A galaxy-driven model of type Ia supernova luminosity variations

DES Collaboration

doi:10.1093/mnras/stac1984

A galaxy-driven model of type Ia supernova luminosity variations

DES Collaboration

Workflow Systems

Research output: Contribution to journal › Article › peer-review

14 Scopus citations

Abstract

Type Ia supernovae (SNe Ia) are used as standardizable candles to measure cosmological distances, but differences remain in their corrected luminosities which display a magnitude step as a function of host galaxy properties such as stellar mass and rest-frame U-R colour. Identifying the cause of these steps is key to cosmological analyses and provides insight into SN physics. Here we investigate the effects of SN progenitor ages on their light-curve properties using a galaxy-based forward model that we compare to the Dark Energy Survey 5-yr SN Ia sample. We trace SN Ia progenitors through time and draw their light-curve width parameters from a bimodal distribution according to their age. We find that an intrinsic luminosity difference between SNe of different ages cannot explain the observed trend between step size and SN colour. The data split by stellar mass are better reproduced by following recent work implementing a step in total-to-selective dust extinction ratio (RV) between low- and high-mass hosts, although an additional intrinsic luminosity step is still required to explain the data split by host galaxy U-R. Modelling the RV step as a function of galaxy age provides a better match overall. Additional age versus luminosity steps marginally improve the match to the data, although most of the step is absorbed by the width versus luminosity coefficient α. Furthermore, we find no evidence that α varies with SN age.

Original language	English
Pages (from-to)	4587-4605
Number of pages	19
Journal	Monthly Notices of the Royal Astronomical Society
Volume	515
Issue number	3
DOIs	https://doi.org/10.1093/mnras/stac1984
State	Published - Sep 1 2022

Funding

We thank the referee Mickael Rigault for comments which significantly impro v ed this paper. P.W. acknowledges support from the Science and Technology Facilities Council (STFC) grant ST/R000506/1. MS acknowledges support from EU/FP7-ERC grant 615929. LK thanks the UKRI Future Leaders Fellowship for support through the grant MR/T01881X/1. LG acknowledges financial support from the Spanish Ministerio de Ciencia e Innovacion (MCIN), the Agencia Estatal de Investigacion (AEI) 10.13039/501100011033, and the European Social Fund (ESF) 'Investing in your future' under the 2019 Ramon y Cajal program RYC2019-027683-I and the PID2020115253GA-I00 HOSTFLOWS project, from Centro Superior de Investigaciones Cientýficas (CSIC) under the PIE project 20215AT016, and the program Unidad de Excelencia Marýa de Maeztu CEX2020001058-M. This project has received funding from the European Research Council (ERC) under the European Union's Horizon 2020 research and innovation program (grant agreement number 759194 USNAC). 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 of Cosmological Physics at the University of Chicago, the Center for Cosmology and Astro-Particle Physics at the Ohio State University, the Mitchell Institute for Fundamental Physics and Astronomy at Te xas A&M Univ ersity, Financiadora de Estudos e Projetos, Fundaçao Carlos Chagas Filho de Amparo `a Pesquisa do Estado do Rio de Janeiro, Conselho Nacional de Desenvolvimento Cientýfico e Tecnologico and the Ministerio da Ciencia, Tecnologia e Inovaçao, the Deutsche Forschungsgemeinschaft, and the Collaborating Institutions in the Dark Energy Surv e y. The Collaborating Institutions are Argonne National Laboratory, the University of California at Santa Cruz, the University of Cambridge, Centro de Investigaciones Energeticas, Medioambientales y Tecnologicas-Madrid, the University of Chicago, University College London, the DES-Brazil Consortium, the University of Edinburgh, the Eidgen ¨ossische Technische Hochschule (ETH) Z ¨urich, Fermi National Accelerator Laboratory, the University of Illinois at UrbanaChampaign, the Institut de Ci `encies de l'Espai (IEEC/CSIC), the Institut de Fýsica d'Altes Energies, Lawrence Berkeley National Laboratory, the Ludwig-Maximilians Universit ¨at M ¨unchen and the associated Excellence Cluster Universe, the University of Michigan, NSF's NOIRLab, the University of Nottingham, The Ohio State University, the University of Pennsylvania, the University of Portsmouth, SLAC National Accelerator Laboratory, Stanford Uni versity, the Uni versity 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-20160597, 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 Se venth Frame work Program (FP7/2007-2013) including ERC grant agreements 240672, 291329, and 306478. We acknowledge support from the Brazilian Instituto Nacional de Ciencia e Tecnologia (INCT) do e-Universo (CNPq grant 465376/2014-2). This manuscript has been authored by Fermi Research Alliance, LLC under Contract No. DE-AC02-07CH11359 with the U.S. Department of Energy, Office of Science, Office of High Energy Physics.

Funders	Funder number
Brazilian Instituto Nacional de Ciencia e Tecnologia
Centro Superior de Investigaciones Cientýficas	20215AT016
Collaborating Institutions are Argonne National Laboratory
Collaborating Institutions in the Dark Energy Surv e y
Fermi Research Alliance, LLC	DE-AC02-07CH11359
Institut de Ci `encies de l'Espai
MCIN
Mitchell Institute for Fundamental Physics and Astronomy at Te xas A&M Univ ersity
Science and Technology Facilities Council of the United Kingdom
Spanish Ministerio de Ciencia e Innovacion
Uni versity of Sussex, Texas A&M University	2012B-0001
Unidad de Excelencia Marýa de Maeztu CEX2020001058-M
National Science Foundation	AST-1138766, AST-1536171
U.S. Department of Energy
Stanford University
Office of Science
High Energy Physics
Fermilab
Lawrence Berkeley National Laboratory
University of California, Santa Cruz
University of Pennsylvania
Ohio State University
University of Chicago
University of Michigan
University of Portsmouth
University of Illinois System
National Centre for Supercomputing Applications
Horizon 2020 Framework Programme
SLAC National Accelerator Laboratory
Higher Education Funding Council for England
UK Research and Innovation	MR/T01881X/1
Science and Technology Facilities Council	615929, ST/R000506/1
University College London
European Commission
European Research Council
University of Nottingham
University of Edinburgh
Deutsche Forschungsgemeinschaft
Generalitat de Catalunya	FP7/2007-2013, 240672, 306478, 291329
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, PGC2018-094773, PGC2018-102021, SEV-20160597, ESP2017-89838
European Social Fund	PID2020115253GA-I00, RYC2019-027683-I
Instituto Nacional de Ciência e Tecnologia para Excitotoxicidade e Neuroproteção
Horizon 2020	759194
Ministry of Education and Science of Ukraine
European Regional Development Fund
Agencia Estatal de Investigación
Neurosciences Foundation
Institut de Física d'Altes Energies

Keywords

cosmology: observations
dust, extinction
galaxies: evolution
supernovae: general

Access to Document

10.1093/mnras/stac1984

Cite this

@article{08390cf7bbfc4120b1e85e03c2828b74,

title = "A galaxy-driven model of type Ia supernova luminosity variations",

abstract = "Type Ia supernovae (SNe Ia) are used as standardizable candles to measure cosmological distances, but differences remain in their corrected luminosities which display a magnitude step as a function of host galaxy properties such as stellar mass and rest-frame U-R colour. Identifying the cause of these steps is key to cosmological analyses and provides insight into SN physics. Here we investigate the effects of SN progenitor ages on their light-curve properties using a galaxy-based forward model that we compare to the Dark Energy Survey 5-yr SN Ia sample. We trace SN Ia progenitors through time and draw their light-curve width parameters from a bimodal distribution according to their age. We find that an intrinsic luminosity difference between SNe of different ages cannot explain the observed trend between step size and SN colour. The data split by stellar mass are better reproduced by following recent work implementing a step in total-to-selective dust extinction ratio (RV) between low- and high-mass hosts, although an additional intrinsic luminosity step is still required to explain the data split by host galaxy U-R. Modelling the RV step as a function of galaxy age provides a better match overall. Additional age versus luminosity steps marginally improve the match to the data, although most of the step is absorbed by the width versus luminosity coefficient α. Furthermore, we find no evidence that α varies with SN age.",

keywords = "cosmology: observations, dust, extinction, galaxies: evolution, supernovae: general",

author = "{DES Collaboration} and P. Wiseman and M. Vincenzi and M. Sullivan and L. Kelsey and B. Popovic and B. Rose and D. Brout and Davis, {T. M.} and C. Frohmaier and L. Galbany and C. Lidman and A. Moller and D. Scolnic and M. Smith and M. Aguena and S. Allam and F. Andrade-Oliveira and J. Annis and E. Bertin and S. Bocquet and D. Brooks and Burke, {D. L.} and {Carnero Rosell}, A. and {Carrasco Kind}, M. and J. Carretero and Castander, {F. J.} and M. Costanzi and Pereira, {M. E.S.} and S. Desai and Diehl, {H. T.} and P. Doel and S. Everett and I. Ferrero and D. Friedel and J. Frieman and J. Garcia-Bellido and M. Gatti and E. Gaztanaga and D. Gruen and J. Gschwend and G. Gutierrez and Hinton, {S. R.} and Hollowood, {D. L.} and K. Honscheid and James, {D. J.} and M. March and F. Menanteau and R. Miquel and R. Morgan and E. Suchyta",

note = "Publisher Copyright: {\textcopyright} 2022 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society.",

year = "2022",

month = sep,

day = "1",

doi = "10.1093/mnras/stac1984",

language = "English",

volume = "515",

pages = "4587--4605",

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

issn = "0035-8711",

publisher = "Oxford University Press",

number = "3",

}

TY - JOUR

T1 - A galaxy-driven model of type Ia supernova luminosity variations

AU - DES Collaboration

AU - Wiseman, P.

AU - Vincenzi, M.

AU - Sullivan, M.

AU - Kelsey, L.

AU - Popovic, B.

AU - Rose, B.

AU - Brout, D.

AU - Davis, T. M.

AU - Frohmaier, C.

AU - Galbany, L.

AU - Lidman, C.

AU - Moller, A.

AU - Scolnic, D.

AU - Smith, M.

AU - Aguena, M.

AU - Allam, S.

AU - Andrade-Oliveira, F.

AU - Annis, J.

AU - Bertin, E.

AU - Bocquet, S.

AU - Brooks, D.

AU - Burke, D. L.

AU - Carnero Rosell, A.

AU - Carrasco Kind, M.

AU - Carretero, J.

AU - Castander, F. J.

AU - Costanzi, M.

AU - Pereira, M. E.S.

AU - Desai, S.

AU - Diehl, H. T.

AU - Doel, P.

AU - Everett, S.

AU - Ferrero, I.

AU - Friedel, D.

AU - Frieman, J.

AU - Garcia-Bellido, J.

AU - Gatti, M.

AU - Gaztanaga, E.

AU - Gruen, D.

AU - Gschwend, J.

AU - Gutierrez, G.

AU - Hinton, S. R.

AU - Hollowood, D. L.

AU - Honscheid, K.

AU - James, D. J.

AU - March, M.

AU - Menanteau, F.

AU - Miquel, R.

AU - Morgan, R.

AU - Suchyta, E.

PY - 2022/9/1

Y1 - 2022/9/1

N2 - Type Ia supernovae (SNe Ia) are used as standardizable candles to measure cosmological distances, but differences remain in their corrected luminosities which display a magnitude step as a function of host galaxy properties such as stellar mass and rest-frame U-R colour. Identifying the cause of these steps is key to cosmological analyses and provides insight into SN physics. Here we investigate the effects of SN progenitor ages on their light-curve properties using a galaxy-based forward model that we compare to the Dark Energy Survey 5-yr SN Ia sample. We trace SN Ia progenitors through time and draw their light-curve width parameters from a bimodal distribution according to their age. We find that an intrinsic luminosity difference between SNe of different ages cannot explain the observed trend between step size and SN colour. The data split by stellar mass are better reproduced by following recent work implementing a step in total-to-selective dust extinction ratio (RV) between low- and high-mass hosts, although an additional intrinsic luminosity step is still required to explain the data split by host galaxy U-R. Modelling the RV step as a function of galaxy age provides a better match overall. Additional age versus luminosity steps marginally improve the match to the data, although most of the step is absorbed by the width versus luminosity coefficient α. Furthermore, we find no evidence that α varies with SN age.

AB - Type Ia supernovae (SNe Ia) are used as standardizable candles to measure cosmological distances, but differences remain in their corrected luminosities which display a magnitude step as a function of host galaxy properties such as stellar mass and rest-frame U-R colour. Identifying the cause of these steps is key to cosmological analyses and provides insight into SN physics. Here we investigate the effects of SN progenitor ages on their light-curve properties using a galaxy-based forward model that we compare to the Dark Energy Survey 5-yr SN Ia sample. We trace SN Ia progenitors through time and draw their light-curve width parameters from a bimodal distribution according to their age. We find that an intrinsic luminosity difference between SNe of different ages cannot explain the observed trend between step size and SN colour. The data split by stellar mass are better reproduced by following recent work implementing a step in total-to-selective dust extinction ratio (RV) between low- and high-mass hosts, although an additional intrinsic luminosity step is still required to explain the data split by host galaxy U-R. Modelling the RV step as a function of galaxy age provides a better match overall. Additional age versus luminosity steps marginally improve the match to the data, although most of the step is absorbed by the width versus luminosity coefficient α. Furthermore, we find no evidence that α varies with SN age.

KW - cosmology: observations

KW - dust, extinction

KW - galaxies: evolution

KW - supernovae: general

UR - http://www.scopus.com/inward/record.url?scp=85140963316&partnerID=8YFLogxK

U2 - 10.1093/mnras/stac1984

DO - 10.1093/mnras/stac1984

M3 - Article

AN - SCOPUS:85140963316

SN - 0035-8711

VL - 515

SP - 4587

EP - 4605

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 3

ER -

A galaxy-driven model of type Ia supernova luminosity variations

Abstract

Funding

Keywords

Access to Document

Other files and links

Fingerprint

Cite this