GRB 130122A

L. P. Singer (Caltech), S. B. Cenko (UC Berkeley), and D. A. Brown
(Syracuse) report on behalf of a larger collaboration:

We have imaged the 3-sigma Swift UVOT error circle (P. Evans, GCN
14143
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 ) of GRB130122A (Swift546731, S. Barthelmy, GCN 14140
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 ) with the
Palomar 48 inch Oschin telescope (P48) as part of the Palomar
Transient Factory (PTF).  Images were obtained in the Mould R filter
at 2013-01-23 at 06:27:39 and 07:11:25 UTC, 6.7 and 7.5 hours after
the trigger.

With sporadic cloud cover and a bright moon, we find no point source,
fading or otherwise, to 5-sigma limiting magnitudes of 19.1 and 18.4.

A. Galeev (KFU/AST), I. Khamitov (TUG),
I. Bikmaev, N. Sakhibullin (KFU/AST),
R. Burenin, M. Pavlinsky, R. Sunyaev (IKI),
H. Kirbiyik (TUG), U. Kiziloglu (METU), E. Gogus (Sabanci Uni.)

report:

The field of the optical afterglow of GRB 130122A (Lien et al., GCN 14140
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 )
was observed with Russian-Turkish 1.5-m telescope (RTT150, Bakirlitepe, 
TUBITAK National Observatory, Turkey) in partially cloudy conditions.
Using the TFOSC instrument we obtained BVR images by 300s starting at 
January 23, 02:38:31 UT, i.e. 2.91 hours after the burst. The afterglow is 
clearly detected in all images.

On our images we find the optical transient at the coordinates with 
uncertainty of 0.1 arcsec:
  R.A. (J2000) =  12 57 08.317
  Dec. (J2000) = +59 00 53.62

Using the same USNO-B1 star reported by Sonbas et al. (GCN 14141
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 ) as a 
reference, we estimated the R-magnitudes of the afterglow:

T-T0,  Mag. +/- Mag.err
(hour)
2.95  19.88 +/- 0.13
3.06  20.07 +/- 0.10
3.17  19.94 +/- 0.20
3.28  20.00 +/- 0.09
3.33  19.79 +/- 0.13

The combined image of the field can be found at:
http://hea.iki.rssi.ru/grb/130122a/indexeng.html

This message may be cited.

A. Zauderer and E. Berger (Harvard) report on behalf of the
CARMA Key Project "A Millimeter View of the Transient Universe":

"We observed the position of GRB 130122A (Lien et al.;
GCN 14140
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 ) beginning 2013 Jan 23.47 (dt=0.48 d) with the
Combined Array for Research in Millimeter Astronomy.  At
a mean frequency of 85 GHz with 78 m integration, we do not
detect significant millimeter emission at the Swift/UVOT
position (Breeveld et al.; GCN 14149
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 ) to a 3-sigma limit
of ~0.9 mJy.

We thank the CARMA observatory staff for their support."

A. A. Breeveld (MSSL-UCL) and A. Y. Lien (NASA/GSFC/ORAU) report on behalf
of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 130122A 121 s
after the BAT trigger (Lien et al., GCN Circ. 14140
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 ). A source consistent
with the XRT position reported in (Beardmore et al., GCN Circ. 14143
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 ) is
seen in the initial exposures.

The preliminary UVOT position is:
    RA  (J2000) =  12:57:08.30 = 194.28459 (deg.)
    Dec (J2000) = +59:00:53.5  =  59.01487 (deg.)
with an estimated uncertainty of 0.53 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 finding
chart (FC) and earliest exposures are:

Filter         T_start(s)   T_stop(s)      Exp(s)           Mag

white_FC           121          271          148         18.75 �� 0.09
white              559          579           19         18.57 �� 0.23
v                  609          629           19        >17.9
b                  535          555           19         18.35 �� 0.32
u                  279          529          246         18.49 �� 0.14
uvw1              3974         5610          393        >20.9
uvm2              5205         5404          197        >20.0
uvw2              4795         4995          197        >20.4

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).

A. Volnova (SAI MSU/IKI), V. Linkov (ISON-Kislovodsk),  I. Molotov (KIAM), 
V. Kouprianov (GAO), A. Pozanenko (IKI),  report on behalf of larger 
collaboration:

We observed the field of  GRB 130122A (Lien  et al., GCN 14140
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 ) with 
SANTEL-400AN (0.4-m f/3)  telescope of ISON-Kislovodsk observatory. 
Observations started on  Jan. 22 (UT) 23:44  and we obtained  several 
unfiltered images  of 60 s and 100 s exposures. Initial part of our 
observations were carried under unfavorable weather conditions. Starting on 
Jan.23 (UT) 00:14:14 we clearly detect optical afterglow of GRB 130122A 
(Lien  et al., GCN 14140
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 ; Sonbas et al., GCN 14141
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 ; Gorbovskoy  et al., GCN 
14142
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 ) in single images of 60 s exposure. A  preliminary photometry of 
stacked  images is based  on USNO-B1.0 (R2)  nearby  stars:

T_start,     T0+,       Exp,     Filter,       OT
(UT)          mid (d)   (s)

00:14:14  0.00899  8x60    none      18.0 +/-0.1
00:47:45  0.04474   100     none      18.5 +/- 0.5
01:02:07  0.05579  4x60    none       >17.3

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 (UCSC),
Eleonora Troja (GSFC), Enrico Ramirez‐Ruiz (UCSC), José A. de
Diego (UNAM), Leonid Georgiev (UNAM), Jesús González (UNAM),
Carlos Román-Zúñiga (UNAM), Neil Gehrels (GSFC), and Harvey
Moseley (GSFC) report:

Through intermittent clouds and in poor seeing conditions, we observed the
field of GRB 130122A (Lien, et al., GCN 14140
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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 Astronómico Nacional on Sierra
San Pedro Mártir.  Between 2013 Jan 23.30 to 2013 Jan 23.52 UTC (7.6
to 12.7 hours after the BAT trigger), we obtained approximately 45 minutes
of useful data in the r', i', Z, Y, and J bands.

In comparison with SDSS DR8 and 2MASS, we derive the following detection
and upper limits (3-sigma) in the AB magnitude system for a source
spatially coincident with the UVOT position (GCN 14140
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 ):

 r' >20.7
 i' 21.1 +/- 0.2
 Z  >20.3
 Y  >20.2
 J  >18.2

These magnitudes are not corrected for Galactic extinction in the direction
of the GRB.  Continued observations are planned.

We thank the staff of the Observatorio Astronómico Nacional in San
Pedro Mártir.

S. D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC), J. R. Cummings (GSFC/UMBC),
E. E. Fenimore (LANL), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA),
A. Y. Lien (NASA/GSFC/ORAU), C. B. Markwardt (GSFC), D. M. Palmer (LANL),
A. M. Parsons (GSFC), T. Sakamoto (GSFC/UMBC), G. Sato (ISAS),
M. Stamatikos (OSU), J. Tueller (GSFC), T. N. Ukwatta (GWU)
(i.e. the Swift-BAT team):
 
Using the data set from T-61 to T+242 sec from recent telemetry downlinks,
we report further analysis of BAT GRB 130122A (trigger #546731)
(Lien, et al., GCN Circ. 14140
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 ).  The BAT ground-calculated position is
RA, Dec = 194.307, 59.003 deg, which is 
   RA(J2000)  =  12h 57m 13.8s 
   Dec(J2000) = +59d 00' 09.2" 
with an uncertainty of 3.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 89%.
 
The mask-weighted light curve shows a single roughly FRED-like peak
starting at ~T+0 sec, peaking at ~T+10 sec, and ending at ~T+100 sec.
T90 (15-350 keV) is 64 +- 36 sec (estimated error including systematics).
 
The time-averaged spectrum from T-12.6 to T+67.4 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.34 +- 0.24.  The fluence in the 15-150 keV band is 7.4 +- 1.1 x 10^-7 erg/cm2.
The 1-sec peak photon flux measured from T+10.92 sec in the 15-150 keV band
is 0.4 +- 0.1 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/546731/BA/

V. D'Elia (ASDC), D.N. Burrows (PSU), J.A. Kennea (PSU), M.C. Stroh
(PSU), C. Pagani (U. Leicester), A.P. Beardmore (U. Leicester), P.A.
Evans (U. Leicester), A. Maselli  (INAF-IASFPA), V. Mangano
(INAF-IASFPA) and A.Y. Lien report on behalf of the Swift-XRT team:

We have analysed 9.6 ks of XRT data for GRB 130122A (Lien  et al. GCN
Circ. 14140
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 ),  from 102 s to 29.4 ks after the	BAT trigger. The data
comprise 76 s in Windowed Timing (WT) mode (the first 8 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 Beardmore
et al. (GCN. Circ 14143).

The light curve can be modelled with  a power-law decay with a decay
index of alpha=1.27 (+/-0.04).

A spectrum formed from the PC mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.67 (+0.21, -0.20). The
best-fitting absorption column is  6.3 (+5.3, -4.6) x 10^20 cm^-2, in
excess of the Galactic value of 9.3 x 10^19 cm^-2 (Kalberla et al.
2005). The counts to observed (unabsorbed) 0.3-10 keV flux conversion
factor deduced from this spectrum  is 4.3 x 10^-11 (4.8 x 10^-11) erg
cm^-2 count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:	     6.3 (+5.3, -4.6) x 10^20 cm^-2
Galactic foreground: 9.3 x 10^19 cm^-2
Excess significance: 1.9 sigma
Photon index:	     1.67 (+0.21, -0.20)

If the light curve continues to decay with a power-law decay index of
1.27, the count rate at T+24 hours will be 1.3 x 10^-3 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 5.4 x
10^-14 (6.1 x 10^-14) erg cm^-2 s^-1.

The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00546731.

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

L.P. Xin (NAOC), D. Xu (DARK/NBI), Z.Y. Wu, J.Y. Wei, Y.L. Qiu, T.M.
Zhang, J. Wang, J.S. Deng, C. Wu, X.H. Han (NAOC) report on behalf of
a larger collaboration:

We began to observe the field of GRB 130122A (Lien et.al. GCN 14140
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 )
using the Xinglong 2.16m telescope located in Heibei Province, China
at 18:14:12 UT on 2013-01-23. We obtained 5x300s R-band images in a
poor seeing, with a median time of 19.7 hr after the BAT trigger.

The afterglow is not detected in the stacked image, down to a 3sigma
limit of R~20.2 mag, calibrated with nearby USNO B1 stars.

This message may be cited.

For more information about Xinglong GRBs Follow-up observations,
please visit the website:
http://www.xinglong-naoc.org/grb/

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

Using 488 s of XRT Photon Counting mode data and 1 UVOT
images for GRB 130122A, 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 = 194.28517, +59.01455 which is equivalent
to:

RA (J2000): 12h 57m 8.44s
Dec (J2000): +59d 00' 52.4"

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.

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

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

V.Yurkov, Yu.Sergienko, D.Varda, E.Sinyakov
Blagoveschensk Educational State University, Blagoveschensk

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

V.Krushinski, I.Zalozhnih,  A. Popov
Ural Federal University, Kourovka

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

Claudio Mallamaci, Carlos Lopez and Federico Podest
Observatorio Astronomico Felix Aguilar (OAFA)


MASTER II  robotic telescope (MASTER-Net: http://observ.pereplet.ru) 
located in Kislovodsk was pointed to the  GRB130122A  28 sec s after 
notice time and 91 sec after GRB time at 2013-01-22 23:45:40 UT in two 
polarizations.
The weather conditions were not very good and continuosly deteriorated. 
On our first (20s exposure) double set we marginally find an optical 
transient at the Swift UVOT position (Lien et al., GCN 14140
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 ) with 
unfiltered magnitude 16.8+-0.3 (m = 0.8R + 0.2B from USNO-B).

This message may be cited.

E. Sonbas (Adiyaman Univ.), T. Guver (Sabanci Univ.), O. Uysal
(Akdeniz Univ./TUG), E. Gogus (Sabanci Univ.), H. Kirbiyik (TUG) report on
behalf of a larger collaboration

We observed the field of Swift GRB 130122A (Lien et al. GCN#14140
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 )
with the 1.0 meter T100 telescope (TUBITAK National Observatory,
Antalya - Turkey), starting January, 23, 00:50 UT (~ 1 hour after
the trigger). Observations were carried out in the R filter
under moderate weather conditions. The afterglow is clearly detected in
stacked (4x300s) R band images and consistent with UVOT coordinates
reported by Lien et al. GCN#14140
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 .

There is ~10 arcsec offset between afterglow candidate and SDSS
J125709.02+590053.1
and USNO-B1 1490-0209231 (RA= 12:57:09.00, Dec = +59:00:53.35) objects.
Using USNO-B1 star USNO-B1 1490-0209196 (RA= 12:56:56.61, Dec= +59:02:39.11)
in the field magnitude of the OT were estimated 20.8 +/- 0.2.

We are grateful to the TUBITAK National Observatory staff for promptly
scheduling the observations and their technical support.

A. Y. Lien (NASA/GSFC/ORAU), S. D. Barthelmy (GSFC),
W. H. Baumgartner (GSFC/UMBC), A. P. Beardmore (U Leicester),
N. Gehrels (NASA/GSFC), K. L. Page (U Leicester), D. M. Palmer (LANL),
T. Sakamoto (AGU), B. Sbarufatti (INAF-OAB/PSU), M. H. Siegel (PSU)
and E. Troja (NASA/GSFC/UMCP) report on behalf of the Swift Team:

At 23:44:09 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130122A (trigger=546731).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 194.218, +59.015 which is 
   RA(J2000)  =  12h 56m 52s
   Dec(J2000) = +59d 00' 55"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve shows a single peak
with a duration of about 30 sec.  The peak count rate
was ~1000 counts/sec (15-350 keV), at ~1 sec after the trigger. 

The XRT began observing the field at 23:46:06.3 UT, 116.9 seconds after
the BAT trigger. Using promptly downlinked data we find a fading,
uncatalogued X-ray source located at RA, Dec 194.28337, 59.01331 which
is equivalent to:
   RA(J2000)  = 12h 57m 08.01s
   Dec(J2000) = +59d 00' 47.9"
with an uncertainty of 3.6 arcseconds (radius, 90% containment). This
location is 121 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 consistent with the Galactic value of 9.34
x 10^19 cm^-2 (Kalberla et al. 2005). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 121 seconds after the BAT trigger. There is a candidate afterglow in
the list of sources generated on-board at
  RA(J2000)  =	12:57:08.34 = 194.28476
  DEC(J2000) = +59:00:53.9  =  59.01496
with a 90%-confidence error radius of about 1.10 arc sec. This position is 6.2
arc sec. from the center of the XRT error circle. The estimated magnitude is
18.95. No correction has been made for the expected extinction corresponding to
E(B-V) of 0.01. 

Burst Advocate for this burst is A. Y. Lien (yarleen AT gmail.com). 
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.)