Rates and delay times of Type Ia supernovae in the Dark Energy Survey

DES Collaboration

doi:10.1093/mnras/stab1943

Rates and delay times of Type Ia supernovae in the Dark Energy Survey

DES Collaboration

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Abstract

We use a sample of 809 photometrically classified Type Ia supernovae (SNe Ia) discovered by the Dark Energy Survey (DES) along with 40 415 field galaxies to calculate the rate of SNe Ia per galaxy in the redshift range 0.2 < z < 0.6. We recover the known correlation between SN Ia rate and galaxy stellar mass across a broad range of scales 8.5 ≤ log (M∗/M⊙) ≤ 11.25. We find that the SN Ia rate increases with stellar mass as a power law with index 0.63 ± 0.02, which is consistent with the previous work. We use an empirical model of stellar mass assembly to estimate the average star formation histories (SFHs) of galaxies across the stellar mass range of our measurement. Combining the modelled SFHs with the SN Ia rates to estimate constraints on the SN Ia delay time distribution (DTD), we find that the data are fit well by a power-law DTD with slope index β = -1.13 ± 0.05 and normalization A = 2.11 ± 0.05 × 10-13 SNe M⊙-1 yr-1, which corresponds to an overall SN Ia production efficiency NIa/M∗ = 0.9-0.7+4.0 × 10-3SNe M⊙-1. Upon splitting the SN sample by properties of the light curves, we find a strong dependence on DTD slope with the SN decline rate, with slower-declining SNe exhibiting a steeper DTD slope. We interpret this as a result of a relationship between intrinsic luminosity and progenitor age, and explore the implications of the result in the context of SN Ia progenitors.

Original language	English
Pages (from-to)	3330-3348
Number of pages	19
Journal	Monthly Notices of the Royal Astronomical Society
Volume	506
Issue number	3
DOIs	https://doi.org/10.1093/mnras/stab1943
State	Published - Sep 1 2021

Funding

We thank J. Michael Burgess for discussions regarding model fitting in Stan. We thank the reviewer, Mickael Rigault, for constructive comments on the manuscript. PW acknowledges support from the Science and Technology Facilities Council (STFC) grant ST/R000506/1. MSu and MSm acknowledge support from EU/FP7-ERC grant 615929. MSm is funded by the European Research Council (ERC) under the European Union's Horizon 2020 Framework Programme (grant agreement no 759194 - USNAC). LG acknowledges financial support from the Spanish Ministry of Science, Innovation and Universities (MICIU) under the 2019 Ramón y Cajal program RYC2019-027683 and from the Spanish MICIU project PID2020-115253GA-I00. Funding for the DES Projects has been provided by the U.S. Department of Energy, the U.S. National Science Foundation, the Ministry of Science and Education of Spain, the Science and Technology Facilities Council of the United Kingdom, the Higher Education Funding Council for England, the National Center for Supercomputing Applications at the University of Illinois at Urbana- Champaign, the Kavli Institute for Cosmological Physics at the University of Chicago, the Center for Cosmology and AstroParticle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University, Financiadora de Estudos e Projetos, Fundaç ão Carlos Chagas Filho de Amparo `a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Científico e Tecnológico and the Ministério da Ciência, Tecnologia e Inovaç ão, the Deutsche Forschungsgemeinschaft and the Collaborating Institutions in the Dark Energy Survey. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energéticas, Medioambientales y Tecnológicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgenössische Technische Hochschule (ETH) Zürich, Fermi NationalAccelerator Laboratory, theUniversity of Illinois atUrbana- Champaign, the Institut de Cìencies de l'Espai (IEEC/CSIC), the Institut de Física d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universität München and the associated Excellence Cluster Universe, the University of Michigan, NFS's NOIRLab, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford University, the University of Sussex, Texas A&M University, and the OzDES Membership Consortium. Based in part on observations at Cerro Tololo Inter-American Observatory at NSF's NOIRLab (NOIRLab Prop. ID 2012B-0001; PI: J. Frieman), which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. The DES data management system is supported by the National Science Foundation under grant numbers AST-1138766 and AST-1536171. The DES participants from Spanish institutions are partially supported by MICINN under grants ESP2017-89838, PGC2018-094773, PGC2018-102021, SEV-2016-0588, SEV-2016- 0597, and MDM-2015-0509, some of which include ERDF funds from the European Union. IFAE is partially funded by the CERCA program of the Generalitat de Catalunya. Research leading to these results has received funding from the European Research Council under the European Union's Seventh Framework Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciência e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2).

Funders	Funder number
Brazilian Instituto Nacional de Ciência e Tecnologia
Collaborating Institutions are Argonne National Laboratory
Collaborating Institutions in the Dark Energy Survey
EU/FP7-ERC	615929
European Union's Horizon 2020 Framework Programme	759194 - USNAC
Fermi NationalAccelerator Laboratory
Institut de Cìencies de l'Espai
Mitchell Institute for Fundamental Physics and Astronomy at Texas A&M University
Science and Technology Facilities Council of the United Kingdom
National Science Foundation	2012B-0001, AST-1138766, AST-1536171
U.S. Department of Energy
Stanford University
Lawrence Berkeley National Laboratory
University of California, Santa Cruz
University of Pennsylvania
Ohio State University
University of Chicago
University of Michigan
Texas A and M University
University of Portsmouth
Seventh Framework Programme	240672, 306478, 291329
SLAC National Accelerator Laboratory
Higher Education Funding Council for England
Ministerio de Ciencia, Innovación y Universidades	PID2020-115253GA-I00, RYC2019-027683
Kavli Institute for Cosmological Physics, University of Chicago
Science and Technology Facilities Council	ST/R000506/1
University College London
European Commission
European Research Council
University of Nottingham
University of Sussex
University of Edinburgh
Deutsche Forschungsgemeinschaft
Generalitat de Catalunya
Eidgenössische Technische Hochschule Zürich
Ministério da Ciência, Tecnologia e Inovação
Conselho Nacional de Desenvolvimento Científico e Tecnológico	465376/2014-2
Fundação Carlos Chagas Filho de Amparo à Pesquisa do Estado do Rio de Janeiro
Financiadora de Estudos e Projetos
Ministerio de Ciencia e Innovación	SEV-2016-0588, MDM-2015-0509, SEV-2016- 0597, PGC2018-094773, PGC2018-102021, ESP2017-89838
Seventh Framework Programme
Ludwig-Maximilians-Universität München
Instituto Nacional de Ciência e Tecnologia para Excitotoxicidade e Neuroproteção
Ministry of Education and Science of Ukraine
European Regional Development Fund
Institut de Física d'Altes Energies

Keywords

galaxies: evolution
supernovae: general
white dwarfs

Access to Document

10.1093/mnras/stab1943

Cite this

@article{eb313d3c343d4377a2f8a8adc20bf17b,

title = "Rates and delay times of Type Ia supernovae in the Dark Energy Survey",

abstract = "We use a sample of 809 photometrically classified Type Ia supernovae (SNe Ia) discovered by the Dark Energy Survey (DES) along with 40 415 field galaxies to calculate the rate of SNe Ia per galaxy in the redshift range 0.2 < z < 0.6. We recover the known correlation between SN Ia rate and galaxy stellar mass across a broad range of scales 8.5 ≤ log (M∗/M⊙) ≤ 11.25. We find that the SN Ia rate increases with stellar mass as a power law with index 0.63 ± 0.02, which is consistent with the previous work. We use an empirical model of stellar mass assembly to estimate the average star formation histories (SFHs) of galaxies across the stellar mass range of our measurement. Combining the modelled SFHs with the SN Ia rates to estimate constraints on the SN Ia delay time distribution (DTD), we find that the data are fit well by a power-law DTD with slope index β = -1.13 ± 0.05 and normalization A = 2.11 ± 0.05 × 10-13 SNe M⊙-1 yr-1, which corresponds to an overall SN Ia production efficiency NIa/M∗ = 0.9-0.7+4.0 × 10-3SNe M⊙-1. Upon splitting the SN sample by properties of the light curves, we find a strong dependence on DTD slope with the SN decline rate, with slower-declining SNe exhibiting a steeper DTD slope. We interpret this as a result of a relationship between intrinsic luminosity and progenitor age, and explore the implications of the result in the context of SN Ia progenitors.",

keywords = "galaxies: evolution, supernovae: general, white dwarfs",

author = "{DES Collaboration} and P. Wiseman and M. Sullivan and M. Smith and C. Frohmaier and M. Vincenzi and O. Graur and B. Popovic and P. Armstrong and D. Brout and Davis, {T. M.} and L. Galbany and Hinton, {S. R.} and L. Kelsey and R. Kessler and C. Lidman and A. M{\"o}ller and Nichol, {R. C.} and B. Rose and D. Scolnic and M. Toy and Z. Zontou and J. Asorey and D. Carollo and K. Glazebrook and Lewis, {G. F.} and Tucker, {B. E.} and Abbott, {T. M.C.} and M. Aguena and S. Allam and F. Andrade-Oliveira and J. Annis and D. Bacon and E. Bertin and D. Brooks and E. Buckley-Geer and Burke, {D. L.} and Rosell, {A. Carnero} and Kind, {M. Carrasco} and J. Carretero and M. Costanzi and {Da Costa}, {L. N.} and Pereira, {M. E.S.} and S. Desai and Diehl, {H. T.} and P. Doel and S. Everett and I. Ferrero and B. Flaugher and P. Fosalba and E. Suchyta",

note = "Publisher Copyright: {\textcopyright} 2021 The Author(s) Published by Oxford University Press on behalf of Royal Astronomical Society.",

year = "2021",

month = sep,

day = "1",

doi = "10.1093/mnras/stab1943",

language = "English",

volume = "506",

pages = "3330--3348",

journal = "Monthly Notices of the Royal Astronomical Society",

issn = "0035-8711",

publisher = "Oxford University Press",

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T1 - Rates and delay times of Type Ia supernovae in the Dark Energy Survey

AU - DES Collaboration

AU - Wiseman, P.

AU - Sullivan, M.

AU - Smith, M.

AU - Frohmaier, C.

AU - Vincenzi, M.

AU - Graur, O.

AU - Popovic, B.

AU - Armstrong, P.

AU - Brout, D.

AU - Davis, T. M.

AU - Galbany, L.

AU - Hinton, S. R.

AU - Kelsey, L.

AU - Kessler, R.

AU - Lidman, C.

AU - Möller, A.

AU - Nichol, R. C.

AU - Rose, B.

AU - Scolnic, D.

AU - Toy, M.

AU - Zontou, Z.

AU - Asorey, J.

AU - Carollo, D.

AU - Glazebrook, K.

AU - Lewis, G. F.

AU - Tucker, B. E.

AU - Abbott, T. M.C.

AU - Aguena, M.

AU - Allam, S.

AU - Andrade-Oliveira, F.

AU - Annis, J.

AU - Bacon, D.

AU - Bertin, E.

AU - Brooks, D.

AU - Buckley-Geer, E.

AU - Burke, D. L.

AU - Rosell, A. Carnero

AU - Kind, M. Carrasco

AU - Carretero, J.

AU - Costanzi, M.

AU - Da Costa, L. N.

AU - Pereira, M. E.S.

AU - Desai, S.

AU - Diehl, H. T.

AU - Doel, P.

AU - Everett, S.

AU - Ferrero, I.

AU - Flaugher, B.

AU - Fosalba, P.

AU - Suchyta, E.

PY - 2021/9/1

Y1 - 2021/9/1

N2 - We use a sample of 809 photometrically classified Type Ia supernovae (SNe Ia) discovered by the Dark Energy Survey (DES) along with 40 415 field galaxies to calculate the rate of SNe Ia per galaxy in the redshift range 0.2 < z < 0.6. We recover the known correlation between SN Ia rate and galaxy stellar mass across a broad range of scales 8.5 ≤ log (M∗/M⊙) ≤ 11.25. We find that the SN Ia rate increases with stellar mass as a power law with index 0.63 ± 0.02, which is consistent with the previous work. We use an empirical model of stellar mass assembly to estimate the average star formation histories (SFHs) of galaxies across the stellar mass range of our measurement. Combining the modelled SFHs with the SN Ia rates to estimate constraints on the SN Ia delay time distribution (DTD), we find that the data are fit well by a power-law DTD with slope index β = -1.13 ± 0.05 and normalization A = 2.11 ± 0.05 × 10-13 SNe M⊙-1 yr-1, which corresponds to an overall SN Ia production efficiency NIa/M∗ = 0.9-0.7+4.0 × 10-3SNe M⊙-1. Upon splitting the SN sample by properties of the light curves, we find a strong dependence on DTD slope with the SN decline rate, with slower-declining SNe exhibiting a steeper DTD slope. We interpret this as a result of a relationship between intrinsic luminosity and progenitor age, and explore the implications of the result in the context of SN Ia progenitors.

AB - We use a sample of 809 photometrically classified Type Ia supernovae (SNe Ia) discovered by the Dark Energy Survey (DES) along with 40 415 field galaxies to calculate the rate of SNe Ia per galaxy in the redshift range 0.2 < z < 0.6. We recover the known correlation between SN Ia rate and galaxy stellar mass across a broad range of scales 8.5 ≤ log (M∗/M⊙) ≤ 11.25. We find that the SN Ia rate increases with stellar mass as a power law with index 0.63 ± 0.02, which is consistent with the previous work. We use an empirical model of stellar mass assembly to estimate the average star formation histories (SFHs) of galaxies across the stellar mass range of our measurement. Combining the modelled SFHs with the SN Ia rates to estimate constraints on the SN Ia delay time distribution (DTD), we find that the data are fit well by a power-law DTD with slope index β = -1.13 ± 0.05 and normalization A = 2.11 ± 0.05 × 10-13 SNe M⊙-1 yr-1, which corresponds to an overall SN Ia production efficiency NIa/M∗ = 0.9-0.7+4.0 × 10-3SNe M⊙-1. Upon splitting the SN sample by properties of the light curves, we find a strong dependence on DTD slope with the SN decline rate, with slower-declining SNe exhibiting a steeper DTD slope. We interpret this as a result of a relationship between intrinsic luminosity and progenitor age, and explore the implications of the result in the context of SN Ia progenitors.

KW - galaxies: evolution

KW - supernovae: general

KW - white dwarfs

UR - http://www.scopus.com/inward/record.url?scp=85112567786&partnerID=8YFLogxK

U2 - 10.1093/mnras/stab1943

DO - 10.1093/mnras/stab1943

M3 - Review article

AN - SCOPUS:85112567786

SN - 0035-8711

VL - 506

SP - 3330

EP - 3348

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 3

ER -

Rates and delay times of Type Ia supernovae in the Dark Energy Survey

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