Emmanuel Schaan

CMB-S4 Science Book, First Edition

This book lays out the scientific goals to be addressed by the next-generation ground-based cosmic microwave background experiment, CMB-S4, envisioned to consist of dedicated telescopes at the South Pole, the high Chilean Atacama plateau and possibly a northern hemisphere site, all equipped with new superconducting cameras. CMB-S4 will dramatically advance cosmological studies by crossing critical thresholds in the search for the B-mode polarization signature of primordial gravitational waves, in the determination of the number and masses of the neutrinos, in the search for evidence of new light relics, in constraining the nature of dark energy, and in testing general relativity on large scales.

The Atacama Cosmology Telescope: Two-Season ACTPol Spectra and Parameters

Author(s): Louis, T; Grace, E; Hasselfield, M; Lungu, M; Maurin, L; Addison, GE; Ade, PAR; Aiola, S; Allison, R; Amiri, M; Angile, E; Battaglia, N; Beall, JA; De Bernardis, F; Bond, JR; Britton, J; Calabrese, E; Cho, HM; Choi, SK; Coughlin, K; Crichton, D; Crowley, K; Datta, R; Devlin, MJ; Dicker, SR; Dunkley, J; Dunner, R; Ferraro, S; Fox, AE; Gallardo, P; Gralla, M; Halpern, M; Henderson, S; Hill, JC; Hilton, GC; Hilton, M; Hincks, AD; Hlozek, R; Patty Ho, SP; Huang, Z; Hubmayr, J; Huffenberger, KM; Hughes, JP; Infante, L; Irwin, K; Kasanda, SM; Klein, J; Koopman, B; Kosowsky, A; Li, D; Madhavacheril, M; Marriage, TA; McMahon, J; Menanteau, F; Moodley, K; Munson, C; Naess, S; Nati, F; Newburgh, L; Nibarger, J; Niemack, MD; Nolta, MR; Nunez, C; Page, LA; Pappas, C; Partridge, B; Rojas, F; Schaan, E; Schmitt, BL; Sehgal, N; Sherwin, BD; Sievers, J; Simon, S; Spergel, DN; Staggs, ST; Switzer, ER; Thornton, R; Trac, H; Treu, J; Tucker, C; Engelen, AV; Ward, JT; Wollack, EJ | Abstract:

Evidence for the kinematic Sunyaev-Zel'dovich effect with the Atacama Cosmology Telescope and velocity reconstruction from the Baryon Oscillation Spectroscopic Survey

Emmanuel Schaan, ∗ Simone Ferraro, 2 Mariana Vargas-Magaña, Kendrick M. Smith, Shirley Ho, Simone Aiola, Nicholas Battaglia, J. Richard Bond, Francesco De Bernardis, Erminia Calabrese, 9 Hsiao-Mei Cho, Mark J. Devlin, Joanna Dunkley, Patricio A. Gallardo, Matthew Hasselfield, Shawn Henderson, J. Colin Hill, Adam D. Hincks, Renée Hlozek, Johannes Hubmayr, John P. Hughes, Kent D. Irwin, 10 Brian Koopman, Arthur Kosowsky, Dale Li, Thibaut Louis, Marius Lungu, Mathew Madhavacheril, Löıc Maurin, Jeffrey John McMahon, Kavilan Moodley, Sigurd Naess, Federico Nati, Laura Newburgh, Michael D. Niemack, Lyman A. Page, Christine G. Pappas, Bruce Partridge, Benjamin L. Schmitt, Neelima Sehgal, Blake D. Sherwin, 2 Jonathan L. Sievers, 26 David N. Spergel, Suzanne T. Staggs, Alexander van Engelen, and Edward J. Wollack Dept. of Astrophysical Sciences, Peyton Hall, Princeton University, Princeton, NJ USA 08544 Miller Institute for Basic Research in Science, University of California, Berkeley, CA, 94720, USA Instituto de Fisica, Universidad Nacional Autónoma de México, Apdo. Postal 20-364, México Perimeter Institute for Theoretical Physics, Waterloo, ON N2L 2Y5, Canada Department of Physics, Carnegie Mellon University, 5000 Forbes Avenue, Pittsburgh, PA 15213, USA Department of Physics and Astronomy, University of Pittsburgh, Pittsburgh, PA 15260 USA and Pittsburgh Particle Physics, Astrophysics, and Cosmology Center, University of Pittsburgh, Pittsburgh PA 15260 Canadian Institute for Theoretical Astrophysics, University of Toronto, Toronto, ON, Canada M5S 3H8 Department of Physics, Cornell University, Ithaca, NY 14853, USA Sub-Department of Astrophysics, University of Oxford, Keble Road, Oxford, UK OX1 3RH SLAC National Accelerator Laboratory, 2575 Sandhill Hill Road, Menlo Park, CA 94025 Department of Physics and Astronomy, University of Pennsylvania, 209 South 33rd Street, Philadelphia, PA, USA 19104 Dept. of Astronomy, Pupin Hall, Columbia University, New York, NY, USA 10027 UBC (University of British Columbia, Department of Physics and Astronomy, 6224 Agricultural Road, Vancouver BC V6T 1Z1, Canada) National Institute of Standards and Technology, Boulder, CO USA 80305 Department of Physics and Astronomy, Rutgers University, 136 Frelinghuysen Road, Piscataway, NJ 08854-8019 Dept. of Physics, Stanford, CA 94305 Physics and Astronomy Department, Stony Brook University, Stony Brook, NY USA 11794 Instituto de Astrof́ısica, Pontifićıa Universidad Católica de Chile, Santiago, Chile Department of Physics, University of Michigan, Ann Arbor, USA 48103 Astrophysics and Cosmology Research Unit, School of Mathematics, Statistics and Computer Science, University of KwaZulu-Natal, Durban 4041, South Africa Dunlap Institute, University of Toronto, 50 St. George St., Toronto ON M5S3H4 Joseph Henry Laboratories of Physics, Jadwin Hall, Princeton University, Princeton, NJ, USA 08544 Department of Physics and Astronomy, Haverford College, Haverford, PA, USA 19041 Berkeley Center for Cosmological Physics, LBL and Department of Physics, University of California, Berkeley, CA, USA 94720 Astrophysics and Cosmology Research Unit, School of Chemistry and Physics, University of KwaZulu-Natal, Durban 4041, South Africa National Institute for Theoretical Physics (NITheP), University of KwaZulu-Natal, Private Bag X54001, Durban 4000, South Africa NASA/Goddard Space Flight Center, Greenbelt, MD, USA 20771

Looking through the same lens: Shear calibration for LSST, Euclid, and WFIRST with stage 4 CMB lensing

The next-generation weak lensing surveys (i.e., LSST, Euclid, and WFIRST) will require exquisite control over systematic effects. In this paper, we address shear calibration and present the most realistic forecast to date for LSST/Euclid/WFIRST and CMB lensing from a stage 4 CMB experiment (“CMB S4”). We use the cosmolike code to simulate a joint analysis of all the two-point functions of galaxy density, galaxy shear, and CMB lensing convergence. We include the full Gaussian and non-Gaussian covariances and explore the resulting joint likelihood with Monte Carlo Markov chains. We constrain shear calibration biases while simultaneously varying cosmological parameters, galaxy biases, and photometric redshift uncertainties. We find that CMB lensing from CMB S4 enables the calibration of the shear biases down to 0.2%–3% in ten tomographic bins for LSST (below the ∼ 0.5 % requirements in most tomographic bins), down to 0.4%–2.4% in ten bins for Euclid, and 0.6%–3.2% in ten bins for WFIRST. For a given lensing survey, the method works best at high redshift where shear calibration is otherwise most challenging. This self-calibration is robust to Gaussian photometric redshift uncertainties and to a reasonable level of intrinsic alignment. It is also robust to changes in the beam and the effectiveness of the component separation of the CMB experiment, and slowly dependent on its depth, making it possible with third-generation CMB experiments such as AdvACT and SPT-3G, as well as the Simons Observatory.

On the reach of perturbative descriptions for dark matter displacement fields

We study Lagrangian Perturbation Theory (LPT) and its regularization in the Effective Field Theory (EFT) approach. We evaluate the LPT displacement with the same phases as a corresponding

The stability of stratified, rotating systems and the generation of vorticity in the Sun

N

On the reach of perturbative methods for dark matter density fields

-body simulation, which allows us to compare perturbation theory to the non-linear simulation with significantly reduced cosmic variance, and provides a more stringent test than simply comparing power spectra. We reliably detect a non-vanishing leading order EFT coefficient and a stochastic displacement term, uncorrelated with the LPT terms. This stochastic term is expected in the EFT framework, and, to the best of our understanding, is not an artifact of numerical errors or transients in our simulations. This term constitutes a limit to the accuracy of perturbative descriptions of the displacement field and its phases, corresponding to a

First detection of cosmic microwave background lensing and Lyman-α forest bispectrum

1\%

Joint likelihood function of cluster counts andn-point correlation functions: Improving their power through including halo sample variance

error on the non-linear power spectrum at

Detection of the pairwise kinematic Sunyaev-Zel'dovich effect with BOSS DR11 and the Atacama Cosmology Telescope

k=0.2 h