Main.DM History
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Gravitational lensing is commonly used to derive the slope of the radial distribution of dark matter in galaxies. Recently, I have followed a different route, looking to the
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Gravitational lensing is commonly used to derive the slope of the radial distribution of dark matter in galaxies. Recently, I have followed a different route, looking at the
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%lframe width=600px% Attach:PA-Ell.png | Correlations observed between the shape of the light and of the total mass distribution in 12 strongly lensed quasars ([[http://adsabs.harvard.edu/abs/2012A%26A...538A..99S | Sluse et al. 2012a]])
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%lframe width=600px% Attach:PA-Ell.png | Correlations observed between the shape of the light and of the total mass distribution in 12 strongly lensed quasars ([[http://adsabs.harvard.edu/abs/2012A%26A...538A..99S | Sluse et al. 2012a]]).
Changed lines 9-11 from:
is its sensitivity to the ''clumpy content of matter'' of
galaxies, allowing one to estimate the fraction of substructures (pure dark matter or dwarf galaxies) with masses > 10'^5^' M'_sun_' in galaxies at redshfits typically z > 0.1. In my work, I develop techniques to get more robust flux ratios in lensed quasars, needed to estimate the amount of susbstructures (e.g. [[http://adsabs.harvard.edu/abs/2006A%26A...449..539S | Sluse et al. 2006]], [[http://adsabs.harvard.edu/abs/2012A%26A...544A..62S| 2012b]], 2012c-submitted). I also search for perturbation of the lensed image
astrometry induced by these matter clumps ([[http://adsabs.harvard.edu/abs/2010A%26A...522A..95C| Chantry, Sluse & Magain 2010]], [[http://adsabs.harvard.edu/abs/2012A%26A...538A..99S | Sluse et al. 2012a]]).
galaxies, allowing one to estimate the fraction of substructures (
astrometry induced by these matter clumps
to:
is its sensitivity to the ''clumpy content of matter'' in
galaxies, allowing one to estimate the fraction of substructures (which can be made of pure dark matter or regular matter in the form of dwarf galaxies) with masses > 10'^5^' M'_sun_' in galaxies at redshfits typically z > 0.1. In my work, I developed techniques to get more robust flux ratios in lensed quasars, which are needed to estimate the amount of susbstructures (e.g. [[http://adsabs.harvard.edu/abs/2006A%26A...449..539S | Sluse et al. 2006]], [[http://adsabs.harvard.edu/abs/2012A%26A...544A..62S| 2012b]], 2012c-submitted). I also search for perturbations in the lensed image
astrometry induced by these clumps of matter ([[http://adsabs.harvard.edu/abs/2010A%26A...522A..95C| Chantry, Sluse & Magain 2010]], [[http://adsabs.harvard.edu/abs/2012A%26A...538A..99S | Sluse et al. 2012a]]).
galaxies, allowing one to estimate the fraction of substructures (which can be made of pure dark matter or regular matter in the form of dwarf galaxies) with masses > 10'^5^' M'_sun_' in galaxies at redshfits typically z > 0.1. In my work, I developed techniques to get more robust flux ratios in lensed quasars, which are needed to estimate the amount of susbstructures (e.g. [[http://adsabs.harvard.edu/abs/2006A%26A...449..539S | Sluse et al. 2006]], [[http://adsabs.harvard.edu/abs/2012A%26A...544A..62S| 2012b]], 2012c-submitted). I also search for perturbations in the lensed image
astrometry induced by these clumps of matter ([[http://adsabs.harvard.edu/abs/2010A%26A...522A..95C| Chantry, Sluse & Magain 2010]], [[http://adsabs.harvard.edu/abs/2012A%26A...538A..99S | Sluse et al. 2012a]]).
Changed line 6 from:
%lframe width=300px% Attach:PA-Ell.png | Correlations found between the shape of the total mass distribution and of the light distribution ([[http://adsabs.harvard.edu/abs/2012A%26A...538A..99S | Sluse et al. 2012a]])
to:
%lframe width=600px% Attach:PA-Ell.png | Correlations observed between the shape of the light and of the total mass distribution in 12 strongly lensed quasars ([[http://adsabs.harvard.edu/abs/2012A%26A...538A..99S | Sluse et al. 2012a]])
Added lines 5-6:
%lframe width=300px% Attach:PA-Ell.png | Correlations found between the shape of the total mass distribution and of the light distribution ([[http://adsabs.harvard.edu/abs/2012A%26A...538A..99S | Sluse et al. 2012a]])
Changed lines 3-4 from:
Gravitational lensing is commonly used to derive the slope of the radial distribution of dark matter in galaxies. Recently, I have investigated the shape of the dark matter profile and its correlation with the light distribution ([[http://adsabs.harvard.edu/abs/2012A%26A...538A..99S | Sluse et al. 2012a]]). \\
to:
Gravitational lensing is commonly used to derive the slope of the radial distribution of dark matter in galaxies. Recently, I have followed a different route, looking to the
shape of the dark matter profile and its correlation with the light distribution ([[http://adsabs.harvard.edu/abs/2012A%26A...538A..99S | Sluse et al. 2012a]]). \\
shape of the dark matter profile and its correlation with the light distribution ([[http://adsabs.harvard.edu/abs/2012A%26A...538A..99S | Sluse et al. 2012a]]). \\
Changed line 3 from:
Gravitational lensing is commonly used to study the slope of the mass distribution and derive the slope of the radial distribution of dark matter in galaxies. Recently, I have investigated the shape of the dark matter profile and its correlation with the light distribution ([[http://adsabs.harvard.edu/abs/2012A%26A...538A..99S | Sluse et al. 2012a]]). \\
to:
Gravitational lensing is commonly used to derive the slope of the radial distribution of dark matter in galaxies. Recently, I have investigated the shape of the dark matter profile and its correlation with the light distribution ([[http://adsabs.harvard.edu/abs/2012A%26A...538A..99S | Sluse et al. 2012a]]). \\
Changed line 3 from:
Gravitational lensing is commonly used to study the slope of the mass distribution and derive the slope of the radial distribution of dark matter in galaxies. Recently, I have investigated the shape of the dark matter profile and its correlation with the light distribution ([[http://adsabs.harvard.edu/abs/2012A%26A...538A..99S | Sluse et al. 2012a]]. \\
to:
Gravitational lensing is commonly used to study the slope of the mass distribution and derive the slope of the radial distribution of dark matter in galaxies. Recently, I have investigated the shape of the dark matter profile and its correlation with the light distribution ([[http://adsabs.harvard.edu/abs/2012A%26A...538A..99S | Sluse et al. 2012a]]). \\
Added lines 1-8:
(:title Dark Matter:)
Gravitational lensing is commonly used to study the slope of the mass distribution and derive the slope of the radial distribution of dark matter in galaxies. Recently, I have investigated the shape of the dark matter profile and its correlation with the light distribution ([[http://adsabs.harvard.edu/abs/2012A%26A...538A..99S | Sluse et al. 2012a]]. \\
[[<<]]
A more unique property of gravitational lensing
is its sensitivity to the ''clumpy content of matter'' of
galaxies, allowing one to estimate the fraction of substructures (pure dark matter or dwarf galaxies) with masses > 10'^5^' M'_sun_' in galaxies at redshfits typically z > 0.1. In my work, I develop techniques to get more robust flux ratios in lensed quasars, needed to estimate the amount of susbstructures (e.g. [[http://adsabs.harvard.edu/abs/2006A%26A...449..539S | Sluse et al. 2006]], [[http://adsabs.harvard.edu/abs/2012A%26A...544A..62S| 2012b]], 2012c-submitted). I also search for perturbation of the lensed image
astrometry induced by these matter clumps ([[http://adsabs.harvard.edu/abs/2010A%26A...522A..95C| Chantry, Sluse & Magain 2010]], [[http://adsabs.harvard.edu/abs/2012A%26A...538A..99S | Sluse et al. 2012a]]).
Gravitational lensing is commonly used to study the slope of the mass distribution and derive the slope of the radial distribution of dark matter in galaxies. Recently, I have investigated the shape of the dark matter profile and its correlation with the light distribution ([[http://adsabs.harvard.edu/abs/2012A%26A...538A..99S | Sluse et al. 2012a]]. \\
[[<<]]
A more unique property of gravitational lensing
is its sensitivity to the ''clumpy content of matter'' of
galaxies, allowing one to estimate the fraction of substructures (pure dark matter or dwarf galaxies) with masses > 10'^5^' M'_sun_' in galaxies at redshfits typically z > 0.1. In my work, I develop techniques to get more robust flux ratios in lensed quasars, needed to estimate the amount of susbstructures (e.g. [[http://adsabs.harvard.edu/abs/2006A%26A...449..539S | Sluse et al. 2006]], [[http://adsabs.harvard.edu/abs/2012A%26A...544A..62S| 2012b]], 2012c-submitted). I also search for perturbation of the lensed image
astrometry induced by these matter clumps ([[http://adsabs.harvard.edu/abs/2010A%26A...522A..95C| Chantry, Sluse & Magain 2010]], [[http://adsabs.harvard.edu/abs/2012A%26A...538A..99S | Sluse et al. 2012a]]).