[standard] baryonic acoustic oscillations (bao), redshift ... · [standard] baryonic acoustic...
TRANSCRIPT
[standard]Baryonic Acoustic Oscillations (BAO),
Redshift Space Distortions (RSD),and some (renewed) ideas...
Carlo Schimd
on behalf of the Cosmology-Dark Energy WG:
Jean-Paul Kneib (EPFL Lausanne), Martin Makler (CBPF, Rio de Janeiro), Charling Tao (CPPM Marseille & Tsingua University), Keiichi Umetsu (ASIAA, Taiwan)
see Kendrick Smith’s talk (later in the afternoon)ngCFHT meeting
U of Hawaii at Hilo, March 27-30, 2013
dark energy:cosmological constant, quintessence, cosmon, k-essence, spintessence, generalized Chaplygin gas, ...
=
dark gravity:[superstring-inspired/justified]scalar-tensor and/or f(R) theories of gravity, 5D gravity, massive gravity, ...
=
=
inhomogeneous gravity:non-linear GR backreaction by matter inhomogeneities on average (“global”?) observables & dynamics, Swiss-Cheese models, non-trivial space-time topology, ...
General Relativityon large scales
Cosmological Principlehomogeneity & isotropy on
large scales
+
Baryons& Cold Dark Matter
+
ngCFHT meetingU of Hawaii at Hilo, March 27-30, 2013
dark energy:cosmological constant, quintessence, cosmon, k-essence, spintessence, generalized Chaplygin gas, ...
=
dark gravity:[superstring-inspired/justified]scalar-tensor and/or f(R) theories of gravity, 5D gravity, massive gravity, ...
=
=
inhomogeneous gravity:non-linear GR backreaction by matter inhomogeneities on average (“global”?) observables & dynamics, Swiss-Cheese models, non-trivial space-time topology, ...
BAO
RSD
and renewed ideas...
General Relativityon large scales
Cosmological Principlehomogeneity & isotropy on
large scales
+
Baryons& Cold Dark Matter
+
ngCFHT meetingU of Hawaii at Hilo, March 27-30, 2013
ngCFHT meetingU of Hawaii at Hilo, March 27-30, 2013
3 methods
...less standard clustering measurements
Baryonic Acoustic Oscillations:
Redshift Space Distortions:
ngCFHT meetingU of Hawaii at Hilo, March 27-30, 2013
3 methods
...less standard clustering measurements
Baryonic Acoustic Oscillations:
Redshift Space Distortions:
log P(k)/Psmooth
SDSS DR7
kBAO ~ 2!/rBAO
! standard ruler at zsurvey:
rBAO, =∆z
H(z)DE
rBAO,⊥ = ∆θ DA(z)DE
ngCFHT meetingU of Hawaii at Hilo, March 27-30, 2013
3 methods
...less standard clustering measurements
Baryonic Acoustic Oscillations:
Redshift Space Distortions:
log P(k)/Psmooth
SDSS DR7
kBAO ~ 2!/rBAO
∇2Φ∗f(r, t) = 4πGN ρ δ∇2Φ∗f(r, t) = 4πGN ρ δ
– Small separations on sky: ʻFinger-of-Godʼ;– Large separations on sky: flattening along line of sight
angular 2-PCF coherent flow
virialized motion
"
! standard ruler at zsurvey:
rBAO, =∆z
H(z)DE
rBAO,⊥ = ∆θ DA(z)DE
ngCFHT meetingU of Hawaii at Hilo, March 27-30, 2013
3 methods
...less standard clustering measurements
Baryonic Acoustic Oscillations:
Redshift Space Distortions:
log P(k)/Psmooth
SDSS DR7
kBAO ~ 2!/rBAO
Φ = −GNM
re−r/rls with rls =
mc
Φ = −GNM
re−r/rls with rls =
mc
– Small separations on sky: ʻFinger-of-Godʼ;– Large separations on sky: flattening along line of sight
angular 2-PCF coherent flow
virialized motion
"
! standard ruler at zsurvey:
rBAO, =∆z
H(z)DE
rBAO,⊥ = ∆θ DA(z)DE
ngCFHT meetingU of Hawaii at Hilo, March 27-30, 2013
3 methods
...less standard clustering measurements
Baryonic Acoustic Oscillations:
global geometry and topology of LSS:volume, surface, mean curvature, Euler characteristic (genus) ! planarity, filamentarity, ...
Redshift Space Distortions:
log P(k)/Psmooth
SDSS DR7
kBAO ~ 2!/rBAO
Φ = −GNM
re−r/rls with rls =
mc
Φ = −GNM
re−r/rls with rls =
mc
– Small separations on sky: ʻFinger-of-Godʼ;– Large separations on sky: flattening along line of sight
angular 2-PCF coherent flow
virialized motion
"
! standard ruler at zsurvey:
rBAO, =∆z
H(z)DE
rBAO,⊥ = ∆θ DA(z)DE
: Minkowski functionals
homogeneity scale # “averaging problem”, Cosmological Principle
ngCFHT meetingU of Hawaii at Hilo, March 27-30, 2013
Redshift surveys: a useful classification
eBOSS
BigBOSS
EuclidPFS
..
BAO
gala
xy e
volu
tion
RSD
weak lensing
?HETDEX
6 (>Aug 2014)
ngCFHT meetingU of Hawaii at Hilo, March 27-30, 2013
1÷10k class spectroscopic surveysngCFHT
(10)
1.5
1500-5000 (20000)could be HSC?
g,r,i < 24.5, +u (QSO)10,000 (QSO 3,000)
> 2000*8
10 (20-40) 1-2 (ELG) 3-6 (LAE)
< 2.2& 1.5-2.5 [OII] doubletif adding 1-1.3µm band
g < 22.3r < 23.5
0.2-0.8
240
ELG
19.910,000
25
VIPERS
since WiggleZ: ELG (Emission Line Galaxies): faint blue galaxies for which broadband colors are dominated by emission lines! Less biased than LRG (even though...) but more numerous at high redshift ! ok for DE studies!(~100 in SDSS-DR9/BOSS)
3,200
0,4 (0,28 LRG)
LRG (0.6 < z < 0.8) : 47+ deg-2 out of 50 targets, 7500 deg2
ELG (0.6 < z < 1.0) : 175+ deg -2 out of 230 targets, 1500 deg2
QSO (1 < z < 2.15) : !80+ deg -2 out of 90 targets to g < 22, 7500 deg2
LyA QSO (z > 2.15) : !5+ deg -2 out of 50 targets, 7500 deg2
*(VIPERS: 2170 deg-2)
3200-5000
1.7
MS-DESI
ngCFHT meetingU of Hawaii at Hilo, March 27-30, 2013
BAO
ngCFHT meetingU of Hawaii at Hilo, March 27-30, 2013
BAO @ SDSS-III/BOSS [CMASS]
DR7Padmanabhan+ 2012
Reid+ 2013
Kazin+ 2012Sanchez+ 2013
0 < µ < 0.5:
0.5 < µ < 1:
10%
5%
ΔwDE @ 20%
ngCFHT meetingU of Hawaii at Hilo, March 27-30, 2013
Baryonic Acoustic Oscillations: requirements
10000 deg2
8000 deg2
1500 deg2
0.0002 0.0004 0.0006 0.0008 0.0010
0.04
0.06
0.08
0.10
0.12
0.14
ng h3Mpc3
ΣPP
fractional error on power spectrum...
constant galactic bias
0.0002 0.0004 0.0006 0.0008 0.0010
0.02
0.04
0.06
0.08
0.10
ng h3Mpc3
ΣPP
... @ k = kBAO ~ 0.063 h Mpc-1 ... @ k = 2kBAO
evolving galactic bias (constant Ngal) but w/o halo history
σP
P= 2π
2
Vsurveyk2∆k∆µ
1 +
1nb2(z)P (k, z)
PFS
ngCFHT
ngCFHT meetingU of Hawaii at Hilo, March 27-30, 2013
Baryonic Acoustic Oscillations
0.5 1.0 1.5 2.01
2
3
4
5
6
redshift
ΣlnD A
0.5 1.0 1.5 2.02
4
6
8
10
12
redshift
ΣlnH
PFS-like (all ELG)
ngCFHT
LRG
ELG
evolving galactic bias (constant Ngal)
constant bias
angular diameter distance
Hubble parameter (radial distance)
CMB prior (WMAP)
+marginalization
0.6 0.8 1.0 1.2 1.4 1.6 1.8 2.00.010
0.005
0.000
0.005
0.010
redshift
K
0.6 0.8 1.0 1.2 1.4 1.6 1.8 2.03
2
1
0
1
2
3
redshift
Σln m
PFS-like
ngCFHTELG
ngCFHTLRG
0.6 0.8 1.0 1.2 1.4 1.6 1.8 2.01.10
1.05
1.00
0.95
0.90
redshift
w DE
ngCFHT meetingU of Hawaii at Hilo, March 27-30, 2013
RSD
ngCFHT meetingU of Hawaii at Hilo, March 27-30, 2013
RSD - the most recent measurements
De la Torre & VIPERS team, 2013
Blake &WiggleZ Team, 2011
VIPERSBOSS
Reid& BOSS team, 2012
0.5 1.0 1.5 2.00.20
0.25
0.30
0.35
0.40
0.45
0.50
0.55
0.60
redshift
fzΣ8z
ngCFHT meetingU of Hawaii at Hilo, March 27-30, 2013
Redshift Space Distortions (RSD)
"CDM ±10%σβ
β≈ C
V 0.5b0.7 exp
B
b4n2g
remark: volume limited subsamples
Fisher matrix approx
P (k, µ) = b2gal
(1 + βµ2)2
1 + (kσvµ)2P (lin)
mat (k), β ≡ f
bgal≈ [Ωm(z)]0.545+δ
bgal
VIPERS 24 deg2, Ng = 2170 deg-2
eBOSS (ELG only, 1500 deg2, Ng = 175 deg-2)*PFS-like (if all ELG! 1500 deg2, Ng = 1500 deg-2)
ngCFHT 8000 deg2, Ng = 1611 deg-2, 16M (ng = 20% smaller) (ELG: 637 deg-2, 6.3M; LAE: 974 deg-2, 9.7M [not shown])
ngCFHT 10000 deg-2, Ng = 2014 deg-2, 20M (optimal baseline) (ELG: 796 deg-2, 8M; LAE: 1218 deg-2, 12M [not shown])
*ngCFHT 10000 deg-2, Ng = 2014 deg-2, 20M; not evolving bias
0.5 1.0 1.5 2.00.20
0.25
0.30
0.35
0.40
0.45
0.50
0.55
0.60
redshift
fzΣ8z
ngCFHT meetingU of Hawaii at Hilo, March 27-30, 2013
Redshift Space Distortions (RSD)
"CDM ±10%σβ
β≈ C
V 0.5b0.7 exp
B
b4n2g
remark: volume limited subsamples
Fisher matrix approx
P (k, µ) = b2gal
(1 + βµ2)2
1 + (kσvµ)2P (lin)
mat (k), β ≡ f
bgal≈ [Ωm(z)]0.545+δ
bgal
0.5 1.0 1.5 2.00.20
0.25
0.30
0.35
0.40
0.45
0.50
0.55
0.60VIPERS 24 deg2, Ng = 2170 deg-2
eBOSS (ELG only, 1500 deg2, Ng = 175 deg-2)*PFS-like (if all ELG! 1500 deg2, Ng = 1500 deg-2)
ngCFHT 8000 deg2, Ng = 1611 deg-2, 16M (ng = 20% smaller) (ELG: 637 deg-2, 6.3M; LAE: 974 deg-2, 9.7M [not shown])
ngCFHT 10000 deg-2, Ng = 2014 deg-2, 20M (optimal baseline) (ELG: 796 deg-2, 8M; LAE: 1218 deg-2, 12M [not shown])
*ngCFHT 10000 deg-2, Ng = 2014 deg-2, 20M; not evolving bias
0.5 1.0 1.5 2.00.20
0.25
0.30
0.35
0.40
0.45
0.50
0.55
0.60
redshift
fzΣ8z
ngCFHT meetingU of Hawaii at Hilo, March 27-30, 2013
Redshift Space Distortions (RSD)
"CDM ±10%σβ
β≈ C
V 0.5b0.7 exp
B
b4n2g
remark: volume limited subsamples
Fisher matrix approx
P (k, µ) = b2gal
(1 + βµ2)2
1 + (kσvµ)2P (lin)
mat (k), β ≡ f
bgal≈ [Ωm(z)]0.545+δ
bgal
0.5 1.0 1.5 2.00.20
0.25
0.30
0.35
0.40
0.45
0.50
0.55
0.60
0.5 1.0 1.5 2.00.20
0.25
0.30
0.35
0.40
0.45
0.50
0.55
0.60VIPERS 24 deg2, Ng = 2170 deg-2
eBOSS (ELG only, 1500 deg2, Ng = 175 deg-2)*PFS-like (if all ELG! 1500 deg2, Ng = 1500 deg-2)
ngCFHT 8000 deg2, Ng = 1611 deg-2, 16M (ng = 20% smaller) (ELG: 637 deg-2, 6.3M; LAE: 974 deg-2, 9.7M [not shown])
ngCFHT 10000 deg-2, Ng = 2014 deg-2, 20M (optimal baseline) (ELG: 796 deg-2, 8M; LAE: 1218 deg-2, 12M [not shown])
*ngCFHT 10000 deg-2, Ng = 2014 deg-2, 20M; not evolving bias
0.5 1.0 1.5 2.00.20
0.25
0.30
0.35
0.40
0.45
0.50
0.55
0.60
redshift
fzΣ8z
ngCFHT meetingU of Hawaii at Hilo, March 27-30, 2013
Redshift Space Distortions (RSD)
"CDM ±10%σβ
β≈ C
V 0.5b0.7 exp
B
b4n2g
remark: volume limited subsamples
Fisher matrix approx
P (k, µ) = b2gal
(1 + βµ2)2
1 + (kσvµ)2P (lin)
mat (k), β ≡ f
bgal≈ [Ωm(z)]0.545+δ
bgal
ngCFHT
0.5 1.0 1.5 2.00.20
0.25
0.30
0.35
0.40
0.45
0.50
0.55
0.60
0.5 1.0 1.5 2.00.20
0.25
0.30
0.35
0.40
0.45
0.50
0.55
0.60
0.5 1.0 1.5 2.00.20
0.25
0.30
0.35
0.40
0.45
0.50
0.55
0.60VIPERS 24 deg2, Ng = 2170 deg-2
eBOSS (ELG only, 1500 deg2, Ng = 175 deg-2)*PFS-like (if all ELG! 1500 deg2, Ng = 1500 deg-2)
ngCFHT 8000 deg2, Ng = 1611 deg-2, 16M (ng = 20% smaller) (ELG: 637 deg-2, 6.3M; LAE: 974 deg-2, 9.7M [not shown])
ngCFHT 10000 deg-2, Ng = 2014 deg-2, 20M (optimal baseline) (ELG: 796 deg-2, 8M; LAE: 1218 deg-2, 12M [not shown])
*ngCFHT 10000 deg-2, Ng = 2014 deg-2, 20M; not evolving bias
ngCFHT meetingU of Hawaii at Hilo, March 27-30, 2013
Redshift Space Distortions (RSD)
"CDM ±10%
remark: volume limited subsamplesngCFHT w/ Lyman-A emitters
2 3 4 5 60.0
0.2
0.4
0.6
0.8
1.0Lyman-alpha emitters:
HETDEX 480 deg2, Ng = 1904 deg-2, 0.8M, z = 1.9 - 3.5
ngCFHT 8000 deg2, Ng = 974 deg-2, 9.7M(total: 1611 deg-2, 16M)
ngCFHT 10000 deg-2, Ng = 1218 deg-2, 12M, (optimal baseline)(total: 2014 deg-2, 20M)
P (k, µ) = b2gal
(1 + βµ2)2
1 + (kσvµ)2P (lin)
mat (k), β ≡ f
bgal≈ [Ωm(z)]0.545+δ
bgal
ngCFHT meetingU of Hawaii at Hilo, March 27-30, 2013
Redshift Space Distortions (RSD)
σβ
β≈ C
V 0.5b0.7 exp
B
b4n2g
WARNING!
1.0 1.5 2.0 2.5 3.0 3.5 4.00.005
0.010
0.015
0.020
0.025
linear bias
Σ ΒΒ10
00deg2
z = 0.6-2.1, ng = 10-3
z = 0.6-2.1, ng = 0.5!10-3
z = 0.6-2.1, ng = 0.2!10-3
z = 1.0-2.1, ng = 10-3
δgal ≈ b δmat
"CDM ±10%
VIPERSeBOSS - ELG*PFS-like - all ELG
ngCFHTngCFHT*ngCFHT
0.5 1.0 1.5 2.00.20
0.25
0.30
0.35
0.40
0.45
0.50
0.55
0.60
redshift
fzΣ8z
0.5 1.0 1.5 2.00.20
0.25
0.30
0.35
0.40
0.45
0.50
0.55
0.60
0.5 1.0 1.5 2.00.20
0.25
0.30
0.35
0.40
0.45
0.50
0.55
0.60
0.5 1.0 1.5 2.00.20
0.25
0.30
0.35
0.40
0.45
0.50
0.55
0.60
ngCFHT meetingU of Hawaii at Hilo, March 27-30, 2013
Redshift Space Distortions (RSD)
σβ
β≈ C
V 0.5b0.7 exp
B
b4n2g
WARNING!
1.0 1.5 2.0 2.5 3.0 3.5 4.00.005
0.010
0.015
0.020
0.025
linear bias
Σ ΒΒ10
00deg2
1.0 1.5 2.0 2.5 3.0 3.5 4.00.005
0.010
0.015
0.020
0.025
z = 0.6-2.1, ng = 10-3
z = 0.6-2.1, ng = 0.5!10-3
z = 0.6-2.1, ng = 0.2!10-3
z = 1.0-2.1, ng = 10-3
HETDEX
PFS
ngCFHT
δgal ≈ b δmat
"CDM ±10%
VIPERSeBOSS - ELG*PFS-like - all ELG
ngCFHTngCFHT*ngCFHT
0.5 1.0 1.5 2.00.20
0.25
0.30
0.35
0.40
0.45
0.50
0.55
0.60
redshift
fzΣ8z
0.5 1.0 1.5 2.00.20
0.25
0.30
0.35
0.40
0.45
0.50
0.55
0.60
0.5 1.0 1.5 2.00.20
0.25
0.30
0.35
0.40
0.45
0.50
0.55
0.60
0.5 1.0 1.5 2.00.20
0.25
0.30
0.35
0.40
0.45
0.50
0.55
0.60
ngCFHT meetingU of Hawaii at Hilo, March 27-30, 2013
0. full-shape of 2-PCF
Advanced/more recent techniques:
1. clustering/RSD + weak-lensing (Cai & Bernstein 2011)
2. clustering w/ cross-correlation between different galaxy types (McDonald & Seljak 2009)
3. BAO in Lyman-α forest (McDonald 2003; White 2003; ...)
4. BAO reconstruction (reverse engineering) (Padmanabhan 2012)
Kendrick Smith’s talk?
to investigate (and fix) bias, degeneracies, systematics:
ngCFHT meetingU of Hawaii at Hilo, March 27-30, 2013
Weak-lensing + (angular) clustering
Comparat, Jullo, Kneib, Schimd et al. 2013, submitted
zCOSMOS 10kVVDS
DEEP2
@Stripe 82:BOSS-ELG (clustering)+ CFHT-Stripe 82 (lensing)
photo-z only
ngCFHT meetingU of Hawaii at Hilo, March 27-30, 2013
volume - v0
number density
area - v1
integral mean curvature - v2
radius [h-1Mpc]
Euler characteristic - v3
radius [h-1Mpc]
larger volume connected
DR3
DR7
disjointvoids (super)clusters
“shift”
Clustering by Minkowski functionalsChoi+ 2010
SDSS-DR7
ngCFHT meetingU of Hawaii at Hilo, March 27-30, 2013
Clustering by Minkowski functionals- integral properties of matter distribution (unlike n-PCF, which probe differential p.)- precision cosmology (see fig)- scale of homogeneity- luminosity (e.g. galaxy) bias (SDSS DR7)
0 5 10 15 200
5000
10000
15000
20000
25000
30000
radius of sphere h1 Mpc
V 0h3 M
pc3
volume
0 5 10 15 200
200
400
600
800
radius of sphere h1 Mpc
V 1h2 M
pc2
surface
0 5 10 15 201.0
0.5
0.0
0.5
1.0
radius of sphere h1 MpcV 3
Euler characteristic
Poisson (unclustered)Gauss-Poisson (WMAP7)tiny (!) variation ~neutrino
0 5 10 15 200
5
10
15
20
25
radius of sphere h1 Mpc
V 2h1 M
pc
mean curvature
ngCFHT meetingU of Hawaii at Hilo, March 27-30, 2013
Clustering by Minkowski functionals- integral properties of matter distribution (unlike n-PCF, which probe differential p.)- precision cosmology (see fig)- scale of homogeneity- luminosity (e.g. galaxy) bias (SDSS DR7)
0 5 10 15 200
5000
10000
15000
20000
25000
30000
radius of sphere h1 Mpc
V 0h3 M
pc3
volume
0 5 10 15 200
200
400
600
800
radius of sphere h1 Mpc
V 1h2 M
pc2
surface
0 5 10 15 200
5
10
15
20
25
radius of sphere h1 Mpc
V 2h3 M
pc3
mean curvature
0 5 10 15 201.0
0.5
0.0
0.5
1.0
radius of sphere h1 MpcV 3
Euler characteristic
Poisson (unclustered)Gauss-Poisson (WMAP7)tiny (!) variation ~neutrino
ngCFHT meetingU of Hawaii at Hilo, March 27-30, 2013
Conclusion
eBOSS
BigBOSS
EuclidPFS
ngCFHT
BAO
gala
xy e
volu
tion
RSD
weak lensing
?HETDEX
(definitely a useful classification)