Talks & Events

KICP Friday Noon Seminars Current & Future KICP Seminars
Past KICP Seminars
Helical Magnetic Fields in the Cosmos It is often necessary to study cosmological phase transitions, such as inflation and thermal symmetrybreaking phenomena, through the relics that they leave behind. In this sense, the cosmological magnetic field may be a powerful probe of the early universe, which has yet to be tapped. In this talk, I will survey various topics related to primordial magnetic fields (PMFs) with helicity. We will ask: how might a PMF have been generated in the early universe, how would it have evolved in the cosmological medium, and how could it be detected today? In the first part, we discuss the interesting connection between baryogenesis and magnetogenesis, which may link the sign of the cosmological baryon asymmetry to the sign of the magnetic helicity. In the second part, we discuss the interplay between the PMF and other magneticallyactive objects, such as monopoles and axions. Finally we turn to detection prospects, with an emphasis on the frontier field of magneticallybroadened TeV blazar halos. Modified gravity inside astrophysical bodies: breaking of the Vainshtein mechanism Any infrared modification of gravity, which explains the current cosmic acceleration, should not spoil the successes of general relativity in solarsystem observations. In many theories of modified gravity, it is ensured by the Vainshtein mechanism that works near dense sources. Recently, it has been found that the Vainshtein mechanism can be broken inside a dense source, although not outside, in a general class of scalartensor theories. In this talk, after reviewing how the Vainshtein mechanism can be broken, I will discuss its impact on the density profile of a star, modeling simply it as a polytropic sphere. I also show the existence of a universal upper bound on the amplitude of this type of modification, independently of the details of the equation of state. New tests of notsodark matter The nature of dark matter remains one of the major unsolved problems in physics, and one must leave no stone unturned when exploring empirical probes. In this talk I will discuss two different test of dark matter properties. First, I will show that dark matter interactions with standard model particles at high redshift can be probed through spectral distortions of the cosmic microwave background. In particular, I will show that upper limits from FIRAS measurements allow to constrain dark matter interactions for masses below 0.1 MeV. In the second part, I will discuss an interesting possible consequence of clumpy dark matter: flares following tidal compression events by supermassive black holes. A 3D view of the Dark Universe: illuminating intergalactic gas at high redshift with fluorescent Lymanalpha emission Gravitational collapse during the Universe's first billion years transformed a nearly homogeneous matter distribution into a network of filaments  the Cosmic Web  where galaxies form and evolve. Because most of this material is too diffuse to form stars, its study has been limited so far to absorption probes against background sources. In this talk, I will present the results of a new program to directly detect and study highredshift cosmic gas in emission using bright quasars and galaxies as external "source of illumination’’. In particular, I will show results from ultradeep narrowband imaging and recent integralfieldspectroscopy as a part of the MUSE Guaranteed Time of Observation program that revealed numerous giant Lymanalpha emitting filaments around quasars and bright galaxies. Finally, I will discuss how the unexpectedly high luminosities of the giant Lymanalpha filaments, together with the constraints from Helium and metal extended emission, present a serious challenge for our current understanding of the Intergalactic and Circumgalactic media based on hydrodynamical cosmological simulations. Putting the Cosmology in "21 cm Cosmology" 21 cm cosmology  the concept of using radio telescopes to observe the highly redshifted 21 cm line of neutral hydrogen on cosmological scales  is a field on the verge of a breakthrough. The first generation of 21 cm cosmology experiments (LOFAR, MWA, and PAPER, among others) have been operating for several years, and first results at the level of design sensitivity are potentially forthcoming. In this talk, I will focus on the work needed to establish the reliability of any putative detection of the cosmological signal and the paths forward for bringing 21 cm experiments into the "precision cosmology" fold, alongside the CMB and galaxy surveys. Recent results from the MWA and PAPER will be presented, including the first limits on the z = 8.4 IGM temperature from PAPER. Quantifying discordance in the 2015 Planck CMB spectrum In this talk I will discuss the internal consistency of the Planck 2015 cosmic microwave background (CMB) temperature anisotropy power spectrum and show that tension exists between the determination of some cosmological parameters from multipoles l<1000 (roughly the scales accessible to WMAP) and l>=1000. I will show that the l>=1000 constraints are also in tension with lowredshift data sets, including Planck’s own measurement of the CMB lensing power spectrum (2.4 sigma), and the most precise determinations of the baryon acoustic oscillation scale (2.5 sigma), and Hubble constant (3.0 sigma). Finally, I will discuss some possible explanations for these disagreements. Modeling the Outskirts of Galaxy Clusters The observational study of galaxy cluster outskirts is a new territory to probe the thermodynamic and chemical structure of the Xray emitting intracluster medium (ICM). Cluster outskirts are particularly important for modeling the SunyaevZel'dovich effect, which is sensitive to hot electrons at all radii and has been used to detect hundreds of galaxy clusters with recent microwave cluster surveys. In clusterbased cosmology, measurements of cluster outskirts are an important avenue for estimating the cluster mass, as the outskirts are less sensitive to baryonic processes that dominate the cluster core. However, recent observations of cluster outskirts deviate from theoretical expectations, indicating that cluster outskirts are more complicated than previously thought. Computational modeling of cluster outskirts is necessary to interpret these observations. I will present cosmological simulations of galaxy cluster formation that follow the thermodynamic and chemical structures in the virialization regions of the ICM and transition to the IGM. Specifically, I will discuss how observational signatures of galaxy clusters are affected by gas flows, inhomogeneities in the ICM, and nonequilibrium physics. Gravity at the horizon: from the cosmic dawn to ultralarge scales Recent advances in cosmology provide both the motivation and the data to probe gravity on the largest scales available to observation. I will revise the landscape of gravitational theories, focusing on modern scalartensor theories and their cosmological implications. Then I will present the ongoing effort to test gravity in novel regimes such as the early universe, nonlinear effects and ultralarge scales. I will also introduce the hi_class code (www.hiclasscode.net), which is central to this program. HighScale Axions without Isocurvature from Inflationary Dynamics If the PQbreaking scale f is larger than the inflationary Hubble scale HI, the PQ symmetry is broken during inflation. In the most straightforward models, this gives rise to a light axion field during inflation, which acquires isocurvature fluctuations. Such fluctuations are very stringently constrained by current CMB measurementsin fact, supposing the nearfuture observation of primordial tensor modes (i.e., a measurement of a nonzero scalartotensor ratio r, indicating a high inflationary scale), these constraints would exclude simple models of QCD axion dark matter in which f is larger than HI. This is particularly problematic for the nearPlanckian values of f favored by, for instance, string theory. A variety of solutions have been proposed to ''resurrect'' highscale axions. Many seek to leverage inflationary dynamics to modify the behavior or potential of the PQ field during inflation in order to suppress isocurvature. However, inflation and the axion potential are both very fragile, and readily disrupted by additional interactions or couplings. As such, it is important to carefully consider the viability of influencing the PQ field via inflationary dynamics; in other words, can this really be accomplished without messing up either inflation or the solution to the strong CP problem? In this talk, I'll discuss the variety of issues that can arise in these constructions, and highlight the steps one must take to build a viable model. A New Measurement of the Hubble Constant I will present a new, local, measurement by the SHOES team of the current rate of expansion (H0) of the universe from HST observations of Cepheid variables in host galaxies of Type Ia Supernovae. This measurement is a significant improvement from past measurements, and reduces many systematic uncertainties in past analyses. I will discuss the level of consistency of local measurements with measurements of H0 from the CMB. More Is Different: The Power of MultiProbe CMB/LSS CrossCorrelations Overlapping multiwavelength surveys allow qualitatively new cosmological constraints. In this talk, I will describe three recent such results. (1) I will present a measurement of the kinematic SunyaevZel’dovich (SZ) effect with Planck, WMAP, and WISE data using a novel estimator that does not require redshift estimates for individual tracers. This measurement yields the tightest kinematic SZderived constraint on the lowredshift baryon fraction to date, and the result is consistent with the expectation from analyses of the primordial CMB and Big Bang nucleosynthesis. (2) I will describe an updated measurement of the thermal SZ  CMB lensing crosscorrelation using the 2015 Planck full mission data. This signal constrains the mass dependence of the "hydrostatic mass bias" afflicting Xraybased galaxy cluster mass estimates, a key systematic in clusterbased cosmological constraints. (3) I will discuss a constraint on the multiplicative shear bias in CFHTLenS data based on crosscorrelations with Planck CMB lensing and CFHTLenS galaxy density maps, the first demonstration of this method on actual data. The result is consistent with a value of the shear bias that would alleviate the tension between cosmological constraints from CFHTLenS and the Planck CMB temperature power spectrum. ETHOS – From Dark Particle Physics to the Matter Distribution of the Universe and Beyond We formulate an effective theory of structure formation (ETHOS) that enables cosmological structure formation to be computed in a vast array of microphysical model of dark matter physics. This framework maps the detailed microphysical theories of particle dark matter interactions into the physical effective parameters that shape the linear matter power spectrum and the selfinteraction transfer cross section of nonrelativistic dark matter. These are the input to structure formation simulations, which follow the evolution of the cosmological and galactic dark matter distributions. These effective parameters in ETHOS allow the classification of dark matter theories according to their structure formation properties rather than their intrinsic particle properties, paving the way for future simulations to span the space of viable dark matter physics relevant for structure formation. Resolving the Isotropic GammaRay Background in the Search for Dark Matter The presence of allsky, diffuse gammaray emission has been known for several decades, but its origins remain an open question. While astrophysical sources such as Active Galactic Nuclei and starforming galaxies almost certainly contribute to this Isotropic GammaRay Background (IGRB), darkmatter annihilation may also leave an imprint. Therefore, resolving the components of the IGRB is an important step in pushing the sensitivity to signals of dark matter annihilation, particularly in the wellmotivated parameter regime for Weakly Interacting Massive Particles. In my talk, I will present a new analysis method that takes advantage of photoncount statistics to distinguish astrophysical point sources from a potential darkmatter signal. I will show results obtained by applying this technique to public data from the Fermi Large Area Telescope. Using these datadriven methods, we can start to resolve the diffuse emission from ~1189 GeV. I will discuss the possible nature of these sources and the implications for dark matter. CMB Lensing Measurements, Present and Future By directly probing the cosmic mass distribution, measurements of gravitational lensing in the CMB provide a wealth of information about neutrino masses, inflation, dark energy, and galaxy biases. In my talk, I will discuss current and future work in this new but rapidly advancing field. In particular, I will discuss current measurements of the CMB lensing power spectrum with the ACTPol experiment and future measurements with the CMB StageIV experiment, explaining the promise and challenges of upcoming ultrahighprecision studies of this lensing signal. Lensing is not only a signal, however, but also a source of noise that limits how much we can learn about the early universe via Bmode polarization. In my talk, I will explain why delensing  removing the lensing effect to reveal the primordial sky  is crucial for the future of CMB science and will discuss recent work in delensing theory and data analysis. Higgs Relaxation Leptogenesis The recent discovery of the Higgs boson, with a mass of 125 GeV, raises interesting possibilities for early universe cosmology. Its relatively flat potential means that it will typically acquire a large vacuum expectation value during inflation, ushering in a postinflationary epoch of relaxation. In this talk, I will explore the possibilities for baryogenesis during this epoch. Towards precision cosmology with large scale structures: the halo model and perturbative approaches The theoretical modeling of the statistical observables of the largescale structures of the Universe, like galaxy clustering, weak lensing etc., is necessary in order to derive any constraints on the cosmological parameters. One of the most important ingredients of the theoretical model is the twopoint correlation function, or its Fourier transform the matter power spectrum. I will discuss the precision in its calculations based on a modified halo model, and the systematic effects due to the baryonic processes. Further, I will also discuss the covariance matrix of the matter power spectrum and its estimators based on the halo model and the perturbation theory. We find the agreement with the simulations is at a 10% level up to k ∼ 1 h/Mpc. We show that all the connected components are dominated by the largescale modes (k < 0.1h/Mpc), regardless of the value of the wavevectors of the covariance matrix. Finally, I will provide a prescription for how to evaluate the covariance matrix from small box simulations without the need to simulate large volumes. 