GRB 140713A

Poonam Chandra (NCRA-TIFR) and A. J. Nayana (NCRA-TIFR)  report on behalf
of a larger collaboration:

We carried out the Giant Metrewave Radio Telescope (GMRT) observations of
GRB 140713A  (GCN Circ. 16581
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 ) in the 1390 MHz band on 2014 July 24.86 UT.
We do not detect the radio afterglow of the GRB. The 3-sigma upper limit
at the GRB position (GCN Circ. 16585
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 ) is 114 uJy and the map resolution is
"3.53 x 1.96".

We thank GMRT staff for making these observations possible.

-- 

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Poonam Chandra                          +91 20 2571 9290 (Off)
National Centre for Radio Astrophysics  +91 20 2569 7257 (Fax)
Tata Institute of Fundamental Research  poonam@ncra.tifr.res.in
Post Bag 3, Pune University campus    www.ncra.tifr.res.in:8081/~poonam/
Ganeshkhind, Pune 411 007, INDIA

G. E. Anderson, R. P. Fender, T. D. Staley (University of Oxford),
A. J. van der Horst (University of Amsterdam), A. Rowlinson (CASS)

We observed the position of GRB 140713A (GCN 16581
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 ) at 15 GHz with
the Arcminute Microkelvin Imager (AMI-LA) starting on 2014 July 16.88
to 17.05 UT, corresponding to 3.1 days post-burst. We have detected the
radio counterpart (GCN 16593
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 ) with a preliminary flux of 0.66 +/- 0.07 mJy.


Earlier observations were conducted on 2014 July 13.78 to 13.87 UT and
July 14.79 to 14.96 UT, corresponding to <5 minutes and 1 day post-burst,
yielding a 3 sigma flux upper limit of 0.24 mJy and marginal detection of
0.18 +/- 0.6 mJy, respectively.


Further AMI monitoring is planned. We thank the AMI staff for scheduling these observations.

A. J. Castro-Tirado (IAA-CSIC, ISA-UMA), S. Jeong (IAA-CSIC), J. Gorosabel (IAA-CSIC, UPV-EHU) and D. Reverte (GTC, IAC), on behalf of a larger collaboration, report:

�Following the detection of GRB 140713A by Swift (Mangano et al. GCN 16581
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 ), we observed the field with the 10.4m GTC telescope starting on July 16, 21:28 UT (i.e. 3.11 days postburst). In the coadded frame (900s in r�) we identify in the outskirts of the enhanced Swift-XRT error box  a m_AB~24 source at RA (J2000): 18h 44m 25.48s and Dec (J2000): +59d 38' 00.5"  which we suggest as the potential host galaxy for this dark GRB, taking into account the previously reported optical limits (Cano et al. GCNC 16587) and the detection of a mm afterglow (Zauderer et al. GCN 16593
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 ).�

B. A. Zauderer, W. Fong, and E. Berger (Harvard) report on behalf of a
larger collaboration
as part of the CARMA Key Project "A Millimeter View of the Transient
Universe":

"We observed the position of GRB 140713A (Mangano et al., GCN 16581
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 ) with
the Combined
Array for Research in Millimeter Astronomy (CARMA) beginning 2014 Jul 15.27
(dt = 0.49 d)
at a mean frequency of 85 GHz.  Observations were conducted in the compact
E configuration.
In 3.2 hours of on-source integration, we detect a radio source with a peak
brightness of
1.5 (+/- 0.3) mJy/bm at a position consistent with the enhanced Swift-XRT
position (Beardmore et al.,
GCN 16585
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 ).  We consider this source to be the putative radio afterglow.
Further observations are planned.

We thank the CARMA observers and staff for prompt execution of
these observations."

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

"At 18:43:45.30 UT on 13 July 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 140713A (trigger 426969828 / 140713780)
which was also detected by Swift (Mangano et al. 2014, GCN 16581
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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 70 degrees.

The GBM light curve consists of two main overlapping peaks, with a
total duration of about 4.9 s (50-300keV). The time-averaged
spectrum from T0+0 s to T0+4.6 s is well fit
by a power law function with an exponential high-energy cutoff.
The power law index is -1.2 +/- 0.2 and the cutoff energy,
parameterized as Epeak, is 96 +/- 24 keV.

The event fluence (10-1000 keV) in this time interval is
(5.2 +/- 0.7)E-07 erg/cm^2. The 1.024-sec peak photon flux measured
starting from T0+0 s in the 10-1000 keV band is 3.3 +/- 0.2 ph/s/cm^2.

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

J.A. Kennea (PSU), K.L. Page (U. Leicester), C. Pagani (U. Leicester),
A.P. Beardmore (U. Leicester), A. Melandri (INAF-OAB), B. Sbarufatti
(INAF-OAB/PSU), P. D'Avanzo (INAF-OAB), M.C. Stroh (PSU) and V. Mangano
report on behalf of the Swift-XRT team:

We have analysed 6.7 ks of XRT data for GRB 140713A (Mangano  et al.
GCN Circ. 16581
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 ),  from 5.4 ks to 47.8 ks after the  BAT trigger. The
data are entirely in Photon Counting (PC) mode. The enhanced XRT
position for this burst was given by Beardmore et al. (GCN Circ.
16585
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 ).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=1.20 (+0.27, -0.24).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.8 (+/-0.5). The
best-fitting absorption column is  6.8 (+3.8, -3.2) x 10^21 cm^-2, in
excess of the Galactic value of 5.0 x 10^20 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 4.9 x 10^-11 (7.6 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:	     6.8 (+3.8, -3.2) x 10^21 cm^-2
Galactic foreground: 5.0 x 10^20 cm^-2
Excess significance: 3.2 sigma
Photon index:	     1.8 (+/-0.5)

If the light curve continues to decay with a power-law decay index of
1.20, the count rate at T+24 hours will be 3.0 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.5 x
10^-13 (2.3 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/00604232.

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

A. A. Breeveld (UCL-MSSL) and V. Mangano (PSU) report on behalf of the 
Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140713A 76 
s after the BAT trigger (Mangano et al., GCN Circ. 16581
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 ).
No optical afterglow consistent with the XRT position (Beardmore et al. 
GCN Circ. 16585
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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            76          226          147         >21.8
u_FC               288          538          246         >20.8
white               76         7155          608         >22.9
v                  618         7547          313         >20.9
b                  544        29522          422         >21.5
u                  288        29406         2244         >21.8
w1                 669        17514         1084         >21.3
m2                 644        11576          357         >20.5
w2                 594         7361          333         >20.7

The magnitudes in the table are not corrected for the Galactic 
extinction due to the reddening of E(B-V) = 0.05 in the direction of the 
burst (Schlegel et al. 1998).

������Z. Cano (U. Iceland), D. Malesani (DARK/NBI) and M. Nielsen (Max Planck,
Gottingen) report on behalf of a larger collaboration:

We observed the field of GRB 140713A (Mangano et al., GCN Circ. 16581
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 ) with
the 2.5-m Nordic Optical Telescope (NOT) equipped with ALFOSC starting at
22:02 UT on 13-Jul-2014. We obtained 5x180 s frames in both SDSS-r and
SDSS-i, and 5x300s in SDSS-z.

No new object is found in the refined XRT error circle (Beardmore et al.,
GCN Circ. 16585
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 ) down to limiting magnitudes of:

  filter                t-t0 (hr)
---------------------------------
R (Vega) > 23.9    3.46
I (Vega)  > 23.0    3.77
z (AB)     > 22.5    4.17

The upper limits for an isolated point source in our combined images have
been determined using nearby USNO star at RA=18:44:21.50, Dec=+59:38:04.0,
which has R2=19.23, Imag=17.85, and z=17.87.  The z-band magnitude has been
determined using transformation equations from Table 3 in Jordi et al.
(2006,A&A,460,339).  These magnitudes have not been corrected for
foreground extinction.

L. P. Xin,   J.  Z, Yan,  J. Y. Wei,  Y. L. Qiu, J. S. Deng,  
J. Wang, X. H. Han and C. Wu on behalf of EAFON report:

We began to observe GRB 140713A (Mangano et al., GCN 16581
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 )  
with Xinglong  0.8-m TNT telescope at 18:44:47 (UT) , 
62 sec after the burst.

No any new optical transient was detected in our single or stacked image
in the XRT error box (Mangano et al., GCN 16581
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 ).
Calibrated by nearby USNO B1.0 R2 mag, 
the 3-sigma upper limit magnitudes are shown in the following: 

T-T0(sec,mid)  exposure(sec)    Filter     Upper limit
72                       20                       W          18.0
282                     20*20                  W           19.5

The message may be cited.

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

Using 2110 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 140713A, 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 = 281.10470, +59.63356 which is equivalent
to:

RA (J2000): 18h 44m 25.13s
Dec (J2000): +59d 38' 00.8"

with an uncertainty of 2.0 arcsec (radius, 90% confidence).

This position may be improved as more data are received. The latest
position can be viewed at http://www.swift.ac.uk/xrt_positions. Position
enhancement is described by Goad et al. (2007, 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.

M. Stamatikos (OSU), 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), V. Mangano (PSU),
D. M. Palmer (LANL), T. Sakamoto (AGU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(i.e. the Swift-BAT team):
 
Using the data set from T-239 to T+325 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 140713A (trigger #604232)
(Mangano, et al., GCN Circ. 16581
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 ).  The BAT ground-calculated position is
RA, Dec = 281.141, 59.623 deg which is 
   RA(J2000)  =  18h 44m 33.9s 
   Dec(J2000) = +59d 37' 22.3" 
with an uncertainty of 1.2 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 97%.
 
The mask-weighted light curve shows two peaks starting at ~T-0.2 sec, peaking
at ~T+0.2 and ~T+5 sec, and ending at ~T+10 sec.  T90 (15-350 keV) is
5.30 +- 0.66 sec (estimated error including systematics).
 
The time-averaged spectrum from T-0.11 to T+6.68 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.84 +- 0.14.  The fluence in the 15-150 keV band is 3.7 +- 0.3 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T-0.11 sec in the 15-150 keV band
is 1.9 +- 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/604232/BA/

Sonbas, E. (Adiyaman Univ.), Avdan, H., Dolek, F. (Cukurova Univ.), Guver,
T. (Istanbul Univ.), Gogus, E. (Sabanci Univ.), Erece, O. (Akdeniz Univ.),
Kirbiyik, H. (TUG) on behalf of a larger collaboration.


We observed the field of GRB 140713A (Mangano et al., GCN #16581
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 ) with the
1.0 meter T100 telescope (TUBITAK National Observatory, Antalya - Turkey),
starting on July 13, 20:14:06 UT (~ 1.5 hours after the trigger). We
obtained 5 x 300 s exposures with R filters under good weather conditions.


We do not detect an optical afterglow within the reported XRT error circle
down to a limiting magnitude of >19.9 (2-sigma) in the combined R band
image.


We are grateful to the TUBITAK National Observatory staff for promptly
scheduling the observations and their technical support.

V. Mangano (PSU), S. D. Barthelmy (GSFC), M. M. Chester (PSU),
J. R. Cummings (NASA/UMBC), J. A. Kennea (PSU) and
B. Sbarufatti (INAF-OAB/PSU) report on behalf of the Swift Team:

At 18:43:45 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140713A (trigger=604232).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 281.114, +59.625 which is 
   RA(J2000)  =  18h 44m 27s
   Dec(J2000) = +59d 37' 29"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows two peaks
with a total duration of about 7 sec.  The peak count rate
was ~3500 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 18:44:57.8 UT, 72.8 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source with an enhanced position: RA, Dec 281.1053, 59.6333 which
is equivalent to:
   RA(J2000)  = 18h 44m 25.28s
   Dec(J2000) = +59d 37' 59.8"
with an uncertainty of 2.0 arcseconds (radius, 90% containment). This
location is 33 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.  We
cannot determine whether the source is fading at the present time. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (4.97 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 7.8
(+5.23/-4.19) x 10^21 cm^-2 (90% confidence). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 76 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 19.6 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
0.05. 

Burst Advocate for this burst is V. Mangano (vxm22 AT 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.)