GRB 140709B

C. A. Swenson (PSU), W. H. Baumgartner (GSFC/UMBC),
D. N. Burrows (PSU), S. B. Cenko (GSFC), M. M. Chester (PSU),
J. R. Cummings (NASA/UMBC), P. A. Evans (U Leicester),
N. Gehrels (NASA/GSFC), J. A. Kennea (PSU),
H. A. Krimm (CRESST/GSFC/USRA), V. Mangano (PSU),
F. E. Marshall (NASA/GSFC), K. L. Page (U Leicester),
D. M. Palmer (LANL) and M. H. Siegel (PSU) report on behalf of the
Swift Team:

At 15:15:45 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140709B (trigger=603866).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 146.071, +63.505 which is 
   RA(J2000) = 09h 44m 17s
   Dec(J2000) = +63d 30' 20"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a multi-peaked
structure with a duration of about 150 sec.  The peak count rate
was ~1500 counts/sec (15-350 keV), at ~20 sec after the trigger. 

The XRT began observing the field at 15:17:15.9 UT, 91.0 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source located at RA, Dec 146.05394, 63.53040 which
is equivalent to:
   RA(J2000)  = 09h 44m 12.95s
   Dec(J2000) = +63d 31' 49.4"
with an uncertainty of 3.9 arcseconds (radius, 90% containment). This
location is 95 arcseconds from the BAT onboard position, within the BAT
error circle. This position may be improved as more data are received;
the latest position is available at http://www.swift.ac.uk/sper. No
spectrum from the promptly downlinked event data is yet available to
determine the column density. 

The initial flux in the 2.5 s image was 3.60e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 250 seconds with the U filter starting 96
seconds after the BAT trigger. No credible 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 19.2 mag. The
8'x8' region for the list of sources generated on-board covers 100% of the XRT
error circle. The list of sources is typically complete to about 18.0 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. A. Swenson (cswenson AT astro.psu.edu). 
Please contact the BA by email if you require additional information
regarding Swift followup of this burst. In extremely urgent cases, after
trying the Burst Advocate, you can contact the Swift PI by phone (see
Swift TOO web site for information: http://www.swift.psu.edu/too.html.)

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

E. Gorbovskoy, V. Lipunov, M.Pruzhinskaya, V.Kornilov, D.Kuvshinov,
  N.Tyurina,  P.Balanutsa, A.Kuznetsov, V.V.Chazov, D.Denisenko, 
Lomonosov Moscow State University,
Sternberg Astronomical Institute

V.Yurkov, Yu.Sergienko, D.Varda, E.Sinyakov, A.Gabovich
Blagoveschensk Educational State University, Blagoveschensk

V.Krushinski, I.Zalozhnih,  A. Popov
Ural Federal University, Kourovka

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

Hugo Levato and Carlos Saffe
Instituto de Ciencias Astronomicas, de la Tierra y del Espacio (ICATE)

Claudio Mallamaci, Carlos Lopez and Federico Podest
Observatorio Astronomico Felix Aguilar (OAFA)

MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Tunka was pointed to the  GRB140709B  40 sec after Notice 
time and 94 sec after trigger 
time at 2014-07-09 15:17:19 UT (Swenson et al., GCN 16551
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 ). On our first 
(20s exposure)  set we  haven`t found optical transient  within SWIFT 
BAT error-box.
The 5-sigma upper limit has been about 17.1mag
We have number images with out OT brighter 18.2  at
  94s < T - T_trigger < 289s.

The message may be cited.

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

Using 787 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 140709B, 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 = 146.05423, +63.52934 which is equivalent
to:

RA (J2000): 09h 44m 13.02s
Dec (J2000): +63d 31' 45.6"

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

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

A. Sota (IAA-CSIC), J. Gorosabel (IAA-CSIC, UPV-EHU) and A. J.
Castro-Tirado (IAA-CSIC, ISA-UMA), on behalf of a larger collaboration,
report:

Following the detection of GRB 140709B by Swift (Swenson et al. GCNC
16551), we have taken I-band frames with the 1.5m OSN telescope at
Observatorio de Sierra Nevada (Granada, Spain) starting at 20:45 UT (5.5 h
post burst) at high airmass. Within the enhanced XRT position (Goad et al.
GCNC 16556) we find no credible counterpart down to the DSS-2 limiting
magnitude when all the images are co-added (10 x 150s). Near-infrared
imaging is encouraged.

A. Volnova (IKI), S. Schmalz (AIP), N. Tungalag (Research Centre of 
Astronomy and  Geophysics MAS),  I.Molotov (KIAM),  A. Pozanenko (IKI) 
report on behalf of larger GRB follow-up collaboration:

We observed the field of GRB 140709B (Swenson et al., GCN 16551
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 ) with ORI-40 
telescope of Khureltogot observatory starting on
Jul., 09 (UT) 15:31:51. In the first unfiltered images of 60 s exposure we 
do not detect any object in the enhanced XRT error circle  (Goad et al., GCN 
16556
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 ) down to 17.7m in each separate image. The photometry is based on 
nearby USNO-B1.0 stars.

D. M. Palmer (LANL), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
A. Y. Lien (NASA/UMBC), C. B. Markwardt (GSFC), T. Sakamoto (AGU),
M. Stamatikos (OSU), C. A. Swenson (PSU), 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 the recent telemetry downlink,
we report further analysis of BAT GRB 140709B (trigger #603866)
(Swenson, et al., GCN Circ. 16551
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 ).  The BAT ground-calculated position is
RA, Dec = 146.040, 63.536 deg which is
    RA(J2000)  =  09h 44m 09.5s
    Dec(J2000) = +63d 32' 10.0"
with an uncertainty of 1.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 99%.

The mask-weighted light curve shows a complex structure.  The first peak has a
broad, symmetrical shape, starting at T-20 sec, peaking at T+25 sec and ending
at T+60 sec.  Then the second episode begins at T+80 sec, with multiple short
(~1-2 second) peaks extending to T+140 sec, before cutting off.  The highest of
these short peaks is at T+125 sec. T90 (15-350 keV) is 155.0 +- 22.3 sec
(estimated error including systematics).

The time-averaged spectrum from T-13.94 to T+197.51 sec is best fit by a power 
law with an exponential cutoff.  This fit gives a photon index 0.79 +- 0.30,
and Epeak of 152.6 +- 111.0 keV (chi squared 48.15 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 4.2 +- 0.2 x 10^-06 erg/cm2
and the 1-sec peak flux measured from T+123.63 sec in the 15-150 keV band is
0.9 +- 0.1 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.22 +- 0.07 (chi squared 54.91 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/603866/BA/

Bin-Bin Zhang (UAH) reports on behalf of the Fermi GBM Team:

"At 15:17:52.85 UT on 09 July 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140709B (trigger 426611875 / 140709637)
which was also detected by Swift (Swenson et al. 2014, GCN 16551
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 ).
The GBM on-ground location, using the Fermi GBM trigger data,
is consistent with the Swift/BAT location.

The angle from the Fermi LAT boresight is 60 degrees.

The GBM light curve consists of two main peaks with a total duration
of about 150 s (50-300keV). The time-averaged spectrum from T0-132 s��
to T0+15 s is well fit by a power law function with an exponential��
high-energy cutoff. The power law index is -1.32 +/- 0.07 and the��
cutoff energy, parameterized as Epeak, is 530 +/- 232 keV.


The event fluence (10-1000 keV) in this time interval is
(1.6 +/- 0.1)E-05 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0-1.28 s in the 10-1000 keV band is 1.9 +/- 0.2 ph/s/cm^2.

The spectral analysis results presented above are preliminary;
final results will be published in the GBM GRB Catalog."

M. de Pasquale (INAF-IASFPA), M.C. Stroh (PSU), D.N. Burrows (PSU),
J.A. Kennea (PSU), B.P. Gompertz (U. Leicester), J.P. Osborne (U.
Leicester), K.L. Page (U. Leicester), A. Maselli  (INAF-IASFPA), A.
Melandri (INAF-OAB) and C.A. Swenson report on behalf of the Swift-XRT
team:

We have analysed 10.0 ks of XRT data for GRB 140709B (Swenson  et al.
GCN Circ. 16551
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 ),  from 85 s to 28.9 ks after the  BAT trigger. The
data comprise 207 s in Windowed Timing (WT) mode (the first 4 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 Goad
et al. (GCN Circ. 16556
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 ).

The late-time light curve (from T0+4.8 ks) can be modelled with  a
power-law decay with a decay index of alpha=0.99 (+0.13, -0.12).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index	of 1.14 (+/-0.07). The
best-fitting absorption column is  2.2 (+0.5, -0.4) x 10^21 cm^-2, in
excess of the Galactic value of 4.3 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 2.05 (+0.14, -0.13)
and a best-fitting absorption column of 1.9 (+/-0.4) x 10^21 cm^-2. The
counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.4 x 10^-11 (4.7 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:	     1.9 (+/-0.4) x 10^21 cm^-2
Galactic foreground: 4.3 x 10^20 cm^-2
Excess significance: 5.7 sigma
Photon index:	     2.05 (+0.14, -0.13)

If the light curve continues to decay with a power-law decay index of
0.99, the count rate at T+24 hours will be 0.010 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.5 x
10^-13 (4.9 x 10^-13) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00603866.

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

A. Volnova (IKI), S. Schmalz (AIP), N. Tungalag (Research Center of 
Astronomy and  Geophysics MAS),  I.Molotov (KIAM),  A. Pozanenko (IKI) 
report on behalf of larger GRB follow-up collaboration:

After receiving a full data set we report details of the  observation of 
the   field of GRB 140709B (Swenson et al., GCN 16551
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 ) with ORI-40 
telescope of Khureltogot observatory.  We started observation on July 09 
(UT) 15:31:51 and obtained 60 unfiltered images of 60 s exposure. 
Within enhanced XRT error circle  (Goad et al., GCN 16556
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 ) we do not 
detect any new object neither in separate, nor in stacked images. 
Details of a photometry is following

UT start   t-T0,d   Exp,s  Filter Up_lim (3 sigma)

15:31:51  0.01334   5*60   None   18.9
15:31:51  0.01940  20*60   None   19.5

The photometry is based on SDSS star J094401.61+633253.8 assuming 
R=16.010+/-0.013 (using gri -> R Lupton transformations).

C. A. Swenson (PSU) reports on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140709B
97 s after the BAT trigger (Swenson et al., GCN Circ. 16551
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 ).
No optical afterglow consistent with the XRT position
(Goad et al. GCN Circ. 16556
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 )
is detected in the initial UVOT exposures.
Preliminary 3-sigma upper limits using the UVOT photometric system
(Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for the first
finding chart (FC) exposure and subsequent exposures are:

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

white_FC          4835         4985          147         >20.8
u_FC                97          346          246         >20.6
white             4835         6626          541         >21.7
v                  633         7037          491         >20.5
b                  352         6422          534         >20.9
u                   97         6216          668         >21.2
w1                 683        11259          922         >20.8
m2                1087         7230          440         >21.2
w2                 758         6832          471         >20.6

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.04 in the direction of the burst
(Schlegel et al. 1998).

A. Volnova (IKI), W. Mundrzyjewski (Fesenkov Astrophysical Institute), 
A. Kusakin (Fesenkov Astrophysical Institute), A. Pozanenko (IKI) report 
on behalf of larger GRB follow-up collaboration:

We observed the field of the Swift GRB 140709B  (Swenson et al., GCN 
16551
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 ) with Zeiss-1000 (West) telescope of Tien Shan Astronomical 
Observatory starting on July 9, (UT) 15:50:27, i.e. 35 minutes after GRB 
trigger. We took several images in R-filter.  Within enhanced XRT error 
circle  (Goad et al., GCN 16556
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 ) we do not detect any new object in 
stacked images.

Details of a photometry of stacked images are following

Date       UT start  t-T0,d  Exp,s   Filter Up_Lim (3 sigma)

2014-07-09 15:50:27  0.09193 13*600  R      20.5
2014-07-10 15:36:01  1.06090 13*600  R      19.8

The photometry is based on SDSS star J094401.61+633253.8 assuming
R=16.010+/-0.013 (using gri -> R Lupton transformations).