pierros ntelis phd advisor: j.c. hamilton...
TRANSCRIPT
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Homogeneity Scale of the Universe
Pierros Ntelis!PhD advisor: J.C. Hamilton!
APC
24 March 2016
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
OUTLINE
Theoretical Framework BOSS Galaxy Survey Method of Measurement Results with DR12 Conclusion & Outlook
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
Theoretical Framework
General Relativity!
ΛCDM - model!best fit on data
Friedman Equations!Dynamics of the Universe
Cosmological Principle! Homogeneity + Isotropy!in large scale structures
Consolidation !Main Pillars of !
modern Cosmology
�T
T⇠ 10�5
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
SDSS-III / BOSS!! Main project:
APO telescope (New Mexico, USA) 2.5 m diameter
Spectroscopic Survey: 360 nm < λ < 1000 nm FoV: 10 400 :
Objectives: Galaxy Clustering Science Cosmological Parameters
How to check for Homogeneity ?
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
BOSS in a Nutshell
PLUGUE Al PLATE
1000 x SPECTRO!METER
SPECTROSCOPY
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
Uniform Galaxy Sample
[S.Alam et al. 1501.00963]
Intrinsically Uniform Sample !
z-Cut ~ dperp-cut 0.43 < z <0.7
i mag-Cut faint-bright limits
passively evolving gals constant-stellar mass ! ! BOSS DR12 CMASS Sample
NGC
SGCDR12
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
Observable ?
Which range to measure?
Account for RSD ?
Theory? !ΛCDM, !wCDM, !sCDM, !Modified Grav
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
DR12 BOSS # Objects: 786950 Large Volume
!Precision 1%Veff = (5.1 + 2.3)h�3Gpc3
WiggleZ Collaboration # Objects: 225297 Small Volume
!Precision 5%Veff ' 1h�3Gpc3
Comparison Statistics
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
Count-in-Spheres
Select a galaxy as a center !
Create a sphere of radius r!!
Compute number of galaxies !
repeat for every galaxy !
compute the mean N(r)!!
repeat for different scales
How to measure density
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
Homogeneous: ! @ large scales!!!!
Inhomogeneous : @ small scales (clustering)
!!
Transition to Homogeneity at: !! Arbitrary Choice
D2(r) =d ln N(< r)
d ln r= 3
D2(r) < 3
Homogeneity Scale Estimator
N(< r) / r3
D2(RH) = 3 @ 1%
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
Matter-Observable Conversion
Theory Dth2 (r)
Dth2 (r)
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
Theory
Simulated galaxy distribution
!
Dth2 (r)
Dgal2 (r; b)
Dth2 (r)
Dgal2 (r; b)
Matter-Observable Conversion
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
Theory
Simulated galaxy distribution
Convert to
!
Dth2 (r)
Dgal2 (r; b)
DMM2 (r; b)
Dgal2 (r; b)
Dth2 (r)
DMM2 (r; b)
Matter-Observable Conversion
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
Theory
Simulated galaxy distribution
Convert to
3 diff Distributions
Need to account for bias
Dth2 (r)
Dgal2 (r; b)
DMM2 (r; b)
Dth2 (r)
DMM2 (r; b)
Matter-Observable Conversion
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
RSD Analysis
Determination: bias, peculiar velocities
Kaiser @ r>10Mpc/h FoG @ r<10Mpc/h
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
Determination: bias, peculiar velocities
Kaiser @ r>10Mpc/h FoG @ r<10Mpc/h Fitting choices according to QPM
RSD Analysis
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
Determination: bias, peculiar velocities
Kaiser @ r>10Mpc/h FoG @ r<10Mpc/h Fitting choices according to QPM
r < 40h�1Mpc
RSD Analysis
Theoretical Model CLASS soft (+Halofit)
⇠(r; b,�p) = FRSD(r; b,�p)⌦ ⇠M (r)
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
Determination: bias, peculiar velocities
Kaiser @ r>10Mpc/h FoG @ r<10Mpc/h Fitting choices according to QPM
Theoretical Model CLASS soft (+Halofit)
r < 40h�1Mpc
RSD Analysis
⇠(r; b,�p) = FRSD(r; b,�p)⌦ ⇠M (r)
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
⇢⇠ij
Determination: bias, peculiar velocities
Kaiser @ r>10Mpc/h FoG @ r<10Mpc/h Fitting choices according to QPM
Theoretical Model CLASS soft (+Halofit)
RSD Analysis
⇠(r; b,�p) = FRSD(r; b,�p)⌦ ⇠M (r)
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
Results
r > 40h�1Mpc
Well Distinct Fitting Space increases with scaleD2
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
Results
Well Distinct Fitting Space increases with scale Cosmological Principle confirmed:
DR12 DATA
D2
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
Results
Well Distinct Fitting Space increases with scale Cosmological Principle confirmed:
DR12 DATA 1000 QPM-ΛCDM
D2
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
Results
Well Distinct Fitting Space increases with scale Cosmological Principle confirmed:
DR12 DATA 1000 QPM-ΛCDM ΛCDM PLANCK 2015
D2
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
Redshift Evolution of !
Confirmation of ΛCDM model !
HomoScale is with time
RH
Results
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
Conclusion
Main Features: Largest Volume ever studied at z~0.5 Precision of measurement ~1% ( Wz ~5% ) Easy application on different surveys High Robustness Through Mocks Tests
General limitations of these studies: Insensitive to radial density dependence Distance calculation assumes ΛCDM RSD Analysis assumes ΛCDM
!Consistency test of ΛCDM at %-level Validation of Cosmological Principle
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
Outlook
!Study alternative estimators
!Predictions for future projects
(EUCLID, LSST) !
Use as Cosmological Standard Ruler Cosmological Parameters Nature of Dark Energy!Acceleration of the Universe
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
Thank You Very Much !
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
Mock Galaxies Catalogues
Basic Method!Predict evolution of mass field Identify DM halos Populate Halos with Galaxies Apply survey characteristics
!Analysis Usage!
Compute Covariance Matrices Use in Analysis Tests !ref: 1309.5532v2, 1203.6609v2
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
Optimal Homogeneity Estimators
2pt-Correlation function: Landy Szalay Estimator !!!
Average number galaxy density !!!
Convert to Matter-distribution estimator !!!
Fractal Correlation dimension
⇠ls(s) =DD(s)� 2 ⇤DR(s) +RR(s)
RR(s)
N (< r) = 1 +3
r3
Z r
0⇠(s)s2ds
NM (< r) =N th
M (< r)� 1
N thb,�p
(< r)� 1[N (< r)� 1] + 1
DM2 (r) =
d ln NM (< r)
d ln r+ 3
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
Analysis Null tests
measurement on mocks !! Spline fitting !!
2 ndf
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
Analysis Null tests
measurement on mocks !! Spline fitting !!CDF [�2
mock
]
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
Analysis Null tests
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
Un-Correlated
eff0.0 north 1000 qpm factor: correcting for inv cov
z2
1000 QPMs
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
Correlation Matrices
⇢D2ij
⇢Nij
⇢⇠ij
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
Correlation Matrices
⇢⇠ij
⇢Nij
⇢D2ij
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
Cosmology independence
D2(r) =d ln N (< r)
d ln r! D2(↵r) =
d ln N (< ↵r)
d ln r
↵ =dmodel
(zm
)
dfiducial
(zm
)DA(z) =
c
H0
p|⌦k|
Z z
0
dz0
H(z0)
d(z) =
D2
Acz
H(z)
�1/3
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
RSD-choices
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
RSD-choices
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
RSD-choices
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
Uniform Galaxy Data Sample
Uniform Sample in Redshift !
christy tremonti 2009
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
Uniform Sample in Redshift !
z-Cut ~ dperp-cut 0.43 < z <0.7
christy tremonti 2009
z-high
z-low
Uniform Galaxy Data Sample
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
Uniform Sample in Redshift !
z-Cut ~ dperp-cut 0.43 < z <0.7
i mag-Cut faint-bright limits
christy tremonti 2009
Uniform Galaxy Data Sample
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
Uniform Sample in Redshift !
z-Cut ~ dperp-cut 0.43 < z <0.7
i mag-Cut faint-bright limits
passively evolving gals constant-stellar mass !! Best BOSS CMASS Sample
christy tremonti 2009
Uniform Galaxy Data Sample
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
Systematic Effects
Rarely 100%: Survey in progress Non-uniform success rate
!Definition:
!!
Importants Weights for: Closed Pairs z-failure Contamination from Stars Shot-noise, Cosmic Variance
- [Feldman, Kaiser, Peacock,1993] wtot
= (wcp
+ wzf
� 1)wsys
wfkp
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
!Landy Szalay Estimator
!!!
Average number galaxy density !!!
Fractal Correlation dimension
⇠ls(s) =DD(s)� 2 ⇤DR(s) +RR(s)
RR(s)
N (< r) = 1 +3
r3
Z r
0⇠(s)s2ds
D2(r) =d ln N (< r)
d ln r+ 3
Optimal Homogeneity Estimator
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
Results
pull(r) =d2(r)� dth2 (r)
�d2(r)
REMOVE IF NOT BETTER WITH ALL POINTS
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Homogeneity Scale of the UniverseP.Ntelis, March 2016
COMPARE RESULTS
Redshift Evolution of !
Confirmation of ΛCDM model !
HomoScale is with time
RH
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Homogeneity Scale of the UniverseP.Ntelis, March 2016