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

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Multi-Gaussian (MGE) Stellar Density • The 3D stellar density, ρs(R,0), is determined using a multi-Gaussian expansion (MGE) fit developed by Cappellari (2002) to 2μ All Sky Survey (2MASS) Ks-band ATLAS images (Skrutskie et al. 2006) or UKIDSS K-band images if available. Characterizes the observed surface brightness as a sum of Gaussians, and allows the photometry to be reproduced in detail. Requires an inclination for deprojection. Estimated from optical dust images. Requires azimuthal symmetry. Most of the early-type sample galaxies are oblate/fast rotators. Doesn't require an assumed stellar scale height.
ρ s Constant with H g ? The MGE stellar density versus radius for several different scale heights. Hs=0 pc, 150 pc, 300 pc above the midplane. YES! Local Milky Way ρs 19
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: ρs is constant over Hg? s>>Hg H Az
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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