1. JWST TFI Non-Redundant Mask the JAMEx team
Anand Sivaramakrishnan (STScI) David Lafreniere (U. de Montreal) Peter Tuthill (Sydney) James Lloyd (Cornell) Michael Ireland (Macquarie) Frantz Martinache (Subaru) Laurent Pueyo (JHU) Barry McKernan (CUNY) Saavik Ford (CUNY) André Martel (STScI) Laura Ferrarese (HIA) John Hutchings Anton Koekemoer (STScI) Doug Johnstone (HIA) Alexandra Greenbaum (JHU)
Exoplanets
1 - NRM mask on JWST - holes exposing 7 mirrors;     undersized (pupl shear) miss spiders, large separations, 3.8-5um R 100
2 - interferometry vs imaging Airy vs Michelson
3 - space vs ground - stability of  phase, quality of phase, quality of amplitude,    chromatic two-or-more waves with TFI, thermal IR background from ground
4 - ground-based NRM data analysis: optical – CP
5 - observing sequence for point sources (binaries) by Lafreniere on HR8799 sim and    contrast ratio curve, SUB256 picture, mag limit ~5 in M
6 - observing sequence by McK+Ford and CA significance for symmetric structure (equal binaries, eg)
7 - ground-based radio interferometry analysis for JWST NRM data (MIRIAD/CASA) -     JW NRM has DC component like ALMA
8 - extended structure in space: multi-month observing and aperture synthesis
9 - NRM can coarse phase and fine phase JWST with TFI
Extragalactic

2. The mask Seven apertures in pupil Undersized for pupil shear
21 interferometers
NR: No repeated baselines
15% throughput
l/dl = R ~100 etalon
Bright limit M ~5
65mas pixel limits NRM to um
1 - NRM mask on JWST - holes exposing 7 mirrors;     undersized (pupl shear) miss spiders, large separations, 3.8-5um R 100
2 - interferometry vs imaging Airy vs Michelson
3 - space vs ground - stability of  phase, quality of phase, quality of amplitude,    chromatic two-or-more waves with TFI, thermal IR background from ground
4 - ground-based NRM data analysis: optical – CP
5 - observing sequence for point sources (binaries) by Lafreniere on HR8799 sim and  contrast ratio curve, SUB256 picture, mag limit ~5 in M
6 - observing sequence by McK+Ford and CA significance for symmetric structure (equal binaries, eg)
7 - ground-based radio interferometry analysis for JWST NRM data (MIRIAD/CASA) -     JW NRM has DC component like ALMA
8 - extended structure in space: multi-month observing and aperture synthesis
9 - NRM can coarse phase and fine phase JWST with TFI

3. Signal is not the problem Throw away light but get the science!
Rayleigh
Criterion
 = /D
Michelson
Criterion
 = 0.5 /D
Huge blob Airy
Price of redundancy of many short baselines
If you know you’re looking for a binary the tight core of fringe is great!
GPI coronograph
FPM dia /D
NRM sweet spot
0.5 to 5 /D 3

4. Space advantage: stability of wavefront AMPLITUDE
PHARO PALAO Martinache, Bernat, Lloyd & PalAO team. Ks, exptime ~3.5s Lafreniere & JAM Team: many noise sources included – target acq error, pointing/jitter, intra-pixel sensitivity, read noise, flat field, TFI throughput. l = 4.6um. PSF modelling following Makidon et al 2008 SPIE and Sivaramakrishnan et al SPIE 2009

5. JWST thermal drift 2011_Strange_fig2.png and eps
Ground L-band Keck - Hinkley et al 2011
2011_Strange_fig2.png and eps
Hinkley et al 7.5mag lam/D K Keck
8mag 73mas Hinkley et al 2011 Lband
Thermal drift modelling following Makidon et al 2008 SPIE

6. Aperture synthesis with JWST
21 interferometers
PSF at left
Single NRM PSF
Parmentier &
Sivaramakrishnan
Stony Brook testbed
UV coverage for TFI aperture synthesis

7. Aperture synthesis with JWST
21 interferometers
12 observations over 2 months
5 degree rotations between them
Single NRM PSF
Parmentier &
Sivaramakrishnan
Stony Brook testbed
UV coverage for TFI aperture synthesis

8. Aperture synthesis with JWST
21 interferometers
7 observations over 2 months
5 degree rotations between them
Single NRM PSF
Parmentier &
Sivaramakrishnan
Stony Brook testbed

9. Aperture synthesis with JWST
MIRIAD radio software applied to TFI NRM
Sivaramakrishnan & Teuben
Single NRM PSF
Parmentier &
Sivaramakrishnan
Stony Brook testbed
~1mas astrometry
Galactic Center in K
Keck Laser guide star AO
Ghez et al. UCLA

10. A JAMEx Science case Well-studied, bright nearby AGN
Key role in galaxy formation, & (via feedback) in LCDM cosmology
Accretion disk outer flared region ~? 1-20 pc in size
Already seen in N1068
Is the accretion torus clumpy?
Is there structure outside the torus?