Mean Estimate Distances for Galaxies with Multiple Estimates in NED-D

Steer, Ian

doi:10.3847/1538-3881/abafba

Cited by 14 publications

(9 citation statements)

References 18 publications

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“…For a historical comparison, our determination agrees to within 1σ with the value of µ 0 = 24.33 ± 0.12 mag to Baade's field I (3 kpc from the center of M31) from Freedman & Madore (1990). Our distance also agrees with all six mean estimate distances (MED) (Steer 2020) and the MED for Cepheid distances only of 790 ± 78 kpc from the NASA/IPAC Extragalactic Database (NED) (I. Steer, 2020, private communication) as well as the the recommended value of µ 0 = 24.45 ± 0.10 mag from de Grijs & Bono (2014).…”

Section: Comparison With Other Studiessupporting

confidence: 84%

A sub-2% Distance to M31 from Photometrically Homogeneous Near-Infrared Cepheid Period-Luminosity Relations Measured with the Hubble Space Telescope

Li,

Riess,

Busch

et al. 2021

Preprint

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We present Period-Luminosity Relations (PLRs) for 55 Cepheids in M31 with periods ranging from 4 to 78 days observed with the Hubble Space Telescope (HST) using the same three-band photometric system recently used to calibrate their luminosities. Images were taken with the Wide Field Camera 3 in two optical filters (F555W and F814W) and one near-infrared filter (F160W) using the Drift And SHift (DASH) mode of operation to significantly reduce overheads and observe widely-separated Cepheids in a single orbit. We include additional F160W epochs for each Cepheid from the Panchromatic Hubble Andromeda Treasury (PHAT) and use light curves from the Panoramic Survey Telescope and Rapid Response System of the Andromeda galaxy (PAndromeda) project to determine mean magnitudes. Combined with a 1.28% absolute calibration of Cepheid PLRs in the Large Magellanic Cloud from Riess et al. (2019a) in the same three filters, we find a distance modulus to M31 of µ 0 = 24.407 ± 0.032, corresponding to 761 ± 11 kpc and 1.49% uncertainty including all error sources, the most precise determination of its distance to date. We compare our results to past measurements using Cepheids and the Tip of the Red Giant Branch (TRGB). This study also provides the groundwork for turning M31 into a precision anchor galaxy in the cosmic distance ladder to measure the Hubble constant together with efforts to measure a fully geometric distance to M31.

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Section: Comparison With Other Studiessupporting

confidence: 84%

A sub-2% Distance to M31 from Photometrically Homogeneous Near-Infrared Cepheid Period-Luminosity Relations Measured with the Hubble Space Telescope

Li,

Riess,

Busch

et al. 2021

Preprint

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“…It can be estimated with a wide range of approaches and accuracies from limited knowledge of many types of astronomical sources, nearly all of which have been utilized in this endeavor over the past century. There have been > 1000 estimates published since 1980, with 1/3 of those in the last five years and 20% in the last two years -a recent quadrupling of the effort indicating the accelerating interest in H 0 (Steer 2020). However, past discrepancies internal to the body of local measurements reveal that systematic errors can dominate determinations of H 0 , and that there is no reason to believe all efforts will regress to the mean or that a more accurate result can be derived from their median (Chen & Ratra 2011).…”

Section: The Sh0es Programmentioning

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

214

393

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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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“…A simple mean of all these estimates could not be adopted as the values are not continuous but at extremes. Steer (2020) has defined a robust method to get enhanced mean estimate distances (MED) using the weighted mean for the distances from various primary and secondary sources. From the various means, we have estimated MED 7, which is a combination of the unweighted (MED 2), error-weighted (MED 3), and dateweighted (MED 4) means with weights of 1:2:4, respectively.…”

Section: Reddening Distance and Metallicitymentioning

confidence: 99%

SN 2020jfo: A Short-plateau Type II Supernova from a Low-mass Progenitor

Teja

Singh

Sahu

et al. 2022

ApJ

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We present spectroscopic and photometric observations of the Type IIP supernova, SN 2020jfo, in ultraviolet and optical wavelengths. SN 2020jfo occurred in the spiral galaxy M61 (NGC 4303), with eight observed supernovae in the past 100 yr. SN 2020jfo exhibited a short plateau lasting < 65 days, and achieved a maximum brightness in Vband of M V = −17.4 ± 0.4 mag at about 8.0 ± 0.5 days since explosion. From the bolometric light curve, we have estimated the mass of 56Ni synthesized in the explosion to be 0.033 ± 0.006 M ⊙. The observed spectral features are typical for a Type IIP supernova except for shallow Hα absorption throughout the evolution and the presence of stable 58Ni feature at 7378 Å, in the nebular phase. Using hydrodynamical modeling in the MESA + STELLA framework, an ejecta mass of ∼5 M ⊙ is estimated. Models also indicate SN 2020jfo could be the result of a red supergiant progenitor with M ZAMS ∼ 12 M ⊙. Bolometric light-curve modeling revealed the presence of a secondary radiation source for initial ∼20 days, which has been attributed to interaction with a circumstellar material of mass ∼ 0.2 M ⊙, which most likely was ejected due to enhanced mass loss about 20 yr prior to the supernova explosion.

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Mean Estimate Distances for Galaxies with Multiple Estimates in NED-D

Cited by 14 publications

References 18 publications

A sub-2% Distance to M31 from Photometrically Homogeneous Near-Infrared Cepheid Period-Luminosity Relations Measured with the Hubble Space Telescope

A sub-2% Distance to M31 from Photometrically Homogeneous Near-Infrared Cepheid Period-Luminosity Relations Measured with the Hubble Space Telescope

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

SN 2020jfo: A Short-plateau Type II Supernova from a Low-mass Progenitor

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