A Molecular Line Observation toward Massive Clumps Associated with Infrared Dark Clouds

TL;DR

This study surveys molecular lines in 55 massive clumps within infrared dark clouds, revealing chemical evolution stages and star formation activity through detection patterns and line width analysis.

Contribution

It provides new observational data on molecular line emissions in massive clumps, highlighting chemical maturity and star formation indicators in IRDCs.

Findings

Most clumps show N2H+ and NH3 detections, indicating common molecular presence.

CCS emission is absent, suggesting advanced chemical evolution.

CH3OH detection correlates with star formation activity and broader linewidths.

Abstract

We have surveyed the N2H+ J=1-0, HC3N J=5-4, CCS J_N=4_3-3_2, NH3 (J, K) = (1, 1), (2, 2), (3, 3), and CH3OH J=7-6 lines toward the 55 massive clumps associated with infrared dark clouds by using the Nobeyama Radio Observatory 45 m telescope and the Atacama Submillimeter Telescope Experiment 10 m telescope. The N2H+, HC3N, and NH3 lines are detected toward most of the objects. On the other hand, the CCS emission is detected toward none of the objects. The [CCS]/[N2H+] ratios are found to be mostly lower than unity even in the Spitzer 24 micron dark objects. This suggests that most of the massive clumps are chemically more evolved than the low-mass starless cores. The CH3OH emission is detected toward 18 out of 55 objects. All the CH3OH-detected objects are associated with the Spitzer 24 micron sources, suggesting that star formation has already started in all the CH3OH-detected objects. The velocity widths of the CH3OH J_K=7_0-6_0 A+ and 7_{-1}-6_{-1} E lines are broader than those of N2H+ J=1-0. The CH3OH J_K=7_0-6_0 A+ and 7_{-1}-6_{-1} E lines tend to have broader linewidth in the MSX dark objects than in the others, the former being younger or less luminous than the latter. The origin of the broad emission is discussed in terms of the interaction between an outflow and an ambient cloud.