A Uniform Type Ia Supernova Distance Ladder with the Zwicky Transient Facility: Absolute Calibration Based on the Tip of the Red Giant Branch (TRGB) Method

Dhawan, Suhail; Goobar, Ariel; Johansson, Joel; Jang, In Sung; Rigault, Mickael; Harvey, Luke; Maguire, Kate; Freedman, Wendy L.; Madore, Barry F.; Smith, Mathew; Sollerman, Jesper; Kim, Young-Lo; Andreoni, Igor; Bellm, Eric C.; Coughlin, Michael W.; Dekany, R.; Graham, Matthew J.; Kulkarni, Shrinivas R.; Laher, Russ R.; Medford, Michael S.; Neill, James D.; Nir, Guy; Riddle, Reed; Rusholme, Ben

doi:10.48550/arxiv.2203.04241

Cited by 4 publications

(6 citation statements)

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“…The possibility of finding at least three more pairs of sibling SNe Ia in galaxies with Cepheid distances would not be negligible in the next decade. The ZTF survey (Bellm et al 2019) discoveries reinforce the previous premise, reporting 1-2 SNe Ia every year in the 20 Mpc volume (Dhawan et al 2022), where HST observations can provide robust distance estimates by means of Cepheids or TRGB. As a back-of-the-envelope calculation, this means reducing the statistical error of H 0 down to 1.7%, similar to what is expected from the entire sample of SNe Ia, and more importantly, it would strongly reduce the systematic error, given that it mainly depends on the uncertainty on the distance modulus of a small number of host galaxies.…”

Section: Discussionsupporting

confidence: 63%

The Hubble constant from two sibling Type Ia supernovae in the nearby galaxy NGC 4414: SN 1974G and SN 2021J

Gallego-Cano

Izzo

Domínguez-Tagle

et al. 2022

A&A

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Having two "sibling" Type Ia supernovae (SNe Ia) in the same galaxy offers additional advantages in reducing a variety of systematic errors involved in estimating the Hubble constant, H 0 . NGC 4414 is a nearby galaxy included in the Hubble Space Telescope Key Project to measure its distance using Cepheid variables. It hosts two sibling SNe Ia: SN 2021J and SN 1974G. This provides the opportunity to improve the precision of the previous estimate of H 0 , which was based solely on SN 1974G. Here we present new optical BVRI photometry obtained at the Observatorio de Sierra Nevada and complement it with Swift UVOT U BV data, which cover the first 70 days of emission of SN 2021J. A first look at SN 2021J optical spectra obtained with the Gran Telescopio Canarias (GTC) reveals typical SN type Ia features. The main SN luminosity parameters for the two sibling SNe are obtained by using SNooPy, a light curve fitting code based on templates. Using a hierarchical bayesian approach, we build the Hubble diagram with a sample of 96 SNe Ia obtained from the Combined Pantheon Sample in the redshift range z = 0.02 − 0.075, and calibrate the zero point with the two sibling type-Ia SNe in NGC 4414. We report a value of the Hubble constant H 0 = 72.19 ± 2.32 (stat.) ±3.42 (syst.) km s −1 Mpc −1 . We expect a reduction of the systematic error after a new analysis of the Cepheids period-luminosity relation using the upcoming Gaia DR4 and additional Cepheids from the HST and JWST.

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Section: Discussionsupporting

confidence: 63%

The Hubble constant from two sibling Type Ia supernovae in the nearby galaxy NGC 4414: SN 1974G and SN 2021J

Gallego-Cano

Izzo

Domínguez-Tagle

et al. 2022

A&A

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“…Cepheids or the tip of the red giant branch (TRGB); (ii) E-mail: dejae ger@ha waii.edu nearby Type Ia supernovae (hereafter SNe Ia) can be calibrated by standardized calibrators -e.g. Cepheids (Freedman et al 2001 ;Sandage et al 2006 ;Riess et al 2009Riess et al , 2011Riess et al , 2016Riess et al , 2018aRiess et al , b , 2019Riess et al , 2021aFreedman & Madore 2010 ;Burns et al 2018 ;Dhawan, Jha & Leibundgut 2018 ), TRGB (Madore, Mager & Freedman 2009 ;Jang & Lee 2017a , b ;Freedman et al 2019 ;Yuan et al 2019 ;Freedman 2021 ;Anand et al 2022 ;Dhawan et al 2022 ), or Mira variable stars (Whitelock, Feast & Van Leeuwen 2008 ;Huang et al 2020 ); and (iii) the calibration to nearby SNe Ia is applied to SNe Ia in the Hubble flow. Owing to a series of efforts which have allowed the scientific community to build the cosmic distance ladder o v er sev eral decades, such as detached eclipsing binary stars in the Large Magellanic Cloud (Pietrzy ński et al 2019 ), Gaia parallaxes (Lindegren et al 2021 ;Riess et al 2021b ), Cepheids (Leavitt & Pickering 1912 ), TRGB (Lee, Freedman & Madore 1993 ), and SNe Ia in the Hubble flow (SH0ES 1 team), the uncertainty in the local measurement of H 0 has impro v ed from ∼10 per cent (Freedman et al 2001 ) to ± 1.4 per cent (Riess et al 2021a ) in the MNRAS 514, 4620-4628 (2022) last 20 yr.…”

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confidence: 99%

A 5 per cent measurement of the Hubble–Lemaître constant from Type II supernovae

Jaeger

Galbany

Riess

et al. 2022

Monthly Notices of the Royal Astronomical Society

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The most stringent local measurement of the Hubble-Lemaître constant from Cepheid-calibrated Type Ia supernovae (SNe Ia) differs from the value inferred via the cosmic microwave background radiation (Planck+ΛCDM) by ∼5σ. This so-called ‘Hubble tension’ has been confirmed by other independent methods, and thus does not appear to be a possible consequence of systematic errors. Here, we continue upon our prior work of using Type II supernovae to provide another, largely-independent method to measure the Hubble-Lemaître constant. From 13 SNe II with geometric, Cepheid, or tip of the red giant branch (TRGB) host-galaxy distance measurements, we derive H$_0= 75.4^{+3.8}_{-3.7}$ km s−1 Mpc−1 (statistical errors only), consistent with the local measurement but in disagreement by ∼2.0σ with the Planck+ΛCDM value. Using only Cepheids (N = 7), we find H$_0 = 77.6^{+5.2}_{-4.8}$ km s−1 Mpc−1, while using only TRGB (N = 5), we derive H$_0 = 73.1^{+5.7}_{-5.3}$ km s−1 Mpc−1. Via 13 variants of our dataset, we derive a systematic uncertainty estimate of 1.5 km s−1 Mpc−1. The median value derived from these variants differs by just 0.3 km s−1 Mpc−1 from that produced by our fiducial model. Because we only replace SNe Ia with SNe II — and we do not find statistically significant difference between the Cepheid and TRGB H0 measurements — our work reveals no indication that SNe Ia or Cepheids could be the sources of the ‘H0 tension.’ We caution, however, that our conclusions rest upon a modest calibrator sample; as this sample grows in the future, our results should be verified.

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“…Despite a wealth of effort, both theoretical and experimental, the problem persists, and, moreover, has become a multidimensional one, with the introduction of a number of new data-sets. These allow alternative probes of the expansion rate, and proceed via a wide number of mechanisms, such as alternative calibration of the distance ladder using tip of the red giant branch (TRGB) methods [e.g., [4][5][6] or megamasers [7], gravitational wave observations [e.g., 8] and time delay cosmography from strongly lensed sources [e.g., 9,10]. For a brief time, H 0 constraints appeared to fall in one of two camps: measurements depending on the full νΛCDM model preferred lower H 0 , whilst those depending only on local physics tended towards higher values [e.g.…”

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confidence: 99%

Determining the Hubble Constant without the Sound Horizon: A $3.6\%$ Constraint on $H_0$ from Galaxy Surveys, CMB Lensing and Supernovae

Philcox¹,

Farren²,

Sherwin³

et al. 2022

Preprint

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Many theoretical resolutions to the so-called "Hubble tension" rely on modifying the sound horizon at recombination, rs, and thus the acoustic scale used as a standard ruler in the cosmic microwave background (CMB) and large scale structure (LSS) datasets. As shown in a number of recent works, these observables can also be used to compute rs-independent constraints on H0 by making use of the horizon scale at matter-radiation equality, keq, which has different sensitivity to high redshift physics than rs. In this work, we present the tightest keq-based constraints on the expansion rate from current data, finding H0 = 64.8 +2.2 −2.5 km s −1 Mpc −1 at 68% CL from a combination of BOSS galaxy power spectra, Planck CMB lensing, and the newly released Pantheon+ supernova constraints, as well as physical priors on the baryon density, neutrino mass, and spectral index. The BOSS and Planck measurements have different degeneracy directions, leading to the improved combined constraints, with a bound of H0 = 67.1 +2.5 −2.9 (63.6 +2.9 −3.6 ) from BOSS (Planck ) alone in km s −1 Mpc −1 units. The results show some dependence on the neutrino mass bounds, with the constraint broadening to H0 = 68.0 +2.9 −3.2 km s −1 Mpc −1 if we instead impose a weak prior on mν from terrestrial experiments rather than assuming mν < 0.26 eV, or shifting to H0 = 64.6 ± 2.4 km s −1 Mpc −1 if the neutrino mass is fixed to its minimal value. Even without any dependence on the sound horizon, our results are in ≈ 3σ tension with those obtained from the Cepheid-calibrated distance ladder, providing evidence against new physics models that vary H0 by changing acoustic physics or the expansion history immediately prior to recombination.

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A Uniform Type Ia Supernova Distance Ladder with the Zwicky Transient Facility: Absolute Calibration Based on the Tip of the Red Giant Branch (TRGB) Method

Cited by 4 publications

References 32 publications

The Hubble constant from two sibling Type Ia supernovae in the nearby galaxy NGC 4414: SN 1974G and SN 2021J

The Hubble constant from two sibling Type Ia supernovae in the nearby galaxy NGC 4414: SN 1974G and SN 2021J

A 5 per cent measurement of the Hubble–Lemaître constant from Type II supernovae

Determining the Hubble Constant without the Sound Horizon: A $3.6\%$ Constraint on $H_0$ from Galaxy Surveys, CMB Lensing and Supernovae

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