Detection of integrated Sachs-Wolfe effect by
This presentation is the property of its rightful owner.
Sponsored Links
1 / 27

Detection of integrated Sachs-Wolfe effect by cross-correlation of the PowerPoint PPT Presentation


  • 83 Views
  • Uploaded on
  • Presentation posted in: General

Detection of integrated Sachs-Wolfe effect by cross-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). [email protected] Hubble Diagram with 42 High-Redshift Supernovae.

Download Presentation

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

An Image/Link below is provided (as is) to download presentation

Download Policy: Content on the Website is provided to you AS IS for your information and personal use and may not be sold / licensed / shared on other websites without getting consent from its author.While downloading, if for some reason you are not able to download a presentation, the publisher may have deleted the file from their server.


- - - - - - - - - - - - - - - - - - - - - - - - - - E N D - - - - - - - - - - - - - - - - - - - - - - - - - -

Presentation Transcript


Detection of integrated sachs wolfe effect by cross correlation of the

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)

[email protected]


Detection of integrated sachs wolfe effect by cross correlation of the

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


Detection of integrated sachs wolfe effect by cross correlation of the

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)

……………


Detection of integrated sachs wolfe effect by cross correlation of the

Statistics of CMB Sky

Geometry of our universe

ISW effect


Detection of integrated sachs wolfe effect by cross correlation of the

  • Observation of CMB first peak alone does not guarantee the existence of dark energy.

  • We are living in low density universe, i.e., m0.3. 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


Detection of integrated sachs wolfe effect by cross correlation of the

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


Detection of integrated sachs wolfe effect by cross correlation of the

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


Detection of integrated sachs wolfe effect by cross correlation of the

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


Detection of integrated sachs wolfe effect by cross correlation of the

Inhomogeneity

Cosmological constant

Dark energy


Detection of integrated sachs wolfe effect by cross correlation of the

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


Detection of integrated sachs wolfe effect by cross correlation of the

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


Detection of integrated sachs wolfe effect by cross correlation of the

  • 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


Detection of integrated sachs wolfe effect by cross correlation of the

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


Detection of integrated sachs wolfe effect by cross correlation of the

  • 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


Detection of integrated sachs wolfe effect by cross correlation of the

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)


Detection of integrated sachs wolfe effect by cross correlation of the

Contribution to Signal from different Redshift

Crittenden & Turok PRL 1996


Detection of integrated sachs wolfe effect by cross correlation of the

First detection of the cross-correlation

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

wiNiwjTj/wiwj

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

Boughn & Crittenden, nature, 2004


Detection of integrated sachs wolfe effect by cross correlation of the

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)


Detection of integrated sachs wolfe effect by cross correlation of the

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


Detection of integrated sachs wolfe effect by cross correlation of the

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 0z2 distribution


Detection of integrated sachs wolfe effect by cross correlation of the

Detail II

41GHz

61GHz

T

T

Q

Q

U

U


Detection of integrated sachs wolfe effect by cross correlation of the

Result I


Detection of integrated sachs wolfe effect by cross correlation of the

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


Detection of integrated sachs wolfe effect by cross correlation of the

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>


Detection of integrated sachs wolfe effect by cross correlation of the

Result II


Detection of integrated sachs wolfe effect by cross correlation of the

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.


  • Login