Date of download: 6/21/2016 Copyright © 2016 SPIE. All rights reserved. The empirical radius of a planet is shown as a function of mass, by the blue curve, as given by the formula in the text. The mass values of the 460 known RV planets are projected onto this curve, and shown as small blue circles, from which point the inferred radii can be read. For comparison, the 264 exoplanets that have known values of radii as well as mass are shown as small red circles, and solar system objects are shown as black triangles. Figure Legend: From: Science yield estimate with the Wide-Field Infrared Survey Telescope coronagraph J. Astron. Telesc. Instrum. Syst. 2016;2(1): doi: /1.JATIS

Date of download: 6/21/2016 Copyright © 2016 SPIE. All rights reserved. Geometric albedo of Jupiter and Uranus, 17 showing the albedo as a function of wavelength, the characteristic widths of spectral features (nearly all CH4), the four proposed filter locations and widths, and the three proposed spectrometer bands and resolution elements, drawn here at a resolution of R=70, chosen to approximately match the widths of the narrowest features in these spectra, and therefore maximize the accuracy of inferred CH4 mixing ratios. Figure Legend: From: Science yield estimate with the Wide-Field Infrared Survey Telescope coronagraph J. Astron. Telesc. Instrum. Syst. 2016;2(1): doi: /1.JATIS

Date of download: 6/21/2016 Copyright © 2016 SPIE. All rights reserved. Contrast versus angular separation for the 127 exoplanets in the RV catalog used in this paper, assuming circular orbits, i=60 deg inclination, θ=70 deg orbital location, p=0.50 visible albedo, and Lambert phase function. Figure Legend: From: Science yield estimate with the Wide-Field Infrared Survey Telescope coronagraph J. Astron. Telesc. Instrum. Syst. 2016;2(1): doi: /1.JATIS

Date of download: 6/21/2016 Copyright © 2016 SPIE. All rights reserved. Transmission factors for the coronagraphs on WFIRST, showing the wavelength dependence of quantum efficiency and mirror reflectivity, and the nominal wavelength independence of the secondary blockage and filter terms. Figure Legend: From: Science yield estimate with the Wide-Field Infrared Survey Telescope coronagraph J. Astron. Telesc. Instrum. Syst. 2016;2(1): doi: /1.JATIS

Date of download: 6/21/2016 Copyright © 2016 SPIE. All rights reserved. Transmission factors for all three coronagraphs, as a function of planet–star separation. The design wavelength is 550 nm, so for other wavelengths, the planet–star axis must be scaled proportional to wavelength. The bottom group, Ω (square arc-second, as2), is the projected solid angle on the sky of the FWHM of the PSF. The middle group, Tpoint, is the transmission factor for point sources, and the upper group, Tdiffuse, is the transmission for a diffuse source, here the solar system zodi. The T values are for single polarization for HLC and PIAACMC, and unpolarized light for SPC. Figure Legend: From: Science yield estimate with the Wide-Field Infrared Survey Telescope coronagraph J. Astron. Telesc. Instrum. Syst. 2016;2(1): doi: /1.JATIS

Date of download: 6/21/2016 Copyright © 2016 SPIE. All rights reserved. Contrast of speckles in the dark hole for each coronagraph, for a small residual jitter (0.4 mas RMS) and a large residual jitter (1.6 mas RMS), at the design wavelength of 550 nm. For other wavelengths, the planet–star angle is replaced by one that is wavelength scaled, as suggested by the λ/D axis at the top. Figure Legend: From: Science yield estimate with the Wide-Field Infrared Survey Telescope coronagraph J. Astron. Telesc. Instrum. Syst. 2016;2(1): doi: /1.JATIS

Date of download: 6/21/2016 Copyright © 2016 SPIE. All rights reserved. Simulated WFIRST-AFTA coronagraph image of the star 47 Ursa Majoris, showing two directly detected planets (from Ref. 1), for HLC, and with a field of view radius of 0.5 arc sec. A PSF reference has been subtracted, improving the raw contrast by a factor of 10. Figure Legend: From: Science yield estimate with the Wide-Field Infrared Survey Telescope coronagraph J. Astron. Telesc. Instrum. Syst. 2016;2(1): doi: /1.JATIS

Date of download: 6/21/2016 Copyright © 2016 SPIE. All rights reserved. Science imaging yield of known RV planets with HLC. Solid symbols are RV planets detectable with HLC in a 15% band centered at 565 nm, in less than a day each, in a single polarization, with a signal strength greater than the worst-case floor (long-dash line, 1.6 mas RMS pointing jitter, and a postprocessing factor of 1/10). The open symbols are for the additional detections possible with the best-case floor (0.4 mas jitter, 1/30 factor). Typical relative uncertainties in contrast and separation (Sec. 2.4) are indicated. Figure Legend: From: Science yield estimate with the Wide-Field Infrared Survey Telescope coronagraph J. Astron. Telesc. Instrum. Syst. 2016;2(1): doi: /1.JATIS

Date of download: 6/21/2016 Copyright © 2016 SPIE. All rights reserved. Science imaging yield of known RV planets with SPC. Solid symbols are RV planets detectable with SPC in a 15% band centered at 565 nm, in less than a day each, in both polarizations simultaneously, with a signal strength greater than the worst-case floor (long- dash line, 1.6 mas RMS pointing jitter, and a postprocessing factor of 1/10). The open symbol is for the additional detection possible with the best-case floor (0.4 mas jitter, 1/30 factor). Typical relative uncertainties in contrast and separation (Sec. 2.4) are indicated. Figure Legend: From: Science yield estimate with the Wide-Field Infrared Survey Telescope coronagraph J. Astron. Telesc. Instrum. Syst. 2016;2(1): doi: /1.JATIS

Date of download: 6/21/2016 Copyright © 2016 SPIE. All rights reserved. Science imaging yield of known RV planets with PIAACMC. The solid symbol is for the single RV planet detectable with PIAACMC in a 15% band centered at 565 nm, in less than a day each, in a single polarization, with a signal strength greater than the worst- case floor (long-dash line, 1.6 mas RMS pointing jitter, and a postprocessing factor of 1/10). The numerous open symbols are for the additional detections possible with the best-case floor (0.4 mas jitter, 1/30 factor). Typical relative uncertainties in contrast and separation (Sec. 2.4) are indicated. Figure Legend: From: Science yield estimate with the Wide-Field Infrared Survey Telescope coronagraph J. Astron. Telesc. Instrum. Syst. 2016;2(1): doi: /1.JATIS