Stéphane Courteau

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λ = halo spin c = halo conc. m d = disk mass (following Mo, Mao, & White 1998) Assumes σ ln=0.3 for each variable. Scaling Relations of Disk Galaxies Dutton etal 2005
Major issues for NNG 2005 • Surface brightness independence of TF relation why should the luminous/dark ratio change so as to keep the TF relation independent of surface brightness? • (Slope), scatter (colour), normalization of scaling relations • Mass models of barred and unbarred galaxies (need to use a common language and same dynamical tests) • What is the final halo shape: Is it NFW + (Blumenthal etal) adiabatic contraction? • Why can’t we reproduce bulgeless exponential disks?
Page 1 and 2: Nearly Normal Galaxies in a ΛCDM U
Page 3 and 4: Ascona/Terschelling Highlights •
Page 5 and 6: The outer regions of M31 Worthey, E
Page 11 and 12: NGC 4656: small bulge and prominent
Page 13 and 14: Ascona/Terschelling Highlights Disk
Page 15 and 16: Interpretations of disk truncations
Page 17 and 18: 0.15 µm 0.4-0.8 µm 1.2-2.2 µm 3.
Page 19 and 20: ΛCDM Formation Models • Failures
Page 21 and 22: ΛCDM Formation Models • predicti
Page 23 and 24: Effect of Adiabatic Contraction (sa
Page 25 and 26: Moving Forward in Mass Modeling Req
Page 29 and 30: An argument for pure stellar disks
Page 31 and 32: Residual Correlations Courteau et a
Page 33 and 34: Comparison With Models • Simple e
Page 36 and 37: Evidence for Sub-Maximal Disks •
Page 38 and 39: SparsePak Study of Barred Galaxies
Page 40 and 41: € Scaling Relations of Galaxies

Stéphane Courteau

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