Cosmic Microwave Background Introductionjgl/a736/cmb_chasse_slides.pdf · Very accurate measurement of the cosmic microwave background anisotropies has enabled very accurate measurent

Cosmic Microwave BackgroundIntroduction

Matt Chassechasse@hawaii.edu

Department of Physics

University of Hawaii at Manoa

Honolulu, HI 96816

Matt Chasse, CMB Intro, May 3, 2005 – p. 1/29

Outline

CMB, what is it good for?

Standard Model of Cosmology

Acoustic Peaks

Polarization

WMAP

Matt Chasse, CMB Intro, May 3, 2005 – p. 2/29

Lots of Good Stuff

Just a few from WMAP...

Total matter density,Ωtot = 1.02+0.02−0.02

Dark energy density,ΩΛ = 0.73+0.04−0.04

Matter density,Ωm = 0.27+0.04−0.04

Baryon density,Ωb = 0.044+0.04−0.04

Hubble constant,h = 0.71+0.04−0.03

Number of light neutrinos

Neutrino mass

Matt Chasse, CMB Intro, May 3, 2005 – p. 3/29

Parameters Table

Matt Chasse, CMB Intro, May 3, 2005 – p. 4/29

Parameters Table (con’t)

Matt Chasse, CMB Intro, May 3, 2005 – p. 5/29

"Big Bang"

Source "http://outreach.web.cern.ch/outreach/public/cern/PicturePacks/BigBang/BigBang.JPG"

Matt Chasse, CMB Intro, May 3, 2005 – p. 6/29

Standard Model Conditions

Before recombination the cosmic plasma is nearly homogeneous, isotropic,

and in thermal equilibrium. The emitted radiation follows an almost perfect

blackbody spectrum. As the temperature of the plasma drops below29670K

it becomes optically transparent.

The baryon-photon fluid is believed to be initially perturbed by small

variations in curvature introduced in inflation and oscillates on a cold dark

matter background. But it can also develop disturbances dueto it’s own

gravitational instabilities; there are isocurvature models which use this as the

sole source.

Matt Chasse, CMB Intro, May 3, 2005 – p. 7/29

Surface of Last Scattering

Source "NASA/WMAP Science Team"

Matt Chasse, CMB Intro, May 3, 2005 – p. 8/29

Acoustic Horizon

Matt Chasse, CMB Intro, May 3, 2005 – p. 9/29

CMB sky

After dipole moment is removed, the tempuraturevariations are 1:100,000 (2.7K:10µK). Dipole variationis 1:1000.

Source "NASA/WMAP Science Team"

Matt Chasse, CMB Intro, May 3, 2005 – p. 10/29

Spherical Harmonics

The angular temperature distribution is described using spherical

harmonics.

∆T (θ, φ) =l=∞∑

l=0,m=−l..l

almYlm(θ, φ)

When there is no preferred direction in space the temperature

distribution can be described by just thel-values. The correlation

between parts of the CMB sky with angular separationθ ≈ 2π/l is

described byCl.

Cl =∑

m

|alm|2/(2l + 1)

Matt Chasse, CMB Intro, May 3, 2005 – p. 11/29

CMB Power Spectrum

Source "Wayne Hu’s website"

Matt Chasse, CMB Intro, May 3, 2005 – p. 12/29

Effect of Ωb

Source "Wayne Hu’s website"

Baryon loading adds effective mass and shifts the equilibrium point

of the oscillations, enhancing the odd numbered peaks in the

spectrum. It also decreases the speed of sound, which shiftsthe

power spectrum to higherl-values.

Matt Chasse, CMB Intro, May 3, 2005 – p. 13/29

Baryon Loading

Source "Wayne Hu’s website"

Matt Chasse, CMB Intro, May 3, 2005 – p. 14/29

Diffusion Damping

The photons aren’t perfectly coupled to the baryons. As the mean

free path for the photons overtakes the wavelength of the

oscillations, they spread energy from the hot areas to the cold ones

and create damping.

Source "Wayne Hu’s website"Matt Chasse, CMB Intro, May 3, 2005 – p. 15/29

Diffusion Damping

Source "Wayne Hu’s website"

Matt Chasse, CMB Intro, May 3, 2005 – p. 16/29

Effect of Ωtot

Source "Wayne Hu’s website"

WhenΩtot = 1, the density of the universe is such that it is spatially

flat. For a closed (Ωtot > 1) universe the CMB anisotropies will

subtend larger angles in the sky for a given length scale, shifting the

power spectrum to lowerl-values.Matt Chasse, CMB Intro, May 3, 2005 – p. 17/29

Power Spectrum and Ωtot

Source "Wayne Hu’s website"

Matt Chasse, CMB Intro, May 3, 2005 – p. 18/29

Polarization

The differences in intensity in the CMB cause polarization at small

scales.

Source "Wayne Hu’s website"

Matt Chasse, CMB Intro, May 3, 2005 – p. 19/29

Polarization

The polarization distribution gives information on quadrapole

anisotropies that can be used to find gravity waves in the CMB.

Polarization distributions also give information on scattering that

can help to further constrain the power spectrum.

Matt Chasse, CMB Intro, May 3, 2005 – p. 20/29

Conditions Effecting Observation

Sachs-Wolfe Effect - Photons from denser regionsare gravitationally red-shifted. Net result is thathotter, denser regions in the CMB appear cooler.

Integrated Sachs-Wolfe (ISW) Effect - As photonstravel through changing gravitational potentials theyacquire a net red/blue-shift.

Doppler Shift - Shows up in dipole moments.

Secondary Scattering from intervening material -Reionization. Secondary scattering has less of aneffect on lower multipoles.

Matt Chasse, CMB Intro, May 3, 2005 – p. 21/29

Wilson Anisotropy Probe (WMAP)

Source "NASA/WMAP Science Team"

Matt Chasse, CMB Intro, May 3, 2005 – p. 22/29

Wilson Anisotropy Probe (WMAP)

Systematics are reduced by taking the difference between the signals

from the opposite facing dishes.

Source "NASA/WMAP Science Team"

Matt Chasse, CMB Intro, May 3, 2005 – p. 23/29

Far Away from Noisy Earth

WMAP Orbits around the L2 lagrange point.

Source "NASA/WMAP Science Team"

Matt Chasse, CMB Intro, May 3, 2005 – p. 24/29

Measurement By Wilson AnisotropyProbe (WMAP)

Source "NASA/WMAP Science Team"

The galaxy signal and random noise are partially removed by cross

correlating different channels (frequencies from "most red"): 23GHz

(K-Band), 33Ghz (Ka-Band), 41GHz (Q-Band), 61GHz (V-Band),

94Ghz (W-Band).

Matt Chasse, CMB Intro, May 3, 2005 – p. 25/29

Measurement By Wilson AnisotropyProbe (WMAP)

But foreground still remains and the area around the galaxy needs to

be masked out. WMAP uses several masks for the galaxy: Kp0

leaves 76.8% of the sky, Kp2 leaves 85.0%, Kp12 leaves 95%.

Known point sources also have to be masked out.

Source "NASA/WMAP Science Team"

Matt Chasse, CMB Intro, May 3, 2005 – p. 26/29

Obtaining the Cl power spectrum

The masking has a larger impact on lowerl-values. If afraction of the skyfsky is sampled then the errors scale

up byf− 1

2

sky. For eachl there arem statisticallyindependant samples which produces an error of:

∆Cl =

√

2

2l + 1Cl

A more conservative mask reduces random errors butintroduces more systematic error.

Matt Chasse, CMB Intro, May 3, 2005 – p. 27/29

Conclusion

Very accurate measurement of the cosmic microwavebackground anisotropies has enabled very accuratemeasurent of many cosmological parameters andinformation on almost all of them.

Measurement of the polarization will yeild even moreinformation.

Matt Chasse, CMB Intro, May 3, 2005 – p. 28/29

Thank You/Refernces

Thanks to Istvan Szapudi, John Tonry, and John Learned.

References

[1] Wayne Hu’s website available at: http://background.uchicago.edu/˜ whu/

[2] WMAP website available at: http://map.gsfc.nasa.gov/

[3] Lambda website available at: http://lambda.gsfc.nasa.gov/

[4] Wayne Hu, Scott Dodelson, Annu. Rev. Astron. Astrophys 2002,

astro-ph/0110414

[5] Istvan Szapudi, Pablo Fosalba, astro-ph/04055589

Matt Chasse, CMB Intro, May 3, 2005 – p. 29/29