The SAMI galaxy survey:predicting kinematic morphology with logistic regression

• Published in: Monthly Notices of the Royal Astronomical Society
• Main Authors: Vaughan, Sam P., van de Sande, Jesse, Fraser-McKelvie, A., Croom, Scott, McDermid, Richard, Liquet-Weiland, Benoit, Barsanti, Stefania, Cortese, Luca, Brough, Sarah, Sweet, Sarah, Bryant, Julia J., Goodwin, Michael, Lawrence, Jon
• Format: Article in Journal/Newspaper
• Language: English
• Published: 2024
• Subjects: galaxies: evolution; galaxies: formation; galaxies: kinematics and dynamics; dynamics; galaxies: kinematics; sami
• Online Access: https://researchers.mq.edu.au/en/publications/34b43e9d-318e-4bb7-8ab3-9fa0f1bb5bd3; https://doi.org/10.1093/mnras/stae409; https://research-management.mq.edu.au/ws/files/323626724/321386594.pdf; http://purl.org/au-research/grants/arc/CE170100013; http://www.scopus.com/inward/record.url?scp=85185397781&partnerID=8YFLogxK

We use the SAMI (Sydney-AAO Multi-object Integral field spectrograph) galaxy survey to study the the kinematic morphology–density relation: the observation that the fraction of slow rotator galaxies increases towards dense environments. We build a logistic regression model to quantitatively study the dependence of kinematic morphology (whether a galaxy is a fast or slow rotator) on a wide range of parameters, without resorting to binning the data. Our model uses a combination of stellar mass, star formation rate (SFR), r-band half-light radius, and a binary variable based on whether the galaxy’s observed ellipticity (ϵ) is less than 0.4. We show that, at fixed mass, size, SFR, and ϵ, a galaxy’s local environmental surface density (log 10 (Σ 5 /Mpc −2 )) gives no further information about whether a galaxy is a slow rotator, that is, the observed kinematic–morphology density relation can be entirely explained by the well-known correlations between environment and other quantities. We show how our model can be applied to different galaxy surveys to predict the fraction of slow rotators which would be observed and discuss its implications for the formation pathways of slow rotators.