Star-forming complexes in the polar ring galaxy NGC660

Ksenia I Smirnova,Dmitri S Wiebe,Alexei V Moiseev

doi:10.1515/astro-2017-0022

Abstract

Abstract Galaxies with polar rings consist of two subsystems, a disk and a ring, which rotate almost in orthogonal planes. In this paper, we analyze the parameters characterizing the composition of the interstellar medium and star formation in star-forming complexes belonging to polar ring galaxy NGC660. We show that star-forming regions in the ring of the galaxy are distinctly different from those in the galaxy disk. They possess substantially lower infrared luminosities, which is indicative of less dust mass in these regions than in a typical disk star-forming region. UV and Hα luminosities also appear to be lower in the ring, which is likely a consequence of its relatively recent formation.

Highlights

The interstellar medium (ISM) is both a stage and a source of material for the star formation process
We analyze the parameters characterizing the composition of the interstellar medium and star formation in star-forming complexes belonging to polar ring galaxy NGC660
Interacting galaxies are especially interesting from this point of view, where there exists a certain perturbing factor triggering the appearance of new starforming regions (SFRs)

Summary

Introduction

The interstellar medium (ISM) is both a stage and a source of material for the star formation process. Its composition defines the rate and spatial distribution of star formation in a galaxy. In order to recover specific details of this process, we need to know the relative contribution of various ISM components (atomic gas, molecular gas, dust, radiation field, etc.). Interacting galaxies are especially interesting from this point of view, where there exists a certain perturbing factor triggering the appearance of new starforming regions (SFRs). This leads to a rejuvenation of the stellar population of the galaxy and may clear up some features of the ISM evolution

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Results

Conclusion