GRB 130606A

T. N. Ukwatta (MSU), S. D. Barthelmy (GSFC), N. Gehrels (NASA/GSFC),
H. A. Krimm (CRESST/GSFC/USRA), D. Malesani (DARK/NBI),
F. E. Marshall (NASA/GSFC), A. Maselli (INAF-IASFPA),
A. Melandri (INAF-OAB), D. M. Palmer (LANL) and
M. Stamatikos (OSU/NASA/GSFC) report on behalf of the Swift Team:

At 21:04:39 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130606A (trigger=557589).  Swift slewed immediately to the burst. 
The BAT on-board calculated location is 
RA, Dec 249.403, +29.791 which is 
   RA(J2000) = 16h 37m 37s
   Dec(J2000) = +29d 47' 27"
with an uncertainty of 3 arcmin (radius, 90% containment, including 
systematic uncertainty).  The BAT light curve showed a double-peaked
structure.  The initial peak is about 10 sec long from T-5 to T+5 sec. 
Then at T+150 sec, there is a second, brighter peak of about 20 sec
duration. The peak count rate was ~2300 counts/sec (15-350 keV), 
at ~155 sec after the trigger. 

The XRT began observing the field at 21:05:51.4 UT, 72.4 seconds after
the BAT trigger. Using promptly downlinked data we find a bright,
fading, uncatalogued X-ray source located at RA, Dec 249.39916,
29.79428 which is equivalent to:
   RA(J2000)  = 16h 37m 35.80s
   Dec(J2000) = +29d 47' 39.4"
with an uncertainty of 3.6 arcseconds (radius, 90% containment). This
location is 16 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 (1.98 x
10^20 cm^-2, Kalberla et al. 2005), with an excess column of 3.3
(+1.76/-1.58) x 10^21 cm^-2 (90% confidence). 

The initial flux in the 2.5 s image was 1.64e-09 erg cm^-2 s^-1 (0.2-10
keV). 

UVOT took a finding chart exposure of 150 seconds with the White filter
starting 80 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, but the trailed images will reduce the sensitivity slightly. 
No correction has been made for the expected extinction corresponding 
to E(B-V) of 0.02. 

The UVOT data shows stars trailing by about 10 arcseconds, which
may indicate pointing instability at this level.  Therefore
this uncertainty should be added to the nominal XRT location
for follow-up searches.  A refined aspect solution will be
generated from the full downlinked data. 

Burst Advocate for this burst is T. N. Ukwatta (tilan.ukwatta 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.)

M. Jelinek (IAA-CSIC), J. Gorosabel (UPV-EY, IAA-CSIC), A. J.
Castro-Tirado (IAA-CSIC),  S. Mottola (DLR), S. Hellmich (DLR), R.
Fern�ndez-Mu�oz (EELM-CSIC) and V. F. Mu�oz-Mart�nez (UMA), on behalf of a
larger collaboration, report:

"Following the detection of GRB 130606 by Swift (Ukwatta et al. GCNC
14781), follow-up observation were taken with the 0.6m TELMA telescope at
the BOOTES-2 station (M�laga) and with the 1.23m CAHA telescope at the
German-Spanish Calar Alto Observatory, starting 21m postburst. At the edge
of the Swift/XRT error box we identify an optical source not present in
the DSS-2 with a magnitude of R about 18.5 which we identify as the
optical afterglow."

[GCN OPS NOTE(06jun13): Per author's request, the GRB name in the Title was corrected.]

D. Xu (DARK/NBI), D. Malesani (DARK/NBI), S. Schulze (PUC and MCSS),
N. R Tanvir (U. Leicester), D. J. Watson (DARK/NBI), J. Hjorth
(DARK/NBI), J. Datson (Tuorla Observatory, U. Turku), R. Salinas
(FINCA) report on behalf of a larger collaboration:

We observed the field of GRB 130606A (Ukwatta et al., GCN 14781
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 ) using
the 2.5m Nordic Optical Telescope (NOT) equipped with the MOSCA
imager. Observations started at 21:35 UT on 2013-06-06 (i.e., 0.5 hr
after the burst) and 2x300 s frames were obtained in the Sloan
r-filter.

Close to the refined XRT position, we detect an object not visible in
the DSS and SDSS images of the field, at the following coordinates:

RA (J2000) = 16:37:35.188
Dec(J2000) = +29:47:47.03

These coordinates are formally outside the XRT error circle, which is
however affected by extra systematic uncertainties due to the problems
in the satellite attitude (Ukwatta et al., GCN 14781
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 ). The object has
m(r) = 20.8, calibrated against the SDSS.

We suggest this object is the afterglow of GRB 130606A. It is probably
the same object reported by Jelinek et al. (GCN 14782
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 ).

Takahiro Nagayama (Nagoya Univ) on behalf of OISTER collaboration.

We observed the field of GRB 130606A (Ukwatta et al, GCN Circular
14781
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 ) with the Infrared Survey Facility 1.4m telescope and
NIR camera SIRIUS at Sutherland Observatory in South Africa.

The observation was started with the JHKs bands simultaneously
from 2013-06-06 21:38 (UT).

We have detected a bright source not detected in 2MASS ALL SKY survey
at RA=16:37:35.14 DEC=+29:47:46.4 (J2000) from the first 300sec
exposure image.

Preliminary photometry results are as follows
J=13.1
H=13.9
Ks=14.7

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

F.J. Virgili, C.G. Mundell (LJMU), A. Melandri (INAF-OAB), and A. Gomboc (U. Ljubljana)
report:

"The 2-m Liverpool Telescope robotically followed up GRB 130606A
(SWIFT trigger 557589; Ukwatta et al., GCN 14781
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 ) 38.52 min after the 
GRB trigger time.
We detect a fading source in i' and z' bands consistent with the 
position reported by Xu et al. (GCN 14783
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 ) with magnitudes

Filter        Magnitude                t since trigger (min)
i'            18.60 +/- 0.02            45.02
i'            18.67 +/- 0.02            55.48
i'            18.89 +/- 0.03             83.00

z'            16.65 +/- 0.02                47.74
z'            16.80 +/- 0.03                61.47

Magnitudes are calibrate against SDSS catalogued field stars.
Observations and analysis are ongoing.

[GCN OPS NOTE(10jun13): Per author's request, AG was added to the author list.]

G. Masi (Ceccano, Italy) and F. Nocentini (Frosinone, Italy) report:

On June 6.96456 2013 UT, we imaged the field around GRB 130606A (Ukwatta et al. 
(GCN 14781
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 ) remotely using the the 0.43m-f/6.8 robotic unit part of the Virtual 
Telescope robotic facility in Italy, 124 minutes after the burst.

4, 300 seconds unfiltered CCD images were coadded and show an object at the 
following coordinates (J2000.0):

R.A. = 16 37 35.13
Decl. +29 47 46.7

We also performed photometry, assuming R-mags from UCAC-4 for the stars in the 
field, getting an estimate for the magnitude of 19.6 (CR).

A. J. Castro-Tirado, R. Sánchez-Ramírez, M. Jelinek (IAA-CSIC), J.
Gorosabel (EHU-UPV), J. C. Tello, P. Ferrero, O. Lara-Gil, R. Cunniffe
(IAA-CSIC), D. Pérez-Ramírez (U. Jaén), P. Kubanek (FZU), J. M. Castro
Cerón (ESAC), A. Fernández-Soto (UV), S. Mottola (DLR), S. Hellmich (DLR),
R. Fernández-Muñoz (EELM-CSIC), V. F. Muñoz-Martínez (UMA), J. Cepa (IAC)
and C. Álvarez-Iglesias (GTC), on behalf of a larger collaboration,
report:

"Following the detection of the optical afterglow (Jelinek et al. GCNC
14782, Xu et al. GCNC 14783) to GRB 130606A ((Ukwatta et al. GCNC
14781), we have obtained an optical spectrum with the 10.4 m GTC (+OSIRIS)
starting aprox. 1.5 hr postburst, covering the 4000-10000 wavelength
range. The continuum is detected only redwards of aprox. 6500 A, with
multiple absorption lines which are indicative of the Lyman forest.
Therefore we infer a (preliminary) redshift of z = 6.1 (to be refined).
This is consistent with the dropout in the optical band (Virgili et al.
GCNC 14785) and the bright nIR afterglow (Nagayama et al. GCNC 14784).
Observations at all wavelengths are encouraged."

Simone Leonini, G. Guerrini, P. Rosi and L.M. Tinjaca Ramirez (Montarrenti 
Observatory, Siena, Italy) report:

We observed the field of GRB 130606A (Swift trigger 557589, Ukwatta et al., 
GCN 14781
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 ) with the automatic 0.53m RC telescope + U47 detector 
at Montarrenti Observatory (Siena, Italy, IAU code C88).

The observations was started at 2013-06-06 22:57:50 UT (~117 minutes after the 
trigger) and we co-added 4 unfiltered CCD exposures of 60s each.

We detect a new source of mag. R=18.9 +/-0.16 (USNO-B1 catalogue, not 
corrected for galactic dust extinction) at the following position:

RA    (J2000.0)  16h 37m 35.13s +/-0.19
Decl. (J2000.0) +29�� 47' 46.9"  +/-0.18

The message may be cited.

Takahiro Nagayama (Nagoya Univ) on behalf of OISTER collaboration.

In the circular 14784, submited by us, the J and Ks magnitudes
are swapped by mistake.

J=14.7
H=13.9
Ks=14.7
are correct.

Takahiro Nagayama (Nagoya Univ) on behalf of OISTER collaboration.

In the circular 14784, submited by us, the J and Ks magnitudes
are swapped by mistake.

J=14.7
H=13.9
Ks=13.1
are correct.

Takahiro Nagayama (Nagoya Univ) on behalf of OISTER collaboration.

In the circular 14792, submited by us, the Ks magnitude is correct.
The circular 14793 are correct.

We apologize for the possible inconvenience.

A. J. Castro-Tirado, R. Sánchez-Ramírez (IAA-CSIC), J. Gorosabel (EHU-UPV,
IAA-CSIC), M. Jelinek, J. C. Tello, P. Ferrero, O. Lara-Gil, R. Cunniffe
(IAA-CSIC), D. Pérez-Ramírez (U. Jaén), S. Guziy (Nikolaev Univ.), P. Kubanek (FZU),
J. M. Castro Cerón (ESAC), A. Fernández-Soto (UV), S. Mottola (DLR), S. Hellmich (DLR),
R. Fernández-Muñoz (EELM-CSIC), V. F. Muñoz-Martínez (UMA), L.
Sabau-Graziati (INTA), A. Martín-Carrillo (UCD), J. Cepa (IAC), A. Tejero
and C. Álvarez-Iglesias (GTC), on behalf of a larger collaboration,
report:

"A detailed analysis of our 10.4m GTC spectrum reported on GCNC 14790
reveals several absorption metallic lines (N V, Si II and Si IV amongst
others) at a common redshift of z = 5.91 which we propose to be the
redshift of GRB 130606A."

[GCN OPS NOTE(10jun13): Per author's request, SG was added to the author list.]

E. Sonbas (Adiyaman Univ.), H. Avdan (Cukurova Univ.), T. Guver (Sabanci
Univ.), M. Kaplan (Akdeniz Univ.), M. Kocak (TUG), E. Gogus (Sabanci
Univ.),
H. Kirbiyik (TUG) report on behalf of a larger collaboration

We observed the field of Swift  GRB 130606A (Ukwatta et al. GCN#14781
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 )
with  the  1.0 meter  T100  telescope  (TUBITAK National  Observatory,
Antalya - Turkey),  starting June, 6,  22:43:53 UT (~ 1.6 hours after
the trigger). Observations were carried out in the R filter under moderate
weather conditions. We detected a new source in 300 s R band
image at a position that is consistent with Xu et al. GCN#14783
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Using USNO-B1 star USNO-B1 1198-0251348  (RA=  16:37:32.14 , Dec=
+29:51:58.15 ) in the field, the magnitude of the OT were estimated as 20.6
+/-0.2.

Further observations using the same filter are ongoing.

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

R. Lunnan, M. Drout, R. Chornock, and E. Berger (Harvard) report:

We observed the optical afterglow (Jelinek et al., GNC 14782; Xu et al., GCN 
14783
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 ; Nagayama et al., GCN 14784
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 ; Virgili et al., 14785; Masi et al., GCN 
14789
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 ; Leonini et al., GCN 14791
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 ; Sonbas et al., GCN 14797
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 ) of GRB 130606A 
(Ukwatta et al., GCN 14781
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 ) using the Blue Channel spectrograph on the 6.5-m MMT 
starting at 04:04 UT on 7 June (7.0 hours after the BAT trigger).  We obtained 
4x1200s of spectroscopy spanning the wavelength range 7450-9350 Angs with a 
resolution of 2.1 Angstroms.

We detect a sharp cutoff in flux blueward of ~8425 Angs, consistent with 
Lyman-alpha at a redshift of z=5.9, with very little transmission between 7850 
and 8400 Angs, although some flux is present blueward of that.  Several metal 
absorption lines are present to the red, including NV, Si II, C II, and O I at 
redshift z=5.913, confirming the GTC redshift of Castro-Tirado et al. (GCN 
14790
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 , GCN 14796
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 ).

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), Owen Littlejohns (ASU), 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:

We observed the field of GRB 130606A (Ukwatta, et al., GCN 14781
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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 from 2013/06 7.19 to 2013/06 7.20 UTC (7.38 to 7.79
hours after the BAT trigger), obtaining a total of 0.36 hours exposure in
the r' and i' bands and 0.15 hours exposure in the Z, Y, J, and H bands.

The optical/NIR afterglow (Jelinek, et al., GCN 14782
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 ; Xu et al., GCN
14783
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 ) is quite red and clearly detected in all bands but r'.  In
comparison with SDSS DR9 and 2MASS, we obtain the following detections and
3-sigma upper limit:

r' > 23.02
i' 21.16 +/- 0.06
Z  18.79 +/- 0.03
Y  18.40 +/- 0.03
J  18.32 +/- 0.03
H  17.92 +/- 0.03

These magnitudes are in the AB system and not corrected for Galactic
extinction in the direction of the GRB.  The lack of detection in r' and
relatively faint flux level in i' are consistent with the high-redshift
determined from spectroscopy (Castro-Tirado, et al., GCN 14790
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 , 14796
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 ;
Lunnan, et al., GCN 14798
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 ).

We thank the staff of the Observatorio Astronómico Nacional in San Pedro
Mártir.  Further observations are planned.

M. Im (CEOU/SNU), H.-I. Sung(KASI), and Y. Urata (NCU) 
on behalf of EAFON

We observed the afterglow of GRB 130606A (Ukwatta et al. GCN 14781
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 ),
using a 1-m telescope at Mt. Lemmon Optical Observatory (LOAO) in
Arizona, US. The observation started at 2013-06-07 03:50:26 UT,
about 6.75 hrs after the burst alert, and a series of images were 
taken in I, Z, and Y-bands for about 1 hr.

We identify the afterglow, in all the three bands,
with approximate magnitudes of I = 20.8 +- 0.1, Z=18.70 +- 0.11,
and Y=18.49 +- 0.29, all in AB magnitude, calibrated against a star
in vicinity using SDSS and 2MASS photometry. This confirms 
earlier reports of the afterglow detection and its sharp drop in
SED between I-band and Z-band that is expected at z=5.91 
(Jelinek et al. GNC 14782; Xu et al.GCN 14783; Nagayama et al. GCN 14784
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 ; 
Virgili et al. 14785; Masi et al. GCN 14789
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 ; Leonini et al. GCN 14791
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 ; 
Sonbas et al., GCN 14797
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 ; Lunnan et al. GCN 14798
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 ; Castro-Tirado et al. 
GCN 14790
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 ; Butler et al. GCN 14799
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 ).

We thank the LOAO operator, Jae-Hyuk Yoon for performing 
the observation.

A. N. Morgan (UC Berkeley) reports:

We observed the field of GRB 130606A (Ukwatta, et al., GCN 14781
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 ) with the
1.3m PAIRITEL located at Mt. Hopkins, Arizona. Observations began at
2013-Jun-07 06h01m22s UT, ~8.9 hours after the Swift Trigger.  In  mosaics
(effective exposure time of ~36.3 minutes) taken simultaneously in the J,
H, and Ks filters, we detect the optical afterglow (e.g. Jelinek, et al.,
GCN 14782
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 ; Xu et al., GCN 14783
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 ; Nagayama et al., GCN 14784
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 ).

The preliminary photometry yields:

post burst
t_mid (hr) exp.(m)  filt  mag   m_err
9.44       36.3     J     17.83  0.06
9.44       36.3     H     17.06  0.07
9.44       36.3     Ks    16.4   0.1

Observations are ongoing. All magnitudes are given in the Vega system,
calibrated to 2MASS. No correction for Galactic extinction has been made to
the above reported values.

D. A. Perley (Caltech) and S. B. Cenko (GSFC) report on behalf of a 
larger collaboration:

We imaged the field of GRB 130606A (Ukwatta et al., GCN 14781
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 ) with the 
robotic Palomar 60-inch telescope throughout the night of 2013-06-07 UT, 
beginning at 04:01 UT and continuing until morning twilight at 11:39 UT. 
  Initial observations consisted of a series of r, i, and z-band frames; 
later in the night we switched to exclusively z-band observations. 
Transparency and seeing conditions were good throughout.

The GRB afterglow (Jelinek et al., GCN 14782
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 ; Xu et al., GCN 14783
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 ; 
Nagayama et al., GCN 14784
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 ) is well-detected in the z-band exposures and 
marginally detected in the other filters.  Preliminary (not 
fringe-corrected) aperture photometry of a few select points yields:

t_start(d)  t_exp(s) filter  magnitude
  0.30679     180     z = 18.62 +/- 0.08
  0.42224     180     z = 19.22 +/- 0.09
  0.50888     180     z = 19.59 +/- 0.11
  0.58040     180     z = 19.73 +/- 0.22

The afterglow decays as a power-law with an index of approximately 
alpha=1.6-1.7 over the course of the observations.

Given the redshift (Castro-Tirado et al., GCN 14796
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 ; Lunnan et al., GCN 
14798
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 ) these relatively bright fluxes indicate an extremely luminous 
afterglow, especially at early times; similar to the luminous 
high-redshift GRB 050904 (e.g. Kann, Masetti, & Klose 2007; AJ 133:1187).

A. Volnova (IKI), R.Inasaridze (AAO), O. Kvaratskhelia (AAO), V. 
Ayvazian(AAO), Yu. Krugly (IA KhNU),  I. Molotov (KIAM), A. Pozanenko 
(IKI)  report on behalf of  larger GRB follow-up collaboration:

We observed the field of the Swift Swift GRB 130606A (Ukwatta et al., 
GCN 14781
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 )with AS-32 (0.7m) telescope of Abastumani Observatory, 
starting on Jun. 06 (UT) 21:47:43. We obtained several unfiltered images 
of 180 s exposure. The afterglow (Jelinek et al., GCN 14782
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 ; Xu et al., 
GCN 14783
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 ; Nagayama et al., GCN 14784
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 ) is well detected in  separate 
images. Preliminary photometry

T_start,   Exp,  T-t0, d    OT +/- err
  UT        s     mid, days
21:47:43   180   0.03095    18.84 +/- 0.05
21:51:24   180   0.03351    18.86 +/- 0.04
21:55:04   180   0.03605    18.95 +/- 0.05
21:58:45 2x180   0.03988    19.16 +/- 0.06

is based on SDSS stars R mag, where R mag obtained via transformations 
ugriz in BVRI (Lupton, 2005):

SDSS                 u     g       r     i      z       R
J163722.96+294541.6 16.747 15.352 14.827 14.598 14.568  14.625
J163734.99+294356.8 18.166 17.023 16.665 16.540 16.503  16.493

P. Afonso (American River College), D. A. Kann, A. Nicuesa Guelbenzu (both
TLS Tautenburg), T. Kruehler (DARK), J. Elliott, and J. Greiner (both MPE
Garching) report on behalf of the GROND team:

We observed the field of GRB 130606A (Swift trigger 557589; Ukwatta et
al., GCN #14781
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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/ESO telescope at La Silla
Observatory (Chile).

Observations started at 03:30 UT on 7th June 2013, 6.4 hours after the GRB
trigger. They were performed at an average seeing of 1.1" and at an
average airmass of 2.0.

We detect the afterglow (Jelinek et al.; GCN #14782
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 ) at the position of Xu
et al. (GCN #14783
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 ), and based on images taken at a mid-time of 05:00 UT,
with total exposures of 7.66 minutes in g'r'i'z' and 8 minutes in JHK, we
estimate preliminary magnitudes (all in AB) of

g' > 24.3 mag,
r' = 23.4 +/- 0.2 mag,
i' = 21.4 +/- 0.1 mag,
z' = 18.8 +/- 0.1 mag,
J = 18.4 +/- 0.1 mag,
H = 18.1 +/- 0.1 mag, and
K = 17.8 +/- 0.2 mag.

The spectral energy distribution is best fit with a small amount of
LMC-like dust and a spectral slope of beta ~ 0.7.

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)=0.024 mag in the
direction of the burst (Schlegel et al. 1998).

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

The long GRB 130606A (Swift-BAT trigger #557589: Ukwatta et al., GCN
14781
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 ) was detected by Konus-Wind in the waiting mode.

The burst light curve shows a weak initial pulse followed in ~150 s by a 
much brighter peak.

As observed by Konus-Wind, the burst had a fluence of (4.4 +/- 
0.8)x10^-6 erg/cm2 (in the 20 - 1300 keV energy range).

Modeling the K-W 3-channel time-integrated spectrum (from T0(BAT)+153 s 
to T0(BAT)+165 s) by a power law with exponential cutoff model:
dN/dE ~ (E^alpha)*exp(-E*(2+alpha)/Ep)
yields alpha = -1.14 +/- 0.15, and Ep = 294(-50,+90) keV.

Assuming z = 5.91 (Castro-Tirado et al., GCN 14796
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 ; Chornock et al. GCN 
14798
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 ) and a standard cosmology model with H_0 = 71 km/s/Mpc, Omega_M = 
0.27, Omega_Lambda = 0.73, the isotropic energy release is E_iso =
(2.83 +/- 0.52)x10^53 erg in 1 keV to 10 MeV at the GRB rest frame
extrapolating the best exponential cutoff function fit.

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

The K-W light curve of this burst is available at
http://www.ioffe.rssi.ru/LEA/GRBs/GRB130606A/

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

Using 3364 s of XRT Photon Counting mode data and 8 UVOT
images for GRB 130606A, 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 = 249.39633, +29.79622 which is equivalent
to:

RA (J2000): 16h 37m 35.12s
Dec (J2000): +29d 47' 46.4"

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.

D.N. Burrows (PSU), B.P. Gompertz (U. Leicester), J.P. Osborne (U.
Leicester), K.L. Page (U. Leicester), V. D'Elia (ASDC), A. Maselli 
(INAF-IASFPA), V. Mangano (INAF-IASFPA), J.A. Kennea (PSU), M.C. Stroh
(PSU) and T.N. Ukwatta report on behalf of the Swift-XRT team:

We have analysed 7.6 ks of XRT data for GRB 130606A (Ukwatta  et al.
GCN Circ. 14781
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 ),  from 62 s to 58.7 ks after the  BAT trigger. The
data comprise 499 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
Osborne et al. (GCN. Circ 14811).

The late-time light curve (from T0+5.3 ks) can be modelled with  a
power-law decay with a decay index of alpha=1.13 (+0.10, -0.09).

A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index	of 1.55 (+/-0.04). The
best-fitting absorption column is  8.4 (+/-1.0) x 10^20 cm^-2, in
excess of the Galactic value of 2.0 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 1.84 (+0.15, -0.14)
and a best-fitting absorption column of 4.5 (+3.1, -2.5) x 10^20 cm^-2.
The counts to observed (unabsorbed) 0.3-10 keV flux conversion factor
deduced from this spectrum  is 3.8 x 10^-11 (4.2 x 10^-11) erg cm^-2
count^-1. 

A summary of the PC-mode spectrum is thus:
Total column:	     4.5 (+3.1, -2.5) x 10^20 cm^-2
Galactic foreground: 2.0 x 10^20 cm^-2
Excess significance: <1.6 sigma
Photon index:	     1.84 (+0.15, -0.14)

If the light curve continues to decay with a power-law decay index of
1.13, the count rate at T+24 hours will be 0.011 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 4.3 x
10^-13 (4.8 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/00557589.

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

T. A. Pritchard (PSU) and T. N. Ukwatta (MSU)
report on behalf of the Swift/UVOT team:

The Swift/UVOT began settled observations of the field of GRB 130606A
84 s after the BAT trigger (Ukwatta et al., GCN Circ. 14781
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 ).
No optical afterglow consistent with the optical position
(Xu et al., GCN Circ 15783
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 ) is detected in the initial UVOT exposures.
Aspect correction was lost in a number of sub-exposures resulting in
image streaks, rough aspect corrections and larger apertures have been
used to calibrate the field, although with a lower sensitivity.
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            84          231          144         >21.1
u_FC               293          543          246         >20.3
white               84         6539          361         >22.1
v                 5314        12245         1148         >20.6
b                  549         6334          236         >20.7
u                  293        18354          561         >20.4
w1                 672        18247         1102         >21.1
m2                5519        15930          625         >20.5
w2                1028         6744          216         >20.1

The magnitudes in the table are not corrected for the Galactic extinction
due to the reddening of E(B-V) = 0.02 in the direction of the burst
(Schlegel et al. 1998).

A. Trotter, A. LaCluyze, D. Reichart, J. Haislip, T. Berger, M. Carroll,
H. T. Cromartie, R. Egger, A. Foster, C. Foster, N. Frank, K. Ivarsen,
D. James, M. Maples, J. Moore, M. Nysewander, E. Speckhard, P. Taylor
and J. A. Crain report:

Skynet observed field of GRB 130606A (Ukwatta et al., GCN 14781
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 , Swift
trigger #557589), using the optical localization of Xu et al. (GCN
14783
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 ).  It took ~150 160-second exposures in each of the g', R and z'
bands with three 16" telescopes of the PROMPT array at CTIO, Chile,
starting at 2013-06-07, 00:47 UT (t=3.75h post-trigger), and continuing
until t=9.7h.

We detect a fading afterglow in the z' band in most individual
exposures, with z~18.5 at t~6.3h, and an approximate temporal index
alpha~-1.4.   We do not detect the afterglow in the R or g' bands in
individual exposures, consistent with the spectroscopic redshift z=5.91
reported by Castro-Tirado et al. (GCN 14796
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 ).  Stacks of ~70 160-second
exposures at a mean time t~5.7h yield a questionable R~21.9 detection
and a 3-sigma upper limit g'>23.7.  Similar stacks at t~8.5h yield
3-sigma upper limits R>22.7 and g'>23.6.  A preliminary light curve is at:

http://www.skynet.unc.edu/grb/grb130606a.png

Photometry is calibrated to 10 SDSS stars in the field; g' and z'  
magnitudes are in the AB system; R-band magnitudes are in the Vega
system, with the SDSS calibration stars transformed according to Jester
(2005).  No correction has been applied for the expected line-of-sight
Milky Way extinction of E(B-V)=0.02 (Schlegel et al. 1998).

Further Skynet observations are scheduled.

D. Xu (DARK/NBI), D. Malesani (DARK/NBI), S. Schulze (PUC and MCSS),
J. P. U. Fynbo (DARK/NBI), Valerio D'Elia (ASI-SDC, INAF OAR), P.
Goldoni (APC/Univ. Paris 7 and SAp/CEA), O. Hartoog (Amsterdam), J.
Hjorth (DARK/NBI), L. Kaper (Amsterdam), T. Kruehler (DARK/NBI), A. J.
Levan (U. Warwick), B. Milvang-Jensen (DARK/NBI), N. R. Tanvir (U.
Leicester), K. Wiersema (U. Leicester) report on behalf of the
X-shooter GRB GTO collaboration:

We observed the optical afterglow of GRB 130606A (Ukwatta et al., GCN
14781
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 ; Jelinek et al., GCN 14782
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 ; Xu et al., GCN 14783
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 ) using the ESO
VLT equipped with the X-shooter spectrograph. The observations started
on 2013-06-07 at 04:09 UT (i.e., 7.08 hr after the burst). A total
exposure of 6x600 s was obtained, covering the spectral range from
~3000 to ~21000 A.

A continuum is detected redward of ~8410 A in the VIS/NIR arms of the
spectra, consistent with a Lyman alpha dropout at z~5.9, while
discrete transmission is present blueward down to ~6505 A. In the
spectra prominent absorption lines are detected, such as NV, C II, O
I, Si IV, C IV, and Si II, all at a common redshift of z=5.913, fully
consistent with the measurements in Castro-Tirado et al. (GCN 14796
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 )
and Lunnan et al. (GCN 14798
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 ). We also identified at least two
intervening absorbers at z=3.451 and at z=2.310 through Mg II and Fe
II, respectively.

We thank the Paranal staff for enthusiastic support, in particular
Cedric Ledoux and Felipe Gaete.

T. Laskar, A. Zauderer, and E. Berger (Harvard) report:

"We observed the position of GRB 130606A (Ukwatta et al; GCN 14781
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 ) with
the EVLA beginning on 2013 June 07.30 UT (0.59 days after the burst). At a
mean frequency of 21.8 GHz, we detect a radio source with a preliminary
flux density of ~ 0.1 mJy at

RA = 16:37:35.134 +/- 0.004
Dec = 29:47:46.47 +/- 0.06,

consistent with the enhanced Swft/XRT position (Burrows et al.; GCN 14812
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 ),
the NIR position (Xu et al.; GCN 14783
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 , Nagayama et al.; GCN 14784
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 ), and
the optical position (Masi and Nocentini; GCN 13891
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 , Leonini et al.; GCN
14791
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 ). Follow-up observations are planned."

Klotz A. (IRAP-CNRS-OMP), Gendre B. (IRAP-CNRS-OMP),
Boer M., Siellez K., Dereli H., Bardho O. (UNS-CNRS-OCA),
Atteia J.L. (IRAP-CNRS-OMP) report:

We imaged the field of GRB 130606A detected by SWIFT
(trigger 557589) with the TAROT robotic telescope (D=25cm)
located at the Calern observatory, France.

The observations started 7.1 min after the GRB trigger
The elevation of the field increased from
63 degrees above horizon and weather conditions
were good.

We detect the optical transient (OT) discovered by
Jelinek et al. (GCNC 14782). TAROT images are unfiltered.
The redshift 5.9 means the OT should emit mainly in the I band.
At the present level of analysis we can not give the
flux of the OT refered in the I band.

We choose the zero point of magnitudes using
the star NOMAD-1 1197-0254828 (R=16.43). We refer the TAROT
magnitudes to the R magnitude of the reference star
(we use CR as the symbol of the clear filtered image
calibrated with the R magnitude of the reference star).

At 7.85 minutes after the GRB, CR=17.1

The OT is measured continuously until 141 minutes
with a mean decay of 0.9.

This message may be cited.

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), T. Sakamoto (AGU), G. Sato (ISAS),
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 the recent telemetry
downlink,
we report further analysis of BAT GRB 130606A (trigger #557589)
(Ukwatta, et al., GCN Circ. 14781
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 ).  The BAT ground-calculated position is
RA, Dec = 249.390, 29.796 deg which is
   RA(J2000)  =  16h 37m 33.6s
   Dec(J2000) = +29d 47' 44.5"
with an uncertainty of 2.0 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 96%.

The mask-weighted light curve shows multiple peaks. The first peak starts
around T-5 secs and last for 15 seconds, a cluster of weak peaks can be seen
from T+80 sec to T+110 sec, bright two peak structure is seen from T+150 sec
to T+ 170 sec, finally very weak extended multi-peak structure is observed
beyond
T+200 sec up to T+500 sec. T90 (15-350 keV) is 276.58 +- 19.31 sec
(estimated error including systematics).

The time-averaged spectrum from T-1.34 to T+297 sec is best fit by a simple
power-law model.  The power law index of the time-averaged spectrum is
1.52 +- 0.12.  The fluence in the 15-150 keV band is 2.9 +- 0.2 x 10^-6
erg/cm2.
The 1-sec peak photon flux measured from T+160.36 sec in the 15-150 keV band
is 2.6 +- 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/557589/BA/

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), Owen Littlejohns (ASU), 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:

We observed the field of GRB 130606A (Ukwatta, et al., GCN 14781
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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 from 2013/06 8.18 to 2013/06 8.46 UTC (31.14 to
37.86 hours after the BAT trigger), obtaining a total of 4.96 hours
exposure in the r' and i' bands and 2.07 hours exposure in the Z, Y, J, and
H bands.

The optical/NIR afterglow (Jelinek, et al., GCN 14782
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 ; Xu et al., GCN
14783
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 ) is well detected.   In comparison with SDSS DR9 and 2MASS, we obtain
the following detections and 3-sigma upper limit:

 r'  >24.06
 i'  24.06 +/- 0.27
 Z   21.50 +/- 0.09
 Y   21.41 +/- 0.12
 J   21.16 +/- 0.12
 H   20.78 +/- 0.12

These magnitudes are in the AB system and not corrected for Galactic
extinction in the direction of the GRB.  In comparison to our observations
on the previous night (2013/06/07; Butler, et al., GCN 14799
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 ), the
afterglow has faded by about 3 magnitudes in all bands.

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

A. Trotter, A. LaCluyze, D. Reichart, J. Haislip, T. Berger, M. Carroll, 
H. T. Cromartie, R. Egger, A. Foster, C. Foster, N. Frank, K. Ivarsen, 
D. James, M. Maples, J. Moore, M. Nysewander, E. Speckhard, P. Taylor 
and J. A. Crain report:

Skynet continued observing the field of GRB 130606A (Ukwatta et al., GCN 
14781
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 , Swift trigger #557589), using the optical localization of Xu et 
al. (GCN 14783
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 ).  It took 109 160-second exposures in the z' band with 
one of the 16" telescopes of the PROMPT array at CTIO, Chile, with a 
mean time t=1.3d post-trigger.

In a stack of all 109 exposures, we detect the afterglow at the 5-sigma 
level, with z'~20.5 at t=1.3d.  Together with the z' detections we 
reported in Trotter et al. (GCN 14815
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 ), this implies an approximate 
temporal index alpha~-1.2.   A preliminary light curve of both nights' 
data is at:
http://www.skynet.unc.edu/grb/grb130606a_2.png

Photometry is calibrated to 10 SDSS stars in the field; g' and z' 
magnitudes are in the AB system; R-band magnitudes are in the Vega 
system, with the SDSS calibration stars transformed according to Jester 
(2005).  No correction has been applied for the expected line-of-sight 
Milky Way extinction of E(B-V)=0.02 (Schlegel et al. 1998).

No further Skynet observations are scheduled.

F.J. Virgili, C.G. Mundell (LJMU), A. Melandri (INAF-OAB), and A. Gomboc 
(U. Ljubljana) report:

Observations of GRB 130606A (Ukwatta et al., GCN 14781
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 ) with the 2-m 
robotic Liverpool Telescope automatically performed between 48 and 80 
minutes after the GRB trigger confirms a detection of the afterglow in 
the r'-band with magnitude

r' = 21.9 � 0.29 at 49.95 minutes

consistent with reported values at similar epochs (Xu et al. 14783) and 
dimmer than times around 100 minutes post trigger (Leonini et al., GCN 
14791
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 ; Masi et al., GCN 14789
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 ; Sonbas et al., GCN 14797
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 ), possibly 
indicating mild re-brightening.  This detection clarifies that the 
afterglow has not yet dropped out of the r'-band at the times coincident 
with our i' and z' band detections (Virgili et al., GCN 14785
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 ) and 
continues to be detected until at least 6.4 hrs after the initial 
trigger (Afonso et al., GCN 14807
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 ).

In addition, the 2-m Faulkes Telescope North and Liverpool Telescope 
performed late-time follow up observations, resulting in a 3-sigma 
upper-limit of

r' > 23.4 at 849.73 min (14.16 hr post-trigger; FTN)
r' > 24 at 1683.67 minutes (= 28.06 hr; LT)

and an additional i'-band detection of

i' = 23.76 � 0.22 @ 28.60 hr (= 1716.51 minutes; LT),

in a co-added series of 6x300s exposures, which are consistent with 
values reported by Trotter et al. (GCN 14815
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 ) and Butler et al. (GCN 
14824
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 ).  FTN images have been acquired with the R-Bessell filter and 
calibrated against nearby SDSS catalogue stars.

V. Rumyantsev (CrAO), N.Pit' (CrAO), ��. Volnova (IKI), A. Pozanenko (IKI) 
report on behalf of  larger GRB  follow-up collaboration:

We observed the field of  the Swift GRB 130606A (Ukwatta  et al., GCN 
14781
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 ) with  AZT-11 telescope of CrAO observatory  starting on  June 06
(UT) 21:59:60. We took  several images in R-filter of 180 s exposure. The 
afterglow (Jelinek et al., GCN 14782
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 ; Xu et al.,  GCN 14783
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 ; Nagayama et 
al., GCN 14784
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 )   is not detected in a combined image.   A photometry  is 
based  on the same SDSS stars we used  in GCN 14806
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 :

Start         T0+,        Filter   Exposure,   OT,        UL (3 sigma)
UT             mid, d                 (s)

21:59:60  0.0489    R        10x180      n/d         20.7

W. Fong, T. Laskar, E. Berger, and R. Margutti (Harvard) report:

"We observed GRB 130606A (Ukwatta et al., GCN 14781
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 ) with the Chandra ACIS
instrument, starting on 2013 June 17 03:05:37 UT (10.3 days after the GRB
trigger), for a total exposure of 30 ks. We detect a point source at the
position of the Swift/XRT afterglow. Using the spectral parameters from the
Swift/XRT PC-mode spectrum (http://www.swift.ac.uk/xrt_products/00557589)
and a redshift of z=5.91 (Chornock et al. 2013, ApJ, 774, 26; Castro-Tirado
et al., GCN 14796
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 ; Lunnan et al., GCN 14798
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 ; Xu et al., GCN 14816
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 ), we find
an unabsorbed flux of (2.4 +/- 0.4)e-15 erg/(s cm^2) in the 0.3-10 keV
band. This measurement is consistent with an extrapolation of the Swift/XRT
observations and shows a continuing decline in flux with a power-law decay
slope of -1.8 +/- 0.1 between 0.1 and 10 days after the burst.

We thank Harvey Tananbaum for approving our DDT request and the CXC staff
for rapidly arranging and executing the observations."