Constraining the SN Ia host galaxy dust law distribution and mass step: hierarchical <scp>BayeSN</scp> analysis of optical and near-infrared light curves

Thorp, Stephen; Mandel, Kaisey S.

doi:10.1093/mnras/stac2714

Cited by 15 publications

(4 citation statements)

References 138 publications

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“…SNe probe extinction much more precisely than our spatially averaged measurements, approaching the point-source probes provided by ordinary stars. Thorp & Mandel (2022) used a hierarchical Bayesian approach to address the possibility of unphysical ranges of R retrieved in SN samples due to observational error, finding R = 2.2-2.6 for Type Ia SNe in the Carnegie Supernova project. They contrast this with R = 1.9 from fits to individual SNe from Johansson et al (2021).…”

Section: Discussionmentioning

confidence: 99%

JWST’s PEARLS: Dust Attenuation and Gravitational Lensing in the Backlit-galaxy System VV 191

Keel

Windhorst

Jansen

et al. 2023

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We derive the spatial and wavelength behavior of dust attenuation in the multiple-armed spiral galaxy VV 191b using backlighting by the superimposed elliptical system VV 191a in a pair with an exceptionally favorable geometry for this measurement. Imaging using the James Webb Space Telescope and Hubble Space Telescope spans the wavelength range 0.3–4.5 μm with high angular resolution, tracing the dust in detail from 0.6–1.5 μm. Distinct dust lanes continue well beyond the bright spiral arms, and trace a complex web, with a very sharp radial cutoff near 1.7 Petrosian radii. We present attenuation profiles and coverage statistics in each band at radii 14–21 kpc. We derive the attenuation law with wavelength; the data both within and between the dust lanes clearly favor a stronger reddening behavior (R = A V /E B−V ≈ 2.0 between 0.6 and 0.9 μm, approaching unity by 1.5 μm) than found for starbursts and star-forming regions of galaxies. Power-law extinction behavior ∝λ −β gives β = 2.1 from 0.6–0.9 μm. R decreases at increasing wavelengths (R ≈ 1.1 between 0.9 and 1.5 μm), while β steepens to 2.5. Mixing regions of different column density flattens the wavelength behavior, so these results suggest a different grain population than in our vicinity. The NIRCam images reveal a lens arc and counterimage from a background galaxy at z ≈ 1, spanning 90° azimuthally at 2.″8 from the foreground elliptical-galaxy nucleus, and an additional weakly lensed galaxy. The lens model and imaging data give a mass/light ratio M/L B = 7.6 in solar units within the Einstein radius 2.0 kpc.

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Section: Discussionmentioning

confidence: 99%

JWST’s PEARLS: Dust Attenuation and Gravitational Lensing in the Backlit-galaxy System VV 191

Keel

Windhorst

Jansen

et al. 2023

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“…Other analyses have found conflicting results. By measuring 𝑅 𝑉 for individual SNe Ia using a hierarchical Bayesian model, Thorp et al (2021) and Thorp & Mandel (2022) found no significant difference in the 𝑅 𝑉 population means between SNe in low and high mass galaxies. There is also some evidence that the step remains when measuring distances using near infra-red (NIR) light curves, where the effects of dust should have a smaller impact (Ponder et al 2021;Uddin et al 2020;Jones et al 2022), although, by contrast, Johansson et al (2021) found the step was removed in both the NIR and when fitting each SN Ia for its 𝑅 𝑉 .…”

Section: Introductionmentioning

confidence: 98%

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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“…On the other hand, recent cosmological studies utilizing SN Ia have proposed host stellar mass as a third parameter (Kelly et al 2010), in addition to the light curve shapes (Phillips 1993) and color (Tripp 1998), for the standardization of SN Ia distance (Hamuy et al 1995;Lampeitl et al 2010;Childress et al 2013a), despite the question as to whether it is an intrinsic property or just an effect of dust (Johansson et al 2021;Thorp & Mandel 2022). Although it is not to be addressed here, exploring the star formation-activity-related luminosity functions and mass functions may offer an alternative perspective.…”

Section: Introductionmentioning

confidence: 99%

Luminosity Functions of the Host Galaxies of Supernova

Liang,

Suzuki,

Doi

et al. 2024

ApJ

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We present the luminosity functions and stellar mass functions of supernova (SN) host galaxies and test if they differ from the functions of normal field galaxies. We utilize homogeneous samples consisting of 273 SNe Ia (z ≤ 0.3) and 44 core-collapse (CC) SNe (z ≤ 0.1) from the Sloan Digital Sky Survey II Supernova Survey and the high-signal-to-noise-ratio photometry of galaxies from the Hyper Suprime-Cam Subaru Strategic Program. SN hosts are classified into star-forming and passive galaxy groups based on the spectral energy distribution fitting. We find that the SN host luminosity functions and stellar mass functions deviate from those of normal field galaxies. Star-forming galaxies dominate the low-mass end of the SN Ia host mass function, while passive galaxies dominate the high-mass end. CC SNe are predominantly hosted by star-forming galaxies. In addition, intermediate-mass hosts produce CC SNe with the highest efficiency, while the efficiency of producing SNe Ia monotonically increases as the hosts become more massive. Furthermore, we derive the pseudo mass normalized SN rates (pSNuM) based on the mass functions. We find that the star-forming component of pSNuM Ia is less sensitive to the changes in stellar mass, in comparison with the total rate. The behavior of pSNuM CC suggests that the CC rate is proportional to the star-forming rate.

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Constraining the SN Ia host galaxy dust law distribution and mass step: hierarchical BayeSN analysis of optical and near-infrared light curves

Cited by 15 publications

References 138 publications

JWST’s PEARLS: Dust Attenuation and Gravitational Lensing in the Backlit-galaxy System VV 191

JWST’s PEARLS: Dust Attenuation and Gravitational Lensing in the Backlit-galaxy System VV 191

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

Luminosity Functions of the Host Galaxies of Supernova

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