Astrochemical Properties of Planck Cold Clumps - Archive ouverte HAL Access content directly
Journal Articles The Astrophysical Journal Supplement Series Year : 2017

Astrochemical Properties of Planck Cold Clumps

, , , , , , , , , , , , , , , , , (1) , , , , , , , , ,
1
Ken'Ichi Tatematsu
  • Function : Author
Tie Liu
  • Function : Author
Satoshi Ohashi
Patricio Sanhueza
Quang Nguyen Lu'O'Ng
  • Function : Author
Tomoya Hirota
Sheng-Yuan Liu
  • Function : Author
Naomi Hirano
  • Function : Author
Minho Choi
  • Function : Author
Miju Kang
  • Function : Author
Mark A. Thompson
  • Function : Author
Gary Fuller
  • Function : Author
Yuefang Wu
  • Function : Author
Di Li
  • Function : Author
James Di Francesco
Kee-Tae Kim
Ke Wang
Mika Juvela
  • Function : Author
Hiroko Shinnaga
Maria Cunningham
  • Function : Author
Masao Saito
  • Function : Author
Jeong-Eun Lee
  • Function : Author
L. Viktor Tóth
  • Function : Author
Jinhua He
  • Function : Author
Takeshi Sakai
Jungha Kim
  • Function : Author

Abstract

We observed 13 Planck cold clumps with the James Clerk Maxwell Telescope/SCUBA-2 and with the Nobeyama 45 m radio telescope. The N2H+ distribution obtained with the Nobeyama telescope is quite similar to SCUBA-2 dust distribution. The 82 GHz HC3N, 82 GHz CCS, and 94 GHz CCS emission are often distributed differently with respect to the N2H+ emission. The CCS emission, which is known to be abundant in starless molecular cloud cores, is often very clumpy in the observed targets. We made deep single-pointing observations in DNC, HN13C, N2D+, and cyclic-C3H2 toward nine clumps. The detection rate of N2D+ is 50%. Furthermore, we observed the NH3 emission toward 15 Planck cold clumps to estimate the kinetic temperature, and confirmed that most targets are cold (≲20 K). In two of the starless clumps we observed, the CCS emission is distributed as it surrounds the N2H+ core (chemically evolved gas), which resembles the case of L1544, a prestellar core showing collapse. In addition, we detected both DNC and N2D+. These two clumps are most likely on the verge of star formation. We introduce the chemical evolution factor (CEF) for starless cores to describe the chemical evolutionary stage, and analyze the observed Planck cold clumps.

Dates and versions

insu-03677081 , version 1 (24-05-2022)

Identifiers

Cite

Ken'Ichi Tatematsu, Tie Liu, Satoshi Ohashi, Patricio Sanhueza, Quang Nguyen Lu'O'Ng, et al.. Astrochemical Properties of Planck Cold Clumps. The Astrophysical Journal Supplement Series, 2017, 228, ⟨10.3847/1538-4365/228/2/12⟩. ⟨insu-03677081⟩
3 View
0 Download

Altmetric

Share

Gmail Facebook Twitter LinkedIn More