GRB 160714A

M. H. Siegel (PSU), J. A. Kennea (PSU), A. Y. Lien (GSFC/UMBC),
F. E. Marshall (NASA/GSFC), D. M. Palmer (LANL) and
B. Sbarufatti (INAF-OAB/PSU) report on behalf of the Swift Team:

At 02:19:15 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 160714A (trigger=704310).  Swift did not slew immediately
due to an observational constraint. 
The BAT on-board calculated location is 
RA, Dec 234.461, +63.831 which is 
   RA(J2000) = 15h 37m 51s
   Dec(J2000) = +63d 49' 53"
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 0.5 sec.  The peak count rate
was ~2000 counts/sec (15-350 keV), at ~0.3 sec after the trigger. 

Due to an observing constraint, Swift will not slew until T0+26.0
minutes. There will be no XRT or UVOT data until this time. 

Burst Advocate for this burst is M. H. Siegel (siegel AT swift.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.)

M. Perri (ASDC), G. Tagliaferri (INAF-OAB), P.A. Evans (U. Leicester),
J.P. Osborne (U. Leicester), D.N. Burrows (PSU) and J.A. Kennea (PSU)
report on behalf of the Swift-XRT team:

The XRT began observing the field of GRB 160714A at 02:47:12.7 UT,
1677.2 seconds after the BAT trigger. No source was detected in 1.0 ks
of promptly downlinked data, which covered 88% of the BAT error circle.
We are waiting for the full dataset to detect and localise the XRT
counterpart.

A. de Ugarte Postigo (IAA-CSIC, DARK/NBI), A. Sota (IAA-CSIC) 
report on behalf of a larger collaboration:

We have observed the field of GRB 160714A (Siegel et al. GCN 
19697
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 ) with the 1.5m OSN telescope, in Granada (Spain). 
Observations started at 2:33 UT (14 min after the GRB onset) and 
consisted of 3x180s + 4x300s I-band images. Each of the 
individual images cover the complete BAT error circle. In a 
preliminary analysis we detect no new source within the BAT error 
box down to a 3-sigma limit of I(AB) > 20.5 mag in the first image, 
and down to I(AB) > 21.5 mag in the combined image (mean time 
2:48 UT, 29 minutes after the burst), as compared to SDSS data.

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

R. Rebolo, M. Serra, N. Lodieu, G. Israelian, L. Suarez-Andres
The Instituto de Astrofisica de Canarias

D.Buckley, S. Potter, A.Kniazev, M.Kotze
South African Astronomical Observatory

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

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

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

Ricardo Podesta, Carlos Lopez and Federico Podest
Observatorio Astronomico Felix Aguilar (OAFA)

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

MASTER-IAC  robotic telescope (MASTER-Net: http://observ.pereplet.ru, 4 
square degrees twin telescope) 
located in IAC was pointed to the  GRB160714A (Siegel et al., GCN 19697
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 ) 
26 sec after notice time and 50 sec after trigger time at 2016-07-14
02:20:05 UT. On our first (10s exposure)  set we not  found optical
transient within SWIFT error-box (ra=15 37 50 dec=+63 49 51 r=0.05 degrees)
brighter then 16.1.

Our automatic results of the first 20 minutes observations after trigger 
tieme are:

   Id 	Pro.type    Time UT       Exp.time	Limit	Filt.   Tube
                                     s

269575     Alert    02:20:05         10          16.1     P|    EAST
269574     Alert    02:20:05         10          16.4     P-    WEST
269582  SumAlert    02:20:05         60          17.7     P|    EAST
269585  SumAlert    02:20:05         60          17.9     P-    WEST
269639  SumAlert    02:20:05        700          19.6     P|    EAST
269626  SumAlert    02:20:05        700          19.9     P-    WEST
269577     Alert    02:20:47         20          17.3     P|    EAST
269576     Alert    02:20:47         20          17.3     P-    WEST
269579	   Alert    02:21:21	     30	         17.5	  P|	EAST
269578	   Alert    02:21:21	     30	         17.8     P-	WEST
269581	   Alert    02:22:05	     30	         17.5	  P|	EAST
269580     Alert    02:22:05         30          17.6     P-    WEST
269588  SumAlert    02:22:05        120          18.6     P|    EAST
269591	SumAlert    02:22:05	    120	         18.6	  P-	WEST
269584	   Alert    02:22:49	     40	         17.8	  P|	EAST
269583	   Alert    02:22:49	     40	         17.9	  P-	WEST
269587	   Alert    02:23:41	     50	         17.9	  P|	EAST 
269586	   Alert    02:23:41   	     50	         17.9	  P-	WEST 
269590	   Alert    02:24:46	     70	         18.2     P|	EAST
269589     Alert    02:24:46         70          18.2     P-    WEST
269597  SumAlert    02:24:46        250          19.1     P|    EAST
269596  SumAlert    02:24:46        250          19.4     P-    WEST
269592     Alert    02:26:11         80          18.2     P|    EAST
269593     Alert    02:26:11         80          18.5     P-    WEST
269595	   Alert    02:27:45	    100	         18.5	  P|	EAST
269594	   Alert    02:27:45	    100	         18.6	  P-	WEST
269599	   Alert    02:29:38	    120	         18.5	  P|	EAST
269598	   Alert    02:29:38	    120	         18.6	  P-	WEST
269601	   Alert    02:31:51	    150	         18.6	  P|	EAST
269600	   Alert    02:31:51	    150	         18.9	  P-	WEST
269603	   Alert    02:34:34	    180	         18.5	  P|	EAST
269602	   Alert    02:34:34        180	         18.6	  P-	WEST
269665  SumAlert    02:34:34       1800          19.6     P|    EAST
269675	SumAlert    02:34:34	   1800	         19.5	  P-	WEST
269604	   Alert    02:38:06	    180	         18.5	  P|	EAST
269605     Alert    02:38:06        180          18.6     P-    WEST
269610  SumAlert    02:38:06        540          19.2     P|    EAST
269613	SumAlert    02:38:06	    540	         19.2	  P-	WEST
269606	   Alert    02:41:33	    180	         18.5	  P|	EAST
269607	   Alert    02:41:33	    180	         18.6	  P-	WEST

The message may be cited.

D. M. Palmer (LANL), S. D. Barthelmy (GSFC), J. R. Cummings (GSFC/UMBC),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), A. Y. Lien (GSFC/UMBC),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), T. Sakamoto (AGU),
M. H. Siegel (PSU), M. Stamatikos (OSU), T. N. Ukwatta (LANL)
(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 160714A (trigger #704310)
(Siegel, et al., GCN Circ. 19697
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 ).  The BAT ground-calculated position is
RA, Dec = 234.490, 63.809 deg which is
   RA(J2000)  =  15h 37m 57.7s
   Dec(J2000) = +63d 48' 32.1"
with an uncertainty of 2.7 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 35%.
 
The mask-weighted light curve shows a double-peak structure starting at
T0, peaking at T+0.05 sec and T+0.2 sec and ending at T+0.3 sec.
T90 (15-350 keV) is 0.35 +- 0.11 sec (estimated error including systematics).
 
The time-averaged spectrum from T+0.02 to T+0.40 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.38 +- 0.37.  The fluence in the 15-150 keV band is 6.9 +- 1.6 x 10^-8 erg/cm2.
The 1-sec peak photon flux measured from T-0.29 sec in the 15-150 keV band
is 1.1 +- 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/704310/BA/

Hoi-Fung Yu (MPE) and Charles A. Meegan (USRA)
report on behalf of the Fermi GBM Team:

"At 02:19:15.62 UT on 14 July 2016, the Fermi Gamma-Ray Burst Monitor
triggered and located GRB 160714A (trigger 490155559/160714097),
which was also detected by the Swift/BAT (Siegel et al. 2016, GCN 19697
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 )
The GBM on-ground location is consistent with the Swift position.

The angle from the Fermi LAT boresight at the GBM trigger time is 51 degrees.

The GBM light curve shows a short pulse with sub-structures
with a duration (T90) of about 0.32 s (50-300 keV).
The time-averaged spectrum from T0-0.064 s to T0+0.192 s is
best fit by a power law function with an exponential
high-energy cutoff. The power law index is -0.5 +/- 0.4 and
the cutoff energy, parameterized as Epeak, is 200 +/- 55 keV.

The event fluence (10-1000 keV) in this time interval is
(1.6 +/- 0.3)E-07 erg/cm^2. The 64-ms peak photon flux measured
starting from T0+0.128 s in the 10-1000 keV band is 6 +/- 1 ph/s/cm^2.

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

J.P. Osborne (U. Leicester), K.L. Page (U. Leicester), A. D'Ai
(INAF-IASFPA), A. Maselli  (INAF-IASFPA), A. Melandri (INAF-OAB), J.A.
Kennea (PSU), B. Sbarufatti (INAF-OAB/PSU), D.N. Burrows (PSU), B.
Mingo (U. Leicester) and D. M. Palmer (LANL) report on behalf of the
Swift-XRT team:

We have analysed 6.2 ks of Photon Counting (PC) mode XRT data for the
Swift/BAT-detected burst GRB 160714A (Palmer et al. GCN Circ. 19705
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 ),
collected between T0+1.7 ks and T0+43.3 ks. 

Three uncatalogued X-ray sources have been detected within 296 arcsec
of the Swift/BAT position, however none of them is above the RASS limit
or shows definitive signs of fading. Therefore, at the present time we
cannot identify which, if any, is the afterglow. Details of these
sources are given below:

Source 1:
  RA (J2000.0):  234.3249  =  15:37:17.98
  Dec (J2000.0): +63.8684  =  +63:52:06.3
  Error: 4.3 arcsec (radius, 90% conf.)
  Count-rate: (5.8 +/- 1.2)e-3 ct s^-1	 
  Distance: 254 arcsec from Swift/BAT position.
  Flux: (1.78 +/- 0.37)e-13 erg cm^-2 s^-1 (observed, 0.3-10 keV)

Source 4:
  RA (J2000.0):  234.5768  =  15:38:18.43
  Dec (J2000.0): +63.7722  =  +63:46:19.8
  Error: 4.8 arcsec (radius, 90% conf.)
  Count-rate: (3.07 +/- 0.95)e-3 ct s^-1   
  Distance: 280 arcsec from Swift/BAT position.
  Flux: (8.3 +/- 2.6)e-14 erg cm^-2 s^-1 (observed, 0.3-10 keV)

Source 9:
  RA (J2000.0):  234.4312  =  15:37:43.50
  Dec (J2000.0): +63.8530  =  +63:51:10.9
  Error: 7.1 arcsec (radius, 90% conf.)
  Count-rate: (1.70 +/- 0.76)e-3 ct s^-1   
  Distance: 92 arcsec from Swift/BAT position.
  Flux: (7.0 +/- 3.2)e-14 erg cm^-2 s^-1 (observed, 0.3-10 keV)

Eight uncatalogued sources were also detected too far from the GRB
position to be likely afterglow candidates.

The results of the XRT-team automatic analysis of the XRT observations,
including a position-specific upper limit calculator, are available at
http://www.swift.ac.uk/ToO_GRBs/00704310.

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

Klotz A., Turpin D., Atteia J.L. (CNRS-OMP-IRAP),
Boer, M., Laugier, R. (CNRS-ARTEMIS),
Gendre B. (UVI - Etelman Obs.) report:

We imaged the field of GRB 160714A detected by SWIFT
(trigger 704310) with the TAROT robotic telescope (D=25cm)
located at the Calern observatory, France.

The observations started 40s after the GRB trigger
(20s after the notice). The elevation of the field decreased from
34 degrees above horizon and weather conditions
were good.

The first image is trailed with a duration of 60.0s
(see the description in Klotz et al., 2006, A&A 451, L39).
We do not detect any OT with a limiting magnitude of:
t0+40.0s to t0+100.0s : Rlim = 16.3

The second image is 30.0s exposure in tracking mode:
t0+115.7s to t0+145.7s : Rlim = 17.5

We co-added a series of exposures:
t0+115.7s to t0+412.9s : Rlim = 18.9

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

M. H. Siegel (PSU)reports on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 160714A
1682 s after the BAT trigger (Siegel et al., GCN Circ. 19697
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 ).
No optical afterglow consistent with the BAT position
is detected in the 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)        1682         1831          147         >20.14
white             1914         8131          292         >21.04
v                 1964         8542          293         >19.67
b                 1889         7926          293         >20.12
u                 1865         7720          490         >20.07
uvw1              1840         2908          293         >20.06
uvw2              1939         8336          235         >20.08

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.02 in the direction of the burst
(Schlegel et al. 1998).

K. P. Mooley, T. D. Staley, R. P. Fender (Oxford), G. E. Anderson 
(Curtin), T. Cantwell (Manchester), C. Rumsey, D. Titterington, S. 
Carey, J. Hickish, Y. C. Perrott, N. Razavi-Ghods, P. Scott (Cambridge), 
K. Grainge, A. Scaife (Manchester)

The AMI Large Array robotically triggered on the Swift alert for GRB 
160714A (Siegel et al., GCN 19697
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 ) as part of the 4pisky program, and 
subsequent follow up observations were obtained up to 10 days 
post-burst. Our observations at 15 GHz on 2016 Jul 14.65, Jul 17.85, and 
Jul 21.85 (UT) do not reveal any variable radio source within the BAT 
error circle (Palmer et al., GCN 19705
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 ), with 3sigma upper limits of 150 
uJy, 213 uJy, and 132 uJy respectively.

We thank the AMI staff for scheduling these observations. The AMI-GRB 
database is a log of all GRB follow up observations with the AMI, and is 
available at http://4pisky.org/ami-grb/.