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Digging in the Large Scale Structure of the Universe

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Digging in the Large Scale Structure of the Universe Digging in the Large Scale Structure of the Universe Shirley Ho Carnegie Mellon University +**Yen-Chi Chen, **Simeon Bird, Roman Garnett, Siamak Ravanbakhsh, Layne Price, *Francois Lanusse, Jeff Schneider, Chris Genovese, Rachel Mandelbaum, Barnabas Pocozs, Larry Wasserman + SDSS3-BOSS Collaboration Cosmo21, Crete, Greece 05/25/16 CMB experiment raw sensitivity over the years Snowmass CF5 Neutrinos Document arxiv:1309.5383 WMAP Planck Adv-ACT SPT-3G CMB-S4 Shirley Ho Number of spectra DESI Euclid BOSS eBOSS SDSSI/II WiggleZ 2MRS CFA Year experiment finishes Shirley Ho Shirley Ho Large Scale Structure • The contents and properties of our Universe affects the phase space distribution of the density field. (x, y, z, vx,vy,vz)=f(w0,wa, ⌦m(z),H(z), m⌫ ,G,...) p w = equation of state of darkX energy ⇢ w(a)=w + w (1 a) time-dependent equation of state 0 a − m⌫ is sum of neutrino masses X Eisenstein & Hu 1997; Eisenstein, Seo & White 2007; Kaiser 1987; Peacock 2001 Shirley Ho How sum of neutrino masses affect the density field 28 10− 29 10− ) 3 30 10− Density (g/cm 31 10− m⌫ =0eV m⌫ =1eVeV X X Figure Credit: Agarwal & Feldman Shirley Ho What do we do with all these interesting datasets? • Standard analyses: 2 point correlation functions / clustering / stacking • Going beyond standard analyses • Going beyond 3D information that these large scale structure surveys provide. Shirley Ho Standard Analyses: Sum of neutrino masses affect the clustering of density field 2 Clustering of Density Field in Redshift Space Monopole * r 2 The sum of matter density and neutrino density is kept constant. Quadrupole * r Giusarma, dePutter, Ho et al. 2013 Shirley Ho Standard Analyses: Dark Energy equation of state affects the clustering of density field 2 Clustering of Density Field in Redshift Space Monopole * r 2 Quadrupole * r Shirley Ho Standard analyses Correlation Function x s2 in 1D 2 Anderson et al. 2014 Vargas, Ho et al. 2014 • Lots of good science are being done with standard 2 point correlation function/ power- spectrum analyses! • Baryon Acoustic Oscillations BAO • Redshift Space Distortions Galaxy Correlations x s Correlations Galaxy Shirley Ho Standard analyses • Lots of good science are being done with standard 2 point correlation function/ power- spectrum analyses! • Baryon Acoustic Oscillations • Redshift Space Distortions Anderson et al. 2014 Vargas, Ho et al. 2014 Shirley Ho But large scale density field is not that gaussian… Shirley Ho What do we do with all these interesting datasets? • Standard analyses: 2 point correlation functions / clustering / stacking • Going beyond standard analyses • Going beyond 3D information that these large scale structure surveys provide. Shirley Ho Going beyond Gaussian field with ● ● ● ● ● ● ● ● ● ● ● ● ●● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ●●● ● ● ● ● ● ●● ● ● ● ● ● ● ● ● ● ● ●● ● ● ● ● ●● ● ● ●●● ● ● ●●● ● ● ● ● ● ●●●● ● ● ● ● ● ● ● ●●●● ● ● ● ●● ● ● ●●● ● ● ●●● ● ● ● ● ● ● ●●●●●●●● ● ● ●● ● ● ●●● ● ● ● ●● ● ●●● ●● ● ● Subspace Constrained●●●● ● Mean Shift (SCMS)●● ● ● ● ●● ● ● ● ●●●●●●●● ● ●● ● ● ● ● ●● ● ●●●●●● ●●● ● ●● ● ● ● ● ● ● ● ● ● ● ●●●● ● ● ●●● ● ● ●●● ● ● ● ● ● ●●● ● ●● ●● ● ●● ● ● ● ●● ●● ● ● ●● ● ●●●●●●●●●●●●● ● ● ● ● ● ●●● ●● ● ● ●●● ●●●●●● ● ● ● ● ● ●● ● ● ● ● ●● ●●●●●● ● ● ● ● ● ●●● ● ● ● ●●●● ●● ● ● ● ●●● ● ● ● ● ●●●●●●●●●● ● ● ● ● ● ● ● ● ●● ● ●●●● ● ●● ● ● ● ● ●● ● ● ● ●●●● ● ●● ● ● ● ●● ● ●●● ● ● ● ● ● ● ●● ● ● ●● ● ● ● ● ● ● ● ●●● ● ●●● ● ● ● ● ● ● ●● ● ● ● ● ● ● ● ● ●●● ● ● ● ●● ●● ●● ● ● ● ● ●●● ● ●● ● ● ●●● ● ● ● ●●●● ● ● ●● ● ● ●● ● ● ● ● ●● ● ● ● ●●● ● ●● ● ●● ● ● ● ● ● ●●● ●●● ● ● ● ●●● ● ● ●● ●●●●● ● ● ●●● ● ● ●●● ● ●●●● ● ● ● ●●● ● ●●●● ● ●●●●● ● ● ●● ● ● ●● ● ●●● ● ● ●●●●● 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● -See Yen-Chi Chen’s talk on ● ●●●●●●● ● ● ● ●●● ●●● ●● ● ● ● ● ● ● ●●●●●● ●● ● ●●● ● ● ● ● ●●●●●●●●●●● ●●● ● ●●● ● ● ● ● ● ● ● ● ● ●●●●●●●●●●●●●●●●●●●●●●●●●●●●●● ●●●●●●● ● ● ●●●● ● ●● ● ●●● ● ● ● ●● ●●●●●●●●●●●●●●●●●●●●●●●●●●●●●●●●●● ●●●● ●● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ● ●●● ● ● ● ● ● ● ● ●● ● ● ● ●● ● ● ●●● ● ● ● ● ●●● ● ● ● ● ● ● ● ● ● ● ●● ● ● ● ●● ●● ● ● ● ● ●● ● ●● ●● ● ● ● ●● ● ● ● ● ● ●● ●● ● ●● ● ● ● ● ●● ●●● ● ● ● ● ● ● ●●● ●●● ●●●● ●●● ● ● ● ●●● ● ● ●●● ● ●●●●●●●● ● ● ●●● ●●● ● ● ● ●●●●●●●●● ● ● ● ● ●● ● ●● ● ●●●●●● ● ●●● ● ●●● ● ● ●●●● ●●●● ●● ● ● ● ● ●●● ● ● ●● ●●●●● ● ● ● ● ● ● ● ●●● ●● ● ● ●●●●●● ● ● ●● ● ●●● ●●● ● ● ●●●●● ● ● ● ● ●● ●● ● ●●●●● ● ● ●● ● ● ●●● ● ● ●●●●●●● ●●● ● ● ● ●● ● ●● ● ●●●●● ● ● ● ● ● *Thursday* to understand the ● ●●●● ● ● ● ●● ●●●● ●● ●●●●●●●●●●●●●●● ● ● ● ● ●● ● ● ● ●●● ●● ●●● ●● ● ●●● ●●●● ● ● ● ●●● ● ● ● ● ● ● ●●●● ● ●●● ● ●● ● ● ● ●● ●●● ● ●●● ● 25 ● ● ●● ● ● ●●● ●● ●● ● ● ●●● ● ● ●●●● ● ● ●● ●●● ● ● ●● ● ● ● ● ● ●●●●●● ● ● ●● ● ● ● ●●● ● ● ● 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●●●●●●●●●●●●●●●●●●●●●●●●●●● ● ● ● ● ● ● ● ● ● ● ●●●●●● ● ●●●●●●●●● ● ● ● ● ●●●●●● ● ● ●●● ● ● ● ● ●●●●● ● ●● ● ●● ●●●● ● -Basic idea is to find ridges● ● in ●● ● ● ●●●● ● ● ● ● ●● ● ●● ● ●● ●● ● ●●●● ● ● ● ●●●● ● ●●●● ● ● ● ● ● ● ●●●● ● ● ●● ● ● ●●●● ● ● ● ●●●● ● ● ●● ● ●●● ● ● ● ● ●●●● ● ● ● ● ●●●●●●● ●●● ● ● ● ●● ●●●● ● ● ● ● ●●●● ● ●●● ● ● ●●● ● ● ● ●● ●● ● ● ● ● ●●●● ● ● ●●● ● ● ● ● ● ● ● ●● ●●●● ● ● ●● ● ● ●● ●● ●● ● ●●● ● ● ● ● ●● ● ●● ● ● ● ●●● ●● ● ● ●●● ● ●● ●●● ●● ● ● ●●●●● ● ●●●● ●● ● ● ● ●● ● ● ● ●● ● ● ●●● ● ● ● ● ● ● ● ● ● ●● ●●● ● ● ● ● ● ●● ● ● ●●●●●● ● ● ● ● ● ● ● ● ● ● ●●●●● ● ●●● ● ● ● ● ●● ● ● ● ● ●●● ● ●●●● ● ● ●● ●● ● ●● ● ● ●●● ● ● ● ● ● ● ● ● ● ● ● ● ●●● the density field by looking● ●● at●● ● ● ● ● ● ●● ●●● ● ● ● ● ● ●● ● ● ● ● ● ●● ● ● ● ●● ●●● ● ●●● ● ●● ● ● ●●●● ● ● ●●●● ● ● ● ●●● ● ●●●● ●●●●● ● ● ● ● ●● ● ● ●●●●●●●●●●●●●●● ●●●● ● ●●● ● ● ● ● ●● ●● ●●● ● ● ● ● ● ● ● ●● ●● ● ● ● ●● ●● ● ●● ● ● ● ● ● ● ● ● ●●●●● ●● ●● ● ● ● ● ● ●● ● ● ● ●●● ● ● ● ● ● ● ● ● ● ● 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  • Mcwilliams Center for Cosmology
    McWilliams Center for Cosmology McWilliams Center for Cosmology McWilliams Center for Cosmology McWilliams Center for Cosmology ,CODQTGG Rachel Mandelbaum (+Optimus Prime) Observational cosmology: • how can we make the best use of large datasets? (+stats, ML connection) • dark energy • the galaxy-dark matter connection I measure this: for tens of millions of galaxies to (statistically) map dark matter and answer these questions Data I use now: Future surveys I’m involved in: Hung-Jin Huang 0.2 0.090 0.118 0.062 0.047 0.118 0.088 0.044 0.036 0.186 0.016 70 0.011 0.011 − 0.011 − 0.011 − 0.011 − 0.011 − 0.011 0.011 − 0.011 0.011 ± ± ± ± ± ± ± ± ± ± 50 η 0.1 30 ∆ Fraction 10 1 24 23 22 21 0.40.81.2 0.20.61.0 0.6 0.2 0.20.6 0.30.50.70.9 1.41.61.82.02.2 0.15 0.25 0.10.30.5 0.4 0.00.4 − − 0−.1 − − − − . 0.090 ∆log(cen. R )[kpc/h] P ∆ 0.011 0.3 cen. Mr cen. color cen. e eff cen log(richness) z cluster e R ± dom 1 0.2 . − cen 0.1 3 Fraction − 21 Research: − 0.118 0.622 0.3 0.011 0.009 Mr 22 1 . ± ± 0.2 0 − . 23 − 0.1 Fraction cen intrinsic alignments in 24 − 0.8 0.062 0.062 0.084 0.7 1.2 0.011 0.011 0.011 0.6 redMaPPer clusters − ± − ± − ± 0.5 color . 0.4 0.8 0.3 Fraction cen 0.2 0.4 0.1 1.0 0.047 0.048 0.052 0.111 0.3 Advisor : 0.011 0.011 0.011 0.011 e − ± − ± − ± − ± .
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  • Deep21: a Deep Learning Method for 21Cm Foreground Removal
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  • Recent Developments in Neutrino Cosmology for the Layperson
    Recent developments in neutrino cosmology for the layperson Sunny Vagnozzi The Oskar Klein Centre for Cosmoparticle Physics, Stockholm University [email protected] PhD thesis discussion Stockholm, 10 June 2019 1 / 27 D'o`uvenons-nous? Que sommes-nous ? O`uallons-nous? Courtesy of Paul Gauguin 2 / 27 The oldest questions... Where do we come from? What are we made of ? Where are we going? 3 / 27 ...and the modern versions of these questions What were the Universe's initial conditions? Where do we come from? −! What is the Universe What are we made of ? −! made of ? Where are we going? −! How will the Universe evolve? 4 / 27 Where do we come from? Cosmic inflation aka (Hot) Big Bang? 5 / 27 What are we made of? Mostly dark stuff (and a bit of neutrinos) 6 / 27 Where are we going? Depends on what dark energy is? 7 / 27 Lots of astrophysical and cosmological data to test theories for the origin/composition/fate of the Universe: 8 / 27 Neutrinos 9 / 27 Neutrino masses 10 / 27 Neutrino mass ordering 11 / 27 Paper I Sunny Vagnozzi, Elena Giusarma, Olga Mena, Katie Freese, Martina Gerbino, Shirley Ho, Massimiliano Lattanzi, Phys. Rev. D 96 (2017) 123503 [arXiv:1701.08172] What does current data tell us about the neutrino mass scale and mass ordering? How to quantify how much the normal ordering is favoured? 12 / 27 Paper I Even a small amount of massive neutrinos leaves a huge trace in the distribution of galaxies on the largest observables scales 13 / 27 Paper I 1 M < kg ν 10000000000000000000000000000000000000 14 / 27 Paper II Elena Giusarma, Sunny Vagnozzi, Shirley Ho, Simone Ferraro, Katie Freese, Rocky Kamen-Rubio, Kam-Biu Luk, Phys.
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  • From Dark Matter to Galaxies with Convolutional Networks
    From Dark Matter to Galaxies with Convolutional Networks Xinyue Zhang*, Yanfang Wang*, Wei Zhang*, Siyu He Yueqiu Sun*∗ Department of Physics, Carnegie Mellon University Center for Data Science, New York University Center for Computational Astrophysics, Flatiron Institute xz2139,yw1007,wz1218,[email protected] [email protected] Gabriella Contardo, Francisco Shirley Ho Villaescusa-Navarro Center for Computational Astrophysics, Flatiron Institute Center for Computational Astrophysics, Flatiron Institute Department of Astrophysical Sciences, Princeton gcontardo,[email protected] University Department of Physics, Carnegie Mellon University [email protected] ABSTRACT 1 INTRODUCTION Cosmological surveys aim at answering fundamental questions Cosmology focuses on studying the origin and evolution of our about our Universe, including the nature of dark matter or the rea- Universe, from the Big Bang to today and its future. One of the holy son of unexpected accelerated expansion of the Universe. In order grails of cosmology is to understand and define the physical rules to answer these questions, two important ingredients are needed: and parameters that led to our actual Universe. Astronomers survey 1) data from observations and 2) a theoretical model that allows fast large volumes of the Universe [10, 12, 17, 32] and employ a large comparison between observation and theory. Most of the cosmolog- ensemble of computer simulations to compare with the observed ical surveys observe galaxies, which are very difficult to model theo- data in order to extract the full information of our own Universe. retically due to the complicated physics involved in their formation The constant improvement of computational power has allowed and evolution; modeling realistic galaxies over cosmological vol- cosmologists to pursue elucidating the fundamental parameters umes requires running computationally expensive hydrodynamic and laws of the Universe by relying on simulations as their theory simulations that can cost millions of CPU hours.
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