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Wide Field Infrared Survey Telescope Science Yield

Wide Field Infrared Survey Telescope Science Yield. . Michael Levi (Lawrence Berkeley National Laboratory), M. Lampton ( UCBerkeley Space Sciences Lab), and M. Sholl ( UCBerkeley Space Sciences Lab ). WFIRST: Top Recommendation of Astro 2010

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Wide Field Infrared Survey Telescope Science Yield

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  1. Wide Field Infrared Survey Telescope Science Yield  Michael Levi (Lawrence Berkeley National Laboratory), M. Lampton (UCBerkeley Space Sciences Lab), and M. Sholl (UCBerkeley Space Sciences Lab) • WFIRST: Top Recommendation of Astro 2010 • Dark energy investigations using Weak Lensing, BAO, and Supernovae • Exoplanetmicrolensing survey in the Galactic Bulge • Wide field guest investigation surveys in the near infrared • New Developments Since Astro 2010 Report • Unobscured aperture shown highly effective at boosting S/N ratio • > Allows higher survey rate for the same aperture: more survey science per year • > Lampton et al., Proc SPIE 7731 (2010) • Focal optical train allows separate focal lengths for imaging and spectroscopy • > Permits high resolution WL survey & EPML with high signal to noise ratio • > Simultaneously delivers wide field slitless spectroscopy with coarser pixel scale • > Sholl et al., Proc SPIE 7731 (2010) and Sholl et al., this AAS conference (2011). • Large focal plane (8x4 MCTs) designed, built, and undergoing space qualification • > Higher pixel count and higher survey rate for the high resolution imager • > Jelinsky et al., this AAS conference (2011) • Four alternative WFIRST Payloads: • Telescope aperture 1.3 or 1.5m unobscured • Pixel scales: imager= 0.18 arcsec; spectrom=0.36 or 0.44 arcsec • Field of view: imager = spectrometer = 0.26 or 0.33 sq degrees simultaneously • Articulated solar panels & 45º front baffle angle for nearly 270 days/year on Bulge • Fully articulated K-band antenna for continuous downlink: 3 ground stations • Orbit: Earth-Sun L2 halo orbit similar to JWST • Weak Lensing Simulation: • > Galaxy sizes & fluxes from zCOSMOS: Leauthaud et al 2008; Jouvel et al 2009 • > Survey rate is set by FoV and exposure time reaching 25th magnitude • BAO Simulation: • > Emission line galaxy fluxes, sizes, and redshifts from Ilbert et al 2005 • > Survey rate chosen to deliver 66% detection at F=2.0e-16 erg/cm2.s • Supernova Simulation: • > Assumes discoveries are given; WFIRST does only the follow-up spectroscopy • > Eight spectra distributed over light curve + one deep spectrum near peak • ExoplanetMicrolensingFoM Scaling: • > Not a simulation; instead scaled from MPF mission projection (ref 6) • > Scaling factor = FoV * Aeff * ObsEffic * Δλ * λ /√NeffPixels • > ObsEffic allows 256 days/year articulated, or 128 days/year fixed panels • > We anticipate that the WFIRST Science Definition Team will do simulations Results Weak Lensing > High survey rate > High galaxy density Exoplanets > Unobscured aperture helps reduce confusion BAO > 2E-16 erg/cm2.s at 66% effic > High survey rate > Can co-observe with WL Supernovae > Can reach redshift z~1.4 > Superior SN yield > Wide λ range and z range help to control systematic errors We gratefully acknowledge the support by the Director, Office of Science, U.S. Department of Energy, through contract DE-AC03-76SF00098. Artwork by R.E.Lafever. Night sky image courtesy of NOAO.

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