Constraining Fundamental Physics with Weak Lensing and Galaxy Clustering. Roland de Pu+er JPL/Caltech COSMO- 14

Transcription

1 Constraining Fundamental Physics with Weak Lensing and Galaxy Clustering Roland de Pu+er JPL/Caltech COSMO- 14

2 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

3 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 EUCLID

4 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)

5 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)

6 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

7 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

8 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

9 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

10 (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)

11 Can cross- correla^ons technique improve cosmic shear constraints by calibra^ng photo- z distribu^on? de Pu\er, Dore & Das 2013

12 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

13 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

14 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

15 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

16 Extra Slides

17 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

18 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)

19 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

20 Cross- correla^ons can par^ally restore EUCLID cosmic shear informa^on lost due to poorly calibrated photo- z s

21 The Hyper Suprime Cam (HSC) wide field imaging survey will measure cosmic shear across 1500 deg Wide 1.5 deg field of view Deep mul^- band imaging (grizy; i 26, y 24) n = 20 arcmin - 2 <z> = 1

22 The Prime Focus Spectrograph (PFS) cosmology survey will measure 3D clustering at z= fibers λ = nm ELG s ([OII])

23 Large same- sky benefits possible in presence of photo- z systema^cs (but requires strong bias prior) EUCLID

24 SuMIRe: 3 tomographic bins Takada et al 2012, Oguri & Takada 2011 EUCLID: 6 tomographic bins Amendola et al 2012

25 (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

26 Cross- correla^ons can par^ally restore HSC cosmic shear informa^on lost due to poorly calibrated photo- z s

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28 Neutrino mass detec^on should be possible with EUCLID (and DESI) σ(σm ν ) = 0.03 ev Dominated by Galaxy Clustering (amplitude informa^on)

29 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

30 RedshiX distribu^on reconstruc^on crucially relies on knowledge of galaxy bias evolu^on (< 10 % needed)

31 SPHEREx: An all-sky spectroscopic survey for cosmology A high throughput, low-resolution infrared spectrometer Optical-IR imaging spectrometer λ= μm λ/δλ=40 and cm 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 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