Angelica de Oliveira-Costa

1
The Cosmic Microwave Background
New Challenges.
Angelica de Oliveira-Costa
University of Pennsylvania
XI Advanced School of Astrophysics
Campos do Jordao, September 2002
2
Cosmology Overview
The Hot Big Bang Model
1. Expansion.
2. Large-scale homogeneity isotropy.
3. Primordial nucleosynthesis.
4. CMB.
3
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.
4
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.
Important things to know (Kamionkowski et al.
1997, Zaldarriaga 1998)
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, ltEBgt and ltTBgt are
zero, ltTEgt has the largest signal, ltEEgt is
smaller, and ltBBgt should be zero (except for the
cases of gravity-waves present in the last
scattering or the existence of polarized
foregrounds).
TT TE TB
TE EE EB
TB EB BB
5
Our Cosmological Model
Polarization Movies
Matter Buget 1. g Photons 2. wb
Baryons (H,He,) 3. wd CDM 4.
fu Neutrinos 5. WL Lambda (Dark
Energy) 6. Wk Curvature Input
Fluctuations 7. As Scalar Normalization
8. At Tensor Normalization 9. ns
Scalar Tilt 10. nt Tensor
Tilt Gastrophysics 11. t Reonization
Optical Depth From Combinations of Parameters
12. h Hubble Constant Others Foregrounds,
Topology, Defects, etc.
www.hep.upenn.edu/angelica/polarization.html
6
Our Cosmological Model
Polarization Movies
Matter Buget 1. g Photons 2. wb
Baryons (H,He,) 3. wd CDM 4.
fu Neutrinos 5. WL Lambda (Dark
Energy) 6. Wk Curvature Input
Fluctuations 7. As Scalar Normalization
8. At Tensor Normalization 9. ns
Scalar Tilt 10. nt Tensor
Tilt Gastrophysics 11. t Reonization
Optical Depth From Combinations of Parameters
12. h Hubble Constant Others Foregrounds,
Topology, Defects, etc.
www.hep.upenn.edu/angelica/polarization.html
7
Our Cosmological Model
Polarization Movies
Matter Buget 1. g Photons 2. wb
Baryons (H,He,) 3. wd CDM (wd Wd
h2) 4. fu Neutrinos 5. WL
Lambda (Dark Energy) 6. Wk
Curvature Input Fluctuations 7. As Scalar
Normalization 8. At Tensor Normalization
9. ns Scalar Tilt 10. nt Tensor
Tilt Gastrophysics 11. t Reonization
Optical Depth From Combinations of Parameters
12. h Hubble Constant Others Foregrounds,
Topology, Defects, etc.
www.hep.upenn.edu/angelica/polarization.html
8
Our Cosmological Model
Polarization Movies
Matter Buget 1. g Photons 2. wb
Baryons (H,He,) 3. wd CDM 4.
fu Neutrinos (fn WHDM/WT) 5. WL
Lambda (Dark Energy) 6. Wk
Curvature Input Fluctuations 7. As Scalar
Normalization 8. At Tensor Normalization
9. ns Scalar Tilt 10. nt Tensor
Tilt Gastrophysics 11. t Reonization
Optical Depth From Combinations of Parameters
12. h Hubble Constant Others Foregrounds,
Topology, Defects, etc.
www.hep.upenn.edu/angelica/polarization.html
9
Our Cosmological Model
Polarization Movies
Matter Buget 1. g Photons 2. wb
Baryons (H,He,) 3. wd CDM 4.
fu Neutrinos 5. WL Lambda (Dark
Energy) 6. Wk Curvature Input
Fluctuations 7. As Scalar Normalization
8. At Tensor Normalization 9. ns
Scalar Tilt 10. nt Tensor
Tilt Gastrophysics 11. t Reonization
Optical Depth From Combinations of Parameters
12. h Hubble Constant Others Foregrounds,
Topology, Defects, etc.
www.hep.upenn.edu/angelica/polarization.html
10
Our Cosmological Model
Polarization Movies
Matter Buget 1. g Photons 2. wb
Baryons (H,He,) 3. wd CDM 4.
fu Neutrinos 5. WL Lambda (Dark
Energy) 6. Wk Curvature Input
Fluctuations 7. As Scalar Normalization
8. At Tensor Normalization 9. ns
Scalar Tilt 10. nt Tensor
Tilt Gastrophysics 11. t Reonization
Optical Depth From Combinations of Parameters
12. h Hubble Constant Others Foregrounds,
Topology, Defects, etc.
www.hep.upenn.edu/angelica/polarization.html
11
Our Cosmological Model
Polarization Movies
Matter Buget 1. g Photons 2. wb
Baryons (H,He,) 3. wd CDM 4.
fu Neutrinos 5. WL Lambda (Dark
Energy) 6. Wk Curvature Input
Fluctuations 7. As Scalar Normalization
8. At Tensor Normalization 9. ns
Scalar Tilt 10. nt Tensor
Tilt Gastrophysics 11. t Reonization
Optical Depth From Combinations of Parameters
12. h Hubble Constant Others Foregrounds,
Topology, Defects, etc.
www.hep.upenn.edu/angelica/polarization.html
12
Our Cosmological Model
Polarization Movies
Matter Buget 1. g Photons 2. wb
Baryons (H,He,) 3. wd CDM 4.
fu Neutrinos 5. WL Lambda (Dark
Energy) 6. Wk Curvature Input
Fluctuations 7. As Scalar Normalization
8. At Tensor Normalization 9. ns
Scalar Tilt 10. nt Tensor
Tilt Gastrophysics 11. t Reonization
Optical Depth From Combinations of Parameters
12. h Hubble Constant Others Foregrounds,
Topology, Defects, etc.
www.hep.upenn.edu/angelica/polarization.html
13
Our Cosmological Model
Polarization Movies
Matter Buget 1. g Photons 2. wb
Baryons (H,He,) 3. wd CDM 4.
fu Neutrinos 5. WL Lambda (Dark
Energy) 6. Wk Curvature Input
Fluctuations 7. As Scalar Normalization
8. At Tensor Normalization 9. ns
Scalar Tilt 10. nt Tensor
Tilt Gastrophysics 11. t Reonization
Optical Depth From Combinations of Parameters
12. h Hubble Constant Others Foregrounds,
Topology, Defects, etc.
www.hep.upenn.edu/angelica/polarization.html
14
Our Cosmological Model
Polarization Movies
Matter Buget 1. g Photons 2. wb
Baryons (H,He,) 3. wd CDM 4.
fu Neutrinos 5. WL Lambda (Dark
Energy) 6. Wk Curvature Input
Fluctuations 7. As Scalar Normalization
8. At Tensor Normalization 9. ns
Scalar Tilt 10. nt Tensor
Tilt Gastrophysics 11. t Reonization
Optical Depth From Combinations of Parameters
12. h Hubble Constant Others Foregrounds,
Topology, Defects, etc.
www.hep.upenn.edu/angelica/polarization.html
15
Princeton IQU Experiment (PIQUE)
Ground based experiment (roof of Jadwin Hall).
FWHM 0.235o (100ltllt600).
Operates at 90 (and 40) GHz.
Scans a ring of radius 1o around the NCP (144
pixels).
HEMT correlation receiver.
Sensitivity 3mK
Expected foregrounds lt 0.5mK.
Team
D. Barkats
J. Gundersen
M. Hedman
S. Staggs
B. Winstein
Part of analysis effort
A. de Oliveira-Costa
M. Tegmark
M. Zaldarriaga
Hedman et al. (2001)
16
PIQUE Analysis
We compute 5 power spectra T,E,B,TE TB with a
QE method, and later complement
it with the Likelihood analysis.
50 bands w/ dl20 till l1000
Netterfield et al. (1997)
dTSK 50mK
Headman et al. (2001)
dTE lt14mK 211 (294,-146)
dTB lt13mK 212 (229,-135)
dTE(dTB0) lt10mK
de Oliveira-Costa et al (2002)
dTTE lt17mK
dTTB lt20mK
dTEB ???
To do better we need reduce PIQUE pixel noise.
17
Polarization Observations of the Large Angular
Regions (POLAR)
Ground based experiment (Madison, WI).
FWHM7o (2ltllt20).
Operates at 30 GHz
Scans at fixed d43o (300 pixels).
HEMT correlation receiver.
Expected sensitivity 1-5mK.
ODell (2002)
Team
B. Keating
C. ODell
A. Polnarev
J. Steinberger
P. Timbie
Part of analysis effort
A. de Oliveira-Costa
M. Tegmark
Keating et al. (2001)
18
POLAR Results
3 bands w/ dl10 till l30
Smoot et al. (1992)
dTDMR 20mK
Keating et al. (2001)
(Normalized Likelihood Contours)
dTE lt10mK
dTB lt10mK
dTE(dTB0) lt 8mK
de Oliveira-Costa et al (2002)
(Band power estimates - same results when average
the bands)
dTTE lt13mK
dTTB lt11mK
dTEB lt 4mK
ODell, Ph.D Thesis (2002)
19
Leakage Tegmark de Oliveira-Costa et al.
(2001).
B2002, l20
B2002, l70
1. E and B are symmetric
There are equal leakage from
E to B and vise-versa.
2. Leakage drops with l (E/B
separation works well for
lgtgtdl).
3. Map-shape is important
The narrowest dimension of
Circle, l70
B2002, l20 (disentangle)
the map is the limiting factor.
4. Sensitivity is negligible
compared with sky coverage
In a situation where sample
variance is dominant, this
tends to make windowns
slightly lobsided.
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).
20
Balloon Observations Of Millimetric Extragalactic
Radiation
ANd Geophysics (BOOMERanG)
Ballon experiment (two 10 day flight).
FWHM10 (50ltllt1000).
de Bernardis et al. (2000)
Operates between 150 to 450 GHz.
1st flight 80 800(o)2.
2nd flight 80 800(o)2.
Bolometers.
Sensitivity 7mK (small regions) and 22mK
otherwise.
Team
UCSB J. Ruhl, K. Coble, T.
Montroy, E. Torbet
Caltech A. Lange, B. Crill, V.
Hristov, B. Jones, K. Ganga, P. Manson
JPL J. Bock
U.Mass P. Mauskopf
U.Penn A. de Oliveira-Costa, M.
Tegmark
U.Toronto B. Netterfield
U.La Sapienza P. de Bernardis, S. Masi, F.
Piacentini, F. Scaramuzzi, N. Vittorio
IROE A. Boscareli
Queen Mary P. Ade
21
Boomerang Performace
ltEEgt
Foregrounds are
Syn, Free-Free, dust, rot.dust PtS
22
Microwave Anisotropy Probe (MAP)
Frequencies(GHz) 22 30 40 60
90
FWHM(o) 0.93 0.68 0.53 0.35
0.23
Sensitivity 35mK (all channels
0.3o x 0.3o pixels)
Detector Differential Radiometer
(with polarization)
Data release Jan 2003! Data from 1st
full sky scan
More info at http//map.gsfc.nasa.gov
23
Other CMB Polarization Experiments
Experiment FWHM n(GHz)
Receiver Sensitivity Area
Site
CapMap 3 30,90
HEMT 0.2mK 3(o)2
Princeton
(300ltllt2000)
CBI 3-6o 30
Interferometer 3 of
100(o)2 Atacama
(2ltllt2000)
DASI 10-15 30
HEMT
10(o)2 SP
(100ltllt900)
Polatron 2.5 100
Bolometer 11mK 5313()2
OVRO
(300ltllt2000)

• RoPE 2o 9
  HEMT 5mK
  560(o)2 LBNL

(2ltllt50)
Compass 15 30,4090
HEMT 8mK
U.Wisc.
(llt650)
BOOMERanG 10 150,250450
Bolometer 7mK,22mK 80-800(o)2
SP
(50ltllt1000)
Maxipol 10 140420
Bolometer 1.4mK
NM
MAP 13-41 30,40,6090
HEMT 19mK All sky
Space L2
(llt600)
Planck-LFI 1410 70100
HEMT 6mK All sky
Space L2
(llt1500)
Planck-HFI 85 143217
Bolometer 6mK All sky
Space L2
SPOrt 7o 22,32,6090
HEMT 80 sky
Space Station
(2ltllt20)
24
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).
Ground based experiment at Atacama desert, Chile.
Operates at frequencies 145, 225 265 GHz.
FWHM1.7, 1.1 0.93.
Scans only in azimuth with the ability to
cross-link elevations.
Sensitivity/pixel 2, 8 16mK (64 nights of
quality data).
Team
Princeton N. Jarosik, R. Lupton, L. Page,
U. Seljak, D. Spergel, S. Staggs, D. Wilkinson
U.Penn A. de Oliveira-Costa, M. Devlin,
B. Jain, M. Tegmark
Haverford S. Boughn, B. Partridge
Rutgers A. Kosowsky
U.Toronto B. Netterfield
NASA/GSFC H. Moseley
NIST K. Irwin
25
CfHRC Goals
Measure the primary anisotropy beyond the MAP
Planck resolution limits.
Find galaxy clusters at zlt1 through SZ effect.
Measure the amplitude of the CMB gravitational
lensing, and therefore probe the mass power
spectrum at 1Mpc scales at z1-2.
Detect signature of reonization at z10 through
Vishniac effect.
Find all extragalactic mm-wave point sources in
200(o)2 to a sensitivity of 1mJy.
26
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)
27
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)
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29
Quantifying Galactic Emission in a CMB data
30
Synchrotron Emission
31
Dust Emission
32
Free-Free Emission
Reynolds et al. (2001)
33
COBE/DMR
Smoot et al. (1992)
At 31GHz we expect DIRBE traces free-free.
34
Saskatoon
OVRO result (Leitch et al. 1997) is much higher
than expected for a free-free component.
35
19 GHz
Spinning dust grains predicts a turn-over at
lower frequencies (Draine Lazarian 1998).
36
QMAP
37
QMAP
38
Tenerife
Jones (1999)
Smoking gun evidence for a turn-over and WHAM
correlations only at blt15o.
39
Frequency Dependence for 4 Latitude Slices
Colors are for DIRBE, Haslam WHAM
40
IRAS images from Cloud MBM20
A simple visual comparison of these images
suggests that although the large scale features
match up, small scale features can be quite
different.
Therefore spinning dust should be traced by
shorter wavelenght dust maps.
41
Dust Correlations for the 12-240mm DIRBE Maps
42
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)
43
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)
44
QMAP data analysis
We introduced new methods for removal of
1/f-noise and scan-synchronous offsets.
45
Xu et al. (2001)
Other experiments
Boomerang Maxima.
46
Tegmark Efstathiou (1996)
47
QMAP Foregrounds
48
QMAP Power Spectrum
49
Polarized Foregrounds
Residual foregrounds after cleaning 5 MAP
channels
50
Conclusions
Our ability to measure cosmological parameters
using the CMB will only be as good as our
understanding of the microwave foregrounds.
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.