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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

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

mupp i mu lti p hase p article i ntegrator
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

slide3

MASS FLOWS

STAR FORMATION

COOLING

EVAPORATION

On hotphase!

RESTORATION

On coldphase!

=

MOLECULAR GAS

MH2 ->SF

=

=

Disk Galaxy Formation in a cosmological(context) content

slide4

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

slide5

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

more characteristics
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

dynamical sk relation
Dynamical SK relation

Monaco, Murante, Borgani,Dolag, 2012, MNRAS, 421, 2485

Disk Galaxy Formation in a cosmological(context) content

cosmological disk galaxy simulations
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

our best disk galaxy
Our best disk galaxy

Disk Galaxy Formation in a cosmological(context) content

how does the gas accrete
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

accretion channels
Accretionchannels

Warm gas

GADGET

Disk Galaxy Formation in a cosmological(context) content

ga vs aq
GA vs AQ

Galaxy

Halo

Disk Galaxy Formation in a cosmological(context) content

multiphase properties of gas in channels
Multiphasepropertiesof gas in channels

Aq-C-5

Disk Galaxy Formation in a cosmological(context) content

resolution
Resolution

(resultsforaccretion on galaxy)

Disk Galaxy Formation in a cosmological(context) content

metal cooling
Metal cooling

(resultsfor GA1)

Disk Galaxy Formation in a cosmological(context) content

clumpiness
Clumpiness

Cold gas isclumpy!

Our gas clumpshave DM… (107Msolmin)

Disk Galaxy Formation in a cosmological(context) content

(resultsfor GA2)

conclusions
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