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|Title:||The stellar orbit distribution in present-day galaxies inferred from the CALIFA survey||Authors:||Zhu, Ling
van de Ven, Glenn
van den Bosch, Remco
Grand, Robert J. J.
Dutton, Aaron A.
Macciò, Andrea V.
Gómez, Facundo A.
Walcher, Jakob C.
Sánchez, Sebastian F.
|Issue Date:||2018||Journal:||NATURE ASTRONOMY||Number:||2||First Page:||233||Abstract:||Galaxy formation entails the hierarchical assembly of mass, along with the condensation of baryons and the ensuing, self-regulating star formation<SUP>1,2</SUP>. The stars form a collisionless system whose orbit distribution retains dynamical memory that can constrain a galaxy's formation history<SUP>3</SUP>. The orbits dominated by ordered rotation, with near-maximum circularity λ<SUB>z</SUB> ≈ 1, are called kinematically cold, and the orbits dominated by random motion, with low circularity λ<SUB>z</SUB> ≈ 0, are kinematically hot. The fraction of stars on `cold' orbits, compared with the fraction on `hot' orbits, speaks directly to the quiescence or violence of the galaxies' formation histories<SUP>4,5</SUP>. Here we present such orbit distributions, derived from stellar kinematic maps through orbit-based modelling for a well-defined, large sample of 300 nearby galaxies. The sample, drawn from the CALIFA survey<SUP>6</SUP>, includes the main morphological galaxy types and spans a total stellar mass range from 10<SUP>8.7</SUP> to 10<SUP>11.9</SUP> solar masses. Our analysis derives the orbit-circularity distribution as a function of galaxy mass and its volume-averaged total distribution. We find that across most of the considered mass range and across morphological types, there are more stars on `warm' orbits defined as 0.25 ≤ λ<SUB>z</SUB> ≤ 0.8 than on either `cold' or `hot' orbits. This orbit-based `Hubble diagram' provides a benchmark for galaxy formation simulations in a cosmological context.||URI:||http://hdl.handle.net/20.500.12386/27952||URL:||https://www.nature.com/articles/s41550-017-0348-1||ISSN:||2397-3366||DOI:||10.1038/s41550-017-0348-1||Bibcode ADS:||2018NatAs...2..233Z||Fulltext:||open|
|Appears in Collections:||1.01 Articoli in rivista|
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|1711.06728.pdf||preprint||2.77 MB||Adobe PDF||View/Open|
|Nature astr.s41550-017-0348-1.pdf||[Administrators only]||3.69 MB||Adobe PDF|
checked on Jun 21, 2021
checked on Jun 21, 2021
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