Scott Gaudi Matthew Penny The Ohio State University Exoplanet Science with WFIRST-AFTA Microlensing 18

Kepler is revolutionizing our understanding of exoplanets here!

Ground-based Surveys. Ground-based surveys only sensitive to masses greater than ~M earth. Narrow range near near peak sensitivity, roughly 1-4 times the snow line. Only sensitive to giant free-floating planets.

Earth Mass and Below? Monitor hundreds of millions of bulge stars continuously on a time scale of ~10 minutes. –Event rate ~10 -5 /year/star. –Detection probability ~0.1-1%. –Shortest features are ~30 minutes. Relative photometry of a few %. –Deviations are few – 10%. Main sequence source stars for smallest planets. Masses: resolve background stars for primary mass determinations.

Ground vs. Space. Infrared. –More extincted fields. –Smaller sources. Resolution. –Low-magnification events. –Isolate light from the lens star. Visibility. –Complete coverage. Smaller systematics. –Better characterization. –Robust quantification of sensitivities. SpaceGround The field of microlensing event MACHO 96-BLG-5 (Bennett & Rhie 2002) Science enabled from space: sub-Earth mass planets, habitable zone planets, free-floating Earth-mass planets, mass measurements.

History. NASA Proposals (GEST/MPF) – PI David Bennett. –Submitted to Midex in 2001, Discovery in 2000, 2004, 2006 –Not selected. Decadal Survey White Papers: –Bennett et al. A Census of Exoplanets in Orbits Beyond 0.5 AU via Space-based Microlensing –Gould, Wide Field Imager in Space for Dark Energy and Planets Wide-Field Infrared Survey Telescope (WFIRST). –Top Decadal Survey recommendation for a large space mission (Dark Energy, Exoplanets, Galactic Plane, GO Program) –Science Definition Team – DRM1 and DRM2 –No funding until JWST is launched (~2017). National Reconnaissance Office (NRO) telescopes. –Two 2.4m space-qualified telescopes, donated to NASA. –Mirrors and spacecraft assemblies. –SDT formed to assess use for WFIRST, consider a coronagraph and serviceability. Euclid. –ESA M class Dark Energy Mission –Microlensing is not part of the core science.

WFIRST-2.4 AFTA- WFIRST Eff. Aperture2.28m FOV0.281 deg 2 Wavelengths0.7-2 μm Pixel Size0.11 Lifetime5 years +? OrbitGeo (?) Wide-Field Instrument Imaging & spectroscopy over 1000's sq deg.Imaging & spectroscopy over 1000's sq deg. Monitoring of SN and microlensing fieldsMonitoring of SN and microlensing fields 0.7 – 2.0 micron bandpass0.7 – 2.0 micron bandpass 0.28 sq deg FoV (100X JWST FoV)0.28 sq deg FoV (100X JWST FoV) 18 H4RG detectors (288 Mpixels)18 H4RG detectors (288 Mpixels) 4 filter imaging, grism + IFU spectroscopy4 filter imaging, grism + IFU spectroscopy Coronagraph (descopeable) Imaging of ice & gas giant exoplanetsImaging of ice & gas giant exoplanets Imaging of debris disksImaging of debris disks 400 – 1000 nm bandpass400 – 1000 nm bandpass contrast10 -9 contrast 200 milli-arcsec inner working angle200 milli-arcsec inner working angle

Comparing Designs. Euclid (Opt/NIR) WFIRST DRM1 WFIRST DRM2 AFTA- WFIRST Eff. Aperture1.13m1.3m1.1m2.28m FOV0.44 deg deg deg deg 2 WavelengthsRIZ/YJH μm μm Pixel Size0.1/ Time0 (300d)432d266d432d (?) Lifetime6 years5 years3 years5+1 years +? OrbitL2 Geo ?

Hardware Yields. Yields scale with: –Yield ~propto total observing time –Yield ~propto number of stars –Yield ~propto (photon rate) α, with α~0.3 to 1. Primary hardware dependencies: –FOV. –Aperture. –Bandpass (total throughput + red cutoff). –Resolution (background). –Pointing constraints. Secondary hardware dependencies: –Data downlink, slew and settle

Microlensing Simulations. (Matthew Penny)

2.2 AU (~28 sigma) Free floating Mars (~23 sigma)

Predicted Planet Yields. M/M Earth EuclidDRM1DRM2AFTA- WFIRST , Total EuclidDRM1DMR2WFIRST Bound F.F. Earth All yields by Matthew Penny.

Exoplanet Demographics with WIFRST. WFIRST will: Detect 2800 planets, with orbits from the habitable zone outward, and masses down to a few times the mass of the Moon. Have some sensitivity toouter habitable zone planets (Mars-like orbits). Be sensitive to analogs of all the solar systems planets except Mercury. Measure the abundance of free-floating planets in the Galaxy with masses down to the mass of Mars Characterize the majority of host systems. WFIRST will: Detect 2800 planets, with orbits from the habitable zone outward, and masses down to a few times the mass of the Moon. Have some sensitivity toouter habitable zone planets (Mars-like orbits). Be sensitive to analogs of all the solar systems planets except Mercury. Measure the abundance of free-floating planets in the Galaxy with masses down to the mass of Mars Characterize the majority of host systems. Together, Kepler and WFIRST complete the statistical census of planetary systems in the Galaxy. WFIRST/2.4 Search Area WFIRST/2.4 Search Area Kepler Search Area Kepler Search Area

Exoplanet Demographics with WIFRST. WFIRST will: Detect 2800 planets, with orbits from the habitable zone outward, and masses down to a few times the mass of the Moon. Have some sensitivity toouter habitable zone planets (Mars-like orbits). Be sensitive to analogs of all the solar systems planets except Mercury. Measure the abundance of free-floating planets in the Galaxy with masses down to the mass of Mars Characterize the majority of host systems. WFIRST will: Detect 2800 planets, with orbits from the habitable zone outward, and masses down to a few times the mass of the Moon. Have some sensitivity toouter habitable zone planets (Mars-like orbits). Be sensitive to analogs of all the solar systems planets except Mercury. Measure the abundance of free-floating planets in the Galaxy with masses down to the mass of Mars Characterize the majority of host systems. Together, Kepler and WFIRST complete the statistical census of planetary systems in the Galaxy. Synergy with JWST!!

WFIRST + Coronagraph

Exoplanet Direct Imaging WFIRST-2.4 will: Characterize the spectra of roughly a dozen radial velocity planets. Provide crucial information on the physics of planetary atmospheres and clues to planet formation. Respond to decadal survey to mature coronagraph technologies, leading to first images of a nearby Earth. WFIRST-2.4 will: Characterize the spectra of roughly a dozen radial velocity planets. Provide crucial information on the physics of planetary atmospheres and clues to planet formation. Respond to decadal survey to mature coronagraph technologies, leading to first images of a nearby Earth. Spectra at R=70 easily distinguishes between a Jupiter- like and Neptune-like planet at 2 AU about stars of different metalicity.

Debris Disk Imaging WFIRST/2.4 will: Measure the amount and distribution of circumstellar dust, Measure the large scale structure of disks, revealing the presence of asteroid belts and gaps due to unseen planets., Measure the size and distribution of dust grains, Provide measurements of the zodiacal cloud in other systems. WFIRST/2.4 will: Measure the amount and distribution of circumstellar dust, Measure the large scale structure of disks, revealing the presence of asteroid belts and gaps due to unseen planets., Measure the size and distribution of dust grains, Provide measurements of the zodiacal cloud in other systems. Debris disk around the young (~100 Myr), nearby (28 pc) sun-like (G2 V0) star HD

Guest Investigator Science. HST aperture with ~200 the FOV. Archival science in bulge, SNe and HLS surveys. ~25% of time to GO programs. High Latitude Survey ~2000 sq. degrees in four filters + slitless grism spectrscopy.

To Do. HST imaging of target fields. Spitzer/Kepler monitoring of microlensing events. HST follow-up of planet detections. H-band ground-based microlensing survey. Manpower!

Summary. The demographics of planets beyond the snow line provides crucial constraints on planet formation theories and habitability. AFTA-WFIRST enables qualitatively new, exciting science: sub-Earth-mass planets, free-floating planets, outer habitable zone planets, mass measurements. AFTA-WIFRST will complete the census begun by Kepler, and will revolutionize our understanding of cold planets. But, lots to do!

Exoplanet Science with WFIRST.

WFIRST+C Exoplanet Science Microlensing Survey High Contrast Imaging Monitor 200 million Galactic bulge stars every 15 minutes for 1.2 years 2800 cold exoplanets 300 Earth-mass planets 40 Mars-mass or smaller planets 40 free-floating Earth-mass planets Survey up to 200 nearby stars for planets and debris disks at contrast levels of on angular scales > 0.2 R=70 spectra and polarization between nm Detailed characterization of up to a dozen giant planets. Discovery and characterization of several Neptunes Detection of massive debris disks. The combination of microlensing and direct imaging will dramatically expand our knowledge of other solar systems and will provide a first glimpse at the planetary families of our nearest neighbor stars. Complete the Exoplanet Census Complete the Exoplanet Census Discover and Characterize Nearby Worlds How do planetary systems form and evolve? What are the constituents and dominant physical processes in planetary atmospheres? What kinds of unexpected systems inhabit the outer regions of planetary systems? What are the masses, compositions, and structure of nearby circumstellar disks? Do small planets in the habitable zone have heavy hydrogen/helium atmospheres? How do planetary systems form and evolve? What are the constituents and dominant physical processes in planetary atmospheres? What kinds of unexpected systems inhabit the outer regions of planetary systems? What are the masses, compositions, and structure of nearby circumstellar disks? Do small planets in the habitable zone have heavy hydrogen/helium atmospheres?

Toward the Pale Blue Dot Microlensing Survey High Contrast Imaging Inventory the outer parts of planetary systems, potentially the source of the water for habitable planets. Quantify the frequency of solar systems like our own. Confirm and improve Keplers estimate of the frequency of potentially habitable planets. When combined with Kepler, provide statistical constraints on the densities and heavy atmospheres of potentially habitable planets. Provide the first direct images of planets around our nearest neighbors similar to our own giant planets. Provide important insights about the physics of planetary atmospheres through comparative planetology. Assay the population of massive debris disks that will serve as sources of noise and confusion for a flagship mission. Develop crucial technologies for a future mission, and provide practical demonstration of these technologies in flight. WIFRST will lay the foundation for a future flagship direct imaging mission capable of detection and characterization of Earthlike planets. Science and technology foundation for the New Worlds Mission. Courtesy of Jim Kasting.