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Progenitor and close-in circumstellar medium of type II supernova 2020fqv from high-cadence photometry and ultra-rapid UV spectroscopy.

Authors :
Tinyanont, Samaporn
Ridden-Harper, R
Foley, R J
Morozova, V
Kilpatrick, C D
Dimitriadis, G
DeMarchi, L
Gagliano, A
Jacobson-Galán, W V
Messick, A
Pierel, J D R
Piro, A L
Ramirez-Ruiz, E
Siebert, M R
Chambers, K C
Clever, K E
Coulter, D A
De, K
Hankins, M
Hung, T
Source :
Monthly Notices of the Royal Astronomical Society; May2022, Vol. 512 Issue 2, p2777-2797, 21p
Publication Year :
2022

Abstract

We present observations of SN 2020fqv, a Virgo-cluster type II core-collapse supernova (CCSN) with a high temporal resolution light curve from the Transiting Exoplanet Survey Satellite (TESS) covering the time of explosion; ultraviolet (UV) spectroscopy from the Hubble Space Telescope (HST) starting 3.3 d post-explosion; ground-based spectroscopic observations starting 1.1 d post-explosion; along with extensive photometric observations. Massive stars have complicated mass-loss histories leading up to their death as CCSNe, creating circumstellar medium (CSM) with which the SNe interact. Observations during the first few days post-explosion can provide important information about the mass-loss rate during the late stages of stellar evolution. Model fits to the quasi-bolometric light curve of SN 2020fqv reveal  0.23 M<subscript>⊙</subscript> of CSM confined within  1450 R<subscript>⊙</subscript> (10<superscript>14</superscript> cm) from its progenitor star. Early spectra (<4 d post-explosion), both from HST and ground-based observatories, show emission features from high-ionization metal species from the outer, optically thin part of this CSM. We find that the CSM is consistent with an eruption caused by the injection of ∼5 × 10<superscript>46</superscript> erg into the stellar envelope ∼300 d pre-explosion, potentially from a nuclear burning instability at the onset of oxygen burning. Light-curve fitting, nebular spectroscopy, and pre-explosion HST imaging consistently point to a red supergiant (RSG) progenitor with |$M_{\rm ZAMS}\approx 13.5\!-\!15 \, \mathrm{M}_{\odot }$|⁠ , typical for SN II progenitor stars. This finding demonstrates that a typical RSG, like the progenitor of SN 2020fqv, has a complicated mass-loss history immediately before core collapse. [ABSTRACT FROM AUTHOR]

Details

Language :
English
ISSN :
00358711
Volume :
512
Issue :
2
Database :
Complementary Index
Journal :
Monthly Notices of the Royal Astronomical Society
Publication Type :
Academic Journal
Accession number :
156217733
Full Text :
https://doi.org/10.1093/mnras/stab2887