David Spergel Princeton University Center for Computational Astrophysics Flatiron Institute Outline Next generation CMB experiments Simons Observatory CMBS4 Next generation opticalIR surveys WFIRST ID: 627879
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Slide1
Next Generation Data Sets: An Overview of CMB-S4 and WFIRST
David
Spergel
Princeton University
Center for Computational Astrophysics, Flatiron InstituteSlide2
Outline
Next generation CMB experiments: Simons Observatory + CMB-S4
Next generation optical/IR surveys: WFIRST
Combining CMB + Optical data – two recent examples from Emmanuel
Schaan’s
PhD thesis workSlide3
Future CMB Observations
Measure EE spectrum to l of 4000-5000 across most of the sky (4 x Planck modes)
2x improvement on non-
Gaussianity
constraints
Measure BB spectrum
> 100
s
detection of gravitational lensing
r ~0.001 sensitivity for gravitational waves
Probe of low redshift universe
Clusters
KSZ effect (large-scale flows)Slide4
4
The rms deflection is about 2.7 arcmins, but the deflections are coherent on degree scales.
CMB as a Backlight
Gravitational Lensing [Projected Mass]
TSZ [Projected Pressure]
KSZ [Projected Momentum]Slide5
Improved Parameter Constraints
Galli
et al. 2010Slide6
Search for Primordial Gravitational Waves
Ground-based experiments
BICEP “family” – small deep maps
ACT/SPT/
PolarBear
Simons ObservatoryCLASSBalloonsSPIDER,PIPERSpaceLiteBIRD, PIXIE, CORE+ CHALLENGES: Systematics (T,E leaking to B) and Foregrounds (Dust, Synch.)Slide7Slide8Slide9Slide10
The Simons Observatory
POLARBEAR/Simons Array
ACT
A five year, $45M+ program to pursue key Cosmic Microwave Background science targets, and advance technology and infrastructure in preparation for CMB-S4.
Merger of the ACT and POLARBEAR/Simons Array teams.
Tentative plans include:
Major site infrastructure
Technology development (detectors, optics, cameras)Demonstration of new high throughput telescopes.CMB-S4 class receivers with partially filled focal planes.Data analysis
http://simonsobservatory.orgSlide11
Wide or Deep?Slide12
12
Introduction
WFIRST highest ranked large space mission in 2010 Decadal Survey
Study Dark Energy, Exoplanet Census, NIR Sky Survey
Use of 2.4m telescope enables
Hubble quality imaging over 100x more sky
Imaging of exoplanets with 10-9 contrast with a coronagraphDark EnergyExoplanets
M
icrolensingCoronagraph
Astrophysics
M63
HSTWFIRSTSlide13
WFIRST Instruments
Wide Field Instrument
Imaging & spectroscopy over 1000s of sq. deg.
Monitoring of SN and microlensing fields
Near infrared
bandpass
Field of view 100 x HST and JWST18 H4RG detectors (288 Mpixels)CoronagraphImage and spectra of
exoplanets from super-Earths to giantsImages of debris disks Visible bandpass
Contrast of 10-9 or betterExoplanet images from 0.1 to 1.0 arcsec
13Slide14
Observing Modes
14
High Latitude Survey: Optimized to study dark energy
2227 deg
2
area YJHF184
7 s line flux of 1.2 x 10-16 erg/cm2/s (R=600)26.7 AB mag YJH (4-5 dithers at each of two roll angles/174 s integration)SN surveys: 27.44/8.96/5.04 deg2 with depths increasing to J=29.3/H=29.4 (LSST deep drilling fields + Subaru fields)Bulge Survey: Optimized for exoplanet discussion6 season of 72 days 10 contiguous field (2.8 degrees) each observed every 15 minutes in W149 and once every 52 seconds in W149 (33000 epochs) and 290 seconds in Z087 (7000)Fields are “confusion-limited”Potential for high precision astrometry (50-700 mas/epoch) and seismology 2.6 billion photons from a H=19.6 mag star!GO ObservationsCoronagraphSlide15
High Latitude Survey
15Slide16
WFIRST combines all techniques
to determine the nature of Dark Energy.
Only observatory doing such comprehensive observations
High precision measurements will be optimally combined for the best measurement
Premier Dark Energy
Observatory16Weinberg & SDT 2015
WFIRST Probes of Expansion and GrowthSlide17
17
Premier Dark Energy
Observatory
WFIRST will be the first mission to fully exploit the powerful IR band for dark energy measurements.
It will be much more sensitive and have higher angular resolution than any other dark energy instrument.
WFIRST
HaOIII
Euclid
IROptical
redshift (distance)
BAO Density ParameterSlide18
Detailed 3D Map of Large Scale Structure at z = 1-2
18
WFIRST
2,200 deg
2
@ 9 x 10
-4 gal/Mpc3Euclid15,000 deg2 @ 1 x 10-4 gal/Mpc3Large scale structure simulations from 2015 SDT Report – courtesy of Ying ZuThin and thick red circles mark clusters with
masses exceeding 5 x 1013 MSun
and 1014 MSun, respectively
Large scale structure simulation showing 0.1% of the total WFIRST-AFTA Galaxy Redshift Survey Volume
z = 1.5Slide19Slide20Slide21
Kepler
WFIRST
21
2600 planets
370 Earth mass & less
100's free-floaters
WFIRST complements
Kepler, TESS, Plato
M. Perry Complete the Census of
Exoplanets - MicrolensingSlide22
04/30/2014
WFIRST-AFTA SDT Interim Report
22
AFTA Brings Humanity Closer to Characterizing EarthsSlide23
Combining LSST + CMB-S4 Data
Emmanuel
Schaan
(Princeton),
Eifler
, Krause, et al. in prep.
CMB lensing adds a high redshift source plane with very different systematics and can be used to determine the multiplicative bias in optical lensing surveysSlide24Slide25Slide26Slide27
Cross-correlating CMB lensing + Lyman alpha Power Spectrum
Vallinotto
, Das, Spergel &
Viel
(2009): use cross-correlation to probe relationship between Lyman alpha forest + underlying mass distribution
Cyrille
Doux (APC), Emmanuel Schaan et al. combine DR12 Lyman alpha forest data with Planck lensingSlide28Slide29
Combining KSZ + LSS Data
KSZ traces the large-scale distribution of electrons. Cross-correlations measure the relationship between the large-scale distribution of electrons and the distribution of galaxies
Two examples:
Spectroscopic data + CMB (SDSSIII + ACTPOL):
Schaan
et al. (2016)
Imaging data + CMB (WISE + Planck): Hill et al. (2016)Slide30
Schaan
, Ferraro et al. (2016)Slide31
Hill et al. 1603.01608
WISE galaxies x Planck TemperatureSlide32
Conclusions
Lots of exciting data in the coming decade
WFIRST
Simons Observatory
Exciting Opportunities to use this data to learn about the large scale distribution of electrons, pressure, galaxies and matter. These observations will enable a deeper understanding of important questions in cosmology.Slide33
Mission Schedule – 2024 LRD
Overguide
Schedule
33
82
month B/C/D development schedule
2024 LRD requires over-guide funding starting FY18