SDSS-IV MaNGA: the different quenching histories of fast and slow rotators

Smethurst, R.J. and Masters, Karen L. and Lintott, Chris J. and Weijmans, Anne-Marie and Merrifield, Michael R. and Penny, Samantha J. and Aragón-Salamanca, Alfonso and Brownstein, J. and Bundy, Kevin and Drory, Niv and Law, D.R. and Nichol, Robert C. (2017) SDSS-IV MaNGA: the different quenching histories of fast and slow rotators. Monthly Notices of the Royal Astronomical Society . ISSN 1365-2966

[img]
Preview
PDF - Requires a PDF viewer such as GSview, Xpdf or Adobe Acrobat Reader
Download (1MB) | Preview

Abstract

Do the theorised different formation mechanisms of fast and slow rotators produce an observable difference in their star formation histories? To study this we identify quenching slow rotators in the MaNGA sample by selecting those which lie below the star forming sequence and identify a sample of quenching fast rotators which were matched in stellar mass. This results in a total sample of 194 kinematically classified galaxies, which is agnostic to visual morphology. We use u − r and NUV − u colours from SDSS and GALEX and an existing inference package, STARPY, to conduct a first look at the onset time and exponentially declining rate of quenching of these galaxies. An Anderson-Darling test on the distribution of the inferred quenching rates across the two kinematic populations reveals they are statistically distinguishable (3.2σ). We find that fast rotators quench at a much wider range of rates than slow rotators, consistent with a wide variety of physical processes such as secular evolution, minor mergers, gas accretion and environmentally driven mechanisms. Quenching is more likely to occur at rapid rates (τ≲1 Gyr) for slow rotators, in agreement with theories suggesting slow rotators are formed in dynamically fast processes, such as major mergers. Interestingly, we also find that a subset of the fast rotators quench at these same rapid rates as the bulk of the slow rotator sample. We therefore discuss how the total gas mass of a merger, rather than the merger mass ratio, may decide a galaxy’s ultimate kinematic fate.

Item Type: Article
Additional Information: This article has been accepted for publication in monthly Notices of the Royal Astronomical Society © 2017 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
Keywords: galaxies-photometry, galaxies-statistics, galaxies-morphology
Schools/Departments: University of Nottingham, UK > Faculty of Science > School of Physics and Astronomy
Identification Number: 10.1093/mnras/stx2547
Depositing User: Eprints, Support
Date Deposited: 09 Oct 2017 09:57
Last Modified: 18 Oct 2017 11:58
URI: http://eprints.nottingham.ac.uk/id/eprint/47084

Actions (Archive Staff Only)

Edit View Edit View