Irene Sendra

Hubble Space Telescope Combined Strong and Weak Lensing Analysis of the CLASH Sample: Mass and Magnification Models and Systematic Uncertainties

We present results from a comprehensive lensing analysis in HST data, of the complete CLASH cluster sample. We identify new multiple-images previously undiscovered allowing improved or first constraints on the cluster inner mass distributions and profiles. We combine these strong-lensing constraints with weak-lensing shape measurements within the HST FOV to jointly constrain the mass distributions. The analysis is performed in two different common parameterizations (one adopts light-traces-mass for both galaxies and dark matter while the other adopts an analytical, elliptical NFW form for the dark matter), to provide a better assessment of the underlying systematics - which is most important for deep, cluster-lensing surveys, especially when studying magnified high-redshift objects. We find that the typical (median), relative systematic differences throughout the central FOV are

A free-form lensing grid solution for A1689 with new multiple images

\sim40\%

Oscillations in the dark energy equation of state: New MCMC lessons

in the (dimensionless) mass density,

SN and BAO constraints on (new) polynomial dark energy parametrizations: current results and forecasts

\kappa

Improved limits on short-wavelength gravitational waves from the cosmic microwave background

, and

Improving dark energy constraints with high-redshift Type Ia supernovae from CANDELS and CLASH

\sim20\%

DBI models for the unification of dark matter and dark energy

in the magnification,

Tension between SNeIa and BAO: current status and future forecasts

\mu

Nonparametric reconstruction of the cosmic expansion with local regression smoothing and simulation extrapolation

. We show maps of these differences for each cluster, as well as the mass distributions, critical curves, and 2D integrated mass profiles. For the Einstein radii (

Revisiting a model-independent dark energy reconstruction method

z_{s}=2