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List of Figures

1.1 An example of the effects of seeing
1.2 Short exposure point spread functions
1.3 PSF shape changes induced by changing turbulence strength
1.4 Diagram of a typical LGS AO system
1.5 The capabilities of currently-available ground based imaging systems
1.6 Strehl ratio probabilities
2.1 The November 2005 version of LuckyCam (1)
2.2 The November 2005 version of LuckyCam (2)
2.3 A sketch of the optical layout of the 2005 version of LuckyCam.
2.4 L3CCD layout
2.5 L3CCD output signal probabilities
2.6 LuckyCam linearity verification
2.7 Typical LuckyCam output signal histogram
2.8 Photon counting
2.9 L3CCD gain measurement
2.10 The average horizontal shape of single-photon events
2.11 Calibration of LuckyCam photometry against SDSS standards
2.12 PixCel LC: LuckyCam data acquisition
2.13 PixCel LC data processing path
2.14 Realtime compression
2.15 The LuckyCam control interface.
2.16 Schematic of the LuckyCam control system
3.1 Comparison between the brightest speckle position and the centroid position
3.2 The distance between the PSF centroid and the brightest speckle, as a function of frame quality
3.3 The LuckyCam data reduction pipeline
3.4 Automated selection of guide stars
3.5 Cleanup processing
3.6 Lucky imaging processing flowchart
3.7 An example LUCKY settings file
3.8 The Drizzle process
3.9 Image reconstruction methods
3.10 Autoguider simulations
3.11 Rapid variations in cloud transmission
3.12 Detripling
4.1 Lucky Imaging of the core of M15
4.2 Average radial Lucky Imaging profiles
4.3 Resolution as a function of seeing and percentage selection
4.4 FWHM & FWHEF improvements
4.5 Airy rings
4.6 Isoplanatic patch example
4.7 Fast seeing variations
4.8 Lucky Imaging in B-band
4.9 Spectroscopy
4.10 Lucky Imaging of the Crab Nebula
4.11 High-time-resolution imaging of the Crab Pulsar
4.12 A comparison of HST and LuckyCam I-band imaging
4.13 Lucky Imaging SNR model
4.14 Guide star flux requirements
4.15 Frame rate requirements
5.1 Automated PSF fitting
5.2 PSF fitting accuracy
5.3 Speckle imaging example
5.4 L3CCD speckle imaging calibration process
5.5 Fitting binary parameters to power spectra
6.1 Known VLM binaries
6.2 Sample colour-magnitude diagram
6.3 The distribution of the target sample in K magnitude and V-K colour
6.4 Calibration of the LuckyCam photometry against SDSS standards
6.5 Contrast ratio sensitivity
6.6 Simulated faint companion PSFs
6.7 Lucky imaging of the five new binaries.
6.8 Mass models for LSPM J1735+2634
6.9 The companion to Ross 530
6.10 Mass ratios
6.11 Orbital radii
7.1 The two samples in K, V-K and distance
7.2 The observed samples, plotted in a V/V-K colour-magnitude diagram. The background distribution shows all stars in the LSPM-North catalogue.
7.3 The newly discovered binaries
7.4 The stars in the sample which have a spectral type listed in the SIMBAD database
7.5 LuckyCam and HST imaging of the triple system GJ1245AC
7.6 The orbit of GJ 1245AC
7.7 The fraction of stellar luminosity which appears as X-Ray emission in the X-ray sample targets.
7.8 The i-band contrast ratios of the detected binaries vs. separation in arcsecs
7.9 The i-band contrast ratios of the detected binaries vs. separation in AU
7.10 The histogram distribution of orbital radii of the detected binaries in the sample.
7.11 Orbital radius in the detected binaries as a function of colour
7.12 Cumulative orbital radius distributions

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