Toward a renewed Galactic Cepheid distance scale from Gaia and optical interferometry

被引：1

作者：

Kervella, Pierre ^{[1
,2
]}

Merand, Antoine ^{[3
]}

Gallenne, Alexandre ^{[3
]}

Trahin, Boris ^{[1
,2
]}

Nardetto, Nicolas ^{[4
]}

Anderson, Richard I. ^{[5
]}

Breitfelder, Joanne ^{[2
,3
]}

Szabados, Laszlo ^{[6
]}

Bond, Howard E. ^{[7
]}

Borgniet, Simon ^{[1
,2
]}

Gieren, Wolfgang ^{[8
]}

Pietrzynski, Grzegorz ^{[9
]}

机构：

[1] Univ Chile, Dept Astron, Unidad Mixta Int Franco Chilena Astron CNRS UMI 3, Las Condes, Chile

[2] Univ Paris Diderot, UPMC, CNRS, LESIA CNRS UMR 8109,Observ Paris,PSL, Paris, France

[3] European Southern Observ, Alonso de Cordova 3107,Casilla 19001, Santiago 19, Chile

[4] Univ Nice Sophia Antipolis, Observ Cote dAzur, CNRS, Lab Lagrange,UMR 7293, Nice, France

[5] Johns Hopkins Univ, Dept Phys & Astron, Baltimore, MD 21218 USA

[6] MTA CSFK, Konkoly Observ, Konkoly Thege M Ut 15-17, H-1121 Budapest, Hungary

[7] Penn State Univ, Dept Astron & Astrophys, 525 Davey Lab, University Pk, PA 16802 USA

[8] Univ Concepcion, Dept Astron, Casilla 160-C, Concepcion, Chile

[9] Polish Acad Sci, Nicolaus Copernicus Astron Ctr, Warsaw, Poland

来源：

WIDE-FIELD VARIABILITY SURVEYS: A 21ST CENTURY PERSPECTIVE | 2017年 / 152卷

基金：

欧洲研究理事会;

关键词：

HUBBLE-SPACE-TELESCOPE; PROJECTION FACTOR; RS-PUPPIS; OBSERVATIONAL CALIBRATION; GEOMETRIC DISTANCE; CLASSICAL CEPHEID; PARALLAX; ENVELOPES; STARS; III;

D O I：

10.1051/epjconf/201715207002

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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.

引用

页数：5

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