J/A+A/659/A39 GRB190114C spectra and light curves (Melandri+, 2022)
The supernova of the MAGIC gamma-ray burst GRB190114C.
Melandri A., Izzo L., Pian E., Malesani D.B., Della Valle M., Rossi A.,
D'Avanzo P., Guetta D., Mazzali P.A., Benetti S., Masetti N., Palazzi E.,
Savaglio S., Amati L., Antonelli L.A., Ashall C., Bernardini M.G.,
Campana S., Carini R., Covino S., D'Elia V., de Ugarte Postigo A.,
De Pasquale M., Filippenko A.V., Fruchter A.S., Fynbo J.P.U., Giunta A.,
Hartmann D.H., Jakobsson P., Japelj J., Jonker P.G., Kann D.A., Lamb G.P.,
Levan A.J., Martin-Carrillo A., Moller P., Piranomonte S., Pugliese G.,
Salvaterra R., Schulze S., Starling R.L.C., Stella L., Tagliaferri G.,
Tanvir N., Watson D.
<Astron. Astrophys. 659, A39 (2022)>
=2022A&A...659A..39M 2022A&A...659A..39M (SIMBAD/NED BibCode)
ADC_Keywords: GRB ; Supernovae ; Photometry ; Spectroscopy
Keywords: gamma-ray burst: individual: GRB190114C -
supernovae: individual: SN 2019jrj
Abstract:
We observed GRB190114C (redshift z=0.4245), the first gamma-ray
burst (GRB) ever detected at TeV energies, at optical and
near-infrared wavelengths with several ground-based telescopes and the
Hubble Space Telescope, with the primary goal of studying its
underlying supernova, SN 2019jrj. The monitoring spanned the time
interval between 1.3 and 370 days after the burst, in the observer
frame. We find that the afterglow emission can be modelled with a
forward shock propagating in a uniform medium modified by
time-variable extinction along the line of sight. A jet break could be
present after 7 rest-frame days, and accordingly the maximum
luminosity of the underlying supernova (SN) ranges between that of
stripped-envelope core-collapse SNe of intermediate luminosity and
that of the luminous GRB-associated SN 2013dx. The observed spectral
absorption lines of SN 2019jrj are not as broad as in classical GRB
SNe and are instead more similar to those of less-luminous
core-collapse SNe. Taking the broad-lined stripped-envelope
core-collapse SN 2004aw as an analogue, we tentatively derive the
basic physical properties of SN 2019jrj. We discuss the possibility
that a fraction of the TeV emission of this source might have had a
hadronic origin and estimate the expected high-energy neutrino
detection level with IceCube.
Description:
We observed the field of GRB190114C between 1.34 and ∼51.5 days (in the
observer frame) after the burst event with several facilities: the
3.58m New Technology Telescope (NTT), the 4.2m William Herschel
Telescope (WHT), the 3.58mGalileo National Telescope (TNG), the 8.2m
Very Large Telescope (VLT), and the Large Binocular Telescope (LBT;
two twin 8.4m telescopes at Mt. Graham in Arizona, USA).
We also observed the location of GRB190114C with the Hubble Space
Telescope (HST) at five epochs 27-370 days after the burst with the
Advanced Camera for Surveys Wide Field Channel (ACS/WFC) and three
optical/near-infrared (NIR) filters (F606W, F775W, and F850LP).
We observed GRB190114C in the optical/NIR band with the LBT using the
Multi-Object Double Spectrographs MODS-1 and MODS-2 in dual-grating
mode (grisms G400L and G670L) on 2019 January 29 (mid-observation time
of 13.25 days after the burst trigger).
We also obtained spectra of GRB190114C with the VLT/FORS2, using the
low-resolution 300I-OG590 grism, at 19.17, 22.15, 27.19, and 51.2
observer days after the GRB detection.
Objects:
----------------------------------------------------
RA (2000) DE Designation(s)
----------------------------------------------------
03 38 01.18 -26 56 47.8 GRB190114C = GRB 190114C
----------------------------------------------------
File Summary:
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FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
table2.dat 54 5 Summary of spectroscopic observations
sp/* . 5 Individual spectra
rband.dat 136 34 r-band Photometry table of GRB190114C (Fig. 2)
compiled by A. Melandri (data are all
dereddened for Galactic extinction)
iband.dat 137 23 i-band Photometry table of GRB190114C (Fig. 2)
compiled by A. Melandri (data are all
dereddened for Galactic extinction)
zband.dat 136 20 z-band Photometry table of GRB190114C (Fig. 2)
compiled by A. Melandri (data are all
dereddened for Galactic extinction)
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Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 11 A11 "YYYY/MMM/DD" Date Observation date
13- 17 F5.2 d Phase Phase with respect to the time of
burst (T0) are in the rest frame
19- 21 F3.1 arcsec Slit Slit
23- 27 A5 --- Texp Exposure time (s)
29- 32 F4.2 arcsec Seeing Seeing
34- 42 A9 --- Tel Telescope/Instrument
44- 54 A11 --- FileName Name of the spectrum file in
subdirectory sp
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Byte-by-byte Description of file: sp/*
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 17 F17.11 0.1nm lambda Wavelength
19- 32 E14.7 --- Flux Flux in arbitrary units
--------------------------------------------------------------------------------
Byte-by-byte Description of file: iband.dat rband.dat zband.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 5 A5 --- Inst Instrument (1)
7- 16 E10.4 s dt Mid-time of the observation from the burst
17- 23 F7.1 s texp Exposure time
25- 33 E9.4 s tstart Starting time of the observation =
mid-time-(exposure_time/2)
35- 43 E9.4 s tend Ending time of the observation =
mid-time+(exposure_time/2)
45- 55 F11.9 mJy fopt Optical flux in filter (2)
58- 66 F9.7 mJy e_fopt Optical flux in filter error (2)
68- 73 F6.3 mag mag Magnitude in filter (2)
75- 79 F5.3 mag e_mag Magnitude in filter error (2)
81- 94 F14.11 ---- fHGsub Optical flux in filter, after the Host Galxy
flux subtraction (3)
96-115 E20.16 --- f(AG) Estimate (from the optical fit) of the
afterglow contribution at that epoch (3)
116-137 E22.14 --- fSN Estimate of the SN contribution in filter,
fSN=fHGsub-f(AG) (3)
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Note (1): "---" for this paper observations from NTT, WHT, TNG, LBT, and VLT
telescopes.
Note (2): The observed quantities "fopt" and "mag" must be corrected (with the
exception of the HST measurements themselves!) to account for calibration
against the HST std stars, i.e. to the mags must be added an offset of
0.095 mags and the fluxes must be multiplied by 0.91622 for rband,
0.16 mags and the fluxes must be multiplied by 0.86298 for iband,
-0.21 mags and the fluxes must be multiplied by 1.09144 for zband.
Note (3): fHGsub, f(AG) and fSN fluxes are already corrected.
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Acknowledgements:
Andrea Melandri, andrea.melandri(at)inaf.it
(End) Patricia Vannier [CDS] 25-Feb-2022