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We use data from the Sydney-AAO Multi-object Integral-field spectroscopy (SAMI) Galaxy Survey to study the dynamical scaling relation between galaxy stellar mass M∗ and the general kinematic parameter SK = √KV2rot + σ2 that combines rotation velocity Vrot and velocity dispersion σ. 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 Vrot) for late types or the Faber.Jackson relation (logM∗ - log σ) 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 (σ3″ ). We find that while SK and σ3″ are in general tightly correlated, the logM∗ - log SK relation has less scatter than the logM∗ - log σ3″ relation.
|Number of pages||13|
|Journal||Monthly Notices of the Royal Astronomical Society|
|Publication status||Published - Aug 2019|
Bibliographical noteThis article has been accepted for publication in Monthly Notices of the Royal Astronomical Society, Volume 487, Issue 2, August 2019, Pages 2924–2936, https://doi.org/10.1093/mnras/stz1439. Copyright 2019 The Author(s). Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
- Galaxy stellar content
- Galaxy structure
- Galaxy: kinematics and dynamics
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The impact of impact: what stops star formation in cluster galaxies?
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