| 1. | |
| 2. | |
| 3. | |
| 4. | |
| 5. | Elena Aprile, Columbia The Next Step in the Search for WIMPs with Noble Liquid Targets October 7, 2019 PDF, 51.13 MB |
| 6. | |
| 7. | Arka Banerjee, Stanford University The signatures of self-interacting dark matter on cluster density profile and subhalo distributions October 7, 2019 PDF, 4.17 MB |
| 8. | Keith Bechtol, University of Wisconsin-Madison Impact of the Large Magellanic Cloud on the Full-sky Milky Way Satellite Population October 5, 2019 PDF, 18.38 MB |
| 9. | Jose Luis Bernal, Johns Hopkins University The Cosmic Expansion History from Line-Intensity Mapping October 5, 2019 PDF, 10.81 MB Line-intensity mapping (LIM) of emission form star-forming galaxies can be used to measure the baryon acoustic oscillation (BAO) scale as far back as the epoch of reionization. This provides a standard cosmic ruler to constrain the expansion rate of the Universe at redshifts which cannot be directly probed otherwise. In light of growing tension between measurements of the current expansion rate using the local distance ladder and those inferred from the cosmic microwave background, extending the constraints on the expansion history to bridge between the late and early Universe is of paramount importance. Using a newly derived methodology to robustly extract cosmological information from LIM, which minimizes the inherent degeneracy with unknown astrophysics, we show that present and future experiments can gradually improve the measurement precision of the expansion rate history, ultimately reaching percent-level constraints on the BAO scale. Specifically, we provide detailed forecasts for the SPHEREx satellite, which will target the H α and Lyman- α lines, and for the ground-based COMAP instrument---as well as a future stage-3 experiment---that will target the CO rotational lines. Besides weighing in on the so-called Hubble tension, reliable LIM cosmic rulers can enable wide-ranging tests of dark matter, dark energy and modified gravity. |
| 10. | Gary Bernstein Cosmological structure in the evolved Universe - DES measurements and the accuracy of future measures October 6, 2019 |
| 11. | Alain Blanchard, IRAP SZ Clusters and the amplitude of matter fluctuations October 5, 2019 PDF, 2.12 MB The present-day amplitude of matter fluctuations derived from Planck CMB for LCDM scenario is higher than current local estimates including the amplitude derived from Planck SZ clusters counts, leading to one of the tension of the LCDM. I will present some of the possible alternatives that have been proposed and discuss their relevance. |
| 12. | |
| 13. | Richard Bond, CITA Webskying the Universe Searching for Beyond-the-SMc October 7, 2019 PDF, 53.3 MB A toolkit for CMB and LSS experiments creating websky-ensembles to test BSMc theories on the Universe with PeakPatches+Hydro+early Universe simulations: armed with coarse-grain halo (via PeakPatches)+field (via 2LPT) and fine-grain response functions we look Buried BSMc Treasure. Examples: COMAP-CHIME .. SphereX LIM and nonGaussianity; CIB nonGaussianity, for both unlensed cf. lensed CIB; Planck-ACT tSZ X DES+BOSS a way to locally map for oriented asymmetric superclustering treasures; fDM aka wavy DM aka information-diffusing-DM, with future CMB lensing constraints in Hybrid fCDM models; ζ(x) maps - 2D from Planck ET, ζ-power-maps from CMB TEB and the 3D future target for ζ(x) maps. |
| 14. | Louise Breuval, Paris Observatory, LESIA The Cepheid Leavitt law from Gaia DR2 parallaxes of resolved companions October 8, 2019 |
| 15. | |
| 16. | |
| 17. | Clare Burrage, Nottingham Screening dark energy and modified gravity October 6, 2019 PDF, 1.64 MB Attempts to explain the accelerated expansion of the universe, or to modify gravity for cosmology introduce new physics that has significant effects on cosmological scales. However those theories still need to be consistent with precision tests which are consistent with the Standard Model and general relativity on terrestrial and solar system scales. Screening is a way to allow this to happen dynamically through the non-linearities of the theory. I will focus on scalar-tensor theories with screening, discussing how to build consistent theories, the phenomenology of these theories, and how they can be detected or constrained. |
| 18. | |
| 19. | |
| 20. | |
| 21. | Frederic Courbin, Ecole Polytechnique Fédérale de Lausanne (EPFL, Switzerland) H0 Measurements with Strong Gravitational Lensing Time Delays October 5, 2019 PDF, 11.08 MB |
| 22. | Francis-Yan Cyr-Racine, University of New Mexico Lessons on solving the Hubble tension October 5, 2019 PDF, 9.34 MB |
| 23. | |
| 24. | Harry Desmond, University of Oxford The impact of screened fifth forces on the local distance ladder October 5, 2019 PDF, 0.58 MB A generic prediction of theories beyond LCDM is the emergence of a fifth fundamental force, typically from new dynamical degrees of freedom. To escape local tests of gravity such a force must be "screened", introducing a dependence of its strength or range on the density of its environment. I will describe the impact of a screened fifth force on the distance ladder measurement of H0, primarily through modification of Cepheid's periods and luminosities. In particular, I will show that there exist regions of parameter space in which the galaxies anchoring the Cepheid period-luminosity relation are screened while a significant fraction of supernova hosts are not; assuming environment-independent Cepheid physics then causes the distances to the SNe to be underestimated, biasing the local H0 inference high. Imposing bounds on fifth-force strength from consistency tests within the distance ladder (most stringently by comparing Cepheid and TRGB distances to the same galaxies), I identify viable models capable of reconciling the SH0ES and Planck H0 results at 1.5 sigma. Based on arXiv:1907.03778. |
| 25. | |
| 26. | |
| 27. | |
| 28. | Rouven Essig, Stony Brook University The next decade in the Direct Detection of Sub-GeV Dark Matter October 7, 2019 PDF, 19.09 MB |
| 29. | Jonathan Feng, UC Irvine What tools are critical for progress in dark matter in the coming decades? October 7, 2019 PDF, 23.72 MB |
| 30. | |
| 31. | |
| 32. | Wendy Freedman, University of Chicago Ho Tension Panel October 5, 2019 PDF, 6.85 MB What is the status of Ho measurements? What is the status of theoretical models that for resolving the Ho tension? Have we been able to rule out systematic uncertainties in the measurements? If not, what is required to resolve the tension? |
| 33. | |
| 34. | Juan Garcia-Bellido, Universidad Autonoma de Madrid Primordial Black Holes and the Nature of Dark Matter October 7, 2019 PDF, 14.22 MB Twenty-three years ago, we predicted that massive primordial black holes (PBH) would form via the gravitational collapse of radiation and matter associated with high peaks in the spectrum of curvature fluctuations, and that they could constitute all of the dark matter (DM) today. In 2015, we predicted the clustering and broad mass distribution of PBH, which peaks at several Msun, and whose high-mass tails could be responsible for the seeds of all galaxies. Since then, AdvLIGO-Virgo interferometers have detected gravitational waves from at least thirty merger events of very massive and spinless black hole binaries, and we propose that they are PBH. We have recently understood that a universal mechanism associated with rapid changes in the number of relativistic species in the early universe could have been responsible for the formation of PBH at specific scales and thus have a very concrete prediction for the mass spectrum of DM-PBH, with broad peaks at 10^{-5}, 1, 100, and 10^6 Msun. In particular, the QCD quark-hadron transition could be responsible for the efficient production of baryons over antibaryons at PBH collapse, thus explaining the presence of baryons today and the relative abundance of DM to Baryons. We predict that, within a few months, a 100 Msun and a less than 1 Msun PBH will be detected by AdvLIGO-Virgo, and that in a few years an array of GW detectors could be used to determine the mass and spin distribution of PBH dark matter with 10% accuracy. Thus, gravitational wave astronomy could be responsible for a new paradigm shift in the understanding of the nature of dark matter and galaxy formation. |
| 35. | |
| 36. | |
| 37. | Alan Guth, MIT The Multiverse October 7, 2019 PDF, 1.32 MB I first argue that scientists should not regard the existence of many universes to be an extraordinary claim. Quite the opposite: there is nothing that we know of in science, which can be described in scientific terms, that happens only once. I then argue that there are three "winds" that seem to be pointing us toward the multiverse hypothesis: (1) almost all inflationary models allow eternal inflation; (2) cosmic acceleration strongly suggests that the energy density of our vacuum is extraordinarily fine-tuned, about equal to 10^(-120) times its estimated order of magnitude; (3) the multiverse hypothesis, combined with the landscape of string theory and selection effects, can potentially explain the smallness of the vacuum energy density. |
| 38. | ChangHoon Hahn, Lawrence Berkeley National Lab Constraining Neutrino Mass with the Bispectrum: Breaking Parameter Degeneracies October 7, 2019 PDF, 9.06 MB |
| 39. | |
| 40. | Yashar Hezaveh, Stanford University Probing the particle nature of dark matter with strong gravitational lensing October 5, 2019 |
| 41. | Hendrik Hildebrandt, Ruhr-University Bochum KiDS+VIKING: Cosmic shear tomography with optical+infrared data October 6, 2019 PDF, 8.78 MB |
| 42. | Craig Hogan, KICP Pattern of perturbations from a coherent inflationary horizon October 6, 2019 PDF, 5.52 MB It is proposed that emergent, holographic quantum gravity leads to primordial curvature perturbations with a distinctive pattern of correlations that differs from the standard quantum theory of inflation. Holographic and causal constraints are used to formulate candidate directional symmetries of perturbations at large angular separation. It is suggested that these constraints might account in a unified way for some well known anomalies measured in CMB anisotropy. New exact symmetries are predicted, such as a vanishing temperature correlation function at 90 degrees angular separation. |
| 43. | |
| 44. | |
| 45. | |
| 46. | |
| 47. | |
| 48. | Manoj Kaplinghat, UC Irvine Is a model beyond CDM needed to describe structure formation? October 5, 2019 PDF, 1.8 MB |
| 49. | Justin Khoury, Penn Inflation, Search Optimization, and Dynamical Criticality October 6, 2019 PDF, 31.47 MB |
| 50. | Lloyd Knox, UC Davis The Hubble Hunter’s Guide October 5, 2019 PDF, 4.08 MB I give an overview of efforts to find cosmological solutions to the H0 problem and the challenges to finding such solutions that don't violate known constraints. |
| 51. | |
| 52. | |
| 53. | Alexander Krolewski, UC Berkeley Measuring the amplitude of density fluctuations to z~2 using unWISE October 6, 2019 PDF, 6.63 MB The joint measurement of galaxy autocorrelation and cross-correlation with CMB lensing breaks the degeneracy between galaxy bias and the amplitude of matter clustering, enabling constraints on cosmological parameters. We use infrared-selected galaxies from the unWISE catalog to measure galaxy-CMB lensing cross-correlation out to z=2. The combination of infrared color cuts and a point-source cut from Gaia allows us to select ~100 million galaxies across the full sky with <5% contamination, yielding a ~80 sigma detection of CMB lensing cross-correlation in three color-selected redshift bins. The primary uncertainty on this measurement arises from the uncertain redshift distribution; with only two infrared bands, we use cross-correlations with spectroscopic samples (BOSS galaxies and quasars and eBOSS quasars) to constrain the redshift distribution. These measurements can shed light on cosmic acceleration in a variety of ways, e.g. by testing modified gravity models that could explain cosmic acceleration. |
| 54. | Ohkyung Kwon, Astronomy & Astrophysics, KICP Direct Laboratory Probes of Planck Scale Correlations in the Space-Time Vacuum October 6, 2019 PDF, 28 MB Cosmic acceleration has long been hypothesized to originate from the quantum vacuum, but an estimate from standard physics yields an energy density 10^122 larger than observations. However, in a holographic reformulation of the "background" space-time, the reduced degrees of freedom may lead to emergent quantum fluctuations at levels consistent with existing data. The Fermilab Holometer is the first apparatus to directly measure space-time uncertainties that scale with Planck strain spectral density, adopting LIGO technology at frequencies higher than inverse light crossing time to probe nonlocal correlations. This talk will present the current status of our analysis and systematics, an interpretation of experimental signatures, and to the extent available, a preview of the latest preliminary data. |
| 55. | |
| 56. | |
| 57. | |
| 58. | Weikang Lin, North Carolina State University Investigating the Hubble Constant Tension - Two Numbers in the Standard Cosmological Model October 8, 2019 PDF, 1.28 MB The current Hubble constant tension is usually presented by comparing constraints on H0 only. However, the post-recombination background cosmic evolution is determined by two parameters in the standard LCDM model, the Hubble constant and today's matter energy fraction. If we therefore compare all constraints individually in the this two-parameter plane, (1) various constraints can be treated as independently as possible, (2) single-sided constraints are easier to consider, (3) compatibility among different constraints can be viewed in a more robust way, and (4) whether or not a nonstandard model is able to reconcile all constraints in tension can be seen more effectively. We perform a systematic comparison of independent constraints based on a flat LCDM model. Constraints along different degeneracy directions consistently overlap in one region of the space, with the exception of the local measurement from Cepheid variable-calibrated supernovae. Due to the different responses of individual constraints to a modified model, it is difficult for nonstandard models with modifications at high-, mid- or low-redshifts to reconcile all constraints if none of them have unaccounted-for systematic effects. Based on our analysis, the local measurement is the most outlying and therefore drives the bulk of the tension. This may suggest that the most likely solution to the tension is an alteration to the local result, either due to some previously unseen feature in our local cosmic environment, or some other unknown systematic effect. |
| 59. | |
| 60. | |
| 61. | Barry Madore, Carnegie Observatories The Tip of the Red Giant Branch (TRGB) Distance Scale October 5, 2019 PDF, 36.86 MB We give a broad review of the Tip of the Red Giant Branch (TRGB) Method as it has been empirically developed and theoretically understood over the past 100 years. It is shown that the TRGB Method has the advantage of being the only stellar distance indicator that is truly a "standard candle" given that in the I band the Tip Magnitude is a universal constant requiring no further "standardizing" as is required for Type Ia SNe (using decline rates) or for Cepheids that require periods and intrinsic colors in order to be standardized. In addition since they are found in the halos of galaxies TRGB stars are minimally affected by reddening and their photometry can be controlled for crowding, in stark contrast to the Cepheids that can only be found in the high-surface-brightness, crowded and dusty environment of gas-rich spiral galaxies. The TRGB when used to calibrate the SNIa absolute magnitudes and applied to the distant Hubble flow results in a Hubble constant of H_o = 69.5 +/- 1.7 km/s/Mpc. |
| 62. | Sam McDermott, Fermilab Dark Radiation and Superheavy Dark Matter from Black Hole Domination October 7, 2019 PDF, 6.28 MB |
| 63. | |
| 64. | Jurgen Mifsud, Korea Astronomy and Space Science Institute Current status of an interacting dark sector with cosmological observations October 6, 2019 PDF, 9.12 MB The cosmic dark sector, composed of dark energy and dark matter, might be coupled, and hence mediate a fifth-force which gives rise to distinctive cosmological signatures. I will consider an interacting dark sector, in which dark energy and dark matter are coupled via specific well-motivated coupling functions. I will give an overview of the cosmological imprints characterizing these coupled dark energy models. I will further present the current model parameter constraints derived from the latest cosmological observations which probe the expansion history, and the growth of cosmic structures of our Universe. Moreover, I will demonstrate how different measurements of the Hubble constant, including the GW170817 measurement, influence the inferred constraints on the dark coupling. I will further discuss how one could put tighter constraints on such a dark sector coupling with the upcoming large-scale radio surveys. |
| 65. | Marius Millea, University of California, Berkeley The Hubble Hunter's Guide 2: Sounds of darkness October 7, 2019 PDF, 1.21 MB |
| 66. | Philip Mocz, Princeton University First Star-Forming Structures in Fuzzy Cosmic Filaments October 5, 2019 PDF, 8.07 MB In hierarchical models of structure formation, the first galaxies form in low mass dark matter potential wells, probing the behavior of dark matter on kiloparsec (kpc) scales. Even though these objects are not observed today, telescopes such as the James Webb Space Telescope (JWST) will soon offer an observational window into this emergent world. In this talk I describe how the first galaxies are assembled in a `fuzzy' dark matter (FDM) cosmology where dark matter is an ultralight ~10^-22 eV boson and the primordial stars are expected to form along dense dark matter filaments. Using a first-of-its-kind cosmological hydrodynamical simulation, we explore the interplay between baryonic physics and unique wavelike features inherent to FDM. In our simulation, the dark matter filaments show coherent interference patterns on the boson de Broglie scale, develop cylindrical soliton-like cores, and form stars along the entire structure. The filaments are unstable under gravity and collapse into kpc-scale spherical solitons. Features of the dark matter distribution are largely unaffected by the realistic baryonic feedback; on the contrary, gas and stars follow dark matter filaments and their profiles exhibit flattened cores -- smoking gun signatures of FDM. I contrast these results against first structures in cold and warm dark matter cosmologies. |
| 67. | Jessica Muir, Stanford Checking the consistency of growth and expansion with the Dark Energy Survey October 7, 2019 PDF, 12.34 MB |
| 68. | Ethan Nadler, Stanford/KIPAC Milky Way Satellites: Probes of Dark Matter Microphysics October 7, 2019 PDF, 15.71 MB |
| 69. | Jens Niemeyer, Göttingen Granules, solitons, and miniclusters: axion-like particles gone nonlinear October 7, 2019 |
| 70. | |
| 71. | Antonella Palmese, Fermilab Measuring the Hubble constant with gravitational wave black-hole mergers and galaxy surveys October 7, 2019 PDF, 14.78 MB |
| 72. | Minsu Park, Princeton University Lambda CDM or self-interacting neutrinos? How CMB data can tell the two models apart October 8, 2019 PDF, 2.21 MB |
| 73. | |
| 74. | Samuel Passaglia, KICP Primordial Black Hole Dark Matter: Slow-roll inflation and the Higgs Instability Mechanism October 6, 2019 |
| 75. | |
| 76. | Annika Peter, Ohio State University Flipping the script on tests of CDM with satellite galaxies October 5, 2019 |
| 77. | |
| 78. | Marco Regis, University of Turin and INFN Particle dark matter searches via cross-correlation between gravitational lensing and gamma rays October 7, 2019 PDF, 6.57 MB |
| 79. | |
| 80. | |
| 81. | Daniel Scolnic, Duke University New Constraints on H0 and w from Large Supernova Surveys October 5, 2019 |
| 82. | |
| 83. | |
| 84. | Alessandra Silvestri, Leiden University What can cosmology tell us about gravity? October 6, 2019 PDF, 16.08 MB |
| 85. | Constantinos Skordis, Czech Academy of Sciences New gravitational degrees of freedom as a proxy for dark matter October 7, 2019 |
| 86. | Tracy Slatyer, MIT What indirect searches teach us about particle dark matter October 7, 2019 PDF, 4.64 MB |
| 87. | Tristan Smith, Swarthmore College Oscillating cosmological scalar fields and a potential resolution to the Hubble tension October 7, 2019 PDF, 7.35 MB |
| 88. | Marcelle Soares-Santos, Brandeis University DESGW: Results from the DES Standard Sirens Program and Lessons Learned for Cosmology in the LSST era October 5, 2019 |
| 89. | Glenn Starkman, Case Western Reserve University Between a rock and a black hole: looking for dense chunks of dark matter October 7, 2019 PDF, 7.66 MB The need for dark matter has long been taken to be evidence of Beyond the Standard Model physics. But from early on, there have been Standard Model, or nearly Standard Model candidates in the forms of macroscopic assemblages of quarks or baryons with substantial strangeness. Such objects may be stable in the SM, or only with the addition of BSM physics; they may or may not be produced in appropriate abundances to be all of the dark matter. One thing is for certain -- we can and should look for them. Harder than we have been. I discuss some simple ideas for extending the reach of past searches for macroscopic dark matter candidates -- "macros" -- that make use of existing or planned detectors for other phenomena, accidental detectors like your kitchen counters, and the fact that the death rate from dark matter is consistent with zero. |
| 90. | Albert Stebbins, Fermilab/KICP Could Supermassive Black Holes be Primordial? October 7, 2019 PDF, 15.68 MB |
| 91. | |
| 92. | |
| 93. | |
| 94. | Yu-Dai Tsai, Fermi National Accelerator Laboratory Resonant Self-Interacting Dark Matter from Hidden QCD October 7, 2019 |
| 95. | |
| 96. | |
| 97. | |
| 98. | Cumrun Vafa, Harvard Swampland Perspective on Early and Late Time Cosmology’ October 6, 2019 PDF, 4.83 MB |
| 99. | Georgios Valogiannis, Cornell University An Accurate Model for Redshiift Space Clustering of Biased Tracers in Modified Gravity October 8, 2019 PDF, 2.92 MB |
| 100. | |
| 101. | |
| 102. | |
| 103. | Simon White, Max-Planck-Institut fuer Astrophysik Cosmic controversies: boon or bane? October 5, 2019 PDF, 17.79 MB I provide an historical overview of the role of controversies in the development of cosmological science, suggesting analogies between past controversies and those which are animating present-day cosmologists, as will be discussed at this conference. |
| 104. | |
| 105. |
| Home | Overview | Participants | Program | Presentations | KICP |
