J/ApJ/781/37 Multi-band photometry of GRB 130427A (Perley+, 2014)
The afterglow of GRB 130427A from 1 to 1016 GHz.
Perley D.A., Cenko S.B., Corsi A., Tanvir N.R., Levan A.J., Kann D.A.,
Sonbas E., Wiersema K., Zheng W., Zhao X.-H., Bai J.-M., Bremer M.,
Castro-Tirado A.J., Chang L., Clubb K.I., Frail D., Fruchter A., Gogus E.,
Greiner J., Guver T., Horesh A., Filippenko A.V., Klose S., Mao J.,
Morgan A.N., Pozanenko A.S., Schmidl S., Stecklum B., Tanga M.,
Volnova A.A., Volvach A.E., Wang J.-G., Winters J.-M., Xin Y.-X.
<Astrophys. J., 781, 37 (2014)>
=2014ApJ...781...37P 2014ApJ...781...37P (SIMBAD/NED BibCode)
ADC_Keywords: Gamma rays ; Photometry
Keywords: gamma-ray burst: individual: GRB 130427A -
radiation mechanisms: non-thermal
Abstract:
We present multiwavelength observations of the afterglow of
GRB130427A, the brightest (in total fluence) Gamma-Ray Burst (GRB) of
the past 29yr. Optical spectroscopy from Gemini-North reveals the
redshift of the GRB to be z=0.340, indicating that its unprecedented
brightness is primarily the result of its relatively close proximity
to Earth; the intrinsic luminosities of both the GRB and its afterglow
are not extreme in comparison to other bright GRBs. We present a large
suite of multiwavelength observations spanning from 300s to 130days
after the burst and demonstrate that the afterglow shows relatively
simple, smooth evolution at all frequencies, with no significant
late-time flaring or rebrightening activity. The entire data set from
1GHz to 10GeV can be modeled as synchrotron emission from a
combination of reverse and forward shocks in good agreement with the
standard afterglow model, providing strong support to the
applicability of the underlying theory and clarifying the nature of
the GeV emission observed to last for minutes to hours following other
very bright GRBs. A tenuous, wind-stratified circumburst density
profile is required by the observations, suggesting a massive-star
progenitor with a low mass-loss rate, perhaps due to low metallicity.
GRBs similar in nature to GRB 130427A, inhabiting low-density media
and exhibiting strong reverse shocks, are probably not uncommon but
may have been difficult to recognize in the past owing to their
relatively faint late-time radio emission; more such events should be
found in abundance by the new generation of sensitive radio and
millimeter instruments.
Description:
We present multiwavelength observations of the afterglow of
GRB130427A, the brightest (in total fluence) gamma-ray burst (GRB) of
the past 29yr.
GRB 130427A triggered the Burst Alert Telescope (BAT) on board the
Swift satellite on 2013 April 27 at 07:47:57.
UltraViolet-Optical Telescope (UVOT) data were also acquired by
Swift in parallel with XRT follow-up observations.
The Palomar 60inch telescope responded automatically to the BAT
trigger and began imaging the field starting at 07:52:21.7.
Shortly following the discovery of GRB 130427A and its afterglow, we
initiated observations with the Gemini-North telescope on Mauna Kea.
Follow-up observations of the associated SN were conducted on 2013 May
16 and 17.
We observed the field of GRB 130427A with the United Kingdom Infrared
Telescope (UKIRT) using the Wide Field Camera in the JHK filters at a
range of epochs from a few hours to a few weeks post-burst.
Imaging observations were carried out each night between 2013 April 27
and April 30 with the Yunnan Faint Object Spectrograph and Camera
instrument of the Lijiang 2.4 m Gao-Mei-Gu (GMG) telescope in Yunnan
Observatories, China. Data were taken with the Briz filters on the
first night following the GRB and with the r filter exclusively during
the three subsequent nights.
Images of GRB 130427A were also acquired with the 1.0m Telescope
(T100) at TUBITAK National Observatory in Turkey. We obtained six sets
of R-band observations on April 27.75, 28.73, 29.77, and 30.73, and on
May 1.80 and 2.79.
Imaging was acquired with the simultaneous seven-color Gamma-Ray burst
Optical and Near-infrared Detector (GROND) mounted on the 2.2m Max
Planck Gesellschaft (MPG)/ESO telescope at La Silla Observatory,
Chile. We observed the field on 2013 April 28, April 29, May 11, May
13, and May 19.
GRB 130427A was also observed with the 0.76m Katzman Automatic Imaging
Telescope (KAIT), the 1m Nickel Telescope, and the 3m Shane
telescope at Lick Observatory. KAIT and Nickel observations were
performed in the BVRI filters from one to several days after the burst
when the afterglow was still bright, while late-time Shane data were
in BVR using the Kast spectrograph in imaging mode.
We observed the location of GRB 130427A with the Large-Format Camera
on the Palomar 200inch telescope on 2013 May 5. We acquired five
dithered exposures in the g band and four in r.
We obtained two epochs of observations on May 5 and May 12 using the
1.34m Schmidt telescope of the Thuringer Landessternwarte
Tautenburg, Germany. Images were acquired using the 4k camera in the
first and the 2k camera in the second epoch.
Images of GRB 130427A were taken using the Low Resolution Imaging
Spectrometer (LRIS) on 2013 May 9 in the g and V filters and on 2013
May 10 in the g and R filters. Further imaging was conducted with the
Deep Imaging Multi-Object Spectrograph on 2013 June 9 in the R band.
Observations of GRB 130427A were completed with the 22m radio
telescope RT-22 at 36.8GHz in the Crimean Astrophysical Observatory.
We observed the position of GRB 130427A with the Combined Array for
Research in Millimeter Astronomy (CARMA) on several occasions over 3
days following the burst.
The IRAM Plateau de Bure Interferometer (PdBI) using the Wideband
Express correlator was pointed to the GRB 130427A location on six
occasions at 86.7GHz.
The position of GRB 130427A was observed with the Karl G. Jansky Very
Large Array (VLA) in its D, DnC, and C configurations, under programs
13A-411 (PI: A. Corsi), 13A-046 (PI: E. Berger), S50386 (PI: S. B.
Cenko), and SE0851 (PI: A. Fruchter). The data were taken between 2013
April 27 and 2013 September 2 in several bands (K, Ka, Ku, X, C, and
S), covering overall a frequency range between 1.4GHz and 37GHz.
While nearly all of the optical photometry of the burst and afterglow
is from our own observations, we use some data from the literature and
other sources to supplement these during gaps in our temporal
coverage: specifically, the early-time R measurements of Wren et al.
(2013GCN..14476...1W) (taken during prompt emission and only used in
plotting), ugriz photometry of Xu et al. (2013GCN..14478...1X), BVRI
photometry from Hermansson et al. (2013GCN..14596...1H), and JH
photometry from Butler et al. (2013GCN..14483...1B,
2013GCN..14506...1B, 2013GCN..14514...1B). Our late-time observations
of the SN are also supplemented by the r-band photometry of Xu et al.
(2013ApJ...776...98X 2013ApJ...776...98X). We also take LAT observations from Figure 2 of
Tam et al. (2013ApJ...771L..13T 2013ApJ...771L..13T) and radio observations (GMRT and a
few supplementary CARMA and VLA points) from Laskar et al.
(2013ApJ...776..119L 2013ApJ...776..119L).
Objects:
----------------------------------------------------------
RA (ICRS) DE Designation(s)
----------------------------------------------------------
11 32 32.63 +27 41 51.7 GRB 130427A = GRB 130427A
----------------------------------------------------------
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table1.dat 80 713 Photometry of GRB 130427A
table2.dat 37 56 Radio observations of GRB 130427A
table4.dat 37 120 Coeval spectral energy distributions (SEDs)
--------------------------------------------------------------------------------
See also:
J/ApJ/778/128 : GRB-host galaxies photometry (Perley+, 2013)
J/ApJ/746/156 : Radio afterglow observations of GRBs (Chandra+, 2012)
J/ApJ/743/154 : GRB110205A+110213A multi-band photometry (Cucchiara+, 2011)
J/AJ/141/163 : Ultimate light curve of SN 1998bw/GRB 980425
(Clocchiatti+, 2011)
J/ApJ/720/1513 : The afterglows of Swift-era GRBs. I. (Kann+, 2010)
J/ApJ/711/495 : Durations of Swift/BAT GRBs (Butler+, 2010)
J/MNRAS/397/1177 : Swift-XRT observations of GRBs (Evans+, 2009)
J/ApJ/693/1484 : Early optical afterglow catalog (Cenko+, 2009)
J/ApJ/691/723 : BVIJHKs observations of GRB 080319B (Bloom+, 2009)
J/ApJ/672/449 : GRB 061126 light curves (Perley+, 2008)
Byte-by-byte Description of file: table1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 10 A10 --- Tel Telescope identifier (1)
12- 19 F8.5 d Tmid [0/41] Exposure mid-time (G1)
21- 24 A4 --- Flt Filter used
26- 32 F7.1 s Exp [5/10815]? Exposure time
34- 39 F6.3 mag mag [7/22] Observed magnitude in Filter (2)
41- 45 F5.3 mag e_mag [0/0.6] Uncertainty in mag
47- 57 F11.3 uJy Flux [-1/4.2e+06] Observed flux density in Filter (3)
59- 69 F11.3 uJy e_Flux [0.3/1.6e+06] Uncertainty in Flux
71 A1 --- Out [e] Indicates an outlier observation
(e=excluded from analysis)
73- 80 A8 --- Ref Gamma-Ray Burst (GRB) Coordinates Network (GCN)
circular reference (4)
--------------------------------------------------------------------------------
Note (1): The telescope codes are defined as below:
GMG = Yunnan Faint Object Spectrograph and Camera instrument of the
Lijiang 2.4m Gao-Mei-Gu (GMG) telescope in Yunnan Observatories,
China;
GROND = Gamma-Ray burst Optical and Near-infrared Detector (GROND) mounted
on the 2.2m Max Planck Gesellschaft (MPG)/ESO telescope at La
Silla Observatory, Chile;
Gemini-N = The Gemini-North telescope on Mauna Kea;
KAIT = The 0.76m Katzman Automatic Imaging Telescope (KAIT) at Lick
Observatory;
KAST = The Kast spectrograph on the 3m Shane telescope at Lick
Observatory;
Keck = The Low Resolution Imaging Spectrometer (LRIS) and the Deep
Imaging Multi-Object Spectrograph;
Nickel = The 1m Nickel Telescope at Lick Observatory;
P200 = Large-Format Camera on the Palomar 200inch (P200) telescope;
P60 = Palomar 60inch telescope;
RAPTOR = The wide-field RAPid Telescopes for Optical Response (RAPTOR)
monitored the evolution of the optical afterglow throughout the
gamma-ray activity, recording a peak of R∼7mag
(Wren et al., 2013GCN..14476...1W);
RATIR = Reionization And Transients InfraRed camera;
Sandvreten = Sandvreten Observatory;
T100 = The 1.0m Telescope (T100) at TUBITAK National Observatory in
Turkey;
Tautenburg = The 1.34m Schmidt telescope of the Thuringer Landessternwarte
Tautenburg, Germany;
UKIRT = United Kingdom Infrared Telescope;
UVOT = UltraViolet-Optical Telescope.
Note (2): Not corrected for Galactic extinction and including host-galaxy flux.
Note (3): Corrected for Galactic extinction (E(B-V)=0.02mag) and host-galaxy
contribution. Except for the Palomar 60inch telescope (P60) observations,
uncertainties do not include the uncertainty resulting from subtraction of
the host flux; this is negligible over most of the afterglow evolution but
contributes a large, systematic uncertainty during the supernova (SN)
phase.
Note (4): The reference codes are defined as follows:
GCN14476 = Wren et al. (2013GCN..14476...1W);
GCN14478 = Xu et al. (2013GCN..14478...1X);
GCN14483 = Butler et al. (2013GCN..14483...1B);
GCN14506 = Butler et al. (2013GCN..14506...1B);
GCN14514 = Butler et al. (2013GCN..14514...1B);
GCN14596 = Hermansson et al. (2013GCN..14596...1H).
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 A5 --- Tel Telescope identifier (1)
7 A1 --- f_Tel [c] From Laskar et al. (2013ApJ...776..119L 2013ApJ...776..119L)
9- 17 F9.5 d Tmid [0.3/129] Integration mid-time (G1)
19- 21 A3 --- Band Band
23- 27 F5.2 GHz Freq [1/93] Central frequency
29- 32 I4 uJy Flux [86/6100] Flux density
34- 37 I4 uJy e_Flux [7/2023] Error in Flux
--------------------------------------------------------------------------------
Note (1): The telescope codes are defined as follows:
CARMA = Combined Array for Research in Millimeter Astronomy;
GMRT = Giant Metrewave Radio Telescope;
PdBI = The IRAM Plateau de Bure Interferometer;
RT22 = The 22m radio telescope at 36.8GHz in the Crimean Astrophysical
Observatory;
VLA = Very Large Array.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: table4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 7 F7.3 d Time [0/130] Effective time
9- 17 E9.3 Hz Freq [1.3e+09/3.5e+24] Frequency
19- 27 E9.3 uJy Flux [0/53800] Flux density at Freq
29- 37 E9.3 uJy e_Flux [0/5459] Uncertainty in Flux
--------------------------------------------------------------------------------
Global Notes:
Note (G1): Measured from the Fermi-GBM trigger (UT 07:47:06.42).
History:
From electronic version of the journal
(End) Prepared by [AAS]; Sylvain Guehenneux [CDS] 02-Dec-2015