G. Murante – INAF OATo P. Monaco – Univ. Ts M. Calabrese – SISSA Ts G. De Lucia - INAF OATs S. Borgani – Univ. Ts K. Dolag – Obs..Munchen Heidelberg, May 15th, Disk Galaxy Formation in a cosmological(context) content

MUPPI: MUlti Phase Particle Integrator  Star formation & feedback algorithm  Implemented in GADGET-3  Integrates ISM equations for each particle at each SPH time step  Effective thermal feedback  Obtains SK relation without imposing it  Gives ISM characteristics Heidelberg, May 15th, 2012 Disk Galaxy Formation in a cosmological(context) content2 Murante, Monaco, Giovalli, Borgani, Diaferio, 2010, MNRAS, 405, 1491 (See Monaco, Murante, Borgani, Dolag, 2012, MNRAS, 421, 2485)

MOLECULAR GAS = = = MASS FLOWS MASS FLOWS STAR FORMATION RESTORATION COOLING EVAPORATION M H2 -> SF On hot phase! On cold phase! Heidelberg, May 15th, Disk Galaxy Formation in a cosmological(context) content

Ė hot = -Ė cool +Ė sn +Ė hydro Multi-Phase particle Δt, ΔS Ė hydro = ΔS/(γ-1)ρ (γ-1) Δt SPH new ΔS etc... Heidelberg, May 15th, Disk Galaxy Formation in a cosmological(context) content Energy exchanges

ENERGY FLOW(S..) Hot phase energy ENERGY RELEASED BY SNeENERGY LOSS DUE TO COOLING ENERGY CONTRIBUTION DUE TO HYDRODYNAMICS this is the ENTROPY variation due to SPH hydrodynamics PRESSURE-DRIVEN SF Phenomenological (Blitz & Rosolowsky 2006) P ext  P therm with P 0 = Heidelberg, May 15th, Disk Galaxy Formation in a cosmological(context) content

More characteristics Heidelberg, May 15th, 2012 Disk Galaxy Formation in a cosmological(context) content6 Thermal energy given to neighbouring particles in a directional way Chemical evolution (Tornatore et al 2007) Primordial AND metal dependent cooling Stocastic kinetic winds: a fraction of particles continously receive also kinetic energy from neighbouring particles. They decouple from the gas. Wind speed depends on local SF. In cosmological simulations, velocities up to 1000 km/s

Dynamical SK relation Heidelberg, May 15th, Disk Galaxy Formation in a cosmological(context) content Monaco, Murante, Borgani, Dolag, 2012, MNRAS, 421, 2485

Cosmological disk galaxy simulations Heidelberg, May 15th, 2012 Disk Galaxy Formation in a cosmological(context) content8 (Stoehr+, 2002, MNRAS, 355, 84) (See The Aquila comparison project, Scannapieco+, 2012, MNRAS, in press)

Our best disk galaxy Heidelberg, May 15th, 2012 Disk Galaxy Formation in a cosmological(context) content9

How does the gas accrete? Heidelberg, May 15th, 2012 Disk Galaxy Formation in a cosmological(context) content10 use simulations without chemical evolution/metal cooling identify stars/gas particles at z=0 within R 200, R gal =0.1 R 200 follow back particles and recorded their maximum T also construct SUBFIND merger trees of haloes use three temperature ranges: 1.0 < Tmax < 250,000 K (cold); 2.250,000 K < Tmax < 10 6 K (warm) 3.Tmax > 10 6 K see to which accretion channel gas particles belong, if they ever were into clumps, both for particles within R 200 and R gal. We: Murante, Calabrese, De Lucia, Monaco Borgani, Dolag, 2012, ApJL, 749, 34

Heidelberg, May 15th, 2012 Disk Galaxy Formation in a cosmological(context) content11

Accretion channels Heidelberg, May 15th, Disk Galaxy Formation in a cosmological(context) content Warm gas GADGET

GA vs AQ Heidelberg, May 15th, Disk Galaxy Formation in a cosmological(context) content GalaxyHalo

Multiphase properties of gas in channels Heidelberg, May 15th, Disk Galaxy Formation in a cosmological(context) content Aq-C-5

Resolution Heidelberg, May 15th, Disk Galaxy Formation in a cosmological(context) content (results for accretion on galaxy)

Metal cooling Heidelberg, May 15th, Disk Galaxy Formation in a cosmological(context) content (results for GA1)

Clumpiness Heidelberg, May 15th, Disk Galaxy Formation in a cosmological(context) content (results for GA2) Cold gas is clumpy! Our gas clumps have DM… (10 7 Msol min)

Conclusions Heidelberg, May 15th, Disk Galaxy Formation in a cosmological(context) content MUPPI can produce reasonable disk galaxies Accretion on halo is mainly cold With an efficient thermal feedback scheme, a new gas accretion channel on galaxy arises: warm accretion Warm accretion is fuelled by gas heated by Sne feedback Cold accretion on galaxies is at least 50% clumpy Our result does not depend upon resolution, our chosen halo, chemical evolution/metal cooling: only on the efficiency of thermal feedback MUPPI can produce reasonable disk galaxies Accretion on halo is mainly cold With an efficient thermal feedback scheme, a new gas accretion channel on galaxy arises: warm accretion Warm accretion is fuelled by gas heated by Sne feedback Cold accretion on galaxies is at least 50% clumpy Our result does not depend upon resolution, our chosen halo, chemical evolution/metal cooling: only on the efficiency of thermal feedback