Adaptive optics calibration for a wide-field microscope

2008 ◽  
Author(s):  
Janice Castillo ◽  
Thomas Bifano
Keyword(s):  
Adaptive Optics ◽  
Wide Field

scholarly journals Wide field astronomical image compensation with multiple laser-guided adaptive optics

2009 ◽  
Author(s):  
Michael Hart ◽  
N. Mark Milton ◽  
Christoph Baranec ◽  
Thomas Stalcup ◽  
Keith Powell ◽  
...  
Keyword(s):  
Adaptive Optics ◽  
Wide Field ◽  
Astronomical Image ◽  
Image Compensation

scholarly journals Using ground based data as a precursor for Gaia in getting proper motions of satellites

2017 ◽  
Vol 12 (S330) ◽  
pp. 210-213
Author(s):  
Tobias K. Fritz ◽  
Sean T. Linden ◽  
Paul Zivick ◽  
Nitya Kallivayalil ◽  
Jo Bovy
Keyword(s):  
Adaptive Optics ◽  
Globular Cluster ◽  
Proper Motion ◽  
Milky Way ◽  
Dwarf Galaxy ◽  
Optical Data ◽  
Line Of Sight ◽  
Wide Field ◽  
Proper Motions ◽  
Tidal Stream

AbstractWe present our effort to measure the proper motions of satellites in the halo of the Milky Way with mainly ground based telescopes as a precursor on what is possible with Gaia. For our first study, we used wide field optical data from the LBT combined with a first epoch of SDSS observations, on the globular cluster Palomar 5 (Pal 5). Since Pal 5 is associated with a tidal stream it is very useful to constrain the shape of the potential of the Milky Way. The motion and other properties of the Pal 5 system constrain the inner halo of the Milky Way to be rather spherical. Further, we combined adaptive optics and HST to get an absolute proper motion of the globular cluster Pyxis. Using the proper motion and the line-of-sight velocity we find that the orbit of Pyxis is rather eccentric with its apocenter at more than 100 kpc and its pericenter at about 30 kpc. The dynamics excludes an association with the ATLAS stream, the Magellanic clouds, and all satellites of the Milky Way at least down to the mass of Leo II. However, the properties of Pyxis, like metallicity and age, point to an origin from a dwarf of at least the mass of Leo II. We therefore propose that Pyxis originated from an unknown relatively massive dwarf galaxy, which is likely today fully disrupted. Assuming that Pyxis is bound to the Milky Way we derive a 68% lower limit on the mass of the Milky Way of 9.5 × 1011 M⊙.

scholarly journals Active optics in astronomy – modeling of deformable substrates: freeform surfaces for FIREBall and MESSIER

2018 ◽  
Vol 27 (5-6) ◽  
Author(s):  
Gérard Rene Lemaitre
Keyword(s):  
Adaptive Optics ◽  
Large Scale ◽  
Wide Field ◽  
Freeform Surfaces ◽  
Aspheric Surfaces ◽  
Massive Black Holes ◽  
Active Optics ◽  
Minimum Number ◽  
Co Addition ◽  
Large Telescopes

AbstractActive optics techniques on large telescopes and astronomical instrumentations provide high imaging quality. For ground-based astronomy, the co-addition of adaptive optics again increases angular resolution up to providing diffraction-limited imaging at least in the infrared. Active and adaptive optics marked milestone progress in the detection of exoplanets, super-massive black holes, and large-scale structure of galaxies. This paper is dedicated to highly deformable active optics that can generate non-axisymmetric aspheric surfaces – or freeform surfaces – by use of a minimum number of actuators: a single uniform load acts over the surface of a vase-form substrate whilst under reaction to its elliptical perimeter ring. Two such instruments are presented: (1) the Faint Intergalactic Redshifted Emission Balloon (FIREBall) telescope and multi object spectrograph (MOS) where the freeform reflective diffraction grating is generated by replication of a deformable master grating, and (2) the MESSIER wide-field low-central-obstruction three-mirror-anastigmat (TMA) telescope proposal where the freeform mirror is generated by stress figuring and elastic relaxation. Freeform surfaces were obtained by plane super-polishing. Preliminary analysis required use of the optics theory of 3rd-order aberrations and elasticity theory of thin elliptical plates. Final cross-optimizations were carried out with Zemax raytracing code and Nastran FEA elasticity code in order to determine geometry of the deformable substrates.

Wide field of view retinal imaging using one-micrometer adaptive optics scanning laser ophthalmoscope

2011 ◽  
Author(s):  
Kazuhiro Sasaki ◽  
Kazuhiro Kurokawa ◽  
Shuichi Makita ◽  
Daiki Tamada ◽  
Yiheng Lim ◽  
...  
Keyword(s):  
Adaptive Optics ◽  
Retinal Imaging ◽  
Scanning Laser Ophthalmoscope ◽  
Field Of View ◽  
Scanning Laser ◽  
Wide Field ◽  
Wide Field Of View

Imaka: a test bench for very wide field adaptive optics at the UH2.2m telescope

2020 ◽  
Author(s):  
Olivier Lai ◽  
Mark Chun ◽  
Jessica Lu ◽  
Doug Toomey ◽  
Christoph Baranec ◽  
...  
Keyword(s):  
Adaptive Optics ◽  
Test Bench ◽  
Wide Field

Wide field adaptive optics correction for the GMT using natural guide stars

2014 ◽  
Author(s):  
Marcos A. van Dam ◽  
Antonin H. Bouchez ◽  
Brian A. McLeod
Keyword(s):  
Adaptive Optics ◽  
Wide Field

Static and predictive tomographic reconstruction for wide-field multi-object adaptive optics systems

2013 ◽  
Vol 31 (1) ◽  
pp. 101 ◽  
Author(s):  
C. Correia ◽  
K. Jackson ◽  
J.-P. Véran ◽  
D. Andersen ◽  
O. Lardière ◽  
...  
Keyword(s):  
Adaptive Optics ◽  
Tomographic Reconstruction ◽  
Wide Field
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