1. Next Generation Data Sets: An Overview of CMB-S4 and WFIRST David Spergel Princeton University Center for Computational Astrophysics, Flatiron Institute

2. 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 work

3. 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  detection of gravitational lensing – r ~0.001 sensitivity for gravitational waves Probe of low redshift universe – Clusters – KSZ effect (large-scale flows)

4. 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]

5. Improved Parameter Constraints Galli et al. 2010

6. Search for Primordial Gravitational Waves Ground-based experiments – BICEP “family” – small deep maps – ACT/SPT/PolarBear Simons Observatory – CLASS Balloons – SPIDER,PIPER Space – LiteBIRD, PIXIE, CORE+ CHALLENGES: Systematics (T,E leaking to B) and Foregrounds (Dust, Synch.)

10. 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.org

11. Wide or Deep?

12. 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 coronagraph Dark EnergyExoplanets Microlensing Coronagraph Astrophysics M63 HST WFIRST

13. 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 JWST 18 H4RG detectors (288 Mpixels) Coronagraph Image and spectra of exoplanets from super-Earths to giants Images of debris disks Visible bandpass Contrast of 10 -9 or better Exoplanet images from 0.1 to 1.0 arcsec 13

14. Observing Modes 14 High Latitude Survey: Optimized to study dark energy – 2227 deg 2 area YJHF184 7  line flux of 1.2 x 10 -16 erg/cm 2 /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 deg 2 with depths increasing to J=29.3/H=29.4 (LSST deep drilling fields + Subaru fields) Bulge Survey: Optimized for exoplanet discussion – 6 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 Observations Coronagraph

15. High Latitude Survey 15

16. 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 Observatory 16 Weinberg & SDT 2015 WFIRST Probes of Expansion and Growth

17. 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 HH OIII Euclid IR Optical redshift (distance) BAO Density Parameter

18. Detailed 3D Map of Large Scale Structure at z = 1-2 18 WFIRST 2,200 deg 2 @ 9 x 10 -4 gal/Mpc 3 Euclid 15,000 deg 2 @ 1 x 10 -4 gal/Mpc 3 Large scale structure simulations from 2015 SDT Report – courtesy of Ying Zu Thin and thick red circles mark clusters with masses exceeding 5 x 10 13 M Sun and 10 14 M Sun, respectively Large scale structure simulation showing 0.1% of the total WFIRST-AFTA Galaxy Redshift Survey Volume z = 1.5

21. Kepler WFIRST 21 2600 planets 370 Earth mass & less 100's free- floaters 2600 planets 370 Earth mass & less 100's free- floaters WFIRST complements Kepler, TESS, Plato M. Perry Complete the Census of Exoplanets - Microlensing

22. 04/30/2014WFIRST-AFTA SDT Interim Report 22 AFTA Brings Humanity Closer to Characterizing Earths

23. 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 surveys

27. 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 lensing

29. 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)

30. Schaan, Ferraro et al. (2016)

31. Hill et al. 1603.01608 WISE galaxies x Planck Temperature

32. 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.

33. Mission Schedule – 2024 LRD Overguide Schedule 33 82 month B/C/D development schedule 2024 LRD requires over-guide funding starting FY18