Old-Aged Primary Distance Indicators |
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| Authors: | Rachael L Beaton Giuseppe Bono Vittorio Francesco Braga Massimo Dall’Ora Giuliana Fiorentino In Sung Jang Clara E Martínez-Vázquez Noriyuki Matsunaga Matteo Monelli Jillian R Neeley Maurizio Salaris |
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| Institution: | 1.Department of Astrophysical Sciences,Princeton University,Princeton,USA;2.The Observatories of the Carnegie Institution for Science,Pasadena,USA;3.Department of Physics,University of Rome Tor Vergata,Rome,Italy;4.INAF-Osservatorio Astronomico di Roma,Rome,Italy;5.ASDC,Rome,Italy;6.INAF-Osservatorio Astronomico di Capodimonte,Naples,Italy;7.INAF—OAS Osservatorio di Astrofisica & Scienza dello Spazio di Bologna,Bologna,Italy;8.Leibniz-Institut für Astrophysics Potsdam,Potsdam,Germany;9.Cerro Tololo Inter-American,National Optical Astronomy Observatory,La Serena,Chile;10.Department of Astronomy, School of Science,The University of Tokyo,Tokyo,Japan;11.IAC-Instituto de Astrofísica de Canarias,La Laguna,Spain;12.Departmento de Astrofísica,Universidad de La Laguna,La Laguna,Spain;13.Department of Physics,Florida Atlantic University,Boca Raton,USA;14.Astrophysics Research Institute,Liverpool John Moores University,Liverpool,UK |
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| Abstract: | Old-aged stellar distance indicators are present in all Galactic structures (halo, bulge, disk) and in galaxies of all Hubble types and, thus, are immensely powerful tools for understanding our Universe. Here we present a comprehensive review for three primary standard candles from Population II: (i) RR Lyrae type variables (RRL), (ii) type II Cepheid variables (T2C), and (iii) the tip of the red giant branch (TRGB). The discovery and use of these distance indicators is placed in historical context before describing their theoretical foundations and demonstrating their observational applications across multiple wavelengths. The methods used to establish the absolute scale for each standard candle is described with a discussion of the observational systematics. We conclude by looking forward to the suite of new observational facilities anticipated over the next decade; these have both a broader wavelength coverage and larger apertures than current facilities. We anticipate future advancements in our theoretical understanding and observational application of these stellar populations as they apply to the Galactic and extragalactic distance scale. |
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