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A&A Supplement Ser., Vol. 124, August 1997, 329-347

Received August 2; accepted November 26, 1996

Be stars in open clusters

II. Balmer line spectroscopygif

J.M. Torrejóntex2html_wrap1545 - J. Fabregattex2html_wrap1547 - G. Bernabeutex2html_wrap1549 - S. Albatex2html_wrap1551

Send offprint request: J.M.

tex2html_wrap1553  Departamento de Astronomıa y Astrofısica, Universidad de Valencia, 46100 Burjassot, Valencia, Spain
tex2html_wrap1555  Departamento de Ingenierıa de Sistemas y Comunicaciones, Universidad de Alicante, Apdo. 99, 03080 Alicante, Spain


We present Htex2html_wrap_inline1513 line profiles (tex2html_wrap_inline1515, tex2html_wrap_inline1517 at continuum level, tex2html_wrap_inline1519 for some objects) for 58 stars in 8 northern open clusters and associations, complemented with Htex2html_wrap_inline1521 and Htex2html_wrap_inline1523 profiles for 36 of them as well as Htex2html_wrap_inline1525 and Htex2html_wrap_inline1527 for 16 programme stars. Our observations, though lower in resolution, yield results which are in good agreement with those obtained in earlier works based mainly on field Be stars. Our data suggest a similar spectroscopic behavior for both field and cluster Be stars.

The line parameters (EW, FWHM, tex2html_wrap_inline1531) have been obtained for each line. Nearly the whole set of stars have previously published quasi-simultaneous tex2html_wrap_inline1533 photometry, so a study of reliable correlations between photometric and spectroscopic data can be undertaken.

keywords: lines: profiles -- stars: emission line, be -- open clusters and associations: general

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