Luis F. Rodríguez,1 Luis Zapata,1,2 and Paul T. P. Ho3,2
1 Centro de Radiostronomía y Astrofísica, Universidad Nacional Autónoma de México, Apdo. Postal 3–72, (Xangari), 58089 Morelia, Michoacán, Mexico (l.rodriguez@astrosmo.unam.mx, l.zapata@astrosmo.unam.mx)
2 Harvard–Smithsonian Center for Astrophysics and Submillimeter Array, 60 Garden Street, Cambridge, MA 02138, USA (ho@cfa.harvard.edu)
3 Academia Sinica, Institute of Astronomy and Astrophysics, P.O. Box 23–141, Taipei 106, Taiwan (pho@asiaa.sinica.edu.tw)
Received 2006 June 27
Accepted 2006 November 8
RESUMEN
Presentamos observaciones de alta resolución angular y alta sensitividad, hechas con el Very Large Array a 3.6 cm, de la estrella Ae de Herbig AB Aur. Esta estrella es de interés porque su disco circunestelar muestra características que se han atribuido a la presencia de una companera de baja masa o de un planeta gaseoso gigante, aún sin detectar. Nuestra imagen confirma la emisión de continuo que se sabe existe en asociación con la estrella, y detecta una débil protuberancia que se extiende aproximadamente 0".3 al SE de la estrella. Consideraciones teóricas y resultados observacionales previos son consistentes con la presencia de una companera de AB Aur con la separación y ángulo de posición derivados de nuestros datos de radio. También determinamos los movimientos propios de AB Aur comparando nuestras nuevas observaciones con datos tomados 17 años atrás, y encontramos valores consistentes con los determinados por Hipparcos.
ABSTRACT
We present high angular resolution, high–sensitivity Very Large Array observations at 3.6 cm of the Herbig Ae star AB Aur. This star is of interest since its circumstellar disk exhibits characteristics that have been attributed to the presence of an undetected low mass companion or giant gas planet. Our image confirms the continuum emission known to exist in association with the star, and detects a faint protuberance that extends about 0".3 to its SE. Previous theoretical considerations and observational results are consistent with the presence of a companion to AB Aur with the separation and position angle derived from our radio data. We also determine the proper motion of AB Aur by comparing our new observations with data taken about 17 years ago and find values consistent with those found by Hipparcos.
Key Words: BINARIES: VISUAL - RADIO CONTINUUM: STARS - STARS: EMISSION–LINE, BE - STARS: FORMATION - STAR: MASS LOSS
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