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The Single-cloud Star Formation Relation - IOPscience

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The Single-cloud Star Formation Relation

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Published 2021 May 4 © 2021. The Author(s). Published by the American Astronomical Society.
, , Citation Riwaj Pokhrel et al 2021 ApJL 912 L19 DOI 10.3847/2041-8213/abf564

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2041-8205/912/1/L19

Abstract

One of the most important and well-established empirical results in astronomy is the Kennicutt–Schmidt relation between the density of interstellar gas and the rate at which that gas forms stars. A tight correlation between these quantities has long been measured at galactic scales. More recently, using surveys of YSOs, a KS relationship has been found within molecular clouds relating the surface density of star formation to the surface density of gas; however, the scaling of these laws varies significantly from cloud to cloud. In this Letter, we use a recently developed, high-accuracy catalog of young stellar objects from Spitzer combined with high-dynamic-range gas column density maps of 12 nearby (<1.5 kpc) molecular clouds from Herschel to re-examine the KS relation within individual molecular clouds. We find a tight, linear correlation between clouds' star formation rate per unit area and their gas surface density normalized by the gas freefall time. The measured intracloud KS relation, which relates star formation rate to the volume density, extends over more than two orders of magnitude within each cloud and is nearly identical in each of the 12 clouds, implying a constant star formation efficiency per freefall time epsilonff ≈ 0.026. The finding of a universal correlation within individual molecular clouds, including clouds that contain no massive stars or massive stellar feedback, favors models in which star formation is regulated by local processes such as turbulence or stellar feedback such as protostellar outflows, and disfavors models in which star formation is regulated only by galaxy properties or supernova feedback on galactic scales.

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Footnotes

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    The reason that YSO motion is related to the freefall time is that the natural timescale for YSO motion is the crossing time, and for a region with virial parameter αあるふぁvir ∼ 1, this is roughly equal to the freefall time (e.g., Krumholz & Tan 2007).

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10.3847/2041-8213/abf564