Extra Solar Planet Science With a Non Redundant mask Stefenie N. Minto (UMES, STScI) Alexandra Greenbaum (JHU, STScI) Anand Sivaramakrishnan(STScI) Deepashri Thatte(STScI) Kathryn St. Laurent (STScI

Non Redundant Mask Aperture Masked Interferometry (AMI) mode For high angular resolution imaging We use a 7 hole nrm in the pupil of the telescope .The NRM is used for high angular resolution imaging for the AMI mode in NIRISS

Fringe Phase & Visibility Wide Diffraction Pattern Single slit Narrow Diffraction Pattern Double slit Where the sharp fringes are within the broad pattern Is the fringe phase Clarity of the fringe is the fringe visibility As the image becomes more resolved the fringes becomes less noticeable this is why the interferometer is sensitive to image size and structure -when you have a single narrow slit -we measure fringe phase a visibility (begin)) Single narrow slit makes a wide diffraction pattern V ~ 0.5 V = 0 V ~ 1

Object seen through telescope in sky Object seen through telescope Star seen through telescope Single Star Image Same Star with Planet

Image With and Without Planet Different stretch in DS9 -Heres a different view with a different gray scale The planet light fills in the dark part of the single star image

Find Companions in three steps Measure Fringe Phases & Fringe Amplitudes in the image Calibrate the Data Look at Single Stars to Remove Instrument Effects Fit Model to Star & Planet Data Fitting fringe Phases to the Model The model is the mathematical model which is coded up in python The model is what the data will look like if you assumed the contrast seperation and posistion angle and then we find which contrast seperation and posistion fit the fringe phases best

How will Pixel Scale affect the results? Experimental Set up How will Pixel Scale affect the results? - Simulate NIRISS data at one pixel scale Fit data with different pixel scales Measure parameters at different pixel scales To know how reliable our data reduction method will be for NIRISS images The pixel scale is the angular size of the pixel What that means is when you take a picture with NIRISS what angel in the sky spans one pixel

Results Very small change to position angle and contrast ratio Whatever our uncertainty is in the pixel scale error tell us the uncertainty in our measurement . A small pixel scale error does not change the measured position angel and contrast ratio however the measured separation is more sensitive to the pixel scale error

Next Steps Apply my code to explore new problems like Higher contrast binary Smaller separation Under sampled data The exact orientation of the NRM Any other instrument parameters we can simulate This program explores different effects on our simulated measurements so we have a good idea of how well we can rely on our measurements which gives us a structure to explore other uncertainties in the data

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