An analysis of star formation with Herschel in the Hi-GAL Survey. II. The tips of the Galactic bar

TL;DR

This study analyzes star formation at the tips of the Galactic bar using Herschel data, estimating star-formation rates and efficiencies, and finding that activity is driven by available material rather than triggering mechanisms.

Contribution

It introduces a new Monte Carlo-based method to estimate star-formation rates from turbulent core evolution, applied specifically to the Galactic bar region.

Findings

Star-formation rate density at the bar tips is approximately 1.2-1.5 x 10^-3 Msol/yr/kpc^2.

Conversion efficiency of star formation is around 0.5-0.8%, with no significant difference near the bar.

Star formation activity correlates with dust and molecular material abundance, not triggering processes.

Abstract

We present the physical and evolutionary properties of prestellar and protostellar clumps in the Herschel Infrared GALactic plane survey (Hi-GAL) in two large areas centered in the Galactic plane and covering the tips of the long Galactic bar at the intersection with the spiral arms. The areas fall in the longitude ranges 19 < l < 33 and 340 < l < 350, while latitude is -1 < b < 1. Newly formed high mass stars and prestellar objects are identified and their properties derived and compared. A study is also presented on five giant molecular complexes at the further edge of the bar. The star-formation rate was estimated from the quantity of proto-stars expected to form during the collapse of massive turbulent clumps into star clusters. This new method was developed by applying a Monte Carlo procedure to an evolutionary model of turbulent cores and takes into account the wide multiplicity of sources produced during the collapse. The star-formation rate density values at the tips are 1.2 +- 0.3 10-3 Msol/yr/kpc2 and 1.5+-0.3 10-3 Msol/yr/kpc2 in the first and fourth quadrant, respectively. The same values estimated on the entire field of view, that is including the tips of the bar and background and foreground regions, are 0.9+-0.2 10-3 Msol/yr/kpc2 and 0.8+-0.2 10-3 Msol/yr/kpc2. The conversion efficiency is approximately 0.8% in the first quadrant and 0.5% in the fourth quadrant, and does not show a significant difference in proximity of the bar. The star forming regions identified through CO contours at the further edge of the bar show star-formation rate densities larger than the surrounding regions but their conversion efficiencies are comparable. Our results suggest that the star-formation activity at the bar is due to a large amount of dust and molecular material rather than being due to a triggering process.