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Precise distances to red giant stars with seismic data using the near-IR surface-brightness relation

Published online by Cambridge University Press:  02 August 2018

Jesper Storm Open the ORCID record for Jesper Storm [Opens in a new window] ,
Dariusz Graczyk ,
Marica Valentini Open the ORCID record for Marica Valentini [Opens in a new window] ,
Friedrich Anders Open the ORCID record for Friedrich Anders [Opens in a new window] ,
Cristina Chiappini ,
Wolfgang Gieren  and
Grzegorz Pietrzynski
Jesper Storm
Affiliation:
Leibniz-Institut für Astrophysik Potsdam, Germany, email: jstorm@aip.de
Dariusz Graczyk
Affiliation:
Universidad de Concepción, Chile Millenium Institute of Astrophysics (MAS), Concepción, Chile Centrum Astronomiczne im. Mikołaja Kopernika (CAMK), Warsaw, Poland
Marica Valentini
Affiliation:
Leibniz-Institut für Astrophysik Potsdam, Germany, email: jstorm@aip.de
Friedrich Anders
Affiliation:
Leibniz-Institut für Astrophysik Potsdam, Germany, email: jstorm@aip.de
Cristina Chiappini
Affiliation:
Leibniz-Institut für Astrophysik Potsdam, Germany, email: jstorm@aip.de
Wolfgang Gieren
Affiliation:
Universidad de Concepción, Chile Millenium Institute of Astrophysics (MAS), Concepción, Chile
Grzegorz Pietrzynski
Affiliation:
Universidad de Concepción, Chile Centrum Astronomiczne im. Mikołaja Kopernika (CAMK), Warsaw, Poland
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Abstract

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The Kepler and CoRoT satellites have determined precise asteroseismic radii for large samples of red giant stars. Combining these data with data from spectroscopic and photometric surveys has led to precise distance determinations using comprehensive Bayesian methods. Here we determine angular diameters and thus distances using the interferometrically calibrated near-IR surface-brightness method finding good agreement with previous results. The method can easily be reversed when accurate Gaia parallaxes for these stars become available to calibrate the asteroseismic scaling relations.

Keywords

stars: distancesstars: late-typestars: oscillations
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 13 , Symposium S334: Rediscovering our Galaxy , July 2017 , pp. 368 - 369
Copyright
Copyright © International Astronomical Union 2018 

References

Anders, F., Chiappini, C., Rodrigues, T., et al., 2017, A&A, 597, A30Google Scholar
di Benedetto, G. P., 2005, MNRAS, 357, 858Google Scholar
Casagrande, L., Ramirez, I., Melendez, J., et al., 2010, A&A, 512, A54Google Scholar
Gonzales Hernandez, J. I. & Bonifacio, P., 2009, A&A, 497, 497Google Scholar
Pietrzynski, G., Graczyk, D., Gieren, W., et al., 2013, Nature, 495, 76Google Scholar
Pinsonneault, M. H., Elsworth, Y., Epstein, C., et al., 2014, ApJS, 215, 19Google Scholar
Rodrigues, T. S., Girardi, L., Miglio, A., et al., 2014, MNRAS, 445, 2758Google Scholar