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The ATLAS3D Project - XXVIII. Dynamically-driven star formation suppression in early-type galaxies

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1403.4850v1_davis_2014.pdf (762.2Kb)
Date
11/11/2014
Author
Davis, Timothy A.
Young, Lisa M.
Crocker, Alison F.
Bureau, Martin
Blitz, Leo
Alatalo, Katherine
Emsellem, Eric
Naab, Thorsten
Bayet, Estelle
Bois, Maxime
Bournaud, Frederic
Cappellari, Michele
Davies, Roger L.
de Zeeuw, P. T.
Duc, Pierre-Alain
Khochfar, Sadegh
Krajnovic, Davor
Kuntschner, Harald
McDermid, Richard M.
Morganti, Raffaella
Oosterloo, Tom
Sarzi, Marc
Scott, Nicholas
Serra, Paolo
Weijmans, Anne-Marie
Keywords
Stars: mass-loss
ISM: molecules
Galaxies: elliptical and lenticular, cD
Galaxies: ISM
QB Astronomy
QC Physics
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Abstract
We present measurements of the star formation rate (SFR) in theearly-type galaxies (ETGs) of the ATLAS3D sample, based on Wide-field Infrared Survey Explorer (WISE) 22um and Galaxy Evolution Explorer (GALEX) far-ultraviolet emission. We combine these with gas masses estimated from 12CO and HI data in order to investigate the star formation efficiency (SFE) in a larger sample of ETGs than previously available. We first recalibrate (based on WISE data) the relation between old stellar populations (traced at Ks-band) and 22um luminosity, allowing us to remove the contribution of 22um emission from circumstellar dust. We then go on to investigate the position of ETGs on the Kennicutt-Schmidt (KS) relation. Molecular gas-rich ETGs have comparable star formation surface densities to normal spiral galaxy centres, but they lie systematically offset from the KS relation, having lower star formation efficiencies by a factor of ~2.5 (in agreement with other authors). This effect is driven by galaxies where a substantial fraction of the molecular material is in the rising part of the rotation curve, and shear is high. We show here for the first time that although the number of stars formed per unit gas mass per unit time is lower in ETGs, it seems that the amount of stars formed per free-fall time is approximately constant. The scatter around this dynamical relation still correlates with galaxy properties such as the shape of the potential in the inner regions. This leads us to suggest that dynamical properties (such as shear or the global stability of the gas) may be important second parameters that regulate star formation and cause much of the scatter around star-formation relations.
Citation
Davis , T A , Young , L M , Crocker , A F , Bureau , M , Blitz , L , Alatalo , K , Emsellem , E , Naab , T , Bayet , E , Bois , M , Bournaud , F , Cappellari , M , Davies , R L , de Zeeuw , P T , Duc , P-A , Khochfar , S , Krajnovic , D , Kuntschner , H , McDermid , R M , Morganti , R , Oosterloo , T , Sarzi , M , Scott , N , Serra , P & Weijmans , A-M 2014 , ' The ATLAS 3D Project - XXVIII. Dynamically-driven star formation suppression in early-type galaxies ' , Monthly Notices of the Royal Astronomical Society , vol. 444 , no. 4 , pp. 3427-3445 . https://doi.org/10.1093/mnras/stu570
Publication
Monthly Notices of the Royal Astronomical Society
Status
Peer reviewed
DOI
https://doi.org/10.1093/mnras/stu570
ISSN
0035-8711
Type
Journal article
Rights
© 2014. The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society. This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society
Collections
  • University of St Andrews Research
URL
http://adsabs.harvard.edu/abs/2014arXiv1403.4850D
URI
http://hdl.handle.net/10023/5451

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