Type Ia Supernovae Are Excellent Standard Candles in the Near-infrared

Avelino, Arturo; Friedman, Andrew S.; Mandel, Kaisey S.; Jones, D. O.; Challis, Peter; Kirshner, R.

doi:10.3847/1538-4357/ab2a16

Cited by 48 publications

(52 citation statements)

References 141 publications

(173 reference statements)

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“…Near-infrared (NIR; 1 < λ < 2.5 µm) observations offer many advantages for standardising SNe Ia (Elias et al 1985;Meikle 2000). Not only is the NIR less prone to extinction from dust, but SNe Ia are more naturally standard candles at these wavelengths, requiring no or significantly smaller corrections to their peak luminosity to yield similar precision as compared to the optical (Krisciunas et al 2004;Wood-Vasey et al 2008;Mandel et al 2009;Burns et al 2011;Dhawan et al 2018a;Burns et al 2018;Avelino et al 2019). Theoretical models further corroborate these observations (Kasen 2006;Blondin et al 2015).…”

Section: Introductionmentioning

confidence: 74%

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

Johansson,

Cenko,

Fox

et al. 2021

Preprint

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We present optical and near-infrared (NIR, Y JH-band) observations of 42 Type Ia supernovae (SNe Ia) discovered by the untargeted intermediate Palomar Transient Factory (iPTF) survey. This new data-set covers a broad range of redshifts and host galaxy stellar masses, compared to previous SN Ia efforts in the NIR. We construct a sample, using also literature data at optical and NIR wavelengths, to examine claimed correlations between the host stellar masses and the Hubble diagram residuals. The SN magnitudes are corrected for host galaxy extinction using either a global total-to-selective extinction ratio, R V =2.0 for all SNe, or a best-fit R V for each SN individually. Unlike previous studies which were based on a narrower range in host stellar mass, we do not find evidence for a "mass-step", between the color-and stretch-corrected peak J and H magnitudes for galaxies below and above log(M * /M ) = 10. However, the mass-step remains significant (3σ) at optical wavelengths (g, r, i) when using a global R V , but vanishes when each SN is corrected using their individual best-fit R V . Our study confirms the benefits of the NIR SN Ia distance estimates, as these are largely exempted from the empirical corrections dominating the systematic uncertainties in the optical.

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Section: Introductionmentioning

confidence: 74%

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

Johansson,

Cenko,

Fox

et al. 2021

Preprint

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“…We believe that additional observations and analysis, in particular at NIR wavelengths, are needed to shed light on this problem. Compared to optical LCs, NIR SNe Ia LCs have a narrow luminosity distribution and are less sensitive to host galaxy dust extinction (Avelino et al 2019). Moreover, the possibility of investigating the immediate environments, using, for example, integral field spectrographs, of nearby SNe Ia can provide important clues to the fundamental physical properties of the circumstellar gas surrounding SN progenitors.…”

Section: Discussionmentioning

confidence: 99%

A new measurement of the Hubble constant using Type Ia supernovae calibrated with surface brightness fluctuations

Khetan

Izzo

Branchesi

et al. 2021

A&A

122

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We present a new calibration of the peak absolute magnitude of Type Ia supernovae (SNe Ia) based on the surface brightness fluctuations (SBF) method, aimed at measuring the value of the Hubble constant. We build a sample of calibrating anchors consisting of 24 SNe hosted in galaxies that have SBF distance measurements. Applying a hierarchical Bayesian approach, we calibrate the SN Ia peak luminosity and extend the Hubble diagram into the Hubble flow by using a sample of 96 SNe Ia in the redshift range 0.02 < z < 0.075, which was extracted from the Combined Pantheon Sample. We estimate a value of H0 = 70.50 ± 2.37 (stat.) ± 3.38 (sys.) km s−1 Mpc−1 (i.e., 3.4% stat., 4.8% sys.), which is in agreement with the value obtained using the tip of the red giant branch calibration. It is also consistent, within errors, with the value obtained from SNe Ia calibrated with Cepheids or the value inferred from the analysis of the cosmic microwave background. We find that the SNe Ia distance moduli calibrated with SBF are on average larger by 0.07 mag than those calibrated with Cepheids. Our results point to possible differences among SNe in different types of galaxies, which could originate from different local environments and/or progenitor properties of SNe Ia. Sampling different host galaxy types, SBF offers a complementary approach to using Cepheids, which is important in addressing possible systematics. As the SBF method has the ability to reach larger distances than Cepheids, the impending entry of the Vera C. Rubin Observatory and JWST into operation will increase the number of SNe Ia hosted in galaxies where SBF distances can be measured, making SBF measurements attractive for improving the calibration of SNe Ia, as well as in the estimation of H0.

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“…SNe Ia in the H band have been shown to be standard to 0.15-0.2 mag without light-curve corrections (Wood-Vasey et al 2008;Folatelli et al 2010;Barone-Nugent et al 2012;Kattner et al 2012;Weyant et al 2014;Stanishev et al 2018;Avelino et al 2019), whereas optical light curves before brightness standardization have significantly larger scatter of ∼0.8 mag (Hamuy et al 1995). However, there are only ∼220 NIR light curves publicly available compared to the >1000 available for optically observed SNe Ia.…”

Section: Introductionmentioning

confidence: 99%

Are Type Ia Supernovae in Rest-frame H Brighter in More Massive Galaxies?

Ponder

Wood‐Vasey

Weyant

et al. 2021

ApJ

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We analyze 143 Type Ia supernovae (SNe Ia) observed in H band (1.6–1.8 μm) and find that SNe Ia are intrinsically brighter in H band with increasing host galaxy stellar mass. We find that SNe Ia in galaxies more massive than 1010.43 M ⊙ are 0.13 ± 0.04 mag brighter in H than SNe Ia in less massive galaxies. The same set of SNe Ia observed at optical wavelengths, after width–color–luminosity corrections, exhibit a 0.10 ± 0.03 mag offset in the Hubble residuals. We observe an outlier population ( ∣ Δ H max ∣ > 0.5 mag) in the H band and show that removing the outlier population moves the mass threshold to 1010.65 M ⊙ and reduces the step in H band to 0.08 ± 0.04 mag, but the equivalent optical mass step is increased to 0.13 ± 0.04 mag. We conclude that the outliers do not drive the brightness–host-mass correlation. Less massive galaxies preferentially host more higher-stretch SNe Ia, which are intrinsically brighter and bluer. It is only after correction for width–luminosity and color–luminosity relationships that SNe Ia have brighter optical Hubble residuals in more massive galaxies. Thus, finding that SNe Ia are intrinsically brighter in H in more massive galaxies is an opposite correlation to the intrinsic (pre-width–luminosity correction) optical brightness. If dust and the treatment of intrinsic color variation were the main driver of the host galaxy mass correlation, we would not expect a correlation of brighter H-band SNe Ia in more massive galaxies.

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Type Ia Supernovae Are Excellent Standard Candles in the Near-infrared

Cited by 48 publications

References 141 publications

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

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

A new measurement of the Hubble constant using Type Ia supernovae calibrated with surface brightness fluctuations

Are Type Ia Supernovae in Rest-frame H Brighter in More Massive Galaxies?

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