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Journal Article

Physical properties and chemical composition of the cores in the California molecular cloud

MPS-Authors

Zhang,  Guo-Yin
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Xu,  Jin-Long
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Vasyunin,  A. I.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Semenov,  D. A.
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Wang,  Jun-Jie
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Dib,  Sami
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Liu,  Tie
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Liu,  Sheng-Yuan
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Zhang,  Chuan-Peng
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Liu,  Xiao-Lan
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Wang,  Ke
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Li,  Di
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Wu,  Zhong-Zu
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Yuan,  Jing-Hua
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Li,  Da-Lei
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

Gao,  Yang
Max Planck Institute for Astronomy, Max Planck Society and Cooperation Partners;

External Resource

https://ui.adsabs.harvard.edu/abs/2018A&A...620A.163Z
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Citation

Zhang, G.-Y., Xu, J.-L., Vasyunin, A. I., Semenov, D. A., Wang, J.-J., Dib, S., et al. (2018). Physical properties and chemical composition of the cores in the California molecular cloud. Astronomy and Astrophysics, 620.


Cite as: https://hdl.handle.net/21.11116/0000-0005-CA1E-7
Abstract

Aims: We aim to reveal the physical properties and chemical composition of the cores in the California molecular cloud (CMC), so as to better understand the initial conditions of star formation.
Methods: We made a high-resolution column density map (18.2'') with Herschel data, and extracted a complete sample of the cores in the CMC with the fellwalker algorithm. We performed new single-pointing observations of molecular lines near 90 GHz with the IRAM 30m telescope along the main filament of the CMC. In addition, we also performed a numerical modeling of chemical evolution for the cores under the physical conditions.
Results: We extracted 300 cores, of which 33 are protostellar and 267 are starless cores. About 51% (137 of 267) of the starless cores are prestellar cores. Three cores have the potential to evolve into high-mass stars. The prestellar core mass function (CMF) can be well fit by a log-normal form. The high-mass end of the prestellar CMF shows a power-law form with an index α = -0.9 ± 0.1 that is shallower than that of the Galactic field stellar mass function. Combining the mass transformation efficiency (∊) from the prestellar core to the star of 15 ± 1% and the core formation efficiency (CFE) of 5.5%, we suggest an overall star formation efficiency of about 1% in the CMC. In the single-pointing observations with the IRAM 30m telescope, we find that 6 cores show blue-skewed profile, while 4 cores show red- skewed profile. [HCO+]/[HNC] and [HCO+]/[N2H+] in protostellar cores are higher than those in prestellar cores; this can be used as chemical clocks. The best-fit chemical age of the cores with line observations is 5 × 104 yr. Tables 3 and 4 are only available at the CDS via anonymous ftp to <A href="http://cdsarc.u-strasbg.fr">http://cdsarc.u-strasbg.fr</A> (ftp://130.79.128.5) or via <A href="http://cdsarc.u-strasbg.fr/viz- bin/qcat?J/A+A/620/A163">http://cdsarc.u-strasbg.fr/viz- bin/qcat?J/A+A/620/A163</A>