ATLASGAL -- A Galaxy-wide sample of dense filamentary structures

TL;DR

This paper presents a comprehensive catalog of dense filamentary structures across the Galaxy from the ATLASGAL survey, analyzing their properties, distribution, and relation to star formation and Galactic dynamics.

Contribution

It provides the first large-scale, Galaxy-wide catalog of dense filaments with detailed physical properties, linking filament characteristics to spiral arms and star formation.

Findings

Filaments have a median distance of 3.8 kpc and a mean mass of a few 10^3 solar masses.

Approximately 20% of filaments are sites of ongoing massive star formation.

Filaments are aligned with the Galactic mid-plane and correlated with spiral arms.

Abstract

[Abridged] Aims. We study the properties of filamentary structures from the ATLASGAL survey. Methods. We use the DisPerSE algorithm to identify spatially coherent structures located across the inner-Galaxy (300 < l < 60 and |b| < 1.5). Results. We have determined distances, masses and physical sizes for 241 of the filamentary structures. We find a median distance of 3.8 kpc, a mean mass of a few 10^3 m_sun, a mean length of ~6pc and a mass-to-length ratio of (M/L) ~200-2000M_sun/ pc. We also find that these filamentary structures are tightly correlated with the spiral arms in longitude and velocity, and that their semi-major axis is preferentially aligned parallel to the Galactic mid-plane and therefore with the direction of large-scale Galactic magnetic field. We find many examples where the dense filaments identified in ATLASGAL are associated with larger scale filamentary structures (~100 pc), and argue that this is likely to be common, and as such these may indicate a connection between large-scale Galactic dynamics and star formation. Conclusions. We have produced a large and Galaxy-wide catalogue of dense filamentary structures that are representative of a particular size and mass range not previously well studied in the literature. Analyses of the properties and distribution of these filaments reveals that they are correlated with the spiral arms and make a significant contribution to star formation in the Galaxy. Massive star formation is ongoing within ~20% of the filaments and is strongly correlated with the filaments with the largest mass-to- length ratios. The luminosity of the embedded sources has a similar distribution to the Galactic-wide samples of young massive stars and can therefore be considered to be representative.