Shear-only reconstruction for CMB lensing
CMB foregrounds can be confused with lensing magnification but not with lensing shear. A shear-only CMB lensing estimator is thus immune to foregrounds. The signal-to-noise lost by discarding the magnification information is more than recovered by the ability to use higher temperature multipoles.
Weak lensing of intensity maps: the case of the cosmic infrared background (CIB)
Intensity mapping promises to efficiently sample the large-scale structure over a large fraction of the observable universe. However, the resulting intensity maps require complex modeling of the relationship between matter density and emissivity, and are affected by foregrounds/interlopers and missing modes. For these reasons, lens reconstruction from intensity maps would be useful. We showed how to measure lensing from any weakly non-Gaussian source field, and that current Planck CIB data is sufficient to detect this effect.
First detection of the correlation between Lyman-alpha forest and CMB lensing
Does the Lyman-alpha transmission trace the matter density in the way we typically assume? Can CMB help? We used CMB lensing as a tracer of the matter, to try to constrain the relation between Lyman-alpha transmission and matter density. We detected for the first time the bispectrum between the Lyman-alpha squared and the CMB lensing.
Optical shear calibration with CMB lensing
Can CMB help constrain galaxy lensing systematics? A lot of effort is invested in future lensing surveys (LSST, Euclid, WFIRST). Lensing systematics are challenging, e.g. shear calibration, photo-z estimation, intrinsic alignments, uncertainties in the matter power spectrum. Shear multiplicative bias can mimic a redshift dependence of the growth of structure. We made the most realistic forecast to date for CMB S4 lensing and LSST, and showed that CMB lensing can calibrate the shear biases for LSST. This is a self-calibration, purely empirical, and does not rely on any assumption about the galaxy population and morphologies, contrary to image simulations.
kSZ measurement with ACTPol and BOSS
How are the baryons distributed on the scale of a halo? Can CMB help? The matter power spectrum on small scales is uncertain, because of complex galaxy formation physics which changes the baryon density profile inside halos (“baryonic 1-halo term”). We detected the kSZ effect with a somewhat novel method, estimating velocities from the density field (as in BAO reconstruction). Our small signal-to-noise is already sufficient to show that the gas profile is more extended than the NFW profile.
A stringent test of the effective field theory of large-scale structure
Can we predict analytically the effect of non-linearities on the matter density field on small scales? We compared the EFT to N-body simulation at the level of the field instead of just the power spectrum. This allows for a comparison without sample variance. It is also a more stringent test, since power spectra are smooth functions, easy to match, and since two fields may have the same power spectrum without being identical. We showed that the EFT counterterms make the perturbative expansion convergent.
Supersample covariance for n-point functions and cluster number counts
Non-linear evolution makes the density field non-Gaussian and takes the information away from the power spectrum. What is the best way to extract information from this non-Gaussian density field? How can one recover some of this information, by combining power spectrum with higher n-point functions and halo counts? How to jointly analyze observables consistently, without double-counting the information? We used the halo model to compute the non-Gaussian covariances between matter/lensing n-point functions and halo counts, including the supersample covariance.