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Evolutionary Trends in Star Formation

Published online by Cambridge University Press:  07 February 2024

J. S. Urquhart Open the ORCID record for J. S. Urquhart [Opens in a new window]
J. S. Urquhart*
Affiliation:
Centre for Astrophysics and Planetary Science, University of Kent, Canterbury, CT2 7NH, UK.
*
email: j.s.urquhart@kent.ac.uk
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Abstract

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Over the past 20 years, the Galactic plane has been surveyed at high resolution at wavelengths from 1 micron through to 20 cm. The combination of these surveys has produced large samples of deeply embedded young stars located across the Galactic disc. These continuum surveys are complemented by spectral line surveys of thermal, radio recombination, and molecular maser (OH, H2O, CH3OH) lines. The identified sources cover the whole range of evolutionary stages in the star formation process, allowing the physical properties of these stages to be measured. This information has been used to calculate the star formation efficiency and star formation rate of the Milky Way and to evaluate the impact of environment and location within the disc. This review provides an overview of some of the most significant studies in recent years and discusses how the evolutionary sequence has been used to investigate the correlation of other star formation tracers and maser associations.

Keywords

Masersstar: formationISM: moleculesISM: surveys
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 18 , Symposium S380: Cosmic Masers: Proper Motion toward the Next-Generation Large Projects , December 2022 , pp. 135 - 151
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This is an Open Access article, distributed under the terms of the Creative Commons Attribution licence (http://creativecommons.org/licenses/by/4.0/), which permits unrestricted re-use, distribution and reproduction, provided the original article is properly cited.
Copyright
© The Author(s), 2024. Published by Cambridge University Press on behalf of International Astronomical Union

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