Star formation in L 1251. II. "The next generation" - NH_3_ cores.

Details Star formation in L 1251. II. "The next generation" - NH_3_ cores. Star formation in L 1251. II. "The next generation" - NH_3_ cores.

Jul 1996

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1996a%26a...311..981t&link_type=abstract

Astronomy and Astrophysics, v.311, p.981-988

Astronomy and Astrophysics

Astrophysics

20

Interstellar Medium: Clouds, Molecules, Individual Objects: L 1251, Cepheus Flare

Scientific paper

We have mapped the NH_3_(1,1) and (2,2) transitions towards the L 1251 dark cloud . Our observations covered an area of 0.12 square degrees sampled at intervals of 80" (2 times the HPBW). We detected eight ammonia cores with typical sizes (at half power) of 2' (0.2pc at 350pc distance). We estimate that the cores have a maximum H_2_ density of order 10^5^cm^-3^ and average T_kin_ of 10K. Their masses are in the range of 5-34Msun_ and they typically are close to virial equilibrium, By comparison with earlier maps of C^18^O, we estimate the fraction of the cloud material in the form of dense (>10^4^cm^-3^) cores to be of order 40 percent.

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