Missions In the Coming Decade Moderator: Chryssa Kouveliotou (GWU) Panelists: Jeffrey Kruk (NASA), Randall Smith (CfA), Ira Thorpe (NASA) Introductory Remarks Chryssa Kouveliotou (GWU) Missions of the Coming Decade

• Are there overlaps between ESA-NASA missions and how could these exploited to achieve the best outcome? • Are there synergies between missions and how could these exploited to achieve the best outcome? • Are there obvious gaps in the overall science goals that may need to be filled with e.g., explorer or probe missions? • What are the lessons learned from the US – International collaborations? 2019 2022 2025 2030 2034 EUCLID

ATHENA IXPE WFIRST XRISM LISA LIGO A+

3G Detectors SVOM, SRG, eXTP, GECAM +++….. WFIRST and Euclid

Jeffrey Kruk (NASA) WFIRST Project Scientist

(Euclid information courtesy of Jason Rhodes, Mike Seiffert, Harry Teplitz) EUCLID – M2 Measuring Dark Energy and Dark matter Dark Energy causes accelerated expansion of the Universe Tim This expansion is locked up in: e • The geometry of the universe • Distance (scale) as a function of redshift • Growth of density perturbations • Evolution of structure (“clustering”) as a function of cosmic time

The Euclid mission is optimized for two complementary dark energy probes: Weak Lensing and Galaxy Clustering Requiring: • Shapes and orientations of field galaxies distorted by intervening dark matter due to weak lensing • Photometric redshifts [∆z /(z+1)< 0.05] of the WL galaxies • Spectroscopic redshifts [∆z/(z+1) < 0.001] to trace the galaxy clustering Over a minimum survey area of 15,000 deg2 (36% of the sky)

Springel et al , MPIA Mission and Spacecraft Key Systems ▪ Wide-field telescope with 1.2 diameter primary mirror ▪ High image quality: up to 0.18 arcsec resolution in visual ▪ Low noise attitude control providing extremely stable pointing ▪ K-band telemetry: more than 100 Gbyte/day compressed science data

Mission and operation ▪ Soyuz-Fregat ST-2.1B carrier, ~2150 kg spacecraft mass ▪ Mission nominal lifetime of 6 years + cruise + commissioning ▪ Lissajous orbit around SEL2, with line of sight nearly 90 degrees from Sun, to ensure thermal stability

4k HST: (VIS) WFPC3

ESO 7x7 Euclid Field of View arcmin 42x44 arcmin 609 Mpixels in Visual 67 Mpixels in NIR Euclid Instruments Instruments are provided by the Euclid Consortium (~1500 members in 14 participating countries) VIS instrument

o NISP: Near-IR Spectrometer and Photometer - 0.92 < λ < 2.0 micron NISP instrument 16 (2kx2k) HgCdTe detectors – 0.3” pixels – 0.763°x0.722° 3 Photometric bands Y, J, H Hα Spectroscopy 1.25-1.85 micron, R~360

o VIS: Visual imager - 0.55 < λ < 0.92 micron 36 (4kx4k) CCDs operating at ~150 K – 0.1” pixels – 0.787°x0.709° single bandpass (r+i+z) In combination with telescope, VIS will provide excellent image quality for weak lensing measurement Sensors are optimised for Euclid ▪Teledyne Imaging Systems (USA) for NISP H2RG sensors, NASA contract ▪e2v/Teledyne (UK) for VIS CCDs, ESA contract visual instrument: 609 Mpixel camera Euclid Survey

Euclid will survey >36% of sky down to AB >24 mag (~500TB raw data) in 6 years ▪ Excellent image quality (~0.18 arcsec FWHM) in visual band (0.55-0.9 micron): over 1.5 billion resolved galaxies with z<2

▪ Near-IR Imaging Photometry (Y, J, H bands) of these galaxies and Hα Spectroscopy (1.25-1.85 micron) of >25 million galaxies ▪ The Euclid Consortium will perform the scientific data processing in 10 Euclid data centres WFIRST Science Program

Dark Energy and the ? Fate of the Universe Wide-Field Infrared Surveys of ? the Universe (General Observer & Archival Research)

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The full distribution of planets around stars

10

Technology Development for Exploration of New Worlds WFIRST Mission

2.4m telescope @ Sun-Earth L2 WFIRST Wide-field Instrument FOV 2 instruments: • Wide-field instrument: • 0.28 sq deg, 0.11” /pix • 0.48-2.0 훍m imaging • 1.0-1.93 훍m R~460훌 slitless spectra • 0.75-1.8 훍m R~80-170 slitless spectra • Coronagraph

Launch: late 2025 Science programs to be competed

All data public upon processing HST/ACS HST/WFC3 JWST/NIRCAM

Partners: JAXA,11 ESA, DLR, CNES, … Representative WFIRST Surveys

Cumulative 5σ point-source imaging depth in wide-area surveys: 2 High Latitude Survey, Wide: 2000 deg : AB ~26.5 2 High Latitude Survey, Deep: 20 deg : AB ~28.2 2 Supernova Survey (5-day cadence), Wide: 14 deg : AB ~28 2 Supernova Survey (5-day cadence), Deep: 5 deg : AB ~29.4

Microlensing: 2, Monitor 2+ deg 15 minute cadence over 72-days, S/N=100 @ AB=21.4 per visit Exoplanet detections by microlensing, other time-domain astronomy, Precision astrometry (tens of micro-arcsec) Coronagraph Technology Development

Autonomous First Use of Image Processing Ultra-Precise Deformable at Unprecedented Wavefront Sensing & Mirrors in Space Contrast Levels Control System

High Contrast Coronagraph Ultra-low Noise Masks Photon Counting Visible Detectors Euclid Summary WFIRST Summary 2 2 • • 15,000 deg wide survey 2,000 deg wide survey - mIR>26.5 2 • m >24, m >26 • IR V >20 deg deep survey - mIR> 28 2 2 • 40 deg deep survey • >2 deg Galactic Bulge - mIR > 30 – confusion limited • m > 26, m > 28 IR V • TBD GO surveys • Launch: mid-2022 • Launch: late-2025 • Prime mission: 6 years + ?? extd • Prime mission: 5 years + 5 yrs extended • GO program: not in prime mission • GO: 25% prime mission, 100% after • Data releases: • Data releases: • DR1: 2500 deg2 2 yrs after obs start • Basic products w/in 72 hours of observation • DR2: 7500 deg2 4 yrs after obs start • High-level products TBD; depends on program • DR3: 15000 deg2 7 yrs after obs start

Both missions will provide treasure trove of objects for follow-up with JWST, E-ELT, TMT, ALMA, GAIA, etc Both missions will have strong synergy with LSST, SKA, e-ROSITA Athena, XRISM, & IXPE Randall Smith (CfA)

LIGO, LISA, & Beyond

Ira Thorpe (NASA) GW Astronomy has arrived!

● Past ○ International network of three interferometers (LIGO+VIRGO) ○ 10 BH-BH detections, 1 NS-NS detection, 1 Nobel Prize ● Present ○ Increased sensitivity, longer observing runs, public alerts ○ O3 starts today! ● Future ○ Additional detectors (KAGRA, LIGO-India, …) ○ Improved sensitivities (LIGO A+, Voyager) ○ 3rd-generation observatories (Cosmic Explorer, Einstein Telescope) The Gravitational Wave Spectrum

Science opportunities and instrumental challenges depend on the waveband, just like EM astronomy LISA Science (in one very busy slide)

Massive Black Hole Mergers ● ~100s events Milky Way Compact Binaries 4 7 ● Millions of systems in band ● 10 M☉ < Mtot < 10 M☉ ● 1 < z < 30 ● Few x 104 resolvable ● Measure masses & spins ● WD-WD, WD-NS, NS-BH, ... ● Structure Formation, MBH ● Demographics of compact objects, formation and growth,... mass transfer measurements, … ● guaranteed persistent EM counterparts

Extreme Mass Ration Inspirals LIGO-type BH mergers ● 10s to 1000s of events ● Event rates TBD by LIGO 4 7 ● 10 M☉ < M1 < 10 M☉, M2 ~ 10 M☉ ● Same source will radiate in LISA and ● 1 < z < 4 LIGO bands over period of weeks ● Measure masses & spins ● Advance notice (including location) for ● Precision GR tests, dynamics in LIGO and EM partners, GR tests,... dense nuclear clusters,... Few x 104 sources of various classes over 0 < z < 20+ LISA Mission Summary

● Mission concept ○ Triangular constellation, 2.5 million km on a side ○ Earth-trailing heliocentric orbit ○ 4 year baseline science operations, 10 year design

● Technology ○ Drag-free operation around free-flying test masses (demonstrated on LISA Pathfinder in 2016) ○ Optical heterodyne interferometry between spacecraft (demonstrated over 300km baselines by GRACE-FO)

● International Partnership ○ ESA: mission lead, spacecraft, launch vehicle ○ European National Agencies: payload and science lead ○ NASA: key payload components, spacecraft elements, and science contributions Q & A

Moderator: Chryssa Kouveliotou (GWU)

Panelists: Jeffrey Kruk (NASA), Randall Smith (CfA), Ira Thorpe (NASA)