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The Mass in Galaxy Clusters
from X-ray/SZ observables
Stefano EttoriINAF-OA / INFN Bologna
X-ray Planck SDSS
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z=8.55 z=5.7 z=1.4 z=0
P(k)+ΛCDM
Structure formation in the Universe
We know how the gravity forms structures on cluster scales. X-rays (SZ) provide a direct probe of the thermalized gas
in a cluster’s potential.
cluster
R2500(~0.3 R200~CXO limit)
R500(~0.7 R200~few best CXO & XMM cases)
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Bkg: dominant in GCs outskirts
Simulation for 3keV cluster @ R200 (Ettori & Molendi arXiv:1005.0382)
Gal foreground
Ins. background
Residual CXB
Source
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z=8.55 z=5.7 z=1.4 z=0
P(k)+ΛCDM
Structure formation in the Universe
We know how the gravity forms structures on cluster scales. X-rays (SZ) provide a direct probe of the thermalized gas
in a cluster’s potential.
cluster
Coma Planck+13
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Total mass from SZ/X-rays
€
Mtot < r( ) = −kTgas(r) rGµmp
∂ ln ngas∂ ln r
+∂ ln Tgas∂ ln r
$
% &
'
( )
€
Mtot ∝ ΔRΔ3 ⇒∝ T 3 / 2 ∝ Mg ∝ L
3 / 4 ∝YX3 / 5
• low counts statistic: scaling relations (for galaxy clusters mass function: Mtot vs L/T/Mgas/YX or a combination of these…)Ettori et al., 2012; Ettori, 2013 & 2014
• high counts statistic: mass profiles (calibration & hydrostatic bias; ~200 out of 1743 obj known, Piffaretti et al. 11)Ettori et al., 2010, A&A, 524, 68; Baldi, Ettori et al., 2012, A&A, 537, 142; Eckert et al., 2013, A&A, 551, 23; Planelles et al., 2013, MNRAS; Roncarelli et al., 2013, MNRAS; Ettori et al., 2013, SSRv, arXiv:1303.3530
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X-ray mass: CLASH (Donahue+14)
MCXO/MWL@0.5Mpc: 0.88±0.07 MCXO/MSWL@0.5Mpc: 1.11±0.07
MXMM/MSWL@0.5Mpc: 0.82±0.10MXMM/MWL@0.5Mpc: 0.76±0.05
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X-WL mass: CoMaLit (Sereno+Ettori14) Comparing Masses in Literature (CoMaLit)
I. Bias and scatter in WL and X-ray mass estimates of clusters II. The scaling relation between M and Planck YSZ
III. Literature Catalogs of weak lensing galaxy clustersIV. Evolution and self-similarity of scaling relations:
the cases of M – {σopt, R, LX, YSZ}
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Thermodynamic properties of the ICM for 18 objects in common with Planck SZ thermal pressure and the ROSAT X-ray gas density profiles
(Eckert et al. 13a & 13b)
The X-ray/SZ view out to R200
CC / nCC
T = P/n K = P/n5/3 M = -r2/(G μ m n) dP/dr
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The X-ray/SZ view out to R200
500R/R0.5 1 1.5 2
gas
f
0.05
0.1
0.15
0.2
6obj CC12obj NCCAverage CCAverage NCC
WMAP7
200RPlanck+ROSAT (Eckert et al. 2013b)
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The X-ray/SZ view out to R200
500R/R0.5 1 1.5 2
gas
f
0.05
0.1
0.15
0.2
6obj CC12obj NCCAverage CCAverage NCC
WMAP7
200R
HE violation?Clumping?
Planck+ROSAT (Eckert et al. 2013b)
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Clusters of galaxies: outskirtsXMM-LP (PI: Eckert):
12 objects @z=0.04-0.1, to cover up to R200,
& S/N>10 in Planck data
A2255
A2319
A644
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Clusters of galaxies: outskirtsA2142 (~1.3e15 M¤, z=0.09)
Combined X-SZ analysis (Tchernin+15)
XMM Planck
R200 deproj(Smean) / deproj(Smedian)
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The Athena Observato ry
L2 orbit Ariane V Mass < 5100 kg Power 2500 W 5 year mission
X-ray Integral Field Unit: ΔE: 2.5 eV Field of View: 5 arcmin Operating temp: 50 mk
Wide Field Imager: ΔE: 125 eV Field of View: 40 arcmin High countrate capability
Silicon Pore Optics: 2 m2 at 1 keV 5 arcsec HEW Focal length: 12 m Sensitivity: 3 10-17 erg cm-2 s-1
Rau et al. 2013 arXiv1307.1709 Barret et al., 2013 arXiv:1308.6784
Willingale et al, 2013 arXiv1308.6785
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The fo rmat ion and evo lu t ion o f c lus te r s and g roups o f ga lax ies
How and when was the energy contained in the hot intra-cluster medium generated?
How does ordinary matter assemble into the large-scale structures that we see today?
Ettori, Pratt et al., 2013 arXiv1306.2322
With 100k-sec WFI exposure, gas emissivity, T, Z with 2, 3, 18% (90% c.l.) can be measured at R200.
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The fo rmat ion and evo lu t ion o f c lus te r s and g roups o f ga lax ies
How and when was the energy contained in the hot intra-cluster medium generated?
How does ordinary matter assemble into the large-scale structures that we see today?
Ettori, Pratt et al., 2013 arXiv1306.2322
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The fo rmat ion and evo lu t ion o f c lus te r s and g roups o f ga lax ies
How and when was the energy contained in the hot intra-cluster medium generated?
How does ordinary matter assemble into the large-scale structures that we see today?
Ettori, Pratt et al., 2013 arXiv1306.2322
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The fo rmat ion and evo lu t ion o f c lus te r s and g roups o f ga lax ies
How and when was the energy contained in the hot intra-cluster medium generated?
Bulk motion and turbulent broadening of FeXXV Ka line. With 100k-sec X-IFU exposure, 0+20, 200±5, 400±10 km/s can be resolved.
Simulated Velocity map
100 km/s 500
Ettori, Pratt, et al., 2013 arXiv1306.2322
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Total mass from SZ/X-rays
Mtot ∝ Lα M βg T
γ ; 4α +3β + 2γ = 3
• low counts statistic: scaling relations (for galaxy clusters mass function: Mtot vs L/T/Mgas/YX or a combination of these…)Ettori et al. 2012; Ettori 2013 & 2014
Total mass is the fundamental tool to use Galaxy clusters as cosmological probes
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Total mass from SZ/X-rays
Mtot ∝ Lα M βg T
γ ; 4α +3β + 2γ = 3
• low counts statistic: scaling relations (for galaxy clusters mass function: Mtot vs L/T/Mgas/YX or a combination of these…)Ettori et al. 2012; Ettori 2013 & 2014
Total mass is the fundamental tool to use Galaxy clusters as cosmological probes
Mtot ~ Mgas α T -1.5α+1.5
α = 0 … Mtot ~ T 1.5α = 1 … Mtot ~ Mgasα = 3/5 … Mtot ~ (Mgas T) 3/5 ~ Y 3/5
Mtot ~ L α T -2α+1.5
α = 0 … Mtot ~ T 1.5α = 3/4 … Mtot ~ L 3/4α = 1/2 … Mtot ~ (LT) 1/2
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X-ray/SZ scaling relations: Self-similar +{fg, C, β}
The self-similar scenario predictsslope and z-evolution of the power-law
relations between Mtot & X-ray/SZ quantities
and also the normalization
The self-similar predictions on normalization & slope can fully
explain the observed X-SZ SL once {fg(M), βP(M), C} are considered
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X-ray/SZ scaling relations: Self-similar +{fg, C, β}
Here, the normalizations & slopes are analytic
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X-ray/SZ scaling relations: Self-similar +{fg, C, β}
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X-ray/SZ scaling relations: Self-similar +{fg, C, β}
(Ettori14)
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Conclusions (waiting for Athena)
• from simulations, we are understanding biases & scatter in hydrostatic & lensing masses; the measured distribution explains the observed MHE/Mlens (but still large deviations btw different samples)
• Combining X-ray+SZ profiles is a promising tool to recover (clumping-free) cluster physical quantities (and also MHE)
• generalized-SRs & physical-SRs define a framework for X-ray/SZ scaling laws that permit to reconstruct M with the lowest scatter (up to 50% lower than the one from standard-SRs)
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