COSMO 2016

August 8-12, 2016

International Conference on Particle Physics and Cosmology, 2016

CONFERENCE PROGRAM

Ann Arbor, MIPlenary Speakers
ı Elena Aprile
Columbia University

ı Celine Boehm
Durham University

ı Alessandra Buonanno
MPG, Potsdam

ı Marcela Carena
Fermilabı John Carlstrom
University of Chicago

ı Kiwoon Choi
Inst. for Basic Sci., Korea

ı Cora Dvorkin
Harvard University

ı Carlos Frenk
Durham University

ı Joshua Frieman
University of Chicago

ı Takaaki Kajita
University of Tokyo

ı Eiichiro Komatsu
MPA, Garchingı Andrei Linde
Stanford University

ı Joe Lykken
Fermilabı Rachel Mandelbaumı Vuk MandiÊ
Carnegie-Mellon University
University of Minnesota

ı Malcolm Perry
Cambridge University

ı Adam Riess
Johns Hopkins University

ı Rachel Rosen
Columbia University

ı Enrico SessoloNat. Centre for Nuclear
Res., Warsaw

ı Pierre Sikivie
University of Florida

ı Douglas Spolyar
Stockholm University

ı Monica Valluri
University of Michigan

Local Organizing Committee
ı David Cinabro
Wayne State University

ı Gus Evrard
University of Michigan

ı Katherine Freese
University of Michigan

ı David Gerdes
University of Michigan

ı Dragan Huterer
University of Michigan

ı Gordy Kane
University of Michigan

ı Wolfgang Lorenzon
University of Michigan

ı Tim McKay
University of Michigan

ı Jeffrey McMahon
University of Michigan

ı Chris Miller
University of Michigan

ı Alexey Petrov
Wayne State University

ı Keren Sharon
University of Michigan

ı Greg Tarle
University of Michigan

1International Steering Committee
ı Vernon Barger
University of
Wisconsin-Madison

ı Daniel Baumann
Cambridge University

ı John Beacom
Ohio State University

ı David Caldwell
Stanford University

ı Jonathan Ellis
CERNı Kari Evqvist
University of Helsinkiı Evalyn Gates
Cleveland Museum of
Natural History

ı Ruth Gregory
Durham University

ı Francis Halzen
University of
Wisconsin-Madison

ı Stephen Hawking
University of Cambridgeı Mark Hindmarsh
University of Sussex

ı Stavros Katsanevas
Université Paris VII

ı Jihn Kim
Seoul National University

ı Rocky Kolb
University of Chicago

ı Julien Lesgourgues
CERN

ı Andrei Linde
Stanford University

ı David Lyth
Lancaster University

ı Carlos Martins
Centro de Astrofisica daUniv do Portoı Hans-Peter Nilles
Physikalisches Institut der
Universität Bonnı Michael Ramsey-Musolf ı Antonio Riotto
University of
University of Geneva
Massachusetts Amherstı Matts Roos
University of Helinskiı Leszek Roszkowski
University of Sheffieldı Jun’ichi Yokoyamaı Hu Zhan
RESCEU, The University of
National Astronomical
Tokyo
Observatories, Chinese
Academy of Sciencesı Goran Senjanovic
International Centre for
Theoretical Physics
ı2

Table of Contents
4 Conference Program.
4 Monday6 Tuesday
7 Wednesday
8 Thursday
9 Friday

10 Parallel Sessions.
10 Monday
13 Tuesday
16 Wednesday
19 Friday

21 Poster Presentations.
25 Abstracts for Plenary Talks.
25 Monday
27 Tuesday
28 Wednesday
30 Thursday
31 Friday

32 Abstracts for Parallel Sessions.
32 Monday
45 Tuesday
59 Wednesday
71 Friday

77 COSMO-16 Participants.
84 Code of Conduct.

3

Conference Program
Monday, August 8, 2016
8:00 am Registration and Continental Breakfast, Michigan League – Ballroom.
9:00 am Welcome, Mendelssohn Theatre.
PLENARY SESSION, Mendelssohn Theatre.
9:15 am Eiichiro Komatsu, MPA, Garching.

From initial conditions to structure formation, and back

10:00 am Rachel Rosen, Columbia University.
A Massive Gravity Status Report

10:35 am COFFEE BREAK, Michigan League – Ballroom.
11:10 am Enrico Sessolo, Nat. Centre for Nuclear Res., Warsaw.

Dark matter — What it is and how to determine its properties

11:45 am Carlos Frenk, Durham University.

Searching for the identity of the dark matter in our cosmic backyard

12:20 am Leszek Roszkowski, NCBJ, Warsaw.
History of COSMOs

12:30 pm LUNCH BREAK.
2:00 pm PARALLEL SESSIONS.
CMB/Large Scale Structure, Mendelssohn Theatre.
Chairs: Brad Benson, Rachel Mandelbaum

Dark Energy, Michigan League – Hussey Room.
Chairs: Anne Davis, Roland de Putter

Primordial/Inflation, Michigan League – Vandenberg Room.
Chairs: Andrei Linde

3:30 pm COFFEE BREAK, Michigan League – Ballroom.
4:00 pm PARALLEL SESSIONS.
CMB/Large Scale Structure, Mendelssohn Theatre.
Chairs: Brad Benson, Rachel Mandelbaum

Dark Energy, Michigan League – Hussey Room.
Chairs: Anne Davis, Roland de Putter

Primordial/Inflation, Michigan League – Vandenberg Room.
Chairs: Andrei Linde4

5:30 pm END OF SESSIONS.
5:30-6:00 pm Poster Presentations, Michigan League – Ballroom and Room 6.
6:00-9:00 pm Reception and Dinner, UM Museum of Art.

5

Tuesday, August 9, 2016
8:00 am Continental Breakfast, Michigan League – Ballroom.
PLENARY SESSION, Mendelssohn Theatre.
9:00 am Celine Boehm, Durham University.

Dark Matter: the past and future of the field.

9:35 am Joe Lykken, Fermilab.

Whatever happened to BSM physics?

10:10 am COFFEE BREAK, Michigan League – Ballroom.
10:45 am Monica Valluri, University of Michigan.

The orbital structure of dark matter halos and implications for dark matter detection

11:20 am Rachel Mandelbaum, Carnegie-Mellon University.

Weak gravitational lensing cosmology: status and future prospects

11:55 am Elena Aprile, Columbia University.

Present and Future Prospects for WIMPs Direct Detection

12:30 pm LUNCH BREAK.
2:00 pm PARALLEL SESSIONS.
Future Probes, Mendelssohn Theatre.
Chairs: Tim Eifler, Elisabeth Krause

Dark Energy, Michigan League – Hussey Room.
Chairs: Anne Davis, Roland de Putter

LIGO and Black Holes, Michigan League – Vandenberg Room.
Chair: Dejan Stojkovic

Dark Matter Experiment, Michigan League – Michigan Room.
Chairs: Mariangela Lisanti, Leszek Roszkowski

3:30 pm COFFEE BREAK and Poster Presentations, Michigan League – Ballroom.
4:00 pm PARALLEL SESSIONS.
CMB/Large Scale Structure, Mendelssohn Theatre.
Chairs: Brad Benson, Rachel Mandelbaum

Dark Energy/Dark Matter, Michigan League – Hussey Room.

Chairs: Mariangela Lisanti, Leszek Roszkowski, Anne Davis, Roland de Putter

LIGO and Black Holes/Primordial/Inflation, Michigan League – Vandenberg Room.
Chairs: Dejan Stojkovic, Andrei Linde

5:30 pm END OF SESSIONS.

6

Wednesday, August 10, 2016
8:00 am Continental Breakfast, Michigan League – Ballroom.
PLENARY SESSION, Mendelssohn Theatre.
9:00 am Joshua Frieman, University of Chicago.
Early Results from the Dark Energy Survey

9:35 am Vuk MandiÊ, University of Minnesota.

First Direct Detections of Gravitational Waves

10:10 am COFFEE BREAK, Michigan League – Ballroom.
10:45 am Martina Gerbino, NORDITA.

Neutrinos in cosmology: an overview

11:20 am Roland de Putter, Caltech.

Probing Inflation with Future Galaxy Surveys

11:55 am Adam Riess, Johns Hopkins University.

A New Measurement of the Expansion Rate of the Universe

12:30 pm LUNCH BREAK.
2:00 pm PARALLEL SESSIONS.
CMB/Large Scale Structure, Mendelssohn Theatre.
Chairs: Brad Benson, Rachel Mandelbaum

Dark Matter, Michigan League – Hussey Room.
Chairs: Mariangela Lisanti, Leszek Roszkowski

Dark Energy, Michigan League – Vandenberg Room.
Chairs: Anne Davis, Roland de Putter

3:30 pm COFFEE BREAK, Michigan League – Ballroom.
4:00 pm PARALLEL SESSIONS.
CMB/Large Scale Structure, Mendelssohn Theatre.
Chairs: Brad Benson, Rachel Mandelbaum

Dark Matter, Michigan League – Hussey Room.
Chairs: Mariangela Lisanti, Leszek Roszkowski

Primordial/Inflation, Michigan League – Vandenberg Room.
Chairs: Andrei Linde

5:30 pm END OF SESSIONS.
6:30-10 pm Banquet, Henry Ford Museum, Detroit.

7

Thursday, August 11, 2016
8:00 am Continental Breakfast, Michigan League – Ballroom.
PLENARY SESSION, Mendelssohn Theatre.
9:00 am Kiwoon Choi, Inst. for Basic Science, Korea.

Natural inflation and relaxion with multiple axions

9:35 am COFFEE BREAK, Michigan League – Ballroom.
10:10 am Takaaki Kajita, University of Tokyo.

Neutrino oscillation experiments — Discovery, status and prospects

10:45 am John Carlstrom, University of Chicago.

Cosmology with the Cosmic Microwave Background

11:30 am Depart for activities (box lunch provided).
6:30 pm PUBLIC TALK: Astronaut Mario Runco, Mendelssohn Theatre.

8

Friday, August 12, 2016
8:00 am Continental Breakfast, Michigan League – Ballroom.
9:00 am PARALLEL SESSIONS.
CMB/Large Scale Structure, Mendelssohn Theatre.
Chairs: Brad Benson, Rachel Mandelbaum

Dark Matter, Michigan League – Hussey Room.
Chairs: Mariangela Lisanti, Leszek Roszkowski

Primordial/Inflation, Michigan League – Vandenberg Room.
Chairs: Andrei Linde

10:30 am COFFEE BREAK, Michigan League – Ballroom.
PLENARY SESSION, Mendelssohn Theatre.
11:00 am Alessandra Buonanno, Max Planck Inst. for Grav. Physics.
What did we learn from LIGO first black holes?

11:35 am Malcolm Perry, Cambridge University.

The Black Hole Paradox Revisited: Soft Black Hole Hair

12:10 pm LUNCH BREAK.
2:00 pm Pierre Sikivie, University of Florida.
Axion Dark Matter

2:35 pm Cora Dvorkin, Harvard University.

Traces of the Early Universe in the CMB and the Large-Scale Structure

3:10 pm Andrei Linde, Stanford University.

Inflation, dark energy, and SUSY breaking

3:45 pm END OF CONFERENCE.

9

Parallel Sessions
Monday, August 8, 2016
CMB/LARGE SCALE STRUCTURE, Mendelssohn Theatre.
Chairs: Brad Benson and Rachel Mandelbaum

2-3:30 pm Bjoern Soergel.

Detection of the kinematic Sunyaev-Zel dovich effect with DES Year 1 and SPT

Sebastian Bocquet.

The Growth of Cosmic Structure Measured with Galaxy Clusters in the South Pole Telescope
SPT-SZ Survey

Carles Sánchez.

Weak Gravitational Lensing in the Dark Energy Survey

Siddharth Satpathy.

Measurement of the growth rate of structure using galaxy correlation functions

Juliana Kwan.

Cosmology from large scale galaxy clustering and galaxy-galaxy lensing with Dark Energy Survey
Science Verification data

Ema Dimastrogiovanni.

Testing early Universe physics with upcoming observations

4-5:30 pm Kevin Huffenberger.

Are there localized B-mode dust foregrounds in the BICEP/Keck field?

Jessica Muir.

Integrated Sachs-Wolfe signal reconstruction using galaxy surveys

Arya Farahi.

Forward modeling of galaxy clusters

Joyce Byun.

Recovering information beyond the power spectrum of large-scale structure

Masato Shirasaki.

Covariance of galaxy-galaxy lensing: Jackknife vs. Mock

Jonathan Braden.

Constraining cosmological ultra-large scale structure using numerical relativity

DARK ENERGY, Michigan League – Hussey Room.
Chairs: Anne Davis and Roland de Putter

2-3:30 pm Elise Jennings.

Cosmological constraints from Supernovae using Approximate Bayesian Analysis

Takahiro Hayashinaka.

Fermionic Schwinger Effect and Induced Current in de Sitter spacetime
10Sebastian Zell.

On the substructure of the cosmological constantJanina Renk.

Gravity at the horizon: testing gravity with relativistic effects in large scale structure observables

Jounghun Lee.

A Bound Violation on the Galaxy Group Scale: The Turn Around Radius of NGC 5353/4 as a
Test of Gravity

Shuntaro Mizuno.

Vainshtein mechanism in massive gravity nonlinear sigma models

4-5:30 pm Amol Upadhye.

Redshift-space distortions constrain massive neutrinos and evolving dark energyFrank Koennig.

A spectre is haunting the cosmos: Quantum stability of massive gravity with ghosts

Mark Hertzberg.

Gravitation, Quantum Consistency, and Causality

Stefano Anselmi.

Quasidilaton massive gravity faces cosmological constraints

Matteo Fasiello.

LSS probes for Dark Energy and Modified Gravity

Shuang-Yong Zhou.

The Lambda2 limit of dRGT massive gravity

PRIMORDIAL/INFLATION, Michigan League – Vandenberg Room.
Chair: Andrei Linde

2-3:30 pm Peter Adshead.

Asymmetric reheating and chilly dark sectors

Mustafa Amin.

From Wires to Cosmology: Stochastic Particle Production during Inflation and Reheating

Damien Easson.

Stability of cosmological models with unusual scalar fluids

Tommi Tenkanen.

A Strong Electroweak Phase Transition from the Inflaton Field

Scott Watson.

The End of Inflation

Gonzalo Palma.

On the role of light fields during inflation

4-5:30 pm Ivonne Zavala.

Axion Inflation in String Theory and Primordial Gravitational Waves

11Shuichiro Yokoyama.

Revisiting matter isocurvature fluctuations in the curvaton scenario

Mohammad Hossein Namjoo.

Probing the Primordial Universe using Massive Fields

Jinn-Ouk Gong.

Consistency relation and inflaton redefinition in the delta-N formalism

Kaloian Lozanov.

The Equation of State and Duration to Radiation Domination After Inflation

Jason Evans.

Naturalizing Supersymmetry with a Two-Field Relaxion Mechanism

12

Tuesday, August 9, 2016
FUTURE PROBES, Mendelssohn Theatre.
Chairs: Tim Eifler and Elisabeth Krause

2-3:30 pm Benjamin Saliwanchik.

Design and Scientific Forecast of the Hydrogen Intensity and Real-time Analysis eXpermiment(HIRAX)

Seth Siegel.

CHIME: A Stage IV Dark Energy Experiment

Jon Gudmundsson.

Lessons learned from SPIDER’s first flight and implications for future ballooning and satellite
missions

Roland de Putter.

Probing Inflation with Galaxy Clustering on Ultra-Large Scales

Caroline Heneka.

Probing Reionization: Cross-correlation of 21-cm and Lyman-alpha fluctuations

Inh Jee.

Strong Lensing Cosmography: method, predictions and measurements

CMB/LARGE SCALE STRUCTURE, Mendelssohn Theatre.
Chairs: Brad Benson and Rachel Mandelbaum

4-5:30 pm Paul Shapiro.

Simulating Cosmic Reionization and Its Observable Consequences

Anson D’Aloisio.

Probing Cosmological Reionization with the High-redshift Lyman-alpha Forest

Hao-Yi Wu.

A physical model for the anisotropies of cosmic far-infrared background

Marcelo Alvarez.

Mock LSS Surveys with the Peak Patch Approach

Joel Meyers.

Light Relics and Next Generation CMB Observations

Chen Heinrich.

Lensing Bias to Compensated Isocurvature Perturbations

DARK ENERGY, Michigan League – Hussey Room.
Chairs: Anne Davis and Roland de Putter

2-3:30 pm Miguel Zumalacarregui.

New probes of gravity and cosmic acceleration
13

Lucas Lombriser.

Challenges to Self-Acceleration in Modified Gravity from Gravitational Waves and Large-Scale
Structure

Shahab Joudaki.

KiDS+2dFLenS: Testing Gravity on Cosmic Scales with Weak Lensing and Redshift Space
Distortions

Eva-Maria Mueller.

BOSS DR12 Combined Sample Analysis constraints on modified gravity

Sebastian Cespedes.

Modifications of the speed of gravitational waves at early times

Chi-Ting Chiang.

Fake Separate Universe: A new trick for simulating clustered quintessence cosmologies

DARK ENERGY/DARK MATTER, Michigan League – Hussey Room.

Chairs: Anne Davis, Roland de Putter, Mariangela Lisanti, and Leszek Roszkowski

4-5:30 pm Brian Nord.

DeepLensing: The Use of Deep Learning to Find Strong Lenses in the Dark Energy Survey

Joseph DeRose.

Simulating the Dark Energy Survey Sky

Evan Grohs.

Precision big bang nucleosynthesis and neutrino cosmology

Tanja Rindler-Daller.

Dark stars as progenitors of supermassive black holes in the early Universe

Jayden Newstead.

Neutrino floors for non-standard direct dark matter detection scenarios

LIGO AND BLACK HOLES, Michigan League – Vandenberg Room.
Chair: Dejan Stojkovic

2-3:30 pm Dejan Stojkovic.

Quantum aspects of gravitational collapse: non-singularity and non-locality

Liang Dai.

Lensing magnification bias on the apparent distribution of black hole mergers

Ruth Gregory.

Screened Scalars and Black Holes

Alexandre Dolgov.

LIGO-observed gravitational waves: problems and solution

Tomohiro Nakama.

New primordial black hole constraints to primordial gravitational waves

14David Weir.

Simulating a first-order electroweak phase transition

LIGO AND BLACK HOLES/PRIMORDIAL/INFLATION, Michigan League – Vandenberg Room.
Chairs: Dejan Stojkovic and Andrei Linde

4-5:30 pm Simeon Bird.

Did LIGO Detect Dark Matter?

Florian Kuhnel.

Primordial Black Holes

Riccardo Penco.

Effective Field Theory of Inflation with Broken Spatial Diffeomorphisms

Emil Mottola.

Scalar Gravitational Waves in the Effective Theory of Gravity

Tomohiro Fujita.

Inflationary Gravitational Waves - beyond vacuum fluctuation

Bohua Li.

Complex Scalar Field Dark Matter and its Imprint on the Gravitational Wave Background from
Inflation

DARK MATTER EXPERIMENT, Michigan League – Michigan Room.
Chairs: Mariangela Lisanti and Leszek Roszkowski

2-3:30 pm Evan Pease.

Current Status of the LUX Dark Matter Experiment

Kaixuan Ni.

Recent Results from the XENON Dark Matter Experiments

Wolfgang Lorenzon.

The LZ Dark Matter experiment

Anthony Villano.

Pushing the limits of low-energy calorimetry in SuperCDMS

Eric Dahl.

Recent Results from PICO

Phillip Urquijo.

The SABRE Dark Matter Experiment: A pair of sodium iodide detectors located in Italy andAustralia

15

Wednesday, August 10, 2016
CMB/LARGE SCALE STRUCTURE, Mendelssohn Theatre.
Chairs: Brad Benson and Rachel Mandelbaum

2-3:30 pm Martina Gerbino.

The hunt for neutrino hierarchy

Thomas Tram.

The Intrinsic Matter Bispectrum

Jerome Gleyzes.

Non Gaussianity in two-field inflation

Christian Fidler.

A Relativistic Interpretation of Newtonian Large Scale Structure Simulations

Grant Mathews.

Possible Evidence for Resonant Superstring Excitations during Inflation

Neil Barrie.

Gravitational Wave Instabilities in the Cosmic Neutrino Background

4-5:30 pm Craig Copi.

CMB Anomalies: Status and Future Directions

Graeme Addison.

Quantifying discordance in the 2015 Planck CMB spectrum

Marius Millea.

Features in the Planck power spectrum and shifts in cosmological parameters

Melanie Simet.

Weak Lensing Measurement of the Mass-Richness Relation of SDSS redMaPPer Clusters

Jonathan Blazer.

Streaming velocities and baryonacoustic oscillations

Sukhdeep Singh.

Galaxy-galaxy and galaxy-CMB Lensing with SDSS-III BOSS galaxies

DARK MATTER, Michigan League – Hussey Room.
Chairs: Mariangela Lisanti and Leszek Roszkowski

2-3:30 pm Francesc Ferrer.

A robust halo-independent upper limit on the dark matter cross section

Francis-Yan Cyr-Racine.

From dark particle physics to the matter distribution of the Universe

Tim Linden.

Dark Matter, Pulsar, and Diffuse Emission Models for the Galactic Center GeV Excess

16Annika Peter.

How self-interacting dark matter shapes the Milky Way satellite population

Savvas Koushiappas.

Cosmological constraints to dark matter with two- and many-body decays

Mei-Yu Wang.

Revealing the nature of dark matter with Milky Way dwarf satellite galaxies

4-5:30 pm Haipeng An.

Dark matter annihilation via dark bound state formation

Hongwan Liu.

The Darkest Hour Before Dawn: Contributions to Cosmic Reionization from Dark Matter
Annihilation and Decay

Sebastian Trojanowski.

Reconstructing WIMP properties through an interplay of signal measurements in direct
detection, Fermi-LAT, and CTA searches for dark matter

Isabel M. Oldengott.

Reionization and dark matter decay

Keisuke Harigaya.

Light Chiral Dark Sector

Sam Cormack.

Superfluid fermion dark matter

DARK ENERGY, Michigan League – Vandenberg Room.
Chairs: Anne Davis and Roland de Putter

2-3:30 pm David Cinabro.

No Evidence for Type Ia Supernova NUV-Optical Subclasses

Dan Scolnic.

New Cosmology Results with Type Ia Supernovae

Tom Giblin.

Toward Full General Relativity in Cosmology

James Mertens.

Deviations from Homogeneity in an Inhomogeneous Universe

Tony Padilla.

The“sequestering” approach to the cosmological constant problem

Christoph Schmid.

Einstein’s equations from Einstein’s inertial motion and Newton’s laws

17

PRIMORDIAL/INFLATION, Michigan League – Vandenberg Room.
Chair: Andrei Linde

4-5:30 pm Sonia Paban.

On primordial equation of state transitions

Robert Caldwell.

Gravitational Wave – Gauge Field Oscillations

Martin Winkler.

Modulated Natural Inflation

Raghavan Rangarajan.

Constraints on just enough inflation preceded by a thermal era

Nadia Bolis.

Observational Consequences of Scalar-Tensor Entanglement during Inflation

Krzysztof Turzynski.

Initial state entanglement and inflation

18

Friday, August 12, 2016
CMB/LARGE SCALE STRUCTURE, Mendelssohn Theatre.
Chairs: Brad Benson and Rachel Mandelbaum

9-10:30 am Pieter Daniel Meerburg.
The Holiest Grail

Laura Mocanu.

Measuring the CMB gravitational lensing potential with SPTpol

Alexander van Engelen.

CMB Lensing with ACTPol and successors

Kyle Story.

Delensing CMB B modes with the South Pole Telescope polarimeter

Kimmy Wu.

BICEP3 performance overview and the BICEP/Keck program

Alexandra Rahlin.

Status report on the first flight of the SPIDER balloon-borne polarimeter

DARK MATTER, Michigan League – Hussey Room.
Chairs: Mariangela Lisanti and Leszek Roszkowski

9-10:30 am Julian Munoz.

Probing compact dark matter with fast radio bursts

Adam Christopherson.

Astrophysical bounds on ultra light axion-like particles

James Dent.

Dark Matter, Light Mediators, and the Neutrino Floor

Stacy Kim.

Constraining Self-Interacting Dark Matter through Equal Mass Galaxy Cluster Mergers

Patrick Stengel.

Charged Mediators in Dark Matter Scattering

19

PRIMORDIAL/INFLATION, Michigan League – Vandenberg Room.
Chair: Andrei Linde

9-10:30 am Marco Drewes.

Experimental tests of leptogenesis

Zachary Kenton.

The Separate Universe Approach to Soft Limits

Austin Joyce.

Three-dimensional inflation

Kohei Kamada.

Large-scale magnetic fields and baryogenesis via chiral anomaly

Evangelos Sfakianakis.

Magnetogenesis from axion inflation

Naritaka Oshita.

A baby universe from a black hole20

Poster Presentations
Primordial Cosmology and Inflation
Shin’ichi Hirano, Rikkyo University.
Ultra slow-roll G-inflation

Natacha Altamirano, Perimeter Institute/University of Waterloo.
Cosmological perturbations in the Holographic Big Bang model

Jai-chan Hwang, Kyungpook National University.
Special relativistic hydrodynamics with gravity

Elizabeth Gould, Perimeter Institute for Theoretical Physics.

Observational Constraints of Holographic Cosmology from PLANCKHenry Stoltenberg, UC Davis.

Non Bunch-Davies Initial Conditions and the CMB

Zach Weiner, University of Illinois Urbana-Champaign.
Preheating with Non-Abelian Gauge Fields

Pablo Gonzalez, Universidad de Chile.
Inflation in ”˜ Gravity.

Matthew Hull, ICG, Portsmouth University.
Galileonic Higgs Cosmology

Igor Rudenok, Taras Shevchenko National University of Kyiv.

Evolution of magnetic fields and chiral asymmetry in primordial plasma with chiral asymmetry

Caner Unal, University of Minnesota.

Scale-dependent gravitational waves from a rolling axion

Andrea Quadri, INFN, Sez. di Milano.

The Cosmological Slavnov-Taylor Identity from BRST Symmetry in Inflationary Models

Nelson Videla, Universidad de Chile.

Natural inflation and electroweak baryogenesis on the brane

Pablo Morales, The University of Tokyo.
Field Theory of the Perfect Fluid

David Edwards, University of Edinburgh.
David Edwards

Andrew Long, University of Chicago, KICP.
Baryogenesis from Decaying Magnetic Helicity

Rob Allen, Sam Houston State University.

Previously Unsolved Problems in Physics Ranging from Cosmology to Quark Characteristics have
Many Solution Equations Containing Basic Numbers.

Dhrubo Jyoti, Dartmouth College.

Inflation and the quantum measurement problem

Carisa Miller, UNC.

Quartic Chameleons: Safely Scale-Free in the Early Universe
21

CMB and Large Scale Structure
Alexandra Terrana, York University & Perimeter Institute.

Mapping the Universe with the large-scale kinetic Sunyaev-Zel’dovich

Chiamaka Okoli, Perimeter Institute/University of Waterloo.
Neutrino Masses from Gravitational Wakes

Xiao Fang, Ohio State University.

FAST-PT: An Extremely Efficient Algorithm For Cosmological Perturbation Theory

Marcio O’Dwyer, Case Western Reserve University.

The ISW effect and the lack of large-angle CMB temperature correlations

Derek Inman, University of Toronto.

Non-Linear Neutrino Effects in Large Scale Structure

Utane Sawangwit, National Astronomical Research Institute of Thailand.
Cosmic void profile measurement from PLANCK lensing potential

Lee Whittaker, University of Manchester.

Investigating the simultaneous measurement of cosmology and intrinsic alignments using Gaussian
random simulations

Minji Oh, KASI/UST.

Excavating neutrino mass buried under the larges scale structure of the Universe

Denise Schmitz, California Institute of Technology.
Effects of Advection on Intrinsic Alignments of Galaxies

George Stein, CITA, University of Toronto.

A Multi-Tracer Approach to Primordial non-Gaussianity

Nilanjan Banik, University of Florida.

Optimally weighting galaxy pairs for BAO measurement in the context of DES Y1Aditya Rotti, Florida State University.
Aditya Rotti

Keir Rogers, University College London.

Spin-SILC: CMB polarisation component separation for next-generation experiments

Johnathan Hung, DAMTP, Cambridge.

Measuring Non-Guassianity in Galaxy Surveys: A new window on the Universe

Daniel Martens, The Ohio State University.

The Effects of Resonant Line Scattering at Recombination on the Observed CMB Power Spectrum

Adri Duivenvoorden, Oskar Klein Centre, Stockholm University.
CMB polarisation with SPIDER

Yuanyuan Zhang, Fermilab.

The Evolving abundance of cluster red sequence galaxies from redshift 0.1 to 1.05

Xinyi Chen, University of Michigan.

Galaxy Cluster Counts: Comparing Multi-wavelength Samples and Simulations

22

Cosmic Acceleration, Dark Energy, and Modified Gravity
Maxim Eingorn, North Carolina Central University, CREST and NASA Research Centers.
All-scale cosmological perturbations and screening of gravity in inhomogeneous Universe

Eugene Tatum, Independent Researcher.
FLAT SPACE QUANTUM COSMOLOGY

Viraj Sanghai, Queen Mary University of London.

Relativistic cosmological modeling with non-linear structures

Taketo Ariki, Nagoya University.

Vacuum and Negative-Mass States of the Perfect Fluid

Santiago Casas, Institute for Theoretical Physics, University of Heidelberg.
Neutrino lump dynamics in growing neutrino quintessence

Babar Qureshi, LUMS, Lahore, Pakistan.

A non-perturbative analysis of the cosmological constant problem

Stephen Stopyra, Imperial College London.

Standard Model vacuum decay and non-minimal coupling

Mariana Jaber, UNAM.

Constraints on a Steep Equation of State for Dark Energy

Pavel Motloch, University of Chicago.

Perturbations around cosmological solutions of dRGT massive gravity

Daniel Shafer, Johns Hopkins University.

Testing Lambda-CDM at the lowest redshifts with SN Ia and galaxy peculiar velocities

Dark Matter and Other Relics
Ben Broerman, Queen’s University.

Status of the DEAP-3600 Dark Matter Search Experiment

Mohammadreza Zakeri, University of California, Riverside.
Asymmetric Reheating of the Dark and Visible Sectors

Jennings Deskins, Case Western Reserve University.

Numerical Simulations of Binary Pulsars in Galileon Theories

Jong-Chul Park, Chungnam National University.

Electro-Weak Dark Matter: Non-perturbative effect on its indirect detections

Hyerim Noh, Korea Astronomy and Space Science Institute.

Axion as a cold dark matter candidate: fully relativistic and nonlinear analysis

Alexandra Davis, the Ohio State University.

Effects of suppressed power spectra due to early Universe baryon-dark matter scattering on thesubhalo statistic of Milky Way-like galaxies.

Isaac Waldstein, The University of North Carolina at Chapel Hill.

A Quasi-Decoupled State for Dark Matter during an Early Matter-Dominated Era
23

Kayla Redmond, University of North Carolina Chapel Hill.
New Constraints on Kination Domination

Alex Kavner, University of Michigan.

Search for Low-Mass WIMPs Using CCDs at SNOLAB

Shoaib Munir, KIAS, Seoul.

Exploring the Higgs boson production in heavy chargino decays for dark matter searches at theLHC

Cosmic Probes and Future Experiments
Traci Johnson, University of Michigan.

Resolving star formation in a lensed galaxy at z=2.5

Wang Kei Wong, Carnegie Mellon University.

FILTERING INTERLOPERS FROM GALAXY SURVEYS

LIGO/Black Holes

Yukio Tomozawa, University of Michigan.

Masses of black hole merger of gravitational waves, GW150914

24

Abstracts for Plenary Talks
Monday, August 8, 2016
9:25 am Eiichiro Komatsu, MPA, Garching.

From initial conditions to structure formation, and backPrecise measurements of temperature and polarisation anisotropies of the cosmic microwave
background (CMB) taught us a remarkable story. We now think that all the structures in ourobservable universe, such as galaxies, stars, planets, and eventually ourselves, originated from tinyquantum fluctuations generated during cosmic inflation. This remarkable hypothesis has passed all
the observational tests to date, and we have learned a great deal about the physics of inflation.
The current model for the subsequent evolution of initial fluctuations due to gravity and baryonicphysics on large scales also agrees with the observational data. Turning this around, we can learn
more about inflation and the late-time evolution of the universe using the large-scale structure of
the universe. In this presentation I review the recent progress in this area of cosmology, andpresent three new results from our group over the last few years: testing symmetry of space-time
during inflation, state-of-the-art calculation of the thermal gas pressure distribution in the universeand comparison to observations, and a new way to look at the large-scale structure of the universe
using the â position-dependent power spectrumâ . But, are we totally convinced that inflation
did occur? Not yet, because extraordinary claims require extraordinary evidence. The CMB
community agrees that the next big step is to find a signature of primordial gravitational waves(GW) from inflation in the so-called B-mode polarisation of the CMB. Unlike the GW detected by
LIGO recently, which has a wavelength of thousands of kilometres, the wavelength of theprimordial GW from inflation affecting CMB is on the order of billions of light years. To this end, I
will describe our proposal for the next-generation CMB polarisation mission called “LiteBIRD”, aproposed JAXA mission with a target launch date in mid 2020.

10:10 am Rachel Rosen, Columbia University.

A Massive Gravity Status Report
The predictions of General Relativity (GR) have been confirmed to a remarkable precision in a wide
variety of tests. From the theoretical viewpoint, consistent and well-motivated modifications of GR
have been notoriously difficult to obtain. However, in recent years a conceptually simple
modification has been shown to be free of the traditional pathologies. This is the theory ofmassive gravity, in which the graviton has a small mass. In this talk I will give a general review ofmassive gravity, discuss potential observational signatures and present the current challenges facing
this theory.

11:20 am Enrico Sessolo, Nat. Centre for Nuclear Res., Warsaw.

Dark matter — What it is and how to determine its properties
I will review the present status of particle dark matter, with some attention to the case of
supersymmetry. I will focus on the interplay of collider, direct, and indirect detection searches,with prospects and challenges for detection in a reasonable time scale.

25

11:55 am Carlos Frenk, Durham University.

Searching for the identity of the dark matter in our cosmic backyard
There are competing claims that the dark matter may have already been discovered through theannihilation of cold dark matter or the decay of warm dark matter. Both hypotheses result inindistinguishable model universes on the large scales probed by temperature anisotropies in the
microwave background radiation and the clustering of galaxies. The identity of the dark matter,
however, manifests itself in the properties of small, dwarf galaxies. I will discuss predictions fromcosmological simulations for the properties of these galaxies for different types of dark matter anddiscuss whether astronomical observations can, in principle, distinguish amongst them.

26

Tuesday, August 9, 2016
9:00 am Celine Boehm, Durham University.

Dark Matter: the past and future of the field.
In the last decade, particle physics models of Dark Matter have evolved considerably. Much more
attention is given to cosmology. Many of the previous assumptions are being questioned andchallenged. I will review the new directions that the field has taken.

9:35 am Joe Lykken, Fermilab.

Whatever happened to BSM physics?

10:45 am Monica Valluri, University of Michigan.

The orbital structure of dark matter halos and implications for dark matter detection
Collisionless simulations of cosmological structure formation in the Lambda CDM paradigm resultin dark matter halos that are strongly triaxial with significant velocity anisotropy. In contrast,
simulations which include the dissipative processes and feedback associated with baryons, aresignificantly more spherical/oblate and isotropic at small radii (although the halos remain triaxial
at large radii). I will review our efforts to understand why halo shapes change in response tobaryonic condensation, and how the orbital structure of halos is affected. Since the evolution of
halo shape occurs rapidly, the orbits of both dark matter particles and halo stars reflect theformation and accretion history of the halo rather than their current shape. The detailed orbital
structure of dark matter halos with baryons has implications for two possible observable signatures
of WIMP dark matter: (a) the formation of supermassive dark stars, which could be detectable infuture JWST surveys; and (b) the ability of direct detection experiments to detect WIMP dark
matter through annual modulation. I will also briefly describe ongoing efforts to measure the shapeof the Milky Wayâ ès dark matter halo from the kinematics of field stars in the stellar halo.

11:20 am Rachel Mandelbaum, Carnegie-Mellon University.

Weak gravitational lensing cosmology: status and future prospects
First, I will review the current state of the field of weak lensing, including the beginnings of science
results from ongoing surveys: Hyper-SuprimeCam (HSC), Dark Energy Survey (DES), and the
Kilo-Degree Survey (KIDS). I will then discuss some of the challenges for science with even larger
future surveys, and the prospects for overcoming them to enable weak lensing to achieve its fullpower as a probe of our cosmological model.

11:55 am Elena Aprile, Columbia University.

Present and Future Prospects for WIMPs Direct Detection
I will review the status of the field and discuss the experiments which are likely to have the largest
impact on WIMPs direct detection before the end of this decade.

27

Wednesday, August 10, 2016
9:00 am Joshua Frieman, University of Chicago.

Early Results from the Dark Energy Survey

9:35 am Vuk MandiÊ, University of Minnesota.

First Direct Detections of Gravitational Waves
During their first observation run the Advanced LIGO gravitational-wave detectors recorded
signatures of mergers of binary black hole systems. These events mark the beginning ofgravitational-wave astrophysics, enabling a new approach to studying various astrophysicalphenomena. I will describe the LIGO detectors that enabled such break-through discoveries. I will
also discuss the events they recorded, focusing on the implications of these observations and on
expectations for future observations.

10:45 am Martina Gerbino, NORDITA.

Neutrinos in cosmology: an overview
The existence of a cosmic neutrino background (CNB) is nowadays well established. Even though
we still cannot detect it directly, we can infer its properties by investigating the impact that the
CNB has on cosmological observables, such as the cosmic microwave background (CMB) and large
scale structures (LSS). In this talk, I will present what cosmology can tell us about neutrinos,
focusing in particular on the number of relativistic species and neutrino masses. Finally, I will
discuss the effect that uncertainties on neutrino parameters could have on constraining inflationarymodels.

11:20 am Roland de Putter, Caltech.

Probing Inflation with Future Galaxy Surveys
The large-scale distribution of galaxies is a powerful probe of the physics of inflation. In particular,
scale-dependent halo bias presents a unique opportunity for galaxy surveys to study primordial
non-Gaussianity with clustering on ultra-large scales. In this talk, I will discuss how near-futuregalaxy surveys may be able to use this signal to distinguish between single- and multifield inflationand to study other fundamental properties of inflation. I will discuss both general requirements ongalaxy surveys for them to take optimal advantage of the signal, and opportunities with specificfuture surveys, including the recently proposed SPHEREx mission. While the focus will be onscale-dependent bias due to local non-Gaussianity, I will also comment on other inflationary signals
in the clustering of galaxies.

28

11:55 am Adam Riess, Johns Hopkins University.

A New Measurement of the Expansion Rate of the Universe
The Hubble constant remains one of the most important parameters in the cosmological model,
setting the size and age scales of the Universe. Present uncertainties in the cosmological model
including the nature of dark energy, the properties of neutrinos and the scale of departures fromflat geometry can be constrained by measurements of the Hubble constant made to higher
precision than was possible with the first generations of Hubble Telescope instruments. A
streamlined distance ladder constructed from infrared observations of Cepheids and type Ia
supernovae with ruthless attention paid to systematics now provide 2.4% precision and offer themeans to do much better. By steadily improving the precision and accuracy of the Hubble
constant, we now see evidence for significant deviations from the standard model, referred to as
LambdaCDM, and thus the exciting chance, if true, of discovering new fundamental physics suchas exotic dark energy, a new relativistic particle, or a small curvature to name a few possibilities. I
will review recent and expected progress.

29

Thursday, August 11, 2016
9:00 am Kiwoon Choi, Inst. for Basic Science, Korea.

Natural inflation and relaxion with multiple axions
Two applications of axion-like field for cosmology and particle physics, i.e. natural inflation and therelaxion solution of the weak scale hierarchy problem, both require hierarchical axion scales in theeffective theory of inflaton or relaxion. We propose a scheme (clockwork mechanism) to generate
exponentially big hierarchy among the effective axion scales, which can be realized in underlying
theory involving multiple axions.

10:10 am Takaaki Kajita, University of Tokyo.

Neutrino oscillation experiments — Discovery, status and prospects
Discovery of neutrino oscillations and the small neutrino masses have been the first experimental
hint toward our deeper understanding of elementary particles and their interactions beyond theStandard Model of particle physics. In this talk, I will review the discovery of neutrino oscillations
and the status of the neutrino oscillation studies. Finally, the future directions of neutrino
oscillation experiments will be discussed.

10:45 am John Carlstrom, University of Chicago.

Cosmology with the Cosmic Microwave BackgroundCosmic Microwave Background (CMB) measurements have driven our understanding of the
Universe, from the primordial quantum fluctuations to its present state. The CMB provides thefoundation for the CDM cosmological model, which fits all cosmological data (with someinteresting tensions). There is still a lot to learn from the CMB measurements. We are searchingfor the unique B-mode polarization that would be induced on the CMB by inflationary
gravitational waves. We are able to detect the impact of the neutrino background on the CMB,
which can be used to provide precise constraints on the number and masses of the neutrinos, aswell as constrain other light relics. We are untangling the correlations in the CMB induced bygravitational lensing to make maps of all the mass in the universe. We are measuring thescattering of the CMB by ionized structures, the Sunyaev-Zelâ èdovich effects, to detect clustersof galaxies and soon to map the momentum of the universe in addition to its density. This talkwill review the present status and the ambitious advances planned for the next decade, including inparticular those with the next generation ground-based experiment, CMB-S4.

30

Friday, August 12, 2016
11:00 am Alessandra Buonanno, Max Planck Inst.of Grav. Physics.

What did we learn from LIGO first black holes?
The detection by LIGO of GW150914 and GW151226 mark the beginning of a new era in physics
and astrophysics. I will review theoretical work that paved the way to observe suchgravitational-wave signals and discuss the results of the discovery focusing on its gravitational,
astrophysical and fundamental physics aspects.

11:35 am Malcolm Perry, Cambridge University.

The Black Hole Paradox Revisited: Soft Black Hole Hair
I discuss the black hole paradox and show how soft black hole hair provides some insight into blackhole physics. Whilst not a solution to the information paradox, we will show that soft hair provides
a means to escape the usual reasoning that leads to the paradox without the introduction of new
physics. We speculate on how the paradox might be resolved.

2:00 pm Pierre Sikivie, University of Florida.

Axion Dark Matter
The axion provides a solution to the Strong CP Problem of the Standard Model of elementary
particles and is a cold dark matter candidate as well. I’ll briefly review the limits on the axion fromparticle physics, stellar evolution and cosmology. I’ll describe the ongoing axion searches andrecently proposed methods that make possible the search for axion dark matter over most of theplausible axion mass range. Finally, I’ll discuss the Bose-Einstein condensation of dark matteraxions and the implications thereof for observation.

2:35 pm Cora Dvorkin, Harvard University.

Traces of the Early Universe in the CMB and the Large-Scale Structure
Cosmological observations have provided us with answers to age-old questions, involving the age,geometry, and composition of the universe. However, there are profound questions that still remainunanswered. In this talk, I will describe ongoing efforts to shed light on some of these questions.
The origin of the small anisotropies that later grew into the stars and galaxies that we see today is
still unknown. However, the nature of the anisotropies in the Cosmic Microwave Background(CMB) provides strong evidence that they were generated long before the CMB radiation had its
last interaction with ordinary matter. In this talk, I will explain how we can use measurements of
the CMB and the large-scale structure of the universe to reconstruct the detailed physics of muchearlier epochs, when the universe was only a tiny fraction of a second old.

3:10 pm Andrei Linde, Stanford University.

Inflation, dark energy, and SUSY breaking
I will give an overview of the present status of inflationary cosmology, and describe a solution of
the problem of initial conditions for the models favored by Planck. Then I will concentrate on the
recent generation of inflationary models in supergravity which can simultaneously describe inflation,
dark energy, and supersymmetry breaking.

31

Abstracts for Parallel Sessions
Monday, August 8, 2016
CMB/LARGE SCALE STRUCTURE.
2-3:30 pm Bjoern Soergel, Institute of Astronomy, University of Cambridge.

Detection of the kinematic Sunyaev-Zeldovich effect with DES Year 1 and SPT
The kinematic Sunyaev-Zel’dovich effect (kSZ) is a Doppler shift to the CMB signal imparted by
the bulk motion of the hot gas in clusters of galaxies. Despite its small amplitude, the kSZ signal
can be isolated using a differential statistic which probes the mean pairwise velocity of galaxy
clusters. This pairwise kSZ signal is sensitive to a combination of cosmology and the baryonicphysics of galaxy clusters, and may eventually be used to probe gravity at 100 Mpc scales. In thistalk I will present a statistically significant ( 4 sigma) detection of the pairwise kSZ signal by
combining a cluster catalogue from the first year of Dark Energy Survey (DES) data with CMB
temperature maps from the South Pole Telescope (SPT). This measurement is the first evidenceof the kSZ using cluster redshifts derived from photometric data, and one of the first science
results from the first year of DES data.

Sebastian Bocquet, Argonne National Laboratory.

The Growth of Cosmic Structure Measured with Galaxy Clusters in the South Pole
Telescope SPT-SZ Survey
We discuss constraints on the growth rate of cosmic structure obtained using galaxy clusters fromthe 2500 deg2 SPT-SZ survey. The sample contains 377 uniformly selected cluster candidates with
Sunyaev-Zeldovich effect detection significance greater than five and redshift z > 0.25. Of these,
82 also have Chandra X-ray data, and 101 have galaxy velocity dispersions measurements that areused for calibrating the mass-observable relation.
We assume a flat CDM background cosmology with the additional degree of freedom , describing
the growth rate. Using our cluster data set with H0 and BBN priors we constrain and obtain
results that are in agreement with the prediction by General Relativity. At this point, I will discuss
the impact of the choice of the different mass calibrators on cosmological and astrophysical results.
Adding cosmic microwave background anisotropy data further improves these constraints by precise
measurements of the background cosmology, and through the impact of on the integrated
Sachs-Wolfe-effect. Additionally allowing for the dark energy equation of state parameter to vary,
we simultaneously constrain the growth and expansion histories of the Universe. We find notevidence for departure from the CDM model.
Measuring the amplitude of the matter power spectrum at four redshifts in the range
0.25 < z < 1.7 further confirms the agreement with the concordance model. i will conclude thistalk outlying the path forward for measuring cosmic growth with current and future cluster data
sets.

32

Carles Sánchez, IFAE Barcelona.

Weak Gravitational Lensing in the Dark Energy Survey
During fall 2012 the Dark Energy Survey (DES) collaboration installed and commissioned DECam,a 570 mega-pixel optical and near-infrared camera with a large 3 sq. deg. field of view, set at theprime focus of the 4-meter Blanco telescope in CTIO, Chile. Since then, DES has completed 3 ofits 5 years of observations, mapping more than 2000 sq. deg. of the southern sky tounprecedented depth.
In this talk, the current status of weak lensing results from DES will be presented. I will review thelatest and most important results from the Science Verification period of observations, including
cosmological constraints from cosmic shear, shear peaks and from the combination of galaxy
clustering and galaxy-galaxy lensing, and other recent analyses like the detection of void lensing or
the weak lensing mass calibration of galaxy clusters. Afterwards, the production and validation of
weak lensing shear catalogs with DES-Year1 observations will be summarized, and I will describe
the outlook of the key science analyses to be performed with this unique data set, namely the full
exploitation of large-scale structure and weak lensing probes through the combination of the threepossible two-point correlation functions and the advantages of including yet another two additional
measurements coming from CMB cross-correlations with the overlapping SPT and Planck data
sets. Finally, additional Y1 science cases will be described, like the first DES study of the so-calledsplashback radius around galaxy clusters, using galaxy profiles as well as weak lensing, or the
potential constraints on modified gravity theories using void lensing with this data set.

Siddharth Satpathy, Carnegie Mellon University.

Measurement of the growth rate of structure using galaxy correlation functions
We worked with the measurement of the linear growth rate of structure, f from the Sloan Digital
Sky Survey III (SDSS III) Baryon Oscillation Spectroscopic Survey (BOSS) Data Release 12(DR12). The analysis draws on the use of the Convolution Lagrangian Perturbation Theory(CLPT) with Gaussian Streaming Redshift-Space Distortions (GSRSD) to model the two point
statistics of BOSS galaxies in DR12. The BOSS-DR12 dataset includes 1,198,006 galaxies spreadover the redshift range 0.2 < z < 0.75. these galaxy samples are categorized in three redshift bins.
using clpt-gsrsd, our group was able to report one of the first measurements of f ‡8 from the
combined sample of the three redshift bins. we find f ‡8 = 0.430 ± 0.054 at zef f = 0.38,
f ‡8 = 0.452 ± 0.057 at zef f = 0.51 and f ‡8 = 0.457 ± 0.052 at zef f = 0.61. our results are
consistent with the predictions of planck ⁄cdm-gr. also, our results are combined with bao only
results to provide constraints on the growth rates of structure in the universe at different redshifts
and thereby serve as a useful probe which can help to distinguish between a model of the universe
based on dark energy and models based on modified theories of gravity.

33

Juliana Kwan, The University of Pennsylvania.

Cosmology from large scale galaxy clustering and galaxy-galaxy lensing with Dark
Energy Survey Science Verification data
We present cosmological constraints from the Dark Energy Survey (DES) using a combined
analysis of angular clustering of red galaxies and their cross-correlation with weak gravitational
lensing of background galaxies. We use a 139 square degree contiguous patch of DES data fromthe Science Verification (SV) period of observations. Using large scale measurements, we constrain
the matter density of the Universe as m = 0.31 ± 0.09 and the clustering amplitude of the matter
power spectrum as ‡8 = 0.74 ± 0.13 after marginalizing over seven nuisance parameters and three
additional cosmological parameters. This translates into S8 = ‡8 ( m /0.3)0.16 = 0.74 ± 0.12 forour fiducial lens redshift bin at 0.35 < z < 0.5, while s8 = 0.78 ± 0.09 using two bins over therange 0.2 < z < 0.5. we study the robustness of the results under changes in the data vectors,
modelling and systematics treatment, including photometric redshift and shear calibration
uncertainties, and find consistency in the derived cosmological parameters. we show that our
results are consistent with previous cosmological analyses from des and other data sets andconclude with a joint analysis of des angular clustering and galaxy-galaxy lensing with planck cmb
data, baryon accoustic oscillations and supernova type ia measurements.

Ema Dimastrogiovanni, ASU.

Testing early Universe physics with upcoming observations
Cosmology has seen tremendous progress thanks to precision measurements and is bound to
greatly benefit from upcoming Large Scale Structure and Cosmic Microwave Background data. I
will point out a number of interesting directions. In particular, I discuss how the microphysics ofinflation may be tested in galaxy surveys through fossil signatures originating from squeezed
primordial correlations. I further elaborate on the constraining power of CMB spectral distortions
on small-scale cosmological fluctuations and on particle decays in the very early Universe inrelation to reheating.

4-5:30 pm Kevin Huffenberger, Florida State University.

Are there localized B-mode dust foregrounds in the BICEP/Keck field?
Rotti & Huffenberger (2016) demonstrated that isotropy violation tests can be used to assess thelevel of foreground contamination to the Cosmic Microwave Background polarization. The first
application of this method to Planck 353 GHz B-mode polarization data indicated a potential
foreground source in the BICEP/Keck survey field. Here we look closer, optimally combining maps
derived from auto- and cross-correlations to make a foreground power map with higher signal tonoise, and discuss the significance of of foregrounds in light of these refinements. We explore
similar analysis at other frequencies.

34

Jessica Muir, University of Michigan.

Integrated Sachs-Wolfe signal reconstruction using galaxy surveys
The Integrated Sachs-Wolfe (ISW) effect is a large-angle modulation of the cosmic microwave
background (CMB), generated when CMB photons traverse evolving potential wells associatedwith large scale structure (LSS). Recent efforts have been made to reconstruct maps of the ISW
signal using galaxy distributions, but there has been only limited investigation into how survey
systematics affect their reliability. Using simulated maps, we study the impact of galaxy survey
properties and uncertainties on the accuracy of reconstructed ISW signal. We find that systematics
associated with modeling the distribution of galaxies along the line of sight have a relatively minor
impact on reconstruction quality, but that direction-dependent calibration errors can be very
harmful. Specifically, we find that in order to avoid significant degradation of our quality statistics,
direction-dependent number density fluctuations due to systematics must be controlled so that
their variance is smaller than 1e6 (which corresponds to a 0.1% calibration). Additionally, we
explore the implications of our results for attempts to use reconstructed ISW maps to comment on
the origins of large-angle CMB alignments.

Arya Farahi, University of Michigan.

Forward modeling of galaxy clusters
Relating observations of cluster galaxies or the gas component to the total mass of the system is a
key challenge in the current cluster cosmology community. In Evrard et al. (2014), we develop a
convenient and powerful mathematical framework for modeling counts and conditional statistics ina space of multiple observable properties and total mass. The model make explicit how counts andscaling relations are sensitive to covariance between pairs of observable properties. In the first partof this talk, I discuss a forward likelihood model to constrain the scaling relation properties,
including covariance, of a cluster sample using a cosmological mass function prior. I then present
results of this method applied to multi-wavelength data from the LoCuSS survey sample. A related
challenge for cosmological analysis of cluster counts, is good understanding of the systematics andthe selection function of survey. Cosmological N-body simulations can be thought of as a way tocharacterise systematics and the selection of given survey. We have developed a flexible simulation
method designed to enable testing of X-ray survey selection, and are applying this approach to
10,000 deg2 synthetic sky simulations (Farahi et al. (in prep)). For the second part, we discuss
lessons we learned so far and the potential prospects for future analysis, like the interesting andobservationally unconfirmed strong anti-correlation between galaxies and hot gas inside clusters(Wu et al. 2015).

35

Joyce Byun, University of Sussex.

Recovering information beyond the power spectrum of large-scale structure
Future large-scale structure surveys will provide a wealth of new data and make higher-order
statistics beyond the power spectrum, such as the bispectrum, more competitive for constraining
galaxy clustering and bias, the standard LCDM cosmology, and many of its possible extensions,
including non-Gaussianity from inflation. However, given the complexity of measuring the fullbispectrum, it may be possible to use recently devised alternative statistics, such as the line
correlation function and position-dependent power spectrum, to recover information encoded in
the bispectrum while avoiding a full bispectrum analysis. We use Fisher forecasts to quantify how
much of the information encoded in the matter power spectrum and bispectrum can be recovered
using these alternate statistics to constrain the concordance cosmology, and we also compare
Fisher constraints using analytic (diagonal) covariance matrices vs covariance matrices from
N-body simulations to assess the impact of non-linear clustering on the resulting degradation of
constraints. Weighing the relative constraining power of these competing bispectrum measures willshed more light on the complementarity of these observables and inform more efficient, robust
ways of analyzing future data sets.

Masato Shirasaki, National Astrnomical Observatory of Japan.

Covariance of galaxy-galaxy lensing: Jackknife vs. Mock
Galaxy-galaxy lensing (GGL) provides a statistical method to probe the cross correlation between
matter and a given foreground object such as galaxy and cluster of galaxies. The signal of GGL on
large scale would be determined by clustering of neighboring halos, which contains richcosmological information. In practice, the error of GGL signal on large scale is evaluated with aninternal method so-called jackknife method. In this talk, we focus on how accurate GGL
covariances jackknife method would provide. We utilize a set of full-sky simulations to create
realistic mock catalogs of foreground/background galaxies found in Sloan Digital Sky Survey(SDSS). Then, we perform GGL analysis in the same way as the real data set, and compare of
GGL signals and jackknife covariance with mock and real data. Our mock catalog can reproduce
both signals and jackknife covariances measured in the case of SDSS. We also find that jackknife
covariance tends to overestimate the underlying covariance of GGL on large scale of 10 Mpc. We
will discuss the reason why jackknife estimates would be invalid on large scale. Some applicationsof our mock catalogs to estimate GGL covariances willbe presented.

36

Jonathan Braden, University College London.

Constraining cosmological ultra-large scale structure using numerical relativity
Although the local universe is well described by a homogeneous and isotropic cosmological modelwith an early stage of inflation, theoretical considerations suggest that our observable universe may
be embedded within a much larger landscape of ultra-large scale superhorizon density fluctuations.
If present, this superhorizon complexity encodes information on both the initial conditions for anddynamics of inflation, which themselves depend on the microphysical laws governing our universe.
This provides an interesting framework to investigate "anomalies” in cosmological data, as well as
to constrain models of fundamental physics. It is therefore of great interest to investigate theeffects of this superhorizon structure on local observables. Using planar symmetric numerical
relativity simulations, we investigate the ultra-large scale structure arising from superhorizon
fluctuations present at the beginning of inflation. We focus specifically on the signature in the
CMB quadrupole, the Grischuk-Zel’dovich effect, although our framework is easily generalised toinclude additional correlated anomalies. Due to the gravitational nonlinearities, we find thecontribution of the superhorizon fluctuations to the local quadrupole becomes increasingly
non-Gaussian as the amplitude of the initial fluctuations is increased. This superhorizon
contribution is combined with the usual Gaussian contribution generated by the inflationary phaseto produce the observed quadrupole. We find the non-Gaussianity induced by the gravitational
nonlinearities significantly alters the predictions of the observed CMB quadrupole power relative tothe case of Gaussian superhorizon fluctuations. In a wide range of inflationary models, this in turnsignificantly alters inferences about the scale of approximate homogeneity and our ability toconstrain the initial fluctuation amplitude.

DARK ENERGY.
2-3:30 pm Elise Jennings, Fermilab.

Cosmological constraints from Supernovae using Approximate Bayesian Analysis
Approximate Bayesian Analysis is a new sampling method where cosmological parameter inference
is done without any likelihood assumptions by full forward modeling of the data. This sampling
procedure requires a complete simulation to be run at every proposed point in parameter space
and then compared with the data using a suitable metric.
This method allows us to avoid assuming anything about the likelihood which is important in cases
where the distribution for the data is intractable e.g. multimodal or non-Gaussian. Covariances
between parameters and systematics are naturally included in the simulation, and marginalized
over, which avoids the need to estimate the covariance matrix with the same precision as
demanded by standard MCMC methods.
We shall present our new method as applied to a mock DES supernovae sample using the SNANA
simulation code and present some preliminary results showing the impact of systematics on darkenergy parameter constraints.

37

Takahiro Hayashinaka, RESCEU, university of Tokyo.

Fermionic Schwinger Effect and Induced Current in de Sitter spacetime
We explore a response of inflationary universe to background electric field using spinor QED in
1+3 dimensional de Sitter spacetime. We analytically calculate the vacuum expectation value ofthe spinor current which is induced by the produced particles in the electric field. The
renormalization is performed with the adiabatic subtraction scheme. We find that the current
becomes negative, namely it flows in the direction opposite to the electric field, if the electric field
is weaker than a certain threshold value depending on the fermion mass, which is also known tohappen in the case of scalar charged particles in 1+3 de Sitter spacetime. Contrary to the scalarcase, however, the IR hyperconductivity is absent in the spinor case.

Sebastian Zell, Max Planck Institute for Physics, Fhringer Ring 6, 80805 Munich, Germany.

On the substructure of the cosmological constant
We investigate if we can equip the cosmological constant with a substructure by viewing de Sitter
spacetime as the classical expectation value of a multi-graviton state. For small times, we are able
to define the notion of a bound-state graviton, as opposed to an asymptotically free one.
Subsequently, we construct a quantum state with the classical metric as expectation value. The
rest energy of the bound state gravitons matches the classical energy associated with thecosmological constant.
In this fully-quantum picture, we calculate redshift as the stimulated emission of a graviton. An
external particle loses energy because it deposits gravitons in the bound state. Similarly, particle
production in a de Sitter background no longer happens in vacuum, but arises as a scattering
process. It is caused by the decay of bound-state gravitons.
In contrast to the semi-classical treatment, a crucial novelty of this approach is that it naturally
predicts the back-reaction of these processes on the metric. Since the number of gravitons changes
during scattering, the bound state starts to evolve. This leads to quantum corrections of thecorresponding rates. More importantly, we conclude that the classical metric ceases to be valid
after a finite time.
This point of view fundamentally changes the question about the naturalness of the cosmologicalconstant. Its smallness is required to ensure that the description by a classical metric does notbreak down on any observable time scale.
Based on G. Dvali, C. Gomez and S. Zell, in preparation

Janina Renk, Stockholm Unversity.

Gravity at the horizon: testing gravity with relativistic effects in large scale structure
observables
Upcoming galaxy surveys will map out new regimes of our universe in the next decades. With
these data we can test gravity on scales near the horizon by studying the signatures of modified
gravity models on large scale structure observables. I will address the impact of consistentmodifications of gravity on the largest observable scales, focusing on relativistic effects in galaxy
number counts and the cross-correlation between the matter LSS distribution and the CMB. As an
example for scalar-tensor theories encoded in the Horndeski Lagrangian, self-accelerating Covariant
Galileons and parameterizations based on the effective field theory of dark energy are considered.
Especially effects which involve integrals along the line of sight (lensing convergence, time delay
and the ISW effect) can be considerably modified, and even lead to deviations of order 1000%
from General Relativity. The ISW effect is isolated using the cross-correlation between LSS and
CMB temperature anisotropies to constrain the considered models with current data. Forthcoming
large-volume galaxy surveys using multiple-tracers will search for all these effects, opening a new
window to probe gravity and cosmic acceleration at the largest scales available in our universe.

38

Jounghun Lee, Seoul National University.

A Bound Violation on the Galaxy Group Scale: The Turn Around Radius of NGC 5353/4
as a Test of Gravity
The following abstract is extracted from Lee et al. (2015, Astrophys.J. 815, 43): The firstobservational evidence for the violation of the maximum turn-around radius on the galaxy groupscale is presented. The NGC 5353/4 group is chosen as an ideal target for our investigation of thebound-violation because of its proximity, low-density environment, optimal mass scale, andexistence of a nearby thin straight filament. Using the observational data on the line-of-sightvelocities and three-dimensional distances of the filament galaxies located in the bound zone of the
NGC 5353/4 group, we construct their radial velocity profile as a function of separation distancefrom the group center and then compare it to the analytic formula obtained empirically by Falco etal. (2014) to find the best-fit value of an adjustable parameter with the help of the maximum
likelihood method. The turn-around radius of NGC 5353/4 is determined to be the separation
distance where the adjusted analytic formula for the radial velocity profile yields zero. The
estimated turn-around radius of NGC 5353/4 turns out to substantially exceed the upper limit
predicted by the spherical model based on the LambdaCDM cosmology. Even when the restrictive
condition of spherical symmetry is released, the estimated value is found to be only marginallyconsistent with the LambdaCDM expectation.

Shuntaro Mizuno, Waseda University.

Vainshtein mechanism in massive gravity nonlinear sigma models
We study the stability of the Vainshtein screening of the bigravity based on the effective action
inside the Vainshtein radius. The effective action is obtained by taking the 2 decoupling limit
around a curved spacetime. First we show that the Vainshtein screening solution is generally
unstable when the vector graviton is not excited. Then we explicitly show that the static andspherically symmetric solution suffers from a ghost and/or a gradient instability for any parametersof the theory. This instability suggests that the nonlinear excitation of the scalar graviton is not
sufficient to obtain a successful Vainshtein screening in bigravity.

4-5:30 pm Amol Upadhye, UW-Madison.

Redshift-space distortions constrain massive neutrinos and evolving dark energy
The amplitude and shape of the redshift-space matter power spectrum contain a wealth of
information about fundamental physics and the cosmological parameters. I begin by developing a
non-linear perturbative model of the redshift-space power spectrum using theTime-Renormalization Group (Time-RG) approach, designed to accommodate the scale-dependent
growth in massive neutrino cosmologies. Through comparison with a suite of high-resolution
N-body simulations, I show that redshift-space Time-RG perturbation theory accurately predicts
the power spectrum over a large range of scales and for a diverse set of cosmological models,
including those with massive neutrinos and rapidly-varying dark energy equations of state. Finally,
I apply Time-RG to the redshift-space power spectrum from BOSS Data Release 11 in conjunction
with Planck cosmic microwave background data. I present constraints on the cosmologicalparameters and discuss their dependence on the modeling of scale-dependent bias.

39

Frank Koennig, ITP, University of Heidelberg.

A spectre is haunting the cosmos: Quantum stability of massive gravity with ghosts
Many theories of modified gravity with higher order derivatives are usually ignored because ofserious problems that appear due to an additional ghost degree of freedom. Most dangerously, itcauses an immediate decay of the vacuum. However, breaking Lorentz invariance can cure suchabominable behavior. By analyzing a model that describes a massive graviton together with aremaining Boulware-Deser ghost mode we show that even ghostly theories of modified gravity canyield models that are viable at both classical and quantum levels and, therefore, they should not
generally be ruled out. Furthermore, we identify the most dangerous quantum scattering processthat has the main impact on the decay time and find differences to simple theories that only
describe an ordinary scalar field and a ghost. Additionally, constraints on the parameters of thetheory including some upper bounds on the Lorentz-breaking cutoff scale are presented. In
particular, for a simple theory of massive gravity we find that a Lorentz violation needs to occur
below 200 eV, which still agrees with observations. Finally, we discuss the relevance to othertheories of modified gravity.

Mark Hertzberg, Tufts University.

Gravitation, Quantum Consistency, and Causality
General relativity was historically introduced as arising from various principles, such as equivalenceprinciple and general co-ordinate invariance. From the modern point of view, we view it as simply
a theory of massless spin 2 particles. Modifications of general relativity are often motivated bydark energy, inflation, etc. In this talk, I begin by reviewing this modern perspective. I then point
out quantum mechanical inconsistencies in some of the most popular ways to modify generalrelativity, namely the F(R) scalar-tensor theories. Then I consider a new class of spin 2 theories
that involve higher derivatives, and explain that they fail due to causality violation. This goes
towards deriving general relativity from very fundamental principles.

Stefano Anselmi, Case Western Reserve University.

Quasidilaton massive gravity faces cosmological constraints
The mysterious acceleration of the Universe may be successfully explained by a modification of thestandard gravity paradigm. In this regard theories that give mass to the graviton result being very
promising candidates. It is thus mandatory to study the cosmological phenomenology of them toallow an accurate comparison with present and future observational data. In this context I will
focus on the cosmology of quasidilaton massive gravity, a theory with three additional parameters
w.r.t LCDM. Interestingly, already at the background level, it shows a non-trivial behavior,
enforcing a fine-tuning of the fundamental parameters of the theory. The evolution of gravity
waves reveals that the mass of the graviton may be negative in the past while today is always
larger than the Hubble parameter. An effect that may be observed by future surveys. The analysis
I will present is a first step toward the investigation of the more stable extended quasidilaton
massive gravity.

Matteo Fasiello, Stanford University.

LSS probes for Dark Energy & Modified Gravity
The perturbative treatment of LSS dynamics, especially in its effective theory realization, can welldescribe the quasi-linear regime. I will elaborate on recent progress towards including a dynamical
dark energy or a modified gravity component in this framework.

40

Shuang-Yong Zhou, Case Western Reserve University.

The 2 limit of dRGT massive gravity
dRGT massive gravity is a candidate for dark energy. From the EFT point of view, the model isusually associated with a strong coupling scale at 3 (10≠13 eV). With de Rham and Tolley, weshow that, by including non-trivial effects from the Stueckelberg modes, one can push the strong
coupling scale to much higher values, close to 2 (meV). About these non-trivial vacua, thepeculiar linear vDVZ-discontinuity is also absent. For generic parameters of the theory and genericvacua for the Stueckelberg fields, the 2 -decoupling limit of the theory is well-behaved and free ofany ghost or gradient-like instabilities. This means that these 2 backgrounds are theoreticallywell-controlled, can easily recover the phenomenological successes of General Relativity and are
well suited to explain the dark energy problem.

PRIMORDIAL/INFLATION.
2-3:30 pm Peter Adshead, University of Illinois at Urbana-Champaign.

Asymmetric reheating and chilly dark sectors
In a broad class of theories, the relic abundance of dark matter is determined by interactions
internal to a thermalized dark sector, with no direct involvement of the Standard Model. These
theories raise an immediate cosmological question: how was the dark sector initially populated in
the early universe? I will discuss one possibility, asymmetric reheating, which can populate athermal dark sector that never reaches thermal equilibrium with the SM.

Mustafa Amin, Rice University.

From Wires to Cosmology: A statistical approach to particle production during inflation
and reheating
Current observations provide precise but limited information about inflation and reheating.
Theoretical considerations, however, suggest that the early universe might be filled with a large
number of interacting fields with unknown interactions. How can we quantitatively understandparticle production and the dynamics of perturbations during inflation and reheating in such
scenarios and when only limited constraints are available from observations? Based on a precise
mapping between particle production in cosmology to resistivity in disordered, quasi
one-dimensional wires, I will provide a statistical framework to resolve such seemingly intractablecalculations. A number of phenomenon in disordered wires find an analogue in particle production.
For example, Anderson localization in quasi one-dimensional wires can be directly mapped toexponential particle production in the early universe. In this talk, I will present our generalframework (arXiv: 1512.02637), and discuss ongoing calculations of observables from inflation andreheating.

41

Damien Easson, Arizona State University.

Stability of cosmological models with unusual scalar fluids
I will discuss cosmological solutions in standard Einstein gravity sourced by non-standard,
non-canonical scalar field fluids. Examples of such fluids include k-essence, DBI, Galileon fields,
Horndeski models and the new oscillatory models recently proposed by Nobel Laureate Wilczek et
al. I will focus on the stability of these fluids emphasizing the common occurrence of negative
kinetic energy degrees of freedom (ghosts),gradient instabilities (imaginary sound speed),superluminal propagating modes and singularities and the physical conditions required for such
pathologies to be avoided. The analysis is relevant for a variety of popular cosmological scenarios
including K-inflation, Galilean Genesis super-inflation, and the G-bounce models.

Tommi Tenkanen, University of Helsinki.

A Strong Electroweak Phase Transition from the Inflaton Field
We study a singlet scalar extension of the Standard Model. The singlet scalar is coupled
non-minimally to gravity and assumed to drive inflation, and also couple sufficiently strongly with
the SM Higgs field in order to provide for a strong first order electroweak phase transition.
Requiring the model to describe inflation successfully, be compatible with the LHC data and yielda strong first order electroweak phase transition, we identify for the first time the regions of theparameter space where the model is viable. We also include a singlet fermion with scalar coupling
to the singlet scalar to probe the sensitivity of the constraints on the additional degrees of freedom
and their couplings in the singlet sector.

Scott Watson, Syracuse University.

The End of Inflation
It is typically assumed that inflation will end providing a "hot Big Bang", where (at least)
Standard Model fields and dark matter will eventually be populated. However, little is known
about the end of inflation, and prior to BBN direct probes on the cosmic history are elusive. Yet,
collider probes and dark matter detection experiments continue to search for physics Beyond theStandard Model at precisely these scales. Moreover, the process by which the inflationary sectortransfers its energy to the Standard Model and other hidden sectors can be quite involved. This
process can be non-perturbative, chaotic, can exhibit turbulence, and significantly alter the
expansion history – presenting a number of theoretical challenges. I will review recent progress inboth theory and observations.

Gonzalo Palma, Departamento de Fsica, FCFM, Universidad de Chile.

On the role of light fields during inflation
A large coupling between curvature perturbations and light fields can enhance the super-horizon
growth of curvature perturbations, alleviating the tension that exists a priori between multi-fieldmodels of inflation and the statistical properties of the CMB. In this paper we study this situation
for the case where the additional light fields stay exactly massless during inflation, which ispossible thanks a non-trivial shift symmetry that may appear at quadratic order in the Lagrangianof fluctuations, involving the simultaneous transformation of curvature perturbations and themassless field. The spectra that result from this situation is such that the power spectrum of
isocurvature modes is suppressed in comparison to the power spectrum of curvature perturbations.
In addition, the tensor to scalar ratio is predicted to be generically very suppressed. We offer
concrete multi-field scenarios where this class of dynamics is realized and in which the coupling
between the inflaton and the massless fields are purely determined by the geometry of the
field-space manifold. Interestingly, these effects are predicted to be large only in the region where
the effective field theory for fluctuations can be trusted.

42

4-5:30 pm Ivonne Zavala, Swansea University.

Axion Inflation in String Theory and Primordial Gravitational Waves
An attractive candidate for the inflaton is an axion slowly rolling down a flat potential protected bya perturbative shift symmetry. Realisations of this idea within large field, natural and monomial
inflation have been disfavoured by observations and are difficult to embed in string theory. I will
discuss the implications and prospects of these type of models for primordial gravity waves instring inflation. I will then show how subleading, but significant non-perturbative corrections to theaxion potential can help bringing single-field natural and monomial inflation in UV complete
theories like string theory, back into the favour of current observations, with distinctive signatures.

Shuichiro Yokoyama, Department of Physics, Rikkyo University, Japan.

Revisiting matter isocurvature fluctuations in the curvaton scenario
We investigate dark matter isocurvature perturbations in the curvaton scenario in detail,analytically and also numerically. In analytic estimation, we employ the delta-N formalism, and use
the approximation that dark matter, which is initially in thermal equilibrium, is instantaneously
decoupled from the thermal equilibrium. By comparing such approximation with numerical results,
we find that we need to take into account the effect of the dilute gas produced from the decay ofthe curvaton. We explicitly show that even if the freeze-out of the dark matter occurs before thecomplete decay of the curvaton, dark matter isocurvature perturbations could be much suppressed
when the freeze-out occurs deep in the curvaton-dominated Universe. We also discuss theimplication of the above result on the constraint on model parameters in the scenario where thedark matter was produced in the curvaton scenario, and find that the allowed region in theparameter space is significantly enlarged by taking the dilute gas effect into account.

Mohammad Hossein Namjoo, Center for Astrophysics, Harvard.

Probing the Primordial Universe using Massive Fields
Inflation is the leading paradigm of the early universe cosmology. There are however several
alternative-to-inflation scenarios which are consistent with currently available observational data,
making them indistinguishable from inflation. In this talk I will discuss how one can probe thephysics (i.e. mass spectroscopy of the particles) of the early universe by studying specific featureson cosmological observables. Furthermore, I will show that the fingerprints of the presence ofmassive fields during early universe (i.e. the so called standard clocks) can reveal the time
evolution of the universe at that era, thus discriminating between different scenarios. Future
theoretical and observational prospects of the primordial standard clocks will also be discussed.

Jinn-Ouk Gong, Asia Pacific Center for Theoretical Physics.

Consistency relation and inflaton redefinition in the delta-N formalism
We compute for general single-field inflation the intrinsic non-Gaussianity due to theself-interactions of the inflaton field in the squeezed limit. We recover the consistency relation in
the context of the delta-N formalism, and argue that there is a particular field redefinition thatmakes the intrinsic non-Gaussianity vanishing, thus improving the estimate of the local
non-Gaussianity using the delta-N formalism.

43Kaloian Lozanov, Institute of Astronomy, University of Cambridge, UK.

The Equation of State and Duration to Radiation Domination After Inflation
We calculate particle production during inflation and in the early stages of reheating after inflationin models with a charged scalar field coupled to Abelian and non-Abelian gauge fields. A detailed
analysis of the power spectra of primordial electric fields, magnetic fields and charge fluctuations at
the end of inflation and preheating is provided. We carefully account for the Gauss constraints
during inflation and preheating, and clarify the role of the longitudinal components of the electricfield. We calculate the timescale for the back-reaction of the produced gauge fields on the inflaton
condensate, marking the onset of non-linear evolution of the fields. We provide a prescription for
initial conditions for lattice simulations necessary to capture the subsequent nonlinear dynamics.
On the observational side, we find that the primordial magnetic fields generated are too small to
explain the origin of magnetic fields on galactic scales and the charge fluctuations are well within
observational bounds for the models considered in this paper.

Jason Evans, Korea Institute for Advanced Study.

Naturalizing Supersymmetry with a Two-Field Relaxion Mechanism
We present a supersymmetric version of a two-field relaxion model that naturalizes tuned versionsof supersymmetry. This arises from a relaxion mechanism that does not depend on QCD dynamics
and where the relaxion potential barrier height is controlled by a second axion-like field. During
the cosmological evolution, the relaxion rolls with a nonzero value that breaks supersymmetry andscans the soft supersymmetric mass terms. Electroweak symmetry is broken after the soft masses
become of order the supersymmetric Higgs mass term and causes the relaxion to stop rolling forsuperpartner masses up to 109 GeV. This can explain the tuning in supersymmetric models,
including split-SUSY models, while preserving the QCD axion solution to the strong CP problem.
Furthermore, we show that the second field, of this two-field model, can be the inflaton.

44

Tuesday, August 9, 2016
FUTURE PROBES.
2-3:30 Benjamin Saliwanchik, University of KwaZulu-Natal.

Design and Scientific Forecast of the Hydrogen Intensity and Real-time Analysis
eXpermiment (HIRAX)The Hydrogen Intensity and Real-time Analysis eXperiment (HIRAX) is a planned radio telescopearray that will consist of 1000 close packed 6 m dishes that will be deployed in South Africa.
HIRAX will survey the majority of the southern sky to measure baryon acoustic oscillations (BAO)
using the 21 cm hyperfine transition of neutral hydrogen. The telescope is optimized to measure
the 100 h≠ 1 Mpc BAO scale by measuring integrated emission from many neutral hydrogensources (intensity mapping). It will operate between 400-800 MHz in 1024 frequency bins,
corresponding to a redshift range of 0.8 < z < 2.5 and a minimum deltaz/z of 0.003. bymeasuring the bao length scale as a function of redshift, hirax will chart the expansion history of
the universe and place constraints on the dark energy equation of state. in addition to bao
cosmology, the large survey area and real-time analysis capabilities of the hirax array will make it apowerful tool for identifying pulsars and astrophysical transients such as fast radio bursts. hirax
will additionally provide an excellent platform for studying neutral hydrogen absorbers, and theextensive overlap with the large synoptic survey telescope (lsst) will enable cross-correlation studiesof radio and optical tracers of large scale structure. the testing of the first prototype hirax dish has
begun in durban, and an eight-element prototype array is scheduled for construction anddeployment at the hartebeesthoek radio astronomy observatory (hartrao) in early 2016. thispresentation describes the telescope design, current plans for deployment and calibration, andpreliminary forecasts of scientific constraints.

45

Seth Siegel, McGill University.

CHIME: A Stage IV Dark Energy Experiment
The Canadian Hydrogen Intensity Mapping Experiment (CHIME) is a radio interferometer that iscurrently being deployed at the Dominion Radio Astrophysical Observatory (DRAO) near Penticton,
British Columbia and is expected to begin observations in late 2016. It consists of four adjacentcylindrical dishes, each 100 x 20 meters, populated with a total of 1024 dual-polarization antenna
feeds sensitive to 400-800 MHz. The cylinders are stationary and oriented in the north-south
direction, forming a transit telescope that maps approximately half of the sky each day with asynthesized beam resolution of 20-40 arcminutes. CHIME will make a three-dimensional intensity
map of the 21 cm radiation from neutral hydrogen over a 600 cubic Gpc volume. This will enablea measurement of the scale of the Baryon Acoustic Oscillations (BAO) in both the angular andline-of-sight direction across the redshift range z=0.8-2.5, which will probe the angular diameter
distance versus redshift relation and time evolution of the expansion rate during the epoch whendark energy starts to dominate the energy density of the Universe. CHIME will carry out a five year
survey that is expected to yield Stage IV constraints on the dark energy equation of state. One ofthe primary challenges facing CHIME and 21 cm intensity mapping experiments in general is thatthe cosmological signal must be separated from foregrounds that are five orders of magnitude
brighter. We employ the m-mode analysis formalism combined with the Karhunen-Loeve transformto efficiently separate the 21 cm signal from the contaminating foregrounds using their respective
spectral and spatial statistics. This method requires a detailed understanding of the instrument,
including precise knowledge of the antenna primary beam patterns and time-variable complex
receiver gains. We have developed a number of calibration techniques to address theserequirements and are testing them on a smaller scale Pathfinder instrument that consists of two
cylinders, each 36 x 20 meters, populated with a total of 128 dual-polarization antenna feeds. In
this talk I will give an update on the status of CHIME, discuss calibration strategies, and present
an initial look at data from the Pathfinder, which began a two-year survey in December 2015.

Jon Gudmundsson, Oskar Klein Centre for Cosmoparticle Physics, Stockholm University.

Lessons learned from SPIDER’s first flight and implications for future ballooning andsatellite missions
SPIDER is a balloon-borne experiment designed to image the polarization of the cosmic microwave
background with the aim of constraining models of the early universe, including the inflationary
paradigm. I will examine the detector performance from SPIDER’s first flight and discuss theimplications for future ballooning and satellite missions. I will review emerging ballooning
technology and show how ballooning missions provide essential complementary to ground based
experiments.

Roland de Putter, Caltech.

Probing Inflation with Galaxy Clustering on Ultra-Large Scales
The large-scale distribution of galaxies is a powerful probe of the physics of Inflation. In this talk, I
will explain what it would take for a future galaxy survey to use galaxies as a probe of primordial
non-Gaussianity in order to distinguish between single-field and multi-field Inflation, and I will
introduce a specific proposal for such a survey, called SPHEREx. I will also revisit the prediction
for the exact level of non-Gaussianity and scale-dependent bias in single-field Inflation.

46

Caroline Heneka, NBI, University of Copenhagen.

Probing Reionization: Cross-correlation of 21-cm and Lyman-alpha fluctuations
Line intensity mapping opens up a new and exciting window for probing cosmology during the
Epoch of Reionization and at higher redshifts than previously tested by galaxy surveys. The
cross-correlation of line fluctuations like 21-cm, Lyman-alpha and H-alpha is a promising tool toprobe the IGM during the Epoch of Reionization. It enables us to track the evolution of theionisation fraction and is a measure of the average size of ionised bubbles. We simulate
Lyman-alpha, 21-cm and H-alpha line fluctuations, in order to calculate their respective power andcross-power spectra. The impact of foreground induced anisotropies on the power spectra isinvestigated by separating perpendicular and parallel Fourier modes and we test dependencies of
the cross-correlation on reionization parameters like the escape fraction, on cosmologicalparameters and on the modelling of Lyman-alpha emitters. We furthermore forecast the ability ofprobes of the Epoch of Reionization such as SPHEREx, a proposed all-sky spectroscopic survey
satellite that will also perform intensity mapping of the Lyman-alpha line, to measure thecross-correlation of 21-cm and Lyman-alpha jointly with upcoming 21-cm surveys like SKA.

Inh Jee, Max-Planck Institute for Astrophysics.

Strong Lensing Cosmography : method, predictions and measurements
One of the major ongoing efforts in cosmology is the measurement of the distance-redshift relationand constraining cosmological models from it. The most popular approaches are to use
Supernovae type Ia as standard candles, and Baryon Acoustic Oscillation as a standard ruler. I will
present a new standard ruler, strong gravitational lenses with time delay measurements, tocalculate the angular diameter distances at the cosmological scale. This is a measurement of
distances which is independent to other probes, and also an efficient way to populate the Hubble
diagram, as individual objects give a distance to the corresponding redshift. I first introduce thebasic idea behind the method and discuss the systematics. Then I introduce the constraining
power of the method using the simulated observations based on predictions for Large Synoptic
Survey Telescope, highlighting where the constraints are coming from. Finally, I present actual
measurements applied to real data.

47

CMB/LARGE SCALE STRUCTURE.
4-5:30 pm Paul Shapiro, The University of Texas at Austin.

Simulating Cosmic Reionization and Its Observable Consequences
I will summarize recent progress in modelling the epoch of reionization by large- scale simulationsof cosmic structure formation, radiative transfer and their interplay, which trace the ionization
fronts that swept across the IGM and ionized it, to predict observable signatures of this process.
Cosmic reionization by starlight from early galaxies affected their evolution, thereby impacting
reionization, itself, and imprinting the galaxies with a memory of reionization. Star formation
suppression, for example, may explain the observed underabundance of Local Group dwarfs relative
to N-body predictions for Cold Dark Matter. With this in mind, I will describe the first
fully-coupled radiation-hydrodynamical simulation of reionization and galaxy formation in the Local
Universe, in a volume large enough to model the global history of cosmic reionization and withenough resolving power to follow the formation and evolution of all the atomic-cooling galactic
halos in that volume. A representative comoving box 90 Mpc on a side was simulated from a
constrained realization of the primordial fluctuations, chosen to reproduce the present-day featuresof the Local Group, including the Milky Way and M31, and the local universe beyond, including
the Fornax and Virgo clusters. The new RAMSES-CUDATON hybrid CPU-GPU code took 11 days
to perform this simulation on the Titan supercomputer at Oak Ridge National Laboratory, with
4096-cubed N-body particles for the dark matter and 4096-cubed cells for the atomic gas andionizing radiation. The simulation is called CoDa, for "Cosmic Dawn".

Anson D’Aloisio, University of Washington.

Probing Cosmological Reionization with the High-redshift Lyman-alpha Forest
When the first galaxies emerged, 100 - 500 million years after the Big Bang, their starlight likely
reionized and heated the intergalactic hydrogen that had existed since cosmological recombination.
Much is currently unknown about this process, including what spatial structure it had, when it
started and completed, and even which sources drove it. Recent observations of high-redshiftquasars show large-scale spatial variations in the opacity of the z 5.5 intergalactic medium to
Lyman-alpha photons. These spatial variations grow rapidly with redshift, far in excess of
expectations from previous empirically motivated models. I will discuss possible explanations forthe excess, as well as what they imply about the reionization process.

Hao-Yi Wu, California Institute of Technology.

A physical model for the anisotropies of cosmic far-infrared backgroundCosmic far-infrared background (CFIRB) originates from unresolved dusty star-forming galaxies
across cosmic time. It is a powerful probe for the star formation rate (SFR) history and theconnection between dark matter and baryons. In this talk, I will interpret the measurements of
CFIRB by Planck using a physical model based on continuity equations for baryons. This model
simultaneously provides good descriptions for the CFIRB power spectra, correlation between CMB
lensing potential and CFIRB, FIR flux functions, and IR luminosity functions. I will then present
constraints on SFR-halo mass relation, galaxy bias, SFR history, and dust properties. Base on thephysical model, I will also discuss how to optimize future experiments for CFIRB as part of the
CMB Stage-IV experiments.

48

Marcelo Alvarez, Canadian Institute for Theoretical Astrophysics.

Mock LSS Surveys with the Peak Patch Approach
Large scale structure surveys contain information on the initial conditions and properties of theuniverse not otherwise available. In order to optimize the methods to extract this information, we
have developed an approach based on the peak patch picture, in which primordial fluctuations areconnected explicitly with the formation of bound objects to create mock observations. First
applications, to Sunyaev-Zel’dovich and HI intensity mapping surveys, will be presented.

Joel Meyers, CITA.

Light Relics and Next Generation CMB Observations
Ongoing and future cosmic microwave background observations will greatly improve ourmeasurement of the temperature and polarization power spectra at small angular scales. These
improvements will allow for fundamentally new insights into physics beyond the standard modeland the very early universe. I will discuss theoretical targets for CMB constraints on light relics
and the path toward reaching those goals.

Chen Heinrich, University of Chicago.

Lensing Bias to Compensated Isocurvature Perturbations
Compensated isocurvature perturbations (CIPs) are modes in which the baryon and dark matter
density fluctuations cancel. They arise in the curvaton scenario as well as some models of
baryogenesis. While they leave no observable effects on the cosmic microwave background (CMB)
at linear order, they do spatially modulate two-point CMB statistics and can be reconstructed in amanner similar to gravitational lensing. Due to the similarity between the effects of CMB lensing
and CIPs, lensing contributes nearly Gaussian random noise to the CIP estimator thatapproximately doubles the reconstruction noise power. Additionally, the cross correlation between
lensing and the integrated Sachs-Wolfe (ISW) effect generates a correlation between the CIP
estimator and the temperature field even in the absence of a correlated CIP signal. For
cosmic-variance limited temperature measurements out to multipoles l2500, subtracting a fixedlensing bias degrades the detection threshold for CIPs by a factor of 1.3, whether or not they arecorrelated with the adiabatic mode.

DARK ENERGY.
2-3:30 pm Miguel Zumalacarregui, Nordita.

New probes of gravity and cosmic acceleration
Recent advances in cosmology provide both the motivation and the data to probe gravity on thelargest scales available to observation. I will revise the landscape of gravitational theories, focusing
on modern scalar-tensor theories and their cosmological implications. Then I will present theongoing effort to test gravity in novel regimes such as the early universe, non-linear effects andultra-large scales. I will also introduce the hi_class code (www.hiclass-code.net), which is central
to this program.

49

Lucas Lombriser, University of Edinburgh.

Challenges to Self-Acceleration in Modified Gravity from Gravitational Waves andLarge-Scale Structure
Scalar-tensor modifications of gravity have long been considered as an alternative explanation forthe late-time accelerated expansion of our Universe. I will first show that a rigorous discrimination
between acceleration from modified gravity and from a cosmological constant or dark energy is notpossible with observations of the large-scale structure alone. I will then demonstrate how
gravitational-wave observations break this dark degeneracy and how the combination of the twochallenges the concept of cosmic acceleration from a genuine scalar-tensor modification of gravity.

Shahab Joudaki, Swinburne University.

KiDS+2dFLenS: Testing Gravity on Cosmic Scales with Weak Lensing and Redshift
Space Distortions
The apparent existence of "dark energy" compels us to test the laws of gravity across the scale ofthe universe in multiple ways. Only a powerful combination of two observables, gravitational
lensing and galaxy velocities, will pin down the physics of gravity. In this talk I will present new
tomographic weak lensing measurements from one of the largest existing cosmic shear surveys, theKilo Degree Survey (KiDS), accounting for key astrophysical systematics from intrinsic alignments,
baryons, and photometric redshifts. I will discuss the sensitivity of the cosmological constraints tothe astrophysical systematics, provide new bounds on extensions to the standard cosmologicalmodel, and assess the level of concordance between KiDS and Planck. I will then examine
standard cosmology and modified gravity constraints from KiDS in combination with overlapping
spectroscopic surveys, given by the 2-degree Field Lensing Survey (2dFLenS) and the Baryon
Oscillation Spectroscopic Survey (BOSS), including the full covariance between the RSD monopoleand quadrupole spectra, shear-galaxy correlation function, and shear-shear correlation functions.

Eva-Maria Mueller, Institute for Cosmology and Gravity.

BOSS DR12 Combined Sample Analysis constraints on modified gravity
I will present updated constraints on modified gravity models using the newest/upcoming BOSS
DR12 Combined Sample Analysis results in combination with other data sets. The focus is on
phenomenological models that alter the Einstein equations, introducing GM (k,z) and GL (k,z) inbins as additional parameters, as well as tensor-scalar theory inspired unifying approaches(BZ-parameterization) and f(R) models. Additionally, I will discuss forecasts for LSST and DESI
for these modified gravity models, particularly pointing out challenges due to systematic effects.

Sebastian Cespedes, DAMTP, University of Cambridge.

Modifications of the speed of gravitational waves at early times.
A speed different from one for tensor modes can arise in several contexts, such as Galileons
theories or massive gravity, nevertheless the speed is very constrained to be one by observations ofgravitational wave emission. It has been shown that in inflation a disformal transformation allows
to set the speed for tensor modes to one without making changes to the curvature power
spectrum. Here we show that this invariance does not hold when considering the CMB anisotropy
power spectrum. It turns out that the after doing the transformation there is an imprint on the
acoustic peaks and the diffusion damping. This has interesting consequences; and we explore
which others observational constraint could be imposed by employing cosmology.

50

Chi-Ting Chiang, C. N. Yang Institute for Theoretical Physics, Stony Brook University.

Fake Separate Universe: A new trick for simulating clustered quintessence cosmologies
The separate universe technique provides a way to absorb the long-wavelength matter fluctuation
into the change of background cosmology. The cosmological N-body simulations can thus beperformed in the separate universes to study how the small-scale structure formation (such as
power spectrum and halo mass function) responds to the long-wavelength perturbation. In thepresence of an additional fluid, its density fluctuation may cluster with the matter. Depending onwhether the long-wavelength matter fluctuation is below or above the sound horizon of the fluid,
the evolution of the long-wavelength matter fluctuation would be affected differently. This thus
produces two distinct separate universes, and so as the responses of the small-scale structureformation. We use the separate universe simulations with clustered dark energy to show that there
will be a new scale (sound horizon of dark energy) dependence of the matter squeezed-limit
bispectrum and the halo bias. This novel feature could potentially be useful to probe the extra
fluid such as dynamic dark energy or massive neutrinos.

DARK ENERGY/DARK MATTER.
4-5:30 pm Brian Nord, Fermilab.

DeepLensing: The Use of Deep Learning to Find Strong Lenses in the Dark Energy
SurveyStrong gravitational lenses have potential to be very powerful probes of dark energy and cosmic
structure. However, efficiently finding lenses poses a significant challenge—especially in the era oflarge-scale surveys cosmological surveys. I will present the strong lens discovery program for the
Dark Energy Survey (DES), as well as a new application of deep learning to finding lenses.
Over five observing seasons, which started in August 2013, DES will carry out a wide-field surveyof 5000 square degrees of the Southern Galactic Cap. DES has identified nearly 200 strong lensing
candidates in the first two seasons of data. We have performed spectroscopic follow-up on a
subsample of these candidates at Gemini South, confirming over a dozen new strong lenses.
I will first present the DES program, including searches and spectroscopic follow-up of galaxy-scale,cluster-scale and time-delay lensing systems. Then, I will discuss the successful search for lenses
using deep learning methods: in particular, we show that convolutional neural nets present a new
set of tools for efficiently finding lenses, including the types of configurations that will be criticalfor cosmological studies.

Joseph DeRose, Stanford University.

Simulating the Dark Energy Survey Sky
The challenges associated with simulating wide field galaxy surveys, especially those intending to
use weak lensing as a primary cosmological probe, have become pressing issues for ongoing andfuture cosmological studies. In this talk, I will describe the 100 mock skies, including galaxies,
gravitational lensing, and realistic observational errors, that have been created for the analysis of
the first year of Dark Energy Survey data. These mocks use a novel algorithm, ADDGALS, tocreate large volume galaxy catalogs to depths that are beyond the reach of typical
HOD/SHAM/SAM methods. I will describe the use of these mocks for covariance matrix
estimation, modeling of observables and systematic error analysis. To conclude I will discuss thechallenges that will be faced in upcoming years of the Dark Energy Survey as well as for future
surveys such as LSST, Euclid and WFIRST.

51

Evan Grohs, University of Michigan.

Precision big bang nucleosynthesis and neutrino cosmology
We present detailed numerical calculations related to big bang nucleosynthesis and cosmologicalneutrino physics. Specifically, we investigate how increased precision on the primordial deuterium
and helium abundances supply new constraints on the neutrino-antineutrino asymmetry,characterized as a lepton number. At previous levels of precision, the observationally-inferredhelium abundance placed an upper limit of 0.1 on the lepton number. Future precision of thehelium and deuterium measurements will lower the upper limit by an order of magnitude. To
quantitatively determine the leverage the abundances have on lepton numbers, our calculations
utilize a model consistent with the standard cosmology except for the presence of nonzero lepton
numbers. The anticipated level of precision in the abundances requires the integration of a nuclear
reaction network to determine the abundances, and the integration of a series of Boltzmann
equations to follow the out-of-equilibrium neutrino spectra. In this manner, we obtain precise
values of the abundances and other cosmological quantities such as the effective number ofneutrinos. Our work has implications for nuclear and beyond standard model physics. Such physics
could manifest itself with measurements using next generation cosmic microwave background andthirty-meter-class telescopes.

Tanja Rindler-Daller, University of Vienna.

Dark stars as progenitors of supermassive black holes in the early Universe?
Over the past years, observations of high-redshift galaxies have shown that supermassive black
holes (SMBHs) with billions of solar masses have already existed a few hundred million years after
the Big Bang. Since the timescale for traditional mechanisms of accretion onto stellar BHs is too
long, other models have been considered. These include the monolithic collapse of giant gas
clouds, or the collapse of early supermassive stars. In this talk, I will elaborate how anotherproposal, namely early dark-matter-powered stars (“dark stars”), could explain SMBHs. Early darkstars have primordial composition, but they are powered by the energy release of dark matter
self-annihilation. I will contrast previous results on the evolution of supermassive stars with ourmodels of supermassive dark stars, where we compute the latter using the state-of-the-art stellar
evolution code MESA. By following the evolution of these stars in atomic-cooling halos, using
different dark matter particle parameters, we can investigate when supermassive dark stars might
become the progenitors of SMBHs. In this talk, I will report on these and other forecasts ofsupermassive dark stars.

Jayden Newstead, Arizona State University.

Neutrino floors for non-standard direct dark matter detection scenarios
The next generation of direct dark matter detection experiments will be sensitive to coherent
scattering of solar neutrinos, providing an irreducible background to dark matter searches. While
technology may eventually be able to mitigate the effect of this background, non-standard dark
matter interactions do not necessarily exhibit a neutrino floor. In this talk I will survey examples of
non-standard dark matter interactions and demonstrate the how their discovery potential iseffected by the neutrino background.

LIGO AND BLACK HOLES.

52

2-3:30 pm Dejan Stojkovic, SUNY at Buffalo.

Quantum aspects of gravitational collapse: non-singularity and non-locality
Singularities in classical general relativity are unavoidable, but perhaps only represent the fact that
we are extrapolating our theory beyond its region of validity. We study the end stages ofgravitational collapse using the functional Schrodinger formalism to capture quantum effects in thenear singularity limit. We find that that the equations of motion which govern the behavior of thecollapsing object near the classical singularity become strongly non-local. We managed to solve thenon-local equations, and found an explicit form of the wavefunction describing the collapsing
object. This wavefunction and the corresponding probability density are non-singular at the origin,thus indicating that quantization should be able to rid gravity of singularities, just as it was thecase with the singular Coulomb potential.

Liang Dai, Institute for Advanced Study.

Lensing magnification bias on the apparent distribution of black hole mergers
The recent detection of gravitational waves indicates that stellar-mass black hole binaries are likely
to be a key population of sources for forthcoming observations. With future upgrades,
ground-based detectors could detect merging black hole binaries out to cosmological distances.
Gravitational wave bursts from cosmological redshifts can be strongly magnified by intervening
galaxies along the line of sight. In the absence of electromagnetic counterparts, the mergers’
intrinsic mass scale and redshift are degenerate with the unknown magnification factor. Hence,strongly magnified low-mass mergers from high redshifts appear as higher-mass mergers from lower
redshifts. We assess the impact of this degeneracy on the mass-redshift distribution of observable
events in generic models of binary black hole formation. We find that strong magnification
generally creates a heavy tail of apparently massive mergers. For LIGO and its future upgrades,
this tail may dominate the population of intrinsically massive, but unlensed mergers in some binary
black hole formation models. Modeling the statistics of lensing magnification can help account forthis magnification bias when testing astrophysical scenarios of black hole binary formation andevolution.

Ruth Gregory, Durham University.

Screened Scalars and Black Holes
I will discuss screened scalar hair around black holes, first explaining why “no hair” theorems do
not work in this case, then deriving the scalar profile around the accretion disc of a Kerr black hole.
I will also discuss astrophysical implications and model constraints.

Alexandre Dolgov, Novosibirsk State University, ITEP, University of Ferrara.

LIGO-observed gravitational waves: problems and solution.
The direct registration of gravitational waves (GW) by LIGO created several problems related totheir possible source: the origin of 30 solar mass black holes (BH), the probability of BH binary
formation, the too low value of the primary black hole spins. The model of primordial BH
formation is presented which naturally solves the observed problems and predicts some properties
the future events of GW observations. The model also explains the observed rich astrophysicalpopulation of the universe at redshifts 6-10.

53

Tomohiro Nakama, Johns Hopkins University.

New primordial black hole constraints to primordial gravitational waves
Recently we have proposed a novel method to probe primordial gravitational waves from upperbounds on the abundance of primordial black holes (PBHs). When the amplitude of primordial
tensor perturbations generated in the early universe is very large, they induce large scalar
perturbations due to their second-order effects. If the amplitude of resultant scalar perturbations is
too large at the moment of their horizon reenty, then PBHs are overproduced to a level that isinconsistent with a variety of existing observations constraining the abundance of PBHs. Thisconsideration leads to upper bounds on the amplitude of primordial tensor perturbations onsuper-horizon scales. In contrast to our recent paper in which we only present simple estimationsof the upper bounds from PBHs, in this paper, we present detailed derivations, by solving theEinstein equations for scalar perturbations induced at second order in tensor perturbations. We
also derive an approximate formula for the probability density function of induced density
perturbations, necessary to relate the abundance of PBHs to the primordial tensor power spectrum,
assuming primordial tensor perturbations follow Gaussian distributions. Comparison is presented of
the upper bounds from PBHs with other existing bounds obtained from Big Bang Nucleosynthesis,
Cosmic Microwave Background, LIGO/Virgo and pulsar timing arrays.

David Weir, University of Stavanger.

Simulating a first-order electroweak phase transition
In various extensions of the Standard Model it is possible that the electroweak phase transition was
first order. This would have been a violent process, involving the formation of bubbles andassociated shock waves. The collision of these bubbles and shock waves could be a detectablesource of gravitational waves. I will summarise recent work to model such a phase transition usinglarge-scale hydrodynamical simulations. In addition, I will demonstrate some generic features of
the resulting gravitational wave power spectrum, and the implications for detectability of specificscenarios at future gravitational wave observatories.

LIGO AND BLACK HOLES/PRIMORDIAL/INFLATION.
4-5:30 pm Simeon Bird, Johns Hopkins University.

Did LIGO Detect Dark Matter?
There is a possibility that the recent LIGO detection of gravitational waves originated from themerger of two primordial black holes, making up the dark matter. Thirty solar mass black holes, asdetected by LIGO, lie within an allowed mass window for primordial black hole dark matter.
Interestingly, our best estimates of the number of observable mergers fall within the range impliedby current LIGO data. I will explain these estimates, discuss the (considerable!) theoreticaluncertainties, and finish with prospects for testing the model.

54

Florian Kuhnel, Stockholm University.

Primordial Black Holes
Primordial black holes are black holes that may have formed in the early Universe. Their masses
span potentially a range from as low as the Planck mass up to many orders of magnitude above
the solar mass. Besides their conceptual importance regarding our understanding of quantum
effects and gravity, they may provide the dark matter. In order to constrain this possibility, aproper understanding of their formation mechanism is crucial. In my talk, after a general
introduction on primordial black holes, I will discuss recent investigations on this issue, including
so-called critical collapse, non-sphericity and non-Gaussianity. Furthermore, I will discuss how toproperly compare extended primordial black-hole mass spectra to observational constraints, such as
those deriving from recent microlensing surveys.

Riccardo Penco, Columbia University.

Effective Field Theory of Inflation with Broken Spatial Diffeomorphisms
The vast majority of inflationary models in the literature are based on the premise that one ormore fields evolve in time while their total energy density remains approximately constant. This
time evolution leads to the spontaneous breaking of time diffeomorphisms. The behavior of
cosmological perturbations in these models is captured by the well-known EFT of Inflation (and its
multi-field generalization). It is perhaps less well-known that inflation can also be generated bytime-independent field configurations with a non-trivial spatial profile. This is much less studied
scenario, which is realized for instance if inflation is driven by a solid. In this talk, I will first review
the peculiarities of solid inflation, and then discuss the analog of the EFT of inflation for models
that break spatial rather than time diffeomorphisms.

Emil Mottola, Los Alamos National Laboratory.

Scalar Gravitational Waves in the Effective Theory of Gravity
Classical General Relativity as a Low Energy Effective Theory receives an infrared relevant
modification from the conformal trace anomaly of the energy-momentum tensor of massless, ornearly massless, quantum fields. The local form of the effective action associated with the trace
anomaly is expressed in terms of a dynamical scalar field that couples to the conformal factor of
the spacetime metric, allowing it to propagate over macroscopic distances. Linearized around flatspacetime, this semi-classical EFT admits scalar gravitational wave solutions in addition to thetransversely polarized tensor waves of the classical Einstein theory. Astrophysical sources for scalar
gravitational waves are considered, with the excited gluonic condensates in the interiors of neutronstars in merger events with other compact objects likely to provide the strongest burst signals. The
QCD phase transition is a possible source of a cosmological stochastic background of scalar
gravitational radiation, also potentially detectable by the next generation of gravitational wave
detectors.

Tomohiro Fujita, Stanford University.

Inflationary Gravitational Waves - beyond vacuum fluctuation
It is well known that the amplitude of the gravitational wave (GW) produced from the vacuum
fluctuation during inflation is proportional to the energy scale of inflation. Thus the observation of
the inflationary GW by CMB B-mode is expected to reveal the energy scale of new physics as wellas pin down the inflation model. However, alternative production mechanisms of GW during
inflation has been discussed recently. We consider a coupled system between an axion and SU(2)gauge fields whose energy density is subdominant. We found the GW generated by the spectator
fields can be much larger than the GW from vacuum fluctuation without a fine-tuning. The
produced GW is chiral, its tilt is arbitrary and the production of additional scalar perturbation issuppressed. Therefore, with our spectator fields, a low energy inflation model can produce
detectable GW.
55

Bohua Li, The University of Texas at Austin.

Complex Scalar Field Dark Matter and its Imprint on the Gravitational Wave
Background from Inflation
Coauthor: Paul Shapiro, Tanja Rindler-Daller We consider an alternative dark matter candidate to
WIMP cold dark matter (CDM), ultralight bosonic dark matter (m > 10≠22 eV) described by acomplex scalar field (SFDM), of which the comoving particle number density, or charge density, isconserved after particle production during standard reheating (w=0). In a Lambda-SFDM universe,
SFDM starts relativistic, evolving from stiff (w=1) to radiationlike (w=1/3), before becoming
nonrelativistic at late times (w=0). Thus, before the familiar radiation-dominated phase, there isan earlier phase of stiff-matter-domination, and the expansion rate in the early Lambda-SFDM
universe is increased compared with that in Lambda-CDM. The transitions between these phases,
determined by SFDM particle mass and self-interaction coupling strength, are therefore
constrained by cosmological observables, particularly Nef f , the effective number of neutrino
species during BBN, and zeq , the redshift of matter-radiation equality. Furthermore, primordial
tensor fluctuations that reenter the horizon during or before the stiff phase are amplified by thestiff phase and contribute a homogeneous energy density as a stochastic gravitational wave (GW)
background. Hence, detection of GWs from inflation is then made possible at high frequencies by
current laser interferometer experiments, e.g., aLIGO/Virgo and eLISA. In fact, our calculation fora few fiducial cases shows that for a broad range of reasonable reheat temperature Treheat , theamplified GW background within the sensitive frequency band of aLIGO can reach a signal-to-noise
ratio of 3 by the end of the final stage of aLIGO/Virgo experiment should it exist, for currently
allowed values of tensor-to-scalar ratio r according to CMB polarization measurements.

DARK MATTER EXPERIMENT.
2-3:30 pm Evan Pease, Yale University.

Current Status of the LUX Dark Matter Experiment
The LUX experiment searches for direct evidence of galactic dark matter. Located roughly 1.5 km
underground at the Sanford Underground Research Facility in Lead, South Dakota (USA), thedetector contains a 350-kg active liquid xenon target. LUX operates as a dual-phase (liquid/gas)time projection chamber with 122 photomultiplier tubes, and it is capable of three-dimensional
position reconstruction and discrimination of electronic and nuclear recoils. The initial 95 live-days
exposure reached a record-setting sensitivity to Weakly Interacting Massive Particles (WIMPs),
excluding WIMP-nucleon couplings greater than 5.6e-46 cm2 for WIMPs of mass 33 GeV.
Following this result, LUX has performed detailed calibrations and has recently completed
accumulating a new exposure in excess of 300 live days. I discuss implications of the LUX results
and present the current status of this search.

56

Kaixuan Ni, University of California, San Diego.

Recent Results from the XENON Dark Matter Experiments
The XENON program carries out dark matter searches with unprecedented sensitivity using thepioneering two-phase xenon technology at the Gran Sasso Underground Laboratory in Italy. We
have performed searches for various dark matter candidates using the one-hundred-kg scale
XENON100 detector. Recent results on the searches for dark matter elastic scattering signals,
low-mass dark matter signals, dark matter induced electron recoil signals, and the annual
modulation signals in XENON100 will be presented. We will also present the recent operational
results from XENON1T, the largest running dark matter detector with a 2-ton sensitive liquid
xenon target.

Wolfgang Lorenzon, University of Michigan.

The LZ Dark Matter experiment
The LUX-Zeplin (LZ) experiment is the most advanced next-generation direct detection
experiment under construction to search for Dark Matter in the Universe. It contains a dual-phaseliquid xenon time projection chamber with a total active mass of 7 tons. LZ is implementing
various low background techniques to significantly reduce radioactive background and reach an
unprecedented level of sensitivity to spin-independent WIMPs. For a WIMP mass of 50 GeV, anultimate sensitivity of 2 10-48 cm2 is expected in three years of operation. LZ will be located at
the Sanford Underground Research Facility (SURF) in South Dakota, at the same location as thecurrently running LUX experiment. In this presentation, an overview of the experimental
techniques and science reach will be presented.

Anthony Villano, University of Minnesota.

Pushing the limits of low-energy calorimetry in SuperCDMS
The SuperCDMS SNOLAB experiment aims for world-leading sensitivity to low-mass WIMPs. This
goal underscores the need for an excellent understanding of the energy scale for extremely low
energy recoils, especially nuclear recoils less than 1keV. Such an understanding is difficult to obtainbecause of complicated energy-loss mechanisms in crystalline solid-state matter. I will discuss theexperimental and theoretical subtleties of these mechanisms and the future of precision calibrationsin this energy regime. I will also present the current analysis status of SuperCDMS detector
nuclear-recoil energy calibration with monoenergetic neutrons.

Eric Dahl, Northwestern University.

Recent Results from PICOThe PICO collaboration has set the world-leading direct-detection limits on the spin-dependent
WIMP-proton cross section with the PICO-60 and PICO-2L bubble chambers at SNOLAB. The
PICO-60 result, with a 37-kg CF3I target and 3,415 kg-day exposure, represents the largest
bubble-chamber dark matter search to date, while the most recent run of PICO-2L (3-kg C3F8
target and 129 kg-day exposure) successfully eliminates the particulate-induced events that havebeen the chief background in past PICO experiments. I will cover both of these results, give an
update on the next physics run of PICO-60 which is set to begin at the end of summer 2016, andwill describe our progress on new zero-buffer-fluid chambers that aim to further reduce particulateand droplet backgrounds, including our first prototype scintillating xenon bubble chamber.

57

Phillip Urquijo, The University of Melbourne.

The SABRE Dark Matter Experiment: A pair of sodium iodide detectors located in Italy
and Australia
The interaction rate of hypothesised dark matter particles in Earth bound detectors is expected toundergo annual modulation due to the planets orbital motion. The DAMA/LIBRA experiment has
observed such a modulation with high significance in an array of scintillating NaI(Tl) crystals,
however this result remains to be confirmed by independent experiments using the same detection
method.
SABRE aims to test the DAMA/LIBRA results by performing a higher sensitivity measurementwith NaI(Tl) crystals, and to investigate the nature of dark matter interactions. The key
innovations in the detector setup will be the use of high purity NaI(Tl) crystals, improving uponthat of DAMA/LIBRA, an active background rejection system using a liquid scintillator, andimproved photomultiplier tubes with lower background and a higher quantum efficiency.
The most unique aspect of the experiment will to operate a pair of such detectors, located at
LNGS (Laboratori Nazionali del Gran Sasso, Italy) and the new deep underground laboratory in
Stawell, Australia (SUPL, Stawell Underground Physics Laboratory). The combined analysis ofdata sets from the two hemispheres will provide critical information on any terrestrial contribution
to the modulation signal.
In this presentation we will present the progress on crystal development, the status of a proof ofprinciple detector currently being installed at LNGS, and the design and physics potential of theultimate detector configuration.

58

Wednesday, August 10, 2016
CMB/LARGE SCALE STRUCTURE.
2-3:30 pm Martina Gerbino, OKC and Nordita, Stockholm University.

The hunt for neutrino hierarchy
Neutrino physics is one of the most exciting arena for a combined research in cosmology andparticle physics. Even though we know from oscillation experiments that neutrinos do have masses,
we still fail in assessing the neutrino mass scale. Cosmological probes such as the cosmic
microwave background radiation and large scale structures currently provide the tightest
constraints on the sum of neutrino masses, though in the form of upper bounds. In this talk, I will
discuss the sensitivity of current cosmological probes to the neutrino mass splitting, in light of theresults from neutrino oscillation measurements. Even if the differences in the bounds for possible
neutrino mass schemes are tiny, there is indeed a difference, implying that present cosmologicalmeasurements are mildly sensitive to the distribution of hot dark matter and radiation at latetimes. This should be regarded as an example of how close we are to the limit at which analyses
involving an accurate inclusion of information from oscillation measurements, along with astatistical model comparison able to assess the preference for a hierarchy, become pressing.

Thomas Tram, Institute of Cosmology and Gravitation (ICG), University of Portsmouth.

The Intrinsic Matter Bispectrum
Upcoming large scale structure surveys will map the structure of the Universe on very large scales
where General Relativistic (GR) effects become important. In order to extract information fromthese surveys, we must have a fast and accurate analytic model. This is well known on small scales
where the precision of Newtonian N-body codes is constantly being pushed but it is equally true atlarge scales. In this talk I will present numerical and analytic computations of the matter
bispectrum generated from Gaussian initial conditions, i.e. the intrinsic matter bispectrum. Fromthe point of view of inflationary non-Gaussianity, this intrinsic matter bispectrum acts as aforeground which must be subtracted in order to extract the primordial signal.

Jerome Gleyzes, Jet Propulsion Laboratory.

Non Gaussianity in two-field inflation
Thanks to the fantastic results of the Planck mission, we now have a better understanding of thevery early Universe. The evidence points towards a phase of inflation, where the Universe
underwent exponential expansion, leaving it very smooth. Moreover, inflation predicts the
distribution of initial fluctuations that lead to the galaxies we observe today. In the simplest model,
those fluctuations are Gaussian. However, in some models where multiple fields cause inflation, non
Gaussianity can arise. Therefore, measuring the non-Gaussianity can allow to distinguish between
models. I will show that contrarily to what is sometimes claimed, non-Gaussianity is not a genericfeature in multi-field inflation. Through example, I will identify when large non-Gaussianity arise.
The bottom line is that, if measuring large non-Gaussianity would clearly means that our simplest
picture of inflation is wrong, a non detection would not rule out more complicated scenarios

59Christian Fidler, CP3 - UCL.

A Relativistic Interpretation of Newtonian Large Scale Structure Simulations
General relativistic effects in structure formation have to be taken into account for the next
generation of large-scale structure surveys such as the SKA and the EUCLID mission. In contrast,
simplified Newtonian N-body simulations are often employed to solve the gravitational clustering ofmatter. While this is accurate on the small scales, important corrections are expected on the large
scales. We present how unmodified Newtonian simulations can be interpreted in agreement withgeneral relativity, obtaining a consistent relativistic large scale result. The idea is to define a
specific gauge in which the dark matter particles move on Newtonian trajectories and employ
CLASS to compute the metric potentials in this particular gauge. A relativistic interpretation of
the Newtonian simulation is then obtained by interpreting the particle positions on this space-timeinstead of the Newtonian flat space. We present an analysis in a Universe filled with dark energy,
dark matter, baryons and radiation, which a special focus on radiation which is typically neglected
in ordinary Newtonian simulations. The advantage of our method is creating a split between the
non-linear Newtonian gravitational collapse, solved in a N-body simulation, and the computationof the typically linear metric potentials in an Einstein-Boltzmann code. In addition, the method
provides a framework for the inclusion of new physics into relativistic simulations, such as forexample theories of modified gravity.

Grant Mathews, University of Notre Dame.

Possible Evidence for Resonant Superstring Excitations during Inflation
We show that both the suppression of the l=2 moment of the power spectrum cosmic microwave
background temperature fluctuations and the possible dip in the power spectrum for l= 10-30 canbe explained as the result of the resonant creation of successive excitations of a single fermionic(or bosonic) open superstring that couples to the inflaton field. For our best-fit models, we candeduce the number of oscillations on the string during inflation. From the deduced degeneracy ofthe string we can infer the coupling constant between the string and the inflaton field along withthe masses of these states. Although the evidence of the dip at l=10-30 is of marginal statisticalsignificance, and there are other possible interpretations of these features, this could constitute thefirst observational evidence of the existence of a superstring in Nature.

Neil Barrie, University of Sydney.

Gravitational Wave Instabilities in the Cosmic Neutrino BackgroundWe investigate the propagation of gravitational waves through the cosmic neutrino background,assuming it carries a non-zero lepton asymmetry. In this background, the graviton dispersion
relation is found to exhibit birefringent behaviour leading to an enhancement/suppression of thegravitational wave amplitudes depending on the polarisation, where the magnitude of this effect isrelated to the size of the lepton asymmetry. The heralding of the new era of gravitational wave
astronomy may allow the investigation of this behaviour and provide an indirect way to learn about
the properties of the cosmic neutrino background and the neutrino sector.

60

4-5:30 pm Craig Copi, Case Western Reserve University.

CMB Anomalies: Status and Future Directions
A number of anomalies in the observed CMB temperature anisotropies were first identified in the
WMAP data and subsequently confirmed by Planck, greatly reducing the likelihood that they were
just systematic effects. These anomalies typically are rare – at the 2 to 3 sigma level. Thoughmany have been discovered, it is unclear how to combine them, that is, which of the anomalies are
independent of the others. Further, all have been discovered a posteriori by looking at the dataand seeing something strange. The simplest explanation for them is that our Universe is just a rarerealization (the fluke hypothesis). Since we only have one Universe, new observations of thetemperature anisotropies will not provide new tests of these anomalies. Even so, future
measurements of other correlated observables, such as polarization, can provide new insights andhelp identify whether our Universe is a rare fluke or if new physics is required. In this talk we will
briefly review the status of the anomalies, categorize them, and discuss on-going work to make apriori predictions for future observations.

Graeme Addison, Johns Hopkins University.

Quantifying discordance in the 2015 Planck CMB spectrum
I will discuss the internal consistency of the Planck 2015 CMB temperature anisotropy power
spectrum and show that tension exists between the determination of some cosmologicalparameters from multipoles l < 1000 (roughly the scales accessible to wmap) and l Ø 1000. I willshow that the l Ø 1000 constraints are also in tension with low-redshift data sets, including
Plancks own measurement of the CMB lensing power spectrum (2.4 sigma), the most precise
determination of the baryon acoustic oscillation scale (2.5 sigma), and the local Hubble constant(3.8 sigma). Disagreement between parameters inferred from the Planck and South Pole Telescopemeasurements of the CMB damping tail disfavors a cosmological explanation and suggests the
Planck values result from an unusual statistical fluctuation or remaining systematic errors in the
Planck data.

Marius Millea, Intitut Lagrange de Paris.

Features in the Planck power spectrum and shifts in cosmological parameters
One of the legacies of the results from the Planck satellite is the continued success of the standard
six-parameter CDM model. Along with this are a tightening of constraints and a set of shifts inthe best-fit values of these six parameters as compared to previous estimates from CMB data. For
example, the Planck data prefer a LCDM model with a lower Hubble constant than previously
thought, and a higher amplitude of matter fluctuations, ‡8 . These shifts have attracted muchattention, particularly since some of them serve to drive tensions with other cosmological probes.
These tensions are at the forefront of our search for evidence of new physics or of systematic errors
in one or more of these probes. In this talk we will take a critical look at these parameter shifts.
Are they at the level one should have expected given the increase in precision of the Planck dataover its predecessors? What features in the data are driving them, and are these features robust?
And what is the physical explanation for why these features impacted the parameters in the waythat they have? While some of these questions have been partially addressed, others have neverbeen at all, and we will do so in this talk.

61

Melanie Simet, Carnegie Mellon University.

Weak Lensing Measurement of the Mass-Richness Relation of SDSS redMaPPer
Clusters
I will describe a measurement of the mass–richness relation of the redMaPPer galaxy cluster
catalogue using weak lensing data from the Sloan Digital Sky Survey. My collaborators and I used
an updated forward-modeling approach to better match the expected signal, allowing us tomeasure rather than assume some features of the model. We also carefully characterized a broad
range of systematic uncertainties in our measurement and our signal modeling. Finally, we
compared measurements of the lensing signal from two independently-produced shear andphotometric redshift catalogues to demonstrate the reliability of both the measurement and theassociated systematic and statistical errors.

Jonathan Blazek, CCAPP - Ohio State University.

Streaming velocities and baryon-acoustic oscillations
At the epoch of decoupling, cosmic baryons had supersonic velocities relative to the dark matterthat were coherent on large scales. These velocities subsequently slow the growth of small-scale
structure and, via feedback processes, can influence the formation of larger galaxies. I will discuss
the potential impact of these streaming velocities on the baryon acoustic oscillation (BAO) feature.
In particular, the combination of galaxy advection and gradients in these streaming velocities yields
a significant contribution which must be considered in the analysis of upcoming BAO
measurements. This effect also opens a new window to the astrophysics of galaxy formation.

Sukhdeep Singh, Carnegie Mellon University.

Galaxy-galaxy and galaxy-CMB Lensing with SDSS-III BOSS galaxies
Weak lensing has emerged as an important cosmological probe for our understanding of dark
matter and dark energy. The low redshift spectroscopic sample of SDSS-III BOSS survey, with awell-understood galaxy population is ideal to probe cosmology using galaxy-galaxy lensing andgalaxy-CMB lensing. I will present results from two methods that combine information fromlensing and galaxy clustering.
The first involves combining lensing and galaxy clustering to directly measure galaxy bias and thus
recover the matter correlation function, which is directly predicted from theory. Using scales where
linear perturbation theory is valid, we carry out a joint analysis of galaxy-galaxy clustering,galaxy-galaxy lensing, and CMB-galaxy lensing, and constrain linear galaxy bias b = 1.80 ± 0.06,
m = 0.284 ± 0.024, and relative calibration bias between CMB and galaxy lensing,bl = 0.82 ± 0.15.
The second method involves including information about redshift-space distortions to measure theEG statistic and test gravitational physics at cosmological scales. This statistic is independent ofgalaxy bias and the amplitude of the matter power spectrum. Different theories of gravity predicta different EG value, making it a clean and stringent test of GR at cosmological scales. Using the
BOSS low redshift sample, we have measured EG at z = 0.27 with 10% (22%) accuracy using
galaxy (CMB) lensing, with results consistent with LCDM predictions.

62

DARK MATTER.
2-3:30 pm Francesc Ferrer, Washington University in St Louis.

A robust halo-independent upper limit on the dark matter cross section
I will describe a method that allows to place an upper limit on the dark matter elastic scatteringcross section with nucleons which is independent of the velocity distribution. This approachcombines null results from direct detection experiments with indirect searches at neutrino
telescopes, and goes beyond previous attempts to remove astrophysical uncertainties in that it
directly constrains the particle physics properties of the dark matter. The resulting
halo-independent upper limits on the scattering cross section of dark matter are remarkably strong,within a factor of a few of limits that assume a Standard Halo Model.
References: F. Ferrer. A. Ibarra and S. Wild, JCAP 1509 (2015) no.09, 052 [arXiv: 1506.03386]

Francis-Yan Cyr-Racine, Harvard University.

From dark particle physics to the matter distribution of the Universe
The effective theory of structure formation (ETHOS) allows the classification of dark mattertheories according to their structure formation properties rather than their intrinsic particle
properties. This makes ETHOS a particularly useful framework for comparing theoreticalpredictions of extended dark matter scenarios to actual cosmological and astrophysicalobservations. Using this effective theory, we describe how the details of the dark matter physics
actually affect the shape of the linear matter power spectrum, hence clarifying the link between
dark matter microphysics and structure formation. We then use the ETHOS framework to put
cosmological and astrophysical constraints on broad classes of dark matter microphysics. We
finally discuss how nonminimal dark matter theories can be used to remove apparent tension
between various cosmological probes.

Tim Linden, The Ohio State University.

Dark Matter, Pulsar, and Diffuse Emission Models for the Galactic Center GeV Excess
Fermi-LAT observations have discovered a gamma-ray excess emanating from the Galactic centerof the Milky Way. While the existence of this excess is now certain, its origin is not. Three distinct
classes of models have been posited to explain its key features: dark matter annihilation, a
population of sub-threshold gamma-ray pulsars, and diffuse emission from the intense Galactic
center environment. In this talk, I will describe the successes and failures of each model as an
explanation for the Galactic center excess outlining several significant advances in modeling pulsars
and diffuse emission properties near the Galactic center. Finally, I will describe smoking gun testsof each scenario which may rule out, or lend credence to each model within the next five years.

Annika Peter, The Ohio State University.

How self-interacting dark matter shapes the Milky Way satellite population
Using a suite of high-resolution dark-matter-only simulations tagged with star, we investigate theeffects of self-interacting dark matter (SIDM) on the tidal stripping and evaporation of satellite
galaxies in a Milky Way-like host. We find that stars are stripped at a higher rate in SIDM than incold dark matter cosmologies. We show that this enhanced stripping is almost entirely due to theenhanced tidal stripping resulting from the SIDM-induced shallow gravitational potentials of thesatellites. This leads to a suppression in the abundance of ultra-faint dwarf galaxies and growth in
the satellite’s half-light radius after infall. Ultra-faint dwarfs are thus prime targets for constraining
SIDM models.

63

Savvas Koushiappas, Brown University.

Gamma-ray emission and the dark matter content of the dwarf galaxy Reticulum II
I will present results on the analysis of gamma-ray emission from the recently discovered dwarf
galaxy Reticulum II. Using Fermi-LAT data and a suite of background models we quantify theprobability that the observed gamma-ray emission is due to background. Reticulum II is found tohave the most significant gamma-ray emission from any other known dwarf galaxy. I will also
discuss the dark matter content of Reticulum II as derived from kinematic studies of its member
stellar population and show that Reticulum II has a dark matter halo similar to other nearby dwarf
galaxies. If the gamma ray emission is due to dark matter annihilation, the annihilation crosssection is consistent with the s-wave relic abundance cross section. I will conclude by discussing
further tests that are needed in order to ascertain the likelihood of this emission to be due to aconventional astrophysical interpretation.

Mei-Yu Wang, Texas A&M University.

Revealing the nature of dark matter with Milky Way dwarf satellite galaxies
The dwarf galaxies surrounding the Milky Way provide a unique and powerful way to explore thenature of dark matter. They are the most extreme dark matter dominated objects known to us
with central mass to light ratios typically of the order of tens to hundreds. Through measurementsof their stellar kinematics, we can study their dark matter content in exquisite precision. This
allows us to probes their halo structure that is sensitive to different dark matter physics such as
warm dark matter, self-interaction, and decay instabilities. In this talk, I present frameworks that
address these questions by combining high-precision stellar kinematic measurements withstate-of-art cosmological N-body simulations and detailed kinematic modeling. I will demonstratethat the properties of the dark matter are linked to the mechanisms that drive satellite galaxy andhalo evolution such as infall time and the effects of tides. In the CDM scenario some dwarf
galaxies explicitly require to be shaped under significant gravitational tidal forces, which will leave
imprints on their stellar distribution and kinematics. I also show how to determine the optimized
kinematic observational strategies for achieving precision measurement of dark matter contents in
newly discovered faint dwarf galaxies with current and future spectroscopic follow-up facilities, andforecast their constraining power on WIMP dark matter models. I will discuss how these results are
driving advances in both astronomy and particle physics, and having the potential to shed lights on
the nature of dark matter.

4-5:30 pm Haipeng An, Caltech.

Dark matter annihilation via dark bound state formation
We study the impact of bound state formation on dark matter annihilation rates in models where
dark matter interacts via a light mediator. For indirect detection, our result shows that dark
matter annihilation inside bound states can play an important role in enhancing signal rates over
the rate for direct dark matter annihilation with Sommerfeld enhancement.

64

Hongwan Liu, Massachusetts Institute of Technology.

The Darkest Hour Before Dawn: Contributions to Cosmic Reionization from Dark
Matter Annihilation and Decay
Dark matter annihilation or decay could have a significant impact on the ionization and thermal
history of the universe. We have studied the potential contribution of dark matter annihilation(s-wave- or p-wave-dominated) or decay to cosmic reionization, via the production of electrons,
positrons and photons. We map out the possible perturbations to the ionization and thermal
histories of the universe due to dark matter processes, over a broad range of velocity-averaged
annihilation cross-sections/decay lifetimes and dark matter masses. We have employed recent
numerical studies of the efficiency with which annihilation/decay products induce heating andionization in the intergalactic medium, and in this work extended them down to a redshift of 1 + z= 4 for two different reionization scenarios. We also improve on earlier studies by using the resultsof detailed structure formation models of dark matter haloes and subhaloes that are consistent
with up-to-date N-body simulations, with estimates on the uncertainties that originate from thesmallest scales. We find that for dark matter models that are consistent with experimental
constraints, a contribution of more than 10% to the ionization fraction at reionization is disallowed
for all annihilation scenarios. Such a contribution is possible only for decays into electron/positronpairs, for light dark matter with a mass of about 100 MeV within a limited range of decay lifetimes.

Sebastian Trojanowski, National Center for Nuclear Research, Poland / UC Irvine.

Reconstructing WIMP properties through an interplay of signal measurements in direct
detection, Fermi-LAT, and CTA searches for dark matterIn the presentation I will examine the projected ability to reconstruct the mass, scattering, andannihilation cross section of dark matter in the new generation of large underground detectors,e.g., XENON-1T, in combination with diffuse gamma radiation from expected 15 years of datafrom Fermi-LAT observation of 46 local spiral dwarf galaxies and projected CTA sensitivity to asignal from the Galactic Center. To this end I will consider several benchmark points spanning awide range of WIMP mass, different annihilation final states, and large enough event rates towarrant detection in one or more experiments. As previously shown, below some 100 GeV only
direct detection experiments will in principle be able to reconstruct the WIMP mass well. Thismay, in case a signal at Fermi-LAT is also detected, additionally help restricting ‡ v and theallowed decay branching rates. On the other hand at large WIMP mass, 1 TeV, CTA will have theability to reconstruct mass, annihilation cross section, and the allowed decay branching rates tovery good precision for the or purely leptonic final state, good for the WW case, and rather poor
for bb. A substantial improvement can potentially be achieved by reducing the systematic
uncertainties, increasing exposure, or by an additional measurement at Fermi-LAT that would help
reconstruct the annihilation cross section and the allowed branching fractions to different final
states. The presentation will be based on astro-ph.CO/1603.06519

65Isabel M. Oldengott, Bielefeld University.

Reionization and dark matter decay
Cosmic reionization and dark matter decay can impact observations of the cosmic microwave sky
in a similar way. A simultaneous study of both effects is required to constrain unstable dark matterfrom cosmic microwave background observations. We compare two reionization models with andwithout dark matter decay. We find that a reionization model that fits also data from quasars andstar forming galaxies results in tighter constraints on the reionization optical depth ·reio , but
weaker constraints on the spectral index ns than the conventional parametrization. We use thePlanck 2015 data to constrain the effective decay rate of dark matter to ef f < 2.9 ◊ 10≠25 /s at
95% c.l. this limit is robust and model independent. it holds for any type of decaying dark matterand it depends only weakly on the chosen parametrization of astrophysical reionization. for lightdark matter particles that decay exclusively into electromagnetic components this implies a limit of“ < 5.3 ◊ 10≠26 /s at 95% c.l. specifying the decay channels, we apply our result to the case of
kev-mass sterile neutrinos as dark matter candidates and obtain constraints on their mixing angle
and mass, which are comparable to the ones from the diffuse x-ray background.

Keisuke Harigaya, UC Berkeley/LBNL.

Light Chiral Dark Sector
An interesting possibility for dark matter is a scalar particle of mass of order 10 MeV - 1 GeV,
interacting with a U(1) gauge boson (dark photon) which mixes with the photon. We present a
simple and natural model realizing this possibility. The dark matter arises as a composite pseudo
Nambu-Goldstone boson (dark pion) in a non-Abelian gauge sector, which also gives a mass to thedark photon. The gauge symmetry of the model does not allow any mass term for the dark quarks,
and stability of the dark pion is understood as a result of an accidental global symmetry. The
model has a significant parameter space in which thermal relic dark pions comprise all of the dark
matter, consistently with all experimental and cosmological constraints. In a corner of theparameter space, the discrepancy of the muon g-2 between experiments and the standard model
prediction can also be ameliorated due to a loop contribution of the dark photon. Smoking-gun
signatures of the model include a monophoton signal from the e+ e- collision into a photon and a“dark rho meson.” Observation of two processes in e+ e- collision, the mode into the dark photon
and that into the dark rho meson, would provide strong evidence for the model.

Sam Cormack, Dartmouth College.

Superfluid fermion dark matter
There has recently been significant interest in the idea that dark matter could form a many bodyquantum state. Previous work has focused on Bose-Einstein condensates and degenerate Fermi
matter. We investigate the possibility that fermionic dark matter becomes a superfluid via a BCS
transition. This requires an attractive interaction which alters the density profile of the halo andwe consider whether this interaction could be torsion-induced. If the halo is indeed a superfluid it
may contain interesting features such as vortices.

66

DARK ENERGY.
2-3:30 pm David Cinabro, Wayne State University.

No Evidence for Type Ia Supernova NUV-Optical Subclasses
In response to a recent reported observation by Milne and collaborators, we search for evidence of
two classes of Type Ia supernovas (SNIa) distinguished by their brightness in the rest-frame near
ultra-violet. Using the SNANA supernova analysis package, we develop a model of two classes of
SNIa that reproduce the features described by Milne et al. We simulate the appearance of thelight curves of these objects in the Sloan Digital Sky Survey Supernova Search (SDSS) and theSupernova Legacy Survey (SNLS) showing that we could easily observe the two classes ascompared to the more conventional explanation for the diversity of SNIa ultraviolet brightnesses
with the SALT-II SNIa model. We compare the simulation of the two models to 158 observed
SNIa light curves in the SDSS and SNLS data sets. We see no evidence of two classes of SNIa andfind good agreement between the observed data and the predictions of the SALT-II model of SNIa
light curves.

Dan Scolnic, KICP at University of Chicago.

New Cosmology Results with Type Ia Supernovae
I will describe recent progress to measure the equation-of-state of dark energy and the Hubble
constant using Type Ia Supernovae. I will primarily focus on new measurements of w with the
Pan-STARRs spectroscopic SN sample and discuss new techniques to remove biases in the
supernova distances and recalibrate the full compilation of SN lightcurves. I also will show how
these improvements impact the latest measurement of the Hubble constant.

Tom Giblin, Kenyon College/CWRU.

Toward Full General Relativity in Cosmology
The principles of homogeneity and isotropy have been the cornerstones of cosmology since thebirth of our field. Nonetheless, these approximations are just that and must be tested, especially inlight of cosmological scenarios where a density contrast may lead to meaningful departures fromhomogeneity – for example, the creation of compact objects or the generation of structure in the
Universe. I will discuss exciting new advances in infrastructure that allow full, non-linear General
Relativity to be applied to cosmological models that will pave the way for precision tests ofcosmology.

James Mertens, Case Western Reserve University.

Deviations from Homogeneity in an Inhomogeneous Universe
It has long been wondered to what extent the observable properties of an inhomogeneous universe
will be measurably different from a corresponding FLRW model. Here, we use tools fromnumerical relativity to study the properties of photons traversing an inhomogeneous universe. We
evolve the full, unconstrained Einstein field equations for a spacetime containing dust and vacuum
energy in proportions similar to our Universe, with a spectrum of long-wavelength density
perturbations similar to the observed one. We then integrate the optical scalar equations along
paths through this numerical spacetime, with all paths terminating at an observer situated similarly
to ourselves, and construct the resulting Hubble diagrams.

67

Tony Padilla, University of Nottingham.

The “sequestering” approach to the cosmological constant problem.
I will discuss recent developments in the sequestering approach to the cosmological constantproblem. Sequestering is a mechanism for eliminating the contributions to vacuum energy frommatter loops. It represents an extremely conservative modification of gravity, only deviating from
GR at the global level, while exploiting the fact that vacuum energy is the unique source ofenergy-momentum that is locally constant and spacetime filling. I will show how the mechanism
can be rendered manifestly local, how it can be adapted to include graviton loops, and other new
developments.

Christoph Schmid, ETH Zurich.

Einstein’s equations from Einstein’s inertial motion and Newton’s laws
With Einstein’s concept of inertial motion as freefalling-nonrotating, Newton’s law for relative
acceleration of freefalling neighbouring test-particles, spherically averaged, gives the exact R0̂0̂
equation of general relativity for non-relativistic matter and for arbitrarily strong gravitational
fields. This equation of Newton for relative acceleration and Einstein’s R0̂0̂ field-equation forspace-time curvature are explicitely identical, if one uses our adapted space-time slicing (by theobserver’s radial 4-geodesics), our adapted Local Ortho-Normal Bases, LONBs (radially parallelwith the observer’s LONBs), and Riemann normal 3-coordinates. Hats on indices denote LONB
components.— With Einstein’s principle of equivalence between fictitious forces and gravitational
forces, the gravitational field equation of 19th-century Newtonian physics and Einstein’s field
equation for R0̂0̂ are both linear for inertial observers, but both bilinear for non-inertial
observers. — Full general relativity follows by using Lorentz covariance and the Bianchi identity.
˛ g and Rî0̂ = ≠(curlB˛ g /2)î hold exactly in general relativity for inertial observers.
R0̂0̂ = ≠divE
˛ g and the gravitomagnetic B
˛ g fields are defined and measured exactly with
The gravitoelectric E
nonrelativistic test-particles via (d/dt)(pî ) and (d/dt)(Sî ) in direct correspondence with the
˛ B)
˛ fields. — The (E˛g, B˛ g ) fields are identical with the Ricci connection forelectromagnetic (E,
LONBs for displacements along the observer’s worldline, (Êâb̂ )0̂ . R0̂0̂ and R0̂î can be measured
exactly with non-relativistic test particles. For inertial observers, (R0̂0̂ , Rî0̂ ) are linear in thegravitational fields. For non-inertial observers, and with the equivalence of fictitious andgravitational forces, the gravitational field equations of 19th-century Newtonian physics and˛ g and
Einstein’s field equations for R0̂0̂ and R0̂î are all bilinear in the gravitational fields, i.e. in E0̂0̂˛
Bg . Einstein’s R equation for non-relativistic matter and for inertial observers gives the Gauss˛ g = ≠4ﬁGN ﬂmass , and Einstein’s R0̂î equation gives the gravito-magnetic Ampère law,
law, divE
˛ g = ≠16ﬁGN J˛mass . — For relativistic matter and inertial observers, Einstein’s R0̂0̂ equationcurlB
˛ g = ≠4ﬁGN (ﬂÁ + 3p̃), where ﬂÁ is the energy density, and (3p̃) is the trace of thegives div E
momentum-flow 3-tensor, and Einstein’s R0̂î equation gives the relativistic gravitomagnetic
˛ g = ≠16ﬁGN JÁî . The remaining six Ricci components, Rîĵ , involve theAmpère law, curlB
curvature of space-space plaquettes, which are unmeasurable with non-relativistic particles inquasi-local experiments.

68

PRIMORDIAL/INFLATION.
4-5:30 pm Sonia Paban, University of Texas at Austin.

On primordial equation of state transitions
We revisit the physics of transitions from a general equation of state pa- rameter to the final stageof slow-roll inflation. We show that it is unlikely for the modes comprising the cosmic microwave
background to contain imprints from a pre- inflationary equation of state transition and still beconsistent with observations. We accomplish this by considering observational consistency bounds
on the amplitude of excitations resulting from such a transition. As a result, the physics which
initially led to inflation likely cannot be probed with observations of the cosmic microwave background. Furthermore, we show that it is unlikely that equation of state transitions may explain theobserved low multipole power suppression anomaly.

Robert Caldwell, Dartmouth College.

Gravitational Wave – Gauge Field Oscillations
Gravitational waves propagating through a stationary gauge field transform into gauge field waves
and back again. When multiple families of flavor-space locked gauge fields are present, thegravitational and gauge field waves exhibit novel dynamics. At high frequencies, the systembehaves like coupled oscillators in which the gravitational wave is the central pacemaker. Due toenergy conservation and exchange among the oscillators, the wave amplitudes lie on amulti-dimensional sphere, reminiscent of neutrino flavor oscillations. This phenomenon has
implications for cosmological scenarios based on flavor-space locked gauge fields.

Martin Winkler, University of Bonn.

Modulated Natural Inflation
I discuss natural inflation and its embedding into supergravity / string theory. As a consequence ofstringy duality symmetries the pure cosine potentials of natural inflation are replaced by modular
functions. This leads to "wiggles" on top of the leading potential which induce deviations of thescalar power spectrum from the standard power law form. The consistency of natural inflation withthe latest CMB data is improved. I will also show that the wiggles reconcile trans-Planckian
excursions of the axion with the weak gravity conjecture.

Raghavan Rangarajan, Physical Research Laboratory, Ahmedabad, India.

Constraints on just enough inflation preceded by a thermal era
If the inflaton was in thermal equilibrium at some time in a radiation dominated era prior to
inflation then the CMB data places an upper bound on the comoving temperature of the(decoupled) inflaton quanta.
If one considers models of “just enough" inflation (where the number of e-foldings of inflation isjust enough to solve the horizon and flatness problems) then in the above thermal scenario we geta lower bound on the Hubble parameter during inflation, Hi nf , which is in severe conflict with theupper bound from tensor perturbations. Alternatively, imposing the tensor upper bound on Hi nf
implies an extremely large number of relativistic degrees of freedom in the thermal bath in the
pre-inflationary Universe (greater than 109 or 101 1), which is not feasible in known cosmologicalscenarios. So a thermal initial state for the inflaton is incompatible with just enough inflation.
[Phys. Rev. D93 (2016) 023516]

69

Nadia Bolis, UC Davis.

Observational Consequences of Scalar-Tensor Entanglement during Inflation
We consider the effects of entanglement in the initial quantum state of scalar and tensor
fluctuations during inflation. We allow the gauge-invariant scalar and tensor fluctuations to beentangled in the initial state and compute modifications to the various cosmological power spectra.
We compute the angular power spectra (Cl ’s) for some specific cases of our entangled state anddiscuss what signals one might expect to find in CMB data. This entanglement also can breakrotational invariance, allowing for the possibility that some of the large scale anomalies in the
CMB power spectrum might be explained by this mechanism.

Krzysztof Turzynski, University of Warsaw.

Geometrical destabilization of heavy scalar fields during inflation
We show the existence of a general mechanism by which heavy scalar fields can be destabilized
during inflation, relying on the fact that the curvature of the field space manifold can dominate thestabilizing force from the potential and destabilize inflationary trajectories. We describe a simple
and rather universal setup in which apparently benign higher-order operators trigger this instability.
This phenomenon can prematurely end inflation, thereby leading to important observational
consequences and sometimes excluding models that would otherwise perfectly fit the data. Moregenerally, it modifies the interpretation of cosmological constraints in terms of fundamental physics.

70

Friday, August 12, 2016
CMB/LARGE SCALE STRUCTURE.
9-10:30 am Pieter Daniel Meerburg, CITA.

The Holiest GrailI will discuss to what degree the cosmic microwave background (CMB) can be used to constrain
primordial non-Gaussianity involving one tensor and two scalar fluctuations, focusing on thecorrelation of one B-mode polarization fluctuation correlated with two E or T modes, i.e. BTT,BTE and BEE. In the simplest models of inflation, the tensor-scalar-scalar primordial bispectrum is
non-vanishing and is of the same order in slow-roll parameters as the scalar-scalar-scalarbispectrum. I will show that constraints from an experiment like CMB-Stage IV using thisobservable are more than an order of magnitude better than those on the same primordial couplingobtained from temperature measurements alone. I will argue that B-mode non-Gaussianity opens
up an as-yet-unexplored window into the early Universe, demonstrating that significant information
on primordial physics remains to be harvested from CMB anisotropies. BTT, BTE and BEE
present measures of both primordial tensors and primordial non-Gaussianity, two of the mostsought after signatures of the inflationary paradigm. A detection would provide profound insight
into the workings of the early Universe.

Laura Mocanu, The University of Chicago.

Measuring the CMB gravitational lensing potential with SPTpol
Weak gravitational lensing by large-scale structure in the universe causes deflections in the paths ofcosmic microwave background (CMB) photons. This effect introduces non-Gaussian correlations in
the observed CMB temperature and polarization fields. The signature of lensing can be used toreconstruct the projected gravitational lensing potential with a quadratic estimator technique; thisprovides a measure of the integrated mass distribution out to the surface of last scattering,sourced primarily from redshifts between 0.1 and 5. The power spectrum of the lensing potential
encodes information about the geometry of the universe and the growth of structure and can beused to place constraints on the sum of neutrino masses and dark energy. High signal-to-noise
mass maps from CMB lensing are also powerful for cross-correlating with other tracers oflarge-scale structure and for delensing the CMB in search for primordial gravitational waves. In thistalk, I will describe recent progress on measuring the CMB gravitational lensing potential and its
power spectrum using data from 500 square degrees of sky observed with the polarization-sensitive
receiver installed on the South Pole Telescope, SPTpol.

Alexander van Engelen, Canadian Institute for Theoretical Astrophysics.

CMB Lensing with ACTPol and successors
Lensing of the CMB is quickly becoming a precision cosmological tool. I will discuss the ACTPol
survey, the recently-begun Advanced ACTPol survey, and successors, focussing on the status of thegravitational lensing measurements and on other, related probes of the growth of structure out tohigh redshift.

71

Kyle Story, Stanford University - KIPAC.

Delensing CMB B modes with the South Pole Telescope polarimeter
Cosmic inflation in the early universe is expected to have produced a background of primordial
gravitational waves (PGW), which induce a curl or "B-mode" component in the polarization of theCosmic Microwave Background (CMB). In many inflation models, this B-mode signal is predicted
to be at a level detectable in the near future. Observed B modes also contain a "lensing B-mode"
component that is produced by gravitationally lensing primordial E modes; current searches for
PGW are already limited by contamination from these lensing B modes. In order to potentiallydetect the PGW signal from B-mode measurements, lensing B modes must be characterized andremoved in a process referred to as "delensing." This process has been studied extensively
theoretically and with simulations, but has not been performed on data. In this talk, we present ananalysis to delens the CMB B-mode spectrum using polarization data from the South Pole
Telescope polarimeter, SPTpol.

Kimmy Wu, UC Berkeley.

BICEP3 performance overview and the BICEP/Keck program
BICEP3 is a 520mm aperture, compact two-lens refractor telescope observing the Cosmic
Microwave Background (CMB) at 95 GHz, designed in pursuit of a potential B-mode signal frominflationary gravitational waves. It is the latest addition to the BICEP/Keck Array series
inflationary probes located at the South Pole, which has provided the most stringent constraints
on the tensor-to-scalar ratio r to date. For the 2016 observing season, the BICEP3 receiver was
upgraded to its full focal plane configuration with 2560 TES detectors. In this talk, we will give an
overview of the BICEP/Keck program and summarize BICEP3s design and performance.

Alexandra Rahlin, Princeton University.

Status report on the first flight of the SPIDER balloon-borne polarimeter
SPIDER is a balloon-borne polarimeter designed to characterize degree-scale microwave emission
on the sky. The goals of the SPIDER program are to (1) characterize the anisotropy spectrum of
the microwave sky with high fidelity over many angular modes, with a focus on the polarized
B-mode signal at degree angular scales, (2) separate the angular and frequency spectrum ofintervening galactic foregrounds from that of the primordial microwave background, and (3) verify
the statistical isotropy of the primordial signal across the sky. The first instance of the SPIDER
payload flew successfully in January 2015, observing for 16 days over 12% of the sky (6% whenweighted by integration time), with an instantaneous sensitivity of 6-7 uK-rts at frequencies of 94
and 150 GHz. In parallel with analysis of the flight data, an upgraded payload is underdevelopment in preparation for a December 2017 flight, with the addition of a 285 GHz band to
improve the characterization of Galactic dust in the SPIDER field. This talk will present an updateon the ongoing data analysis, along with build progress and forecasts for the second mission.

72

DARK MATTER.
9-10:30 am Julian Munoz, Johns Hopkins University.

Probing compact dark matter with fast radio bursts
The possibility that part of the dark matter is made of massive compact halo objects (MACHOs)
remains poorly constrained over a wide range of masses, and especially in the window between 20
and 100 solar masses. It has been recently argued that primordial black holes in this mass window
could make up the dark matter, and that they might produce gravitational wave events, such as
the one detected by the LIGO collaboration. We show that strong gravitational lensing ofextragalactic fast radio bursts (FRBs) by MACHOs (which includes PBHs) of masses larger than
20M§ would result in repeated FRBs with an observable time delay. Considering the expected
FRB detection rate by upcoming experiments, such as CHIME, of tens of thousands of FRBs per
year, we should observe from tens to hundreds of repeated bursts yearly, if MACHOs in thiswindow make up all the dark matter. A null search for echoes with just 104 FRBs, would constrain
the fraction of dark matter in MACHOs to be smaller than 10% for all masses larger than 20M§ .

Adam Christopherson, University of Florida.

Astrophysical bounds on ultra light axion-like particles
Motivated by tension between the predictions of ordinary cold dark matter (CDM) andobservations at galactic scales, ultra-light axion-like particles (ULALPs), with mass of the order102 2eV have been proposed as an alternative CDM candidate. The ULALP fluid is ordinarily
described by classical field equations. However, we show that, like QCD axions, the ULALPs
thermalize by gravitational self-interactions and form a Bose-Einstein condensate, a quantum
phenomenon. A lower limit of order 102 3eV on the ULALP mass is obtained from the requirementthat the infall of ULALPs onto the galaxy does not excessively heat the galactic disk. A tighter
limit of order 102 0eV on the ULALP mass is obtained from the requirement that the wave natureof ULALP dark matter does not excessively smooth the caustic rings of the galaxy.

James Dent, University of Louisiana at Lafayette.

Dark Matter, Light Mediators, and the Neutrino Floor
The next generation of direct detection of dark matter experiments will be sensitive to an
irreducible background provided by coherent neutrino-nucleus scattering from solar neutrinos which
can well mimic low mass dark matter scattering. Within a general effective field theory framework
I will discuss which operators describing dark matter-nucleus elastic scattering will have theirdiscovery potential as a function of detector exposure saturated, which is known as the neutrino
floor. I will also show that this effect changes in character with the mass of the particle mediating
the scattering interaction. The distinguishability of dark matter recoils from backgrounds is vital,
and this work addresses this area of importance. This work is based on PRD 93 (2016) 075018,
arXiv:1602.05300 and work currently in progress with collaborators Bhaskar Dutta, Jayden
Newstead, and Louis Strigari.

73

Stacy Kim, The Ohio State University.

Constraining Self-Interacting Dark Matter through Equal Mass Galaxy Cluster Mergers
While the LCDM model has been wildly successful at explaining structure on large scales, it fails to
do so on small scales. Dark matter halos of scales comparable to that of galaxy clusters andsmaller are more cored and less numerous than LCDM predicts. One potential solution challenges
the canonical assumption that dark matter is collisionless and instead assumes that it isself-interacting. The most stringent upper limits on the dark matter self-interaction cross section
have come from observations of merging galaxy clusters. Self-interactions cause the merging dark
matter halos to evolve differently from the galaxies, which are effectively collisionless, which leads
to a spatial offset between the peaks in the dark matter and galaxy distributions. We show that inequal mass mergers, offsets matching those observed do not develop except under a narrow rangeof merger conditions that promote extreme dark mass loss during collision. Furthermore, offset
formation cannot be described by a drag force nor by tail formation alone, as has previously been
claimed. Self-interactions have a significant influence on other aspects of merger evolution, which
can be exploited to derive stronger constraints on the self-interaction cross section. In particular,
we expect a large fraction of BCGs in relaxed clusters to be miscentered by order 100s of kpc withcross sections greater than 1 cm2 /g; the lack of such large miscenterings implies a cross section nolarger than 0.1 cm2 /g.

Patrick Stengel, Stockholm University.

Charged Mediators in Dark Matter Scattering
We consider a scenario, within the framework of the MSSM, in which dark matter is bino-like anddark matter-nucleon spin-independent scattering occurs via the exchange of light squarks which
exhibit left-right mixing. We show that direct detection experiments such as LUX and SuperCDMS
will be sensitive to a wide class of such models through spin-independent scattering. Moreover,these models exhibit properties, such as isospin violation, that are not typically observed for the
MSSM LSP if scattering occurs primarily through Higgs exchange. The dominant nuclear physics
uncertainty is the quark content of the nucleon, particularly the strangeness content. We also
investigate parameter space with nearly degenerate neutralino and squark masses, thus enhancing
dark matter annihilation and nucleon scattering event rates.

PRIMORDIAL/INFLATION.
9-10:30 am Marco Drewes, TU Munich.

Experimental tests of leptogenesis
The extension of the Standard Model by heavy right handed neutrinos can simultaneously explain
the observed neutrino masses via the seesaw mechanism and the baryon asymmetry of the universe
via leptogenesis. If the mass of the heavy neutrinos is at or below the TeV scale, they can be foundin collider or fixed target experiments. We study the generation of the baryon asymmetry of theuniverse via low scale leptogenesis from first principles of nonequilibrium quantum field theory,
including spectator processes and feedback effects. This allows to derive predictions for theproperties of heavy neutrinos from the requirement to explain the observed baryon asymmetry of
the universe. If any heavy neutral leptons are found in the future, our predictions can be used as acriterion to assess whether these new particles can be responsible for the origin of matter in theuniverse.

74

Zachary Kenton, Queen Mary University of London.

The Separate Universe Approach to Soft Limits
In this talk I’ll calculate soft limits of n-point inflationary correlation functions using separate
universe techniques. Our approach naturally allows for multiple fields and leads to an elegant
diagrammatic approach. We apply this to the bispectrum and trispectrum, giving explicit formulae
for all possible single- and double-soft limits. When compared to previous work on the bispectrum
we find a 20% theoretical correction to observable parameters relevant for future cosmologicalexperiments. We also investigate consistency relations and present an infinite tower of inequalities
between soft correlation functions which generalise the Suyama-Yamaguchi inequality.

Austin Joyce, University of Chicago.

Three-dimensional inflation
There has been considerable recent interest in the soft limits of inflationary correlation functions,and restrictions placed upon them by symmetry considerations. Parallel to this, there has been aresurgence of interest in soft limits of flat-space scattering amplitudes, particularly with respect toasymptotic symmetries. I will describe a connection between these ideas in the context of inflationin three spacetime dimensions. In this case, the asymptotic symmetry transformations of
three-dimensional de Sitter space are in one-to-one correspondence with the adiabatic modes
familiar from cosmology. Further, these transformations lead to an infinite number of softtheorems for inflationary correlators.

Kohei Kamada, Arizona State University.

Large-scale magnetic fields and baryogenesis via chiral anomaly
It is known that time-dependent helical hypermagnetic fields can generate baryon (and lepton)
asymmetry through chiral anomaly. In this talk, I will show that if the present magnetic fields
indicated by the blazer observations is originated by a mechanism before the electroweak phasetransition, it is enough to explain the present baryon asymmetry of the Universe. While thismechanism does not generate B-L asymmetry, the electroweak sphaleron cannot wash out the B
and L asymmetry completely due to the source from the helical hypermagnetic fields.

Evangelos Sfakianakis, University of Illinois at Urbana-Champaign.

Magnetogenesis from axion inflation
The origin of magnetic fields in galaxies and intergalactic voids remains largely unknown. There
have been several attempts to provide a primordial magnetic field seed through inflation. I will
discuss magnetogenesis in models of axion inflation coupled to the hypercharge sector of theStandard Model through a Chern-Simons interaction term.
I will describe the use of lattice simulations to calculate the magnetic field strength, helicity andcorrelation length at the end of inflation. For a small value of the axion-gauge coupling strength
the results agree with no-back-reaction calculations and estimates found in the literature. For
larger couplings the helicity of the magnetic field differs from the no-back-reaction estimate anddepends strongly on the comoving wavenumber.
I will present a mechanism through which the hypercharge gauge bosons that populate thepreheated state thermalize and estimate the scattering rate of these particles into Standard Modelparticles. This scattering rate is efficient enough to allow the formation of a charged primordial
plasma with a high temperature within a few e-folds from the end of inflation.
Estimating the evolution of the magnetic fields until the present day, I will show that they can belarge enough to have phenomenological consequences (e.g. Blazar observations). This result isinsensitive to the exact value of the coupling, as long as the coupling is large enough to allow for
instantaneous preheating.

75

Naritaka Oshita, University of Tokyo.

A baby universe from a black hole
We investigate the effect of a black hole as a nucleation cite of a false vacuum bubble based on
the Euclidean actions of relevant configurations. As a result we find a wormhole-like configuration
may be spontaneously nucleated once the black hole mass falls below a critical value of order ofthe Hubble parameter corresponding to the false vacuum energy density. As the space beyond thewormhole throat can expand exponentially, this may be interpreted as creation of anotherinflationary universe in the final stage of the black hole evaporation.

76

COSMO-16 Participantsı Graeme Addison
Johns Hopkins University

ı Saroj Adhikari
University of Michigan

ı Peter Adshead
University of Illinois,
Physicsı Zeeshan Ahmed
SLAC National Lab

ı Rob AllenSam Houston State
University

ı Natacha Altamirano
Perimeter
Institute/University ofWaterlooı Mustafa Amin
Rice University

ı Haipeng An
Caltechı Stefano Anselmi
Case Western Reserve
University

ı Elena Aprile
Columbia University

ı Taketo Ariki
Nagoya University

ı Kam Arnold
University of
Wisconsin-Madisonı Taylor Baildon
University of Michigan

ı Nilanjan Banik
University of Florida

ı Neil Barrie
University of Sydneyı Sebastian Baum
OKC Stockholm

ı Brad Benson
University of Chicago

ı Stevie Bergman
Princeton University

ı Sanggyu Biern
Univ. of Zurich/APCTPı Simeon Bird
Johns Hopkins University

ı Jonathan Blazek
CCAPP Ohio State
University

ı Sebastian Bocquet
Argonne National
Laboratory

ı Celine Boehm
Durham University

ı Nadia Bolis
UC Davis

ı Jonathan Braden
University College London

ı Suddhasattwa Brahma
Fudan University

ı Benjamin Broerman
Queen’s University

ı Alessandra Buonanno
Max Planck Institute forGravitational Physics

ı Joyce Byun
University of Sussex

ı Robert Caldwell
Dartmouth College

ı Marcela Carena
Fermilabı John Carlstrom
University of Chicago

ı Sebastian Cespedes
University of Cambridge

ı Anthony Charles
University of Michigan

ı Xinyi Chen
University of Michigan

ı Chi-Ting Chiang
Stony Brook University

ı Kiwoon Choi
IBS

ı Adam Christopherson
University of Florida

ı David Cinabro
Wayne State University

ı Brian Cook
University of Michigan

ı Craig Copi
Case Western Reserve
University

ı Sam Cormack
Dartmouth College77ı Francis-Yan Cyr-Racine
Harvard University

ı Augusto Medeiros da
Rosa
Washington University in
St. Louis

ı Eric Dahl
Northwestern University

ı Liang Dai
Institute for AdvancedStudyı Anson D’Aloisio
University of Washington

ı Anne-Christine Davis
University of Cambridge

ı Bianca Davis
Ohio State University

ı Roland de Putter
Caltechı James Dent
University of Louisiana at
Lafayette

ı Joseph DeRose
Stanford University

ı Jennings Deskins
Case Western Reserve
University

ı Ema Dimastrogiovanni
ASU

ı Alexander Dolgov
Novosibirsk State
University

ı Marco Drewes
TU Munichı Adri Duivenvoorden
Stockholm University

ı Cora Dvorkin
Harvard University

ı Damien Easson
Arizona State University

ı David Edwards
University of Edinburghı Tim Eifler
JPL/Caltech

ı Maxim Eingorn
North Carolina Central
University

ı Jason Evans
KIASı August Evrard
University of Michigan

ı Xiao Fang
Ohio State University

ı Arya Farahi
University of Michigan

ı Matteo FasielloStanford University

ı Francesc Ferrer
Washington University in
St Louisı Christian Fidler
University Louvain la
Neuveı Katie Freese
University of Michigan

ı Carlos Frenk
Durham University

ı Josh Frieman
Fermilab/U. Chicago

ı Tomohiro Fujita
Stanford University

ı Praful GagraniKansas State University

ı Martina Gerbino
OKC and Nordita
Stockholm University

ı Tom Giblin
Kenyon College/CWRU

ı Jerome Gleyzes
Jet Propulsion
Laboratory/Caltech

ı Jinn-Ouk Gong
Asia Pacific Center for
Theoretical Physics

ı Pablo Gonzalez
Universidad de Chile

ı Elizabeth Gould
Perimeter Institute for
Theoretical Physics

ı Ruth Gregory
Durham University

ı Evan Grohs
University of Michigan

ı Jon Gudmundsson
Stockholm University

ı Vitali Halenka
University of Michigan

78ı Emil Hanzevackı Keisuke Harigaya
College of William & MaryUC Berkeley/LBNL

ı Takahiro Hayashinaka
RESCEU university of
Toyko

ı Chen Heinrichı Caroline Heneka
University of Chicago KICPNBI University of
Copenhagenı Mark Hertzberg
Tufts University

ı Shin’ichi Hirano
Rikkyo University

ı Christopher Hirata
The Ohio State University

ı Dan Hooper
Fermilabı Kevin Huffenberger
Florida State University

ı Matthew Hull
ı Johnathan Hung
ICG-Portsmouth University
University of Cambridge

ı Dragan Huterer
University of Michigan

ı Jai-chan Hwang
Kyungpook National
University

ı Derek Inman
University of Torontoı Mariana Jaber
UNAM

ı Mark Jackson
Fiat Physica

ı Inh Jee
Max-Planck Institute for
Astrophysics

ı Elise Jennings
Fermilabı Ryusuke Jinno
High Energy Accelerator
Research Organization(KEK)ı Traci Johnson
University of Michigan

ı Callum Jones
University of Michigan

ı Lawrence Jones
University of Michigan

ı Shahab Joudaki
Swinburne University

ı Austin Joyce
University of Chicago

ı Dhrubo Jyoti
Dartmouth College

ı Takaaki Kajita
University of Tokyoı Kohei Kamada
Arizona State University

ı Tanvi Karwal
Johns Hopkins University

ı Ronald Kashuba
LANL retired

ı Zachary Kenton
Queen Mary University of
Londonı Stacy Kim
The Ohio State University

ı Frank Koennig
ITP University of
Heidelberg

ı Kazunori Kohri
KEKı Eiichiro Komatsu
Max-Planck-Institut fr
Astrophysik

ı Savvas Koushiappas
Brown University

ı Elisabeth Krause
Stanfordı Anthony Kremin
University of Michigan

ı Florian Khnel
Stockholm University

ı Juliana Kwan
The University ofPennsylvania

ı Jounghun Lee
Seoul National University

ı Bohua Li
The University of Texas atAustinı Shi-Yu Li
Beijing Normal University

ı Andrei Linde
Stanford University

ı Tim Linden
The Ohio State University
79ı Mariangela LisantiPrinceton University

ı Hongwan Liu
MITı Lucas Lombriser
University of Edinburghı Andrew Long
University of Chicago

ı Wolfgang Lorenzon
University of Michigan

ı Kaloian Lozanov
University of Cambridge

ı Tony Lund
National Geographic

ı Joe Lykken
Fermilabı Joseph Lykken
Fermi National Accelerator
Laboratory

ı Maeve MadiganFermilabı Rachel Mandelbaumı Vuk Mandic
Carnegie Mellon University
University of Minnesota

ı Daniel Martens
The Ohio State University

ı Ali Masoumi
Tufts University

ı Grant Mathews
University of Notre Dameı Pieter Meerburg
CITA

ı James Mertens
Case Western Reserve
University

ı Joel Meyers
CITAı Marius Millea
Intitut Lagrange de Parisı Carisa Miller
UNCı Shuntaro Mizuno
Waseda University

ı Laura Monica Mocanu
The University of Chicago

ı Pablo Morales
The University of Tokyoı Pavel Motloch
University of Chicago

ı Emil Mottola
LANLı Eva-Maria Mueller
University of Portsmouth

ı Jessie Muir
University of Michigan

ı David Mulryne
Queen Mary University of
Londonı Shoaib Munir
KIAS

ı Julian Munoz
Johns Hopkins University

ı Ryan Muzio
Kenyon College

ı Tomohiro Nakama
Johns Hopkins University

ı Mohammad Hossein
NamjooHarvardı Tyler Natoli
Dunlap Instituteı Eva Nesbit
Kenyon/Syracuseı Laura Newburgh
Univ. of Torontoı Jayden Newstead
Arizona State University

ı Kaixuan Ni
ı Hyerim Noh
University of California San
Korea Astronomy andDiegoSpace Science Instituteı Brian Nord
Fermilabı Marcio O’Dwyer
CWRUı Minji Oh
KASI/USTı Chiamaka Okoli
Perimeter
Institute/University ofWaterlooı Isabel Mira Oldengott
Bielefeld University

ı Nicholas Orlofsky
University of Michigan

80ı Naritaka Oshita
The University of Tokyoı Sonia Paban
University of Texas atAustinı Tony Padilla
University of Nottinghamı Gonzalo Palma
FCFM University of Chileı Jong-Chul Park
Chungnam National
University

ı Evan Pease
Yale U./LBNL

ı Riccardo Penco
Columbia University

ı Malcolm Perry
Cambridge University

ı Annika PeterThe Ohio State University

ı Daniel Pfeffer
Johns Hopkins University

ı Caroline Popiel
Kenyon College

ı Chanda
Prescod-Weinstein
University of Washington

ı Andrea Quadri
INFN- Sezione di Pisa

ı Alexandra Rahlin
Princeton University

ı Hector Ramirez
University of Valencia

ı Raghavan Rangarajan
ı Kayla RedmondPhysical Research Institute
University of NC Chapel
Hillı Janina Renk
Stockholm University

ı Adam Riess
Johns Hopkins University

ı Adam Riess
JHU/STScIı Tanja Rindler-Daller
University of Vienna

ı Keir Rogers
University College London

ı Rachel Rosen
Columbia University

ı Leszek Roszkowski
NCBJ and Univ. of
Sheffield

ı Mario Runco
NASA-Johnson Space
Centerı Susan Runco
NASA-Johnson Space
Center

ı Benjamin Saliwanchik
University of kwazulu natal

ı Carles Sanchez
IFAE Barcelona

ı Viraj Sanghai
Queen Mary University of
Londonı Siddharth Satpathy
Carnegie Mellon University

ı Utane Sawangwit
National Astronomical
Research Institute ofThailandı Christoph Schmid
ETH Zurichı Denise Schmitz
California Institute ofTechnology

ı Timothy Scully
University of Illinois at
Urbana Champaign

ı Enrico Maria Sessolo
NCBJ Warsaw

ı Evangelos Sfakianakis
University of Illinois at
Urbana-Champaign

ı Daniel Shafer
Johns Hopkins University

ı Bibhushan Shakya
University of Michigan

ı Paul Shapiro
The University of Texas atAustinı Masato Shirasaki
National Astronomical
Observatory of Japanı Seth Siegel
McGill University

ı Pierre Sikivie
University of Florida

81ı Melanie Simetı Sukhdeep Singhı Tristan Smith
Carnegie Mellon University
Carnegie Mellon University
Swarthmore College
ı Bjoern Soergel
University of Cambridge

ı Douglas Spolyar
Stockholm University

ı George Stein
CITA University of Toronto

ı Patrick Stengel
Stockholm University

ı Dejan Stojkovic
SUNY at Buffalo

ı Henry Stoltenberg
UC Davis

ı Stephen Stopyra
Imperial College London

ı Kyle Story
Stanford University KIPAC

ı Gregory Tarle
University of Michigan

ı Eugene Tatum
Independent Researcherı Tommi Tenkanen
University of Helsinkiı Alexandra Terrana
York University &Perimeter Instituteı Jess Thorne
University of Western
Australia

ı Yukio Tomozawa
University of Michigan

ı Thomas Tram
University of Portsmouthı Sebastian Trojanowski
ı Krzysztof Turzynski
National Center for Nuclear
University of Warsaw
Research Poland / UC
Irvineı Caner Unal
University of Minnesota

ı Amol Upadhye
UW-Madisonı Phillip Urquijo
The University of
Melbourneı Sunny Vagnozzi
Oskar Klein Centre
Stockholm University &NORDITAı Monica Valluri
University of Michigan

ı Engelen Alexander van
CITAı Nelson Videla
Universidad de Chile

ı Anthony Villano
University of Minnesota

ı Luca Visinelli
Stockholm U / Norditaı Isaac Waldstein
University of North
Carolina at Chapel Hill

ı Mei-Yu Wang
Texas A&M University

ı Xin Wang
ı Scott Watson
University of California Los
Syracuse University
Angelesı Noah Weaverdyck
University of Michigan

ı Nicholas Weinberg
University of Michigan

ı Zach Weiner
University of Illinois
Urbana-Champaign

ı David Weir
University of Stavangerı Lee Whittaker
University of Manchesterı Matt Williams
KU Leuvenı Martin Winkler
Bonn University

ı Wang Kei Wong
ı Hao-Yi Wu
Carnegie Mellon University
California Institute ofTechnology82ı Kimmy Wu
UC Berkeley

ı Shuichiro Yokoyama
Rikkyo University

ı Mijin Yoon
University of Michigan

ı Mohammadreza Zakeri
UC Riversideı Ivonne Zavala
Swansea University

ı Sebastian Zell
Max Planck Institute forPhysics Munichı Tong-Jie Zhang
Beijing Normal University

ı Yuanyuan Zhang
Fermilabı Shuang-Yong Zhou
Case Western Reserve
University

ı Miguel Zumalacarregui
Nordita83

Code of Conduct
The organizers are committed to making this meeting productive and enjoyable for everyone,
regardless of gender, sexual orientation, disability, physical appearance, body size, race,
nationality or religion. We will not tolerate harassment of participants in any form. Please
follow these guidelines.
ı Behave professionally. Harassment and sexist, racist, or exclusionary comments or jokes
are not appropriate. Harassment includes sustained disruption of talks or other events,
inappropriate physical contact, sexual attention or innuendo, deliberate intimidation, stalking,and photography or recording of an individual without consent. It also includes offensive
comments related to gender, sexual orientation, disability, physical appearance, body size,
race or religion.
ı All communication should be appropriate for a professional audience including people ofmany different backgrounds. Sexual language and imagery is not appropriate.
ı Be kind to others. Do not insult or put down other attendees.
Any participant who wishes to report a violation of this policy is asked to speak, in confidence,
to Katie Freese (ktfreese@umich.edu) or Dragan Huterer (huterer@umich.edu). We wanteveryone to enjoy the conference!.

Program design by Taylor Baildon
84