Enhanced cluster lensing models with measured galaxy kinematics. (arXiv:1905.13236v1 [astro-ph.GA])

Enhanced cluster lensing models with measured galaxy kinematics. (arXiv:1905.13236v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Bergamini_P/0/1/0/all/0/1">P. Bergamini</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rosati_P/0/1/0/all/0/1">P. Rosati</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mercurio_A/0/1/0/all/0/1">A. Mercurio</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Caminha_G/0/1/0/all/0/1">G. B. Caminha</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Meneghetti_M/0/1/0/all/0/1">M. Meneghetti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Agnello_A/0/1/0/all/0/1">A. Agnello</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Biviano_A/0/1/0/all/0/1">A. Biviano</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Calura_F/0/1/0/all/0/1">F. Calura</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Giocoli_C/0/1/0/all/0/1">C. Giocoli</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lombardi_M/0/1/0/all/0/1">M. Lombardi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rodighiero_G/0/1/0/all/0/1">G. Rodighiero</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Vanzella_E/0/1/0/all/0/1">E. Vanzella</a>

We present improved mass models of three CLASH/HFF massive clusters, MACS
J1206.2-0847, MACS J0416.1-0403, Abell S1063. We reconstruct the subhalo mass
component with robust stellar kinematics of cluster galaxies, coupled with
precise strong lensing models from large samples of spectroscopically confirmed
multiple images. We use VLT/MUSE integral-field spectroscopy in the cluster
cores to measure the stellar velocity dispersion $sigma$ of 40-60 member
galaxies per cluster, covering 4-5 magnitudes to $m_{F160W}simeq 21.5$. We
test the accuracy of velocity dispersion measurements on mock spectra, thus
quantifying the limiting signal-to-noise and minimum velocity
($sigma>80$,vel) for the depth of the spectra presented here. With these
data, we determine the normalization and slope of the Faber-Jackson relation in
each cluster and use it a prior for the scaling relations of the sub-halo
population in the lensing mass models. Compared to our previous lens models,
the inclusion of stellar kinematics yields a similar precision in the predicted
positions of the multiple images. However, the inherent degeneracy between the
central effective velocity dispersion, $sigma_0$, and truncation radius,
$r_{cut}$, of subhalos is strongly reduced, significantly alleviating
systematics in the measurements of subhalo masses. The three independent
determinations of the $sigma_0mbox{-}r_{cut}$ relation in each cluster are
fully consistent, enabling a statistical determination of subhalo sizes at
given $sigma_0$ or mass. Finally, we derive the galaxy central velocity
dispersion functions of the three clusters projected within 16% of their
virial radii, finding that they are well in agreement with each other. This
methodology, when applied to high-quality kinematics and strong lensing data,
allows the subhalo mass functions to be determined and compared with
predictions from cosmological simulations.

We present improved mass models of three CLASH/HFF massive clusters, MACS
J1206.2-0847, MACS J0416.1-0403, Abell S1063. We reconstruct the subhalo mass
component with robust stellar kinematics of cluster galaxies, coupled with
precise strong lensing models from large samples of spectroscopically confirmed
multiple images. We use VLT/MUSE integral-field spectroscopy in the cluster
cores to measure the stellar velocity dispersion $sigma$ of 40-60 member
galaxies per cluster, covering 4-5 magnitudes to $m_{F160W}simeq 21.5$. We
test the accuracy of velocity dispersion measurements on mock spectra, thus
quantifying the limiting signal-to-noise and minimum velocity
($sigma>80$,vel) for the depth of the spectra presented here. With these
data, we determine the normalization and slope of the Faber-Jackson relation in
each cluster and use it a prior for the scaling relations of the sub-halo
population in the lensing mass models. Compared to our previous lens models,
the inclusion of stellar kinematics yields a similar precision in the predicted
positions of the multiple images. However, the inherent degeneracy between the
central effective velocity dispersion, $sigma_0$, and truncation radius,
$r_{cut}$, of subhalos is strongly reduced, significantly alleviating
systematics in the measurements of subhalo masses. The three independent
determinations of the $sigma_0mbox{-}r_{cut}$ relation in each cluster are
fully consistent, enabling a statistical determination of subhalo sizes at
given $sigma_0$ or mass. Finally, we derive the galaxy central velocity
dispersion functions of the three clusters projected within 16% of their
virial radii, finding that they are well in agreement with each other. This
methodology, when applied to high-quality kinematics and strong lensing data,
allows the subhalo mass functions to be determined and compared with
predictions from cosmological simulations.

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