ASTR 610 Theory of Galaxy Formation Lecture 16

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Disk Galaxies: Observational Facts Exponential Surface Brightness Profiles Because of their close-to-exponential appearance, disk galaxies are often modelled as infinitesimally thin, exponential disks: surface brightness surface mass density I(R) =I 0 e −R/R d Σ(R) =Σ 0 e −R/R d L d =2π M d =2π ∞ 0 ∞ 0 I(R) R dR =2π I 0 R 2 d Σ(R) R dR =2π Σ 0 R 2 d circular velocity V 2 c,d(R) =−4πGΣ 0 R 2 d y [I 0 (y) K 0 (y) − I 1 (y) K 1 (y)] disk scale length R d stellar mass-to-light ratio M d /L d =Σ 0 /I 0 y ≡ R/(2 R d ) modified Bessel functions I n (x) K n (x) The circular velocity curve reaches a maximum at R 2.16 R d For more realistic models, with non-zero thickness, see MBW §11.1.1... ASTR 610: Theory of Galaxy Formation © Frank van den Bosch: Yale 2012
gas mass fraction Disk Galaxies: Observational Facts Scaling Relations Brighter disks are larger are redder have higher central SB have smaller gas mass fractions rotate faster (Tully-Fisher relation) McGaugh & de Blok, 1997, ApJ, 534, 146 MBW, Fig. 2.20 red blue vdBosch & Dalcanton, 2000, ApJ, 534, 146 ASTR 610: Theory of Galaxy Formation © Frank van den Bosch: Yale 2012
Page 1 and 2: ASTR 610 Theory of Galaxy Formation
Page 3 and 4: Structure & Formation of Disk Galax
Page 5: Disk Galaxies: Observational Facts
Page 9 and 10: The Formation of Disk Galaxies Hot
Page 11 and 12: Angular Momentum Transport J For a
Page 13 and 14: Disk Formation: The Standard Pictur
Page 15 and 16: Disk Formation: The Standard Pictur
Page 17 and 18: Adiabatic Contraction When baryons
Page 19 and 20: Dutton, vdBosch, Dekel & Courteau,
Page 21 and 22: Stellar Mass-to-Light Ratios MMW mo
Page 23 and 24: Models Without Scatter Source: Dutt
Page 25 and 26: Models Without Scatter Source: Dutt
Page 27 and 28: Three Succesful Models with Scatter
Page 29: The Origin of Exponential Disks Unf

ASTR 610 Theory of Galaxy Formation Lecture 16

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