GRB 140614B

K. L. Page (U Leicester), J. R. Cummings (NASA/UMBC),
N. P. M. Kuin (UCL-MSSL), T. Sakamoto (AGU) and M. H. Siegel (PSU)
report on behalf of the Swift Team:

At 06:38:11 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140614B (trigger=601662).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 322.625, +14.920 which is 
   RA(J2000) = 21h 30m 30s
   Dec(J2000) = +14d 55' 13"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a single weak broad 
peak with a duration of about 35 sec.  The peak count rate was ~1248 
counts/sec (15-350 keV), at ~2 sec after the trigger. 

The XRT began observing the field at 06:40:16.9 UT, 125.2 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
uncatalogued X-ray source with an enhanced position: RA, Dec 322.6313,
14.9299 which is equivalent to:
   RA(J2000)  = 21h 30m 31.50s
   Dec(J2000) = +14d 55' 47.5"
with an uncertainty of 2.1 arcseconds (radius, 90% containment). This
location is 41 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 (8.06 x
10^20 cm^-2, Willingale et al. 2013), with an excess column of 3.7
(+2.77/-2.35) x 10^21 cm^-2 (90% confidence). 

The initial flux in the 2.5 s image was 1.21e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 132 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
0.08. 

Burst Advocate for this burst is K. L. Page (kpa 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.)

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

Using 1221 s of XRT Photon Counting mode data and 2 UVOT
images for GRB 140614B, 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 = 322.63127, +14.92970 which is equivalent
to:

RA (J2000): 21h 30m 31.50s
Dec (J2000): +14d 55' 46.9"

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

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

---------- Forwarded message ----------
From: "Nat Butler" <natbutler@asu.edu>
Date: Jun 14, 2014 7:32 AM
Subject: GRB 140614B: RATIR Optical and NIR Observations
To: "Nat Butler" <natbutler@asu.edu>
Cc:

Nat Butler (ASU), Alan M. Watson (UNAM), Alexander Kutyrev (GSFC), William
H. Lee (UNAM), Michael G. Richer (UNAM), Chris Klein (UCB), Ori Fox (UCB),
J. Xavier Prochaska (UCSC), Josh Bloom (UCB), Antonino Cucchiara
(ORAU/GSFC), Eleonora Troja (GSFC), Owen Littlejohns (ASU), Enrico
Ramirez-Ruiz (UCSC), Jos�� A. de Diego (UNAM), Leonid Georgiev (UNAM), Jes��s
Gonz��lez (UNAM), Carlos Rom��n-Z����iga (UNAM), Neil Gehrels (GSFC), and
Harvey Moseley (GSFC) report:

We observed the field of GRB 140614B (Page, et al., GCN 16394
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 ) with the
Reionization and Transients Infrared Camera (RATIR; www.ratir.org) on the
1.5m Harold Johnson Telescope at the Observatorio Astron��mico Nacional on
Sierra San Pedro M��rtir from 2014/06 14.28 to 2014/06 14.47 UTC (0.11 to
4.62 hours after the BAT trigger), obtaining a total of 0.71 hours exposure
in the r and i bands and 0.30 hours exposure in the Z, Y, J, and H bands.

For a source within the Swift-XRT error circle, in comparison with 2MASS,
we obtain the following upper limits (3-sigma):

  r     > 22.70
  i     > 22.53
  Z     > 21.64
  Y     > 21.08
  J     > 21.04
  H     > 20.51

These magnitudes are in the AB system and are not corrected for Galactic
extinction in the direction of the GRB.

We thank the staff of the Observatorio Astron��mico Nacional in San Pedro
M��rtir.

N. P. M. Kuin (UCL-MSSL) and K. L. Page (U Leicester)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140614B
132 s after the BAT trigger (Page et al., GCN Circ. 16394
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 ).
No optical afterglow consistent with the XRT position
(Evans et al. GCN Circ. 16395
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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           132          282          147         >21.0
u_FC               291          540          246         >20.4
white              132         6723          766         >22.2
v                  621         7133          490         >20.1
b                  546         6518          471         >20.9
u                  291         6314          697         >20.8
w1                 670         6108          293         >20.5
m2                1073         7222          298         >20.1
w2                 597         6929          471         >21.0

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),
N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/UMBC),
C. B. Markwardt (GSFC), D. M. Palmer (LANL), K. L. Page (U Leicester),
T. Sakamoto (AGU), M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (MSU)
(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 140614B (trigger #601662)
(Page, et al., GCN Circ. 16394
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 ).  The BAT ground-calculated position is
RA, Dec = 322.636, 14.895 deg, which is 
   RA(J2000)  =  21h 30m 32.6s 
   Dec(J2000) = +14d 53' 41.5" 
with an uncertainty of 2.1 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 71%.
 
The mask-weighted light curve shows a FRED pulse starting at ~T0,
peaking at ~T+5 sec, and ending at ~T+75 sec.  T90 (15-350 keV) is
49.8 +- 7.9 sec (estimated error including systematics).
 
The time-averaged spectrum from T-3.28 to T+55.59 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
2.04 +- 0.26.  The fluence in the 15-150 keV band is 5.5 +- 1.0 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+6.93 sec in the 15-150 keV band
is 0.5 +- 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/601662/BA/

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

We observed the field of GRB 160614B (Page et al., GCNC 16394)
with the optical three color (g', Rc and Ic) CCD camera attached
to the MITSuME 50cm telescope of Okayama Astrophysical Observatory.

The observation started on 2014-06-14 16:44:18 (~10.1 h after the burst).
We did not find any new point source within the enhanced XRT circle
(Evans et al., GCNC 16395) in all the three bands.

Three sigma upper limits of the OT are listed below.
We used GSC 2.3 catalog for flux calibration.

#T0+[day]  MID-UT    T-EXP[sec]   g'     Rc     Ic
-----------------------------------------------------
0.46713    17:50:51    6060.0   >19.2  >19.3  >18.6
-----------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]

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

We have analysed 7.8 ks of XRT data for GRB 140614B (Page  et al. GCN
Circ. 16394
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 ),  from 115 s to 52.7 ks after the	BAT trigger. The data
comprise 86 s in Windowed Timing (WT) mode (the first 9 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. 16395
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 ).

The light curve can be modelled with an initial power-law decay with an
index of alpha=1.35 (+/-0.13), followed by a break at T+515 s to an
alpha of 3.93 (+0.28, -0.26).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index	of 0.99 (+0.20, -0.18). The
best-fitting absorption column is  3.6 (+2.1, -1.6) x 10^21 cm^-2, in
excess of the Galactic value of 8.1 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 1.46 (+0.19, -0.18)
and a best-fitting absorption column of 2.3 (+1.0, -0.9) x 10^21 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 5.1 x 10^-11 (5.9 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:	     2.3 (+1.0, -0.9) x 10^21 cm^-2
Galactic foreground: 8.1 x 10^20 cm^-2
Excess significance: 2.9 sigma
Photon index:	     1.46 (+0.19, -0.18)

If the light curve continues to decay with a power-law decay index of
3.93, the count rate at T+24 hours will be 3.7 x 10^-9 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.9 x
10^-19 (2.2 x 10^-19) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00601662.

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

S. Kurita, T. Yoshii, Y. Saito, Y. Tachibana, H. Ohuchi, Y. Yano, 
Y. Ono, T. Fujiwara, Y. Yatsu, and N. Kawai (Tokyo Tech)
report on behalf of the MITSuME collaboration:

We observed the field of GRB 140614B (K. L. Page et al., GCN Circular #16394
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 ) with the 
optical three color (g, Rc, and Ic) CCD cameras attached to the MITSuME 50 cm
telescope of Akeno Observatory, Yamanashi, Japan.

The observation started on 2014-06-14 14:18:14 UT ( 7.7h after the burst).
We did not find any new point source within XRT circle in all the three bands.


The measured magnitudes were listed below.

T0+[sec] MID-UT T-EXP[sec] g' Rc Ic
27602 16:26:47 14280 >19.7 >19.8 >18.9

T0+ : Elapsed time after the burst 
T-EXP: Total Exposure time 
We used GSC2.3 catalog for flux calibration.

D. A. Perley (Caltech) reports:

I imaged the field of GRB 140614B (Page et al., GCN 16394
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 ) using MOSFIRE 
on the Keck I 10m telescope in the Ks-band filter.  A sequence of 12 
36-second images was obtained at a midtime of 13:18 UT on 2014-06-15 
(1.27 days after the Swift trigger).

No sources are detected within the XRT error circle (Evans et al, GCN 
16395
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 ) to a limiting mag of approximately Ks > 21.9 mag (3-sigma, 
calibrating relative to 2MASS.)

A faint source (Ks = 21.5 +/- 0.2 mag) is detected outside the XRT error 
circle, at a position of RA = 21:30:31.364, dec = +14:55:48.79 (J2000).