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Correlations of DM Halo Properties: Building the Hyades Suite

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Correlations of DM Halo Properties: Building the Hyades Suite Correlations of DM halo properties: Building the Hyades Suite Jose O~norbe Fulbright Postdoctoral Fellow @ University of California Irvine ([email protected]) In collaboration with S. Garrison-Kimmel (UCI), J. Bullock (UCI), A. Maller (CUNY), M. Rocha (UCI) and G. Bryan (CU). August 11, 2011 2011 Santa Cruz Galaxy Workshop Hyades Simulations Suite Zoom-in simulations of galaxy halos spanning Mvir = 0:05 5E12M − Identical initial conditions (MUSIC, Hahn & Abel 2011) with multiple codes: ENZO, GADGET, GASOLINE Ultimate goal: How robust are halo (& galaxy) properties from code to code? First step: Obtain a reliable and representative sample of halos Jose O~norbe Correlations of DM halo properties: the Hyades Suite 2 Q: How big of a volume do we need to use to get no contamination? Q: Can we pick 5rvir small volumes without bias? Hyades Simulations Suite z = 0 Volume @ z = 250 2 halos ini same mass @ z=0 Red one would be much quicker run 2rvir The initial high redshift volume can be defined by the convex hull (minimal polyhedron that englobes all particles) Jose O~norbe Correlations of DM halo properties: the Hyades Suite 3 Hyades Simulations Suite 2 halos z = 0 Volume @ zini = 250 same mass @ z=0 Red one would be much quicker run 2rvir Q: How big of a volume do we need to use to get no contamination? Q: Can we pick 5rvir small volumes without bias? Jose O~norbe Correlations of DM halo properties: the Hyades Suite 3 3 Use Lbox = 50Mpc=h, Np = 512 , = 1kpc=h sim to explore how halo properties depend on the volhz Dark Matter Halo Properties 50 Mvir , Vmax , Rmax , shape, λ, Nneig , aform, Nmergers , subhalo, volhz (1 × rvir),... Cosmology: ΛCDM WMAP7 Sample: Halos with Npart > 500 Which halo properties contain more information? (Skibba & Maccio 2011, Jeeson-Daniel et al. 2011) How can we build a reliable sample with the lowest number of halos? How selective can we be with volhz ? Jose O~norbe Correlations of DM halo properties: the Hyades Suite 4 Selecting a Milky Way Halo: How selective can we be? MW Mass bin: 12 [1 3] 10 M −No subhalos× How is correlated volhz for a fixed mass? For some specific halo properties can we choose a low volhz ? Jose O~norbe Correlations of DM halo properties: the Hyades Suite 5 Selecting a Milky Way Halo: How selective can we be? MW Mass bin: 12 [1 3] 10 M −No subhalos× How is correlated volhz for a fixed mass? For some specific halo properties can we choose a low volhz ? Jose O~norbe Correlations of DM halo properties: the Hyades Suite 5 Selecting a Milky Way Halo: How selective can we be? Color map and black points: full MW sample White points: small initial volume No bias with volhz Jose O~norbe Correlations of DM halo properties: the Hyades Suite 6 Testing reliability in Zoom-in simulations Using MUSIC (Hahn & Abel 2011) Set of dark matter zoom-in simulations. mp = 6:88E7 1:67E4 M =h − Comparison between Dark-Matter full box and zoom-in runs Initial high-res volume: no contamination and stability of halo parameters. Mass and spatial resolution tests. Lower resolution levels sizes and resolution. Code differences. Katz & White 1993, Klypin et al. 2001 Jose O~norbe Correlations of DM halo properties: the Hyades Suite 7 Testing reliability in Zoom-in simulations 5E12M ∼ 1E12M ∼ 5E11M 4 ∼ Contamination: Any low res particles inside rvir ? Log (Volume computed at high resolution) Jose O~norbe Correlations of DM halo properties: the Hyades Suite 8 Testing reliability in Zoom-in simulations 5E12M ∼ 1E12M ∼ 5E11M Only4 ∼ runs with no contamination Vmax and most halo properties are very stable from run to run and as a function of initial volume. Some problems with ENZO because the halo moves within grid... Jose O~norbe Correlations of DM halo properties: the Hyades Suite 9 Testing reliability in Zoom-in simulations 5E12M ∼ 1E12M ∼ 5E11M Only4 ∼ runs with no contamination Spin parameter less stable Jose O~norbe Correlations of DM halo properties: the Hyades Suite 10 Conclusions: Preliminary results For a fixed halo mass, there is no strong bias with the initial volume (good news for zoom simulations) Zoom volume need to be at least 2 rvir for no ∼ × contamination within rvir Halo properties are stable for non-contaminated zooms, except for spin parameter. Enzo approach needs higher initial volume and more detailed information on halo history. Jose O~norbe Correlations of DM halo properties: the Hyades Suite 11 Thank you! Hyades: Daughters of Atlas, nurses of Dionysus. A sisterhood of nymphs that bring rain Ambrosia Coronis Phyto Would you like to try Erudora Cardie any Hyades nymph Niseis Phaesyle with your code? Cleeia Pedile Phyto Please contact us!!! Polyxo Synecho Niseis ([email protected]) Phaeo Jose O~norbe Correlations of DM halo properties: the Hyades Suite 12 Some Important Parameters Full Box Parameters Lbox = 50 Mpc=h, = 1 kpc=h, 3 Npart = 512 , zini = 250, 7 mdm = 6:88 10 M =h WMAP 7 Cosmology. × Model: lcdm + sz + lens Full Box Halo Sample ΩΛ = 0:734, Ωm = 0:266, Npart > 500 Ωb = 0:0449, h = 0:71, !10 M > 3:4 10 M =h σ8 = 0:801, ns = 0:963 × "MW" Mass Bin Halo Sample 12 12 1 10 M < Mhalo < 3 10 M No× subhalos × Jose O~norbe Correlations of DM halo properties: the Hyades Suite 13 Other Figures: Full Sample log Mvir vs log volhz: 0.552 3.5 3.0 2.5 com. 3 ) 2.0 Mpc/h ( 1.5 hz vol 1.0 log 0.5 11.0 11.5 12.0 12.5 13.0 log Mvir (M /h) Jose O~norbe Correlations of DM halo properties: the Hyades Suite 14 Other Figures: MW bin Jose O~norbe Correlations of DM halo properties: the Hyades Suite 15.
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