Probing correlated compensated isocurvature perturbations using scale-dependent galaxy bias
The equivalence principle dictates that no local interaction could care about the local gravitational potential, in turn protecting the longest cosmological modes against effects of complicated non-linear physics. This fundamental and simple fact in turn makes the large-scale observables a very powerful probe of the type of effects that are not caused by local interactions (i.e. that are non-local) such as those that determine the characteristics of the curvature fluctuations at the early Universe. It has long been understood that one such observable is the galaxy bias (i.e. the fudge-factor that relates the galaxy number-densities to the total-matter number-density). This bias turns out to be scale invariant on large scales in the absence of non-local effects due to equivalence principle. The bias becomes scale dependent, however, in the presence of local non-Gaussianity, for example, as well as a specific type compensated isocurvature perturbations (CIPs) that are correlated with the primordial curvature perturbations. CIPs are modulations of the relative baryon and dark matter density that leave the total matter density constant. The best current constraints from the primary cosmic microwave background (CMB) are consistent with CIPs some two orders of magnitude larger in amplitude than adiabatic perturbations, suggesting that there may be a huge gap in our knowledge of the early Universe!
Combining a galaxy survey with an unbiased tracer of the density field facilitates a measurement of the amplitude of correlated CIPs that is free from cosmic variance, the main limitation on constraints from the primary CMB. This is often called the 'sample variance cancellation'.
Among the most promising tracers to use for this purpose is the remote dipole field, reconstructed using the technique of kinetic Sunyaev Zel'dovich (kSZ) tomography.
With James Mertens, Matthew Johnson and Marc Kamionkowski, we evaluated the detection significance on the amplitude of correlated CIPs possible with next-generation CMB and galaxy surveys using kSZ tomography. We find that kSZ tomography can probe CIPs of comparable amplitude to the adiabatic fluctuations, representing an improvement of over two orders of magnitude upon current constraints, and an order of magnitude over what will be possible using future CMB or galaxy surveys alone.
Transverse Velocities with the Moving Lens Effect
[CMB by PLANCK]
Thanks to experiments such as WMAP and PLANCK, statistics of the primary cosmic microwave background (CMB) is very well described. We have constraints on densities, curvature, age of the univers as well as some properties of the initial fluctuations such as Gaussianity, scale-invariance and adiabaticity.
Remaining questions for the next generations large-scale cosmology experiments such as SO, CMB-S4, LSST and others are related to the growth of structure, and will involve better understanding the nature of neutrinos, dark photons, dark energy, modified gravity, inflation and dark matter.
But going beyond the primary CMB; we should note that a CMB photon traverses the Universe and is subject to many effects such as deflection by gravitational potential (weak gravitational lensing); scattering on baryons in clusters (Sunyaev Zel’dovich effects); and getting redshifted due to evolving potentials, which at linear level includes the Sachs-Wolfe effect and also integrated Sachs Wolfe effect (at the non-linear order, is often called the Rees-Sciama effect).
In addition, gravitational potentials which change in time induce fluctuations in the observed CMB temperature. Cosmological structure moving transverse to our line of sight provides a specific example known as the moving lens effect.
The moving lens effect (shown above) has a dipolar shape on the CMB, centred around the gravitational potential and aligned with the velocity.
We showed recently that the upcoming CMB experiments together with large-scale structure experiments will be able to detect the moving lens effect to high signal-to-noise ratio.
You can find out more in our paper here https://arxiv.org/abs/1812.03167
This project also involves many great scientists!
Effect of reheating on predictions following multiple-field inflation
Inflation, a period of accelerated expansion in the early Universe, solves many of the classical problems associated with the hot Big Bang scenario, and provides a natural mechanism for generating primordial cosmological fluctuations.
Observations are currently consistent with the simplest single-field, slow-roll models of inflation, e.g., the Planck observations of the cosmic microwave background (CMB) indicate a featureless power-law shape for the primordial power spectrum of scalar fluctuations and no detectable primordial non-Gaussianity or tensor fluctuations.
Single-field models are phenomenologically successful, however, they often lack the generality of more complex scenarios. More notably, they are not always natural from a theoretical point of view, e.g., string compactifications often result in hundreds of scalar fields appearing in the low energy effective action.
Models with multiple fields naturally produce fluctuations that are non-adiabatic, whose presence allows the curvature perturbation and its correlation functions to evolve outside the Hubble radius. Therefore, in order to make predictions in multifield models, it is necessary to understand the evolution of the correlation functions until either the curvature fluctuations become adiabatic or they are directly observed.
In a recent paper at https://arxiv.org/pdf/1710.08913.pdf, we provided a general methodology for calculating the adiabatic power spectrum of curvature perturbations after multifield inflation for any number of scalar fields. Scenarios with many fields also tend to predict an amount of isocurvature perturbations at the end of inflation which increases with the number of fields, thereby elevating the importance of studying the effects of reheating for these models.
We found that details of reheating can effect the inflationary observables significantly.
The search for anisotropy in the gravitational-wave background with pulsar-timing arrays and astrometry
Pulsar-timing arrays (PTAs) are seeking gravitational waves from supermassive-black-hole binaries, and there are prospects to complement these searches with stellar-astrometry measurements.
Theorists still disagree, however, as to whether the local gravitational-wave background will be isotropic, as arises if it is the summed contributions from many SMBH binaries, or whether it exhibits the type of anisotropy that arises if the local background is dominated by a handful (or even one) bright source.
In a recent work with Prof. Marc Kamionkowski and Prof. Andrew Jaffe, we derive, using bipolar spherical harmonics, the optimal PTA estimators for anisotropy in the GW background and simple estimates of the detectability of this anisotropy.
We found that the GWB needs to be detected to very high precision before we will be able to tell, unambiguously, whether it is statistically isotropic or not.
You can read our paper here: https://arxiv.org/abs/1904.05348
Delensing the CMB: An all-orders, full-spectra, iterative approach
Image copyright: ESA and the Planck Collaboration
In this near-complete project, we have calculated and coded a fast and accurate delensing algorithm of CMB TT, TE, EE and BB spectra with the quadratic estimator up-to all orders in lensing potential. The scientific goal here is assessing how much we can recover the peak locations and the damping tail of the primary CMB spectra from a rigorous application of delensing with the quadratic estimator.
Project will produce public code to calculate the delensed CMB spectra and lensing reconstruction noise accompanied with an analysis and forecast paper in the near future. The code is planned as a user-friendly extension to the publicly available CLASS Boltzmann solver.
Weak gravitational lensing plays a crucial role in many areas in cosmology including the potential detection of gravitational waves from the CMB polarization; determining the radiation content of the Universe; and uniquely probing dark matter at high redshifts. Mitigation procedure of this effect, also called 'delensing', improves the constraining power of the cosmological surveys significantly on a wide range of parameters and understood to be essential to future cosmological inference. My research focuses on developing the analytic framework for estimating prospects of optimal delensing the CMB observables with high fidelity. In this upcoming work we will aim leading the community towards the most fruitful directions forward through understanding the benefits of delensing.
Utilizing 21cm Velocity Acoustic Oscillations for fundamental physics
As matter clusters under gravity, its components can behave very differently. While the majority of matter is collisionless, dark and cold, a fraction of it are baryons which couple to photons before the recombination at redshift z≈1100, giving rise to the baryon acoustic oscillations (BAOs) observed from the CMB and galaxy-surveys. The same physics also induces a bulk relative velocity between DM and baryons [1,2]. More recently, it was shown in  that for reasonable models of epochs up-to the end of reionization, detecting a velocity-induced acoustic feature, so called velocity acoustic oscillations (VAOs), may be possible from the measurement of 21cm hydrogen-line with the upcoming experiments such as HERA. The VAO feature provides an effective probe of the early Universe physics that affect the relative behaviour of DM and baryons. Unlike the matter power-spectrum, where the effect of BAO is small, the VAO feature is O(1) in the 21cm power-spectrum.
Measurements of the 21cm hydrogen-line provides a unique window into the cosmic-dawn era when the first stars were formed (z=15-20). During these early times the typical mass of collapsed baryonic objects fall near the critical mass below which gas pressure prevents their collapse. The abundance of Lyman-α photons that excite the hyperfine transition in neutral hydrogen and allow it to absorb 21cm photons from the CMB will depend on the collapse-fraction of baryons and will be directly impacted by effects that alter early structure growth, such as local modulations of relative DM-baryon densities due to bulk CIPs. Furthermore, as is the case for the BAO feature in the CMB and LSS observables, some characteristics of the VAO will be unaffected from the complicated local physics related to various feedback mechanisms that play role during the epoch of reionization and can be utilised to constrain effects that have a coherent impact of the observables on large-scales, such as CIPs. In this paper we discuss the detection significance of CIPs from measurement of the 21cm hydrogen line.
[Artist impression of the first stars, image credit: APS, Adolf Schaller for STScI]
While measurements of the 21cm brightness temperature power-spectrum allow discriminating between models of cosmology, measured variances of the modes (as well as the features of the power-spectrum themselves) are a set of cosmological observables too, whose properties can be described independently of any model. Some characteristics of these observables such as the amplitudes of individual Fourier modes are expected to be sensitive to the details of local mechanisms such as baryonic feedback. These effects need to be modelled and the model parameters need to be marginalised, weakening the constraining power of the measurements, making it hard to unambigiously distinguish between fundamental physics and astrophysical effects, for example. Observations VAOs, on the other hand, provide a unique measure whose various large-scale properties that are unaffected under these effects.
The difficulty for local interactions to produce coherent effects on long distances outside the sound horizon of primordial inhomogeneities allow the VAO scale and the VAO peak locations to be protected from details of the baryonic feedback. In an upcoming work with Marc Kamionkowski, we demonstrate the use of VAO peak locations for inferring details of the fundamental properties of our Universe.
[Demonstration of 21cm power-spectrum VAO peak locations, upcoming work]