Future Cosmic Microwave observations from Space: A

Future Cosmic Microwave observations from Space: A European perspective

Jacques DelabrouilleLaboratoire APC, CNRS/IN2P3, Paris

IRFU, CEA-Saclay

Outline

•Context and overview• Science case

- Cosmology and fundamental physics from the CMB- The CMB as a backlight to probe the Hubble volume- Microwave observations of large scale structure- CMB spectral distortions

•Mission

The Context : ESA science in 2035-2050

Four coordinated "CMB" white papers

Spectral distortionsJens Chluba et al.

CMB BacklightKaustuv Basu et al.

High redshift LSSMarta Silva et al.

Microwave surveyJacques Delabrouille et al.

Key Observables: microwave backgrounds

1- CMB polarization survey• E and B-modes: Inflation (r, ns, NG, ...)

• TEB on all scales: extend LCDM (FOM x 109)

• Lensing: Dark matter structures

2- SZ survey of ionised gas• Galaxy cluster counts: extend LCDM

• Cosmic web, galaxies and clusters

• Velocity flows: gravitation

3- CIB and line intensity mapping• Map structures across redshift

• First objects: stars, galaxies, clusters

4- CMB spectral distortions• Inflation (ns, ...)

• Reionization, Clusters (diffuse gas)

• Dark Matter interactions or decay

• Recombination lines

Key Observables: microwave backgroundsFinelli, Lesgourgues, Di Valentino, ...

Basu, Melin, Remazeilles, ...

Silva, Kovetz, ... Dannerbauer, De Zotti, ...

Chluba, ...

1- CMB polarization survey• E and B-modes: Inflation (r, ns, NG, ...)• TEB on all scales: extend LCDM (FOM x 109)• Lensing: Dark matter structures

2- SZ survey of ionised gas• Galaxy cluster counts: extend LCDM• Cosmic web, galaxies and clusters• Velocity flows: gravitation

3- CIB and line intensity mapping• Map structures across redshift• First objects: stars, galaxies, clusters

4- CMB spectral distortions• Inflation (ns, ...)• Reionization, Clusters (diffuse gas)• Dark Matter interactions or decay• Recombination lines

Outline



•Mission

CMB Spectra

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PrimordialB modes?

Gaussian beamsfrom 1' to 3'

10 orders of magnitude

Constraints on extended LCDMCosmic Variance Limit

Delabrouilleet al., Voyage 2050 W

hite Paper

>9 orders of

magnitude

6 orders of

magnitude

10 orders of

magnitude

Constraints on extended LCDM

Scrutinize LCDM to solve or

confirm tensions

(such as that on Hubble H0)

...

possibly uncover new ones !

Cosmic Variance Limit

De

lab

rou

illee

t al., V

oya

ge

20

50

Wh

ite P

ap

er

(figure from E. di Valentino)

Outline



•Mission

Backlight

Basuet al., Voyage 2050 W

hite Paper

The CMB is a backlightthat interacts with structuresin many different ways,and probes the distribution of mass, of atoms, of electron gas, and of velocity flowsin the full Hubble volume.

Cluster catalog and cluster counts (PRISM 2013)

1100000

220000

10000

detectionlimitsfor S/N>5and # of detections for a full-sky survey

Exact numbers to be updated

SZ and CIB confusion (even at 150 GHz)

0° 1° 2° 3°

Clusters onlyM > 1014 Msun

Clusters and CIBM > 1014 Msun

Clusters only1014 Msun > M > 5.1013 Msun

Clusters and CIB1014 Msun > M > 5.1013 Msun

0° 1° 2° 3°

0° 1° 2° 3° 0° 1° 2° 3°

0° 1° 2° 3° 0° 1° 2° 3°

Clusters and 20% CIBM > 1014 Msun

Clusters and 20% CIB1014 Msun > M > 5.1013 Msun

If one can reduce the level of CIBcontamination to 20% of its original level at 150 GHz, thermal SZ emissiondominates.

However, better decontamination willbe required for kinematic SZ and formeasuring relativistic corrections (clustertemperatures).

This requires channels above 300 GHz.

For a large sky parch, this can be realistically done only from space.

Cluster spectroscopy

A precise measurement of cluster spectra across frequencies allows to recover - thermal SZ effect (gas pressure), non thermal SZ effect- relativistic corrections (cluster temperature)- kinematic SZ effect (cluster flows)- contamination by radio and IR sources, early clusters in the FIR- modeling uncertainties

Basuet al., Astro2020 W

hite PaperBasu

et al., Voyage 2050 White Paper

Cluster spectroscopy: avoiding biases

Biases from inaccurate estimates using only limited available frequencies;Spectroscopy allows estimation of IR and line emission through stacking.Combination with CMB lensing for cluster masses.

Basuet al., Astro2020 W

hite PaperChen, Rem

azeilles& Dickinson, 2018

Mapping the Dark Matter

COBE/DMR DTS/N ~ 1, at 7°

WMAP DTS/N ≫ 1, at 20'

Planck fS/N ~ 1, at 7°

Future fS/N ≫ 1, at 20'

Measuring cluster velocities and masses

Outline



•Mission

3- CIB tomography, Line Intensity Mapping

Kovetzet al., Astro2020 White Paper)

Spectroscopy on largesky areas (tens of %)allows inversion ! → #C+, CO across cosmic timeCIB in redshift shells

LIM gives access to "emission shells" forcosmological constraints across cosmic time.(e.g. handle on cosmic expansion at high redshift)

CIB tomography, Line Intensity Mapping

Outline



•Mission

Spectral distortions

see Chlubaet al., Voyage 2050 W

hite Paper

Spectral distortions

Constrain / observe

Inflation (small scale spectrum)Total amount of hot gas in clustersAverage group/cluster gas temperatureLines from primordial atoms

Foreground emissions

see Chlubaet al., Voyage 2050 W

hite Paper

Outline



•Mission

Concept inspired from PRISMFull-sky spectro-polarimetric survey in the microwaveSubmitted to ESA for L2-L3 in 3013, with Paolo de Bernardis (lead), François Bouchet, Martin Bucher, ...

• Rich science case- Galaxy clusters- CMB polarization- CMB spectral distortions- High redshift galaxies and CIB- Dusty magnetised ISM

• Rich legacy value• Main instruments

- a polarised imager and a spectro-imager with a 3.5m telescope- a Fourier Transform Spectrometer (similar to PIXIE)

Good feedback in 2013 (among 5 audited)but not selected (lost the competition to Athena and LISA)

Possible L-class missionLarge (2-3m) cold telescope with 2 focal plane instruments• A polarised imager (for CMB polarisation and lensing, cluster science), e.g. CORE, PICO

- Resolution for CMB ranging from 5' at 100 GHz to 2' at 250 GHz- 20 bands within 15-1500 GHz (TBD), resolution from 30' to 20" depending on frequency

• A spectrometer (for mapping line emission, both galactic and extragalactic)- R = 300 (TBD)- Frequency range within 50-2000 GHz, angular resolution at the arcminute scale

• Possibility of an additional guest instrument?• Must be an L-class mission (or M-class contribution to international L-class mission)

CMB sensitivity (µK.arcmin) SZ sensitivity (y.arcmin)

full-sky 2 years

5% sky 6 months

0.66 1.7 x 10-7

0.29 7.7 x 10-8

Absolute spectrometer modules

One or more small Fourier Transform Spectrometers modules• For zero-level of intensity maps and CMB spectral distortions

- Coarse resolution, typically degree-scale to few degree scale (TBC)

- Frequency range within 10 GHz – 2000 GHz

• Can be a separate M-class mission, e.g. a revision of PIXIE / PRISTINE

Observation modes

Optimize the spread of observing time• Full sky survey for ~ 25% of the mission lifetime• Deeper observation of selected wide areas

- possibly 'clean' sky at high galactic latitude- observed ~25% of the time

• Deep observation on selected patches (galactic or extragalactic)- possibility of 'observatory mode' for ~50% of the mission lifetime

• The Cosmic Microwave Background remains a key observable to understand the Universe

• In 2035+, an ambitious space mission can harvest a fantastic data set for Cosmology – very rich science case

• Observational objective : sensitive spectro-polarimetric full sky survey in 10-2000 GHz at all scales down to 1'

• ESA recommendations expected mid-2020

Summary

Thank you for your attention !

Documents

Future Cosmic Microwave observations from Space: A