New period-luminosity and period-color relations of classical Cepheids

2010/12/31 by G. Tammann, G. A. Tammann, B. Reindl +2 · 40 citations
Physics and Astronomy · #Astronomy #Astrophysics #Astrophysics and Star Formation Studies #Cepheid variable #Galaxies: Formation, Evolution, Phenomena #Galaxy #Luminosity #Period (music) #Physics #Stars #Stellar, planetary, and galactic studies #astro-ph.CO

paper · pdf · doi:10.1051/0004-6361/201016382

published in Astronomy and Astrophysics 531, A134 (EDP Sciences) · 14 pages, 10 figures, 5 tables, accepted for publication in Astronomy and Astrophysics. v2: restructured the whole paper and redrawn all figures

arxiv created 2011/05/16 · openalex publication_date 2011/05/18 · arxiv updated 2015/05/20 · openalex created_date 2022/09/22 · openalex updated_date 2026/08/05

Abstract

The metal-poor, fundamental-mode (P0) and first-overtone (P1) Cepheids in the dwarf galaxies IC 1613, WLM, Pegasus, Sextans A, Sextans B, and Leo A are compared with the about equally metal-poor Cepheids of the Small Magellanic Cloud (SMC). The period-color (P-C) and period-luminosity (P-L) relations of the seven galaxies are indistinguishable, but differ distinctly from those in the Large Magellanic Cloud (LMC) and the solar neighborhood. Adopting from independent evidence, one can determine reliable distance moduli for the other dwarf galaxies of (m − M)0 = 24.34 ± 0.03, 24.95 ± 0.03, 24.87 ± 0.06, 25.60 ± 0.03 (mean for Sextans A & B), and 24.59 ± 0.03, respectively.

Citations

• Oxygen and Nitrogen in Leo A and GR 8
• The expansion field: the value of H 0
• Further empirical evidence for the non-linearity of the period-luminosity relations as seen in the Large Magellanic Cloud Cepheids
• Investigations of the Nonlinear LMC Cepheid Period‐Luminosity Relation with Testimator and Schwarz Information Criterion Methods
• NICMOS Observations of Extragalactic Cepheids. I. Photometry Database and a Test of the Standard Extinction Law