GRB 140412A

V. D'Elia (ASDC), D. N. Burrows (PSU), S. T. Holland (STScI),
L. Izzo (URoma/ICRA), F. E. Marshall (NASA/GSFC), T. Sakamoto (AGU)
and B. Sbarufatti (INAF-OAB/PSU) report on behalf of the Swift Team:

At 22:20:49 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140412A (trigger=595608).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 145.050, -65.809 which is 
   RA(J2000) = 09h 40m 12s
   Dec(J2000) = -65d 48' 31"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a FRED-like 
structure with a duration of about 20 sec.  The peak count rate
was ~2000 counts/sec (15-350 keV), at ~0 sec after the trigger. 

The XRT began observing the field at 22:24:17.0 UT, 207.2 seconds after
the BAT trigger. Using promptly downlinked data we find an uncatalogued
X-ray source with an enhanced position: RA, Dec 144.9713, -65.8226
which is equivalent to:
   RA(J2000)  = 09h 39m 53.11s
   Dec(J2000) = -65d 49' 21.3"
with an uncertainty of 3.2 arcseconds (radius, 90% containment). This
location is 125 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. 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 236 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 none of
the XRT error circle. 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 0.22. 

Burst Advocate for this burst is V. D'Elia (delia AT asdc.asi.it). 
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.R. Goad, J.P. Osborne, A.P. Beardmore and P.A. Evans (U. Leicester) 
report on behalf of the Swift-XRT team.

Using 862 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 140412A, 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 = 144.97315, -65.82169 which is equivalent
to:

RA (J2000): 09h 39m 53.55s
Dec (J2000): -65d 49' 18.1"

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.

T. N. Ukwatta (MSU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), V. D'Elia (ASDC), N. Gehrels (GSFC),
H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/UMBC), C. B. Markwardt (GSFC),
D. M. Palmer (LANL), T. Sakamoto (AGU), M. Stamatikos (OSU), J. Tueller (GSFC)
(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 140412A (trigger #595608)
(D'Elia, et al., GCN Circ. 16097
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 ).  The BAT ground-calculated position is
RA, Dec = 145.032, -65.826 deg, which is 
   RA(J2000)  =  09h 40m 07.6s 
   Dec(J2000) = -65d 49' 33.7" 
with an uncertainty of 1.7 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 77%.
 
The mask-weighted light curve shows two peaks strting at ~T-35 sec,
peaking at ~T+1 sec, and ending at ~T+35 sec.
T90 (15-350 keV) is 39.6 +- 8.2 sec (estimated error including systematics).
 
The time-averaged spectrum from T-36.94 to T+12.18 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.95 +- 0.19.  The fluence in the 15-150 keV band is 7.2 +- 0.8 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+0.04 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/595608/BA/

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

We have analysed 6.1 ks of XRT data for GRB 140412A (D'Elia  et al. GCN
Circ. 16097
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 ),  from 198 s to 41.3 ks after the	BAT trigger. The data
are entirely in Photon Counting (PC) mode. The enhanced XRT position
for this burst was given by Goad et al. (GCN Circ. 16100
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 ).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=0.60 (+0.10, -0.09).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 3.2 (+0.9, -0.6). The
best-fitting absorption column is  9.1 (+4.6, -3.3) x 10^21 cm^-2, in
excess of the Galactic value of 2.6 x 10^21 cm^-2 (Willingale et al.
2013). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 2.8 x 10^-11 (1.7 x 10^-10) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:	     9.1 (+4.6, -3.3) x 10^21 cm^-2
Galactic foreground: 2.6 x 10^21 cm^-2
Excess significance: 3.3 sigma
Photon index:	     3.2 (+0.9, -0.6)

If the light curve continues to decay with a power-law decay index of
0.60, the count rate at T+24 hours will be 3.7 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.0 x
10^-13 (6.4 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/00595608.

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

S. T. Holland (STScI) and V. D'Elia (ASDC) report on behalf of the
Swift/UVOT team:

    Swift/UVOT began settled observations of the field of GRB 140412A
237 s after the BAT trigger (D'Elia et al. 2014, GCNC 16097).  We do
not detect any new source consistent with the UVOT-enhanced XRT
afterglow position (Goad et al. 2014, GCNC 16100) in any of the UVOT
exposures.  Preliminary 3-sigma upper limits, using the UVOT
photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373),
for the finding chart and summed exposures are presented below.

---------------------------------------------------
Filter        TSTART     TSTOP   Exposure       Mag
---------------------------------------------------
v                393      1055         69     >19.0
b                491      6805        255     >21.0
u                466      6599        309     >20.6
uvw1             442      4815        255     >20.0
uvm2             418      4610        255     >19.6
uvw2             541      1040         58     >18.7
white            237      6811        336     >21.8
---------------------------------------------------

    The quoted upper limits have not been corrected for the expected
extinction due to the Galactic reddening along the line of sight to
this burst of E(B-V) = 0.19 mag (Schlafly et al. 2011, ApJS, 737,
103).