1 Key Types Introduction Michelson Summer School on High-Contrast Imaging Caltech, Pasadena July 2004 Wesley A. Traub Harvard-Smithsonian Center for Astrophysics

2 C, IWA, OWA types perturbations Reminders of main topics

3 C Ref: McCarthy & Zuckerman (2004); Macintosh et al (2003) 20 arcsec radius circle K~20 mag Bkgd objects 7 arcsec wand J~21 mag Bkgd object

4 Search space: best to date Airy Halo 1.Keck 2.IRCAL, Lick AO, K 3.Ks, AO, NACO, VLTI 4.WFPC2, HST, I 5.CFHT, AO, H 6.Keck NICMOS, 10sig 7.50% det, HST, H 8.XAO, 10m, R, 2007

5 Earth & Jupiter-Saturn, 100 stars Simulations by Bob Brown, STScI

6 Earth & Jupiter-Saturn Regions

7 Radial-velocity Stars

8 RV stars and brown dwarfs

9 1.8-m range

10 TPF-C Range

11 C, IWA, OWA Contrast C: Example: C = driven by Earth/Sun = 2x Inner working angle IWA: Example: IWA = 3 /D driven by 1 AU/10pc = arcsec. Outer working angle OWA: Example: OWA = 48 /D driven by N = 96 actuator DM.

12 Image-plane coronagraph simulation Ref.: Pascal Borde st pupil 1st image with Airy rings mask, centered on star image 2nd pupil Lyot stop, blocks bright edges 2nd image, no star, bright planet

13 Wide-band (quadrant-phase) mask

14 Shaped-pupil mask Kasdin, Vanderbei, Littman, & Spergel, preprint, 2004 Pupil: Spergel-Kasdin prolate-spheroidal mask Image: dark areas < transmission Image: cut along the x-axis v u A(x, 0) = exp(-(  x/ ) 2 ) A(0, y) = periodic & messy x y

15 Discrete-mapped pupil (2): Densification Entrance pupil, sparsely filled FOV is small. Image with many aliases Densified pupil Clean image, narrow FOV

16 Continuous-mapped pupil Compact star image, easily blocked Input wavefront: uniform amplitude. Mirror 1 Mirror 2 Output wavefront: prolate-spheroidal amplitude. 100 dB = = 25 mag Output image: prolate spheroid

17 Nulling-shearing coronagraph

18 Phase ripple and speckles No DM: With DM: Phase ripples from primary mirror errors Polishing errors on primary Speckles generated by 3 sinusoidal components of the polishing errors Pupil plane Image plane

19 Phase + amplitude ripple and speckles h(u) =  n (a n +ia n ')cos(Knu) + (b n +ib n ')sin(Knu) = total ripples Describes all possible phase and amplitude ripples (= errors). DM can give I(  ) =  (0) +  n [(b n ’) 2 + (a n ’) 2 ]  (k  +Kn)  bigger speckles + [ ]  (k  -Kn)]  smaller (zero) speckles