MIT Center for Theoretical Physics – a Leinweber Institute

Boosted, hadronically decaying $W$ and $Z$ bosons are among the most abundant heavy objects at colliders, and their vector nature makes their substructure qualitatively richer than that of a scalar. We initiate precision studies of the hadronic decays of boosted polarized vector bosons with energy correlators. In the narrow-width limit, the laboratory-frame two-point energy correlator is a sum of longitudinal and transverse decay spectra, each weighted by its polarized production rate and obtained by a closed-form boost kernel acting on rest-frame correlators. Combining polarized production density matrices, computed at NNLO in QCD for $ppto V+X$ and at leading order for $e^+e^-to W^+W^-$, with decay correlators that combine NNLO fixed order with NNLL collinear and N$^4$LL back-to-back resummation, we find for high-$p_T$$W/Z$ production that polarization shifts the spectrum by $mathcal{O}(10%)$ relative to a naive unpolarized treatment. Even without any reconstruction, hadronic $W/Z$ decays stand out over the realistic QCD background of untagged jet samples as a localized angular bump. Our results open the door to using energy correlators for polarimetry of electroweak bosons through their hadronic decays, for standard-candle measurements of electroweak bosons inside jets, and in sharper searches for new resonances.

The Dark Energy Spectroscopic Instrument (DESI) measures baryon acoustic oscillations (BAO) in the Lyman-$α$ (Lyman-alpha) forest and provides a robust probe of the expansion history in the matter-dominated era. Yet, non-linear structure formation broadens and shifts the BAO peak. To undo these effects, we extend standard Zel'dovich reconstruction, routinely applied to galaxy surveys, to the Lyman-alpha forest. We validate our methodology on large-volume idealized Lyman-alpha forest mocks painted on top of the textsc{AbacusSummit}$N$-body simulations, using linear control variates to suppress sample variance and thereby reduce the error bars by a factor of up to $approx sqrt{50}$. In fully sampled periodic boxes, reconstruction halves the radial BAO damping scale and reduces the uncertainties on the radial ($apar$) and transverse ($aperp$) scaling parameters by $approx25%$ and $approx15%$, respectively. It also reduces the non-linear shift from $Δapar=+0.3%$ to $+0.10pm0.07%$, while $aperp$ remains unbiased. To make this approach readily applicable to observational data, we demonstrate the impact of a survey mask with a DESI-like density of $50,mathrm{deg}^{-2}$. For this mask, we compare two approaches to estimate the displacement field: either directly from the Lyman-alpha forest or using an external tracer with a number density of $bar n simeq 10^{-3},h^3mathrm{Mpc}^{-3}$, such as Lyman-break galaxies and Lyman-$α$ emitters---both key targets for DESI-II. Both approaches give comparable gains and reduce the uncertainties on $apar$ and $aperp$ by $approx 27%$ and $approx 10%$, respectively, with mild improvements for futuristic high-density surveys with $160,mathrm{deg}^{-2}$. Correspondingly, the figure of merit improves by factors of $1.66$ for fully sampled boxes, $1.65$ for a DESI-like, and $1.76$ for a high-density survey.

We develop an effective field theory (EFT) of intrinsic alignments at the level of spin-2 field fluctuations of large-scale structure tracers, such as the shapes of galaxies and dark matter halos. Our perturbative model includes the non-linear treatment of the Zel'dovich displacement, and contains all necessary shape operators through the third order. We apply our field-level model to the full 3D distribution of galaxy shapes, whose sky projections are a known contaminant of cosmic shear measurements. Our field-level EFT model achieves a better description of the helicity fields of dark matter halo shapes than the standard non-linear alignment (NLA) and tidal torquing + tidal alignment (TATT) models in the literature, as evidenced by improved correlations with the simulations' initial conditions. We perform precision measurements of field-level bias parameters by means of a generalized least-squares problem, for which we derive an optimal estimator and analytic covariance matrices. We measure the full set of linear, quadratic, and cubic shape bias coefficients as a function of halo mass in the $texttt{Quijote}$ N-body simulations. We then study the intrinsic alignments of galaxies in the $texttt{FLAMINGO}$ hydrodynamical simulation, focusing on observationally relevant samples: spirals, ellipticals, luminous red galaxies (LRG) and emission-line galaxies (ELG). We detect linear and nonlinear alignment coefficients at high significance for LRG, spiral and elliptical galaxies. We also find evidence for non-zero density-weighted tidal bias coefficient of the simulated ELG. This work supports the notion that EFT-based models of alignments will be paramount in optimally extracting constraints from future shape correlations, and lays the foundation for the development of simulation-based priors for future galaxy shape samples.

We revisit the scenario of critical Higgs inflation, in which inflation is driven by the Standard Model Higgs boson with parameters chosen close to a critical point, giving rise to an inflection point in its potential. After reviewing this model, we perform a systematic study of its viability centered around three criteria: (1) consistency with electroweak-scale measurements, (2) ability to reproduce the cosmic microwave background (CMB) observables, and (3) sensitivity of the model predictions to unknown UV physics, based on a breakdown of perturbative unitarity. We first show that compliance with electroweak-scale measurements is controlled by the parameters in the Higgs potential at inflationary scales, also updating the literature values. We then demonstrate how for any choice of potential parameters, agreement with the CMB observables can be achieved through the choice of the nonminimal coupling, in both metric and Palatini formulations of gravity. However, we also find that there exist no regions of parameter space, in either the metric or Palatini formulations, in which compliance with all three physical criteria is possible. While this does not exclude the possibility of the Higgs field driving inflation, it means that predictions for any observable are in principle sensitive to the details of the model's UV completion.