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Inner dark matter distribution of the Cosmic Horseshoe (J1148+1930) with gravitational lensing and dynamics

MPS-Authors
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Schuldt,  S.
Physical Cosmology, MPI for Astrophysics, Max Planck Society;

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Chirivì,  G.
Physical Cosmology, MPI for Astrophysics, Max Planck Society;

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Suyu,  S. H.
Physical Cosmology, MPI for Astrophysics, Max Planck Society;

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Yildirim,  A.
Physical Cosmology, MPI for Astrophysics, Max Planck Society;

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Citation

Schuldt, S., Chirivì, G., Suyu, S. H., Yildirim, A., Sonnenfeld, A., Halkola, A., et al. (2019). Inner dark matter distribution of the Cosmic Horseshoe (J1148+1930) with gravitational lensing and dynamics. Astronomy and Astrophysics, 631: A40. doi:10.1051/0004-6361/201935042.


Cite as: http://hdl.handle.net/21.11116/0000-0005-6238-E
Abstract
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 counterimage zs, r = 1.961 ± 0.001 from Gemini observations. To disentangle the dark and luminous matter, we considered three different profiles for the dark matter (DM) distribution: a power law profile, the Navarro, Frenk, and White (NFW) profile, and a generalized version of the NFW profile. For the luminous matter distribution, we based the model 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 mass-to-light ratio (M/L). To constrain the model further, we included published velocity dispersion measurements of the lens galaxy and performed a self-consistent lensing and axisymmetric Jeans dynamical modeling. Our model fits well to the observations including the radial arc, independent of the DM profile. Depending on the DM profile, we get a DM fraction between 60% and 70%. With our composite mass model we find that the radial arc helps to constrain the inner DM distribution of the Cosmic Horseshoe independently of the DM profile.