GRB 130505A
GCN Circular 14602
Subject
GRB 130505A: MITSuME Akeno Optical observation
Date
2013-05-08T11:41:21Z (13 years ago)
From
Taketoshi Yoshii at Tokyo Tech <yoshii.t.ac@m.titech.ac.jp>
T. Yoshii, Y. Yatsu, Y. Yano, R. Usui, Y. Tachibana, K. Ito,
S. Kurita, Y. Saito, and N. Kawai (Tokyo Tech)
report on behalf of the MITSuME collaboration:
We observed GRB 130505A (Maselli et al., GCNC 14563) with an
optical tri-color (g, Rc, and Ic) camera attached to the MITSuME
50 cm telescope of Akeno Observatory, Yamanashi, Japan.
The observation started at 2013-05-05 11:04:17 UT (9709 sec after the
trigger).
And we detected the previously reported afterglow .
The measured magnitudes were listed below.
T0+[MID] MID-UT T-EXP[sec] g' Rc Ic
-----------------------------------------------------------------------------------------------------
15550s 12:41:38 3480 18.8+/-0.1 18.9+/-0.2 18.0+/-0.1
-----------------------------------------------------------------------------------------------------
T-EXP: Total Exposure time [sec]
(The photon flux were calibrated against GSC2.3 catalog.)
GCN Circular 14599
Subject
GRB 130505A: Suzaku WAM observation of the prompt emission
Date
2013-05-08T04:30:49Z (13 years ago)
From
Makoto Tashiro at Saitama U/Swift <tashiro@phy.saitama-u.ac.jp>
T. Yasuda, M. Tashiro, Y. Terada, Y. Ishida, H. Ueno, S. Sugimoto
(Saitama U.), M. Ohno, K. Takaki, T. Kawano, R. Nakamura, S. Furui,
Y. Fukazawa (Hiroshima U.), M. Yamauchi, N. Ohmori, M. Akiyama
(Univ. of Miyazaki), K. Yamaoka (Nagoya U.), S. Sugita (Ehime U.),
Y. E. Nakagawa, M. Kokubun, T. Takahashi (ISAS/JAXA), W. Iwakiri
(RIKEN), Y. Hanabata (ICRR), Y. Urata (NCU), K. Nakazawa,
K. Makishima (Univ. of Tokyo) on behalf of the Suzaku WAM team, report:
The bright, long GRB 13505A (GCN 14563; Cannizzo et al.)
triggered the Suzaku Wide-band All-sky Monitor (WAM) which covers an
energy range of 50 keV - 5 MeV at UT 08:22:24.527 (=T0).
The observed light curve shows a bright peak followed by a weaker
emission seen up to T0+30 s with a duration (T90) of about 14 seconds.
The fluence in 100 - 1000 keV was 1.06 (+0.05/-0.05) x10^-4 erg/cm^2.
The 1-s peak flux measured from T0+4 s was
53.1 (+2.0/-2.5) photons/cm^2/s in the same energy range.
Preliminary result shows that the time-averaged spectrum from
T0-2 s to T0+30 s is well fitted by a GRB Band model as follows.
the low-energy photon index alpha: -0.99 (+0.17/-0.11),
the high-energy photon index beta: -2.33 (+0.06/-0.07),
and the peak energy Epeak: 1094 (+131/-175) keV (chi^2/d.o.f = 23.9/23).
Using a redshift of z = 2.27 (Tanvir et al., GCN 14567), we estimate
the isotropic energy release in the 1 keV - 10 MeV range to be
2.55 (+0.12/- 0.11) x10^54 erg and the peak energy at the rest frame
to be 3615 (+532/-469) keV, where cosmological parameters of the Omega
matter, the Omega lambda and the Hubble constant are fixed at 0.27, 0.73
and 70 km/s/Mpc respectively.
Due to the brightness of this burst, a 3% systematic error was added for
low energy channels.
All the quoted errors are at statistical 90% confidence level.
The light curves for this burst are available at:
http://www.astro.isas.jaxa.jp/suzaku/HXD-WAM/WAM-GRB/grb/trig/grb_table.html
GCN Circular 14595
Subject
GRB 130505A: RATIR Optical and NIR Observations
Date
2013-05-07T18:14:30Z (13 years ago)
Edited On
2024-11-07T19:57:07Z (a year ago)
From
Alan M. Watson at Instituto de Astronomia UNAM <alan@astro.unam.mx>
Edited By
Vidushi Sharma at NASA GSFC/UMBC <vidushi.sharma@nasa.gov> on behalf of Leo P. Singer at NASA/GSFC <leo.p.singer@nasa.gov>
Alan M. Watson (UNAM), Nat Butler (ASU), 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 130505A (Cannizzo, et al., GCN Circular
14563) 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 2013/05 7.13 to
2013/05 7.22 UTC (42.84 to 44.87 hours after the BAT trigger), obtaining
a total of 0.36 hours exposure in the r' and i' bands and 0.14 hours
exposure in the Z, Y, J, and H bands.
The optical counterpart (Evans et al., GCN Circular 14569) is clearly
identified. We obtain the following detections and 3-sigma upper limits:
r' = 21.10 ± 0.27
i' = 20.98 ± 0.23
Z > 21.17
Y > 19.15
J > 18.38
H > 17.15
These magnitudes are in the AB system, are calibrated by comparison with
SDSS DR8 and 2MASS, and not corrected for Galactic extinction in the
direction of the GRB. The quoted uncertainties on the detections are 1
sigma.
We thus confirm the fading reported by other observers at earlier epochs
(Kuroda et al., GCN Circular 14568; Xu et al, GCN Circular 14570; Xin et
al., GCN Circular 14571; Hentunen et al, GCN Circular 14572; Krugly et
al., GCN Circular 14585; and Kann et al., GCN Circular 14593).
No further observations of this source are planned.
We thank the staff of the Observatorio Astronómico Nacional in San Pedro
Mártir.
GCN Circular 14593
Subject
GRB 130505A: Tautenburg afterglow observations
Date
2013-05-06T22:41:36Z (13 years ago)
From
Alexander Kann at TLS Tautenburg <kann@tls-tautenburg.de>
D. A. Kann, B. Stecklum, and F. Ludwig (TLS Tautenburg) report:
We observed the optical afterglow (Cannizzo et al., GCN 14563) of the
extremely luminous GRB 130505A (Cannizzo et al., GCN 14563; Golenetskii et
al., GCN 14575) with the 1.34m Schmidt telescope of the Thueringer
Landessternwarte Tautenburg equipped with a 4k CCD camera under good
weather conditions. We obtained 3 x 300 sec frames in the Rc band. The
afterglow is detected in each frame.
For a nearby SDSS star (RA = 137.082047, Dec. = 17.486120), using the
transformations of Lupton (2005), we find: B = 18.118, V = 17.080, Rc =
16.501, Ic = 15.967.
Using this star for calibration, we derive a preliminary magnitude of Rc =
19.09 +/- 0.06 at 0.49118 days after the GRB.
This message may be cited.
GCN Circular 14589
Subject
GRB 130505A, Swift-BAT refined analysis
Date
2013-05-06T17:01:01Z (13 years ago)
From
Amy Lien at GSFC <amy.y.lien@nasa.gov>
A. Y. Lien (NASA/GSFC/ORAU), J. R. Cummings (GSFC/UMBC), T. Sakamoto (AGU),
C. B. Markwardt (GSFC), S . D. Barthelmy (GSFC), W. H. Baumgartner (GSFC/UMBC),
J. K. Cannizzo (NASA/UMBC), N. Gehrels (GSFC), H. A. Krimm (GSFC/USRA), D. M. Palmer (LANL),
M. Stamatikos (OSU), E. Troja (NASA/GSFC/UMCP), 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 130505A (trigger #555163)
(Cannizzo, et al., GCN Circ. 14563). The BAT ground-calculated position is
RA, Dec = 137.060, 17.485 deg which is
RA(J2000) = 09h 08m 14s
Dec(J2000) = +17d 29' 06"
with an uncertainty of 1.5 arcmin, (radius, sys+stat, 90% containment).
The partial coding was 2%.
The mask-weighted light curve starts at ~T-3 sec, peaks at ~T+0.3 sec,
drops sginificantly at ~T+5 sec, and then has a long tail out to ~T+350 sec.
T90 (15-350 keV) is 88 +- 10 sec (estimated error including systematics).
The time-averaged spectrum from T-3.0 to T+363.3 sec is best fit by a simple
power-law model. The power law index of the time-averaged spectrum is
1.18 +- 0.07. The fluence in the 15-150 keV band is 2.1 +- 0.1 x 10^-05 erg/cm2.
The 1-sec peak photon flux measured from T+1.44 sec in the 15-150 keV band
is 30.0 +- 3.1 ph/cm2/sec. All the quoted errors are at the 90% confidence
level. The spectral results may be skewed toward harder values because of
the effects of the extreme partial coding.
The results of the batgrbproduct analysis are available at
http://gcn.gsfc.nasa.gov/notices_s/555163/BA/
GCN Circular 14585
Subject
GRB 130505A: optical observations
Date
2013-05-06T02:27:34Z (13 years ago)
From
Alexei Pozanenko at IKI, Moscow <apozanen@iki.rssi.ru>
Yu. Krugly (IA KhNU), I. Slyusarev (IA KhNU), I. Molotov (KIAM), A.
Pozanenko (IKI) report on behalf of larger collaboration:
We observed a filed of the Swift GRB 130505A (Cannizzo et al. GCN 14563)
with 0.7m telescope of Institute of Astronomy, Kharkiv National University
between May 05 (UT) 20:52:35 - 21:19:57. A set of images of 180 s were
taken in R-filter. In the combined image we clearly detect optical
afterglow (Cannizzo et al., GCN 14563; Tanvir et al., GCN 14567; Kuroda et
al., GCN 14568). Preliminary photometry is based on the nearby SDSS stars:
T_start (UT) T0+ Filter Exp. OT
mid,days s mag
2013-05-05T20:52:35 0.5309 R 8x180 19.4 +/- 0.07
GCN Circular 14580
Subject
GRB 130505A: E_iso record retraction
Date
2013-05-05T21:56:21Z (13 years ago)
From
Alexander Kann at TLS Tautenburg <kann@tls-tautenburg.de>
D. A. Kann (TLS Tautenburg), and S. Schulze (PUC, MCSS) report:
Following the corrected Konus-Wind energy range (Frederiks, GCN 14578), we
recalculated E_iso for GRBs 130505A and 130427A (affected by the same
error in GCN 14487, Frederiks, GCN 14579), finding log E_iso,bol = 54.48
+/- 0.01 and 53.89 +/- 0.002, respectively.
This makes GRB 130505A comparable to GRB 080916C, and still one of the
most energetic GRBs ever discovered, but not the most energetic of all.
GCN Circular 14578
Subject
GRB 130505A: correction to GCN 14575
Date
2013-05-05T21:14:09Z (13 years ago)
From
Dmitry Frederiks at Ioffe Institute <fred@mail.ioffe.ru>
D. Frederiks, on behalf of the Konus-Wind team, reports:
We have found a typo in our GCN Circ. 14575 "Konus-Wind observation of GRB 130505A":
the correct energy range for the K-W energy fluence and peak flux estimations
for GRB 130505A is 20-10000 keV, not "20 - 1200 keV", as mentioned.
The 20-10000 keV range is a standard for the K-W estimations of GRB energetics
in the observer frame.
We are sorry for the inconvenience.
GCN Circular 14577
Subject
GRB 130505A: Swift-XRT refined Analysis
Date
2013-05-05T20:36:04Z (13 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
D.N. Burrows (PSU), C. Pagani (U. Leicester), A.P. Beardmore (U.
Leicester), P.A. Evans (U. Leicester), G. Stratta (ASDC), P. D'Avanzo
(INAF-OAB), V. D'Elia (ASDC), J.A. Kennea (PSU), M.C. Stroh (PSU) and
J.K. Cannizzo report on behalf of the Swift-XRT team:
We have analysed 11 ks of XRT data for GRB 130505A (Cannizzo et al.
GCN Circ. 14563), from 102 s to 29.4 ks after the BAT trigger. The
data comprise 503 s in Windowed Timing (WT) mode with the remainder in
Photon Counting (PC) mode. The enhanced XRT position for this burst was
given by Evans et al. (GCN. Circ 14569).
The late-time light curve (from T0+3.7 ks) can be modelled with a
power-law decay with a decay index of alpha=1.06 (+0.03, -0.04).
A spectrum formed from the WT mode data can be fitted with an absorbed
power-law with a photon spectral index of 1.86 (+/-0.03). The
best-fitting absorption column is 10.0 (+/-0.7) x 10^20 cm^-2, in
excess of the Galactic value of 3.6 x 10^20 cm^-2 (Kalberla et al.
2005). The PC mode spectrum has a photon index of 1.92 (+/-0.07) and a
best-fitting absorption column of 8.8 (+1.6, -1.5) 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 (4.7 x 10^-11) erg cm^-2
count^-1.
A summary of the PC-mode spectrum is thus:
Total column: 8.8 (+1.6, -1.5) x 10^20 cm^-2
Galactic foreground: 3.6 x 10^20 cm^-2
Excess significance: 5.6 sigma
Photon index: 1.92 (+/-0.07)
If the light curve continues to decay with a power-law decay index of
1.06, the count rate at T+24 hours will be 0.27 count s^-1,
corresponding to an observed (unabsorbed) 0.3-10 keV flux of 1.0 x
10^-11 (1.3 x 10^-11) erg cm^-2 s^-1.
The results of the XRT-team automatic analysis are available at
http://www.swift.ac.uk/xrt_products/00555163.
This circular is an official product of the Swift-XRT team.
GCN Circular 14576
Subject
GRB 130505A: Largest E_iso ever measured
Date
2013-05-05T20:03:36Z (13 years ago)
From
Alexander Kann at TLS Tautenburg <kann@tls-tautenburg.de>
D. A. Kann (TLS Tautenburg), and S. Schulze (PUC, MCSS) report:
Using the energetics provided by the Konus-Wind detection (Golenetskii et
al. 2013, GCN 14575) of the extremely intense Swift GRB 130505A (Cannizzo
et al. 2013, GCN 14564), and employing k-correction (Bloom et al. 2003,
ApJ, 594, 674), we determine the isotropic energy release in the
bolometric band (rest-frame 1 keV - 10 MeV) to be (5.65 +/- 0.13) x 10^54
erg (log E_iso = 54.75 +/- 0.01).
The most isotropically energetic GRBs known so far (all in the rest-frame
bolometric band) are GRBs 990123, 080916C and 090323, for which log E_iso
~ 54.5 - 54.6 has been found (e.g., Kann et al. 2010, ApJ, 720, 1513).
This makes GRB 130505A the most energetic GRB known, and may indicate
either an ultra-luminous event or a high degree of collimation.
We additionally note that the nearby GRB 130427A (Maselli et al. 2013, GCN
14448; Golenetskii et al. 2013, GCN 14487) is also highly energetic, with
log E_iso,bol = 54.21 +/- 0.05, but this is about 3.5 times less than GRB
130505A.
This message may be cited.
GCN Circular 14575
Subject
Konus-Wind observation of GRB 130505A
Date
2013-05-05T19:19:22Z (13 years ago)
From
Dmitry Frederiks at Ioffe Institute <fred@mail.ioffe.ru>
S. Golenetskii, R.Aptekar, D. Frederiks, E. Mazets, V. Pal'shin,
P. Oleynik, M. Ulanov, D. Svinkin, and T. Cline on behalf
of the Konus-Wind team, report:
The long very intense GRB 130505A (Swift-BAT trigger #555136:
Cannizzo et al., GCN 14564) triggered Konus-Wind (K-W)
at T0=30147.038s UT (08:22:27.038).
The K-W light curve shows a bright pulse with a duration of ~5s
followed by a weaker decaying emission out to ~T0+30s with
a slight increase in the count rate at ~T0+15s.
The emission is seen up to ~10 Mev.
The Konus-Wind light curve of this GRB is available at
http://www.ioffe.ru/LEA/GRBs/GRB130505_T30147/
As observed by Konus-Wind, the main phase of the burst had
a fluence of (3.13 � 0.06)x10^-4 erg/cm2 and a 64-ms peak flux,
measured from T0+2.496 s, of (6.9 � 0.3)x10^-5 erg/cm2/s
(both in the 20 - 1200 keV energy range).
The time-averaged spectrum (measured from T0 to T0+21.248 s)
is best fit in the 20 keV-15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.69 � 0.04,
the high energy photon index beta = -2.03 � 0.03,
the peak energy Ep = 631 � 31 keV,
chi2 = 113/92 dof.
The spectrum at the maximum count rate
(measured from T0+2.304 to T0+2.816 s)
is best fit in the 20 keV - 15 MeV range
by the GRB (Band) function with the following model parameters:
the low-energy photon index alpha = -0.31 � 0.09,
the high energy photon index beta = -2.26 � 0.07,
the peak energy Ep = 604 � 49 keV,
chi2 = 105/90 dof.
Assuming z=2.27 (Tanvir et al., GCN 14567)
and a standard cosmology model with H_0 = 70 km/s/Mpc,
Omega_M = 0.27, and Omega_Lambda = 0.73,
the isotropic energy release E_iso is ~3.8x10^54 erg,
the peak luminosity (L_iso)_max is ~2.7x10^54 erg/s,
and the rest-frame peak energy Ep,i = 2030 keV
All the quoted errors are estimated at the 1 sigma confidence level.
GCN Circular 14573
Subject
Swift/UVOT observations of GRB130505A
Date
2013-05-05T16:28:36Z (13 years ago)
From
Massimiliano de Pasquale at MSSL-UCL <m.depasquale@ucl.ac.uk>
M. De Pasquale (MSSL/UCL) and J. K. Cannizzo (NASA/UMBC) report on behalf
of the Swift/UVOT team:
The Swift/UVOT began settled observations of the field of GRB 130505A
107 s after the BAT trigger (Cannizzo et al., GCN Circ. 14563). A bright
but
rapidly fading source is detected in the finding chart and initial exposures
within the XRT error circle (Evans et al., GCN Circ. 14569).
The preliminary UVOT position is:
RA(J2000) = 09:08:14.64 = 137.0610
DEC(J2000) = +17:29:05.2 = +17.48478
with a 90%-confidence error radius of about 0.5 arc sec.
Preliminary detections and 3-sigma upper limits using the UVOT
photometric system (Breeveld et al. 2011, AIP Conf. Proc. 1358, 373) for
the early exposures are:
Filter T_start(s) T_stop(s) Exp(s) Mag
white (FC) 107 256 147 14.14 � 0.05
white 3952 4151 197 17.96 � 0.07
v 4362 4561 197 17.50 � 0.11
b 3503 3946 197 17.71 � 0.08
u 320 542 218 14.66 � 0.04
uvw1 4772 4971 197 19.28 � 0.29 (~3
sigma)
uvm2 4567 4766 197 >19.6
uvw2 4158 4357 197 >19.9
The non-detection of the optical source in um2 and uw2 filters is
consistent with the redshift z=2.27 found by Tanvir et al (GCN Circ. 14567)
The magnitudes in the table are not corrected for the Galactic
extinction due to the reddening of E(B-V) = 0.04 in the direction of
the burst (Schlegel et al. 1998).
GCN Circular 14572
Subject
GRB 130505A: iTelescope T12 optical observations
Date
2013-05-05T15:03:03Z (13 years ago)
From
Veli-Pekka Hentunen at Taurus Hill Obs,A95 <veli-pekka.hentunen@kassiopeia.net>
Veli-Pekka Hentunen, Markku Nissinen and Tuomo Salmi (Taurus Hill
Observatory, Varkaus, Finland) report:
We have detected GRB 130505A optical afterglow at iTelescope
observatory T12 (Siding Spring, Australia) Takahashi FSQ ED
0.10m/5.0 astrograph and SBIG STL-11000M CCD. Five
unfiltered images with 600 sec and 300 sec exposure time were made.
The afterglow was detected at following position RA 09:08:14.6 and
DEC +17:29:04.
The following magnitudes were obtained from the observations using
NOMAD1 1075-0205635 (R=14.240) as the comparison:
Tmid(sec)+T0 Filter Exp. time Mag Mag err.
2485 unfiltered 600 16.78CR 0.06
3370 unfiltered 3x300 17.15CR 0.02
5061 unfiltered 600 17.45CR 0.08
GCN Circular 14571
Subject
GRB 130505A: Xinglong TNT optical observations
Date
2013-05-05T14:32:29Z (13 years ago)
From
L.P. Xin at NAOC <xlp@bao.ac.cn>
L. P. Xin, J. Y. Wei, Y. L. Qiu, J. Wang,
J. S. Deng, C. Wu, X. H. Han report on behalf of EAFON team:
We began to observe the field of GRB 130505A (Cannizzo, et al., GCN 14563)
using 80cm TNT telescope located at Xinglong observatory, China
at 12:25:39 UT on 2013-05-05. We obtained several R-band images.
The reported optical counterpart (Cannizzo, et al., GCN 14563) is detected in all images.
A prelinary analysis shows that its brightness is decaying from R~18.05 to R~18.68 mag
during 4.05h and 4.85h after the trigger time.
These magnitudes are calibrated with USNO B1.0 R2 stars,
This message may be cited.
GCN Circular 14570
Subject
GRB 130505A; Weihai optical observations
Date
2013-05-05T13:43:31Z (13 years ago)
From
Dong Xu at DARK/NBI <dong.dark@gmail.com>
D. Xu (DARK/NBI), C. Cao, S.-M. Hu, J.-M. Ai (SDU) report:
We observed the field of GRB 130505A (Cannizzo et al., GCN 14563) with
the 1m telescope located in Weihai, Shandong Province, China. We
obtained 2x600s frames in the solan r-filter with a mean time of
3.3724 hr after the BAT trigger.
The optical afterglow is clearly detected at the UVOT position with
r=18.4 +/- 0.1 mag, calibrated against the SDSS field.
GCN Circular 14569
Subject
GRB 130505A: Enhanced Swift-XRT position
Date
2013-05-05T13:07:03Z (13 years ago)
From
Phil Evans at U of Leicester <pae9@leicester.ac.uk>
P.A. Evans, M.R. Goad, J.P. Osborne and A.P. Beardmore (U. Leicester)
report on behalf of the Swift-XRT team.
Using 1875 s of XRT Photon Counting mode data and 5 UVOT
images for GRB 130505A, 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 = 137.06069, +17.48471 which is equivalent
to:
RA (J2000): 09h 08m 14.57s
Dec (J2000): +17d 29' 05.0"
with an uncertainty of 1.7 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.
GCN Circular 14568
Subject
GRB 130505A: MITSuME Okayama Optical Observation
Date
2013-05-05T12:02:12Z (13 years ago)
From
Daisuke Kuroda at OAO/NAOJ <dikuroda@oao.nao.ac.jp>
D. Kuroda, K. Yanagisawa, Y. Shimizu, H. Toda (OAO, NAOJ),
S. Nagayama (NAOJ), M. Yoshida (Hiroshima), K. Ohta (Kyoto)
and N. Kawai(Tokyo Tech)
report on behalf of the MITSuME collaboration:
We observed the field of GRB 130505A (Cannizzo et al., GCNC 14563)
with the optical three color (g', Rc and Ic) CCD camera attached
to the MITSuME 50cm telescope of Okayama Astrophysical Observatory.
The observation started on 2013-05-05 10:52:56 UT (~2.5 h after the burst).
We detected the previously reported afterglow (Cannizzo et al., GCNC 14563)
in all the three bands.
Photometric results of the OT are listed below.
We used SDSS catalog for flux calibration.
#T0+[day] MID-UT T-EXP[sec] g' g'_err Rc Rc_err Ic Ic_err
-----------------------------------------------------------------------
0.11507 11:08:09 1620.0 18.2 0.1 18.2 0.1 17.6 0.1
------------------------------------------------------------------------
T0+ : Elapsed time after the burst [day]
T-EXP: Total Exposure time [sec]
GCN Circular 14567
Subject
GRB 130505A - Gemini-N/GMOS redshift determination
Date
2013-05-05T10:30:19Z (13 years ago)
From
Nial Tanvir at U.Leicester <nrt3@star.le.ac.uk>
N. R. Tanvir (U. Leicester), A. J. Levan (U. Warwick), T. Matulonis
and A. B. Smith (Gemini) report on behalf of a larger collaboration:
We observed the afterglow of GRB 130505A (Cannizzo et al. GCN 14563)
with the GMOS-N spectrograph on Gemini-N, beginning approximately 60 min
after the BAT trigger.
In our provisional reduction we detect numerous absorption lines, including
Lyman alpha, SiII/SiII*1260, SiII*1264, OI1302, SiII/OI*1304, SiII*1309,
CII/CII* 1334/1335, SiIV1394/1403, SiII 1527, SiII* 1533, CIV 1548/1551,
FeII 1608, AlII 1671 and AlIII 1855/1863 at a common redshift of z=2.27.
The presence of fine structure lines, in particular, confirms this to be the
redshift of this burst.
GCN Circular 14566
Subject
GRB 130505A: MAXI/GSC detection
Date
2013-05-05T10:13:07Z (13 years ago)
From
Satoshi Nakahira at JAXA/MAXI <nakahira.satoshi@jaxa.jp>
GRB 130505A: MAXI/GSC detection
S. Nakahira (JAXA), M. Serino (RIKEN), H. Negoro (Nihon U.),
S. Ueno, H. Tomida, M. Kimura, M. Ishikawa (JAXA),
T. Mihara, M. Sugizaki, M. Morii, T. Yamamoto, J. Sugimoto, T. Takagi, M. Matsuoka (RIKEN),
N. Kawai, R. Usui, K. Ishikawa, T. Yoshii (Tokyo Tech),
A. Yoshida, T. Sakamoto, Y. Nakano (AGU),
H. Tsunemi, M. Sasaki (Osaka U.),
M. Nakajima, T. Onodera, K. Fukushima, K. Suzuki (Nihon U.),
Y. Ueda, M. Shidatsu, T. Kawamuro, (Kyoto U.),
Y. Tsuboi, M. Higa (Chuo U.),
M. Yamauchi, K. Yoshidome, Y. Ogawa, H. Yamada (Miyazaki U.),
K. Yamaoka (Nagoya U.) report on behalf of the MAXI team
At 2013-05-05T08:22:29 UT, the MAXI/GSC detected an uncatalogued X-ray
transient source. Assuming that the source flux was constant over the
transit, we obtain the source position at
(R.A., Dec.) = (136.955 deg, 17.585 deg)= (09 07 49 , +17 35 05)(J2000)
with a 90% C.L. statistical error of 0.07 deg and an additional systematic
uncertainty of 0.1 deg (90% containment radius).
The position and time are consistent with those of GRB 130505A (Cannizzo
et al, GCN #14563). The transit by MAXI occurred from
2013-05-05T08:22:18 (=T0-10 s, where T0 is the Swift/BAT trigger time) to T0+40s.
The averaged X-ray flux was 3.17 +/- 0.21 Crab (2-20 keV).
The spectrum is fitted by a power-law model with a photon index of
1.37 (-0.10/+0.10). There was no significant excess flux at the previous
transit at 2013/05/05 06:46 UT and at the next transit at 2013/05/05
09:55 UT with an upper limit of 20 mCrab for each.
GCN Circular 14563
Subject
GRB 130505A: Swift detection of a burst with optical afterglow
Date
2013-05-05T08:36:39Z (13 years ago)
From
Scott Barthelmy at NASA/GSFC <scott@milkyway.gsfc.nasa.gov>
J. K. Cannizzo (NASA/UMBC), S. D. Barthelmy (GSFC),
J. R. Cummings (NASA/UMBC), V. D'Elia (ASDC),
C. B. Markwardt (NASA/GSFC), F. E. Marshall (NASA/GSFC),
A. Melandri (INAF-OAB), P. T. O'Brien (U Leicester),
B. Sbarufatti (INAF-OAB/PSU) and M. Stamatikos (OSU/NASA/GSFC) report
on behalf of the Swift Team:
At 08:22:28 UT, the Swift Burst Alert Telescope (BAT) triggered and
located GRB 130505A (trigger=555163). Swift slewed immediately to the burst.
The BAT on-board calculated location is
RA, Dec 137.060, +17.485 which is
RA(J2000) = 09h 08m 14s
Dec(J2000) = +17d 29' 06"
with an uncertainty of 3 arcmin (radius, 90% containment, including
systematic uncertainty). The BAT light curve shows a bright peak
followed by a much weaker peak with a total duration of about 20 sec.
The peak count rate was ~35,500 counts/sec (15-350 keV), at ~0 sec
after the trigger.
The XRT began observing the field at 08:24:04.7 UT, 96.4 seconds after
the BAT trigger. XRT found a bright, uncatalogued X-ray source located
at RA, Dec 137.0626, 17.4857 which is equivalent to:
RA(J2000) = +09h 08m 15.02s
Dec(J2000) = +17d 29' 08.5"
with an uncertainty of 4.8 arcseconds (radius, 90% containment). This
location is 9.3 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 7.35e-09 erg cm^-2 s^-1 (0.2-10
keV).
UVOT took a finding chart exposure of 150 seconds with the White filter
starting 106 seconds after the BAT trigger. There is a candidate afterglow in
the rapidly available 2.7'x2.7' sub-image at
RA(J2000) = 09:08:14.64 = 137.06100
DEC(J2000) = +17:29:05.2 = 17.48479
with a 90%-confidence error radius of about 0.74 arc sec. This position is 6.4
arc sec. from the center of the XRT error circle. The estimated magnitude is
14.14 with a 1-sigma error of about 0.14. No correction has been made for the
expected extinction corresponding to E(B-V) of 0.04.
Burst Advocate for this burst is J. K. Cannizzo (cannizzo AT milkyway.gsfc.nasa.gov).
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.)