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PILOT: Pathfinder for an International Large Optical Telescope -performance specifications. Jon Lawrence. JACARA Science Meeting PILOT Friday March 26 Anglo Australian Observatory. DOME C. The data. South Pole. Turbulence: SODAR (winter 2000/1) DIMM (winter 2000/01)

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pilot pathfinder for an international large optical telescope performance specifications

PILOT:Pathfinder for an International Large OpticalTelescope-performance specifications

Jon Lawrence

      • JACARA Science Meeting
        • PILOT
  • Friday March 26
  • Anglo Australian Observatory
the data

DOME C

The data

South Pole

  • Turbulence:
    • SODAR (winter 2000/1)
    • DIMM (winter 2000/01)
    • microthermals (winter 1996)
  • Sky temperature and opacity
    • SUMMIT (winter 2003/4)
    • MIR FTI (summer 2002/3)
    • MISM (winter 1998)
    • NISM (winter 2000)
  • Met data
    • AWS
    • met balloons
  • Turbulence:
    • SODAR (winter 2003/4)
    • MASS (winter 2004)
    • DIMM (summer 2003/04)
  • Sky temperature and opacity
    • SUMMIT (winter 2003/4)
    • MIR FTI (summer 2003/4)
  • Met data
    • COBBER (winter 2003/4)
    • ICECAM (summer 2003/4)
    • AWS (winter 2004)
    • met balloons (summer 2000-04)
seeing data dome c 2002 3
Seeing Data Dome C - 2002/3

DIMM summer 2002: median seeing 1.2 arcsec (Aristidi et al, 2003)

SODAR summer/ winter 2003:

median seeing ~0.08 arcsec

(33 % floor 0.05)

seeing data dome c 2003 4
Seeing Data Dome C - 2003/4
  • DIMM summer 2003/4:
  • data not yet reduced
  • median seeing < 1.1 arcsec (~0.4-0.7 arcsec)
  • isoplanatic angle ~ 10 arcsec
c n 2 profile dome c bad
CN2 profile Dome C Bad

iso= 9.5 arcsec fG = 30 Hz

iso= 13.5 arcsec fG = 7 Hz

r0= 0.05 m (1.8 arcsec seeing)

r0= 0.2 m (0.5 arcsec seeing)

c n 2 profile dome c good
CN2 profile Dome C Good

iso= 9.5 arcsec fG = 30 Hz

iso= 13.5 arcsec fG = 7 Hz

iso= 30 arcsec fG = 2Hz

r0= 0.05 m (1.8 arcsec seeing)

r0= 0.2 m (0.5 arcsec seeing)

r0= 0.7 m (0.15 arcsec seeing)

c n 2 profile mauna kea
CN2 profile Mauna Kea

iso= 9.5 arcsec fG = 30 Hz

iso= 13.5 arcsec fG = 7 Hz

iso= 30 arcsec fG = 2Hz

iso= 2 arcsec fG = 50 Hz

r0= 0.05 m (1.8 arcsec seeing)

r0= 0.2 m (0.50 arcsec seeing)

r0= 0.7 m (0.15 arcsec seeing)

r0= 0.20 m (0.50 arcsec seeing)

atmospheric parameters
Atmospheric parameters

seeing (arcsec) isoplanatic angle Greenwood (arcsec) Frequency (Hz)

Mauna Kea 0.50 2-3 50

Dome C 0.15 - 0.50 10-30 2-10

atmospheric parameters1
Atmospheric parameters

seeing (arcsec) isoplanatic angle Greenwood (arcsec) Frequency (Hz)

Mauna Kea 0.50 2-3 50

Dome C 0.15 - 0.50 10-30 2-10

?

?

slide10

Adaptive Optics

object

guide star

to tip-tilt secondary

tip-tilt control

telescope optics

centroid sensor

dichroic

beam splitters

deformable mirror

image camera

wavefront control

wavefront sensor

wavefront analysis

pilot ao systems
PILOT AO systems
  • Tip-tilt
    • tip-tilt mirror + quad sensor
  • Low Order AO
    • ds=0.3 (30-50 actuators)
  • High Order AO
    • ds=0.08 (500-1000 actuators)
pilot ao system performance
PILOT AO system performance
  • Low Greenwood frequency:
    • lower feedback loop frequency
    • higher integration time
    • fainter stars

lower SNR/bandwidth errors

  • Large isoplanatic angle
    • larger fields
    • brighter stars

low anisoplanatic error

  • Better seeing (lower r0)
    • less actuators

lower fitting error

strehl ratio v band
Strehl ratio - V band

On-axis low order

DCG

DCB

MK

slide16

Uncomp DCB

Uncomp DCG

Diff lim 2m

slide17

Uncomp DCB

Uncomp DCG

DCB off-axis

DCG off-axis

on-axis

Diff lim 2m

slide18

Uncomp DCB

Uncomp MK

Uncomp DCG

DCB off-axis

DCG off-axis

Gemini altair

Diff lim 8 m

on-axis

Diff lim 2m

sky emission
Sky emission

MK

Emission = 5% @ 0° C

sky emission1
Sky emission

SP

Emission = 5% @ -63° C

sky emission2
Sky emission

DC

Emission = 5% @ -66° C

slide29

Possible PILOT Instruments

Visible (AO-on) imaging:

 4k array (0.03 arcsec/pixel) = 2.3 arcmin FOV

NIR wide field imaging JHK bands:

 4k array (0.6 arcsec/pixel) = 10 arcmin FOV

DF imaging KLM bands:

 1k array (0.23 arcsec/pixel) = 4 arcmin FOV

MIR imaging N band:

 0.5k array (0.7 arcsec/pixel) = 6 arcmin FOV

v band imaging ao on
V band imaging - AO on

Point source

ext object

slide31

Point source

K band imaging - tip tilt

ext object

slide32

Point source

N band imaging

ext object

summary
Summary
  • Visible AO system (40-100 actuators plus tip-tilt):
    • near diff lim for on-axis stars 8-12 mag
    • off-axis reasonable performance up to 1-2 arcmin
    • highest ground based resolution!!
    • mirror figure error is very important < 50 nm rms required
    • spectroscopy?
  • Near Infrared K band imaging:
    • tip-tilt correction is enough for near diff lim (0.2-0.3 arcsec)
    • equivalent to 8m ML telescope for extended object, 5m for point source
    • wide field or narrow field science?
  • Mid-Infrared imaging:
    • niche is wide field sensitivity