Planet-hunting with Adaptive Optics & Interferometry

JWST Aperture Synthesis with NIRISS Non-Redundant Mask

~65 mas angular resolution imagingin F380M F430M & F480MAnand SivaramakrishnanSTScI, JWST NIRISS Science Team, JAM leadSaavik Ford, Barry McKernanCity University of New YorkDavid Lafrenire University of Montral, JWST NIRISS Science TeamPeter Tuthill University of Sydney

11NIRISS (ne TFI)2

Fullerton2NIRISS (ne TFI)3

F430M PSF CLEARFullertonF430M PSF NRM

65 mas pixelsNyquist at 4 micronWebbPSF Python module (Perrin)Primary Beam 40 pixels 2.53

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7Wilner (CfA) NRAO Summer School notes78Wilner (CfA) NRAO Summer School notes

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ONE VOLTAGEper antenna

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E1(t)E2(t)Correlator t One fringe per antenna pairVisibility (amplitude) & phase

t visibilityV12 = V12 exp{if12}14ONE VOLTAGEper antenna

15V12 = V12 exp{if12}V21 = V12 exp{-if12}

15Fourier transform image data

V = Abs(V ) displayed here f array has same areas of dataf is still a FRINGE PHASE 16

V = V(u,v) exp{if(u,v}Subapertures in pupilImage on detector

Each pixel points to different part of sky, acts like a different t in correlatorPixel records square of electric field1617

Fourier transform image data

V = Abs(V ) displayed here f array has same areas of dataf is still a FRINGE PHASE Subapertures in pupilImage on detector

Each pixel points to different part of sky, acts like a different t in correlatorPixel records square of electric fieldV = V(u,v) exp{if(u,v}17

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Good uv-coverage if you repeat an observationwith~ 60 degrees rotation (2 months ~1 fortnight)2223

Sivaramakrishnan, McKernan, Ford, Lafrenire, Tuthill, Teuben & Koda 03/2012MIRIAD invert; clean; restore using the normalized point source dirty map as cleans beam= 500 mas= 25pc @10MpcAGN with bar.Integrated magnitude of bar is 1 mag fainter than AGN core

Bar length 7 pix ~ 3.5 l/D2324

Sivaramakrishnan, McKernan, Ford, Lafrenire, Tuthill, Teuben & Koda 03/2012MIRIAD invert; clean; restore using the normalized point source dirty map as cleans beam= 500 mas= 25pc @10MpcAGN with bar.Integrated magnitude of bar is 1 mag fainter than AGN core

Bar length 7 pix ~ 3.5 l/DAdd noise to data, current Flight and possible future Gen2 Flight H2RG detectorsDevelop exposure time estimates and observing templatesSimulate various 2-orient exposures (probably dont need more)Introduce complicated structure in skyUse full aperture PSFs in mosaicing?Deliver our IDL + python(MIRIAD) pipeline (or algorithm definition) to STScIDevelop science cases for eg SODRM/GTO observationsRefine data simulatorEncourage advances in algorithms by NG NRMers Fourier or Image plane?24