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Astrophysical Constraints on Dark Matter: Warm or Cold ?

Astrophysical Constraints on Dark Matter: Warm or Cold ?. Charling TAO CPPM, IN2P3, France Tsinghua Center for Astrophysics, Tsinghua University, China Cooks’ Branch workshop on SN, april 2012. Euclid, an ESA M-class mission. A geometrical probe of the universe proposed for Cosmic Vision.

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Astrophysical Constraints on Dark Matter: Warm or Cold ?

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  1. Astrophysical Constraints on Dark Matter: Warm or Cold ? Charling TAO CPPM, IN2P3, France • Tsinghua Center for Astrophysics, Tsinghua University, China • Cooks’ Branch workshop on SN, april 2012

  2. Euclid, an ESA M-class mission A geometrical probe of the universe proposed for Cosmic Vision All-sky optical imaging for gravitational lensing All-sky near-IR spectra to H=22 for BAO = +

  3. The Euclid Concept • Named in honour of the pioneer of geometry • Euclid will survey the extra-galactic sky (15 000 deg2) to simultaneously measure its two principal dark energy probes: • Weak lensing: • Diffraction limited galaxy shape measurements in one broad visible R/I/Z band. • Redshift determination by photo-z measurements in 3 YJH NIR bands to H(AB)=24 mag, 5σ point source • Baryonic Acoustic Oscillations: • Spectroscopic redshifts for 33% of all galaxies brighter than H(AB)=22 mag, σz<0.006 • With constraints: • Aperture: max 1.2 m diameter • Mission duration: ~ 6 years,… In october 2011, we have been chosen over PLATO for launch in 2019 Official (financial) approval expected June 2012

  4. Euclid and SN? • About 20 people in SN WG • Leads: I. Hook, E. Capellaro, CT • Use opportunity of NIR YJH filters in space • (no atmospheric transmission)! • Challenge : propose best possible SN survey within existing constraints • Dedicated Deep Survey for 6 months at end of mission (2024-?) or other options under study (survey strategy, choice of fields, calibrations,…) • Synergy with Pan-Starrs, LSST,JWST, Antarctica, …? • to develop if we can have an independent DS field

  5. A mysterious Dark Universe with DE and DM ! What we know is only 4% of the energy density of the Universe We measure with precision the extent of our ignorance! An exciting lesson in humility ! Concordance Model LCDM Graph source: Wikipedia

  6. Before 2000: Nature of DMHot orCold? • CDM is non-relativistic at decoupling, forms structures in a hierarchical, bottom-up scenario. • HDM is tightly bound by observations and LSS formation

  7. LSS structures

  8. N-Body Simulations LSS favour LCDM VIRGO Consortium 1996 http://www.mpa-garching.mpg.de/~virgo/virgo/ Boxsize 239.5 Mpc/h, 2563 particles

  9. ~2000 :Problems with CDM at small scales • Comparing more data with more precise N-body hydrodynamical simulations • Number of galactic satellites • cusp/core at GC

  10. Too low number of visible satellite galaxies? Satellite galaxies are seen in Milky Way, e.g. Saggittarius, MCs Predicted number Observed number of luminous satellite galaxies 10km/s 20km/s 100km/s

  11. Dark matter distribution—Density profiles Universal Density Profile NFW Navarro, Frenk, White 1996 Cusp

  12. Salucci & • Frigerio Martins 2009

  13. DM Cores in Dwarf galaxies • Oh et al. 2011 Data prefer Burkert Core Profile

  14. Galaxy core vs cusp • Salucci & Frigerio Martins, 2009

  15. Alternatives to CDM • Self-Interacting Dark Matter (Spergel & Steinhardt 2000) • Strongly Interacting Massive Particle • Annihilating DM • Decaying DM • Fuzzy DM • WDM: reduce the small scale power

  16. WDM vs CDM Velocity function Density profile From Jing 2000

  17. Nature of DMHot orCold, or Warm? • CDM is non-relativistic at decoupling, forms structures in a hierarchical, bottom-up scenario. • HDM is tightly bound by observations and LSS formation WDM?

  18. But doubts on Lya results by SDSS people!

  19. A fashionable candidate Sterile neutrinos

  20. Constraints on sterile neutrinos

  21. Limits on mass of WDM particles • Stellardynamics in MW satellites (Boyanovsky, de Vega, Sanchez 2008; de Vega and Sanchez 2009) • High-z QSO LF(e.g. Song and Lee 2009) • Ly-alpha forest to constrain P(k) atsmallscales and differentz’s(Most popularmethod: Narayanan et al 2000; Viel et al 2005;2008) • Ly-a + SDSS results (Boyarsky et al 2009) • QSO lensing( Miranda & Maccio 2007 ) • Abundance of dwarf satellites of MW (Maccio & Fontanot 2010; Polysensky & Ricotti, 2010)  Mass WDM ~ 1- 5 keV

  22. Cosmic shear power spectra Markovic et al. 2010Euclid-like DE space survey+Planck: Sensitive to m_WDM < 2.5 keV

  23. Nonthermal production of dark matter • Non thermal production in the early universe, • Large annihilation cross section, • Large velocity depresses the small scale structure. • Possible constraints from galactic center gamma-ray Lin, Huang, Zhang, Brandenberger, PRL86,954 (2001) Bi, Brandenberger, Gondolo, Li, Yuan, Zhang, 0905.1253 CDM scenario with WDM?

  24. “Evidence” for WDM ? • ''cusp-core problem'', • "missing satellite problem'',

  25. Hot topic, eg WARM DARK MATTER IN THE GALAXIES: THEORETICAL AND OBSERVATIONAL PROGRESSES CIAS Observatoire de Paris, Château de Meudon, Meudon campus 8, 9 and 10 June 2011

  26. CLUES simulations, Yepes, 2010

  27. Velocity widths in Galaxies Velocitywidths in galaxies from 21 cm HI surveys Papastergis et al, 2011; Zavala et al., 2009 NB: The redcurveis for 1 keV WDM Or inability of HI to trace the maximum halo rotational velocity of low-mass systems?

  28. CDM vs WDM: HI velocity functions Virgo and Anti Virgo directions arXiv:1005.2687: Constrained Local UniversE Simulations (CLUES) Gottloeber, Hoffman , Yepes « No simple feedback mechanism to explain the factor 10 depletion from CDM » ?

  29. “Evidence” for WDM ? • "missing satellite problem'', • ''cusp-core problem'', • mini-voids The sizes of mini-voids in the local universe: an argument in favor of a warm dark matter model? Tikhonov et al. • HI determinations of velocity function profiles • N-Body simulation Comparisons with Virgo results by Arecibo Legacy (ALFALFA)

  30. “Evidence” for WDM ? • "missing satellite problem'', • ''cusp-core problem'', • mini-voids The sizes of mini-voids in the local universe: an argument in favor of a warm dark matter model? Tikhonov et al. • HI determinations of velocity function profiles • N-Body simulation Comparisons with Virgo results by Arecibo Legacy (ALFALFA) • Detection of 2.5 keV X-ray from dark dwarf galaxy?

  31. Before we get too depressed or excited …

  32. Before we get too depressed or excited … • Do not trust fashion fads ! • How much can one trust N-Body simulations? • Beware of data analysis bias ! Blind analysis?

  33. Strong Reliance on N-body simulations eg Gao et al., Jing et al., Yepes et al., WDM and CDM simulations. - Non-linear collapse of WDM structures - A replacement for the NFW model (WDM) • - Effects of Baryons

  34. LCDM Dark matter halo profile from N-Body simulations Cusps? Old CDM Simulations  cusps (Navarro, Frenk, White 1996): The latest cosmological N-body simulations find two intriguing properties for dark matter haloes: (1) their radial density profile, ρ, is better fit by a form that flattens to a constant at the halo center (the Einastoprofile) than the widely-used NFW form; (2) the radial profile of the pseudo-phase-space density, continues to be well fit by a power law, as seen in earlier lower-resolution simulations.

  35. Einasto vs NFW • Ma Chung Pei, Chang, P., Zhang, 2009 • Predict the two properties cannot hold at all scales

  36. Nature of dark matter or astrophysics process? eg, Maschenko et al. 2006, Nature, or 2008, science, etc…

  37. SN feedback and Radiation pressureanswer the cuspy/cored issue for spiral galaxy • Maccio et al. ApJ 2012 • High resolution cosmological hydro-dynamical simulations  effects of dissipative processes on the inner distribution of dark matter in Milky-Way like objects (M ≈ 1012 M ⊙ ). • supernova feedback + effects of radiation pressure of massive stars before explosion • increased stellar feedback  expansion of the DM halo instead of contraction with respect to N-body simulations. • Baryons erase the DM cuspy distribution flat , cored DM density profile, well fit by a Burkert profile, with fitting parameters consistent with observations.

  38. More faint or dark galaxies discovered • Eg, Belokurov et al, 2010

  39. Missing satellites: CDM way out • satellites do exist, but star formation suppressed (after reionization?) • satellites orbit do not bring them to close interaction with disk, so they will not heat up the disk. • Local Group dwarf velocity dispersion underestimated • Galaxies may not follow dwarves • Halo substructures may be probed by • Lensing • local Milky Way structures

  40. Future Measurements of DM properties with lensing • I. Cosmic shear power spectra: Mass constraints? • II. Galaxy-scale DM density profiles: • Galaxy-galaxy lensing • Magnification Sensitivity of detection scales by lensing Strong lensing: 1-10 kpc Flexion: 10-100 kpc Weak lensing: <100 kpc

  41. Cosmic shear power spectra Markovic et al. 2010 Euclid-like DE space survey +Planck: • Integral effects → better than matter power spectrum

  42. Cosmic shear power spectra Markovic et al. 2010 Euclid-like DE space survey +Planck: Sensitive to m_WDM < 2.5 keV

  43. Power spectra and sensitivity to WDM Is that interesting ? Lyman a constraints m > 2 or 4 keV or even higher – But doubts on Lya results!

  44. Baryon physics (AGN feedback) affects Matter Power Spectrum • Semboloni et al. (2011) • Van Daalen et al.(2011) • Shale et al :OWLS simulation • Consequences on WL • cosmological parameters fits

  45. Baryon effects different from neutrino or WDM effects • Semboloni et al. 2011

  46. Probing DM Particle properties CL0024 Mandelbaum et al. (2006) Stacked galaxy—galaxy weak lensing signal fit with various profiles. Tyson, Kochanski, & Dell’Antonio (1998)

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