The SAMI Galaxy Survey:mass-kinematics scaling relations

• Published in: Monthly Notices of the Royal Astronomical Society
• Main Authors: Barat, Dilyar, D'Eugenio, Francesco, Colless, Matthew, Brough, Sarah, Catinella, Barbara, Cortese, Luca, Croom, Scott M., Medling, Anne M., Oh, Sree, Van De Sande, Jesse, Sweet, Sarah M., Yi, Sukyoung K., Bland-Hawthorn, Joss, Bryant, Julia, Goodwin, Michael, Groves, Brent, Lawrence, Jon, Owers, Matt S., Richards, Samuel N., Scott, Nicholas
• Format: Article in Journal/Newspaper
• Language: English
• Published: 2019
• Subjects: Galaxy stellar content; Galaxy structure; Galaxy: kinematics and dynamics; sami
• Online Access: https://researchers.mq.edu.au/en/publications/a950151f-2fba-43e0-acf4-7f7684a7d66d; https://doi.org/10.1093/mnras/stz1439; https://research-management.mq.edu.au/ws/files/106308706/106300320.pdf; http://www.scopus.com/inward/record.url?scp=85071155577&partnerID=8YFLogxK; http://purl.org/au-research/grants/arc/CE1101020; http://purl.org/au-research/grants/arc/CE170100013; http://purl.org/au-research/grants/arc/FT140100255

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 S K = √KV 2 rot + σ 2 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 V rot ) 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 (σ 3″ ). We find that while SK and σ 3″ are in general tightly correlated, the logM ∗ - log SK relation has less scatter than the logM ∗ - log σ 3″ relation.