Artículo de revista
Molecular cloud cores with a high deuterium fraction: Nobeyama single-pointing survey
Fecha
2020Registro en:
The Astrophysical Journal Supplement Series, 249:33 (53pp), 2020
10.3847/1538-4365/aba746
Autor
Kim, Gwanjeong
Tatematsu, Ken'ichi
Liu, Tie
Yi, Hee-Weon
He, Jinhua
Hirano, Naomi
Liu, Sheng-Yuan
Choi, Minho
Sanhueza, Patricio
Tóth, L. Viktor
Evans II, Neal J.
Feng, Siyi
Juvela, Mika
Kim, Kee-Tae
Vastel, Charlotte
Lee, Jeong-Eun
Lu'o'ng, Quang Nguyễn
Kang, Miju
Ristorcelli, Isabelle
Fehér, Orsolya
Wu, Yuefang
Ohashi, Satoshi
Wang, Ke
Kandori, Ryo
Hirota, Tomoya
Sakai, Takeshi
Lu, Xing
Thompson, Mark A.
Fulle, Gary A.
Li, Di
Shinnaga, Hiroko
Kim, Jungha
Institución
Resumen
We present the results of a single-pointing survey of 207 dense cores embedded in Planck Galactic Cold Clumps distributed in five different environments (lambda Orionis, Orion A, Orion B, the Galactic plane, and high latitudes) to identify dense cores on the verge of star formation for the study of the initial conditions of star formation. We observed these cores in eight molecular lines at 76-94 GHz using the Nobeyama 45 m telescope. We find that early-type molecules (e.g., CCS) have low detection rates and that late-type molecules (e.g., N(2)H(+)and c-C3H2) and deuterated molecules (e.g., N(2)D(+)and DNC) have high detection rates, suggesting that most of the cores are chemically evolved. The deuterium fraction (D/H) is found to decrease with increasing distance, indicating that it suffers from differential beam dilution between the D/H pair of lines for distant cores (>1 kpc). For lambda Orionis, Orion A, and Orion B located at similar distances, D/H is not significantly different, suggesting that there is no systematic difference in the observed chemical properties among these three regions. We identify at least eight high-D/H cores in the Orion region and two at high latitudes, which are most likely to be close to the onset of star formation. There is no clear evidence of the evolutionary change in turbulence during the starless phase, suggesting that the dissipation of turbulence is not a major mechanism for the beginning of star formation as judged from observations with a beam size of 0.04 pc.