PYRAMIR: a near-infrared pyramid wavefront sensor for the Calar Alto adaptive optics system

2003 ◽  
Author(s):  
Joana B. Costa ◽  
Stefan Hippler ◽  
Markus Feldt ◽  
Simone Esposito ◽  
Roberto Ragazzoni ◽  
...  
Keyword(s):  
Adaptive Optics ◽  
Near Infrared ◽  
Wavefront Sensor ◽  
Adaptive Optics System ◽  
Calar Alto

scholarly journals Simulation Study of a Low-Light-Level Wavefront Sensor Driving a Low-Order, Near-IR Adaptive Optics System

1994 ◽  
Vol 158 ◽  
pp. 308-310
Author(s):  
David W. Tyler ◽  
Gary C. Loos
Keyword(s):  
Adaptive Optics ◽  
System Performance ◽  
Near Infrared ◽  
Light Level ◽  
Wavefront Sensor ◽  
High Fidelity ◽  
Low Light ◽  
Near Ir ◽  
Adaptive Optics System ◽  
Low Order

Two high-fidelity computer simulations are used to study low-order adaptive optics systems operating in the near-infrared. We study obtainable system performance using very dim reference sources at three IR wavelengths.

OPTICAL AND MECHANICAL DESIGN OF THE CHARA ARRAY ADAPTIVE OPTICS

2013 ◽  
Vol 02 (02) ◽  
pp. 1340007 ◽  
Author(s):  
X. CHE ◽  
L. STURMANN ◽  
J. D. MONNIER ◽  
T. A. TEN BRUMMELAAR ◽  
J. STURMANN ◽  
...  
Keyword(s):  
Adaptive Optics ◽  
Near Infrared ◽  
Angular Resolution ◽  
Mechanical Design ◽  
Wavefront Sensor ◽  
High Angular Resolution ◽  
Stellar Systems ◽  
Tilt Correction ◽  
Chara Array ◽  
Adaptive Optics System

The CHARA array is an optical/near infrared interferometer consisting of six 1-meter diameter telescopes with the longest baseline of 331 m. With high angular resolution, the CHARA array provides a unique and powerful way of studying nearby stellar systems. In 2011, the CHARA array was funded by NSF-ATI for an upgrade of adaptive optics systems to all six telescopes to improve the sensitivity by several magnitudes. The initial grant covers Phase I of the adaptive optics system, which includes an on-telescope Wavefront Sensor and fast tip/tilt correction. We are currently seeking funding for Phase II which will add fast deformable mirrors at the telescopes to close the loop. This paper will describe the design of the project, and show simulations of how much improvement the array will gain after the upgrade.

scholarly journals Companion Detection Limits with Adaptive Optics Coronagraphy

2004 ◽  
Vol 202 ◽  
pp. 99-102
Author(s):  
B. R. Oppenheimer ◽  
R. G. Dekany ◽  
M. Troy ◽  
T. Hayward ◽  
B. Brandl
Keyword(s):  
Adaptive Optics ◽  
Focal Plane ◽  
Near Infrared ◽  
Dynamic Range ◽  
Infrared Camera ◽  
Nearby Star ◽  
Point Spread ◽  
Spread Function ◽  
Adaptive Optics System ◽  
Circular Disks

We present a study of the Palomar Adaptive Optics System and the PHARO near infrared camera in coronagraphic mode. The camera provides two different focal plane occulting masks–opaque circular disks 0.43 and 0.97″ across. Three different pupil plane apodizing masks (Lyot masks) are also provided. The six different combinations of Lyot mask and focal plane mask suppress differently the point spread function of a bright star centered on the focal plane mask. We obtained images of the bright nearby star Gliese 614 with all six different configurations in the K filter. We measured the dynamic range achievable with these configurations. Within 2.5″, the dynamic range is at least 8 magnitudes at the 5σ level and as high as 12 in a 1 s exposure. This represents a substantial gain over similar techniques without adaptive optics.

scholarly journals Morphology of z ~ 1 galaxies from deep K-band AO imaging

2006 ◽  
Vol 2 (S235) ◽  
pp. 405-405
Author(s):  
Marc Huertas-Company ◽  
Daniel Rouan ◽  
Geneviève Soucail ◽  
Olivier Le Fèvre ◽  
Lidia Tasca
Keyword(s):  
Adaptive Optics ◽  
Spatial Resolution ◽  
Near Infrared ◽  
High Spatial Resolution ◽  
Integration Time ◽  
Early Type ◽  
Distant Galaxies ◽  
First Time ◽  
Concentration Asymmetry ◽  
Adaptive Optics System

AbstractWe present the results of observations of distant galaxies (z ~ 0.8) at high spatial resolution (~0.1"). We observed 7 fields of 1' × 1' with the NACO Adaptive Optics system (VLT) in Ks (2.2μm) band with typical V ~ 14 guide stars and 3h integration time per field. Observed fields are selected within the COSMOS survey area. We analyze the morphologies by means of B/D (Bulge/Disk) decomposition with GIM2D and CAS (Concentration-Asymmetry) estimators for 79 galaxies with magnitudes between Ks = 17 − 23 and classify them in three main morphological types (Late Type, Early Type and Irregulars). We obtain for the first time an estimate of the distribution of galaxy types at redshift z ~ 1 as measured from the near infrared at high spatial resolution.

Testing the pyramid wavefront sensor without modulation used in the closed-loop adaptive optics system

2012 ◽  
Author(s):  
Shengqian Wang ◽  
Changhui Rao ◽  
Ang Zhang ◽  
Xuejun Zhang ◽  
Kai Wei ◽  
...  
Keyword(s):  
Adaptive Optics ◽  
Closed Loop ◽  
Wavefront Sensor ◽  
Adaptive Optics System

Near-Infrared Observations of Neptune’s Tropospheric Cloud Layer with the Lick Observatory Adaptive Optics System

2001 ◽  
Vol 122 (3) ◽  
pp. 1636-1643 ◽  
Author(s):  
Henry G. Roe ◽  
Donald Gavel ◽  
Claire Max ◽  
Imke de Pater ◽  
Seran Gibbard ◽  
...  
Keyword(s):  
Adaptive Optics ◽  
Near Infrared ◽  
Cloud Layer ◽  
Infrared Observations ◽  
Adaptive Optics System

No wavefront sensor adaptive optics system for compensation of primary aberrations by software analysis of a point source image 1 Methods

2007 ◽  
Vol 46 (25) ◽  
pp. 6434 ◽  
Author(s):  
Enrico Grisan ◽  
Fabio Frassetto ◽  
Vania Da Deppo ◽  
Giampiero Naletto ◽  
Alfredo Ruggeri
Keyword(s):  
Point Source ◽  
Adaptive Optics ◽  
Wavefront Sensor ◽  
Source Image ◽  
Software Analysis ◽  
Adaptive Optics System
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