Day 1182

Friday.  Monday.

1611.01315
Measuring weak lensing correlations of Type Ia Supernovae
Scovacricchi, et al

Study the feasibility of detecting WL spatial correlations between SN Ia magnitudes with present (DES) and future (LSST) surveys.  Investigate the angular auto-correlation function of SN magnitudes (once the background cosmology has been subtracted) and cross-correlation with galaxy catalogues.  Examine both analytical and numerical predictions, the latter using simulated galaxy catalogues from the MICE Grand Challenge Simulation.  Predict that: unable to detect the SN auto-correlation in DES, while it should be detectable with the LSST SN deep fields (15,000 She on 70 deg2) at ~6 sigma level of confidence (assuming 0.15 magnitudes of intrinsic dispersion).  The SN- galaxy cross-correlation function will deliver much higher S/N, being detectable in both surveys with an integrated S/N of ~100 (up to 30 arcmin separations).  Predict joint constraints on the matter density parameter (Omega_m) and the clustering amplitude (sigma_8) by fitting the auto-correlation function of the mock LSST deep fields.  When assuming a Gaussian prior for Omega_m, can achieve a 25% measurement of sigma_8 from just these LSST SNe (assuming 0.15 mags of intrinsic dispersion).  These constraints will improve significantly if the intrinsic dispersion of SNe Ia can be reduced.


1611.01486
Cosmological constraints from the convergence 1-point probability distribution
Patton, Blazek, ... Huff, Melchior, et al

Examine the cosmo information available from the 1-pt PDF of the WL convergence field, utilizing fast L_PICOLA simulations and a Fisher analysis.  Find competitive constraints in the Omega_m-sigma_8 plain from the convergence PDF with 188 arcmin2 pixels compared to the cosmic shear power spectrum with an equivalent number of modes (ell<886). The convergence PDF also partially breaks the degeneracy cosmic shear exhibits in that parameter space.  A joint analysis of the convergence PDF and shear 2-pt function also reduces the impact of shape measurement systematics, to which the PDF is less susceptible, and improves the total figure of merit by a factor of 23, depending on the level of systematics.  Finally, present a correction factor necessary for calculating the unbiased Fisher information from finite differences using a limited number of cosmo sims.