content 12-December-2017 13:26:49

CMB Polarisation: Cosmic Microwave Background Polarisation mission

ESA's Concurrent Design Facility (CDF) has completed a short study of a Cosmic Microwave Background Polarisation mission (CMB Polarisation). The purpose of this study is to support the European and Japanese science community in defining a collaborative mission studying the Polarisation of the Cosmic Microwave Background for calls for Cosmic Vision Medium-sized mission. A brief outline of the mission is given here, while further details can be found in the CDF presentations: CMB Polarisation mission - summary and CMB Polarisation mission - full presentation.

Mission Justification

The highly successful ESA Planck space mission has demonstrated the capability of precision Cosmic Microwave Background (CMB) observations to constrain models of fundamental physics in the primordial Universe. Planck was primarily designed as the near-ultimate space mission for measuring the angular power spectrum of CMB temperature anisotropies, and has also made the most constraining measurements so far of E-mode polarisation. However, much remains to be learned from CMB polarisation, especially with regard to the much fainter B-modes, which are the signature of gravitational waves generated during inflation.

 

Science Objectives

The mission is primarily designed for the detection and characterization of primordial B-modes generated by inflation, targeting a detection and confirmation of the inflationary origin of the observed B-modes down to a tensor-to-scalar ratio level of r = 10-3. The primordial B-mode signal appears primarily at angular scales larger than about 20 degrees on the celestial sphere (the reionization peak at l ≤ 10), and at angular scales of a few degrees (recombination peak at l ~ 100). Observing the reionization peak with adequate statistics requires covering as much of the sky as possible (at a minimum more than 75%).

Lensing of E-modes by intervening matter introduces a B-mode signal which for r ~ 10-3 is the dominant signal at l > 10. Polarised galactic emission dominates the entire sky and introduces an additional B-mode signal which is most significant at the largest angular scales. To measure the primordial B-mode signals, strategies have to be put in place to estimate and remove the contribution of both foreground and lensing-induced B-mode signals. These strategies require a wider frequency coverage and higher angular resolution than required by the CMB signal alone.

Expected sensitivity of CMB Polarisation to the B-mode power spectrum. The blue lines show the theoretical B-mode power spectra from tensor modes with r = 0.1, 0.01, and 0.001. The left and right panels show the expected error bars on the B-mode power spectrum for the fiducial amplitudes of tensor modes with r = 0.01 and 0.001, respectively. Image courtesy: Core+ Consortium.

 

Mission Requirements

The main mission requirements for this study are:

  • A telescope with 1.2m effective aperture, operating below 60K.
  • Frequency coverage of ~50-500 GHz spread over ~15 bands, and a sensitivity to the CMB signal of ~2 µK arcmin. Reaching this typically implies a ~50 cm-diameter Focal Plane Array with >2000 detectors operating at 100mK.
  • Orbit: Large amplitude Halo orbit around L2 (like Herschel).
  • Launch Vehicle: Japanese H-II/H-III launcher or European Ariane 6.2.
  • Full sky coverage with scanning law consisting of three combined rotations:
    • Spin @ 2 RPM around axis at β = 45 deg with respect to optical axis
    • 4-day precession of spin axis with α = 50 deg with respect to Sun line
    • Daily Sun-Spacecraft line rotation to follow the solar orbit
CMB Polarisation mission orbit and scan strategy. Image Courtesy: Core+ consortium

 

Study results: baseline

CMB Polarisation System Characteristics

Total mass (with margin)

Dry mass: 1840 kg

Total: 2185 kg

Service Module – System Characteristics

Power

Solar Array

  • 1971 W required 
  • Current baseline: Reduced 10m2 body-mounted Solar Array plus deployable solar panels extending the body-mounted Solar Array
  • Alternative: Re-use of body-mounted Solar Array plus body-mounted solar panels around Sun-shield

Communications

Ka-Band with steerable antenna

Payload Module System Characteristics

Payload module mass (with margin)

Total: 920 kg (no propellant in payload module)

Telescope

1.2m aperture Gregorian Silicon Carbide (SiC) telescope

Active Cooling

7 x 20K-class 2-stage Stirling Coolers

2 x 4K-class Joule-Thomson Coolers

2 x 1K-class Joule-Thomson Cooler

Passive Cooling

3 thermal shields: Aluminium Sandwich Panel

Sunshield: Sandwich Panel

Bipod structure:

GFRP struts

Further details can be found in the CDF summary slides (CMB Polarisation mission - summary presentation) and the CDF Final Presentation slides (CMB Polarisation mission - full presentation).


Last Update: 09 May 2016

For further information please contact: SciTech.editorial@esa.int

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