observational constraints on galaxy clusters and dm dynamics doron lemze tel-aviv university / johns...
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![Page 1: Observational Constraints on Galaxy Clusters and DM Dynamics Doron Lemze Tel-Aviv University / Johns Hopkins University Collaborators : Tom Broadhurst,](https://reader035.vdocuments.site/reader035/viewer/2022062519/56649ecb5503460f94bd9555/html5/thumbnails/1.jpg)
Observational Constraints on Galaxy
Clusters and DM Dynamics
Doron Lemze
Tel-Aviv University / Johns Hopkins University
Collaborators:Tom Broadhurst, Yoel Rephaeli, Rennan Barkana, Keiichi
Umetsu,
Rick Wagner, & Mike Norman
21/9/10
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Overview:
• Observational constraints on galaxy clusters.
Study case: the high-mass cluster A1689
• DM Dynamics
Lemze, Broadhurst, Rephaeli , Barkana, & Umetsu 2009
Lemze, Rephaeli , Barkana, Broadhurst, Wagner, & Norman 2010
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Subaru/suprime-cam
VLT/VIMOS
The measuring instruments
Hubble
Strong lensing
Weak lensing Imaging of cluster galaxies
Cluster galaxies
spectroscopy
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cD galaxy
0 0.5’Lemze, Barkana, Broadhurst & Rephaeli 2008
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Galaxy surface number density
About 1900 cluster members.
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Velocity-Space Diagram
Velocity caustics method:Diaferio & Geller 1997
Diaferio 1999
About 500 cluster members.
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Methodology
2
22)()(
)()()(2
)()(r
rrGMrr
r
rrr
dr
d gal
rgalrgal
)(
)(1)(
2
2
r
rr
r
t
R
galgal
Rr
rdrrR
22
)(2)(
R
rgal
gal
pRr
rdrrR
rrr
RR
22
2
2
2
2
2
))(1)(()(
)(
2)(
Jeans eq.
Velocity anisotropy
Galaxy surface number density
Projected velocity dispersion
The unknowns: rgal M is taken from lensing
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Galaxy surface number density
data points : 20
Projected velocity dispersion
data points : 10
The number of free
parameters : 5
---------------------------------------
dof : 25
Galaxy surface
number density fit
Projected velocity
dispersion fit
)530/(6.15/22 dofr
)210/(6.32 r
)320/(122 r
The fit results
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Galaxy number density profile
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Velocity anisotropy profile
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Galaxy velocity anisotropy data vs. simulations
Arieli, Rephaeli, & Norman 2010
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Mass profiles
r
caustics dxxFxAGrM0
2 )()(/1)( Here M is not taken from lensing!
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The high concentration problem
Broadhurst et al. 2008
Zitrin et al. 2010
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A1689 MS2137
Can we trust the high value found?
Comerford & Natarajan 2007
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13virc
sunvirMhM 11510)4.03.1(
Virial mass vs. concentration parameter
Here M is not taken from lensing!
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Comerford & Natarajan 2007
Hennawi et al. 2007
Bullock et al. 2007
62 clusters
Building statistical samples
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Duffy et al. 2007
10 halos per data bin
N-body simulations using WMAP5 parameters
X-ray measurements
Building statistical samples
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Johnston et al. 2007
Weak lensing measurements of stacked
SDSS groups and galaxy clusters
In agreement with Mandelbaum et al.
2006
Large samples
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Conclusions
• We estimated for the first time
a detailed 3D velocity profile.
• We found that the caustic
mass is a good estimation for
the mass profile.
• Our three independent
estimates for the mass profile
are consistent with each
other.
• We constrained the virial
mass using galaxy positions
and velocities data.
• We deduced high values for
the concentration parameter
using two independent
methods.
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DM dynamics
Question: how one can determine DM dynamics when
“DM spectroscopy” is hard to obtain?
Answer: by using a surrogate Measurement. The first
Choice should be other kind of collisionless particles - galaxies.
The orbit of a test particle in a collisionless gravitational system is
independent of the particle mass. This would presumably imply
that once hydrostatic equilibrium is attained, most likely as a result
mixing and mean field relaxation, DM and galaxies should have the
same mean specific kinetic energy, i.e., ,
where
)()( 2,
2, rr totgaltotDM
))(23)(()()()()( 2,
2,
2,
2,
2, rrrrrr iriiiritoti
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Host et al. 2009
DM velocity anisotropy
Best-fit value:13.027.049.0
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DM density
All other colors
DM density
Galaxy density
Total matter density
1])/1)(/[( ssDM rrrr12106061330
sr27.176.079.2
Best-fit values:
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Model-dependent Model-independent
)(
)()( 2
,
2,
r
rrf
totgal
totDM
coll
The collisionless profile
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Model-independentModel-dependent
colltotDM
totgalf
r
rrb /1
)(
)()(
,
,
The velocity bias profile
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Conclusions
• We obtain the mean value of the
DM velocity anisotropy parameter,
and the DM density profile.
• r 1/3 r_vir seems to be a ∼transition region interior to which
collisional effects significantly modify
the dynamical properties of the
galaxy population with respect to
those of DM in A1689
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Comerford & Natarajan 2007
Hennawi et al. 2007
Bullock et al. 2007
??C is measured using lensing and X-ray???
62 clusters
Building statistical samples
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Duffy et al. 2007
10 halos per data bin
N-body simulation using WMAP5 parameters – lower sigma_8
X-ray measurements
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X-ray data
dr
rd
dr
rd
rmG
Trk gasgas
gasp
B)()(
)(21
2 21 gasgasgas
Assuming
a gas density profile
Double model
Assuming
a temperature profile
Isothermal
Fitting a double
Surface brightness
model
Where a single model is
2
3
2
2
1)0()(
c
gasgas r
rnrn
For gas in hydrostatic equilibriumdr
d
dr
dPgas
gas
1
,2
)(
r
rGM
dr
d
, and Tk
mP
B
p
gas
gas
.
For the isothermal assumption:
where
For obtaining the mass profile:
Lensing data )(rM
What has been done previously?
)(rM
crit
Assuming
a DM profile
NFW
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Doron Lemze
Tel-Aviv University
Collaborators:Tom Broadhurst , Rennan Barkana, Yoel Rephaeli, Keiich Umetsu
Collaborators:
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Johnston et al. 2007
Weak lensing measurements of stacked
SDSS groups and galaxy clusters
In agreement with Mandelbaum et al.
2006
Large samples
Black points are from the shear profile
fits for the L200 luminosity bins and the
red points are from the N200 richness bins.
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In
Rachel Mandelbaum, Uros Seljak, Christopher M. Hirata 2008
Astro-ph 0805.2552v2
FIG. 5: The best-fit c(M) relation at z = 0.22 with the 1
allowed region indicated. The red points with errorbars show
the best-fit masses and concentrations for each bin when we
fit them individually, without requiring a power-law c(M) relation.
The blue dotted lines show the predictions of [39] for
our mass definition and redshift, for theWMAP1 (higher) and
WMAP3 (lower) cosmologies. The prediction for theWMAP5
cosmology falls in between the two and is not shown here.
Their measurements are actually lower than the theoretical model
Eventhough they have used WMAP1 (which gives a lower curve see
Duffy et al. 2007). This indicate that they stack the clusters without
Exactly center them ontop of each other and didn’t separate the background
From the cluster galaxy good. These two effect lowers the concentration value.
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