1. 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

2. 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

3. 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

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

5. 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

6. 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

7. 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

8. 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

9. 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

10. Thank You