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Optical interferometry and Gaia parallaxes for a robust calibration of the Cepheid distance scale

Published online by Cambridge University Press:  07 March 2018

Pierre Kervella Open the ORCID record for Pierre Kervella [Opens in a new window] ,
Antoine Mérand ,
Alexandre Gallenne ,
Boris Trahin ,
Simon Borgniet ,
Grzegorz Pietrzynski ,
Nicolas Nardetto  and
Wolfgang Gieren
Pierre Kervella
Affiliation:
Unidad Mixta Internacional Franco-Chilena de Astronomía (CNRS UMI 3386), Departamento de Astronomía, Universidad de Chile, Santiago, Chile LESIA (UMR 8109), Observatoire de Paris, PSL Research University, CNRS, UPMC, Univ. Paris-Diderot, 92195 Meudon, France, email: pierre.kervella@obspm.fr
Antoine Mérand
Affiliation:
European Southern Observatory, Karl-Schwarzschild-str. 2, D-85748 Garching, Germany.
Alexandre Gallenne
Affiliation:
European Southern Observatory, Alonso de Córdova 3107, Casilla 19001, Santiago 19, Chile.
Boris Trahin
Affiliation:
Unidad Mixta Internacional Franco-Chilena de Astronomía (CNRS UMI 3386), Departamento de Astronomía, Universidad de Chile, Santiago, Chile
Simon Borgniet
Affiliation:
Unidad Mixta Internacional Franco-Chilena de Astronomía (CNRS UMI 3386), Departamento de Astronomía, Universidad de Chile, Santiago, Chile
Grzegorz Pietrzynski
Affiliation:
Nicolaus Copernicus Astronomical Center, Polish Academy of Sciences, Warszawa, Poland Universidad de Concepción, Departamento de Astronomía, Casilla 160-C, Concepción, Chile
Nicolas Nardetto
Affiliation:
Laboratoire Lagrange, UMR7293, Université de Nice Sophia-Antipolis, CNRS, Observatoire de la Côte d'Azur, 06000 Nice, France
Wolfgang Gieren
Affiliation:
Universidad de Concepción, Departamento de Astronomía, Casilla 160-C, Concepción, Chile
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Abstract

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We present the modeling tool we developed to incorporate multi-technique observations of Cepheids in a single pulsation model: the Spectro-Photo-Interferometry of Pulsating Stars (SPIPS). The combination of angular diameters from optical interferometry, radial velocities and photometry with the coming Gaia DR2 parallaxes of nearby Galactic Cepheids will soon enable us to calibrate the projection factor of the classical Parallax-of-Pulsation method. This will extend its applicability to Cepheids too distant for accurate Gaia parallax measurements, and allow us to precisely calibrate the Leavitt law's zero point. As an example application, we present the SPIPS model of the long-period Cepheid RS Pup that provides a measurement of its projection factor, using the independent distance estimated from its light echoes.

Keywords

stars: distancesstars: individual (RS Pup)stars: oscillationsstars: variables: Cepheidscosmology: distance scale
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S330: Astrometry and Astrophysics in the Gaia sky , April 2017 , pp. 305 - 308
Copyright
Copyright © International Astronomical Union 2018 

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