Gravitationally bound cores in a molecular cirrus cloud

Details Gravitationally bound cores in a molecular cirrus cloud Gravitationally bound cores in a molecular cirrus cloud

Feb 2002

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2002a%26a...383..591h&link_type=abstract

Astronomy and Astrophysics, v.383, p.591-597 (2002)

Astronomy and Astrophysics

Astrophysics

20

Stars: Formation, Ism: Abundances, Ism: Clouds, Ism: Individual Objects: Mcld 123.5+24.9, Ism: Molecules, Ism: Dust

Scientific paper

Using MAMBO at the IRAM 30 m telescope we have observed a dense core in the cirrus cloud MCLD 123.5+24.9 in the dust continuum emission at 250 GHz. The core is detected as an elongated filament with an extent of 4. '2x 0. '7, corresponding to 0.18 pcx0.03 pc at an adopted distance of 150 pc. We find a close correlation between the continuum emission and previously observed C18O (1->0) line emission. Using standard dust models we derive hydrogen column densities of up to 1022 cm-2. The total mass for the filament is about 0.66 Msolar. We also present observations of the HC3N (3->2), (4->3), and (10->9) emission lines obtained with the MPIfR 100 m and the IRAM 30 m telescopes. The distribution is very different from the dust continuum and the C18O (1->0) line emission. HC3N is concentrated in two distinct clumps located at the ends of the filament seen in the other tracers. Based on a LVG analysis of the HC3N transitions we derive column densities of N(HC3N)/Delta v~1013cm-2/kms and volume densities of n(H_2)~105 cm-3. We find that the HC3N clumps have masses of 0.13 and 0.19 Msolar. Our data demonstrate that the cirrus cloud cores are gravitationally bound, and that they show chemical structure indicating different evolutionary stages within the cloud.

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