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Latest results, current data-analysis and upcoming upgrades of the

POLARBEAR/Simons Array experiments

Dominic Beck (APC, Université Paris Diderot)

on behalf of the POLARBEAR/Simons Array collaboration

53rd Rencontres de Moriond, La Thuile, Italy 2018-03-18

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Context of CMB B-Mode Measurements

Cre

dits: Y

uji

Ch

ino

ne

large angular scales to targetmeasurement of tensor-to-scalar ratio r

to constrain Inflation theories

in the presence of galactic foregrounds, atmosphere emission and limited by instrumental

sensitivity, systematics, etc.

small angular scales to targetmeasurements of CMB lensing

tracing large-scale structure in the universe

restricted by instrumental sensitivity, resolution, systematics, astrophysical foregrounds, etc.

B

E

primordialgravitational

waves

B

matter along line

of sight

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POLARBEAR CollaborationInstitute D’AstrophysiqueSpatialeGiulio Fabbian

UC BerkeleyShawn Beckman

Darcy Barron

Yuji Chinone

Ari Cukierman

Tijmen de Haan

Neil Goeckner-Wald

John Groh

Charles Hill

William HolzapfelOliver JeongAdrian LeeDick PlambeckChris RaumPaul RichardsAritoki SuzukiBen Westbrook

Kavli IPMUDaisuke KanekoNobuhiko KatayamaFrederick Matsuda

Tomotake Matsumura

Lawrence Berkeley NLJulian BorrillReijo Keskitalo

Theodore KisnerAkito KusakaEric LinderAlex MadurowiczBlake SherwinRaymond Tat

CU BoulderNils HalversonGreg JaehnigHayley Roberts

UC San DiegoKam Arnold

Kevin Crowley

Tucker Elleflot

George Fuller

Nicholas Galitzki

Logan Howe

Brian Keating

David Leon

Lindsay Lowry

Martin Navaroli

Gabriel Rebeiz

Max Silva-Feaver

Praween Siritanasak

Grant Teply

Calvin Tsai

Alex Zahn

KEKYoshiki Akiba

Takaho Hamada

Masaya Hasegawa

Masashi Hazumi

Yuto MinamiHaruki Nishino

Yuuko Segawa

Osamu Tajima

Satoru Takakura

Sayuri Takatori

Daiki Tanabe

Takayuki Tomaru

DalhousieScott Chapman

Colin Ross

Kaja Rotermund

Alexei Tikhomirov

Cardiff UPeter Ade

Imperial CollegeAndrew Jaffe

Daisy Mak

McGill UniversityMatt DobbsAdam GilbertJosh Montgomery

Laboratoire

Astroparticule &

Cosmologie

Dominic Beck

Josquin Errard

Maude Le Jeune

Radek Stompor

Clara Vergès

NASA GoddardNathan Miller

Católica (PUC)David BoettgerRolando Dunner

U. MelbourneFederico BianchiniChristian ReichardtAnh Pham

SISSACarlo BaccigalupiNicoletta

KrachmalnicoffDavide Poletti

UC IrvineChang Feng

Argonne NLAmy Bender

And many more in years past…

Laboratoire de l'accélérateur linéaireJulien Peloton

U Manchester

Gabriele Coppi

Andrew May

Lucio Piccirillo

U ChileMario Aguilar

C Computational AstrophysicsStephen Feeney

Stanford UGiuseppe Puglisi

UC Los Angeles

Nathan Whitehorn

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POLARBEAR Collaboration

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5

• Focal plane temperature 250 mK

• 1,274 TES bolometers at 150 GHz

• Lenslet-coupled double slot antennas

POLARBEAR-1

↑私

• Off-axis Gregorian-Dragone design

• 2.5 m primary mirror

• 3.5‘ FWHM beam

• Located in the Atacama desert, Chile

• 5,200 m above sea level

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B-Mode Measurement Campaigns of POLARBEAR-1

First light in Chile in January 2012

Initial science results•Reject null B-mode spectrum at 97.2% confidence level [POLARBEAR collaboration 2014c]• Lensing auto power spectrum from polarized CMB at 4.2 σ [POLARBEAR collaboration 2014a]•Cross correlation lensing power spectrum with CIB HERSCHEL-ATLAS at 4.0 σ [POLARBEAR

collaboration 2014b]

Second season results [POLARBEAR collaboration 2017]Installed continuously rotating half wave plateStarted large patch (20×35 degree) observations

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B-Mode Measurement Campaigns of POLARBEAR-1

RA12

RA4p5RA23

large patch

80 % of the sky observable by

POLARBEAR

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• Two-year observation of three 3×3 degree patches

• Adding 61 % of data volume to first season data: 5 𝜇𝐾-arcmin in deepest patch

• Improved calibration and instrumental systematic/foreground estimation

• Implementation of a second data analysis pipeline [Poletti et al 2017]

POLARBEAR-1 Second Season ResultsPOLARBEAR Collaboration ApJ 848, 121 (2017)

PIP

EL

INE

AP

IPE

LIN

E B

PLANCK temperature

(SMICA)

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The Data Analysis Pipeline

POLARBEAR-1 Second Season ResultsPOLARBEAR Collaboration ApJ 848, 121 (2017)

simulating instrumental systematic effects𝐶ℓ𝐵𝐵 statistical uncertainty

combination

PointingPolarization angle

Relative gain-calibrationGain drift

Readout crosstalkDifferential beam shape

Differential beam ellipticity

• Implementation of a second and complementary pipeline for more robust results through consistencychecks and improved systematic error control

• Analysis performed blind and validated by passing a suite of null-tests and simulating instrumental systematic effects

• The systematics pipeline follows exactly all the data analysis pipeline steps

𝐶ℓ𝐵𝐵

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POLARBEAR-1 Second Season ResultsPOLARBEAR Collaboration ApJ 848, 121 (2017)

3.1𝜎 rejection of no B-modes

Reduced band-power uncertainties by factor two

Measured amplitude of lensing B-modes:𝐴𝐵𝐵 = 0.60−0.24

+0.26 stat. −0.04+0.00 inst. ± 0.14 foreground ± 0.04 mult.

Lensing auto power spectrum in preparation

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POLARBEAR-1 Third Season (2014+): CRHWP

Detectors

• Demonstrated 1/f noise suppression in [Takakura et al 2017]• B-mode power spectrum at degree angular-scales in preparation

Input polarizationOutput polarization

(Credits: Satoru Takakura)

ωt

Atmosphere produces noise in temperature which is correlated among detectors→ Low frequency (1/f) noise through T→P leakage challenging for large-scale B-mode

detection→ Continuously rotating half wave plate at prime focus, which modulates sky polarization

at 8 Hz→ Allows for subtraction of T→P leakage

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• Broadband sinuous antennas

• 7,588 bolometers observing in 95 GHz and 150 GHz band

• Nominal array sensitivity of 5.8 𝜇𝐾𝐶𝑀𝐵 𝑠(150 GHz) [Suzuki et al 2015]

• Broadband HWP at secondary focus [Hill and Beckman et al 2016]

POLARBEAR-2a

POLARBEAR-1

150 GHz

1,274 detectors

2.3° field-of-view

POLARBEAR-2

95/150 GHz

7,588 detectors

4.8° field-of-view

19 cm

36.5 cm

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• 3 receivers, 22,764 bolometers total, observing in four frequency bands

• Full array projected to achieve ~ 2.5 𝜇𝐾𝐶𝑀𝐵 𝑠

Simons Array

POLARBEAR-2a

95 / 150 GHz

POLARBEAR-2b

95 / 150 GHz

POLARBEAR-2c

220 / 270 GHz

currently housing POLARBEAR-1

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Will be deployed in a few months!

Will be deployed later this year

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• 3 receivers, 22,764 bolometers total, observing in four frequency bands

• Full array projected to achieve ~ 2.5 𝜇𝐾𝐶𝑀𝐵 𝑠

Simons Array

Science prospects [Stebor et al 2016]

• 𝜎 ∑𝑚𝜈 = 40 𝑚𝑒𝑉 (with DESI BAO, including foreground contamination)

• 𝜎 𝑟 = 0.1 = 6 × 10−3

• cross-correlations

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POLARBEAR-2a

95 / 150 GHz

POLARBEAR-2b

95 / 150 GHz

POLARBEAR-2c

220 / 270 GHz

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Results with POLARBEAR-1

• Lensing power spectrum: POLARBEAR Collab. PRL 113, 021301 (2014a)

• Galaxy cross-correlation: POLARBEAR Collab. PRL 112, 131302 (2014b)

• One-year angular power spectrum: POLARBEAR Collab. ApJ 794, 171 (2014c)

• Constraints on cosmic birefringence and primordial magnetic fields: POLARBEAR Collab. PRD 92, 123509 (2015)

• Unbiased mapmaking technique: Poletti et al A&A Vol 600 (2017)

• Two-year angular power spectrum: POLARBEAR Collab. ApJ 848, 121 (2017)

• Continuously rotating HWP demonstration: Takakura et al JCAP 05 008 (2017)

• Two-year deflection power spectrum in preparation

• Ongoing large patch analysis

POLARBEAR-2: Inoue et al SPIE 2016

Simons Array: Stebor et al SPIE 2016

…and there is more: Josquin will present the Simons Observatory on Thursday!

Summary

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