
of I~20.8 (USNO-B1.0 was used as photometric reference) as compared to
SDSS
i-band frame.

This message may be cited.


GRB_name: GRB080315A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7420
SUBJECT: Swift trigger 306323: Swift-BAT/XRT refined analysis
DATE:    08/03/15 21:12:22 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.a.krimm@nasa.gov>

S. D. Barthelmy (GSFC), D. N. Burrows (PSU), J. Cummings (GSFC/UMBC),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC/UMD),
K. L. Page (U Leicester), D. Palmer (LANL)

After analysis of the data from the Swift BAT and XRT instruments, the 
Swift team is unable to conclude whether or not trigger is a real but 
faint burst or a statistical fluctuation.  The source is detected at 7.1 
sigma in the BAT 15-50 keV energy band.  However, no bright source was 
found in the XRT data.

Using the data set from T-239 to T+303 sec from recent telemetry 
downlinks, we report further analysis of trigger 306323 (reported as GRB 
080315, Page, et al., GCN Circ. 7416).

The BAT ground-calculated position is
RA, Dec = 155.124 +41.701 deg which is
    RA(J2000)  =  10h 20m 29.8s
    Dec(J2000) = +41d 42' 3.6"
with an uncertainty of 3.3 arcmin, (radius, sys+stat, 90% containment).
The image significance at this location is 7.1 sigma. The partial coding 
was 98%.

The mask-weighted light curve shows a a single smooth bump starting at 
~T-5 sec and and ending at ~T+65 sec.  It appears only in the 15-50 keV 
band. T90 (15-350 keV) is 65 +- 5 sec (estimated error including 
systematics).

The time-averaged spectrum from T+0.0 to T+64.0 sec is best fit by a 
simple power-law model.  The power law index of the time-averaged 
spectrum is 2.51 +- 0.59.  The fluence in the 15-150 keV band is 1.4 +- 
0.5 x 10-7 erg/cm2. The 1-sec peak photon flux measured from T+0.00 sec 
in the 15-150 keV band is 0.04 +- 0.01 ph/cm2/sec.  All the quoted 
errors are at the 90% confidence level.

In 20 ks of XRT Photon Counting mode data, a weak source is detected 
within the BAT error circle at a count rate of (9.5  3.0) X 10-4 
count/s. The coordinates of this source are RA, Dec (J2000) = 155.0856, 
+41.6847, which is equivalent to
    RA  =  10 20 20.55
    Dec = +41 41 04.8
with an estimated uncertainty of 5 arcsec (90% containment). It is not
possible to determine whether this source is fading because of the 
limited statistics. With the exception of this source, the 3-sigma upper 
limit within the BAT error circle is 5.9 X 10-4 count/s.

It is unusual, but not unprecedented for there to be no XRT detection of 
a Swift source.  Among the BAT triggers of long GRBs with prompt slews, 
XRT sees a source approximately 97% of the time.  Given the XRT 
non-detection and the faintness of the BAT source, we cannot tell 
whether this trigger is a statistical fluctuation or a real burst.

The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/306323/BA/


GRB_name: GRB080315A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7421
SUBJECT: Swift/UVOT observations of GRB 080315
DATE:    08/03/15 21:36:41 GMT
FROM:    Patricia Schady at MSSL/Swift  <ps@mssl.ucl.ac.uk>

P. Schady (MSSL/UCL) and K. L. Page (U Leicester) report on behalf of the 
Swift UVOT team:

The Swift/UVOT observed the field of GRB 080315 starting 125 s after the 
BAT trigger (Page et al., GCN 7416). We do not find any source in any of 
the individual or co-added exposures, either within the BAT error circle 
or at the location of the weak source detected by XRT (Barthelmy et al. 
GCN 7420).

The 5-sigma upper limits for detecting a source at the position of the XRT 
candidate in the co-added images are:

Filter  T_start T_stop Exp      Mag
         (s)     (s)    (s)      (5-sigma upper limit)
-----------------------------------------------------
v       127     42160   6078.4  > 20.79
b       608     40422   5815.6  > 21.84
u       582     7467    620.7   > 20.30
uvw1    558     7281    468.7   > 19.82
uvm2    533     7075    858.7   > 20.00
uvw2    113     41328   5847.3  > 21.63
-----------------------------------------------------

The quoted upper limits have not been corrected for the expected Galactic 
extinction along the line of sight corresponding to a reddening of E(B-V) 
= 0.01 mag. All photometry is on the UVOT light flight system described in 
Poole et al. (2008, MNRAS, 383, 627).


GRB_name: GRB080315A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7422
SUBJECT: GRB080315: Bok Optical Observations
DATE:    08/03/16 05:24:26 GMT
FROM:    Peter A. Milne at Super-LOTIS  <pmilne@as.arizona.edu>

P.A.Milne (Steward Obs) and A. Updike report on behalf of the
Super-LOTIS GRB team:
 
We observed the field of GRB 080315 starting at UT=02:43:58
(~19min since GRB) with the 2.3m Bok telescope at Kitt Peak, AZ.
We obtained 23 x 60-sec and 7 x 120-sec images in the R-band filter.
 
We do not detect emission at the location of the faint XRT source
(Palmer et al., GCN 7416) to a limiting magnitude of R~23.5.
 
We do not detect any sources other than ones apparent in the DSS,
to the limit of the DSS image. We do not detect a fading/rising source
between the initial 10 and final 10 images.
 
This message may be cited.


GRB_name: GRB080310A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7423
SUBJECT: GRB080310, LBT and MDM photometry
DATE:    08/03/17 01:52:38 GMT
FROM:    Peter Garnavich at U of Notre Dame  <pgarnavi@nd.edu>

G. Wegner (Dartmouth), P. Garnavich (Notre Dame), J. L. Prieto,
and K. Z. Stanek (OSU) report:

We observed the position of GRB 080310 (Chornock et al. GCN 7381;
Cummings et al., GCN 7382) with the Large Binocular Telescope
(LBC red and blue cameras) on March 13.40 (UT) and with the
MDM 2.4-m Hiltner telescope (Retrocam) on March 14.39 (UT) through
Sloan-r filters.

Using stars calibrated by the SDSS, we estimate the following
r-band magnitudes:

age (days)  r mag   error   telescope
3.04        22.45    0.05     LBT
4.03        23.10    0.10     MDM

The photometry indicates that the afterglow has resumed a steep
decline. Including LBT photometry from March 12 (Garnavich et al.,
GCN 7414), we estimate a power-law decline index of 2.1 between
2 and 4 days after the burst.

A plot of the light curve is available at:
http://www.nd.edu/~pgarnavi/LBT/grb080310/LBT_lightcurve.jpg

The LBT is an international collaboration among institutions in the
United States, Italy and Germany. The LBT Corporation partners are:
*  The University of Arizona on behalf of the Arizona university system
*  Istituto Nazionale di Astrofisica, Italy
*  LBT Beteiligungsgesellschaft, Germany, representing the Max Planck
Society, the Astrophysical Institute Potsdam, and Heidelberg University
*  The Ohio State University
*  The Research Corporation, on behalf of The University of Notre Dame,
University of Minnesota and University of Virginia

This message may be cited.


GRB_name: GRB080319A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7426
SUBJECT: GRB 080319A: Swift detection of a burst
DATE:    08/03/19 06:18:20 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

C. Pagani (PSU), P. A. Evans (U Leicester), N. Gehrels (NASA/GSFC),
S. T. Holland (CRESST/USRA/GSFC), J. A. Kennea (PSU),
C. B. Markwardt (CRESST/GSFC/UMD), D. M. Palmer (LANL),
J. L. Racusin (PSU) and M. Stamatikos (NASA/ORAU) report on behalf of
the Swift Team:

At 05:45:42 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 080319A (trigger=306754).  The Swift slew to the burst was
delayed because of an earth constraint. The BAT on-board calculated 
location is RA, Dec 206.354, +44.079 which is 
   RA(J2000) = 13h 45m 25s
   Dec(J2000) = +44d 04' 44"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a multiple peaks
with a duration of about 40 sec.  The peak count rate
was ~800 counts/sec (15-350 keV), at ~10 sec after the trigger. 

The XRT began observing the field at 05:54:59.4 UT, 557.4 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source with an enhanced position: RA, Dec 206.33306, 44.08029
which is equivalent to:
   RA(J2000)  = 13h 45m 19.94s
   Dec(J2000) = +44d 04' 49.1"
with an uncertainty of 2.6 arcseconds (radius, 90% containment). This
location is 54 arcseconds from the BAT onboard position, within the BAT
error circle. 

A power-law fit to a spectrum formed from promptly downlinked event
data does not constrain the column density, so we cannot provide limits
on the redshift using spectroscopy and the relation from Grupe et al. 
(2007). A summary of the promptly downlinked data is given at
http://www.swift.ac.uk/sper/306754/. 

UVOT took a finding chart exposure of 100 seconds with the White 
(160-650 nm)  filter starting 562 seconds after the BAT trigger. A 
possible low-significance afterglow candidate has  been found at the
XRT  position in the  initial data products.  The magnitude is white
= 21.7 mag.  No  correction has been made for the expected extinction
 corresponding to E(B-V) of  0.01. 

Burst Advocate for this burst is C. Pagani (pagani AT astro.psu.edu). 
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.)


GRB_name: GRB080319B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7427
SUBJECT: GRB 080319B: Swift detection of an intense burst with a bright optical counterpart
DATE:    08/03/19 06:32:26 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

J. L. Racusin (PSU), N. Gehrels (NASA/GSFC),
S. T. Holland (CRESST/USRA/GSFC), J. A. Kennea (PSU),
C. B. Markwardt (CRESST/GSFC/UMD), C. Pagani (PSU),
D. M. Palmer (LANL) and M. Stamatikos (NASA/ORAU) report on behalf of
the Swift Team:

At 06:12:49 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 080319B (trigger=306757).  Swift slewed immediately to
the burst. The BAT on-board calculated location is 
RA, Dec 217.926, +36.303 which is
   RA(J2000) = 14h 31m 42s
   Dec(J2000) = +36d 18' 10"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed one bright but
complex peak with a duration of about 50 sec, with an extended tail.  
The peak count rate was ~70,000 counts/sec (15-350 keV), at ~20 sec 
after the trigger. 

The XRT began observing the field at 06:13:49.7 UT, 60.5 seconds after
the BAT trigger. XRT found a very bright fading, uncatalogued X-ray 
source located at RA, Dec 217.9196, +36.3041 which is equivalent to:
   RA(J2000)  = 14h 31m 40.7s
   Dec(J2000) = +36d 18' 14.7"
with an uncertainty of 4.7 arcseconds (radius, 90% containment). This
location is 18 arcseconds from the BAT onboard position, within the BAT
error circle. No event data are yet available to assess possible
redshift constraints using X-ray spectroscopy and the nH-z relation
from Grupe et al. (2007). 

UVOT took a finding chart exposure of 400 seconds with the V filter
starting  175 seconds after the BAT trigger. There is a candidate
afterglow in the  rapidly available 2.7'x2.7' sub-image. This
position is consistent with  the XRT error circle, but the source is
so bright that a precise UVOT position  is not possible due to
saturation effects. The estimated magnitude is 11.5 with a  1-sigma
error of about 0.5 mag. No correction has been made for the expected 
extinction of about 0.04 magnitudes. 

Burst Advocate for this burst is J. L. Racusin (racusin AT astro.psu.edu). 
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.)


GRB_name: GRB080319B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7428
SUBJECT: GRB 080319B: UVOT Position
DATE:    08/03/19 06:45:10 GMT
FROM:    Stephen Holland at USRA/NASA/GSFC/SSC  <sholland@milkyway.gsfc.nasa.gov>

S. T. Holland (CRESST/USRA/GSFC) and J. L. Racusin (PSU) reports on  
behalf of the Swift/UVOT team:

     The UVOT position of GRB 080319B (Racusin et al. 2008 GCN Circ.  
7427) is

RA(J2000) =  14:31:40.98
Dec(J2000) = +36:18:08.8

with an estimated uncertainty of 0.5 arcsec (radius, 90% confidence).

Please update my e-mail address in your Address Book to <Stephen.T.Holland@nasa.gov 
 >.

NOMAD: You had mail.
/
\
/


GRB_name: GRB080319A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7429
SUBJECT: GRB080319A: P60 Optical Afterglow Observations
DATE:    08/03/19 06:49:33 GMT
FROM:    S. Bradley Cenko at Caltech  <cenko@srl.caltech.edu>

S. B. Cenko reports on behalf of a larger collaboration:

We have imaged the field of GRB080319A (Pagani et al., GCN 7426) with the
automated Palomar 60-inch telescope beginning approximately 2.5 minutes
after the burst.  Inside the XRT error circle (and consistent with the
UVOT candidate) we find a single faint, fading point source at coordinates
(J2000):

 RA: 13:45:20.01
        Dec: +44:04:48.6

with an estimated uncertainty of ~ 0.3".  Using the USNO-B catalog as a
reference, we measure a magnitude of R ~ 20.25 +/- 0.2 in our initial
R-band image.

Further observations are planned.


GRB_name: GRB080319B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7430
SUBJECT: GRB 080319B: KAIT OA
DATE:    08/03/19 06:56:36 GMT
FROM:    Weidong Li at UC Berkeley KAIT/LOSS  <weidong@astron.berkeley.edu>

W. Li, J. S. Bloom, R. Chornock, R. Foley, D. A. Perley, and A. V. Filippenko,
University of California at Berkeley, on behalf of the KAIT GRB team, report:

KAIT responded to GRB 080319B (Swift trigger 306757) and was taking 
images. There is a bright afterglow at position

RA = 14:31:40.97
DEC = +36:18:07.9
(equinox J2000)

The measured magnitude is R = 15.4 at 06:49:07 UT.

This message can be cited.


GRB_name: GRB080319B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7431
SUBJECT: GRB 080319B: REM observations
DATE:    08/03/19 08:06:39 GMT
FROM:    Stefano Covino at Brera Astronomical Observatory  <stefano.covino@gmail.com>

S. Covino, P. D'Avanzo, D. Fugazza, L.A. Antonelli, L.  Calzoletti,   
S. Campana, G.  Chincarini, M.L. Conciatore, S. Cutini, V. D'Elia, F.
D'Alessio, F.  Fiore, P. Goldoni, D. Guetta,  C. Guidorzi, G.L.   
Israel, E. Maiorano, N. Masetti, A. Melandri, E. Meurs, L. Nicastro,
E. Palazzi, E. Pian, S. Piranomonte, L.  Stella, G.  Stratta, G.  
Tagliaferri, G. Tosti, V.Testa, S.D. Vergani,  F. Vitali report on  
behalf of the REM
team:

The robotic 60-cm REM telescope located at La Silla (Chile) observed  
automatically the field of the GRB 080319B  on March 19 06:13:32 UT  
(about 43 seconds after the burst).

We clearly detect the afterglow reported in GCN 7427, 7428, 7430  
(Racusin et
al.; Holland et al.; Li et al.).

The object was still at H~12.5 at about 22 min from the burst time.

Further analyses and observations are in progress.


GRB_name: GRB080319B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7432
SUBJECT: GRB 080319B: Super-LOTIS Detection of a Bright OT
DATE:    08/03/19 08:09:38 GMT
FROM:    Grant Williams at Steward Observatory  <ggwilli@gmail.com>

P. A. Milne (Steward Observatory) and G. G. Williams (MMTO), on behalf
of the Super-LOTIS Collaboration, report:

The robotic 0.6-m Super-LOTIS telescope began observing the error box
of GRB 080319B (Swift Trigger 306757, Racusin et al. GCN 7427) at
06:27:00.3 UT, 851 seconds after the trigger.  We identify a bright
source consistent within the UVOT candidate.

Using the USNO-B1.0 star (1263-0223138) at RA=14:31:39.66,
Dec=+36:18:54.5 with R2MAG=14.98 as a reference, we estimate the
following R-band magnitude for the transient:

t_start (UT) exp t (s) t_start-t_0 (s) R Mag
----------------------------------------------------------------
06:27:00.3 60   851   R = 13.52 +/- 0.01

Additional observations and analysis are ongoing.


GRB_name: GRB080319B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7433
SUBJECT: GRB080319B Liverpool Telescope optical afterglow candidate 
DATE:    08/03/19 08:25:53 GMT
FROM:    James Smith at ARI,Liverpool John Moors U  <rjs@astro.livjm.ac.uk>

R.J. Smith (Liverpool JMU), A. Gomboc (U. Ljubljana), N. Tanvir (Leicester) A. 
Melandri, C.G. Mundell, I.A. Steele, S. Kobayashi, D. Bersier (Liverpool JMU) 
report:

The 2-m Liverpool Telescope (La Palma) observed the position of
GRB 080319B (SWIFT trigger 306757) starting 30 min after the GRB trigger
time. We detect an optical afterglow candidate in r' filter at
14:31:41 +36:18:09 J2000 consistent with the uncatalogued source
visible in the UVOT data.

Filter    t_mid (min from GRB)    Tot_Exp (s)       R
--------------------------------------------------------------
   r'           30.64                 120           14.9
   r'           32.83                 120           15.1
   r'           35.02                 120           15.2
  -------------------------------------------------------------

Observations were performed in SDSS r' filter and
magnitudes calibrated vs R2 USNO-B1 magnitudes for a few selected stars.

No further observations were possible due to approaching twilight.


GRB_name: GRB080319B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7434
SUBJECT: GRB 080319b: Early IR Imaging from PAIRITEL
DATE:    08/03/19 08:30:12 GMT
FROM:    Josh Bloom at UC Berkeley  <jbloom@astron.berkeley.edu>

J. S. Bloom, D. Starr, and D. A. Perley (UC Berkeley) report:

We began observations of GRB080319b with PAIRITEL at 2008-03-19   
06:14:51 UT and will continue for several hours until sunrise. The  
source is exceedingly bright in the first few minutes, visible on  
individual 7.8 sec exposures in JHKs bands. Preliminary photometry,  
which may be affected to non-linearities at these bright flux levels,  
is given below.

# t (MJD)       terr (day)      filt     mag     merr
#####################################

54544.262141    0.000454        k       8.613900         
0.033214        0       0
54544.261788    0.000454        j       9.110600         
0.041347        0       0

A comparison with 2MASS may be found at:
    http://lyra.berkeley.edu/~jbloom/grb080319b.png

This message may be cited.


GRB_name: GRB080319B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7435
SUBJECT: GRB0 080319B : LOAO optical observation
DATE:    08/03/19 09:10:40 GMT
FROM:    Yuji Urata at Saitama U  <urata@asiaa.sinica.edu.tw>

Y. Urata, M. Im, I. Lee, K.Y Huang, W.K. Zheng, L.P. Xin
on behalf of EAFON report:

"We have been monitoring the GRB 080319B optical afterglow (Racusin et
al. GCN 7427) using Mt. Lemmon 1m telescope with B, V, R, I and z'
band filter. The brightness at about 80 min after the burst is R~16.0
mag. derived from USNO-B1.0 catalog. Comparing with the further reports
by Li et al (GCN 7430), and Milen & Williams (GCN 7432), the light
curve shows shallower decay from around 0.05 days after the burst.

Further analysis and observations are in progress."


GRB_name: GRB080319A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7436
SUBJECT: GRB 080319A: optical observations at the NOT
DATE:    08/03/19 11:06:34 GMT
FROM:    Daniele Malesani at Niels Bohr Inst,Dark Cosmology Center  <malesani@astro.ku.dk>

D. Malesani, J. P. U. Fynbo, P. M. Vreeswijk (DARK), C. Villforth (NOT), 
report on behalf of a larger collaboration:

We observed the field of GRB 080319A (Pagani et al., GCN 7426) with the 
Nordic Optical Telescope, starting on 2008 March 19.265 UT. Exposures in 
the R and I bands were secured.

We detect the afterglow reported by Cenko (GCN 7429). Compared to the 
USNO-B1 star 1340-0249427 at RA = 13:45:26.457, Dec = +44:04:45.56 (R1 = 
15.79), we measure R = 21.03 +- 0.09 on Mar 19.27088 UT (44.4 min after 
the GRB).

A finding chart is posted at:

http://www.astro.ku.dk/~malesani/GRB/080319A/080319A_finder.jpg

We acknowledge excellent support from the NOT observing staff.


GRB_name: GRB080319B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7437
SUBJECT: GRB 080319B: Gemini-South Spectroscopy
DATE:    08/03/19 11:28:33 GMT
FROM:    Ryan Foley at UC Berkeley  <rfoley@astro.berkeley.edu>

R. J. Foley, D. Perley, and J. S. Bloom (UCB) on behalf of the GRAASP
collaboration report:

We obtained 2x1800 sec exposures of the optical afterglow (GCN 7428, 7430)
of GRB 080319B (GCN 7427) using GMOS on the Gemini-South telescope with
the R831 grating.  The observations started at 20080319.35 (~2 hours after
the initial Swift trigger).  Initial reductions show a featureless
continuum with no strong absorption systems, emission lines, or breaks.
Given our wavelength range of 595 - 815 nm, we can place the following
constraints on the redshift (in order of descending confidence):

(1) The lack of a Lyman limit implies z < 5.5.
(2) The lack of damped Lya or obvious Lya forest implies z < 3.9.
(3) The lack of obvious Mg II absorption implies z < 1.1.

Further analysis is in progress.


GRB_name: GRB080319B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7438
SUBJECT: GRB 080319B: Change in power law decay index
DATE:    08/03/19 11:36:37 GMT
FROM:    Weidong Li at UC Berkeley KAIT/LOSS  <weidong@astron.berkeley.edu>

W. Li, R. Chornock, D. A. Perley, and A. V. Filippenko, University of
California at Berkeley, on behalf of the KAIT GRB team:

We have analyzed the KAIT data on GRB 080319B (GCN 7472, 7428) as reported
in GCN 7430. Preliminary reduction of the unfiltered data, calibrated to
SDSS observations of the field, shows a smooth light curve from t = 20 to
120 minutes after the BAT trigger, with an apparent change in power-law
decay index at t ~ 35 minutes. The power-law decay index is measured to be
-1.89 +/- 0.04 between t = 20.1 to 26.3 minutes after the BAT trigger, and
-1.23 +/- 0.02 between t=60.9 to 117.2 minutes after the BAT trigger.
The shallower decay is also observed at t ~ 80 minutes as noted in GCN 7435.
We note this change in power-law decay index is reminiscent of what has
been observed in GRB 990123 (e.g. Akerlof et al. 1999, Nature 398, 400) and
GRB 021211 (e.g. Li et al. 2003, ApJ 586, L9), and suggests a transition from
reverse shock to forward shock emission.

Selected KAIT unfiltered photometry, all unfiltered data calibrated to
the R band via the SDSS calibration:

t(start; seconds after BAT trigger)  exp    mag   merr

       1207                         20.0   14.110 0.008 
       1394                         20.0   14.417 0.011
       1576                         20.0   14.645 0.011
       1991                         20.0   15.063 0.011
       2912                         20.0   15.710 0.014
       3770                         20.0   16.053 0.015
       4380                         20.0   16.247 0.014
       5005                         20.0   16.415 0.019
       6820                         20.0   16.843 0.017


GRB_name: GRB080319B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7439
SUBJECT: GRB 080319b prompt optical observation by Pi-of-the-Sky
DATE:    08/03/19 11:55:07 GMT
FROM:    Grzegorz Wrochna at Soltan Inst.for Nuclear Studies  <wrochna@fuw.edu.pl>

M.Cwiok, W.Dominik, G.Kasprowicz, A.Majcher, A.Majczyna,
K.Malek, L.Mankiewicz, M.Molak, K.Nawrocki, L.W.Piotrowski,
D.Rybka, M.Sokolowski, J.Uzycki, G.Wrochna, A.F.Zarnecki
on behalf of "Pi of the Sky" collaboration http://grb.fuw.edu.pl

"Pi of the Sky" apparatus located at Las Campanas Observatory
imaged the region of GRB 080319b (Swift triger 306757 at 06:12:49 UT)
before, during and after the GRB with 10s exposures (IR-cut filter only).
We observe optical emission at the position given by Swift XRT.
   start -   end     comment
6:12:33 - 6:12:43   not visible (>12 mag)
6:12:47 - 6:12:57   visible (~10 mag)
6:13:01 - 6:13:11   max. brightness (~6 mag)

Full light curve fill be published later.


GRB_name: GRB080319A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7440
SUBJECT: GRB 080319A: REM observations
DATE:    08/03/19 11:59:06 GMT
FROM:    Stefano Covino at Brera Astronomical Observatory  <stefano.covino@gmail.com>

S. Covino, P. D'Avanzo, D. Fugazza, L.A. Antonelli, L.  Calzoletti,   
S. Campana, G.  Chincarini, M.L. Conciatore, S. Cutini, V. D'Elia, F.  
D'Alessio, F.  Fiore, P. Goldoni, D. Guetta,  C. Guidorzi, G.L.  
Israel, E. Maiorano, N. Masetti, A. Melandri, E. Meurs, L. Nicastro,  
E. Palazzi, E. Pian, S. Piranomonte, L.  Stella, G.  Stratta, G.  
Tagliaferri, G. Tosti, V.Testa, S.D. Vergani,  F. Vitali report on  
behalf of the REM team:

The robotic 60-cm REM telescope located at La Silla (Chile) observed  
automatically the field of the GRB 080319A (GCN 7426, Pagani et al.)  
about 40 seconds after the burst.

We do no detect any source at the position of the optical afterglow  
identified by Cenko et al. (GCN 7429) and Malesani et al. (GCN 7436)
with a 3sigma upper limit of  H~15.0 in the first coadded frame
at about 100sec after the burst.

[GCN OPS NOTE(19mar08): Per author's request, the Cenko reference
was added.]


GRB_name: GRB080319C
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7441
SUBJECT: GRB 080319C: KAIT OA candidate
DATE:    08/03/19 12:33:15 GMT
FROM:    Weidong Li at UC Berkeley KAIT/LOSS  <weidong@astron.berkeley.edu>

W. Li, R. Chornock, and A. V. Filippenko, University of California 
at Berkeley, on behalf of the KAIT GRB team, report:

KAIT responded to GRB 080319C (Swift trigger 306778) and was taking 
images. There is an afterglow candidate at position

RA  = 17:15:55.54
DEC = +55:23:30.8
(equinox J2000)

The measured magnitude is R = 17.4 at 12:27:55 UT. Further observations
are ongoing.


GRB_name: GRB080319C
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7442
SUBJECT: GRB 080319C: Swift detection of a burst with an optical afterglow
DATE:    08/03/19 12:45:58 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

C. Pagani (PSU), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), A. P. Beardmore (U Leicester),
D. N. Burrows (PSU), P. A. Evans (U Leicester),
N. Gehrels (NASA/GSFC), O. Godet (U Leicester),
S. T. Holland (CRESST/USRA/GSFC), J. A. Kennea (PSU),
V. Mangano (INAF-IASFPA), J. P. Osborne (U Leicester),
K. L. Page (U Leicester), A. M. Parsons (GSFC), J. L. Racusin (PSU),
B. Sbarufatti (INAF-IASFPA), M. Stamatikos (NASA/ORAU),
R. L. C. Starling (U Leicester), G. Stratta (ASDC) and
T. N. Ukwatta (GSFC/GWU) report on behalf of the Swift Team:

At 12:25:56 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 080319C (trigger=306778).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 258.973, +55.410 which is 
   RA(J2000)  =  17h 15m 54s
   Dec(J2000) = +55d 24' 35"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows several overlapping FRED-like
peaks starting at T+0 and ending around T+20 sec.  The peak count rate
was ~8000 counts/sec (15-350 keV), at ~T+0 sec after the trigger. 

The XRT began observing the field at 12:29:40 UT, 224 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source with an enhanced position: RA, Dec 258.9828, 55.3920
which is equivalent to:
   RA(J2000)  = 17h 15m 55.86s
   Dec(J2000) = +55d 23' 31.2"
with an uncertainty of 4.5 arcseconds (radius, 90% containment). This
location is 3 arcseconds from the optical afterglow candidate position. 

UVOT took a finding chart exposure of 100 seconds with the White   
(160-650 nm) filter starting 227 seconds after the BAT trigger. There
is a candidate afterglow in the rapidly available 2.7'x2.7' 
sub-image at   

  RA(J2000)  = 17:15:55.51 = 258.9813   
  DEC(J2000) = +55:23:30.8  = +55.3919    

with a 1-sigma error radius of  about 0.5 arc sec. This position
is 67.4 arc sec. from the center of  the BAT error circle.  This
is consistent with the KAIT position (Li  et al., 2008, GCNC 7441). 
The estimated magnitude is white = 18.8 with a  1-sigma  error of
about 0.5 mag. No correction has been  made for the  expected
extinction corresponding to E(B-V) of 0.03. 

Burst Advocate for this burst is C. Pagani (pagani AT astro.psu.edu). 
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.)


GRB_name: GRB080319C
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7443
SUBJECT: GRB 080319C: Early Super-LOTIS Observations
DATE:    08/03/19 13:30:10 GMT
FROM:    Grant Williams at Steward Observatory  <ggwilli@gmail.com>

G. G. Williams (MMTO) and P. A. Milne (Steward Observatory), on behalf
of the Super-LOTIS Collaboration, report:

The robotic 0.6-m Super-LOTIS telescope began observing the error box
of GRB 080319C (Swift Trigger 306778, Pagani et al. GCN 7442) at
12:26:38.5 UT, 42.5 seconds after the trigger.  Our initial
observations include 5 x 10s exposures, 5 x 20s exposures, and 30 x
60s exposures, all in the R-band.

We detect the afterglow reported by Li et al. (GCN 7441) in our
earliest 10 second exposure.  Using the USNO-B1.0 star (453-025776) at
RA=17:15:51.7, Dec=55:23:38.4 with R2MAG=14.61, we estimate the
following R-band magnitude for the OT:

t_start (UT) exp t (s) t_start-t_0 (s) R Mag
----------------------------------------------------------------
12:26:38.5 10   42.5   R = 16.83 +/- 0.13

Additional observations and analysis are ongoing.


GRB_name: GRB080319B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7444
SUBJECT: VLT/UVES redshift of GRB 080319B
DATE:    08/03/19 13:34:33 GMT
FROM:    Paul Vreeswijk at Dark Cosmology Centre,U.of Copenhagen  <pmv@dark-cosmology.dk>

P.M. Vreeswijk (DARK), A. Smette (ESO), D. Malesani, J.P.U. Fynbo, Bo
Milvang-Jensen (DARK), P. Jakobsson (U. Hertfordshire), A.O. Jaunsen
(U. Oslo) and C. Ledoux (ESO) report on behalf of a larger
collaboration:

We observed the optical afterglow of GRB 080319B (Racusin et al., GCN
7427) with the Ultraviolet and Visual Echelle Spectrograph (UVES)
mounted at ESO's VLT Kueyen. Observations were performed in
rapid-response mode starting on 2008 March 19 at 07:18 UT.

The highest redshift system that we identify based on the MgII doublet
and various other features has z=0.937, the presumed redshift of GRB
080319B. Another system is identified at z=0.530.

We acknowledge excellent support from the observing staff at Paranal,
in particular Swetlana Hubrig and Elena Mason.


GRB_name: GRB080319B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7445
SUBJECT: GRB 080319b light curve by Pi-of-the-Sky
DATE:    08/03/19 13:38:20 GMT
FROM:    Grzegorz Wrochna at Soltan Inst.for Nuclear Studies  <wrochna@fuw.edu.pl>

M.Cwiok, W.Dominik, G.Kasprowicz, A.Majcher, A.Majczyna,
K.Malek, L.Mankiewicz, M.Molak, K.Nawrocki, L.W.Piotrowski,
D.Rybka, M.Sokolowski, J.Uzycki, G.Wrochna, A.F.Zarnecki
on behalf of "Pi of the Sky" collaboration http://grb.fuw.edu.pl

Following GCN 7439 we give the preliminary light curve of GRB 080319b
(IR-cut filter only):

  start  - end       frame    magnitudo
6:12:33 - 6:12:43    <=96    limit >11.48
6:12:47 - 6:12:57     97     9.83
6:13:01 - 6:13:11     98     5.76
6:13:16 - 6:13:26     99     6.00
6:14:03 - 6:14:13    100     8.26
6:14:17 - 6:14:27    101     8.77
6:14:32 - 6:14:42    102     9.10
6:14:46 - 6:14:56    103    10.27
6:15:27 - 6:14:37    104    10.50
6:15:41 - 6:14:51    105    11.10
6:15:56 - 6:16:06    106    11.21
6:16:40 - 6:16:50    107    11.79
6:16:54 - 6:17:04    108    11.95

More information will be published at http://grb.fuw.edu.pl


GRB_name: GRB080319B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7446
SUBJECT: GRB 080319B: REM early data
DATE:    08/03/19 13:44:13 GMT
FROM:    Stefano Covino at Brera Astronomical Observatory  <stefano.covino@gmail.com>

S. Covino, P. D'Avanzo, D. Fugazza, L.A. Antonelli, L.  Calzoletti,  
S. Campana, G.  Chincarini, M.L. Conciatore, S. Cutini, V. D'Elia, F.  
D'Alessio, F.  Fiore, P. Goldoni, D. Guetta,  C. Guidorzi, G.L.  
Israel, E. Maiorano, N. Masetti, A. Melandri, E. Meurs, L. Nicastro,  
E. Palazzi, E. Pian, S. Piranomonte, L.  Stella, G.  Stratta, G.  
Tagliaferri, G. Tosti, V.Testa, S.D. Vergani,  F. Vitali report on  
behalf of the REM team:


We started a refined analysis of the REM observations of GRB 080319B  
(GCN 7427, Racusin et al.). As already reported by Cwiok et al. (GCN  
7439 and 7445) the optical counterpart of this GRB was exceptionally  
bright at early time. We measured, about 1 min after the burst, R~6.4  
assuming R=11.20 for the USNO star at coordinates RA,DEC =  
14:31:23.61, 36:21:56.5. The source was already almost 2 mag fainter  
half a minute later. In the H band the source was H~5 around the same  
epoch.

Further analyses are in progress.


GRB_name: GRB080319A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7447
SUBJECT: GRB 080319A, Swift-BAT refined analysis
DATE:    08/03/19 15:04:20 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), J. Cummings (GSFC/UMBC), E. Fenimore (LANL),
N. Gehrels (GSFC), H. Krimm (GSFC/USRA), C. Markwardt (GSFC/UMD),
K. McLean (GSFC/UMD), C. Pagani (PSU), D. Palmer (LANL),
A. Parsons (GSFC), T. Sakamoto (GSFC/UMBC), G. Sato (GSFC/ISAS),
M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC), T. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using the data set from T-120 to T+182 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 080319A (trigger #306754)
(Pagani, et al., GCN Circ. 7426).  The BAT ground-calculated position is
RA, Dec = 206.352, 44.080 deg, which is 
   RA(J2000)  =  13h 45m 24.6s 
   Dec(J2000) = +44d 04' 47.3" 
with an uncertainty of 1.7 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 7%.
 
The mask-weighted light curve shows two main over-lapping FRED-like peaks
starting at ~T-5 sec, peaking at T+5 and T+25 sec, and ending at ~T+70 sec.
T90 (15-350 keV) is 64 +- 36 sec (estimated error including systematics).
 
The time-averaged spectrum from T-7.7 to T+72.3 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.60 +- 0.13.  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+31.80 sec in the 15-150 keV band
is 1.2 +- 0.2 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/306754/BA/

Due to a large backlog in downlinking the full data on this burst,
we currently do not have the usual data set out to long times yet.
Should the remaining data show that there is ongoing activity 
for this burst past the data cutoff at T+182sec, then we will
issue an updated 'refined analysis' circular.


GRB_name: GRB080319A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7448
SUBJECT: GRB 080319A: Enhanced Swift-XRT position
DATE:    08/03/19 16:01:24 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.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 596 s of overlapping XRT Photon Counting mode and UVOT
data for GRB 080319A, 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 = 206.33318, +44.08038 which is equivalent
to:

RA (J2000): 13h 45m 19.96s
Dec (J2000): +44d 04' 49.4"

with an uncertainty of 1.8 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
http://www.swift.ac.uk/xrt_positions/Goad.pdf).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB080319B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7449
SUBJECT: GRB 080319B: Enhanced Swift-XRT position
DATE:    08/03/19 16:04:51 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.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 1859 s of overlapping XRT Photon Counting mode and UVOT
data for GRB 080319B, 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 = 217.92113, +36.30269 which is equivalent
to:

RA (J2000): 14h 31m 41.07s
Dec (J2000): +36d 18' 09.7"

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
http://www.swift.ac.uk/xrt_positions/Goad.pdf).

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB080319A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7450
SUBJECT: GRB 080319A/B/C: INTEGRAL SPI-ACS light curves available 
DATE:    08/03/19 16:08:28 GMT
FROM:    Volker Beckmann at ISDC  <Volker.Beckmann@obs.unige.ch>

V. Beckmann (ISDC), S. Mereghetti (INAF/IASF-Milano), A. von Kienlin
(MPE), M. Beck, V. Savchenko (ISDC), J. Borkowski (CAMK/Torun), D. Gotz 
(CEA/Saclay) report on behalf of the INTEGRAL SPI-ACS GRB team:

The three GRB reported on 2008-03-19 by the Swift team (GCN 7426, 7427,
7442) have been independently detected by the SPI Anti-Coincidence 
System (ACS) on-board INTEGRAL.

Burst         T0     duration    max counts in 50 msec
------------------------------------------------------
GRB080319A  05:45:41    10s        370
GRB080319B  06:12:47    57s       5500
GRB080319C  12:25:55    25s       1200

The SPI-ACS light curves are available (both as images and data files) 
at http://isdc.unige.ch/Soft/ibas/ibas_acs_web.cgi

The light curves, binned at 50 ms, are derived from 91 independent
detectors with different lower energy thresholds (mainly between 50 keV 
and 150 keV) and an upper threshold at about 100 MeV. The ACS response 
varies as a function of the GRB incident angle. For these reasons we 
caution that the count rates cannot be easily translated into physical 
flux units.


GRB_name: GRB080319B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7451
SUBJECT: VLT/UVES redshift of GRB 080319B from FeII fine-structure lines
DATE:    08/03/19 16:36:37 GMT
FROM:    Paul Vreeswijk at Dark Cosmology Centre,U.of Copenhagen  <pmv@dark-cosmology.dk>

P.M. Vreeswijk, Bo Milvang-Jensen (DARK), A. Smette (ESO),
D. Malesani, J.P.U. Fynbo (DARK), P. Jakobsson (U. Hertfordshire),
A.O. Jaunsen (U. Oslo) and C. Ledoux (ESO) report on behalf of a
larger collaboration:

Besides the absorption systems at z=0.937 and z=0.530 reported in GCN
7444, we also note the presence of two other systems at z=0.715 and
z=0.760 along the sightline toward GRB 080319B. The rest-frame
equivalent width of MgII 2796 for both the z=0.937 and z=0.715 systems
is large: greater than 1A.  Finally, we detect several transitions
from FeII fine-structure levels from the z=0.937 system. Assuming that
the GRB afterglow is responsible for the FeII excitation (see
Prochaska et al. 2006, ApJ, 648, 95; Vreeswijk et al. 2007, A&A, 468,
83), this confirms the z=0.937 system to be the host of GRB 080319B.


GRB_name: GRB080319B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7452
SUBJECT: GRB 080319B: TORTORA synchronous observation
DATE:    08/03/19 17:33:14 GMT
FROM:    Sergey Karpov at SAO RAS  <karpov@sao.ru>

S. Karpov, G. Beskin, S. Bondar, C. Bartolini, G. Greco, A. Guarnieri,
D. Nanni, A. Piccioni, F. Terra, E. Molinari, G. Chincarini, F.M. Zerbi,
S. Covino, V. Testa, G. Tosti, F. Vitali, L.A. Antonelli, P. Conconi, G.
Cutispoto, G. Malaspina, L. Nicastro, E. Palazzi, E. Meurs, P.  Goldoni

report on behalf of the TORTOREM team:

TORTORA wide-field optical camera (12 cm diameter, 20x25 deg FOV, TV-CCD,
unfiltered) mounted on REM robotic 60-cm telescope located at La Silla
(Chile) observed the field of GRB 080319B (GCN 7427, Racusin et al.)
before, during and after the gamma-emission with 0.13 s time resolution.

We observe optical emission at the position given by Swift XRT:

1. We did not detect any transient  brighter than 8.5m (unfiltered,
near B) at T-100 - T+16 s 

2. We detect rapidly rising OT (~5 second rise front) and observe it
between T+16 and T+30, the peak brightness has been around 5 m

3. Between T+30 and T+36 the observations have been paused due to
repointing of REM telescope

4. Since T+36 we continuously observe the transient until it faded below
the detection limit (~8.5m) at T+90 s

The detailed analysis is in progress.

This message may be cited.


GRB_name: GRB080319D
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7453
SUBJECT: GRB 080319D: Swift detection of a burst with a possible optical afterglow
DATE:    08/03/19 17:42:09 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

P. J. Brown (PSU), S. D. Barthelmy (GSFC), D. N. Burrows (PSU),
M. M. Chester (PSU), N. Gehrels (NASA/GSFC), O. Godet (U Leicester),
S. T. Holland (CRESST/USRA/GSFC), S. Immler (CRESST/GSFC/UMD),
J. A. Kennea (PSU), H. A. Krimm (CRESST/GSFC/USRA),
P. T. O'Brien (U Leicester), J. P. Osborne (U Leicester),
C. Pagani (PSU), K. L. Page (U Leicester), D. M. Palmer (LANL),
M. Perri (ASDC), J. L. Racusin (PSU), M. Stamatikos (NASA/ORAU),
R. L. C. Starling (U Leicester), E. Troja (U Leicester/INAF-IASFPA)
and T. N. Ukwatta (GSFC/GWU) report on behalf of the Swift Team:

At 17:05:09 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 080319D (trigger=306793).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 99.480, +23.933 which is 
   RA(J2000) = 06h 37m 55s
   Dec(J2000) = +23d 56' 01"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  As is usual with an image trigger, the prompt light 
curve does not not show any clear structure.  We will be able to tell more with 
the full data set. 

The XRT began observing the field at 17:07:36.9 UT, 147.5 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued, 
variable X-ray source with an enhanced position: RA, Dec 99.47270, 23.94306
which is equivalent to:
   RA(J2000)  = 06h 37m 53.45s
   Dec(J2000) = +23d 56' 35.5"
with an uncertainty of 3.0 arcseconds (radius, 90% containment). This
location is 44 arcseconds from the BAT onboard position, within the BAT
error circle. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of
2.17e+21 cm^-2 (Kalberla et al. 2005), so we cannot constrain the
redshift at this time using the relation from Grupe et al. (2007). A
summary of the promptly downlinked data is given at
http://www.swift.ac.uk/sper/306793/. 

UVOT took a finding chart exposure of 100 seconds with the White (160-650 nm)
filter starting 152 seconds after the BAT trigger. A possible afterglow 
candidate has been found in the initial data products, at a magnitude of 
~19 mag. No correction has been made for the expected extinction corresponding
to E(B-V) of 0.19. The position of the tentative UVOT source is:
   RA(J2000)  = 06h 37m 53.6s
   Dec(J2000) = +23d 56' 34.1"

Burst Advocate for this burst is P. J. Brown (pbrown AT astro.psu.edu). 
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.)


GRB_name: GRB080319C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7454
SUBJECT: GRB 080319C: MASTER-VWF-Kislovodsk optical observation   
DATE:    08/03/19 17:46:32 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

MASTER-Net Team:

V. Lipunov, V.Kornilov, D.Kuvshinov, E.Gorbovskoy, N.Tyurina, 
A.Belinski,  A.Krylov, N.Shatskiy, A.Sankovich, V.Vladimirov,
  P.Gritsyk, V.Vibornov, A.Kuznetsov, P.Balanutsa
Sternberg Astronomical Institute, Moscow Union 'Optic'

A. Tlatov, I.Golubov
Kislovodsk Solar Station of the Pulkovo observatory

K.Ivanov
Irkutsk State University

I.Zalognikh
Ural State University, Kourovka

MASTER Very Wide Field Camera located at Kislovodsk Solar Station
(http://observ.pereplet.ru, D=70 mm, 420 square degrees, 11 Mpixel's CCD) 
has moved to the Swift-BAT trigger 306793 and it has taken a series of 5s
exposures starting 92 s after notice arrivel time  708 s after GRB time at 
17 16  57 UT under good weather  condition and moon.


There is no OT was found inside Swift error box brighter than 11.5m.

MASTER-Net team  congratulate "Pi of the Sky" - Team 
with wonderfull and long-awaited  result (Cwiok et al. GCN 7445)!

This message can be cited.
Mailto: lipunov@sai.msu.ru


GRB_name: GRB080319D
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7455
SUBJECT: GRB 080319D: MASTER-VWF-Kislovodsk optical observation  
DATE:    08/03/19 17:49:54 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

Correction to GCN 7454!

MASTER-Net Team:

V. Lipunov, V.Kornilov, D.Kuvshinov, E.Gorbovskoy, N.Tyurina, A.Belinski, 
A.Krylov, N.Shatskiy, A.Sankovich, V.Vladimirov,
  P.Gritsyk, V.Vibornov, A.Kuznetsov, P.Balanutsa
Sternberg Astronomical Institute, Moscow Union 'Optic'

A. Tlatov, I.Golubov
Kislovodsk Solar Station of the Pulkovo observatory

K.Ivanov
Irkutsk State University

I.Zalognikh
Ural State University, Kourovka

MASTER Very Wide Field Camera located at Kislovodsk Solar Station
(http://observ.pereplet.ru, D=70 mm, 420 square degrees, 11 Mpixel's CCD) has 
moved to the Swift-BAT trigger 306793 and it has taken a series of 5s
exposures starting 92 s after notice arrivel time  708 s after GRB time at 17 
16  57 UT under good weather  condition and moon.


There is no OT was found inside Swift error box brighter than 11.5m.

MASTER-Net team  congratulate "Pi of the Sky" - Team with wonderfull and 
long-awaited  result (Cwiok et al. GCN 7445)!

This message can be cited.
Mailto: lipunov@sai.msu.ru


GRB_name: GRB080319B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7456
SUBJECT: GRB 080319B:  Hobby-Eberly Telescope Spectroscopy 
DATE:    08/03/19 17:58:58 GMT
FROM:    Antonino Cucchiara at PSU  <cucchiara@astro.psu.edu>

A. Cucchiara & D. B. Fox (PSU) report on behalf of a larger
collaboration:

"Starting on 2008 March 18.49 UT we used the Marcario LRS spectrograph
on the Hobby-Eberly Telescope (R ~ 230 ) to obtain one 1200s spectra
of the optical afterglow (Holland et al., GCN 7428) of GRB 080319B
(Racusin et al., GCN 7427).  The spectrum covers the wavelength range
4100 to 10,500 Angstrom.  We observe multiple metal absorption
features including the MgII doublet (2796, 2803 A) and MgI (2852 A) at
z ~ 0.937. We also detect lines at z ~ 0.760 (MnII 2576, MnII 2594 and
CaI 4227), z ~ 0.715 (MgII doublet) and z ~ 0.530 (NaI 5890,5896).
Our observations are consistent with the redshift and features
reported by Vreeswijk et al. (GCN 7444, 7451)."

[GCN OPS NOTE(19mar08): Per author's request, the date in the Subject-line
was changed from "080519B" to "080319B".  And the date in the first line
was changd from "18.49" to 19.49".]


GRB_name: GRB080319C
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7457
SUBJECT: GRB 080319C: AGILE-MCAL observation of the prompt emission
DATE:    08/03/19 19:09:02 GMT
FROM:    Sandro Mereghetti at IASF/CNR  <sandro@iasf-milano.inaf.it>

M. Marisaldi (INAF/IASF Bologna), F. Fornari (INAF/IASF Milano), C. 
Labanti, F. Fuschino, M. Galli, A. Bulgarelli, F. Gianotti, M. Trifoglio, 
G. Di Cocco (INAF/IASF Bologna), E. Costa, E. Del Monte, I. Donnarumma, Y. 
Evangelista, M. Feroci, I. Lapshov, F. Lazzarotto, L. Pacciani, M. 
Rapisarda, P. Soffitta (INAF/IASF Roma), A. Giuliani, S. Vercellone, A. 
Chen, S. Mereghetti, A. Pellizzoni, F. Perotti, M. Fiorini, P. Caraveo 
(INAF/IASF Milano), M. Tavani, G. Pucella, F. D'Ammando, V. Vittorini, A. 
Argan, A. Trois (INAF/IASF Rome), G. Barbiellini, F. Longo, E. Vallazza 
(INFN Trieste), P. Picozza, A. Morselli (INFN Roma-2), M. Prest 
(Universita' dell'Insubria), P. Lipari, D. Zanello (INFN Roma-1), and P. 
Giommi, C. Pittori, (ASDC) and L. Salotti (ASI), on behalf of the AGILE 
Team, report:

"The Swift localized GRB 080319C (Pagani et al., GCN 7442) triggered the 
Mini-Calorimeter (MCAL) instrument onboard the AGILE satellite at 12:25:56 
UT (=T0). The MCAL instrument covers the energy range 350 keV - 10 MeV, 
without imaging capabilities.

The MCAL light curve shows two main overlapping broad peaks, the first 
peaking at T0 and the second peaking at T0+9s in the 350-700 keV energy 
band. Above 700 keV only the first peak is still detected, with 5 sigma 
detection also in the 1.4-2.8 MeV energy band. Using the preliminary 
in-flight calibration, we can estimate the 1-s peak flux in the 350-700 
keV energy band at T0 to be 2.0(-0.8,+0.9) photons/cm2/s.

The Swift localization is out of the field of view of the AGILE Gamma-Ray 
Imaging Detector (GRID), sensitive in the 50 MeV - 50 GeV energy range. 
Analysis of the GRID count rate does not show any detection. The event was 
well outside of the SuperAGILE field of view as well, but the event passed 
through the collimator shield and was weakly detected in the count rate."

We incidentally note that the brighter GRB 080319B (Racusin et al. GCN 
7427) was not observed by the AGILE instruments due to Earth occultation.

This message may be cited.


GRB_name: GRB080319D
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7458
SUBJECT: GRB 080319D: Swift/UVOT Refined Analysis of the Fading Optical Afterglow Candidate
DATE:    08/03/19 19:54:49 GMT
FROM:    Stefan Immler at NASA/GSFC  <stefan.m.immler@nasa.gov>

S. Immler (CRESST/GSFC/UMD) and P. J. Brown (PSU) report on behalf
of the Swift UVOT team:

The Swift/UVOT observations of the field of GRB 080319D (trigger 306793)
starting 151 seconds after the BAT trigger (Brown, et al., GCN Circ. 7453)
reveal a fading optical afterglow candidate. The white and v-filter 
magnitudes
are as follows:

Filter        T_start (s)    T_stop (s)        Exp (s)    Mag (3-sigma UL)
----------------------------------------------------------------------------------------------
White    151        251            100        19.7+/-0.3
White    866        966            100        20.2+/-0.4
v        257        657            400        >19.5
v        972        1362        400        >19.5
----------------------------------------------------------------------------------------------

No correction has been made for the expected Galactic extinction 
corresponding
to E(B-V) of 0.19 (Schlegel, et al. 1998). The position of the optical 
afterglow
candidate is

RA (2000) = 06h 37m 53.6s
Dec (2000) = +23d 56' 34.2"

with an uncertainty of 0.5 arcsec, which is 2.2 arcsec offset from the XRT
position (Brown, et al., GCN Circ. 7453).


GRB_name: GRB080319B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7459
SUBJECT: GRB 080319B: Swift-XRT Team Refined Analysis
DATE:    08/03/19 20:06:16 GMT
FROM:    Judith Racusin at PSU  <racusin@astro.psu.edu>

J. Racusin (PSU), D. N. Burrows (PSU), P. A. Evans (U Leicester), C.
Pagani (PSU), report on behalf of the Swift-XRT Team:

We have analysed the first four orbits of Swift-XRT data obtained for GRB
080319B (Racusin et al. GCN Circ. 7427), totaling 1.1 ks of Windowed
Timing (WT) data beginning 64 s after the BAT trigger, and 4 ks of Photon
Counting (PC) data beginning 5 ks after the BAT trigger.

The UVOT-enhanced XRT position has been given by Evans et al. in GCN Circ
7449.

The bright X-ray light-curve can be fit by a broken power-law, with an
initial decay index of 1.46 +/- 0.01 followed, after a break at 6100 +/-
440 seconds, by a steeper decay index of 2.48 +/- 0.10.

Both the WT and PC spectra are strongly affected by photon pile-up, which
can alter the spectral fits.  To eliminate these effects, we exclude the
central 8 pixel radius region of the WT data, and the central 3 pixel
radius region of the PC data when creating the spectra.  Preliminary fits
to the WT spectrum (64-4943 seconds), modeled with an absorbed power-law,
result in a photon index of 1.65 +/- 0.02 and an absorbing column at
z=0.937 (Vreeswijk et al., GCN Circ. 7444) of NH = (5.28 +/- 1.03)e20
cm^-2, in addition to Galactic absorption of 1.12e20 cm^-2 in the
direction of the burst, with a reduced Chi^2=1.05.  The PC spectrum (5-19
ks) can be modeled as an absorbed power-law, with photon index of 1.92 +/-
0.07 and an absorbing column at z=0.937 of NH = (23.5 +/- 5.6)e20 cm^-2,
in addition to the Galactic absorption, with a reduced Chi^2=1.06.  If we
freeze the NH in the PC model to the WT fitted value, we fit a photon
index of 1.73 +/ 0.04, with a reduced Chi^2=1.4, which excludes this model
as a viable fit.  As another attempt to model the spectra without NH
evolution, we freeze the WT NH to the value from the PC spectral fits and
add an additional low energy thermal component.  The resulting fits yield
a photon index of 1.73 +/- 0.02, kT=0.06 +/- 0.01 keV, and a reduced
Chi^2=1.07.  Therefore, the extra thermal component is a possible
explanation for the apparent spectral evolution.

Assuming the source continues to decay with the same decay index of 2.5,
we predict an XRT count rate of 8.8e-4 counts/s at T+24 hours, which
corresponds to an 0.3-10.0 keV observed (unabsorbed) flux of 6.1e-14
(6.2e-14) ergs cm^-2 s^-1.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB080319C
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7460
SUBJECT: GRB 080319C: Swift-XRT Team Refined Analysis
DATE:    08/03/19 20:13:43 GMT
FROM:    Claudio Pagani at PSU/Swift-XRT  <pagani@astro.psu.edu>

C. Pagani, J. L. Racusin, J.A. Kennea, D. N. Burrows (PSU) and P. A. Evans (U
Leicester) report on behalf of the Swift-XRT team:

The Swift-XRT started observing GRB 080319C (trigger=306778, Pagani et al. GCN
7442) at 12:29:40 UT, 224 seconds after the BAT trigger. The Swift slew to the
burst was delayed because of an Earth constraint. The current dataset consist
of 2.2ks of Photon Counting mode data from the first orbit of observation.

Using 595 s of overlapping XRT Photon Counting mode and UVOT data, 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 = 258.97980,
55.39197 which is equivalent to:

RA (J2000):  17 15 55.15
Dec (J2000): +55 23 31.1

with an uncertainty of 1.7 arcsec (radius, 90% confidence).

The 0.3-10 keV X-ray light curve starts at a count rate of ~7 counts/s and peaks
at ~18 counts/s at T+360 seconds, after which it shows a decline with a decay
slope of 0.9 +/- 0.1 with hints of superimposed flaring activity.

The spectrum of the PC data can be well fit by an absorbed powerlaw with photon
index 1.73 +/- 0.06 and column density of (1.5 +/- 0.1)e21 cm^-2, in excess of
the Galactic column density of 2.21e20 cm^-2 in this direction. The average
observed 0.3-10 keV flux is 1.0e-10 erg cm^-2 s^-1, which corresponds to an
unabsorbed flux of 1.3e-10 erg cm^-2 s^-1. The counts to observed flux
conversion factor at the time of this spectrum is 4.3e-11 erg cm^-2 count^-1.

If the underlying powerlaw decay continues as is, we predict an XRT count rate
of 0.11 counts/s at T+24hr, which corresponds to an observed 0.3-10keV flux of
4.7e-12 erg cm^-2 s^-1.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB080319B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7461
SUBJECT: GRB080319B: Prompt PROMPT Detections
DATE:    08/03/19 20:21:30 GMT
FROM:    Mark Schubel at UNC/PROMPT  <mschubel@physics.unc.edu>

M. Schubel, D. Reichart, M. Nysewander, A. LaCluyze, K. Ivarsen, J. A. 
Crain, A. Foster, T. Brennan, J. Haislip, J. Styblova, and A. Trotter report:

Skynet observed the localization of GRB 080319B (Racusin et al., GCN 7427) 
with three of the 16" PROMPT telescopes at CTIO beginning 32 seconds after 
the trigger (15 seconds after notification) in UVRI.

We detect the afterglow (Racusin et al., GCN 7428) in all filters.  At 92 
seconds after the burst we measure V ~ 8.6 mag (calibrated to 3 NOMAD 
stars), and at 147 seconds we measure I ~ 8.9 mag (calibrated to 6 USNO B1 
stars).


GRB_name: GRB080319B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7462
SUBJECT: GRB 080319B, Swift-BAT refined analysis
DATE:    08/03/19 20:21:44 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

J. Cummings (GSFC/UMBC), S. D. Barthelmy (GSFC), E. Fenimore (LANL),
N. Gehrels (GSFC), H. Krimm (GSFC/USRA), C. Markwardt (GSFC/UMD),
K. McLean (GSFC/UMD), D. Palmer (LANL), A. Parsons (GSFC),
J. L. Racusin (PSU), T. Sakamoto (GSFC/UMBC), G. Sato (GSFC/ISAS),
M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC), T. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using the data set from T-120 to T+182 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 080319B (trigger #306757)
(Racusin, et al., GCN Circ. 7427).  The BAT ground-calculated position is
RA, Dec = 217.919, 36.300 deg which is 
   RA(J2000)  =  14h 31m 40.7s 
   Dec(J2000) = +36d 17' 58.4" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.
 
The mask-weighted light curve shows a large long bump of a peak
starting at ~T-10 sec, ramping up until ~T+10 sec, then mostly a flat top
with some small structure superposed, then starting to decay at ~T+50 sec.
It returns nearly to background by ~T+64 sec at which point there is
a loss of data due to an on-board data product buffer overflow.
The data resumes at T+120 sec.  There is still detectable emission
in the BAT 15-350 keV band out to T+180 sec (the limit of the data
downlinked so far).  From other count rate data products, we can say
that there is no other peaks during the 60-sec missing event data window
and that the low-level emission is about 10-15% of the peak emission.
Given the missing data, T90 (15-350 keV) has to be >50 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-3.8 to T+62.2 and T+120 to T+151 sec
is fit by a simple power-law model.  The power law index
of the time-averaged spectrum is 1.04 +- 0.02.  The fluence
in the 15-150 keV band is 8.1 +- 0.1 x 10^-05 erg/cm2.
The 1-sec peak photon flux measured from T+16.87 sec in the 15-150 keV band
is 24.8 +- 0.5 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/306757/BA/

Due to a large backlog in downlinking the full data on this burst,
we currently do not have the usual data set out to long times yet.
Should the remaining data show that there is ongoing activity 
for this burst past the data cutoff at T+182sec, then we will
issue an updated 'refined analysis' circular.


GRB_name: GRB080319A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7463
SUBJECT: GRB 080319A: Swift-XRT Team Refined Analysis
DATE:    08/03/19 22:07:29 GMT
FROM:    Claudio Pagani at PSU/Swift-XRT  <pagani@astro.psu.edu>

C. Pagani and J. L. Racusin (PSU) report on behalf of the Swift-XRT team:

The Swift-XRT started observing GRB 080319A (trigger=306754, Pagani et al. GCN
7426) at 05:54:59.4 UT, 557.4s after the trigger. The Swift slew to the burst
was delayed because of an Earth constraint and XRT observations were
interrupted by the Swift trigger on GRB 080319B. The current observations
consist of Photon Counting mode data from T+560s to T+1632s and from T+35ks to
T+37ks.

The best XRT position is the UVOT-enhanced position from Beardmore et al. (GCN
7448), consistent with the optical afterglow position reported by Cenko (GCN
7429).

The 0.3-10 keV X-ray light curve starts at a count rate of ~1 counts/s and shows
a decline with a decay slope of 0.94 +/- 0.05.

The spectrum of the PC data from T+560s to T+1632s can be well fit by an
absorbed powerlaw with photon index 2.1 +/- 0.3 and column density of (1.0 +/-
0.7)e21 cm^-2, in excess of the Galactic column density of 1.45e20 cm^-2 in
this direction. The average observed 0.3-10keV flux is 1.6e-11 erg cm^-2 s^-1,
which corresponds to an unabsorbed flux of 2.1e-11 erg cm^-2 s^-1.  The counts
to observed flux conversion factor at the time of this spectrum is 3.7e-11 erg
cm^-2 count^-1.

If the underlying powerlaw decay continues as is, we predict an XRT count rate
of 0.008 counts/s at T+24hr, which corresponds to an observed 0.3-10keV flux of
2.9e-13 erg cm^-2 s^-1.

This circular is an official product of the Swift-XRT team.


GRB_name: GRB080319B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7464
SUBJECT: GRB 080319B: RAPTOR observations of a naked eye burst
DATE:    08/03/19 22:09:52 GMT
FROM:    Przemyslaw R. Wozniak at LANL  <wozniak@lanl.gov>

P. Wozniak, W.T. Vestrand, J. Wren, and H. Davis
(Los Alamos National Laboratory)

The RAPTOR sky monitoring system began observing the location
of GRB 080319B more than an hour before the Swift BAT trigger
306757 (Racusin et al., GCN 7427). The first exposure with detectable
optical emission started ~2 seconds after the trigger at 06:12:50.9 UT.
A peak brightness of 5.6 mag was recorded in time interval from
06:13:21.2 to 06:13:31.2 UT, before the end of the gamma-ray emission.
Using the redshift z=0.937 from Vreeswijk et al. (GCN 7444) the
estimated luminosity of GRB 080319B exceeds that of GRB 990123.

Our response arrays RAPTOR-P and T began imaging at 06:14:24.3 UT
following the XRT localization trigger that interrupted the ongoing
follow-up measurements of GRB 080319A. The OT is detected by both
response instruments including all channels (V,R,I,clear) of the
simultaneous multicolor imager RAPTOR-T.


GRB_name: GRB080319B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7465
SUBJECT: GRB080319B - SDSS Pre-Burst Observations
DATE:    08/03/19 22:57:48 GMT
FROM:    Richard J. Cool at U.of AZ/Steward Obs  <rcool@as.arizona.edu>

Richard J. Cool (Arizona), Daniel J. Eisenstein (Arizona),
David W. Hogg (NYU), Michael R. Blanton (NYU), David J. Schlegel
(LBNL), J. Brinkmann (APO), Donald Q. Lamb (Chicago), Donald
P. Schneider (PSU), and Daniel E. Vanden Berk (PSU) report:

The Sloan Digital Sky Survey (SDSS) imaged the field of burst
GRB080319B prior to the burst.  As these data should be useful
as a pre-burst comparison and for calibrating photometry,
we are supplying the images and photometry measurements for
this GRB field to the community.

Data from the SDSS, including 5 FITS images, 3 JPGS, and
3 files of photometry and astrometry, are being placed at
http://mizar.as.arizona.edu/~grb/public/GRB080319B

We supply FITS images in each of the 5 SDSS bands of a 8'x8'
region centered on the GRB position (ra=217.920 (14:31:40.7),
dec=36.3041 (36:18:14.8); GCN 7427), as well as 3 gri
color-composite JPGs (with different stretches). The units
in the FITS images are nanomaggies per pixel.  A pixel is
0.396 arcsec on a side. A nanomaggie is a flux-density unit
equal to 10^-9 of a magnitude 0 source or, to the extent that
SDSS is an AB system, 3.631e-6 Jy.  The FITS images have WCS
astrometric information.

In the file GRB080319B_sdss.calstar.dat, we report photometry
and astrometry of 193 bright stars (r<20.5) within 15' of the
burst location.  The magnitudes presented in this file are asinh
magnitudes as are standard in the SDSS (Lupton 1999, AJ, 118,
1406). Beware that some of these stars are not well-detected
in the u-band; use the errors and object flags to monitor
data quality.


In the files GRB080319B_sdss.objects_flux.dat and
GRB080319B_sdss.objects_magnitudes.dat, we report photometry
of 705 objects detected within 6' of the GRB position.
We have removed saturated objects and objects with model
magnitudes fainter than 23.0 in the r-band.  The fluxes listed
in GRB080319B_sdss.objects_flux.dat are in nanomaggies while
the magnitudes listed in GRB080319B_sdss.objects_magnitudes.dat
are asinh magnitudes.

All quantities reported are standard SDSS photometry, meaning
that they are very close to AB zeropoints and magnitudes are
quoted in asinh magnitudes.  Photometric zeropoints are known
to about 2% rms.  None of the photometry is corrected for
dust extinction.  The Schlegel, Finkbeiner, and Davis (1998)
predictions for this region are A_U=0.059 mag, A_g=0.043 mag,
A_r = 0.031 mag, A_i=0.024 mag, and A_z=0.017 mag.

The file GRB080319B_sdss.spectro.dat contains a list of the
3 objects with SDSS spectroscopy within 6 arcminutes of the
GRB position.  In addition to the redshift and 1-sigma error
for each object, this file also lists the object spectroscopic
classification.


SDSS astrometry is generally better than 0.1 arcsecond per
coordinate.  Users requiring high precision astrometry should
take note that the SDSS astrometric system can differ from
other systems such as those used in other notices; we have
not checked the offsets in this region.

More detailed information pertaining to our SDSS GRB releases
can be found in our initial data release paper (Cool et
al. 2006, PASP 118, 733).  See the SDSS DR4 documentation for
more details: http://www.sdss.org/dr5.

These data have been reduced using a slightly different
pipeline than that used for SDSS public data releases.
We cannot guarantee that the values here will exactly match
those in the data release in which these data are included.
In particular, we expect the photometric calibrations to differ
by of order 0.01 mag.

This note may be cited, but please also cite the SDSS data
release paper, Adelman-McCarthy et al. (2007, ApJS, 172, 634),
when using the data or referring to the technical documentation.


GRB_name: GRB080319A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7467
SUBJECT: GRB 080319A  SDSS Pre-Burst Observations
DATE:    08/03/19 23:12:13 GMT
FROM:    Richard J. Cool at U.of AZ/Steward Obs  <rcool@as.arizona.edu>

Richard J. Cool (Arizona), Daniel J. Eisenstein (Arizona),
David W. Hogg (NYU), Michael R. Blanton (NYU), David J. Schlegel
(LBNL), J. Brinkmann (APO), Donald Q. Lamb (Chicago), Donald
P. Schneider (PSU), and Daniel E. Vanden Berk (PSU) report:

The Sloan Digital Sky Survey (SDSS) imaged the field of burst
GRB080319A prior to the burst.  As these data should be useful
as a pre-burst comparison and for calibrating photometry,
we are supplying the images and photometry measurements for
this GRB field to the community.

Data from the SDSS, including 5 FITS images, 3 JPGS, and
3 files of photometry and astrometry, are being placed at
http://mizar.as.arizona.edu/~grb/public/GRB080319A

We supply FITS images in each of the 5 SDSS bands of a 8'x8'
region centered on the GRB position (ra=206.333 (13:45:19.9),
dec=44.0803 (44:04:49.1); GCN 7426), as well as 3 gri
color-composite JPGs (with different stretches). The units
in the FITS images are nanomaggies per pixel.  A pixel is
0.396 arcsec on a side. A nanomaggie is a flux-density unit
equal to 10^-9 of a magnitude 0 source or, to the extent that
SDSS is an AB system, 3.631e-6 Jy.  The FITS images have WCS
astrometric information.

In the file GRB080319A_sdss.calstar.dat, we report photometry
and astrometry of 227 bright stars (r<20.5) within 15' of the
burst location.  The magnitudes presented in this file are asinh
magnitudes as are standard in the SDSS (Lupton 1999, AJ, 118,
1406). Beware that some of these stars are not well-detected
in the u-band; use the errors and object flags to monitor
data quality.

In the files GRB080319A_sdss.objects_flux.dat and
GRB080319A_sdss.objects_magnitudes.dat, we report photometry
of 404 objects detected within 6' of the GRB position.
We have removed saturated objects and objects with model
magnitudes fainter than 23.0 in the r-band.  The fluxes listed
in GRB080319A_sdss.objects_flux.dat are in nanomaggies while
the magnitudes listed in GRB080319A_sdss.objects_magnitudes.dat
are asinh magnitudes.

All quantities reported are standard SDSS photometry, meaning
that they are very close to AB zeropoints and magnitudes are
quoted in asinh magnitudes.  Photometric zeropoints are known
to about 2% rms.  None of the photometry is corrected for
dust extinction.  The Schlegel, Finkbeiner, and Davis (1998)
predictions for this region are A_U=0.075 mag, A_g=0.055 mag,
A_r = 0.040 mag, A_i=0.030 mag, and A_z=0.021 mag.

The file GRB080319A_sdss.spectro.dat contains a list of the
6 objects with SDSS spectroscopy within 6 arcminutes of the
GRB position.  In addition to the redshift and 1-sigma error
for each object, this file also lists the object spectroscopic
classification.


SDSS astrometry is generally better than 0.1 arcsecond per
coordinate.  Users requiring high precision astrometry should
take note that the SDSS astrometric system can differ from
other systems such as those used in other notices; we have
not checked the offsets in this region.

More detailed information pertaining to our SDSS GRB releases
can be found in our initial data release paper (Cool et
al. 2006, PASP 118, 733).  See the SDSS DR4 documentation for
more details: http://www.sdss.org/dr5.

These data have been reduced using a slightly different
pipeline than that used for SDSS public data releases.
We cannot guarantee that the values here will exactly match
those in the data release in which these data are included.
In particular, we expect the photometric calibrations to differ
by of order 0.01 mag.

This note may be cited, but please also cite the SDSS data
release paper, Adelman-McCarthy et al. (2007, ApJS, 172, 634),
when using the data or referring to the technical documentation.


GRB_name: GRB080319C
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7468
SUBJECT: GRB 080319C - SDSS Pre-Burst Observations
DATE:    08/03/19 23:20:53 GMT
FROM:    Richard J. Cool at U.of AZ/Steward Obs  <rcool@as.arizona.edu>

Richard J. Cool (Arizona), Daniel J. Eisenstein (Arizona),
David W. Hogg (NYU), Michael R. Blanton (NYU), David J. Schlegel
(LBNL), J. Brinkmann (APO), Donald Q. Lamb (Chicago), Donald
P. Schneider (PSU), and Daniel E. Vanden Berk (PSU) report:

The Sloan Digital Sky Survey (SDSS) imaged the field of burst
GRB080319C prior to the burst.  As these data should be useful
as a pre-burst comparison and for calibrating photometry,
we are supplying the images and photometry measurements for
this GRB field to the community.

Data from the SDSS, including 5 FITS images, 3 JPGS, and
3 files of photometry and astrometry, are being placed at
http://mizar.as.arizona.edu/~grb/public/GRB080319C

We supply FITS images in each of the 5 SDSS bands of a 8'x8'
region centered on the GRB position (ra=258.983 (17:15:55.9),
dec=55.3920 (55:23:31.2); GCN 7442), as well as 3 gri
color-composite JPGs (with different stretches). The units
in the FITS images are nanomaggies per pixel.  A pixel is
0.396 arcsec on a side. A nanomaggie is a flux-density unit
equal to 10^-9 of a magnitude 0 source or, to the extent that
SDSS is an AB system, 3.631e-6 Jy.  The FITS images have WCS
astrometric information.

In the file GRB080319C_sdss.calstar.dat, we report photometry
and astrometry of 467 bright stars (r<20.5) within 15' of the
burst location.  The magnitudes presented in this file are asinh
magnitudes as are standard in the SDSS (Lupton 1999, AJ, 118,
1406). Beware that some of these stars are not well-detected
in the u-band; use the errors and object flags to monitor
data quality.

In the files GRB080319C_sdss.objects_flux.dat and
GRB080319C_sdss.objects_magnitudes.dat, we report photometry
of 508 objects detected within 6' of the GRB position.
We have removed saturated objects and objects with model
magnitudes fainter than 23.0 in the r-band.  The fluxes listed
in GRB080319C_sdss.objects_flux.dat are in nanomaggies while
the magnitudes listed in GRB080319C_sdss.objects_magnitudes.dat
are asinh magnitudes.


All quantities reported are standard SDSS photometry, meaning
that they are very close to AB zeropoints and magnitudes are
quoted in asinh magnitudes.  Photometric zeropoints are known
to about 2% rms.  None of the photometry is corrected for
dust extinction.  The Schlegel, Finkbeiner, and Davis (1998)
predictions for this region are A_U=0.134 mag, A_g=0.098 mag,
A_r = 0.071 mag, A_i=0.054 mag, and A_z=0.038 mag.

The file GRB080319C_sdss.spectro.dat contains a list of the
4 objects with SDSS spectroscopy within 6 arcminutes of the
GRB position.  In addition to the redshift and 1-sigma error
for each object, this file also lists the object spectroscopic
classification.


SDSS astrometry is generally better than 0.1 arcsecond per
coordinate.  Users requiring high precision astrometry should
take note that the SDSS astrometric system can differ from
other systems such as those used in other notices; we have
not checked the offsets in this region.

More detailed information pertaining to our SDSS GRB releases
can be found in our initial data release paper (Cool et
al. 2006, PASP 118, 733).  See the SDSS DR4 documentation for
more details: http://www.sdss.org/dr5.

These data have been reduced using a slightly different
pipeline than that used for SDSS public data releases.
We cannot guarantee that the values here will exactly match
those in the data release in which these data are included.
In particular, we expect the photometric calibrations to differ
by of order 0.01 mag.

This note may be cited, but please also cite the SDSS data
release paper, Adelman-McCarthy et al. (2007, ApJS, 172, 634),
when using the data or referring to the technical documentation.


GRB_name: GRB080319B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7469
SUBJECT: GRB 080319B: optical observations
DATE:    08/03/20 00:35:10 GMT
FROM:    Martin Jelinek at Inst.Astrophys.Andalucia,Granada  <mates@iaa.es>

Martin Jelinek, Alberto J. Castro-Tirado (IAA-CSIC Granada),
Virginie Chantry (Universit de Liege) and
Jorge Pl (IAC La Laguna), on behalf of a larger collaboration,

report:

"We are imaging the naked eye GRB 080319B detected by Swift
(GCN 7427) using.both the 1.2m Mercator Telescope at Obs. del
Roque de los Muchachos in La Palma, and the 0.8m IAC80 at
Obs. del Teide in Tenerife. Our R-band magnitude measured on
an image starting at 22:56UT (16.75 hr after the burst) is
about R=21.0. Further images are planned throughout the whole
night."

This message can be cited.

-- 
Martin Jelinek, +420602105255, +34617840945, sirrah.cz/mates
       Instituto de Astrofisica de Andalucia, Granada

# vim:set ai et sts=8 tw=60:


GRB_name: GRB080319B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7470
SUBJECT: GRB 080319B: ROTSE-III Observations of Optical Counterpart
DATE:    08/03/20 01:07:48 GMT
FROM:    Heather Swan at U.of Michigan/ROTSE  <hflewell@umich.edu>

H. Swan (U Mich), F. Yuan (U Mich), W. Rujopakarn (Steward)

ROTSE-IIIb, located at McDonald Observatory, Texas, responded to GRB  
080319B (Swift trigger 306757; Racusin et al., GCN 7427) and began  
imaging at 06:13:11.06 UT  (5.3 sec after the GCN notice time) under  
suboptimal conditions, because of condensation present on the CCD.  
Observations continued until about 5 hours after the trigger.  This  
condensation made the analysis very difficult, but we detect the OT  
first reported in GCN 7428.  Further analysis is ongoing.  These  
unfiltered images are calibrated to the USNO B1.0 R2 catalog.

start UT          end UT          mag        mlim(of image)
06:13:11.06   06:13:16.06    5.35        9.8
06:14:30.66   06:14:50.66    8.49        13.0


GRB_name: GRB080319B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7471
SUBJECT: GRB 080319B : Lulin observation of temporal break at 0.2 days 
DATE:    08/03/20 01:26:15 GMT
FROM:    Yuji Urata at Saitama U  <urata@asiaa.sinica.edu.tw>

Y. Urata, K.Y. Huang, C.Y. Shih, T.W. Chen, M. Im, I. Lee,
on behalf of EAFON report:

"We have monitored the GRB 080319B optical afterglow using Lulin 1-m
telescope with B, V, R, I and z' bands from 16:18 to 21:19 (UT).
Comparing with former observations made by the LOAO (Urata et al. GCN
7435), the R and I band light curves show an apparent temporal break
again at ~0.2 days after the burst. The decay index of the post-break
is ~-0.8."

This message may be cited.


GRB_name: GRB080320A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7472
SUBJECT: GRB 080320: ROTSE-III Optical Limits
DATE:    08/03/20 05:01:51 GMT
FROM:    Fang Yuan at ROTSE  <yuanfang@umich.edu>

F. Yuan (U Mich), E.S. Rykoff (UCSB), W. Rujopakarn (Steward), report on 
behalf of the ROTSE collaboration:

ROTSE-IIIb, located at McDonald Observatory, Texas, responded to GRB 
080320 (Swift trigger 306858), producing images beginning 6.5 s after 
the GCN notice time. An automated response took the first image at 
04:38:10.5 UT, 32.1 s after the burst, under fair conditions. We took 10 
5-sec, 10 20-sec and 20 60-sec exposures. These unfiltered images are 
calibrated relative to USNO A2.0 (R). Imaging is on going.

Comparison to the DSS (second epoch) reveals no new sources within the 
3-sigma Swift/BAT error circle or the XRT error circle, for both single 
images and coadding into sets of 10. Individual images have limiting 
magnitudes ranging from 16.4-17.5; we set the following specific limits.

start UT       end UT      t_exp(s)   mlim   t_start-tGRB(s)  Coadd?
--------------------------------------------------------------------
04:38:10.5   04:38:15.5         5     16.5           32.1       N
04:38:10.4   04:39:17.5        67     18.1           32.0       Y


GRB_name: GRB080320A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7473
SUBJECT: GRB 080320: Swift detection of a burst
DATE:    08/03/20 05:08:16 GMT
FROM:    David Burrows at PSU/Swift  <dxb15@psu.edu>

D. Grupe (PSU), D. N. Burrows (PSU), M. M. Chester (PSU),
N. Gehrels (NASA/GSFC), S. Immler (CRESST/GSFC/UMD),
J. A. Kennea (PSU), C. B. Markwardt (CRESST/GSFC/UMD),
D. M. Palmer (LANL), A. M. Parsons (GSFC), J. L. Racusin (PSU),
M. Stamatikos (NASA/ORAU), T. N. Ukwatta (GSFC/GWU),
D. E. Vanden Berk (PSU) and L. Vetere (PSU) report on behalf of the
Swift Team:

At 04:37:38 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 080320 (trigger=306858).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 177.780, +57.144 which is 
   RA(J2000) = 11h 51m 07s
   Dec(J2000) = +57d 08' 38"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a FRED
structure with a duration of about 25 sec.  The peak count rate
was ~1200 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 04:40:29.4 UT, 171.0 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source with an enhanced position: RA, Dec 177.73502,
57.15776 which is equivalent to:
   RA(J2000)  = 11h 50m 56.41s
   Dec(J2000) = +57d 09' 27.9"
with an uncertainty of 2.5 arcseconds (radius, 90% containment). This
location is 100 arcseconds from the BAT onboard position, within the
BAT error circle. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density consistent with the Galactic value of
1.35e+20 cm^-2 (Kalberla et al. 2005), so we cannot constrain the
redshift at this time using the relation from Grupe et al. (2007). A
summary of the promptly downlinked data is given at
http://www.swift.ac.uk/sper/306858/. 

UVOT took a finding chart exposure of 100 seconds with the White (160-650 nm)
filter starting 177 seconds after the BAT trigger. No afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 25% of
the BAT error circle but does not overlap the XRT error circle. The typical 
3-sigma upper limit has been about 18.5 mag. 
The 8'x8' region for the list of sources generated on-board covers 100% of the
BAT 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
0.01. 

Burst Advocate for this burst is D. Grupe (grupe AT astro.psu.edu). 
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.)


GRB_name: GRB080320A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7474
SUBJECT: GRB 080320 - SDSS Pre-Burst Observations
DATE:    08/03/20 05:24:06 GMT
FROM:    Richard J. Cool at U.of AZ/Steward Obs  <rcool@as.arizona.edu>

Richard J. Cool (Arizona), Daniel J. Eisenstein (Arizona),
David W. Hogg (NYU), Michael R. Blanton (NYU), David J. Schlegel
(LBNL), J. Brinkmann (APO), Donald Q. Lamb (Chicago), Donald
P. Schneider (PSU), and Daniel E. Vanden Berk (PSU) report:

The Sloan Digital Sky Survey (SDSS) imaged the field of burst
GRB080320 prior to the burst.  As these data should be useful
as a pre-burst comparison and for calibrating photometry,
we are supplying the images and photometry measurements for
this GRB field to the community.

Data from the SDSS, including 5 FITS images, 3 JPGS, and
3 files of photometry and astrometry, are being placed at
http://mizar.as.arizona.edu/~grb/public/GRB080320

We supply FITS images in each of the 5 SDSS bands of a 8'x8'
region centered on the GRB position (ra=177.780 (11:51:07.2),
dec=57.1440 (57:08:38.4); Swift-BAT Trigger 306858), as well
as 3 gri color-composite JPGs (with different stretches). The
units in the FITS images are nanomaggies per pixel.  A pixel
is 0.396 arcsec on a side. A nanomaggie is a flux-density unit
equal to 10^-9 of a magnitude 0 source or, to the extent that
SDSS is an AB system, 3.631e-6 Jy.  The FITS images have WCS
astrometric information.

In the file GRB080320_sdss.calstar.dat, we report photometry
and astrometry of 178 bright stars (r<20.5) within 15' of the
burst location.  The magnitudes presented in this file are asinh
magnitudes as are standard in the SDSS (Lupton 1999, AJ, 118,
1406). Beware that some of these stars are not well-detected
in the u-band; use the errors and object flags to monitor
data quality.

In the files GRB080320_sdss.objects_flux.dat and
GRB080320_sdss.objects_magnitudes.dat, we report photometry
of 349 objects detected within 6' of the GRB position.
We have removed saturated objects and objects with model
magnitudes fainter than 23.0 in the r-band.  The fluxes listed
in GRB080320_sdss.objects_flux.dat are in nanomaggies while
the magnitudes listed in GRB080320_sdss.objects_magnitudes.dat
are asinh magnitudes.

All quantities reported are standard SDSS photometry, meaning
that they are very close to AB zeropoints and magnitudes are
quoted in asinh magnitudes.  Photometric zeropoints are known
to about 2% rms.  None of the photometry is corrected for
dust extinction.  The Schlegel, Finkbeiner, and Davis (1998)
predictions for this region are A_U=0.079 mag, A_g=0.058 mag,
A_r = 0.042 mag, A_i=0.032 mag, and A_z=0.023 mag.

The file GRB080320_sdss.spectro.dat contains a list of the
6 objects with SDSS spectroscopy within 6 arcminutes of the
GRB position.  In addition to the redshift and 1-sigma error
for each object, this file also lists the object spectroscopic
classification.


SDSS astrometry is generally better than 0.1 arcsecond per
coordinate.  Users requiring high precision astrometry should
take note that the SDSS astrometric system can differ from
other systems such as those used in other notices; we have
not checked the offsets in this region.

More detailed information pertaining to our SDSS GRB releases
can be found in our initial data release paper (Cool et
al. 2006, PASP 118, 733).  See the SDSS DR4 documentation for
more details: http://www.sdss.org/dr5.

These data have been reduced using a slightly different
pipeline than that used for SDSS public data releases.
We cannot guarantee that the values here will exactly match
those in the data release in which these data are included.
In particular, we expect the photometric calibrations to differ
by of order 0.01 mag.

This note may be cited, but please also cite the SDSS data
release paper, Adelman-McCarthy et al. (2007, ApJS, 172, 634),
when using the data or referring to the technical documentation.


GRB_name: GRB080319C
Detection_method: KAIT
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7475
SUBJECT: GRB 080319C: KAIT OA observations
DATE:    08/03/20 05:43:41 GMT
FROM:    Weidong Li at UC Berkeley KAIT/LOSS  <weidong@astron.berkeley.edu>

W. Li and A. V. Filippenko, University of California, Berkeley,
report on behalf of the KAIT GRB team:

We have analyzed the KAIT observations of the optical afterglow (OA) of GRB
080319C (GCN 7442, GCN 7460) as reported in GCN 7441. Our first 5 s unfiltered
observation started at 12:27:11 UT, 75 s after the BAT trigger. Four subsequent
5 s exposures from t = 81 s to 100 s indicate a smoothly decaying behavior (but
perhaps not power law). After reaching a minimum at t = 180 s (or perhaps a bit
earlier), the OA brightened steeply to a second prominent peak centered at t ~
320 s, after which the OA decayed as an approximate power law, with evidence
for a gradually steepening decay index. Selected photometry, all unfiltered but
calibrated to the R band via USNO B1:

  t_start (s) exp (s)    mag  mag_err

          75    5.0      17.353 0.057 
         100    5.0      17.71  0.062 
         180   20.0      17.95  0.051
         271   20.0      17.322 0.022
         362   20.0      17.32  0.023 
         453   20.0      17.487 0.027
         845   20.0      18.06  0.048 
        1429   20.0      18.866 0.096 


GRB_name: GRB080319B
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7476
SUBJECT: GRB 080319B: second epoch imaging from Canarias (correction to GCN7469)
DATE:    08/03/20 05:47:23 GMT
FROM:    Martin Jelinek at Inst.Astrophys.Andalucia,Granada  <mates@iaa.es>

Martin Jelinek, Alberto J. Castro-Tirado (IAA-CSIC Granada),
Virginie Chantry (Universit de Liege) and
Jorge Pl (IAC La Laguna), on behalf of a larger collaboration,

report:

"We were imaging the naked eye GRB 080319B detected by Swift
(GCN 7427) using.both the 1.2m Mercator Telescope at Obs. del
Roque de los Muchachos in La Palma, and the 0.8m IAC80 at
Obs. del Teide in Tenerife.

Between two epochs of imaging, one started at 22:56 (~16.75hr
after the GRB), the other at 3:27UT (20h after) we measure an
aproximate decay index of ~1.3. Our R-band magnitude measured
on an image starting at 22:56UT (16.75 hr after the burst) was
about R=19.8. The value reported in the previous GCN 7469 has
been incorrect."

This message can be cited.


GRB_name: GRB080319C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7477
SUBJECT: GRB 080319C: Early RAPTOR Observations
DATE:    08/03/20 06:07:34 GMT
FROM:    James Wren at LANL  <jwren@nis.lanl.gov>

J. Wren, W.T. Vestrand, P.R. Wozniak, H. Davis
of Los Alamos National Laboratory report:

Our RAPTOR telescopes responded to Swift trigger 306778
(Pagani et al., GCN 7442) at 12:26:30.66 UTC, 33.70 seconds
after the trigger.  We detect the optical counterpart
initially reported by Li (GCN 7441).  Our measurements are
consistent with those reported by KAIT (GCN 7441 and 7475)
and Super-LOTIS (7443).  Our images became dominated by the
morning twilight at about 12:35 UTC.  The unfiltered
measurements reported in the following table are calibrated
to the USNO-B1 R band.

t-mid(s)    exp(s)     mag     mag-err
-----------------------------------------
47.60       5.0       16.97     0.32
85.27       80.3      17.65     0.18
177.36      61.5      18.22     0.36
228.87      61.1      17.32     0.16
293.28      61.7      17.41     0.20
358.12      62.1      17.13     0.16


GRB_name: GRB080320A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7478
SUBJECT: GRB 080320: optical limit from IAC80
DATE:    08/03/20 06:13:06 GMT
FROM:    Martin Jelinek at Inst.Astrophys.Andalucia,Granada  <mates@iaa.es>

Martin Jelinek, Alberto J. Castro-Tirado (IAA-CSIC Granada),
and Jorge Pl (IAC La Laguna), on behalf of a larger
collaboration,

report:

"We observed the XRT localization of the GRB080320 (Grupe et
al. GCN 7473) with the 0.8m IAC80 at Obs. del Teide in
Tenerife, with exposure mean time 5:33UT (i.e. 1hour after
the GRB). We do not detect any source within or near the XRT
error box down to the limiting magnitude of  R~20.0."

this message may be cited


GRB_name: GRB080320A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7479
SUBJECT: GRB 080320: Enhanced Swift-XRT position
DATE:    08/03/20 09:14:08 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

M.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 995 s of overlapping XRT Photon Counting mode and UVOT
data for GRB 080320, 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 = 177.73526, +57.15746 which is equivalent
to:

RA (J2000): 11h 50m 56.46s
Dec (J2000): +57d 09' 26.8"

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
http://www.swift.ac.uk/xrt_positions/Goad.pdf), the current algorithm is an
extension of this method.

This circular was automatically generated, and is an official product of the
Swift-XRT team.


GRB_name: GRB080320A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7480
SUBJECT: GRB 080320: SDSS source and Gemini-N observations
DATE:    08/03/20 09:51:59 GMT
FROM:    Nial Tanvir at IofA U.Cambridge  <nrt@ast.cam.ac.uk>

N. R. Tanvir, P. T. O'Brien, J. Osborne and P. Evans (U. Leicester) note:

We note here is an SDSS source in the centre of the UVOT enhanced
XRT error circle (GCN 7479).  The source is reported as having r=22.38
and a photometric redshift estimate of z=0.35+/-0.13 according to
the SDSS web site:

 http://cas.sdss.org/dr6/en/tools/explore/obj.asp?id=587731890577605599

A provisional analysis of Gemini-N/GMOS observations obtained about 90
mins post-burst also shows this source (at roughly the same magnitude),
but nothing else in the error circle.

If this is the host, then the photo-z is interestingly low, and the burst
interestingly faint in the optical.

Further analysis is ongoing.


GRB_name: GRB080319B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7481
SUBJECT: GRB 080319B: WSRT Radio Observations
DATE:    08/03/20 10:56:40 GMT
FROM:    Alexander van der Horst at NASA/MSFC  <avdhorst@science.uva.nl>

A.J. van der Horst (NASA/ORAU) reports on behalf of a large collaboration:

"We observed the position of the GRB 080319B afterglow at 4.9 GHz with the
Westerbork Synthesis Radio Telescope at March 19 20.24 UT to March 20
8.22 UT, i.e. 14.0 - 26.0 hours after the burst (GCN 7427).
We do not detect a radio source at the position of the optical counterpart
(GCN 7428). The three-sigma rms noise in the map around that position is
84 microJy per beam. The formal flux measurement for a point source at the
position of the optical counterpart is 59 +/- 26 microJy.

We would like to thank the WSRT staff for rapidly scheduling and obtaining
these observations."


GRB_name: GRB080319B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7482
SUBJECT: Konus-Wind observation of GRB 080319B
DATE:    08/03/20 12:04:43 GMT
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 bright GRB 080319B (Swift-BAT trigger #306757: Racusin et al., GCN 
7427, Cummings et al., GCN 7462) triggered
Konus-Wind at T0=22370.339 s UT (06:12:50.339).

The burst light curve shows a single complex pulse
with a duration of ~60 s, followed by a long decaying tail
seen up to T-T0 ~200 s in the G1(18-70 keV) and G2(70-300 keV) bands
and even beyond in the G1 band.

Preliminary analysis of the Konus-Wind data
yields the burst fluence of 5.72(-0.13, +0.14)x10^-4 erg/cm2,
and a 64-ms peak flux measured from T0+19.2 s
of (2.17 +/- 0.21)x10^-5 erg/cm2/s
(both in the 20 keV - 7 MeV energy range).

The time-integrated spectrum of the main pulse
(from T0 to T0+59.648 s) can be fitted
(in the 25 keV - 7 MeV range)
by GRBM (Band) model for which:
the low-energy photon index is alpha = -0.822(-0.012, +0.014),
the high energy photon index beta = -3.87(-1.09, +0.44),
the peak energy Ep = 651 (-14, +13) keV (chi2 = 96.2/81 dof).

All the quoted errors are at the 90% confidence level.

Assuming z = 0.937 (Vreeswijk et al., GCN 7444, 7451) and a standard
cosmology model with H_0 = 70 km/s/Mpc, Omega_M = 0.3, Omega_\Lambda =
0.7, the isotropic energy release is E_iso ~1.32x10^54 erg,
the maximum luminosity is (L_iso)_max ~9.67x10^52 erg/s, and
Ep_rest ~1261 keV.

The Konus-Wind light curve of this GRB is available
at http://www.ioffe.rssi.ru/LEA/GRBs/GRB080319_T22370/


GRB_name: GRB080319C
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7483
SUBJECT: GRB 080319C, Swift-BAT refined analysis
DATE:    08/03/20 13:57:13 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

M. Stamatikos (GSFC/ORAU), S. D. Barthelmy (GSFC), J. Cummings (GSFC/UMBC),
E. Fenimore (LANL), N. Gehrels (GSFC), H. Krimm (GSFC/USRA),
C. Markwardt (GSFC/UMD), K. McLean (GSFC/UMD), C. Pagani (PSU),
D. Palmer (LANL), A. Parsons (GSFC), T. Sakamoto (GSFC/UMBC),
G. Sato (GSFC/ISAS), J. Tueller (GSFC), T. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using the data set from T-120 to T+88 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 080319C (trigger #306778)
(Pagani, et al., GCN Circ. 7442).  The BAT ground-calculated position is
RA, Dec = 259.006, 55.393 deg which is 
   RA(J2000)  =  17h 16m 01.4s 
   Dec(J2000) = +55d 23' 33.0" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 30%.
 
For the limited event-by-event data we have received on this burst,
the mask-weighted light curve shows 2 (possibly 3) overlapping
FRED-like peaks starting at T-0.5 sec, peaking at T+0.2 sec, and
ending at ~T+50 sec.  The event-by-event data for this m-w lightcurve
ends at T+88 sec.  The on-board raw countrate lightcurve shows
no activity after the T+88 sec limit of the event data, but the sensitivity
is significantly less for this data product.  T90 (15-350 keV) is 34 +- 9 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-0.3 to T+51.2 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.37 +- 0.07.  The fluence in the 15-150 keV band is 3.6 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+0.13 sec in the 15-150 keV band
is 5.2 +- 0.3 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/306778/BA/

If we receive any more data on this burst and it shows any on-going
activity beyond the current data limit of T+88 sec, then we will
issue a revised circular.


