dark matter a simple model for the universe
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Dark Matter A simple model for the Universe Standard model: homogeneous, isotropic, expanding Universe Astronomers time unit: redshift z [z+1: inverse of expansion factor] Simple composition: Dark Energy Dark Matter

  1. Dark Matter

  2. A simple model for the Universe ★ Standard model: homogeneous, isotropic, expanding Universe ★ Astronomer’s time unit: redshift z [z+1: inverse of expansion factor] ★ Simple composition: ★ Dark Energy ★ Dark Matter ★ Baryons Planck team KAS16/MT Lecture1I - Dark Matter 2

  3. A simple model for the Universe ★ Standard model: homogeneous, isotropic, expanding Universe ★ Astronomer’s time unit: redshift z [z+1: inverse of expansion factor] ★ Simple composition: ★ Dark Energy ★ Dark Matter ★ Baryons Planck team KAS16/MT Lecture1I - Dark Matter 3

  4. A simple model for the Universe ★ Standard model: homogeneous, isotropic, expanding Universe ★ Astronomer’s time unit: redshift z [z+1: inverse of expansion factor] ★ Simple composition: ★ Dark Energy ★ Dark Matter s s a ★ Baryons l c t x e n e r a s n Planck team o y r a B KAS16/MT Lecture1I - Dark Matter 4

  5. Outline ★ What dark matter might be ★ Dark matter halos ★ Formation ★ Mass function ★ Growth and evolution ★ Substructure ★ How warm is dark matter? KAS16/MT Lecture1I - Dark Matter 5

  6. What is dark matter? ★ We don’t really know... ★ Must interact gravitationally only ★ We see small scale structure: ★ DM non-relativistic at decoupling ★ Generic leading idea is that of a weakly interacting massive particle ( ~ 100GeV range) ★ Neutralino? KAS16/MT Lecture1I - Dark Matter 6

  7. Primordial fluctuations: The leading idea ★ Universe is initially very homogenous ★ But... quantum fluctuations at very early times amplified by inflation ★ Scale invariant and Gaussian density field [ simplest inflation model ... active field of research] KAS16/MT Lecture1I - Dark Matter 7

  8. Primordial fluctuations: Growth Evolved Power Spectrum = Primordial Power Spectrum * Transfer function * Growth Function KAS16/MT Lecture1I - Dark Matter 8

  9. Primordial fluctuations: Growth ★ Transfer function T(k): “early time” processing ★ Matter dominated Universe, all scales grow equally. Transfer function trivial ★ Radiation dominated Universe: Slow-growth only [expansion faster than collapse] ★ Small scales (smaller than horizon) erased by “free streaming” while DM relativistic ★ DM needs to be cold (or warm) otherwise T(k) is suppressed KAS16/MT Lecture1I - Dark Matter 9

  10. Primordial fluctuations: Growth ★ CMB allows us to quantify fluctuations at decoupling KAS16/MT Lecture1I - Dark Matter 10

  11. Growing the cosmic web ★ Choose a cosmological model [ Ω m , Ω Λ , Ω b ,h,P(k)] ★ Choose computational setup [box size, resolution] ★ Create a discrete realization of the density field ★ Evolve it analytically to initial redshift ★ Run the N-body simulation ★ Identify halos, post-process/characterize them: ★ Publish papers! KAS16/MT Lecture1I - Dark Matter 11

  12. Building a (MilkyWay) halo KAS16/MT Lecture1I - Dark Matter 12

  13. What is a dark matter halo? ★ Halos are self-gravitating systems ★ Halos are non-linear peaks in the dark- matter density field whose self-gravity won over Hubble expansion ★ Operationally: A halo is a non-linear peak in the density field with boundaries defined by a given density contrast ★ [this can be used for defining halos numerically in simulations] KAS16/MT Lecture1I - Dark Matter 13

  14. A simple approximation for halos KAS16/MT Lecture1I - Dark Matter 14

  15. Dark matter halo formation in spherical collapse credit: R. Wechser KAS16/MT Lecture1I - Dark Matter 15

  16. Where does a halo end? ★ The simple spherical collapse model can be used to define a “virial radius” [typical halo size] ★ In reality: lot of discussion! [see Shull 2014, “Where do galaxies end?”] ★ Quotes from a meeting: “The virial radius is actually at three virial radii” “Let’s define the virial radius as the virial radius” ★ Bound, virialized material can exist outside the virial radius ★ There is continuous accretion KAS16/MT Lecture1I - Dark Matter 16

  17. The density profile of halos ★ Simple, quasi-universal profile for dark-matter halos clear from early simulations Navarro, Frenk & White (1995) What does it mean? KAS16/MT Lecture1I - Dark Matter 17

  18. The density profile of halos ★ Simple, quasi-universal profile for dark-matter halos clear from early simulations Navarro, Frenk & White (1995) • Cusp at the center (with finite mass) • Divergence at large radii (but there is tidal truncation) KAS16/MT Lecture1I - Dark Matter 18

  19. The halo mass function from simulations ★ Consensus to ~ 5% level on DM halo mass z=0 function at z=0 [at fixed cosmology] Warren et al. 2004 KAS16/MT Lecture1I - Dark Matter 19

  20. The halo mass function from simulations ★ Strong evolution with redshift ★ Note flattening at z=0 for low masses Reed et al. 2003 KAS16/MT Lecture1I - Dark Matter 20

  21. The halo mass function from Press-Schechter ★ Halos arise from density fluctuations (Gaussian Random field) which grow with redshift ★ Smooth density field on scale such as to enclose mass M h ★ Count peaks with density above a critical threshold (typically 1.69 in linear growth) ★ This is the basic idea for Press Schechter mass function KAS16/MT Lecture1I - Dark Matter 21

  22. The halo assembly time ★ Time needed to grow from M h /2 to M h ★ On average : ★ High-z halos grow fast ★ Weak dependence on halo mass But don’t forget it is a stochastic process! KAS16/MT Lecture1I - Dark Matter 22

  23. Halo growth with time ★ Halo growth is a stochastic process ★ Can be modeled with “Extended Press- Schechter” formalism ★ Growth by ~ 10 7 for rare halo from z ~ 40 to z ~ 0 ★ Growth by ~ 100x from z=6 to z=0 for Milky Way like halo KAS16/MT Lecture1I - Dark Matter 23

  24. Merger and growth of halos ★ Are the most massive dark matter halos at high redshift evolving into the most massive halos at lower redshift? ★ Given the most massive dark matter halos, are their progenitors the most massive at earlier times? ★ We can use simulations, or theory, to address the question, but what do you expect? KAS16/MT Lecture1I - Dark Matter 24

  25. Merger and growth of halos ★ In the Millennium Run, the most massive z ~ 6 halo evolves into an unimpressive z=0 cluster KAS16/MT Lecture1I - Dark Matter 25

  26. Distribution of progenitor halos ★ Most massive halo at z 1 <z 2 does not correspond to most massive progenitor at z 2 Trenti, Santos & Stiavelli (2008) KAS16/MT Lecture1I - Dark Matter 26

  27. A random walk interpretation ★ Rarest walks are regressing toward the mean as time passes Trenti, Santos & Stiavelli (2008) KAS16/MT Lecture1I - Dark Matter 27

  28. Substructure ★ Halos have internal sub-structure ★ Let’s go beyond the spherical cow approximation! KAS16/MT Lecture1I - Dark Matter 28

  29. Substructure: An overview credit: R. Wechser KAS16/MT Lecture1I - Dark Matter 29

  30. Substructure: the drivers ★ Competition between accretion and disruption of subhalos credit: R. Wechser KAS16/MT Lecture1I - Dark Matter 30

  31. The warmness of dark matter ★ Substructure dramatically affected KAS16/MT Lecture1I - Dark Matter 31

  32. The warmness of dark matter ★ Fraction of mass in substructure depends on DM properties ★ We can use halo structure to learn about fundamental physics KAS16/MT Lecture1I - Dark Matter 32

  33. The warmness of dark matter ★ How can we observationally measure clumpiness (substructure) of DM halos? KAS16/MT Lecture1I - Dark Matter 33

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