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Revista mexicana de astronomía y astrofísica

Print version ISSN 0185-1101

Rev. mex. astron. astrofis vol.42 n.2 Ciudad de México Oct. 2006

 

New T tauri stars associated with IRAS 05555-14051

 

Marco A. Moreno-Corral2, Carlos Chavarría-K2 and E. de Lara2

 

2 Instituto de Astronomía, UNAM, Apdo. Postal 877, 22860 Ensenada, B. C., México (Chavarri, Estela, mam@astrosen.unam.mx).

 

Received 2006 January 18
Accepted 2006 April 24

 

RESUMEN

Se presenta por primera vez espectroscopía de rendija de resolución media (∆λ/λ = 1320 Å) y la clasificación espectral MK para las estrellas más brillantes que forman el trapecio estelar asociado con la fuente IRAS 05555-1405, en la nebulosa de reflexión vdB64. Los espectros de los cinco miembros más brillantes del conglomerado presentan la línea del Li I λ6708, característica propia de estrellas de Pre-Secuencia Principal (PMS). Nuestros datos se confrontaron con los reportados en el cercano infrarrojo (NIR) en el 2 Micron All Sky Survey (2MASS) para las estrellas, los cuales confirman nuestros resultados.

 

ABSTRACT

We present for the first time medium resolution (∆λ/λ = 1320 Å) slit spectroscopy and MK classifications for the brightest stars that comprise the stellar trapezium associated with IRAS point source IRAS 05555-1405, in the vdB64 reflection nebula. The five brightest members of the trapezium are found through their Li I λ6708 feature to be pre-main sequence (PMS) stars. Our data are compared with those of the near infrared (NIR) 2 Micron All Sky Survey (2MASS) which confirms our results.

Key Words: STARS: INDIVIDUAL (IRAS 05555-1405) - STARS: PRE-MAIN SEQUENCE.

 

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Acknowledgements

The authors acknowledge the logistic support of the personnel of SPMO, particularly that of the technical staff and of the night assistants F. Montalvo, G. García, S. Monroy, and the comments of an anonymous referee. Dr. Lynne Valencic proofread the manuscript. This work makes use of data products of the Two Micron Sky Survey by the University of Massachusetts and the Infrared and Processing Analysis Center/California Institute of Technology, funded by the NASA and NSF (USA), and of the Centre de Données Astronomiques de Strasbourg, CDS (France). The present work was supported with grants of Consejo Nacional de Ciencia y Tecnología de México (grants 400340-4-2243-PE and 400354-5-277757-E).

 

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NOTE:

1 Based on observations collected at the Observatorio Astronómico Nacional, San Pedro Mártir, B. C., México.

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