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Sergio Colafrancesco Sergio Colafrancesco ASI-ASDCASI-ASDC INAF- OARINAF- OAR EmailEmail: [email protected] [email protected]
Cosmology with the SZE
News & Views
Vulcano Workshop 2010Vulcano Workshop 2010 May 24, 2010
Cosmological scenarioProbe
CMB
SN-BAOWL CLCMBSNeSNeSN-BAOCMBCL-WLCMB-CLCMB
SN-CL
Main parameters
Geometry: Ωk,0
Matter/Energy - Dark ΩDE
ΩDM
- Ordinary: Ωb
Ων
Scales: H0
Dynamics: ä/aEq. of state: wT/S ratio: rPower spec: σ8
ns
Reionization zr
Modified - Gravity
Cosmological scenarioProbe
CMB
SN-BAOWL CLCMBSNeSNeSN-BAOCMBCL-WLCMB-CLCMB
SN-CL
Main parameters
Geometry: Ωk,0
Matter/Energy - Dark ΩDE
ΩDM
- Ordinary: Ωb
Ων
Scales: H0
Dynamics: ä/aEq. of state: wT/S ratio: rPower spec: σ8
ns
Reionization zr
Modified - Gravity
SZ
The SZ Effect
thermal NR e-
relativistic e- 2
34 γ
νν ≈∆
24cm
kT
e
e≈∆ν
ν
I0(x) I(x)
Irel(x)
Thermal
Relativistic
S.Colafrancesco 2007, NewAR, 51, 394Beyond the Standard Lore of the SZ effect
y(Pe,ℓ) = Comptonization factor ğ(ν,T0,Pe) = Spectral distribution
SZE: Observational fact
This ― This
The origin of the SZ effect
1957 A.S. Kompaneets publishes his Compton scattering Fokker-Planck equation
1 Ya. B. Zel’dovich & R. Sunyaev derive the thermal SZ effect
(i.e., applied the Kompaneets eq.)
Non-coherent Compton Scattering Fall-out effect of the Cold War
(derived by A.S. Kompaneets in Soviet Union ∼ 1950 but was classified due to nuclear bomb research until 1956)
Intensity change
Spectral shape
Thermal
Relativistic
Redistribution function
Pressure
[Colafrancesco et al. 2003, A&A, 397, 27]
∫∞
=0
);()()( psPpdpfsP se
SZE: general relativistic derivation
SZE from various e- populations
SZrel
SZDM
SZkin
SZwarm
SZth
CMBKThν=
SZE amplitude:degeneracy in physical parameters
SZE spectra:sensitivity to physical parameters
∫∞
=0
);()()( psPpdpfsP se
)()()(2 2
30 xgy
hckTI thth =∆
∫= 2cmkTndy
e
eeTth σ
Physics with the SZE: thermal plasma
g (x)
2,0 eeth cbaX θθ ++≈
≡ 2cm
Tk
e
eBeθ
The best way to measure Te are:- SZE at high frequencies (> 300 GHz)- spectral slope around 220 GHz
[Colafrancesco, Prokhorov, Dogiel 2009]
Density
Temperature
Pressure
Astrophysics & Cosmology
The SZE is independent of redshiftand therefore it is an optimal toolfor Cosmological applications
Standard-rod “physical” effect
The SZE depends directly on the electron distribution in the atmospheres of cosmic structures and therefore it is an optimal tool for Astrophysical applications
X-rays
X-rays
X-rays
~n2(kT)1/2
~∫n kT
Power-law
Maxwellian
Astrophysical relevance
Thermal particlesEe ∼ 0.1 – 10 keV
WIMPsMχ ∼ 10–500 GeV 1ES0657-556
B-fieldsB-fields
Acceleration proc.Acceleration proc.
Galaxy clusters AGN jets/cavities DM nature Plasma physics
Cosmic raysEe∼16GeV Bµ
1/2(νGHz)1/2
Cluster CavitiesMS0735+7421 (Chandra)
Radio Galaxy Lobes3C432 (Chandra)
SZE
Cosmological relevanceGalaxy clusters AGN jets/cavities DM nature Plasma physics
Hubble diagramHubble diagram
Cluster countsCluster counts
TT CMBCMB(z)(z) SUSY DMSUSY DM
Light DMLight DM
Baryon fractionBaryon fraction
WHIMWHIM
Excluded by SZE in Coma
Excluded by BBN
Excluded by WMAP
Excluded by WMAP
2/)1(min
)1(min
3)(
−−−−
−
⋅×
∝∆
ααγ X
CMBIC
E
kTF
T
ΩDM ΩDE
3C432
TT CMBCMB(z)(z)
C RG
CR fractionCR fraction
WMAP (95%)Ex
clud
ed b
y B
BN
Bremsstrahlung
in-flight annihilation
SNe
e- anomalous magnetic moment
Excl
uded
by
BB
N
A few exemplary cases (Cosmology)Cosmological scenario
ΛCDM model: cosmological parametersExtended-G model: ModG scales
TCMB(z) Galaxy clusters (thermal SZE)RGs (non-thermal SZE)
DM natureSZDM effect
Relevant Cosmic Parameters
15
Clusters: cosmological probesClusters are excellentCosmo-evolu-meters
Understand their physics M proxy → YSZ (DM, baryons, Galaxy feedback, CRs, B-field) Y~∫n•T
Derive their total gravitational mass YSZ → Mtot
Collect large, unbiased catalogues N(YSZ,z) → N(M,z)
N(M
,z) [
#/M
V]
SZE: Cosmology
Sensitivity to theDE equation of state
Good DE probeif Mtot well sampled
ΛCDMmodel
DE model
SZE
SZE Clusters and DE probes
SZE optimal tool
DE
prob
es
SZE from space
SZE in galaxy clusterseliminates weaknesses& systematics
SZE spectroscopy will allow to derive spatially resolved T-profiles for nearby clusters out to large distances:
Perseus
SZE spectroscopy: T-profiles
X-rays
Lensing(total mass)
[Colafrancesco & Marchegiani 2009]
T profile with uncertainties similar to those of X-ray observations
T profile uniquely sampled in the outer parts of the cluster
Determination of temperature and density profiles from SZE observations will allow to estimate the total mass of the cluster, including the outer regions.
Unbiased probes for Cosmology
Inversion Technique SZE → T, τ, Vp, TCMB
SZE X-Ray
SZE
SZE: modified GHilbert-Einstein action in f(R) models
[Capozziello, Colafrancesco, DeLaurentis, Milano 2010]
Modified-G potential
Modified-G mass assemblyModG1ModG2
Variance Increaseat high-M
Mod-G vs DE: SZ Clusters + SNe
Mod-G (DGP)
SNe Clusters (SZE)
SNe + SZ clusters can distinguish ModG from DE models → Need ~200 clusters in bins of width ∆z = 0.1 [Tang et al. 2006]
CMB temperature
TCMB(z)
(From Lima et al. 2000)
Clusters: TCMB(z) from SZE spectra
)(zkThx
CMB
ν= 2cmkT
e
ee =θ
Four unknown
• TCMB(z)• Vr
• τ• Te
Full SZE spectrum
∼ 90-500 GHz
[Colafrancesco et al. 2010]
RGs: TCMB(z) from SZE + X-rays
2/)1(min
)1(min
3)( −−−−− ⋅×∝∆ ααγ XCMBIC
SZ EkTFT
TCMB(z)measure
[Colafrancesco 2008]
IC emissionfrom lobes
AGN central source
3C432
SZE and TCMB(z)
Probe energy release mechanisms at high-z with the SZE (Colafrancesco et al. 2010)
Clusters RGs
SZE and Dark Matter nature
1ES0657-556Hot gasDark Matter
SZDM from 1ES0657-556
Isolating SZDM at ∼223 GHzFr
eque
ncy
(M
χ= 2
0 G
eV)
Neu
tral
ino
mas
s (
ν=22
3 G
Hz)
[S.C. et al. 2007]
Cosmology vs. Astrophysics
SZ & Cosmology: astrophysical caveatsX-ray gas models overpredict SZE
• X-ray gas modeling• Gas clumpiness• Non-thermal phenomena
[Diego & Partridge 2009; Bonamente et al. 2007]
Gas pressure ≠ gas emissivity
ATCA+ROSAT
[Malu et al. 2010; Massardi et al. 2010]
ATCA+Chandra
Lack of detailed knowledge of cluster physics is a limitation to the use of SZE for cosmologyObsv.
Estd.
SZE @ mm frequencyHerschel SPIRE view of Bullet cluster
[Zemkov et al. 2010]
250 µm
350 µm
500 µm
Large impact of pointsources at mm frequency
Spatially resolved spectroscopic SZE RXJ1347-1145
Spatially resolved spectroscopic SZE
Multi-T gas
Single-T gas
AGN non-th
RXJ1347-1145
News and Views
New ideas
New technology
SZE probe in cluster atmospheres
SZrel
SZDM
SZkin
SZwarm
CMBKThν=
Continuous spectroscopy
)(00 ePxx =)(00 ePxx =
xxiSlope
∆∆= )(
Wide ν-band spectroscopyHigh-ν spectroscopy
Degenerate w.r.t.Vp, ECR, MDM, PWHICM
Unbiased probe at ~x0
[Colafrancesco, Prokhorov, Dogiel 2009]
SZth
Observational requirements
3) A high-ν band to determine the electron temperature T from the shape of the SZ spectrum(→ highly sensitive to T)
2) A medium-ν band to determinethe crossover of the spectrum thatallows to obtain information on- electron pressure Pe
- TCMB(z)- Vpec
4) Very high-ν band to monitor the foregrounds (Galaxy, Point-like Sources)
Thermal SZE spectra
1 2 3 4Bands:
1) A low-ν band to determine the overall amplitude of the SZE that isproportional to y = ∫dl n∙Tmainly depending on τ = σT ∫dl n(→ insensitive to T)
Observational requirements1) A low-ν band to determine the overall amplitude of the SZE that isproportional to y = ∫dl n∙Tmainly depending on τ = σT ∫dl n(→ insensitive to T)
3) A high-ν band to determine the electron temperature T from the shape of the SZ spectrum(→ highly sensitive to T)
2) A medium-ν band to determinethe crossover of the spectrum thatallows to obtain information on- electron pressure Pe
- TCMB(z)- Vpec
4) Very high-ν band to monitor the foregrounds (Galaxy, Point-like Sources)
Thermal SZE spectra
1 2 3 4Bands:
Batm>10K
State of the Art … so farSPT
Deep integrations, high resolution, ~103 deg2 survey. - No access to positive peak of SZE (ν>300 GHz)- No spectroscopy.
SZ + LABOCA150-215 345 GHz
- No spectroscopy- Different instruments
In contrast, we would need
PLANCK PLANCK Full sky, but shallow survey. A few thousand clusters with low-moderate S/N ratio. Low-Moderate spatial resolution
• Spectroscopic capabilities first time• Wider & continuous frequency coverage first time• Better calibration (no multi-band, no atmosphere)• Better knowledge of foregrounds first time• Deeper integrations on selected targets/fields first time
SZE in Space
MILLIMETRON
12m dish12 m dishActive cooling (4 K)Θ< 0.1-1.0 arcminNoise<0.1 mJy/√HzSpectroscopyPolarimetrySuper VLBI
MILLIMETRON 12m
3 m dishPassive cooling (50 K)Θ= 0.7-4.2 arcminNoise=18 mJy/√HzSpectroscopy
Millimetron 3m
Large-survey modePointed mode
Observatory modeSmall-survey mode
3m dish
OLIMPOPLANCK
SZE spectroscopy: precision
MILLIMETRON (3m)10 min. exposureR=20
CMBkThx /ν≡
MITOWMAPOVRO
COMA in SZE: Current data(Battistelli et al. 2003, ApJ 598, L75)
[Colafrancesco 2004]
MILLIMETRON (12m)10 min. exposureR=100
SZE spectroscopy: physics
Spectroscopic capabilities will allow to separate the cluster parameters:
ne Te Vp TCMB
- the main physical quantities of the cluster thermal plasma (density ne, temperature Te)
- the cluster peculiar velocity Vp
- the value of the CMB temperature TCMB(z) at the cluster redshift z
All with good precision(independent derivation !)
ne Te Vp TCMB
Low-resolution space spectrometer vs. ground based multiband (3-BP)
3-BPMillimetron (3 m.)
Millimetron (12 m.)
SZE: resolving cluster atmospheres
150 GHz
350 GHz
3 m. 12 m.X-ray
MS0735150 GHz
350 GHz
R=100Millimetron
SZE: spectro-polarimetryPolarizations arises as a natural outcome of electron-radiation scattering
→ various polarizations
Polarization due to transverse motion of clusters
Polarization in galaxy clusters due to transverse motions of plasma within the cluster
Polarization in galaxy clusters due to multiple scattering γ-e within the cluster
τβ 21.0 t≈
201.0 τβ t≈
2201.0 τ
≈
cmkT
e
Other polarization effects …
SZE polarization: general formalism
τβ 2t∝
22 τ
∝
mckT
2τβ t∝
Polarization due to galaxy clusters transverse motion
Polarization due to transverse motions of plasma within the cluster
Polarization due to multiple scattering γ-e within the cluster
SZE: spectro-polarimetry
SZth
tpSZ
SZkin
kpSZ
[Sazonov & Sunyaev 1999][Colafrancesco et al. 2010]
Qpf(x)
x
QpkpSZ
tpSZ tpSZ
Cosmology & Astrophysics @ mm’s
LSS BH SFRSZEDEDM
PA
← 100 GHz5 THz
ModG
THANKS
for your attention