Future Cosmic Microwave observations from Space: A ...
Transcript of Future Cosmic Microwave observations from Space: A ...
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Future Cosmic Microwave observations from Space: A European perspective
Jacques DelabrouilleLaboratoire APC, CNRS/IN2P3, Paris
IRFU, CEA-Saclay
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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
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The Context : ESA science in 2035-2050
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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.
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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
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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
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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
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CMB Spectra
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PrimordialB modes?
Gaussian beamsfrom 1' to 3'
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10 orders of magnitude
Constraints on extended LCDMCosmic Variance Limit
Delabrouilleet al., Voyage 2050 W
hite Paper
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>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)
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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
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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.
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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
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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.
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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
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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
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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'
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Measuring cluster velocities and masses
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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
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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)
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CIB tomography, Line Intensity Mapping
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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
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Spectral distortions
see Chlubaet al., Voyage 2050 W
hite Paper
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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
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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
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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)
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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
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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
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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
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• 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
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Thank you for your attention !