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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Notes
These stars likely have some intrinsic variability—as most stars do, but it is on a much smaller scale than the pulsational variables that have amplitudes ∼0.3 to \({>}1\) mag.
The full variable star catalog can be queried here: http://ogledb.astrouw.edu.pl/~ogle/OCVS/.
Data is available here: http://djuma.as.arizona.edu/~dennis/mcsurvey/.
We also refer the reader to Sobel (2016) for a description of the role of Williamina Fleming in these discoveries. More specifically, Williamina Fleming was first E. C. Pickering’s maid, became the first of the Harvard ‘computers,’ and was involved in a large number of projects at the Harvard Observatory. Her accomplishments were honored when she became the first American woman elected to the Royal Astronomical Society.
Several authors also cite Ritter’s work from a series of papers published between 1878 and 1883 in Wiedemann’s Annalen 5–20 that the authors of the present manuscript have been unable to find. Such references begin as early as Shapley (1914) and are cited as recently as Smeyers and van Hoolst (2010).
The models are publicly available: http://basti.oa-teramo.inaf.it/.
The consensus of the scientific community present for the Thanks to Henrietta Leavitt Symposium held on Nov 8, 2008 was to officially adopt the term ‘Leavitt Law’ for the Cepheid PL relationship. The Council of the American Astronomical Society provided similar advice shortly thereafter. The reader is referred to https://www.cfa.harvard.edu/events/2008/leavitt/ and https://aas.org/archives/Newsletter/Newsletter_146_2009_05_May_June.pdf, respectively.
Available: http://www.sai.msu.su/gcvs/gcvs/.
Additional non-parametric studies are listed in Jang et al. (2018).
An impressive and detailed tabulation of all known variables in clusters, which includes RRL, T2Cs, and EBs among other types, has been updated by Christine Clement regularly for many years and is available at this URL: http://www.astro.utoronto.ca/~cclement/cat/listngc.html.
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Acknowledgements
The authors warmly acknowledge the hospitality of ISSI-BJ for an engaging conference and the conference organizer Richard De Grijs for his leadership in completing these chapters. We further thank the anonymous referees for useful comments and perspectives that have improved and broadened this review. RLB acknowledges many insightful discussions with Barry Madore, Wendy Freedman, and the Carnegie–Chicago program team, as well as helpful conversations and data for figures from Mark Seibert, Erika Carlson, Andrew Monson, Victoria Scowcroft, Julianne Dalcanton, and Ben Williams. Support for this work was provided by NASA through Hubble Fellowship grant #51386.01 awarded to RLB by the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., for NASA, under contract NAS 5-26555. GB thanks A Severo Ochoa research grant at the Instituto de Astrofisica de Canarias, where part of this manuscript was written. VFB warmly thank Prof. R.P. Kudritzski for many useful discussions concerning stellar atmospheres and non-LTE effects in giant stars and Dr. P.B. Stetson for his superb-quality photometric reduction work, which has been a key component of the work presented here. VFB acknowledges PRIN–INAF 2011 “Tracing the formation and evolution of the Galactic halo with VST” (P.I.: M. Marconi), PRIN–MIUR (2010LY5N2T) “Chemical and dynamical evolution of the Milky Way and Local Group galaxies” (P.I.: F. Matteucci). VFB thank the Japan Society for the Promotion of Science for a research grant (L15518) and the support from FIRB 2013 (grant: RBFR13J716). We also thank the Education and Science Ministry of Spain (grants AYA201016717). VFB finally acknowledge the financial support from the PO FSE Abruzzo 2007–2013 through the grant “Spectrophotometric characterization of stellar populations in Local Group dwarf galaxies”, prot. 89/2014/OACTe/D (PI: S. Cassisi). GF has been supported by the Futuro in Ricerca 2013 (grant RBFR13J716). CEMV and MM acknowledges support from the Spanish Ministry of Economy and Competitiveness (MINECO) under the grant (project reference AYA2014-56795-P) NM is grateful to Grant-in-Aid (KAKENHI No. 26287028) from the Japan Society for the Promotion of Science.
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Astronomical Distance Determination in the Space Age
Edited by Richard de Grijs and Maurizio Falanga
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Beaton, R.L., Bono, G., Braga, V.F. et al. Old-Aged Primary Distance Indicators. Space Sci Rev 214, 113 (2018). https://doi.org/10.1007/s11214-018-0542-1
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DOI: https://doi.org/10.1007/s11214-018-0542-1