J/MNRAS/482/384 Core-collapse supernovae ages and metallicities (Xiao+, 2019)
Core-collapse supernovae ages and metallicities from emission-line diagnostics
of nearby stellar populations.
Xiao L., Galbany L., Eldridge J.J., Stanway E.R.
<Mon. Not. R. Astron. Soc., 482, 384-401 (2019)>
=2019MNRAS.482..384X 2019MNRAS.482..384X (SIMBAD/NED BibCode)
ADC_Keywords: Stars, double and multiple ; Supernovae ; H II regions ; Galaxies
Keywords: binaries: general - supernovae: general - HII regions -
galaxies: general
Abstract:
Massive stars are the main objects that illuminate HII regions and
they evolve quickly to end their lives in core-collapse supernovae
(CCSNe). Thus, it is important to investigate the association between
CCSNe and HII regions. In this paper, we present emission-line
diagnostics of the stellar populations around nearby CCSNe, which
include their host HII regions, from the Potsdam Multi-Aperture
Spectrophotometer (PMAS)/PPak integral-field supernova hosts
compilation (PISCO). We then use bpass stellar population models to
determine the age, metallicity and gas parameters for HII regions
associated with CCSNe, contrasting models that either consider
single-star evolution alone or incorporate interacting binaries. We
find that binary-star models, which allow for ionizing photon loss,
provide a more realistic fit to the observed CCSN hosts, with
metallicities that are closer to those derived from the oxygen
abundance in O3N2. We also find that Type II and Type Ibc SNe arise
from progenitor stars of similar age, mostly from 7 to 45Myr, which
corresponds to stars with masses =<20M☉. However, these two
types of SNe have little variations in their host environment
metallicity measured by oxygen abundance or in progenitor initial
mass. We note that at lower metallicities the SNe are more likely to
be Type II.
Description:
The sample of HII regions with CCSN hosts used in this work comes from
PISCO (Galbany et al. 2018ApJ...855..107G 2018ApJ...855..107G, Cat. J/ApJ/855/107), which
started as an extension of the Calar Alto Legacy Integral Field Area
(CALIFA) survey targeting low-mass SN host galaxies that were missing
in the CALIFA mother sample. So, the instrumental configuration,
observations and reduction are performed following CALIFA procedures
and reduction pipeline. All of this information is well established
and is available in Galbany et al. (2018ApJ...855..107G 2018ApJ...855..107G, Cat.
J/ApJ/855/107) and references therein, as well as in the third CALIFA
data release (Sanchez et al. 2016A&A...594A..36S 2016A&A...594A..36S, Cat. J/A+A/594/A36,
and references therein), including sky subtraction and flux
calibration.
The observational sample we use consists of 152 CCSNe with 107 SNe II
and 45 SNe Ibc, and their observed flux is derived within 1kpc2
centred at the SN location. This is to provide us with adequate S/N in
our spectra, while limiting the observation to the likely host stellar
population around the SN site and preventing the varying distance to
the host galaxy from causing artefacts in our analysis.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
tablea1.dat 103 152 Best-fitting parameters for the no-leakage case
for each CCSN host HII region, from single-star
and binary-star populations
tablea2.dat 103 152 Best-fitting parameters for the leakage case
for each CCSN host HII region, from single-star
and binary-star populations
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Byte-by-byte Description of file: tablea1.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 13 A13 --- Name Supernova name
15- 21 A7 --- Type Supernova type
23- 26 F4.2 [yr] logAgeSNL Age of the inner ionizing stellar
population source from single-star model
best fit for the no-leakage case
28- 31 F4.2 [yr] e_logAgeSNL Error on logAgeSNL
33- 36 F4.2 [cm-3] lognHSNL Hydrogen density from single-star model
best fit for the no-leakage case
38- 41 F4.2 [cm-3] e_lognHSNL Error on lognHSNL
43- 47 F5.2 [-] logUSNL Ionization parameter from single-star model
best fit for the no-leakage case
49- 52 F4.2 [-] e_logUSNL Error on logUSNL
54- 57 F4.2 [-] log(O/H)SNL Oxygen abundance 12+log(O/H) from
single-star model best fit for the
no-leakage case
59- 62 F4.2 [-] e_log(O/H)SNL Error on log(O/H)SNL
64- 67 F4.2 [yr] logAgeBNL Age of the inner ionizing stellar
population source from binary-star model
best fit for the no-leakage case
69- 72 F4.2 [yr] e_logAgeBNL Error on logAgeBNL
74- 77 F4.2 [cm-3] lognHBNL Hydrogen density from binary-star model
best fit for the no-leakage case
79- 82 F4.2 [cm-3] e_lognHBNL Error on lognHBNL
84- 88 F5.2 [-] logUBNL Ionization parameter from binary-star model
best fit for the no-leakage case
90- 93 F4.2 [-] e_logUBNL Error on logUBNL
95- 98 F4.2 [-] log(O/H)BNL Oxygen abundance 12+log(O/H) from
binary-star model best fit for the
no-leakage case
100-103 F4.2 [-] e_log(O/H)BNL Error on log(O/H)BNL
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tablea2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 13 A13 --- Name Supernova name
15- 21 A7 --- Type Supernova type
23- 26 F4.2 [yr] logAgeSL Age of the inner ionizing stellar population
source from single-star model best fit for
the leakage case
28- 31 F4.2 [yr] e_logAgeSL Error on logAgeSL
33- 36 F4.2 [cm-3] lognHSL Hydrogen density from single-star model best
fit for the leakage case
38- 41 F4.2 [cm-3] e_lognHSL Error on lognHSL
43- 47 F5.2 [-] logUSL Ionization parameter from single-star model
best fit for the leakage case
49- 52 F4.2 [-] e_logUSL Error on logUSL
54- 57 F4.2 [-] log(O/H)SL Oxygen abundance 12+log(O/H) from
single-star model best fit for the leakage
case
59- 62 F4.2 [-] e_log(O/H)SL Error on log(O/H)SL
64- 67 F4.2 [yr] logAgeBL Age of the inner ionizing stellar population
source from binary-star model best fit for
the leakage case
69- 72 F4.2 [yr] e_logAgeBL Error on logAgeBL
74- 77 F4.2 [cm-3] lognHBL Hydrogen density from binary-star model best
fit for the leakage case
79- 82 F4.2 [cm-3] e_lognHBL Error on lognHBL
84- 88 F5.2 [-] logUBL Ionization parameter from binary-star model
best fit for the leakage case
90- 93 F4.2 [-] e_logUBL Error on logUBL
95- 98 F4.2 [-] log(O/H)BL Oxygen abundance 12+log(O/H) from
binary-star model best fit for the leakage
case
100-103 F4.2 [-] e_log(O/H)BL Error on log(O/H)BL
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History:
From electronic version of the journal
(End) Ana Fiallos [CDS] 20-Jun-2022