Giant molecular filaments in the Milky Way

II. The fourth Galactic quadrant^⋆

¹ Max-Planck-Institut für Astronomie (MPIA), Königstuhl 17, 69117 Heidelberg, Germany
e-mail: abreu@mpia-hd.mpg.de
² School of Physics and Astronomy, University of Leeds, Leeds, LS2 9JT, UK

Received: 2 November 2015
Accepted: 16 March 2016

Abstract

Context. Filamentary structures are common morphological features of the cold, molecular interstellar medium (ISM). Recent studies have discovered massive, hundred-parsec-scale filaments that may be connected to the large-scale, Galactic spiral arm structure. Addressing the nature of these giant molecular filaments (GMFs) requires a census of their occurrence and properties.

Aims. We perform a systematic search of GMFs in the fourth Galactic quadrant and determine their basic physical properties.

Methods. We identify GMFs based on their dust extinction signatures in the near- and mid-infrared and the velocity structure probed by ¹³CO line emission. We use the ¹³CO line emission and ATLASGAL dust emission data to estimate the total and dense gas masses of the GMFs. We combine our sample with an earlier sample from literature and study the Galactic environment of the GMFs.

Results. We identify nine GMFs in the fourth Galactic quadrant: six in the Centaurus spiral arm and three in inter-arm regions. Combining this sample with an earlier study using the same identification criteria in the first Galactic quadrant results in 16 GMFs, nine of which are located within spiral arms. The GMFs have sizes of 80–160 pc and ¹³CO-derived masses between 5−90 × 10⁴M_⊙. Their dense gas mass fractions are between 1.5–37%, which is higher in the GMFs connected to spiral arms. We also compare the different GMF-identification methods and find that emission and extinction-based techniques overlap only partially, thereby highlighting the need to use both to achieve a complete census.