GRB 110801A

M. De Pasquale (UCL-MSSL), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), A. P. Beardmore (U Leicester),
D. N. Burrows (PSU), J. R. Cummings (NASA/UMBC),
P. A. Evans (U Leicester), N. Gehrels (NASA/GSFC),
S. T. Holland (CRESST/USRA/GSFC), E. A. Hoversten (PSU),
J. A. Kennea (PSU), A. Melandri (INAF-OAB),
C. J. Mountford (U Leicester), K. L. Page (U Leicester),
D. M. Palmer (LANL), T. Sakamoto (NASA/UMBC),
B. Sbarufatti (INAF-OAB/IASFPA), M. H. Siegel (PSU),
E. Sonbas (GSFC/USRA/Adiyaman Univ.), C. A. Swenson (PSU),
E. Troja (NASA/GSFC/ORAU) and T. N. Ukwatta (MSU) report on behalf of
the Swift Team:

At 19:49:42 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 110801A (trigger=458521).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 89.285, +80.988 which is 
   RA(J2000)  =  05h 57m 08s
   Dec(J2000) = +80d 59' 18"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a few weak peaks
with a duration of about 70 sec.  The peak count rate
was ~700 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 19:51:21.9 UT, 98.9 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 89.4307, +80.9548 which is equivalent to:
    RA(J2000)  = 05h 57m 43.36s
    Dec(J2000) = +80d 57' 17.2"
with an uncertainty of 4.9 arcseconds (radius, 90% containment). This
location is 146 arcseconds from the BAT onboard position, within the
BAT error circle. No event data are yet available to determine the
column density using X-ray spectroscopy. 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 108 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
  RA(J2000)  =	05:57:44.73 =  89.43637
  DEC(J2000) = +80:57:21.6  =  80.95600
with a 90%-confidence error radius of about 0.62 arc sec. This position is 5.4
arc sec. from the center of the XRT error circle. The estimated magnitude is
18.03 with a 1-sigma error of about  0.14. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.08. 

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 110801A: ROTSE-III Detection of re-brightening from OT

W. Zheng (U Mich), T. Guver (U Arizona), report on behalf of the ROTSE
collaboration: 


ROTSE-IIId, located at the Turkish National Observatory at Bakirlitepe,
Turkey, responded to GRB 110801A (Swift trigger 458521; Pasquale et al.
GCN 12228
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 ). The first image was at 19:52:57.7 UT, 194.7 s after the
burst. The unfiltered images are calibrated relative to USNO A2.0.
We detect the OT at UVOT location (GCN 12228
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 ), the OT appeared
to be re-brightening to ~15.0 mag at ~1400s after the burst.
Continuing observations are in progress.

[GCN OPS NOTE(01aug11): Per author's request (at GCN's request),
the language was changed to remove the implication that the delay
in observing was tied to the Notice arrival time.  The delay was due
to weather and dome operations.  The "(8.7 s after the GCN notice time)"
was removed from the text.]

GRB 110801A: TLS Optical afterglow Confirmation

A. Nicuesa Guelbenzu, X. Luo, S. Klose, U. Laux, B. Stecklum (all
at TLS Tautenburg) report:

We observed the afterglow of GRB 110801A (M. De Pasquale et al., GCN 12228
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 )
with the 2m/1.34m Schmidt telescope of the Thueringer
Landessternwarte Tautenburg starting about 20 min after the GRB trigger.

The afterglow is clearly detected in the R band images at the position
of the UVOT detection.

We confirm the re-brightening of the afterglow as reported by
ROTSE III (Zheng et al. 2011, GCN 12229
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 ).

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

Using 1989 s of XRT Photon Counting mode data and 5 UVOT
images for GRB 110801A, 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 = 89.43603, +80.95615 which is equivalent
to:

RA (J2000): 05h 57m 44.65s
Dec (J2000): +80d 57' 22.2"

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) and Evans
et al. (2009, MNRAS, 397, 1177).

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

D. Kuroda (OAO, NAOJ),  H. Hanayama, T. Miyaji, J. Watanabe (IAO, NAOJ),
K. Yanagisawa (OAO, NAOJ), S.Nagayama (NAOJ), M. Yoshida (Hiroshima),
K. Ohta (Kyoto) and N. Kawai(Tokyo Tech)
report on behalf of the MITSuME collaboration:

We observed the field of GRB 110801A (Pasquale et al., GCNC 12228)
with the optical three color (g', Rc and Ic) CCD camera attached
to the Murikabushi 1m telescope of Ishigakijima Astronomical
Observatory.

The observation started on 2011-08-01 19:53:51 UT (~4 min after the burst).
We detected the previously reported afterglow (Pasquale et al.,
GCNC 12228; Zheng and Guver, GCNC 12229; Guelbenzu et al., GCNC 12230)
in all the three bands.

Photometric results of the OT are listed below. We used GSC2.3 catalog
for flux calibration.

#T0+[day]  MID-UT    T-EXP[sec]   g'  g'_err   Rc  Rc_err   Ic  Ic_err
----------------------------------------------------------------------
0.00323    19:54:21     60.0    16.16  0.07  15.14  0.04  14.44  0.04
0.00404    19:55:31     60.0    15.35  0.06  14.29  0.04  13.57  0.04
0.00485    19:56:41     60.0    15.38  0.06  14.28  0.04  13.56  0.04
0.00731    20:00:14     60.0    15.54  0.06  14.51  0.04  13.79  0.04
0.00976    20:03:45     60.0    15.71  0.07  14.67  0.04  13.98  0.04
0.01222    20:07:18     60.0    15.77  0.07  14.79  0.04  14.12  0.04
0.01466    20:10:48     60.0    15.89  0.07  14.91  0.04  14.24  0.04
----------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]

A. Cabrera Lavers (GTC), A. de Ugarte Postigo (DARK/NBI), A.J.
Castro-Tirado, J. Gorosabel, C.C. Thoene (IAA-CSIC), R. Dom�nguez (GTC)
report on behalf of a larger collaboration:

We have observed the afterglow of GRB 110801A (De Pasquale et al. GCNC
12228) using OSIRIS at the 10.4m GTC telescope (La Palma, Spain).
Observations consisted on 2x900s + 1x600s exposures using the R1000B
grating (resolution ~1000) with coverage between 3600 and 7500 Angstrom.
Observations started at 3:30 UT (7.7h after the burst). In a preliminary
analysis, using archival calibrations, we detect a high signal to noise
ratio continuum with absorption features that include CII, SiIV, SiII,
CIV, FeII, AlII, AlIII, NiII, ZnII, and MnII, as well as fine structure
FeII* and NiII* at a common redshift of z=1.858, which we identify as the
redshift of the afterglow. We also identify two intervening systems at
z=1.246 and z=0.745 through the presence of the MgII doublet.

A.P. Beardmore (U. Leicester) and M. De Pasquale (UCL-MSSL) report on
behalf of the Swift-XRT team:

We have analysed 9.9 ks of XRT data for GRB 110801A (De Pasquale  et
al. GCN Circ. 12228
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 ), from 89 s to 24.0 ks after the  BAT trigger. The
data comprise 566 s in Windowed Timing (WT) mode (the first 7 s were
taken while Swift was slewing) with the remainder in Photon Counting
(PC) mode. The enhanced XRT position for this burst was given by Evans
et al. (GCN. Circ 12232).

The light curve initially shows a number of flares, the largest peaking
at 500-600 count/s  between T+355 s and T+390 s after the trigger. Once
this flare has decayed, the light curve after T+800 s can be modelled
by a power-law with a slope of 1.12 +/- 0.06.

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index	of 1.754 (+0.025, -0.026). The
best-fitting absorption column is  6.4 (+/-0.6) x 10^21 cm^-2, at a
redshift of 1.858, in addition to the Galactic value of 6.2 x 10^20
cm^-2 (Kalberla et al. 2005). We note this spectrum includes strong
spectral evolution through the flare. The PC mode spectrum has a photon
index of 2.04 (+/-0.09) and a best-fitting absorption column of 1.6
(+1.6, -1.4) x 10^21 cm^-2. The counts to observed (unabsorbed) 0.3-10
keV flux conversion factor deduced from this spectrum  is 3.6 x 10^-11
(4.5 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Galactic foreground: 6.2 x 10^20 cm^-2
Intrinsic column:    1.6 (+1.6, -1.4) x 10^21 cm^-2 at z=1.858
Photon index:	     2.04 (+/-0.09)

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00458521.

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

M. De Pasquale (MSSL-UCL) reports on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 110801A
109 s after the BAT trigger (De Pasquale et al., GCN Circ. 12228
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 ).
A source consistent with the XRT position (Evans et al., GCN Circ. 12232
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 )
is detected in the initial and summed UVOT exposures, except in um2 
filter and a detection in uw2, at 2 sigma confidence level. Since
the redshift of this event is 1.86 (Cabrera Lavers, GCN Circ. 12234
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 ),
we think the weak detection in uw2 is due to flux in the reddest part
of this filter.

The refined UVOT position is:
     RA  (J2000) =  05:57:44.87 =  89.43695 (deg.)
     Dec (J2000) = +80:57:21.1  =  80.95592 (deg.)
with an estimated uncertainty of 0.51 arc sec. (radius, 90% confidence).

The afterglow shows a quick rise from the first exposure up to ~300s.

Preliminary detections and 3-sigma upper limits using the UVOT photometric 
system (Poole et al. 2008, MNRAS, 383, 627) for the early exposures are:

Filter         T_start(s)   T_stop(s)      Exp(s)           Mag

white (fc)         109        259          147         18.06 � 0.07
white              109       6337          727         17.23 � 0.05
v                  598       6747          451         17.07 � 0.06
b                  523       6132          432         17.47 � 0.05
u (fc)             267        517          246         15.89 � 0.05
u                  267       5927          488         15.68 � 0.04
w1                 647       5722          255         17.92 � 0.11
m2                 622       6904          404         >20.2
w2                 573       6543          452         20.48 � 0.41

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.08 in the direction of the burst
(Schlegel et al. 1998).

S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
M. De Pasquale (UCL-MSSL), E. E. Fenimore (LANL), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
T. Sakamoto (GSFC/UMBC), G. Sato (ISAS), M. Stamatikos (OSU),
J. Tueller (GSFC), T. N. Ukwatta (MSU)
(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 110801A (trigger #458521)
(De Pasquale, et al., GCN Circ. 12228
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 ).  The BAT ground-calculated position is
RA, Dec = 89.415, 80.958 deg, which is 
   RA(J2000)  =  05h 57m 39.6s 
   Dec(J2000) = +80d 57' 28.5" 
with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 78%.
 
The mask-weighted light curve shows two main clusters of peaks.  The first
starts at ~T-30 sec, with a maximum at ~T+2 sec, and a long exponental decay
almost down to background before the second cluster.  The second cluster
starts ~T+310 sec, peaks at ~T+340 sec, and ending at ~T+550 sec.
T90 (15-350 keV) is 385 +- 10 sec (estimated error including systematics).
 
The time-averaged spectrum from T-24.2 to T+385.0 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.84 +- 0.10.  The fluence in the 15-150 keV band is 4.7 +- 0.3 x 10^-6 erg/cm2.
The 1-sec peak photon flux measured from T+341.78 sec in the 15-150 keV band
is 1.1 +- 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/458521/BA/

A.V. Parhomenko, A. Tlatov, D. Dormidontov
  Kislovodsk Solar Station of the Pulkovo Observatory


  K.Ivanov, V.A.Poleshchuk, S.Yazev, N.M.Budnev, O.Gres, 
O.Chuvalaev,E.Konstantinov,
  Irkutsk State University

  E. Gorbovskoy, V. Lipunov, V.Kornilov, D.Kuvshinov, A.Belinski, N.Tyurina, 
N.Shatskiy, P.Balanutsa, V.V.Chazov, P.V.Kortunov, A.Kuznetsov, D.Zimnukhov, M. 
Kornilov,A.Sankovich
  Sternberg Astronomical Institute, Moscow State University


  V.Krushinski, I.Zalozhnich, T.Kopytova, A. Popov
  Ural State University, Kourovka

  V.Yurkov, Yu.Sergienko, D.Varda, I.Kudelina
  Blagoveschensk Educational State University, Blagoveschensk


MASTER II robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Tunka(Siberia) was pointed to the GRB110801A 101 sec after GRB 
time at  2011-08-01 19:51:23 UT. Unfortunatelly the objects was not in 
focus  because recently photometer modification.  On our first (20s
exposure) set we haven`t found optical transient within SWIFT error-box
(De Pasquale et al., GCN 12228
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 ).
The 3-sigma upper limit has been about 14.0 mag (white+polarizator).


MASTER II robotic telescope (MASTER-Net: http://observ.pereplet.ru) located 
near Kislovodsk (Caucasus Mountains)  closed roof 20 min before 
trigger due to cloudy condidtions. The telescope was repointed to the
GRB110901A  only 47 min 40 sec after trigger time at 2011-08-01 20:37:22 UT.
We found OT at UVOT postion (De Pasquale et al., GCN 12228
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 ).
The results of our photometry are:

Time_Start    T_mean-T_trig  exp time       m        error      Band 
UT                  s          s 
20:37:22          2950        180         16.13       0.06        R
20:44:29          3377        180         16.12       0.06        R 
20:48:01          3589        180         16.29       0.08        R
20:48:01          3589        180         16.03       0.06     White 
20:51:24          3792        180         16.43       0.06        R
20:51:24          3792        180         16.19       0.06     White
23:20:14         12722        180         17.75       0.10        R

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.08 in the direction of the burst
(Schlegel et al. 1998).

The power low index (F~t^-aplha) apha ~1.0+-0.1     during this 
observations in R-band.

The message may be cited.

A. Nicuesa Guelbenzu, S. Klose, S. Schmidl, A. Rossi, U. Laux, B. Stecklum
(all at TLS Tautenburg) report:

We re-observed the afterglow of GRB 110801A (M. De Pasquale et al., GCN
12228
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 )
with the 2m/1.34m Schmidt telescope of the Thueringer Landessternwarte
Tautenburg starting about 24 hours after the GRB trigger.

A stacking of the first 15 minutes of the second epoch data does not show
the afterglow in the R band down to 21 mag (Vega system). We conclude that
a jet break has occurred within the last 24 hours.

D. Kuroda (OAO, NAOJ),  H. Hanayama, T. Miyaji, J. Watanabe (IAO, NAOJ),
K. Yanagisawa (OAO, NAOJ), S.Nagayama (NAOJ), M. Yoshida (Hiroshima),
K. Ohta (Kyoto) and N. Kawai(Tokyo Tech)
report on behalf of the MITSuME collaboration:

We observed the field of GRB 110801A (De Pasquale et al., GCNC 12228)
with the optical three color (g', Rc and Ic) CCD camera attached
to the Murikabushi 1m telescope of Ishigakijima Astronomical
Observatory.

The observation started on 2011-08-02 17:38:02 UT (~21.8 h after the burst).
We detected the previously reported afterglow (Pasquale et al.,
GCNC 12228; Zheng and Guver, GCNC 12229; Guelbenzu et al., GCNC 12230;
Kuroda et al., GCNC 12233) in all the three bands.

Photometric results of the OT are listed below. We used GSC2.3 catalog
for flux calibration.

#T0+[day]  MID-UT    T-EXP[sec]   g'  g'_err   Rc  Rc_err   Ic  Ic_err
----------------------------------------------------------------------
0.95038    18:38:15   5760.0     21.5  0.3    20.3  0.2   19.1   0.2
----------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]

V. V. Sokolov, A. S. Moskvitin, T. A. Fatkhullun, (SAO RAS) report on
behalf of a larger collaboration:

We observed the field of GRB 110801A (De Pasquale et al., GCN 12228
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 )
with the 6-m BTA of SAO RAS (Russia) equipped with the Scorpio.
The observations were carried out in the B and Rc bands
at 00:07:36 -- 00:13:36 UT, August, 02 (since 4.35 hours after the trigger).
The weather conditions were tolerable, seeing around 2".5.

Magnitudes of optical transient are as follows:
B = 19.02 +/- 0.02
R = 18.10 +/- 0.01
Calibration were done against the magnitudes B2 = 16.74 and R2 = 15.73
of the USNO-B.1 star 1709-0023450 (R.A. = 05:57:24.91 Dec.= +80:57:39.8,
Epoch = 2000). The magnitudes of OT were not corrected for the Galactic
extinction E(B-V) = 0.08 in the direction of the burst (Schlegel et al.
1998).

Also we obtained 2 x 600 sec. spectrum (range = 4000 -- 8400A, resolution
FWHM = 10A) at 00:19:54 -- 00:41:24 UT. At the noisy relatively blue
continuum we marginally detected only the C IV absorption line
corresponding to the red shift reported by Cabrera Lavers et al.
(GCN 12234
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 ).

The message may be cited.

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

We observed the field of GRB 110801A (Pasquale  et al. GCN 12228
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 ) with Shajn 
telescope of CrAO  observatory  on  between Aug. 2 (UT) 22:03 and Aug. 3 
(UT) 00:27 under variable weather conditions and a mean  seeing of  2.1 
arsces. We took several frames with exposure of 60 s in R-band. On a stacked 
image we detected the optical counterpart (Pasquale  et al. GCN 12228
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 , Zheng 
et al. GCN 12229
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 ). A  photometry is based on the USNO B1.0 star 1709-0023450 
(05 57 24.91 +80 57 39.8) assuming R=15.73.

T0+         Filter,   Exposure, mag.                  uplim (3 sigma)
(mid, d)               (s)

1.1428    R         74x60       21.60 +/- 0.09   23.2

M. Andreev, N. Parakhin, A. Sergeev (Terskol Branch of Institute of
Astronomy), A. Pozanenko (IKI) on behalf of larger GRB follow up
collaboration report:

We observed field of the Swift  GRB 110801A (Pasquale  et al. GCN 12228
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 )
with Zeiss-600 telescope of Mt.Terskol observatory in R filter starting on
Aug. 02 (UT) 00:25.  In a stacked image we clearly detect optical afterglow
(Pasquale  et al. GCN 12228
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 , Zheng et al. GCN 12229
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 ). A  photometry is based
on the USNO B1.0 star 1709-0023450 (05 57 24.91 +80 57 39.8) assuming
R=15.73.

T0+         Filter,   Exposure, mag.
(mid, d)               (s)

0.1951   R         4x180       18.35 +/- 0.10

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), D. Palmer (LANL), 
M. Stamatikos (OSU), J. Tueller (GSFC), and T. Ukwatta (MSU)

V. Pal'shin, S. Golenetskii, R.Aptekar, E. Mazets, D. Frederiks, and
T. Cline on behalf of the Konus-Wind team,

We performed the Konus-Wind and the Swift/BAT joint spectral analysis 
of GRB 110801A (Swift/BAT trigger #458521: De Pasquale et al., GCN Circ. 12228
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 , 
Barthelmy et al. GCN Circ. 12237
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 ).  Since the Konus-Wind observed this GRB 
in the waiting mode, we only have 3 channel spectral data for the Konus-Wind 
which cover the energy range from 20 keV to 1.2 MeV.  The joint spectral 
analysis of the Konus-Wind and the Swift/BAT data allows us to derive 
the broad-band spectral parameters of this burst. 

The time interval of the spectral data is chosen from T0(BAT)-26.43 to 
T0(BAT)+64.83 sec and from T0(BAT)+332.74 to T0(BAT)+388.67 sec where T0(BAT) 
is the trigger time of BAT at 19:49.43 UTC to include two time-separated episodes.  
The energy ranges which we used in the joint spectral analysis are 20-1200 keV 
and 14-150 keV for the Konus-Wind and the Swift/BAT respectively.  The spectral 
data of two instruments are fitted with the spectral model multiplied by the 
constant factor to take into account the systematic effective area uncertainties 
in the response matrices of each instrument. 

The spectrum is well fitted with a power-law with exponential cutoff model: 
dN/dE ~ E^{alpha}*exp(-(2+alpha)*E/Epeak).  The constant factors of each 
instrument agree within 10%. No systematic residual from the best fit model is 
seen in the spectral data of each instrument (see Sakamoto et al. 2011, PASJ, 63, 
215 for the spectral cross-calibration).  The best fit spectral parameters are: 
alpha = -1.70 (-0.15/+0.12) and Epeak = 140 (-60/+900) keV (chi2/dof = 74/58).  
The best fit spectral parameters for the GRB (Band) model fixing beta = -2.5 are: 
alpha = -1.70 (-0.15/+0.22), and Epeak = 140 (-50/+1270) keV (chi2/dof = 74/58). 
The energy fluence in the 15-1200 keV band calculated by a power-law with 
exponential cutoff model for this 147.2 sec interval is 7.3 (-0.9/+ 1.7)x10^-6 erg/cm2.  

Assuming z=1.858 (Cabrera Lavers et al. GCN Circ. 12234
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 ) and a standard cosmology 
model with H_0 = 71 km/s/Mpc, Omega_M = 0.27, Omega_Lambda = 0.73, the isotropic 
energy release is E_iso = 1.0 (-0.2/+0.3) x10^53 erg in 1 keV to 10 MeV at the 
GRB rest frame extrapolating the best Band function fit fixing beta = -2.5. 

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

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB110801A/