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Anand Sivaramakrishnan STScI , JWST NIRISS Science Team, JAM lead Saavik Ford, Barry McKernan

JWST Aperture Synthesis with NIRISS ’ Non-Redundant Mask ~65 mas angular resolution imaging in F380M F430M & F480M. Anand Sivaramakrishnan STScI , JWST NIRISS Science Team, JAM lead Saavik Ford, Barry McKernan City University of New York David Lafrenière

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Anand Sivaramakrishnan STScI , JWST NIRISS Science Team, JAM lead Saavik Ford, Barry McKernan

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  1. JWST Aperture Synthesis with NIRISS’ Non-Redundant Mask~65 mas angular resolution imagingin F380M F430M & F480M Anand Sivaramakrishnan STScI, JWST NIRISS Science Team, JAM lead Saavik Ford, Barry McKernan City University of New York David Lafrenière University of Montréal, JWST NIRISS Science Team Peter Tuthill University of Sydney

  2. NIRISS (née TFI) Fullerton

  3. F430M PSF CLEAR F430M PSF NRM 65 mas pixels Nyquist at 4 micron Primary Beam  40 pixels 2.5” NIRISS (née TFI) WebbPSF Python module (Perrin) Fullerton

  4. Wilner (CfA) NRAO Summer School notes

  5. Wilner (CfA) NRAO Summer School notes

  6. Wilner (CfA) NRAO Summer School notes

  7. Wilner (CfA) NRAO Summer School notes

  8. Wilner (CfA) NRAO Summer School notes

  9. Wilner (CfA) NRAO Summer School notes

  10. Wilner (CfA) NRAO Summer School notes

  11. Wilner (CfA) NRAO Summer School notes

  12. Wilner (CfA) NRAO Summer School notes

  13. E1(t) E2(t) Correlator t ONE VOLTAGE per antenna One fringe per antenna pair Visibility (amplitude) & phase V12 = V12 exp{if12} visibility t

  14. V21 = V12 exp{-if12} ONE VOLTAGE per antenna V12 = V12 exp{if12}

  15. Subapertures in pupil Image on detector Each pixel points to different part of sky, acts like a different tin correlator Pixel records square of electric field Fourier transform image data V = Abs(V ) displayed here f array has same areas of data f is still a FRINGE PHASE V= V(u,v) exp{if(u,v}

  16. Subapertures in pupil Image on detector Each pixel points to different part of sky, acts like a different tin correlator Pixel records square of electric field Fourier transform image data V = Abs(V ) displayed here f array has same areas of data f is still a FRINGE PHASE V= V(u,v) exp{if(u,v}

  17. Good uv-coverage if you repeat an observation with~ 60 degrees rotation (2 months ± ~1 fortnight)

  18. MIRIAD invert; clean; restore – using the normalized point source dirty map as clean’s beam AGN with bar. Integrated magnitude of bar is 1 mag fainter than AGN core Bar length 7 pix ~ 3.5 l/D = 500 mas = 25pc @10Mpc Sivaramakrishnan, McKernan, Ford, Lafrenière, Tuthill, Teuben & Koda 03/2012

  19. MIRIAD invert; clean; restore – using the normalized point source dirty map as clean’s beam AGN with bar. Integrated magnitude of bar is 1 mag fainter than AGN core Bar length 7 pix ~ 3.5 l/D = 500 mas = 25pc @10Mpc Add noise to data, current Flight and possible future Gen2 Flight H2RG detectors Develop exposure time estimates and observing templates Simulate various 2-orient exposures (probably don’t need more) Introduce complicated structure ‘in sky’ Use full aperture PSFs in mosaicing? Deliver our IDL + python(MIRIAD) pipeline (or algorithm definition) to STScI Develop science cases for eg SODRM/GTO observations Refine data simulator Encourage advances in algorithms by NG NRM’ers – Fourier or Image plane? Sivaramakrishnan, McKernan, Ford, Lafrenière, Tuthill, Teuben & Koda 03/2012

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