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Date and Time of the Query: 2019-03-26 T07:40:46 PDT
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For refcode 2014MNRAS.444.3427D:
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Copyright by Royal Astronomical Society. 2014MNRAS.444.3427D The ATLAS^3D^ Project - XXVIII. Dynamically driven star formation suppression in early-type galaxies 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 Abstract. We present measurements of the star formation rate (SFR) in the early-type galaxies (ETGs) of the ATLAS^3D^ sample, based on Wide-field Infrared Survey Explorer (WISE) 22 micron and Galaxy Evolution Explorer far-ultraviolet emission. We combine these with gas masses estimated from ^12^CO and H I 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 K_s_ band) and 22 micron luminosity, allowing us to remove the contribution of 22 micron 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 SFEs 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. Key words: stars: mass-loss, ISM: molecules, galaxies: elliptical and lenticular, cD, galaxies: ISM
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