Stellar Populations in type Ia supernova host galaxies at intermediate-high redshift: Star formation and metallicity enrichment histories

Millán-Irigoyen, I; G., del Valle-Espinosa, M.; Aranda, R. Fernández; Galbany, L.; Gomes, J. M.; Moreno-Raya, M. E.; López-Sánchez, Á. R.; Mollá, M.

doi:10.1093/mnras/stac2696

Cited by 3 publications

(1 citation statement)

References 70 publications

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“…★ E-mail: p.s.wiseman@soton.ac.uk (PW) Lampeitl et al 2010;Sullivan et al 2010), star-formation rate (SFR; Sullivan et al 2010), morphology (Sullivan et al 2003;Hakobyan et al 2020), stellar age (Rose et al 2019(Rose et al , 2021Millán-Irigoyen et al 2022), metallicity (Gallagher et al 2008;Childress et al 2013;Moreno-Raya et al 2016;Millán-Irigoyen et al 2022), or galaxy rest-frame colour (Roman et al 2018;Jones et al 2018;Kelsey et al 2021Kelsey et al , 2022. The relationships usually take the form of a 'step', where the mean standardized luminosities of SNe Ia on different sides of a threshold in a given host galaxy parameter (e.g., a stellar mass of log(𝑀 * /M ) = 10) differ by a fixed amount.…”

Section: Introductionmentioning

confidence: 99%

Further evidence that galaxy age drives observed type Ia supernova luminosity differences

Wiseman¹,

Sullivan²,

Smith³

et al. 2023

Preprint

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Type Ia supernovae (SNe Ia) are explosions of white dwarf stars that facilitate exquisite measurements of cosmological expansion history, but improvements in accuracy and precision are hindered by observational biases. Of particular concern is the apparent difference in the corrected brightnesses of SNe Ia in different host galaxy environments. SNe Ia in more massive, passive, older environments appear brighter after having been standardized by their light-curve properties. The luminosity difference commonly takes the form of a step function. Recent works imply that environmental characteristics that trace the age of the stellar population in the vicinity of SNe show the largest steps. Here we use simulations of SN Ia populations to test the impact of using different tracers and investigate promising new models of the step. We test models with a total-to-selective dust extinction ratio 𝑅 𝑉 that changes between young and old SN Ia host galaxies, as well as an intrinsic luminosity difference between SNe from young and old progenitors. The data are well replicated by a model driven by a galaxy-age varying 𝑅 𝑉 and no intrinsic SN luminosity difference, and we find that specific star-formation rate measured locally to the SN is a relatively pure tracer of this galaxy age difference. We cannot rule out an intrinsic difference causing part of the observed step and show that if luminosity differences are caused by multiple drivers then no single environmental measurement is able to accurately trace them. We encourage the use of multiple tracers in luminosity corrections to negate this issue.

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Section: Introductionmentioning

confidence: 99%

Further evidence that galaxy age drives observed type Ia supernova luminosity differences

Wiseman¹,

Sullivan²,

Smith³

et al. 2023

Preprint

View full text Add to dashboard Cite

show abstract

Further evidence that galaxy age drives observed Type Ia supernova luminosity differences

Wiseman

Sullivan

Smith

et al. 2023

Monthly Notices of the Royal Astronomical Society

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Type Ia supernovae (SNe Ia) are explosions of white dwarf stars that facilitate exquisite measurements of cosmological expansion history, but improvements in accuracy and precision are hindered by observational biases. Of particular concern is the apparent difference in the corrected brightnesses of SNe Ia in different host galaxy environments. SNe Ia in more massive, passive, older environments appear brighter after having been standardized by their light-curve properties. The luminosity difference commonly takes the form of a step function. Recent works imply that environmental characteristics that trace the age of the stellar population in the vicinity of SNe show the largest steps. Here we use simulations of SN Ia populations to test the impact of using different tracers and investigate promising new models of the step. We test models with a total-to-selective dust extinction ratio RV that changes between young and old SN Ia host galaxies, as well as an intrinsic luminosity difference between SNe from young and old progenitors. The data are well replicated by a model driven by a galaxy-age varying RV and no intrinsic SN luminosity difference, and we find that specific star-formation rate measured locally to the SN is a relatively pure tracer of this galaxy age difference. We cannot rule out an intrinsic difference causing part of the observed step and show that if luminosity differences are caused by multiple drivers then no single environmental measurement is able to accurately trace them. We encourage the use of multiple tracers in luminosity corrections to negate this issue.

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Tracing back the birth environments of Type Ia supernova progenitor stars: a pilot study based on 44 early-type host galaxies

Kim,

Galbany,

Hook

et al. 2024

Monthly Notices of the Royal Astronomical Society

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The environmental dependence of Type Ia supernova (SN Ia) luminosities is well established, and efforts are being made to find its origin. Previous studies typically use the currently observed status of the host galaxy. However, given the delay time between the birth of the progenitor star and the SN Ia explosion, the currently observed status may differ from the birth environment of the SN Ia progenitor star. In this paper, employing the chemical evolution and accurately determined stellar population properties of 44 early-type host galaxies, we, for the first time, estimate the SN Ia progenitor star birth environment, specifically [Fe/H]Birth and [α/Fe]Birth. We show that [α/Fe]Birth has a $30.4^{\text{+10.6}}_{-10.1}{{\ \rm per\ cent}}$ wider range than the currently observed [α/Fe]Current, while the range of [Fe/H]Birth is not statistically different ($17.9^{\text{+26.0}}_{-27.1}{{\ \rm per\ cent}}$) to that of [Fe/H]Current. The birth and current environments of [Fe/H] and [α/Fe] are sampled from different populations (p-values of the Kolmogorov–Smirnov test <0.01). We find that light-curve fit parameters are insensitive to [Fe/H]Birth (<0.9σ for the non-zero slope), while a linear trend is observed with Hubble residuals (HRs) at the 2.4σ significance level. With [α/Fe]Birth, no linear trends (<1.1σ) are observed. Interestingly, we find that [α/Fe]Birth clearly splits the SN Ia sample into two groups: SN Ia exploded in [α/Fe]Birth-rich or [α/Fe]Birth-poor environments. SNe Ia exploded in different [α/Fe]Birth groups have different weighted-means of light-curve shape parameters: 0.81 ± 0.33 (2.5σ). They are thought to be drawn from different populations (p-value = 0.01). Regarding SN Ia colour and HRs, there is no difference (<1.0σ) in the weighted-means and distribution (p-value > 0.27) of each [α/Fe]Birth group.

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Stellar Populations in type Ia supernova host galaxies at intermediate-high redshift: Star formation and metallicity enrichment histories

Cited by 3 publications

References 70 publications

Further evidence that galaxy age drives observed type Ia supernova luminosity differences

Further evidence that galaxy age drives observed type Ia supernova luminosity differences

Further evidence that galaxy age drives observed Type Ia supernova luminosity differences

Tracing back the birth environments of Type Ia supernova progenitor stars: a pilot study based on 44 early-type host galaxies

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