Angelica de Oliveira-CostaUniversity of Pennsylvania

The Cosmic Microwave Background:

New Challenges.

XI Advanced School of Astrophysics Campos do Jordao, September

2002

The Importance of CMB Polarization:

1. Polarization measurements can substantially improve accuracy with which parameters are measured by breaking the degeneracy between certain parameter combinations.2. It also offers an independent test of the basic assumptions that underly the standard cosmological model.

Where does CMB Polarization comes from (Hu & White 1997)?

CMB polarization is induced via Thomson scattering, either at decoupling or during a later epoch of reonization.

The level of polarization induced is linked to the local quadrupole anisotropy of radiation incident on the scattering eletrons. The level of polarization is expected to be 1%-10% of the amplitude of the temperature anisotropies.

Under coordinate transformations, the Q and U maps transform into a “vector” field on the celestial sphere described by the quantities E and B.E and B can correlate with each other, and with the temperature T. By parity, <EB> and <TB> are zero, <TE> has the largest signal, <EE> is smaller, and <BB> should be zero (except for the cases of gravity-waves present in the last scattering or the existence of polarized foregrounds).

Important things to know (Kamionkowski et al. 1997,

Zaldarriaga 1998):

TT TE TB

TE EE EBTB EB BB

Matter Buget

1. g = Photons

2. b = Baryons (H,He,…)

3. d = CDM

4. fu = Neutrinos

5. L = Lambda (Dark Energy)

6. k = Curvature

Input Fluctuations

7. As = Scalar Normalization

8. At = Tensor Normalization

9. ns = Scalar Tilt

10. nt = Tensor Tilt

Gastrophysics

11. = Reonization Optical Depth

From Combinations of Parameters

12. h = Hubble Constant

Others

Foregrounds, Topology, Defects, etc.

Our Cosmological Model: Polarization Movies:

www.hep.upenn.edu/~angelica/polarization.html

Matter Buget

1. g = Photons

2. b = Baryons (H,He,…)

3. d = CDM

4. fu = Neutrinos

5. L = Lambda (Dark Energy)

6. k = Curvature

Input Fluctuations

7. As = Scalar Normalization

8. At = Tensor Normalization

9. ns = Scalar Tilt

10. nt = Tensor Tilt

Gastrophysics

11. = Reonization Optical Depth

From Combinations of Parameters

12. h = Hubble Constant

Others

Foregrounds, Topology, Defects, etc.

Our Cosmological Model: Polarization Movies:

www.hep.upenn.edu/~angelica/polarization.html

Matter Buget

1. g = Photons

2. b = Baryons (H,He,…)

3. d = CDM (d = d h2)

4. fu = Neutrinos

5. L = Lambda (Dark Energy)

6. k = Curvature

Input Fluctuations

7. As = Scalar Normalization

8. At = Tensor Normalization

9. ns = Scalar Tilt

10. nt = Tensor Tilt

Gastrophysics

11. = Reonization Optical Depth

From Combinations of Parameters

12. h = Hubble Constant

Others

Foregrounds, Topology, Defects, etc.

Our Cosmological Model: Polarization Movies:

www.hep.upenn.edu/~angelica/polarization.html

Matter Buget

1. g = Photons

2. b = Baryons (H,He,…)

3. d = CDM

4. fu = Neutrinos (fn =HDM/T)

5. L = Lambda (Dark Energy)

6. k = Curvature

Input Fluctuations

7. As = Scalar Normalization

8. At = Tensor Normalization

9. ns = Scalar Tilt

10. nt = Tensor Tilt

Gastrophysics

11. = Reonization Optical Depth

From Combinations of Parameters

12. h = Hubble Constant

Others

Foregrounds, Topology, Defects, etc.

Our Cosmological Model: Polarization Movies:

www.hep.upenn.edu/~angelica/polarization.html

Matter Buget

1. g = Photons

2. b = Baryons (H,He,…)

3. d = CDM

4. fu = Neutrinos

5. L = Lambda (Dark Energy)

6. k = Curvature

Input Fluctuations

7. As = Scalar Normalization

8. At = Tensor Normalization

9. ns = Scalar Tilt

10. nt = Tensor Tilt

Gastrophysics

11. = Reonization Optical Depth

From Combinations of Parameters

12. h = Hubble Constant

Others

Foregrounds, Topology, Defects, etc.

Our Cosmological Model: Polarization Movies:

www.hep.upenn.edu/~angelica/polarization.html

Matter Buget

1. g = Photons

2. b = Baryons (H,He,…)

3. d = CDM

4. fu = Neutrinos

5. L = Lambda (Dark Energy)

6. k = Curvature

Input Fluctuations

7. As = Scalar Normalization

8. At = Tensor Normalization

9. ns = Scalar Tilt

10. nt = Tensor Tilt

Gastrophysics

11. = Reonization Optical Depth

From Combinations of Parameters

12. h = Hubble Constant

Others

Foregrounds, Topology, Defects, etc.

Our Cosmological Model: Polarization Movies:

www.hep.upenn.edu/~angelica/polarization.html

Matter Buget

1. g = Photons

2. b = Baryons (H,He,…)

3. d = CDM

4. fu = Neutrinos

5. L = Lambda (Dark Energy)

6. k = Curvature

Input Fluctuations

7. As = Scalar Normalization

8. At = Tensor Normalization

9. ns = Scalar Tilt

10. nt = Tensor Tilt

Gastrophysics

11. = Reonization Optical Depth

From Combinations of Parameters

12. h = Hubble Constant

Others

Foregrounds, Topology, Defects, etc.

Our Cosmological Model: Polarization Movies:

www.hep.upenn.edu/~angelica/polarization.html

Matter Buget

1. g = Photons

2. b = Baryons (H,He,…)

3. d = CDM

4. fu = Neutrinos

5. L = Lambda (Dark Energy)

6. k = Curvature

Input Fluctuations

7. As = Scalar Normalization

8. At = Tensor Normalization

9. ns = Scalar Tilt

10. nt = Tensor Tilt

Gastrophysics

11. = Reonization Optical Depth

From Combinations of Parameters

12. h = Hubble Constant

Others

Foregrounds, Topology, Defects, etc.

Our Cosmological Model: Polarization Movies:

www.hep.upenn.edu/~angelica/polarization.html

Matter Buget

1. g = Photons

2. b = Baryons (H,He,…)

3. d = CDM

4. fu = Neutrinos

5. L = Lambda (Dark Energy)

6. k = Curvature

Input Fluctuations

7. As = Scalar Normalization

8. At = Tensor Normalization

9. ns = Scalar Tilt

10. nt = Tensor Tilt

Gastrophysics

11. = Reonization Optical Depth

From Combinations of Parameters

12. h = Hubble Constant

Others

Foregrounds, Topology, Defects, etc.

Our Cosmological Model: Polarization Movies:

www.hep.upenn.edu/~angelica/polarization.html

Matter Buget

1. g = Photons

2. b = Baryons (H,He,…)

3. d = CDM

4. fu = Neutrinos

5. L = Lambda (Dark Energy)

6. k = Curvature

Input Fluctuations

7. As = Scalar Normalization

8. At = Tensor Normalization

9. ns = Scalar Tilt

10. nt = Tensor Tilt

Gastrophysics

11. = Reonization Optical Depth

From Combinations of Parameters

12. h = Hubble Constant

Others

Foregrounds, Topology, Defects, etc.

Our Cosmological Model: Polarization Movies:

www.hep.upenn.edu/~angelica/polarization.html

Princeton IQU Experiment (PIQUE):

Ground based experiment (roof of Jadwin Hall).FWHM = 0.235o (100<l<600).Operates at 90 (and 40) GHz.Scans a ring of radius 1o around the NCP (144 pixels).

Hedman et al. (2001)

Sensitivity ~ 3KHEMT correlation receiver.

Team:

M. Hedman

D. BarkatsJ. Gundersen

S. StaggsB. Winstein

A. de Oliveira-CostaM. TegmarkM. Zaldarriaga

Part of analysis effort:

Expected foregrounds < 0.5K.

PIQUE Analysis:

Headman et al. (2001):TE <14K 211 (+294,-146)TB <13K 212 (+229,-135)TE(TB=0) <10K

de Oliveira-Costa et al (2002):TTE <17K

TTB <20K

We compute 5 power spectra T,E,B,TE & TB with a QE method, and later complement it with the Likelihood analysis.

TSK =50K

Netterfield et al. (1997):

TEB ???

50 bands w/ dl=20 till l=1000

To do better we need reduce PIQUE pixel noise.

Polarization Observations of the Large Angular Regions (POLAR):

Ground based experiment (Madison, WI).FWHM=7o (2<l<20).Operates at 30 GHzScans at fixed =43o (300 pixels).

O’Dell (2002)

Keating et al. (2001)

Expected sensitivity ~ 1-5K.HEMT correlation receiver.

Team:B. KeatingC. O’Dell

P. Timbie

A. PolnarevJ. Steinberger

Part of analysis effort:A. de Oliveira-

CostaM. Tegmark

POLAR Results:

O’Dell, Ph.D Thesis (2002)

Keating et al. (2001):

TE <10K

TB <10K

TE(TB=0) < 8K

de Oliveira-Costa et al (2002):

TTE <13K

TTB <11K

TDMR =20K

Smoot et al. (1992):

TEB < 4K

3 bands w/ dl=10 till l=30

(Normalized Likelihood Contours)

(Band power estimates - same results when average the bands)

“Leakage”: Tegmark & de Oliveira-Costa et al. (2001).

1. E and B are symmetric:

2. Leakage drops with l (E/B

3. Map-shape is important:

4. Sensitivity is negligible

variance is dominant, this

There are equal leakage from

E to B and vise-versa.

separation works well for

l>>dl).

The narrowest dimension of

the map is the limiting factor.

compared with sky coverage:In a situation where sample

tends to make windowns

slightly lobsided.

B2002, l=20: B2002, l=70:

Circle, l=70:

B2002, l=20 (disentangle):

5. There is no leakage between T & TE and E & TE.

6. There is no leakage between TE & TB, E & EB and B & EB: de Oliveira-Costa et al. (2002). 7. Leakage between E & B can be completed removed: Bunn et al. (2002).

Balloon Observations Of Millimetric Extragalactic Radiation

ANd Geophysics (BOOMERanG):

Ballon experiment (two 10 day flight).Operates between 150 to 450 GHz.

FWHM=10’ (50<l<1000).

Bolometers. Sensitivity ~ 7K (“small regions”) and ~22K otherwise.

2nd flight: 80 & 800(o)2.

de Bernardis et al. (2000)

1st flight: 80 & 800(o)2.

Team:UCSB: J. Ruhl, K. Coble, T. Montroy, E. TorbetCaltech: A. Lange, B. Crill, V. Hristov, B. Jones, K. Ganga, P. MansonJPL: J. BockU.Mass: P. MauskopfU.Penn: A. de Oliveira-Costa, M. TegmarkU.Toronto: B. NetterfieldU.La Sapienza: P. de Bernardis, S. Masi, F. Piacentini, F. Scaramuzzi, N. VittorioIROE: A. BoscareliQueen Mary: P. Ade

Microwave Anisotropy Probe (MAP):

Frequencies(GHz): 22 30 40 60 90

FWHM(): 0.93 0.68 0.53 0.35 0.23

Sensitivity: ~35K (all channels & 0.3 x 0.3 pixels)Detector: Differential Radiometer (with polarization)

More info at: http://map.gsfc.nasa.gov

Data release: Jan 2003! Data from 1st full sky scan

Other CMB Polarization Experiments:

Experiment FWHM n(GHz) Receiver Sensitivity Area Site

Polatron 2.5’ 100 Bolometer 11K 5313(’)2 OVRO

†RoPE 2o 9 HEMT 5K 560(o)2 LBNL Compass 15’ 30,40&90 HEMT 8K U.Wisc.

MAP 13-41’ 30,40,60&90 HEMT 19K All sky Space L2

Planck-LFI 14’&10’ 70&100 HEMT 6K All sky Space L2

Planck-HFI 8’&5’ 143&217 Bolometer 6K All sky Space L2SPOrt 7o 22,32,60&90 HEMT 80% sky Space Station

(300<l<2000)

(2<l<50)

(l<650)

(l<600)

(l<1500)

(2<l<20)

BOOMERanG 10’ 150,250&450 Bolometer 7K,22K 80-800(o)2 SP (50<l<1000)

Maxipol 10’ 140&420 Bolometer 1.4K NM

DASI 10-15’ 30 HEMT 10(o)2 SP(100<l<900)

CBI 3’-6o 30 Interferometer 3 of 100(o)2 Atacama (2<l<2000)

CapMap 3’ 30,90 HEMT 0.2K 3(o)2 Princeton (300<l<2000)

Small Scale CMB Experiments:

We propose a Center for High Resolution CMB studies (CfHRC). This center will develop a Millimeter Bolometer Camera (MBC) which will be implemented in the Atacama Cosmology Teslescopy (ACT).

Operates at frequencies 145, 225 & 265 GHz.Ground based experiment at Atacama desert, Chile.

Sensitivity/pixel ~ 2, 8 & 16K (64 nights of quality data).

FWHM=1.7, 1.1 & 0.93’.Scans only in azimuth with the ability to cross-link elevations.

Team:

Haverford: S. Boughn, B. Partridge

U.Penn: A. de Oliveira-Costa, M. Devlin, B. Jain, M. Tegmark

Princeton: N. Jarosik, R. Lupton, L. Page, U. Seljak, D. Spergel, S. Staggs, D. Wilkinson

Rutgers: A. Kosowsky

U.Toronto: B. Netterfield

NASA/GSFC: H. Moseley

NIST: K. Irwin

CfHRC Goals:

Measure the primary anisotropy beyond the MAP & Planck resolution limits.

Measure the amplitude of the CMB gravitational lensing, and therefore probe the mass power spectrum at 1Mpc scales at z~1-2.

Find galaxy clusters at z<1 through SZ effect.

Detect signature of reonization at z~10 through Vishniac effect.

Find all extragalactic mm-wave point sources in 200(o)2 to a sensitivity of 1mJy.

Galactic Microwave Emission:

Objectives

1. Accurate modeling and subtraction of Galactic foreground contamination in order to correct measure the CMB power spectrum.

2. Unique opportunity to understand the Galactic emission processes between 10 to 103 GHz.

Smoot et al. (1992)

Galactic Microwave Emission:

Objectives

1. Accurate modeling and subtraction of Galactic foreground contamination in order to correct measure the CMB power spectrum.

2. Unique opportunity to understand the Galactic emission processes between 10 to 103 GHz.

Smoot et al. (1992)

Synchrotron Emission:

Dust Emission:

Free-Free Emission:

Reynolds et al. (2001)

COBE/DMR

At 31GHz we expect DIRBE traces free-free.

Smoot et al. (1992)

Saskatoon

OVRO result (Leitch et al. 1997) is much higher than expected for a free-free component.

19 GHz

Spinning dust grains predicts a turn-over at lower frequencies (Draine & Lazarian 1998).

QMAP

Tenerife

Smoking gun: evidence for a turn-over and WHAM correlations only at b<15o.

Jones (1999)

Galactic Microwave Emission:

Objectives

1. Accurate modeling and subtraction of Galactic foreground contamination in order to correct measure the CMB power spectrum.

2. Unique opportunity to understand the Galactic emission processes between 10 to 103 GHz.

Smoot et al. (1992)

Galactic Microwave Emission:

Objectives

1. Accurate modeling and subtraction of Galactic foreground contamination in order to correct measure the CMB power spectrum.

2. Unique opportunity to understand the Galactic emission processes between 10 to 103 GHz.

Smoot et al. (1992)

QMAP Foregrounds:

QMAP Power Spectrum:

Polarized Foregrounds:

Residual foregrounds after cleaning 5 MAP channels:

Conclusions:

CMB Polarization is likely to be a goldmine of cosmological information, allowing improved measurements of many cosmological parameters and numerous important cross-checks and tests of the underlying theory.

CMB Small Angular Scale maps enables new fundamental cosmological tests.

Our ability to measure cosmological parameters using the CMB will only be as good as our understanding of the microwave foregrounds.