The straight and isolated G350.54+0.69 filament: density profile and star formation content

TL;DR

This study analyzes the properties and star formation activity of the isolated, straight filament G350.54+0.69, revealing its structure, core distribution, and ongoing low-mass star formation, and comparing it to similar nearby filaments.

Contribution

It provides detailed observational analysis of G350.54+0.69's density profile, core properties, and star formation, highlighting its intermediate evolutionary stage and the role of filament morphology.

Findings

G350.54+0.69 consists of two filaments with distinct lengths and masses.

Core separations and line mass follow sausage instability predictions.

Evidence of ongoing low-mass star formation in the filament.

Abstract

We investigate the global properties of the straight and isolated filamentary cloud G350.54+0.69 using Herschel continuum and APEX molecular line data. The overall straight morphology is similar to two other well studied nearby filaments (Musca and Taurus-B211/3) while the isolated nature of G350.54+0.69 appears similar to Musca. G350.54+0.69 is composed of two distinct filaments with a length ~5.9 pc for G350.5-N (~2.3 pc for G350.5-S), a total mass of ~810 $M_{\odot}$ (~ 110 $M_{\odot}$), and a mean temperature of ~ 18.2 K (~17.7 K). We identify 9 dense and gravitationally bound cores in the whole cloud G350.54+0.69. The separations between cores and the line mass of the whole cloud appear to follow the predictions of the "sausage" instability theory, which suggests that G350.54+0.69 could have undergone radial collapse and fragmentation. The presence of young protostars is consistent with this hypothesis. The line masses of the two filaments (~120 $M_{\odot}$ pc$^{-1}$ for G350.5-N, and ~45 $M_{\odot}$ pc$^{-1}$ for G350.5-S), mass-size distributions of the dense cores, and low-mass protostars collectively suggest that G350.54+0.69 is a site of ongoing low-mass star formation. Based on the above evidence, we place G350.54+0.69 in an intermediate evolutionary state between Musca and Taurus-B211/3. We suggest that investigations into straight (and isolated) versus those distributed inside molecular clouds may provide important clues into filament formation and evolution.