Molecular filament formation and filament-cloud interaction: Hints from Nobeyama 45m telescope observations

TL;DR

This study uses Nobeyama 45m telescope observations to analyze the velocity structure and interactions of an interstellar filament in the Taurus molecular cloud, revealing complex dynamics and possible formation mechanisms.

Contribution

It provides new insights into filament-cloud interactions and proposes a multi-interaction scenario involving sheet-like structures affecting filament evolution.

Findings

Filament is a ~1pc long, ~0.06pc wide structure with a single velocity component.

Extended structures with different velocities surround the filament, indicating complex interactions.

A faint filament suggests formation via magnetic field convergence and shock compression.

Abstract

We present Nobeyama 45m telescope C18O, 13CO, and 12CO(1-0) mapping observations towards an interstellar filament in the Taurus molecular cloud. We investigate the gas velocity structure along the filament and in its surrounding parent cloud. The filament is detected in the optically thin C18O emission as a single velocity component, ~1pc long, ~0.06pc wide structure. The C18O emission traces dust column densities larger than ~5x10^21 cm-2. The line-of-sight (LOS) velocity fluctuates along the filament crest with an average amplitude of ~0.2 km/s. The 13CO and 12CO integrated intensity maps show spatially extended emission around the elongated filament. We identify three extended structures with LOS velocities redshifted and blueshifted with respect to the average velocity of the filament identified in C18O. Based on combined analyses of velocity integrated channel maps and intensity variations of the optically thick 12CO spectra on and off the filament, we propose a 3-dimensional structure of the cloud surrounding the filament. We further suggest a multi-interaction scenario where sheet-like extended structures interact, in space and time, with the filament and are responsible for its compression and/or disruption, playing an important role in the star formation history of the filament. We also identify, towards the same field, a very faint filament showing a velocity field compatible with the filament formation process proposed by Inoue et al. (2017), where a filament is formed due to convergence of a flow of matter generated by the bending of the ambient magnetic field structure induced by an interstellar shock compression.