Low-mass star formation in the high galactic latitude dark cloud L 1642

Details Low-mass star formation in the high galactic latitude dark cloud L 1642 Low-mass star formation in the high galactic latitude dark cloud L 1642

Jul 1987

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1987a%26a...181..283s&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 181, no. 2, July 1987, p. 283-288. Research supported by the Danish Board for

Astronomy and Astrophysics

Astronomy

30

Astronomical Photometry, Infrared Astronomy, Pre-Main Sequence Stars, Star Formation, Hydrogen Clouds, Interstellar Matter, Near Infrared Radiation, Nebulae

Scientific paper

CCD imaging, spectroscopy, and infrared photometry have been carried out in a study of young stars in the high galactic latitude cloud L 1642. Two infrared sources, L 1642-1 and L 1642-2, both associated with IRAS point sources, are identified with faint nebulous binary stars. L 1642-1A is spectroscopically identified as a K 71V T Tauri star, obscured by a magnitude of about 2 of visual extinction. The secondary becomes quite bright in the far-red, and may possibly dominate the infrared emission. L 1642-2A is associated with a small compact reflection nebula. Its secondary is also very red and might be responsible for the far-infrared emission. Both binaries have very low luminosity, less than about 0.5 solar luminosities, if a distance of 100 pc is adopted. Both secondaries appear very active, L 1642-1B has Br-gamma emission, while L 1642-2B exhibits molecular hydrogen emission in the infrared. L 1642 is one of the very nearest star forming clouds.

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