The remarkable pre-main sequence object V1318 Cygni

Details The remarkable pre-main sequence object V1318 Cygni The remarkable pre-main sequence object V1318 Cygni

Feb 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994a%26a...282l..25a&link_type=abstract

Astronomy and Astrophysics (ISSN 0004-6361), vol. 282, no. 2, p. L25-L28

Astronomy and Astrophysics

Astronomy

26

Infrared Astronomy, Light (Visible Radiation), Pre-Main Sequence Stars, Radio Astronomy, Star Clusters, Stellar Envelopes, Astronomical Photometry, Astronomical Spectroscopy, Charge Coupled Devices, Interstellar Extinction, Stellar Luminosity

Scientific paper

We present optical, near-IR, and sub-mm observations of the young pre-main sequence (PMS) star V1318 Cygni. Together with the Herbig Ae/Be (HAEBE) stars BD+40 4124 and V1686 Cygni, these objects form a small cluster of young emission line stars. The optically brightest member is BD+40 4124. At wavelengths greater than or = 5 micrometers however, V1318 Cygni is the dominant source. In the optical and near-IR, V1318 Cygni resolves into three distinct components oriented north-south with a total separation of 5 sec. The northern (N) and southern (S) sources appear stellar. Both are photometrically variable. The middle (M) source appears to be a nebulous knot in the optical while at 2 micrometers, its morphology suggests it may be a nebulous bridge or stream joining N ans S. We suggest that V1318 Cygni is a young, PMS binary, possible interacting, with a projected separation of approximately 5000 A.U. The southern object is likely of intermediate-mass and probably a very young HAEBE stars. The northern object is possible a young, low-mass star.

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