Young Stellar Groups and Their Most Massive Stars
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We analyze the masses and spatial distributions of fourteen young stellar groups in Taurus, Lupus3, ChaI, and IC348. These nearby groups, which typically contain 20 to 40 members, have membership catalogs complete to ~0.02 M_sun, and are sufficiently young that their locations should be similar to where they formed. These groups show five properties seen in clusters having many more stars and much greater surface density of stars: (1) a broad range of masses, (2) a concentration of the most massive star towards the centre of the group, (3) an association of the most massive star with a high surface density of lower-mass stars, (4) a correlation of the mass of the most massive star with the total mass of the group, and (5) the distribution of a large fraction of the mass in a small fraction of the stars.
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Cited by 1 Pith paper
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Global and Local Infall in the ASHES Sample (GLASHES). II. Asymmetric Line Profiles around Dense Cores in 70 $\mu$m Dark Massive Clumps
Blue-asymmetric spectral lines appear in 50-60% of dense cores within massive dark clumps, showing that gravitational collapse operates at core scales from prestellar stages onward and supports hierarchical star formation.
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