# GCN_circulars

GRB_name: GRB080520A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7754
SUBJECT: GRB 080520: Swift XRT Refined Analysis
DATE:    08/05/21 04:32:15 GMT
FROM:    Dirk Grupe at PSU/Swift-XRT  <grupe@astro.psu.edu>

Dirk Grupe reports on behalf of the Swift-XRT team:


The XRT began observing the field of GRB 080520 (trigger=312047; Grupe 
et al.,
GCN Circ 7753) on 2008-May-20 at 22:22:04.3 UT, 99.5 seconds after
the BAT trigger.


The 0.3-10 keV X-ray light curve of the first two orbits
displays a single decay with a slope alpha=1.04+/-0.07.  

The spectrum of the Photon Counting data of the first two orbits
can be well fitted by an absorbed single powerlaw model with a photon
index Gamma = 2.12 +/- 0.20 and a column density consistent with the 
Galactic
value of 6.48e20 cm-2

If the underlying powerlaw decay continues as is, we predict an XRT 
count rate
of 1e-3 counts/s at T+24 hours or 5e-14 ergs/s/cm2 and at T+48 hours 4e-4
counts/s or 2e-14 ergs/s/cm2.

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


GRB_name: GRB080520A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7755
SUBJECT: GRB 080520: Enhanced Swift-XRT position
DATE:    08/05/21 04:32:43 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 497 s of overlapping XRT Photon Counting mode and UVOT
data for GRB 080520, 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 = 280.19385, -54.99160 which is equivalent
to:

RA (J2000): 18h 40m 46.52s
Dec (J2000): -54d 59' 29.8"

with an uncertainty of 1.9 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, 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: GRB080520A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7756
SUBJECT: GRB 080520, GROND observations
DATE:    08/05/21 06:24:35 GMT
FROM:    Andrea Rossi at TLS Tautenburg  <rossi@tls-tautenburg.de>

This is a multi-part message in MIME format.

--bound1211350827
Content-Type: text/plain
Content-Transfer-Encoding: 7bit

A.Rossi, R. Filgas (Tautenburg), T. Kruehler, J. Greiner (MPE Garching),
S. Klose (Tautenburg), A. Kupcu-Yoldas, A. Yoldas, and
G. Szokoly (Eoetvoes Univ. Budapest and MPE)
report on behalf of the GROND team:

We observed the field of GRB 080520 observed by SWIFT (D. Grupe et al. GCN 7753)  simultaneously in grizJHK with GROND (Greiner et al. 2008, PASP 120, 405) mounted at the 2.2m MPI/ESO telescope at La Silla (Chile).
Observations started at 01:19 UT, about 2.9 hrs after the GRB.
At this time, the GRB location was becoming visible at 20 degrees
above horizon.
Observations were performed at relatively high airmass and under challenging sky conditions with cirrus and a bright moon.

The afterglow candidate detected by UVOT, reported by D.Grupe et al. 
(GCN 7753) is detected in g'r'i'z' J , implying a redshift smaller than 3.5.

We estimate a rough magnitude of i'=21.38 +/-0.4 at 3.25 hrs after the GRB, 
calibrated against USNO-B field stars. We stop observations due to bad sky
conditions.

--bound1211350827--


GRB_name: GRB080520A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7757
SUBJECT: GRB 080520: VLT redshift
DATE:    08/05/21 11:38:56 GMT
FROM:    Pall Jakobsson at U Hertfordshire  <P.Jakobsson@herts.ac.uk>

Pall Jakobsson (U. Hertfordshire), Johan P. U. Fynbo,
Daniele Malesani, Jens Hjorth and Bo Milvang-Jensen
(DARK, NBI) report on behalf of a larger collaboration:

Using FORS2 on the Very Large Telescope, we have obtained
3*30 min spectra (grism 300V) of the optical afterglow of
GRB 080520 (Grupe et al., GCN 7753). The acquisition image
shows it to have R = 23.0 +/- 0.5 on May 21.235 (7.3 hours
post burst).

A firm upper limit of z < 2.4 can be placed on the redshift
of GRB 080520 from the lack of Ly-alpha forest lines in the
spectrum of the afterglow. This is consistent with the GROND
observations (Rossi et al., GCN 7756).

The combined spectrum shows an emission line, presumably
corresponding to [O II] 3727 at z = 1.545. At this redshift
we also find the Mg II doublet (2796,2803) and Mg I (2852).

We thank the Paranal staff for excellent support, especially
Yuri Beletsky and Patricia Guajardo.


GRB_name: GRB080520A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7758
SUBJECT: GRB080520: Swift/UVOT observations
DATE:    08/05/21 13:12:58 GMT
FROM:    Samantha Oates at MSSL  <sro@mssl.ucl.ac.uk>

S.R. Oates (MSSL/UCL) and D. Grupe (PSU) report on behalf of
the Swift/UVOT team

The Swift/UVOT began settled observations of the field of GRB 080520, 105s 
after the BAT trigger (Grupe et al., GCN 7753). We detect the afterglow in 
the white, v filters at the position:

RA(J2000)  =  18:40:46.30
DEC(J2000) = -54:59:31.0

with an estimated uncertainty of 0.5 arcsec (radius, 90% confidence).
This position is consistent with the UVOT enhanced XRT position (Goad et 
al., GCN 7755).

UVOT magnitudes and 3 sigma upper limits are reported below for the single
and coadded images:

Filter    Tstart(s)  Tstop   Expo(s)   Magnitude/3sigUL
-----------------------------------------------------
white       105      204    98       19.59 +/- 0.12
white       858      958    98       20.58 +/- 0.28
v           211      610    400      20.26 +/- 0.38
v           964      1299   330      19.96 +/- 0.45
b           691      6273   216      > 20.92
u           666      6068   197      > 20.60
w1          641      5862   236      > 20.33
m2          617      7079   418      > 20.38
w2          720      6684   216      > 20.25
-----------------------------------------------------

These magnitudes are not corrected for the Galactic extinction
corresponding to a reddening of E{B-V} = 0.08 mag (Schlegel et al.
1998). The photometry is on the UVOT flight system described in Poole
et al. (2008, MNRAS, 383, 627).


GRB_name: GRB080514B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7759
SUBJECT: GRB 080514B: UVOT Observations
DATE:    08/05/21 14:07:20 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/UVOT
team:

     The Swift/UVOT observed the field of GRB 080514B starting 37,005 s
after the SuperAGILE/IPN detection (Rapisarda et al., GCN Circ. 7715).
We detect the optical afterglow in the b, u, uvw1, and uvm2 filters at
the location of the IAC80 optical afterglow (de Ugarte Postigo, et al.,
2008, GCNC 7719).  The UVOT source position is

  RA(J2000) =  21:31:22.71
Dec(J2000) = +00:42:28.4

with an estimated uncertainty of +/-0.60 arcsec (radius, 90%
confidence).

     Magnitudes and upper limits are reported below.

Filter    T_start (s) T_stop  Exposure   Mag    Err  Comment
   v       38,184     43,906      352    >20.1        3-sigma UL
   b       37,449     48,630      559     20.92 0.27
   u       37,229     48,415      559     19.97 0.17
  uvw1     37,005     48,198     1118     20.74 0.24
  uvm2     38,333     44,537     1030     20.83 0.32
  uvw2     37,601     49,441     2199    >22.1        3-sigma UL
white    209,879    228,394     5360    >23.3        3-sigma UL

The above magnitudes and upper limits are not corrected for the
Galactic extinction along the line of sight corresponding to a
reddening of E_{B-V} = 0 .06 mag (Schlegel et al., 1998, ApJS,
500, 525).  The photometry is on the UVOT flight system described
in Poole et al. (2008, MNRAS, 383,627).  The non-detections in
the uvw2 filters may indicate that the redshift is z >~ 1.9.


GRB_name: GRB080514B
Detection_method: IPN Triangulation
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7760
SUBJECT: GRB 080514B: pseudo-z= 1.8 from prompt emission spectrum
DATE:    08/05/21 15:09:41 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 GRB 080514B
provided by Golenetskii et al. (GCNC 7751) to compute
the spectral pseudo-redshift(**) of this burst localized
by SuperAGILE/IPN (Rapisarda et al., GCN 7715).

We find a pseudo-redshift pz= 1.76  0.30

We note that this redshift estimate is consistent with
the observations of the afterglow in B band performed
with the NOT, that may imply a redshift z < 3.7
(Malesani et al., GCNC 7734). This is also consistent
with the observations of the Swift/UVOT (Holland et al.,
GCNC 7759), in which the non-detection of the afterglow
in uvw2 filters may suggest z >~ 1.9

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


GRB_name: GRB080520A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7761
SUBJECT: GRB 080520, Swift-BAT refined analysis
DATE:    08/05/21 17:04:22 GMT
FROM:    Takanori Sakamoto at NASA/GSFC  <takanori.sakamoto-1@nasa.gov>

T. Sakamoto (GSFC/UMBC), S. D. Barthelmy (GSFC), W. Baumgartner (GSFC/UMBC),
J. Cummings (GSFC/UMBC), E. Fenimore (LANL), N. Gehrels (GSFC),
D. Grupe (PSU), H. Krimm (GSFC/USRA), C. Markwardt (GSFC/UMD),
K. McLean (GSFC/UMD), D. Palmer (LANL), 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 080520 (trigger #312047)
(Grupe, et al., GCN Circ. 7753).  The BAT ground-calculated position is
RA, Dec = 280.179, -54.964 deg which is 
   RA(J2000)  =  18h 40m 42.9s 
   Dec(J2000) = -54d 57' 51.2" 
with an uncertainty of 2.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.
 
The mask-weighted light curve shows a single peak starting at T_zero and
ending at ~T+3 sec.  T90 (15-350 keV) is 2.8 +- 0.7 sec (estimated error
including systematics).
 
The time-averaged spectrum from T-0.3 to T+2.8 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.90 +- 0.51.  The fluence in the 15-150 keV band is 5.5 +- 1.4 x 10^-8 erg/cm2.
The 1-sec peak photon flux measured from T-0.31 sec in the 15-150 keV band
is 0.5 +- 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/312047/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 1.88.  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, 679, 570).  


GRB_name: GRB080515A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7762
SUBJECT: GRB 080515: Swift-XRT position and analysis
DATE:    08/05/22 13:58:50 GMT
FROM:    Kim Page at U.of Leicester  <kpa@star.le.ac.uk>

K.L. Page, A.P. Beardmore (U. Leicester) and S.T. Holland 
(CRESST/USRA/GSFC) report on behalf of the Swift-XRT and UVOT teams:

A follow-up observation of GRB 080515 was performed about 1.5 days after 
the initial trigger (Holland et al., GCN Circ. 7721), when the burst was 
no longer Sun-constrained. An X-ray source was identified within the BAT 
ground-calculated error circle (Fenimore et al., GCN Circ. 7726). A 
further observation, 3.5 days later, confirmed that the source is fading, 
with alpha = 1.0 +0.7/-0.5. We therefore believe this is the X-ray 
afterglow of the GRB.

The position of this source is RA, Dec = 3.16343, 32.57894, which is 
equivalent to:

RA(J2000) =   00 12 39.22
Dec(J2000) = +32 34 44.2

with an uncertainty of 3.8 arcsec (radius, 90% containment). This is 54 
arcsec from the BAT position given by Fenimore et al. in GCN Circ. 7726.

A spectrum of the source can be fitted with a power-law of Gamma = 1.95 
+/- 0.34, absorbed by the Galactic column of 4.65x10^20 cm^-2. This 
spectrum, averaged over 1.5-6.6 days after the burst, has an observed 
(unabsorbed) flux of 2.28x10^-13 (2.59x10^-13) erg cm^-2 s^-1.

The field was observed by UVOT with the v filter for 6262 s between 
~1.5 and 2.4 days after the BAT trigger.  The XRT error circle is
located in the scattered light halo of the B = 11.4 star TYC 2264-1051-1, 
so it is not possible to constrain the presence of an afterglow in the 
UVOT data.

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


GRB_name: GRB080516A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7763
SUBJECT: GRB 80516: Swift/UVOT Observations
DATE:    08/05/22 14:57:08 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/UVOT
team:

      The Swift/UVOT began settled observations the field of GRB 080516
starting 81 s after the BAT trigger (Holland et al., GCN Circ. 7733).
We do not detect the GROND optical afterglow reported by Filgas et al.
(2008a, GCN Circ. 7740) in any of the UVOT data.  The ground-based
position of the afterglow is 10.6 arcsec from the USNO-B1.0 star
638-018182, which has a magnitude of B = 12.  The afterglow is located
in the scattered light halo, and in the coincidence loss pattern of
this star, which makes our photometry somewhat uncertain.

      Upper limits from the coadded data are reported below.

Filter    T_start (s) T_stop  Exposure   Mag    Comment
    v           81     41,277    2950   >21.1    3-sigma UL
    b          560     47,700    2243   >22.2    3-sigma UL
    u          536     47,184    4409   >22.3    3-sigma UL
  uvw1         511     46,278    4913   >22.1    3-sigma UL
  uvm2         486     41,915    3648   >22.1    3-sigma UL
  uvw2         576     40,364    2223   >21.8    3-sigma UL

These upper limits are not corrected for the Galactic extinction along
the line of sight to the source corresponding to a reddening of
E_{B-V} = 0.40 mag (Schlegel et al., 1998, ApJS, 500, 525).  The
photometry is on the UVOT flight system described in Poole et
al. (2008, MNRAS, 383,627).


GRB_name: GRB080515A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7765
SUBJECT: GRB 080515: KPNO 4m NIR afterglow detection
DATE:    08/05/23 08:24:31 GMT
FROM:    Adria C. Updike at Clemson U  <aupdike@clemson.edu>

Adria C. Updike, Ginger Bryngelson, and Dieter H. Hartmann (Clemson
University) report on behalf of the Clemson GRB Follow-Up Team:

We observed the field of GRB 080515 (GCN 7721, Holland et al.) twice using
the Kitt Peak 4m telescope + NEWFIRM in the J band under decent weather
conditions.  The first observation was performed 5 hours and 20 minutes
after the burst; the second 29 hours and 20 minutes after the burst.  We
detect a fading source inside the XRT error circle (GCN 7762, Page et al.)
at RA (J2000) = 00:12:39, Dec (J2000) = +32:34:41 (+/- 2 arcsec).  We
therefore conclude that this is the afterglow of GRB 080515.

At 5.33 hours after the burst, the J-band magnitude of the afterglow was
16.4 +/- 0.1 mag (10 minute stack).  29.33 hours after the burst, the
magnitude was at our detection limit near 20.7 mag (20 minute stack).  All
magnitudes were calibrated to the 2MASS catalog.  An image of the
afterglow can be found here
http://www.ces.clemson.edu/~aupdike/GRB080515/080515.jpg .

This message may be cited.


GRB_name: GRB080515A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7766
SUBJECT: GRB 080515: NIR magnitude correction
DATE:    08/05/23 08:39:04 GMT
FROM:    Adria C. Updike at Clemson U  <aupdike@clemson.edu>

Adria C. Updike, Ginger Bryngelson, and Dieter H. Hartmann (Clemson
University) report on behalf of the Clemson GRB Follow-Up Team:

The J-band magnitude at 5.33 days should have read 19.6 +/- 0.1 mag.  We
apologize for the mistake.


GRB_name: GRB080523A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7767
SUBJECT: GRB 080523: Swift detection of a burst
DATE:    08/05/23 21:34:28 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

M. C. Stroh (PSU), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), A. P. Beardmore (U Leicester),
C. Gronwall (PSU), D. Grupe (PSU), S. T. Holland (CRESST/USRA/GSFC),
H. A. Krimm (CRESST/GSFC/USRA), V. Mangano (INAF-IASFPA),
P. T. O'Brien (U Leicester), D. M. Palmer (LANL),
D. Perez (U Leicester), J. L. Racusin (PSU),
M. Stamatikos (NASA/ORAU), T. N. Ukwatta (GSFC/GWU) and
D. E. Vanden Berk (PSU) report on behalf of the Swift Team:

At 21:21:51 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 080523 (trigger=312242).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 20.732, -64.053 which is 
   RA(J2000) = 01h 22m 56s
   Dec(J2000) = -64d 03' 12"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a single peak
with a duration of about 15 sec.  The peak count rate
was ~700 counts/sec (15-350 keV), at ~5 sec after the trigger. 

The XRT began observing the field at 21:23:17.7 UT, 86.4 seconds after
the BAT trigger. XRT found a bright, uncatalogued, fading X-ray source located
at RA, Dec 20.7992, -64.0322 which is equivalent to:
   RA(J2000)  = 01h 23m 11.8s
   Dec(J2000) = -64d 01' 55.9"
with an uncertainty of 5.0 arcseconds (radius, 90% containment). This
location is 129 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 100 seconds with the White (160-650 nm)
filter starting 110 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 typical 3-sigma upper limit has been about 18.5 mag. 
data for the list of sources generated on-board are not available at this time. 
No correction has been made for the expected extinction corresponding to E(B-V)
of 0.03. 

Burst Advocate for this burst is M. C. Stroh (stroh AT astroh.org). 
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: GRB080523A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7768
SUBJECT: GRB 080523: Enhanced Swift-XRT position
DATE:    08/05/24 04:34:35 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 463 s of overlapping XRT Photon Counting mode and UVOT
data for GRB 080523, 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 = 20.79796, -64.03081 which is equivalent
to:

RA (J2000): 01h 23m 11.51s
Dec (J2000): -64d 01' 50.9"

with an uncertainty of 1.5 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, 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: GRB080523A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7769
SUBJECT: Swift/UVOT observations of GRB 080523
DATE:    08/05/24 12:02:56 GMT
FROM:    Paul Kuin at MSSL  <npkuin@googlemail.com>

N. P. M. Kuin (MSSL/UCL), and M. C. Stroh (PSU), report on behalf
of the Swift UVOT team

The Swift UltraViolet/Optical Telescope (UVOT) began observations
of GRB 080523, on May 23, 2008, at  UT,  112 seconds after the initial
Swift BAT trigger (Stroh et al., GCN Circ. 7767). We detect no source
at the enhanced Swift XRT position (Osborne, GCN Circ.7768).

The 3-sigma limiting magnitudes for GRB080523 are given below for
the two initial observations, and for summed observations in each
of the UVOT filters:

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

white    112       211     99.8    > 20.78
v        218       617    399.8    > 19.93

white    112     12001   1211.2    > 21.80
v        218      6037    819.2    > 19.86
uvm2     624      6242    439.2    > 20.15
uvw1     649      6448    439.2    > 20.20
u        673      6649    435.9    > 19.92
b        698     11088   1118.9    > 21.56
uvw2     728     12430    841.6    > 20.77


The values quoted above are on the UVOT Photometric System
(Poole et al, 2008, MNRAS 383,627). They are not corrected for the
expected galactic reddening of E(B-V) = 0.025 in the direction of
the burst (Schlegel et al. 1998).


GRB_name: GRB080523A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7770
SUBJECT: GRB 080523: VLT optical observations
DATE:    08/05/24 14:32:01 GMT
FROM:    Daniele Malesani at Niels Bohr Inst,Dark Cosmology Center  <malesani@astro.ku.dk>

Johan P. U. Fynbo, Daniele Malesani (DARK), Pall Jakobsson (Univ. 
Hertfordshire), Bo Milvang-Jensen and Jens Hjorth (DARK), report on 
behalf of a larger collaboration:

We observed the field of GRB 080523 (Stroh et al., GCN 7767) with the 
ESO VLT equipped with FORS2. Photometric observations were conducted on 
2008 May 24, between 8:14 and 8:27 UT (about 10.9 hr after the GRB). 
Inside the revised XRT error circle (Osborne et al., GCN 7768), we 
detect a faint source at coordinates (J2000):

RA = 01:23:11.61
Dec = -64:01:51.8

Lacking any information on variability, we cannot assess whether this 
source is associated with GRB 080523.

A spectrum of the object shows detection of continuum in the blue down 
to 4200 AA, implying a redshift limit z < 2.5. Further analysis is underway.

We note the presence of two further, faint sources close to, but 
slightly outside of, the refined XRT error circle at (RA, Dec) = 
(01:23:11.21, -64:01:53.9) and (01:23:10.88, -64:01:50.4).

We acknowledge excellent support and positive initative from the ESO 
observing staff, particularly Yuri Beletsky and Patricia Guajardo.


GRB_name: GRB080520A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7771
SUBJECT: GRB 080520: VLT host detection
DATE:    08/05/24 15:19:17 GMT
FROM:    Daniele Malesani at Niels Bohr Inst,Dark Cosmology Center  <malesani@astro.ku.dk>

D. Malesani (DARK), P. Jakobsson (Univ. Hertfordshire), J. P. U. Fynbo, 
J. Hjorth, B. Milvang-Jensen (DARK), report on behalf of a larger 
collaboration:

We further inspected our images and spectra (Jakobsson et al., GCN 7757) 
of the afterglow of GRB 080520 (Grupe et al., GCN 7753). A faint 
extension is visible in our images (seeing 0.7") underlying the 
afterglow emission, which may be due to a relatively bright host galaxy. 
This is consistent with the 2D trace of the spectrum, which reveals the 
proposed [O II] line to be also spatially extended.

Using the relations by Kennicutt (1998, ARA&A, 36, 189), the flux of the 
[O II] line (not corrected for extinction) corresponds to a star 
formation rate (SFR) of approximately 15 M_Sun/yr.


GRB_name: GRB080523A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7772
SUBJECT: GRB 080523, Swift-BAT refined analysis
DATE:    08/05/24 21:16:50 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

D. Palmer (LANL), S. D. Barthelmy (GSFC), W. Baumgartner (GSFC/UMBC),
J. Cummings (GSFC/UMBC), E. Fenimore (LANL), N. Gehrels (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),
M. C. Stroh (PSU), 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 080523 (trigger #312242)
(Stroh, et al., GCN Circ. 7767).  The BAT ground-calculated position is
RA, Dec = 20.769, -64.060 deg, which is 
   RA(J2000)  =  01h 23m 04.4s 
   Dec(J2000) = -64d 03' 36.0" 
with an uncertainty of 1.7 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.
 
The mask-weighted light curve shows a FRED-like peak starting at ~T-10 sec,
peaking at ~T+4, and ending at ~T+80 sec.  There is a weak second peak
starting,ending at 80,110 sec, respectively.  T90 (15-350 keV) is
102 +- 15 sec (estimated error including systematics).
 
The time-averaged spectrum from T-6.1 to T+111.9 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.65 +- 0.18.  The fluence in the 15-150 keV band is 8.8 +- 1.0 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+3.89 sec in the 15-150 keV band
is 0.5 +- 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/312242/BA/
 
This burst satisfies Sakamoto/Ukwatta Swift-BAT possible high-z criteria
(Ukwatta et al. arXiv:0802.3815).
1) Power Law photon index = 1.65     (PL photon index < 2)
2) 1-s peak photon flux   = 0.51     (1-s peak photon flux < 1.0 ph/cm2/s)
3) Light curve variance   = 1.2e-05  (Variance < 0.0001)
4) T90/(Peak photon flux) = 201      (T90/(Peak photon flux) > 100)
Based on a limited sample of bursts, these criteria yield an 85% chance
it has a redshift greater than 3.5. 


GRB_name: GRB080523A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7773
SUBJECT: GRB 080523: Swift-XRT refined analysis
DATE:    08/05/24 22:00:24 GMT
FROM:    Michael Stroh at PSU/Swift  <stroh@astroh.org>

M. C. Stroh and D. Grupe (PSU) report on behalf of the Swift-XRT Team:

We have analyzed the first eight orbits of Swift-XRT data obtained for  
GRB 080523 (Stroh et al. GCN Circ. 7767), totaling 250 s of Windowed  
Timing (WT) data and 11.8ks of Photon Counting (PC) data.

The light curve can be described as a single broken power-law with an  
initial decay index of 2.17 +/- 0.04 followed by a shallower decay  
index of 0.56 +/- 0.27 with a break at T+3.5ks. We predict a count  
rate at T+48 hours of 3.2e-3 cts/s.

The WT data (93 - 343 seconds) can be modeled as an absorbed power law  
with photon index of 2.17 +/- 0.04 and a total absorbing column  
density that is consistent with the Galactic value of 2.1e20 cm^-2.  
The 0.3-10 keV absorbed (unabsorbed) flux during this time is 4.58e-10  
(4.99e-10) erg cm^-2 s^-1.

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


GRB_name: GRB080524A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7774
SUBJECT: GRB 080524: Swift-BAT detection of a burst in ground analysis
DATE:    08/05/25 19:41:39 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <jayc@milkyway.gsfc.nasa.gov>

G. Sato (GSFC/ISAS), L. Barbier (GSFC), S. Barthelmy (GSFC),
W. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
E. Fenimore (LANL), N. Gehrels (GSFC), D. Grupe (PSU),
D. Hullinger (BYU-Idaho), H. Krimm (GSFC/USRA), M. Koss (GSFC/UMD),
C. Markwardt (GSFC/UMD), D. Palmer (LANL), A. Parsons (GSFC),
T. Sakamoto (GSFC/ORAU), M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC),
on behalf of the Swift-BAT team:


At 04:13:00 UT on May 24, 2008, BAT triggered on GRB 080524. The onboard
processing found a source that was not significant enough to initiate a
burst response. Routine processing on the ground of failed triggers found
a significant source (9.7 sigma) at RA, Dec 268.449, +80.143 which is:

RA 17h 53m 47.7s (J2000)
Dec 80d 8m 35s (J2000)

with an uncertainty radius of 2.5 arcmin (90% containment). The source
was 58% coded.

T90 was 9 +- 2 sec. The peak count rate was 600 counts/sec (15-350 keV).
Using the data set from T-2 to T+8 sec, the mask-weighted light curve
shows a single roughly symmetrical peak.

The power-law index of the time averages spectrum is 1.1 +- 0.2. The
fluence in the 15-150 keV range from T-2 to T+8 sec was
(2.9 +- 0.5) x 10-07 ergs/cm2. The 1-sec peak flux was 0.4 +- 0.2
counts/cm2/sec. All uncertainties are 90% confidence.

Swift is executing a TOO to the position of this burst, and preliminary
XRT and UVOT results should be available in a few hours.


GRB_name: GRB080503A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7775
SUBJECT: GRB 080503: 2nd Epoch Chandra X-ray Observations
DATE:    08/05/26 23:50:35 GMT
FROM:    Nat Butler at MIT/CSR  <nrbutler@space.mit.edu>

N. R. Butler (UC Berkeley), J. S. Bloom (UCB), W. Li (UCB), A. J. Levan (U.
Warwick), D. A. Perley (UCB),  N. R. Tanvir (U. Leicester), H-W. Chen (U.
Chicago), R. Chornock (UCB), J. X. Prochaska (UCO/Lick), C. D. Bailyn (Yale),
A. Bunker (U. Exeter), B. Cobb (Yale), P. B. Hall (York U.), A. V. Filippenko
(UCB), N. Gehrels (NASA/GSFC), D. Burrows (PSU), K. Glazebrook (Swinburne),
J. Granot (U. Hertfordshire), K. C. Hurley (UCB), D. Kocevski (UCB), B.
Metzger (UCB), M. Modjaz (UCB), A. Miller (UCB), W.  Lee (I. de Astronomia),
S. Lopez (U. Chile), J. Norris (NASA/Ames), P. E.  Nugent (LBNL), M. Pettini
(U. Cambridge), D. Poznanski (UCB), A. L. Piro (UCB), E. Quataert (UCB), E.
Ramirez-Ruiz (UCSC), J. Shiode (UCB), and T.  Sakamoto (GSFC/UMBC) report:

From 2008/05/25 18:11:36 UT to 2008/05/26 03:04:28 UT (22.24 - 22.61 days post
burst), Chandra Director's Discretionary Time observations with ACIS-S were
conducted of the field of GRB 080503 (e.g., Mao et al. 2008; GCN 7665) for a
total exposure of 29.8 ksec (livetime).  In a 3-pixel radius source extraction
region centered around the first epoch Chandra source (Butler et al. 2008;
GCN 7704), we find no source counts in the 0.5-8.0 keV band.

We derive a 2-sigma upper limit to the source flux of Fx(0.3-10 keV) < 9.9 x
10^(-16) erg/cm^2/s.  Relative to the first epoch flux ~18 days earlier,
the 2nd epoch flux implies a fade steeper in time than t^(-1.6).  A similarly
steep or steeper fade is implied in the optical band from Gemini and HST
observations of this source (Perley et al. 2008; GCNs 7667, 7678, 7679, 7680,
7695, 7703, 7749).  Combined with a rough agreement in the extrapolated flux
levels assuming a GRB afterglow external shock model (e.g., GCN 7704), the
lightcurve similarity supports an interpretation where the external shock is
responsible for both the X-ray and optical emission.

More detailed analyses are ongoing.

We thank Harvey Tananbaum and the Chandra observatory staff for their
impressive rapid scheduling and execution of this observation.

This message can be cited.


GRB_name: GRB080524A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7776
SUBJECT: GRB 080524: Swift XRT and UVOT analysis
DATE:    08/05/28 19:35:41 GMT
FROM:    Dirk Grupe at PSU/Swift-XRT  <grupe@astro.psu.edu>

Dirk Grupe (PSU), Paul Kuin (MSSL), Jay Cummings (GSFC), and Kim Page (U
Leicester) report of behalf of the Swift team:


Swift observed the field of GRB 080524 (Sato et al., GCN Circ. 7774) as 
a Target
of Opportunity for 10 ks starting on 2008-05-25 at 16:43:45 UT, 36h 30m 
after
the burst. The exposures in XRT and UVOT V were 8.9 and 9.7 ks, 
respectively.
Within the 2.5' BAT error circle no new source was found. In XRT the 3sigma
upper limit is in the 0.5-8.0 keV band is 1.1e-3 counts/s which converts to
roughly 4.7e-14 ergs/s/cm2 in the 0.3-10.0 keV band assuming an
absorbed power law model with Galactic NH (5.19e20 cm-2) and a canonical 
X-ray
Photon index Gamma=2.0.
The 3sigma upper limit in the UVOT V-Filter is 20.0 mag.

No further Swift observations are planned for this GRB.

 This circular is an official product of the Swift team.


GRB_name: GRB080523A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7779
SUBJECT: GRB 080523: afterglow confirmation and redshift constraints
DATE:    08/05/29 18:22:30 GMT
FROM:    Daniele Malesani at Niels Bohr Inst,Dark Cosmology Center  <malesani@astro.ku.dk>

D. Malesani, J. P. U. Fynbo (DARK/NBI), A. de Ugarte Postigo (ESO), P. 
Jakobsson (Univ. Hertfordshire), J. Hjorth, B. Milvang-Jensen 
(DARK/NBI), report on behalf of a larger collaboration:

We observed again the field of GRB 080523 (Stroh et al., GCN 7767) with 
the ESO VLT equipped with the FORS2 camera. Observations were carried 
out on 2008 May 28, at mean time 9:35 UT (4.5 days after the GRB) in the 
R band.

The optical source identified by Fynbo et al. (GCN 7770) has clearly 
faded since our previous observation by at least 1.5 mag. This confirms 
that the object is the afterglow of GRB 080523. The refined coordinates 
(J2000, against USNO-B1.0) are

RA = 01:23:11.56
Dec = -64:01:51.59

Residual, marginally significant emission is still detected close to the 
afterglow position. It is unclear whether this is related to the GRB.

A finding chart showing the field in the two epochs is posted at

http://www.astro.ku.dk/~malesani/GRB/080523/080523_finder.jpg

Close inspection of our spectra (Fynbo et al., GCN 7770) fails to reveal 
any convincing absorption or emission feature. The object has a blue 
continuum, and flux is detected down to ~4070 AA. A conservative limit 
to the redshift is set by the absence of Lyman-alpha forest redward of 
~4900 AA, which implies z < 3. This limit rules out a high redshift as 
suggested by the burst gamma-ray properties (Palmer et al., GCN 7772).

We acknowledge significant support from the ESO staff at Paranal, 
particularly Linda Schmidtobreick.


GRB_name: GRB080602A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7781
SUBJECT: GRB 080602: Swift detection of a burst
DATE:    08/06/02 01:41:09 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

A. P. Beardmore (U Leicester), S. D. Barthelmy (GSFC),
J. R. Cummings (NASA/UMBC), N. Gehrels (NASA/GSFC),
S. T. Holland (CRESST/USRA/GSFC), E. A. Hoversten (PSU),
J. A. Kennea (PSU), C. B. Markwardt (CRESST/GSFC/UMD),
F. E. Marshall (NASA/GSFC), K. M. McLean (GSFC/UMD),
K. L. Page (U Leicester), D. M. Palmer (LANL) and
T. N. Ukwatta (GSFC/GWU) report on behalf of the Swift Team:

At 01:30:28 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 080602 (trigger=312958).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 19.173, -9.251 which is 
   RA(J2000) = 01h 16m 41s
   Dec(J2000) = -09d 15' 02"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed two well-separated
peaks with a total duration of about 70 sec.  The peak count rate
was ~3000 counts/sec (15-350 keV), at ~60 sec after the trigger. 

The XRT began observing the field at 01:32:19.7 UT, 111.6 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 19.1766, -9.2336 which is equivalent to:
   RA(J2000)  = 01h 16m 42.3s
   Dec(J2000) = -09d 14' 00.9"
with an uncertainty of 5.8 arcseconds (radius, 90% containment). This
location is 63 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 123 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 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 0.03. 




Burst Advocate for this burst is A. P. Beardmore (apb 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: GRB080602A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7782
SUBJECT: GRB 080602: Enhanced Swift-XRT position
DATE:    08/06/02 05:50:40 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 16 s of overlapping XRT Photon Counting mode and UVOT
data for GRB 080602, 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 = 19.17563, -9.23212 which is equivalent
to:

RA (J2000): 01h 16m 42.15s
Dec (J2000): -09d 13' 55.6"

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), 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: GRB080602A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7783
SUBJECT: GRB 080602: NOT R-band upper limit
DATE:    08/06/02 08:31:42 GMT
FROM:    Johan U. Fynbo at U.Copenhagen  <jfynbo@astro.ku.dk>

Daniele Malesani (DARK/NBI), Pierre-Olivier Quirion (Univ. AArhus), and
Johan Peter Uldall Fynbo (DARK/NBI), Pll Jakobsson (Univ. Hertfordshire)
report on behalf of a larger collaboration:

We observed the field of GRB 080602 (Beardmore et al., GCN 7781) with the
NOT telescope. Observations were carried out in the R band at high airmass
(~6) and close to twilight. Mean time was June 2.203 UT, 3.4 hr after the
trigger. Inside the refined XRT error circle (Beardmore et al., GCN 7782),
we do not detect any source down to a limiting magnitude R=22.3.
Observations will be attempted with the VLT on Cerro Paranal, but due to
weather the outlook for data is bad. We encourage observations from other
sites.


GRB_name: GRB080602A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7784
SUBJECT: Konus-Wind observation of GRB 080602
DATE:    08/06/02 16:44:25 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 second, most intense pulse of the GRB 080602 (Swift-BAT trigger 
#312958: Beardmore et al., GCN 7781) triggered Konus-Wind
at T0=5486.229 s UT (01:31:26.229).

As observed by Konus-Wind the burst
had a fluence of 7.92(-1.45, +1.47)x10^-6 erg/cm2,
and a 256-ms peak flux measured from T0+1.280 s
of (1.92 +/- 0.58)x10^-6 erg/cm2/s
(both in the 20 keV - 1 MeV energy range).

The spectrum of the most intense part
(from T0 to T0+8.448 s) is well fitted (in the 20 keV-1 MeV range)
by a simple power law with the photon index of 1.48(-0.17, +0.18) (chi2 
= 39.7/53 dof). We note that because of the derived photon index is <2,
the fluence is very sensitive to the upper boundary of the energy range.
Fitting by a power law with exponential cutoff model:
dN/dE ~ (E^-alpha)*exp(-E*(2-alpha)/Ep)
yields alpha = 0.96(-0.76, +0.52),
and only a lower limit on the peak energy: Ep > 226 keV
(chi2 = 36.6/52 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/GRB080602_T05486/


GRB_name: GRB080602A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7785
SUBJECT: GRB 080602: Swift-XRT refined analysis
DATE:    08/06/02 20:03:58 GMT
FROM:    Andy Beardmore at U Leicester  <apb@star.le.ac.uk>

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

The Swift-XRT observed GRB 080602 (trigger 312958, Beardmore et
al. GCN 7781) for one orbit which consisted of 71 s of Windowed
Timing mode data starting 118 s after the trigger and 1.23 ks  of
Photon Counting mode data, 193 s after the trigger.

Using 930 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 = 19.17574, -9.23207 which is equivalent to:

RA (J2000): 01 16 42.18
Dec (J2000): -09 13 55.4

with an uncertainty of 1.7 arcsec (radius, 90% confidence). The position 
is 6.3 arcsec from the on-board position reported in GCN 7781 and 0.4 
arcsec from the initial refined XRT position reported in GCN 7782.

At first, the X-ray light curve shows signs of a steep decay with a slope 
of 4.7 +2.1/-0.9, breaking to a shallower decay of 0.21 +/- 0.16 at 
a time of 145 +11/-6 s after the trigger. This is followed by a further 
steepening  to a slope of 0.76 +0.41/-0.23 at a time of 561 +276/-201 s.

A spectrum of the Windowed Timing data can be well fit by an absorbed
power-law, with a photon index Gamma = 1.63 +/- 0.21 and a column
density Nh = (1.0 +/- 0.5) e21 cm^-2, compared with the Galactic
column density in this direction of 3.5e20 cm^-2. The observed
(unabsorbed) 0.3-10 keV flux is 3.13e-10 (3.61e-10) erg cm^-2 s^-1.

The Photon Counting mode spectrum is also well fit by an absorbed
powerlaw, with Nh = (2.1 +/- 0.4) e21 cm^-2 and Gamma = 2.12 +/- 0.15.
The observed (unabsorbed) 0.3-10 keV flux is 1.66 e-10 (2.59e-10)
erg cm^-2 s^-1.  The observed count to flux conversion factor for this
data is 3.5e-11 erg cm^-2 count^-1.

Due to the limited XRT data available, no count rate prediction at T+1 day
has been made. No further observations with Swift are planned.

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


GRB_name: GRB080602A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7786
SUBJECT: GRB 080602, Swift-BAT refined analysis
DATE:    08/06/02 22:31:48 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

G. Sato (GSFC/ISAS), S. D. Barthelmy (GSFC), W. Baumgartner (GSFC/UMBC),
A. P. Beardmore (U Leicester), 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), 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-296 to T+302 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 080602 (trigger #312958)
(Beardmore, et al., GCN Circ. 7781).  The BAT ground-calculated position is
RA, Dec = 19.177, -9.239 deg, which is 
   RA(J2000)  =  01h 16m 42.6s 
   Dec(J2000) = -09d 14' 19.8" 
with an uncertainty of 1.7 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 19%.
 
The mask-weighted light curve shows 4 or 5 peaks, the first starting at ~T-25 sec,
the second at ~T-15 sec, the 3rd at ~T-5 sec, peaking at ~T+1 sec and 
ending at ~T+15 sec; the 4th starts at ~T+55 sec and ends at ~T+65 sec.
T90 (15-350 keV) is 74 +- 7 sec (estimated error including systematics).
 
The time-averaged spectrum from T-11.5 to T+69.3 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.43 +- 0.13.  The fluence in the 15-150 keV band is 3.2 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+59.60 sec in the 15-150 keV band
is 2.9 +- 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/312958/BA/


GRB_name: GRB080603A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7788
SUBJECT: Possible GRB080603: Faulkes Telescope North optical afterglow candidate
DATE:    08/06/03 12:01:54 GMT
FROM:    Andreja Gomboc at LT,ARI,Liverpool JMU  <ag@astro.livjm.ac.uk>

A. Gomboc (U. Ljubljana), I.A. Steele (Liverpool JMU), E. Rol, P. O'Brien 
(U. Leicester), A, Melandri, D. Bersier, C.G. Mundell, R.J. Smith, D. 
Carter, S. 
Kobayashi, M. Burgdorf, M. Bode (Liverpool JMU), C. Guidorzi (INAF-OAB), 
N. Bannister, N. Tanvir 
(U. Leicester) report:

The 2-m Faulkes Telescope North (Hawaii) automatically reacted to the 
INTEGRAL trigger 5283 and possible GRB 080603 and started observing the 
field at 1.3 min after the trigger.

We detect an optical afterglow candidate at:
RA 18:37:38.1,
dec +62:44:39.4.

We estimate the magnitude of the source (calibrated to USNO-B1.0 
catalogue) to be I=20.3+-0.3 at t_0+5.93 min and R=19.6+-0.3 at t_0+7.37 min.


GRB_name: GRB080603A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7789
SUBJECT: GRB 080603 OA candidate
DATE:    08/06/03 12:02:13 GMT
FROM:    Ryan Chornock at UC Berkeley  <chornock@astro.berkeley.edu>

R. Chornock, D. Perley, W. Li, and A. V. Filippenko (UC Berkeley) report that:

The Katzman Automatic Imaging Telescope (KAIT) at Lick Observatory slewed to the 
position of GRB 080603 and detected a new source not present in the DSS at 
coordinates:
(J2000)  18:37:38.06  +62:44:39.3

The new source was first detected in a 60s image starting at 11:28:55 UT and is 
near magnitude 18.7 in unfiltered and I band images.


GRB_name: GRB080603A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7790
SUBJECT: GRB 080603: A long GRB detected by INTEGRAL
DATE:    08/06/03 13:04:48 GMT
FROM:    Sandro Mereghetti at IASF/CNR  <sandro@iasf-milano.inaf.it>

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

A GRB lasting about 180 s has been detected by IBAS in IBIS/ISGRI data at 
11:18:11 UT of June 3. The coordinates (J2000)  are:

 RA:  279.409 [degrees]
 DEC: +62.735 [degrees]

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

A preliminary analysis gives a peak flux in the 20-200 keV range of about 
0.5 ph/cmq/s (1-s integration time) and a fluence over the same energy 
range of about 10e-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: GRB080603A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7791
SUBJECT: GRB 080603: Gemini-North redshift
DATE:    08/06/03 15:29:48 GMT
FROM:    Daniel Perley at U.C. Berkeley  <dperley@astro.berkeley.edu>

D. A. Perley, J. S. Bloom (UC Berkeley), and J. X. Prochaska (UCO/Lick) 
report on behalf of a larger collaboration:

Following the KAIT detection (Chornock et al., GCN 7789) of the 
afterglow candidate of GRB 080603 (Paizis et al., GCN 7790; Gomboc et 
al., GCN 7788) we began a spectroscopic sequence at Gemini-North using 
GMOS.  We acquired 2x1200s longslit exposures starting at UT 13:24.  We 
detect very strong resonance lines of MgII and FeII and the 
fine-structure transitions of FeII which establish the redshift of the 
GRB to be z=1.6880.  In addition, we identify intervening MgII 
absorption systems at z=1.5635 (90% c.l.) and z=1.271 (100% c.l.)

In addition, in a single acquisition exposure starting at UT 13:05:05 
(107 minutes after the trigger) the object has a magnitude (relative to 
USNO B1.0) of R~19.7, suggesting it has not faded significantly since 
the observations of Gomboc et al. (GCN 7788).

We thank Richard McDermid and the Gemini staff and for support.


GRB_name: GRB080603B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7792
SUBJECT: GRB 080603B: ROTSE-III Detection of Optical Counterpart
DATE:    08/06/03 19:55:01 GMT
FROM:    Wiphu Rujopakarn at U AZ/Steward  <wiphu@as.arizona.edu>

W. Rujopakarn (Steward), T. Guver (U Arizona), D.A. Smith (Guilford),
report on behalf of the ROTSE collaboration:

ROTSE-IIId, located at the Turkish National Observatory at Bakirlitepe,
Turkey, responded to GRB 080603B (Swift trigger 313087). The first image
was at 19:38:36.2 UT, 22.9 s after the burst (8.3 s after the GCN notice
time). The unfiltered images are calibrated relative to USNO A2.0. We
detect a new, rapidly fading object, not visible in the DSS (second
epoch), with coordinates:

     11:46:07.8      +68:03:39.9    (J2000), with positional uncertainty
of 1" or better

start UT     mag     mlim(of image)
----------------------------------
19:38:36.2     14.1     14.9

A jpeg image is available at
http://www.rotse.net/images/gsb313087_3d00_img.jpg (OT circled in yellow
and blue)

[GCN OPS NOTE(03jun08): Per author's request, the "B" was added to the 
GRB name.]


GRB_name: GRB080603A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7793
SUBJECT: GRB080603: Super-LOTIS detection of Optical Counterpart
DATE:    08/06/03 19:58:42 GMT
FROM:    Peter A. Milne at Super-LOTIS  <pmilne@as.arizona.edu>

P.A. Milne (U Arizona) and A. Updike (Clemson U) report on behalf of the
Super-LOTIS team:

The 0.6m Super-LOTIS telescope began R-band observations of the error
region of GRB080603 at 11:19:04 UT.  The OT detected by Gomboc et al.
(GCN 7788) and Chornock et al. (GCN 7789) is not
apparent in the initial images, but is clearly visible in
subsequent images. Using a stack of 10 x 60sec images obtained between
11:22:44 -> 11:33:46, we estimate the magnitude of the source to be
R=19.3 +/- 0.3.

We used the USNO-B star at RA=18:37:55, Dec=+62:44:32 to derive the
R2 magnitude.

Analysis continues to better characterize the rise of the emission from
the OT.

This message can be cited.


GRB_name: GRB080603B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7794
SUBJECT: GRB 080603B: Swift detection of a burst with optical afterglow
DATE:    08/06/03 19:59:18 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

V. Mangano (INAF-IASFPA), S. D. Barthelmy (GSFC),
A. P. Beardmore (U Leicester), P. J. Brown (PSU),
G. Cusumano (INAF-IASFPA), N. Gehrels (NASA/GSFC),
C. Guidorzi (INAF-OAB), S. T. Holland (CRESST/USRA/GSFC),
J. A. Kennea (PSU), H. A. Krimm (CRESST/GSFC/USRA),
N. P. M. Kuin (MSSL), C. B. Markwardt (CRESST/GSFC/UMD),
F. E. Marshall (NASA/GSFC), K. M. McLean (GSFC/UMD),
P. T. O'Brien (U Leicester), C. Pagani (PSU), D. M. Palmer (LANL),
A. M. Parsons (GSFC), J. L. Racusin (PSU), T. Sakamoto (NASA/UMBC),
B. Sbarufatti (INAF-IASFPA), M. Stamatikos (NASA/ORAU),
T. N. Ukwatta (GSFC/GWU), D. E. Vanden Berk (PSU) and
H. Ziaeepour (UCL-MSSL) report on behalf of the Swift Team:

At 19:38:13 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 080603B (trigger=313087).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 176.528, +68.076 which is 
   RA(J2000)  =  11h 46m 07s
   Dec(J2000) = +68d 04' 33"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows three main peaks
with a duration of about 70 sec.  The peak count rate
was ~8000 counts/sec (15-350 keV), at ~2 sec after the trigger. 

The XRT began observing the field at 19:39:55 UT. XRT found a bright, 
uncatalogued X-ray source located at:
   RA(J2000)  = 11h 46m 07.7s
   Dec(J2000) = +68d 03' 35.2"
with an uncertainty of 4.7 arcseconds (radius, 90% containment). 

UVOT took a finding chart exposure of nominal 100 seconds with the White
(160-650 nm) filter starting 72 seconds after the BAT trigger. There is a
candidate afterglow in the list of sources generated on-board at
  RA(J2000)  = 11:46:07.70 = 176.5321
  DEC(J2000) = +68:03:40.0  =  68.0611
with a 1-sigma error radius of about 0.5 arc sec. This position is 4.9 arc sec. 
from the center of the XRT error circle. The estimated magnitude is 15.9 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 0.01. 

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


GRB_name: GRB080603B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7795
SUBJECT: GRB 080603B: TAROT Calern observatory detection of a plateau in the light curve
DATE:    08/06/03 21:54:31 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 080603 detected by SWIFT
(trigger 313087) with the TAROT robotic telescope (D=25cm)
located at the Calern observatory, France.

The observations started 62 min after the GRB trigger
(burst occured at the sunset). The elevation of the field
decreased from from 63 degrees above horizon and weather
conditions were good.

We detected the candidate couterpart mentioned by
Rujopakarn et al. (GCNC 7792). We note that the afterglow
stays at about the same magnitude between 68 to 109
minutes. Magnitudes derived from two R filtered images are:

t0+68 min  to t0+ 71 min R=17.4
t0+106 min to t0+109 min R=17.5

The afterglow seems to exhibit a plateau phase
in its optical light curve. We continue the follow-up.

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

This message may be cited.


GRB_name: GRB080603B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7796
SUBJECT: GRB 080603B: BOOTES2/TELMA  optical observations
DATE:    08/06/03 22:44:26 GMT
FROM:    Alberto Castro-Tirado at Inst.de Astro. de Andalucia  <ajct@iaa.es>

A. J. Castro-Tirado, M. Jelinek, J. Gorosabel (IAA-CSIC Granada), P.
Kubnek (GACE, U. Valencia), S. Vitek (CVUT Praha), A. de Ugarte Postigo
(ESO Santiago), R. Cunniffe (Cork Univ.), R. Fernndez-Muoz (EELM-CSIC
La Mayora), P. Martn-Almendros (Fundacin Mlaga) and L. Sabau-Graziati
(INTA Madrid), report:

"We are observing the field of GRB 080603B (Mangano et al. GCN 7794)
with the recently installed 60cm robotic telescope BOOTES-2/TELMA in
Mlaga (south Spain). The first observations (120s each, with the
r'-band filter) were obtained starting at 20:31 UT (i.e. 51 min after
the onset of the event). We detect the optical afterglow (Rujopakarn et
al. GCN 7792, Mangano et al.) with 17.3 mag, based on a preliminary
calibration using USNO-A2.0. We also confirm the early plateau phase
reported by Klotz et al.(GCNC 7795). From our last frame taken at 22:30
UT we derive a 0.3 mag decay. Further images (in g'r'i'Z filters) are
on their way. Spectroscopic observations are encouraged."

This message can be quoted.


GRB_name: GRB080603B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7797
SUBJECT: GRB080603B: NOT redshift
DATE:    08/06/03 23:00:16 GMT
FROM:    Johan U. Fynbo at U.Copenhagen  <jfynbo@astro.ku.dk>

Johan Fynbo (DARK/NBI), Pierre-Olivier Quirion (Univ. Aarhus), Dong Xu,
Daniele Malesani, C. C. Thoene, J. Hjorth, B. Milvang-Jensen (DARK/NBI),
and Pall Jakobsson (Univ. Hertfordshire) report on behalf of a larger
collaboration:

We observed the field of GRB 080603B (Mangano et al., GCN 7794) with the
NOT telescope. We obtained R-band imaging and a low resolution
spectrum using the AlFOSC instrument. Based on the detection of
Lyman-alpha and a number of relatively strong metal lines we infer a
redshift of 2.69.

[GCN OPS NOTE(04jun08): Per author's request, a "B" was added in the Subject.
And Dong Xu was added to the author list.]


GRB_name: GRB080516A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7798
SUBJECT: GRB 080516: TAROT La Silla observatory optical observations
DATE:    08/06/03 23:32:33 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 080516 detected by SWIFT
(trigger 311762) with the TAROT robotic telescope (D=25cm)
located at the European Southern Observatory,
La Silla observatory, Chile.

The observations started 64.6s after the GRB trigger
(49.9s after the notice). The elevation of the field decreased
from 48 degrees above horizon and weather conditions
were excellents.

The date of trigger : t0 = 2008-05-16T00:17:07.296

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 the OT noticed by Filgas et al.
(GCNC 7740) with a limiting magnitude of:

t0+64.6s to t0+124.6s : R > 13.5
(the poor detectivity is due to the 10 magnitude
close star).

The second image is 30.0s exposure in tracking mode:

t0+131.0s to t0+161.0s : R > 15
(we substracted an image taken at t0+20 min to
minimize the effect of the 10 magnitude close star).

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

N.B. Galactic coordinates are lon=244.1279 lat= +2.4429
and the galactic extinction in R band is 1.1 magnitude
estimated from D. Schlegel et al. 1998ApJ...500..525S.

This message may be cited.


GRB_name: GRB080603B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7799
SUBJECT: GRB 080603B: TAROT Calern observatory confirmation of slow optical decay
DATE:    08/06/04 00:41:39 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 080603B from
68 min to 240 min after the trigger with TAROT.
The light curve displays a slow optical
decay compatible with alpha=0.62 +/- 0.1.
R~18.2 at t0+225 min.


GRB_name: GRB080604A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7800
SUBJECT: GRB 080604: Swift detection of a burst with an optical afterglow
DATE:    08/06/04 07:38:24 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

V. La Parola (INAF-IASFPA), P. A. Evans (U Leicester),
N. Gehrels (NASA/GSFC), C. Guidorzi (INAF-OAB),
S. T. Holland (CRESST/USRA/GSFC), N. P. M. Kuin (MSSL),
J. Mao (INAF-OAB), P. T. O'Brien (U Leicester),
K. L. Page (U Leicester), D. M. Palmer (LANL),
D. Perez (U Leicester), B. Sbarufatti (INAF-IASFPA),
R. L. C. Starling (U Leicester), D. E. Vanden Berk (PSU) and
H. Ziaeepour (UCL-MSSL) report on behalf of the Swift Team:

At 07:27:01 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 080604 (trigger=313116).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 236.970, +20.555 which is 
   RA(J2000) = 15h 47m 53s
   Dec(J2000) = +20d 33' 19"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a broad single peak
structure with a duration of about 70 sec.  The peak count rate
was ~300 counts/sec (15-350 keV), at ~10 sec after the trigger. 

The XRT began observing the field at 07:29:00.4 UT, 119.3 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 236.9648, +20.5572 which is equivalent to:
   RA(J2000)  = 15h 47m 51.5s
   Dec(J2000) = +20d 33' 25.9"
with an uncertainty of 5.4 arcseconds (radius, 90% containment). This
location is 19 arcseconds from the BAT onboard position, within the BAT
error circle. No event data are yet available to determine the column
density using X-ray spectroscopy. 


UVOT took a finding chart exposure of 100 seconds with the White (160-650 nm)
filter starting 128 seconds after the BAT trigger. There is a candidate
afterglow in the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 15:47:51.70 = 236.9654
  DEC(J2000) = +20:33:28.1  =  20.5578
with a 1-sigma error radius of about 0.5 arc sec. This position is 3.4 arc sec. 
from the center of the XRT error circle. The estimated magnitude is 20.1 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 0.05. 




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


GRB_name: GRB080604A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7801
SUBJECT: GRB080604: confirmation of optical afterglow
DATE:    08/06/04 08:04:00 GMT
FROM:    Evert Rol at U.Leicester  <er45@star.le.ac.uk>

E. Rol (U. Leicester), C. Guidorzi (INAF-OAB), A. Gomboc (U. Ljubljana), 
I.A. Steele (Liverpool JMU), P. O'Brien (U. Leicester), A, Melandri, D. 
Bersier, C.G. Mundell, R.J. Smith, D. Carter, S. Kobayashi, M. Burgdorf, 
M. Bode (Liverpool JMU), N. Bannister, N. Tanvir (U. Leicester) report:

The Faulkes Telescope North observed the position of GRB080604. We confirm 
the detection of an optical transient (La Parola, GCN 7800), with a 
position of (J2000):

RA =   15 47 51.65
Dec = +20 33 28.1

In the first 10 second exposure, starting 5:42 minutes after the BAT 
trigger, we estimate a magnitude of R = 20.12 +/- 0.15 with respect to the 
USNO-B1.0 star at 15:47:52.50, +20:34:24.4.


GRB_name: GRB080604A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7802
SUBJECT: GRB 080604: Early Super-LOTIS Observations
DATE:    08/06/04 09:32:05 GMT
FROM:    Grant Williams at Steward Observatory  <ggwilli@gmail.com>

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

The robotic 0.6-m Super-LOTIS telescope began observing the error box
of GRB 080604 (Swift Trigger 313116, La Parola et al. GCN 7800) at
07:28:59.0 UT, 118 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 do not detect the afterglow reported by La Parola et al. (GCN 7800)
and confirmed by Rol et al. (GCN 7801) in our earliest exposure to the
following 5-sigma limiting magnitude determined using the nearby
USNO-B1.0 star 1105-0256520 at RA=15:47:45.32, Dec=+20:33:38.4 with
R2mag=14.56:

t_start (UT) exp t (s) t_start-t_0 (s) Limit
--------------------------------------------------------
07:28:59.0 10   118.0   R > 17.5

We also do not detect the afterglow in our later images or the sum of
our 20s images and 6x60s images.  Additional observations and analysis
are ongoing.


GRB_name: GRB080603B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7803
SUBJECT: GRB080603B: RTT150 optical observations, break in light curves
DATE:    08/06/04 09:46:50 GMT
FROM:    Irek Khamitov at TUG  <irekk@tug.tug.tubitak.gov.tr>

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

report:

The optical counterpart (GCN7792, 7793, 7794, 7795, 7796, 7797, 7799)
of GRB 080603B (GCN 7794, SWIFT trigger=313087) was observed with
Russian-Turkish 1.5-m  telescope (RTT150, Bakirlitepe, TUBITAK
National Observatory, Turkey), starting at  03 June, 20:55 UT,
i.e. ~1.3 hours after the burst, using Andor CCD.

A series of 70 frames with 60sec exposure in the R and V bands were taken 
for a time span ~ 4.5 hours. The afterglow is clearly detected  in all 
images. Using RTT150 preliminary calibrated magnitudes for USNO-A2 
1575-03195804 star R.A. = 11 46 09.53,  Dec. = +68 01 51.3,  V=14.2, 
R=13.8 mag, the brightness of the OT was estimated on each frame.

V,R light curves are shown at:

http://www.tug.tubitak.gov.tr/~irekk/grb/grb080603B/GRB080603B_lc.jpg

Higher dispersion at (T-T0) > 4 hours must be due to high airmass
( Z ~ 65-70 degrees).

The VR-light curves are well fitted with two power law decay functions
with a break about 3 hours after the burst.

A power law decay indices were estimated in OT VR-light curves as follow:

before the break
alpha_R=-0.59+/-0.03
alpha_V=-0.60+/-0.03

after the break
alpha_R=-1.14+/-0.09
alpha_V=-1.03+/-0.07

The alpha indices before the break are in good agreement with Klotz et al. 
(GCN7799) calculated for the time span between 1 and 4 hours after
the burst.

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GRB_name: GRB080603A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7804
SUBJECT: GRB 080603A: Swift/UVOT detection of the afterglow
DATE:    08/06/04 11:39:42 GMT
FROM:    Paul Kuin at MSSL  <npkuin@googlemail.com>

N. P. M. Kuin (MSSL/UCL), and V. Mangano (INAF), report on behalf
of the Swift UVOT team

The Swift UltraViolet/Optical Telescope (UVOT) began observations of INTEGRAL
burst GRB080603A (INTEGRAL trigger number 5283, Paizis et al., GCN Circ. 7790),
on June 3, 2008, at 14:11:20 UT, 173 minutes after the initial trigger in
the UVOT v filter.

We detect a fading source at position :

RA=18:37:38.21 Dec=+62:44:38.40 (279.40921 +62.74400 ddeg (J2000)).

The initial magnitude observed for GRB080603A  is given below for the
first observation in the UVOT v filters:

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

v      10389     10499     109.   19.16 +/- 0.35

The magnitude decrease observed was 1.2 magnitudes per hour.

The values quoted above are on the UVOT Photometric System
(Poole et al, 2008, MNRAS 383,627). They are not corrected for the
expected galactic reddening of E(B-V) = 0.044 in the direction of
the burst (Schlegel et al. 1998).


GRB_name: GRB080604A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7805
SUBJECT: GRB 080604: Hobby-Eberly Telescope spectroscopy
DATE:    08/06/04 11:39:53 GMT
FROM:    Antonino Cucchiara at PSU  <cucchiara@astro.psu.edu>

A. Cucchiara and D. B. Fox (Penn State) report:

"Starting on 2008 June 4.35 UT we used the Marcario LRS spectrograph
on the Hobby-Eberly Telescope (R ~ 230) to obtain a 1200s spectrum
of the optical afterglow of GRB 080604 (La Parola et al., GCN 7800).
The spectrum covers the wavelength range 4500 to 10,000 Angstrom.
Based on a preliminary calibration we detect absorption features
corresponding to the MgII doublet (2796, 2803 A) and MgI (2852 A)
as well as other metal absorption features at redshift z = 1.28.

The absence of Lyman break in our dataset suggests z < 2.7.

A refined analysis will be posted.

We thank the HET staff for performing this observation,
in particular Matthew Shetrone."


GRB_name: GRB080603B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7806
SUBJECT: GRB 080603B, Swift-BAT refined analysis
DATE:    08/06/04 12:32:40 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

J. Tueller (GSFC), S. D. Barthelmy (GSFC), W. Baumgartner (GSFC/UMBC),
J. Cummings (GSFC/UMBC), E. Fenimore (LANL), N. Gehrels (GSFC),
H. Krimm (GSFC/USRA), V. Mangano (INAF-IASFPA), C. Markwardt (GSFC/UMD),
K. McLean (GSFC/UMD), D. Palmer (LANL), A. M. 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+470 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 080603B (trigger #313087)
(Mongano, et al., GCN Circ. 7794).  The BAT ground-calculated position is
RA, Dec = 176.554, 68.061 deg, which is 
   RA(J2000)  =  11h 46m 13.0s 
   Dec(J2000) = +68d 03' 40.5" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.
 
The mask-weighted light curve shows three main clusters of peaks.  The first
starts at T-1 sec, peaks at T+1 sec, and ends at ~T+7 sec.  The second 
starts at T+8 sec and ends at T+20 sec.  The third starts at ~T+42 sec
and ends at ~T+80 sec.  T90 (15-350 keV) is 60 +- 4 sec (estimated error
including systematics).
 
The time-averaged spectrum from T-0.1 to T+68.6 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 1.21 +- 0.30, 
and Epeak of 71.0 +- 16.0 keV (chi squared 63.16 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 2.4 +- 0.1 x 10^-6 erg/cm2
and the 1-sec peak flux measured from T+0.96 sec in the 15-150 keV band is
3.5 +- 0.2 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.78 +- 0.07 (chi squared 75.18 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/313087/BA/


GRB_name: GRB080604A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7807
SUBJECT: GRB 080604: Enhanced Swift-XRT position
DATE:    08/06/04 13:01:16 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 749 s of overlapping XRT Photon Counting mode and UVOT
data for GRB 080604, 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 = 236.96516, +20.55777 which is equivalent
to:

RA (J2000): 15h 47m 51.64s
Dec (J2000): +20d 33' 28.0"

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: GRB080603B
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7808
SUBJECT: GRB 080603B: Swift/UVOT detection of the afterglow
DATE:    08/06/04 13:57:29 GMT
FROM:    Paul Kuin at MSSL  <npkuin@googlemail.com>

N. P. M. Kuin (MSSL/UCL), and V. Mangano (INAF-IASFPA), report on behalf
of the Swift UVOT team

The Swift UltraViolet/Optical Telescope (UVOT) began observations
of GRB 080603A, on June 3, 2008, at  19:39:07 UT,  63 seconds after
the initial Swift BAT trigger (Mangano et al., GCN Circ. 7794)..

The refined uvot position is

 RA  = 11:46:07.66 = 176.5316
 DEC =+68:03:39.99 = 68.061105

with an error or 0.3".

The first finding chart in the wh filter has problems due to the
brightness of the image, and needs detailed analysis. We start
our report with the second finding chart.

The magnitudes with 1-sigma errors for GRB080603B are given below
for the initial observation sequence.

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

v       187.8      393.1    202    16.48 +/- 0.06
uvm2   5778.0     5977.8    197    > 19.51 (3-sigma UL)
uvw1   5983.9     6183.7    197    20.02 +/- 0.56
u      6188.8     6388.6    197    18.80 +/- 0.23
b      6395.3    12274.3    643    19.34 +/- 0.14

The absence of a detection in the uvm2 filter is consitent with
the reported redshift of 2.69 (Fynbo et al., GCN Circ. 7797).

Magnitude variation in the b observations shor evidence
of flaring or rebrightening..

The values quoted above are on the UVOT Photometric System
(Poole et al, 2008, MNRAS 383,627). They are not corrected for the
expected galactic reddening of E(B-V) = 0.013 in the direction of
the burst (Schlegel et al. 1998).


GRB_name: GRB080430A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7809
SUBJECT: GRB 080430: optical observations 
DATE:    08/06/04 15:58:14 GMT
FROM:    Graziella Pizzichini at IASF/CNR,Bologna  <pizzichini@iasfbo.inaf.it>

     F. Terra (Second University of Roma "Tor Vergata"),  F. Munz (INAF/IASF
     Bologna) G. Greco, C. Bartolini, A. Guarnieri,A. Piccioni (Bologna
     University), D. Nanni (INAF/OAR and Second University of Rome "Tor
     Vergata"), G. Pizzichini(INAF/IASF Bologna), S. Galleti and S. Bernabei
     (Bologna Observatory) report:

    During the night between 08/04/30 and 08/05/01 we observed the OT of
    GRB080430 (Guidorzi et al., GCN 7647, Klotz, Boer & Atteia, GCN 7646)
    with the 1.52  cm telescope of the Bologna Observatory in Loiano in good
    weather conditons, airmass  between 1 and 1.6, seeing less than 4".
    We obtained a total of 14 frames in Rc, V, B and I.
    Rc magnitudes went from 19.47 +- 0.11 at 2454587.40325 UT to 20.53 +- 0.10
    at 2454587.54819 UT.
    Rc calibration was obtained from the NOMAD catalog.

     Our  images have been posted in our public directory
     from where they can be retrieved by sftp using
     hostname: ermione.bo.astro.it
     username: publicGRB
     password: GRB_bo
     directory: /home/publicGRB/GRB080430/


GRB_name: GRB080603A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7810
SUBJECT: GRB 080603A: Swift-XRT detection of the afterglow
DATE:    08/06/04 16:08:03 GMT
FROM:    Boris Sbarufatti at INAF-IASF-Pa  <sbarufatti@ifc.inaf.it>

B. Sbarufatti, V. Mangano, V. La Parola (INAF-IASF Pa) report on behalf
of the Swift-XRT team

The Swift XRT began observations of the INTEGRAL burst GRB 080603A
(Paizis et al., GCN Circ 7790) on June 3, 14:11 UT, 173 minutes after
the trigger. The data consist of 3.9 ks observed in Photon Counting
mode.

We detect an X-ray counterpart at position (astrometrically corrected 
using the XRT-UVOT alignment and matching UVOT field sources to the 
USNO-B1 catalogue): RA, Dec = 279.40858, 62.74446 which is equivalent to:

RA (J2000):  18 37 38.06
Dec (J2000): +62 44 40.1

with an uncertainty of 1.9 arcsec (radius, 90% confidence).
The light curve is dominated by a flare-like structure which covers all
the observed time interval, making it impossible to estimate the
behaviour of the underlying continuum and to predict the evolution of
the source.
The spectrum can be fitted with a powerlaw with an intrinsic absorbing
column of (8+/-5)e21 cm-2 at z=1.688 (Perley et al., GCN Circ 7791)
and photon index 2.4 0.3. The observed (unabsorbed) 0.3-10 keV flux
is 3.23 (3.57)e-12 erg cm-2 s-1.

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


GRB_name: GRB080603B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7811
SUBJECT: GRB 080603B: Swift-XRT refined analysis
DATE:    08/06/04 16:37:24 GMT
FROM:    Boris Sbarufatti at INAF-IASF-Pa  <sbarufatti@ifc.inaf.it>

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

The Swift-XRT observed GRB 080603B (trigger 313087, Mangano et
al. GCN Circ 7794) for three orbits which consisted of 200 s of
Windowed Timing mode data starting 68 s after the trigger and
990 s of Photon Counting mode data, 274 s after the trigger.

We obtained a refined XRT position at
RA, Dec = 176.53312  68.06058 which is equivalent to:

RA (J2000):  11 46 07.95
Dec (J2000): 68 03 38.11

with an uncertainty of 3.7 arcsec (radius, 90% confidence).
The position is 3.2 arcsec from the on-board position reported
in GCN Circ. 7794 and 0.7 arcsec from the refined UVOT position
(Kuin et al. GCN Circ 7808).

The X-ray light curve shows an initial steep decay with a slope
of 3.4  0.1, breaking to a shallower decay of 0.8  0.1  at
a time of 161  6 s after the trigger.

A spectrum of the Windowed Timing data can be well fit by an absorbed
power-law, with a photon index Gamma = 1.68  0.06 and a column
density Nh = (7.9  0.2) e21 cm-2 in excess with respect to the Galactic
column density in this direction of 1.2e20 cm-2. The observed
(unabsorbed) 0.3-10 keV flux is 7.0e-10 (7.7e-10) erg cm-2 s-1.

The Photon Counting mode spectrum is also well fit by an absorbed
powerlaw, with an Nh = (1.3  0.2) e22 cm-2 and Gamma = 2.0  0.2.
The observed (unabsorbed) 0.3-10 keV flux is 1.55 e-11 (1.91e-11)
erg cm-2 s-1.

The predicted XRT count rate after 24 hours from burst is 6.0e-2 counts/s

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


GRB_name: GRB080603B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7812
SUBJECT: Konus-Wind observation of GRB 080603B
DATE:    08/06/04 17:04:26 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 080603B (Swift-BAT trigger #313087: Mangano et al., GCN
7794, Tueller et al., GCN 7806) triggered Konus-Wind at T0=70692.383 s 
UT (19:38:12.383).

The burst light curve shows several pulses with a total duration of ~70s.

As observed by Konus-Wind the burst
had a fluence of 4.50(-0.90, +1.53)x10^-6 erg/cm2,
and a 256-ms peak flux measured from T0+0.624 s
of 1.51(-0.38, +0.40)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+73.984 s) can be fitted (in the 20-500 keV range)
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with alpha = -1.23(-0.54, +0.75),
and Ep = 102(-28, +119) keV (chi2 = 50.5/42 dof).
Fitting by GRBM (Band) model yields:
the low-energy photon index is alpha = -0.94(-0.75, +1.21),
the high energy photon index beta < -1.96,
the peak energy Ep =  85(-30, +91) keV (chi2 = 49.7/41 dof).

The spectrum of the most intense part (from T0 T0+16.640 s)
is well fitted (in the 20 keV - 1 MeV range)
by a power law with exponential cutoff model
with alpha =  -1.20(-0.32, +0.26)
and Ep = 200(-56, +131) keV (chi2 = 63.5/56 dof).
The fluence of this part is 3.51(-0.58, +0.69)x10^-6 erg/cm2.

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

Assuming z = 2.69 (Fynbo et al., GCN 7797) and a standard
cosmology model with H_0 = 70 km/s/Mpc, Omega_M = 0.27, Omega_\Lambda =
0.73, the isotropic energy release is E_iso ~7.7x10^52 erg,
the maximum luminosity is (L_iso)_max ~9.4x10^52 erg/s, and
Ep_rest ~350 keV.

The Konus-Wind light curve of this GRB is available
at http://www.ioffe.rssi.ru/LEA/GRBs/GRB080603_T70692/


GRB_name: GRB080603B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7813
SUBJECT: GRB 080603B : Liverpool Telescope Observations
DATE:    08/06/04 17:13:50 GMT
FROM:    Andrea Melandri at Liverpool John Moores U  <axm@astro.livjm.ac.uk>

A. Melandri, (Liverpool JMU), A. Gomboc (U. Ljubljana), C. Guidorzi
(INAF-OAB), R.J. Smith, I.A. Steele, D. Bersier, C.G. Mundell, D. Carter,
S. Kobayashi, M. Burgdorf, M. Bode (Liverpool JMU), E. Rol, P. O'Brien,
N. Bannister, N. Tanvir (U. Leicester) report:


On 2008 Jun 03 at 21:32:57UT we observed the Swift GRB 080603B
(trigger=313087, Mangano et al., GCN 7794) with the Liverpool Telescope
using SDSS-I, SDDS-R and Bessell-B filters.

The OT reported by Rujopakarn et al. (GCN 7792), Mangano et al. (GCN
7794), Klotz et al. (GCN 7795, 7799), Castro-Tirado et al. (GCN 7796)
and Zhuchkov et al.(GCN 7803) is well detected in all our single 300s
exposures.

We calibrated the afterglow magnitude using B, R and I magnitudes of few
USNO B1 stars in the field of view.

Our observations started soon after the plateau phase reported by Klotz et
al. (GCN 7795) and Castro-Tirado et al. (GCN 7796) but our I-band and
R-band images were acquired before and after the optical break reported by
Zhuchkov et al.(GCN 7803).

We found alpha_I= 0.55 +/- 0.03 before the optical break and
alpha_R= 1.03 +/- 0.02 after the break, confirming the values found by
Zhuchkov et al.(GCN 7803).


GRB_name: GRB080603B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7814
SUBJECT: GRB 080603B : Xinglong EST observations 
DATE:    08/06/04 17:43:05 GMT
FROM:    W.K. Zheng at NAOC  <zwk@bao.ac.cn>

L.P.Xin, Q.C.Feng, M.Zhai, Y.L.Qiu, J.Y.Wei, J.Y.Hu, J.S.Deng,
J.Wang, Y.Urata and W.K.Zheng on behalf of EAFON report:

Xinglong EST started to observe the GRB080603B (Mangano et al.,
GCN 7794) from 14:42 UT Jun 04 with R and V filters. with the
same calibration star as used in GCN7803 (Zhuchkov et al.)
USNO-A2 1575-03195804 R=13.8 mag, we estimated the brightness
of OT R ~ 20.3 +/- 0.15, which is consistent with the powler
decay after the break given it GCN7803. Observation is still
under going.
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: GRB080603B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7815
SUBJECT: GRB 080603B: Hobby-Eberly Telescope redshift confirmation
DATE:    08/06/04 17:51:00 GMT
FROM:    Antonino Cucchiara at PSU  <cucchiara@astro.psu.edu>

A. Cucchiara and D. B. Fox (Penn State) report:

"Starting on 2008 June 4.13 UT we used the Marcario LRS spectrograph
on the Hobby-Eberly Telescope (R ~ 230) to obtain 2 x 900s spectra
of the optical afterglow of GRB 080603B (GCN 7792, GCN 7794).
The spectrum covers the wavelength range 4500 to 10,000 Angstrom.

We clearly detect the Lyman break and several metal absorption features
corresponding to a redshift z = 2.69.
No other systems are detected and our result confirms the redshift
determination by Fynbo et al. (GCN 7797).

We thank the HET staff for performing this challenging observation,
in particular Matthew Shetrone."


GRB_name: GRB080604A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7816
SUBJECT: GRB 080604: Swift-XRT refined analysis
DATE:    08/06/04 17:55:28 GMT
FROM:    Valentina La Parola at INAF-IASPA  <laparola@ifc.inaf.it>

V. La Parola, B. Sbarufatti, V. Mangano (INAF-IASF Pa) report on behalf
of the Swift-XRT team

The Swift-XRT observed GRB 080604 (trigger 313116, La Parola et
al. GCN Circ 7800) for 6.3 ksec, starting 119.3 seconds after
the BAT trigger.

We detect an X-ray counterpart at the position
(astrometrically corrected using the XRT-UVOT alignment and matching UVOT field sources to the USNO-B1 catalogue): RA, Dec = 236.96516, +20.55777 which is equivalent to:

RA (J2000): 15h 47m 51.64s
Dec (J2000): +20d 33' 28.0"

with an uncertainty of 1.7 arcsec (radius, 90% confidence).

The X-ray light curve shows a power law decay with slope -2.18 +/-0.06, with a hint of a flare at ~T+1000 s.

The spectrum accumulated over the whole observation can be modelled with an absorbed powerlaw with the following parameters (Galactic nH is
4.0e20cm**-2):

nH = (8 +/- 4)e20 cm**-2
Gamma= 1.8 +/- 0.2
Flux (0.3-10 keV) 4.18E-12 ergs cm**-2 s**-1
Unabsorbed Flux (0.3-10 keV) = 4.9E-12 ergs cm**-2 s**-1

The predicted XRT count rate after 24 hours from the burst is 1.5e-5
counts/s

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

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GRB_name: GRB080604A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7817
SUBJECT: GRB 080604, Swift-BAT refined analysis
DATE:    08/06/04 18:03:17 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), W. Baumgartner (GSFC/UMBC), J. Cummings (GSFC/UMBC),
E. Fenimore (LANL), N. Gehrels (GSFC), H. Krimm (GSFC/USRA),
V. La Parola (INAF-IASFPA), C. Markwardt (GSFC/UMD), K. McLean (GSFC/UMD),
D. Palmer (LANL), T. Sakamoto (GSFC/UMBC), G. Sato (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 080604 (trigger #313116)
(La Parola, et al., GCN Circ. 7800).  The BAT ground-calculated position is
RA, Dec = 236.960, 20.557 deg, which is 
   RA(J2000)  =  15h 47m 50.3s 
   Dec(J2000) = +20d 33' 25.4" 
with an uncertainty of 2.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 100%.
 
The mask-weighted light curve shows a single peak starting at ~T-25 sec
and ending at ~T+100 sec.  T90 (15-350 keV) is 82 +- 13 sec (estimated error
including systematics).
 
The time-averaged spectrum from T-27.3 to T+67.2 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.78 +- 0.18.  The fluence in the 15-150 keV band is 8.0 +- 0.9 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T-3.02 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/313116/BA/
 
This burst satisfies Sakamoto/Ukwatta Swift-BAT possible high-z criteria
(Ukwatta et al. arXiv:0802.3815):
1) Pawer Law photon index = 1.78 (PL photon index < 2)
2) 1-s peak photon flux   = 0.4 (1-s peak photon flux < 1.0 ph/cm2/s)
3) Light curve variance   = 1.1e-05 (Variance < 0.0001)
4) T90/(Peak photon flux) = 218 (T90/(Peak photon flux) > 100)
Based on a limited sample of bursts, these criteria yield an 85% chance
it has a redshift greater than 3.5.  We note that the Cucchiara (GCN Circ 7805)
HET spectrum yields a z = 1.28.


GRB_name: GRB080604A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7818
SUBJECT: GRB 080604: Gemini-North spectroscopy
DATE:    08/06/04 20:46:50 GMT
FROM:    Klaas Wiersema at U of Leicester  <kw113@star.le.ac.uk>

K. Wiersema (U. of Leicester), J. Graham (STScI), N. Tanvir, E. Rol (U. of 
Leicester), A. Levan (U. of Warwick) and A. Fruchter (STScI) report on 
behalf of a larger collaboration:

We observed the optical afterglow of GRB 080604 (GCNC 7800, 7801) with 
Gemini-North, using the GMOS-N instrument. Spectroscopy was performed with 
the R400 grism, using 4 x 450 seconds integration time, starting at
2008 June 04, 08:58 UT.

Several absorption lines of, among others, Fe II (2382,2586,2600), Mg II 
(2796,2803) and Mg I (2026,2852) are found at a redshift of 1.416. The 
discrepancy with respect to the redshift reported in GCN 7805 may be due 
to provisional calibration files used for the HET reduction (Cucchiara 
priv. comm.).

We thank the Gemini staff astronomers for their support in obtaining these 
observations.


GRB_name: GRB080604A
Detection_method: retraction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7819
SUBJECT: GRB080604: HET redshift retraction
DATE:    08/06/04 20:56:18 GMT
FROM:    Antonino Cucchiara at PSU  <cucchiara@astro.psu.edu>

A. Cucchiara and D. B. Fox  (Penn State) report:

Based on updated calibration files we re-analyzed the GRB080604 spectrum
taken at HET (GCN 7805). The features reported in the previous GCN are no
longer significant at a 3-sigma confidence level.
Furthermore, only an upper limit of z < 2.8 can be derived from our dataset.

Our revised results are consistent with the results from Gemini-North 
spectroscopy
(Wiersama et al., GCN 7818).  The low signal to noise of our spectrum 
does not
permit detection of the absorption features associated with the z=1.416 
system
seen in those data.


GRB_name: GRB080604A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7820
SUBJECT: Swift/UVOT observations of GRB080604 
DATE:    08/06/04 21:27:12 GMT
FROM:    Massimiliano de Pasquale at MSSL-UCL  <mdp@mssl.ucl.ac.uk>

  M. De Pasquale (MSSL/UCL), V. La Parola (INAF-IASFPA),
F. E. Marshall (GSFC) report:
The Swift UltraViolet/Optical Telescope (UVOT) began its
first finding chart exposure of GRB080604 (La Parola
et al., GCN circ. 7800) 129 seconds after the trigger
in white filter and detected the optical afterglow (GCN
circ. 7800). The coordinates of this transient are:

  Dec:  15:47:51.68
  RA:  +20:33:28.0

  The afterglow is detected only in the white filter.
Magnitudes and 3 sigma upper limits are listed in the
table below.


  Filter  T_start(s)  T_stop(s)  Exp(s)     Magnitude

  white     129         228       99     20.1 +/- 0.2

  white     730         739       10        > 19.7

  white     869         968       99     21.0 +0.3 -0.2

  white    1479        1651       39        > 20.7

  white    5369        7031      393     21.8 +0.5 -0.4


   v        235         635      393        > 20.1

   v        769        1373      412        > 20.0

   v       1519        1701       39        > 18.8

   v       5807        7441      393        > 19.9

   v      17489       18395      885        > 20.3


   b       716          725       10        > 19.0

   b      1454         1637       39        > 19.8

   b      5191         6826      393        > 21.0


   u      691           862       39        > 19.4

   u      1430         1612       39        > 19.4

   u      4896         6621      393        > 20.7

   u     12600        13306      689        > 21.0


  uw1     667          1738       46        > 19.6

  uw1    6217         12591     1082        > 21.2


  um2     641        19090      1931        > 21.6


  uw2     745        17482      1395        > 21.4



  The values quoted above are on the UVOT Photometric System
(Poole et al, 2008, MNRAS 383,627). They are not corrected
for the expected Galactic reddening of E(B-V) = 0.049 in the
direction of the burst (Schlegel et al. 1998).

_______________________________________________
Uvot_cal mailing list
Uvot_cal@phoenix.astro.psu.edu
https://phoenix.astro.psu.edu/mailman/listinfo/uvot_cal


GRB_name: GRB080604A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7821
SUBJECT: GRB 080604: MITSuME Okayama observation
DATE:    08/06/05 10:00:56 GMT
FROM:    Michitoshi Yoshida at Okayama Astrophysical Obs  <yoshida@oao.nao.ac.jp>

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

We observed the field of GRB 080604 (La Parola et al., GCN7800) with
the 50cm MITSuME Telescope at Okayama Astrophysical Observatory on
June 4 UT. We detected a faint point source at the UVOT position
(La Parola et al., GCN7800; Rol et al., GCN7801; De Pasquale et al.,
GCN7820) in our Ic band image. Photometric calibration was done using
USNO-B1.0 catalog.

      mid-UT        exp-T      g'      Rc           Ic
------------------------------------------------------------
2008-6-4 12:41:48   49min    >20.0    >19.2    18.6 +/- 0.4
------------------------------------------------------------


GRB_name: GRB080603A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7822
SUBJECT: GRB 080603A: TLS Afterglow Observation
DATE:    08/06/05 15:22:40 GMT
FROM:    Alexander Kann at TLS Tautenburg  <kann@tls-tautenburg.de>

D. A. Kann, U. Laux and S. Ertel (TLS Tautenburg) report:

We observed the field of the INTEGRAL GRB 080603A (Paizis et al., GCN 
7790) with the TLS 1.34m Schmidt telescope in mediocre observing 
conditions (low airmass but high humidity and moderate transparency). We 
obtained a total of 6 x 600 sec images at mid-time June 5.023368. The 
afterglow (Gomboc et al., GCN 7788; Chornock et al., GCN 7789) is faintly 
visible in each image. We stacked all six images. Assuming the USNOB1.0 
star with ID 1527-0313986 at RA = 18:37:55.186, Dec. +62:45:32.28 to have 
R1 = 16.74 mag, we measure for the afterglow:

dt Rc dRc

1.55241 21.39 0.03 (statistical only)

We note the presence of a fainter source several arcseconds east of the OT 
which may slightly influence the photometry.

In comparison to the magnitude measured by Perley et al. (GCN 7791), this 
implies a slow decay of alpha ~ 0.5. Further observations are warranted.

This message may be cited.


GRB_name: GRB080603B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7823
SUBJECT: GRB 080603B: TLS Afterglow Observation
DATE:    08/06/05 15:24:14 GMT
FROM:    Alexander Kann at TLS Tautenburg  <kann@tls-tautenburg.de>

D. A. Kann, U. Laux and S. Ertel (TLS Tautenburg) report:

We observed the field of the Swift GRB 080603B (Mangano et al., GCN 7794) 
with the TLS 1.34m Schmidt telescope in mediocre observing conditions (low 
airmass but high humidity and moderate transparency). We obtained a total 
of 6 x 600 sec images at mid-time June 4.980179. The afterglow 
(Rujopakarn, Guver, & Smith, GCN 7792) is faintly visible in each image. 
We stacked all six images. Assuming the USNOB1.0 star with ID 1580-0163070 
at RA = 11:46:29.297, Dec. +68:03:23.43 (USNOB1.0 catalog value) to have 
R1 = 17.97 mag, we measure for the afterglow:

dt Rc dRc

1.16197 21.32 0.04 (statistical only)

In comparison to the magnitude measured by Xin et al. (GCN 7814) 0.8 days 
after the GRB, this implies a steep decay of alpha ~ 2.5. It is unclear if 
this is due to a break or to the use of different comparison stars. The 
comparison star used by Zhuchkov et al. GCN 7803, and Xin et al., GCN 
7814, is saturated in our images. Further observations are warranted.

This message may be cited.


GRB_name: GRB080603A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7824
SUBJECT: GRB 080603A: Xinglong R band observation
DATE:    08/06/05 16:23:07 GMT
FROM:    W.K. Zheng at NAOC  <zwk@bao.ac.cn>

X.M. Meng, Y.N. Zhu, L.P. Xin, Q.C. Feng, M. Zhai,
Y.L. Qiu, J.Y. Wei, J.Y. Hu, J.S. Deng, J. Wang,
Y. Urata and W.K. Zheng on behalf of EAFON report:

We observed GRB080603A (Paizis et al., GCN 7790), with
Xinglong 2.16m telescope + BFOSC on Jun 4, 1.321 Days
after the burst. We marginally detected the OT (Gomboc et al.,
GCN 7788; Chornock et al., GCN 7789; Kuin et al., GCN 7804
Kann et al. GCN 7822) at 3 sigma level. With the same
calibration star as used in GCN 7822 (Kann et al.) USNOB1.0
1527-0313986 at RA = 18:37:55.186, Dec. +62:45:32.28  
R1 = 16.74, we estimated the OT brightness was R ~ 21.3
+/- 0.3. We also detected the faint star at east side of OT
noted by Kann et al.
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: GRB080604A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7825
SUBJECT: GRB 080604: Xinglong R band observation
DATE:    08/06/05 16:25:28 GMT
FROM:    W.K. Zheng at NAOC  <zwk@bao.ac.cn>

X.M. Meng, Y.N. Zhu, L.P. Xin, Q.C. Feng, M. Zhai,
Y.L. Qiu, J.Y. Wei, J.Y. Hu, J.S. Deng, J. Wang,
Y. Urata and W.K. Zheng on behalf of EAFON report:

We observed GRB080604 (La Parola et al., GCN 7800) with
Xinglong 2.16m telescope + BFOSC on Jun 4, 8.024 hours
after the burst. We marginally detected the OT (La Parola et al.,
GCN 7800; Rol et al., GCN 7801; De Pasquale et al., GCN 7820)
at 3 sigma level. The estimated brightness was R ~ 21.6
+/- 0.3 calibrated to USNO-A2.0 stars.
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: GRB080603A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7826
SUBJECT: GRB 080603A: PAIRITEL infrared detection
DATE:    08/06/05 22:02:45 GMT
FROM:    Daniel Perley at U.C. Berkeley  <dperley@astro.berkeley.edu>

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

We observed the optical afterglow of GRB080603A (Paizis et al., GCN 
7790; Gomboc et al., GCN 7788; Chornock et al; GCN 7789) with the 1.3m 
Peters Automated Infrared Imaging Telescope (PAIRITEL) starting 18.89 
hours post trigger on June 04, 2008 UT. We detected the afterglow in a 
2927 sec mosaic of simultaneous 7.8 sec exposures in the J, H, and Ks 
filters. Preliminary photometry for the afterglow in exposures beginning 
on Jun 04.26 UT yields J = 18.9 +- 0.15, H = 17.9+- 0.15, and Ks = 16.8 
+- 0.15, calibrated to the 2MASS system.


GRB_name: GRB080603B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7827
SUBJECT: GRB 080603B: PAIRITEL infrared detection
DATE:    08/06/05 22:02:59 GMT
FROM:    Daniel Perley at U.C. Berkeley  <dperley@astro.berkeley.edu>

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

We observed the optical afterglow of GRB080603B (Mangano et al., GCN 
7794) with the 1.3m Peters Automated Infrared Imaging Telescope 
(PAIRITEL) starting 7.66 hours post trigger on June 04, 2008 UT. We 
detected the afterglow in a 2291 sec mosiac of 7.8 sec simultaneous 
exposures in the J,  H, and Ks filters. Preliminary photometry for the 
afterglow in exposures beginning on Jun 04.14 UT yields J = 17.9 +- 0.1, 
H = 17.2 +- 0.1, and Ks = 16.7 +- 0.15, calibrated to the 2MASS system.


GRB_name: GRB080605A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7828
SUBJECT: GRB 080605: Swift detection of a burst with an optical afterglow
DATE:    08/06/06 00:13:48 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

B. Sbarufatti (INAF-IASFPA), S. D. Barthelmy (GSFC),
D. N. Burrows (PSU), N. Gehrels (NASA/GSFC),
S. T. Holland (CRESST/USRA/GSFC), V. La Parola (INAF-IASFPA),
V. Mangano (INAF-IASFPA), C. B. Markwardt (CRESST/GSFC/UMD),
D. M. Palmer (LANL), A. M. Parsons (GSFC), T. Sakamoto (NASA/UMBC),
T. N. Ukwatta (GSFC/GWU) and D. E. Vanden Berk (PSU) report on behalf
of the Swift Team:

At 23:47:57 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 080605 (trigger=313299).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 262.127, +4.002 which is 
   RA(J2000)  = 17h 28m 31s
   Dec(J2000) = +04d 00' 06"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows multiple overlapping
peaks lasting at least to T+8 sec (at which the TDRSS lightcurve is
truncated).  The peak count rate was ~17000 counts/sec (15-350 keV),
at ~1 sec after the trigger. 

The XRT began observing the field at 23:49:28.2 UT, 90.4 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 262.1249, +4.0153 which is equivalent to:
   RA(J2000)  = 17h 28m 29.9s
   Dec(J2000) = +04d 00' 55.0"
with an uncertainty of 5.0 arcseconds (radius, 90% containment). This
location is 48 arcseconds from the BAT onboard position, within the BAT
error circle. No event data are yet available to determine the column
density using X-ray spectroscopy. 

The UVOT detects a new source within the XRT error circle.  We are unable to 
obtain a position or magnitude at this time.  The source is very close to a 
known source in the DSS.  Further information will be provided when it is available. 

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


GRB_name: GRB080605A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7829
SUBJECT: GRB 080605: TLS RRM Afterglow
DATE:    08/06/06 00:17:51 GMT
FROM:    Alexander Kann at TLS Tautenburg  <kann@tls-tautenburg.de>

This is a multi-part message in MIME format.

--bound1212711210
Content-Type: text/plain
Content-Transfer-Encoding: 7bit

D. A. Kann, U. Laux, S. Klose, S. Ertel (TLS Tautenburg) and J. Greiner (Garching) report:

We observed the location of Swift GRB 080605 with the TLS Tautenburg 1.34m Schmidt telescope in RRM Mode (Klose et al., GCN 3609).

At the in-flight XRT position, in a 120 sec Ic band frame, we detect a new source not present in the DSS at:

RA (J2000) = 17:28:29.96
Dec. (J2000) = +04:00:57.5

The source is blended with a star to the southeast but clearly discernible.

We propose this to be the afterglow of GRB 080605. Spectroscopy is encouraged.

This message may be cited.

--bound1212711210--


GRB_name: GRB080605A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7830
SUBJECT: GRB 080605: Swift/UVOT Position of the Optical Afterglow 
DATE:    08/06/06 00:27:40 GMT
FROM:    Stephen Holland at USRA/NASA/GSFC/SSC  <sholland@milkyway.gsfc.nasa.gov>

S. T. Holland (CRESST/USRA/GSFC) and B. Sbarufatti (INAF-IASFPA)
report on behalf of the Swift Team:

Swift/UVOT began observing the field of GRB 080605 (Sbarufatti et
al. 2008, GCN Circ. 7828) with a 99 s white exposure starting 104 s
after the BAT trigger.  The preliminary Swift/UVOT position of the
optical afterglow candidate is

  RA(J2000) =  17:28:30.07
Dec(J2000) = +04:00:56.0

with an estimated position uncertainty of 1.0 arcsec.  There is a
known source (USNO-B1.0 940-028965) 3 arcsec from this position.


GRB_name: GRB080605A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7831
SUBJECT: GRB 080605: Liverpool Telescope optical afterglow candidate
DATE:    08/06/06 00:40:18 GMT
FROM:    Andreja Gomboc at LT,ARI,Liverpool JMU  <ag@astro.livjm.ac.uk>

A. Gomboc (U. Ljubljana), A. Melandri, R.J. Smith, C.G. Mundell, I.A. 
Steele, D. Bersier, S. Kobayashi, D. Carter, M. Burgdorf, M.F. Bode 
(Liverpool JMU), C. Guidorzi (INAF-OAB) report:

The Liverpool Telescope (La Palma) automatically reacted to the Swift 
trigger 313299 and started observing the field 3 min after the trigger.

We find an un-catalogues source at
RA 17:28:29.9,
dec +04:00:55.0
consistent with the XRT position.

The magnitude of the source is R=18.3 at 11.3 min after the trigger.


GRB_name: GRB080605A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7832
SUBJECT: GRB 080605: VLT redshift
DATE:    08/06/06 03:56:15 GMT
FROM:    Pall Jakobsson at U Hertfordshire  <P.Jakobsson@herts.ac.uk>

Pall Jakobsson (U. Hertfordshire), Paul M. Vreeswijk,
Dong Xu and Christina C. Thoene (DARK, NBI) 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 080605 (Sbarufatti et al., GCN 7828). The acquisition 
image shows it to have R = 20.4 on June 6.063 (1.7 hours
post burst).

A firm upper limit of z < 2.1 can be placed on the redshift
of GRB 080605 from the lack of Ly-alpha forest lines in the
spectrum of the afterglow.

The spectrum is rich in absorption features, including Si II,
C IV, Al II, Al III, Zn II, Fe II, Mg II and Mg I, corresponding 
to a redshift of z = 1.6398 +/- 0.0006.

We thank the Paranal staff for excellent support, especially
Linda Schmidtobreick.


GRB_name: GRB080605A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7833
SUBJECT: GRB080605: optical observations
DATE:    08/06/06 04:22:14 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

V. Rumyantsev (CrAO),  A. Pozanenko (IKI) report on behalf of larger GRB 
follow-up collaboration:

We observed the optical afterglow (Kann,  et al., GCN 7829; Holland et al., 
GCN 7830; Gomboc et al., GCN 7831) of  Swift GRB 080605 (Sbarufatti  et al., 
GCN 7828) in R and I bands on June 05  Zeiss-1000 (Simeiz) telescope of CrAO 
observatory under not optimal weather conditions.  Based on  USNO-B1.0 star 
RA (J2000) = 17 28 29.92, Dec.
(J2000) = +04 00 36.5, R2=15.90 we estimated brightness of  the optical 
afterglow in first frames:

UT,       Exposure,   R_mag,
(start time)

2008-06-05T23:55:58    120 s     17.9
2008-06-06T00:00:34    120 s     18.4

During observations the afterglow is clearly faded.
Coordinates of the afterglow with uncertainties of 0.3":

RA(2000):  17 28 30.01
Dec(2000): +04 00 56.4

A finding chart can be found at 
http://grb.rssi.ru/GRB080605/grb080605_080605_z1000.gif
The message may be cited. 


GRB_name: GRB080605A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7834
SUBJECT: GRB 080605: GROND detection of the optical afterglow candidate
DATE:    08/06/06 04:30:38 GMT
FROM:    Christian Clemens at MPE  <cclemens@mpe.mpg.de>

C. Clemens, T. Kruehler, J. Greiner, A. Kupcu Yoldas, A. Yoldas (all MPE 
Garching) and G. Szokoly (Eoetvoes Univ., Budapest and MPE Garching) report 
on behalf of the GROND team:

We observed the field of GRB 080605 (Swift trigger 313299; Sbarufatti et al., 
GCN #7828) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, 
PASP 120, 405) mounted at the 2.2m ESO/MPI telescope at La Silla Observatory 
(Chile).

Observations started at 01:10:59 UT on June 6th, 2008, 83 mins after the GRB 
trigger, and are continuing.

We found a single and relatively bright point source within the 1.0'' 
Swift-UVOT error circle reported by Holland et al. (GCN #7830) at

RA (J2000) = 17h 28m 30.05s
DEC (J2000) = +04d 00' 56.2"

with a typical uncertainty of 0.8", which is consistent with the sources 
reported by Kann et al. (GCN #7829) and Gomboc et al. (GCN #7831).

Based on 460 s and 1500 s of effective exposures taken 1.65 hrs and 2.78 hrs 
after the trigger, we estimate preliminary magnitudes of

r' = 20.3 and i' = 19.4, as well as
r' = 20.7 and i' = 19.9

with typical errors of +/- 0.1. (Given magnitudes are calibrated against 
USNO-B1 field stars and might be affected by the bright, nearby star.)

This indicates a clear fading of the source, which we therefore suggest to be 
the optical afterglow of GRB 080605.


GRB_name: GRB080605A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7835
SUBJECT: GRB 080605: Enhanced Swift-XRT position
DATE:    08/06/06 11:41:27 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 426 s of overlapping XRT Photon Counting mode and UVOT
data for GRB 080605, 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 = 262.12533, +4.01608 which is equivalent
to:

RA (J2000): 17h 28m 30.08s
Dec (J2000): +04d 00' 57.9"

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), 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: GRB080605A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7836
SUBJECT: GRB 080605: MASTER VWF 46 s AT observation
DATE:    08/06/06 11:52:33 GMT
FROM:    Vladimir Lipunov at Moscow State U/Krylov Obs  <gcncirc@observ.inetcomm.ru>

MASTER-Net Team:

D.Kuvshinov, V. Lipunov, V.Kornilov,  E.Gorbovskoy,
A.Belinski, N.Shatskiy, N.Tyurina,
Sternberg Astronomical Institute, Moscow Union 'Optic'

A. Tlatov, I.Golubov
Kislovodsk Solar Station of the Pulkovo observatory

V.Krushinski, I.Zalognikh
Ural State University, Kourovka


S.Yazev, K.Ivanov
Irkutsk State University


MASTER Very Wide Field Camera located at Kislovodsk Solar Station
(http://observ.pereplet.ru, D=50 mm, 1015 square degrees, 35'' per pix) 
has moved to the Swift-BAT trigger 313299 (23:47:57 UT) and it has taken a 
series of 5s exposures  starting 46s after the GRB time and 12 s after 
notice arrivel time at   23:48:43 UT under good weather  condition, but 
large zenit distance.

These unfiltered images are calibrated relative to USNO A2.0 (R).
There is no OT was found inside Swift error box
(B. Sbarufatti, S. D. Barthelmy et al., GCN Circ 7828).

T-Tgrb    Mean Time     Limit   Coadd?           Note

46s        48.5s      >9.0      no             moving

51s        53.5s      >10.0     no

51s        56.0s      >10.2     2

51s        76.0s      >11.0    10

51s       101.0s      >11.5    20

The message can be cited.
mailto: lipunov@sai.msu.ru

PS. AT = After Trigger


GRB_name: GRB080605A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7837
SUBJECT: GRB080605: observation by BOOTES
DATE:    08/06/06 12:36:57 GMT
FROM:    Martin Jelinek at Inst.Astrophys.Andalucia,Granada  <mates@iaa.es>

M. Jelinek, A.J.Castro-Tirado, J. Gorosabel (IAA CSIC Granada),
Petr Kubanek (GACE Valencia), S. Vitek (FEL CVUT Praha),
A. de Ugarte Postigo (ESO Santiago), on behalf of a larger
Collaboration:

report:

"We observed the optical afterglow of GRB 080605 (Kann et al.
GCN 7829, Sbarufatti et al. GCN 7828, Gomboc et al. GCN 7831)
with the 30cm BOOTES-1B and with the 60cm BOOTES-2/TELMA
robotic telescopes in southern Spain.

The sequence of observations started 43s after the GRB trigger.
We clearly detect a 15th mag transient outshining the nearby star
in R-band (BOOTES-2/TELMA) and without filter (BOOTES-1B). "


GRB_name: GRB080605A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7838
SUBJECT: GRB 080605: Swift-XRT refined analysis
DATE:    08/06/06 17:22:59 GMT
FROM:    Boris Sbarufatti at INAF-IASF-Pa  <sbarufatti@ifc.inaf.it>

B. Sbarufatti, V. Mangano, V. La Parola (INAF-IASF Pa) report on
behalf of the Swift-XRT team

The XRT began observations of GRB 080605 (trigger=313299,
Sbarufatti et al., GCN circ. 7828) started on 2008 May 05 at 23:49:36 UT,
97 s after the BAT trigger. The data consist of 642 s in Windowed Timing
mode and 4.3 ks s in Photon Counting mode.

The light curve is described by a powerlaw with initial slope
0.65 (+/-0.05) until T+ 280s (+90, - 45), at which point the decay
steepens to an index 1.32 (+/-0.03).

The spectrum of the WT mode data can be fitted by a powerlaw with
photon index 1.78 (+/- 0.04) and an intrinsic absorbing column of
6.6 (+/-0.9)E21 cm^-2 at z=1.6398 (Jakobsson et al., GCN circ. 7832),
in excess over the Galactic value of 6.67E20 cm^-2.
The observed (unabsorbed) flux is 7.5 (8.1)E-10 erg cm^-2 s^-1.
The first orbit PC mode spectrum  (379 s of exposure) can be
fit by a powerlaw with photon index 1.6 (+/- 0.2) and an
intrinsic absorbing column of 4.8 (+/-4)E21 cm^-2. The observed
(unabsorbed) flux is 3.0 (3.3)E-10 erg cm^-2 s^-1.

The countrate to flux conversion factor is 4.87e-11 erg cm^-2 s^-1.
The predicted countrate 24 h after the trigger is 1.6E-2 counts/s,
equivalent to an observed flux of 7.8E-13 erg cm^-2 cts^-1.

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


GRB_name: GRB080605A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7839
SUBJECT: GRB 080605, Swift-BAT refined analysis
DATE:    08/06/06 17:37:12 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

J. Cummings (GSFC/UMBC), S. D. Barthelmy (GSFC), W. Baumgartner (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 (ISAS),
M. Stamatikos (GSFC/ORAU), B. Sbarufatti (INAF-IASFPA), J. Tueller (GSFC),
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 080605 (trigger #313299)
(Sbarufatti, et al., GCN Circ. 7828).  The BAT ground-calculated position is
RA, Dec = 262.130, 4.010 deg, which is 
   RA(J2000)  =  17h 28m 31.1s 
   Dec(J2000) = +04d 00' 35.6" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 41%.
 
The mask-weighted light curve shows a cluster of overlapping peaks
starting at ~T-3 sec, the largest peak at ~T+8 sec, and all ending at ~T+70 sec.
At the 1-2 sigma level, there is appears to be persistant emmission
in the T+300 to T+700 sec range.  T90 (15-350 keV) is 20 +- 1 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-5.5 to T+30.0 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 1.11 +- 0.14, 
and Epeak of 223 +- 133 keV (chi squared 28.10 for 56 d.o.f.).   For this
model the total fluence in the 15-150 keV band is 1.33 +- 0.02 x 10^-5 erg/cm2
and the 1-sec peak flux measured from T+7.57 sec in the 15-150 keV band is
19.9 +- 0.6 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.36 +- 0.03 (chi squared 37 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/313299/BA/


GRB_name: GRB080603B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7840
SUBJECT: GRB 080603B: VLA radio upper limit
DATE:    08/06/06 17:38:37 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
080603B (GCN 7794) at a frequency of 8.46 GHz on 2008 June 05.16 UT.
The GRB radio afterglow is undetected and the peak radio flux at the
SWIFT-UVOT position (GCN 7794) is 11  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: GRB080605A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7841
SUBJECT: GRB 080605, Swift-BAT refined analysis
DATE:    08/06/06 17:44:56 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

J. Cummings (GSFC/UMBC), S. D. Barthelmy (GSFC), W. Baumgartner (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 (ISAS),
M. Stamatikos (GSFC/ORAU), B. Sbarufatti (INAF-IASFPA), J. Tueller (GSFC),
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 080605 (trigger #313299)
(Sbarufatti, et al., GCN Circ. 7828).  The BAT ground-calculated position is
RA, Dec = 262.130, 4.010 deg, which is 
   RA(J2000)  =  17h 28m 31.1s 
   Dec(J2000) = +04d 00' 35.6" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 41%.
 
The mask-weighted light curve shows a cluster of overlapping peaks
starting at ~T-3 sec, the largest peak at ~T+8 sec, and all ending at ~T+70 sec.
At the 1-2 sigma level, there is appears to be persistant emmission
in the T+300 to T+700 sec range.  T90 (15-350 keV) is 20 +- 1 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-5.5 to T+30.0 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 1.11 +- 0.14, 
and Epeak of 223 +- 133 keV (chi squared 28.10 for 56 d.o.f.).   For this
model the total fluence in the 15-150 keV band is 1.33 +- 0.02 x 10^-5 erg/cm2
and the 1-sec peak flux measured from T+7.57 sec in the 15-150 keV band is
19.9 +- 0.6 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.36 +- 0.03 (chi squared 37 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/313299/BA/


GRB_name: GRB080604A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7842
SUBJECT: GRB 080604: VLA radio upper limit
DATE:    08/06/06 17:49:20 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
080604 (GCN 7800) at a frequency of 8.46 GHz on 2008 June 05.22 UT.
The GRB radio afterglow is undetected and the peak radio flux at the
SWIFT-UVOT position (GCN 7800) is -8  39 uJy.

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


GRB_name: GRB080603A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7843
SUBJECT: Possible VLA radio detection on INTEGRAL burst GRB 080603A
DATE:    08/06/06 18:06:15 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 INTEGRAL
GRB 080603A (GCN 7790) at a frequency of 8.46 GHz on 2008 June 05.39 UT.
We detect a possible radio afterglow at KAIT optical afterglow position
(GCN 7789) at a flux density level of 116 +/- 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: GRB080605A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7844
SUBJECT: GRB 080605: Swift-UVOT refined analysis
DATE:    08/06/06 20:45:57 GMT
FROM:    Paul Kuin at MSSL  <npkuin@googlemail.com>

N. P. M. Kuin (MSSL/UCL),  B. Sbarufatti (INAF-IASFPA), F. Marshall (GSFC),
and P.Schady (MSSL/UCL), report on behalf of the Swift UVOT team

The Swift UltraViolet/Optical Telescope (UVOT) began observations
of GRB 080605, on June 5, 2008, at  23:49:19 UT,  82 seconds after
the initial Swift BAT trigger (Mangano et al., GCN Circ. 7794), and
started the finding chart exposure in the white filter at 102
seconds after the trigger.

The refined uvot position of GRB080605 is RA=262.12522, Dec=+4.01555
deg.(= 17:28:30.05 +04:00:55.97), with an accuracy of 0.5", consistent
with the positions reported in GCN Circ. 7830 (Holland et al.) and
7835 (Goad et al.).

The GRB is found close (about 4" distant) to a star, which may cause
an error in the measured flux, especially at later times. For this
analysis we use a small 2" aperture which which reduces the
contamination, and apply a standard aperture correction. We note that
the DSS image indicates the presence of a weak, possibly extended
source near the position of the afterglow.

The magnitudes with 1-sigma errors for GRB080605 are given below
for the initial observation sequence.

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

wh      102      201     98.2    18.11 +/- 0.06
v       208      607    393.5    18.53 +/- 0.11
wh      858      957     98.2    20.02 +/- 0.17
uvm2    615      788     38.9   >18.38 (3 sigma UL)
uvw1    639      813     38.9   >18.95 (3 sigma UL)
uvw2    720      739     19.5   >18.16 (3 sigma UL)
b     27679    28264    571.7    21.10 +/- 0.27
u     18432    41856    550.7    21.17 +/- 0.43

The values quoted above are on the UVOT Photometric System
(Poole et al, 2008, MNRAS 383,627). They are not corrected for the
expected galactic reddening of E(B-V) = 0.137 in the direction of
the burst (Schlegel et al. 1998).


GRB_name: GRB080605A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7845
SUBJECT: GRB 080605: TLS RRM Analysis, Plateau/Rebrightening, Red OT
DATE:    08/06/07 02:27:14 GMT
FROM:    Alexander Kann at TLS Tautenburg  <kann@tls-tautenburg.de>

D. A. Kann, U. Laux and S. Ertel (TLS Tautenburg) report:

We continue observations of the afterglow of GRB 080605 (independently 
discovered by Sbarufatti et al., GCN 7828, Kann et al., GCN 7829, and 
Gomboc et al., GCN 7831). We acquired one 300 sec image each in V, R, and 
I around 0.95 days after the GRB, and further imaging 0.1 days later until 
dawn. Astonishingly, the afterglow is still clearly visible in R and I 
bands.

As mentioned in the above-cited GCNs, the afterglow is close to a star and 
affected by its PSF in images with low-quality seeing or large pixel 
scale, such as the TLS camera. To obtain a qualitative description of the 
afterglow evolution, we perform aperature photometry in a 3 pixel 
aperature, and derive the aperature correction for each image by comparing 
the counts for a reference star in the 3 pixel aperature with that in a 7 
pixel (which is typically seeing-matched) aperature. As a reference star, 
we use the star to the south of the afterglow, USNOB1.0 ID 0940-0289655 at 
(catalog position): RA = 17:28:29.920, Dec. = +04:00:36.51, which has R2 = 
15.90 mag, I = 14.54 mag. We derive the following magnitudes for selected 
images in the I band (the error is estimated to be 0.1 magnitudes in all 
cases):

dt  I

0.00478791 16.74
0.00674681 17.18
0.00869923 17.36
0.01064872 17.61
0.01849396 18.19
0.02433042 18.19
0.05922051 18.48
0.96109933 18.51
1.05275325 18.71

The early afterglow decay (0.00479 to 0.01849 days) is well-described by a 
power-law with decay slope alpha=0.97. After this, the afterglow decay 
seems to flatten. Between 0.06 days and 0.95 days, the afterglow magnitude 
remains unchanged, indicating a plateau phase. As the afterglow has 
resumed its decay 0.1 days later, this probably implies that the 
afterglow underwent a strong rebrightening which we caught after the 
peak. This is reminiscent of GRB 071003, which lies at a very similar 
redshift (Perley et al. 2008, ApJ, submitted, arXiv:0805.2394) of ~ 1.6 
(Jakobsson et al., GCN 7832).

Furthermore, we determined the R band magnitude at two epochs:

dt  R

0.01655957 19.87
0.95457023 20.75

Corrected for the moderate Galactic foreground extinction of E(B-V) = 
0.136, we find R - I ~ 2 mag. This is a very red color for an afterglow, 
indicating strong internal reddening due to dust. We caution that the 
USNOB1.0 comparison star may have incorrect photometry, on the other hand, 
a simple image comparison shows that the R band magnitude is much fainter 
than the I band magnitude.

The strong rebrightening combined with the large correction for dust 
extinction that is needed imply that this is an intrinsically extremely 
luminous afterglow. Further follow-up, especially in the NIR bands, is 
highly encouraged.

This message may be cited.


GRB_name: GRB080607A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7846
SUBJECT: GRB 080607: ROTSE-III Detection of Optical Counterpart
DATE:    08/06/07 06:11:50 GMT
FROM:    Wiphu Rujopakarn at U AZ/Steward  <wiphu@as.arizona.edu>

W. Rujopakarn (Steward), E.S. Rykoff (UCSB), report on behalf of the ROTSE
collaboration:

ROTSE-IIIb, located at McDonald Observatory, Texas, responded to GRB
080607 (Swift trigger 313417). The first image was at 06:07:49.0 UT, 22.0
s after the burst (6.0 s after the GCN notice time). The unfiltered images
are calibrated relative to USNO A2.0. We detect a 14.8 magnitude, fading
source with coordinates:

     12:59:47.3      +15:55:10.8    (J2000), with positional uncertainty
of 1" or better

start UT     mag     mlim(of image)
----------------------------------
06:07:49.0     14.8     16.4


This source is not visible in DSS (second epoch), 2MASS or the MPChecker
database.

A jpeg image is available at
http://www.rotse.net/images/gsb313417_3b00_img.jpg Note that the object
marked 11 is the candidate in question.

Continuing observations are in progress.


GRB_name: GRB080607A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7847
SUBJECT: GRB 080607: Swift detection of a burst with optical afterglow
DATE:    08/06/07 06:21:44 GMT
FROM:    Vanessa Mangano at INAF-IASFPA  <vanessa@ifc.inaf.it>

V. Mangano (INAF-IASFPA), J. R. Cummings (NASA/UMBC),
G. Cusumano (INAF-IASFPA), N. Gehrels (NASA/GSFC),
V. La Parola (INAF-IASFPA), C. B. Markwardt (CRESST/GSFC/UMD),
J. P. Osborne (U Leicester), B. Sbarufatti (INAF-IASFPA) and
D. E. Vanden Berk (PSU) report on behalf of the Swift Team:

At 06:07:27 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 080607 (trigger=313417).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 194.967, +15.900 which is 
   RA(J2000) = 12h 59m 52s
   Dec(J2000) = +15d 54' 01"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a multi-peak
structure with a duration of about 80 sec.  The peak count rate
was ~35000 counts/sec (15-350 keV), at ~2 sec after the trigger. 

The XRT began observing the field at 06:08:49.1 UT, 82.1 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 194.9462, +15.9208 which is equivalent to:
   RA(J2000)  = 12h 59m 47.0s
   Dec(J2000) = +15d 55' 14.8"
with an uncertainty of 5.0 arcseconds (radius, 90% containment). This
location is 103 arcseconds from the BAT onboard position, within the
BAT error circle. No event data are yet available to determine the
column density using X-ray spectroscopy. 


UVOT took a finding chart exposure of 100 seconds with the White (160-650 nm)
filter starting 92 seconds after the BAT trigger. There is a candidate
afterglow in the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  = 12:59:47.21 = 194.9467
  DEC(J2000) = +15:55:10.9  =  15.9197
with a 1-sigma error radius of about 0.5 arc sec. This position is 4.9 arc sec. 
from the center of the XRT error circle. The estimated magnitude is 19.7 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 0.02. 




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


GRB_name: GRB080607A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7848
SUBJECT: GRB 080607: Super-LOTIS early observations
DATE:    08/06/07 06:50:38 GMT
FROM:    Adria C. Updike at Clemson U  <aupdike@clemson.edu>

Adria C. Updike (Clemson University), Peter A. Milne (Steward
Observatory), and G. Grant Williams (MMTO) report:

Super-LOTIS began observing GRB 080607 35 second after the trigger
(313417).  We detect the fading source reported by Rujopakarn et al. (GCN
7846) at R = 15.2 +/- 0.05 mag (as compared to a nearby star in the USNO
B1.0 catalog) 40 seconds after the trigger. Observations are continuing.

This message may be cited.


GRB_name: GRB080607A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7849
SUBJECT: GRB 080607: Keck/LRIS spectroscopy and redshift
DATE:    08/06/07 07:47:19 GMT
FROM:    Daniel Perley at U.C. Berkeley  <dperley@astro.berkeley.edu>

J. X. Prochaska (UCO/Lick), J. Shiode, J. S. Bloom, D. A. Perley, A. A. 
Miller, J. Shiode, D. Starr, R. Kennedy, and J. Brewer (UC Berkeley) report:

Upon receiving the GCN alert we immediately slewed with Keck I (+LRIS) 
to the field of GRB 080607 (GCN 7847, Mangano et al.).  The optical 
transient (GCN 7846, Rujopakarn et al.) was visually identified on the 
guider.  Spectroscopic observations began at 06:20:35 UT, 13 minutes 
after the trigger, using the 600 and 400 line gratings on the blue and 
red cameras, respectively, for wavelength coverage between 3000-9300 A.

Our preliminary reduction of the LRIS-b spectrum reveals a very strong, 
damped Lya profile and metal-line transitions of OI, SiII, CII, SiII* 
among others.  These establish the redshift of the GRB to be z=3.036.


GRB_name: GRB080607A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7850
SUBJECT: GRB 080607 - PAIRITEL NIR detection
DATE:    08/06/07 07:53:03 GMT
FROM:    Adam Miller at UC Berkeley  <amiller@astro.berkeley.edu>

A. A. Miller, J. S. Bloom, D. A. Perley (UC Berkeley), D. Starr (UCB, 
LCOGT) report:

We observed the optical afterglow of GRB 080607 (Mangano et al., GCN 
7847, Rujopakarn et al., GCN 7846) with the 1.3m Peters Automated Infrared 
Imaging Telescope (PAIRITEL). Observations began at 06:08:44 Jun 07, 
2008 UT. We detect the afterglow in a 612 sec mosaic of 7.8 sec 
simultaneous exposures in the J, H, and Ks filters. Preliminary 
photometry for the afterglow in exposures beginning on 06:10:32 Jun 07, 
2008 UT yields J = 17.1 +- 0.1, H = 15.3 +- 0.1, and  Ks = 13.7 +- 0.1, 
calibrated to the 2MASS system.


GRB_name: GRB080605A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7851
SUBJECT: GRB 080605: GROND 2nd epoch observations
DATE:    08/06/07 09:44:28 GMT
FROM:    Christian Clemens at MPE  <cclemens@mpe.mpg.de>

C. Clemens, A. Kupcu Yoldas, J. Greiner, T. Kruehler, A. Yoldas (all MPE 
Garching) and G. Szokoly (Eoetvoes Univ., Budapest and MPE Garching) report 
on behalf of the GROND team:

We observed the field of GRB 080605 for a second time at 02:43 UT on June 7th, 
2008 about 1.12 days after the GRB trigger with 25 mins of effective 
exposures in g'r'i'z'.

We still detect the bright afterglow within the refined 0.5'' Swift-UVOT error 
circle (Kuin et al., GCN #7844) to the following preliminary magnitudes of

r' = 22.3,
i' = 21.7 and
z' = 21.4

with typical errors of +/- 0.1. Given magnitudes are calibrated against 
USNO-B1 field stars and might be affected by the bright, nearby star.

This indicates a clear fading of the optical afterglow compared to our first 
epoch observations (C. Clemens et al., GCN #7834).

Please note, that no correction for the galactic foreground reddening of 
E(B-V) = 0.136 mag (Schlegel et al., 1998) has been applied.


GRB_name: GRB080607A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7852
SUBJECT: GRB 080607, Swift-BAT refined analysis
DATE:    08/06/07 12:03:45 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

M. Stamatikos (GSFC/ORAU), S. D. Barthelmy (GSFC), W. Baumgartner (GSFC/UMBC),
J. Cummings (GSFC/UMBC), E. Fenimore (LANL), N. Gehrels (GSFC),
H. Krimm (GSFC/USRA), V. Mangano (INAF-IASFPA), C. Markwardt (GSFC/UMD),
K. McLean (GSFC/UMD), D. Palmer (LANL), T. Sakamoto (GSFC/UMBC),
G. Sato (ISAS), J. Tueller (GSFC), T. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using the data set from T-240 to T+302 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 080607 (trigger #313417)
(Mangano, et al., GCN Circ. 7847).  The BAT ground-calculated position is
RA, Dec = 194.964, 15.910 deg, which is 
   RA(J2000)  =  12h 59m 51.4s 
   Dec(J2000) = +15d 54' 37.6" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 11%.
 
The mask-weighted light curve shows multiple peaks.  The first starts at ~T-5 sec.
The main cluster of overlapping peaks starts at ~T-1 sec, with the brightest
peak at T+2.0 sec, and ending at ~T+10 sec.  Following that is a series 
of weak peaks out to ~T+180 sec.  T90 (15-350 keV) is 79 +- 5 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-5.9 to T+154.7 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.31 +- 0.04.  The fluence in the 15-150 keV band is 2.4 +- 0.0 x 10^-05 erg/cm2.
The 1-sec peak photon flux measured from T+1.50 sec in the 15-150 keV band
is 23.1 +- 1.1 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/313417/BA/


GRB_name: GRB080607A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7853
SUBJECT: GRB 080607: Enhanced Swift-XRT position
DATE:    08/06/07 13:22:23 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 818 s of overlapping XRT Photon Counting mode and UVOT
data for GRB 080607, 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 = 194.94644, +15.91935 which is equivalent
to:

RA (J2000): 12h 59m 47.15s
Dec (J2000): +15d 55' 09.7"

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: GRB080605A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7854
SUBJECT: Konus-Wind observation of GRB 080605
DATE:    08/06/07 16:02:39 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 080605 (Swift-BAT trigger #313299: Sbarufatti et al., GCN
7828, Cummings et al., GCN 7839) triggered Konus-Wind at T0=85682.336 s 
UT (23:48:02.336).

The burst light curve shows a multipeaked structure with a total 
duration of ~20s.

As observed by Konus-Wind the burst
had a fluence of 3.02(-0.12, +0.13)x10^-5 erg/cm2,
and a 16-ms peak flux measured from T0+7.984 s
of (1.60 +/- 0.33)x10^-5 erg/cm2/s
(both in the 20 keV - 2 MeV energy range).

The time-integrated spectrum of the burst
(from T0 to T0+18.944 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 = -1.03 +/- 0.07,
and Ep = 252(-17, +20) keV (chi2 = 57.2/61 dof).
Fitting by GRBM (Band) model yields:
the low-energy photon index is alpha = -1.02 +/- 0.08,
the high energy photon index beta < -2.75,
the peak energy Ep =  246(-18, +23) keV (chi2 = 56.7/60 dof).

The spectrum of the most intense peak (from T0+7.168 s to T0+8.960 s)
is well fitted (in the 20 keV - 2 MeV range)
by a power law with exponential cutoff model
with alpha =  -0.94 +/- 0.10
and Ep = 333(-34, +42) keV (chi2 = 60.6/54 dof).
Fitting by GRBM (Band) model yields:
the low-energy photon index is alpha = -0.87(-0.12, +0.13),
the high energy photon index beta = -2.58(-0.84, +0.31),
the peak energy Ep =  297(-40, +46) keV (chi2 = 56.6/53 dof).

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

Assuming z = 1.640 (Jakobsson et al., GCN 7832) and a standard
cosmology model with H_0 = 70 km/s/Mpc, Omega_M = 0.27, Omega_\Lambda =
0.73, the isotropic energy release is E_iso ~2.1x10^53 erg,
the maximum luminosity is (L_iso)_max ~3.0x10^53 erg/s, and
Ep_rest ~660 keV.

The Konus-Wind light curve of this GRB is available
at http://www.ioffe.rssi.ru/LEA/GRBs/GRB080605_T85682/


GRB_name: GRB080603A
Detection_method: VLA Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7855
SUBJECT: VLA detection of INTEGRAL burst GRB 080603A
DATE:    08/06/07 16:36:25 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 re-observe the field of view toward 
INTEGRAL GRB 080603A (GCN 7790) at a frequency of 8.46 GHz on 2008 June 
07.42 UT. We clearly detect a radio afterglow at KAIT optical afterglow 
position (GCN 7789) at a flux density level of 154  28 uJy.

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


GRB_name: GRB080607A
Detection_method: KAIT
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7856
SUBJECT: GRB 080607 KAIT observations
DATE:    08/06/07 19:16:14 GMT
FROM:    Ryan Chornock at UC Berkeley  <chornock@astro.berkeley.edu>

R. Chornock, W. Li, and A. V. Filippenko (UC Berkeley) report:

The Katzman Automatic Imaging Telescope (KAIT) at Lick Observatory responded to 
the Swift alert for GRB 080607 (Mangano et al., GCN 7847) and detected the 
optical afterglow previously announced by several other teams (Rujopakarn et 
al., GCN 7846; Mangano et al., GCN 7847; Updike et al., GCN 7848; Prochaska et 
al., GCN 7849; Miller et al., GCN 7850).

KAIT took a series of V, I, and unfiltered images starting at 06:09:25 (UT), 
118s after the BAT trigger.  The KAIT position is:
   (J2000) 12:59:47.22  +15:55:11.0

The preliminary unfiltered light curve shows a power-law decay from magnitude 
17.60 at t=188s with a decay index of alpha = -1.27 +/- 0.09.


GRB_name: GRB080605A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7857
SUBJECT: GRB 080605: optical observations
DATE:    08/06/07 19:42:52 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

V. Rumyantsev (CrAO),  A. Pozanenko (IKI) report on behalf of larger GRB 
follow-up collaboration:

We observed the optical afterglow of  Swift GRB 080605 (Sbarufatti  et al., 
GCN 7828) in second epoch on June 06  with Zeiss-1000 (Simeiz) telescope of 
CrAO observatory with favorable weather conditions and seeing about 2".  Our 
first epoch astrometry of the source  (Rumyantsev et al., GCN 7833) is in 
agreement with  refined UVOT position of GRB080605 (Kuin et al.,  GCN 7844).
The observation of the first epoch started  8 minute after burst onset 
(Rumyantsev et al., GCN 7833) was performed under descending weather 
conditions with seeing about 3". Improved photometry of the first epoch 
observation as well as observation on June 6 is based on USNO-B1.0 star RA 
(J2000) = 17 28 29.92, Dec.(J2000) = +04 00 36.5, assuming R=15.90, I=14.54:


T0+          Exposure,   Filter,  mag,
(d,mid time)

  0.006251 120    R  18.04 +/- 0.08
  0.007698 120    R  18.43 +/- 0.06
  0.009457 120    R  18.62 +/- 0.06
  0.010985 120    R  18.63 +/- 0.23
  0.015163 120    R  18.93 +/- 0.23
  0.018068 120    R >19.04
  0.019504 120    R  18.86 +/- 0.20
  0.026031 120    I  18.12 +/- 0.28
  0.033219 120    V >17.50
  0.034654 120    V >18.20
  0.904028 34x120 R  21.13 +/- 0.06

The photometry is still preliminary and not corrected for Galaxy extinction 
and  might be affected by the bright, nearby star.

It is evident that the source is faded between June 5 and June 6. Power law 
index of early afterglow decay ~0.8 is compatible with index obtained in 
I-band (Kann et al., GCN 7845). However our absolute photometry in R-band 
have a significant offset in comparison with early observations by Kann et 
al. (GCN 7845) and compatible with photometry of Gomboc et al. (GCN 7831). 
Our early observation suggests R-I ~ 1.2, however we caution the color of 
the afterglow is also depending on photometry which is affected by bright, 
nearby star.

The message may be cited. 


GRB_name: GRB080607A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7858
SUBJECT: Swift/UVOT Observations of GRB080607
DATE:    08/06/07 21:15:59 GMT
FROM:    Patricia Schady at MSSL/Swift  <ps@mssl.ucl.ac.uk>

P. Schady (MSSL/UCL) and V. Mangano (INAF-IASFPA) report on behalf of the
Swift UVOT team

The Swift UltraViolet/Optical Telescope (UVOT) began taking settled 
observations of GRB 080607 92 seconds after the initial Swift BAT trigger 
(Mangano et al., GCN Circ. 7847). A faint afterglow is detected in the first 
white and v-band finding chart exposures only at the refined uvot position of 
RA=194.94665, Dec=+15.91965 deg.(= 12:59:47.20 +15:55:10.74), with an accuracy 
of 0.5". This is consistent with the GRB being at a redshift of z=3.036, as 
reported in GCN Circ. 7849 (Prochaska et al.)

The first white and v-band finding chart magnitudes with 1-sigma errors are 
given below, as well as the 3-sigma upper limits for co-added images from later 
observations.

Filter Tmid(s) Exp(s)  Magnitude/3-sig UL
---------------------------------------------
wh     190.9     98.2    19.79 +/- 0.13
wh     4806.9    510.6   > 22.07
v      594.6     393.5   19.44 +/- 0.19
v      4048.5    300.2   > 20.11
b      5527.9    412.5   > 21.28
u      4934.2    432.2   > 20.93
uvw1   4934.2    432.1   > 20.80
uvm2   4745.1    432.1   > 20.57
uvw2   5745.6    358.5   > 20.83
---------------------------------------------

where Tmid is the weighted mid time of the observation. The values quoted above 
are on the UVOT Photometric System (Poole et al, 2008, MNRAS 383,627). They are 
not corrected for the expected galactic reddening of E(B-V) = 0.02 in the 
direction of the burst (Schlegel et al. 1998).


GRB_name: GRB080607A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7859
SUBJECT: GRB 080607: Swift-XRT refined analysis
DATE:    08/06/07 22:46:45 GMT
FROM:    Boris Sbarufatti at INAF-IASF-Pa  <sbarufatti@ifc.inaf.it>

B. Sbarufatti, V. Mangano, V. La Parola (INAF-IASF Pa) report on  
behalf of
the Swift-XRT team.


Swift-XRT began observations of the field of GRB 080607 (trigger 313417,
Mangano et al., GCN circ. 7847) on date 2008 June 07, 06:08:54 UT, 87 s
after the BAT trigger. The data consist of 478 s in Windowed timing mode
and 3 ks in Photon Counting mode.

The lightcurve shows a complex behaviour. After an initial steep decay
(index 5.8 +/- 0.4) we observe a double peaked flare, starting at
T+ 118 (+/- 1) s and peaking at T+120 s and T+140 s. The underlying
decay breaks at T+ 119 (+ 5, - 2) s to a slope of 1.7 (+/- 0.1). A
second break at t+700 (+/- 300) marks the beginning of a plateau phase
(index 0.5 +/- 1.3). The lightcurve breaks again around
T+1600 (+/- 500) s, with a final decay index of -2.0 +/- 0.5.
The countrate predictions for T+24h and T+48h are 2.1E-3 counts/s
and 5.5E-4 count/s respectively.

The WT spectrum can be fit by a powerlaw with photon index 1.81 +/- 0.02
and an intrinsic absorbing column density of (4.0 +/- 0.2)E22 cm^-2 at
z=3.036 (Prochaska et al. GCN Circ. 7849), in excess with
respect to the Galactic value of 1.69E+20 cm^-2 (Kalberla et al. 2005).
The observed (unabsorbed) flux in the 0.3 - 10 keV band is
2.9 (3.0)E-9 erg cm^-2 s^-1.
The PC spectrum can be fit by a powerlaw with photon index 2.1 +/- 0.1
and an intrinsic absorbing column density of (4.0 +/- 0.8)E22 cm^-2 at
z=3.036, in excess with respect to the Galactic value. The observed
(unabsorbed) flux in the 0.3 - 10 keV band is
5.3 (5.4)E-11 erg cm^-2 s^-1.

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

[GCN OPS NOTE(08jun08): Per author's request, the "(4.0 +/- 0.8)E21"
was changed to "(4.0 +/- 0.8)E22".]


GRB_name: GRB080603A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7860
SUBJECT: GRB 080603A: optical observations
DATE:    08/06/07 22:52:28 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

V. Rumyantsev (CrAO),  A. Pozanenko (IKI) report on behalf of larger GRB 
follow-up collaboration:

We observed  a field of  INTEGRAL GRB 080603A (Paizis et al., GCN 7790) in 
R-band on June 06 between (UT) 22:32 - 23:55 with  Zeiss-1000 (Simeiz) 
telescope of CrAO observatory.   Extended object is found ~1" south from the 
position of optical afterglow (Gomboc et al., GCN 7788; Chornock  et al., 
GCN 7789), and the position of the extended object is consistent with 
coordinates reported by Kuin et al. (GCN 7804). Therefore, we suggest it as 
a host galaxy of  080603A.

Based on  USNOB1.0 star with ID 1527-0313986 at RA = 18:37:55.186, Dec. 
+62:45:32.28 (R1 = 16.74)  we estimated brightness of  the extended object:

UT,       Exposure,   R_mag, UL
(mid time)

3.496  41x120  21.90  +/- 0.17  22.85

If the extended source is the host galaxy then contamination by the host can 
explain slow decay of light curve noted by Kann et al. (GCN 7822).

A combined image can be found at
http://grb.rssi.ru/GRB080603A/GRB080603A_2080606.gif

The message may be cited. 


GRB_name: GRB080607A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7861
SUBJECT: GRB080607: RTT150 optical observations
DATE:    08/06/08 00:23:07 GMT
FROM:    Irek Khamitov at TUG  <irekk@tug.tug.tubitak.gov.tr>

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

report:

We observed the field of optical afterglow (GCN7846) of GRB080607
(GCN 7847, SWIFT trigger=313417) with Russian-Turkish 1.5-m  telescope
(RTT150, Bakirlitepe, TUBITAK National Observatory, Turkey), starting
at 07 June, 18:35 UT, i.e. ~12.4 hours after the burst, using Andor CCD.

We made a set of 4*300s exposures in BRc bands. We detect nothing at the 
position of the OT (GCN7846, GCN7858) on co-added frames with limiting 
magnitudes B~22.2 and Rc~22.2

-- 
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GRB_name: GRB080607A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7862
SUBJECT: Konus-Wind observation of GRB 080607
DATE:    08/06/08 15:49:55 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, P. 
Oleynik, M. Ulanov, D. Svinkin, and
T. Cline on behalf of the Konus-Wind team report:

The bright GRB 080607 (Swift-BAT trigger #313417: Mangano et al., GCN
7847, Stamatikos et al., GCN 7852) triggered Konus-Wind at T0=22043.336 
s UT (06:07:23.336).

The burst light curve consists of the main part, which shows a 
multipeaked structure with a duration of ~16 s, and the extended 
emission, which shows many weak pulses up to ~T0+85 s in the soft energy 
band (~18-70 keV).

As observed by Konus-Wind the burst
had a fluence of 8.93(-0.47, +0.52)x10^-5 erg/cm2,
and a 16-ms peak flux measured from T0+7.168 s
of (2.69 +/- 0.54)x10^-5 erg/cm2/s
(both in the 20 keV - 4 MeV energy range).

The time-integrated spectrum of the burst
(from T0 to T0+84.48 s) can be fitted (in the 20 keV - 4 MeV range)
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with alpha = -1.08(-0.06, +0.07),
and Ep = 419(-38, +46) keV (chi2 = 78.8/73 dof).
Fitting by GRBM (Band) model yields:
the low-energy photon index is alpha = -1.06(-0.08, +0.09),
the high energy photon index beta < -2.28,
the peak energy Ep = 394(-54, +58) keV (chi2 = 77.2/72 dof).

The spectrum of the main part
(from T0 to T0+18.944 s) can be fitted (in the 20 keV - 4 MeV range)
by GRBM (Band) model for which:
the low-energy photon index is alpha = -0.76(-0.06, +0.07),
the high energy photon index beta = -2.57(-0.26, +0.18),
the peak energy Ep = (348 +/- 27) keV (chi2 = 99.6/72 dof).
The fluence of this part is (8.59 +/- 0.40)x10^-5 erg/cm2.

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

Assuming z = 3.036 (Prochaska et al., GCN 7849) and a standard
cosmology model with H_0 = 70 km/s/Mpc, Omega_M = 0.27, Omega_\Lambda =
0.73, the isotropic energy release is E_iso = 1.87(-0.10, +0.11)x10^54 
erg, the peak luminosity is (L_iso)_max = (2.27 +/- 0.46)x10^54 erg/s, 
and Ep_rest ~1600 keV.
This isotropic energy release is one of the largest ever measured
(the current record holder is GRB 990123 for which the isotropic energy 
release is ~2.8x10^54 erg), and this peak luminosity is the highest ever 
reported.

The Konus-Wind light curve of this GRB is available
at http://www.ioffe.rssi.ru/LEA/GRBs/GRB080607_T22043/


GRB_name: GRB080605A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7863
SUBJECT: GRB080605: optical observation with the MITSuME-OAO telescope 
DATE:    08/06/09 00:24:33 GMT
FROM:    Michitoshi Yoshida at Okayama Astrophysical Obs  <yoshida@oao.nao.ac.jp>

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

We performed optical imaging observation (Rc, and Ic) of the field
of GRB 080605 (Sbarufatti et al., GCN 7828) with 50cm MITSuME
telescope at Okayama Astrophysical Observatory June 6 2008 UT.
We detected a point source at the UVOT position of the optical
afterglow (Kuin et al., GCN 7844). Differential photometry was
made using a USNO B1.0 star, USNO-ID 0940-0289655 (Kann et al.,
GCN 7845). The Ic-band magnitude of the source was almost constant
from T-T0 = 0.516 to 0.756. The source is about 1.5 magnitude
fainter in Rc-band than in Ic-band. These results are consistent
with other reports (Kann et al., GCN 7845, Rumyantsev et al.,
GCN 7857).


MITSuME observation start: 2008-06-06 11:35:11 UT

mid-UT        T-T0(days)   exp-T         Ic
(2008-06-06)
---------------------------------------------------
12:11:27      0.516314     60 min    19.03 +/- 0.38
12:48:05      0.541753     60 min    19.00 +/- 0.29
14:00:54      0.592315     60 min    18.85 +/- 0.18
15:15:44      0.644288     60 min    19.03 +/- 0.22
16:30:50      0.696429     60 min    18.82 +/- 0.21
17:56:24      0.755856     80 min    18.87 +/- 0.30
---------------------------------------------------

mid-UT
(2008-06-06)  T-T0(days)   ext-T          Rc
---------------------------------------------------
15:52:20      0.669745     120 min   20.58 +/- 0.32
---------------------------------------------------


GRB_name: GRB080605A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7864
SUBJECT: GRB 080605: TLS 3rd Epoch - Source Confusion
DATE:    08/06/09 01:24:01 GMT
FROM:    Alexander Kann at TLS Tautenburg  <kann@tls-tautenburg.de>

D. A. Kann, U. Laux & S. Ertel (TLS Tautenburg) report:

We obtained further images of the Swift GRB 080605 (Sbarufatti et al., GCN 
7828). A 300 second Ic frame obtained under excellent observing conditions 
shows the field remains unchanged in comparison to the second epoch as 
well as the final images of the first epoch (Kann et al., GCN 7845). 
Recently, Yoshida et al. (GCN 7863) also claimed detection of a plateau 
phase. Clemens et al. (GCN 7851), on the other hand, report a clear fading 
of the afterglow, as well as only a moderately red color in comparison to 
Kann et al. (GCN 7845), which can possibly be explained by the moderate 
Galactic reddening alone.

Comparison with a multicolor finding chart taken by GROND (C. Clemens, 
priv. comm.) reveals the culprit: source confusion. Near the position of 
the afterglow, there are in total three sources, all seemingly stellar in 
GROND images, along a line. The star to the southeast (Source #1) was 
immediately reported (Sbarufatti et al., GCN 7828, Kann et al., GCN 7829) 
and is clearly visible in the DSS. To the northwest, there is another 
source (Source #2), also clearly visible in the DSS. An inspection of the 
DSS IR frame reveals that #2 is hardly visible at all, but a new source 
(Source #3), inbetween #1 and #2, now becomes clearly visible. This source 
is extremely red, possibly a red dwarf, and it is THIS source which begins 
to dominate the photometry reported in Kann et al. (GCN 7845) (and 
presumably Yoshida et al., GCN 7863), which is mostly I band. The small 
offset from source #1 lead us to believe that this is the afterglow (and 
explained the puzzling observation that it seemed to slightly shift 
position).

Therefore, we retract the identification of a plateau phase of the 
afterglow of GRB 080605, as well as the claim of extreme redness and the 
resulting high lumonisity around 1 day in the observer frame. On the other 
hand, the afterglow IS clearly detected on the early I band frames of the 
TLS RRM observation, as well as in the R band and a stacked V band frame. 
The early photometry, which leads to a decay slope of alpha ~ 1, is still 
valid. Image subtraction will have to be performed to see how many 
detections we have actually gotten.

This message may be cited.


GRB_name: GRB080603B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7865
SUBJECT: GRB 080603B - TLS 2nd Epoch: Another Break
DATE:    08/06/09 02:33:11 GMT
FROM:    Alexander Kann at TLS Tautenburg  <kann@tls-tautenburg.de>

D. A. Kann, U. Laux and S. Ertel (TLS Tautenburg) report:

We observed again the field of the Swift GRB 080603B (Mangano et al., GCN 
7794) with the TLS 1.34m Schmidt telescope. The observing conditions 
changed rapidly, from passing clouds and moonlight to excellent 
conditions. We obtained a total of 11 x 600 sec images in the R band. The 
first five images were lost due to high background as well as passing 
clouds. We stacked the final six images, which have a mid-time of June 
8.98085. The afterglow (Rujopakarn, Guver, & Smith, GCN 7792) is not 
detected anymore in the stack. Using the same comparison star as Kann et 
al. (GCN 7823), we derive a 2 sigma upper limit of R > 23.7 at 5.132644 
days after the GRB.

Comparing this value with the one determined at 1.16 days after the GRB by 
Kann et al. (GCN 7823) (R = 21.32), we find a decay slope alpha > 1.47. 
While this does not allow any assertion on the reality of the steep decay 
slope (alpha ~ 2.5) reported by Kann et al. (GCN 7823), it is steeper than 
the slope reported (alpha_R=-1.14+/-0.09) by Zhuchkov et al. (GCN 7803) 
and confirmed by Xin et al. (GCN 7814), indicating that another break in 
the light curve must have occurred, independent of calibration issues. As 
the slope reported by Zhuchkov et al. (GCN 7803) is much too shallow to be 
a post-jet break slope, this indicates that the second break is very 
probably a jet break. The slope reported by Kann et al. (GCN 7823) is in 
accordance with a post-jet break slope. This then leads to the interesting 
question of the origin of the first break Zhuchkov et al. detected, as it 
is much to strong to be a cooling break (Delta alpha_R = 0.55 versus the 
theoretical value of Delta alpha = 0.25 for a cooling break).

This message may be cited.


GRB_name: GRB080607A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7866
SUBJECT: GRB 080607: AGILE-MCAL observation of the prompt emission
DATE:    08/06/09 15:44:57 GMT
FROM:    Marco Feroci at IASF/INAF  <feroci@iasf-roma.inaf.it>

M. Marisaldi, F. Fuschino, M. Galli, C. Labanti, 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), F. 
Fornari, 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 080607 (Mangano et al., GCN 7847; Stamatikos et 
al., GCN 7852) triggered the Mini-Calorimeter (MCAL) instrument onboard 
the AGILE satellite at 06:07:23 UT (=T0). The MCAL instrument covers the 
energy range 350 keV - 10 MeV, without imaging capabilities.

Using the preliminary in-flight calibration and assuming a Crab-like 
spectrum, we can estimate the fluence in the 350-700 keV energy band to be 
(23 +/- 7) photons/cm2 corresponding to (1.8 +/- 0.5)x10^-5 erg/cm2, in 
the time interval T0-T0+14 s. The 1-s peak flux measured at T0+5.1 s is 
(4.2 +/- 1.2) photons/cm2/s in the same energy band. The GRB was detected 
also in the 1.4-2.8 MeV energy band with a 10 sigma significance in the 
256-ms time window. 

We note that the quoted fluence is in agreement within errors with that 
obtained using the Konus-Wind spectrum reported in Golenetskii et al., GCN 
7862. Assuming the spectral model reported in GCN 7862, an agreement in 
flux within 10% for the energy band 350-700 keV is obtained.

The Swift localization is at about 113 degrees off-axis with respect to 
the AGILE pointing, so well 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. 

This GRB triggered also SuperAGILE and was detected at about 17 sigma 
significance level in the 18-60 keV band, although it was well outside the 
field of view, and was detected through the collimator shielding." 

This message may be cited.


GRB_name: GRB080603A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7867
SUBJECT: GRB 080603A: final Swift-XRT observations.
DATE:    08/06/10 16:14:56 GMT
FROM:    Boris Sbarufatti at INAF-IASF-Pa  <sbarufatti@ifc.inaf.it>

B. Sbarufatti, V. Mangano, V. La Parola (INAF-IASF Pa) report
on behalf of the Swift-XRT team.

Swift-XRT continued observing the afterglow of the INTEGRAL-detected
GRB 080603A. After the first  detection of the X-ray afterglow, showing
flare like activity previously reported (Sbarufatti et al., GCN Circ.
7810) Swift detected the source also at T+234 ks, with count-rate
(8+/-2)E-3 counts/s (2.6 ks exposure) and at T+578 ks, with count-rate
(2.5+/-0.8)E-3 counts/s (6.9 ks exposure). Extrapolation from these two
points gives a power-law decay index of 1.3 +/- 0.4 (1-sigma CL) for
the afterglow.

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


GRB_name: GRB080603B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7869
SUBJECT: GRB 080603b: optical observation
DATE:    08/06/11 23:29:52 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

V. Rumyantsev (CrAO),  A. Pozanenko (IKI) report on behalf of larger GRB
follow-up collaboration:

We observed the field of  Swift GRB 080603b (Mangano et al., GCN 7794)  on
June 06 betwen (UT) 19:20:31 - 20:27:07  with Zeiss-1000 (Simeiz) telescope
of  CrAO observatory with favorable weather conditions. We do not detect
optical afterglow (Rujopakarn, et al., GCN 7792) in a combined image  of
R-band up to 22.5 (3sigma). A photmetry is obtained in comparison with
nearby USNOB-1.0 stars:

UT,       Exposure,   UL
(mid time)

3.011 d   33x120 s    22.5 (3sigma)

The message may be cited.


GRB_name: GRB080603A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7870
SUBJECT: GRB 080603A: Late-time Keck imaging and spectroscopy
DATE:    08/06/13 00:28:58 GMT
FROM:    Daniel Perley at U.C. Berkeley  <dperley@astro.berkeley.edu>

D. A. Perley, J. S. Bloom, A. A. Miller, J. Shiode, J. Brewer, D. Starr, 
and R. Kennedy (UC Berkeley) report:

On the night of 2008-06-07 (UT) we re-observed the location of GRB 
080603A (GCN 7790, Paizis et al.) with Keck I / LRIS in g and R filters 
for 785s and 690s respectively, starting at 12:30 UT.  The optical 
afterglow (Gomboc et al., GCN 7788; Chornock et al., GCN 7789) is 
well-detected as the northern member of a complex of sources. 
Calibrating relative to four nearby USNO B1.0 stars we estimate an 
afterglow magnitude of

R = 23.7 +/- 0.1  (t = 4.05 days)

The extended source reported by Rymyantsev et al. (GCN 7860) is clearly 
detected and is well-resolved into the afterglow plus two extended 
sources in the g-band frame, with the southern source significantly 
redder than the afterglow and the faint western source.

A color image of the field is posted to:

http://lyra.berkeley.edu/~dperley/080603a/080603a_color.png

Given the very strong absorption lines reported in our spectroscopic 
observations (Perley et al., GCN 7791), this complex may be a bright 
host galaxy of this burst, as suggested by Rumyantsev et al.  However, 
the sources above are offset significantly from the afterglow (which 
itself is not obviously extended), suggesting instead that they may 
represent one or both of the intervening absorbers.

Later the same night, we acquired 2x900s spectra using a slit covering 
the northern (afterglow) source and southern source, and an additional 
1x600 spectrum using a slit covering the faint western source and the 
bright, clearly separated eastern source noted by Kann et al. (GCN 
7822).  No obvious emission lines are evident in any spectrum.  At any 
of the host and absorber redshifts of z=1.688, z=1.563 and z=1.271 
respectively, the bright potential emission features (Ly-alpha, OII) are 
expected to fall outside our wavelength coverage, on top of sky lines, 
or be strongly attenuated by the atmosphere, so this result is mildly 
supportive of an association of these sources with the host and/or 
absorbers.  However, the integrations were relatively short, and further 
follow-up is warranted.


GRB_name: GRB080613A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7871
SUBJECT: GRB 080613 : a long GRB detected with INTEGRAL
DATE:    08/06/13 10:31:23 GMT
FROM:    Diego Gotz at CEA  <diego.gotz@cea.fr>

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

A GRB lasting about 30 s has been detected by IBAS in IBIS/ISGRI data at
09:35:21 UT of June 13 2008. The coordinates (J2000)  are:

  RA:  213.2742 [degrees]
  DEC: +5.1687 [degrees]

with an uncertainty of 1.5 arcmin (90% c.l.).

A preliminary analysis yields a peak flux integrated over 1 s of about
1.3 ph/cmsq/s (20-200 keV) and a fluence over the same energy
range of about  1.3e-6 erg/cmsq.

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: GRB080613A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7872
SUBJECT: GRB 080613: Faulkes Telescope North optical candidate
DATE:    08/06/13 11:00:20 GMT
FROM:    Cristiano Guidorzi at INAF-OAB  <cristiano.guidorzi@brera.inaf.it>

C. Guidorzi (INAF-OAB), E. Rol (U. Leicester), I. Steele, A. Melandri,
C.G. Mundell, D.F. Bersier, M.F. Bode, M.J. Burgdorf, S.N. Fraser,
S. Kobayashi, C.J. Mottram, R.J. Smith (Liverpool JMU),
A. Gomboc (U. Ljubljana), P. O'Brien, N. Bannister, N. Tanvir (U. Leicester)
report on behalf of larger GRB collaboration:

The 2-m Faulkes Telescope North observed the field of the INTEGRAL
GRB 080613 (Gotz et al. GCN Circ. 7871) starting 3.9 min after the
trigger time.
We detect an uncatalogued, likely fading source in R (~19 mag)
also visible in B and i' bands and not visible in the DSS,
within the offline INTEGRAL error circle at the following position
(J2000):

RA = 14:13:05.02
Dec= +5:10:23.5

Further observations are being taken.


GRB_name: GRB080613B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7873
SUBJECT: GRB 080613B: Swift detection of a burst
DATE:    08/06/13 11:27:48 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

C. B. Markwardt (CRESST/GSFC/UMD), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), G. Cusumano (INAF-IASFPA),
C. Gronwall (PSU), C. Guidorzi (INAF-OAB),
S. T. Holland (CRESST/USRA/GSFC), J. Mao (INAF-OAB),
F. E. Marshall (NASA/GSFC), P. T. O'Brien (U Leicester),
J. P. Osborne (U Leicester), K. L. Page (U Leicester),
M. Stamatikos (NASA/ORAU), R. L. C. Starling (U Leicester),
G. Tagliaferri (INAF-OAB) and H. Ziaeepour (UCL-MSSL) report on
behalf of the Swift Team:

At 11:12:37 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 080613B (trigger=313954).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is
RA, Dec 173.797, -7.098 which is
   RA(J2000) = 11h 35m 11s
   Dec(J2000) = -07d 05' 53"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty).  The BAT light curve shows multiple overlapping
peaks with a duration of about 50 sec.  The peak count rate
was ~10000 counts/sec (15-350 keV), at ~T+0 sec after the trigger. 

The XRT began observing the field at 11:13:47.4 UT, 69.5 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 173.79896, -7.10590 which
is equivalent to:
   RA(J2000)  = 11h 35m 11.75s
   Dec(J2000) = -07d 06' 21.2"
with an uncertainty of 3.9 arcseconds (radius, 90% containment). This
location is 29 arcseconds from the BAT onboard position, within the BAT
error circle. No event data are yet available to determine the column
density using X-ray spectroscopy. 

The initial flux in the 2.5 s image was 3.83e-09 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 79 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 is 19.7 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 0.04. 

Burst Advocate for this burst is C. B. Markwardt (Craig.Markwardt 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: GRB080514B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7874
SUBJECT: GRB 080514B: Spectroscopic constraints and probable host galaxy
DATE:    08/06/13 16:18:12 GMT
FROM:    Daniel Perley at U.C. Berkeley  <dperley@astro.berkeley.edu>

D. A. Perley, J. S. Bloom (UC Berkeley), H.-W. Chen (U Chicago), R. J. 
Foley, A. A. Miller, J. Shiode, J. Brewer, D. Starr, and R. Kennedy 
(UCB) report:

On the night of 2008-06-07 (UT) we observed the location of the 
Super-AGILE burst GRB 080514B (GCN 7715, Rapisarda et al.) with Keck I / 
LRIS in g and R filters for 1080s and 960s respectively, starting at 
12:53 UT.  We detect a source consistent with the afterglow position (de 
Ugarte Postigo et al., GCN 7719) in both filters.  Photometry within a 
1.1" radius aperture gives an magnitude (calibrated to three nearby USNO 
B1.0 stars) of:

R = 23.9 +/- 0.2 (t = 24.1 days)

Compared to the measurement of Malesani et al. (R = 22.52 at 1.77 days, 
GCN 7734), this would suggest a decay index of only about alpha = 0.5 
were this the GRB afterglow, which is unlikely at such late times.  More 
likely, the source represents a relatively bright host galaxy of this burst.

However, analysis of a 2x1200s Gemini-North spectrum using GMOS taken at 
the afterglow location (offset <0.5" from the host from a comparison 
from the Gemini i-band acquisition image) 1.9 days after the GRB shows 
no significant emission or absorption features over the usable spectral 
range from 4000-6720 Angstroms.  The continuum flux extends all the way 
to 4000 Angstroms without evidence of Lyman-alpha forest absorption, 
which imposes a redshift constraint of z < 2.3.  Further follow-up is 
encouraged.

A colorized image of the field is available at:

http://lyra.berkeley.edu/~dperley/080514b/080514b_color.png


GRB_name: GRB080613B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7875
SUBJECT: GRB 080613B: Swift-XRT refined analysis
DATE:    08/06/13 18:11:13 GMT
FROM:    Cristiano Guidorzi at INAF-OAB  <cristiano.guidorzi@brera.inaf.it>

J. Mao, C. Guidorzi, F. Pasotti (INAF-OAB) and C. B. Markwardt 
(CRESST/GSFC/UMD),
report on behalf of the Swift-XRT team:

The Swift-XRT began observing GRB 080613B (trigger=313954, Markwardt et
al., GCN Circ. 7873) in Windowed Timing (WT) mode, 76 s after the BAT
trigger. The data of the first orbit consist of 149 s in Windowed Timing
mode and 794 s in Photon Counting mode.

Using 757 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 = 173.79773, -7.10501 which is equivalent to:

RA (J2000): 11 35 11.46
Dec (J2000): -07 06 18.0

with an uncertainty of 2.3 arcsec (radius, 90% confidence).

The light curve from 76 to 219 s can be modelled  as a power law with a 
photon index
of 2.15 +/- 0.11 (90%), followed by a sudden drop of about 2 orders of 
magnitudes up to ~400 s,
after which the decay resumes a value around 1.5.

The WT mode spectrum spanning from 76 to 219 s can be fit by a
power-law model, with a spectral photon index of 1.17 +/- 0.07 and an 
absorbing column
density of 3.7 (-2.0, +2.3)e20 cm^-2 , consistent with the average Galactic
one, 3.2e20 cm^-2.

The corresponding observed (unabsorbed) 0.3-10 keV flux is 1.05e-9 (1.09e-9)
erg cm^-2 s^-1.

If the burst continues to decay at the same rate, we predict an
XRT count rate of 6e-5 count/s at T+24 hours, which corresponds
to an observed 0.3-10 keV flux of approximately 3.5e-15 erg cm^-2 s^-1.
However, we caution about this prediction due to the presently large
uncertainty on the decay rate.

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


GRB_name: GRB080613B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7876
SUBJECT: GRB 080613B, Swift-BAT refined analysis
DATE:    08/06/13 18:41:44 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

T. Ukwatta (GWU), S. D. Barthelmy (GSFC), W. Baumgartner (GSFC/UMBC),
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), T. Sakamoto (GSFC/UMBC), G. Sato (ISAS),
M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC)
(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 080613B (trigger #313954)
(Markwardt, et al., GCN Circ. 7873).  The BAT ground-calculated position is
RA, Dec = 173.806, -7.102 deg, which is 
   RA(J2000)  =  11h 35m 13.3s 
   Dec(J2000) = -07d 06' 06.5" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 89%.
 
The mask-weighted light curve shows several overlapping peaks in a FRED-like
envelope lasting out to ~T+180 sec.  T90 (15-350 keV) is 105 +- 35 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-5.3 to T+236.5 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.39 +- 0.06.  The fluence in the 15-150 keV band is 5.8 +- 0.2 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+2.23 sec in the 15-150 keV band
is 2.7 +- 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/313954/BA/


GRB_name: GRB080613B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7877
SUBJECT: GRB080613B: Swift/UVOT Upper Limits 
DATE:    08/06/13 22:13:41 GMT
FROM:    Wayne Landsman at GSFC/SSAI  <wayne.b.landsman@nasa.gov>

W.Landsman (GSFC/Adnet) and C. Markwardt (CRESST/GSFC/UMD) , on behalf 
of the Swift/UVOT team.

The Swift Ultra-Violet/Optical Telescope (UVOT) began settled 
observations of GRB 080613B (trigger 313954) 79 seconds after the BAT 
trigger (Markwardt et al.,GCN Circ. 7873).  No afterglow is detected at 
the enhanced XRT position (Mao et al., GCN Circ.7875) in the initial 
white finding chart or subsequent summed images. The limiting 
magnitudes  (3-sigma in 5" radius apertures) in each of the UVOT filters 
are as follows:

Filter  T_start(s)  T_stop(s)  Exp(s)  Mag UL (3sig)

white       79       180        98     >20.4
white       79      7227       627     >21.4
v          185      7566      1167     >20.1
b          665      7023       451     >20.5
u          640     13348       312     >20.1
uvw1       616     13323      1179     >20.8
uvm2       591     12415      1102     >21.2
uvw2       695     18103       936     >21.0

The values quoted above are in the UVOT photometric system (Poole et al. 
2008, MNRAS, 383, 627).  They are not corrected for the expected 
Galactic extinction corresponding to a reddening of E(B-V)=0.04 mag in 
the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB080613B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7878
SUBJECT: GRB 080613B - NOT optical and IR nondetections
DATE:    08/06/14 01:17:22 GMT
FROM:    Christina Thoene at Niels Bohr Institute,DARK Cosmo Ctr  <cthoene@astro.ku.dk>

Christina C. Thoene, Daniele Malesani, Johan P. U. Fynbo (DARK), Lison Malo
(Universite de Montreal), Richardo J. Cardenes and Anlaug Amanda
Djupvik (NOT) report:

We observed the field of GRB 080613B (Markwardt et al., GCN 7873) on
June 13 with the NOT on La Palma using StanCam
and NOTCAM. Observations of 4x300s in R band were obtained with
StanCam starting at UT 21:57 and 5x270s with NOTCAM in the Ks band
starting UT 23:17.
In the stacked images of both filters we do not detect any optical
counterpart within the XRT error circle (Mao et al. GCN 7875). The
limiting magnitudes are about R=22 mag and Ks=17.6 based on USNO and
2MASS stars in the field respectively.

[GCN OPS NOTE(14jun08): Per author's request, the two references
were added and the author list order was chanegd.]


GRB_name: GRB080613B
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7879
SUBJECT: GRB 080613B: GROND Upper Limits
DATE:    08/06/14 02:16:10 GMT
FROM:    Christian Clemens at MPE  <cclemens@mpe.mpg.de>

C. Clemens, A. Updike (Clemson University), T. Kruehler, J. Greiner, A. Kupcu 
Yoldas, A. Yoldas (all MPE Garching) and G. Szokoly (Eoetvoes Univ., Budapest 
and MPE Garching) report on behalf of the GROND team:

We observed the field of GRB 080613B (Swift trigger 313954; Markwardt et al., 
GCN #7873) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, 
PASP 120, 405) mounted at the 2.2m ESO/MPI telescope at La Silla Observatory 
(Chile).

Observations started at 22:47 UT on June 13th, 2008, 11.6 hrs after the GRB 
trigger.

We do not detect any object within the refined 3.6'' Swift-XRT error circle 
reported by Mao et al. (GCN #7875) to the following 3-sigma upper limits:

g' > 24.4,
r' > 24.4,
i' > 23.5,
z' > 23.5 and
J > 22.4.

Given upper limits are calibrated against USNO-B1 as well as 2MASS field 
stars.


GRB_name: GRB080613A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7880
SUBJECT: GRB 080613A: GROND Confirmation of the Afterglow Candidate
DATE:    08/06/14 02:28:48 GMT
FROM:    Christian Clemens at MPE  <cclemens@mpe.mpg.de>

C. Clemens, A. Updike (Clemson University), T. Kruehler, J. Greiner, A. Kupcu 
Yoldas, A. Yoldas (all MPE Garching) and G. Szokoly (Eoetvoes Univ., Budapest 
and MPE Garching) report on behalf of the GROND team:

We observed the field of GRB 080613A (INTEGRAL trigger 5288; Gotz et al., GCN 
#7871) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 
120, 405) mounted at the 2.2m ESO/MPI telescope at La Silla Observatory 
(Chile).

Observations started at 00:25 UT on June 14th, 2008, 14.8 hrs after the GRB 
trigger with 25 mins of effective exposures in g'r'i'z' and 20 mins in JHK.

We do not detect any object at the position reported by Guidorzi et al., GCN 
#7872) to the following 3-sigma upper limits:

g' > 24.2,
r' > 23.9,
i' > 23.5,
z' > 23.4,
J > 22.3 and
H > 21.3.

Given upper limits are calibrated against SDSS as well as 2MASS field stars.

This indicates a clear fading of the source. We therefore confirm this to be 
the afterglow of GRB 080613A.


GRB_name: GRB080613A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7881
SUBJECT: GRB080613A: Swift/UVOT Upper Limits
DATE:    08/06/14 02:43:26 GMT
FROM:    Erik Hoversten at Swift/Penn State  <hoversten@astro.psu.edu>

E. A. Hoversten (PSU) and S. T. Holland (CRESST/USRA/GSFC) on behalf
of the Swift/UVOT team.

The Swift Ultra-Violet/Optical Telescope (UVOT) began settled
observations of the INTEGRAL-detected GRB 080613A (Gotz, et al., GCN
Circ. 7871) 6.7 hours after the trigger.  No afterglow is detected at the
position of the R-band detection by the Faulkes Telescope North
(Guidorzi, et al., GCN Circ. 7872).  The 22.2 magnitude upper limit in
the white band suggests the R~19 object seen by Guidorzi, et al. 3.9
minutes after the trigger has faded and is indeed the afterglow.


Filter  T_start(s)  T_stop(s)  Exp(s)  Mag UL (3sig)

white     24725      25189      456     >22.2
v         25195      25638      436     >20.5
b         24257      24720      456     >21.5

The values quoted above are in the UVOT photometric system (Poole et al.
2008, MNRAS, 383, 627).  They are not corrected for the expected
Galactic extinction corresponding to a reddening of E(B-V)=0.023 mag in
the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB080613A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7882
SUBJECT: GRB 080613A: Swift-XRT detection of the afterglow
DATE:    08/06/14 09:15:27 GMT
FROM:    Cristiano Guidorzi at INAF-OAB  <cristiano.guidorzi@brera.inaf.it>

C. Guidorzi (INAF-OAB) and C. B. Markwardt (CRESST/GSFC/UMD) report
on behalf of the Swift-XRT team:

The Swift XRT began observing the INTEGRAL GRB 080613A
(Gotz et al., GCN Circ 7871) on June 13, 16:19 UT, 24.2 ks after
the INTEGRAL trigger. The data consist of 3.6 ks observed in Photon 
Counting
mode.

We detect a single X-ray source within the INTEGRAL error circle at the 
position
RA, Dec = 213.27213, +5.17256 which is equivalent to:

RA (J2000):  14 13 05.31
Dec (J2000): +05 10 21.2

with an uncertainty of 5.2 arcsec (radius, 90% confidence).
This position lies 4.9" from the optical afterglow found with the 
Faulkes Telescope North
(Guidorzi et al., GCN Circ. 7872) and later confirmed by GROND (Clemens 
et al. GCN Circ. 7880)
and Swift-UVOT (Hoversten and Holland, GCN Circ. 7881), and is
therefore consistent with being the X-ray afterglow of GRB 080613A.

Presently there is marginal evidence for fading: a power-law fit of the 
light curve
gives a decay index of 1.2  1.5, so still compatible with a constant 
rate of
of (2.8  0.3)e-2 counts/s.

Forced by the small number of counts, we extracted the 0.3-10 keV spectrum
from a 10-pixel radius circular region and adopted the Cash statistics.
The spectrum can be fit with a power law with an absorbing column
density fixed to the Galactic value (2.0e20 cm-2) and a photon index of
1.3  0.3. The observed (unabsorbed) 0.3-10 keV flux
is 1.50 (1.53)e-12 erg cm-2 s-1.

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


GRB_name: GRB080603A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7883
SUBJECT: GRB 080603A: optical observations on June 04
DATE:    08/06/14 11:28:28 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

V. Rumyantsev (CrAO),  A. Pozanenko (IKI) report on behalf of larger GRB 
follow-up collaboration:

We observed  a field of  INTEGRAL GRB 080603A (Paizis et al., GCN 7790) in 
R-band on June 04 between (UT) Jun.04 23:18:41 - Jun.05 00:12:41 with 
Zeiss-1000 (Simeiz) telescope of CrAO observatory.   At  the place of the 
optical afterglow (Gomboc et al., GCN 7788; Chornock  et al., GCN 7789) we 
detect an object with coordinates

RA(J2000):  18 37 38.02
Dec(J2000): +62 44 39.44

Within uncertainties (0.5" or better ) the coordinates of the object are 
consistent with reported early (Gomboc et al., GCN 7788; Chornock  et al., 
GCN 7789) and one can consider the object as afterglow of GRB 080603A.

A group of two extended sources (Perley et al., GCN 7870)  is not resolved 
in our later observation on 3.496 d (Rumyantsev et al. GCN 7860). The 
unresolved  source (Rumyantsev et al. GCN 7860)  lies ~1.8" south from the 
afterglow position. And tentatively one can consider the upper limit of the 
observation on 3.496 days  R=22.85 (3sigma) as an upper limit of the 
afterglow brightness.

Based on  USNOB1.0 star with ID 1527-0313986 at RA = 18:37:55.186, Dec. 
+62:45:32.28 (R1 = 16.74)  we estimated brightness of  the afterglow on 
1.521 days:

UT,       Exposure,   R_mag, UL
(mid time)

1.521 d  27x120 s  22.2 +/- 0.2   22.9

This message may be cited. 


GRB_name: GRB080613B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7884
SUBJECT: Konus-Wind observation of GRB 080613B
DATE:    08/06/15 15:01:08 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, P.
Oleynik, M. Ulanov, D. Svinkin, and T. Cline on behalf of the Konus-Wind 
team report:

The long GRB 080613B (Swift-BAT trigger
#313954: Markwardt et al., GCN 7873, Ukwatta et al., GCN 7876) triggered 
Konus-Wind at T0=40358.636 s UT (11:12:38.636).

The burst light curve shows a multipeaked structure with a duration of ~30s.

As observed by Konus-Wind the burst
had a fluence of 2.21(-0.38, +0.44)x10^-5 erg/cm2,
and a 256-ms peak flux measured from T0-0.144 s
of 4.76(-1.24, +1.39)x10^-6 erg/cm2/s
(both in the 20 keV - 3 MeV energy range).

The time-integrated spectrum of the burst
(from T0 to T0+33.024 s) is well fitted (in the 20 keV-3 MeV range)
by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
with alpha = -1.05 +/- 0.18
and Ep = 733(-200, +285) keV (chi2 = 56.6/65 dof).
Fitting by GRBM (Band) model yields the same alpha and Ep,
and only an upper limit on the high energy photon index: beta < -2.05
(chi2 = 56.5/64 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/GRB080613_T40358/


GRB_name: GRB080613A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7885
SUBJECT: GRB080613A: Optical upper limits with Okayama MITSuME telescope
DATE:    08/06/17 23:26:42 GMT
FROM:    Michitoshi Yoshida at Okayama Astrophysical Obs  <yoshida@oao.nao.ac.jp>

M. Yoshida, K. Yanagisawa, Kuroda, D., Y. Shimizu, S. Nagayama,
Toda, H. (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 080613A (Gotz et al. GCN 7871) with 50cm MITSuME
telescope at Okayama Astrophysical Observatory from 13:44:35 UT
(4h 9m after the trigger) to UT 15:13:05 on June 13 2008.

We found no new source within a 10 arcsec radius of the position
of the optical afterglow candidate reported by Guidorzi et al.
(GCN 7872). Three sigma limiting magnitudes of our observation
are listed below.


Start-UT              mid-UT    exp-T    g'      Rc      Ic
--------------------------------------------------------------
2008-06-13 13:44:35   14:28:50  77min    >18.4   >17.7   >16.7
--------------------------------------------------------------


GRB_name: GRB080613B
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7886
SUBJECT: GRB080613B: MITSuME upper limits
DATE:    08/06/17 23:33:43 GMT
FROM:    Michitoshi Yoshida at Okayama Astrophysical Obs  <yoshida@oao.nao.ac.jp>

M. Yoshida, K. Yanagisawa, Kuroda, D., Y. Shimizu, S. Nagayama,
Toda, H. (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 080613B (Markwardt et al. GCN 7873) with 50cm MITSuME
telescope at Okayama Astrophysical Observatory from 11:19:09 UT
(6m 31s after the trigger) to UT 12:43:30 on June 13 2008.

We could not identify any new source in the XRT error circle
(Mao et al. GCN7875). Three sigma limiting magnitudes of our
observation are listed below.


Observation date: 2008-06-13 UT

Start-UT   mid-UT    exp-T    g'      Rc      Ic
----------------------------------------------------
11:19:09   11:31:16  10min    >18.4   >18.3   >18.0
11:31:26   12:07:28  60min    >18.7   >18.4   >18.1
----------------------------------------------------


GRB_name: GRB080603A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7887
SUBJECT: GRB 0800603A: optical observation
DATE:    08/06/18 00:38:23 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 (Gomboc et al., GCN 7788; Chornock  et al., GCN 7789)
of GRB 0800603A  (Paizis et al., GCN 7790)  with 1.5 m telescope of Sayan
observatory (Mondy) on Jun.03 between (UT) 18:21:30 - 18:43:55. The
afterglow is detected in each frame of 120 s exposure.
Coordinates  of the afterglow obtained from a combined image are R.A.(J2000)
= 18 37 38.04  Dec.(J2000) = +62 44 39.4 with uncertainties of 0.3". A
photometry of the afterglow obtained against several USNO-A2.0 stars is
following:

T0+       Exposure  R_mag
(mid)

0.3015 d  8x120 s   20.49 +/- 0.03

The photometry might be slightly contaminated by the nearby source(s)
(Perley
et al., GCN 7870, Rumyantsev et al., GCN 7860).

In comparison to the magnitude measured in early epoch (Perley et al. GCN
7791) the index of power law decay is ~ 0.5 which is compatible with slow
decay index (alpha ~ 0.5) obtained by Kann et al. (GCN 7822).

The combined image can be found at
http://grb.rssi.ru/GRB080603A/GRB080603A_R_AZT33.jpg

The message may be cited.


GRB_name: GRB080613A
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7888
SUBJECT: VLA upper limit on INTEGRAL burst GRB 080613A
DATE:    08/06/20 13:13:45 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
080613A (GCN 7871) at a frequency of 8.46 GHz on 2008 June 16.17 UT.
The GRB radio afterglow is undetected and the peak radio flux at the
XRT afterglow position (GCN 7882) is 7  45 uJy.

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


GRB_name: GRB080603B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7890
SUBJECT: GRB 080603b: optical observation
DATE:    08/06/21 11:40:18 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 (Rujopakarn, et al., GCN 7792) of Swift GRB 0800603b 
(Mangano et al., GCN 7794)  with 1.5 m telescope of Sayan observatory 
(Mondy) on Jun.04 between (UT) 18:35 - 19:11. The afterglow is detected in a 
combined image of 8x120 s exposure. A photometry of the afterglow obtained 
against several USNO-A2.0 stars is following:

T0+       Exposure  R_mag
(mid)

0.9686 d  8x120 s   21.10 +/- 0.10

This photometry confirms the steep decay of a light curve (alpha ~ 2.5) 
suggested by Kann et al. (GCN 7824).
The message may be cited.


GRB_name: GRB080607A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7891
SUBJECT: GRB080607: optical observation
DATE:    08/06/21 12:16:51 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

V. Rumyantsev (CrAO),  A. Pozanenko (IKI) report on behalf of larger GRB 
follow-up collaboration:

We observed the field of  Swift GRB 080607 (Mangano  et al., GCN 7847)  on 
June 07 between (UT) 19:54 - 21:05  with Zeiss-1000 (Simeiz) telescope of 
CrAO observatory. We detect faint optical  source in coordinates

RA(J2000):  12 59 47.24
Dec(J2000): +15 55 08.74

with uncertainties of 0.5".

The source looks extended. The source is within enhanced XRT position 
(Osborne et al., GCN 7853), however the source position is apart ~2" from 
coordinates reported for the afterglow (Rujopakarn et al., GCN 7846, Mangano 
et al., GCN 7847, Chornock et al., GCN 7856).
 It is not clear is the source of  a putative host galaxy + afterglow or the 
source is not  related.
A photometry is obtained in comparison with nearby USNOB-1.0 star 12 59 
45.62   +15 54 19.10  assuming R=17.91:

T0+       Exposure  R_mag  UL
(mid)

0.5985 d   35x120  s    22.00 +/- 0.25  22.5

The message may be cited. 


GRB_name: GRB080623A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7894
SUBJECT: GRB 080623: Swift detection of a burst
DATE:    08/06/23 10:43:00 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

T. N. Ukwatta (GSFC/GWU), S. D. Barthelmy (GSFC),
A. P. Beardmore (U Leicester), P. A. Evans (U Leicester),
N. Gehrels (NASA/GSFC), O. Godet (U Leicester),
S. T. Holland (CRESST/USRA/GSFC), S. D. Hunsberger (PSU),
J. A. Kennea (PSU), A. Moretti (INAF-OAB), K. L. Page (U Leicester),
D. M. Palmer (LANL), D. Perez (U Leicester), M. Perri (ASDC) and
G. Stratta (ASDC) report on behalf of the Swift Team:

At 10:25:28 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 080623 (trigger=315080).  Swift did not immediately slew
because of an Earth observing constraint. 
The BAT on-board calculated location is 
RA, Dec 237.660, -62.038, which is 
   RA(J2000)  =  15h 50m 38s
   Dec(J2000) = -62d 02' 16"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showes several overlapping peaks
with a duration of about 25 sec.  The peak count rate
was ~2500 counts/sec (15-350 keV), at ~7 sec after the trigger. 

XRT and UVOT observations will begin when the source comes out of 
Earth constraint near T+21 minutes. 

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: GRB080623A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7895
SUBJECT: GRB 080623: Swift XRT prompt analysis 
DATE:    08/06/23 11:13:13 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

D. Perez (U. Leicester-U. Jaen), K. Page, P. Evans, A. Beardmore (U. 
Leicester) report on behalf of the Swift XRT Team

The XRT began observing the field at 10:47:31.4 UT, 22.0 minutes after the 
BAT trigger. Using promptly downlinked data we find a fading, uncatalogued 
X-ray source located at RA, Dec 237.66083, -62.04897 which is equivalent 
to:
   RA(J2000)  = 15h 50m 38.60s
   Dec(J2000) = -62d 02' 56.3"
with an uncertainty of 3.0 arcseconds (radius, 90% containment). This
location is 39 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
2.59e+21 cm^-2 (Kalberla et al. 2005).


GRB_name: GRB080623A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7896
SUBJECT: GRB 080623: Swift/UVOT Non-Detection of an Optical Afterglow  
DATE:    08/06/23 11:35:42 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/UVOT
Team:

    UVOT took a finding chart exposure of 100 seconds with the White
(160-650 nm) filter starting 1331 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 (Perez, et
al., 2008, GCN Circ. 7895). The 3-sigma upper limit is 21.1 mag.  No
correction has been made for the large expected extinction
corresponding to E(B-V) of 0.35 mag.  The USNO B1.0 star 279-072176 is
located 2.07 arcsec from the centre of the XRT error circle.


GRB_name: GRB080623A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7897
SUBJECT: GRB 080623: TAROT La Silla observatory optical observations
DATE:    08/06/23 12:26:04 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 080623 detected by SWIFT
(trigger 315080) with the TAROT robotic telescope (D=25cm)
located at the European Southern Observatory,
La Silla observatory, Chile.

The observations started 425.1s after the GRB trigger
(14.8s after the notice). The elevation of the field
decreased from 12 degrees above horizon and weather
conditions were good but only four images of 90s were
taken due to the end of the night.

The date of trigger : t0 = 2008-06-23T10:25:28.44

We do not detect any optical transient
at the XRT position (Ukwatta et al. GCNC 7894)
with the following limiting magnitudes:

The first image is 90.0s exposure:
t0+425s to t0+515s : R > 16.2

We co-added the four exposures:
t0+425s to t0+802.0s : R > 17.0

This last value is conservative because
the star density is high and the spatial
sampling of TAROT (i.e. 3.3 arcsec/pix) is not
adapted to separate close sources fainter than
mag 17.0 at the XRT position.

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

N.B. Galactic coordinates are lon=322.3398 lat= -6.1221
and the galactic extinction in R band is 0.94 magnitudes
estimated from D. Schlegel et al. 1998ApJ...500..525S.

This message may be cited.


GRB_name: GRB080623A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7898
SUBJECT: GRB 080623: Enhanced Swift-XRT position
DATE:    08/06/23 16:00:38 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
data for GRB 080623, 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 = 237.66166, -62.04919 which is equivalent
to:

RA (J2000): 15h 50m 38.80s
Dec (J2000): -62d 02' 57.1"

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), 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: GRB080623A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7899
SUBJECT: GRB 080623, Swift-BAT refined analysis
DATE:    08/06/23 17:35:06 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

W. Baumgartner (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),
T. Sakamoto (GSFC/UMBC), G. Sato (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+1390 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 080623 (trigger #315080)
(Ukwatta, et al., GCN Circ. 7894).  The BAT ground-calculated position is
RA, Dec = 237.667, -62.044 deg which is 
   RA(J2000)  =  15h 50m 40.1s 
   Dec(J2000) = -62d 02' 36.7" 
with an uncertainty of 1.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 33%.
 
The mask-weighted light curve shows four overlapping peaks starting
at ~T-1 sec and ending at ~T+18 sec.  T90 (15-350 keV) is 15.2 +- 5 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-0.7 to T+16.0 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.35 +- 0.15.  The fluence in the 15-150 keV band is 1.0 +- 0.1 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+7.23 sec in the 15-150 keV band
is 2.0 +- 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/315080/BA/


GRB_name: GRB080623A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7900
SUBJECT: GRB 080623: Swift-XRT refined analysis
DATE:    08/06/23 20:06:49 GMT
FROM:    Dolores Perez-Ramirez at U.Leicester  <dpr9@star.le.ac.uk>

D. Perez (U. Leicester-U. Jaen), K.L. Page (U. Leicester), T. N. Ukwatta
(GSFC/GWU), report on behalf of the Swift-XRT team:


We have analysed the first three orbits of data obtained for GRB 080623
(Ukwatta et al., GCN Circ. 7894), covering 4.3ks of Photon Counting (PC)
mode data. The UVOT-enhanced XRT position was given by Beardmore et al.
in GCN Circ. 7898.

The light-curve can be fitted with a single powerlaw with a decay of
alpha ~1.0 +/- 0.1.


The first three orbits of PC data can be modelled with an absorbed
powerlaw, with Gamma = 2.03 +/- 0.14 and total NH = (0.37 +/-
0.05)x10^22 cm^-2, in excess of the Galactic value of 0.26x10^22 cm^-2.

The observed (unabsorbed) flux over this time interval is 8.05 x10^-12
(1.34x10^-11) erg cm^-2 s^-1.  The counts to observed flux conversion is
5.3x10^-11 erg cm^-2 count^-1.

If the light-curve continues to decay at alpha ~ 1.0, the count rate at
24 hours is predicted to be 0.0086 count s^-1, corresponding to an
observed flux of 4.5x10^-13 erg cm^-2 s^-1.

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


GRB_name: GRB080623A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7901
SUBJECT: GRB080623: Swift UVOT followup observations
DATE:    08/06/23 20:43:04 GMT
FROM:    Alice Breeveld at MSSL-UCL  <aad@mssl.ucl.ac.uk>

A. A. Breeveld (MSSL/UCL) and T. N. Ukwatta (GSFC/GWU) report on behalf
of the Swift/UVOT team.

The Swift Ultra-Violet/Optical Telescope (UVOT) began settled
observations of GRB 080623 (Ukwatta et al., GCN Circ. 7894) 22.15 
minutes after the trigger, as reported in Holland, GCN Circ. 7896.  We 
confirm that no afterglow is detected at the position of the enhanced 
XRT position (Beardmore et al., GCN Circ. 7898) in the initial finding 
chart or subsequent summed images.

The following table gives the 3 sigma upper limits in all filters.

Filter  T_start(s)  T_stop(s)  Exp(s)  Mag UL (3sig)

white   1329        1428       98.1    >20.4
white   1559        2713       76.9    >20.3
white   8133        8332      196.6    >20.8
v       1436        2598      155.6    >19.0
b       1535        2698      155.5    >19.9
u       1510        2673      155.4    >19.7
uvw1    1486        2648      155.5    >19.4
uvm2    1460        2623      155.6    >19.1
uvw2    1575        2573      136.1    >19.3

The values quoted above are in the UVOT photometric system (Poole et al.
2008, MNRAS, 383, 627).  No correction has been made for the large 
expected extinction corresponding to E(B-V) of 0.35 mag in
the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB080623A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7902
SUBJECT: GRB 080623: GROND upper limits
DATE:    08/06/25 02:42:32 GMT
FROM:    Adria C. Updike at Clemson U  <aupdike@clemson.edu>

A. Updike (Clemson Univ.), S. Loew, J. Greiner, T. Kruehler,
A. Kuepcue Yoldas, A. Yoldas,  (all MPE Garching),
G. Szokoly (Eoetvoes Univ., Budapest and MPE Garching),
report for the GROND team:

We observed the field of GRB 080623 detected by Swift/BAT (Ukwatta et al.
2008, GCN 7894) simultaneously in g'r'i'z'JHK with GROND (Greiner et al.
2008, PASP 120, 405), mounted at the 2.2m MPI/ESO telescope at La Silla
(Chile). A first epoch started on Jun. 23 at 22:50 UT (12.3 hrs after the
GRB) and continued for 2.5 hours; the second epoch was obtained on Jun. 24
at 23:50 UT (mid-time).

We do not detect any new source within the astrometrically corrected XRT
position (Beardmore et al. 2008, GCN 7898).

We note that there is a bright star at the border of the XRT error circle
and a fainter one just outside the XRT error circle.  A finding chart can
be found at http://www.mpe.mpg.de/~jcg/grb080623.html .  Both objects are
visible in DSS2-R and are constant between our two epochs.  Image
subtraction revealed no hidden sources.

Limiting magnitudes inside the XRT error circle are g'>24.3, r'>23.5,
i'>21.8, z'>21.7, J>20.2, H>19.4, K>17.5, calibrated against USNO-B1 and
2MASS stars.


GRB_name: GRB080625A
Detection_method: superAGILE
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7903
SUBJECT: GRB 080625: Gamma Ray Burst Localization by SuperAGILE
DATE:    08/06/25 15:34:22 GMT
FROM:    Marco Feroci at IASF/INAF  <sa.grb@iasf-roma.inaf.it>

L. Pacciani, I. Donnarumma, E. Del Monte, M. Feroci, Y. Evangelista,
E. Costa, 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,
(ASDC) and L. Salotti (ASI), on behalf of the AGILE Team, report:

"SuperAGILE detected and localized a gamma ray burst
on June 25th 2008, at 12:28:31 UT. The event was approximately
22 degrees off-axis. The observed duration in the 20-60 keV
energy range is about 80 seconds, with a single peak structure.
The burst was triggered and localized on ground.
The burst position was reconstructed as (RA, Dec) (298.4423 deg,
56.2653 deg), which is:

RA(J2000) = 19h 53m 46.14s
Dec(J2000) = 56d 15' 55.1"

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: GRB080625A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7904
SUBJECT: GRB 080625: Observations at OSN
DATE:    08/06/25 22:27:30 GMT
FROM:    Antonio Deugarte at IAA-CSIC  <deugarte@iaa.es>

A. de Ugarte Postigo (ESO), F. Aceituno,
A.J. Castro-Tirado, J. Gorosabel (IAA-CSIC)
report on behalf of a larger collaboration:

We have observed the field of GRB080625, detected
by SuperAGILE (Pacciani et al. GCN 7903), from
the 1.5m OSN telescope starting at June 25.8591
(8.14 hours after the burst). Preliminary analysis
does not show any evident new source within the
3' error box as compared with the DSS2 IR frame.
We note, however, that our combined 4x300s I-band
frame yields a limit of I < 21.5, significantly
deeper than the catalogue.

Further imaging is scheduled in order to determine
if any of the objects that we detect at or beyond the
limit of the catalogue is the afterglow of GRB 080625.


GRB_name: GRB080625A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7905
SUBJECT: GRB 080625: Swift/UVOT Detection of an Optical Afterglow
DATE:    08/06/26 02:09:08 GMT
FROM:    Stefan Immler at NASA/GSFC  <stefan.m.immler@nasa.gov>

S. Immler (NASA/CRESST/GSFC) reports on behalf of the Swift/UVOT team:

The Swift Ultra-Violet/Optical Telescope (UVOT) started observing
GRB 080625 (Pacciani et al., GCN Circ. 7903) ~5.0 hours after the
AGILE trigger.

A candidate afterglow is found in UVOT White, v, and b filter
images which cover the entire AGILE error circle. The preliminary
Swift/UVOT position of the optical afterglow candidate is:

  RA(J2000)  = 19:53:37.06 = 298.4044
  DEC(J2000) = +56:16:40.5 = 56.2779

with a 1-sigma error radius of about 0.5 arcsec.
The following table gives the measured magnitudes:

Filter   T_start [s]   T_stop [s]   Exp [s]   Magnitude

White   18769   19567   799    20.3 +/- 0.1
White   24551   25179   1427   20.6 +/- 0.1
V       19575   20350   776    19.6 +/- 0.1
B       17964   18762   799    20.1 +/- 0.1
B       23746   24544   799    20.7 +/- 0.2
U       17880   23741   240    >20.4 (3-sigma UL)

The values quoted above are in the UVOT photometric system
(Poole et al. 2008, MNRAS, 383, 627). No correction has been
made for the expected extinction corresponding to E(B-V) of
0.44 mag in the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB080625A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7906
SUBJECT: GRB 080625:Swift-XRT detection of the afterglow
DATE:    08/06/26 02:25:11 GMT
FROM:    Michael Stroh at PSU/Swift  <stroh@astroh.org>

M.C. Stroh, C. Pagani and L. Vetere (PSU) report on behalf of the  
Swift-XRT team

The Swift-XRT began observations of the SuperAGILE burst GRB 080625  
(Pacciani et al., GCN Circ 7903) ~5 hours after the trigger. The data  
consist of 3.9 ks observed in Photon Counting mode.

We detect an X-ray counterpart at position: RA, Dec = 298.40420,  
56.27747 which is equivalent to:

RA (J2000):  19 53 37.0
Dec (J2000): +56 16 38.9

with an uncertainty of 4 arcsec (radius, 90% confidence). This is  
consistent with the UVOT position (Immler, GCN 7905).

We are unable to determine whether the source is decaying at this  
time. Observations are continuing and further analysis regarding the  
fading nature of this source will be issued as the data become  
available.

The spectrum can be fitted with a powerlaw with an intrinsic absorbing  
column of (2.5+/-0.9) e21 cm-2 and photon index 2.31+/- 0.17. The  
observed (unabsorbed) 0.3-10 keV flux is 2.91 (3.00) e-12 erg cm-2 s-1.

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


GRB_name: GRB080625A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7907
SUBJECT: GRB 080625: Further observations from OSN
DATE:    08/06/26 07:25:24 GMT
FROM:    Antonio Deugarte at IAA-CSIC  <deugarte@iaa.es>

A. de Ugarte Postigo (ESO), F. Aceituno,
A.J. Castro-Tirado, J. Gorosabel (IAA-CSIC)
report on behalf of a larger collaboration:

We have observed again the field of GRB 080625 (Pacciani et al.
GCN 7903) using the 1.5m OSN telescope at Sierra Nevada
Observatory (Granada, Spain) at a mean epoch of 14.76h after the
burst. The object identified by Immler et al. (GCN 7905) is well
detected in this and in our previous epoch (GCN 7904). A preliminary
photometry against USNO-B1.0 stars shows the object decaying, as
seen in the following table:

t-t0 (hours)  Exp (s)   I mag
8.325           4x300    19.3+/-0.2
14.769         3x300    20.0+/-0.2


GRB_name: GRB080625A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7908
SUBJECT: GRB 080625: Swift/UVOT Follow-Up Observations
DATE:    08/06/27 19:17:20 GMT
FROM:    Stefan Immler at NASA/GSFC  <stefan.m.immler@nasa.gov>

S. Immler (NASA/CRESST/GSFC) reports on behalf of the Swift/UVOT team:

Swift Ultra-Violet/Optical Telescope (UVOT) follow-up observations
of GRB 080625 (Pacciani et al., GCN Circ. 7903), starting ~25.9 hrs
after the AGILE trigger, confirm the fading of the optical afterglow
(Immler et al., GCN Circ. 7905; de Ugarte Postigo et al., GCN Circ. 7907).

The following magnitude is measured in the co-added image obtained
in the White filter:

Filter   T_start [s]   T_stop [s]   Exp [s]   Magnitude

White    93,092        162,754      5,776      21.3 +/- 0.1

The magnitude quoted above is in the UVOT photometric system
(Poole et al. 2008, MNRAS, 383, 627). No correction has been
made for the expected extinction corresponding to E(B-V) of
0.14 mag in the direction of the burst (Schlegel et al. 1998).
Note the corrected value for the extinction compared to Immler
2008 (GCN Circ. 7905).


GRB_name: GRB080623A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7909
SUBJECT: GRB 080623: Suzaku WAM observation of the prompt emission
DATE:    08/06/28 02:39:45 GMT
FROM:    Yoshitaka Hanabata at Hiroshima U  <hanabata@hep01.hepl.hiroshima-u.ac.jp>

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

The long GRB 080623 (Swift/BAT trigger #315080 ; Ukwatta et al., GCN 7894) 
was detected by the Suzaku Wide-band  All-sky Monitor (WAM) which covers 
an energy range of 50 keV - 5 MeV at 10:25:28 UT on 23 July 2008 (=T0). 
The observed light curve shows a multi-peaked structure starting at T0, 
ending at T0+10 s with a duration (T90) of about 7 seconds. The fluence in 
100 - 1000 keV was (1.6 +/- 0.4) E-6 erg/cm^2. The 1-s peak flux measured 
from T0+ 8 s was 0.5 +/- 0.4 photons/cm^2/s in the same energy range.

Preliminary result shows that the time-averaged spectrum from T0 to T0+10 s
is well fitted by a single power-law with a photon index of 2.0 -0.9+1.0
(chi^2/d.o.f =  5.6 / 8) at the 150 - 600 keV bandpass.
----

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

[GCN OPS NOTE(30jun08): Per author's request, the Subject was changed
from "080523" to "080623".]


GRB_name: GRB080701A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7910
SUBJECT: GRB 080701: Swift detection of a burst
DATE:    08/07/01 10:37:05 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

M. C. Stroh (PSU), A. P. Beardmore (U Leicester), D. N. Burrows (PSU),
P. A. Evans (U Leicester), N. Gehrels (NASA/GSFC),
C. Guidorzi (INAF-OAB), E. A. Hoversten (PSU), C. Pagani (PSU),
K. L. Page (U Leicester), D. M. Palmer (LANL),
D. Perez (U Leicester), P. Romano (INAF-IASFPA),
T. Sakamoto (NASA/UMBC), R. L. C. Starling (U Leicester),
T. N. Ukwatta (GSFC/GWU), L. Vetere (PSU) and H. Ziaeepour (UCL-MSSL)
report on behalf of the Swift Team:

At 10:13:37 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 080701 (trigger=315615).  Swift did not immediately slew
due to an Earth limb constraint.  The BAT on-board calculated location is 
RA, Dec 45.837, +75.492 which is 
   RA(J2000) = 03h 03m 21s
   Dec(J2000) = +75d 29' 30"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a smooth peak
structure with a duration of ~15 sec.  The peak count rate
was ~2500 counts/sec (15-350 keV), at ~1 sec after the trigger. 

Swift was unable to slew to the source due to due to Earth limb
constraints. X-ray telescope and UV/optical telescope observations of
this region will become possible at T+50 minutes. 

Burst Advocate for this burst is M. C. Stroh (stroh AT astroh.org). 
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: GRB080701A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7911
SUBJECT: GRB 080701: Swift-XRT Prompt Analysis
DATE:    08/07/01 12:16:48 GMT
FROM:    Michael Stroh at PSU/Swift  <stroh@astroh.org>

M.C. Stroh, C. Pagani (PSU) and P. Evans (U. Leicester) report on  
behalf of the Swift-XRT team.

The XRT began observing the field at 11:00:14.4 UT, 2796.8 seconds
after the BAT trigger. Using promptly downlinked data we find an
uncatalogued X-ray source located at RA, Dec 45.83937, 75.47535 which
is equivalent to:
  RA(J2000)  = 03h 03m 21.45s
  Dec(J2000) = +75d 28' 31.3"
with an uncertainty of 3.1 arcseconds (radius, 90% containment). This
location is 59 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 in excess of the Galactic value (1.78e+21
cm-2, Kalberla et al. 2005), with an excess column of 6.3
(+3.88/-3.07) x 10^21 cm-2 (90% confidence).

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


GRB_name: GRB080701A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7913
SUBJECT: GRB 080701A, Swift-BAT refined analysis
DATE:    08/07/01 13:30:11 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

E. Fenimore (LANL), S. D. Barthelmy (GSFC), W. Baumgartner (GSFC/UMBC),
J. Cummings (GSFC/UMBC), N. Gehrels (GSFC), H. Krimm (GSFC/USRA),
C. Markwardt (GSFC/UMD), K. McLean (GSFC/UMD), D. Palmer (LANL),
T. Sakamoto (GSFC/UMBC), G. Sato (ISAS), M. Stamatikos (GSFC/ORAU),
M. C. Stroh (PSU), J. Tueller (GSFC), T. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using the data set from T-120 to T+285 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 080701A (trigger #315615)
(Stroh, et al., GCN Circ. 7910).  The BAT ground-calculated position is
RA, Dec = 45.944, 75.481 deg which is 
   RA(J2000)  =  03h 03m 46.5s 
   Dec(J2000) = +75d 28' 50.7" 
with an uncertainty of 1.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 55%.
 
The mask-weighted light curve shows a single FRED-like peak starting
at ~T-2 sec, peaking at ~T+0 sec, and ending at ~T+20 sec.
T90 (15-350 keV) is 18 +- 9 sec (estimated error including systematics).
 
The time-averaged spectrum from T-2.7 to T+24.6 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.24 +- 0.17.  The fluence in the 15-150 keV band is 7.1 +- 0.7 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T-0.08 sec in the 15-150 keV band
is 2.2 +- 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/315615/BA/


GRB_name: GRB080701A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7914
SUBJECT: GRB 080701: Enhanced Swift-XRT position
DATE:    08/07/01 21:01:51 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 699 s of overlapping XRT Photon Counting mode and UVOT
data for GRB 080701, 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 = 45.83882, +75.47479 which is equivalent
to:

RA (J2000): 03h 03m 21.32s
Dec (J2000): +75d 28' 29.3"

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: GRB080701A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7915
SUBJECT: GRB 080701A: Early Super-LOTIS Observations
DATE:    08/07/01 21:05:17 GMT
FROM:    Peter A. Milne at Super-LOTIS  <pmilne@as.arizona.edu>

P.A. Milne (U Arizona) reports on behalf of the Super-LOTIS team:

The robotic 0.6m Super-LOTIS telescope began R-band observations of the error
region of GRB 080701A at 10:14:25 UT, 49 seconds after the trigger.
Initial 10 and 20 second exposures reveal no sources other than those
present in the relevant DSS image. A stack of 30x60sec images
reveals no source at the location of the XRT source (Stroh et al.,
GCN 7911), down to a 3-sigma limiting magnitude of R~19.5. Comparisons of
initial and final images reveals no brightening or fading sources.

We used the USNO-B star at RA=03:02:55.5, Dec=+75:28:42 to derive the
R2 magnitude upper-limit.

This message can be cited.


GRB_name: GRB080701A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7916
SUBJECT: GRB 080701A: Swift/UVOT Upper Limits
DATE:    08/07/01 22:11:42 GMT
FROM:    Frank Marshall at GSFC  <marshall@milkyway.gsfc.nasa.gov>

F.E. Marshall (NASA/GSFC) and M.C. Stroh (PSU)
report on behalf of the Swift/UVOT team:

The Swift/UVOT observed the field of GRB 080701A starting 2983 s after
the BAT trigger (Stroh et al., GCN Circ. 7910).  We do not find a source
in any of the UVOT observations inside the enhanced XRT error circle
(Evans et al., GCN Circ. 7914). The 3-sigma upper limits for detecting
a source in the first finding chart (FC) exposure and co-added frames are:

Filter            T_start(s)   T_stop(s)     Exp(s)     Mag (3-sigma UL)

white (FC)        2983         3082           98        >19.7
white             2983         9403          736        >21.0
v                 3914         4113          197        >19.1
b                 3298         4934          393        >20.2
u                 3093         4728          393        >19.9
uvw1              4324         4523          197        >20.0
uvm2              4119         4318          197        >19.6
uvw2              3709         3908          197        >20.2

The values quoted above are not corrected for the expected Galactic
extinction corresponding to a reddening of E(B-V) = 0.54 mag in
the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB080701A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7917
SUBJECT: TLS I-Band Observation of GRB 080701A
DATE:    08/07/01 22:28:54 GMT
FROM:    Andrea Rossi at TLS Tautenburg  <rossi@tls-tautenburg.de>

Rossi, A. (TLS Tautenburg), Gonsalves, E. (U. Dartmouth), Schulze, S. (TLS  
Tautenburg), Klose, S. (TLS  Tautenburg), Filgas, R. (TLS  Tautenburg), 
and Ludwig, F. (TLS  Tautenburg) 
report on behalf of a larger collaboration:

We observed the X-ray error circle of the Swift GRB 080701A (Evans, P. A. 
et al., GCN 7914; Stroh, M. C. et al., GCN 7910) with the TLS 1.34m Schmidt 
telescope under good  observing conditions (seeing is about 1-2 arcsec and 
very good visibility). We obtained in total 10 x 150 sec images starting at 
21:02 UT and 5 x 300 sec images starting at 21:40 UT in the I band. We did 
not find any new source in the stacked image down to the 3-sigma limiting 
magnitude of 21.7 mag calibrated on USNO-B1 field.

This message can be cited.


GRB_name: GRB080701A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7918
SUBJECT: GRB 080701A, VATT optical upper limit
DATE:    08/07/01 22:43:48 GMT
FROM:    Peter Garnavich at U of Notre Dame  <pgarnavi@nd.edu>

C. Peters (Goshen College) and P. Garnavich (Notre Dame) report:

We observed the field of GRB 080701A with the Vatican Advanced Technology
Telescope (VATT) beginning July 1.46 (UT) or 45 minutes after
the bursts (Stroh et al. GCN 7910). Four exposures totaling 190 sec
in the R-band were obtained. The combined image was calibrated assuming
the
brightness of the USNO-B1 star at RA=3:03:21.50 DEC=75:28:15.48
is R=16.52.

No source is detected down to R=22.0 at the improved XRT
position (Evans et al. GCN 7914).


GRB_name: GRB080701A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7919
SUBJECT: GRB 080701: Swift-XRT refined analysis
DATE:    08/07/02 00:12:31 GMT
FROM:    Michael Stroh at PSU/Swift  <stroh@astroh.org>

M.C. Stroh (PSU) reports on behalf of the Swift-XRT team.

We have analyzed the first four orbits of Swift-XRT data obtained for  
GRB 080701 (Stroh et al., GCN Circ. 7910), totaling 2.4ks of Photon  
Counting data.

The UVOT-enhanced XRT position has been given by Evans et al. in GCN  
Circ 7914.

The X-ray light-curve can be fit by a power-law with a decay index of  
1.04 +/- 0.27. Assuming a constant decay rate, we predict counting  
rates at T+24 and T+48 hours of 4.55e-3 and 2.21e-3 cts/s respectively.

The spectrum can be fit with a power-law in excess of the Galactic  
value (1.78e21 cm-2, Kalberla et al. 2005), with an excess column of  
9.21 (+6.43/-4.78)e21 cm^-2 and a photon index of 2.93 (+0.79/-0.59).  
The observed (unabsorbed) 0.3-10 keV flux is 3.55e-12 (1.976e-11) ergs/ 
cm^2/s.

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


GRB_name: GRB080702A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7920
SUBJECT: GRB 080702: Swift detection of a short burst
DATE:    08/07/02 12:10:31 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

M. De Pasquale (UCL-MSSL), W. H. Baumgartner (GSFC/UMBC),
A. P. Beardmore (U Leicester), D. N. Burrows (PSU),
P. A. Evans (U Leicester), N. Gehrels (NASA/GSFC),
C. Guidorzi (INAF-OAB), J. A. Kennea (PSU), V. Mangano (INAF-IASFPA),
F. E. Marshall (NASA/GSFC), C. Pagani (PSU), K. L. Page (U Leicester),
D. M. Palmer (LANL), P. Romano (INAF-IASFPA), T. Sakamoto (NASA/UMBC),
B. Sbarufatti (INAF-IASFPA), P. Schady (MSSL-UCL),
M. Stamatikos (NASA/ORAU), E. Troja (INAF-IASFPA),
T. N. Ukwatta (GSFC/GWU) and P. A. Ward (MSSL-UCL) report on behalf
of the Swift Team:

At 11:50:43 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 080702 (trigger=315710).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 312.853, +72.308 which is 
   RA(J2000) = 20h 51m 25s
   Dec(J2000) = +72d 18' 28"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a double-peaked
structure with the second peak larger and a total duration of 
about 1.5 sec.  The peak count rate was ~3000 counts/sec (15-350 keV), 
at ~0.5 sec after the trigger, during the second peak. 

The XRT began observing the field at 11:51:50.0 UT, 66.3 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source with an enhanced position: RA, Dec 313.05101,
72.31271 which is equivalent to:
   RA(J2000)  = 20h 52m 12.24s
   Dec(J2000) = +72d 18' 45.8"
with an uncertainty of 3.0 arcseconds (radius, 90% containment). This
location is 217 arcseconds from the BAT onboard position, slightly outside 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
1.53e+21 cm^-2 (Kalberla et al. 2005). 

UVOT took a finding chart exposure of 100 seconds with the White (160-650 nm)
filter starting 72 seconds after the BAT trigger. No afterglow candidate has
been found in the initial data products. The XRT position is outside the 
2.7'x2.7' sub-image. 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 0.67. 

Burst Advocate for this burst is M. De Pasquale (mdp 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: GRB080702A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7923
SUBJECT: GRB 080702A: Enhanced Swift-XRT position
DATE:    08/07/02 19:59:51 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 95 s of overlapping XRT Photon Counting mode and UVOT
data for GRB 080702A, 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 = 313.05081, +72.31271 which is equivalent
to:

RA (J2000): 20h 52m 12.20s
Dec (J2000): +72d 18' 45.8"

with an uncertainty of 1.9 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, 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: GRB080702B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7924
SUBJECT: GRB 080702B : Burst detected in BAT during Swift slew
DATE:    08/07/02 20:18:23 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <jayc@milkyway.gsfc.nasa.gov>

Jay R. Cummings (NASA/UMBC), A. Copete (Harvard),
J. Grindlay (Harvard), D. Palmer (LANL),
for the Swift-BAT and BATSS teams


At 01:10:41, Swift-BAT observed GRB 080702B. The burst occurred
during a preplanned Swift slew maneuver. The rate increase was
noted during a routine check of the counting rates for missed out-
of-field and slew bursts. A GRB candidate was automatically 
detected by the BAT Slew Survey (BATSS) with 5.9 sigma in the 
S band (15-50 keV) and 6.5 sigma in the B band (15-150keV). 
The burst profile is FRED-like with ~3sec rise and ~30sec decay. 
The peak count rate is 0.05cts/sec (S band) and 0.04cts/sec (B band). 
BATSS automated analysis measured T90 = 10.5sec and T50 = 5.5sec, 
and a position 

RA = 23h 42m 24s, DEC = -05d 29' 23" 

with a 90% confidence radius of 6.4arcmin. 

Further ground analysis of this GRB yielded a location 
RA, Dec 355.616,  -5.424 (J2000) or

RA = 23h 42m 27.8s
Dec = -05d 25' 26.4"

with an estimated error radius of 3 arcmin. A Swift TOO request was 
submitted, and Swift/XRT and UVOT began observing at about 18:30, 
approximately 17.3 hours after the burst.


GRB_name: GRB080702A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7925
SUBJECT: GRB 080702A: Swift-XRT Team refined analysis
DATE:    08/07/02 21:03:07 GMT
FROM:    Kim Page at U.of Leicester  <kpa@star.le.ac.uk>

K.L. Page (U. Leicester) & M. De Pasquale (UCL-MSSL) report on behalf of 
the Swift-XRT team:

We have analysed the first 3 orbits of Swift-XRT data obtained for GRB 
080702A (De Pasquale et al., GCN Circ. 7920), covering 5.2 ks of Photon 
Counting mode data, between ~75 and 12.6 ks after the trigger. The 
UVOT-enhanced XRT position was given by Goad et al. in GCN Circ. 7923.

The light-curve can be modelled by a broken power-law, with a flat decay 
of alpha = 0.5 +/- 0.3 until around the end of the first orbit of data. At 
this point, the decay steepens to 1.6 +0.9/-0.3. The afterglow is already 
faint by the end of the third orbit.

A spectrum extracted from the first orbit of data can be modelled with an 
absorbed power-law, with Gamma = 2.05 +0.71/-0.64 and NH = (6.2 
+5.4/-3.6)x10^21 cm^-2, in excess of the Galactic column in this direction 
of 1.53x10^21 cm^-2. The observed (unabsorbed) flux over this time 
interval (75-800 s post-trigger) is 5.7x10^-12 (1.0x10^-11) erg cm^-2 
s^-1.

If the light-curve continues to decay with alpha ~ 1.6, the count rate 24 
hours after the burst is estimated to be 3.3x10^-5 count s^-1, which 
corresponds to an observed flux of 2x10^-15 erg cm^-2 s^-1.

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


GRB_name: GRB080702A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7926
SUBJECT: GRB 080702A, Swift-BAT refined analysis
DATE:    08/07/02 21:52:54 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

H. Krimm (GSFC/USRA), S. D. Barthelmy (GSFC), W. Baumgartner (GSFC/UMBC),
J. Cummings (GSFC/UMBC), E. Fenimore (LANL), N. Gehrels (GSFC),
C. Markwardt (GSFC/UMD), K. McLean (GSFC/UMD), D. Palmer (LANL),
M. De Pasquale (UCL-MSSL), T. Sakamoto (GSFC/UMBC), G. Sato (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 080702A (trigger #315710)
(De Pasquale, et al., GCN Circ. 7920).  The BAT ground-calculated position is
RA, Dec = 313.049, 72.278 deg, which is 
   RA(J2000)  =  20h 52m 11.8s 
   Dec(J2000) = +72d 16' 39.7" 
with an uncertainty of 3.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 81%.
 
The mask-weighted light curve shows a weak single spike.
T90 (15-350 keV) is 0.5 +- 0.2 sec (estimated error including systematics).
 
The time-averaged spectrum from T-0.0 to T+0.5 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.34 +- 0.42.  The fluence in the 15-150 keV band is 3.6 +- 1.0 x 10^-8 erg/cm2.
The 1-sec peak photon flux measured from T-0.22 sec in the 15-150 keV band
is 0.7 +- 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/315710/BA/


GRB_name: GRB080701A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7928
SUBJECT: GRB 080701A: Early RAPTOR optical limits
DATE:    08/07/02 23:24:50 GMT
FROM:    James Wren at LANL  <jwren@nis.lanl.gov>

J. Wren, W.T. Vestrand, P.R. Wozniak, H. Davis, B. Norman
of Los Alamos National Laboratory report:

The RAPTOR telescope system responded to Swift trigger
315615 (Stroh et al., GCN 7910) under good observing conditions.
Our narrow-field instruments began observing the location at
10:14:06.47 UTC, 28.8 s after the Swift trigger.  We detect no
counterpart at the improved XRT position (Evans et al., GCN 7914).
The limiting magnitudes of our unfiltered observations when
calibrated to the USNO-B1 R-band are given in the following table.
The GRB location was also within the field of view of our
continuous all-sky monitoring system.  We can place 3 sigma limits
at or below magnitude 9.4 during the time period within 2
minutes both before and after the trigger.  

t-mid(s)    exp(s)     mag     mag-err
--------------------------------------------
-11.68      10.0       9.7     3 sigma limit
11.57       10.0      10.0     3 sigma limit
34.80       10.0       9.9     3 sigma limit
71.45       45.0      19.3     3 sigma limit
173.93     100.0      19.8     3 sigma limit
300.65     100.0      19.9     3 sigma limit
561.10     270.0      20.5     3 sigma limit


GRB_name: GRB080702A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7929
SUBJECT: GRB 080702A: MITSuME Akeno optical upper limits
DATE:    08/07/03 00:07:25 GMT
FROM:    Nobuyuki Kawai at Tokyo Tech  <nkawai@hp.phys.titech.ac.jp>

Y.A. Mori, T. Shimokawabe, Y. Kudou, H. Nakajima and N. Kawai (Tokyo
Tech) report on behalf of the MITSuME collaboration: 

The 3-color 50cm MITSuME Telescope at Akeno, Japan, responded to GRB
080702A (de Pasquale et al. GCN 7920) at 43 sec after the trigger,
though we obtained the first sky image 20 min after the trigger
due to the poor sky condition with frequent cloud coverage.  
In the co-added images of Ic, Rc, and g' bands, we did not detect any
afterglow candidate in the XRT error circle.  The 3-sigma limiting
magnitudes based on USNO-B1.0 (I-band) and NOMAD (R-band,g'-band)
stars are following.

Filter   start UT    end UT    Exposure   LimitMag   
---------------------------------------------------
  g'    12:16:37    13:11:35   23 x 60 s    16.6   
  Rc    12:16:37    13:11:35   23 x 60 s    17.7
  Ic    12:16:37    13:11:35   23 x 60 s    16.5
---------------------------------------------------


GRB_name: GRB080625A
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7930
SUBJECT: GRB 080625: Suzaku WAM observation of the prompt emission
DATE:    08/07/03 03:43:57 GMT
FROM:    Takeshi Uehara at Hiroshima U  <uehara@hirax7.hepl.hiroshima-u.ac.jp>

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

The long GRB 080625 (SuperAGILE ; Marco et al., GCN 7903)
was detected by the the Suzaku Wide-band  All-sky Monitor (WAM) which covers an
energy range of 50 keV - 5 MeV at 12:28:41 UT on 25 July 2008 (=T0).

The observed light curve shows a single peak, starting at T0s, ending
at T0+62s with a duration
(T90) of about 62 seconds. The fluence in 100 - 1000 keV was 2.3(+1.3/-0.7) E-6 erg/cm^2.
The 1-s peak flux measured from T0+33s was 0.4(+0.2/-0.3) photons/cm^2/s in the same
energy range.

Preliminary result shows that the time-averaged spectrum from T0-15s to
T0+50s is well fitted by a single power-law with a photon index
of 1.7 (+1.2/-0.8) (chi^2/d.o.f = 9.6/8) at the 120 - 500 keV bandpass.

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: GRB080702B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7931
SUBJECT: GRB 080702B: Swift XRT and UVOT observations
DATE:    08/07/03 10:46:22 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

P.A. Evans (U. Leicester), P. Schady and M. de Pasquale (MSSL-UCL)
report on behalf of the Swift team:

Swift began observing the field of GRB 080702B (Cummings et al. GCN circ
7924) at 2008 July 02 at 17:38 UT, 17.3 hours after the burst. In 4 ks
of XRT data we do not detect any sources within the refined error circle
presented in GCN Circ 7924, down to a 3-sigma upper limit of 2.2 x 10-3
counts s-1.

There are two sources within the original error circle in GCN Circ 7924.
The brightest lies at RA, Dec=355.6326, -5.5318 degrees, with an
estimated uncertainty of 4.7" (radius, 90% confidence). This is
coincident with a known optical source, and is not fading; this is
thus not the GRB afterglow.

The second object lies at RA,Dec=355.5665, -5.51410, which is equivalent
to:

RA (J2000)  = 23 42 15.95
Dec (J2000) = -05 30 50.8

with an estimated uncertainty of 6.3" (radius, 90% containment). The
source count rate is around 3e-3 counts per second, and we are  unable
to determine at present whether this source is fading.

In 3.7 ks of UVOT data obtained using the White filter, no new sources are
detected. The 3-sigma upper limit at the position of the second XRT source
is 22.4 mag.


This circular is an official product of the Swift team.


GRB_name: GRB080702A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7932
SUBJECT: Swift/UVOT observation of GRB080702A 
DATE:    08/07/03 11:42:40 GMT
FROM:    Massimiliano de Pasquale at MSSL-UCL  <mdp@mssl.ucl.ac.uk>

  M. De Pasquale (MSSL/UCL) on the behalf of the
Swift/UVOT team:


The Swift/UVOT began settled exposures of the field of
GRB080702A 73s after the BAT trigger (De Pasquale et al.,
GCN Circ. 7920). We do not find any newsource in any
of the exposures inside the enhanced XRT error circle
(Goad et al., GCN Circ. 7923).

The 3-sigma upper limits for detecting a source in the
first finding chart (FC) exposure and co-added frames are:

Filter        T_start(s)   T_stop(s)    Exp(s)  Mag (3-sigma UL)

white (FC)        73          172          98      >20.8
white            674         5688         314      >21.4
v                179          578         393      >20.0
v                713         6099         305      >19.8
b                659         6840         334      >20.8
u                634         6714         432      >20.6
uvw1             610         6509         432      >20.2
uvm2             585         6303         432      >20.3
uvw2             689         5894         235      >20.3

The values quoted above are not corrected for the expected
high Galactic extinction corresponding to a reddening of
E(B-V) = 0.67 mag in the direction of the burst (Schlegel et
al. 1998).


GRB_name: GRB080702B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7933
SUBJECT: GRB 080702b:  LCO optical observations
DATE:    08/07/03 14:16:49 GMT
FROM:    Edo Berger at Princton U  <eberger@astro.princeton.edu>

E. Berger (Princeton/OCIW) and B. Madore (OCIW) report:

"Starting on 2008 July 2.36 UT we observed the BAT error circle of GRB 
080702b (GCN #7924) using the du Pont 100-inch telescope at Las Campanas 
Observatory.  A total of 1500 sec were obtained in R-band in good seeing 
conditions (0.9").  A comparison to DSS reveals no new sources to the 
limit of the survey.  Further observations are planned."


GRB_name: GRB080702A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7934
SUBJECT: No radio detection from the short  GRB 080702A
DATE:    08/07/03 14:34:32 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
080702A (GCN 7920) at a frequency of 8.46 GHz on 2008 July 03.33 UT.
The GRB radio afterglow is undetected and the peak radio flux at the
XRT afterglow position (GCN 7923) is -22  52 uJy.

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


GRB_name: GRB080703A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7935
SUBJECT: GRB 080703A: ROTSE-III Detection of Optical Counterpart 
DATE:    08/07/03 19:06:08 GMT
FROM:    Eli Rykoff at UCSB  <erykoff@physics.ucsb.edu>

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

ROTSE-IIIa, located at Siding Spring Observatory, Australia, responded 
to GRB 080703A (Swift trigger 315819). The first image was at 19:00:45.1 
UT, 31.5 s after the burst (11.1 s after the GCN notice time). The 
unfiltered images are calibrated relative to USNO A2.0. We detect a 14.7 
magnitude, steady source with coordinates:

      06:47:12.7      -63:13:08.6    (J2000), with positional 
uncertainty of 1" or better

start UT     mag     mlim(of image)
----------------------------------
19:00:45.1     14.7     15.9


This source is not visible in DSS (second epoch), 2MASS or the MPChecker 
database.

A jpeg image is available at 
http://www.rotse.net/images/gsb315819_3a00_img.jpg Note that the object 
marked 18 is the candidate in question.

Continuing observations are in progress.


GRB_name: GRB080703A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7936
SUBJECT: GRB 080703: Swift detection of a burst with optical afterglow
DATE:    08/07/03 19:17:07 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

H. Ziaeepour (UCL-MSSL), S. D. Barthelmy (GSFC), M. M. Chester (PSU),
J. R. Cummings (NASA/UMBC), P. A. Evans (U Leicester),
N. Gehrels (NASA/GSFC), O. Godet (U Leicester),
H. A. Krimm (CRESST/GSFC/USRA), 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. Schady (MSSL-UCL),
R. L. C. Starling (U Leicester), M. C. Stroh (PSU),
T. N. Ukwatta (GSFC/GWU), D. E. Vanden Berk (PSU) and
P. A. Ward (MSSL-UCL) report on behalf of the Swift Team:

At 19:00:13 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 080703 (trigger=315819).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 101.867, -63.222 which is 
   RA(J2000)  =  06h 47m 28s
   Dec(J2000) = -63d 13' 19"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a single peak
with a duration of about 5 sec.  The peak count rate
was ~1500 counts/sec (15-350 keV), at ~0 sec after the trigger. 

Using promptly downlinked data we find a bright, uncatalogued
X-ray source. The position, astrometrically enhanced by aligning promptly
available UVOT field source  positions to the USNO-B1 catalogue, is RA,Dec =
101.80538,  -63.22039 (degrees) which is equivalent to:

RA  (J2000) =  06 47 13.29
DEC (J2000) =  -63 13 13.4

with an uncertainty of 3.04 arcsec (radius, 90% containment). 
This position is 100.1 arcsec from the BAT position, inside the BAT
error circle and 6.3 arcseconds from the UVOT position. 

UVOT took a finding chart exposure of nominal 100 seconds with the White
(160-650 nm) filter starting 100 seconds after the BAT trigger. There is a
candidate afterglow in the list of sources generated on-board at
  RA(J2000)  =  06:47:12.65 = 101.8027
  DEC(J2000) = -63:13:08.8  = -63.2191
with a 1-sigma error radius of about 0.8 arc sec. This position is 104.9 arc
sec. from the center of the BAT error circle. The estimated magnitude is 17.6
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 0.07. 

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: GRB080702B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7937
SUBJECT: GRB 080702B Swift-BAT refined analysis
DATE:    08/07/03 20:04:06 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <jayc@milkyway.gsfc.nasa.gov>

C. Markwardt (GSFC/UMD), S. D. Barthelmy (GSFC),
W. Baumgartner (GSFC/UMBC),A. Copete (Harvard), J. Cummings (GSFC/UMBC),
E. Fenimore (LANL), N. Gehrels (GSFC), J. Grindlay (Harvard),
H. Krimm (GSFC/USRA),K. McLean (GSFC/UMD), D. Palmer (LANL),
T. Sakamoto (GSFC/UMBC), G. Sato (ISAS), M. Stamatikos (GSFC/ORAU),
J. Tueller (GSFC), T. Ukwatta (GWU)
On behalf of the Swift-BAT and BATSS teams:


Using the event data from T-83 to T+37 seconds, we present further
analysis of GRB 080702B.  The best-determined position in BAT was
RA, Dec 355.616,  -5.424 (J2000) or

RA = 23h 42m 27.8s
Dec = -05d 25' 26.4"

with an uncertainty of 3.5 arcmin (radius, sys+stat, 90% containment).
The partial coding was varying (the entire burst occurred during a
preplanned Swift slew manuever), but was approximately 60% during
the entire burst.

The mask-weighted light curve shows a single peak with a few
second rise, and slow decay.  T90 was 20 +- 3 seconds (estimated
error including systematics). 

The time-averaged spectrum from T-2 to T+21 seconds is best fit by a
simple power-law model.  The power law index of the time-averaged
spectrum is 1.44  0.13.  The fluence in the 15-150 keV band was
(5.0  0.9) x 10^-7 ergs/cm2/s.  The 1-sec peak photon flux measured
from T+4 sec in the 15-150 keV band was 0.5 +- 0.1 photons/cm2/s. 
All the quoted errors are at the 90% confidence level.


GRB_name: GRB080703A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7938
SUBJECT: GRB 080703, Swift-BAT refined analysis
DATE:    08/07/03 23:21:52 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

T. Sakamoto (GSFC/UMBC), S. D. Barthelmy (GSFC), W. Baumgartner (GSFC/UMBC),
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), G. Sato (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-120 to T+183 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 080703 (trigger #315819)
(Ziaeepour, et al., GCN Circ. 7936).  The BAT ground-calculated position is
RA, Dec = 101.822, -63.211 deg, which is 
   RA(J2000)  =  06h 47m 17.2s 
   Dec(J2000) = -63d 12' 40.7" 
with an uncertainty of 2.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 53%.
 
The mask-weighted light curve shows a single peak starting at ~T-5 sec,
peaking at ~T+0 sec, and ending at ~T+4 sec.
T90 (15-350 keV) is 3.4 +- 0.8 sec (estimated error including systematics).
 
The time-averaged spectrum from T-1.7 to T+2.1 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.53 +- 0.22.  The fluence in the 15-150 keV band is 2.0 +- 0.3 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+0.04 sec in the 15-150 keV band
is 1.0 +- 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/315819/BA/


GRB_name: GRB080703A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7939
SUBJECT: GRB 080703: Enhanced Swift-XRT position
DATE:    08/07/04 06:30:32 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 3392 s of overlapping XRT Photon Counting mode and UVOT
data for GRB 080703, 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 = 101.80180, -63.21893 which is equivalent
to:

RA (J2000): 06h 47m 12.43s
Dec (J2000): -63d 13' 08.2"

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), 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: GRB080703A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7940
SUBJECT: GRB 080703: VLT observations of the afterglow
DATE:    08/07/04 10:58:08 GMT
FROM:    Daniele Malesani at Niels Bohr Inst,Dark Cosmology Center  <malesani@astro.ku.dk>

D. Malesani, P. M. Vreeswijk, J. P. U. Fynbo, J. Hjorth (DARK/NBI), P. 
Jakobsson (Univ. Hertfordshire), report on behalf of a larger collaboration:

We observed the field of GRB 080703 (Ziaeepour et al., GCN 7936) with 
the ESO VLT equipped with FORS1. Due to visibility constraints, 
observations could only be carried out during twilight at high airmass.

The optical afterglow first reported by Rykoff & Schaefer (GCN 7935; see 
also Ziaeepour et al., GCN 7936) is detected in our image (15 s 
exposure). On 2008 Jul 3.948 UT (3.76 hr after the GRB), the afterglow 
had R ~ 21.6 assuming R = 15.92 for the USNO star at (06:47:12.61, 
-63:12:31.7).

A finding chart is posted at

http://www.astro.ku.dk/~malesani/GRB/080703/080703_finder.png

No further observations are planned. We acknowledge excellent support 
from the ESO staff in executing this challenging observation, 
particularly Thomas Szeifert and Dominique Naef.


GRB_name: GRB080703A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7941
SUBJECT: GRB 080703: UVOT Follow-Up Observation
DATE:    08/07/04 11:15:48 GMT
FROM:    Paul Ward at MSSL  <paw@mssl.ucl.ac.uk>

P. Ward (MSSL-UCL) and H. Ziaeepour (UCL-MSSL) report on behalf of the 
Swift/UVOT team:

The Swift Ultra-Violet/Optical Telescope (UVOT) started observing
GRB 080703 (Rykoff et al. GCN 7935, Ziaeepour et. al, GCN 7936) ~100 
seconds after the trigger.

A quickly fading candidate afterglow is found in the UVOT White and V 
filters. The preliminary Swift/UVOT position of the optical afterglow 
candidate is:

  RA(J2000)  = 06:47:12.639 = 101.8027
  DEC(J2000) = -63:13:08.96 = -63.2192

with a 1-sigma error radius of about 0.5 arcsec.
The following table gives the measured magnitudes:

Filter T_start T_stop Exp     Mag

White  101    200    99.8     17.40 +/- 0.03
White  857    956    99.8     20.27 +/- 0.35
White  5905   6102   196.6    21.29 +/- 0.49
White  5905   19222  869.5  > 21.77 (1.9-sigma)
V      207    606    399.8    18.02 +/- 0.10
V      963    1362   399.8    19.06 +/- 0.27
V      6315   6512   196.6  > 19.65 (0.2-sigma)
V      6315   12021  1081.7 > 20.83 (0.9-sigma)
B      687    1788   78.9   > 19.48 (1.8-sigma)
B      663    1764   99.0   > 19.33 (1.5-sigma)
UVW1   638    1885   99.9   > 19.55 (0.1-sigma)
UVM2   613    1878   118.7  > 19.67 (1.7-sigma)
UVW2   718    1829   79.1   > 19.55 (0.9-sigma)


The values quoted above are in the UVOT photometric system
(Poole et al. 2008, MNRAS, 383, 627). No correction has been
made for the expected extinction corresponding to E(B-V) of
0.071 mag in the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB080703A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7942
SUBJECT: GRB 080703: Swift-XRT refined analysis
DATE:    08/07/04 13:45:39 GMT
FROM:    Olivier Godet at U.of Leicester  <og19@star.le.ac.uk>

We analysed 12.1 ks of data in Photon Counting (PC) mode obtained for GRB
080703 (Ziaeepour et al., GCN Circ 7936) between 106 s and 3.1e4s after the
trigger (T0). The UVOT-enhanced XRT position was given by Osborne et al. in
GCN Circ. 7939.

The X-ray light-curve shows an initial rise from T0+106s to ~T0+200s and
then
decays with a slope of ~1.2. From ~T0+700s to ~T0+2000s, the XRT light-curve
shows some flaring activities. The light-curve after ~T0+1e4s decays with a
slope of 1.57 +/-0.21.

The hardness ratio does not show any significant spectral variation from
T0+106s to T0+3.1e4s. The PC spectrum from T0+106s to T0+3.1e4s is well
fitted
by an absorbed power-law with a photon index of 1.7 +/-0.1 and an absorption
column of (8.9 +3.9/-3.3)e20 cm**-2, in excess with respect to the Galactic
one (5.2e20 cm**-2; Kalberla et al. 2005). The observed 0.3-10 keV flux over
this time interval is (8.2 +0.8/-1.2)e-12 erg/cm**2/s.

If the light-curve continues to decay with alpha = 1.6, the count rate at 24
hours after the trigger is estimated to be 7e-3 counts/s, which
corresponds to
an observed flux of 6.7e-13 erg/cm**2/s.

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


GRB_name: GRB080702B
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7943
SUBJECT: GRB 080702B: GROND Upper Limits
DATE:    08/07/04 17:10:15 GMT
FROM:    Christian Clemens at MPE  <cclemens@mpe.mpg.de>

C. Clemens, S. Loew, J. Greiner, A. Yoldas, T. Kruehler (all MPE Garching), A. 
Kupcu Yoldas (ESO) and G. Szokoly (Eoetvoes Univ., Budapest and MPE Garching) 
report on behalf of the GROND team:

We observed the field of GRB 080702B (Swift; Cummings et al., GCN #7924) 
simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 120, 405) 
mounted at the 2.2 m ESO/MPI telescope at La Silla Observatory (Chile).

Observations started at 09:14 UT on July 3rd, 2008, 32.1 hr after the GRB 
trigger with 53.6 min of effective exposures in g'r'i'z' and 56.0 min in JHK. 
They were carried out at an average seeing of 0.9".

We do not detect any object at the position of the 2nd XRT source within the 
6.3'' error circle reported by Evans et al. (GCN #7931) to the following 3 
sigma (optical) and 6 sigma (infrared) upper limits:

g' > 24.6 mag,
r' > 24.5 mag,
i' > 23.6 mag,
z' > 23.3 mag,
J > 22.0 mag,
H > 21.0 mag and
K > 19.0 mag.

Given upper limits are calibrated against USNO-B1 as well as 2MASS field 
stars.


GRB_name: GRB080703A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7944
SUBJECT: GRB 080703: GROND Upper Limits
DATE:    08/07/04 18:25:08 GMT
FROM:    Christian Clemens at MPE  <cclemens@mpe.mpg.de>

C. Clemens, S. Loew, J. Greiner, A. Yoldas, T. Kruehler (all MPE Garching), A. 
Kupcu Yoldas (ESO) and G. Szokoly (Eoetvoes Univ., Budapest) report on behalf 
of the GROND team:

We observed the field of GRB 080703 (Swift trigger 315819; Ziaeepour et al., 
GCN #7936) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, 
PASP 120, 405) mounted at the 2.2 m ESO/MPI telescope at La Silla Observatory 
(Chile).

Observations started at 23:04 UT on July 3rd, 2008, 4.1 hrs after the GRB 
trigger with 4.7 min of effective exposures in g'r'i'z' and 8.0 min in JHK, 
and were performed at an average seeing of 1.8" during astronomical twilight.

We do not detect any object within the 0.5'' Swift-UVOT error circle reported 
by Ward & Ziaeepour (GCN #7941) to the following upper limits:

g' > 22.1 mag,
r' > 22.6 mag,
i' > 21.8 mag,
z' > 21.3 mag,
J > 19.3 mag,
H > 18.1 mag and
K > 17.0 mag.

These upper limits are calibrated against USNO-B1 as well as 2MASS field 
stars.


GRB_name: GRB080707A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7947
SUBJECT: GRB 080707: Swift detection of a burst
DATE:    08/07/07 08:47:33 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

P. Schady (MSSL-UCL), W. H. Baumgartner (GSFC/UMBC),
A. P. Beardmore (U Leicester), A. A. Breeveld (MSSL),
P. A. Evans (U Leicester), N. Gehrels (NASA/GSFC),
C. Guidorzi (INAF-OAB), H. A. Krimm (CRESST/GSFC/USRA),
C. B. Markwardt (CRESST/GSFC/UMD), A. Moretti (INAF-OAB),
P. T. O'Brien (U Leicester), C. Pagani (PSU),
K. L. Page (U Leicester), D. M. Palmer (LANL),
D. Perez (U Leicester), R. L. C. Starling (U Leicester) and
H. Ziaeepour (UCL-MSSL) report on behalf of the Swift Team:

At 08:27:53 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 080707 (trigger=316204).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 32.632, +33.103 which is 
   RA(J2000) = 02h 10m 32s
   Dec(J2000) = +33d 06' 11"
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 40 sec.  The peak count rate
was ~3000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 08:29:02.0 UT, 68.3 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source with an enhanced position: RA, Dec
32.61815, 33.10967 which is equivalent to:
   RA(J2000)  = 02h 10m 28.36s
   Dec(J2000) = +33d 06' 34.8"
with an uncertainty of 3.1 arcseconds (radius, 90% containment). This
location is 48 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
6.99e+20 cm^-2 (Kalberla et al. 2005). 

The initial flux in the 2.5 s image was 3.59e-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 79 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 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
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
0.10. 




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: GRB080707A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7948
SUBJECT: GRB 080707: GROND Detection of the Optical Afterglow Candidate
DATE:    08/07/07 12:01:41 GMT
FROM:    Christian Clemens at MPE  <cclemens@mpe.mpg.de>

C. Clemens, S. Loew, J. Greiner, A. Yoldas, T. Kruehler (all MPE Garching), A. 
Kupcu Yoldas (ESO) and G. Szokoly (Eoetvoes Univ., Budapest) report on behalf 
of the GROND team:

We observed the field of GRB 080707 (Swift trigger 316204; Schady et al., GCN 
#7947) simultaneously in g'r'i'z'JHK with GROND (Greiner et al. 2008, PASP 
120, 405) mounted at the 2.2 m ESO/MPI telescope at La Silla Observatory 
(Chile).

Observations started at 10:00 UT on July 7th, 2008, 92.2 min after the GRB 
trigger, and were performed at an average seeing of 2.2" and at an average 
airmass of 2.6.

We found a faint source within the 2.9'' Swift-XRT error circle at

RA (J2000) = 02h 10m 28.40s
DEC (J2000) = +33d 06' 34.3''

with an uncertainty of 0.8".

The object is detected in g' band, implying a redshift smaller than 3.5.

Based on the first 4.4 min of effective exposures in g'r'i'z', we estimate 
preliminary magnitudes of

g' ~ 22.1 mag,
r' ~ 21.5 mag,
i' ~ 21.4 mag and
z' ~ 21.2 mag

with typical errors of +/- 0.3. Given magnitudes are calibrated against 
USNO-B1 field stars.

Please note, that no correction for the galactic foreground reddening of 
E(B-V) = 0.1 mag (Schlegel et al., 1998) has been applied.


GRB_name: GRB080707A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7949
SUBJECT: GRB 080707: VLT redshift
DATE:    08/07/07 12:42:24 GMT
FROM:    Daniele Malesani at Niels Bohr Inst,Dark Cosmology Center  <malesani@astro.ku.dk>

Johan P. U. Fynbo, Daniele Malesani, & Bo Milvang-Jensen (DARK), report 
on behalf of a larger collaboration:

We observed the field of GRB 080707 (Schady et al., GCN 7947) with the 
ESO VLT equipped with FORS1.

Inside the XRT error circle, we detect the object first reported by 
Clemens et al. (GCN 7948) in the R and I bands. The source had R ~ 19.6 
on 2008 Jul 7.385 UT (47 min after the trigger), calibrated against 
USNO-B1. This object is not visible in the DSS (which reaches a deeper 
limit) and seems brighter than in the later observation reported by 
Clemens et al. (GCN 7948). It is thus very likely the optical afterglow 
of GRB 080707. A finding chart is posted at

http://www.astro.ku.dk/~malesani/GRB/080707/080707_finder.jpg

FORS1 spectra were acquired between Jul 7.397 and 7.441 UT with grism 
300V. From detection of FeII and MgII absorption features, we infer a 
redshift z = 1.23. A conservative upper limit z < 2.2 can be set from 
the lack of Lyman alpha forest in the blue

We acknowledge excellent and enthusiastic support from the observing 
staff at Paranal, in particular Chris Lidman, Lorena Faundez, Claudia 
Reyes, and Dominique Naef.

[GCN OPS NOTE(07jul08): The two occurances of "GCN 7984" was changed
to "GCN 7948".]


GRB_name: GRB080707A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7950
SUBJECT: GRB 080707: Enhanced Swift-XRT position
DATE:    08/07/07 18:11:09 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 83 s of overlapping XRT Photon Counting mode and UVOT
data for GRB 080707, 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 = 32.61905, +33.11020 which is equivalent
to:

RA (J2000): 02h 10m 28.57s
Dec (J2000): +33d 06' 36.7"

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, 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: GRB080707A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7951
SUBJECT: GRB 080707: Swift XRT refined analysis
DATE:    08/07/07 20:35:47 GMT
FROM:    Rhaana Starling at U of Leicester  <rlcs1@star.le.ac.uk>

R.L.C. Starling (U. Leicester) and P. Schady (MSSL-UCL) report, on behalf 
of the Swift XRT team:

We have analysed the first 4 orbits of Swift XRT data (from T0+64s to 
T0+17.8 ks) for GRB 080707 (trigger=316204, Schady et al., GCN Circ. 
7947).

Using 1482 seconds of overlapping XRT Photon Counting (PC) mode and UVOT 
data, we find an updated astrometrically corrected X-ray position (using 
the XRT-UVOT alignment and matching UVOT field sources to the USNO-B1 
catalogue): RA, Dec = 32.61860, 33.10983 deg which is equivalent to:
 
RA(J2000) = 02 10 28.46 
Dec(J2000)= +33 06 35.4 

with an uncertainty of 1.5 arcseconds (radius, 90% confidence). This 
position lies 1.35 arcseconds from the optical counterpart reported in 
Clemens et al. (GCN Circ. 7948).

The light curve can be fit by an initial steep decay followed by a shallow 
plateau phase. The final orbit of data so far collected may indicate a 
further break to a steeper slope, but this is not required by the fit. 
A  singly broken power law gives alpha1=5.6+1/-0.8, Tbk=145+17/-13 and 
alpha2=0.35+0.06/-0.07. 
A doubly broken power law model gives the following parameters: 
alpha1=5.5+0.9/-0.8, Tbk1=151+6/-15s, alpha2=0.2+0.1/-0.5, 
Tbk2=5300+5400/-4200s and alpha3=0.7+0.6/-0.3.

The PC mode spectrum comprising 1.64 ks of data from the latter part of 
orbit 1 and from orbit 2 (T0+96s - T0+6384s) is well fit with a power law 
of photon index Gamma=2.1+0.4/-0.5 (90%) absorbed by the Galactic column 
of 6.99E+20 cm^-2 (Kalberla et al. 2005) and by a column at the inferred 
redshift of the host galaxy (z=1.23, Fynbo et al. GCN Circ. 7949) which 
can only be constrained to be nH<1.23e22 cm^-2. The 0.3-10 keV observed 
(unabsorbed) flux is 5.4e-12 (6.73-12) erg/cm^2/s, corresponding to a 
count rate of 0.12 count/s, hence the observed count rate to flux 
conversion is 1 count/s = 4.5e-11 erg/cm^2/s.

The predicted count rate at T0+24h is 0.011 counts/s, assuming a decay 
rate of alpha=0.7 from the doubly broken power law model.

This is an official product of the Swift XRT team.


GRB_name: GRB080707A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7952
SUBJECT: GRB 080707, Swift-BAT refined analysis
DATE:    08/07/07 22:50:07 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.a.krimm@nasa.gov>

G. Sato (ISAS), S. D. Barthelmy (GSFC), W. Baumgartner (GSFC/UMBC),
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),
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-240 to T+480 sec from the recent telemetry 
downlink, we report further analysis of BAT GRB 080707 (trigger #316204) 
(Schady et al., GCN Circ. 7947).  The BAT ground-calculated position is
RA, Dec = 32.627, 33.100 deg which is
    RA(J2000)  =  02h 10m 30.5s
    Dec(J2000) = +33d 06' 01.1"
with an uncertainty of 1.8 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 93%.

The mask-weighted light curve consists of two main peaks of roughly 
equivalent peak flux, the first a boxcar shape from T-2 to T+4 sec, and 
the second a FRED beginning at T+23 sec and decaying to background by 
T+32 sec. T90 (15-350 keV) is 27.1 +- 1.1 sec sec (estimated error 
including systematics).

The time-averaged spectrum from T-1.8 to T+26.6 sec is best fit by a 
simple power-law model.  The power law index of the time-averaged 
spectrum is 1.77 +- 0.19.  The fluence in the 15-150 keV band is
5.2 +- 0.6 x 10^-07 erg/cm2. The 1-sec peak photon flux measured from 
T+0.22 sec in the 15-150 keV band is 1.0 +- 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/316204/BA/


GRB_name: GRB080707A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7953
SUBJECT: UVOT observations of GRB080707
DATE:    08/07/07 22:52:44 GMT
FROM:    Patricia Schady at MSSL/Swift  <ps@mssl.ucl.ac.uk>

P. Schady (MSSL-UCL) and F.E. Marshall (NASA/GSFC) report on behalf of the 
Swift/UVOT team:

The Swift/UVOT starting taking settled exposures of the field of GRB 
080707 80 s after the BAT trigger (Schady et al., GCN Circ. 7947). A faint 
source is detected in the early white and v-band observations at

     RA(J2000)  = 02:10:28.40 = 32.61833
     Dec(J2000) = +33:06:34.2 = 33.10950

with an of 1.1 arcseconds (90% confidence), consistent with the enhanced 
XRT error circle (Starling et al., GCN Circ. 7951) and the GROND position 
(Clemens et al., GCN 7948).

The early-time afterglow and 3-sigma upper limits the in co-added frames 
are as follows:

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

white   80          5469        294.0    21.40+/-0.31 (3.4 sigma)
white   11355       12221       844.3    > 21.93
v       186         5880        590.1    19.97+/-0.31 (3.4 sigma)
b       3971        18004       1502.6   > 21.74
u       640         17362       1040.0   > 21.18
uvw1    616         16449       1101.7   > 21.41
uvm2    591         22234       1101.7   > 21.29
uvw2    5477        5676        196.6    > 20.22

The values quoted above are not corrected for the expected 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: GRB080707A
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7954
SUBJECT: GRB 080707: GROND Confirmation of the Optical Afterglow
DATE:    08/07/08 11:34:35 GMT
FROM:    Christian Clemens at MPE  <cclemens@mpe.mpg.de>

C. Clemens, S. Loew, J. Greiner, A. Yoldas, T. Kruehler (all MPE Garching), A. 
Kupcu Yoldas (ESO) and G. Szokoly (Eoetvoes Univ., Budapest) report on behalf 
of the GROND team:

We observed the field of GRB 080707 for a second time at 09:54 UT on July 8th, 
2008, 25.4 hr after the GRB trigger with 25.0 min of effective exposures in 
g'r'i'z'. The observations were performed at an average seeing of 1.6" and at 
an average airmass of 2.4.

We still detect the faint source mentioned in GCN #7948 within the 1.1'' 
Swift-UVOT error circle (Schady et al., GCN #7953) with the following 
preliminary magnitudes of

g' ~ 23.8 mag,
r' ~ 23.2 mag and
i' ~ 23.1 mag

and typical uncertainties of +/- 0.3 (calibrated against USNO-B1 field stars).

With a magnitude change of delta g' ~ 1.7 mag within 23.9 hr (similarily in r' 
and i' band) these measurements strongly suggest that the source mentioned in 
Clemens et al. (GCN #7948) is the afterglow of GRB 080707.


GRB_name: GRB080707A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7956
SUBJECT: GRB 080707: possible break in the X-rays 
DATE:    08/07/09 15:49:07 GMT
FROM:    Rhaana Starling at U of Leicester  <rlcs1@star.le.ac.uk>

R.L.C. Starling (U. Leicester) and P. Schady (MSSL-UCL) report on behalf 
of the Swift XRT team:

We have analysed the Swift XRT X-ray light curve out to T0+162 ks for GRB 
080707 (trigger=316204, Schady et al., GCN Circ. 7947). The light curve 
can be fit with a multiply broken power law as described in GCN Circ. 
7951, and we note a possible further break. A fit including this possible 
break places it at (9 +6/-8)e4 s and the current decay rate is then 
approximately alpha=2.2.
The Swift XRT light curve can be viewed in the on-line repository (Evans 
et al. 2007) at http://www.swift.ac.uk/xrt_curves/00316204/

Swift XRT continues to observe this source to constrain the current decay 
and confirm/reject the presence of a late-time break. Ground-based optical 
observations are strongly encouraged.

This is an official product of the Swift XRT team.


GRB_name: GRB080710A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7957
SUBJECT: GRB 080710: Swift detection of a burst
DATE:    08/07/10 07:29:01 GMT
FROM:    Boris Sbarufatti at INAF-IASF-Pa  <sbarufatti@ifc.inaf.it>

B. Sbarufatti (INAF-IASFPA), W. H. Baumgartner (GSFC/UMBC),
P. A. Evans (U Leicester), C. Guidorzi (INAF-OAB),
E. A. Hoversten (PSU), V. La Parola (INAF-IASFPA),
V. Mangano (INAF-IASFPA), C. B. Markwardt (CRESST/GSFC/UMD),
K. L. Page (U Leicester), P. Romano (INAF-IASFPA) and
T. N. Ukwatta (GSFC/GWU) report on behalf of the Swift Team:

At 07:13:10 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 080710 (trigger=316534).  The BAT on-board calculated location is 
RA, Dec 8.257, +19.492 which is 
   RA(J2000) = 00h 33m 02s
   Dec(J2000) = +19d 29' 31"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single-peaked
structure with a duration of about 20 sec.  The peak count rate
was ~1,000 counts/sec (15-350 keV), at 0 sec after the trigger. 

Due to an observing constraint, Swift will not slew until 
T0+49.5 minutes. There will be no XRT or UVOT data until
this time. 

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


GRB_name: GRB080710A
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7958
SUBJECT: GRB 080710: Swift XRT position 
DATE:    08/07/10 08:29:46 GMT
FROM:    Vanessa Mangano at INAF-IASFPA  <vanessa@ifc.inaf.it>

B. Sbarufatti (INAF-IASFPA), P. A. Evans (U Leicester)
and V. Mangano (INAF-IASFPA) report on behalf of the Swift Team:

The XRT began observing the field at 08:05:22.4 UT, 3131.6 seconds
after the BAT trigger. Using promptly downlinked data we find an
uncatalogued X-ray source located at RA, Dec 8.27344, 19.50157 which is
equivalent to:
   RA(J2000)  = 00h 33m 5.63s
   Dec(J2000) = +19d 30' 05.7"
with an uncertainty of 3.2 arcseconds (radius, 90% containment). This
location is 65 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 in excess of the Galactic value
(4.1e+20 cm^-2, Kalberla et al. 2005), with an excess column of
2 (+2.03/-1.73) x 1021 cm^-2 (90% confidence).


GRB_name: GRB080710A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7959
SUBJECT: GRB 080710: KAIT OA candidate
DATE:    08/07/10 09:46:14 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, report:

KAIT responded to GRB 080710 (Swift trigger 316534; Sbarufatti et al.,
GCN 7957; Sbarufatti et al., GCN 7958) and started to take images at
09:10:20 UT, 1.953 hours after the BAT trigger. There is an optical
afterglow at position

RA = 00:33:05.64
DEC = +19:30:05.7
(equinox J2000)

The measured magnitude is R = 16.8 in a 20s unfiltered image,
calibrated to USNO B1. Observations are ongoing. 


GRB_name: GRB080710A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7960
SUBJECT: GRB 080710: REM afterglow confirmation & brightening
DATE:    08/07/10 10:05:04 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

P. D'Avanzo, D. Fugazza, L.A. Antonelli, L.  Calzoletti,  S. Campana, 
G.  Chincarini, S. Covino, 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 080710 (Sbarufattion et al. GCN 7957, 
7958) on July 10 starting at 07:14:36 UT.

We can detect in optical and NIR bands the object reported by Li et al. 
(GCN 7959). The object is variable and we measure a brightening from H ~ 
15.0 to H ~14.3 between two epochs of observations (arount 07:21 and 
08:47 UT, respectively). Further analysis is ongoing.


GRB_name: GRB080710A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7961
SUBJECT: UVOT white band observations of GRB080710
DATE:    08/07/10 10:42:45 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 UVOT began observing the field of GRB 080710 3138.2s after the BAT 
trigger. A single white band finding chart was downlinked promptly, and 
a bright, uncatalogued source with magnitude wh = 16.88+/-0.02 is 
detected at
 RA  =  00:33:05.67   = 8.27363
 Dec = +19:30:04.69 = 19.50130
with an uncertainty of 0.5 arcseconds (90% confidence), consistent with 
the XRT position (Sbarufatti et al., GCN 7958) and KAIT position 
(Chornock et al., GCN 7959).

The value quoted above has not been 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: GRB080710A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7962
SUBJECT: GRB 080710: Gemini spectroscopy and probable redshift
DATE:    08/07/10 12:00:49 GMT
FROM:    Daniel Perley at U.C. Berkeley  <dperley@astro.berkeley.edu>

D. A. Perley, R. Chornock, and J. S. Bloom report on behalf of a larger 
collaboration:

Starting at 09:25 UT on 2008 July 10 we began spectroscopy of the 
optical counterpart (Li et al., GCN 7959) of GRB 080710 (Sbarufatti et 
al., GCN 7957) using Gemini-South (+GMOS).  We acquired 2x1200s 
integrations using the B600 grism, covering a wavelength range from 3800 
to 6700 Angstroms.

The spectrum shows several strong absorption features, corresponding to 
the Mg II (2796+2803) doublet, Fe II (2586+2600) doublet, Mg I (2853), 
and Fe II (2344+2374+2382) at a common redshift of z=0.845.  We 
tentatively associate this redshift with GRB 080710.  Additional 
analysis of the spectrum is ongoing.

We thank the Gemini staff for conducting these observations.


GRB_name: GRB080710A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7963
SUBJECT: GRB 080710: Faulkes Telescope North observations
DATE:    08/07/10 14:20:13 GMT
FROM:    David Bersier at Liverpool John Moores U  <dfb@astro.livjm.ac.uk>

D. Bersier (Liverpool JMU) and A. Gomboc (U. Ljubljana)
report on behalf of a larger collaboration:

We observed GRB 080710 (Sbarufatti et al. GCN 7957) with the 2m
robotic Faulkes Telescope North. We obtained multi-colour images
(BVRi) starting 4.2 hours after the burst. We confirm the presence of
a fading source at the position of the afterglow (Li et al. GCN 7959;
D'Avanzo et al GCN 7960). At a time of 4.4 hours after burst we
measure an R-band magnitude of 17.8 (calibrated with respect to USNO
R2). The decay rate is approximately -0.82.

We note that the afterglow is well detected in the B band, indicating
a rather low redshift (in agreement with Perley et al. GCN 7962).

Observations are continuing.


GRB_name: GRB080710A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7964
SUBJECT: GRB 080710: Enhanced Swift-XRT position
DATE:    08/07/10 18:00:38 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 8101 s of XRT Photon Counting mode data and 10 UVOT
images for GRB 080710, 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 = 8.27364, +19.50158 which is equivalent
to:

RA (J2000): 00h 33m 5.67s
Dec (J2000): +19d 30' 05.7"

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), 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: GRB080710A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7965
SUBJECT: GRB080710: Swift/UVOT observations
DATE:    08/07/10 18:50:43 GMT
FROM:    Wayne Landsman at GSFC/SSAI  <wayne.b.landsman@nasa.gov>

W.B. Landsman (NASA/GSFC) and B. Sbarufatti(INAF-OAB) report on behalf 
of the Swift/UVOT team

The Swift/UVOT observed the field of GRB 08710 starting at 3186s after 
the BAT trigger ( Sbarufatti et al., GCN 7957). We detect the afterglow 
in  all seven UVOT filters at the position

RA(J2000)  =   00:33:05.65
DEC(J2000) =  +19:30:05.3

with an estimated uncertainty of 0.5 arcsec (radius, 90% confidence).  
This position is consistent with the enhanced XRT position (Evans et al. 
GCN 7964) and the KAIT afterglow position (Li et al., GCN 7959).     The 
detection in the UVW2 (1950 A) filter is consistent with the redshift of 
~0.845 estimated from spectroscopic observations by Perley et al. (GCN 
7962).   The
white and v exposure are consistent with a decay slope of alpha ~-0.8, 
as also found by Bersier and Gomboc (GCN 7963).

The magnitudes with 1 sigma errors are reported below.

Filter    TMid(s)    Expo(s)               Magnitude
-----------------------------------------------------
white     3185          98              16.88 +/- 0.02
white     5615         186              17.37 +/- 0.03
v         3342         197              17.06 +/- 0.06
v        10560         295              17.79 +/- 0.08
b         5416         197              17.56 +/- 0.05
u         5211         197              16.70 +/- 0.04
uvw1      5006         197              16.86 +/- 0.06
uvm2      3477          58              17.08 +/- 0.17
uvw2      9344         777              17.88 +/- 0.05
-----------------------------------------------------

The above magnitudes are not corrected for the Galactic extinction  
corresponding to a reddening of E{B-V} = 0.07 mag (Schlegel et al. 
1998).  The photometry is on the UVOT flight system described in Poole 
et al. (2008,MNRAS,383,627).


GRB_name: GRB080710A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7966
SUBJECT: GRB 080710: Swift-XRT refined analysis
DATE:    08/07/10 22:14:47 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

Swift XRT began observations of GRB 080710 (Sbarufatti et al., GCN
Circ. 7957) at 08:02 UT, 49 minutes after the trigger. The refined  
position for
the afterglow, obtained using the XRT-UVOT alignment and matching UVOT
field sources to the USNO-B1 catalogue (see Evans et al., GCN Circ.  
7964)
is RA, Dec = 8.27364, 19.50158 which is equivalent to:

RA (J2000):  00 33 5.67
Dec (J2000): +19 30 05.7

with an uncertainty of 1.4 arcsec (radius, 90% confidence).

The XRT observations consist of 7.9 ks in Photon Counting mode. The
light-curve can be fitted by a simple power-law model with slope (1.0  
+/- 0.1),
with superposed flaring activity.

The average spectrum can be modeled by a power-law with photon index  
2.09
+/-0.1 and an intrinsic absorbing column of (1.6 +/-0.7) E21 cm^-2 at
z=0.845 (Perley et al., GCN Circ. 7962) in excess with respect to the  
Galactic
value (4.1E+20 cm^-2, Kalberla et al. 2005). The observed  
(unabsorbed) flux in
the 0.3-10 keV band is 5.35 (5.84)E-12 ergs cm^-2 s^-1. The count  
rate to flux
conversion factor is 4.1E-11.

The predicted flux for tomorrow, 07:13 UT (24 h after the trigger) is
6.9E-13 ergs cm^-2 s^-1.

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


GRB_name: GRB080710A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7967
SUBJECT: GRB 080710: Rapid PROMPT Observations
DATE:    08/07/10 22:30:01 GMT
FROM:    Thomas Summers Brennan at UNC/GRB Group  <bre@email.unc.edu>

E. Weaver, J. P. West, D. Reichart, M. Nysewander, A. LaCluyze, K. 
Ivarsen, J. A. Crain, A. Foster, T. Brennan, J. Haislip, R. Holmes, R. 
Rhine, M. Schubel, J. Styblova, and A. Trotter report:

Skynet observed the localization of GRB 080710 (Sbarufatti et al., GCN 
7957) with three of the 16" PROMPT telescopes at CTIO beginning 64 
seconds after the trigger in BVRI.

We detect the afterglow (Sbarufatti et al., GCN 7957) in BVRI.  At 627
seconds after the burst we measure B ~ 17.7 mag (calibrated to 9 USNO
B1 stars), at 626 seconds we measure V ~ 17.6 mag (calibrated to 12
USNO B1 stars), at 535 seconds we measure R ~ 17.6 mag (calibrated to
13 NOMAD stars), and at 444 seconds we measure I ~ 16.9 mag
(calibrated to 11 USNO B1 stars).


GRB_name: GRB080707A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7968
SUBJECT: GRB 0800707: optical observations
DATE:    08/07/10 23:04:02 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

V. Rumyantsev (CrAO),  A. Pozanenko (IKI) report on behalf of larger GRB 
follow-up collaboration:

We observed  the afterglow  (Clemens et al., GCN 7948, Fynbo et al., GCN 
7949) of GRB 080707 (Schady et al., GCN  7947)  in R-band on July 8 between 
(UT) 00:00:26 - 00:49:43  with Zeiss-1000 (Simeiz) telescope of CrAO 
observatory.

Based on  USNOB1.0 star with ID 1231-0038095  at RA = 02:10:27.08 , Dec. 
+33:06:32.5  (R2 = 17.11)  we estimated brightness of  the afterglow on 
0.6647 days:

T0+       Exposure  R_mag
(mid)

0.6647 d  16x180 s   21.22 +/- 0.25

Taking into account early photometry  (Fynbo et al., GCN 7949, Clemens et 
al., GCN 7948) one may suggest a plateau or re-brightening phase of the 
afterglow light curve between 0.07 and ~1 days after burst onset..

The combined image can be found at
http://grb.rssi.ru/GRB080707/GRB080707.gif

This message may be cited. 


GRB_name: GRB080710A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7969
SUBJECT: GRB 080710, Swift-BAT refined analysis
DATE:    08/07/11 01:16:10 GMT
FROM:    Takanori Sakamoto at NASA/GSFC  <takanori.sakamoto-1@nasa.gov>

J. Tueller (GSFC), S. D. Barthelmy (GSFC), W. Baumgartner (GSFC/UMBC),
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 (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 the recent telemetry downlink,
we report further analysis of BAT GRB 080710 (trigger #316534)
(Sbarufatti, et al., GCN Circ. 7957).  The BAT ground-calculated position is
RA, Dec = 8.259, 19.484 deg which is 
   RA(J2000)  =  00h 33m 02.2s 
   Dec(J2000) = +19d 29' 00.8" 
with an uncertainty of 2.3 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 48%.
 
The mask-weighted light curve shows a weak emission starting around T-120 sec, 
and then, following a FRED like spike starting from T+0 sec and ending at 
T+43 sec.  T90 (15-350 keV) is 120 +- 17 sec (estimated error including systematics).
 
The time-averaged spectrum from T-96.9 to T+43.3 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.47 +- 0.23.  The fluence in the 15-150 keV band is 1.4 +- 0.2 x 10^-06 erg/cm2.
The 1-sec peak photon flux measured from T+0.89 sec in the 15-150 keV band
is 1.0 +- 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/316534/BA/


GRB_name: GRB080710A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7970
SUBJECT: GRB 080710: Lick IR detection
DATE:    08/07/11 03:20:32 GMT
FROM:    Daniel Perley at U.C. Berkeley  <dperley@astro.berkeley.edu>

D. A. Perley (UC Berkeley) and C. Melis (UCLA) report:

On the night of 2008-07-10 starting at 10:32:30 UT, we began a series of 
IR exposures with the Lick Shane 3 meter telescope, equipped with the 
GEMINI IR imager.  We acquired imaging in J and K' filters 
simultaneously between 10:32 and 10:44.  We returned to the field during 
morning twilight and took additional imaging between 12:19 and 12:25 in 
H and K' simultaneously.

Calibrating to two nearby 2MASS stars, we estimate a preliminary 
magnitude in the first epoch J-band imaging of:

J = 16.24 +/- 0.05

between 10:32 and 10:44 (mid-time of 206 minutes after the GRB.)

The GRB afterglow displays tentative evidence of brightening over the 
exposure period.  Additional analysis is ongoing.


GRB_name: GRB080702B
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7971
SUBJECT: GRB 080702B: Swift XRT confirmation of the afterglow
DATE:    08/07/11 09:18:26 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

P.A. Evans (U. Leicester) and M. de Pasquale (MSSL/UCL) report on behalf
of the Swift team.

Swift has reobserved the field of GRB 080702B (Cummings et al. GCN Circ.
7924) in two pointings on 2008 July 8 and 2008 July 10 (six and eight
days after the burst respectively), obtaining 7 ks of data in total.

The second X-ray source reported in our previous circular (Evans et al.
(GCN Circ 7931) is not detected in these data, with a 3-sigma
upper limit of 1.3e-3 counts per second. The count-rate in the initial
observation was (5.4 +/- 1.8)e-3 counts per second, thus the source has
faded.

We therefore conclude that this was the afterglow of GRB 080702B.

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


GRB_name: GRB080710A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7972
SUBJECT: GRB 080710: TLS observations, steepening afterglow decay
DATE:    08/07/11 14:14:53 GMT
FROM:    Alexander Kann at TLS Tautenburg  <kann@tls-tautenburg.de>

S. Schulze, D. A. Kann, A. Rossi, E. Gonsalves, C. Hoegner and B. Stecklum 
(TLS Tautenburg) report:

We observed the optical afterglow location (Li et al., GCN 7959) of Swift 
GRB 080710 (Sbarufatti et al., GCN 7957) with the TLS 1.34m Schmidt 
telescope under inclement but improving conditions. 600 second B and V 
observations were affected by passing clouds and yielded no detections and 
shallow upper limits only. We detect the afterglow clearly in a single Rc 
image as well as in four Ic images (600 seconds each) before dawn shut us 
down. We measure afterglow magnitudes against eight USNOB1.0 stars in each 
case:

time (days) filter magnitude exposure

0.7275  Rc 20.05 +/- 0.12 600

0.7468  Ic 19.75 +/- 0.13 4 x 600

In comparison with the magnitude as well as the slope reported from the 
Faulkes Telescope North (Bersier et al., GCN 7963) (R = 17.8 at 4.4h, 
alpha = 0.82), our measurement implies a significant steepening of the 
decay, we find alpha = 1.5 between 4.4 and 17.5 hours after the GRB. This 
implies that a break must have occurred inbetween, and possibly the slope 
during the time of our observations is already > 2 and the break is a jet 
break.

Using the redshift of 0.845 (Perley et al., GCN 7962) as well as the 
values derived in the BAT refined analysis (Tueller et al., GCN 7969) and 
estimating the peak energy following equation 3 of Liang et al. (2007, 
ApJ, 670, 565), we derive a bolometric isotropic energy release of 6.8 
+2.0 -1.9 x 10^51 erg. If there is a jet break before 17 hours, this would 
imply a low collimation-corrected energy release.

No further observations from TLS are possible due to an instrument change.

This message may be cited.


GRB_name: GRB080710A
Detection_method: MITSuME
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7973
SUBJECT: GRB 080710: Optical observation with MITSuME Okayama
DATE:    08/07/11 23:35:57 GMT
FROM:    Michitoshi Yoshida at Okayama Astrophysical Obs  <yoshida@oao.nao.ac.jp>

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

We observed the optical afterglow (Li et al. GCN 7959; D'Avanzo
et al. GCN 7960; Schady GCN 7961) of GRB 080710 (Sbarufatti
et al. GCN 7957) with the optical three color (g', Rc and Ic)
imager attached to the MITSuME 50cm telescope of Okayama
Astrophysical Observatory. We started the observation at
2008-07-10 15:37:23 UT. Photometric results are listed below.
We used four USNO-B1.0 stars around the afterglow. The Rc band
magnitude is consistent with the power-law decay with alpha = 1.5
reported by Schulze et al. (GCN 7972).

mid-UT of the observation:
   2008-07-10 16:27:00 (0.384595 days after trigger)

T-T0(days) exp-T        g'              Rc              Ic
----------------------------------------------------------------
0.384595   86min  18.79 +/- 0.08  18.96 +/- 0.06  18.57 +/- 0.06
----------------------------------------------------------------


GRB_name: GRB080603B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7974
SUBJECT: GRB 080603B: optical observations in CrAO
DATE:    08/07/12 08:53:15 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

V. Rumyantsev, K. Antoniuk (CrAO),  A. Pozanenko (IKI) report on behalf of 
larger GRB follow-up collaboration:

We observed the afterglow  (Rujopakarn, et al., GCN 7792) of the Swift GRB 
080603B (Mangano et al., GCN 7794)  on June 04 between (UT) 19:49:07 - 
20:49:27  with AZT-11 (Nauchny) telescope of  CrAO observatory in R-band. 
In a combined image we detect the afterglow. A photometry is obtained in 
comparison with nearby USNOB-1.0 stars:

T0+     Exposure  R_mag            UL
(mid)

1.0087 d  19x180    21.30 +/- 0.25   21.8

The message may be cited. 


GRB_name: GRB080603B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7975
SUBJECT: GRB 080603B: optical observations in MAO
DATE:    08/07/12 08:57:45 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

M. Ibrahimov, R. Karimov (MAO), V. Rumyantsev (CrAO),  A. Pozanenko (IKI) 
report on behalf of larger GRB follow-up collaboration:

We observed the afterglow  (Rujopakarn, et al., GCN 7792) of the Swift GRB 
080603B (Mangano et al., GCN 7794)  on June 04 between (UT) 16:12:24 - 
16:34:23  with AZT-22 (Maidanak) telescope of  MAO observatory in R-band. 
The afterglow is well detected in each individual frame.

A photometry of the two combined images is obtained in comparison with 
nearby USNOB-1.0 stars:

T0+     Exposure  R_mag
(mid)

0.8571 d 2x300 20.49 +/- 0.07
0.8703 d 3x300 20.71 +/- 0.08

The message may be cited. 


GRB_name: GRB080603A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7976
SUBJECT: GRB 080603A: CrAO optical observations
DATE:    08/07/12 15:18:05 GMT
FROM:    Alexei Pozanenko at IKI, Moscow  <apozanen@iki.rssi.ru>

V. Rumyantsev, K. Antoniuk (CrAO),  E. Klunko (ISTP),  A. Pozanenko (IKI) 
report on behalf of larger GRB follow-up collaboration:

We observed  the field of  INTEGRAL GRB 080603A (Paizis et al., GCN 7790) in 
R-band on June 03 between (UT)  19:16:25 - 19:43:54 with AZT-11(Nauchny) 
telescope of CrAO observatory.   We detect optical afterglow (Gomboc et al., 
GCN 7788; Chornock  et al., GCN 7789)  in coordinates

RA(J2000):  18 37 37.97
Dec(J2000): +62 44 38.9

with uncertanitie is 0.5".

Based on  USNOB1.0 star with ID 1527-0313986 at RA = 18:37:55.186, Dec. 
+62:45:32.28 (R1 = 16.74)  we estimated brightness of  the afterglow in a 
combined image at  0.3424 days:

T0+,       Exposure,   R_mag, UL
(mid time)

0.3424 d  10x180 s  20.62 +/- 0.13   21.8

This message may be cited. 


GRB_name: GRB080702A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7977
SUBJECT: GRB 080702A: optical upper limit
DATE:    08/07/14 14:40:04 GMT
FROM:    Giuseppe Greco at U Bologna  <giuseppe.greco2@studio.unibo.it>

G. Greco (Bologna University), F. Terra (Second University of Roma "Tor
Vergata"), C. Bartolini, A. Guarnieri, A. Piccioni (Bologna University),
F. Munz, G. Pizzichini (INAF/IASF Bologna), D. Nanni (INAF/OAR and Second
University of Rome "Tor Vergata"), I. Bruni (Bologna Observatory) report:

We observed the field of GRB 080702A (GCN 7920, de Pasquale et al.)
with the 152 cm telescope located in Loiano under
clear sky conditions (seeing~2").

By adding three consecutive 10 min exposures in the Rc filter
at mean time 2008 July 02.996 UT we do not detect any afterglow
candidate in the XRT error circle (GCN 7923, Goad et al.).

Our 3-sigma limiting magnitude is R~21 (based on Nomad1 catalogue).
The image has been posted in our public directory
from where it can be retrieved by sftp using

hostname: ermione.bo.astro.it
username: publicGRB
password: GRB_bo.
directory: GRB080702A


GRB_name: GRB080714A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7978
SUBJECT: GRB 080714: Swift detection of a burst
DATE:    08/07/14 18:11:28 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

M. Perri (ASDC), S. D. Barthelmy (GSFC), J. R. Cummings (NASA/UMBC),
N. Gehrels (NASA/GSFC), S. T. Holland (CRESST/USRA/GSFC),
E. A. Hoversten (PSU), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), V. Mangano (INAF-IASFPA),
F. E. Marshall (NASA/GSFC), P. T. O'Brien (U Leicester),
J. P. Osborne (U Leicester), D. M. Palmer (LANL),
D. Perez (U Leicester), B. Preger (ASDC), P. Schady (MSSL-UCL),
M. Stamatikos (NASA/ORAU), R. L. C. Starling (U Leicester),
G. Stratta (ASDC), M. C. Stroh (PSU), D. E. Vanden Berk (PSU) and
L. Vetere (PSU) report on behalf of the Swift Team:

At 17:52:56 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 080714 (trigger=316910).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 188.109, -60.279 which is 
   RA(J2000) = 12h 32m 26s
   Dec(J2000) = -60d 16' 42"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single-peaked
structure with a duration of about 40 sec.  The peak count rate
was ~5000 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 17:54:16.4 UT, 79.7 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 188.10733, -60.27708 which
is equivalent to:
   RA(J2000)  = 12h 32m 25.76s
   Dec(J2000) = -60d 16' 37.5"
with an uncertainty of 3.1 arcseconds (radius, 90% containment). This
location is 7.5 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
5.44e+21 cm^-2 (Kalberla et al. 2005). 

The initial flux in the 2.5 s image was 5.01e-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 89 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.  Because of the density of catalogued stars, further
analysis is required to report an upper limit for any afterglow in the
sub-image.    No correction has been made for the large, but uncertain extinction
expected. 

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


GRB_name: GRB080714A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7979
SUBJECT: GRB 080714: Swift-BAT refined analysis 
DATE:    08/07/15 02:59:58 GMT
FROM:    Jay R. Cummings at NASA/GSFC/Swift  <jayc@milkyway.gsfc.nasa.gov>

S. D. Barthelmy (GSFC), W. Baumgartner (GSFC/UMBC), 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), M. Perri (ASDC), T. Sakamoto (GSFC/UMBC),
G. Sato (ISAS), M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC), T. Ukwatta 
(GWU)
on behalf of the Swift-BAT team:

Using the data set from T-240 to T+963 sec from the recent telemetry 
downlink,
we report further analysis of BAT GRB 080714 (trigger #316910)
(Perri, et al., GCN Circ. 7978).  The BAT ground-calculated position is
RA, Dec = 188.104, -60.274 deg which is
   RA(J2000) = 12h 32m 24.9s 
   Dec(J2000) = -60d 16' 28.2"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment). The
partial coding was 43%. 

The mask-weighted lightcurve shows a single peak with a rise time of about
3 seconds and an exponential decay with a time constant of about 10 
seconds. 
T90 (15-350 keV) is 33 +- 9 sec (estimated error including systematics).
There is a small peak in the raw light curve, mostly above 25 keV, at about
T-90 sec that appears to be from a different source, out of the field of 
view.

The time-averaged spectrum from T-3.6 to T+50.3 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
1.52 +- 0.08. The fluence in the 15-150 keV band is 2.5 +- 0.1 x 10^-06 
erg/cm2.
The 1-sec peak photon flux measured from T-0.37 sec in the 15-150 keV band
is 4.2 +- 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/316910/BA/


GRB_name: GRB080714A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7980
SUBJECT: GRB 080714: Enhanced Swift-XRT position
DATE:    08/07/15 06:31:13 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 4736 s of XRT Photon Counting mode data and 4 UVOT
images for GRB 080714, 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 = 188.10601, -60.27775 which is equivalent
to:

RA (J2000): 12h 32m 25.44s
Dec (J2000): -60d 16' 39.9"

with an uncertainty of 2.3 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: GRB080714A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7981
SUBJECT: GRB 080714: Swift-XRT refined analysis
DATE:    08/07/15 14:04:07 GMT
FROM:    Giulia Stratta at ASDC  <giulia.stratta@gmail.com>

G. Stratta, M. Perri, B. Preger (ASDC) report on behalf of the
Swift-XRT team:

We analysed the first 3 orbits of XRT data for GRB 080714 (Perri et al.,
GCN Circ. 7978) taken from 88s after the trigger (T0) in Windowed Timing
(WT)
mode and then in Photon Counting (PC) mode from T0+233 s to T0+9874 s.
The UVOT-enhanced XRT position was given by Goad et al. (GCN Circ. 7980).

The X-ray light curve from T0+88s up to ~T0+300s shows an initial 40 seconds
long flat segment followed by an increasingly steepening decay. Starting
from
T0+300s (PC data) the light curve can be fit with a power law model with a
best fit slope of 1.0+/-0.1.

The WT data spectrum from T0+88s to T0+231s is well fitted by an absorbed
power law model with photon index Gamma=1.14+/-0.05 and a total equivalent
hydrogen column density of NH=(0.3+/-0.1)e22 cm**-2. The Galactic NH is
5.44e21 cm**-2 (Kalberla et al. 2005). The 0.3-10 keV observed (unabsorbed)
flux is (3.4+/-0.2)e-10 erg/cm**2/s ((3.9+/-0.2)e-10 erg/cm**2/s).

If the light-curve continues to decay with the same rate, the count rate
24 hours after the trigger is estimated to be ~6e-3 counts/s, which
corresponds to an observed flux of ~5e-13 erg/cm**2/s.

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


GRB_name: GRB080714A
Detection_method: Swift-UVOT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7982
SUBJECT: GRB 080714: Swift/UVOT Detection of an Optical Afterglow
DATE:    08/07/15 16:06:40 GMT
FROM:    Frank Marshall at GSFC  <marshall@milkyway.gsfc.nasa.gov>

F.E. Marshall (NASA/GSFC) and M. Perri (ASDC)
report on behalf of the Swift/UVOT team:

The Swift/UVOT observed the field of GRB 080714 starting 90 s after
the BAT trigger (Perri et al., GCN Circ. 7978).  The burst is in
a crowded field only 2.5 degrees from the Galactic Plane. 
We find a fading source inside the enhanced XRT error circle 
(Goad et al., GCN Circ. 7980) in observations with the White and 
V filters. The preliminary position for the afterglow is:

  RA(J2000)  =  12:32:25.44 = 188.1060
  DEC(J2000) = -60:16:40.4  = -60.2779

with a 90% confidence error radius of about 0.8 arcsec.

The measured magnitudes in the UVOT photometric system (Poole et al.
2008, MNRAS, 383, 627) and 3-sigma upper limits for detecting
a source in the first two finding chart (FC) exposures and 
subsequent co-added exposures are:

Filter          T_start(s)   T_stop(s)      Exp(s)       Mag 

white (FC)          90          189           98         20.2 +/- 0.2
white             4290         4489          197        >20.7
v (FC)             197          596          393         19.1 +/- 0.2
v                 5896         6095          197        >19.7
b                  677         4284          206        >20.2
u                  652        12382         1137        >20.7
uvw1               628         6505          236        >19.7
uvm2               602         6300          236        >19.9
uvw2               707        16498         1007        >20.8

The values quoted above are not corrected for the predicted large, but uncertain,
Galactic extinction the direction of the burst (Schlegel et al. 1998).


GRB_name: GRB080714A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7983
SUBJECT: Konus-Wind observation of GRB 080714
DATE:    08/07/15 18:22:34 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, P.
Oleynik, M. Ulanov, D. Svinkin, and T. Cline on behalf of the Konus-Wind
team report:

The long GRB 080714 (Swift-BAT trigger
#316910: Perri et al., GCN 7978, Barthelmy et al., GCN 7979) triggered
Konus-Wind at T0=64378.478 s UT (17:52:58.478).

The burst light curve shows a single pulse with a duration of ~20s.

As observed by Konus-Wind the burst
had a fluence of 3.64(-0.60, +0.87)x10^-6 erg/cm2,
and a 256-ms peak flux measured from T0+0.544 s
of 6.84(-1.79, +2.01)x10^-7 erg/cm2/s
(both in the 20 keV - 1 MeV energy range).

The time-integrated spectrum of the burst
(from T0 to T0+16.640 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 = -1.24(-0.39, +0.46)
and Ep = 137(-34, +100) keV (chi2 = 48.3/52 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/GRB080714_T64378/


GRB_name: GRB080714A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7984
SUBJECT: GRB 080714: GROND confirmation of the optical/NIR afterglow
DATE:    08/07/16 06:43:03 GMT
FROM:    Thomas Kruehler at MPE/MPI  <kruehler@mpe.mpg.de>

T. Kruehler, J. Greiner, C. Clemens, A. Yoldas (all MPE Garching), A.
Kupcu Yoldas (ESO) and G. Szokoly (Eoetvoes Univ., Budapest) report on
behalf of the GROND team: 

We observed the field of GRB 080714 (Swift trigger 316910; M. Perri et
al., GCN #7978) in two epochs, simultaneously in g'r'i'z'JHK with GROND
(Greiner et al. 2008, PASP 120, 405) mounted at the 2.2m ESO/MPI telescope
at La Silla Observatory (Chile). 

We detect the optical afterglow reported by Marshall & Perri (GCN #7982) at 

RA (J2000) = 13h 32m 25.49s
DEC (J2000) = -60d 16' 39.3" 

with an absolute uncertainty of 0.6". 

Preliminary photometry yields the following magnitudes against USNO-B1 and
2MASS field stars in stacked images: 


Band  T_mid(h)     Exp(min)   Mag 

g'    6.4058       50         > 24.3
g'    30.3847      32         > 23.4
r'    6.4058       50         22.76 +- 0.08
r'    30.3847      32         > 23.6
i'    6.4058       50         21.15 +- 0.07
i'    30.3847      32         22.68 +- 0.24
z'    6.4058       50         20.39 +- 0.06
z'    30.3847      32         21.82 +- 0.29
J     6.2827       40         18.58 +- 0.11
J     30.2958      30         20.00 +- 0.16
H     6.2827       40         17.25 +- 0.14
H     30.2958      30         18.52 +- 0.24 

not corrected for the expected Galactic foreground reddening of around
E(B-V) =  1.15 mag (Schlegel et al., 1998).
Given the high foreground extinction, the non detection in g' is
consistent with the powerlaw slope of the broad band SED derived from r to
H and does not necessarily imply a high redshift. 

Additionally, we note the presence of a nearby, faint (r'~ 24.1 +- 0.2)
source at 

RA (J2000) = 13h 32m 25.60s
DEC (J2000) = -60d 16' 37.7" 

roughly 1.8" away from the afterglow, which may influence the photometry
in the second epoch.


GRB_name: GRB080721A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7988
SUBJECT: GRB 080721: Swift detection of a burst with a bright optical counterpart. 
DATE:    08/07/21 10:42:45 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

F. E. Marshall (NASA/GSFC), A. P. Beardmore (U Leicester),
D. N. Burrows (PSU), P. A. Evans (U Leicester),
N. Gehrels (NASA/GSFC), C. Gronwall (PSU), C. Guidorzi (INAF-OAB),
S. T. Holland (CRESST/USRA/GSFC), V. Mangano (INAF-IASFPA),
P. T. O'Brien (U Leicester), J. P. Osborne (U Leicester),
K. L. Page (U Leicester), D. M. Palmer (LANL),
D. Perez (U Leicester), M. Perri (ASDC), B. Preger (ASDC),
P. Romano (INAF-IASFPA), M. Stamatikos (NASA/ORAU),
R. L. C. Starling (U Leicester), T. N. Ukwatta (GSFC/GWU),
P. A. Ward (MSSL-UCL) and H. Ziaeepour (UCL-MSSL) report on behalf of
the Swift Team:

At 10:25:16 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 080721 (trigger=317508).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 224.471, -11.712 which is 
   RA(J2000) = 14h 57m 53s
   Dec(J2000) = -11d 42' 43"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed at least 4 peaks
structure with a duration of about 35 sec.  The peak count rate
was ~19k counts/sec (15-350 keV), at ~0 sec after the trigger,
during the second peak. 

The XRT began observing the field at 10:27:04.1 UT, 107.2 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 224.4899, -11.7242 which is equivalent to:
   RA(J2000)  = 14h 57m 55.9s
   Dec(J2000) = -11d 43' 27.3"
with an uncertainty of 4.7 arcseconds (radius, 90% containment). This
location is 79 arcseconds from the BAT onboard position, within the BAT
error circle. No event data are yet available to determine the column
density using X-ray spectroscopy. 

UVOT took a finding chart exposure of nominal 100 seconds with the White
(160-650 nm) filter starting 180 seconds after the BAT trigger. There is a
candidate afterglow in the list of sources generated on-board at
  RA(J2000)  =  14:57:55.8 = 224.48268
  DEC(J2000) = -11:43:25   = -11.72361
with a 1-sigma error radius of about 1.0 arc sec. The estimated white
magnitude is 14.6 with a 1-sigma error of about 0.01 mag. No correction
has been made for Galactic extinction. 

Burst Advocate for this burst is F. E. Marshall (marshall 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: GRB080721A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7989
SUBJECT: GRB 080721: Swift-XRT correct position
DATE:    08/07/21 12:34:14 GMT
FROM:    Cristiano Guidorzi at INAF-OAB  <cristiano.guidorzi@brera.inaf.it>

C. Guidorzi (INAF-OAB), P. A. Evans and K. L. Page (U Leicester)
report on behalf of the Swift-XRT team:

We note that the correct XRT position of GRB 080721 (Marshall et al.,
GCN Circ. 7988) is that given in sexagesimal coordinates, which
corresponds to RA, Dec 224.48292, -11.72425 degrees (J2000; 4.7 arcsec
radius, 90%) and is also consistent with the UVOT position.
The XRT position given in degrees in the same circular, which has also
been distributed in the XRT position notice, is not correct.
We apologise for any inconvenient this may have caused.


GRB_name: GRB080721A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7990
SUBJECT: GRB 080721 : Lulin Optical follow-ups
DATE:    08/07/21 13:04:35 GMT
FROM:    Yuji Urata at Saitama U  <urata@asiaa.sinica.edu.tw>

T-W Chen, L-C Huang, Y-T Chen (NCU)
K.Y Huang (ASIAA) and Y. Urata (Saitama U./ASIAA)
on behalf of the EAFON report;

"We have been monitoring the optical afterglow of GRB080721 (Marshall
et al. GCN Circ 7988) using the Lulin 1 m telescope after the twilight
(~ 96 min after the burst). Based on Lulin R-band data, the optical
afterglow is located at RA=14:57:55.835, Dec=-11:43:24.76 with less
than 1" position error.  The brightness of the optical afterglow at 98
min after the burst is R~18.1.

Further optical observation is in progress."
    


GRB_name: GRB080721A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7991
SUBJECT: GRB 080721: Swift/UVOT Photometric Redshift
DATE:    08/07/21 15:05:46 GMT
FROM:    Stephen Holland at USRA/NASA/GSFC/SSC  <sholland@milkyway.gsfc.nasa.gov>

S. T. Holland, P. A. Ward (MSSL-UCL), and F. E. Marshall (NASA/GSFC)
report on behalf of the Swift/UVOT Team:

Preliminary UVOT photometry of the afterglow of GRB 080721 (Marshall,
et al. 2008, GCN Circ. 7988) shows that the afterglow is strongly
detected in the U band, but not in the UVW1, UVM2, or UVW2 bands at
approximately 825 s after the BAT trigger.  This suggests that the
redshift of GRB 080721 may be greater than approximately 2.3.


GRB_name: GRB080721A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7992
SUBJECT: GRB 080721, Swift-BAT refined analysis
DATE:    08/07/21 15:19:27 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

J. Cummings (GSFC/UMBC), S. D. Barthelmy (GSFC), W. Baumgartner (GSFC/UMBC),
E. Fenimore (LANL), N. Gehrels (GSFC), H. Krimm (GSFC/USRA),
C. Markwardt (GSFC/UMD), F. E. Marshall (NASA/GSFC), K. McLean (GSFC/UMD),
D. Palmer (LANL), T. Sakamoto (GSFC/UMBC), G. Sato (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+750 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 080721 (trigger #317508)
(Marshall, et al., GCN Circ. 7988).  The BAT ground-calculated position is
RA, Dec = 224.481, -11.709 deg, which is 
   RA(J2000)  =  14h 57m 55.4s 
   Dec(J2000) = -11d 42' 33.3" 
with an uncertainty of 1.3 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 4%.
 
The mask-weighted light curve shows approximately six peaks.  The first starts
at ~T-11 sec and peaks at ~T-7 sec.  The second and third peaks are much 
brighter.  They peak at ~T+1 and ~T+7 sec.  The remaining peaks are much smaller
and stretch out to ~T+370 sec.  T90 (15-350 keV) is 16.2 +- 4.5 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-2.6 to T+25.8 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.11 +- 0.08.  The fluence in the 15-150 keV band is 1.2 +- 0.1 x 10^-5 erg/cm2.
The 1-sec peak photon flux measured from T-0.16 sec in the 15-150 keV band
is 20.9 +- 1.8 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/317508/BA/


GRB_name: GRB080721A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7993
SUBJECT: GRB 080721: Enhanced Swift-XRT position
DATE:    08/07/21 16:20:26 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 2722 s of XRT Photon Counting mode data and 6 UVOT
images for GRB 080721, 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 = 224.48231, -11.72363 which is equivalent
to:

RA (J2000): 14h 57m 55.75s
Dec (J2000): -11d 43' 25.1"

with an uncertainty of 1.5 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, 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: GRB080721A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7994
SUBJECT: GRB 080721: Swift-XRT refined analysis
DATE:    08/07/21 17:16:43 GMT
FROM:    Cristiano Guidorzi at INAF-OAB  <cristiano.guidorzi@brera.inaf.it>

C. Guidorzi, F. Pasotti (INAF-OAB), F. E. Marshall (NASA/GSFC)
report on behalf of the Swift-XRT team:

We have analysed the first three orbits of Swift-XRT data obtained for GRB
080721 (Marshall et al., GCN Circ. 7988), covering 1.3 ks and 2.8 ks
of Windowed Timing (WT) and Photon Counting (PC) modes data, respectively,
between 113 s and 10.6 ks after the trigger.
Notably, the whole first orbit data are taken in WT mode.
The UVOT-enhanced XRT position was given by Osborne et al. in GCN Circ. 
7993.

The light-curve can be modelled by an initial power law with index
0.75 +/- 0.04 followed by a constant rate step from ~260 to 330 s,
after which the curve resumes a power-law decay with an index of
1.06 +/- 0.01 up to 10.6 ks (chisq/dof = 1292/1207).

A spectrum extracted from the first orbit of data can be modelled with an
absorbed power-law, with Gamma = 1.90 +/- 0.02 and
NH = (1.10 +/- 0.05)x1e21 cm^-2, in excess of the Galactic column
in this direction of 6.9e20 cm^-2. We found no evidence for spectral
evolution during this time interval.
The observed (unabsorbed) flux over this time interval (113-1370 s
post-trigger) is 2.2e-9 (2.7e-9) erg cm^-2 s^-1.

If the light-curve continues to decay with alpha ~1.06, the count rate 24
hours after the burst is estimated to be 0.23 count s^-1, which
corresponds to an observed flux of 9.6e-12 erg cm^-2 s^-1.

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


GRB_name: GRB080721A
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7995
SUBJECT: Konus-Wind observation of GRB 080721
DATE:    08/07/21 18:44:21 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, P.
Oleynik, M. Ulanov, D. Svinkin, and
T. Cline on behalf of the Konus-Wind team report:

The bright GRB 080721 (Swift-BAT trigger #317508: Marshall et al., GCN
7988, Cummings et al., GCN 7992) triggered Konus-Wind at T0=37510.927 s 
UT (10:25:10.927).

The burst light shows multipeaked structure with a duration of ~30 s.

As observed by Konus-Wind the burst
had a fluence of 8.38(-0.60, +0.62)x10^-5 erg/cm2,
and a 64-ms peak flux measured from T0+9.648 s
of (1.96 +/- 0.31)x10^-5 erg/cm2/s
(both in the 20 keV - 5 MeV energy range).

The time-integrated spectrum of the burst
(from T0 to T0+23.808 s) is well fitted (in the 20 keV - 5 MeV range)
by GRBM (Band) model for which:
the low-energy photon index is alpha = -0.933(-0.084, +0.106),
the high energy photon index beta = -2.43(-0.42, +0.24),
the peak energy Ep = 485(-59, +67) keV (chi2 = 60.6/76 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/GRB080721_T37510/


GRB_name: GRB080721A
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7996
SUBJECT: GRB 080721: UVOT Follow-Up Observations
DATE:    08/07/21 20:55:10 GMT
FROM:    Paul Ward at MSSL  <paw@mssl.ucl.ac.uk>

P. Ward (MSSL-UCL),  S. T. Holland (CRESST/USRA/GSFC) and F. E. Marshall 
(NASA/GSFC) report on behalf of the Swift/UVOT team:

The Swift Ultra-Violet/Optical Telescope (UVOT) started observing
GRB 080721 (Marshall et al., GCN 7988) ~118 seconds after the trigger.

A fading afterglow is found in the UVOT White, V, B and U filters. The 
refined Swift/UVOT position of the optical afterglow candidate is:

  RA(J2000)  = 14:57:55.855 =  224.48273
  DEC(J2000) = -11:43:24.54 = -11.723483

with an estimated uncertainty of 0.5 arcsec (radius, 90% confidence).
The following table gives the measured magnitudes:

Filter  T_start T_stop Exp     Mag

white  118    217   99.8   14.58 +/- 0.00
white  858    957   99.8   16.94 +/- 0.03
white 5173   5372  199.8   19.12 +/- 0.08
white 6609   6808  199.8   19.43 +/- 0.11
v      225    624  399.7   14.98 +/- 0.01
v      964   1363  399.8   16.47 +/- 0.03
v     5583   5782  199.8   18.27 +/- 0.17
v     7020   7157  137.7   18.40 +/- 0.23
b      704   6603  409.4   16.56 +/- 0.12
u      680   6398  439.3   16.58 +/- 0.12
uvw1   655   6192  439.2   > 18.01
uvm2   631   5987  245.3   > 17.58
uvw2   734   7014  419.4   > 18.03

Using the measured magnitudes we find a power law decay index of -1.2 and 
-1.01 in the white and V filters respectively. The strong detection in the 
U band, but not in the UVW1, UVM2, or UVW2 bands gives an estimated 
photometric redshift in the range of 2.3 < z < 2.8.

The values quoted above are in the UVOT photometric system
(Poole et al. 2008, MNRAS, 383, 627). No correction has been
made for the expected extinction corresponding to E(B-V) of
0.100 mag in the direction of the burst (Schlegel et al. 1998).

[GCN OPS NOTE(12aug08): Per author's request, the "080703" was changed to
"080721" in the first sentence.]


GRB_name: GRB080721A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7997
SUBJECT: TNG/DOLORES redshift for GRB080721
DATE:    08/07/21 23:16:34 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

P. D'Avanzo (INAF-OAB), V. D'Elia (INAF-OAR), G. Adreuzzi, G. Tessicini 
(INAF-TNG), L. A. Antonelli, F. Fiore (INAF-OAR), D. Fugazza, C. 
Guidorzi (INAF-OAB) and G. Chincarini (Univ. Bicocca) report, on behalf 
of the CIBO collaboration:

Following the Swift detection of GRB080721 (Marshall et al., GCN 7988), 
we triggered observations with the DOLORES low resolution spectrograph, 
mounted at the Italian TNG telescope located in the Canary Islands 
(Spain). The observations were performed using the LR-B grism. We took a 
1800 s spectrum starting around Jul 21 at 21:30 UT (about 11.0 hours 
after the burst) and covering the range 300-780 nm with a resolution of 
R ~ 600.

A preliminary analysis of the spectra shows a broad absorption feature 
at lambda_obs ~ 440 nm (based on a preliminary wavelength calibration). 
Interpreting this feature as Ly-alpha we infer a redshift z = 2.602, in 
agreement with the UVOT photometric redshift estimate (Holland et al., 
GCN 7991; Ward et al. GCN 7996). At this redshift we can detect also 
(rest frame) other absorption features like: CII (133.4 nm), SiIV 
doublet (139.3-140.2 nm), SiII (152.6 nm), CIV doublet (154.8-155.0 nm).

We are very grateful for the excellent support of the TNG staff.


GRB_name: GRB080721A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7998
SUBJECT: GRB 080721: OA fading and redshift
DATE:    08/07/22 08:45:39 GMT
FROM:    Pall Jakobsson at U Hertfordshire  <P.Jakobsson@herts.ac.uk>

P. Jakobsson (U. Hertfordshire), D. Malesani, P. M. Vreeswijk,
J. P. U. Fynbo, B. Milvang-Jensen (DARK/NBI), A. de Ugarte Postigo (ESO),
B. Nordstrom (NBI), E. Stonkute (ITPA, Vilnius) and P. Sorensen (NOT)
report on behalf of a larger collaboration:

We observed the optical afterglow of GRB 080721 (Marshall et al., GCN 7988;
Chen et al., GCN 7990) with ALFOSC on the Nordic Optical Telescope at
La Palma. The afterglow is well detected in a single 300 s exposure
starting on 21.875 July 2008 (10.6 hr after the GRB). Comparison with
several USNO-B1 stars (R1 magnitudes) yields R = 20.0 +/- 0.2, where most
of the error comes from the calibration. Using the R-band magnitude
provided by Chen et al., the inferred decay index is alpha ~ 0.9.

Low resolution spectra (3 x 30 min) were also obtained. The combined
spectrum displays a strong absorption feature around 4350 A, with the flux
dropping substantially blueward of this feature. Associating it with
Ly-alpha gives a redshift of z ~ 2.6 for the burst. We find several other
absorption features, including O I, Si II, C II, Si IV, C IV, Fe II
and Al II, corresponding to a redshift of z = 2.591 +/- 0.001, consistent
with the redshift reported by D'Avanzo et al. (GCN 7997) and the UVOT
photometric redshift (Ward et al., GCN 7996).


GRB_name: GRB080721A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  7999
SUBJECT: GRB 080721 : Lulin 2nd optical follow-ups
DATE:    08/07/23 03:05:45 GMT
FROM:    Yuji Urata at Saitama U  <urata@asiaa.sinica.edu.tw>

L-C Huang, T-W Chen, Y-T Chen (NCU)
K.Y Huang (ASIAA) and Y. Urata (Saitama U./ASIAA)
on behalf of the EAFON report;

"We made further optical observations for the optical afterglow of GRB
080721 (Marshall et al., GCN 7988; Chen et al., GCN 7990) using the
Lulin 1 m telescope. The single R-band image with 300 sec exposure
shows the afterglow well with R=21.3 (mid term of the exposure is
26.19 hours after the burst). Comparison with our previous report
(Chen et al. GCN 7990), the temporal decay index is ~1.0. This is
consistent with the result reported by Jakobsson et al. (GCN 7998).


GRB_name: GRB080723A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8000
SUBJECT: GRB 080723: Swift detection of a burst
DATE:    08/07/23 04:40:07 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

M. Stamatikos (NASA/ORAU), W. H. Baumgartner (GSFC/UMBC),
A. P. Beardmore (U Leicester), S. T. Holland (CRESST/USRA/GSFC),
S. D. Hunsberger (PSU), H. A. Krimm (CRESST/GSFC/USRA),
C. B. Markwardt (CRESST/GSFC/UMD), F. E. Marshall (NASA/GSFC),
K. L. Page (U Leicester), D. M. Palmer (LANL) and
T. N. Ukwatta (GSFC/GWU) report on behalf of the Swift Team:

At 04:19:24 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 080723 (trigger=317662).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 274.512, -6.923 which is 
   RA(J2000) = 18h 18m 03s
   Dec(J2000) = -06d 55' 20"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  Because the BAT light curve has not been
received, we cannot comment on the burst profile at this time.  However,
there is a strong 8.4 sigma excess detected in the scaled map image, 
which strongly suggests a real gamma-ray burst occurred. 

The XRT began observing the field at 04:20:50.2 UT, 85.8 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source with an enhanced position: RA, Dec 274.48985,
-6.89931 which is equivalent to:
   RA(J2000)  = 18h 17m 57.56s
   Dec(J2000) = -06d 53' 57.5"
with an uncertainty of 2.7 arcseconds (radius, 90% containment). This
location is 116 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 in excess of the Galactic value (3.94e+21
cm^-2, Kalberla et al. 2005), with an excess column of 5.7
(+6.36/-4.59) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 100 seconds with the White (160-650 nm)
filter starting 92 seconds after the BAT trigger. No afterglow candidate has
been found in the initial data products. The 2.7'x2.7' sub-image covers 0% of
the XRT error circle.  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 large Galactic 
expected extinction corresponding to E(B-V) of 1.3 mag. 

Burst Advocate for this burst is M. Stamatikos (michael 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: GRB080723A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8001
SUBJECT: GRB 080723: Enhanced Swift-XRT position
DATE:    08/07/23 10:42:19 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 5309 s of XRT Photon Counting mode data and 9 UVOT
images for GRB 080723, 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 = 274.49035, -6.89952 which is equivalent
to:

RA (J2000): 18h 17m 57.68s
Dec (J2000): -06d 53' 58.3"

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: GRB080723B
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8002
SUBJECT: GRB 080723B : a long GRB detected with INTEGRAL
DATE:    08/07/23 14:28:26 GMT
FROM:    Diego Gotz at CEA  <diego.gotz@cea.fr>

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

A bright GRB lasting about 105 s has been detected by IBAS in IBIS/ 
ISGRI data at 13:22:19 UT on July 23rd 2008. The refined position is

R.A.:  176.8354 deg
Dec.: -60.2452 deg

with an uncertainty of 1.5 arcmin (90% c.l.).

The burst is very bright and has saturated the available telemetry  
share. Hence the following preliminary spectral results are to be  
considered lower limits. The peak flux over 3 s in the 20-200 keV  
energy range is 6 ph/cmsq/s, and the fluence integrated over the  
whole burst duration is 1.3e-5 erg/cmsq.

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: GRB080723B
Detection_method: superAGILE
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8003
SUBJECT: GRB 080723B: Detection and Localization by SuperAGILE
DATE:    08/07/23 14:47:13 GMT
FROM:    Marco Feroci at IASF/INAF  <feroci@iasf-roma.inaf.it>

E. Del Monte, I. Donnarumma, Y. Evangelista, M. Feroci,
E. Costa, 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, P. 
Caraveo (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, B. Preger,
P. Santolamazza, F. Verrecchia (ASDC) and L. Salotti (ASI), 
on behalf of the AGILE Team, report:

"SuperAGILE detected and localized a very bright gamma ray burst
on July 23rd 2008, at 13:22:19 UT. The event was approximately
13 degrees off-axis. The observed duration in the 20-60 keV
energy range is about 110 seconds, with a multi-peaked structure.
The burst position was reconstructed as (RA, Dec) (176.823 deg,
-60.262 deg), which is:

RA(J2000) = 11h 47m 17.42s
Dec(J2000) = -60d 15' 43.7"

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

The same event was also localized and announced by INTEGRAL/ISGRI 
(BACODINE trigger n. 5311, and Gotz et al., GCN 8002). 
The SuperAGILE position lies at 1.1 arcmin from the one 
reported in the INTEGRAL off-line analysis.

A SuperAGILE light curve of the event will shortly be posted on the AGILE 
Science Data Center website: http://agile.asdc.asi.it .

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

This message may be cited.


GRB_name: GRB080723A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8004
SUBJECT: GRB 080723A: Swift-XRT refined analysis
DATE:    08/07/23 15:35:27 GMT
FROM:    Andy Beardmore at U Leicester  <apb@star.le.ac.uk>

A.P. Beardmore (U. Leicester) and M. Stamatikos (NASA/ORAU)
report on behalf of the Swift-XRT team :

We have analysed the first two orbits of Swift-XRT data obtained
from GRB 080723A (trigger 317662;  Stamatikos et al., GCN Circ. 8000).
The data were taken in photon counting mode and have an exposure of
2.83 ks,  spanning 88 s to 7.44 ks after the trigger. The UVOT-enhanced
XRT position was given by Beardmore et al. in GCN Circ. 8001.

The light curve can be modelled by a doubly broken power-law, with
an inital decay of alpha1 = 1.77 +0.34 -0.25 which flattens to a shallow
decay of alpha2 = 0.05 +/- 0.24 at a time tbreak1 = 365 +68 -46 s. This is
followed by a further steepening to  alpha3 = 1.39 +/- 0.75 at a time
tbreak2 = 3.4 +1.2 -1.8 ks.

The spectrum of the photon counting mode data from the first two orbits
can be fit with an absorbed power-law to give a photon index gamma =
2.39 +0.30 -0.28 and NH = (7.7 +2.5 -2.2)e21 cm^-2, in addition to the
Galactic column of 3.9e+21 cm^-2 in the direction of the GRB. The observed
0.3-10 keV flux is  (1.14 +0.10 -0.22)e-11 erg cm^-2 s^-1, which corresponds
to an unabsorbed flux of 3.57e-11 erg cm^-2 s^-1.

If the light curve continues to decay at the same rate we estimate the count
rate will be 3.2e-2 count/s  one day after the trigger, which corresponds to
an observed  flux of 1.9e-13 erg cm^-2 s^-1.

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


GRB_name: GRB080723B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8005
SUBJECT: GRB 080723B : Planned XMM-Newton observation
DATE:    08/07/23 17:30:53 GMT
FROM:    Norbert Schartel at XMM-Newton/ESA  <too@xmm.esac.esa.int>

XMM-Newton will observe GRB 080723B at location
(RA=11h 47m 20s, DEC=-60d 14' 41", J2000),
starting at 18:30:00 UT, on July 23, 2008,
for an exposure of 79800 seconds.

XMM-Newton SOC


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GRB_name: GRB080723B
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8006
SUBJECT: GRB 080723B: AGILE GRID and MCAL results
DATE:    08/07/23 18:38:49 GMT
FROM:    Sandro Mereghetti at IASF/CNR  <sandro@iasf-milano.inaf.it>

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

Analysis of the AGILE Gamma Ray Imager Detector (GRID) data of the 
INTEGRAL GRB 080723B (Gotz et al.  GCN 8002, Del Monte et al. GCN 8003) 
does not reveal significant high-energy emission during the time interval 
of the prompt emission.

A preliminary estimate of the fluence, integrated over 100 s, gives a 99% 
c.l. upper limit of 0.03 photons/cm^2 for energy greater than 50 MeV.

GRB 080723B has also triggered on-board the AGILE Mini-Calorimeter (MCAL) 
at 13:22:33 UT (=T0). Using the preliminary in-flight calibration and 
assuming a Crab-like spectrum we can estimate a fluence of (8 +/- 2)x10^-6 
erg/cm^2 in the 350-700 keV energy range in the time interval between T0 
and T0+48 s.

This message may be cited.


GRB_name: GRB080723A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8007
SUBJECT: GRB 080723, Swift-BAT refined analysis
DATE:    08/07/23 18:48:45 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.a.krimm@nasa.gov>

M. Stamatikos (GSFC/ORAU), S. D. Barthelmy (GSFC), W. Baumgartner 
(GSFC/UMBC),
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 (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 080723 (trigger #317662)
(Stamatikos, et al., GCN Circ. 8000).  The BAT ground-calculated position is
RA, Dec = 274.461, -6.910 deg which is
    RA(J2000)  =  18h 17m 50.6s
    Dec(J2000) = -06d 54' 34.8"
with an uncertainty of 1.6 arcmin, (radius, sys+stat, 90% containment).
The burst was in the fully coded part of the BAT field of view.

The mask-weighted light curve showed a double-peaked structure, with the
first peak extending from T-1 sec to T+4 sec, and the second smaller 
peak from T+6 sec to T+20 sec. T90 (15-350 keV) is 17.3 +- 3.0 sec 
(estimated error including systematics).

The time-averaged spectrum from T-0.2 to T+18.7 sec is best fit by a 
simple power-law model.  The power law index of the time-averaged 
spectrum is 1.77 +- 0.21.  The fluence in the 15-150 keV band is
3.3 +- 0.4 x 10-7 erg/cm2. The 1-sec peak photon flux measured from 
T-0.13 sec in the 15-150 keV band is 0.9 +- 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/317662/BA/


GRB_name: GRB080723B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8008
SUBJECT: GRB 080723B - Swift-XRT position
DATE:    08/07/23 20:58:43 GMT
FROM:    Kim Page at U.of Leicester  <kpa@star.le.ac.uk>

K.L. Page (U. Leicester) reports on behalf of the Swift-XRT team:

Swift started observing the INTEGRAL- and Super-AGILE-detected GRB 080723B
~13.4 ks after the trigger (Gotz et al., GCN Circ. 8002; Del Monte et al., 
GCN Circ. 8003). In ~560 s of data, the XRT clearly detects a source 
within the error circles, at a position of RA, Dec = 176.83393,
-60.2414, which is equivalent to

RA(J2000) =   11 47 20.14
Dec(J2000) = -60 14 29.1

with an uncertainty of 3.9 arcsec (radius, 90% containment).

Currently there are insufficient data to say whether the source is fading. 
An updated circular will be written when further data have been obtained.

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


GRB_name: GRB080723B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8009
SUBJECT: GRB 080723B - Swift-XRT refined analysis 
DATE:    08/07/24 07:01:14 GMT
FROM:    Kim Page at U.of Leicester  <kpa@star.le.ac.uk>

K.L. Page (U. Leicester) reports on behalf of the Swift-XRT team:

The INTEGRAL/Super-AGILE-detected GRB 080723B has now been observed by the 
Swift-XRT for three orbits (a total of ~2.3 ks of Photon Counting mode 
data). The source reported in GCN Circ. 8008 can now be seen to be fading 
(alpha = 1.27 +/- 0.23), so is confirmed as the X-ray afterglow.

A spectrum formed from the combined data (~1.3 - 30 ks after the triggers) 
can be fitted by a power-law of Gamma = 1.87 +/- 0.14, absorbed by the 
Galactic column in this direction, of 7.42x10^21 cm^-2. The average 
observed (unabsorbed) flux over this time is 1.49 (2.57) x 10^-9 erg cm^-2 
s^-1, which provides an observed counts to flux conversion of 5.9x10^-9 
erg cm^-2 count^-1.

If the decay were to continue with alpha ~1.27, the count rate 24 hours 
after the trigger woule be 0.04 count s^-1 (corresponding to an observed 
flux of 2.4x10^-10 erg cm^-2 s^-1).

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


GRB_name: GRB080723B
Detection_method: correction
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8010
SUBJECT: GRB 080723B - correction to flux conversion factor
DATE:    08/07/24 08:15:47 GMT
FROM:    Kim Page at U.of Leicester  <kpa@star.le.ac.uk>

K.L. Page and J.P. Osborne (U. Leicester) report on behalf of the 
Swift-XRT team:

The counts to flux conversion factor in GCN Circ. 8009 was inadvertantly 
mistyped. The actual conversion is 5.9x10^-11 erg cm^-2 count^-1 (a factor 
of 100 lower than that previously given). This implies that the predicted 
flux at 24 hours is 2.4x10^-12 erg cm^-2 s^-1.

We apologise for the mistake and any inconvenience it may have caused.


GRB_name: GRB080721A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8011
SUBJECT: VLA radio upper limit on GRB 080721
DATE:    08/07/24 14:13:47 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
optically bright GRB 080721 (GCN 7988) at a frequency of 8.46 GHz
on 2008 July 24.15 UT. The GRB radio afterglow is undetected and
the peak radio flux at the UVOT afterglow position (GCN 7988) is
93  48 uJy.

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


GRB_name: GRB080723A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8012
SUBJECT: GRB 080723A: Swift/UVOT Upper Limits 
DATE:    08/07/24 14:32:06 GMT
FROM:    Stephen Holland at USRA/NASA/GSFC/SSC  <sholland@milkyway.gsfc.nasa.gov>

S. T. Holland (CRESST/GSFC/USRA) and M. Stamatikos (NASA/ORAU) report
on the behalf of the Swift UVOT team:

         The Swift/UVOT observed the field of GRB 080723A starting 68 s
after the BAT trigger (Stamatikos et al. 2008, GCN Circ. 8000).  We do
not find any source, in any of the UVOT observations, at the
UVOT-enhanced XRT position of the afterglow (Beardmore 2008, GCN
Circ. 8001).  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          194     6260     1040    >20.1
    b          674     7080      451    >20.6
    u          649     6874      471    >20.4
   uvw1        625     6670      469    >20.3
   uvm2        600     6465      467    >20.1
   uvw2        704     7468      430    >20.4
  white         88     7284      628    >21.4
-----------------------------------------------------------------

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} = 1.3 mag.  All photometry is on the UVOT flight
system described in Poole et al. (2008, MNRAS, 383, 627).


GRB_name: GRB080723B
Detection_method: INTEGRAL
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8013
SUBJECT: ATCA radio upper limit on  GRB 080723B
DATE:    08/07/25 02:06:42 GMT
FROM:    Poonam Chandra at U Virginia/NRAO  <pc8s@virginia.edu>

Mark H. Wieringa (CSIRO), Poonam Chandra (NRAO/UVA) and Dale A. Frail
(NRAO) report on behalf of a larger collaboration:

"We observed a region centered on the bright INTEGRAL-  and
Super-AGILE-detected GRB 080723B (GCN 8002 and 8003) using the Australia
Telescope Compact Array starting at July 23.97 UT and ending at
July 24.13 UT. No radio emission was seen at 8 GHz frequency band
within the XRT error circle (GCN 8008). The flux upper limit at XRT
position is 170 uJy (rms 67 uJy).

The Australia Telescope Compact Array is part of the Australia
Telescope which is funded by the Commonwealth of Australia for
operation as a National Facility managed by CSIRO.


GRB_name: GRB080725A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8014
SUBJECT: GRB 080725: Swift detection of a burst
DATE:    08/07/25 10:43:53 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

H. A. Krimm (CRESST/GSFC/USRA), W. H. Baumgartner (GSFC/UMBC),
A. P. Beardmore (U Leicester), P. A. Evans (U Leicester),
S. D. Hunsberger (PSU), S. Immler (CRESST/GSFC/UMD),
J. Mao (INAF-OAB), P. T. O'Brien (U Leicester),
K. L. Page (U Leicester), D. M. Palmer (LANL),
D. Perez (U Leicester), B. Preger (ASDC),
R. L. C. Starling (U Leicester), G. Stratta (ASDC) and
L. Vetere (PSU) report on behalf of the Swift Team:

At 10:26:14 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 080725 (trigger=317888).  The BAT on-board calculated location is 
RA, Dec 121.715, -13.990 which is 
   RA(J2000) = 08h 06m 52s
   Dec(J2000) = -13d 59' 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 60 sec.  The peak count rate
was ~2800 counts/sec (15-350 keV), at ~3 sec after the trigger. 

Due to proximity to the Sun, Swift cannot slew to the BAT position. 
The source will not be observable until September. There will thus 
be no XRT or UVOT data for this trigger. 

Burst Advocate for this burst is H. A. Krimm (krimm 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: GRB080723B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8015
SUBJECT: Konus-Wind observation of GRB 080723B
DATE:    08/07/25 11:33:12 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, P.
Oleynik, M. Ulanov, D. Svinkin, and T. Cline on behalf of the Konus-Wind 
team, report:

The bright GRB 080723B localized by IBIS/ISGRI (Gotz et al., GCN 8002) 
and SuperAGILE (Del Monte et al., GCN 8003) triggered Konus-Wind at 
T0=48143.773 s UT (13:22:23.773).

The burst light curve shows multipeaked structure with a duration of ~100 s.

As observed by Konus-Wind the burst
had a fluence of 8.40(-0.56, +0.47)x10^-5 erg/cm2,
and a 64-ms peak flux measured from T0+54.784 s
of (1.11 +/- 0.15)x10^-5 erg/cm2/s
(both in the 20 keV - 2 MeV energy range).

The time-integrated spectrum of the burst
(from T0 to T0+87.808 s) is well fitted (in the 20 keV - 2 MeV range)
by GRBM (Band) model for which:
the low-energy photon index is alpha = -0.755 (-0.102, +0.103),
the high energy photon index beta = -2.42(-0.40, +0.18),
the peak energy Ep = 225(-21, +27) keV (chi2 = 64.2/58 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/GRB080723_T48143/


GRB_name: GRB080725A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8016
SUBJECT: GRB 080725: REM prompt observations
DATE:    08/07/25 11:40:54 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

P. D'Avanzo, D. Fugazza, L.A. Antonelli, L.  Calzoletti,  S. Campana, 
G.  Chincarini, S. Covino, 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 080725 (Krimm et al. GCN 8014) on 
July 25 starting at 10:34:23 UT (about 8 minutes after the burst, 23 
second after the trigger). Observations were carried out during twilight 
and at high airmass. We do not identify any obvious afterglow candidate 
down to R > 16.1 and H > 14.5 (3sigma c.l.) inside the BAT error box.


GRB_name: GRB080723B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8017
SUBJECT: GRB080723B: Swift/UVOT Upper Limits
DATE:    08/07/25 13:03:18 GMT
FROM:    Peter Brown at PSU  <pbrown@astro.psu.edu>

P. J. Brown (Penn State)  reports on behalf of the Swift UVOT team:

The Swift/UVOT observed the field of GRB 080723B (Gotz et al.,
GCN Circ. 8002) starting at 2008-07-23 17:05:44, 13.4 ks after
the Integral detection.  We do not find any source in the UVOT
observations at the XRT position of the afterglow (Page, GCN Circ. 8008).
The 3-sigma upper limits for detecting a source at this location in the
co-added images are:

Filter   T_start(s)   T_stop(s)  Exp(s)  Mag(3-sigma upper limit)
v        13790        13836      45      >18.1
b        13551        35434      473     >20.3
u        13500        35220      661     >20.1
uvw1     13405        40586      1538    >20.4
uvm2     13841        13966      124     >18.8
uvw2     13603        35801      735     >20.1

The values quoted above are in the UVOT photometric system
(Poole et al. 2008, MNRAS, 383, 627).  They have not been corrected
for the expected high but uncertain Galactic extinction along the
line of sight (Galactic latitude < 5 degrees).


GRB_name: GRB080723A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8018
SUBJECT: GRB 080723A: optical upper limit 
DATE:    08/07/25 14:19:30 GMT
FROM:    Graziella Pizzichini at IASF/CNR,Bologna  <pizzichini@iasfbo.inaf.it>

   F. Munz (INAF/IASF Bologna), F. Terra (Second University of Roma "Tor
  Vergata"),,G. Greco, C. Bartolini, A. Guarnieri, A. Piccioni (Bologna
   University), G. Pizzichini (INAF/IASF Bologna), D. Nanni (INAF/OAR and
   Second University of Rome "Tor Vergata"), S. Galleti, R. Gualandi (Bologna
   Observatory) report:

   We observed the field of GRB 080723A (GCN 8000 Stamatikos et al.)
   with the 152 cm telescope located in Loiano under clear sky conditions
   (seeing~2.5").

   In our 20 min exposure in the Rc filter at mean time 2008 July 23
   20.62 UT we do not detect any afterglow candidate in the enhanced Swift-XRT
   position (GCN 8001, Beardmore et al.).

   Our 3-sigma limiting magnitude is R~20 (based on Nomad1 catalogue).
   In this area there is a strong galactic extinction, A_lambda ~ 4 mag in R
   from the NASA/IPAC extragalactic data base.
   The image has been posted in our public directory
   from where it can be retrieved by sftp using

   hostname: ermione.bo.astro.it
   username: publicGRB
   password: GRB_bo
   directory: GRB080723A


GRB_name: GRB080725A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8019
SUBJECT: GRB 080725, Swift-BAT refined analysis 
DATE:    08/07/25 20:29:06 GMT
FROM:    Hans Krimm at NASA-GSFC  <hans.a.krimm@nasa.gov>

T. Ukwatta (GWU), S. D. Barthelmy (GSFC), W. Baumgartner (GSFC/UMBC),
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 (ISAS), M. Stamatikos (GSFC/ORAU), J. Tueller (GSFC),
(i.e. the Swift-BAT team):

Using the data set from T-240 to T+130 sec from the recent telemetry 
downlink, we report further analysis of BAT GRB 080725 (trigger #317888)
(Krimm, et al., GCN Circ. 8014).  The BAT ground-calculated position is
RA, Dec = 121.699, -13.984 deg which is
   RA(J2000)  =  08h 06m 47.7s
   Dec(J2000) = -13d 59' 03.4"
with an uncertainty of 1.3 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 42%.

The mask-weighted light curve starts with a short, faint precursor from
T-105 to T-100 sec.  The main emission peak begins at T-20 sec and rises 
to a peak at T+2 sec.  There is a second peak at T+13 sec, and the 
emission falls to background levels by T+25 sec. T90 (15-350 keV) is 120 
(+5, -75) sec (estimated error including systematics).  The spacecraft 
slewed away from the burst location starting at T+100 sec, so there is 
no data beyond T+130 sec.

The time-averaged spectrum from T-105.5 to T+51.8 sec is best fit by a 
simple power-law model.  The power law index of the time-averaged 
spectrum is 1.50 +- 0.10.  The fluence in the 15-150 keV band is 3.7 +- 
0.2 x 10-6 erg/cm2. The 1-sec peak photon flux measured from T+3.54 sec 
in the 15-150 keV band is 2.3 +- 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/317888/BA/


GRB_name: GRB080726A
Detection_method: superAGILE
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8020
SUBJECT: GRB 080726: GRB Localization by SuperAGILE
DATE:    08/07/26 08:27:39 GMT
FROM:    Marco Feroci at IASF/INAF  <feroci@iasf-roma.inaf.it>

F. Lazzarotto, E. Del Monte, Y. Evangelista, M. Feroci,
E. Costa, I. Donnarumma, I. Lapshov, L. Pacciani, M. Rapisarda,
P. Soffitta, (INAF/IASF Rome), A. Giuliani, S. Vercellone, A. Chen,
S. Mereghetti, A. Pellizzoni, F. Perotti, F. Fornari, P. 
Caraveo (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, B. Preger,
P. Santolamazza, F. Verrecchia (ASDC) and L. Salotti (ASI), 
on behalf of the AGILE Team, report:

"SuperAGILE detected a relatively weak gamma ray burst
on July 26th 2008, at 01:26:10 UT. The event was approximately
25 degrees off-axis, with a duration of about 12s in the 20-60 keV
energy range, with a single peak structure.
The event was detected during the ground processing, and unambigously 
localized in one of the two instrument coordinates, while in the other 
it showed a significance of about 4-sigma. 
Based on this localization, the burst position was reconstructed 
as (RA, Dec) (20.398 deg, 13.913 deg), which is:

RA(J2000)  = 01h 21m 35.50s
Dec(J2000) = 13d 54' 46.6"

with an uncertainty of 5' 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: GRB080727A
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8021
SUBJECT: GRB 080727: Swift detection of a burst
DATE:    08/07/27 06:16:46 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

S. Immler (CRESST/GSFC/UMD), W. H. Baumgartner (GSFC/UMBC),
N. Gehrels (NASA/GSFC), S. D. Hunsberger (PSU), W.B Landsman (GSFC),
C. B. Markwardt (CRESST/GSFC/UMD), K. L. Page (U Leicester),
D. M. Palmer (LANL), A. M. Parsons (GSFC), D. Perez (U Leicester),
T. Sakamoto (NASA/UMBC) and T. N. Ukwatta (GSFC/GWU) report on behalf
of the Swift Team:

At 05:57:39 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 080727 (trigger=318094).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 208.389, -18.549 which is 
   RA(J2000) = 13h 53m 33s
   Dec(J2000) = -18d 32' 55"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single peak
structure with a duration of about 5 sec.  The peak count rate
was ~700 counts/sec (15-350 keV), at ~2 sec after the trigger. 

The XRT began observing the field at 05:59:28.5 UT, 109.2 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source with an enhanced position: RA, Dec 208.39099,
-18.54505 which is equivalent to:
   RA(J2000)  = 13h 53m 33.84s
   Dec(J2000) = -18d 32' 42.2"
with an uncertainty of 2.7 arcseconds (radius, 90% containment). This
location is 15 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
6.75e+20 cm^-2 (Kalberla et al. 2005). 

UVOT took a finding chart exposure of 100 seconds with the White
(160-650 nm)  filter starting 114 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 and 100% of
the XRT error circle. The typical 3-sigma upper limit has been about 
18.5 mag. 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 0.07. 

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: GRB080727B
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8022
SUBJECT: GRB 080727B: Swift detection of a bright burst
DATE:    08/07/27 08:30:44 GMT
FROM:    David Palmer at LANL  <palmer@lanl.gov>

S. Immler (CRESST/GSFC/UMD), W. H. Baumgartner (GSFC/UMBC),
A. P. Beardmore (U Leicester), P. A. Evans (U Leicester),
C. Guidorzi (INAF-OAB), S. D. Hunsberger (PSU), W.B Landsman (GSFC),
C. B. Markwardt (CRESST/GSFC/UMD), K. L. Page (U Leicester),
D. M. Palmer (LANL), A. M. Parsons (GSFC), D. Perez (U Leicester),
T. Sakamoto (NASA/UMBC) and R. L. C. Starling (U Leicester) report on
behalf of the Swift Team:

At 08:13:24 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 080727B (trigger=318101).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 276.870, +1.172 which is 
   RA(J2000) = 18h 27m 29s
   Dec(J2000) = +01d 10' 20"
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 10 sec.  The peak count rate
was ~18,000 counts/sec (15-350 keV), at 6 sec after the trigger. 

The XRT began observing the field at 08:15:05.9 UT, 101.2 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source with an enhanced position: RA, Dec 276.85898,
1.16304 which is equivalent to:
   RA(J2000)  = 18h 27m 26.16s
   Dec(J2000) = +01d 09' 47.0"
with an uncertainty of 2.8 arcseconds (radius, 90% containment). This
location is 51 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 in excess of the Galactic value (3.64e+21
cm^-2, Kalberla et al. 2005), with an excess column of 4.7
(+4.37/-3.38) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 100 seconds with the White
(160-650 nm)  filter starting 105 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 and 100% of
the XRT error circle. The typical 3-sigma upper limit has been about
18.5 mag. No  correction has been made for the expected extinction
corresponding to E(B-V) of  1.94. 

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: GRB080727B
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8023
SUBJECT: GRB 080727B: REM prompt observations
DATE:    08/07/27 09:11:06 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. 
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 080727B (Immler et al. GCN 8022) on 
July 27 starting at 08:14:25 UT (61 seconds after the burst). 
Observations were carried out at high airmass. In a series of 10s and 
30s exposures we do not see any afterglow candidate inside the XRT error 
box down to R > 16.0 and H > 13.0 (3sigma c.l.).


GRB_name: GRB080727B
Detection_method: KAIT
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8024
SUBJECT: GRB 080727B: KAIT observations
DATE:    08/07/27 10:03:20 GMT
FROM:    Weidong Li at UC Berkeley KAIT/LOSS  <weidong@astron.berkeley.edu>

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

The robotic 0.8-m KAIT located at Lick Observatory responded to
GRB 080727B (Immler et al. GCN 8022) automatically on July 27 
starting at 08:14:12 UT (48 seconds after the burst). A series of 
images were taken in the V, I, and clear filters. We detected a
fading new object at the following location:

RA  (J2000) =  18h27m26.05s   +/- 0.3"
Dec (J2000) = +01d09'47.7"    +/- 0.3" , 

suggesting that this is the optical afterglow of the GRB. 
We report the following preliminary photometry (calibrated
to USNO B1): 

UT start  exptime  filter     mag     err

08:14:12  2 s      clear   18.20    0.16
08:14:17  2 s      clear   18.38    0.16
08:14:20  2 s      clear   18.45    0.23

The power-law decay index between t = 49 s and 72 s after the 
burst is -1.44 +/- 0.59. Further analysis is ongoing. 


GRB_name: GRB080727A
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8025
SUBJECT: GRB 080727A: Enhanced Swift-XRT position
DATE:    08/07/27 10:30:36 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 2786 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 080727A, 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 = 208.39050, -18.54479 which is equivalent
to:

RA (J2000): 13h 53m 33.72s
Dec (J2000): -18d 32' 41.2"

with an uncertainty of 1.9 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, 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: GRB080727B
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8026
SUBJECT: GRB 080727B: Enhanced Swift-XRT position
DATE:    08/07/27 11:40:28 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 2097 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 080727B, 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 = 276.85851, +1.16272 which is equivalent
to:

RA (J2000): 18h 27m 26.04s
Dec (J2000): +01d 09' 45.8"

with an uncertainty of 1.9 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, 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: GRB080727A
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8027
SUBJECT: GRB080727A: Swift/UVOT Upper Limits
DATE:    08/07/27 14:38:23 GMT
FROM:    Wayne Landsman at GSFC/SSAI  <wayne.b.landsman@nasa.gov>

W.B. Landsman (NASA/GSFC/Adnet) and S. Immler (PSU) report on behalf of 
the Swift/UVOT team:

The Swift/UVOT observed the field of GRB080727A starting 113s after the 
BAT trigger (Immler et al., GCN Circ. 8021).   We do not find any 
source, in any of the UVOT observations, at the UVOT-enhanced XRT 
position of the afterglow (Evans et al. GCN Circ. 8025).  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          219     7675     1165    >20.6
    b          700     7083      471    >20.9
    u          675     6878      490    >20.6
   uvw1        650     6673      491    >20.5
   uvm2       1541     6468      236    >20.0
   uvw2        730     7486      471    >20.8
  white        113     7284      623    >21.8
-----------------------------------------------------------------

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} = 0.07 mag.  All photometry is on the UVOT flight 
system described in Poole et al. (2008, MNRAS, 383, 627).


GRB_name: GRB080727A
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8028
SUBJECT: GRB 080727A: Swift-XRT refined analysis
DATE:    08/07/27 15:30:20 GMT
FROM:    Kim Page at U.of Leicester  <kpa@star.le.ac.uk>

K.L. Page, J.P. Osborne (U. Leicester) and S. Immler (CRESST/GSFC/UMD) 
report on behalf of the Swift-XRT team:

We have analysed the first three orbits of data obtained for GRB 080727A 
(Immler et al., GCN Circ. 8021), covering 7 ks of Photon Counting mode 
data. The UVOT-enhanced position has been given by Evans et al. (GCM Circ. 
8025).

During the first orbit (117s - 1.9 ks after the trigger), the light-curve 
shows a number of small flares, superimposed on a power-law decay of 
alpha= 2.01 +0.18/-0.17. The source is no longer detected in the combined 
second and third orbits of data (5.3 ks of exposure time, starting 5 ks 
after the trigger). Although the upper limit is consistent with the 
continued decay of alpha = 2.01, it is not possible to determine whether a 
break has occurred.

The spectrum from the first orbit of data can be fitted with a power-law 
of Gamma = 1.43 +0.20/-0.19, absorbed by the Galactic column in this 
direction (6.75x10^20 cm^-2). The average observed (unabsorbed) flux over 
this time is 5.56 (6.02) x 10^-12 erg cm^-2 s^-1. The counts to observed 
flux conversion is 5.3 x 10^-11 erg cm^-2 count^-1.

With the limited information available from a detection only in the first 
orbit, we are unable confidently to predict the flux at 24 hours.

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


GRB_name: GRB080727A
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8029
SUBJECT: GRB 080727A, Swift-BAT refined analysis
DATE:    08/07/27 16:47:32 GMT
FROM:    Takanori Sakamoto at NASA/GSFC  <takanori.sakamoto-1@nasa.gov>

K. McLean (GSFC/UMD), S. D. Barthelmy (GSFC), W. Baumgartner (GSFC/UMBC),
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 (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 080727A (trigger #318094)
(Immler, et al., GCN Circ. 8021).  The BAT ground-calculated position is
RA, Dec = 208.416, -18.572 deg which is 
   RA(J2000)  =  13h 53m 39.9s 
   Dec(J2000) = -18d 34' 18.6" 
with an uncertainty of 2.4 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 97%.
 
The mask-weighted light curve shows a single weak pulse starting 
at T+~0 and ending a T+~5 sec.  
T90 (15-350 keV) is 4.9 +- 1.0 sec (estimated error including systematics).
 
The time-averaged spectrum from T-0.1 to T+5.1 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.25 +- 0.34.  The fluence in the 15-150 keV band is 1.3 +- 0.3 x 10^-07 erg/cm2.
The 1-sec peak photon flux measured from T+1.20 sec in the 15-150 keV band
is 0.3 +- 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/318094/BA/


GRB_name: GRB080727B
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8030
SUBJECT: GRB 080727B, Swift-BAT refined analysis
DATE:    08/07/27 17:12:48 GMT
FROM:    Takanori Sakamoto at NASA/GSFC  <takanori.sakamoto-1@nasa.gov>

W. Baumgartner (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), T. Sakamoto (GSFC/UMBC), G. Sato (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 the recent telemetry downlink,
we report further analysis of BAT GRB 080727B (trigger #318101)
(Immler, et al., GCN Circ. 8022).  The BAT ground-calculated position is
RA, Dec = 276.871, 1.173 deg which is 
   RA(J2000)  =  18h 27m 29.1s 
   Dec(J2000) = +01d 10' 23.2" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 69%.
 
The mask-weighted light curve shows two big FRED-like pulses from 
T-0.5 to T+3 sec and from T+5.5 to T+9.5 sec.  There are several 
pulses starting at T+2.5, T+7.2, T+7.5, and T+8.8 sec.  
T90 (15-350 keV) is 8.6 +- 0.2 sec (estimated error including systematics).
 
The time-averaged spectrum from T-0.2 to T+9.4 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 0.80 +- 0.17, 
and Epeak of 226.6 +- 120.2 keV (chi squared 43.60 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 3.1 +- 0.1 x 10^-06 erg/cm2
and the 1-sec peak flux measured from T-0.04 sec in the 15-150 keV band is
7.6 +- 0.2 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.12 +- 0.04 (chi squared 54.09 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/318101/BA/


GRB_name: GRB080727B
Detection_method: Swift-XRT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8031
SUBJECT: GRB 080727B: Swift-XRT refined analysis
DATE:    08/07/27 17:16:40 GMT
FROM:    Phil Evans at U of Leicester  <pae9@star.le.ac.uk>

P.A. Evans (U. Leicester) and S. Immler (CRESST/GSFC/UMD) report
on behalf of the Swift-XRT team:

We have analysed 1.6 ks of XRT data for GRB 080727B (Immler et al., GCN
Circ 8022). The data were taken in two snapshots; the first started 105
s after the trigger and contained 51 s of Windowed Timing mode data
followed by 500 s of Photon Counting (PC) mode data. The second snapshot
began at T0+11 ks, and contained 1.2 ks of data, all in PC mode.

The UVOT-enhanced XRT position has been given by Goad et al. (GCN Circ.
8026).

The light curve shows an initial steep decay with a power-law index of
2.47 (+1.38, -0.39), with a break to a shallower decay of 1.05 (+0.20,
-0.13). The break occurred at T0+267 (+89, -100) s.

A spectrum formed from all available PC mode data can be modelled by an
absorbed power law with a photon index on 1.61 (+0.43, -0.38). The best
fitting absorption column is 8.7 (+4.1, -2.9) x 10^21 cm^-2, in excess
of the Galactic value in the direction of the burst (3.6 x 10^21,
Kalberla et al. 2005). The counts to observed 0.3-10 keV flux
conversion factor deduced from this spectrum is 5.0 x 10^-11 erg cm^-2
s^-1 count^-1.

If the light curve continues to decay with a slope of 1.05, the count
rate at 24 hours post-trigger will be 1.8 x 10^-3, corresponding to an
observed (unabsorbed) flux of 9.0 x 10^-14 (4.2 x 10^-13) erg cm^-2
s^-1.

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


GRB_name: GRB080727B
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8033
SUBJECT: GRB 080727B: Swift/UVOT Upper Limits
DATE:    08/07/27 18:25:27 GMT
FROM:    Wayne Landsman at GSFC/SSAI  <wayne.b.landsman@nasa.gov>

W.B. Landsman (NASA/GSFC/Adnet) and S. Immler (PSU) report on behalf of 
the Swift/UVOT team:

The Swift/UVOT observed the field of GRB 080727B starting 105s after the 
BAT trigger (Immler et al., GCN Circ. 8022).   We do not find any 
source, in any of the UVOT observations, at either the UVOT-enhanced XRT 
position of the afterglow (Goad et al. GCN Circ. 8026) or the proposed 
KAIT afterglow position (Li et al., GCN 8024).     The 3-sigma upper 
limits for detecting a source at this location in single exposures are:

Filter       T_start      Exp(s)    Mag (3-sigma upper limit)
----------------------------------------------------------
   v          211        393     >20.6
  uvw1        642         15     >17.9
  uvm2        617         19     >17.6
  white       105         98     >21.0
----------------------------------------------------------


The quoted upper limits have not been corrected for the expected 
Galactic extinction along the line of sight corresponding to a large 
reddening of E_{B-V} = 1.9 mag.  All photometry is on the UVOT flight 
system described in Poole et al. (2008, MNRAS, 383, 627).

Combining the UVOT upper limits with the KAIT detection at R~18.3 (Li et 
al., GCN 8024) suggest that there is either high extinction, very fast 
decline in brightness (the UVOT observations began 57 seconds after the 
KAIT observations ), or high redshift.      The UVOT results are 
obtained at shorter wavelengths, and for example, the UVOT v filter is 
expected to suffer an additional ~1.4 mag of extinction, assuming that  
E(B-V) = 1.9 and that the KAIT clear filter corresponds roughly to the R 
band.    The results may also be consistent with a high redshift burst 
(5.5 < z <6.5) which is only observable at wavelengths longward of ~6000 A.


GRB_name: GRB080727C
Detection_method: Swift Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8035
SUBJECT: GRB 080727C: Swift detection of a burst
DATE:    08/07/27 23:28:30 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

A. M. Parsons (GSFC), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), A. P. Beardmore (U Leicester),
D. N. Burrows (PSU), S. T. Holland (CRESST/USRA/GSFC),
E. A. Hoversten (PSU), S. D. Hunsberger (PSU), J. A. Kennea (PSU),
C. B. Markwardt (CRESST/GSFC/UMD), F. E. Marshall (NASA/GSFC),
K. L. Page (U Leicester), D. M. Palmer (LANL),
D. Perez (U Leicester), 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 23:07:35 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 080727C (trigger=318170).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 32.645, +64.151 which is 
   RA(J2000)  = 02h 10m 35s
   Dec(J2000) = +64d 09' 05"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows multiple peaks
with a duration of about 100 sec.  The peak count rate
was ~3500 counts/sec (15-350 keV), at ~25 sec after the trigger. 

The XRT began observing the field at 23:08:47.9 UT, 72.5 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source with an enhanced position: RA, Dec
32.63384, 64.13771 which is equivalent to:
   RA(J2000)  = 02h 10m 32.12s
   Dec(J2000) = +64d 08' 15.8"
with an uncertainty of 2.8 arcseconds (radius, 90% containment). This
location is 50 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 in excess of the Galactic value (6.78e+21
cm^-2, Kalberla et al. 2005), with an excess column of 7.7
(+7.98/-6.22) x 10^21 cm^-2 (90% confidence). 

The initial flux in the 2.5 s image was 1.30e-09 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 81 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 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
XRT error circle. The list of sources is typically complete to about 18 mag. No
correction has been made for the large, but uncertain extinction expected. 




We note that the Galactic latitude of this source is 2.6 deg,
but we believe this to be a GRB based on the BAT and XRT lightcurves
and the spectral information. 

Burst Advocate for this burst is A. M. Parsons (parsons 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: GRB080727C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8036
SUBJECT: GRB080727C: RTT150 optical observations
DATE:    08/07/28 02:23:06 GMT
FROM:    Irek Khamitov at TUG  <irekk@tug.tug.tubitak.gov.tr>

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

report:

The field  of GRB 080727C (GCN 8035, SWIFT trigger=318170) was observed 
with Russian-Turkish 1.5-m  telescope (RTT150, Bakirlitepe, TUBITAK
National Observatory, Turkey), starting at  28 July, 00:58 UT,
i.e. ~2 hours after the burst, using Andor CCD.

We made 2*900 sec exposures in the R band and 900 sec exposure in the I 
band. We found no new source within XRT error circle. Using USNO-B1 stars 
we estimated frame limits as R~23.0 mag, I~21.5 mag.


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GRB_name: GRB080727B
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8037
SUBJECT: GRB 080727B: REM NIR afterglow prompt detection
DATE:    08/07/28 07:27:46 GMT
FROM:    Paolo D'Avanzo at INAF-OAB  <paolo.davanzo@brera.inaf.it>

P. D'Avanzo, S. Covino, L.A. Antonelli, D. Malesani, 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:

Following the KAIT detection of the optical afterglow of GRB 080727B (Li 
et al. GCN 8024) we performed a detailed off-line analysis of our REM 
images (D'Avanzo et al., GCN 8023). While we confirm the non-detection 
of the optical afterglow in the R-band down to the 16th magnitude (30 s 
of total exposure), we find a barely visible object in our coadded 
H-band frame (50 s of total exposure) with a magnitude of H = 11.8  0.2 
(calibrated against the 2MASS catalogue) at a position consistent with 
the one reported by Li et al.

Unfortunately, just after taking the first R and H-band images, the 
telescope experienced tracking problems, due to the low altitude of the 
object with respect to the horizon, and we do not have more images of 
this GRB. The inferred unabsorbed color (R-H = 3.24 mag)  is consistent 
with the hypothesis of an highly absorbed or high redshift event 
(Landsman et al. GCN 8033).


GRB_name: GRB080727C
Detection_method: Swift-XRT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8038
SUBJECT: GRB 080727C: Enhanced Swift-XRT position
DATE:    08/07/28 07:40:27 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 1905 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 080727C, 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 = 32.63485, +64.13754 which is equivalent
to:

RA (J2000): 02h 10m 32.36s
Dec (J2000): +64d 08' 15.2"

with an uncertainty of 1.5 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, 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: GRB080727A
Detection_method: Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8039
SUBJECT: GRB 080727A: VLT upper limits
DATE:    08/07/28 08:05:37 GMT
FROM:    Daniele Malesani at Dark Cosmology Centre, Niels Bohr Inst  <malesani@astro.ku.dk>

D. Malesani (DARK), P. Jakobsson (Univ. Hertfordshire), A. J. Levan 
(Univ. Warwick), E. Rol (Univ. Leicester), J. P. U. Fynbo (DARK), report 
on behalf of a larger collaboration.

We observed the field of GRB 080727A (Immler et al., GCN 8021) with the 
ESO VLT equipped with FORS1. Observations started on 2008 Jul 27.979 UT, 
17.5 hr after the burst, for a total exposure time of 900 s in the R filter.

Inside the refined XRT error circle (Evans et al., GCN 8025), we detect 
no new source down to a limiting magnitude R~26. Calibration was based 
on tabulated zeropoints and is in rough agreement with USNO-B1 stars.

We acknowledge kind support from the observing staff at Paranal, 
particularly Suzanna Randall, Karla Aubel, and Alain Smette.


GRB_name: GRB080727C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8040
SUBJECT: GRB 080727C: Liverpool Telescope observations
DATE:    08/07/28 10:01:03 GMT
FROM:    Cristiano Guidorzi at INAF-OAB  <cristiano.guidorzi@brera.inaf.it>

C. Guidorzi (INAF-OAB), S. Kobayashi, M.J. Burgdorf (Liverpool JMU)
and N. Tanvir (U. Leicester) report on behalf of a larger collaboration:

On 2008 July 28 (01:35:55 UT) we began observing the field of GRB 080727C
(Parsons et al. GCN Circ. 8035) with the Liverpool Telescope.
Observations consisted of 6x300s exposures acquired using the SDSS-i'
filter.

In our coadded frame we do not detect any source inside the refined XRT
error box (Osborne et al. GCN Circ. 8038) down to the limiting magnitude
reported below.

Telescope   Filter  T_mid[s]   Exposure[s]    M_lim (3-sigma)

-------------------------------------------------------------
Liverpool   SDSS-i'  9830        6x300         22.8
-------------------------------------------------------------

The calibration was performed using the I magnitudes of several USNOB-1
catalogue field objects. The value derived by us is consistent with
that given by Bikmaev et al. (GCN Circ. 8036).


GRB_name: GRB080727C
Detection_method: Swift Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8041
SUBJECT: GRB 080727C: Swift XRT refined analysis
DATE:    08/07/28 11:53:51 GMT
FROM:    Rhaana Starling at U of Leicester  <rlcs1@star.le.ac.uk>

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

We have analysed the first five orbits of Swift XRT data for GRB 080727C 
(trigger=318170, Parsons et al. GCN Circ. 8035) beginning at T0+79 s until 
T0+22.6 ks. The enhanced XRT position is given in Osborne et al. 
(GCN Circ. 8038).

Up to approximately T0+110 s the light curve appears to be flat. 
Thereafter the light curve can be fitted with a broken power law with 
alpha1 = 1.5+/-0.1, breaking at Tbk = 740 +1880/-370 s to a slightly 
shallower decay of alpha2 = 1.2 +0.1/-0.3. 

The Photon Counting mode spectrum consisting of 502 s of data during the 
first orbit is well fitted with an absorbed power law of photon index 
Gamma = 1.4+/-0.3 and intrinsic absorption (assuming z=0) of N_H = (1.2 
+0.5/-0.2) e22 cm-2 in addition to the high Galactic absorption in this 
direction of N_H = 6.8e21 cm-2 (Kalberla et al. 2005). 
We measure an average observed (unabsorbed) 0.3-10 keV flux over this time 
of 1.1e-10 (1.7e-10) erg/cm2/s corresponding to an observed count rate to 
flux conversion of 1 count/s = 9.9e-11 erg/cm2/s.

The predicted count rate at T+24 hr is 0.001 count/s corresponding to an
observed 0.3-10 keV flux of 1.35e-13 erg/cm2/s, assuming the decay 
continues with alpha=1.2.

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


GRB_name: GRB080727B
Detection_method: Konus-Wind Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8042
SUBJECT: Konus-Wind observation of GRB 080727B
DATE:    08/07/28 12:43:57 GMT
FROM:    Valentin Pal'shin at Ioffe Inst  <val@mail.ioffe.ru>

S. Golenetskii, R.Aptekar, E. Mazets, V. Pal'shin, D. Frederiks, P.
Oleynik, M. Ulanov, D. Svinkin, and T. Cline on behalf of the Konus-Wind 
team, report:

The long GRB 080727B (Swift-BAT trigger #318101: Immler et al., GCN
8022, Baumgartner et al., GCN 8030) triggered Konus-Wind at T0=29609.825 
s UT (08:13:29.825).

The burst light curve shows two multipeaked pulses with a total duration 
of ~9 s.

As observed by Konus-Wind the burst
had a fluence of 9.46(-0.84, +0.98)x10^-6 erg/cm2,
and a 64-ms peak flux measured from T0+6.080 s
of 5.14(-0.10, +0.11)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+8.448 s) is well 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(-0.18, +0.16),
and Ep = 282(-37, +52) keV (chi2 = 56.6/60 dof).
Fitting by GRBM (Band) model yields:
the low-energy photon index is alpha = -0.73(-0.24, +0.29),
the high energy photon index beta < -2.08,
the peak energy Ep = 242(-48, +69) keV (chi2 = 54.8/59 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/GRB080727_T29609/


GRB_name: GRB080727C
Detection_method: Swift-UVOT Other
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8043
SUBJECT: GRB 080727C: Swift/UVOT Upper Limits
DATE:    08/07/28 19:41:18 GMT
FROM:    Erik Hoversten at Swift/Penn State  <hoversten@astro.psu.edu>

E. A. Hoversten (PSU) and A. M. Parsons (GSFC) report on behalf of the
Swift/UVOT team:

The Swift/UVOT began observing the field of GRB 080727C starting 82
seconds after the BAT trigger (Parsons, et al. GCN Circ. 8035).  We do
not detect any source in any of the filters at the UVOT-enhanced XRT
position (Osborne, et al., GCN Circ. 8038).  The 3-sigma upper limits
at this position for single exposures are:

Filter  T_start    T_stop   Exp(s)  Mag (3-sigma upper limit)
-----------------------------------------------------
white      82.1     181.0    97.3     > 20.81
white    3987.1    4186.8   196.6     > 21.58
v         187.4     587.2   393.5     > 19.89
v        4397.7    4597.5   196.6     > 19.93
b         668.8     673.4     4.6     > 17.79
u         643.0     662.8    19.5     > 18.32
uvw1      618.4     638.2    19.5     > 18.11
uvm2      593.5     613.3    19.5     > 17.61
uvw2     4192.9    4392.7   196.6     > 20.17


The quoted upper limits have not been corrected for the expected
Galactic extinction along the line of sight corresponding to a large
reddening of E_{B-V} = 1.1 mag.  All photometry is on the UVOT flight
system described in Poole et al. (2008, MNRAS, 383, 627).


GRB_name: GRB080727C
Detection_method: Swift-BAT Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8044
SUBJECT: GRB 080727C, Swift-BAT refined analysis
DATE:    08/07/28 20:46:16 GMT
FROM:    Scott Barthelmy at NASA/GSFC  <scott@lheamail.gsfc.nasa.gov>

E. Fenimore (LANL), S. D. Barthelmy (GSFC), W. Baumgartner (GSFC/UMBC),
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 (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+843 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 080727C (trigger #318170)
(Parsons, et al., GCN Circ. 8035).  The BAT ground-calculated position is
RA, Dec = 32.638, 64.130 deg which is 
   RA(J2000)  =  02h 10m 33.2s 
   Dec(J2000) = +64d 07' 48.6" 
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 77%.
 
The mask-weighted light curve shows several overlapping peaks starting
at ~T-5 sec and ending at ~T+200 sec.  T90 (15-350 keV) is 79.7 +- 8.8 sec
(estimated error including systematics).
 
The time-averaged spectrum from T-3.3 to T+116.3 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 0.87 +- 0.20, 
and Epeak of 143.2 +- 50.0 keV (chi squared 66 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 5.2 +- 0.2 x 10^-6 erg/cm2
and the 1-sec peak flux measured from T+15.23 sec in the 15-150 keV band is
2.3 +- 0.2 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.30 +- 0.05 (chi squared 81 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/318170/BA/


GRB_name: GRB080727B
Detection_method: GROND
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8045
SUBJECT: GRB 080727B: GROND redshift limit
DATE:    08/07/28 21:21:10 GMT
FROM:    Jochen Greiner at MPI  <jcg@mpe.mpg.de>

T. Kruehler, J. Greiner, F. Schrey, C. Clemens, A. Yoldas (all MPE Garching), 
A. Kupcu Yoldas (ESO) and G. Szokoly (Eoetvoes Univ., Budapest) report on 
behalf of the GROND team:

Since telescope pointing constraints did not allow a prompt observation of
GRB 080727B (Swift trigger 318101, Immler et al. 2008, GCN #8022), GROND
(Greiner et al. 2008, PASP 120, 405), mounted at the 2.2m ESO/MPI telescope 
at La Silla Observatory (Chile), started observations in g'r'i'z'JHK only 
on Jul 27, 23:08 UT, nearly 15 hrs after the burst. Under mediocre conditions
a total of 90 min effective exposure in g'r'i'z' and 76 min in JHK was
collected. Correcting for foreground extinction of A_V = 6.15 (Schlegel et al.
1998), we measure the following AB magnitudes/limits:
g'>17.7, r'>19.7, i'>19.9, z'=19.8+-0.1, J=19.45+-0.15, H=19.2+-0.1,
K=19.0+-0.15.

The corresponding SED is well fit by a single power law with slope 0.85, 
with no evidence of additional (intrinsic) extinction, and with the 
i'-limit being consistent with that power law. Our SED power law has an 
extinction-corrected R-H=1.0. The best fit Hyper-z redshift to our data 
gives z=5.5-6.5, with a firm upper limit of 6.7. Given the non-constraining 
upper limits at i' and bluer, no lower limit can be placed. If the color 
R-H = 3.24 mag from the combination of KAIT (Li et al. 2008, GCN #8024) 
and REM data (D'Avanzo et al. 2008, GCN #8037) is correct, then the redshift 
of GRB 080727B would be larger than 5.8. 


GRB_name: GRB080727B
Detection_method: KAIT
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8046
SUBJECT: GRB 080727B: KAIT photometry and an early lightcurve break
DATE:    08/07/28 23:49:10 GMT
FROM:    Weidong Li at UC Berkeley KAIT/LOSS  <weidong@astron.berkeley.edu>

W. Li, R. Chornock, D. A. Perley, J. S. Bloom, and A. V. Filippenko,
University of California at Berkeley, on behalf of the KAIT GRB team;
D. A. Kann, TLS Tautenburg, report:

We have analyzed the KAIT observations of the OA of GRB 080727B
as reported in Li et al. (GCN 8024). The imaging sequence started
with 10 x 2 s unfiltered exposures, with the OA detected on each
frame. A series of 20 s V, I, and unfiltered images were then 
obtained, and the OA was detected in the first couple of I and
unfiltered images. Additional photometry (calibrated to USNO B1):

UT start  exptime  filter     mag     err

08:14:46  2  s      clear   18.98    0.28
08:16:03  20 s      clear   19.64    0.07
08:17:35  20 s      clear   20.68    0.23 

Our GRB pipeline used more than 100 USNO B1 stars in calculating the
photometric zero point. However, we suspect that the USNO B1 calibration
for the GRB field may be significantly off.  Based on our experience in
the limiting magnitude of the KAIT 2 s and 20 s unfiltered images, we
estimate that the above photometry and those reported in GCN 8024 should
be made brighter by 1.0 - 2.0 mag.  The corrected KAIT photometry, together
with the REM NIR detection (D'Avanzo et al. GCN 8037), suggests an
optical - NIR color of R-H (Vega)  = 1.2 to 2.2 mag, which is consistent
with the SED fit from the GROND observations (predicted R-H (AB) = 1.0 mag;
Kruehler et al. GCN 8045).  

The KAIT unfiltered light curve of GRB 080727B can be well fit by
a broken power-law with an index of 1.08 +/- 0.07 between t = 49 s
to 169 s, and 1.88 +/- 0.21 between t= 169 s and 524 s. Such an
early break in the light curve is quite extraordinary. 

We plan to obtain photometric calibrations of the GRB field in the
upcoming photometric nights at Lick Observatory.


GRB_name: GRB080727C
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8047
SUBJECT: GRB 080727C: TAROT Calern observatory optical observations
DATE:    08/07/29 11:55:52 GMT
FROM:    Bruce Gendre at LAM-OAMP  <bruce.gendre@oamp.fr>

Gendre, B. (LAM/CNRS), Klotz, A. (CESR-OMP), Boer M. (OHP), Atteia J.L. 
(LATT-OMP) report:

We imaged the field of GRB 080727 detected by SWIFT
(trigger 318170) with the TAROT robotic telescope (D=25cm)
located at the Calern observatory, France.

The observations started 790.7s after the GRB trigger
(765.8s after the notice). The elevation of the field increased from
from 38 degrees above horizon and weather conditions
were good.

The date of trigger : t0 = 2008-07-27T23:07:35.040

At the enhanced XRT position given by Osborne et al.
(GCN #8038) we do not detect any optical transient.

We co-added a series of exposures:
t0+857.5s to t0+1850.1s : R > 18.5

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

N.B. Galactic coordinates are lon=131.4275 lat= +2.5930
and the galactic extinction in R band is 2.8 magnitudes
estimated from D. Schlegel et al. 1998ApJ...500..525S.

This message may be cited. 


GRB_name: GRB080727A
Detection_method: Optical
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8048
SUBJECT: GRB 080727A: Early IR observations
DATE:    08/07/29 15:12:05 GMT
FROM:    Andrew Levan at U.of Leicester  <anl@star.le.ac.uk>

A.J. Levan (U. Warwick) and K. Wiersema (U. Leicester) report for a 
larger collaboration:

We observed the location of GRB 080727A (Immler et al. GCN 
8021) using UKIRT. A series of K-band exposures were taken beginning at
06:24:51 UT, roughly 30 minutes after the burst, a total of 720s
of observtions were taken (36x20s).  We find no evidence for any
source within the XRT error circle (Evans et al. GCN 8025) for GRB
080727A, down to a limit of K=19.8 mag (3-sigma).

Comparing this limit to the extrapolated X-ray flux 30 minutes
post-burst implies that the observed X-ray to optical/IR spectral
slope was beta_KX < ~0.8, thus the non-detection in the IR is likely
down to the rapid fading of the afterglow, rather than suppression
of the optical/IR flux.

We thank the staff of UKIRT for their rapid response to these alerts.


GRB_name: GRB080727B
Detection_method: KAIT
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8049
SUBJECT: GRB 080727B: IR photometry
DATE:    08/07/29 15:15:00 GMT
FROM:    Andrew Levan at U.of Leicester  <anl@star.le.ac.uk>

A.J. Levan (U. Warwick) and K. Wiersema (U. Leicester) report for
a larger collaboration:

We observed the location of GRB 080727B (Immler et al. GCN 8022)
using UKIRT. The automatic observations begin at 08:27:13 UT, roughly
800 seconds after the burst. An initial set of K-band observations
were acquired, followed by a shallower JHK sequence. At the location
of the X-ray (Goad et al. GCN 8026) and optical/IR afterglows
(D'Avanzo et al. GCN 8023; Li et al. GCN 8024) we clearly identify
the fading afterglow of GRB080727B in all filters. The photometry,
calibrated against several 2MASS stars within the field of view is
shown below:

===========================================
T_s T_s-T_b     Band    Mag     err
===========================================
08:27:13 0.00959        K       13.952 0.03
08:31:38 0.01266        K       14.243 0.03
08:36:03 0.01573        K       14.392 0.03
08:50:08 0.02551        K       14.952 0.05
09:00:10 0.03248        K       15.276 0.05
09:10:09 0.03940        K       15.549 0.05
===========================================
08:47:04 0.023389       H       16.144 0.06
08:58:06 0.031042       H       16.560 0.06
09:07:05 0.037280       H       16.775 0.08
==========================================
08:43:13 0.02071        J       17.855 0.10
08:53:15 0.02767        J       18.300 0.10
09:03:16 0.03463        J       18.626 0.11
===========================================
*Data have not been corrected for the significant foreground
extinciton

The K-band is suggestive of a break occurring at t_b ~ 1600s, with
pre- and post-break slopes of alpha_1 =0.84 and alpha_2 =1.26. The
initial slope is significantly shallower than that suggested by the
KAIT observations (Li et al GCN 8046), and implies either that the
afterglow decay flatenned after those observations, or that the
optical and IR were not tracking eachother in this case.

We thank the staff of UKIRT for their rapid response to these alerts.


GRB_name: GRB080727C
Detection_method: Suzaku WAM Det
Circular_text:
TITLE:   GCN CIRCULAR
NUMBER:  8050
SUBJECT: GRB 080727C: Suzaku WAM observation of the prompt emission
DATE:    08/08/01 11:12:42 GMT
FROM:    Kazutaka Yamaoka at Aoyama Gakuin U  <yamaoka@phys.aoyama.ac.jp>

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

The long 080727C (Swift/BAT trigger #318170; Parsons et al., GCN 8035)
triggered the Suzaku Wide-band All-sky Monitor (WAM) which
covers an energy range of 50 keV - 5 MeV at 23:07:51.558 UT (=T0).
The observed light curve shows two peaks, starting at T0-13s, ending
at T0+70s, with a duration (T90) of about 54 seconds. The fluence in 150 - 1000 keV 
was (6.0 +/- 0.7) x 10^-6 erg/cm^2. The 1-s peak flux measured from T0+9s was 
0.78 +/- 0.12 photons/cm^2/s in the same energy range.

Preliminary result shows that the time-averaged spectrum from T0-7s to T0+47s 
is fitted by a single power-law with a photon index of 1.83 +/- 0.18
in the 150 - 1000 keV range (chi^2/d.o.f = 6.1/11). All the quoted errors are at statistical 
90% confidence level, in which the systematic uncertainties are not included.

The light curves with 1/64 sec time resolution for this burst are now available at:
http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html


