The inner dark matter distribution of the Cosmic Horseshoe (J1148+1930) with gravitational lensing and dynamics. (arXiv:1901.02896v1 [astro-ph.GA])

The inner dark matter distribution of the Cosmic Horseshoe (J1148+1930) with gravitational lensing and dynamics. (arXiv:1901.02896v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Schuldt_S/0/1/0/all/0/1">S. Schuldt</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chirivi_G/0/1/0/all/0/1">G. Chiriv&#xec;</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Suyu_S/0/1/0/all/0/1">S. H. Suyu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Yildirim_A/0/1/0/all/0/1">A. Y&#x131;ld&#x131;r&#x131;m</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sonnenfeld_A/0/1/0/all/0/1">A. Sonnenfeld</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Halkola_A/0/1/0/all/0/1">A. Halkola</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lewis_G/0/1/0/all/0/1">G. F. Lewis</a>

We present a detailed analysis of the inner mass structure of the Cosmic
Horseshoe (J1148+1930) strong gravitational lens system observed with the
Hubble Space Telescope (HST) Wide Field Camera 3 (WFC3). In addition to the
spectacular Einstein ring, this systems shows a radial arc. We obtained the
redshift of the radial arc counter image $z_text{s,r} = 1.961 pm 0.001$ from
Gemini observations. To disentangle the dark and luminous matter, we consider
three different profiles for the dark matter distribution: a power-law profile,
the NFW, and a generalized version of the NFW profile. For the luminous matter
distribution, we base it on the observed light distribution that is fitted with
three components: a point mass for the central light component resembling an
active galactic nucleus, and the remaining two extended light components scaled
by a constant M/L. To constrain the model further, we include published
velocity dispersion measurements of the lens galaxy and perform a
self-consistent lensing and axisymmetric Jeans dynamical modeling. Our model
fits well to the observations including the radial arc, independent of the dark
matter profile. Depending on the dark matter profile, we get a dark matter
fraction between 60 % and 70 %. With our composite mass model we find that the
radial arc helps to constrain the inner dark matter distribution of the Cosmic
Hoseshoe independently of the dark matter profile.

We present a detailed analysis of the inner mass structure of the Cosmic
Horseshoe (J1148+1930) strong gravitational lens system observed with the
Hubble Space Telescope (HST) Wide Field Camera 3 (WFC3). In addition to the
spectacular Einstein ring, this systems shows a radial arc. We obtained the
redshift of the radial arc counter image $z_text{s,r} = 1.961 pm 0.001$ from
Gemini observations. To disentangle the dark and luminous matter, we consider
three different profiles for the dark matter distribution: a power-law profile,
the NFW, and a generalized version of the NFW profile. For the luminous matter
distribution, we base it on the observed light distribution that is fitted with
three components: a point mass for the central light component resembling an
active galactic nucleus, and the remaining two extended light components scaled
by a constant M/L. To constrain the model further, we include published
velocity dispersion measurements of the lens galaxy and perform a
self-consistent lensing and axisymmetric Jeans dynamical modeling. Our model
fits well to the observations including the radial arc, independent of the dark
matter profile. Depending on the dark matter profile, we get a dark matter
fraction between 60 % and 70 %. With our composite mass model we find that the
radial arc helps to constrain the inner dark matter distribution of the Cosmic
Hoseshoe independently of the dark matter profile.

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