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

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ρs is constant over Hg? Hs >>Hg (?) • Numerically this approximate solution gives better estimates than the Blitz & Rosolowsky (2006) formalism. ρg/ρs = 4 produces results only 10% off the ”proper” numerical <strong>in</strong>tegration whereas the Blitz & Rosolowsky (2006) approximation is off by about 20% to 30%. Azimuthal symmetry σ g(R)=? ρs>>ρg? Koyama & Ostriker 2009 16
ρs is constant over Hg? s>>Hg H Azimuthal symmetry σg(R)= 10 km/s ρs>>ρg? Koyama & Ostriker 2009 17
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: ρs is constant over Hg? s>>Hg H Ko
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 and 26: Rmol-Pressure Relation •Early-typ
Page 27 and 28: Summary • Observed HI surface den

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

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