astroparticle physics in intergalactic space matteo viel – inaf trieste
DESCRIPTION
Astroparticle Physics in Intergalactic Space Matteo Viel – INAF Trieste APP14 – Amsterdam, 24 th June 2014. OUTLINE . INTRO: the Intergalactic Medium and its main manifestation: the Lyman- a forest QUANTITATIVE CONSTRAINTS: neutrinos and warm dark matter - PowerPoint PPT PresentationTRANSCRIPT
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Astroparticle Physics in Intergalactic
Space
Matteo Viel – INAF TriesteAPP14 – Amsterdam, 24th June 2014
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OUTLINE
INTRO: the Intergalactic Medium and its main manifestation: the Lyman-a forest
QUANTITATIVE CONSTRAINTS: neutrinos and warm dark matter
TOOLS: beyond linear theory with N-body/hydrodynamic simulations
DATA: state-of-the-art observables at high and low resolution (BOSS and UVES spectra)
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INTRO
- why atomic physics is important for intergalactic space- baryons in intergalactic space are diffuse/low density- physics of the IGM is relatively simple (at least at large scales)
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Lyman-a absorption is the main manifestation of the IGM
Tiny neutral hydrogen fraction after reionization…. But large cross-section
The Lyman-a forest
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80 % of the baryons at z=3 are in the Lyman-a forest
baryons as tracer of the dark matter density field
d IGM ~ d DM at scales larger than the
Jeans length ~ 1 com Mpc t ~ (dIGM )1.6 T -0.7
Bi & Davidsen (1997), Rauch (1998)Review by Meiksin (2009)
The Intergalactic Medium: Theory vs. Observations
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Dark matter evolution: linear theory of density perturbation + Jeans length LJ ~ sqrt(T/r) + mildly non linear evolution
Hydrodynamic processes: mainly gas cooling cooling by adiabatic expansion of the universe heating of gaseous structures (reionization)
- photoionization by a uniform Ultraviolet Background - Hydrostatic equilibrium of gas clouds dynamical time = 1/sqrt(G r) ~ sound crossing time= size /gas sound speed
In practice, since the process is mildly non linear you need numerical simulationsTo get convergence of the simulated flux at the percent level (observed)
Size of the cloud: > 100 kpcTemperature: ~ 104 KMass in the cloud: ~ 109 MNeutral hydrogen fraction: 10-5
Modelling the IGM: Physics
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DATA vs THEORY
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DATA vs THEORY P FLUX (k,z) = bias2 (k,z) x P MATTER (k,z)
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DATA vs THEORY
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END OF INTRO
We have characterized the physics of the IGM and we can now fully exploit the fact that:
The IGM is a probe of matter fluctuations and geometry,a laboratory for fundamental physics,a sink (and a reservoir) for (of) galactic baryons
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SDSS- III/BOSS: Dynamics
1D Lyman-a flux power
Palanque-Delabrouille et al. 2013
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SDSS-III/BOSS: Geometry
New regime to be probed with Lyman-a forest in 3D
Slosar et al. 11Busca et al. 13Slosar et al. 13
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SDSS- III
Font-Ribera et al. 2013
3D cross-correlation between Lyman-a flux and quasars
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TO RECAP: WHY LYMAN-a?
1) ONE DIMENSIONAL
2) AND ALSO THREE DIMENSIONAL
3) HIGH REDSHIFT
e.g. Kaiser & Peacock 91
Where you are possibly closer to primordial P(k)
…unfortunately non-linearities and thermal state of the IGM are quite important….
e.g. Viel et al. 02
1D cross spectrum
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CONSTRAINTS ON COSMOLOGICAL NEUTRINOS
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COSMOLOGICAL NEUTRINOS - I: WHAT TO START FROM
COSMOLOGY
constraints on the sum of the neutrino masses
Lesgourgues & Pastor 06
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COSMOLOGICAL NEUTRINOS - II: FREE-STREAMING SCALE
RADIATION ERA z>3400
MATTER RADIATION z<3400
NON-RELATIVISTIC TRANSITION z ~ 500
Neutrino thermalvelocity
Neutrino free-streaming scale Scale of non-relativistic transition
Below knr there is suppression in power at scales that are cosmologically important
THREECOSMICEPOCHS
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COSMOLOGICAL NEUTRINOS - III: LINEAR MATTER POWER
CMB GALAXIES IGM/WEAK LENSING/CLUSTERS
Lesgourgues & Pastor 06
Incr
easin
g ne
utrin
o m
ass
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MASSIVE NEUTRINOS
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COSMOLOGICAL NEUTRINOS : NON-LINEAR MATTER POWER
Bird, Viel, Haehnelt (2012)
P m
assi
ve /
P m
assl
ess
LINEAR THEORY
NON-LINEARNAÏVE EXTENSIONOF LINEAR THEORY
Cosmic Scale
20% more suppression than in linear case, redshift and scale
dependent. FEATURE!!!
http://www.sns.ias.edu/~spb/index.php?p=code
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Xia, Granett, Viel, Bird, Guzzo+ 2012 JCAP, 06, 010
CONSTRAINTS on NEUTRINO MASSES USING NON-LINEARITIES
If using just linear 0.43eV – Improvement is about 20% when extending to non-linear
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NEUTRINOS IN THE IGM
SIMULATIONS
DATA
CONSTRAINTS
Viel, Haehnelt, Springel 2010
Sm n<0.9 eV(2s)
FROM IGM ONLY:
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Sm n<0.93 eV(2s) Costanzi+ 2014
CONSTRAINTS on NEUTRINO MASSES FROM Planck: I
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Sm n<0.24 eV(2s) Costanzi+ 2014
CONSTRAINTS on NEUTRINO MASSES FROM Planck+BAO: II
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Sm n<0.14 eV(2s) Costanzi+ 2014
CONSTRAINTS on NEUTRINO MASSES FROM Planck+BAO+old Lya: III
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THE COLDNESS OF COLD DARK MATTER
Viel, Becker, Bolton, Haehnelt, 2013, PRD, 88, 043502
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THE COSMIC WEB in WDM/LCDM scenarios
z=0
z=2
z=5
Viel, Markovic, Baldi & Weller 2013
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THE WARM DARK MATTER CUTOFF IN THE MATTER DISTRIBUTION
Linear cutoff for WDM 2 keV
Linear cutoff is redshift independent
Fit to the non-linear cut-off
Viel, Markovic, Baldi & Weller 2013
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HISTORY OF WDM LYMAN-a BOUNDS
Narayanan et al.00 : m > 0.75 keV Nbody sims + 8 Keck spectra Marginalization over nuisance not done
Viel et al. 05 : m > 0.55 keV (2s) Hydro sims + 30 UVES/VLT spectra Effective bias method of Croft et al.02
Seljak et al. 06 : m > 2.5 keV (2s) Hydro Particle Mesh method + SDSSgrid of simulation for likelihood
Viel et al. 06 : m > 2 keV (2s) Fully hydro+SDSS Not full grid of sims. but Taylor expans.
Viel et al. 08 : m > 4.5 keV (2s) SDSS+HIRES (55 QSOs spectra)Full hydro sims (Taylor expansion ofthe flux)
Boyarsky et al. 09 : m>2.2 keV (2s) SDSS (frequentist+bayesian analysis) emphasis on mixed ColdWarmDM
models
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DARK MATTER DISTRIBUTION
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GAS DISTRIBUTION
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HI DISTRIBUTION
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“Warm Dark Matter as a solution to the small scale crisis: new constraints from high redshift Lyman-α forest data” MV+ arXiv:1306.2314
DATA: 25 high resolution QSO spectra at 4.48<zem<6.42 from MIKE and HIRES spectrographs. Becker+ 2011
SIMULATIONS: Gadget-III runs: 20 and 60 Mpc/h and (5123,7863,8963)
Cosmology parameters: s8, ns, Wm, H0, mWDM
Astrophysical parameters: zreio, UV fluctuations, T0, g, <F>Nuisance: resolution, S/N, metals
METHOD: Monte Carlo Markov Chains likelihood estimator + very conservative assumptions for the continuum fitting and error bars on the data
Parameter space: mWDM, T0, g, <F> explored fullyParameter space: : s8, ns, Wm, H0, UV explored with second orderTaylor expansion of the flux power
+ second order
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THE HIGH REDSHIFT WDM CUTOFFd F = F/<F>-1
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RESULTS FOR WDM MASS
m > 3.3 keV (2s)
EXCLUDED
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SDSS + MIKE + HIRES CONSTRAINTS
Joint likelihood analysis
SDSS data from McDonald05,06 not BOSS
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M thermal WDM > 3.3 keV (2s C.L.)
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CONSTRAINTS FROM SDSS DATA ON COLD+WARM DM MODELS
Boyarsky, Ruchayasky, Lesguorgues, Viel, 2009, JCAP, 05, 012
mthermal 2keV 1keV
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CONCLUSIONS - NEUTRINOS
Neutrino non-linearities modelled in the matter power spectrum. correlation function, density distribution of haloes, peculiar velocities, redshift space distortions. NEW REGIME!
Galaxy clustering data give <0.3 eV (2s upper limit). IGM still the most constraining probe <0.14-17 eV to be checked soon
Forecasting for Euclid survey: 14 meV error is doable but need to model the power spectrum to higher precision (possibly subpercent) and with physical input on the scale dependence of the effect.Very conservative 20-30 meV
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CONCLUSIONS – WARM DARK MATTER
High redshift Lyman-a disfavours thermal relic models with masses that are typically chosen to solve the small-scale crisis of LCDM
Models with 1 keV are ruled out at 9s 2 keV are ruled out at 4s 2.5 keV are ruled out at 3s 3.3 keV are ruled out at 2s
1) free-streaming scale is 2x108M/h 2) at scales k=10 h/Mpc you cannot suppress
more than 10% compared to LCDM
Of course they remain viable candidate for the Dark Matter (especiallysterile neutrinos) but in terms of structure formation nearly indistinguishable from CDM
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