Constraining Fundamental Physics with Weak Lensing and Galaxy Clustering Roland de Pu+er JPL/Caltech COSMO- 14
Galaxy Clustering: - 3D maps of galaxies - > 3D power spectrum P(k,mu) - BOSS: V = 4.4 (h- 1 Gpc)3, Ω 10,000 deg2 The SDSS telescope at Apache Point, New Mexico Weak Gravita4onal Lensing: - - - Cosmic shear - > angular power spectra Cl of shear and source density CFHTLS: Ω 150 deg2 soon: DES, KIDS, HSC, LSST, EUCLID, The Canada France Hawaii Telescope (Mauna Kea) Major Development: Advent of Large, Overlapping Surveys
SuMIRe: Subaru Measurement of Images and Redshi?s (1500 deg 2 ) 8.2 m Subaru telescope Hyper Suprime Cam (HSC) lensing survey Prime Focus Spectrograph (PFS) redshix survey WFIRST 0.5 1.0 2.0 EUCLID
How much improvement when Weak Lensing and Galaxy Clustering combined? Kilbinger et al 2012 (CFHTLS) How important is overlap between surveys? Mandelbaum et al 2013 (SDSS)
SuMIRe Dark Energy: Strong WL + GC complementarity, but overlap not crucial Tight bounds on ^me- varying DE equa^on of state CMB prior (Planck) included RdP, Dore & Takada 2013 Ω m γ (z)
SuMIRe growth rate: Strong WL + GC complementarity, but overlap not crucial CMB prior (Planck) included Bounds on growth rate of large scale structure Combina^on of WL + GC crucial! Ω m γ (z) in GR RdP, Dore & Takada 2013
Correla^on between shear and galaxy density is modest because of limited redshix overlap global correla^on coefficient of shear with spectroscopic galaxy density The number of modes probed by cross- correla^ons is small compared to that probed my RSD or WL alone
Cosmological informadon in shear- galaxy cross power spectra is limited, but other same- sky benefits do exist See also: Cai & Bernstein 2012, Font- Ribera et al 2013 BUT: Gaztanaga 2012, Kirk et al 2013 imaging survey provides target catalog informaoon from non- linear regime higher order staosocs IdenOfying/constraining systemaocs Hikage, Takada & Spergel 2011 Yoo & Seljak 2012 Hikage et al 2013 Cacciato et al 2013
Upcoming cosmic shear surveys require < 1 % level calibra^on of photometric redshixs Huterer et al 2005; Ma, Hu & Huterer 2005; etc In forecasts, distribuoon defined by sca\er σ z (z) and bias b z (z): p(z ph z) See, e.g. Ma, Hu & Huterer (2006), Huterer et al (2006), Ma & Bernstein (2008), Hearin et al (2010) Ilbert et al 2006
(Source) redshix distribu^ons can be es^mated using cross- correla^ons with overlapping spectroscopic sample Newman 2008, Schulz 2010, Ma\hews & Newman 2010, McQuinn & White 2013, Menard et al 2013, Rahman et al 2014 Blas ps C i b (s) (z i ) b ( p) (z i ) n p (z i ) P( / D i ) BUT: Redshi? distribuoon reconstrucoon crucially relies on knowledge of galaxy bias evoluoon (< 10 % needed)
Can cross- correla^ons technique improve cosmic shear constraints by calibra^ng photo- z distribu^on? de Pu\er, Dore & Das 2013
Cross- correla^ons can par^ally restore HSC cosmic shear informa^on lost due to poorly calibrated photo- z s degrada^on w/o cross- correla^ons perfectly known ph- z distribu^on adding cross- correla^ons
Cross- correla^on technique looks promising, but major challenges remain Breaking the n(z) galaxy bias degeneracy Dealing with outliers/distribuoons beyond Gaussian Non- linear bias Confusion with magnificaoon bias etc
Cosmological neutrino constraints are degenerate with infla^onary physics Primordial Power Spectrum (PPS) current CMB data Bounds become robust against assump^ons about PPS when mul^ple data sets are combined: current data de Pu\er, Linder & Mishra 2014
Summary/Conclusions Combining Weak Lensing and Galaxy Clustering will improve DE FOM by factor 2-3 compared to either probe alone and will lead to strong cosmic growth constraints Cross- correla^ons between WL and GC surveys add limited direct cosmological informa^on, but are crucial for constraining systema^cs such as photo- z calibra^on Robust joint constraints on neutrino mass and infla^on can be obtained using complementary current data sets SPHEREx: measuring the near- IR spectrum of the full sky. A space- based galaxy survey to constrain primordial non- Gaussianity to σ(f NL )~1
Extra Slides
The number of modes probed by cross- correla^ons is small compared to that probed my RSD or WL alone Font- Ribera et al, 2013
EUCLID dark energy: Strong WL + GC complementarity, but overlap not crucial Tight bounds on ^me- varying DE equa^on of state CMB prior (Planck) included Ω m γ (z)
EUCLID growth rate: Strong WL + GC complementarity, but overlap not crucial CMB prior (Planck) included Bounds on growth rate of large scale structure Combina^on of WL + GC crucial! Ω m γ (z) in GR
Cross- correla^ons can par^ally restore EUCLID cosmic shear informa^on lost due to poorly calibrated photo- z s
The Hyper Suprime Cam (HSC) wide field imaging survey will measure cosmic shear across 1500 deg 2 2014 2019 Wide 1.5 deg field of view Deep mul^- band imaging (grizy; i 26, y 24) n = 20 arcmin - 2 <z> = 1
The Prime Focus Spectrograph (PFS) cosmology survey will measure 3D clustering at z=0.6-2.4 2018 2023 2400 fibers λ = 380 1260 nm ELG s ([OII])
Large same- sky benefits possible in presence of photo- z systema^cs (but requires strong bias prior) EUCLID
SuMIRe: 3 tomographic bins Takada et al 2012, Oguri & Takada 2011 EUCLID: 6 tomographic bins Amendola et al 2012
(Source) redshix distribu^ons can be es^mated using cross- correla^ons with overlapping spectroscopic sample Newman 2008, Schulz 2010, Ma\hews & Newman 2010, McQuinn & White 2013, Menard et al 2013 Menard et al 2013 Ma\hews & Newman 2010
Cross- correla^ons can par^ally restore HSC cosmic shear informa^on lost due to poorly calibrated photo- z s
Neutrino mass detec^on should be possible with EUCLID (and DESI) σ(σm ν ) = 0.03 ev Dominated by Galaxy Clustering (amplitude informa^on)
Upcoming cosmic shear surveys require < 1 % level calibra^on of photometric redshixs p(z ph z) Ilbert et al 2006 Huterer et al 2005; Ma, Hu & Huterer 2005; etc
RedshiX distribu^on reconstruc^on crucially relies on knowledge of galaxy bias evolu^on (< 10 % needed)
SPHEREx: An all-sky spectroscopic survey for cosmology A high throughput, low-resolution infrared spectrometer Optical-IR imaging spectrometer λ= 0.9-5 μm λ/δλ=40 and 150 20cm telescope Passively cooled 6 pixel 3.5x7 deg. 2 FOV Inflation)Science Surveys the z < 1 universe to fundamental limits to measure signatures of inflation, non-gaussianity and the primordial spectrum, and dark energy. Cosmology derived from 3D galaxy large-scale structure. Complements Euclid and WFIRST which survey smaller areas at z > 1. (x2.5 better than Euclid on f nl ) σ(f NL loc ) ~ 1 Creates a Legacy All-Sky Survey Extra-galatic sources 8 10 galaxies 7 10 galaxies with σ /(1+z)<0.3% z 6 2x10 QSOs with redshift 0-100 QSOs with redshift > 6 35,000 galaxy clusters 7 10 stellar spectra Galactic sources 6 >10 embedded stars SMEX Concept; >2000 PI: brown J. Bock, dwarf spectra PS: O. Doré Olivier Doré CIFAR Cosmology & Gravitation Program, Québec - May 24th 2014 1