# Presentation: 651768

## Future Directions in Ground Based Optical/IR Cosmology

- James Annis
- Experimental Astrophysics Group
- Fermilab

## SDSS Cosmology

- Power Spectra provide sensitive probes of cosmology

**Tegmark/SDSS**

## SDSS Cosmology

- Constraining a wide range of physical parameters

**Tegmark/SDSS**

## 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

-  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

- 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

- 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

## New Ways of Looking at Data

- B Yanny

**New Ways of Looking at Data**

## 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**

## Sagittarius

**Sagittarius**
**Tidal**
**stream**

**Ring**

- B Yanny

**Leads to new structure in the halo of our Galaxy**

**B Yanny**

## 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

**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

**Too shallow to do much cosmology**
**=> Sky coverage must be combined with depth**

## 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

**WMAP Team**

- Imprint of density field at time of last scattering
**Properties can be calculated from first principles!**

## The SDSS DR1 Galaxy Map

**SDSS LSS Team**

- Tracer of density field at z ~ 0.3

## 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

**Red is predicted ISW. Green predicted SZ.**

## 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

- J. Carlstrom

##  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**

## Example color cluster images from the SDSS

**Notes:**
These images from the SDSS illustrate the point. Cluster galaxies have remarkably uniform colors, colors which change strongly with redshift, allowing accurate 3D cluster identification. Clusters at higher redshift are obviously redder and smaller than those at low redshift. In fact with a bit of practice, you can estimate cluster redshifts by eye very well.

##  Elliptical Galaxy Spectrum 

- g

- r

- i

-  Elliptical Galaxy Spectrum

## 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

- T. Mckay

## 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

- 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

**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...

## 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

-  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:

- 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

**overall scaling and ********8  ****change**

**Haiman, Mohr & Holder 2001**

**redshift**

**0**

**1**

**2**

**3**

**dN/dz/12 deg****2**

**redshift**

**0**

**1**

**2**

**3**

**volume (low-z)  + growth (high-z)**

**w=-1**

**w=-0.6**

**w=-0.2**

## 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

**Notes:**
Check effective bias (old email)

## 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**

**Notes:**
Look for darth vader for “dark side”  

## 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

## Weak Gravitational Lensing Of Clusters

- Abell
- 3667
- z = 0.05

**Joffre etal**

## Weak Gravitational Lensing of Large Scale Structure

- Pen

## Weak Lensing in CMB

- Temperature field

- Lensed temperature field

**Weak Lensing in CMB**

- Hu 2002

## 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

**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) **

**Hu & Haiman (2003)**

- Haiman

**A measurement possible with just the imaging data**

## Errors on DA (z) and H(z)

_**Theorist’s surveys:**_** **
**   ****Galaxies: 10,000 sq.deg**
**                     ****M=10****12.1 ****h****-1 ****M****⊙ ****at  0<z<0.1  (SDSS main)**
**                     ****M=10****13.5 ****h****-1 ****M****⊙ ****at  0<z<0.4  (SDSS LRG)**
**    ****Clusters: 4,000 sq.deg**
**                     ****M=10****14.2 ****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 

**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

- Is a fantastic project
- See Physics Note
- FN-739

## 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?**

## Slide 47

## 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

- 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

- 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