cosmology with the cmb and its polarization

WILLIAM I. FINE THEORETICAL PHYSICS INSTITUTE

Cosmology with the CmB and its Polarization

January 14th to January 16th 2015

TABLE OF CONTENTS

Program..........................................................................................2

Abstracts.........................................................................................9

Participant List..............................................................................20 Talk Uploading Instructions..........................................................24 Maps Dining Guide........................................................................25 Skyway Map.........................................................................27

Poster Presentation List.................................................................28

TABLE

OF

CONTENTS

William I. Fine Theoretical Physics Institute Phone: (612) 624-7366School of Physics & Astronomy Fax: (612) 626-8606University of Minnesota [email protected] Church Street SE www.ftpi.umn.eduMinneapolis, MN 55455




1

Welcome to the COSMOLOGY WITH THE CMB AND ITS POLARIZATION workshop

We are delighted to host the workshop, “Cosmology with the CMB and its Polarization” held in downtown Minneapolis on Wednesday, January 14th to Friday, January 16th 2015 sponsored by our William I. Fine Theoretical Physics Institute. The purpose of the workshop is to assemble the US and international CMB community to assess the current status of experimental and theoretical studies, and to look forward to the future.

The workshop will start with several presentations on the full mission Planck results. There will then be a full review of the status of ground based and sub-orbital experimental programs, and of current theoretical aspects. We will also have a report on the upcoming European M4 proposal for a post-Planck space mission and a discussion about NASA’s plans for CMB and participation in M4. The workshop will end with a discussion regarding the next generation CMB S4 polarization project recently endorsed by the US P5 HEP advisory committee. With all the current activity in the field it should be an exciting meeting!

Scientific Organizing Committee:

Shaul Hanany, University of Minnesota Keith Olive, FTPI, University of Minnesota Marco Peloso, University of Minnestoa Clem Pryke, University of Minnesota




8:45 AM Registration Windows On Minnesota (Universe Room), The 50th floor of the IDSCenter 80 S 8th Street, Downtown Minneapolis

SESSION 1 - NEW RESULTS FROM PLANCK

9:00 AM Welcome and Opening Remarks Clem Pryke University of Minnesota

9:05 AM Planck overview / systematics Charles Lawrence JPL, California Institute of Technology

9:35 AM Cosmology from the Planck 2- and 4- point functions Anthony Challinor University of Cambridge

10:20 AM The astrophysics of dust polarization Francois Boulanger Institut d’ Astrophysique Spatiale, Orsay, France

10:50 AM COFFEE BREAK

11:15 AM Large scale polarization with Planck Matthieu Tristram LAL Orsay, France

11:45 AM Primordial non-Gaussianity: a post-Planck 2014 update Sabino Matarrese University of Padova, Italy

12:30 PM LUNCH BREAK Lunch is on your own. Please refer to the dining guide in the back of this booklet for options.

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WENESDAY, JANUARY 14TH

Windows On Minnesota (Universe Room), The 50th floor of the IDSCenter80 S 8th Street, Downtown Minneapolis

PRO GRAM




SESSION 2 - THEORETICAL ASPECTS 1

2:00 PM Implications of the scalar tilt for the tensor-to-scalar ratio Matias Zaldarriaga Institute for Advanced Study, Princeton, New Jersey

2:30 PM The primordial CMB 4-point function Kendrick Smith University of Waterloo

3:00 PM Signals and degeneracies of the primordial power spectrum Kevork Abazajian University of California, Irvine

3:30 PM COFFEE BREAK AND POSTER SESSION

4:10 PM Cosmic Infrared Background and Connections to Cosmic Microwave Background Asantha Cooray University of California, Irvine

4:40 PM Odd tensor modes from inflation Lorenzo Sorbo University of Massachusetts Amherst

5:10 PM SPHEREx: An All-Sky Spectral Survey to Probe Inflation Olivier Dore JPL, California Institute of Technology

5:30 PM Workshop Ends for the Day

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WENESDAY, JANUARY 14TH





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SESSION 3 - STATUS OF (FUNDED) SUBORBITAL EXPERIMENTS

9:00 AM Polarization Measurements with the South Pole Telescope Bradford Benson University of Chicago

9:30 AM Polarization and the Atacama Cosmology Telescope (ACT) Suzanne Staggs Princeton University

10:00 AM Results from POLARBEAR and plans for Simon’s Array Adrian Lee University of California at Berkeley


11:00 AM Results from BICEP2/Keck and plans for BICEP3 John Kovac Harvard University

11:30 AM Status of EBEX and plans for EBEX6k Shaul Hanany University of Minnesota

11:50 AM A First Post-flight Update on the SPIDER Mission Aurelien Fraisse Princeton University 12:10 PM The Primordial Inflation Polarization Explorer (PIPER) Alan Kogut NASA

THURSDAY, JANUARY 15TH


PRO GRAM




12:30 PM LUNCH BREAK Lunch is on your own. Please refer to the dining guide in the back of this booklet for options. 2:00 PM The Cosmology Large Angular Scale Surveyor (CLASS) Joseph Eimer Johns Hopkins University

2:15PM MKIDs for CMB studies Bradley Johnson Columbia University

2:25 PM QUBIC, C-BASS and Others Peter Timbie University of Wisconsin, Madison

SESSION 4 - THEORETICAL ASPECTS 2

2:45 PM Cosmological Neutrino Phenomology Lloyd Knox University of California, Davis

3:15 PM Gravitational lensing effects in CMB polarization Uros Seljak University of California, Berkeley

3:45 PM COFFEE BREAK AND POSTER SESSION

4:15 PM Primordial B-modes: Foreground modelling and constraints Carlo Contaldi Imperial College, London

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4:45 PM Did m2φ2 bite the dust? A closer look at ns and r Raphael Flauger Carnegie Mellon University

5:15 PM Constraining Fundamental Physics with Planck Graca Rocha JPL/Caltech

5:35 PM Workshop Ends for the Day

Workshop Banquet Held in the Windows on Minnesota

PLANETS ROOM on the 50th Floor of the IDS Center 6:00 PM Social Hour7:00 PM Dinner


Windows On Minnesota (Planets Room), The 50th floor of the IDSCenter80 S 8th Street, Downtown Minneapolis

PRO GRAM




SESSION 5 - THE FUTURE

9:00 AM The Large Scale Polorization Explorer Paolo de Bernardis University of Rome

9:30 AM Planck and post-Planck Simulations Julian Borrill Lawrence Berkeley National Laboratory

9:50 AM Future directions for a space experiment: to B or not to B Joseph Silk University of Oxford


10:45 AM PIXIE Dale Fixsen UMD and Goddard Space Flight Center

11:10 AM Probing the Inflationary Universe with the LiteBIRD Satellite Masashi Hazumi High Energy Accelerator Research Organization (KEK)

11:35 AM The COrE+ mission Jacque Delabrouille APC laboratory, Paris, France

12:00 PM Panel moderated discussion of future space missions TBA

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FRIDAY, JANUARY 16TH





1:00 PM LUNCH BREAK Lunch is on your own. Please refer to the dining guide in the back of this booklet for options.

SESSION 6 - CMB S4

2:00 PM CMB S4 Talks and discussion

5:30 PM Workshop Closing

Thank you for your participation!!!

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FRIDAY, JANUARY 16TH


PRO GRAM




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ABSTRACTS (alphabetical by speaker)

KEVORK ABAZAJIANUniversity of California, Irvine

Signals and degeneracies of the primordial power spectrumUsing the temperature data from Planck we search for departures from a power-law primordial power spectrum, employing Bayesian model-selection and posterior probabilities. We parametrize the spectrum with n knots located at arbitrary values of log k, with both linear and cubic splines. This formulation recovers both slow modulations and sharp transitions in the primordial spectrum. The power spectrum is well-fit by a featureless, power-law. A modulated primordial spectrum yields a better fit relative to Î›CDM at large scales, but there is no strong evidence for a departure from a power-law spectrum. Moreover, using simulated maps we show that a local feature can mimic the suppression of large-scale power. With multi-knot spectra we see only small changes in the posterior distributions for the other free parameters in the standard Î›CDM universe. We explore the degeneracy with other features of primordial power spectrum suppression, namely the effects of massive neutrinos.

BRADFORD BENSON University of Chicago

Polarization Measurements with the South Pole TelescopeI will give an overview of the SPTpol and SPT-3G experiments. SPTpol is a polarization-sensitive camera designed to measure the polarization of the cosmic microwave background (CMB) deployed on the 10 meter South Pole Telescope (SPT) in January 2012. I will present recent results of the E-mode and TE-mode CMB power spectra, derived from 100 square degrees observed in the first year of observations. Additionally I will show B-mode power spectra, measurements of the gravitational lensing potential, and briefly report on the status of the full 500 square degree SPTpol survey. Finally, I will discuss the status of SPT’s next-generation camera, SPT-3G, which will consist of 16,200 polarization-sensitive transition-edge sensors (TES), contained within 2700 multi-chroic pixels with observing bands centered at 95, 150, and 220 GHz, and scheduled to achieve first light in January 2016.




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JULIAN BORRILLLawrence Berkeley National Laboratory

Planck and post-Planck SimulationsSimulations play a critical role in CMB experiments, including optimizing instrument design and deployment, validating and verifying data analysis algorithms and implementations, and debiasing and uncertainty quantification of the analysis results. Generating simulation sets also poses significant challenges, both in ensuring that they faithfully reproduce the critical characteristics of an experimental dataset, and in optimizing their generating to allow for the production of very large ensembles of realizations for Monte Carlo analyses. In this talk I will describe these challenges in the context of the simulation pipeline used in support of the 2nd Planck data release, outline the resulting dataset and its possible extension to support post-Planck experiments, and comment on the developments that will be needed for the next generation of mission-class CMB experiments such as CMB-S4, LiteBIRD and COrE+.

FRANCOIS BOULANGERInstitut d’ Astrophysique Spatiale, Orsay, France

The astrophysics of dust polarizationThe Planck satellite has produced the first whole sky map of polarization|at sub-mm and mm wavelengths. This is an immense step forward from|earlier polarization observations of Galactic dust. The data is revealing a new|sky we have started to explore. For the first time, we have the data needed to characterize the structure of the Galactic magnetic field and its coupling with interstellar matter and turbulence, in the diffuse interstellar medium and molecular clouds. Our analysis of the data also involves the characterization of the polarization properties of dust. I will introduce the science questions we are investigating and review our published results. I will connect what we are learning on the astrophysics of dust polarization to the structure of the dusty polarized screen to CMB polarization at high Galactic latitudes.

ABSTRACTS




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JOHN CARLSTROMUniversity of Chicago

Building towards CMB-S4: A Next Generation Ground Based CMB Program

ANTHONY CHALLINORUniversity of Cambridge

Cosmology from the Planck 2- and 4-point functionsI review constraints on cosmological parameters from the Planck 2014 temperature and polarization data. Particular emphasis will be given to the extraction and interpretation of the effects of weak gravitational lensing.

CARLO CONTALDIImperial College, London

Primordial B-modes: Foreground modelling and constraints I will review the main characteristics of foreground polarization models that have been used to constrain dust and synchrotron polarized emission on large scales (l<100) where primordial B-modes are thought to dominate. These scales are being targeted by experiments such as BICEP/KECK and Spider.

ASANTHA COORAYUniversity of California, Irvine

Cosmic Infrared Background and Connections to Cosmic Microwave Background




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PAOLO DE BERNARDISUniversity of Rome

The Large Scale Polarization ExplorerThe LSPE is a balloon-borne mission aimed at measuring the polarization of the Cosmic Microwave Background (CMB) at large angular scales, and in particular to constrain the curl component of CMB polarization (B-modes) produced by tensor perturbations generated during cosmic inflation, in the very early universe. Its primary target is the detection of the power spectrum of B-modes at multipoles covering both the reionization peak and the recombination peak, with a sensitivity corresponding to r = 0.02, at 99.7% confidence. A second target is to produce wide maps of foreground polarization generated in our Galaxy by synchrotron emission and interstellar dust emission. These will be important to map Galactic magnetic fields and to study the properties of ionized gas and of diffuse interstellar dust in our Galaxy. The mission is optimized for large angular scales, with coarse angular resolution (around 1.5 degrees FWHM), and wide sky coverage (25% of the sky). The payload will fly in a circumpolar long duration balloon mission during the polar night. Using the Earth as a giant solar shield, the instrument will spin in azimuth, observing a large fraction of the northern sky. The payload will host two instruments. An array of coherent polarimeters using cryogenic HEMT amplifiers will survey the sky at 43 and 90 GHz. An array of bolometric polarimeters, using large throughput multi-mode bolometers and rotating Half Wave Plates (HWP), will survey the same sky region in three bands at 140, 220 and 240 GHz. The wide frequency coverage will allow optimal control of the polarized foregrounds, with comparable angular resolution at all frequencies.

JACQUE DELABROUILLEAPC laboratory, Paris, France

The COrE+ mission

ABSTRACTS




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OLIVIER DORE JPL, California Institute of Technology

SPHEREx: An All-Sky Spectral Survey to Probe Inflation SPHEREx (Spectro-Photometer for the History of the Universe, Epoch of Reionization, and Ices Explorer) is a proposed all-sky spectroscopic survey satellite designed to address all three science goals in NASA’s Astrophysics Division: probe the origin and destiny of our Universe; explore whether planets around other stars could harbor life; and explore the origin and evolution of galaxies. SPHEREx will scan a series of Linear Variable Filters systematically across the entire sky. The SPHEREx data-set will contain R=40 spectra spanning the near infrared(0.75$\mu$m$<\lambda<$4.83$\mu$m) for every 6.2 arcsecond pixel over the entire-sky. In this paper, we detail the extra-galactic and cosmological studies SPHEREx will enable and present detailed systematic effect evaluations.

JOSEPH EIMERJohns Hopkins University

The Cosmology Large Angular Scale Surveyor (CLASS)The Cosmology Large Angular Scale Surveyor (CLASS) is an experiment to measure the imprint of gravitational waves from inflation in the polarization of the cosmic microwave background. CLASS is a multi-frequency array of four telescopes to be deployed in the Atacama Desert in Chile. From this site, CLASS will observe 70% of the sky at four frequency bands centered at 38, 93, 148, and 217 GHz - designed to straddle the full-sky galactic foreground minimum. The large survey area enables CLASS to characterize the B-mode and E-mode power spectra on both the reionization and recombination scales. Simulations including the presence of foregrounds suggest the CLASS strategy of combining large sky coverage, control of systematic errors, signal stability, and high sensitivity will allow detection of the tensor-to-scalar ratio down to the level of r=0.01 and enable cosmic-variance-limited measurements of the optical depth to reionization. In this talk, I present an overview of the CLASS strategy for measuring the E-modes and B-modes at the largest angular scales and give an update on the project status.




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DALE FIXSEN UMD and Goddard Space Flight Center

PIXIETalk will include an examination of systematic effects of emission from mirrors,calibrator, grids and other areas within the PIXIE instrument. The systematiceffects of detector non-ideality and asymmetry will also be presented. Theseshow that the residual systematic effects do not jeopardize either the polarization or spectrum measurements and that there are sufficient safeguards to find andcalibrate out the most likely errors.

RAPHAEL FLAUGERCarnegie Mellon University

Did m2φ2 bite the dust? A closer look at ns and r I will review measurements of the angular power spectrum of temperature perturbations from Planck data by the Planck collaboration and by Renee Hlozek, David Spergel and myself and will discuss the small differences in the scalar spectral index between the two. I will then combine these measurements with the recent measurement of the polarization of the cosmic microwave background by BICEP2 as well as the measurements of polarized emission from dust by the Planck collaboration to derive the current (but soon outdated) constraints on the spectral index of scalar perturbations and the amount of primordial gravitational waves. I will show that the data now disfavors the simplest model of inflation at 2-3 sigma depending on the choice of likelihood for the temperature data.

AURELIEN FRAISSE Princeton University

A First Post-flight Update on the SPIDER MissionThe SPIDER balloon-borne polarimeter has been deployed to McMurdo, Antarctica, from where it will fly in December 2014. A second flight, featuring a different frequency coverage, is scheduled for December 2016. Careful control of instrumental systematics and a scanning strategy optimized to reduce the error in the reconstruction of the Stokes parameters will allow for a 3-sigma detection, in the presence of Galactic foregrounds, of the primordial B-mode signal in the Cosmic Microwave Background, provided that the tensor-to-scalar ratio r be greater than 0.03. SPIDER’s first flight will already provide competitive constraints; if polarized foreground emissions were negligible in the SPIDER field, we would detect the r=0.03 primordial B-mode signal after our first flight. In this

ABSTRACTS




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talk, I will review the goals, strategy, and status of the SPIDER experiment a few weeks after its inaugural launch.

SHAUL HANANYUniversity of Minnesota

Status of EBEX and plans for EBEX6kI will review the status of the analysis of data from the EBEX2012 flight and our plans for a follow up experiment EBEX6K

MASASHI HAZUMIHigh Energy Accelerator Research Organization (KEK)

Probing the Inflationary Universe with the LiteBIRD SatelliteLiteBIRD is a satellite to map the polarization of the CMB radiation over the full sky at large angular scales with the ultimate precision. Cosmological inflation, which is the leading hypothesis to resolve the problems in the Big Bang theory, predicts that primordial gravitational waves were created during the inflationary era. Measurements of polarization of the CMB radiation are known as the best probe to detect the primordial gravitational waves. The LiteBIRD working group is authorized by the Japanese Steering Committee for Space Science (SCSS) and is supported by JAXA. It has about 70 members from Japan, USA, Canada and Germany. Studies in the working group are in progress toward the mission definition review, with a target launch year in early 2020â€™s. The scientific objective of LiteBIRD is to test all the representative inflation models that satisfy single-field slow-roll conditions and lie in the large-field regime. To this end, the requirement on the precision of the tensor-to-scalar ratio, r, at LiteBIRD is equal to or better than 0.001. In case of large r values, as suggested by BICEP2, LiteBIRD will be able to scrutinize the power spectrum of the B-mode polarization to further narrow-down inflationary models. The design of the LiteBIRD system is driven by these scientific goals. A 3-year full sky survey will be carried out for at least 6 frequency bands between 50 and 320 GHz to achieve the total sensitivity of 1.8 microKarcmin with the angular resolution of 30 arcmin at 150 GHz. The key components of the mission payload include a half-wave plate system for signal modulation, two reflective mirrors with a diameter of about 60 cm, an array of superconducting polarimeters with distributed band centers for precise foreground removal, the readout system with high multiplexing factors in the frequency domain, and the cryogenic system to provide the 100 mK base temperature.




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LLOYD KNOXUniversity of California, Davis

Cosmological Neutrino PhenomologyI will review CMB signatures of cosmic neutrino number and mass.

ALAN KOGUTNASA

The Primordial Inflation Polarization Explorer (PIPER)The Primordial Inflation Polarization Explorer (PIPER) is a balloon-borne instrument to search for inflationary B modes on angular scales 30 arcmin to 90 degrees (2 < ell < 400). PIPER combines cold (1.5 K) optics, 5120 bolometric detectors, and rapid polarization modulation using VPM grids to achieve both high sensitivity and excellent control of systematic errors. A series of flights alternating between northern and southern hemisphere launch sites will produce maps in Stokes I, Q, U, and V parameters at frequencies 200, 270, 350, and 600 GHz (wavelengths 1500, 1100, 850, and 500 microns) covering 85% of the sky. We describe the PIPER instrument and discuss the current status and expected science returns from the mission.

JOHN KOVACHarvard University

Results from BICEP2/Keck and plans for BICEP3

CHARLES LAWRENCE JPL, California Institute of Technology

Planck overview/systematicsI will give an overview of the Planck 2015 results and discuss the most important systematics affecting the two instruments.

ABSTRACTS




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ADRIAN LEEUniversity of California at Berkeley

The POLARBEAR / Simons Array We will describe recent cosmic microwave background (CMB) results from the POLARBEAR-1 experiment and the future evolution of the POLARBEAR experiment to the Simons Array. POLARBEAR-1 has made a high significance detection of the B-mode gravitational-lensing deflection spectrum and a measurement of the “BB” B-mode autospectrum. We will describe a stringent set of tests for systematic errors and upper limits on foreground contamination. Finally, we will describe the Simons Array which will have three identical 3.5 meter diameter telescopes with a set of three bolometric array receivers that will have 22,764 bolometers distributed among 90, 150, and 220 GHz. The science goals include a deep search for the inflationary B-mode signal at degree-angular scales and a large-area survey to characterize gravitational lensing.

SABINO MATARRESEUniversity of Padova, Italy

Primordial non-Gaussianity: a post-Planck 2014 updateI will review the state of primordial (inflationary) non-Gaussianity after the Planck full mission temperature and polarization data analysis, also in view of recent theoretical achievements in this field.

GRACA ROCHAJPL/Caltech

Constraining fundamental physics with PlanckIn this talk we will present constraints on the temporal and spatial variation of fundamental constants such as fine structure constant, α, mass of the electron, me etc. and investigate the degeneracies with cosmological parameters such as H0 .




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UROS SELJAKUniversity of California, Berkeley

Gravitational lensing effects in CMB polarizationI will review the lensing effects in CMB polarization, both as a science driver and as a nuisance. I will discuss reconstruction methods and delensing methods to remove it from CMB polarization, and the ultimate reach of these methods in terms of gravity wave B modes.

JOSEPH SILKUniversity of Oxford

Future directions for a space experiment: to B or not to B

KENDRICK SMITHUniversity of Waterloo

The primordial CMB 4-point functionWe present a general framework for data analysis of the primordial 4-point function of the CMB. We classify physically motivated signals, discuss data analysis challenges, and present results from WMAP and Planck.

LORENZO SORBOUniversity of Massachusetts Amherst

Odd tensor modes from inflationThe existence of a primordial spectrum of gravitational waves is a generic prediction of inflation. Here I will discuss how the coupling of a pseudoscalar inflaton to a gauge field can induce, in a two-step process, gravitational waves with unusual properties such as: (i) a net chirality (ii) a blue spectrum (iii) being detectable in the (relatively) near future by ground-based gravitational

ABSTRACTS




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interferometers (iv) large nongaussianities even if the scalar perturbations are approximately gaussian.

SUZANNE STAGGSPrinceton University

Polarization and the Atacama Cosmology Telescope (ACT)

MATTHIEU TRISTRAMLAL Orsay, France

Large scale polarization CMB with PlanckI will show the last results on CMB large scale anisotropies based on new Planck 2014 results. In particular, I will give the best current constraints on the reionization history as well as the Planck estimate of the tensor-to-scalar ratio.

MATIAS ZALDARRIAGAInstitute for Advanced Study, Princeton, New Jersey

Implications of the scalar tilt for the tensor-to-scalar ratio




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WORKSHOP PARTICIPANT LIST

Kevork AbazajianUniversity of California, [email protected]

Francois AubinUniversity of [email protected]

Chaoyun BaoUniversity of [email protected]

Darcy BarronUC San [email protected]

Bradford BensonUniversity of [email protected]

Colin BischoffHarvard-Smithsonian Center for [email protected]

Julian [email protected]

Francois BoulangerInstitut d’Astrophysique [email protected]

Sean BryanArizona State [email protected]

Victor BuzaHarvard [email protected]

John Carlstrom University of [email protected]

Anthony ChallinorUniversity of [email protected]

Carlo ContaldiImperial College [email protected]

Asantha CoorayUniversity of California, [email protected]

Abigail CritesCalifornia Institute of [email protected]

S. Gwynne CrowderUniversity of [email protected]

Francis-Yan Cyr-RacineCaltech/[email protected]

Francesco De BernardisCornell [email protected]

Paolo de BernardisDipartimento di Fisica, Sapienza UniversitÃ di [email protected]

Jacques [email protected]

Olivier Dore JPL, California Institute of Technology [email protected] Joseph EimerJohns Hopkins [email protected]

Jason EvansUniversity of Minnesota/[email protected]

Dale [email protected]

Raphael FlaugerCarnegie [email protected]

Stefan FliescherUniversity of [email protected]

Aurelien FraissePrinceton [email protected]

Melanie GallowayUniversity of [email protected]

Marcos Garcia GarciaUniversity of [email protected]

Christopher GeachUniversity of [email protected]

PARTICIPANTS




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Krzysztof GorskiJPL/[email protected]

Riccardo Gualtieri Sapienza, University of Rome [email protected] Nils HalversonUniversity of [email protected]

Shaul HananyUniversity of [email protected]

Kathleen HarringtonJohns Hopkins [email protected]

Masashi HazumiKEK / Kavli [email protected]

Kyle HelsonBrown [email protected]

Shawn HendersonCornell [email protected]

Jason HenningUniversity of [email protected]

Zhiqi HuangUniversity of [email protected]

Hannes HubmayrNIST, [email protected]

Bradley JohnsonColumbia [email protected]

Lloyd KnoxUC [email protected]

Al KogutNASA / [email protected]

John KovacHarvard [email protected]

Chao-Lin KuoStanford/[email protected] Akito Kusaka Lawrence Berkeley National Laboratory [email protected]

Charles [email protected]

Adrian LeeUniversity of California, [email protected]

Marilena LoverdeUniversity of [email protected]

Amy LowitzUniversity of Wisconsin - [email protected]

Mathew MadhavacherilStony Brook [email protected]

Vuk MandicUniversity of [email protected]

Silvia MasiDipartimento di Fisica, Sapienza UniversitÃ di [email protected]

Sabino MatarresePhsyics & Astronomy Dept. G. Galilei, University of Padova, [email protected]

Philip MauskopfArizona State [email protected]

Jeff McMahonUniversity of [email protected]

Amber MillerColumbia [email protected]

Michael MilliganUniversity of Minnesota Supercomputing [email protected]




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Tyler NatoliUniversity of [email protected] Thomas NelsonMinnesota Institute for [email protected] Keith OliveUniversity of [email protected] Lyman PagePrinceton [email protected]

Marco PelosoUniversity of [email protected]

Clem PrykeUniversity of [email protected]

Yong-Zhong QianUniversity of [email protected]

Kate RaachUniversity of [email protected]

Graca RochaJPL/[email protected]

Lawrence RudnickUniversity of [email protected]

Michael RutkowskiUniversity of [email protected] Benjamin SaliwanchikCase Western Reserve [email protected] Kevin Sebesta University of Minnesota [email protected] Neelima SehgalStony Brook [email protected]

Uros SeljakUC [email protected]

Christopher SheehyUniversity of Chicago, [email protected]

Joe [email protected]

Evan SkillmanMinnesota Institute for [email protected]

Kendrick SmithPerimeter [email protected]

Lorenzo SorboUniversity of Massachusetts, [email protected]

Suzanne StaggsPrinceton [email protected]

Zak StaniszewskiCalifornia Institute of [email protected]

Albert [email protected]

Meng [email protected]

Zachary ThomasUniversity of [email protected]

Peter TimbieUW [email protected]

Matthieu [email protected]

Caner UnalU of [email protected]

Joaquin VieiraUniversity of [email protected]

PARTICIPANTS




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WORKSHOP BANQUET WILL BE HELD IN THE PLANETS ROOM 50TH FLOOR OF THE IDS CENTER THURSDAY, JANUARY 15TH AT 6:00 PM

Liliya WilliamsMinnesota Institute for [email protected]

Edward WollackNASA Goddard Space Flight [email protected]

Karl YoungUniversity of [email protected]

Matias ZaldarriagaInstitute for Advanced [email protected]

Jiaming ZhengSchool of Physics and Astronomy, [email protected]


WIRELESS INTERNETWorkshop guests may access the Hotel Wi-Fi with the username and passwords on tent cards located around the room. Please ask workshop staff if you have any questions or concerns.




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INSTRUCTIONS FOR UPLOADING TALKS TO THE WORKSHOP WEBSITE

Please submit a PDF (preferred format) of your talk slides by Friday, February 13, 2015 to be included in the conference web archive. Please include your name in the file name.

1. Use the following link to access the folder: 2015CMBWorkshop:

https://netfiles.umn.edu/xythoswfs/webview/_xy-17179605_1

2. Click on the “Upload” icon at the top right of the page

3. Select your file and click “Start Upload”

The folder page should populte with your file. Alternatively, the screen may display this message: “The document was successfully uploaded to the folder, 2015CMBWorkshop” It may also tell you that the directory is empty, but this just means that you may not have permission to see the files.

All submitted talks will be archived online for general access at the University of Minnesota’s Digital Conservancy. By submitting your talk slides you are agreeing to the Digital Conservancy’s Copyright policy. For policy details see the website at: http://conservancy.umn.edu

Please note that there will be a delay between your upload and final posting on the workshop website. Once all talks have been submitted, participants will be notified by email. As always, any questions may be addressed to [email protected].

***If you are having problems uploading your PDF please email it to the workshop email address [email protected]***

UP L OADING

TALK S




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WORKSHOP DINING GUIDE




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D I N I N G G U I D E




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POSTER SESSION

Component Separation Method for Cosmic Microwave Background PolarimetersChaoyun Bao

University of Minnesota

Development and characterization of the readout system for POLARBEAR-2Darcy Barron

University of California, San Diego

Not all Relativistic Species are Born Equal: Moving Beyond Free-Streaming RadiationFrancis-Yan Cyr-Racine

Caltech/JPL

Constraining cosmology with forthcoming kinematic Sunyaev-Zel’dovich measurementsFrancesco De Bernardis

Cornell University

The Cosmology Large Angular Scale SurveyorKathleen Harrington

Johns Hopkins University

Detector Arrays and Readout for AdvACTPolShawn HendersonCornell University

Peak statistics and Stacking -- Is the CMB Sky Statistically Isotropic and Gaussian?Zhiqi Huang

University of Toronto

Feedhorn-coupled TES focal plane technology for CMB observationsHannes Hubmayr

NIST, Boulder

Design, fabrication, and testing of lumped element kinetic inductance detectors for 3 mm CMB Observations

Amy LowitzUniversity of Wisconsin - Madison

pOSTERS




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ACTPol: Detection of Lensing of the Cosmic Microwave Background by

Dark Matter Halos Mathew Madhavacheril Stony Brook University

OLIMPO: a low-resolution balloon-borne spectrometer for the Sunyzev-Zeldovich effectSilvia Masi

Dipartimento di Fisica, Sapienza UniversitÃ di Roma

Kinetic inductance detectors for CMB polarization experimentsPhilip Mauskopf

Arizona State University




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Thank you for your participation in our workshop

“Cosmology with the CMB and its Polarization”!

cosmology with the cmb and its polarization

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