Astronomy and Astrophysics – Astrophysics
Scientific paper
Aug 1995
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995a%26a...300..525a&link_type=abstract
Astronomy and Astrophysics, v.300, p.525
Astronomy and Astrophysics
Astrophysics
6
Interstellar Medium: Individual Objects: L 1188, Stars: Formation, Stars: Pre-Main Sequence, Ism: Clouds, Molecules, Radio Lines: Ism
Scientific paper
We present a study on the molecular distribution and star formation in L 1188, a dark cloud complex in Cepheus. The spatial distribution of dust particles, derived from IRAS maps, indicates that L 1188 is physically connected to the nearby S140 region, therefore we adopt the distance of S140, 910pc, as that of L 1188. This connection also indicates that L 1188 may belong to the Cepheus Bubble, a giant ring around the Cep OB2 association. ^13^CO observations have been performed with the 4m radiotelescope at Nagoya University, covering a field of 74'x44' around L 1188. Six molecular clumps are found in the observed region, and for each clump physical parameters such as excitation temperature, peak H_2_ column density, and molecular mass are derived, as well as the clumps' virial stability is investigated. The total mass of the complex is estimated to be ~1800Msun_. We have carried out an optical photographic survey for Hα emission line stars with the Schmidt telescope at Konkoly Observatory, and found 15 T Tau candidate stars in the L 1188 region, 10 of which seem to be associated with molecular emission regions. We also searched for YSOs in the IRAS Point Source Catalog, and selected 6 young objects close to the cloud. The number of young infrared sources having L_IR_>10Lsun_ per solar mass was found to be relatively high in L 1188 in comparison with other dark cloud complexes, indicating low-to-intermediate mass star formation in this cloud. The YSO candidates show a highly inhomogeneous spatial distribution: they are associated with clumps located at the lower galactic longitude part of the complex. Clumps with star formation have been found to have slightly higher excitation temperatures, more negative radial velocities, and narrower ^13^CO line profiles, than those without star formation.
Ábrahám Peter
Dobashi Kazuhito
Fukui Yasuo
Mizuno Akira
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