LBT meeting, 15 Novembre 2005, Oss. Arcetri, INAF
First Light AO
system for LBT
Simone Esposito
Osservatorio Astrofisico di Arceri, INAF
LBT meeting, 15 Novembre 2005, Oss. Arcetri, INAF
The focal station f/15 “Front Bent Gregorian”
Adaptive secondary
AGW unit
LUCIFER:
NIR imager & spectrograph
using a 2048x2048 pixel
IR array HAWAII-2
AGW unit
LBT meeting, 15 Novembre 2005, Oss. Arcetri, INAF
AO system network
AO TCS GUI
AO supervisor GUI
Look up
tables
Operating
modes
Scripts
Low level
functions
LBT672 Param/Diag
Real time link
AO loop Param/Diag
LBT672
AGW unit
LBT meeting, 15 Novembre 2005, Oss. Arcetri, INAF
The two key elements of the LBT AO
The adaptive secondary.....
•911 mm convex secondary
Easy
optical
coupling
with the AO system.
•1.7mm
adaptive
shell thickness
Total
optical efficiency AO system is 0.5
•672 actuators
•Stroke 30/40
LowQE).
order, 1 high order
(including
CCD
•Response time 0.5ms
•Mirror fitting error 30-60nm
The pyramid sensor.....
•Small size unit 300x400mm
•2 channels: Sensing and Acq.
Pyramid sensor
has better performance
•Ref. Star FoV 3.2x2.2 arcmin
for both bright
faint30x30,15x15,..5x5
star with respect to
•Pupil and
sampling
Shack-Hartmann
sensor.
•Reference
star acquired translating
the WFS board: 0.6mm/arcsec
LBT meeting, 15 Novembre 2005, Oss. Arcetri, INAF
Large Binocular Telescope
First Light planned
for late September 2004
Second Light planned for
the end of 2005
LBT meeting, 15 Novembre 2005, Oss. Arcetri, INAF
LBT meeting, 15 Novembre 2005, Oss. Arcetri, INAF
LBT meeting, 15 Novembre 2005, Oss. Arcetri, INAF