The HI-H 2 Transition and Star Formation in Early-Type Galaxies

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Rmol-Pressure Relation •Early-type empirical result: P=[(P/k B )/52±4 K cm -3 )] 0.45±0.09 •The Elmegreen (1993) prediction, F mol ≈P 2.2 j(Z) -1 , is only good for R mol 1 results in a much more shallow fitted • R mol =P1.2 for R mol
Summary • Observed HI surface density saturation and total surface density at the transition region are similar to that of early-type galaxies. • The Krumholz et al. (2009) dissociation models do a fair job of predicting the molecular fraction in CO-rich early-type galaxies. • The cold gas systems of CO-rich early-type galaxies fundamentally resemble that of normal • Stability spiral models galaxies! are more or less consistent with observations. Star formation is occurring where we predict it to occur except where the gas is likely not yet settled into the disk. • R mol is a much more shallow function of hydrostatic midplane pressure than observed for disk galaxies.
Page 1 and 2: The giant elliptical galaxy ESO 325
Page 3 and 4: Motivation It is well known that m
Page 5 and 6: Results NGC 807 Five Detections: N
Page 7 and 8: HI detected HI non-detected UGC 150
Page 9 and 10: Σcrit Versus Σtot
Page 11 and 12: Rmol-Pressure Relation Recall that
Page 13 and 14: Blitz & Rosolowsky 2006; Leroy et a
Page 15 and 16: ρs is constant over Hg? s>>Hg H Ko
Page 17 and 18: ρs is constant over Hg? s>>Hg H Az
Page 19 and 20: ρ s Constant with H g ? The MGE st
Page 21 and 22: Koyama & Ostriker 2008 ----> Hg: 5-
Page 23 and 24: Koyama & Ostriker 2008 ----> 23 Gas
Page 25: Rmol-Pressure Relation •Early-typ

The HI-H 2 Transition and Star Formation in Early-Type Galaxies

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