GRB 140619A

M. De Pasquale (INAF-IASFPA), D. N. Burrows (PSU), S. B. Cenko (GSFC),
J. A. Kennea (PSU), H. A. Krimm (CRESST/GSFC/USRA),
N. P. M. Kuin (UCL-MSSL), A. Y. Lien (NASA/GSFC/ORAU),
F. E. Marshall (NASA/GSFC), A. Maselli (INAF-IASFPA),
K. L. Page (U Leicester), B. Sbarufatti (INAF-OAB/PSU) and
T. N. Ukwatta (MSU) report on behalf of the Swift Team:

At 11:38:35 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140619A (trigger=602080).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 27.092, -39.261 which is 
   RA(J2000) = 01h 48m 22s
   Dec(J2000) = -39d 15' 40"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  As is usual with an image trigger, the available
BAT light curve shows no significant structure. 

The XRT began observing the field at 11:40:54.9 UT, 139.1 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 27.1084, -39.2586 which is equivalent to:
   RA(J2000)  = +01h 48m 26.02s
   Dec(J2000) = -39d 15' 31.0"
with an uncertainty of 4.8 arcseconds (radius, 90% containment). This
location is 46 arcseconds from the BAT onboard position, within the BAT
error circle. No event data are yet available to determine the column
density using X-ray spectroscopy. 

The initial flux in the 2.5 s image was 5.85e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of  98 seconds with the White filter
starting 147 seconds after the BAT trigger. There is a weak 20.5 mag source
near the XRT position. No aspect UVOT aspect solution is available
because of the paucity of stars. Confirmation of the afterglow
will require the full data set. No correction has been made
for the expected extinction corresponding to E(B-V) of 0.01. 

Burst Advocate for this burst is M. De Pasquale (mdp AT ifc.inaf.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 2297 s of XRT Photon Counting mode data and 3 UVOT
images for GRB 140619A, 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 = 27.10849, -39.25934 which is equivalent
to:

RA (J2000): 01h 48m 26.04s
Dec (J2000): -39d 15' 33.6"

with an uncertainty of 1.8 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.C. Stroh (PSU), D.N. Burrows (PSU), J.A. Kennea (PSU), A.P. Beardmore
(U. Leicester), P.A. Evans (U. Leicester), B.P. Gompertz (U.
Leicester), P. D'Avanzo (INAF-OAB), V. D'Elia (ASDC), M. de Pasquale
(INAF-IASFPA) and M. De Pasquale report on behalf of the Swift-XRT
team:

We have analysed 7.3 ks of XRT data for GRB 140619A (De Pasquale  et
al. GCN Circ. 16415
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 ),  from 129 s to 30.3 ks after the	BAT trigger.
The data comprise 112 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 Goad et al. (GCN Circ. 16416
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 ).

The late-time light curve (from T0+5.1 ks) can be modelled with  a
power-law decay with a decay index of alpha=0.93 (+/-0.09).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index	of 0.67 (+/-0.05). The
best-fitting absorption column is  1.9 (+/-0.4) x 10^21 cm^-2, in
excess of the Galactic value of 1.6 x 10^20 cm^-2 (Willingale et al.
2013). The PC mode spectrum has a photon index of 2.09 (+0.15, -0.14)
and a best-fitting absorption column of 2.5 (+/-0.5) 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 (5.1 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:	     2.5 (+/-0.5) x 10^21 cm^-2
Galactic foreground: 1.6 x 10^20 cm^-2
Excess significance: 7.7 sigma
Photon index:	     2.09 (+0.15, -0.14)

If the light curve continues to decay with a power-law decay index of
0.93, the count rate at T+24 hours will be 0.031 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.1 x
10^-12 (1.6 x 10^-12) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00602080.

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

M. H. Siegel (PSU), F. E. Marshall (NASA/GSFC), J. Linevsky (PSU),
and M. De Pasquale (INAF-IASFPA) report on behalf of the
Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 140619A
147 s after the BAT trigger (De Pasquale et al., GCN Circ. 16415
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 ).
We confirm a faint afterglow consistent with the XRT position is detected in the
initial UVOT exposures. We have corrected the positions in the 2.7' x 2.7� UVOT
sub-image by comparing positions with the Digital Sky Survey. The UVOT afterglow
is located at:
  RA  (J2000) =  01:48:26.15 =  27.10896 (deg.)
  Dec (J2000) = -39:15:32.6  = -39.25906 (deg.)
with an estimated uncertainty of 1.0 arc sec. (radius, 90% confidence).

Preliminary detections and 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)     147          245        96     20.39+-0.24
white         5112         5312       196     >21.05
b            11745        12179       422     >20.65
u            10833        11740       885     >20.82
uvw1          5933         6133       196     >19.77
uvm2          5727         5927       196     >19.59
uvw2          5317         5517       196     >19.87

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.01 in the direction of the burst
(Schlegel et al. 1998).

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), M. De Pasquale (INAF-IASFPA)
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-239 to T+421 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 140619A (trigger #602080)
(De Pasquale, et al., GCN Circ. 16415
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 ).  The BAT ground-calculated position is
RA, Dec = 27.096, -39.249 deg which is
   RA(J2000)  =  01h 48m 23.2s
   Dec(J2000) = -39d 14' 57.1"
with an uncertainty of 1.8 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 41%.

The mask-weighted light curve shows a complex structure with multiple peaks.
The main visible structure starts with roughly two long weaker pulses from
~T+20 s to T+150 s. The two weak pulses were followed by the major bright
structure lasting until ~T+260 s, and it consists of many sub-pulses. Afterward
there is another weaker long pulse lasting until ~T+350 s. T90 (15-350 keV) is
233.9 +- 13.4 sec (estimated error including systematics).

Note that the main structure of the burst happened at ~150 s after the original image trigger,
and was not described in the first circular (De Pasquale, et al., GCN Circ. 16415
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 ).

The time-averaged spectrum from T+32.3 to T+340.4 sec is best fit by a power law
with an exponential cutoff.  This fit gives a photon index 1.45 +- 0.14,
and Epeak of 117.8 +- 46.2 keV (chi squared 54.23 for 56 d.o.f.).  For this
model the total fluence in the 15-150 keV band is 2.1 +- 0.04 x 10^-5 erg/cm2
and the 1-sec peak flux measured from T+219.52 sec in the 15-150 keV band is
4.6 +- 0.2 ph/cm2/sec.  A fit to a simple power law gives a photon index
of 1.71 +- 0.03 (chi squared 64.34 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/602080/BA/

S. Golenetskii, R.Aptekar, D. Frederiks, V. Pal'shin, P. Oleynik,
M. Ulanov, D. Svinkin, A. Tsvetkova, A. Lyssenko, and T. Cline
on behalf of the Konus-Wind team, report:

The long GRB 140619A (Swift-BAT trigger #602080: De Pasquale, et al.,
GCN Circ. 16415
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 , Palmer, et al., GCN Circ. 16423
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 ) was detected by
Konus-Wind in the waiting mode.

The burst light curve shows a single multipeak episode started
at ~T0(BAT)+35 s with a duration of ~340 s.

The K-W light curve of this burst is available at
http://www.ioffe.ru/LEA/GRBs/GRB140619A/

As observed by Konus-Wind, the burst had a fluence of
5.4(-0.5,+0.2)x10^-5 erg/cm2 and a 2.944-s peak energy flux,
measured from ~T0(BAT)+191 s, of 1.5(-0.3,+0.2)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

Modeling the K-W 3-channel time-integrated spectrum (from T0(BAT)+35 s
to T0(BAT)+374 s) by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
yields alpha = -1.3 �� 0.1, and Ep = 236 (-27,+33) keV.

All the quoted errors are estimated at the 1 sigma confidence level.
All the presented results are preliminary.