DENSE GAS IN MOLECULAR CORES ASSOCIATED WITH PLANCK GALACTIC COLD CLUMPS

Journal Article · Sun Mar 20 04:00:00 EDT 2016 · Astrophysical Journal

DOI:https://doi.org/10.3847/0004-637X/820/1/37· OSTI ID:22524938

Yuan, Jinghua; Li, Jin Zeng; Liu, Hong-Li ^[1]; Wu, Yuefang; Chen, Ping; Hu, Runjie ^[2]; Liu, Tie ^[3]; Zhang, Tianwei ^[4]; Meng, Fanyi ^[5]; Wang, Ke ^[6]

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1. National Astronomical Observatories, Chinese Academy of Sciences, 20A Datun Road, Chaoyang District, Beijing 100012 (China)
2. Department of Astronomy, Peking University, 100871 Beijing (China)
3. Korea Astronomy and Space Science Institute 776, Daedeokdae-ro, Yuseong-gu, Daejeon, 305-348 (Korea, Republic of)
4. Peking University Health Science Center, Xueyuan Road 38th, Haidian District, Beijing 100191 (China)
5. Physikalisches Institut, Universität zu Köln, Zülpicher Str. 77, D-50937 (Germany)
6. European Southern Observatory, Karl-Schwarzschild-Str. 2, D-85748 Garching bei München (Germany)

We present the first survey of dense gas toward Planck Galactic Cold Clumps (PGCCs). Observations in the J = 1–0 transitions of HCO{sup +} and HCN toward 621 molecular cores associated with PGCCs were performed using the Purple Mountain Observatory’s 13.7 m telescope. Among them, 250 sources were detected, including 230 cores detected in HCO{sup +} and 158 in HCN. Spectra of the J = 1–0 transitions from {sup 12}CO, {sup 13}CO, and C{sup 18}O at the centers of the 250 cores were extracted from previous mapping observations to construct a multi-line data set. The significantly low detection rate of asymmetric double-peaked profiles, together with the good consistency among central velocities of CO, HCO{sup +}, and HCN spectra, suggests that the CO-selected Planck cores are more quiescent than classical star-forming regions. The small difference between line widths of C{sup 18}O and HCN indicates that the inner regions of CO-selected Planck cores are no more turbulent than the exterior. The velocity-integrated intensities and abundances of HCO{sup +} are positively correlated with those of HCN, suggesting that these two species are well coupled and chemically connected. The detected abundances of both HCO{sup +} and HCN are significantly lower than values in other low- to high-mass star-forming regions. The low abundances may be due to beam dilution. On the basis of an inspection of the parameters given in the PGCC catalog, we suggest that there may be about 1000 PGCC objects that have a sufficient reservoir of dense gas to form stars.

• OSTI ID: 22524938
• Journal Information: Astrophysical Journal, Journal Name: Astrophysical Journal Journal Issue: 1 Vol. 820; ISSN ASJOAB; ISSN 0004-637X
• Country of Publication: United States
• Language: English

Related Subjects

79 ASTRONOMY AND ASTROPHYSICS
CARBON 12
CARBON 13
CARBON MONOXIDE
CATALOGS
CLOUDS
DETECTION
EMISSION SPECTRA
HYDROCYANIC ACID
LINE WIDTHS
MAPPING
MASS
MOLECULES
OXYGEN 18
STAR EVOLUTION
STARS
TELESCOPES
VELOCITY