Michael Levi (Lawrence Berkeley National Laboratory), M. Lampton (UCBerkeley Space Sciences Lab), and M. Sholl (UCBerkeley Space Sciences Lab) WFIRST:

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Presentation transcript:

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 Exoplanet microlensing survey in the Galactic Bulge Wide field guest investigation surveys in the near infrared Wide Field Infrared Survey Telescope Science Yield We gratefully acknowledge the support by the Director, Office of Science, U.S. Department of Energy, through contract DE-AC03-76SF Artwork by R.E.Lafever. Night sky image courtesy of NOAO. 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 25 th 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 Exoplanet Microlensing FoM 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 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) 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 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 Mission WFIRST AWFIRST BWFIRST CWFIRST DJDEMProbe AProbe B EuclidGESTMPF dichroicno dichroicdichroicno dichroicOmega no dichroicdichroicVISNIRSi CCDMCT ref 1 ref 2ref 3 ref 4ref 5ref 6 TelescopeTelescope Aperture=1.5m unobs1.3m unobs1.5m unobs1.3m unobs1.5m obs1.1m unobs 1.2mobs1.2m obs1.1m obsmeters aperture ImagerWavelength Range=0.5 to to to to to to to to to to 1.7microns Filter Bands=broad V, R, I, J, H V, R, I, JR+I+ZY, J, HRbroad Pixel Scale= arcsec Number of SCAs= SCAs Imager FoV= square degrees RESULTS: WLWL Survey Rate(25th mag)= sqdeg/year relative to JDEM-Omega relative to JDEM-Ω Single Waveband gal/sqarcmin gal/sqarcmin RESULTS: EPExoplanet Discovery Rate FoM= relative to MPF WFIRST w/ fixed solar panels= Data Rate= Mb/sec: 2:1 + 30% Slitless SpectroMethod=1 prism2 prisms1 prism 2 prisms1 prism none4 grismsnone Wavelength Range=1.5 to to to to to to 2.0 microns Halpha redshift range=1.3 to to to to to to 2.0 Pixel scale= arcsec Number of focal planes= FPs SCAs per focal plane= SCAs Spectrometer FoV= sq deg RESULTS: BAOBAO Survey Rate, erg= sqdeg/year relative to JDEM-Omega relative to JDEM-Omega SN SpectromMethod=IFU SlitlessSlit none Wavelength Range=0.4 to to 2.0 Slit scale= arc seconds RESULTS: SNeMax Redshift, SNe per year= : Sholl,M.J., et al.,217th AAS conf (2010); 2:Gehrels,N., arXiv (2010); 3: Content,D.A. et al., Proc SPIE 7731 (2010) 4: Duvet,L., "Euclid Reference Payload Document RD-s" ESA (2010); 5: Bennett,D.P. et al., GEST; Proc SPIE 4854 (2003); 6: Bennett,D.P., MPF; arXiv (2009).