Journal
ASTROPHYSICAL JOURNAL LETTERS
Volume 795, Issue 2, Pages -Publisher
IOP PUBLISHING LTD
DOI: 10.1088/2041-8205/795/2/L37
Keywords
galaxies: evolution; galaxies: fundamental parameters; galaxies: kinematics and dynamics
Categories
Funding
- Australian Research Council [DP130100664]
- Science and Industry Endowment Fund (Australia)
- Australian Research Council Centre of Excellence for All-sky Astrophysics (CAASTRO) [CE110001020]
- STFC [ST/K005596/1, ST/H002456/1] Funding Source: UKRI
- Science and Technology Facilities Council [ST/H002456/1, ST/K005596/1] Funding Source: researchfish
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We take advantage of the first data from the Sydney-AAO Multi-object Integral field Galaxy Survey to investigate the relation between the kinematics of gas and stars, and stellar mass in a comprehensive sample of nearby galaxies. We find that all 235 objects in our sample, regardless of their morphology, lie on a tight relation linking stellar mass (M-*) to internal velocity quantified by the S-0.5 parameter, which combines the contribution of both dispersion (sigma) and rotational velocity (V-rot) to the dynamical support of a galaxy (S-0.5 = root 0.5 V-rot(2) + sigma(2)). Our results are independent of the baryonic component from which sigma and V-rot are estimated, as the S-0.5 of stars and gas agree remarkably well. This represents a significant improvement compared to the canonical M-* versus Vrot and M-* versus s relations. Not only is no sample pruning necessary, but also stellar and gas kinematics can be used simultaneously, as the effect of asymmetric drift is taken into account once V-rot and sigma are combined. Our findings illustrate how the combination of dispersion and rotational velocities for both gas and stars can provide us with a single dynamical scaling relation valid for galaxies of all morphologies across at least the stellar mass range 8.5 < log (M-*/M-circle dot) < 11. Such relation appears to be more general and at least as tight as any other dynamical scaling relation, representing a unique tool for investigating the link between galaxy kinematics and baryonic content, and a less biased comparison with theoretical models.
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