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Detection of integrated Sachs-Wolfe effect by cross-correlation of the

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Detection of integrated Sachs-Wolfe effect bycross-correlation of the

cosmic microwave background

and

radio galaxies

中央研究院

Guo Chin Liu

Collaborators:

Ue-Li Pen (CITA)

K-W Ng(IoP, AS)

2007/12/20@NTHU

Hubble Diagram with 42 High-Redshift Supernovae

Something is missing for the “cosmological principle” based Friedmann universe.

Standard candle?

Evolution of SN Ia is small.

D. Branch et al. 2001

Perlmutter et al. 1998

m+k+=1

Microwave Sky from WMAP

CMB contains richest information of our universe.

Expansion rate

Age of universe

Inflation model

Content of universe

Geometry of universe

Thermal history (reionization)

……………

Statistics of CMB Sky

Geometry of our universe

ISW effect

- Observation of CMB first peak alone does not guarantee the existence of dark energy.
- We are living in low density universe, i.e., m0.3. Allen et al. 2002Carlberg et al. 1997
- Hubble constant is not so small, for example, from SZ clusters measurement, H0=60-70Reese et al. 2002Udomprasert et al 2004.

m+k+=1

Spergal et al. 2007

Astronomical Observation for Dark Energy

- Need to be sensitive on
- Geometry of universe (distance vs. redshift relation)
- 2. Structure formation

Current used observations

- Supernova type Ia : probe the geometry of universeCaution: assuming uniform intrinsic luminosity
- CMB : good constraint on small curvatureCaution : no time evolution data
- Large scale structure : evolution of geometry of universe and growth factor D(z) Caution: depend on CDM model for structure formation

Other possibilities

Dark energy couples with cold dark matter : Changing matter power spectrum

S. Lee, G. Liu & K. Ng PRD 2006

Coupling with CMB photons: Producing parity odd term in CMB polarization power spectra

G. Liu, S. Lee & K. Ng PRL 2006

The physical quantity to be determined:

Equation of state w(z)=p/

Cosmological constant: w=-1

Quintessence : wQ: w0, w0+(1-a)w1, oscillating….

a. Assume flat universe and const. w

w=-1.05+0.15-0.2 Knop et al.2004 (SN)

b. time evolution w=w0+ (1-a)w1w0=-1.146+0.176-0.178

w1=0.6+0.622-0.652 --no dark energy perturbation

w0=-1.118+0.152-0.147

w1=0.499+0.453-0.498 -- with dark energy perturbationG-B Zhao et al. 2006(SN+CMB+galaxy clustering)

CDM explains observation data very well

Inhomogeneity

Cosmological constant

Dark energy

Cosmologists are often in error, but never in doubt Lev Landau

Future observation

Weak lensing:Size of distortion image depends on distance traveled and growth factor

BAO: Baryon Acoustic Oscillation is sensitive to dark energy through its effect on the angular-diameter distance vs. redshiftrelation and through its effect on the time evolution of the expansion rate.

Clusters observation: growth rate and geometry of universe

- Joint Efficient Dark-Energy Investigation (JEDI)* SN Ia 0<z<2* BAO 10-100 M galaxies, 1000-10000 deg^2* Weak lensing 1000-10000 deg^2
- SuperNova Acceleration Probe (SNAP)*SN Ia 0<z<1.7*Weal lensing

2

1

Second Hint from CMB

- ISW effect (late)I
- If the potential decays between the time a photon falls into a potential well andwhen it climbs out it gets a boost in temperature ofdue to the differentialgravitational redshift and due to an accompanying contraction of the wavelength
- No ISW effect in matter dominate epoch.
- The dark energy dominating on late epoch creates the temperatures anisotropies on large scales.

E=|1-2|

T/T=-2 d d/d

- ISW effect II
- Signature of dark energy
- Probe of evolution of structure
- Sensitive on large scale (horizon)
- Difficult to detect

Try to look forcorrelation of CMB with matter

Density fluctuation

Form structures

CMB gains energy

Cross correlation of CMB with matter in local universeProposed by Crittenden & Turok (1996)

- Possible tracers
- NRAO VLA Sky Survey (NVSS)
- Hard X-ray background(HEAO-1)
- Sloan Digital Sky Survey (SDSS)
- Two Micron All Sky Survey Extended Source Catalogue (2MASS XSC)

Contribution to Signal from different Redshift

Crittenden & Turok PRL 1996

First detection of the cross-correlation

Correlating CMB sky to hard X-rays (HEAO-1) and radio galaxy (NVSS)

wiNiwjTj/wiwj

3 sigma detection for hard X-rays and 2.5 sigma for radio galaxy

Boughn & Crittenden, nature, 2004

Contamination

- Sunyaev-Zeldovich Effect: anisotropies generated through the inverse Compton scattering with free e- correlates with the galaxy itself. On small scales
- Emission from the radio galaxyEmission at f<few tens GHz contaminates the microwave sky. On small scales
- Primary CMB itself: △T(ISW) < 30% of △T(total)

Details of this work I

- We work at harmonic spaceSZ and radio emission is ignorable.Low correlation between each mode
- ClNT=<aNlmaT*lm>△T/T()=aTlmYlm()
- Using NVSS as matter distribution tracer.
- Healpix software is used forvisualization and calculating alm

NVSS data

1. 1.4GHz , 82% sky coverage (>-40)

2. Sensitivity 2.5 mJy contains 1.8 million sources

3. Typical luminosity function models indicate 0z2 distribution

Detail II

41GHz

61GHz

T

T

Q

Q

U

U

Result I

CMB anisotropies & polarization on large scales

CMB last scattering surface

△TSW, z=1100

Generate P. for l>100

△Treion, z=10

Generate P for l < 30~50

△TISW, z<2

Dark energy dominates

Observer

Correction by the information of polarization

At large scales T=TSW + Tre+ TISW

E(no ISW) =aT(no ISW) + n

<TE> = a <TT>

<EE>=a2<TT> + n2

T(ISW) =T – E/a * WF

WF=a2<TT>/<EE>

Result II

Discussion & Summary

- Working in harmonics space, signal with 2-sigma is detected in l~ 10-20. Though it is smaller than detection in real space, statistically it gives same information.
- Primary CMB is the dominated noise in this cross-correlation. Using polarization information, we can filter out part of it.
- It suppress the noise about 17%, 3% and 8.7% in band power l=3, 7 and 15. Give a better constrain on dark energy model.