J/MNRAS/438/1391 Host galaxies of Type Ia SN from PTF (Pan+, 2014)
The host galaxies of Type Ia supernovae discovered by the Palomar Transient
Factory.
Pan Y.-C., Sullivan M., Maguire K., Hook I.M., Nugent P.E., Howell D.A.,
Arcavi I., Botyanszki J., Cenko S.B., Derose J., Fakhouri H.K., Gal-Yam A.,
Hsiao E., Kulkarni S.R., Laher R.R., Lidman C., Nordin J., Walker E.S.,
Xu D.
<Mon. Not. R. Astron. Soc., 438, 1391-1416 (2014)>
=2014MNRAS.438.1391P 2014MNRAS.438.1391P
ADC_Keywords: Supernovae
Keywords: supernovae: general - cosmology: observations - distance scale
Abstract:
We present spectroscopic observations of the host galaxies of 82
low-redshift Type Ia supernovae (SNe Ia) discovered by the Palomar
Transient Factory. We determine star formation rates,
gas-phase/stellar metallicities, and stellar masses and ages of these
objects. As expected, strong correlations between the SN Ia
light-curve width (stretch) and the host age/mass/metallicity are
found: fainter, faster declining events tend to be hosted by
older/massive/metal-rich galaxies. There is some evidence that redder
SNe Ia explode in higher metallicity galaxies, but we found no
relation between the SN colour and host galaxy extinction based on the
Balmer decrement, suggesting that the colour variation of these SNe
does not primarily arise from this source. SNe Ia in higher
mass/metallicity galaxies also appear brighter after stretch/colour
corrections than their counterparts in lower mass hosts, and the
stronger correlation is with gas-phase metallicity suggesting this may
be the more important variable. We also compared the host stellar mass
distribution to that in galaxy-targeted SN surveys and the
high-redshift untargeted Supernova Legacy Survey (SNLS). SNLS has many
more low-mass galaxies, while the targeted searches have fewer. This
can be explained by an evolution in the galaxy stellar mass function,
coupled with an SN delay-time distribution proportional to t-1.
Finally, we found no significant difference in the mass-metallicity
relation of our SN Ia hosts compared to field galaxies, suggesting any
metallicity effect on the SN Ia rate is small.
Description:
The SNe Ia studied in this paper were discovered by the PTF, a project
which operated from 2009 to 2012 and used the CFH12k wide-field survey
camera mounted on the Samuel Oschin 48 inch telescope (P48) at the
Palomar Observatory. The observational cadences used to discover the
SNe ranged from hours up to ∼5d. SN candidates were identified in
image subtraction data and ranked using both simple cuts on the
detection parameters and a machine learning algorithm (Bloom et al.
2012PASP..124.1175B 2012PASP..124.1175B), and then visually confirmed by members of the
PTF collaboration or, from mid-2010 onwards, via the citizen science
project 'Galaxy Zoo: Supernova' (Smith et al., 2011MNRAS.412.1309S 2011MNRAS.412.1309S).
The latter identified eight of the SNe studied in this paper.
File Summary:
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FileName Lrecl Records Explanations
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ReadMe 80 . This file
table2.dat 74 90 The observing log of full sample used in this paper
table3.dat 51 82 The SN photometric properties in this paper
table4.dat 46 82 The host photometric properties in this paper
table5.dat 54 82 The host spectroscopic properties in this paper
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See also:
B/sn : Asiago Supernova Catalogue (Barbon et al., 1999-)
Byte-by-byte Description of file: table2.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- SN SN name
11 A1 --- n_SN [c] c: 'Galaxy Zoo Supernovae project'
discovered SNe
13- 14 I2 h RAh Right ascension (J2000)
16- 17 I2 min RAm Right ascension (J2000)
19- 23 F5.2 s RAs Right ascension (J2000)
25 A1 --- DE- Declination sign (J2000)
26- 27 I2 deg DEd Declination (J2000)
29- 30 I2 arcmin DEm Declination (J2000)
32- 35 F4.1 arcsec DEs Declination (J2000)
37- 47 A11 --- Inst Telescope and instrument
49- 52 I4 s texp.r Exposure time for red gratings/grisms
54- 57 I4 s texp.b Exposure time for blue gratings/grisms
59- 64 F6.4 --- zh [0.008/0.09] Heliocentric redshift
66- 71 F6.4 --- zCMB Redshift based on CMB frame
73- 74 I2 --- S/N Signal-to-noise ratio
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Byte-by-byte Description of file: table3.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- SN SN name
12- 20 A9 --- LC Source of light curve (1)
21- 24 F4.2 --- s ? Stretch parameter (2)
26- 29 F4.2 --- e_s ? rms uncertainty on s
31- 35 F5.2 mag col ? B-V colour at B-band maximum light (2)
37- 40 F4.2 mag e_col ? rms uncertainty on C
42- 46 F5.2 mag Bmag ? B magnitude (2)
48- 51 F4.2 mag e_Bmag ? rms uncertainty on Bmag
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Note (1): References are:
P48 = Palomar Transient Factory
P60 = Palomar 60-in
LT = Liverpool Telescope
Note (2): The SN properties derived by SIFTO light-curve fitting code.
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Byte-by-byte Description of file: table4.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- SN SN name
12- 16 F5.2 Msun b_M* ? Lower value of stellar mass interval
18- 22 F5.2 Msun M* Stellar mass (3)
24- 28 F5.2 Msun B_M* ? Upper value of stellar mass interval
30- 34 F5.2 [Msun/yr] b_logSFRp ? Lower value of star formation rate
36- 40 F5.2 [Msun/yr] logSFRp ? Photometric star formation rate (3)
42- 46 F5.2 [Msun/yr] B_logSFRp ? Upper value of star formation rate
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Note (3): The host parameters determined photometrically by z-peg.
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Byte-by-byte Description of file: table5.dat
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Bytes Format Units Label Explanations
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1- 9 A9 --- SN SN name
12- 16 F5.3 [-] e(O) ? Abundance, 12+log(O/H) (4)
18- 22 F5.3 [-] e_e(O) ? rms uncertainty on 12+log(O/H)
24 A1 --- l_logSFRs Limit flag on logSFRs
25- 31 F7.4 [Msun/yr] logSFRs Spectroscopic star formation rate (4)
33- 38 F6.4 [Msun/yr] e_logSFRs ? rms uncertainty on logSFRs
40- 45 F6.3 [Sun] [M/H] ? Metallicity (4)
47- 52 F6.3 [Gyr] logAge ? Age (4)
54 I1 --- AGN [0/1] AGN tag for the host galaxy:
0=normal galaxy, 1=AGN host
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Note (4): The host parameters determined either from emission line or stellar
continuum measurements.
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History:
From electronic version of the journal
(End) Patricia Vannier [CDS] 30-Nov-2014