49 th moriond - cosmology march 28 th , 2014
DESCRIPTION
49 th Moriond - Cosmology March 28 th , 2014. The SZE in the SKA & MILLIMETRON Era. Sergio Colafrancesco Wits University - DST/NRF SKA Research Chair Email : Sergio.C [email protected]. T he SZE: Physics. The SZ effect is a specific form of - PowerPoint PPT PresentationTRANSCRIPT
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49th Moriond - Cosmology March 28th, 2014
Sergio Colafrancesco Wits University - DST/NRF SKA Research Chair Email: [email protected]
The SZE in the SKA & MILLIMETRON
Era
The SZE: Physics
high-energyphoton
The SZ effect is a specific form of Radiation-Matter interaction
Photon fields External ↓ ↓ CMB 21-cm
Internal High-E electrons - thermal (supra-thermal)- relativistic
↑
Use CMB photons to extract
plasma information
The SZE: manifestations
SZE polarization
SZDM
SZkin
SZwarm
SZthSZE Intensity
5 keV
20 keV
SZrel
depends on fe(p) and ICMB vectorial
depends on fe(p) and ICMB scalar
SZE: multi-n Astro Physics
SPTMUSTANG
OVRO
Accessible from Space
Independent of astrophysics
Strongly dependent on astrophysics
)()(
)(2
2
30 xgyhc
kTI thth
kT= 7 keVkT=10 keVkT=15 keVkT=20 keV
Sensitive to CMB Insensitive to CMB
Need:
• wide-n coverage
(≈10 - 800 GHz)
• sensitivity (< mK)
• Imaging (arcsec)
Exploiting SZE information
[DeBernardis, Colafrancesco et al. 2012]
Different spectroscopic configurationsfor studying the SZE in cosmic structures
SZ th
SZ non-th
SZ kin
Foreground
Exploiting SZE information
[DeBernardis, Colafrancesco et al. 2012]
EC23mpassive
EC312mpassive
EC512mactive
Different spectroscopic configurationsfor studying the SZE in cosmic structures
PLANCK
SPT Herschel
OLIMPO
Millimetron
PLANCK
Millimetroncold DFTS, cold telescope (4K) on a satellite in L2(de Bernardis, S.C. et al. 2012)
SZE: parameter extraction1 hour
OLIMPO: warm DFTS, warm telescopeon a balloon
(de Bernardis, S.C. et al. 2012)
SZE: parameter extraction3 hours
SZE: best frequency bands5-30 GHz 100-1000 GHz
DFTS (baseline)
Band 1 Band 2
Band 3
Band 4
Frequency (GHz) 100–200 130–350
350–700
700–1000
FWHM (arcmin) 1.3 1.0 0.36 0.18
# of independent beams/detectors
6/24 9/36 16/48 25/100
Background (pW) 5.4 8.2 9.7 7.8
Detector NEP (aW s1/2)
18 18 6.0 1.2
Spectral Resolution (GHz)
1.25 1.25 1.25 1.25
Spectral sensitivity (aW s1/2 /GHz)
8.7 8.6 2.9 0.95
SKA -1 Mid GHz GHz
Band 1 0.35 1.05
Band 2 0.95 1.76
Band 3 1.65 3.05
Band 4 2.80 5.18
Band 5 4.60 13.8
SKA-1 Low
baseline 0.05 0.35
proposed 0.05 0.65
Square Kilometer Array
Spektr-M
104
0.1
SZE: frequency & sensitivity
VLA
E-VLAMerKAT
SKA-P1 SKA-P2
Square Kilometer Array
Spektr-M
10-17 W Hz-1/2
10-18
10-19
SZE: MILLIMETRON (102 - 103 GHz)
Cluster physics characterizationThermal, non-thermal pressure stratificationMultiple componentsRelativistic plasma physics (thermal, non-thermal)
Spectro-polarimetry: 3D tomographyCosmology
Cluster cosmology (with no physics biases/priors)Radio-galaxy cosmology “Galaxy cosmology “
SZE PolarizationMeasuring CMB polarizationThe Cosmological Principle
DM nature
Millimetron n-range probes the electron plasma physics
… and yields related cosmology
SZE: physics characterizationMACS
J07017.5+3745A Triple-Merger
Cluster ?
[Mroczkowski et al. 2011]
Bullet clusterA multi-plasma stratification ?
Radio + X-rays Radio + Temperature Radio + Lensing
SZE: Bullet tomographyMorphological SZE
A2219
345 GHz Laboca 600 GHz Herschel
GHz
GHz
I
I
345
600
Shockhot
Bulletcold
[Prokhorov, S.C. et al. 2011]
T standard deviationFirst measurement of the
Temperature standard deviation in galaxy clusters using the SZE
[Prokhorov & Colafrancesco 2012]
<T> ~ 13.9 keVs = 10.6 ± 3.8 keV
• Measure of the temperature stratification in clusters • Measure of plasma in-homogeneity (th.+non-th.) along the line-of-sight
Bullet Cluster
SZE: Bullet Astro Physics
kT1= 13.9 keV t=3.5 10-3
kT2= 25 keV, t=5.5 10-3
Multi - Temperature Thermal + non-thermalkT = 13.9 keV t=1.1 10-2
ne~E-2.7, p1=1, t=2.4 10-4
Evidence of non-gravitational activity in the cluster merging
Shock acceleration or MHD acceleration
Stochastic electron acceleration Continuous hadron acceleration
Non-thermal
Thermal
T1
T2
[S.C. et al. 2011] [S.C. et al. 2011]
c2=1.27d.o.f.=1rms fom=1
c2=0.44d.o.f.=2rms fom=0.35
SZE: resolving cluster atmospheres
150 GHz
350 GHz
3 m. 12 m.X-ray
Chandra
MS0735150 GHz
350 GHz
R=100Millimetron
MACS J07017.5+3745
B) kT = 12.8 kev (+2.1/-1.6) V = 3600 km/s (+3440/-2160) V = 3238 km/s (252/-242)
C) kT = 34.0 kev (+11/-7.9) V = -3720 km/s (+2960/-2480) V = -733 k/s (+486/-478)
D) kT ≈ 4 keV V = 831 km/s (843/-700)
A) kT ≈ 2 keV V = 278 km/s (+295/-339)
A Triple-Merger Cluster ?
MACS J07017.5+3745
B) kT = 12.8 kev (+2.1/-1.6) V = 3600 km/s (+3440/-2160) V = 3238 km/s (252/-242)
C) kT = 34.0 kev (+11/-7.9) V = -3720 km/s (+2960/-2480) V = -733 k/s (+486/-478)
D) kT ≈ 4 keV V = 831 km/s (843/-700)
A) kT ≈ 2 keV V = 278 km/s (+295/-339)
A Triple-Merger Cluster ?
E) Non-thermal component s=3.5, p1=0.1 t=5 10-4 – 2 10-2
MACS J07017.5+3745
Comp. B
Comp. C
Comp. C
[S.C. &Marchegiani 2013]
Cluster physicsand Dynamicsat high frequency
n > 350 GHz
SZE spectro-polarimetry
JuttnerMaxwell-BoltzmannNon-relativistic
1) Derive the velocity DF of electrons by using SZE observations at > 4 frequencies [Prokhorov, Colafrancesco, et al. 2011]
2
11
)(
)(40
cm
kT
xf
xgI
etV
5 keV 8 keV13 keV20 keV
BB spectrum
2) Polarization due to finite optical depth t allow to measure density and velocity distribution of the electrons
SZE cluster cosmology
Perseus
[Colafrancesco & Marchegiani 2010]
SZE X-Ray
SZE spectroscopy will allow to derive spatially resolved T-profiles for nearby clusters out to large radii:
Separate thermal and non-thermal pressure components:
T profile uniquely sampled in the outer parts of the cluster
Inversion Technique SZE → T, t, Vp, TCMB
SZE sensitivity (10-100 nK) will allow to reach the mass limit at which clusters and groups can be found
Unbiased total mass reconstruction due to sensitivity to total pressure DI SZE
and internal velocity fields DP SZE
SZE: Cosmology with clusters
Measure the CMB anisotropy at positions U1 and U2 by using galaxy cluster SZE
S
CMB Quadrupole Q2
CMB Quadrupole Q2
Cluster
Cluster
Polarized SZEreflects Q2
[Colafrancesco, Tullio & Emritte 2013-14]
Cosmological Principle
SZE: Cosmology with clusters
Cluster Π−(th) RG Π−(non-th)
Cluster Π−(th) RG Π−(non-th)
S.C. et al.[2012-14]
Measure the CMB multipoles at the position of clusters/RGs in the Universe
1 mJy/arcmin2
0.042 mJy/arcmin2
0.005 mJy/arcmin2
0.05 mJy/arcmin2
Quadrupole Quadrupole
Octupole Octupole
SZE: SKA (10-30 GHz)
Cluster cosmology: SZE and SZE-21cm
CMB spectral modifications at early epochs: SZE-21cm
Dark Ages and EoR: SZE 21cmDM heating: SZE-21cmPrimordial B-field
Fundamental physicsPhoton mass and decay…
SKA n-range probes the background radiation fields
… and yields related cosmology
SZE cluster cosmology
3C2923C294
Bullet cls VLAE-VLA
MerKAT SKA-P1 SKA-P2
The SKA can measure SZE in various objects:
- Clusters- Radiogalaxies- Galaxy halos/winds
SZE-21cm: DA and EoRCMB field modified SZE-21cm
Collision/abs.z=200-30
Ly-az=30-20
X-rayz=20-6
1+z=3
no DM extremeMmin=10-6 Mo
Mmin=10-3 Mo
no DM
(Colafrancesco & Marchegiani 2014)
kTe=7 keV
kTe=7 keV
SZE: the photon0m is not a theoretical requirement
• Classical electrodynamics: Maxwell equations are substituted by Proca (1936) equations for mg ≠ 0
• Quantum theory: QED with Stuckelberg mechanism (1938) allows a non-zero photon mass without violation of Gauge invariance [Goldhaber & Nieto 2010]
0m Photon can decay with lifetime tg ≠ 0 Good limits on
mg:
No tight limit on tg: ?
Experiment Result Reference
Laboratory Williams, Faller & Hill (1971)
Earth B-field Davis, Goldhaber & Nieto (1975)
Solar wind Ryutov (2007)
eV 10 142 cm
eV 10 182 cm
SZE with g decay
eV 105 ; 0 9* E
eV 10 5* E
eV 10 4* E
CMB spectrum modified by photon decay
as function of
keV 15eBTk2101 e
[Colafrancesco & Marchegiani 2014]
eV 10 4* E
Difference between the SZE without g decay and the SZE with g decay
eV 105 9* E
eV 103 9* E
eV 102 9* E
eV 101 9* E
SKA (30 h)
260 h
SZE with g decay: A2163SKA can measure, or set the most stringent limits on, the g decay
(Colafrancesco & Marchegiani 2014, A&A, 562, L2)
ConclusionsMillimetron and SKA observations of the SZE have the potential of addressing several key questions for Cosmology and fundamental
Astro-PhysicsCosmological parameters and standard cosmological probesThe Nature of Dark Matter (DM)The proof of the Cosmological Principle (CP)Origin of Cosmological magnetic field (B)The Dark Ages and EoR (DA - EoR)Fundamental properties of the Photon (g)
This is possible thanks to the un-precedentWide-band spectro-polarimetry High sensitivityHigh spatial resolutionSurvey and pointed observation modes
THANKS
for your attention