J/MNRAS/509/5275 SNe Ia type LF study (Sharon+, 2022)
The ZTF-BTS Type Ia supernovae luminosity function is consistent with
a single progenitor channel for the explosions.
Sharon A., Kushnir D.
<Mon. Not. R. Astron. Soc. 509, 5275-5297>
=2022MNRAS.509.5275S 2022MNRAS.509.5275S (SIMBAD/NED BibCode)
ADC_Keywords: Supernovae ; Galaxies ; Optical ; Infrared ; Photometry, UBV ;
Photometry, ugriz ; Magnitudes, absolute
Keywords: methods: data analysis - surveys - supernovae: general
Abstract:
We construct the Type Ia supernovae (SNe Ia) luminosity function (LF)
using the Zwicky Transient Facility Bright Transient Survey (BTS)
catalogue. While this magnitude-limited survey has an unprecedented
number of objects, it suffers from large distance uncertainties and
lacks an estimation of host extinction. We bypass these issues by
calculating the intrinsic luminosities from the shape parameters of
the light curve's g and r bands, with the luminosities calibrated from
the well observed SNe Ia sample of the Carnegie Supernova Project,
allowing us to construct, for the first time, the intrinsic LF of SNe
Ia. We then use a novel tight relation between the colour stretch and
the synthesized 56Ni mass, MNi56, to determine the MNi56 distribution
of SNe Ia. We find that the LFs are unimodal, with their peaks in line
with previous results, but have a much lower rate of dim events and
luminous events. We show that the features on top of the unimodal
LF-derived distributions are all compatible with statistical noise,
consistent with a single progenitor channel for the explosions. We
further derive, for the first time, the SNe Ia distribution of host
galaxy extinction, and find a mean selective extinction of E(B-V) ~=
0.1 and a non-negligible fraction with large, >1mag, extinction in the
optical bands. The high extinction is typical for luminous SNe,
supporting their young population origin.
Description:
In this work, we use a combination of the ZTF-BTS (Zwicky Transient
Facility - Bright Transient Survey) public catalogue and the CSP
(Carnegie Supernova Project) Ia sample to accurately determine the
intrinsic LF of SNe Ia. We first compare in the pseudo light curve
shapes (luminosity curves are also reconstructed in the section 5
Luminosity function constructed from the colour stretch parameter and
in the appendix C Construction of the LF and volume corrections) of
the CSP and the BTS in order to correlate colour stretch parameter,
decline rates, peak magnitudes and synthesized 56Ni mass in the sloan
g and r bands (i.e section 2 BTS-CSP Comparison, section 3
Determination of the colour stretch parameter and section 6 THE 56NI
Mass distribution). Results are presented in the tabled1.dat for CSP
sample and in the tabled3.dat for the ZTF-BTS sample.
Hereafter, we use CSP Johnson filters B- and V-band data to study LOSS
(Lick Observatory Supernova Search) SNe Ia pseudo-LF similarly to
previous BTS LF. Details on procedure and results are presented in the
appendix A. We exhibit these results in the tabled2.dat for CSP
Johnson sample and in the tabled4.dat for LOSS Johnson sample.
File Summary:
--------------------------------------------------------------------------------
FileName Lrecl Records Explanations
--------------------------------------------------------------------------------
ReadMe 80 . This file
tabled1.dat 96 87 CSP SNe Ia sample sloan filters g- and r-band
colour stretches, decline rates, and luminosity
parameters
tabled2.dat 90 81 CSP SNe Ia sample Johnson filters B- and V-band
colour stretches, decline rates, and luminosity
parameters
tabled3.dat 96 1519 ZTF BTS SNe Ia sample sloan filters g- and
r-band colour stretches, decline rates and
luminosity parameters
tabled4.dat 87 63 LOSS SNe Ia sample Johnson filters B- and V-band
colour stretches and decline rates
--------------------------------------------------------------------------------
See also:
J/ApJ/869/56 : Updated calibration of the CSP-I SNe Ia sample (Burns+,2018)
J/MNRAS/412/1419 : Nearby supernova rates (Leaman+, 2011)
J/ApJ/895/32 : Zwicky Transient Facility BTS. I. (Fremling+, 2020)
J/MNRAS/412/1441 : SNe luminosity functions (Li+, 2011)
https://sites.astro.caltech.edu/ztf/bts/explorer.php : ZTF-BTS sample explorer
https://www.wis-tns.org/ : Transient name server home page
https://ned.ipac.caltech.edu/ : NED home page
https://www.sdss.org/ : SDSS home page
Byte-by-byte Description of file: tabled1.dat
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Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 A6 --- SN Supernova name (YYYYAA) (name) (1)
8- 11 F4.2 --- sgr ?=- The colour stretch parameter sgr
(sgr) (G1)
13- 16 F4.2 --- e_sgr ?=- Mean uncertainty of sgr (e_sgr)
18- 22 A5 --- n_sgr The source for the sgr value (sgr_src) (G2)
24- 27 F4.2 mag dm15g ?=- Magnitude difference between day 1 and
day 5 from the peak magnitude of the g band
(dm15g)
29- 32 F4.2 mag e_dm15g ?=- Mean uncertainty of dm15g (e_dm15g)
34- 37 F4.2 mag dm15r ?=- Magnitude difference between day 1 and
day 5 from the peak magnitude of the r band
(dm15r)
39- 42 F4.2 mag e_dm15r ?=- Mean uncertainty of dm15r (e_dm15r)
44- 47 F4.2 mag dm8g ?=- Magnitude difference between day 8 and
day 0 from the peak magnitude of the g band
(dm8g)
49- 52 F4.2 mag e_dm8g ?=- Mean uncertainty of dm8g (e_dm8g)
54- 57 F4.2 mag dm30r ?=- Magnitude difference between day 3 and
day 0 from the peak magnitude of the r band
(dm30r)
59- 62 F4.2 mag e_dm30r ?=- Mean uncertainty of dm30r (e_dm30r)
64- 69 F6.2 mag PeakgMag ?=- Peak of absolute magnitude Mg reported
in the g band (peak_g)
71- 74 F4.2 mag e_PeakgMag ?=- Mean uncertainty of PeakgMag (errpeakg)
76- 81 F6.2 mag PeakrMag Peak of absolute magnitude Mr reported in
the r band (peak_r)
83- 86 F4.2 mag e_PeakrMag Mean uncertainty of PeakrMag (errpeakr)
88- 91 F4.2 Msun MNi56 ?=- Synthesized 56Ni mass MNi56 (M_Ni) (2)
93- 96 F4.2 Msun e_MNi56 ?=- Mean uncertainty of MNi56 (eMNi)
--------------------------------------------------------------------------------
Note (1): Name format is equivalent to those from SNe survey is the Carnegie
Supernova Project (CSP; Burns et al. 2018ApJ...869...56B 2018ApJ...869...56B,
Cat. J/ApJ/869/56).
Note (2): As explained in the section 6 THE 56 NI Mass distribution we
transform the distributions calculated to a MNi56 distribution,
which is more useful for constraining models. We obtain relation
between sgr, MNi56 and Δm_15(B) as in the equations 7 and 8
of this section. This is done by using the CSP sample to calibrate
a relation between sgr and MNi56. We use the sample of 20 SNe
from Sharon & Kushnir (2020MNRAS.496.4517S 2020MNRAS.496.4517S) with derived MNi56,
supplemented with an additional 5 SNe, where MNi56 is calculated
using the methods of Sharon & Kushnir (2020MNRAS.496.4517S 2020MNRAS.496.4517S). The
bolometric luminosity, photometry, and processed photometry for the
additional SNe is given in the supplementary material. The obtained
relation between sgr and MNi56 is shown in the middle panel of
Figure 1 (i.e introduction section). As can be seen in the figure,
sgr and MNi56 are tightly correlated, and the best fit of the
polynomial form in the equation 7 (section 6 THE 56 NI Mass
distribution).
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Byte-by-byte Description of file: tabled2.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 A6 --- SN Supernova name (YYYYAA) (name) (1)
8- 11 F4.2 --- sBV ?=- The colour stretch parameter sBV (sBV)
(2)
13- 16 F4.2 --- e_sBV ?=- Mean uncertainty of sgr (e_sBV)
18- 21 F4.2 mag dm15B ?=- Magnitude difference between day 1 and
day 5 from the peak magnitude of the B band
(dm15B)
23- 26 F4.2 mag e_dm15B ?=- Mean uncertainty of dm15B (e_dm15B)
28- 31 F4.2 mag dm15V ?=- Magnitude difference between day 1 and
day 5 from the peak magnitude of the V band
(dm15V)
33- 36 F4.2 mag e_dm15V ?=- Mean uncertainty of dm15V (e_dm15V)
38- 41 F4.2 mag dm8B ?=- Magnitude difference between day 8 and
day 0 from the peak magnitude of the B band
(dm8B)
43- 46 F4.2 mag e_dm8B ?=- Mean uncertainty of dm8B (e_dm8B)
48- 51 F4.2 mag dm30V ?=- Magnitude difference between day 3 and
day 0 from the peak magnitude of the V band
(dm30V)
53- 56 F4.2 mag e_dm30V ?=- Mean uncertainty of dm30V (e_dm30V)
58- 63 F6.2 mag PeakBMag ?=- Peak of absolute magnitude MB reported
in the B band (peak_B)
65- 68 F4.2 mag e_PeakBMag ?=- Mean uncertainty of PeakBMag (errpeakB)
70- 75 F6.2 mag PeakVMag ?=- Peak of absolute magnitude MV reported
in the V band (peak_V)
77- 80 F4.2 mag e_PeakVMag ?=- Mean uncertainty of PeakVMag (errpeakV)
82- 85 F4.2 Msun MNi56 ?=- Synthesized 56Ni mass MNi56 (M_Ni) (3)
87- 90 F4.2 Msun e_MNi56 ?=- Mean uncertainty of MNi56 (eMNi)
--------------------------------------------------------------------------------
Note (1): Name format is equivalent to those from SNe survey is the Carnegie
Supernova Project (CSP; Burns et al. 2018ApJ...869...56B 2018ApJ...869...56B,
Cat. J/ApJ/869/56).
Note (2): As shown in the section 2 BTS-CSP Comparison, the parameter sBV is
obtained by measuring the time difference between the B band peak time
and the B-V colour peak time as sBV = tmax,B-V - t_max,B / 30d.
Note (3): As explained in the section 6 THE 56 NI Mass distribution we
transform the distributions calculated to a MNi56 distribution,
which is more useful for constraining models. We obtain relation
between sgr, MNi56 and Δm_15(B) as in the equations 7 and 8
of this section. This is done by using the CSP sample to calibrate
a relation between sBV and MNi56. For B magnitude Johnson filter,
we use Piro et al. (2014MNRAS.438.3456P 2014MNRAS.438.3456P) constructed the MNi56
distribution using the volume-limited LOSS survey
(Leaman et al. 2011MNRAS.412.1419L 2011MNRAS.412.1419L, Cat. J/MNRAS/412/1419; Li et al.
2011MNRAS.412.1441L 2011MNRAS.412.1441L, J/MNRAS/412/1441). MNi56 was estimated from
the B-band decline rate, Δm15(B), using the equation 8 of the
section 6 THE 56 NI Mass distribution. As explained in the appendix A,
we use observations in the B and V bands of the CSP sample to relate
the colour stretch sBV to MNi56 and to the peak magnitudes. We use a
second-order polynomial for MNi56 as the equation A1 of this
section shows.
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Byte-by-byte Description of file: tabled3.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 8 A8 --- SN Supernova name (YYYYAAAA) (name) (1)
10- 14 F5.3 --- sgr ?=- The colour stretch parameter sgr
(sgr) (G1)
16- 20 F5.3 --- e_sgr ?=- Mean uncertainty of sgr (e_sgr)
22- 26 A5 --- n_sgr The source for the sgr value (sgr_src) (G2)
28- 32 F5.3 mag dm15g ?=- Magnitude difference between day 1 and
day 5 from the peak magnitude of the g band
(dm15g)
34- 38 F5.3 mag e_dm15g ?=- Mean uncertainty of dm15g (e_dm15g)
40- 44 F5.3 mag dm15r ?=- Magnitude difference between day 1 and
day 5 from the peak magnitude of the r band
(dm15r)
46- 50 F5.3 mag e_dm15r ?=- Mean uncertainty of dm15r (e_dm15r)
52- 56 F5.3 mag dm8g ?=- Magnitude difference between day 8 and
day 0 from the peak magnitude of the g band
(dm8g)
58- 62 F5.3 mag e_dm8g ?=- Mean uncertainty of dm8g (e_dm8g)
64- 68 F5.3 mag dm30r ?=- Magnitude difference between day 3 and
day 0 from the peak magnitude of the r band
(dm30r)
70- 74 F5.3 mag e_dm30r ?=- Mean uncertainty of dm30r (e_dm30r)
76- 81 F6.2 Mpc D ?=- The distance to the SNe (dist) (2)
83 I1 --- LFflag Flag indicating if the SN is within
the time range of the LF (lf_flag)
85- 90 F6.2 mag iMag ?=- Absolute i magnitude of the host galaxy
(hostabs)
92- 96 F5.2 mag g-i ?=- g - i colour of the host galaxy (hostcol)
--------------------------------------------------------------------------------
Note (1): The ZTF BTS public catalogue (Fremling et al. 2020ApJ...895...32F 2020ApJ...895...32F,
Cat. J/ApJ/895/32; Perley et al. 2020ApJ...904...35P 2020ApJ...904...35P) includes, for
each transient, the light curves in the g and r bands, the observed
peak magnitude, the galactic extinction in the direction of the
transient and the redshift.
ZTF BTS data are available in
https://sites.astro.caltech.edu/ztf/bts/explorer.php,
here data were downloaded on July 2021, with 1519 SNe Ia that passed
the quality cuts described in P20 (Perley et al. 2020ApJ...904...35P 2020ApJ...904...35P).
Note (2): Calculated from the spectroscopic redshift, if available. If not, it
is estimated from the peak magnitudes absolute and observed
magnitudes. SNe without sgr or without observed peak magnitudes
in both bands do not have an estimated distance.
Concerning redshifts, as explained in section 2 BTS-CSP Comparison,
we use the NASA Extragalactic Database (NED,
https://ned.ipac.caltech.edu/) and the Sloan Digital Sky Survey (SDSS,
https://www.sdss.org/) catalogues, we obtained the spectroscopic
redshift of ≃ 35 per cent of the SNe.
--------------------------------------------------------------------------------
Byte-by-byte Description of file: tabled4.dat
--------------------------------------------------------------------------------
Bytes Format Units Label Explanations
--------------------------------------------------------------------------------
1- 6 A6 --- SN Supernova name (YYYYAA) (name) (1)
8- 13 F6.4 --- sBV ?=- The colour stretch parameter sBV (sBV)
(2)
15- 21 F7.5 --- e_sBV ?=- Mean uncertainty of sgr (e_sBV)
23- 27 A5 --- n_sBV The source for the sgr value (sgr_sBV) (3)
29- 34 F6.4 mag dm15B ?=- Magnitude difference between day 1 and
day 5 from the peak magnitude of the B band
(dm15B)
36- 41 F6.4 mag e_dm15B ?=- Mean uncertainty of dm15B (e_dm15B)
43- 48 F6.4 mag dm15V ?=- Magnitude difference between day 1 and
day 5 from the peak magnitude of the V band
(dm15V)
50- 55 F6.4 mag e_dm15V ?=- Mean uncertainty of dm15V (e_dm15V)
57- 62 F6.4 mag dm8B ?=- Magnitude difference between day 8 and
day 0 from the peak magnitude of the B band
(dm8B)
64- 69 F6.4 mag e_dm8B ?=- Mean uncertainty of dm8B (e_dm8B)
71- 75 F5.3 mag dm30V ?=- Magnitude difference between day 3 and
day 0 from the peak magnitude of the V band
(dm30V)
77- 82 F6.4 mag e_dm30V ?=- Mean uncertainty of dm30V (e_dm30V)
84- 87 F4.1 Mpc D ?=- The distance of the host galaxy (dist) (4)
--------------------------------------------------------------------------------
Note (1): Name format is equivalent to those from SNe the volume-limited LOSS
survey (Leaman et al. 2011MNRAS.412.1419L 2011MNRAS.412.1419L, Cat. J/MNRAS/412/1419;
Li et al. 2011MNRAS.412.1441L 2011MNRAS.412.1441L, Cat. J/MNRAS/412/1441).
Note (2): As shown in the section 2 BTS-CSP Comparison, the parameter sBV is
obtained by measuring the time difference between the B band peak time
and the B-V colour peak time as sBV = tmax,B-V - t_max,B / 30d or
by polynomial fits from decline rate values (i.e see section 3
Determination of the colour stretch parameter and figure A1 of the
appendix A).
Note (3): The source options are as follows:
dir = Directly from the light curve
dm15V = From polynomial fit with Δm_15(V) parameter measured as
the equation 4 of the section 3 Determination of the colour
stretch parameter shows
dm8B = From polynomial fit with Δm_80(B) parameter measured as
the equation 4 of the section 3 Determination of the colour
stretch parameter shows
none = Data not available
Note (4): Distance to the host galaxy, as given in Li et al.
(2011MNRAS.412.1441L 2011MNRAS.412.1441L, Cat. J/MNRAS/412/1441).
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Global notes:
Note (G1): As shown in the section 2 BTS-CSP Comparison, the parameter sgr is
obtained by measuring the time difference between the g band peak
time and the g-r colour peak time as
sgr = tmax,g-r - tmax,g / 30d.
If it not possible, we proceed to polynomial fits from decline rate
values (i.e see section 3 Determination of the colour stretch
parameter).
Note (G2): The source options are as follows:
dir = Directly from the light curve
dm15r = From polynomial fit with Δm_15(r) parameter measured as
the equation 4 of the section 3 Determination of the colour
stretch parameter shows
dm30r = From polynomial fit with Δm_30(r) parameter measured as
the equation 4 of the section 3 Determination of the colour
stretch parameter shows
dm8g = From polynomial fit with Δm_80(g) parameter measured as
the equation 4 of the section 3 Determination of the colour
stretch parameter shows
dm15g = From polynomial fit with Δm_15(g) parameter measured as
the equation 4 of the section 3 Determination of the colour
stretch parameter shows
none = Data not available
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History:
From electronic version of the journal
(End) Luc Trabelsi [CDS] 07-Oct-2024