Volume 365, Number 2, January 2001
|Page(s)||110 - 114|
|Section||Interstellar and circumstellar matter|
|Published online||15 January 2001|
EXPORT: Near-IR observations of Vega-type and pre-main sequence stars*
Dpto. Física Teórica, C-XI, Facultad de Ciencias, Universidad Autónoma de Madrid, Cantoblanco, 28049 Madrid, Spain
2 Instituto de Astrofísica de Canarias, 38200 La Laguna, Tenerife, Spain
3 Instituto de Astrofísica de Andalucía, Apartado de Correos 3004, 18080 Granada, Spain
4 TNO/TPD-Space Instrumentation, Stieltjesweg 1, PO Box 155, 2600 AD Delft, The Netherlands
5 CNRS, Institute d'Astrophysique de Paris, 98bis Bd. Arago, 75014 Paris, France
6 NOAO/STIS, Goddard Space Flight Center, Code 681, NASA/GSFC, Greenbelt, MD 20771, USA
7 Physics & Astronomy, University of St. Andrews, North Haugh, St. Andrews KY16 9SS, Scotland, UK
8 Joint Astronomy Centre, 660 N. A'ohoku Place, Hilo, Hawaii 96720, USA
9 DLR Department of Planetary Exploration, Rutherfordstrasse 2, 12489 Berlin, Germany
10 L.A.E.F.F., VILSPA, Apartado de Correos 50727, 28080 Madrid, Spain
11 Department of Physics and Astronomy, University of Leeds, Leeds LS2 9JT, UK
12 Rutherford Appleton Laboratory, Didcot, Oxfordshire OX11 0QX, UK
13 Department of Physics, Center for Astrophysics and Space Sciences, University of California San Diego, Mail Code 0424, La Jolla, CA 92093-0424, USA
14 Observatoire de Paris, 92195 Meudon, France
15 SRON, Universiteitscomplex "Zernike", Landleven 12, PO Box 800, 9700 AV Groningen, The Netherlands
Corresponding author: C. Eiroa, firstname.lastname@example.org
Accepted: 12 October 2000
We present near-IR JHK photometric data of a sample of 58 main-sequence, mainly Vega-type, and pre-main sequence stars. The data were taken during four observing runs in the period May 1998 to January 1999 and form part of a coordinated effort with simultaneous optical spectroscopy and photo-polarimetry. The near-IR colors of the MS stars correspond in most cases to photospheric colors, although noticeable reddening is present towards a few objects, and these stars show no brightness variability within the observational errors. On the other hand, the PMS stars show near-IR excesses and variability consistent with previous data.
Key words: stars: emission-line, Be -stars: pre-main sequence -stars: variable: general -infrared: stars
© ESO, 2001
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