Astrophysical constraints on dark matter
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Astrophysical ConstraintsAstrophysical Constraints on Dark Matter: on Dark Matter: Warm or Cold ?Warm or Cold ?
Charling TAO
CPPM, IN2P3, France
Tsinghua Center for Astrophysics, Tsinghua University, China
Cooks’ Branch workshop on SN, april 2012
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Euclid, an ESA M-class missionA 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
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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 2019Official (financial) approval expected June 2012
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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
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Graph source: Wikipedia
What we know is only 4%
of the energy density of the
Universe
We measure with precision the extent of our ignorance!
Concordance Model CDM
A mysterious Dark Universe with DE and DM !
An exciting lesson in humility !
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Before 2000: Nature of DMHot or Cold?
CDM is non-relativistic
at decoupling, forms
structures in a hierarchical,
bottom-up scenario.
HDM is tightly bound byobservations and LSS formation
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LSS structures
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N-Body Simulations LSS favour CDM
VIRGO Consortium 1996http://www.mpa-garching.mpg.de/~virgo/virgo/
OMEGA = 0.3 LAMBDA = 0.7
H0 = 70 km/(Mpc sec) Sigma8 = 0.9
OMEGA = 1 LAMBDA =0
H0 = 50 km/(Mpc sec) Sigma8 = 0.51
OMEGA = 1 LAMBDA =0
H0 = 50 km/(Mpc sec) Sigma8 = 0.51
OMEGA = 0.3 LAMBDA = 0
H0 = 70 km/(Mpc sec) Sigma8 = 0.85
Boxsize 239.5 Mpc/h, 2563 particles
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~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
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Predicted number
Observed number of luminous
satellite galaxies
Satellite galaxies are seen in Milky Way, e.g. Saggittarius, MCs
20km/s 100km/s10km/s
Too low number of visible satellite galaxies?
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Universal Density ProfileNFW
Navarro, Frenk, White 1996
Cusp
Dark matter distribution—Density profiles
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Salucci &
Frigerio Martins 2009
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DM Cores in Dwarf galaxies
Oh et al. 2011
Data prefer Burkert Core Profile
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Galaxy core vs cusp
Salucci & Frigerio Martins, 2009
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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
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WDM vs CDM
From Jing 2000
Density profileVelocity function
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Nature of DMHot or Cold, or Warm?
CDM is non-relativistic
at decoupling, forms
structures in a hierarchical,
bottom-up scenario.
HDM is tightly bound byobservations and LSS formation
WDM?
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But doubts on Lyresultsby SDSS people!
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A fashionable candidate Sterile neutrinos
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Constraints on sterile neutrinos
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Limits on mass of WDM particles
• Stellar dynamics 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) at small scales and different
z’s (Most popular method: 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
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Cosmic shear power spectra Markovic et al. 2010 Euclid-like DE space survey+Planck:
Sensitive to m_WDM < 2.5 keV
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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
fTv
scmh
13272 103
Lin, Huang, Zhang, Brandenberger, PRL86,954 (2001)
Bi, Brandenberger, Gondolo, Li, Yuan, Zhang, 0905.1253
CDM scenario with WDM?
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•''cusp-core problem'',
•"missing satellite problem'',
“Evidence” for WDM ?
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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
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CLUES simulations, Yepes, 2010
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Velocity widths in Galaxies
Velocity widths in galaxies from 21 cm HI surveysPapastergis et al, 2011; Zavala et al., 2009NB: The red curve is for 1 keV WDM
Or inability of HI to trace the maximum halo rotational velocity of low-mass systems?
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CDM vs WDM: HI velocity functions
Virgo and Anti Virgo directions
« No simple feedback mechanism to explain the factor 10 depletion from CDM » ?
arXiv:1005.2687: Constrained Local UniversE Simulations (CLUES)
Gottloeber, Hoffman , Yepes
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•"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)
“Evidence” for WDM ?
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•"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?
“Evidence” for WDM ?
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Before we get too depressed or excited
…
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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?
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Strong Reliance on N-body Strong Reliance on N-body simulationssimulations
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
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CDM Dark matter halo profilefrom 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 Einasto profile) 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.
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Ma Chung Pei, Chang, P., Zhang, 2009
Predict the two properties cannot hold at all scales
Einasto vs NFW
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Nature of dark matter or astrophysics process?
eg, Maschenko et al. 2006, Nature, or 2008, science, etc…
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SN feedback and Radiation pressure
answer 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.
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More faint or dark galaxies discovered
Eg, Belokurov et al, 2010
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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
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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
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Cosmic shear power spectra Markovic et al. 2010 Euclid-like DE space survey +Planck:
Integral effects → better than matter power spectrum
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Sensitive to m_WDM < 2.5 keV
Cosmic shear power spectra Markovic et al. 2010 Euclid-like DE space survey
+Planck:
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Power spectra and sensitivity to WDM
Is that interesting ? Lyman constraints m > 2 or 4 keV or even higher – But doubts on Lyresults!
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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
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Baryon effects different from neutrino or WDM effects
Semboloni et al. 2011
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Mandelbaum et al. (2006)
Stacked galaxy—galaxy weak lensing signal fit with various profiles.
CL0024
Tyson, Kochanski, & Dell’Antonio (1998)
Probing DM Particle properties
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Galaxy-galaxy lensing
Measure the correlation of shear of the background galaxies with mass of the foreground galaxies
To obtain the galaxy-galaxy lensing signal, we need two important ingredients that we can extract from the data
1)the redshift distribution of the lensed background galaxies
2)the shape of the lensed background galaxies
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Surface density profile measurements obtained from galaxy groups
in the COSMOS survey Leauthaud et al. 2010
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Magnification (Van Waerbeke et al. 2010)
An alternative way to determine the galaxy profile, especially for the high redshift galaxies (z>=1).
- Need: precise photometry (but not shape)
- Measure: number density of galaxies
-Noise:
1. Poisson noise
2. galaxy clustering
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Conclusions• Astrophysical observations existence of non baryonic
Dark Matter
• N-Body simulations of LSS existence of not-hot DM?
• Many problems with CDM simulations
can be solved with O(1keV) WDM
- Or Baryon feedback ?
More work on N-body simulations needed !
-What can WDM be? Sterile neutrinos? -How can O(1keV) WDM be observed? Lensing , X-ray,…-How can massive CDM be observed: Direct and Indirect detection experiments + accelerator production of new particles…
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Thank You!