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#Diffraction glasses toronto software#

Flat fielding errors need to be smaller thanĠ.1 % to reach ∼ 30 mag arcsec − 2. Statistics, but rather by systematic errors. The reason for the slow progress in lowering the limit for the detection of low surfaceīrightness structures is due to the fact that the limit is not defined by photon The missing satellites have very low surface brightnesses. Magnitude lower than expected from numerical simulations) may have a similar solution, if Satellites problem’ (in which the number of dwarf galaxies in the local group is orders of Telescopes for undertaking low surface brightness imaging. Suspect that the ‘missing substructure problem’ finds its origin in the limitations of our Telescopes typically reach surface brightness levels of ‘only’ ∼ 28 mag arcsec − 2 (e.g. However, deep imaging surveys with standard reflecting 2007) indicate that the majority of accreted stars live at surface brightness Detailed simulations of tidal debris around Limits to detect the predicted structures.

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Substructure problem’ is that we have not yet probed the required surface brightness Other studies of individual objects or small

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Spiral galaxies appear stubbornly unperturbed, even in deep images (e.g., Barton & Thompson 1997 Fry et al. (e.g., Toomre & Toomre 1972), a minority of elliptical galaxies and the vast majority of To undertake the first census of ultra-faint substructures in the nearby Universe.Īlthough tidal features in galaxies have been identified and studied for many decades The Dragonfly Telephoto Array is therefore executing aįully-automated multi-year imaging survey of a complete sample of nearby galaxies in order The ‘missing substructure’ and ‘missing satellite’ problems of conventional hierarchical The detection of structures at these surface brightness levels may hold the key to solving Telephoto Array is capable of probing structures with surface brightnesses below μ B = 32 mag arcsec − 2. Longer integrations (50-100h), foreground star removal and modest binning the Dragonfly Limiting the usefulness of much longer integration times has been identified. This is considerably deeper than the surfaceīrightness limit of any existing wide-field telescope. (without binning or foreground star removal). The Dragonfly Telephoto Array is capable of imaging extended structures to surfaceīrightness levels below μ B = 30 mag arcsec − 2 in ∼10h integrations Less scattered light at large radii than well-baffled reflecting telescopes. As a result, the array’s point spread function has a factor of ∼ 10 Surfaces coated with a new generation of anti-reflection coatings based on sub-wavelength System has no obstructions in the light path, optimized baffling, and internal optical Systematic errors that limit the accuracy of background estimation and flat-fielding. Through each lens, and with careful tracking of sky variations in order to minimize Data is collected with non-common optical paths Instrument control and robotic operation.

#Diffraction glasses toronto software#

The system is driven by custom software for Provides an imaging capability equivalent to a 0.4 m aperture f / 1.0 refractor with aĢ.6 ∘ × 1.9 ∘ field of view.

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The lenses are mounted on a common frameworkĪnd are co-aligned to image simultaneously the same position on the sky. The array consists of eight Canon 400 mm f / 2.8 L IS II USM telephoto lenses coupled toĮight science-grade commercial CCD cameras. We describe the Dragonfly Telephoto Array, a robotic imaging system optimized for theĭetection of extended ultra low surface brightness structures.

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