The Mira Distance to M101 and a 4% Measurement of H 0

• DOI: 10.3847/1538-4357/ad1ff8
• Publication Date: 2024-03-01T10:41:26Z
• Authors: Caroline D. Huang; Wenlong Yuan; Adam G. Riess; Warren Hack; Patricia A. White...; Nadia L. Zakamska; Stefano Casertano; Lucas M. Macri; Massimo Marengo; John W. Menzies; Randall K. Smith
• Keywords: Observational cosmology; QB460-466; Asymptotic giant branch stars; Hubble constant; Cosmology and Nongalactic Astrophysics (astro-ph.CO); Stellar distance; Distance indicators; FOS: Physical sciences; Astrophysics; Mira variable stars; Astrophysics - Cosmology and Nongalactic Astrophysics

Abstract The giant spiral galaxy M101 is host to the nearest recent Type Ia supernova (SN 2011fe) and thus has been extensively monitored in near-infrared study late-time light curve of SN. Leveraging this existing baseline observations, we derive first Mira-based distance by discovering classifying a sample 211 Miras with periods ranging from 240–400 days SN field. Combined new Hubble Space Telescope (HST) WFC3/IR channel our data set totals 11 epochs F110W (HST YJ ) 13 F160W H spanning ∼2900 days. We adopt absolute calibrations Mira period–luminosity relation based on geometric distances Large Magellanic Cloud water megamaser NGC 4258, find μ = 29.10 ± 0.06 mag. This 1 σ agreement most other Cepheid tip red branch measurements M101. Including previous host, 1559, 2005df, determine fiducial peak luminosity, <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msubsup> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mi>B</mml:mi> <mml:mn>0</mml:mn> </mml:msubsup> <mml:mo>=</mml:mo> <mml:mo>−</mml:mo> <mml:mn>19.27</mml:mn> <mml:mspace width="0.50em"/> <mml:mo>±</mml:mo> <mml:mn>0.09</mml:mn> </mml:math> With diagram supernovae Ia, 0 72.37 2.97 km s −1 Mpc , 4.1% measurement using Miras. excellent ladder confirm indications that local universe value higher than early at ∼95% confidence. Currently, still dominated statistical uncertainty magnitude.