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Lite (light) satellite for the studies of

B-mode polarization and

Inflation from cosmic background

Radiation

Detection

APC, 24th of January 2024

LiteBIRD �@ APC

LiteBIRD @ APC, March 29th 2022

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Lite (light) satellite for the studies of

B-mode polarization and

Inflation from cosmic background

Radiation

Detection

APC, 24th of January 2024

LiteBIRD �@ APC

Science and data analysis — Guillaume Patanchon
MHFT system thermal model — Michel Piat

LiteBIRD @ APC, March 29th 2022

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us, today

10¹⁷

10^-36

10¹³

last scattering surface

galaxies, clusters, superclusters

10^-32

end of inflation

space expansion

CMB

space

time [sec]

space-time forms

our light cone

LiteBIRD @ APC, March 29th 2022

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Current and (forecasted) upcoming constraints

vs. theory

LiteBIRD @ APC, March 29th 2022

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5

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instrumental systematics

astrophysical systematics

aka galactic foregrounds

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2202.02773

Leloup et al. 2023
Patanchon et al., submitted, astro-ph
Interplanetary Dust as a Foreground for the LiteBIRD CMB Satellite Mission, �K. Ganga et al. (2021)
Detailed study of HWP non-idealities and their impact on future measurements of CMB polarization anisotropies from space, S. Giardello et al (2021)

instrumental modeling / simulation

foregrounds modeling / simulation

scientific analysis + forecasting

CNES Phase A (L3) requirements + JAXA MDR

constraints on large scale CMB polarization

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Systematics studies

Coordination of systematics studies for the collaboration (G. Patanchon)

Beam sidelobes: W. Wang

HWP imperfections: G. Patanchon

Coupled with the CMB-INFLATE project (1.2 M€) coordinated at APC

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Beam systematics

Main identified systematics in LiteBIRD
At APC: Modeling, simulation, link with calibration
Wang Wang thesis and Clément Leloup (before 2022)

-80 dB requirements on the knowledge of FSL mean amplitude (Leloup et al.)

Preliminary

Wang’s analysis: inflight mitigation.

Relaxes requirements on ground calib.

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Component separation

Development of methods of component separation
Analysis for LiteBIRD: In charge of one of the methodologies FGBuster (https://fgbuster.github.io/fgbuster/index.html)

J. Errard

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Component separation

example #1: improving on PTEP� (inclusion of more sky, different �splitting of regions to handle �spatial variability of foreground �SEDs)�
example #2: improvement of the� component separation by explicitly� including beams in the parametric component separation �
example #3: exploring non-parametric component separation �
example #4: main developers of the performance pipeline, from hardware to constraints on r

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example #4: main developers of the performance pipeline, from hardware to constraints on r

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LiteBIRD design and data analysis

Involvement in the requirements definition (Josquin Errard, Arianna Rizzieri):

put requirements on the LB sensitivities by investigating alternative sensitivity configurations and forecasting the corresponding sigma(r=0)
impact on the Lv1 requirements of removing the HWP from MFT or HFT

Involvement in the post PTEP papers (Josquin Errard, Arianna Rizzieri):

Out-of-band rejection requirements for LiteBIRD Medium and High Frequency Telescopes:

Studying the post component separation bias on r

E modes from LiteBIRD:

FGBuster component separation

Co-leading of Cosmic Birefringence group + development of one of the three data analysis pipelines (Josquin Errard)

Other studies of the group applicable to LiteBIRD:

estimating the pure spectra on optimized masks (Magdy Morshed)
developing of map-making maximum likelihood code (Simon Biquard)
HWP modeling (Emma Tsang)

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B. Beringue (postdoc)

M. Bucher

C. Chapron�G. Deniel�S. Dheilly

J. Errard (co-chair of the performance team)

K. Ganga

L. Grandsire

J.-Ch. Hamilton

A. Ilioni

C. Juffroy

M. Karakac�M. Le Jeune

C. Leloup (postdoc, PCCP ➔ IPMU Japan)

D. Pailot

G. Patanchon (JSG systematics co-convener, IGB, PI of RISE CMB-Inflate)

M. Piat (APC point of contact)

D. Prêle

A. Rizzieri (PhD, IN2P3)

R. Stompor (APC ➔ CPB Berkeley)�F. Voisin

J.-P. Thermeau

W. Wang (PhD, IN2P3)

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MHFT �Thermal model

J.-P. Thermeau, L. Grandsire, A. Ilioni, G. Deniel, M. Piat

MHFT Thermal Model

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Planning tendu
Actuellement en phase A2
Key Point CNES/JAXA: mai 2023

5 recommandations
Décalage du planning 2029 -> 2033

Départ chef de projet CNES fin 2023
Revue CNES fin de phase A: mi-2024

Statut développement LiteBird

MHFT Thermal Model

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Current version of the ThermXL nodal thermal model of MFT and HFT instruments includes :

Simplified MHFT configuration with reduced number of nodes
CEA cryochain model (Thomas Prouvé)
30K environment
Optical components:
Thermal characteristics of the polypropylene (HWP, lens 1, lens 2, filter 2K).
Sky input power (Louise Mousset and Ludovic Montier)
Old focal plan design

MHFT thermal model

MHFT Thermal Model

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Thermal model

cryochain thermal model

MFT thermal model

HFT thermal model

MHFT Thermal Model

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Steady state study

Stages	MFT heat dissipation	HFT heat dissipation	Total MHFT dissipations (µW)
T3 - 4.8K	6530	2480	9010
T2 - 1.75K	101	57,9	158.9
T1- 0.38K	13,9	9,12	23.02
T0 - 0.1K	0,428	0,228	0.656

MHFT thermal balance

MFT matrix of heat loads

MHFT Thermal Model

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Thermal budget

Stages	MFT heat dissipation (µW)	HFT heat dissipation (µW)	MHFT JAXA supply (µW)	Total dissipations (µW)	Total Power budget (µW)	Budget / Dissipation ratio
T3 - 4.8K	6530	2480	4610	13620	13910	1.0
T2 - 1.75K	101	57,9		158.9	462	2.9
T1- 0.38K	13,9	9,12		23.02	29,8	1.3
T0 - 0.1K	0,428	0,228		0.656	1,6	2.4

MHFT thermal balance vs budget

4.8K heat loads:

MHFT contributions:

HWP: 2 x 2.2mW
Support truss: 4mW
Radiation heat loads: 0.6mW

MHFT JAXA supply:

Sensor harness: 3.93mW
ADR current wire: 0.18mW
Faraday gauge: 0.5mW

MHFT Thermal Model

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Transient studies

MFT results

- Frequency range: from 1mHz to 10Hz.

- Input temperature oscillation amplitude:

200mK pp at 4.8K and 1.75K
2mK pp at 0.38K and 0.1K

MHFT Thermal Model

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First version of nodal global thermal model completed

Steady state results available:

Thermal loads between nodes
Heat loads of each cold stage

Transient studies:

First results of the the cold stage sensitivity to sinusoidal excitations

Next steps :

Impact of the sky heat load variation on the cold stages
Sensitivity analysis
Integration of HFT focal plane with IAS (J.C. Le Clec’h)

MHFT thermal model

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03/02/2023

Future plan

MHFT Thermal Model

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HFT focal plane thermal model (with IAS)

MHFT Thermal Model

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Demande de financement : 30k€

Vacation : 8k€

2x6 mois de stage niveau M2 et/ou école ingénieur

Mise à jour licence ESATAN-TMS: 10k€
Missions : 12k€

Conférences scientifiques (SPIE, CMB Foregrounds...): �6 missions (5 jours, 2k€ par mission)

Besoin supplémentaire: 4k€ (augmentation licences, informatique)
Reliquats: 3.7k€

Missions: 4.7k€
Fonctionnement: -1k€

Besoin: 30k€

APR 2024

MHFT Thermal Model