The Serpens filament at the onset of slightly supercritical collapse^★

¹ Max-Planck Institute für Radioastronomy, Auf dem Hügel 69, 53121 Bonn, Germany
e-mail: ygong@mpifr-bonn.mpg.de; gongyan2444@gmail.com
² Purple Mountain Observatory & Key Laboratory for Radio Astronomy, Chinese Academy of Sciences, 2 West Beijing Road, 210008 Nanjing, PR China
³ University Observatory Munich, Scheinerstrasse 1, 81679 München, Germany
⁴ South-Western Institute for Astronomy Research, Yunnan University, Kunming, Yunnan 650500, PR China
⁵ Astronomy Department, Faculty of Science, King Abdulaziz University, PO Box 80203, Jeddah 21589, Saudi Arabia
⁶ Xinjiang Astronomical Observatory, Chinese Academy of Sciences, 830011 Urumqi, PR China
⁷ Department of Astronomy, University of Arizona, 933 North Cherry Avenue, Tucson, AZ 85721, USA

Received: 6 June 2018
Accepted: 13 September 2018

Abstract

The Serpens filament, as one of the nearest infrared dark clouds, is regarded as a pristine filament at a very early evolutionary stage of star formation. In order to study its molecular content and dynamical state, we mapped this filament in seven species: C¹⁸O, HCO⁺, HNC, HCN, N₂H⁺, CS, and CH₃OH. Among them, HCO⁺, HNC, HCN, and CS show self-absorption, while C¹⁸O is most sensitive to the filamentary structure. A kinematic analysis demonstrates that this filament forms a velocity-coherent (trans)sonic structure, a large part of which is one of the most quiescent regions in the Serpens cloud. Widespread C¹⁸O depletion is found throughout the Serpens filament. Based on the Herschel dust-derived H₂ column density map, the line mass of the filament is 36–41 M_⊙ pc⁻¹, and its full width at half maximum is 0.17 ± 0.01 pc, while its length is ≈1.6 pc. The inner radial column density profile of this filament can be well fitted with a Plummer profile with an exponent of 2.2 ± 0.1, a scale radius of 0.018 ± 0.003 pc, and a central density of (4.0 ± 0.8) × 10⁴ cm⁻³. The Serpens filament appears to be slightly supercritical. The widespread blue-skewed HNC and CS line profiles and HCN hyperfine line anomalies across this filament indicate radial infall in parts of the Serpens filament. C¹⁸O velocity gradients also indicate accretion flows along the filament. The velocity and density structures suggest that such accretion flows are likely due to a longitudinal collapse parallel to the filament’s long axis. Both the radial infall rate (~72 M_⊙ Myr⁻¹, inferred from HNC and CS blue-skewed profiles) and the longitudinal accretion rate (~10 M_⊙ Myr⁻¹, inferred from C¹⁸O velocity gradients) along the Serpens filament are lower than all previously reported values in other filaments. This indicates that the Serpens filament lies at an early evolutionary stage when collapse has just begun, or that thermal and nonthermal support are effective in providing support against gravity.