GRB 140213A

S. T. Holland (STScI), V. D'Elia (ASDC), N. Gehrels (NASA/GSFC),
J. A. Kennea (PSU), H. A. Krimm (CRESST/GSFC/USRA), V. Mangano (PSU),
F. E. Marshall (NASA/GSFC), C. J. Mountford (U Leicester),
P. T. O'Brien (U Leicester), C. Pagani (U Leicester),
K. L. Page (U Leicester), J. L. Racusin (NASA/GSFC),
M. H. Siegel (PSU) and B.-B. Zhang (UAH) report on behalf of the Swift
Team:

At 19:21:37 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 140213A (trigger=586569).  Swift did not slew to the burst immediately. 
The BAT on-board calculated location is 
RA, Dec 105.218, -73.136 which is 
   RA(J2000) = 07h 00m 52s
   Dec(J2000) = -73d 08' 10"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed two strong peaks 
starting at T-5, with a total duration of about 10 sec, followed by a 
third weaker pulse at T+15.  The peak count rate
was ~18,000 counts/sec (15-350 keV), at ~1 sec after the trigger. 

Due to an observing constraint, Swift will not slew until T0+54.8
minutes. There will be no XRT or UVOT data until this time. 

Burst Advocate for this burst is S. T. Holland (sholland AT stsci.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. H. Siegel (PSU) and S. T. Holland (STScI) report on behalf of the Swift/UVOT team:

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 3428 seconds after the BAT trigger on GRB 140213A (Holland et al., GCN Circ.
15825
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 ). There is a candidate afterglow in the rapidly available 2.7'x2.7' sub-image at
 RA(J2000)  =	07:00:37.09 = 105.15455
 DEC(J2000) = -73:08:13.5  = -73.13707
with a 90%-confidence error radius of about 0.62 arc sec. This position is 6.2
arc sec. from the center of the XRT error circle. The estimated magnitude is
17.74 with a 1-sigma error of about  0.14. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.15.

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

The XRT began observing the field of GRB 140213A at 20:18:43.0 UT,
3425.3 seconds after the BAT trigger. Using promptly downlinked data we
find an uncatalogued X-ray source located at RA, Dec 105.15145,
-73.13570 which is equivalent to:
   RA(J2000)  = 07h 00m 36.35s
   Dec(J2000) = -73d 08' 08.5"
with an uncertainty of 3.6 arcseconds (radius, 90% containment). This
location is 69 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. 

A power-law fit to a spectrum formed from promptly downlinked event
data gives a column density in excess of the Galactic value (1.13 x
10^21 cm^-2, Kalberla et al. 2005), with an excess column of 2.4
(+1.68/-1.51) x 10^21 cm^-2 (90% confidence).

A. Trotter, J. Haislip, D. Reichart, A. LaCluyze, A. Verveer, T. Spuck, 
A. Foster, N. Frank, K. Ivarsen, J. Moore, M. Nysewander, R. Beauchemin, 
T. Berger, M. Carroll, H. T. Cromartie, R. Egger, M. Hinckle, A. 
Ireland, M. Maples, L. Scott, and J. A. Crain report:

Skynet observed the Swift-BAT localization of GRB 140213A (Holland et 
al., GCN 15825
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 , Swift trigger 586569) with the 14-inch R-COP telescope 
at Perth Observatory, Australia.  Observations began at 59s and 
continued until 92m post-trigger, with rotating exposures in the BVRI 
bands increasing from 10s to 80s. We detect a fading optical source in 
all bands at the position of the source detected by the Swift UVOT 
(Siegel & Holland, GCN 15826
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 ). The source faded from R=14.3 at t=113s to 
R=17.8 at t=73m.

A preliminary light curve is at:
http://www.skynet.unc.edu/grb/grb140213a.png 
<https://outlook.unc.edu/owa/redir.aspx?C=y2fEeVtlHEGuQvMGxBu8RSnt2Tap_NAIeyK3ME-qCZACrK94N0zj_7W5zZXZpIb5kE5UKcCeXkY.&URL=http%3a%2f%2fwww.skynet.unc.edu%2fgrb%2fgrb140213a.png>

Photometry is calibrated to five APASS-DR7 stars in the field, and has 
not been corrected for the Galactic foreground extinction corresponding 
to E(B-V)=0.07 (Schlegel et al. 1998).

Skynet observations are ongoing.

J. Elliott, K. Varela (both MPE Garching), D. A. Kann (TLS Tautenburg),
and J. Greiner (MPE Garching) report on behalf of the GROND team:

We observed the field of GRB 140213A (Swift trigger 586569; Holland et
al., GCN #15825
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 ) simultaneously in g'r'i'z'JHK with GROND (Greiner et al.
2008, PASP 120, 405) mounted at the 2.2 m MPG telescope at La Silla
Observatory (Chile).

Observations started at 00:25 UT on 14 February 2014, 5 hours after the
GRB trigger, and are continuing. They were performed at an average seeing
of 1.9" and at an average airmass of 1.4.

We find a single point source within the 0.4" Swift-UVOT error circle
reported by Siegel & Holland (GCN #15826
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 ) and confirmed by Trotter et al.
(GCN #15828
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 ).

Based on the first 4.4 min of total exposures in g'r'i'z' and 4 min in
JHK, we estimate preliminary magnitudes (all in AB) of

g' = 19.7 +/- 0.1 mag,
r' = 19.4 +/- 0.1 mag,
i' = 19.2 +/- 0.1 mag,
z' = 19.1 +/- 0.1 mag,
J  = 18.7 +/- 0.1 mag,
H  = 18.5 +/- 0.1 mag, and
K  = 18.4 +/- 0.1 mag.

The spectral energy distribution is best-fit by a straight power-law with
spectral slope b = 0.8 +/- 0.1.

Given magnitudes are calibrated against GROND zeropoints as well as 2MASS
field stars and are not corrected for the expected Galactic foreground
extinction corresponding to a reddening of E_(B-V)=0.07 mag in the
direction of the burst (Schlegel et al. 1998).

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

Using 3106 s of XRT Photon Counting mode data and 7 UVOT
images for GRB 140213A, 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 = 105.15491, -73.13725 which is equivalent
to:

RA (J2000): 07h 00m 37.18s
Dec (J2000): -73d 08' 14.1"

with an uncertainty of 1.5 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.

S. Schulze (PUC and MCSS), K. Wiersema (U. Leicester), D. Xu, and J. P. U. Fynbo (DARK/NBI) report on behalf of a larger collaboration:
 
We observed the optical counterpart of GRB 140213A (Holland et al., GCN 15825
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 ; Siegel et al., GCN 15826
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 ) with the ESO VLT equipped with the X-shooter spectrograph starting 5.8 hr after the GRB. The spectrum covers the wavelength range from 3,200 to 18,000 AA. The afterglow is well detected throughout. We detect several absorption features, which we interpret as due to Fe II, Mg I, Mg II, Al II, Al III and others, at a common redshift of z = 1.2076 (wavelength solution based on archival calibration lamps).
 
We acknowledge excellent support from the observing staff in Paranal, in particular Yazan Momany.

C. Pagani (U. Leicester), K. L. Page (U. Leicester) and S. T. Holland
(STScI) report on behalf of the Swift-XRT team:

We have analysed 5.0 ks of XRT data for GRB 140213A (Holland  et al.
GCN Circ. 15825
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 ),  from 3.4 ks to 22.3 ks after the  BAT trigger. The
data are entirely in Photon Counting (PC) mode. The enhanced XRT
position for this burst was given by Beardmore et al. (GCN Circ.
15830
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 ).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=1.04 (+/-0.06).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.91 (+/-0.08). The
best-fitting absorption column is  1.4 (+1.0, -0.9) x 10^21 cm^-2, at a
redshift of 1.2076, in addition to the Galactic value of 1.1 x 10^21
cm^-2 (Kalberla et al. 2005). The counts to observed (unabsorbed)
0.3-10 keV flux conversion factor deduced from this spectrum  is 3.9 x
10^-11 (5.2 x 10^-11) erg cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Galactic foreground: 1.1 x 10^21 cm^-2
Intrinsic column:    1.4 (+1.0, -0.9) x 10^21 cm^-2 at z=1.2076
Photon index:	     1.91 (+/-0.08)

If the light curve continues to decay with a power-law decay index of
1.04, the count rate at T+24 hours will be 0.085 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 3.4 x
10^-12 (4.4 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/00586569.

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

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

"At 19:21:32.35 UT on February 13 2014, the Fermi Gamma-Ray Burst Monitor
triggered and located  GRB 140213A (trigger 414012095/140213807), which was also
detected by Swift (Holland et al., GCN 15825
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 ). The GBM on-ground location
is consistent with the Swift/XRT position (Evans et al., GCN 15827
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 ).

The trigger resulted in an Autonomous Repoint Request (ARR) that was
accepted and the spacecraft slewed to the GBM in-flight location. The
pre-ARR angle from LAT boresight was 48.5 deg from the Swift/XRT
position.

The GBM light curve consists of a multiple-peak structure with a duration
of about 18.6 s (50-300 keV). The time-averaged spectrum from T0+0 s to T0+19 s
is well fit with a Band function parameterized as Epeak = 80 +/- 2 keV, 
alpha = -1.01 +/- 0.03 and beta=-2.41 +/-0.04. The event fluence (10-1000 keV) 
in this time interval is (2.04 +/- 0.03)E-05 erg/cm^2. The 1.0-sec peak photon 
flux measured starting from T0+6 s in the 10-1000 keV band is 37 +/- 0.5 ph/s/cm^2.

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

M. H. Siegel (PSU) and S. T. Holland (STScI) report on behalf of the
Swift/UVOT team:

The Swift/UVOT has continued to observe GRB 140213A (Holland
et al., GCN 15825
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 ).  We find that the optical afterglow is slowly fading
but still detected in all UVOT filters as of 68 ks after the BAT trigger.

The preliminary UVOT position is:
   RA  (J2000) =  07:00:37.13 = 105.15472 (deg.)
   Dec (J2000) = -73:08:13.5  = -73.13707 (deg.)
with an estimated uncertainty of 0.51 arc sec. (radius, 90% confidence).

Preliminary detections using the UVOT photometric system (Breeveld et  
al. 2011, AIP Conf. Proc. 1358, 373) are:

Filter      T_start(s)   T_stop(s)    Exp(s)        Mag
white (fc)   3428         3578         147       17.70+-0.04
white        4610         4809         196       18.08+-0.05
v            3584         3784         196       18.03+-0.12
v            9217        10124         885       19.06+-0.13
v           27349        28053         685       19.73+-0.35
b            4405         4605         196       18.40+-0.09
b           61868        62291         412       19.52+-0.13
u (fc)       4200         4399         196       17.40+-0.06
u           21642        22285         625       18.81+-0.11
u           60956        61863         885       18.91+-0.08
uvw1         3995         4194         196       17.65+-0.10
uvw1        14948        21635        1242       18.79+-0.08
uvm2         3789         3989         196       17.77+-0.14
uvm2        10129        10771         632       18.52+-0.12
uvm2        33470        49991        1348       19.47+-0.14
uvm2        66689        67589         885       19.26+-0.15
uvw2         4816         5012         193       18.46+-0.17
uvw2        26443        27343         885       20.06+-0.21

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.15 in the direction of the burst
(Schlegel et al. 1998).

M. Stamatikos (OSU), S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. R. Cummings (GSFC/UMBC), N. Gehrels (GSFC), S. T. Holland (STScI),
H. A. Krimm (GSFC/USRA), A. Y. Lien (NASA/UMBC), C. B. Markwardt (GSFC),
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+963 sec from the recent telemetry downlink,
we report further analysis of BAT GRB 140213A (trigger #586569)
(Holland, et al., GCN Circ. 15825
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 ).  The BAT ground-calculated position is
RA, Dec = 105.166, -73.136 deg which is
    RA(J2000)  =  07h 00m 39.8s
    Dec(J2000) = -73d 08' 10.8"
with an uncertainty of 1.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 50%.

The mask-weighted light curve begins at T-120 sec, when the source position
came into the BAT field-of-view during a pre-planned slew.  The emission
begins faintly at ~T-25 sec, and rises sharply beginning at ~T-5.5 sec,
peaks at T-4 sec and a stronger peak at ~T+1 sec, returning almost to baseline
around T+10 sec. Then there is a second, much weaker and softer pulse
at around T+15 sec, followed by an even weaker pulse at ~T+70 sec,
with extended emission out to ~T+160 sec.  The burst position left
the FoV after another pre-planned slew at T+780 sec. T90 (15-350 keV) is 60.0 +- 
2.6 sec (estimated error including systematics).

The time-averaged spectrum from -5.7 to +82.0 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.80 +- 0.04.  The fluence in the 15-150 keV band is 1.2 +- 0.0 x 10^-5 erg/cm2.
The 1-sec peak photon flux measured from T+0.56 sec in the 15-150 keV band
is 23.5 +- 0.8 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/586569/BA/

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

The long-duration GRB 140213A
(Swift-BAT trigger 586569: Holland et al., GCN 15825
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 ;
Stamatikos et al., GCN 15836
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 ;
Fermi GBM Detection: Zhang, GCN 15833
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 )
triggered Konus-Wind at T0=69693.011 s UT (19:21:33.011).

The burst light curve shows a bright, double-peaked pulse with
a total duration of ~16 s followed by a weaker emission during
the next ~50 s.
The emission is seen up to ~12 MeV.

The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB140213_T69693/

As observed by Konus-Wind, the burst
had a fluence of (1.57 � 0.09)x10^-5 erg/cm2,
and a 64-ms peak flux, measured from T0+1.344 s,
of (4.10 � 0.40)x10^-6 erg/cm2/s
(both in the 20 keV - 10 MeV energy range).

The time-averaged spectrum (measured from T0 to T0+16.640 s)
is best fit in the 20 keV - 18 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -1.39 � 0.06,
the high energy photon index beta = -3.55 � 0.88,
the peak energy Ep = 100 � 4 keV,
chi2 = 142/97 dof.

The spectrum near the maximum count rate
(measured from T0 to T0+8.448 s)
is best fit in the 20 keV - 18 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.46 � 0.12,
the high energy photon index beta = -3.28 � 0.40,
the peak energy Ep = 108 � 4 keV,
chi2 = 137/97 dof.

Assuming the redshift z=1.2076 (Schulze et al., GCN 15831
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 ),
and a standard cosmology model with H_0 = 70 km/s/Mpc,
Omega_M = 0.27, and Omega_Lambda = 0.73,
we estimate the following rest-frame parameters:
the isotropic energy release E_iso is (6.2 � 0.4)x10^52 erg,
the peak luminosity L_iso is (3.6 � 0.4)x10^52 erg/s,
and the rest-frame peak energy Ep,i = (221 � 8) keV

All errors are given at 1 sigma level.
All the quoted values are preliminary.

A. Trotter, J. Haislip, D. Reichart, A. LaCluyze, A. Verveer, T. Spuck, 
A. Foster, N. Frank, K. Ivarsen, J. Moore, M. Nysewander, R. Beauchemin, 
T. Berger, M. Carroll, H. T. Cromartie, R. Egger, M. Hinckle, A. 
Ireland, M. Maples, L. Scott, and J. A. Crain report:

Skynet continued observing the Swift-BAT localization of GRB 140213A 
(Holland et al., GCN 15825
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 , Swift trigger 586569) with the 14-inch R-COP 
telescope at Perth Observatory, Australia, and with 4 16-inch telescopes 
of the PROMPT array at CTIO, Chile.  Previous observations with R-COP 
began at 59s and continued until 92m post-trigger (Trotter et al., GCN 
15828
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 ). Observations resumed with PROMPT-CTIO at t=5.5h, and continued 
at R-COP and PROMPT-CTIO until t=32h, with a total of ~600x160s new 
exposures in the BVRI bands.

We continue to detect an uncatalogued optical source in all bands at the 
position of the source detected by the Swift UVOT (Siegel & Holland, GCN 
15826
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 ). The source faded from R=14.3 at t=113s to R=17.8 at t=73m, 
bottomed out at R=19.0 at t~6h, and then rebrightened to R=18.6 by 
t=23h.  Flattening or rebrightening of the light curve is observed in 
all four bands.

An updated light curve is at:
http://www.skynet.unc.edu/grb/grb140213a_2.png

Magnitudes are in the Vega system, calibrated to ten APASS-DR7 stars in 
the field, and have not been corrected for the Galactic foreground 
extinction corresponding to E(B-V)=0.07 (Schlegel et al. 1998).

Skynet observations are ongoing.

A. Trotter, J. Haislip, D. Reichart, A. LaCluyze, A. Verveer, T. Spuck, 
A. Foster, N. Frank, K. Ivarsen, J. Moore, M. Nysewander, R. Beauchemin, 
T. Berger, M. Carroll, H. T. Cromartie, R. Egger, M. Hinckle, A. 
Ireland, M. Maples, L. Scott, and J. A. Crain report:

Skynet continued observing the Swift-BAT localization of GRB 140213A 
(Holland et al., GCN 15825
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 , Swift trigger 586569) with the 14-inch R-COP 
telescope at Perth Observatory, Australia, and with four 16-inch 
telescopes of the PROMPT array at CTIO, Chile.  Previous observations 
with R-COP began at 59s and continued until 92m post-trigger (Trotter et 
al., GCN 15828
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 ). Observations resumed with PROMPT-CTIO at t=5.5h, and 
continued at R-COP and PROMPT-CTIO until t=32h, during which time the 
afterglow rebrightened (Trotter et al., GCN 15859
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 ).

R-COP and PROMPT-CTIO took a total of 284x160s exposures in BVRI between 
t~5-5.3d. In stacked images, we continue to detect an uncatalogued 
optical source in R and I bands at the position of the source detected 
by the Swift UVOT (Siegel & Holland, GCN 15826
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 ). After the rebrightening 
at t~1d, the source clearly resumed fading.

Band      tmid       mag
I         5.3d       20.7 (+/-0.2)
R         5.2d       21.3 (+/-0.3)
V         5.3d      >21.7
B         5.3d      >21.6

An updated light curve is at:
http://www.skynet.unc.edu/grb/grb140213a_3.png

Magnitudes are in the Vega system, calibrated to ten APASS-DR7 stars in 
the field, and have not been corrected for the Galactic foreground 
extinction corresponding to E(B-V)=0.07 (Schlegel et al. 1998).

No further Skynet observations are scheduled.