Binary star systems where one of the stars is an exoplanet host appear to be more common than expected prior to the Kepler mission. The Kepler mission and subsequent ground-based follow-up work have revealed a number of Kepler Objects of Interest (KOIs) that have nearby stellar companions (within ~1 arcsec). KOIs with stellar companions and at least one suspected exoplanet were selected for this work. Recent work on these stars has mainly focused on placing the companions on the H-R diagram and inferring if they are likely to be gravitationally bound based on whether their locations are consistent with a common isochrone. However, we have been observing these KOI double stars with speckle imaging over several years and are now in a position to assess whether these systems have components with a common proper motion, and can be seen as physically associated on that basis. We will give sample results of KOI double stars that are in fact common proper motion pairs. We compare our results with estimates of the multiplicity rate of exoplanet hosts from other methods and comment on the use of our data for constraining orbital parameters at this point, particularly the inclination angle. For transit observations, the inclination of the planetary orbit is already known, and the relationship between planetary and stellar orbital planes could have implications for star and planet formation.
Here we demonstrate a novel lucky imaging camera which is designed to produce diffraction-limited imaging using
small telescopes similar to ones used by many academic institutions for outreach and/or student training. We
present a design that uses a Meade 12” SCT paired with an Andor iXon fast readout EMCCD. The PSF of the
telescope is matched to the pixel size of the EMCCD by adding a simple, custom-fabricated, intervening optical
system. We demonstrate performance of the system by observing both astronomical and terrestrial targets. The
astronomical application requires simpler data reconstruction techniques as compared to the terrestrial case. We
compare different lucky imaging registration and reconstruction algorithms for use with this imager for both
astronomical and terrestrial targets. We also demonstrate how this type of instrument would be useful for both
undergraduate and graduate student training. As an instructional aide, the instrument can provide a hands-on
approach for teaching instrument design, standard data reduction techniques, lucky imaging data processing,
and high resolution imaging concepts.
An experimental investigation of super-resolution imaging from measurements of projections onto a random
basis is presented. In particular, a laboratory imaging system was constructed following an architecture that
has become familiar from the theory of compressive sensing. The system uses a digital micromirror array
located at an intermediate image plane to introduce binary matrices that represent members of a basis set.
The system model was developed from experimentally acquired calibration data which characterizes the system
output corresponding to each individual mirror in the array. Images are reconstructed at a resolution limited
by that of the micromirror array using the split Bregman approach to total-variation regularized optimization.
System performance is evaluated qualitatively as a function of the size of the basis set, or equivalently, the
number of snapshots applied in the reconstruction.
We describe a prototype of an illumination system, the Ring of Fire (ROF), which is used as part of an internal
calibration system for large focal plane detector arrays in TMA (Three Mirror Anastigmat) telescope designs. Such
designs have been proposed for the SNAP (SuperNova Acceleration Probe) version of a Joint Dark Energy Mission
(JDEM). The ROF system illuminates the focal plane with a light beam the closely matches that of the telescope and is
used for creating high spatial frequency flat fields and monitoring filter bandpasses for experiments that demand a highly
accurate characterization of the detectors. We present measurements of a mockup of this prototype ROF design
including studies in variations in illumination across a large focal plane.
The nature of Dark Energy can by constrained by the precise determination of super-novae distance moduli in ultraviolet
to near IR pass-bands. Space-based observations are required for these moduli to be measured with the scientifically
required photometric accuracies. Consequently, robust pass-band filters operable at cryogenic temperatures (120-140K)
are needed that have challenging performance attributes including high in-band transmission, low ripple, good out-ofband
rejection, and moderate band-edge slope. We describe the requirements and performance of dielectric multi-layer
filters with spectral profiles that are suitable for both achieving the science and for accurate calibration using plausible
on-orbit measurement systems.
We report the effects of radiation damage due to ionizing protons on InGaAs photodiodes. The photodiodes
were irradiated at energies of 30, 52, and 98 MeV and fluences up to 1010 protons/cm2 in experiments at the
Indiana University Cyclotron Facility. The photodiodes were tested for changes in their dark current, their
relative responsivity as a function of wavelength from 1000 - 1600 nm, and their absolute responsivity in narrow
bandpasses spread throughout the same wavelength region. The measurements were all made with detectors
traceable to NIST standards. At these exposures and energies, the most significant effects are seen in the dark
current levels.
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