Quiescent galaxies cluster more strongly than star-forming ones by 0.5-1 dex after halo-mass matching, with one-halo conformity up to z~2 that disappears at higher redshifts.
Journal of Cosmology and Astroparticle Physics, 2019(3), 043
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abstract
This book provides an introduction to the field of star formation at a level suitable for graduate students or advanced undergraduates in astronomy or physics. The structure of the book is as follows. The first two chapters begin with a discussion of observational techniques, and the basic phenomenology they reveal. The goal is to familiarize students with the basic techniques that will be used throughout, and to provide a common vocabulary for the rest of the book. The next five chapters provide a similar review of the basic physical processes that are important for star formation. Again, the goal is to provide a basis for what follows. The remaining chapters discuss star formation over a variety of scales, starting with the galactic scale and working down to the scales of individual stars and their disks. The book concludes with a brief discussion of the clearing of disks and the transition to planet formation. The book includes five problem sets, complete with solutions.
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UNVERDICTED 3representative citing papers
An analytical ab initio model predicts formation of ultra-faint dwarfs, old globular clusters, and Population III star clusters in early low-mass halos, with properties and abundances matching observations for chosen Pop III masses.
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COSMOS-Web: does halo mass alone shape the clustering of star-forming and quiescent galaxies?
Quiescent galaxies cluster more strongly than star-forming ones by 0.5-1 dex after halo-mass matching, with one-halo conformity up to z~2 that disappears at higher redshifts.
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Starbursts at Cosmic Dawn: Formation of Globular Clusters, Ultra-Faint Dwarfs, and Population III star clusters at z > 6
An analytical ab initio model predicts formation of ultra-faint dwarfs, old globular clusters, and Population III star clusters in early low-mass halos, with properties and abundances matching observations for chosen Pop III masses.