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Azadeh (Azi) Fattahi Institute for Computational Cosmology Durham University

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Azadeh (Azi) Fattahi Institute for Computational Cosmology Durham University Azadeh (Azi) Fattahi Institute for Computational Cosmology Durham University Top-hat Spherical Collapose Model Spherical density perturbation The equation of motion is with constant over density very simple: 2 d r 2 =−G M (<r)/r dt 2 r 4 3 M (<r)= π r (t)ρ(t)[1+δ(t)] 3 Solutions: Top-hat Spherical Collapose Model (i) expansion 0 < χ < π (ii) reaching maximum (trun-around, tta) , rmax , at χ=π (iii) collapsing back between π < χ < 2π (iv) final stage at χ=2π (tcol = 2 t ta ) In EdS universe: δ ta ~ 5.55 and δ col = infinity Top-hat Spherical Collapose Model More-realistic: system virializes Virial theorem : rvir = rta / 2 In EdS universe system the above condition yields: 1+δvir ≈ 178 (note: δvir = Δvir ) In non EdS universe with Lamda: 1 + δvir ≈ 360 Virialized Another common adopted vallue: region 1 + δvir = ρ/ρcrit =200 Power spectrum -1 Damping scale (λ) ~ mp Hot dark matter : Relativistic at early times mp ~ 10 ev (neutrinos) 15 λ ~ 10 Msol (galaxy clusters) Cold dark matter: Non-relativistic at early times mp ~ 1 Gev λ ~ earth mass warm dark matter: mp ~ 1 kev λ ~ massive galaxies Hot dark matter (HDM) Clusters collapse first: top-down formation of structure Cold dark matter (CDM) Dwarf galaxies collapse first: bottom-up (hierarchical) formatio Numerical simulations and large scales CfA redshift survey 2dF survey HDM sims. CfA redshift Survey CDM sims. sky projection Millennium simulation Virgo Consortium Millennium simulation series Millennium Sim. 100 Mpc h-1 Assigning galaxies to dark matter halos based on semi- analytic models Virgo Consortium Millennium Sim. II Springel+2005 Boylan-Kolchin+2009 Millennium simulation fly-through ● cosmic web structure Voids Fillaments Sheets ● Bigger objects form at the intersection of fillaments ● Clumpiness ● Hierarchical growth … ● Self-similarity ... CDM Hierarchical Growth Aquarius project: simulations of Milky Way like halos Springel et al. 2008 – Virgo Consortium CDM Hierarchical Growth CDM Hierarchical Growth CDM Hierarchical Growth CDM Hierarchical Growth CDM self-similarity 12 One is a Milky-Way size halo (mass~10 Msol ); 14 another a galaxy cluster halo (mass ~10 Msol ) Wang+2012 Boylan-Kolchin+2009 Substructures mass function mass Substructures Subhalo mass/host mass Subhalo mass Subhalo CDM self-similarity Navarro, Frenk, White 1996, 1997 Frenk, 1996, White Navarro, density profile (mass profile) profile) (mass profile density Dark matter halo density profile in CDM Density profiles of halos spanning 4 orders of magnitude in mass NFW profile Two-parmeters profile: ● rs, ρs ● M200, c Mass-concentration relation: Navarro, Frenk, White (NFW) 1996, 1997 Neto+2007, Maccio+2008, 11 12 13 14 15 Ludlow+2014, Ludlow+2017 Log mass Halo mass function in LCDM Increasing number of small structures Baryons and Galaxy formation within LCDM Dark matter Gas on large scales 100 Mpc color=temperature Eagle simulation - Schaye et al. 2016 Baryons and Galaxy formation within LCDM Gas condensation in the centre of potential of halos (White & Rees 1978) DM halo Dark matter is collisionless: Collapses into a spherical component Gas is collisional: loses energy due to friction, radiation, etc, Settles into a disk due to the conservation of angular momentum Gaseous and stellar disk Sizes are not proportional; e.g for a Milky-Way size galaxy: Stellar disk ~ 20 kpc; halo virial radius ~ 250kpc Baryons and Galaxy formation within LCDM Credit: EAGLE collaboration – Virgo Consortium Baryons and Galaxy formation within LCDM Stellar halo and stellar streams MW stellar halo streams (Credit: A. Bonaca) Bullock & Johnston 2005 Andromeda stellar halo; PAndAS (McConnachie+2008) mechanisms playmechanisms role galaxy in formation scales; different different at is different effeciency Galaxy formation in at the both slopes ends:and SMF of HMF the Note difference Halo mass function mass Halo The relation between stellar mass and halo mass massstellar halo and between relation The How doHow galaxies poplulatehalos? DM Stellar mass function mass Stellar Li & White 2009 How do galaxies poplulate DM halos? The relation between stellar mass and halo mass Supernovae feedback AGN feedback 10 Side note: Cosmic reionization important at smaller scales: Mhalo ~ 10 Msol How do galaxies poplulate DM halos? The relation between stellar mass and halo mass “Abundance Matching” as a powerfull tool: Assuming there is a one-to-one and monotonic relation between stellar mass stars and halo mass Frenk+1983, Guo+2010, Behroozi+2013, Moster+2013 Dark matter Mass * 12 L galaxies (10 Msol halos) are most efficient in retaining their baryons and turning them into stars! How do galaxies poplulate DM halos? The relation between stellar mass and halo mass Supernovae feedback AGN feedback 10 Side note: Cosmic reionization important at smaller scales: Mhalo ~ 10 Msol EAGLE (Schaye+2015) FIRE – (Garrison-Kimmel+2018) Illustris (Vogelsberger+2014) .
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