TY - GEN
T1 - Toward a renewed Galactic Cepheid distance scale from Gaia and optical interferometry
AU - Kervella, Pierre
AU - Mérand, Antoine
AU - Gallenne, Alexandre
AU - Trahin, Boris
AU - Nardetto, Nicolas
AU - Anderson, Richard I.
AU - Breitfelder, Joanne
AU - Szabados, Laszlo
AU - Bond, Howard E.
AU - Borgniet, Simon
AU - Gieren, Wolfgang
AU - Pietrzyński, Grzegorz
N1 - Publisher Copyright:
© 2017 The Authors, published by EDP Sciences.
PY - 2017/9/8
Y1 - 2017/9/8
N2 - Through an innovative combination of multiple observing techniques and modeling, we are assembling a comprehensive understanding of the pulsation and close environment of Cepheids. We developed the SPIPS modeling tool that combines all observables (radial velocimetry, photometry, angular diameters from interferometry) to derive the relevant physical parameters of the star (effective temperature, infrared excess, reddening, ⋯) and the ratio of the distance and the projection factor d/p. We present the application of SPIPS to the long-period Cepheid RS Pup, for which we derive p = 1.25±0.06. The addition of this massive Cepheid consolidates the existing sample of p-factor measurements towards long-period pulsators. This allows us to conclude that p is constant or mildly variable around p = 1.29±0.04 (±3%) as a function of the pulsation period. The forthcoming Gaia DR2 will provide a considerable improvement in quantity and accuracy of the trigonometric parallaxes of Cepheids. From this sample, the SPIPS modeling tool will enable a robust calibration of the Cepheid distance scale.
AB - Through an innovative combination of multiple observing techniques and modeling, we are assembling a comprehensive understanding of the pulsation and close environment of Cepheids. We developed the SPIPS modeling tool that combines all observables (radial velocimetry, photometry, angular diameters from interferometry) to derive the relevant physical parameters of the star (effective temperature, infrared excess, reddening, ⋯) and the ratio of the distance and the projection factor d/p. We present the application of SPIPS to the long-period Cepheid RS Pup, for which we derive p = 1.25±0.06. The addition of this massive Cepheid consolidates the existing sample of p-factor measurements towards long-period pulsators. This allows us to conclude that p is constant or mildly variable around p = 1.29±0.04 (±3%) as a function of the pulsation period. The forthcoming Gaia DR2 will provide a considerable improvement in quantity and accuracy of the trigonometric parallaxes of Cepheids. From this sample, the SPIPS modeling tool will enable a robust calibration of the Cepheid distance scale.
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U2 - 10.1051/epjconf/201715207002
DO - 10.1051/epjconf/201715207002
M3 - Conference contribution
AN - SCOPUS:85029529796
T3 - EPJ Web of Conferences
BT - Wide-Field Variability Surveys
A2 - Gieren, Wolfgang
A2 - Catelan, Marcio
A2 - Gieren, Wolfgang
A2 - Catelan, Marcio
PB - EDP Sciences
T2 - 22nd Los Alamos Stellar Pulsation Conference Series Meeting 2016
Y2 - 28 November 2016 through 2 December 2016
ER -