The Nature of Low-Density Star Formation. (arXiv:1903.05745v1 [astro-ph.GA])

The Nature of Low-Density Star Formation. (arXiv:1903.05745v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Thilker_D/0/1/0/all/0/1">David Thilker</a> (Johns Hopkins University), <a href="http://arxiv.org/find/astro-ph/1/au:+Lee_J/0/1/0/all/0/1">Janice Lee</a> (Caltech / IPAC), <a href="http://arxiv.org/find/astro-ph/1/au:+Capak_P/0/1/0/all/0/1">Peter Capak</a> (Caltech / IPAC), <a href="http://arxiv.org/find/astro-ph/1/au:+Cook_D/0/1/0/all/0/1">David Cook</a> (Caltech / IPAC), <a href="http://arxiv.org/find/astro-ph/1/au:+Dale_D/0/1/0/all/0/1">Daniel Dale</a> (University of Wyoming), <a href="http://arxiv.org/find/astro-ph/1/au:+Elmegreen_B/0/1/0/all/0/1">Bruce Elmegreen</a> (IBM), <a href="http://arxiv.org/find/astro-ph/1/au:+Paz_A/0/1/0/all/0/1">Armando Gil de Paz</a> (Universidad Complutense de Madrid), <a href="http://arxiv.org/find/astro-ph/1/au:+Gallagher_J/0/1/0/all/0/1">John Gallagher</a> (University of Wisconsin), <a href="http://arxiv.org/find/astro-ph/1/au:+Hunter_D/0/1/0/all/0/1">Deidre Hunter</a> (Lowell Observatory), <a href="http://arxiv.org/find/astro-ph/1/au:+Leroy_A/0/1/0/all/0/1">Adam Leroy</a> (Ohio State University), <a href="http://arxiv.org/find/astro-ph/1/au:+Meurer_G/0/1/0/all/0/1">Gerhardt Meurer</a> (University of Western Australia / ICRAR), <a href="http://arxiv.org/find/astro-ph/1/au:+Pisano_D/0/1/0/all/0/1">D. J. Pisano</a> (West Virginia University / GBO), <a href="http://arxiv.org/find/astro-ph/1/au:+Rafelski_M/0/1/0/all/0/1">Marc Rafelski</a> (STScI / JHU), <a href="http://arxiv.org/find/astro-ph/1/au:+Tosi_M/0/1/0/all/0/1">Monica Tosi</a> (INAF – Osservatorio di Astrofisica e Scienza dello Spazio, Bologna), <a href="http://arxiv.org/find/astro-ph/1/au:+Wofford_A/0/1/0/all/0/1">Aida Wofford</a> (Instituto de Astronom&#xed;a, Universidad Nacional Aut&#xf3;noma de M&#xe9;xico – Ensenada)

How do stars manage to form within low-density, HI-dominated gas? Such
environments provide a laboratory for studying star formation with physical
conditions distinct from starbursts and the metal-rich disks of spiral galaxies
where most effort has been invested. Here we outline fundamental open questions
about the nature of star formation at low-density. We describe the wide-field,
high-resolution UV-optical-IR-radio observations of stars, star clusters and
gas clouds in nearby galaxies needed in the 2020’s to provide definitive
answers, essential for development of a complete theory of star formation.

How do stars manage to form within low-density, HI-dominated gas? Such
environments provide a laboratory for studying star formation with physical
conditions distinct from starbursts and the metal-rich disks of spiral galaxies
where most effort has been invested. Here we outline fundamental open questions
about the nature of star formation at low-density. We describe the wide-field,
high-resolution UV-optical-IR-radio observations of stars, star clusters and
gas clouds in nearby galaxies needed in the 2020’s to provide definitive
answers, essential for development of a complete theory of star formation.

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