Angular Momentum Problems in Disk Formation

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1 Angular Momentum Problems in Disk Formation MPIA Theory Group Seminar, 07/03/2006

2 The Standard Picture Disks galaxies are systems in centrifugal equilibrium Structure of disks is governed by angular momentum content The Three Pillars of Disk Formation Angular momentum originates from cosmological torques Baryons and Dark Matter acquire identical angular momentum distributions. During cooling, gas conserves its specific angular momentum Gas settles in disk in centrifugal equilibrium Σ disk (R) M bar (j bar ) M dm (j dm )

3 The Spin Parameter Tidal Torque Theory (second-order perturbation theory): J(t) = γ ρ(r, t)[r(t) r cm(t)] [v(t) v cm (t)]d 3 r conversion to comoving variables yields: J(t) a 2 (t) ρ 0 γ [1 + δ(x, t)] (x x cm) ẋd 3 x It is convenient to express the specific angular momentum, j vir = J vir /M vir, in terms of the dimensionless spin parameter λ j vir R vir V vir Numerical simulations have shown that λ 0.04 Using that j d R d V rot, and assuming that V rot V vir, we see that R d λr vir Thus λ 1 reflects roughly the collapse factor of the baryons

4 Angular Momentum & Dark Matter Cosmological Torques  ½ ¾ Å ¾» ØÓØ Ê Î Ú Ö Ú Ö Bullock et al 2000 Cold Dark Matter haloes have a log normal distribution of halo spin parameters... Cold Dark Matter haloes have a Universal Angular Momentum distribution... Bullock et al 2000

5 Testing the Paradigm TEST: Compare angular momentum distributions of disks and CDM haloes. If standard paradigm is correct, these should be identical. DATA: 14 dwarf galaxies whose rotation curves are in good agreement with CDM haloes (van den Bosch & Swaters 2001). M(< j) = 2π R j 0 Σ disk (R) RdR with j = R j V circ (R j ) Disks and CDM haloes have same p(λ). van den Bosch, Burkert & Swaters 2001

6 Angular Momentum Distributions Typical Angular momentum distribution of dark matter halo. Angular momentum distribution of disk. van den Bosch, Burkert & Swaters 2001 Disks (of dwarf galaxies) have angular momentum distributions that are clearly different than those of cold dark matter haloes!!!

7 The Angular Momentum Catastrophe Steinmetz & Navarro 1999 Disks that form in simulations are an order of magnitude too small Gas looses large fraction of specific angular momentum to dark matter Hierarchical formation & over-cooling are to blaim SOLUTIONS White & Navarro 1993; Navarro & Steinmetz 1999 (1) Prevent Cooling: feedback, preheating (Weil et al. 1998; Sommer-Larsen et al. 1999) (2) Modify Power Spectrum: WDM, BSI, RSI... (Sommer-Larsen & Dolgov 2001)

8 Disk Scaling Relations I Observations: M disk = h 2 M ( V rot j disk = km s 1 h 1 kpc ( Theoretical Predictions: M disk = f m ( Ωb Ω m ) M vir j disk = 2 f j λ R vir V vir 100 km s 1 ) 3.5 (Bell & de Jong 2001) V rot ) km s 1 M vir V 3 vir R vir V vir Example: Ω m = 0.3 h = 0.7 λ = 0.04 V rot /V vir = 1.4 f m = 0.42 ( V vir 200 km s 1 ) 1/2 f j = 0.79 (see also Navarro & Steinmetz 2000)

9 Disk Scaling Relations II f m = 0.42 ( V vir ) 1/2 ( ) f 200 km s 1 j = 0.79 λ M(r) from NFW profile with c = 20 (Navarro, Frenk & White 1997) j(r) r from N-body simulations (Bullock et al. 2001)

10 Disk Scaling Relations III Sample of 1300 galaxies with Hα RCs (Courteau et al. 2006) Note surface brightness independence of TF relation!

11 Model Description Exponential disk in NFW dark matter halo Adiabatic contraction Disk is split in stars and cold gas using star formation threshold density Bulge formation based on disk stability Empirical stellar mass-to-light ratios: Υ = Υ(L) We construct samples with scatter in c, Υ, λ gal, and m gal Sampling of M vir is such that we reproduce observed distribution of L Free parameters: λ gal, m gal, c (cosmology), and Υ (IMF) In addition we tune σ ln c, σ ln λ, σ ln Υ Finally, we can modify adiabatic contraction

12 Zero-Point Constraints Dutton, vdb, Dekel & Courteau, 2006

13 The Model That Works Model fits slopes, zero points and scatter of V L and RL relations Model fits surface brightness independence of V L relation Model is consistent with galaxy luminosity function!!

14 CONCLUSIONS Problems for the Standard Problem cooling very efficient in low mass haloes at high z = Angular Momentum Catastrophe haloes have too much low angular momentum material = Morphology Problem! Too much bulge, too little disk Standard model can not fit TF zero point = Haloes are too centrally concentrated A Revised Model for Disk Formation (1) Disks form out of Merging Clumps (2) Dynamical Friction and 3-Body Interactions cause Halo Expansion (3) Disks form in subset of haloes with quiescent merger history (3) This results in low λ gal and low σ ln λ (4) Formation efficiencies of disks are low (4) In MW sized halo, only 20% of baryons end up in disk.