longRange Oct03

Future Directions in Ground Based Optical/IR Cosmology: 

Future Directions in Ground Based Optical/IR Cosmology James Annis Experimental Astrophysics Group Fermilab

SDSS Cosmology: 

SDSS Cosmology Power Spectra provide sensitive probes of cosmology Tegmark/SDSS

Slide3: 

Constraining a wide range of physical parameters SDSS Cosmology Tegmark/SDSS

Scientific Motivation: 

Scientific Motivation Create the ultimate map of the Universe:  The Cosmic Genome Project! Study the distribution of galaxies:  What is the origin of fluctuations?  What is the topology of the distribution? Measure the global properties of the Universe:  How much dark matter is there? Local census of the galaxy population:  How did galaxies form? Find the most distant objects in the Universe:  What are the highest quasar redshifts?

Fermilab’s Role: 

Fermilab’s Role Project Management Project directed by a Fermilab scientist from 1997-2003 Current director has Fermilab/UC joint appointment Project managed by Fermilab engineer since 1999 Software System Design Led by Fermilab scientist since 1991 Designed whole software environement System worked when confronted with real data Data Processing and Distribution Target selection and plates drilling on time Data releases to collaboration and public Pipeline Development Target section Calibration pipelines Image correction pipelines and on and on Data Acquisition Ambitous (in 1992) system delivered on time Real time data analysis on astrometric data Mountain top software Mountaintop Engineering Plate handling system Camera handling carts Fiber mapper Telescope maintenence Calibration Calibration system design Calibration system software Analysis star/galaxy separation, ellipticities,… These are Fermilab’s strengths

Fermilab’s Role: 

Fermilab’s Role Explaining large software projects to gaggles of astronomers. Steve Kent, designer of the SDSS Pipeline system Another Fermilab strength The SDSS Gaggle, 2002

SDSS Extension: 

SDSS Extension New collaboration (new name?) Starts 2005 (funding willing) Primarily a 2-3 year spectroscopy project 4000 sq-degrees of spectroscopy 100/sq-degree Three core projects Fill In the Gap Structure of the Galactic Halo Supernovae at 0.1 <= z <= 0.3

Slide8: 

B Yanny New Ways of Looking at Data

Slide9: 

11 kpc Galactic Center Stars in the smooth “spheroid” population Pal 5 globular cluster Sagittarius dwarf tidal stream Sagittarius dwarf Tidal stream Sun B Yanny Lead to new ways of looking at the Galaxy

Slide10: 

Sagittarius Tidal stream Ring B Yanny Leads to new structure in the halo of our Galaxy

Slide11: 

B Yanny

Context: 

Context SDSS extension 4000 sq-degrees of spectroscopy LSST DMT/LSST 8m telescope, giant camera PanSTARRS 4 1m telescopes, big cameras 2007? GSMT/CELT 30meter ground telescope, deep spectroscopy JWST (aka NGST) 6m space telescope, infrared spectroscopy/imaging SNAP ! WMAP CMB, flying Planck CMB: last word on fluctuations, but on to polarization

Scientific Motivation: 

Scientific Motivation Create the ultimate map of the Universe  The SDSS was a start In order to study fundamental physics:  What is the dark matter?  What is the dark energy?  What were the conditions during inflation?

The Two Micron All Sky Survey: 

The Two Micron All Sky Survey Too shallow to do much cosmology => Sky coverage must be combined with depth

Wilkonsin Microwave Anisotropy Probe: 

Wilkonsin Microwave Anisotropy Probe The CMB is as deep as one can go Galactic Foreground Cosmic Microwave Bg. Different color! Can be removed

The Cosmic Microwave Background: 

The Cosmic Microwave Background WMAP Team Imprint of density field at time of last scattering Properties can be calculated from first principles!

The SDSS DR1 Galaxy Map: 

The SDSS DR1 Galaxy Map SDSS LSS Team Tracer of density field at z ~ 0.3

Cross correlate CMB & Galaxies: 

Cross correlate CMB & Galaxies The large scale structure of galaxies and dark matter imprint the CMB photons as they pass to through => Cross correlate galaxies with CMB ?!

Integrated Sachs Wolf Effect: 

Integrated Sachs Wolf Effect Red is predicted ISW. Green predicted SZ.

Slide20: 

Sunyaev-Zeldovich Effect  Scattering moves photons from low frequencies (RJ part of the frequency spectrum) to high frequencies (Wien regime) In the language of Sunyaev-Zel’dovich (1980): Frequency shift the CMB blackbody and the difference (wrt to CMB) A. Cooray

The South Pole Telescope: 

The South Pole Telescope J. Carlstrom

SPT 4000 sq degree Survey : 

SPT 4000 sq degree Survey Could be done in one austral winter SZ observations of clusters dN/dz for 4000 sq-degree 20,000 clusters, 80% z <= 1 But All Without Redshifts

Slide23: 

Example color cluster images from the SDSS

Slide24: 

g r i Elliptical Galaxy Spectrum

Finding red sequence clusters: 

Finding red sequence clusters Red sequence galaxies at z=1.27 (van Dokkum et al, 2000) E/SO ridgeline Clustering in position-color space essentially eliminates contamination by projection Gladders & Yee (2000), Goto et al. (2001), Annis et al. (2003) E/SO ridgeline provides extremely accurate (z0.01) photometric redshift Red sequence in place throughout SDSS volume and beyond, to z>1…. T. Mckay

The maxBCG sample: redshift: 

The maxBCG sample: redshift T. Mckay

Limitations of Existing Instruments : 

Limitations of Existing Instruments SDSS: not deep enough z = 0.3 – 0.5 wrong hemisphere, as are: CFHT Legacy Survey 20 N declination (2 airmass @ -40 dec, meridian) PanStarrs 20 N declination (2 airmass @ -40 dec, meridian) LSST 2013 (?) Will definitively survey they sky in optical SPT is at south pole, sees Southern Galactic Cap

A Wide Field Imager on the CTIO Blanco 4m: 

A Wide Field Imager on the CTIO Blanco 4m Collecting area:10 m^2 Prime focus: f/2.87 15 micron pixels => 0.267”/pixel Field of view (diameter): Current: 0.8 degree Need: 1.8 degree Need to build a 20k x 20k pixel Camera 400 Megapixel Big. State of the art last January: Megacam at 16k x 16k 2007-2008? A project in which Fermilab could take a leadership role A four filter survey to i=24 over 4000 sq-degrees

Large format cameras: 

Large format cameras Megacam, at CFHT 36 4k x 2k 300 Megapix 2003 Megacam at MMT 36 4k x 2k 300 Megapix 2003 CFH12k 12 4k x 2k 100 Megapix 2000 SDSS 30 2k x 2k 120 Megapix 1998

We can do that…: 

We can do that…

Elements of a Survey: 

Elements of a Survey Wide field corrector Camera CCDs/detectors Electronics Readout Control Mechanical Vacuum systems Cooling systems Data acquisition system Hardware software Survey observation strategy Standard star strategy Science Software Calibration pipeline Coadd pipeline Galaxy measurement pipeline Cluster finding pipeline Data production Data distribution Simulation Science Analysis Science case! for proposals

Fermilab’s Strengths: 

Fermilab’s Strengths Project Management Software System Design Data Processing and Distribution Pipeline Development Data Acquisition Mountaintop Engineering Calibration Analysis We should add detector/camera construction!

CMB Optical Followup:: 

CMB Optical Followup: One follows up by a 4000 square degree imaging survey, in 4 bandpasses, to i~24. This allows: Photometric redshifts for ~25,000 SZ clusters Optically selected sample of clusters redshift and mass estimates Weak lensing mass estimates of these clusters Weak lensing cosmic shear measurements with photo-z tomography Galaxy clustering on large scales to z ~ 1 Galaxy-galaxy lensing … and much more.

Sensitivity to M ,w in SZE Survey: 

Sensitivity to M ,w in SZE Survey overall scaling and 8 change Haiman, Mohr & Holder 2001 redshift 0 1 2 3 dN/dz/12 deg2 redshift 0 1 2 3 volume (low-z) + growth (high-z) w=-1 w=-0.6 w=-0.2

Cluster Power Spectra: 

Cluster Power Spectra • High bias of galaxy clusters enables accurate measurement of cluster P(k): k/k=0.1 → P(k) to 7% at k=0.1 k<0.2 → P(<k) to 2% • Expected statistical errors from 25,000 clusters: M ~ to 0.013 - geometrical test w ~ to 0.04 - geometrical test h2 ~ to 0.002 - usual shape test  Combine with dN/dM (Majumdar & Mohr 2003) • Noteworthy for survey planning - baryon rings are useful: contain ~ half the information make test robust (CMB, ) - photometric redshift (0.01) sufficient to recover most of the info - including knowledge of bias would much improve constraints - z < 1 clusters are best complement to CMB

An advantage unique to clusters?: 

An advantage unique to clusters? A cluster sample can deliver many observables SZE decrement X-ray flux Angular size Number of galaxies Spatial distribution (2d, 3d) Lensing signatures We can construct several cosmology tests dN/dz – abundance evolution (including mass function dN/dM) P(k) – spatial power spectrum (including Alcock-Paczynski) Scaling relations – between SZ/X-rays/sizes (including dA measurement) Simultaneous determination of cosmological and cluster structural parameters (with their evolution) Best? better good

Weak Gravitational Lensing: 

Weak Gravitational Lensing Distortion Matrix:  Direct measure of the distribution of mass in the universe, as opposed to the distribution of light, as in other methods (eg. Galaxy surveys) Theory

Slide38: 

Abell 3667 z = 0.05 Joffre etal Weak Gravitational Lensing Of Clusters

Weak Gravitational Lensing of Large Scale Structure: 

Weak Gravitational Lensing of Large Scale Structure Pen

Slide40: 

Temperature field Lensed temperature field Weak Lensing in CMB Hu 2002

CMB/Galaxy/Weak Lensing Science: 

CMB/Galaxy/Weak Lensing Science Combine WL and SZ on cluster catalog Cross correlation of WL and secondary CMB Joint Analysis of CMB and WL power spectra Cross correlation of CMB and cluster catalog: SZ Cross correlation of CMB and galaxy catalog: ISW CMB polarization of CMB towards cluster catalog Cross correlate CMB polarization with galaxy catalog Power spectra of cluster catalog with photo-z Redshifting Rings of Power (!) The Cosmology with Sunyaev-Zeldovich Cluster Surveys Conference Cooray 2003 (astroph/0305515) Takada and Sugiyama 2001 (astroph/0110313) Ishak et al 2003 (astroph/03084461) Komatsu et al 2000 (astroph/0012196) Scranton et al 2003 (astroph/0307335) Cooray and Baumann 2002 (astroph/0211095) Benabed et al 2000 (astroph/0003376) Hu and Haiman 2003 (astroph/0306053) http://bubba.ucdavis.edu/~sz03 A rich field with much interesting physics

Acoustic Rings in 2D: 

Power spectrum is measured at fixed angular scale and redshift. Inferred spatial scales depend on the assumed cosmology Forms purely geometrical test, if CMB priors are used Insensitive to z-distortion (c.f. Alcock-Paczynski test) Acoustic Rings in 2D Hu & Haiman (2003) Haiman A measurement possible with just the imaging data

Errors on DA (z) and H(z): 

Errors on DA (z) and H(z) Theorist’s surveys: Galaxies: 10,000 sq.deg M=1012.1 h-1 M⊙ at 0<z<0.1 (SDSS main) M=1013.5 h-1 M⊙ at 0<z<0.4 (SDSS LRG) Clusters: 4,000 sq.deg M=1014.2 h-1 M⊙ at 0<z<1.3 (SPT) - 25,000 clusters CMB priors Hu & Haiman 2003 Haiman galaxies: (w)=0.024 ()=0.007 clusters: (w)=0.040 ()=0.013

Errors on w and DE : 

Errors on w and DE Hu & Haiman 2003 Filled ellipses: b marginalized to an overall scaling Empty ellipses: , b marginalized (b separately in each z=0.1 bin) galaxies: (w)=0.024 ()=0.007 clusters: (w)=0.040 ()=0.013 Haiman

SNAP: 

SNAP Is a fantastic project See Physics Note FN-739

Scientific Motivation: 

Scientific Motivation Create the ultimate map of the Universe  The SDSS was a start In order to study fundamental physics:  What is the dark matter?  What is the dark energy?  What were the conditions during inflation?

Planned Surveys: K band RH = 3/2: 

Planned Surveys: K band RH = 3/2 Name D T Ω n Survey m sec deg2 # years UKIDSS 3.6 2000 0.21 1 RH=3/4 12 Vista 4.0 1800 0.25 1 RH=3/4 9 SNAP 2.0 140 0.06 3 RH=3/4 1 SNAP 2.0 1500 0.06 3 11 Prime-midex 1.0 5000 0.25 4 7 Chicago LT 30. 6000 7.0 1 1 Prime-discovery 4.0 400 0.25 4 0.5 all need 3*survey to obtain photo-z data

Create the ultimate map of the Universe: 

Create the ultimate map of the Universe Photo-z’s out to z=5 and down to 0.3 L-star Optical component can be done from ground with LSST Infrared impossible from ground, requires space based large infrared camera… Ground Space Background on log plot Map all galaxies in the observable universe This is 2015+ thinking…

Changing the Way Astronomy is Done: 

Changing the Way Astronomy is Done Surveys provide The maximum amount of high-quality data To the most scientists For the lowest cost To address the biggest problems of cosmology

Decadal Survey: 

Decadal Survey