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Infrared Differential Photometry of Selected Orbital Binaries1

Published online by Cambridge University Press:  22 February 2018

Patricia Lampens ,
Jean-Louis Prieur  and
Robert Argyle
Patricia Lampens
Affiliation:
Royal Observatory of Belgium, Brussels, Belgium. (patricia.lampens@oma.be)
Jean-Louis Prieur
Affiliation:
Observatoire de Midi-Pyrénées, Toulouse, France
Robert Argyle
Affiliation:
Institute of Astronomy, University of Cambridge, United Kingdom

Abstract

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High-angular resolution observations were acquired for a sample of F-G and K nearby orbital binaries, making use of the ADONIS instrument mounted at the 3.6m ESO telescope from La Silla observatory. The aim is to derive broad-band near-infrared colours for the individual components of those binaries which do not fit well the mean mass-luminosity relation, but which have accurate parallaxes (from the Hipparcos satellite) and high-quality orbits, thanks to many previous efforts. Such colour determinations allow component temperatures and photometric mass ratios to be derived.

Resumen

Resumen

Hemos efectuado observaciones de alta resolución angular para estrellas binarias cercanas de tipo F-G y K usando la técnica de óptica adaptativa - el instrumento ADONIS - y el telescopio ESO de 3.6m del observatorio de La Silla. La meta es obtener índices de color con los filtros (J,H,K) para las componentes individuales de aquellas binarias que no se ajustan a la relación media masa-luminosidad, pero que tienen paralajes exactas y órbitas de alta calidad. Las mediciones de los índices de color permiten la determinación de las temperaturas individuales y de los cocientes de masa

Keywords

BinariesVisual — StarsFundamental Parameters — TechniquesHigh-Angular Resolution
Type
Observational properties and Statistics of Binary Stars in the Field
Information
International Astronomical Union Colloquium , Volume 191: The Environment and Evolution of Double and Multiple Stars , August 2004 , pp. 75 - 76
Copyright
Copyright © Instituto de Astronomia – Mexico 2004

Footnotes

1

Based on observations made at ESO (P66.D-0538)

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