EDP Sciences
Free Access
Issue
A&A
Volume 489, Number 2, October II 2008
Page(s) 627 - 631
Section Interstellar and circumstellar matter
DOI https://doi.org/10.1051/0004-6361:20079117
Published online 01 August 2008


A&A 489, 627-631 (2008)
DOI: 10.1051/0004-6361:20079117

Sub-milliarcsecond precision spectro-astrometry of Be stars

R. D. Oudmaijer1, A. M. Parr1, D. Baines2, 1, and J. M. Porter3

1  School of Physics and Astronomy, University of Leeds, Leeds LS2 9JT, UK
    e-mail: roud@ast.leeds.ac.uk
2  National Physical Laboratory, Hampton Road, Teddington TW11 0LW, UK
3  Astrophysics Research Institute, Liverpool John Moores University, Twelve Quays House, Egerton Wharf, Birkenhead CH41 1 LD, UK

Received 21 November 2007 / Accepted 22 July 2008

Abstract
Context. The origin of the disks around Be stars is still not known. Further progress requires a proper parametrization of their structure, both spatially and kinematically. This is challenging as the disks are very small.
Aims. Here we assess whether a novel method is capable of providing these data.
Methods. We obtained spectro-astrometry around the Pa$\beta$ line of two bright Be stars, $\alpha$ Col and $\zeta$ Tau, to search for disk signatures. The data, with a pixel-to-pixel precision of the centroid position of 0.3..0.4 milliarcsecond is the most accurate such data to date. Artefacts at the 0.85 mas level are present in the data, but these are readily identified as they were non-repeatable in our redundant datasets. This does illustrate the need of taking multiple data to avoid spurious detections.
Results. The data are compared with model simulations of the spectro-astrometric signatures due to rotating disks around Be stars. The upper limits we find for the disk radii correspond to disk sizes of a few dozen stellar radii if they rotate Keplerian. This is very close to observationally measured and theoretically expected disk sizes, and this paper therefore demonstrates that spectro-astrometry, of which we present the first such attempt, has the potential to resolve the disks around Be stars.


Key words: techniques: high angular resolution -- techniques: spectroscopic -- stars: individual: $\alpha$ Col, $\zeta$ Tau -- stars: emission-line, Be



© ESO 2008

Current usage metrics show cumulative count of Article Views (full-text article views including HTML views, PDF and ePub downloads, according to the available data) and Abstracts Views on Vision4Press platform.

Data correspond to usage on the plateform after 2015. The current usage metrics is available 48-96 hours after online publication and is updated daily on week days.

Initial download of the metrics may take a while.