期刊
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
卷 487, 期 2, 页码 2924-2936出版社
OXFORD UNIV PRESS
DOI: 10.1093/mnras/stz1439
关键词
Galaxy: kinematics and dynamics; Galaxy stellar content; Galaxy structure
资金
- Australian Research Council Centre of Excellence for All Sky Astrophysics in 3 Dimensions (ASTRO 3D) [CE170100013]
- Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO) [CE110001020]
- Australia Government Research Training Program Scholarship
- ASTRO 3D
- H2020 ERC Consolidator Grant [683184]
- ARC Laureate Fellowship
- ARC Federation Fellowship
- Australian Research Council Future Fellowship [FT180100231, FT100100457, FT140101202]
- Bland-Hawthorn's ARC Laureate Fellowship [FL140100278]
- University of Sydney Postdoctoral Research Fellowship
- ASTRO 3D [CE170100013]
- Australian Research Council Future Fellowship - Australian Government [FT180100066]
- Australian Research Council through a Future Fellowship [FT140101166, FT140100255]
- NASA through Hubble Fellowship grant - Space Telescope Science Institute [HST-HF2-51377]
- NASA [NAS5-26555]
- Korean National Research Foundation [2017R1A2A1A05001116]
- Yonsei University Future Leading Research Initiative [2015-22-0064]
- National Research Foundation of Korea [2017R1A2A1A05001116] Funding Source: Korea Institute of Science & Technology Information (KISTI), National Science & Technology Information Service (NTIS)
We use data from the Sydney-AAO Multi-object Integral-field spectroscopy (SAMI) Galaxy Survey to study the dynamical scaling relation between galaxy stellar massM* and the general kinematic parameter S-K = root KVrot2 + sigma(2) that combines rotation velocity V-rot and velocity dispersion s. We show that the logM* -logSK relation: (1) is linear above limits set by properties of the samples and observations; (2) has slightly different slope when derived from stellar or gas kinematic measurements; (3) applies to both early-type and late-type galaxies and has smaller scatter than either the Tully-Fisher relation (logM(*) -log V-rot) for late types or the Faber-Jackson relation (logM(*) - log s) for early types; and (4) has scatter that is only weakly sensitive to the value of K, with minimum scatter for K in the range 0.4 and 0.7. We compare SK to the aperture second moment (the 'aperture velocity dispersion') measured from the integrated spectrum within a 3-arcsecond radius aperture (sigma(3)). We find that while SK and sigma(3) are in general tightly correlated, the logM(*) -log SK relation has less scatter than the logM(*)-log sigma(3) relation.
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