H0LiCOW XII. Lens mass model of WFI2033-4723 and blind measurement of its time-delay distance and $H_0$. (arXiv:1905.09338v1 [astro-ph.CO])

H0LiCOW XII. Lens mass model of WFI2033-4723 and blind measurement of its time-delay distance and $H_0$. (arXiv:1905.09338v1 [astro-ph.CO])
<a href="http://arxiv.org/find/astro-ph/1/au:+Rusu_C/0/1/0/all/0/1">Cristian E. Rusu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Wong_K/0/1/0/all/0/1">Kenneth C. Wong</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bonvin_V/0/1/0/all/0/1">Vivien Bonvin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sluse_D/0/1/0/all/0/1">Dominique Sluse</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Suyu_S/0/1/0/all/0/1">Sherry H. Suyu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Fassnacht_C/0/1/0/all/0/1">Christopher D. Fassnacht</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chan_J/0/1/0/all/0/1">James H. H. Chan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hilbert_S/0/1/0/all/0/1">Stefan Hilbert</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Auger_M/0/1/0/all/0/1">Matthew W. Auger</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Sonnenfeld_A/0/1/0/all/0/1">Alessandro Sonnenfeld</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Birrer_S/0/1/0/all/0/1">Simon Birrer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Courbin_F/0/1/0/all/0/1">Frederic Courbin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Treu_T/0/1/0/all/0/1">Tommaso Treu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chen_G/0/1/0/all/0/1">Geoff C.-F. Chen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Halkola_A/0/1/0/all/0/1">Aleksi Halkola</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Koopmans_L/0/1/0/all/0/1">Leon V. E. Koopmans</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marshall_P/0/1/0/all/0/1">Philip J. Marshall</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Shajib_A/0/1/0/all/0/1">Anowar J. Shajib</a>

We present the lens mass model of the quadruply-imaged gravitationally lensed
quasar WFI2033-4723, and perform a blind cosmographical analysis based on this
system. Our analysis combines (1) time-delay measurements from 14 years of data
obtained by the COSmological MOnitoring of GRAvItational Lenses (COSMOGRAIL)
collaboration, (2) high-resolution $textit{Hubble Space Telescope}$ imaging,
(3) a measurement of the velocity dispersion of the lens galaxy based on
ESO-MUSE data, and (4) multi-band, wide-field imaging and spectroscopy
characterizing the lens environment. We account for all known sources of
systematics, including the influence of nearby perturbers and complex
line-of-sight structure, as well as the parametrization of the light and mass
profiles of the lensing galaxy. After unblinding, we determine the effective
time-delay distance to be $4784_{-248}^{+399}~mathrm{Mpc}$, an average
precision of $6.6%$. This translates to a Hubble constant $H_{0} =
71.6_{-4.9}^{+3.8}~mathrm{km~s^{-1}~Mpc^{-1}}$, assuming a flat $Lambda$CDM
cosmology with a uniform prior on $Omega_mathrm{m}$ in the range [0.05, 0.5].
This work is part of the $H_0$ Lenses in COSMOGRAIL’s Wellspring (H0LiCOW)
collaboration, and the full time-delay cosmography results from a total of six
strongly lensed systems are presented in a companion paper (Wong et. al. 2019,
in preparation).

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