# Presentation: 883795

## CMB Constraints on the Intracluster Medium

- Niayesh Afshordi
*Institute for Theory and Computation*
*Harvard College Observatory*

- July 23rd, 2004

##   Yen-Ting Lin
University of Illinois Urbana-Champaign
Princeton
Alastair Sanderson
University of Illinois Urbana-Champaign
University of Birmingham
Daisuke Nagai
CalTech

Afshordi, Lin, & Sanderson 2005 (1st yr)
Afshordi, Lin, Nagai, & Sanderson 2006 (3 yrs)	 in preparation

-   Yen-Ting Lin
*University of Illinois Urbana-Champaign*
*Princeton*
- Alastair Sanderson
*University of Illinois Urbana-Champaign*
*University of Birmingham*
- Daisuke Nagai
*CalTech*
*Afshordi, Lin, & Sanderson 2005 (1st yr)*
*Afshordi, Lin, Nagai, & Sanderson 2006 (3 yrs)**	** in preparation*

- July 23rd, 2004

## Thermal Sunyaev-Zel’dovich (SZ) Effectand Intra-Cluster Medium (ICM)

**Thermal *****Sunyaev-Zel’dovich***** (SZ) Effect****and *****Intra-Cluster Medium***** (ICM)**

- WMAP sees here

-  Probes the thermal energy distribution of electrons in the Intra-Cluster Medium
-  Dominates CMB at angles < 0.1o
-  Generates an anti-correlation between WMAP and galaxy/cluster distribution

- July 23rd, 2004

## Thermal Sunyaev-Zel’dovich (SZ) Effectand the CMB

- Readhead et al. 2004

- Tension with new low WMAP 8  ?!

- July 23rd, 2004

## Can SZ surveys sustain the CMB dominance?

-  SZ clusters can be
- Detected up to high redshifts
-  Their number counts probe Dark Energy/Cosmology
-  Many SZ surveys are underway: APEX, SZA, ACT, SPT, Planck, ...
-  Can they deliver?  Calibration of SZ-Mass relation, Gastrophysics, ...

- Courtesy of John Carlstrom

- July 23rd, 2004

- July 23rd, 2004

## Bennett et al. 2003 (XBAC’s clusters; 2.5)
Fosalba, Gaztanaga, & Castander 2003; Fosalba & Gaztanaga 2004 (SDSS, APM; 2.7)
Myers et al. 2004 (APM+ACO; ~2)
Afshordi, Loh, & Strauss 2004 (2MASS; 3.7)

- Bennett et al. 2003 (XBAC’s clusters; 2.5)
- Fosalba, Gaztanaga, & Castander 2003; Fosalba & Gaztanaga 2004 (SDSS, APM; 2.7)
- Myers et al. 2004 (APM+ACO; ~2)
- Afshordi, Loh, & Strauss 2004 (2MASS; 3.7)

- July 23rd, 2004

## Afshordi, Loh, & Strauss (2MASS Deepest magnitude bin):
data                 best fit model
          ISW            SZ                   Point Sources          

- Afshordi, Loh, & Strauss (2MASS Deepest magnitude bin):
- data                 best fit model
-           ISW            SZ                   Point Sources

-  Cluster physics is mixed with cosmology,
-  and non-linear bias  
-  Does not employ the non-Gaussianity of the signal 

- July 23rd, 2004

## Hernandez-Monteagudo & Rubino-Martin 2004 (BCS, NORAS, etc; 2-5)
Hernandez-Monteagudo et al. 2004,2006 (2MASSxWMAP+Archeops; 5)

- Hernandez-Monteagudo & Rubino-Martin 2004 (BCS, NORAS, etc; 2-5)
- Hernandez-Monteagudo et al. 2004,2006 (2MASSxWMAP+Archeops; 5)

-  Does employ the non-Gaussianity of the signal 
-  Cluster physics is mixed with template making
- procedure in a non-trivial manner 

- July 23rd, 2004

## Most Galaxies are NOT in clusters
Most SZ signal comes from clusters
		       thus...
The SZ detection is more significant if we just look around clusters  Make an SZ template 
The S/N is maximized if the template matches the actual SZ profile  Constraint on the SZ profile  

- Most Galaxies are NOT in clusters
- Most SZ signal comes from clusters
- 		       thus...
- The SZ detection is more significant if we just look around clusters  Make an SZ template
- The S/N is maximized if the template matches the actual SZ profile  Constraint on the SZ profile

- Observed Sky

- Template

- July 23rd, 2004

## Three close-by clusters in the 3yr cleaned map (Tegmark et al)

**WMAP SZ clusters ...**

- Abell 133

- Abell 1656

- Abell 2319

- July 23rd, 2004

## Match-filter SZ detection in an X-ray cluster catalog

**Match-filter SZ detection in an X-ray cluster catalog**

-  Compile a catalog of 116 low-z X-ray clusters with measured temperatures
-  Compile the X-ray estimated gas mass for most of them
-  ICM/ Point Source template:
- NFW gravitational potential
- Hydrostatic equilibrium
- Polytropic equation of state 	Pgas / (gas)eff; eff = 1.2
- Point sources follow DM profile

- July 23rd, 2004

## Gas Fraction vs. Temperature (WMAP 1yr)

-  SZ observation
-  X-ray Observation

**Gas Fraction vs. Temperature (WMAP 1yr)**

-  The mean gas fraction of ICM is 20-40 % less than cosmic budget:
-        <fgas h> = 0.08 ± 0.01(ran) ± 0.01(sys)
-  Comparable S/N to higher resolution interferometers (e.g. OVRO/BIMA Grego et al. 2001)
-  X-ray gas mass estimates consistent with SZ estimates
-  Both X-ray and SZ gas mass estimates show an increasing trend with Tx

- July 23rd, 2004

## Gas Fraction vs. Temperature (WMAP 1yr)

- July 23rd, 2004

## Microwave Luminosity of Cluster Members

- LPS(MK < -21)
- = (2.4 ± 0.8) x 1027 h-2 erg/s/Hz/galaxy
- -Most of the signal comes from Tx < 2 keV
- -Mainly Q-band (lowest frequency)
- -Similar to Milky Way and M31

- Pierpaoli & Perna 2004

- Milky Way

- WMAP cluster sources

- 26

- 30

- 28

- July 23rd, 2004

## WMAP 3 years
Temperature: Q,V,W
Nres = 9 (pixel size '  0.1 deg)
417 clusters 
meaured X-ray temperature

- WMAP 3 years
- Temperature: Q,V,W
- Nres = 9 (pixel size '  0.1 deg)
- 417 clusters
- meaured X-ray temperature

- July 23rd, 2004

## Find R200 for each cluster using M200-TX relation
Constrain pressure within spherical radial bins centered at: 0.25,0.5,1,2,4,8 x R200 + a central radio source :
Only consider pixels close to each cluster, with resolution degrading with distance 	
	 Makes covariance matrix tractable     

- Find R200 for each cluster using M200-TX relation
- Constrain pressure within spherical radial bins centered at: 0.25,0.5,1,2,4,8 x R200 + a central radio source :
- Only consider pixels close to each cluster, with resolution degrading with distance
- 	 Makes covariance matrix tractable

- Abell 2319 in Q-band

- Degraded Abell 2319 in Q-band

- July 23rd, 2004

## Temperature-Weighted Gas Fraction

**Temperature-Weighted Gas Fraction**

- All Clusters

- Q-band    V-band   W-band  Hydro-Simulations

- TX > 5 keV; 144 Clusters

- No significant frequency dependence
-  No significant point source contamination

- July 23rd, 2004

## Universal Pressure Profile

- __ CDM/crit
- __ Hydro-Simulations
- __ WMAP Random Realization
-  WMAP best fit

- TX > 5 keV; 144 Clusters

- 2 ' 110 for the
- simulated profiles
-  10.5 detection

- Prior: gas > 0

- July 23rd, 2004

## Total ICM gas fraction

**Total ICM gas fraction**

- __ Hydro-Simulations
- __ WMAP Random Realization
-  WMAP best fit

- Cosmic Concordance:
- b/CDM = 0.20 ± 0.01
- Scaled simulation to match SZ detection:
- b/CDM = 0.23 ± 0.02 (ran) ± 0.02 (sys)

- 11 model independent measurement of SZ

- July 23rd, 2004

## WMAP does contain information about the low-redshift universe
The way to extract this information is through combination with low-redshift surveys
For a non-Gaussian signal such as SZ, the optimum way to extract the signal is through generating an estimated signal template
Based on an analytic ICM model, we detect SZ signal at 8 and Point Sources at 3 (1st year)
A model-independent analysis of 3 year WMAP data with 144 massive clusters yields:
The first model independent universal pressure profile, closely follow dark matter  
Prefers simulation results to null at » 11
In comparison with simulations, constrains b/m at 11 level, consistent with the concordance model

- WMAP *does *contain information about the low-redshift universe
- The way to extract this information is through combination with low-redshift surveys
- For a non-Gaussian signal such as SZ, the optimum way to extract the signal is through generating an estimated signal template
- Based on an analytic ICM model, we detect SZ signal at 8 and Point Sources at 3 (1st year)
- A model-independent analysis of 3 year WMAP data with 144 massive clusters yields:
- The first model independent universal pressure profile, closely follow dark matter
- Prefers simulation results to null at » 11
- In comparison with simulations, constrains b/m at 11 level, consistent with the concordance model

- July 23rd, 2004

## In the run-up to high resolution SZ surveys, there is much more that can and should be learnt about ICM
Higher Resolution CMB/SZ surveys (Planck, SZA, APEX, SPT, ...) will be able to significantly lower their effective cluster detection mass threshold thru combination with wide-angle X-ray cluster surveys (e.g., DUO) 
X-ray and SZ surveys must be combined to provide reliable tests for models of Dark Energy or Cluster Physics

- In the run-up to high resolution SZ surveys, there is much more that can and should be learnt about ICM
- Higher Resolution CMB/SZ surveys (Planck, SZA, APEX, SPT, ...) will be able to significantly lower their effective cluster detection mass threshold thru combination with wide-angle X-ray cluster surveys (e.g., DUO)
- X-ray and SZ surveys must be combined to provide reliable tests for models of Dark Energy or Cluster Physics

- July 23rd, 2004

## Simulations  NFW dark matter profile

  = 200:

Gravitational Potential: 

- Simulations  NFW dark matter profile
-   = 200:
- Gravitational Potential:

- July 23rd, 2004

## Assume Polytropic Gas; eff =1.2

Hydrostatic Equilibrium+Accretion Shock at rvir 

Assume NFW distribution of point sources with flat spectrum, i.e. T / -2  ; One source per bright galaxy

- Assume Polytropic Gas; eff =1.2
- Hydrostatic Equilibrium+Accretion Shock at rvir
- Assume NFW distribution of point sources with flat spectrum, i.e. T / -2  ; One source per bright galaxy

- July 23rd, 2004

## Estimated X-ray temperature of the Cluster

Given the cosmology, eff, and cvir, the value of Tx fixes the ICM properties, e.g., the SZ flux:

- Estimated X-ray temperature of the Cluster
- Given the cosmology, eff, and cvir, the value of Tx fixes the ICM properties, e.g., the SZ flux:

- July 23rd, 2004