Correlations of mass distributions between dark matter and visible matter
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Correlations of Mass Distributions between Dark Matter and Visible Matter. KIAS-APCTP-DMRC Workshop on “The Dark Side of the Universe” May 24, 2005. Yuriy Mishchenko and Chueng-Ryong Ji NC State University Raleigh, NC. Motivation.

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Correlations of mass distributions between dark matter and visible matter

Correlations of Mass Distributionsbetween Dark Matter and Visible Matter

KIAS-APCTP-DMRC Workshop on

“The Dark Side of the Universe”

May 24, 2005

Yuriy Mishchenko and Chueng-Ryong Ji

NC State University Raleigh, NC


Motivation

Motivation

  • Universal Rotation Curves in Spiral Galaxies and

    Strong Gravitational Lensing in Galaxy Clusters

    provide convincing evidences of Dark Matter.

  • High Resolution Mass Map of CL0024+1654 is now available from the deep imaging with the Hubble Space Telescope.

  • Two dramatically different systems seem to exhibit a consistency in correlations of mass distributions between Dark Matter and Visible Matter.

    Y.Mishchenko and C.Ji, PRD68, 063503 (2003)


Outline

Outline

  • Gravitational Lensing

    -Galaxy Clusters CL0024+1654

    -Mass Map by Tyson et al.

    -Simple but general theromodynamic analysis

  • Universal Rotation Curves

    -Spiral Galaxies with different luminosities

    -Consistency with the thermodynamic analysis

  • Discussions and Conclusions


Gravitational lensing effect

Gravitational Lensing Effect

  • gravitational lensing is phenomenon of light deflection in gravitational field

  • allows to restore 2D projected mass distribution

Einstein Cross Q2237+0305


Correlations of mass distributions between dark matter and visible matter

CL0024+1654


Dark vs visible in galaxy clusters

Dark vs. Visible in Galaxy Clusters

from J. Tyson, G. Kochanski, I. Dell’Antonio, astro-ph/9801193


Power law model

Power Law Model


Correlations of mass distributions between dark matter and visible matter

J. Tyson, G. Kochanski, I. Dell’Antonio, astro-ph/9801193


Dark vs visible in galaxy clusters1

Dark vs. Visible in Galaxy Clusters

J. Tyson, G. Kochanski, I. Dell’Antonio, 1998:

  • presented analysis of Hubble telescope images of strong gravitational lensing in galaxy cluster CL0024+1654

  • presented detailed mass map and radial “averaged” profiles for total and visible matter

  • primary conclusion was about inconsistency with Cold Dark Matter simulations (soft core)


Correlations of mass distributions between dark matter and visible matter

Correlation between Dark Matter and Visible Matter


Correlations of mass distributions between dark matter and visible matter

Flat Region around 100 kpc

  • projected density radial profiles presented on log-log scale for the total and visible matter distribution

  • if profiles were re-plotted on log-linear scale, one would observe exponential decay

anomalous flat region at about 100kpc in the visible mass profile


Thermodynamic principle

Thermodynamic Principle

Log-Log Linear Correlation


Dark matter in spiral galaxies

Dark Matter in Spiral Galaxies

Rotation Curve represents gas/stars circular orbit velocity as function of distance from the galaxy’s center

spiral galaxy NGC2403


Dark vs visible in spiral galaxies

Dark vs. Visible in Spiral Galaxies

M. Persic, P. Salucci, F. Stel, 1996:

  • presented analysis of a sample of spiral galaxies’ Rotation Curves classified by galaxy luminosities and normalized to vopt and ropt .

  • found that majority of normalized RC in given luminosity group follow universal profiles (Universal Rotation Curves).

  • described URC in terms of simple mass model: dark spherical halo + exponential thin stellar disk.


Correlations of mass distributions between dark matter and visible matter

Universal Rotation Curve of Spiral Galaxy


Universal rotation curves in spiral galaxies

Universal Rotation Curves in Spiral Galaxies

  • In Persic, Salucci, Stel visible mass contribution is known but approximated with an analytical fit,

  • Dark halo contribution is parameterized,

  • Final Rotation Curve is described with


Luminosity dependence of urcs

Luminosity Dependence of URCs


Correlation of mass density

Correlation of Mass Density

  • URC can be fit in the region 0 r/ropt 2 with exponential dark hallo for all luminosities

  • For larger r and are linearly correlated

Exponential Thin Disk

It corresponds to T~105 K consistent with the temperature

of the interstellar gas.


Dark vs visible in spiral galaxies1

Dark vs. Visible in Spiral Galaxies


Dark vs visible in spiral galaxies2

Dark vs. Visible in Spiral Galaxies

Log-Log-Linear Correlation in Spiral Galaxies

best fit values of a for different luminositiesM

…remember  obtained for CL0024+1654,


Dark vs visible matter

Dark vs. Visible Matter

We observed Log-Log-Linear correlation with essentially the same correlation coefficient in different spiral galaxies and a galaxy cluster.

This is a remarkable coincidence…

How do we interprete?


Interpretation of results

Interpretation of Results

  • Local Thermodynamic Equilibrium since it is unlikely

    that the molar mass ratio varies in a precise correlation

    with the temperature ratio to make kappa constant both

    for the galaxy clusters and the spiral galaxies.

  • Visible matter primarily consists of H, H2 and He.

Massive neutrinos and/or axions < 25MeV

WIMP ~ 10GeV-1TeV

SUSY lightest particles(e.g. neutralino)>30GeV


Discussions and conclusions

Discussions and Conclusions

  • Correlations of mass distributions between dark matter and visible matter in two dramatically different systems, galaxy cluster and spiral galaxies, are remarkably consistent with each other.

  • Based on an almost isothermal Boltzmann

    distribution, we find K = 2.1~4.4 which indicate

    the typical mass scale of dark matter particles

    around the order of 100 MeV.

  • Since this is right around the QCD mass scale,

    any relation between the dark matter and QCD vacuum

    condensates?


Correlations of mass distributions between dark matter and visible matter

Things to do:

  • Experimental – improve “statistics”

    • large survey of dark vs. visible matter in galaxy clusters…

  • Theoretical – investigate different possibilities

    • role of gravity in thermalization processes…

    • better understanding of galaxy cluster dynamics…

    • better understanding of spiral galaxy dynamics…


Correlations of mass distributions between dark matter and visible matter

C.Ji, Gungwon Kang and Jungjai Lee, work in progress…


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