Cluster Cosmology Constraints from the 2500 deg$^2$ SPT-SZ Survey: Inclusion of Weak Gravitational Lensing Data from Magellan and the Hubble Space Telescope. (arXiv:1812.01679v1 [astro-ph.CO])
<a href="http://arxiv.org/find/astro-ph/1/au:+Bocquet_S/0/1/0/all/0/1">S. Bocquet</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dietrich_J/0/1/0/all/0/1">J. P. Dietrich</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Schrabback_T/0/1/0/all/0/1">T. Schrabback</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bleem_L/0/1/0/all/0/1">L. E. Bleem</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Klein_M/0/1/0/all/0/1">M. Klein</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Allen_S/0/1/0/all/0/1">S. W. Allen</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Applegate_D/0/1/0/all/0/1">D. E. Applegate</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ashby_M/0/1/0/all/0/1">M. L. N. Ashby</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bautz_M/0/1/0/all/0/1">M. Bautz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bayliss_M/0/1/0/all/0/1">M. Bayliss</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Benson_B/0/1/0/all/0/1">B. A. Benson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Brodwin_M/0/1/0/all/0/1">M. Brodwin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Bulbul_E/0/1/0/all/0/1">E. Bulbul</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Canning_R/0/1/0/all/0/1">R. E. A. Canning</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Capasso_R/0/1/0/all/0/1">R. Capasso</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Carlstrom_J/0/1/0/all/0/1">J. E. Carlstrom</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chang_C/0/1/0/all/0/1">C. L. Chang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Chiu_I/0/1/0/all/0/1">I. Chiu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Cho_H/0/1/0/all/0/1">H-M. Cho</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Clocchiatti_A/0/1/0/all/0/1">A. Clocchiatti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Crawford_T/0/1/0/all/0/1">T. M. Crawford</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Crites_A/0/1/0/all/0/1">A. T. Crites</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Haan_T/0/1/0/all/0/1">T. de Haan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Desai_S/0/1/0/all/0/1">S. Desai</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Dobbs_M/0/1/0/all/0/1">M. A. Dobbs</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Foley_R/0/1/0/all/0/1">R. J. Foley</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Forman_W/0/1/0/all/0/1">W. R. Forman</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Garmire_G/0/1/0/all/0/1">G. P. Garmire</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+George_E/0/1/0/all/0/1">E. M. George</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gladders_M/0/1/0/all/0/1">M. D. Gladders</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gonzalez_A/0/1/0/all/0/1">A. H. Gonzalez</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Grandis_S/0/1/0/all/0/1">S. Grandis</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Gupta_N/0/1/0/all/0/1">N. Gupta</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Halverson_N/0/1/0/all/0/1">N. W. Halverson</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hlavacek_Larrondo_J/0/1/0/all/0/1">J. Hlavacek-Larrondo</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hoekstra_H/0/1/0/all/0/1">H. Hoekstra</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Holder_G/0/1/0/all/0/1">G. P. Holder</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Holzapfel_W/0/1/0/all/0/1">W. L. Holzapfel</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hou_Z/0/1/0/all/0/1">Z. Hou</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hrubes_J/0/1/0/all/0/1">J. D. Hrubes</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Huang_N/0/1/0/all/0/1">N. Huang</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Jones_C/0/1/0/all/0/1">C. Jones</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Khullar_G/0/1/0/all/0/1">G. Khullar</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Knox_L/0/1/0/all/0/1">L. Knox</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Kraft_R/0/1/0/all/0/1">R. Kraft</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Lee_A/0/1/0/all/0/1">A. T. Lee</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Linden_A/0/1/0/all/0/1">A. von der Linden</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Luong_Van_D/0/1/0/all/0/1">D. Luong-Van</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mantz_A/0/1/0/all/0/1">A. Mantz</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Marrone_D/0/1/0/all/0/1">D. P. Marrone</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McDonald_M/0/1/0/all/0/1">M. McDonald</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+McMahon_J/0/1/0/all/0/1">J. J. McMahon</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Meyer_S/0/1/0/all/0/1">S. S. Meyer</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mocanu_L/0/1/0/all/0/1">L. M. Mocanu</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Mohr_J/0/1/0/all/0/1">J. J. Mohr</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Morris_R/0/1/0/all/0/1">R. G. Morris</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Padin_S/0/1/0/all/0/1">S. Padin</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Patil_S/0/1/0/all/0/1">S. Patil</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Pryke_C/0/1/0/all/0/1">C. Pryke</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Rapetti_D/0/1/0/all/0/1">D. Rapetti</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Reichardt_C/0/1/0/all/0/1">C. L. Reichardt</a>, et al. (19 additional authors not shown)
We derive cosmological constraints using a galaxy cluster sample selected We derive cosmological constraints using a galaxy cluster sample selected http://arxiv.org/icons/sfx.gif
from the 2500 deg$^2$ SPT-SZ survey. The sample spans the redshift range
$0.25
gravitational lensing measurements of 32 clusters in the range $0.29
from the 2500 deg$^2$ SPT-SZ survey. The sample spans the redshift range
$0.25<z<1.75$ and consists of 377 cluster candidates with SZ detection
significance $xi>5$. The sample is supplemented with optical weak
gravitational lensing measurements of 32 clusters in the range $0.29<z<1.13$
(using data from Magellan and the Hubble Space Telescope) and X-ray
measurements of 89 cluster in the range $0.25<z<1.75$ (from Chandra). We rely
on minimal modeling assumptions: i) weak lensing provides an accurate means of
measuring halo masses, ii) the mean SZ and X-ray observables are related to the
true halo mass through power-law relations in mass and dimensionless Hubble
parameter $E(z)$ with a-priori unknown parameters, iii) there is (correlated,
lognormal) intrinsic scatter and scatter due to measurement uncertainties
relating these observables to their mean relations. Assuming a flat
$nuLambda$CDM model, in which the sum of neutrino masses is a free parameter,
we measure $Omega_mathrm{m}=0.276pm0.047$, $sigma_8=0.781pm0.037$, and the
parameter combination $sigma_8(Omega_mathrm{m}/0.3)^{0.2}=0.766pm0.025$.
The redshift evolution of the X-ray $Y_X$–mass and $M_mathrm{gas}$–mass
relations are both consistent with self-similar evolution to within $1sigma$.
The mass-slope of the $Y_X$–mass relation shows a $2.3sigma$ deviation from
self-similarity. The mass-slope of the $M_mathrm{gas}$–mass relation is
steeper than self-similarity at the $2.5sigma$ level. In a $nu w$CDM
cosmology, we measure the dark energy equation of state parameter
$w=-1.55pm0.41$ from the cluster data. We perform a measurement of the growth
of structure since redshift $zsim1.7$ and find no evidence for tension with
the prediction from General Relativity. (abridged)
