The cosmic microwave background (CMB) gravitational lensing and its cross-correlation with large-scale structure tracers will be important cosmological probes in the coming years. Being able to model these observables and reconstruct them from the data with the level of precision required by future experiments will be mandatory in order to exploit them for robust cosmological applications.

We present a method to reconstruct the probability distribution of the weak lensing magnification of Type Ia supernovae (SNe Ia) from observational data. The method is directly applicable to future data from surveys like WFIRST. With a realistic synthetic catalog, we measure the weak lensing signature and express the observable in terms of the variance of the lensing magnification.

The current and upcoming surveys in cosmology will soon deliver an unprecedented amount of precision measurements, truly opening an era of precision cosmology.  However, this rapid development in experiments and observations demands substantial advances in theoretical modeling to avoid any systematic errors in our interpretation.  The standard theoretical descriptions of galaxy clustering, weak gravitational lensing, and the CMB Boltzmann equations are incomplete an

Close to a decade in the making, the imminent DESI experiment (desi.lbl.gov <http://desi.lbl.gov/> ) promises to revolutionise  our understanding of Dark Energy and extend large-scale structure studies to z~2.  But what comes next?  

We show how kSZ tomography measures a bispectrum containing a cosmological power spectrum of the velocity field and an astrophysical power spectrum of the electron density. While these are degenerate up to an overall amplitude (the "galaxy optical depth"), scale-dependent effects on large scales are much better constrained by the inclusion of kSZ on top of galaxy clustering while assuming nothing about the optical depth of galaxy clusters.

Extracting cosmological information from current survey data is increasingly reliant on computationally-intensive n-body simulations of large-scale structure. For weak-lensing surveys, the matter distribution is directly measured from simulations on scales where linear perturbation theory fails. For galaxy-clustering surveys, haloes are identified in simulations and then populated with galaxies to provide mock catalogues.

The Wide Field Infrared Survey Telescope (WFIRST) is an upcoming NASA observatory that will investigate the origins of cosmic acceleration using weak gravitational lensing.  WFIRST will perform galaxy shape measurements using Teledyne H4RG-10 detectors; thus it is essential to understand inter-pixel non-linear effects like the brighter-fatter effect (BFE) and non-linear inter-pixel capacitance (NL-IPC) that could cause systematic errors in the lensing analysis.  The

On April 10, 2019, the Event Horizon Telescope (EHT), a very long baseline interferometry experiment, released the first image of a black hole resolved to event horizon scales. I will discuss the image of M87 and aim to convince the audience that a flux depression in the image is necessary to fit the data. I will also discuss the parameters we derived based on the image and model fitting results.

The kinematic Sunyaev-Zel'dovich effect enables us to directly probe the density-weighted velocity field up to very large cosmic scales. We investigate the effects of intrinsic alignments (IA) of dark-matter halo shapes on cosmic density and velocity fields on such large scales. In literature IA have been detected with the halo density field up to ~ 100 Mpc/h both in simulations and observations.