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Title:
Extended Envelopes around Galactic Cepheids. III. Y Ophiuchi and α Persei from Near-Infrared Interferometry with CHARA/FLUOR
Authors:
Mérand, Antoine; Aufdenberg, Jason P.; Kervella, Pierre; Foresto, Vincent Coudé du; ten Brummelaar, Theo A.; McAlister, Harold A.; Sturmann, Laszlo; Sturmann, Judit; Turner, Nils H.
Affiliation:
AA(Center for High Angular Resolution Astronomy, Georgia State University, PO Box 3965, Atlanta, GA 30302-3965 ), AB(Physical Sciences Department, Embry-Riddle Aeronautical University, Daytona Beach, FL 32114), AC(LESIA, UMR 8109, Observatoire de Paris, 5 place Jules Janssen, 92195 Meudon, France), AD(LESIA, UMR 8109, Observatoire de Paris, 5 place Jules Janssen, 92195 Meudon, France), AE(Center for High Angular Resolution Astronomy, Georgia State University, PO Box 3965, Atlanta, GA 30302-3965), AF(Center for High Angular Resolution Astronomy, Georgia State University, PO Box 3965, Atlanta, GA 30302-3965), AG(Center for High Angular Resolution Astronomy, Georgia State University, PO Box 3965, Atlanta, GA 30302-3965), AH(Center for High Angular Resolution Astronomy, Georgia State University, PO Box 3965, Atlanta, GA 30302-3965), AI(Center for High Angular Resolution Astronomy, Georgia State University, PO Box 3965, Atlanta, GA 30302-3965)
Publication:
The Astrophysical Journal, Volume 664, Issue 2, pp. 1093-1101. (ApJ Homepage)
Publication Date:
08/2007
Origin:
UCP
Astronomy Keywords:
Stars: Variables: Cepheids, Stars: Circumstellar Matter, stars: individual (Y Ophiuchi), Stars: Individual: Constellation Name: α Persei, Techniques: Interferometric
DOI:
10.1086/518597
Bibliographic Code:
2007ApJ...664.1093M

Abstract

Unbiased angular diameter measurements are required for accurate distances to Cepheids using the interferometric Baade-Wesselink method (IBWM). The precision of this technique is currently limited by interferometric measurements at the 1.5% level. At this level, the center-to-limb darkening (CLD) and the presence of circumstellar envelopes (CSE) seem to be the two main sources of bias. The observations we performed aim at improving our knowledge of the interferometric visibility profile of Cepheids. In particular, we assess the systematic presence of CSE around Cepheids in order determine accurate distances with the IBWM free from CSE biased angular diameters. We observed a Cepheid (Y Oph) for which the pulsation is well resolved and a nonpulsating yellow supergiant (α Per) using long-baseline near-infrared interferometry. We interpreted these data using a simple CSE model we previously developed. We found that our observations of α Per do not provide evidence for a CSE. The measured CLD is explained by an hydrostatic photospheric model. Our observations of Y Oph, when compared to smaller baseline measurements, suggest that it is surrounded by a CSE with characteristics similar to CSEs found previously around other Cepheids. We have determined the distance to Y Oph to be d=491+/-18 pc. Additional evidence points toward the conclusion that most Cepheids are surrounded by faint CSEs, detected by near-infrared interferometry: after observing four Cepheids, all show evidence for a CSE. Our CSE nondetection around a nonpulsating supergiant in the instability strip, α Per, provides confidence in the detection technique and suggests a pulsation driven mass-loss mechanism for the Cepheids.

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