New LiciaVerde% ICREA%&%ICC0UB% hp:// icc.ub.edu/~liciaverde% · 2012. 4. 3. · LSSTinnumbers •...
Transcript of New LiciaVerde% ICREA%&%ICC0UB% hp:// icc.ub.edu/~liciaverde% · 2012. 4. 3. · LSSTinnumbers •...
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LSS in LSST
Licia Verde ICREA & ICC-‐UB
h4p://icc.ub.edu/~liciaverde
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LSST in numbers • EffecDve etendue 319 m2deg2 • FoV 9.9 deg2 • EffecDve aperture 6.7m • Wavelength coverage 320-‐1080 nm, filters u g r I z y • Sky coverage 20,000 sq deg • Single visit depth r ~ 24.5 (5 σ point source) • Seeing 0.7 arcsec in r • Each patch of the sky observed 2000 Dmes (15s-‐days) 1000 visits
• Photometric repeatability 5-‐10 millimags • Astrometric precision be4er than 10 mas (rsm) per visit per coord see e.g., LSST science book at h4p://arxiv.org/abs/0912.0201 or h4p://www.lsst.org/lsst/scibook
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chapters
Solar system, milky way, the variable Universe (TIME DOMAIN), galaxies and cosmology
``The LSST survey data will be public with no proprietary period in the United States with a goal to make it world public”
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Large survey volume
Recall that e.g., error on the Power spectrum is oc 1/(Veff)1/2 and kmin oc 1/V 1/3
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Primordial fluctuaDons and constraints on inflaDon
Yes, it can also do (angular) BAO…
InflaDon solves the flatness/horizon/structure problems
Cosmological perturbaDons arise from quantum fluctuaDons, evolve classically
We do not know the dynamics of inflaDon: parameterize weakly scale dependent funcDons with few numbers to constrain observaDonally
V(φ)à P(k)
P�(k) = ~✓H
2⇡
◆2
PR(k) '~
4⇡2
✓H4
�̇2
◆2
k=aH
Scalar
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Where useful?
Models of slow roll inflaDon: ``only” improve errors by factor of ~2 compared to Planck
Key gain is for models with Features on large scales
Fig from Zhang et al (2006)
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Primordial non-‐Gaussianity from halo bias • Gaussian IC and a non-‐Gaussian IC can have the same P(k) for the dark ma4er
• For Gaussian IC the P(k) of massive halos is completely specified by the dark ma4er P(k)
• For Non Gaussian IC, however, the P(k) of the halos, depends on all higher order correlaDons (i.e. fNL)
For Gaussian fields high peaks (halos) are approx. linearly biased in a scale independent way wrt the dark ma4er (Kaiser result)
For non-‐Gaussian fields bias will not be linear, scale independent
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Non-‐Gaussian halo bias and bispectrum shapes
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Non-‐Gaussian halo bias and bispectrum shapes
Matarrese, Verde 08 Verde, Matarrese 09 Taruya et al 08
Wagner & Verde, 2012
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The effect and forecasted errors local shape
Carbone, Verde, Matarrese 08 Carbone, Mena Verde, ‘10
�fNL ⇠ 0.7 (1� �)
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Verde & Matarrese 2009, ApJL On horizon-‐scales Poisson equaDon gets quadraDc correcDons: Needs IC set up of inflaDon, parallels the TE anD-‐correlaDon.
InflaDonary-‐GR Intrinsic to LSS
At a potenDally detectable level!
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Neutrino properDes • OscillaDons indicate neutrinos have mass:
• Three possible hierarchies
• Physics beyond the standard model! • The standard model has 3 neutrino species, but…
Neutrino mass eigenstates are not the same as flavor
NORMAL INVERTED DEGENERATE
Δmatmo
Δmsol Δmatmo
Δmsol
Total v mass increases
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Cosmology is key in determining the absolute mass scale
Inverted
normal
degenerate
The problem is systemaDc errors
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Physical effects Total mass >~1 eV become non relaDvisDc before recombinaDon CMB
Total mass
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LSST lensing + Planck CMB
Constraints use linear theory; non-‐lineariDes enhance the effect
1σ errors
PL LCDM
Running, w w’
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Evidence for more than 3 neutrinos LSST+Planck
inconclusive
strong
decisive
substanDal
Sterile neutrinos, but any type of “dark radiaDon” Adapted from Kitching et al 2007
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Dirac or Majorana? hierarchy
Jimenez, Kitching, Penya-‐Garay, Verde, arXiv:1003:5918
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Hierarchy effect on the shape of the power spectrum
Δmatmo
Δmsol Δmatmo
Δmsol
NH IH Δ
Neutrinos of different masses have different transition redshifts from relativistic to non-relativistic behavior, and their individual masses and their mass splitting change the details of the radiation-domination to matter- domination regime."
Jimenez, Kitching, Penya-‐Garay, Verde, JACP2010
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Hierarchy effect on the shape of the power spectrum
Δmatmo
Δmsol Δmatmo
Δmsol
NH IH Δ
Neutrinos of different masses have different transition redshifts from relativistic to non-relativistic behavior, and their individual masses and their mass splitting change the details of the radiation-domination to matter- domination regime."
Wagner, Verde, Jimenez, 2012, arXiv:1203.5342
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Hierarchy effect on the shape of the power spectrum
A word of warning!
Jimenez, Kitching, Penya-‐Garay, Verde, JCAP 2010 arXiv:1003:5918
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Detectability?
Wagner, Verde, Jimenez, 2012, arXiv:1203.5342
Only LSS but fixing all other parameters!!!!
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Future surveys like LSST can help!
Jimenez, Kitching, Penya-‐Garay, Verde, arXiv:1003:5918
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TesDng gravity
Lensing only
γ≅0.55 In GR
Fig from Heavens et al. 2007
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Constraining cluster physics
Sealfon et al 2005
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Summary • A biased and incomplete overview of what LSST can do for LSS
• Large survey volume: access to large scales, many Fourier modes, depth in z
• Weak lensing: direct map to DM • Primordial Universe (inflaDon and non-‐Gaussianity); neutrino properDes, tesDng gravity(dark energy)