- Determine a wavelength-dependent Intrapixel Response Function (IPRF), describing the sensitivity of different areas within a single pixel. This will allow us to better analyse past and current data from the Kepler Space Telescope, and determine the extent of sensitivity dependence on wavelength.
Background Info:
- Original Kepler mission was launched into an Earth-trailing heliocentric orbit in March of 2009, with the goal of finding exoplanets around stars within a given area of the sky. The spacecraft would stay pointed at the exact same patch of space, continually observing the same set of stars, looking for the transits of exoplanets.
- Transits can be detected by observing the dips in brightness of stars as their planets pass in front of them.
- All kinds of information about these exoplanets can be gleaned from the data from these transits, planet size, orbital period, etc.
- Two of four reaction wheels on the spacecraft malfunctioned, unfortunately, so Kepler is no longer as stable, and currently has a drift of 3 milliarcseconds every ~6.5 hours..
- As such, it now shifts its field of view along the ecliptic every set number of days
- The current PRFs which are being used in flight were only produced by mathematical modelling and derivation, so taking measured data will greatly improve the accuracy of analysis.
Method and Interpretation:
- By scanning the area (27 microns by 27 microns) of an individual pixel on a copy of the in-flight cameras onboard with a tiny spot of light (2 microns approx.) and taking thousands of measurements, we can determine the response of the pixel across its area.
- Using a monochromator, we can produce any wavelength light within the visible to near IR spectrum.
- We can then map IRPFs for various wavelengths of light, and determine the rate at which different wavelengths of light drop off in sensitivity.
- The light is focused by a microscope lens, which brings it to a focal point about 20 mm away.
Results - TBD
Conclusions - TBD
Next Steps - cont. research
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