Near-IR Type Ia SN distances: host galaxy extinction and mass-step corrections revisited

Johansson, J.; Cenko, S. B.; Fox, O. D.; Dhawan, S.; Goobar, A.; Stanishev, V.; Butler, N.; Lee, W. H.; Watson, A. M.; Fremling, U. C.; Kasliwal, M. M.; Nugent, P. E.; Petrushevska, T.; Sollerman, J.; Yan, L.; Burke, J.; Hosseinzadeh, G.; Howell, D. A.; McCully, C.; Valenti, S.

doi:10.48550/arxiv.2105.06236

Cited by 3 publications

(6 citation statements)

References 81 publications

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“…For more distant galaxies, observed SNIa colors highlight the observed diversity in extinction properties, ranging from R BV V ∼ 1 to values consistent with the MW average (see Krisciunas et al 2006;Nobili & Goobar 2008;Goobar et al 2014;Amanullah et al 2014Amanullah et al , 2015Burns et al 2018, and references therein). For the SNe Ia in the Hubble flow, color corrections are based on the SALT2 lightcurve fitter (Guy et al 2007), which again differ from the CCM parameterization, but are most consistent with values of R BV V ∼ 2.5 (see e.g., Biswas et al 2021, and references therein), although dust extinction differences between host galaxy environments has been suggested as an explanation for a systematic "mass step" in the derived distances (Brout & Scolnic 2021;Johansson et al 2021).…”

Section: Revisiting Dust Extinction Correctionsmentioning

confidence: 91%

Sensitivity of the Hubble Constant Determination to Cepheid Calibration

Mortsell,

Goobar,

Johansson

et al. 2021

Preprint

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Motivated by the large observed diversity in the properties of extra-galactic extinction by dust, we reanalyse the Cepheid calibration used to infer the local value of the Hubble constant, H 0 , from Type Ia supernovae. Unlike the SH0ES team, we do not enforce a universal color-luminosity relation to correct the near-IR Cepheid magnitudes. Instead, we focus on a data driven method, where the measured colors of the Cepheids are used to derive a color-luminosity relation for each galaxy individually. We present two different analyses, one based on Wesenheit magnitudes, a common practice in the field that attempts to combine corrections from both extinction and variations in intrinsic colors, resulting in H 0 = 66.9 ± 2.5 km/s/Mpc, in agreement with the Planck value. In the second approach, we calibrate using color excesses with respect to derived average intrinsic colors, yielding H 0 = 71.8 ± 1.6 km/s/Mpc, a 2.7 σ tension with the value inferred from the cosmic microwave background.Hence, we argue that systematic uncertainties related to the choice of Cepheid color-luminosity calibration method currently inhibits us from measuring H 0 to the precision required to claim a substantial tension with Planck data.

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Section: Revisiting Dust Extinction Correctionsmentioning

confidence: 91%

Sensitivity of the Hubble Constant Determination to Cepheid Calibration

Mortsell,

Goobar,

Johansson

et al. 2021

Preprint

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“…Brout & Scolnic 2021) for the step. However, Burns et al (2018) and Johansson et al (2021) find reduced or zero evidence for a mass step in the NIR or when accounting properly for dust in the optical. Furthermore, Johansson et al (2021) were unable to reproduce the findings of the contradicting papers (Ponder et al 2020;Thorp et al 2021;Uddin et al 2020) and note that these papers may be affected by the biased collection of NIR samples largely at high host stellar mass.…”

Section: Introductionmentioning

confidence: 98%

“…Second, it could explain why bluer, un-extinguished, type Ia SNe tend to make better standard candles (Foley & Kasen 2011;Gonzalez-Gaitan et al 2020;Kelsey et al 2020b;Siebert et al 2020). Lastly it could explain why observations in the NIR are able to achieve less Hubble diagram scatter and smaller 'mass steps' (e.g., Burns et al 2018;Johansson et al 2021), as these observations are less sensitive to dust.…”

Section: Introductionmentioning

confidence: 98%

“…Though recent studies have attempted to prove a direct link between dust and the observed mass step (Burns et al 2018;Ponder et al 2020;Uddin et al 2020;Thorp et al 2021;Johansson et al 2021), they have not reached definitive consensus as of yet. For example, Ponder et al (2020); Uddin et al (2020); Thorp et al (2021) have suggested evidence for the existence of a mass step in the NIR bands which would invalidate dust-based explanations (e.g.…”

Section: Introductionmentioning

confidence: 99%

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The Dark Energy Survey Supernova Program results: type Ia supernova brightness correlates with host galaxy dust

Meldorf

Palmese

Brout

et al. 2022

Monthly Notices of the Royal Astronomical Society

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Cosmological analyses with type Ia supernovae (SNe Ia) often assume a single empirical relation between colour and luminosity (β) and do not account for varying host-galaxy dust properties. However, from studies of dust in large samples of galaxies, it is known that dust attenuation can vary significantly. Here we take advantage of state-of-the-art modeling of galaxy properties to characterize dust parameters (dust attenuation AV, and a parameter describing the dust law slope RV) for 1100 Dark Energy Survey (DES) SN host galaxies. Utilizing optical and infrared data of the hosts alone, we find three key aspects of host dust that impact SN cosmology: 1) there exists a large range (∼1 − 6) of host RV 2) high stellar mass hosts have RV on average ∼0.7 lower than that of low-mass hosts 3) for a subsample of 81 spectroscopically classified SNe there is a significant (>3σ) correlation between the Hubble diagram residuals of red SNe Ia and the host RV that when corrected for reduces scatter by $\sim 13{{\%}}$ and the significance of the ‘mass step’ to ∼1σ. These represent independent confirmations of recent predictions based on dust that attempted to explain the puzzling ‘mass step’ and intrinsic scatter (σint) in SN Ia analyses.

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“…An alternative origin of the observed effect is based on a scenario where the parameter R W could vary across different sightlines and different galaxy distances, morphologies, environments and properties. Dust extinction differences between galaxies could be the origin for a systematic "mass step" (at ∼ 10 10 M ) in the data [179,180]: after standardization, SnIa in a high-mass galaxy appear brighter than those in a low-mass galaxy [76,[181][182][183][184][185]. Such an alternative scenario is testable using the methods presented here and it could also lead to a resolution of the Hubble tension.…”

Section: Conclusion-discussionmentioning

confidence: 81%

Hubble tension or a transition of the Cepheid SnIa calibrator parameters?

Perivolaropoulos,

Skara

2021

Preprint

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We re-analyze the Cepheid data used to infer the value of the Hubble constant H0 by calibrating Type Ia supernovae. We do not enforce a universal value of the empirical Cepheid calibration parameters RW (Cepheid Wesenheit color-luminosity parameter) and M W H (Cepheid Wesenheit Hband absolute magnitude). Instead we allow for variation of either of these parameters for each individual galaxy. We also consider the case where these parameters have two universal values: one for low galactic distances D < Dc and one for high galactic distances D > Dc where Dc is a critical transition distance. We find hints for a 3σ level mismatch between the low and high galactic distance parameter values. We then use model selection criteria (AIC and BIC) which penalize models with large numbers of parameters, to compare and rank the following types of RW and M W H parameter variations: Base models: Universal values for RW and M W H (no parameter variation), I: Individual fitted galactic RW with one universal fitted M W H , II: One universal fixed RW with individual fitted galactic M W H , III: One universal fitted RW with individual fitted galactic M W H , IV: Two universal fitted RW (near and far) with one universal fitted M W H , V: One universal fitted RW with two universal fitted M W H (near and far), VI: Two universal fitted RW (near and far) with two universal fitted M WH (near and far). We find that the AIC and BIC model selection criteria consistently favor model IV instead of the commonly used Base model where no variation is allowed for the Cepheid empirical parameters. The best fit value of the SnIa absolute magnitude MB and of H0 implied by the favored model IV is consistent with the inverse distance ladder calibration based on the CMB sound horizon H0 = 67.4 ± 0.5 km s −1 M pc −1 . Thus in the context of the favored model IV the Hubble crisis is not present. This model may imply the presence of a fundamental physics transition taking place at a time more recent than 100 M yrs ago.

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Near-IR Type Ia SN distances: host galaxy extinction and mass-step corrections revisited

Cited by 3 publications

References 81 publications

Sensitivity of the Hubble Constant Determination to Cepheid Calibration

Sensitivity of the Hubble Constant Determination to Cepheid Calibration

The Dark Energy Survey Supernova Program results: type Ia supernova brightness correlates with host galaxy dust

Hubble tension or a transition of the Cepheid SnIa calibrator parameters?

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