[standard] baryonic acoustic oscillations (bao), redshift ... · [standard] baryonic acoustic...

[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

+



3 methods

...less standard clustering measurements

Baryonic Acoustic Oscillations:

Redshift Space Distortions:


3 methods




log P(k)/Psmooth

SDSS DR7

kBAO ~ 2!/rBAO

! standard ruler at zsurvey:

rBAO, =∆z

H(z)DE

rBAO,⊥ = ∆θ DA(z)DE


3 methods




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

"


rBAO, =∆z

H(z)DE



3 methods




log P(k)/Psmooth

SDSS DR7

kBAO ~ 2!/rBAO

Φ = −GNM

re−r/rls with rls =

mc

Φ = −GNM


mc



virialized motion

"


rBAO, =∆z

H(z)DE



3 methods



global geometry and topology of LSS:volume, surface, mean curvature, Euler characteristic (genus) ! planarity, filamentarity, ...


log P(k)/Psmooth

SDSS DR7

kBAO ~ 2!/rBAO

Φ = −GNM


mc

Φ = −GNM


mc



virialized motion

"


rBAO, =∆z

H(z)DE


: Minkowski functionals

homogeneity scale # “averaging problem”, Cosmological Principle


Redshift surveys: a useful classification

eBOSS

BigBOSS

EuclidPFS

..

BAO

gala

xy e

volu

tion

RSD

weak lensing

?HETDEX

6 (>Aug 2014)


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


BAO


BAO @ SDSS-III/BOSS [CMASS]

DR7Padmanabhan+ 2012

Reid+ 2013

Kazin+ 2012Sanchez+ 2013

0 < µ < 0.5:

0.5 < µ < 1:

10%

5%

ΔwDE @ 20%


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


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


RSD


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


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



"CDM ±10%σβ

β≈ C

V 0.5b0.7 exp

B

b4n2g



P (k, µ) = b2gal

(1 + βµ2)2


mat (k), β ≡ f


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





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



"CDM ±10%σβ

β≈ C

V 0.5b0.7 exp

B

b4n2g



P (k, µ) = b2gal

(1 + βµ2)2


mat (k), β ≡ f


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






0.5 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



"CDM ±10%σβ

β≈ C

V 0.5b0.7 exp

B

b4n2g



P (k, µ) = b2gal

(1 + βµ2)2


mat (k), β ≡ f


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








"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


mat (k), β ≡ f


bgal



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



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


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:


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


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


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


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


V 2h1 M

pc

mean curvature


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


V 0h3 M

pc3

volume

0 5 10 15 200

200

400

600

800


V 1h2 M

pc2

surface

0 5 10 15 200

5

10

15

20

25


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


Conclusion

eBOSS

BigBOSS

EuclidPFS

ngCFHT

BAO

gala

xy e

volu

tion

RSD

weak lensing

?HETDEX

(definitely a useful classification)

[standard] baryonic acoustic oscillations (bao), redshift ... · [standard] baryonic acoustic...

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