wmap reionization: implications · 2017. 1. 3. · wmap reionization i. the case for early...
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WMAP Reionization:Implications
Asantha CoorayCaltech
Daniel Chalonge 8th Paris Cosmology Colloquium
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WMAP Reionization
I. The case for early star-formation
II. First-star signatures in Infrared
III. First-supernovae signature in small scale CMB via SZ
IV. A Complete Picture: (II) and (III) together and why?
Cooray, Bock, Keating, Lange & Matsumoto 2004 ApJ, in pressOh, Cooray & Kamionkowski 2003, MNRASCooray 2004, PRD in press
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http://map.gsfc.nasa.gov
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Douspis et al.
An interesting result
WMAP
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What is it?
z ~ 1000 6-40? Structure formation today
• last scattering: linear physics. Interesting signatures such asacoustic peaks.
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Gravitational EffectsScattering Effects
(via electrons)
Frequency shifts
z ~ 1000 6-40? Structure formation today
Lensing deflectionsTime-delays
Simple but an Important fact: changes to CMB from the local universe
What is it?
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Gravitational EffectsScattering Effects
(via electrons)
Frequency shifts
z ~ 1000 6-40? Structure formation today
Lensing deflectionsTime-delays
Simple but an Important fact: changes to CMB from the local universe
What is it?
Strong evidence for early reionization!!
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Reionized Signature: Scattering of CMB Quadrupole Produces Polarization
Reionization ⇒ Free electrons
Compton scattering of any local quadrupole by electrons lead to polarization
When primordial CMB anisotropies are projected
PPr im ∝τ Qrms(z) ∝ C2(z)
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Grad: Reionization
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PolarizationReionization ⇒ Free electrons
Compton scattering of any local quadrupole by electrons lead to polarization
When primordial CMB anisotropies are projected
PPr im ∝τ Qrms(z) ∝ C2(z)
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Galaxy Clusters ⇒ Tons of Free electrons
Compton scattering of the quadrupole lead to SZ polarization
When primordial CMB anisotropies are projected
PPr im ∝τ Qrms(z) ∝ C2(z)
At large scales, two sources of contribution to Cl= 2(z)
∆T
T=
Φ3 z= LSS
+ 2 dη dΦdη∫
Cosmologically Important contribution
SW ISW
Same, at 250 GHz
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(Reionization aids detection of Gravitational Waves)Cooray 2002
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Douspis et al.
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Douspis et al.
tau~0.17 +/- 0.04z_rei ~ 20 +/- 8
-----------
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Why the reionizationhistory may not beuniform?
(Fan et al. 2001)
Evidence from the Sloan Survey
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Why the reionizationhistory may not beuniform?
Evidence from the Sloan Survey
(Fan et al. 2001) Gunn-Peterson troughs-> Absorption by neutral Hydrogen
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What reionized the universe?
Leading candidates
1. UV radiation from stars
Most likely
2. UV radiation from AGNs
(not enough)
3. The exoticsdecaying dark matterdecaying neutrinos
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What reionized the universe?
Leading candidates
1. UV radiation from stars
Most likely
2. UV radiation from AGNs
(not enough)
3. The exoticsdecaying dark matterdecaying neutrinos
(Loeb, Haiman, Cen)
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Can we detect the signature of first stars directly?
First star spectrum
Black body
T~104.8 to 5 K
L~1038 M/Msolar
ergs sec-1
<~ Ledd
tlife~106 years
(Scherrer 2002; Bromm et al. 2002; Santos et al. 2001)
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Can we detect the signature of first stars directly?
First star spectrum
(Scherrer 2002; Bromm et al. 2002; Santos et al. 2001)
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Can we detect the signature of first stars directly?
First star spectrum
(Scherrer 2002; Bromm et al. 2002; Santos et al. 2001)
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Can we detect the signature of first stars directly?
First star spectrum
(Scherrer 2002; Bromm et al. 2002; Santos et al. 2001)
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Can we detect the signature of first stars directly?
First star spectrum
Model uncertaintiesbut the black-bodyspectrum of thestar alone ismore reliable
(Scherrer 2002; Bromm et al. 2002; Santos et al. 2001)
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Can we detect the signature of first stars directly?
A 300 Msunfirst star at z~15,K-band mag 33(unlikey to be
detectable)
First proto-galaxiescan contain as many as 105 stars.
(Still not detectable)
(Scherrer 2002; Bromm et al. 2002; Santos et al. 2001)
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Reionized by Stars: Reionization is not sudden
(atomic line cooling)
Theoretical expectation: Structure formation at high redshift is natural and the slow reionization follows naturally.
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Reionized by Stars: Reionization is not sudden
To reionize the universe:
A generation of stars(Pop IIIs, Pop IIs or II 1/2s)at z >> 20
If Pop III, top-heavy massfunction => massive stars
If Pop II, star-formationefficiency must be high(ie. relatively more stars)
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But, how (and even if stars, when)?
(stars)(particledecays)
(where scattering happensin CMB)
Both models give the same optical depth to scattering, but large scaleCMB polarization bump cannot be used to separate them precisely
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A 300 Msunfirst star at z~15,K-band mag 33(unlikey to be
detectable)
Can we detect the signature of first stars directly?
First proto-galaxiescan contain as many as 105 stars.
(Still not detectable)
Interesting wavelength range is 1 to 3 microns!!
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Lessons in IR: Observational realities
FIR
CMBIR
(Ned Wright)
Interesting wavelength range is 1 to 3 microns!!
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Interesting wavelength range is 1 to 3 microns!!
Lessons in IR: Absolute background Measured?
Near-IR
Far-IR
Optical
(Dole et al. 2003)
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Interesting wavelength range is 1 to 3 microns!!
Lessons in IR: Absolute background Measured?
(Dole et al. 2003)Near-IR
Far-IR
Optical
Dust-lightStar-light
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~1.6 microns
Problems in IR: Not enough stars at low redshifts?
The total near-IR absolute background cannot easily be explained withgalaxy counts alone. (Cambresy et al. 2001 and many others)
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~2.0 microns~2.2 microns
Problems in IR: Not enough stars at low redshifts?
The total near-IR absolute background cannot easily be explained withgalaxy counts alone. (Cambresy et al. 2001 and many others)
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Problems in IR: Not enough stars at low redshifts?Galaxy counts turnover at thefaint end
(SUBARU: Totani et al. 01)
⇒ The way out:
Background measurementsare wrong (unlikely, givenseveral independent sets ofdata)
Diffuse emissions (low-z low-surface brightness
galaxies or high-zfirst-galaxy population)
(With ISO, > 7.5 micron backgroundsmay be explained with extrapolated counts)
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First stars(either Pop III,Pop II 1/2or Pop IIs)can explain themissing amount
(Easier with Pop III)
Solutions in IR: First stars explain missing CIB?
First stars out to redshift of ~ 10
Santos, Bromm & Kamionkowski 2001
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First stars(either Pop III,Pop II 1/2or Pop IIs)can explain themissing amount
(Easier with Pop III)
Solutions in IR: First stars explain missing CIB?
First stars out to redshift of ~ 10
Many unknowns, a messy subject.Cooray & Yoshida 2004
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Can we detect the signature of first stars directly?
Evidence in the absolute background for a missing contributionnot related to local galaxies.
The search of first stars cannot be done with absolute backgroundmeasurements alone.
First star proto-galaxies will not be directly detectable with currentinstruments, but expectations are these will be with JWST.
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Can we detect the signature of first stars directly?
Evidence in the absolute background for a missing contributionnot related to local galaxies.
The search of first stars cannot be done with absolute backgroundmeasurements alone.
First star proto-galaxies will not be directly detectable with currentinstruments, but expectations are these will be with JWST.
Can we at least look for a potential hint ofsignificant star-formation at higher redshifts?
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Can we detect the signature of first stars directly?
Evidence in the absolute background for a missing contributionnot related to local galaxies.
The search of first stars cannot be done with absolute backgroundmeasurements alone.
First star proto-galaxies will not be directly detectable with currentinstruments, but expectations are these will be with JWST.
Consider spatial fluctuations in the unresolved IR background(after removing most resolved foreground galaxies down to
very deep magnitudes)
(essentially, do a CMB anisotropy type experiment in IR)
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Spatial fluctuations (captures how first-stars are clustered)
(Excess fluctuations at arcminute to few arcminute scales, wherefirst stars cluster)
IR Cls
Allowed Range
<~ few % fluctuations
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Spatial fluctuations (captures how first-stars are clustered)
IR Cls
Not just first-objects: the mess in between
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~1.6 microns
But faint z~3, galaxies may not be a problem
z~3 galaxies
The fractional contribution from z~3 galaxies to CIB is < 10%, while the missing amount > 50% (Cambresy et al. 2001 and many others)
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~1.6 microns
But faint z~3, galaxies may not be a problem
z~3 galaxies
Main source of worry
The fractional contribution from z~3 galaxies to CIB is < 10%, while the missing amount > 50% (Cambresy et al. 2001 and many others)
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Spatial fluctuations (captures how first-stars are clustered)
IR Cls
The real problem would the clustering of flluctuations from unresolved galaxies between z~ 1 to 2 (or K-band magnitides between 17 to 22)
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Spatial fluctuations (captures how first-stars are clustered)
IR Cls
Requirements: Large sky area (>10 square degrees.)high resolution and sensitivity (to resolve foreground galaxies)
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Theory to Reality: Near-IR wide-field surveys
5-sigmapoint sourcedetection
(planned)
(experiments at this endare preferred)
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Fluctuation studies so far: 2MASS
Kashlinsky et al. 03 Some argue2MASSmay havealreadydetectedfirst stars(Magliocchetti
et al. 2003)
(Excess fluctuations at arcminute to few arcminute scales, wherefirst stars cluster)
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Fluctuation studies so far: 2MASS
Expected from deepImaging(existingdata)
18thmagnitudeunresolved
Some argue2MASSmay havealreadydetectedfirst stars(Magliocchetti
et al. 2003)
(probablynot)
(Excess fluctuations at arcminute to few arcminute scales, wherefirst stars cluster)
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Why ground-based data are not good for fluctuation measurements?
(thanks to Jamie)
H-band, same field (9 degrees), images separated by 7 minutes
Airglow dominates - fluctuations at degree scales
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Fluctuation studies so far: DIRBE etc. (all-sky/poor resolution)
Degree-scale (Beam size) variance
Current clustering studies dominated by systematics and foregrounds(A substantial foreground zoadical light from the Solar system dust)
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CIBER(Cosmic Infrared Background ExploRer)
The upcoming rocket experiment(Optimized for spatial fluctuations and first stars)
2 bands between 1 to 3 microns15” or so resolution~16 sqr. deg. field of view(Useful to get about ~ 48 sqr. degrees in 3 flights)
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CIBER(Cosmic Infrared Background ExploRer)
The upcoming rocket experiment(Optimized for spatial fluctuations and first stars)
2 bands between 1 to 3 microns15” or so resolution~16 sqr. deg. field of view(Useful to get about ~ 48 sqr. degrees in 3 flights)
Main collaboration: Caltech: Asantha Cooray, Andrew LangeJPL: Jamie Bock UCSD: Brian KeatingISAS Japan: Toshio Matsumoto
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The life of an IR rocket(Jamie’s previous experiment)
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(A previous rocket data at ~4 microns;not optimized for first stars, but backgroundmeasured in Xu et al. 2003)
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JAKNIFE
We can do the definitive experiment, but unknown related toforegrounds (zodiacal light!) is a major source of uncertainty
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Beyond JAKNIFE: ASTRO-F
(aka IRIS: Infrared Imaging Survey)
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Beyond JAKNIFE: ASTRO-F
Two cameras: Far-IR and Near-IRFIR imaging done first
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Beyond NIFE: ASTRO-F
Two cameras: Far-IR and Near-IRFIR imaging done first
(launched > Feb 2005)
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ASTRO-F (with 500 sec integrations)
IR Cls
High resolution: amazing abaility to resolve and remove foregroundgalactic stars and galaxies.
Near-IR observation details still to be worked out.
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Filling the gaps: SNAP
Imaging data from the weak lensing survey can be used for IRfluctuation studies.
SNAP J-band can fill the gap below 2.5 microns of ASTRO-F!!!
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First Stars
I. The case for early star-formation
II. First-star signatures in IR?
III. First-supernovae signature in small scale CMB via SZ?
IV. Final battle: Putting II and III together and why?
Oh, Cooray & Kamionkowski 2003
Cooray, Bock, Keating, Lange & Matsumoto 2003
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1. From WMAP TE-correlation: τ ~ 0.17 ± 0.04 zri ~ 17 ± 5Interesting Facts and Suggestions
WMAP Kogut bump
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1. From WMAP TE-correlation:
2. An absolute minimum-y distortion for the universe(photoionized gas: 1eV)
τ ~ 0.17 ± 0.04 zri ~ 17 ± 5
y = σT dzdt
dz∫ ne
kBTe
mec2 ~ τ kBTe
mec2
y ~ 2 ×10−7 (FIRAS - y < 1.5 ×10-5)
Interesting Facts and Suggestions
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1. From WMAP TE-correlation:
2. An absolute minimum-y distortion for the universe(photoionized gas: 1eV)
3. Reionization by Very Massive Stars ( > 300 Solar Masses)
τ ~ 0.17 ± 0.04 zri ~ 17 ± 5
y = σT dzdt
dz∫ ne
kBTe
mec2 ~ τ kBTe
mec2
y ~ 2 ×10−7 (FIRAS - y < 1.5 ×10-5)
Interesting Facts and Suggestions
VMS Age ~ 106 yrs ⇒ VMS SN ~ 1053 ergs
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1. From WMAP TE-correlation:
2. An absolute minimum-y distortion for the universe (photoionized gas: 1eV)
3. Reionization by Very Massive Stars ( > 300 Solar Masses)
4. First generation of SNe =>
τ ~ 0.17 ± 0.04 zri ~ 17 ± 5
y = σT dzdt
dz∫ ne
kBTe
mec2 ~ τ kBTe
mec2
y ~ 2 ×10−7 (FIRAS - y < 1.5 ×10-5)
Interesting Facts and Suggestions
VMS Age ~ 106 yrs ⇒ VMS SN ~ 1053 ergs
Taylor - Sedov Expansion : R ~ 2 kpc ESN
1053erg
⎛
⎝ ⎜
⎞
⎠ ⎟
1/ 51+ z
20
⎛ ⎝ ⎜
⎞ ⎠ ⎟
−11/ 5
( 1")
t ~ tCompton ≈107 yrs 1+ z
20
⎛ ⎝ ⎜
⎞ ⎠ ⎟
−4
and SSZ ~ 2 nJyESN
1053erg
⎛
⎝ ⎜
⎞
⎠ ⎟
1+ z
20
⎛ ⎝ ⎜
⎞ ⎠ ⎟
ε0.5
⎛ ⎝ ⎜
⎞ ⎠ ⎟
ε => Fractional energy transferred to CMB
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First Supernovae
(Simulations by Naoki Yoshida)
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QuickTime™ and a Cinepak decompressor are needed to see this picture.
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Reionized by First Stars
1. If massive
2. First generation of SNe =>
VMS Age ~ 106 yrs ⇒ VMS SN ~ 1053 ergs
Taylor - Sedov Expansion : R ~ 2 kpc ESN
1053erg
⎛
⎝ ⎜
⎞
⎠ ⎟
1/ 51+ z
20
⎛ ⎝ ⎜
⎞ ⎠ ⎟
−11/ 5
( 1")
t ~ tCompton ≈107 yrs 1+ z
20
⎛ ⎝ ⎜
⎞ ⎠ ⎟
−4
and SSZ ~ 2 nJyESN
1053erg
⎛
⎝ ⎜
⎞
⎠ ⎟
1+ z
20
⎛ ⎝ ⎜
⎞ ⎠ ⎟
ε0.5
⎛ ⎝ ⎜
⎞ ⎠ ⎟
ε => Fractional energy transferred to CMB
Main cooling mechanism is through cooling off of CMB via inverse-Compton scattering
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Compton Cooling
⇒ Scattering moves photons from low frequencies (RJ part of the frequency spectrum) to high frequencies (Wien regime)
From Sunyaev-Zel’dovich (1980):
Frequency shift the CMB blackbody
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Compton Cooling
⇒ Scattering moves photons from low frequencies (RJ part of the frequency spectrum) to high frequencies (Wien regime)
Frequency shift the CMB blackbody
From Sunyaev-Zel’dovich (1980):
and the difference (wrt to CMB)
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Reionized by First stars
y ~ 4 ×10−6 E
100eV
⎛ ⎝ ⎜
⎞ ⎠ ⎟
151+ z
⎛ ⎝ ⎜
⎞ ⎠ ⎟
(Still below the FIRAS - y limit of 10-5)
Departure from CMB black-body due to first SNe:
The effect is similar to the one due to hot-electrons in galaxy clustersand now observed at arcminute scales (e.g., Carlstrom et al.)
But, fluctuations are not small since halos in which first stars form are highly biased and strongly clustered!!
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Oh, Cooray, Kamionkowski 2003, MNRAS
First stars in
105K halos
(y ~ 10-5)
σ 8 = 0.84 ± 0.08
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Cluster SZ Effect: Dominated by Massive Halos
(Springel et al. 2000)
SZ: dominated by individual clusters where as SNe produce a smoothdiffuse distribution
(small angular scale CMB experiments, with multifrequency information)
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Reionized by Massive stars:
How to detect First SNe fluctuations?
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CMB small angular scale fluctuations are confusing(too many contributions)
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But there is hope: frequency separation
⇒ combine experiments + known properties of foregrounds
Separation of SZ thermal from CMB and rest in upcoming/present data
With Planck sensitivity:
Input SZ SZ+CMB+Foregrounds Recovered SZ
(In real life, this is what we observe)
Cooray, Hu & Tegmark 2000
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SZ separated in Multi-Frequency Data
CMB mess SZ thermals
Cooray, Hu & Tegmark 2000;
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SZ separated in Multi-Frequency Data
Cooray, Hu & Tegmark 2000;
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Cluster SZ Effect: Dominated by Massive Halos
(Springel et al. 2000)
SZ thermal: dominated by individual clusters
SZ can also be separated out in multifrequency data!
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SZ contributions from clusters which are resolved
Pop III SNe Sunyaev-Zel’dovich Effect
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SZ contributions from clusters which are resolved
Who can do this? e.g., South Pole Telescope - 4000 sqr. degree mapAtacama Cosmology Telescope
Pop III SNe Sunyaev-Zel’dovich Effect
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Putting all together: High-z probes of reionization
I. Large scale CMB polarizationII. Fluctuations in the Cosmic IR Background
III. Small scale CMB fluctuations - supernovae
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Putting all together: High-z probes of reionization
I. Large scale CMB polarizationII. Fluctuations in the Cosmic IR Background
III. Small scale CMB fluctuations - supernovae
Unfortunately, (II) and (III) alone are not clean probes of early starformation and (I) measures optical depth.
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Putting all together: High-z probes of reionization
I. Large scale CMB polarizationII. Fluctuations in the Cosmic IR Background
III. Small scale CMB fluctuations - supernovae
Unfortunately, (II) and (III) alone are not clean probes of early starformation and (I) measures optical depth
One can extract a whole lot of information from cross-correlations between these.
We already have WMAP Polarization maps,JAKNIFE will get a first map of IR fluctuations
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One can extract a whole lot of information from cross-correlations between these.
We already have WMAP Polarization maps,JAKNIFE will get a first map of IR fluctuations
21cm
CIBz~3 galaxies
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PolarizationReionization ⇒ Free electrons
Compton scattering of any local quadrupole by electrons lead to polarization
When primordial CMB anisotropies are projected
PPr im ∝τ Qrms(z) ∝ C2(z)
Electron motions generate a kinematic quadrupole
PKin ∝ g(x)τ β t2
(To understand this,
Iν = Cx 3
exγ (1+βµ ) −1when expanded
Iν = Cx 3
ex −1I0 + I1µ + g(x)β 2 µ2 −
13
⎛ ⎝ ⎜
⎞ ⎠ ⎟ + ...
⎡
⎣ ⎢ ⎤
⎦ ⎥
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Galaxy Clusters ⇒ Tons of Free electrons
Compton scattering of the quadrupole lead to SZ polarization
When primordial CMB anisotropies are projected
PPr im ∝τ Qrms(z) ∝ C2(z)
+
Electron motions generate a kinematic quadrupole
PKin ∝ g(x)τ β t2
+
Double scattering effects (Intrinsic Quadrupole)
(First scattering produces a quadrupole which is scattered again
to produce polarization)
Pint ∝τ 2 β t +f(x)kBTe
mec2
⎛
⎝ ⎜
⎞
⎠ ⎟
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Cosmologically Important contribution
Very small
SZ thermal related pol. is not always small, but can be separated through f(x)
Galaxy Clusters ⇒ Tons of Free electrons
Compton scattering of the quadrupole lead to SZ polarization
When primordial CMB anisotropies are projected
PPr im ∝τ Qrms(z) ∝ C2(z)
+
Electron motions generate a kinematic quadrupole
PKin ∝ g(x)τ β t2
+
Double scattering effects (Intrinsic Quadrupole)
(First scattering produces a quadrupole which is scattered again
to produce polarization)
Pint ∝τ 2 β t +f(x)kBTe
mec2
⎛
⎝ ⎜
⎞
⎠ ⎟
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Galaxy Clusters ⇒ Tons of Free electrons
Compton scattering of the quadrupole lead to SZ polarization
When primordial CMB anisotropies are projected
PPr im ∝τ Qrms(z) ∝ C2(z)
+
Electron motions generate a kinematic quadrupole
PKin ∝ g(x)τ β t2
+
Double scattering effects (Intrinsic Quadrupole)
(First scattering produces a quadrupole which is scattered again
to produce polarization)
Pint ∝τ 2 β t +f(x)kBTe
mec2
⎛
⎝ ⎜
⎞
⎠ ⎟
Cosmologically Important contribution
Very small
Combine with SZ thermal tomeasure cluster gas temperature profile
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Clusters in CMB Polarization maps
100GHz
600GHz
(Pol ~ 0.1(tau/0.01) muK)
(100 x kinematic to show randomness of velocities)
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Clusters in CMB Polarization maps
100GHzAt each redshift, spatial distribution of polarization is uniform.
=> One can average over large samples of clusters to determine a sample averaged polarization at each redshift.=> This can be converted to estimate the quadrupole at that redshift
(Pol ~ 0.1(tau/0.01) muK)
(Sunyaev & Sazonov 2002; Cooray & Baumann 2003)
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Clusters in CMB Polarization maps
100GHzAt each redshift, spatial distribution of polarization is uniform.
=> One can average over large samples of clusters to determine a sample averaged polarization at each redshift.=> This can be converted to estimate the quadrupole at that redshift
(Pol ~ 0.1(tau/0.01) muK)
This looks like hard. So, why bother?
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Astrophysical measurements of dark energy
Fundamental structure:
If dark energy is smooth and homogeneous, dark energy onlymodifies the expansion rate:
H (z) ~ f (cosmology )
∝ f (Ωm ,ΩX ,Ωc ,w,z)
All observables in the universe are functions of the expansion rate
r(z) =dz
H(z)0
z
∫For e.g., distance out to some z:
Integrations reduce sensitivity to parameters in the function “f”
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Astrophysical measurements of dark energy
Fundamental structure:
If dark energy is smooth and homogeneous, dark energy onlymodifies the expansion rate:
H (z) ~ f (cosmology )
∝ f (Ωm ,ΩX ,Ωc ,w,z)
All observables in the universe are functions of the expansion rate
r(z) =dz
H(z)0
z
∫For e.g., distance out to some z:
Better to probe derivatives, ie. dr(z)/dz directly. This is usuallyhard in practice.
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In terms of cosmology (ie. Dark energy), this is an amazing measurement
Different Probes compared equally.
10% errorsat z=0.1 … 2at steps of 0.1for each quantity
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In terms of cosmology (ie. Dark energy), this is an amazing measurement
Different Probes compared equally.
distance
volume
growth
time
velocities
Potential evolution
10% errorsat z=0.1 … 2at steps of 0.1for each quantity
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In terms of cosmology (ie. Dark energy), this is an amazing measurement
Different Probes compared equally.
dg/dz determinesISW effect in CMB(ie. The exact quadrupole at lowredshifts)
distance
volume
growth
time
velocities
Potential evolution
10% errorsat z=0.1 … 2at steps of 0.1for each quantity
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In terms of cosmology (ie. Dark energy), this is an amazing measurement
distance
volume
growth
time
10% errorsat z=0.1 … 2at steps of 0.1for each quantity
Better to measure probes which are time/redshift derivativesdirectly!!!! This is why dg/dz gives@20 times better than d(z)
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Same goes for redshift varying w(z)
Different Probes compared equally.
10% errorsat z=0.1 … 2at steps of 0.1
dg/dz determinesISW effect in CMB(ie. The exact quadrupole at lowredshifts)
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In terms of cosmology (ie. Dark energy), this is an amazing measurement
Compared to SNAP, 20 times worse fractional measurementgives equal constraining power with respect to dark energy
10% errorsat z=0.1 … 2at steps of 0.1
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Useful?
(Reconstruct the quadrupole as a function of redshift)
Planck(10^4 clusters, poor noise)
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Beyond Planck…. Cluster Polarization in CMBpol era
Errors for 1 muK/pixel noise @ 1 arcminresolution experiment (with ~10^5 clusters)
(Reconstruct the quadrupole as a function of redshift)
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CMBpol-like
10 times worse These errors include confusionsrelated to other polarizedcontributions
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Summary
starformation
useful clues to the presence
WMAP optical depth to reionization is very interesting andsuggest high-z
IR background cannot be easily explained with galaxies Spatial fluctuations may provide
of first stars.
(~2007 with NIRC observations)
=> useful probe of dark energy
for more details visit http://www.cooray.org
CIBER flights in 2005Significant improvements with ASTRO-F
Cross-correlation studies with CMB polarization a must!!Individual detections with JWST ( > 2012)Cluster polarization