scholarly journals MAPPIT 2: Second Generation High-resolution Imaging at the AAT

1997 ◽  
Vol 14 (2) ◽  
pp. 189-194
Author(s):  
J. G. Robertson
Keyword(s):  
Spatial Resolution ◽  
Speckle Interferometry ◽  
Wavefront Sensor ◽  
One Dimension ◽  
High Resolution Imaging ◽  
Complex Objects ◽  
One Dimensional ◽  
Resolution Imaging ◽  
Ccd Detectors ◽  
Optical Telescopes

AbstractInterferometric methods have been used at a number of observatories to improve the spatial resolution of large optical telescopes, approaching and in some cases reaching the diffraction limit. The principal methods used have been speckle interferometry and non-redundant masking (NRM). The MAPPIT (Masked APerture Plane Interference Telescope) instrument has been used for NRM observations at the 3·9 m Anglo-Australian Telescope. This paper describes a proposed instrument, MAPPIT 2, which would use a Shack-Hartmann wavefront sensor in parallel with an interferometer performing NRM or one-dimensional speckle interferometry. The inclusion of the data from the wavefront sensor will enhance the sensitivity of the instrument, especially for the imaging of relatively complex objects (those giving more than a few resolution elements with non-zero intensities). Limiting the instantaneous spatial resolution to one dimension allows available CCD detectors to operate with 100% duty cycle. Observations at a number of position angles allow two-dimensional images to be obtained.

scholarly journals High Resolution Imaging Forty Years Ago

1994 ◽  
Vol 158 ◽  
pp. 337-341
Author(s):  
R. C. Jennison
Keyword(s):  
High Resolution ◽  
Point Sources ◽  
Resolving Power ◽  
High Angular Resolution ◽  
Electromagnetic Spectrum ◽  
High Resolution Imaging ◽  
Resolution Imaging ◽  
Optical Telescopes ◽  
Very High ◽  
Better Than

This conference is concerned with the very high resolution imaging of cosmic sources in many parts of the electromagnetic spectrum. Various techniques are now available and the equipment is often automated and highly sophisticated but the term ‘very high angular resolution’ is comparative. Many of the problems existed over forty years ago when the best resolving power was about half a degree and the two major radio ‘stars’ appeared to be point sources. Very high resolution imaging in those days was the struggle to reach one minute of arc and Hanbury Brown had set his sights on considerably better than one second of arc with the concept of the intensity interferometer. The dream was to achieve a resolving power comparable to that of optical telescopes.

scholarly journals HST and KECK Observations of High Redshift Radio Galaxies

1996 ◽  
Vol 175 ◽  
pp. 577-580
Author(s):  
W.J.M. Van Breugel
Keyword(s):  
Spatial Resolution ◽  
High Spatial Resolution ◽  
Hubble Space Telescope ◽  
High Redshift ◽  
Radio Galaxies ◽  
Space Telescope ◽  
Comprehensive Program ◽  
Resolution Imaging ◽  
High Spatial Resolution Imaging ◽  
Optical Telescopes

Together with several of my colleagues I have embarked on a comprehensive program to study the radio–aligned restframe UV structures in high redshift radio galaxies (HzRGs) using some of the world's premier optical telescopes: the Hubble Space Telescope for high spatial resolution imaging, and the Keck 10m telescope for high S/N spectropolarimetry. I will discuss some of our latest results from these observations which elucidate, and at the same time obscure, our evolving understanding of HzRGs.

scholarly journals High-Resolution Imaging in the Visible with Faint Reference Stars on Large Ground-Based Telescopes

2019 ◽  
Vol 08 (04) ◽  
pp. 1950015 ◽  
Author(s):  
Craig Mackay
Keyword(s):  
Angular Resolution ◽  
Image Resolution ◽  
Wavefront Sensor ◽  
High Resolution Imaging ◽  
Radon Transforms ◽  
New Approach ◽  
Wide Range ◽  
Resolution Imaging ◽  
Optic Systems ◽  
Low Order

Astronomers working with faint targets will benefit greatly from improved image quality on current and planned ground-based telescopes. At present, most adaptive optic systems are targeted at the highest resolution with bright guide stars. We demonstrate a significantly new approach for measuring low-order wavefront errors by using a pupil-plane curvature wavefront sensor design. By making low order wavefront corrections, we can deliver significant improvements in image resolution in the visible on telescopes in the 2.5–8.2 m range on good astronomical sites. As a minimum, the angular resolution will be improved by a factor of 2.5–3 under any reasonable conditions and, with further correction and image selection, even sharper images may be obtained routinely. We re-examine many of the assumptions about what may be achieved with faint reference stars to achieve this performance. We show how our new design of curvature wavefront sensor combined with wavefront fitting routines based on radon transforms allow this performance to be achieved routinely. Simulations over a wide range of conditions match the performance already achieved in runs with earlier versions of the hardware described. Reference stars significantly fainter than I [Formula: see text]17[Formula: see text]m may be used routinely to produce images with a near diffraction limited core and halo much smaller than that delivered by natural seeing.

scholarly journals The NASA High-Resolution Speckle Interferometric Imaging Program: Validation and Characterization of Exoplanets and Their Stellar Hosts

2021 ◽  
Vol 8 ◽  
Author(s):  
Steve B. Howell ◽  
Nicholas J. Scott ◽  
Rachel A. Matson ◽  
Mark E. Everett ◽  
Elise Furlan ◽  
...  
Keyword(s):  
High Resolution ◽  
Speckle Interferometry ◽  
High Resolution Imaging ◽  
Interferometric Imaging ◽  
High Resolution Imagery ◽  
Current Program ◽  
Crucial Information ◽  
Resolution Imaging ◽  
Stellar Properties

Starting in 2008, NASA has provided the exoplanet community an observational program aimed at obtaining the highest resolution imaging available as part of its mission to validate and characterize exoplanets, as well as their stellar environments, in search of life in the Universe. Our current program uses speckle interferometry in the optical (320–1,000 nm) with new instruments on the 3.5-m WIYN and both 8-m Gemini telescopes. Starting with Kepler and K2 follow-up, we now support TESS and other space- and ground-based exoplanet related discovery and characterization projects. The importance of high-resolution imaging for exoplanet research comes via identification of nearby stellar companions that can dilute the transit signal and confound derived exoplanet and stellar parameters. Our observations therefore provide crucial information allowing accurate planet and stellar properties to be determined. Our community program obtains high-resolution imagery, reduces the data, and provides all final data products, without any exclusive use period, to the community via the Exoplanet Follow-Up Observation Program (ExoFOP) website maintained by the NASA Exoplanet Science Institute. This paper describes the need for high-resolution imaging and gives details of the speckle imaging program, highlighting some of the major scientific discoveries made along the way.

Towards high resolution imaging by speckle interferometry

1978 ◽  
Vol 26 (1) ◽  
pp. 22-26 ◽  
Author(s):  
R.H.T. Bates ◽  
M.O. Milner ◽  
G.I. Lund ◽  
A.D. Seagar
Keyword(s):  
High Resolution ◽  
Speckle Interferometry ◽  
High Resolution Imaging ◽  
Resolution Imaging
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