LiteBIRD: A future satellite mission on CMB polarization

Yuto MINAMI for the LiteBIRD team

KEK2016/12/14 1

LiteBIRD

High energy for new physics search

2016/12/14 2

http://atlasexperiment.org/etours_physics/etours_physics13.html

We searched for new physics with increasing energyHow can we access the very high energy, like GUT scale?

GUT

Use the space!

LiteBIRD

Before the topics of the space …

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𝑚 𝑔 :𝑚 𝜒10 = 6: 1

My previous study is gluino search in the ATLAS

AT LASt, I only excluded gluino masses ≲ 1.5 TeV

LiteBIRD

Inflation

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Exponential expansion of space in the early universe

Hope to explore GUT-scale physics The potential of single field slow-roll model is

Bock et al. (2006, astro-ph/0604101)

𝑉1/4 ~ 1.04 ⋅𝑟

0.01

1

4× 1016 GeV

r: tensor-to-scalar ratioPower-spectrum ratio of the tensor type perturbation and scalar type perturbation

Two types of fluctuation in inflationscalar : density tensor: primordial gravitational wave

(PGW)

~1016 GeV ?

LiteBIRD

Cosmic microwave background (CMB)

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CMB is the relic radiation of hot big bang PGW polarizes CMB in the last scattering just before the

recombination

Test the inflation with CMB!

LiteBIRD

Last scattering at recombination

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http://background.uchicago.edu/~whu/intermediate/polarization/polar1.html

LiteBIRD

E-mode and B-mode polarization

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Primordial gravitational wave

Tensor perturbationScalar perturbation

density

B-mode search is needed to determine r!

r = (tensor perturbation)/(scalar perturbation)

LiteBIRD

Lensing B-mode

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• Better ns from E-mode• Sum of neutrino masses• (Early) Dark energy

E-modes

B-modes atsub-deg. scale

Planck Team

LiteBIRD

Some major measurements for CMB

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Planck WMAP

SPT-pol

BICEP2Keck-Array

South pole

(BICEP2 x 5)

POLARBEAR

LiteBIRD

B-mode power spectrum: measurements status

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PrimordialGravitational waves

LensingBICEP

POLARBEAR

PLANCK

EBEX, (SPIDER)

Satellite

Balloon

After the spherical harmonics transformation

Ground

Large scale Small scale

LiteBIRD

B-mode power spectrum: structures

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Two bumps in ℓ < 200B-mode search in low ℓ region is needed

Observe the full sky with satellite!

Small scaleLarge scale

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Future satellite missions

• LiteBIRD• JAXA-led strategic large mission candidate

• Strong US participation

• The only project in Phase-A (both JAXA and NASA)

• Phase-A1 in JAXA !

• Target launch in 2025

• PIXIE• NASA small PI-led mission proposal Feb 2011, not

selected

• Re-propose to next MIDEX AO (2016 Dec)

• COrE• Mission for ESA M5

• Proposal submitted in Oct 2016

• Planned launch date of 2029-2030

LiteBIRD

Advantages in space

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Frequency bands are much less limited No atmospheric noise Can observe the full sky and lowest multipoles

both bumps Lensing B-mode small even for r <0.01

John Ruhl cmb@50 princeton, june 2015(Atmospheric spectra from “am” model, thanks to Stevie Bergman and Bill Jones)https://www.cfa.harvard.edu/~spaine/am/

Absorption spectrum by molecular in the air

LiteBIRD

LiteBIRD: Lite (Light) Satellite for the studies of B-mode polarization and Inflation from cosmic background Radiation Detection (http://litebird.jp/ )

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LiteBIRD is a next generation scientific satellite aiming to measure polarization of Cosmic Microwave Background (CMB) at unprecedented sensitivity.

Full success mission requirements: Measurement of B-mode polarization spectrum of large angular scale (𝟐 ≤ ℓ ≤ 𝟐𝟎𝟎) by three-year observation of all sky. Measurement of the tensor-to-scaler ratio r, that represents primordial gravitational waves, at 𝜹𝒓 < 𝟎. 𝟎𝟎𝟏 precision. （w/o subtracting the gravitational lensing effect.）

LiteBIRD group

139 members, international and interdisciplinary (as of May 1, 2016)

JAXAT. Dotani

H. Fuke

H. Imada

I. Kawano

H. Matsuhara

T. Matsumura

K. Mitsuda

T. Nishibori

K. Nishijo

A. Noda

A. Okamoto

S. Sakai

Y. Sato

K. Shinozaki

H. Sugita

Y. Takei

S. Utsunomiya

T. Wada

R. Yamamoto

N. Yamasaki

T. Yoshida

K. Yotsumoto

Osaka U.S. Kuromiya

M. Nakajima

S. Takakura

K. Takano

Osaka Pref. U.M. Inoue

K. Kimura

H. Ogawa

N. Okada

Okayama U.T. Funaki

N. Hidehira

H. Ishino

A. Kibayashi

Y. Kida

K. Komatsu

S. Uozumi

Y. Yamada

NIFSS. Takada

Kavli IPMUK. Hattori

N. Katayama

Y. Sakurai

H. Sugai

KEKM. Hazumi

(PI)

M. Hasegawa

N. Kimura

K. Kohri

M. Maki

Y. Minami

T. Nagasaki

R. Nagata

H. Nishino

S. Oguri

T. Okamura

N. Sato

J. Suzuki

T. Suzuki

O. Tajima

T. Tomaru

M. Yoshida

Konan U.I. Ohta

NAOJA. Dominjon

T. Hasebe

J. Inatani

K. Karatsu

S. Kashima

T. Noguchi

Y. Sekimoto

M. Sekine

Saitama U.M. Naruse

NICTY. Uzawa

SOKENDAIY. Akiba

Y. Inoue

H. Ishitsuka

Y. Segawa

S. Takatori

D. Tanabe

H. Watanabe

TITS. Matsuoka

R. Chendra

Tohoku U.M. Hattori

Nagoya U.K. Ichiki

Yokohama

Natl. U.T. Fujino

F. Irie

H. Kanai

S. Nakamura

T. Yamashita

RIKENS. Mima

C. Otani

APC ParisR. Stompor

CU BoulderN. Halverson

McGill U.M. Dobbs

MPAE. Komatsu

NISTG. Hilton

J. Hubmayr

Stanford U.S. Cho

K. Irwin

S. Kernasovskiy

C.-L. Kuo

D. Li

T. Namikawa

W. Ogburn

K. L.

Thompson

UC Berkeley /

LBNLD. Barron

J. Borrill

Y. Chinone

A. Cukierman

T. de Haan

N. Goeckner-wald

P. Harvey

C. Hill

W. Holzapfel

Y. Hori

O. Jeong

R. Keskitalo

T. Kisner

A. Kusaka

A. Lee(US PI)

E. Linder

P. Richards

U. Seljak

B. Sherwin

A. Suzuki

P. Turin

B. Westbrook

N. Whitehorn

UC San DiegoT. Elleot

B. Keating

G. RebeizSuper-conducting

detector developers

CMB

experimenters

IR astronomers

JAXA engineersX-ray

astrophysicists

U. TokyoS. Sekiguchi

T. Shimizu

S. Shu

N. Tomita

Kansei

Gakuin U.S. Matsuura

U. WisconsinK. Arnold

Paris ILPJ. Errard

U. TsukubaM. Nagai

Cardiff U.G. Pisano

15

Kitazato U.T. Kawasaki

LiteBIRD

Main specifications

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Orbit :L2 halo Planck is in L2 Lissajous

Launch year: 2025 For 3 years

Frequencies :40-400 GHz (15 bands) Sensitivity: 3 μK arcmin with margin

Planck: ~20 μK arcmin at 150 GHz

LiteBIRD

What r would be targeted?

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D. Baumann

Target is Lyth bound (r>0.002)!

Search for large field, Δ𝜙 = 𝜙𝐶𝑀𝐵 − 𝜙𝑒𝑛𝑑 > 𝑀𝑝

δr < 0.001 is needed to rule out large field models with 95% C.L.

Lyth bound

𝑟 ≲ 0.00260

𝑁𝑠𝑙𝑜𝑤

2Δ𝜙𝑠𝑙𝑜𝑤𝑀𝑝

2

LiteBIRD

Prospects of LiteBIRD

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LiteBIRD

LiteBIRD

Extra success

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Delensing with ground measurement Removing lensing B-mode

Make δr smaller

Telescope arrays on ground 30 ≤ l ≤ 3000~10000 e.g. Simons array

LiteBIRDσ(r)<0.001 2 ≤ l ≤ 200 Smaller δr

Full success Delsensing

LiteBIRD

Other physics? 1 : τ (optical depth) and neutrino mass

2016/12/14 20

Better E-mode measurement for ℓ<20 improves τ Better τ improves Σmν

Σmν > 58 meV from oscillation measurements

Low ℓ measurement could improve the Σmν measurement

Credit:RupertAllison

LiteBIRD

Credit:RupertAllison

LiteBIRD

Credit:RupertAllison

LiteBIRD

LiteBIRD

Other physics? 2 : Origin of gravitational waves

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Vacuum fluctuation Source fields vs.

Observation of ℓ < 10 is required

to distinguish between two

B-mode bi-spectrum (“BBB”) is

also used to detect source-field-

originating non-Gaussianity

At LiteBIRD, this can be done at

>3s

“Pseudoscalar model” from Namba, Peloso, Shiraishi,

Sorbo, Unal, arXiv1509.07521 as an “evil example

model”; indistinguishable w/ BB for ℓ> 10 alone.

M. Shiraishi, C. Hikage, T. Namikawa, R. Namba, M.Hazumi, arXiv:1606.06082

LiteBIRD

For the success of LiteBIRD

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Foreground removal Synchrotron and dust emissions

Reduction of systematic uncertaintiesScan strategy (point knowledge),

calibration, and so onLow instrumental errorCryogenic sensitive detectors

Need

LiteBIRD

Foreground removal : Synchrotron and dust

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Foreground candidates are Synchrotron emission Dust thermal emission

Template fitting method is planned to remove the foregroundsApJ 737, 78 (2011)

r

LiteBIRD

Scan Strategy: Orbit

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LiteBIRD

Scan Strategy: ongoing studies

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S.Uozumi, JPS2016

Scan strategy study is currently ongoing Decide scan parameter Removal of time-dependent effect etc…

Systematics could be reduced by revisiting the same sky pixel

Revisit time uniformity study

LiteBIRD

LiteBIRD instruments

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LiteBIRD

Continuous rotating Half-Wave Plate (HWP)

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1. Modulate the polarized sky signal Reduce 1/f noise

2. Measure polarization with one detector Reduce systematics from gain of different detectors

JPS_Sep2016_23aSR-9, Sakurai et al.

LiteBIRD

Continuous rotating HWP components

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T. Matsumura et al., Appl. Opt. 55 (2016)3502

HWP lens: Anti-reflection coatings on sapphire substrateRotational system: Superconducting magnetic bearing

Minimize the vibration, and heat from friction

Surface of the HWP

LiteBIRD

HWP lens radiation tests

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In L2, LiteBIRD will be exposed in high energy cosmic rays90%:proton, 10%: α

Radiation test with 160 MeV proton beam Total flux equals to 5 year observation in L2

No significant difference in refractive index, and tanδ(related to absorption)

LiteBIRD

Focal plane detectors

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1. Low Frequency Telescope (LFT) arrays: 12 bands in 40-235 GHz2. High Frequency Telescope (HFT) arrays: 3bands in 280-402 GHz

LFT arraysHFT arrays

Total # of pixel is ~ 2622

𝜎𝑠 =10800

𝜋

4𝜋2𝑁𝐸𝑇𝑑𝑒𝑡2

𝑡𝑜𝑏𝑠𝑁𝑑𝑒𝑡

3 years

Assumptions: Observation efficiency is 72% Yield rate : 80% 25% margin

LiteBIRD

TES bolometers: detectors at focal plane

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Focus with lenslets Catch signal with sinuous antenna Detect signal with transition edge sensor (TES) bolometer

Two orthogonal linear polarization Cooled to 100 mK

lenslets

TES bolometer

Sinuous antenna

http://web.mit.edu/figueroagroup/ucal/ucal_tes/

LiteBIRD

Optics

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Low Frequency Telescope (LFT)Crossed Dragone: Comact configuration

Simulated side-lobes of stray light

High Frequency Telescope (HFT)Refracting telescope

Designs and properties are well studied. Further studies are ongoing.

LiteBIRD

Overall cryogenic system

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K.Mitsuda, Bmode from Space (2015)

Cryogenic system is very important to reduce thermal noise

LiteBIRD

Cryogenic system in 4K shell

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CMB

Detectors are cooled to ~100 mKHWP and mirrors are cooled to ~5 K

LiteBIRD

Future study: Lessons from Planck satellite

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Unexpectedly high level of data loss from cosmic ray interaction with detectors Make “glitch”(pulse) in the bolometer time streams

They modeled it with ballistic phonons and thermal diffusion

A. Catalano et al., Astron. Astrophys. 569, A88 (2014)

We have a plan to mitigate the propagation of phonons We should prepare glitch template before launch

LiteBIRD cannot keep large size raw data to make template by itself

My future study

LiteBIRD

Future study: Phonon simulation

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Phonon propagation in the cylindrical Si wafer which is sandwiched by aluminum. Aluminum absorb phonons.

Phonon simulation is very challenging plan G4CMP software in Geant4 can simulate phonon in

one components It cannot deal the phonon propagation at the

boundary of two materials Just now searching for the boundary properties in low

temperature between Si and another material If nothing, we have to measure by ourselves

LiteBIRD

2016/12/14 37

Now in Phase A1

LiteBIRD

Operation timeline

2016/12/14 38

LiteBIRD

Summary

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Studying inflation could gives us a hint for very high energy scale physics -> inflation!

The inflation model could be studied with the observation of B-mode polarization from primordial gravitational wave

For the verification of inflation Small ℓ search (2<ℓ<200) δr < 0.001 are important and LiteBIRD are required to meet them

The target launch time is 2025 For the success, many studies are done and ongoing

Development of HWP Study of optics Optimization of scan strategy Mitigation of cosmic ray effects…etc

Stay tuned for further updates of LiteBIRD studies!