The Pantheon+ Analysis: The Full Dataset and Light-Curve Release

Scolnic, Dan; Brout, D.; Carr, Antony; Riess, Adam G.; Davis, Tamara M.; Dwomoh, Arianna; Jones, D. O.; Ali, Noor Azman; Charvu, Pranav; Chen, Rebecca; Peterson, Erik R.; Popovic, Brodie; Rose, Benjamin; Wood, Charlotte; Brown, P. J.; Chambers, K.; Coulter, D. A.; Dettman, K.; Dimitriadis, G.; Filippenko, A. V.; Foley, R. J.; Kilpatrick, C. D.; Kirshner, R.; Pan, Y. C.; Rest, A.; Rojas-Bravo, C.; Siebert, M. R.; Stahl, Benjamin E.; Zheng, W.

doi:10.48550/arxiv.2112.03863

Cited by 43 publications

(78 citation statements)

References 47 publications

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“…We benefit from a 3× increase in the sample of Cepheids within NGC 4258 discovered by observing 4 new fields with HST, fully reanalyzed using the same pipeline by Yuan et al (2022a, hereafter Y22a). Extensive details concerning the analysis of SNe Ia data are given by Scolnic et al (2021) and . We present the formalism for measuring H 0 from the distance ladder in §2; new Cepheid data in §3 and in Y22a+Y22b; ancillary data used to measure H 0 in §4; our baseline, local determination of H 0 and a simultaneous measurement of H 0 and the expansion history with high-redshift SNe Ia in §5; extensions to the baseline and variants of the local measurement of H 0 in §6; discussion in §7; and conclusions in §8.…”

Section: This Workmentioning

confidence: 99%

A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km/s/Mpc Uncertainty from the Hubble Space Telescope and the SH0ES Team

Riess¹,

Yuan²,

Macri³

et al. 2021

Preprint

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We report observations from the Hubble Space Telescope (HST) of Cepheid variables in the host galaxies of 42 Type Ia supernovae (SNe Ia) used to calibrate the Hubble constant (H 0 ). These include the complete sample of all suitable SNe Ia discovered in the last four decades at z ≤ 0.01, collected and calibrated from ≥ 1000 HST orbits, more than doubling the sample whose size limits the precision of the direct determination of H 0 . The Cepheids are calibrated geometrically from Gaia EDR3 parallaxes, masers in NGC 4258 (here tripling that sample of Cepheids), and detached eclipsing binaries in the Large Magellanic Cloud. All Cepheids in these anchors and SN Ia hosts were measured with the same instrument (WFC3) and filters (F555W, F814W, F160W) to negate zeropoint errors.We present multiple verifications of Cepheid photometry and six tests of background determinations that show Cepheid measurements are accurate in the presence of crowding. The SNe Ia in these hosts calibrate the magnitude-redshift relation from the revised Pantheon+ compilation, accounting here for covariance between all SNe data and with host properties and SN surveys matched throughout to negate systematics. We decrease the uncertainty in the local determination of H 0 to 1 km s −1 Mpc −1 including systematics. We present results for a comprehensive set of nearly 70 analysis variants to explore the sensitivity of H 0 to selections of anchors, SN surveys, redshift ranges, the treatment of Cepheid dust, metallicity, form of the period-luminosity relation, SN color, peculiar-velocity corrections, sample bifurcations, and simultaneous measurement of the expansion history.Our baseline result from the Cepheid-SN Ia sample is H 0 = 73.04 ± 1.04 km s −1 Mpc −1 , which includes systematic uncertainties and lies near the median of all analysis variants. We demonstrate consistency with measures from HST of the TRGB between SN Ia hosts and NGC 4258, and include them simultaneously to yield 72.53 ± 0.99 km s −1 Mpc −1 . The inclusion of high-redshift SNe Ia yields H 0 = 73.30 ± 1.04 km s −1 Mpc −1 and q 0 = −0.51 ± 0.024. We find a 5σ difference with the prediction of H 0 from Planck CMB observations under ΛCDM, with no indication that the discrepancy arises from measurement uncertainties or analysis variations considered to date. The source of this now long-standing discrepancy between direct and cosmological routes to determining the Hubble constant remains unknown.

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Section: This Workmentioning

confidence: 99%

A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km/s/Mpc Uncertainty from the Hubble Space Telescope and the SH0ES Team

Riess¹,

Yuan²,

Macri³

et al. 2021

Preprint

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214

393

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“…For this analysis, we use the upcoming Pantheon+ sample (Scolnic et al 2021), a collection of publically available and spectroscopically classified photometric light-curves of SNIa. The low-redshift sample is compiled from the Center for Astrophysics SNIa data sets (CfA1-4, Jha et al (2006a,b); Hicken et al (2009bHicken et al ( ,a, 2012), the Carnegie Supernova Project (CSP, Stritzinger ( 2010 The high-redshift sample is comprised of the Dark Energy 3-year sample (Brout et al 2019a,c;Smith et al 2020), the Sloan Digital Sky Survey (SDSS, Sako et al 2018), the Pan-STARRS survey (PS1MD Rest et al 2014;Scolnic et al 2018), the Supernova Legacy Survey (SNLS, Betoule et al 2014), and the Hubble Space Telescope (HST, Riess et al 2018).…”

Section: Datamentioning

confidence: 99%

“…Each sample has survey-specific selection requirements (cuts) as detailed in their data releases and Scolnic et al (2021). Here we implement a more restrictive range of cuts to define the sample:…”

Section: Selectionmentioning

confidence: 99%

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The Pantheon+ Analysis: Forward-Modeling the Dust and Intrinsic Colour Distributions of Type Ia Supernovae, and Quantifying their Impact on Cosmological Inferences

Popovic¹,

Brout²,

Keßler³

et al. 2021

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Recent studies have shown that the observed colour distributions of Type Ia SNe (SNIa) are welldescribed by a combination of distributions from dust and intrinsic colour. Here we present a new forward-modeling fitting method (Dust2Dust) to measure the parent dust and colour distributions, including their dependence on host-galaxy mass. At each fit step, the SNIa selection efficiency is determined from a large simulated sample that is re-weighted to reflect the proposed distributions. We use five separate metrics to constrain the Dust2Dust parameters: distribution of fitted lightcurve colour c, cosmological residual trends with c, cosmological residual scatter with c, fitted colourluminosity relationship β SALT2 , and intrinsic scatter σ int . Using the Pantheon+ data sample, we present results for a Dust2Dust fit that includes 4 parameters describing intrinsic colour variations and 8 parameters describing dust. Furthermore, we propagate the Dust2Dust parameter uncertainties and covariance to the dark energy equation-of-state w and Hubble constant H 0 : we find σw = 0.005 and σH 0 = 0.145 km/s/Mpc. The Dust2Dust code is publically available.

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“…The measurements of the cosmic microwave background (CMB) radiation from Planck satellite [31] give the value H 0 = 67.4 ± 0.5 km s −1 Mpc −1 , whereas a combination of different local measurements [32] yields a representative value of H 0 = 73.1±0.9 km s −1 Mpc −1 , which is 5.7σ discrepant from the Planck result. Recently, the Pantheon collaboration has reanalyzed the calibration used for the photometry of the supernovae type Ia sample, including the calibration used to obtain the SH0ES results [33,34], adding a new value from Pantheon+Cepheid-Supernovae Ia baseline H 0 = 73.04 ± 1.04 km s −1 Mpc −1 [30]. The contribution to the Hubble constant from the systematic supernovae calibration is smaller than ∼ 0.2 km s −1 Mpc −1 , so that the tension cannot be attributed to this type of systematics.…”

Section: Introductionmentioning

confidence: 99%

A New Parameterized Interacting Holographic Dark Energy

Escamilla-Rivera,

Gamboa

2022

Preprint

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We study a cosmological model based on the holographic principle that allows an interaction between dark energy and dark matter with a Hubble infrared cutoff. We adopt an agnostic point of view with respect to the form of the interaction between these dark components by using redshift parameterizations of the dark energy equation of state (DE EoS). Following this approach, we obtain an analytical expression of the Hubble parameter and we test it with four different parameterizations of the DE EoS using currently Pantheon supernovae, Cosmic Chronometers and Galaxy Clustering data sets. Our analyses show that the considered parameterizations on this agnostic proposal allow a late accelerated cosmic expansion in comparison to the results from previous works where specific forms of the interaction are employed but fail to explain this behaviour. Furthermore, we find that our proposal solves the so-called coincidence problem in Cosmology and in this direction shed some light on the problem of the Hubble tension.

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The Pantheon+ Analysis: The Full Dataset and Light-Curve Release

Cited by 43 publications

References 47 publications

A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km/s/Mpc Uncertainty from the Hubble Space Telescope and the SH0ES Team

A Comprehensive Measurement of the Local Value of the Hubble Constant with 1 km/s/Mpc Uncertainty from the Hubble Space Telescope and the SH0ES Team

The Pantheon+ Analysis: Forward-Modeling the Dust and Intrinsic Colour Distributions of Type Ia Supernovae, and Quantifying their Impact on Cosmological Inferences

A New Parameterized Interacting Holographic Dark Energy

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