J/ApJ/854/24 Environmental dependence of SN Ia luminosities (Kim+, 2018)
Environmental dependence of type Ia supernova luminosities from a sample without
a local-global difference in host star formation.
Kim Y.-L., Smith M., Sullivan M., Lee Y.-W.
<Astrophys. J., 854, 24 (2018)>
=2018ApJ...854...24K 2018ApJ...854...24K
ADC_Keywords: Supernovae; Surveys; Redshifts; Stars, masses
Keywords: cosmology: observations ; distance scale ; supernovae: general
Abstract:
It is established that there is a dependence of the luminosity of type
Ia supernovae (SNe Ia) on environment: SNe Ia in young, star-forming,
metal-poor stellar populations appear fainter after light-curve shape
corrections than those in older, passive, metal-rich environments.
This is accounted for in cosmological studies using a global property
of the SN host galaxy, typically the host galaxy stellar mass.
However, recent low-redshift studies suggest that this effect
manifests itself most strongly when using the local star formation
rate (SFR) at the SN location, rather than the global SFR or the
stellar mass of the host galaxy. At high-redshift, such local SFRs are
difficult to determine; here, we show that an equivalent local
correction can be made by restricting the SN Ia sample in globally
star-forming host galaxies to a low-mass host galaxy subset
(≤1010M☉). Comparing this sample of SNe Ia (in locally
star-forming environments) to those in locally passive host galaxies,
we find that SNe Ia in locally star-forming environments are
0.081+/0.018 mag fainter (4.5σ), consistent with the result
reported by Rigault+ (2013A&A...560A..66R 2013A&A...560A..66R), but our conclusion is
based on a sample ∼5 times larger over a wider redshift range. This is
a larger difference than when splitting the SN Ia sample based on
global host galaxy SFR or host galaxy stellar mass. This method can be
used in ongoing and future high-redshift SN surveys, where local SN Ia
environments are difficult to determine.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 63 657 YOnsei Nearby Supernova Evolution Investigation
(YONSEI) Supernova Catalog (Kim+ 2015PKAS...30..485K 2015PKAS...30..485K ;
Kang+ 2016ApJS..223....7K 2016ApJS..223....7K) and host "global" properties
table3.dat 73 110 Host stellar mass and "local" properties for
the low-z sample
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See also:
B/sn : Asiago Supernova Catalogue (Barbon et al., 1999-)
J/AJ/112/2408 : Light Curves of 29 SNe (Hamuy+ 1996)
J/AJ/131/527 : UBVRI light curves of 44 type Ia supernovae (Jha+, 2006)
J/ApJ/666/674 : ESSENCE supernova survey (Miknaitis+, 2007)
J/ApJ/700/331 : Light curves of type Ia supernovae (CfA3) (Hicken+, 2009)
J/ApJ/707/1449 : Local hosts of SNe Ia (Neill+, 2009)
J/AJ/139/519 : Carnegie supernova project. SNe Ia (Contreras+, 2010)
J/A+A/523/A7 : Light curves of type Ia supernovae in SNLS (Guy+, 2010)
J/ApJ/722/566 : Host galaxies of SNIa in SDSS-II SN survey (Lampeitl+, 2010)
J/MNRAS/406/782 : Type Ia supernovae luminosities (Sullivan+, 2010)
J/ApJS/192/1 : Light-curve parameters from the SNLS (Conley+, 2011)
J/ApJ/740/92 : SN.Ia host galaxies properties (Gupta+, 2011)
J/AJ/142/156 : The CSP (DR2): photometry of SNe Ia (Stritzinger+, 2011)
J/ApJS/200/12 : CfA4: light curves for 94 type Ia SNe (Hicken+, 2012)
J/ApJ/755/61 : SN Ia host galaxies SFR from SDSS-II (Smith+, 2012)
J/MNRAS/435/1680 : SN Ia host galaxy properties (Johansson+, 2013)
J/A+A/568/A22 : Joint analysis of the SDSS-II & SNLS SNe Ia (Betoule+, 2014)
J/MNRAS/438/1391 : Host galaxies of Type Ia SN from PTF (Pan+, 2014)
J/MNRAS/450/905 : New SNe in SDSS DR9 (Graur+, 2015)
J/ApJ/812/31 : Local Star Formation effects on type Ia SNe (Jones+, 2015)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 6 A6 --- Name Supernova name
8- 11 A4 --- Survey Survey name (1)
13- 17 F5.3 --- z [0.01/0.9] Redshift in the CMB frame
19- 24 F6.3 mag SALT2HR [-1/0.8] SALT2 Hubble residual
26- 30 F5.3 mag e_SALT2HR [0.04/1.1] Uncertainty in SALT2HR
32- 36 F5.2 [Msun] logM* [7.6/12.2] Log global host galaxy
stellar mass
38- 41 F4.2 [Msun] e_logM* [0/1.5] Lower uncertainty in logM*
43- 46 F4.2 [Msun] E_logM* [0/1.1] Upper uncertainty in logM*
48- 53 F6.2 [yr-1] logsSFR [-21.2/-8] Log global specific star
formation rate
55- 58 F4.2 [yr-1] e_logsSFR [0/4] Lower uncertainty in logsSFR
60- 63 F4.2 [yr-1] E_logsSFR [0/4] Upper uncertainty in logsSFR
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Note (1): Survey as follows:
LOWZ = low-redshift SN surveys: Hamuy+ 1996, J/AJ/112/2408 ;
Riess+ 1999AJ....117..707R 1999AJ....117..707R ; Jha+ 2006, J/AJ/131/527 ;
Hicken+ 2009, J/ApJ/700/331 ; 2012, J/ApJS/200/12 ;
Contreras+ 2010, J/AJ/139/519 ; Stritzinger+ 2011, J/AJ/142/156
(89 occurrences)
SDSS = the SDSS-II SN survey: Sako+ 2018PASP..130f4002S 2018PASP..130f4002S (355 occurrences)
SNLS = the first three years of the Canada-France-Hawaii Telescope
Supernova Legacy Survey: Guy+ 2010, J/A+A/523/A7 (213 occurrences)
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 A6 --- Name Supernova name
8- 12 F5.3 --- z [0.01/0.08] Redshift in the CMB frame
14- 18 F5.2 [Msun] logM* [7.5/12.3] Log global host galaxy
stellar mass
20- 23 F4.2 [Msun] e_logM* [0.02/1.5] Lower uncertainty in logM*
25- 28 F4.2 [Msun] E_logM* [0.02/1.6] Upper uncertainty in logM*
30- 31 A2 --- Class Global Host Class (Pa=passive,
43 occurrences or
SF=Star-Forming, 67 occurrences)
33- 37 F5.2 [Msun/kpc2/yr] logSFR-R15 [-5.8/0]? Log local star formation
rate surface density(1)
39- 43 F5.2 [Msun/kpc2/yr] e_logSFR-R15 [0.1/99]? Lower uncertainty in
logSFR-R15
45- 48 F4.2 [Msun/kpc2/yr] E_logSFR-R15 [0/0.6]? Upper uncertainty in
logSFR-R15
50- 52 I3 % P-R15 [0/100]? Probability that SN has a
locally passive environment (1)
54- 58 F5.2 [Msun/kpc2/yr] logSFR-J15 [-4.6/-1]? Log local star formation
rate surface density (2)
60- 64 F5.2 [Msun/kpc2/yr] e_logSFR-J15 [0.03/99]? Lower uncertainty in
logSFR-J15
66- 69 F4.2 [Msun/kpc2/yr] E_logSFR-J15 [0/0.4]? Lower uncertainty in
logSFR-J15
71- 73 I3 % P-J15 [0/100]? Probability that SN has a
locally passive environment (2)
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Note (1): As determined by Ringault et al. (2015ApJ...802...20R 2015ApJ...802...20R).
Note (2): As determined by Jones et al. (2015, J/ApJ/812/31).
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History:
From electronic version of the journal
(End) Prepared by [AAS], Emmanuelle Perret [CDS] 07-Nov-2018