J/ApJ/932/1 LBT/MODS spectrum of the host galaxy of GRB 200826A (Rossi+, 2022)
The peculiar short-duration GRB 200826A and its supernova.
Rossi A., Rothberg B., Palazzi E., Kann D.A., D'Avanzo P., Amati L.,
Klose S., Perego A., Pian E., Guidorzi C., Pozanenko A.S., Savaglio S.,
Stratta G., Agapito G., Covino S., Cusano F., D'Elia V., De Pasquale M.,
Valle M.D., Kuhn O., Izzo L., Loffredo E., Masetti N., Melandri A.,
Minaev P.Y., Guelbenzu A.N., Paris D., Paiano S., Plantet C., Rossi F.,
Salvaterra R., Schulze S., Veillet C., Volnova A.A.
<Astrophys. J., 932, 1 (2022)>
=2022ApJ...932....1R 2022ApJ...932....1R
ADC_Keywords: GRB ; Galaxies, spectra ; Spectroscopy ; Optical
Keywords: Gamma-ray bursts ; Core-collapse supernovae ; Supernovae
Abstract:
Gamma-ray bursts (GRBs) are classified into long and short events.
Long GRBs (LGRBs) are associated with the end states of very massive
stars, while short GRBs (SGRBs) are linked to the merger of compact
objects. GRB 200826A was a peculiar event, because by definition it
was an SGRB, with a rest-frame duration of ∼0.5s. However, this event
was energetic and soft, which is consistent with LGRBs. The relatively
low redshift (z=0.7486) motivated a comprehensive, multiwavelength
follow-up campaign to characterize its host, search for a possible
associated supernova (SN), and thus understand the origin of this
burst. To this aim we obtained a combination of deep near-infrared
(NIR) and optical imaging together with spectroscopy. Our analysis
reveals an optical and NIR bump in the light curve whose luminosity
and evolution are in agreement with several SNe associated to LGRBs.
Analysis of the prompt GRB shows that this event follows the Ep,i-Eiso
relation found for LGRBs. The host galaxy is a low-mass star-forming
galaxy, typical of LGRBs, but with one of the highest star formation
rates, especially with respect to its mass (logM*/M☉=8.6,
SFR∼4.0M☉/yr). We conclude that GRB 200826A is a typical
collapsar event in the low tail of the duration distribution of LGRBs.
These findings support theoretical predictions that events produced by
collapsars can be as short as 0.5s in the host frame and further
confirm that duration alone is not an efficient discriminator for the
progenitor class of a GRB.
Description:
Optical spectroscopy of GRB 200826A was obtained with the Large
Binocular Telescope (LBT) on Mount Graham, Arizona, USA, on
2020-Aug-28, at UT 09:06:45 (MJD59089.379692) using both optical
Multi-object Double Spectrographs (MODS; R∼1500).
Objects:
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RA (ICRS) DE Designation(s)
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00 27 08.47 +34 01 36.5 GRB 200826A = Fermi bn200826187
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File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
fig10.dat 22 7412 LBT/MODS observed spectrum of the host galaxy
of GRB 200826A
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See also:
I/345 : Gaia DR2 (Gaia Collaboration, 2018)
VII/233 : The 2MASS Extended sources (IPAC/UMass, 2003-2006)
V/147 : The SDSS Photometric Catalogue, Release 12 (Alam+, 2015)
J/ApJ/678/1127 : Optical photometry of GRB 070610 (Kasliwal+, 2008)
J/ApJ/701/824 : Afterglows of short & long-duration GRBs (Nysewander+, 2009)
J/ApJ/720/1513 : The afterglows of Swift-era GRBs. I. (Kann+, 2010)
J/ApJ/778/128 : GRB-host galaxies photometry (Perley+, 2013)
J/A+A/570/A11 : The Hawk-I UDS and GOODS Survey (HUGS) (Fontana+, 2014)
J/ApJ/789/23 : Properties of SN host galaxies (Kelly+, 2014)
J/A+A/609/A30 : Conversion factors to LIR & Mdust (Schreiber+, 2018)
J/MNRAS/486/L46 : Gamma-ray burst redshifts (Amati+, 2019)
J/A+A/625/A152 : Light-curve models of black hole (Barbieri+, 2019)
J/MNRAS/492/1919 : Type I GRBs & the new classification method (Minaev+, 2020)
J/MNRAS/493/3379 : Comparison between GRB afterglows & AT2017gfo (Rossi+, 2020)
J/A+A/646/A50 : GRB 190829A/SN 2019oyw spectra (Hu+, 2021)
J/ApJ/916/89 : 85 short GRB kilonovae opt. & NIR obs. (Rastinejad+, 2021)
J/A+A/659/A39 : GRB190114C spectra and light curves (Melandri+, 2022)
Byte-by-byte Description of file: fig10.dat
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Bytes Format Units Label Explanations
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1- 11 F11.5 0.1nm lambda [3800.23/10100] Wavelength; Angstroms
13- 22 E10.3 cW/m2/nm Flux [-6.42e-18/4.1e-17] Flux density;
erg/s/cm2/Angstrom (1)
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Note (1): Flux is calibrated using the photometry of the host.
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History:
From electronic version of the journal
(End) Prepared by [AAS], Esther Collas [CDS] 22-Mar-2024