Results from the Baryon Oscillation Spectroscopic bccp. Reid for SDSS-III/BOSS collaboration Hubble...

Beth Reid for SDSS-III/BOSS collaborationHubble Fellow
Lawrence Berkeley National Lab
Results from the Baryon Oscillation Spectroscopic Survey (BOSS)
Thursday, January 19, 2012

Outline
No Ly- forest here, but very exciting!! (Slosar et al., arXiv:1104.5244)
Quick theory review -- what are we measuring?
Imaging Survey/Science from 2D maps Spectroscopic Survey/Science in 3D maps

Galaxy clustering lightning theory review
Theory 1: underlying matter power spectrum (determined at z >~ zCMB, neglecting )
Theory II: Expansion history H(0 < z < zGAL)

CMB predicts linear P(k) / (r)
Primordial perturbations
Horizon size at matter-radiation equality ~ mh2
Sound horizon at decoupling(BAO scale)
x
x
x
Arb
itrar
y sc
alin
g fr
om
unkn
own
gala
xy b
ias
P(k)
r2 (r)

Theory I: gastrophysics
Non-linear growth galaxy biasing redshift space distortions These can be dealt with, but do your
homework!

Theory II: geometry
We measure , , and z for each galaxy, and use a cosmological model to convert to comoving coordinates
z1 z2
(z) (or DA(z))
1/H(z)

Theory II: Alcock-Paczynski
(z) =0z c dz/H(z)
20 40 60 80 100 120 140 160 180
20
40
60
80
100
120
140
160
180
-3
-2
-1
0
1
2
3
rp
(rp, )
Imag
e fr
om T
ian
et a
l. ar
Xiv
:101
1.24
81
c z
/ H
(z)
(z)*
(rp, ) appears anisotropic if you assume the wrong cosmogical model (constrain = DA * H)

Imaging survey: making 2d maps

Imaging survey: papers out
Ross et al. (arXiv:1105.2320): Ameliorating Systematic Uncertainties in the Angular Clustering of Galaxies: A study using SDSS-III
Ho et al. (arXiv:1201.2137): Clustering of SDSS-III Photometric Luminous Galaxies: the measurement, systematics, and cosmogical implications
Seo et al. (arXiv:1201.2172): Acoustic Scale from the Angular Power Spectra of SDSS-III DR8 Photometric Luminous Galaxies
De Putter et al. (arXiv:1201.1909): New Neutrino Mass Bounds from SDSS-III DR8 Photometric Luminous Galaxies

Imaging survey: target selection
Color/magnitude cuts select massive red galaxies; all results today are CMASS
Masters et al. arXiv:1106.3331 Eisenstein et al. arXiv:1101.1529

Imaging survey: photo-z slices

Imaging survey: angular clustering

Imaging survey: Results
STARS! Use auto and cross-correlations of data and systematics maps to remove contribution to C

STARS!
Ross et al. (in prep.)

BAOs! Need narrow photo-z slices to avoid being washed out by projection
Method marginalizes over broadband C
to extract BAO information only

Imaging survey: BAO Results
DA(z=0.54) = 2173 100 (comoving) Mpc (4.6%)

Imaging survey: constraints from modeling the full shape of C
The model: + WMAP7 + H0 (73.6 2.4 km/s/Mpc, Riess et al 2011): k = 0.0035 0.0054; ~ 5% improvements in CDM
case
m < 0.36 eV (WMAP7+CMASS+H0)

Outline
Quick theory review -- what are we measuring?
Imaging Survey/Science from 2D maps Spectroscopic Survey/Science in 3D maps

Spectroscopic survey
Redshift surveys measure: , , redshift
, z!

Spectroscopic results: preliminary!
DR9 data final (public July 2012), clustering/covariances ~final, cosmological constraints preliminary
Current uncertainties reported, not central values

BAO fits in P(k)/(r) consistent
2-3% uncertainty on BAO position in angle-averaged P(k)/(r)
Constrains DV (DA2/H)1/3
X. Xu et al. (in prep; DR7)BOSS Galaxy Clustering (in prep.)
Preliminary BAO measurement plot here

BAO fits: interpretation
Current statistical power comparable to DR7, but at z=0.57
Watch for reconstruction on DR7 and DR9!
Eisenstein et al. astro-ph/0504362

Anistropic Clustering: (r, r)R
eid
et a
l., Sa
mus
hia
et a
l. (in
pre
p) PRELIMINARY!!

Big Picture
Two things make observed anistropic: peculiar velocities Geometry: model to convert , z x, y,
z is wrong (Alcock-Paczynski effect)

Redshift Space Distortions
depends on the geometry of the universe
, , redshift
comoving coordinates: x, y, z
(z) = true + vp/aH(a)
(z) =0z c dz/H(z)

Redshift Space Distortions (RSD)
x x
real to redshift space separations
|vp| ~ d 8/d ln a = 8 * fisotropic squashed along line of sight
z vp = -aHf m
f = d ln 8 /d ln a

Redshift Space Distortions: Why
Growth function G(a): (k, a) = aG(a)i(k) In General Relativity G(a) is determined
once H(a) is specified/measured; generically this relation is different in modified gravity models

RSD: linear theory (Kaiser 1987)

Legendre Polynomial moments: P(k)
General Expansion
Linear theory prediction

Legendre Polynomial moments: (r)General Expansion
Relation to P(k)

Modeling RSD: Reid and White 2011 (arXiv:1105.4165)
0, 2 sufficient to constrain b8, f8 ; MOST of 2d clustering information retained
RSD model vs 70 (Gpc/h)3 of sims

Fitting to 2d clustering
Use full model of 0,2(s 25 h-1 Mpc) to constrain: growth of structure (f8) DV (DA2/H)1/3
Alcock-Paczynski ( DA(zeff) * H(zeff)) shape of underlying linear P(k)

Alcock-Paczynski in multipoles

The CMASS measurements
26 log bins in s for 0 and 2 = 52 DOF
Plot of preliminary 0 and 2 measurements

Model Fits
We test the LCDM hypothesis in 4 models, always marginalizing over P(k) shape and 2FOG:
LCDM (b8) LCDM + f8: (b8, f8) LCDM + geometry: (b8, DV, DA*H) LCDM++: (b8, f8, DV, DA*H)

Current status
DV/DV,fid = x 0.019 (i.e., minimal information gain on DV compared to BAO only!)
Geometry LCDM: f8 = xx 0.03 (7%) [WMAP7 LCDM: 0.45 0.025]
f8 LCDM: = xx 0.03 (3%) [WMAP7 LCDM: 1.00 0.012]
Fit both: f8 = xx 0.07, = xx 0.07

Testing alternative models with amplitude of peculiar velocities
BOSS
PRELIMINARY!!

Expansion rate at z=0.57
PRELIMINARY!!

Simultaneous RSD and AP fits vs WMAP CDM

Summary/Conclusions
BOSS DR9 -- coming to a laptop near you in July 2012!
Unprecedented examinations of systematic errors High significance detection of BAO at z=0.57 RSD and AP constraints from 2d clustering

Results from the Baryon Oscillation Spectroscopic bccp. Reid for SDSS-III/BOSS collaboration Hubble...

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