x-ray clusters in conformal gravity antonaldo diaferio universita' degli studi di torino...
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X-RAY CLUSTERS IN CONFORMAL GRAVITY
Antonaldo Diaferio
Universita' degli Studi di TorinoDipartimento di Fisica Generale
“Amedeo Avogadro”
Edinburgh, April 21st, 2006
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Introduction on conformal factor: photon and massive particle geodesics
Gravitational potential energy of extended objects
Virial theorem and average temperature in X-ray clusters
Hydro-static equilibrium and temperature profile
SPH simulations of self-gravitating gas
OUTLINE
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X-RAY CLUSTERS: OBSERVED
CL0016+16 ROSAT PSPC
X-ray spectrum Temperature
ICM mass
radiusT
em
pe
ratu
re
15 clusters observed with XMM-Newton
(De Grandi et al . 2004)
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X-RAY CLUSTERS: SIMULATED(WITH GR + DM)
(Diaferio et al. 2005) (Borgani et al. 2004)
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The Mannheim-Kazanas (MK) parameterization:
(Walker 1994, Edery & Paranjape 1998, Pireaux 2004a,b)
> 0 0
gravitational potentialdeflection angle
metric
geodesicequation
CONFORMAL GRAVITY BASICS (1)
massive particles: E>0photons: E=0
independent of 2
action
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CONFORMAL GRAVITY BASICS (2)
The Mannheim-Kazanas (MK) parameterization
The Horne parameterization (adopted here)
POTENTIAL OF A STATIC POINT SOURCE
To fit galaxy rotation curves:
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POTENTIAL GRADIENT OF SPHERICALLY SYMMETRIC
EXTENDED OBJECTS
Newtoniancomponent
Conformalcomponent
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THE VIRIAL THEOREM (1)
Euler theorem on homogeneous functions
potential energies
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THE VIRIAL THEOREM (2)
Example: sphere of radius “a”with a power-law density profile
<0
>0
1012 Msol
1013 Msol
mas
s
a = 1 Mpc
= 5/3
Applying the virial theorem
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CLUSTERS IN VIRIAL EQUILIBRIUM
ARE HOTTER THAN OBSERVED.
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ICM TEMPERATURE PROFILE
Hydro-static eq.
Solution
Power-lawdensity profile
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AT LARGE RADII,
CLUSTERS IN HYDROSTATIC EQUILIBRIUM
HAVE A TEMPERATURE PROFILE
WHICH INCREASES AT LEAST AS r2.
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SPH SIMULATIONSModified version of Gadget-1.1 (Springel et al. 2001)
extended particles
Potential
Acceleration
x=r/h
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GRAVITATIONAL ACCELERATION DUE TO INDIVIDUAL PARTICLES
Newtonian term
Conformalterm
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A TEST SIMULATION
initial density profile from A2199:
-model with rc=134 kpc
total mass M = 2.7x1013 Msol
# of SPH particles = 4096softening =0.1 kpc
adiabatic simulation with Tin=0
vacuum boundary conditions
NO MULTIPOLE EXPANSION DIRECT SUMMATION
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SIMULATION RESULTS (1)
X-ray surf. bright. evolution
2 Mpc
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SIMULATION RESULTS (2)
Temperature evolution
2 Mpc
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SIMULATION RESULTS (3)
Energy evolution Size evolutionenergy conservation
pot. en.
tot. en.
th. en.
kin. en.
temperature virial ratio
90%
10%
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SIMULATION RESULTS (4)Density profile at eq. Temperature profile at eq.
0=1.6x10-25 g cm-3
rc=142 kpc
=1.65
r2
r1/2
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CONCLUSION X-ray clusters are too hot and have an increasing temperature profile when the MK conformal factor choice is implemented in conformal gravity
N-body simulations confirm the virial theorem estimates
Appropriate boundary conditions needed
Conformal factor choice to be revised?
We have got an SPH/N-body code that can be used for simulations with physically motivated initial conditions