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A warm mode of accretion in simulations of galaxy formation

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. A warm mode of accretion in simulations of galaxy formation. MUPP I : MU lti P hase P article I ntegrator.

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A warm mode of accretion in simulations of galaxy formation

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  1. 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 A warm mode of accretion in simulations of galaxyformation Disk Galaxy Formation in a cosmological(context) content

  2. MUPPI: MUltiPhaseParticleIntegrator Murante, Monaco, Giovalli, Borgani, Diaferio, 2010, MNRAS, 405, 1491 • Star formation & feedback algorithm • Implemented in GADGET-3 • Integrates ISM equations for eachparticleateach SPH time step • Effectivethermal feedback • Obtains SK relation withoutimposingit • Gives ISM characteristics (See Monaco, Murante, Borgani, Dolag, 2012, MNRAS, 421, 2485) Disk Galaxy Formation in a cosmological(context) content

  3. MASS FLOWS STAR FORMATION COOLING EVAPORATION On hotphase! RESTORATION On coldphase! = MOLECULAR GAS MH2 ->SF = = Disk Galaxy Formation in a cosmological(context) content

  4. SPH Energy exchanges Multi-Phase particle Δt, ΔS Ėhydro = ΔS/(γ-1)ρ(γ-1)Δt Ėhot = -Ėcool+Ėsn+Ėhydro new ΔS etc... Disk Galaxy Formation in a cosmological(context) content

  5. ENERGY FLOW(S..) Hot phase energy ENERGY CONTRIBUTION DUE TO HYDRODYNAMICS • ENERGY RELEASED BY SNe • ENERGY LOSS DUE TO COOLING this is the ENTROPY variation due to SPH hydrodynamics PRESSURE-DRIVEN SF Phenomenological (Blitz & Rosolowsky 2006) Pext Ptherm with P0 = 35000 Disk Galaxy Formation in a cosmological(context) content

  6. More characteristics • Thermalenergygiventoneighbouringparticles in a directional way • Chemicalevolution (Tornatore et al 2007) • Primordial AND metal dependentcooling • Stocastickineticwinds: a fractionofparticlescontinouslyreceivealsokineticenergyfromneighbouringparticles. Theydecouplefrom the gas. Wind speeddepends on local SF. In cosmologicalsimulations, velocities up to 1000 km/s Disk Galaxy Formation in a cosmological(context) content

  7. Dynamical SK relation Monaco, Murante, Borgani,Dolag, 2012, MNRAS, 421, 2485 Disk Galaxy Formation in a cosmological(context) content

  8. Cosmological disk galaxysimulations (Stoehr+, 2002, MNRAS, 355, 84) (SeeThe Aquila comparison project, Scannapieco+, 2012, MNRAS, in press) Disk Galaxy Formation in a cosmological(context) content

  9. Our best disk galaxy Disk Galaxy Formation in a cosmological(context) content

  10. Howdoes the gas accrete? We: • usesimulationswithoutchemicalevolution/metal cooling • identifystars/gas particles at z=0 within R200, Rgal=0.1 R200 • followback particles and recordedtheir maximum T • alsoconstructSUBFIND merger trees of haloes • use three temperature ranges: • 0 < Tmax < 250,000 K (cold); • 250,000 K < Tmax < 106 K (warm) • Tmax > 106 K • seetowhichaccretionchannel gas particlesbelong, iftheyeverwereintoclumps, bothforparticleswithin R200 and Rgal. Murante, Calabrese, De Lucia, Monaco Borgani, Dolag, 2012, ApJL, 749, 34 Disk Galaxy Formation in a cosmological(context) content

  11. Disk Galaxy Formation in a cosmological(context) content

  12. Accretionchannels Warm gas GADGET Disk Galaxy Formation in a cosmological(context) content

  13. GA vs AQ Galaxy Halo Disk Galaxy Formation in a cosmological(context) content

  14. Multiphasepropertiesof gas in channels Aq-C-5 Disk Galaxy Formation in a cosmological(context) content

  15. Resolution (resultsforaccretion on galaxy) Disk Galaxy Formation in a cosmological(context) content

  16. Metal cooling (resultsfor GA1) Disk Galaxy Formation in a cosmological(context) content

  17. Clumpiness Cold gas isclumpy! Our gas clumpshave DM… (107Msolmin) Disk Galaxy Formation in a cosmological(context) content (resultsfor GA2)

  18. Conclusions • MUPPI can produce reasonable disk galaxies • Accretion on haloismainlycold • Withanefficientthermal feedback scheme, a new gas accretionchannel on galaxyarises: warmaccretion • Warmaccretionisfuelledby gas heatedbySne feedback • Coldaccretion on galaxiesisatleast 50% clumpy • Ourresultdoesnotdependuponresolution, ourchosenhalo, chemicalevolution/metal cooling: only on the efficiencyofthermal feedback • MUPPI can produce reasonable disk galaxies • Accretion on haloismainlycold • Withanefficientthermal feedbackscheme, a new gas accretionchannelon galaxyarises:warmaccretion • Warmaccretionisfuelledbygas heatedbySne feedback • Coldaccretionon galaxiesisatleast 50% clumpy • Ourresultdoesnotdependuponresolution, ourchosenhalo, chemicalevolution/metal cooling: only on the efficiencyofthermal feedback Disk Galaxy Formation in a cosmological(context) content

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