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26
An Introduction to Adaptive Optics BY , RAHUL KRISHNAN S7 EEE
Transcript

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 126

An Introduction to AdaptiveOptics

BY

RAHUL KRISHNAN

S7 EEE

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 226

Why do we need adaptive optics

To Correct for Irregularities in theTransmission Media ndash Atmospheric (Astronomical)

Scintillation or Twinkling (Eddies ~ radicλL)

Beam Wander or Quiver (Eddies gt Beam Size)

Spreading (Eddies lt Beam Size)

ndash Atmospheric (LASER Transmission) Thermal Blooming

ndash Ocular (Retinal Imaging) Defects in the Lens and Cornea

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 326

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 426

Astronomical AO ExampleNeptune

415

Without adaptive optics With adaptive optics

2

3

a r c

s e c

Credit Keck Observatory LLNL UCB

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 526

Essentials of anAO system

Wavefront sensor

Computer

Phase modulator

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 626

How Turbulence Effects Light

Spherical wavesemitted by thesource (star) areessentially planewaves when theyarrive at the Earthrsquosatmosphere Thewaves are thenrandomly distorted

by turbulence in the

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 726

How does it work

Two Basic Functions

ndash Wavefront sensing

Shack-Hartmann wavefront sensor

Shearing interferometer

ndash Wavefront correction

Tip-tilt optical element

Deformable optical element

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 826

Wavefront Sensing

Shack-HartmannSensor

ndash Has become the

standard type of sensor ndash Uses an array of

spherical ldquolenseletsrdquo

ndash Focuses wavefronts

onto a CCD array ndash (b) is a plane wave

ndash (c) is a distorted wave

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 926

Wavefront Sensing

ShearingInterferometer

ndash Distorted wavefronts

result in phase shiftedoutput signals betweenthe detector arrays

ndash Two interferometers are

required for correctionin the x-y plane

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1026

Wavefront Correction

High speed tip-tiltmirror reduces overallwavefront tilt

Deformable mirror(monolithic orsegmented) correctswavefront shape

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1126

Wavefront Correction Monolithic Deformable Mirror

ndash Reflective face cast on a solid piezoelectric backing (14um)

ndash Thin face supported by an array of electro-mechanical actuators (+- 30um) ndash Thin face supported by an array of piezoelectric actuators (50um)

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1226

Wavefront Correction

Segmented Mirrors

ndash Capable of largercorrections than

monolithic types ndash Requires frequent

calibration

ndash Diffraction due to gaps

between segments

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1326

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1426

Some Definitions

Apparent or VisualMagnitude ndash The relativebrightness of a star asseen by an observer on

Earth Guide Star ndash A sufficiently

bright star to use as areference for imagecompensation The

required magnitude variesas a function of the desiredobservation wavelength

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1526

Limitations of Image Compensation

Compensation in visible wavelengths (05um)requires a guide star of magnitude 10 or brighter

Compensation in infrared wavelengths (22um)

allows guide stars down to magnitude 14

Small isoplanatic region around the guide starlimits total observation area

ndash Visual ndash 1100000 of the sky ndash IR ndash 11000 of the sky

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1626

Guide Stars

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1726

Artificial Guide Stars

The area of sky coverage can beexpanded using artificial guide stars

Created using a LASER aligned withthe telescope optics

Rayleigh beacons take advantage ofRayleigh scattering in theatmosphere ndash Useful for telescopes with apertures lt 2m

ndash Creates a 1 to 2 arc second guide star 5 to

10km in altitude ndash 100W LASER

ndash LASER is pulsed so that backscatter can beeliminated by range gating

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1826

Artificial Guide Stars

Sodium Beaconsexploit a layer ofsodium vapor in the

upper atmosphere ndash 10W LASER at 589nm

ndash Excites sodium atoms90 to 92 km in altitude

Photo - The Sodium laser launching

from the side of the LickObservatory 120 ShaneTelescope This is a 10 minute timeexposure - note the star trails

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1926

Artificial Guide Stars

Natural guide starrequired for tiltcorrection

Limiting magnitude forguide star is about 20

Result is nearly 100

sky coverage

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2026

IR Stellar imaging from Lick

Observatory

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2126

Upper Left Io imagetaken with Keckadaptive optics K-band 22 micron

Upper Right Io imagebased on visible lighttaken with Galileospacecraft orbiter

Lower Left Io imagetaken with Keckadaptive optics L-band35micron

Lower Right Io imagetaken without Keckadaptive optics

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2226

The Lick Observatory CIS

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2326

Non-Astronomical Applications

Most of the current AOtechnology wasdeveloped by DARPA

during the Cold War toimage and shoot downsatellites with LASERweapons

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2426

Retinal Imaging

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2526

References

Carroll Joseph Daniel C Gray Austin Roorda David R Williams ldquoRecent Advances inRetinal Imaging with Adaptive Opticsrdquo Optics and Photonics News Jan 2005 p 36-42

Chaisson Eric and Steve McMillan Astronomy Today 4th Edition Prentice Hall UpperSaddle River NJ 2002

Florence Ronald The Perfect Machine Harper Collins New York NY 1994

Hardy John W Adaptive Optics for Astronomical Telescopes Oxford University PressNew York NY 1998

Hardy John W ldquoAdaptive Opticsrdquo Scientific American June 1994 p 60-65

Hecht Eugene Optics 4th Edition Addison-Wesley Reading MA 2002

Tyson Robert K Principles of Adaptive Optics 2nd Edition Academic Press San DiegoCA 1998

AdaptiveOpticscom 2002 Adaptive Optics Associates Inc httpwwwaoainccom Center for Adaptive Optics 2005 University of California Santa Cruz

httpcfaoucolickorg

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2626

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 226

Why do we need adaptive optics

To Correct for Irregularities in theTransmission Media ndash Atmospheric (Astronomical)

Scintillation or Twinkling (Eddies ~ radicλL)

Beam Wander or Quiver (Eddies gt Beam Size)

Spreading (Eddies lt Beam Size)

ndash Atmospheric (LASER Transmission) Thermal Blooming

ndash Ocular (Retinal Imaging) Defects in the Lens and Cornea

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 326

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 426

Astronomical AO ExampleNeptune

415

Without adaptive optics With adaptive optics

2

3

a r c

s e c

Credit Keck Observatory LLNL UCB

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 526

Essentials of anAO system

Wavefront sensor

Computer

Phase modulator

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 626

How Turbulence Effects Light

Spherical wavesemitted by thesource (star) areessentially planewaves when theyarrive at the Earthrsquosatmosphere Thewaves are thenrandomly distorted

by turbulence in the

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 726

How does it work

Two Basic Functions

ndash Wavefront sensing

Shack-Hartmann wavefront sensor

Shearing interferometer

ndash Wavefront correction

Tip-tilt optical element

Deformable optical element

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 826

Wavefront Sensing

Shack-HartmannSensor

ndash Has become the

standard type of sensor ndash Uses an array of

spherical ldquolenseletsrdquo

ndash Focuses wavefronts

onto a CCD array ndash (b) is a plane wave

ndash (c) is a distorted wave

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 926

Wavefront Sensing

ShearingInterferometer

ndash Distorted wavefronts

result in phase shiftedoutput signals betweenthe detector arrays

ndash Two interferometers are

required for correctionin the x-y plane

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1026

Wavefront Correction

High speed tip-tiltmirror reduces overallwavefront tilt

Deformable mirror(monolithic orsegmented) correctswavefront shape

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1126

Wavefront Correction Monolithic Deformable Mirror

ndash Reflective face cast on a solid piezoelectric backing (14um)

ndash Thin face supported by an array of electro-mechanical actuators (+- 30um) ndash Thin face supported by an array of piezoelectric actuators (50um)

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1226

Wavefront Correction

Segmented Mirrors

ndash Capable of largercorrections than

monolithic types ndash Requires frequent

calibration

ndash Diffraction due to gaps

between segments

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1326

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1426

Some Definitions

Apparent or VisualMagnitude ndash The relativebrightness of a star asseen by an observer on

Earth Guide Star ndash A sufficiently

bright star to use as areference for imagecompensation The

required magnitude variesas a function of the desiredobservation wavelength

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1526

Limitations of Image Compensation

Compensation in visible wavelengths (05um)requires a guide star of magnitude 10 or brighter

Compensation in infrared wavelengths (22um)

allows guide stars down to magnitude 14

Small isoplanatic region around the guide starlimits total observation area

ndash Visual ndash 1100000 of the sky ndash IR ndash 11000 of the sky

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1626

Guide Stars

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1726

Artificial Guide Stars

The area of sky coverage can beexpanded using artificial guide stars

Created using a LASER aligned withthe telescope optics

Rayleigh beacons take advantage ofRayleigh scattering in theatmosphere ndash Useful for telescopes with apertures lt 2m

ndash Creates a 1 to 2 arc second guide star 5 to

10km in altitude ndash 100W LASER

ndash LASER is pulsed so that backscatter can beeliminated by range gating

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1826

Artificial Guide Stars

Sodium Beaconsexploit a layer ofsodium vapor in the

upper atmosphere ndash 10W LASER at 589nm

ndash Excites sodium atoms90 to 92 km in altitude

Photo - The Sodium laser launching

from the side of the LickObservatory 120 ShaneTelescope This is a 10 minute timeexposure - note the star trails

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1926

Artificial Guide Stars

Natural guide starrequired for tiltcorrection

Limiting magnitude forguide star is about 20

Result is nearly 100

sky coverage

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2026

IR Stellar imaging from Lick

Observatory

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2126

Upper Left Io imagetaken with Keckadaptive optics K-band 22 micron

Upper Right Io imagebased on visible lighttaken with Galileospacecraft orbiter

Lower Left Io imagetaken with Keckadaptive optics L-band35micron

Lower Right Io imagetaken without Keckadaptive optics

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2226

The Lick Observatory CIS

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2326

Non-Astronomical Applications

Most of the current AOtechnology wasdeveloped by DARPA

during the Cold War toimage and shoot downsatellites with LASERweapons

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2426

Retinal Imaging

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2526

References

Carroll Joseph Daniel C Gray Austin Roorda David R Williams ldquoRecent Advances inRetinal Imaging with Adaptive Opticsrdquo Optics and Photonics News Jan 2005 p 36-42

Chaisson Eric and Steve McMillan Astronomy Today 4th Edition Prentice Hall UpperSaddle River NJ 2002

Florence Ronald The Perfect Machine Harper Collins New York NY 1994

Hardy John W Adaptive Optics for Astronomical Telescopes Oxford University PressNew York NY 1998

Hardy John W ldquoAdaptive Opticsrdquo Scientific American June 1994 p 60-65

Hecht Eugene Optics 4th Edition Addison-Wesley Reading MA 2002

Tyson Robert K Principles of Adaptive Optics 2nd Edition Academic Press San DiegoCA 1998

AdaptiveOpticscom 2002 Adaptive Optics Associates Inc httpwwwaoainccom Center for Adaptive Optics 2005 University of California Santa Cruz

httpcfaoucolickorg

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2626

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 326

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 426

Astronomical AO ExampleNeptune

415

Without adaptive optics With adaptive optics

2

3

a r c

s e c

Credit Keck Observatory LLNL UCB

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 526

Essentials of anAO system

Wavefront sensor

Computer

Phase modulator

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 626

How Turbulence Effects Light

Spherical wavesemitted by thesource (star) areessentially planewaves when theyarrive at the Earthrsquosatmosphere Thewaves are thenrandomly distorted

by turbulence in the

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 726

How does it work

Two Basic Functions

ndash Wavefront sensing

Shack-Hartmann wavefront sensor

Shearing interferometer

ndash Wavefront correction

Tip-tilt optical element

Deformable optical element

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 826

Wavefront Sensing

Shack-HartmannSensor

ndash Has become the

standard type of sensor ndash Uses an array of

spherical ldquolenseletsrdquo

ndash Focuses wavefronts

onto a CCD array ndash (b) is a plane wave

ndash (c) is a distorted wave

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 926

Wavefront Sensing

ShearingInterferometer

ndash Distorted wavefronts

result in phase shiftedoutput signals betweenthe detector arrays

ndash Two interferometers are

required for correctionin the x-y plane

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1026

Wavefront Correction

High speed tip-tiltmirror reduces overallwavefront tilt

Deformable mirror(monolithic orsegmented) correctswavefront shape

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1126

Wavefront Correction Monolithic Deformable Mirror

ndash Reflective face cast on a solid piezoelectric backing (14um)

ndash Thin face supported by an array of electro-mechanical actuators (+- 30um) ndash Thin face supported by an array of piezoelectric actuators (50um)

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1226

Wavefront Correction

Segmented Mirrors

ndash Capable of largercorrections than

monolithic types ndash Requires frequent

calibration

ndash Diffraction due to gaps

between segments

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1326

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1426

Some Definitions

Apparent or VisualMagnitude ndash The relativebrightness of a star asseen by an observer on

Earth Guide Star ndash A sufficiently

bright star to use as areference for imagecompensation The

required magnitude variesas a function of the desiredobservation wavelength

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1526

Limitations of Image Compensation

Compensation in visible wavelengths (05um)requires a guide star of magnitude 10 or brighter

Compensation in infrared wavelengths (22um)

allows guide stars down to magnitude 14

Small isoplanatic region around the guide starlimits total observation area

ndash Visual ndash 1100000 of the sky ndash IR ndash 11000 of the sky

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1626

Guide Stars

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1726

Artificial Guide Stars

The area of sky coverage can beexpanded using artificial guide stars

Created using a LASER aligned withthe telescope optics

Rayleigh beacons take advantage ofRayleigh scattering in theatmosphere ndash Useful for telescopes with apertures lt 2m

ndash Creates a 1 to 2 arc second guide star 5 to

10km in altitude ndash 100W LASER

ndash LASER is pulsed so that backscatter can beeliminated by range gating

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1826

Artificial Guide Stars

Sodium Beaconsexploit a layer ofsodium vapor in the

upper atmosphere ndash 10W LASER at 589nm

ndash Excites sodium atoms90 to 92 km in altitude

Photo - The Sodium laser launching

from the side of the LickObservatory 120 ShaneTelescope This is a 10 minute timeexposure - note the star trails

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1926

Artificial Guide Stars

Natural guide starrequired for tiltcorrection

Limiting magnitude forguide star is about 20

Result is nearly 100

sky coverage

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2026

IR Stellar imaging from Lick

Observatory

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2126

Upper Left Io imagetaken with Keckadaptive optics K-band 22 micron

Upper Right Io imagebased on visible lighttaken with Galileospacecraft orbiter

Lower Left Io imagetaken with Keckadaptive optics L-band35micron

Lower Right Io imagetaken without Keckadaptive optics

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2226

The Lick Observatory CIS

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2326

Non-Astronomical Applications

Most of the current AOtechnology wasdeveloped by DARPA

during the Cold War toimage and shoot downsatellites with LASERweapons

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2426

Retinal Imaging

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2526

References

Carroll Joseph Daniel C Gray Austin Roorda David R Williams ldquoRecent Advances inRetinal Imaging with Adaptive Opticsrdquo Optics and Photonics News Jan 2005 p 36-42

Chaisson Eric and Steve McMillan Astronomy Today 4th Edition Prentice Hall UpperSaddle River NJ 2002

Florence Ronald The Perfect Machine Harper Collins New York NY 1994

Hardy John W Adaptive Optics for Astronomical Telescopes Oxford University PressNew York NY 1998

Hardy John W ldquoAdaptive Opticsrdquo Scientific American June 1994 p 60-65

Hecht Eugene Optics 4th Edition Addison-Wesley Reading MA 2002

Tyson Robert K Principles of Adaptive Optics 2nd Edition Academic Press San DiegoCA 1998

AdaptiveOpticscom 2002 Adaptive Optics Associates Inc httpwwwaoainccom Center for Adaptive Optics 2005 University of California Santa Cruz

httpcfaoucolickorg

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2626

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 426

Astronomical AO ExampleNeptune

415

Without adaptive optics With adaptive optics

2

3

a r c

s e c

Credit Keck Observatory LLNL UCB

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 526

Essentials of anAO system

Wavefront sensor

Computer

Phase modulator

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 626

How Turbulence Effects Light

Spherical wavesemitted by thesource (star) areessentially planewaves when theyarrive at the Earthrsquosatmosphere Thewaves are thenrandomly distorted

by turbulence in the

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 726

How does it work

Two Basic Functions

ndash Wavefront sensing

Shack-Hartmann wavefront sensor

Shearing interferometer

ndash Wavefront correction

Tip-tilt optical element

Deformable optical element

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 826

Wavefront Sensing

Shack-HartmannSensor

ndash Has become the

standard type of sensor ndash Uses an array of

spherical ldquolenseletsrdquo

ndash Focuses wavefronts

onto a CCD array ndash (b) is a plane wave

ndash (c) is a distorted wave

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 926

Wavefront Sensing

ShearingInterferometer

ndash Distorted wavefronts

result in phase shiftedoutput signals betweenthe detector arrays

ndash Two interferometers are

required for correctionin the x-y plane

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1026

Wavefront Correction

High speed tip-tiltmirror reduces overallwavefront tilt

Deformable mirror(monolithic orsegmented) correctswavefront shape

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1126

Wavefront Correction Monolithic Deformable Mirror

ndash Reflective face cast on a solid piezoelectric backing (14um)

ndash Thin face supported by an array of electro-mechanical actuators (+- 30um) ndash Thin face supported by an array of piezoelectric actuators (50um)

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1226

Wavefront Correction

Segmented Mirrors

ndash Capable of largercorrections than

monolithic types ndash Requires frequent

calibration

ndash Diffraction due to gaps

between segments

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1326

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1426

Some Definitions

Apparent or VisualMagnitude ndash The relativebrightness of a star asseen by an observer on

Earth Guide Star ndash A sufficiently

bright star to use as areference for imagecompensation The

required magnitude variesas a function of the desiredobservation wavelength

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1526

Limitations of Image Compensation

Compensation in visible wavelengths (05um)requires a guide star of magnitude 10 or brighter

Compensation in infrared wavelengths (22um)

allows guide stars down to magnitude 14

Small isoplanatic region around the guide starlimits total observation area

ndash Visual ndash 1100000 of the sky ndash IR ndash 11000 of the sky

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1626

Guide Stars

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1726

Artificial Guide Stars

The area of sky coverage can beexpanded using artificial guide stars

Created using a LASER aligned withthe telescope optics

Rayleigh beacons take advantage ofRayleigh scattering in theatmosphere ndash Useful for telescopes with apertures lt 2m

ndash Creates a 1 to 2 arc second guide star 5 to

10km in altitude ndash 100W LASER

ndash LASER is pulsed so that backscatter can beeliminated by range gating

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1826

Artificial Guide Stars

Sodium Beaconsexploit a layer ofsodium vapor in the

upper atmosphere ndash 10W LASER at 589nm

ndash Excites sodium atoms90 to 92 km in altitude

Photo - The Sodium laser launching

from the side of the LickObservatory 120 ShaneTelescope This is a 10 minute timeexposure - note the star trails

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1926

Artificial Guide Stars

Natural guide starrequired for tiltcorrection

Limiting magnitude forguide star is about 20

Result is nearly 100

sky coverage

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2026

IR Stellar imaging from Lick

Observatory

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2126

Upper Left Io imagetaken with Keckadaptive optics K-band 22 micron

Upper Right Io imagebased on visible lighttaken with Galileospacecraft orbiter

Lower Left Io imagetaken with Keckadaptive optics L-band35micron

Lower Right Io imagetaken without Keckadaptive optics

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2226

The Lick Observatory CIS

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2326

Non-Astronomical Applications

Most of the current AOtechnology wasdeveloped by DARPA

during the Cold War toimage and shoot downsatellites with LASERweapons

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2426

Retinal Imaging

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2526

References

Carroll Joseph Daniel C Gray Austin Roorda David R Williams ldquoRecent Advances inRetinal Imaging with Adaptive Opticsrdquo Optics and Photonics News Jan 2005 p 36-42

Chaisson Eric and Steve McMillan Astronomy Today 4th Edition Prentice Hall UpperSaddle River NJ 2002

Florence Ronald The Perfect Machine Harper Collins New York NY 1994

Hardy John W Adaptive Optics for Astronomical Telescopes Oxford University PressNew York NY 1998

Hardy John W ldquoAdaptive Opticsrdquo Scientific American June 1994 p 60-65

Hecht Eugene Optics 4th Edition Addison-Wesley Reading MA 2002

Tyson Robert K Principles of Adaptive Optics 2nd Edition Academic Press San DiegoCA 1998

AdaptiveOpticscom 2002 Adaptive Optics Associates Inc httpwwwaoainccom Center for Adaptive Optics 2005 University of California Santa Cruz

httpcfaoucolickorg

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2626

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 526

Essentials of anAO system

Wavefront sensor

Computer

Phase modulator

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 626

How Turbulence Effects Light

Spherical wavesemitted by thesource (star) areessentially planewaves when theyarrive at the Earthrsquosatmosphere Thewaves are thenrandomly distorted

by turbulence in the

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 726

How does it work

Two Basic Functions

ndash Wavefront sensing

Shack-Hartmann wavefront sensor

Shearing interferometer

ndash Wavefront correction

Tip-tilt optical element

Deformable optical element

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 826

Wavefront Sensing

Shack-HartmannSensor

ndash Has become the

standard type of sensor ndash Uses an array of

spherical ldquolenseletsrdquo

ndash Focuses wavefronts

onto a CCD array ndash (b) is a plane wave

ndash (c) is a distorted wave

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 926

Wavefront Sensing

ShearingInterferometer

ndash Distorted wavefronts

result in phase shiftedoutput signals betweenthe detector arrays

ndash Two interferometers are

required for correctionin the x-y plane

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1026

Wavefront Correction

High speed tip-tiltmirror reduces overallwavefront tilt

Deformable mirror(monolithic orsegmented) correctswavefront shape

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1126

Wavefront Correction Monolithic Deformable Mirror

ndash Reflective face cast on a solid piezoelectric backing (14um)

ndash Thin face supported by an array of electro-mechanical actuators (+- 30um) ndash Thin face supported by an array of piezoelectric actuators (50um)

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1226

Wavefront Correction

Segmented Mirrors

ndash Capable of largercorrections than

monolithic types ndash Requires frequent

calibration

ndash Diffraction due to gaps

between segments

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1326

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1426

Some Definitions

Apparent or VisualMagnitude ndash The relativebrightness of a star asseen by an observer on

Earth Guide Star ndash A sufficiently

bright star to use as areference for imagecompensation The

required magnitude variesas a function of the desiredobservation wavelength

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1526

Limitations of Image Compensation

Compensation in visible wavelengths (05um)requires a guide star of magnitude 10 or brighter

Compensation in infrared wavelengths (22um)

allows guide stars down to magnitude 14

Small isoplanatic region around the guide starlimits total observation area

ndash Visual ndash 1100000 of the sky ndash IR ndash 11000 of the sky

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1626

Guide Stars

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1726

Artificial Guide Stars

The area of sky coverage can beexpanded using artificial guide stars

Created using a LASER aligned withthe telescope optics

Rayleigh beacons take advantage ofRayleigh scattering in theatmosphere ndash Useful for telescopes with apertures lt 2m

ndash Creates a 1 to 2 arc second guide star 5 to

10km in altitude ndash 100W LASER

ndash LASER is pulsed so that backscatter can beeliminated by range gating

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1826

Artificial Guide Stars

Sodium Beaconsexploit a layer ofsodium vapor in the

upper atmosphere ndash 10W LASER at 589nm

ndash Excites sodium atoms90 to 92 km in altitude

Photo - The Sodium laser launching

from the side of the LickObservatory 120 ShaneTelescope This is a 10 minute timeexposure - note the star trails

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1926

Artificial Guide Stars

Natural guide starrequired for tiltcorrection

Limiting magnitude forguide star is about 20

Result is nearly 100

sky coverage

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2026

IR Stellar imaging from Lick

Observatory

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2126

Upper Left Io imagetaken with Keckadaptive optics K-band 22 micron

Upper Right Io imagebased on visible lighttaken with Galileospacecraft orbiter

Lower Left Io imagetaken with Keckadaptive optics L-band35micron

Lower Right Io imagetaken without Keckadaptive optics

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2226

The Lick Observatory CIS

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2326

Non-Astronomical Applications

Most of the current AOtechnology wasdeveloped by DARPA

during the Cold War toimage and shoot downsatellites with LASERweapons

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2426

Retinal Imaging

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2526

References

Carroll Joseph Daniel C Gray Austin Roorda David R Williams ldquoRecent Advances inRetinal Imaging with Adaptive Opticsrdquo Optics and Photonics News Jan 2005 p 36-42

Chaisson Eric and Steve McMillan Astronomy Today 4th Edition Prentice Hall UpperSaddle River NJ 2002

Florence Ronald The Perfect Machine Harper Collins New York NY 1994

Hardy John W Adaptive Optics for Astronomical Telescopes Oxford University PressNew York NY 1998

Hardy John W ldquoAdaptive Opticsrdquo Scientific American June 1994 p 60-65

Hecht Eugene Optics 4th Edition Addison-Wesley Reading MA 2002

Tyson Robert K Principles of Adaptive Optics 2nd Edition Academic Press San DiegoCA 1998

AdaptiveOpticscom 2002 Adaptive Optics Associates Inc httpwwwaoainccom Center for Adaptive Optics 2005 University of California Santa Cruz

httpcfaoucolickorg

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2626

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 626

How Turbulence Effects Light

Spherical wavesemitted by thesource (star) areessentially planewaves when theyarrive at the Earthrsquosatmosphere Thewaves are thenrandomly distorted

by turbulence in the

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 726

How does it work

Two Basic Functions

ndash Wavefront sensing

Shack-Hartmann wavefront sensor

Shearing interferometer

ndash Wavefront correction

Tip-tilt optical element

Deformable optical element

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 826

Wavefront Sensing

Shack-HartmannSensor

ndash Has become the

standard type of sensor ndash Uses an array of

spherical ldquolenseletsrdquo

ndash Focuses wavefronts

onto a CCD array ndash (b) is a plane wave

ndash (c) is a distorted wave

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 926

Wavefront Sensing

ShearingInterferometer

ndash Distorted wavefronts

result in phase shiftedoutput signals betweenthe detector arrays

ndash Two interferometers are

required for correctionin the x-y plane

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1026

Wavefront Correction

High speed tip-tiltmirror reduces overallwavefront tilt

Deformable mirror(monolithic orsegmented) correctswavefront shape

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1126

Wavefront Correction Monolithic Deformable Mirror

ndash Reflective face cast on a solid piezoelectric backing (14um)

ndash Thin face supported by an array of electro-mechanical actuators (+- 30um) ndash Thin face supported by an array of piezoelectric actuators (50um)

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1226

Wavefront Correction

Segmented Mirrors

ndash Capable of largercorrections than

monolithic types ndash Requires frequent

calibration

ndash Diffraction due to gaps

between segments

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1326

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1426

Some Definitions

Apparent or VisualMagnitude ndash The relativebrightness of a star asseen by an observer on

Earth Guide Star ndash A sufficiently

bright star to use as areference for imagecompensation The

required magnitude variesas a function of the desiredobservation wavelength

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1526

Limitations of Image Compensation

Compensation in visible wavelengths (05um)requires a guide star of magnitude 10 or brighter

Compensation in infrared wavelengths (22um)

allows guide stars down to magnitude 14

Small isoplanatic region around the guide starlimits total observation area

ndash Visual ndash 1100000 of the sky ndash IR ndash 11000 of the sky

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1626

Guide Stars

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1726

Artificial Guide Stars

The area of sky coverage can beexpanded using artificial guide stars

Created using a LASER aligned withthe telescope optics

Rayleigh beacons take advantage ofRayleigh scattering in theatmosphere ndash Useful for telescopes with apertures lt 2m

ndash Creates a 1 to 2 arc second guide star 5 to

10km in altitude ndash 100W LASER

ndash LASER is pulsed so that backscatter can beeliminated by range gating

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1826

Artificial Guide Stars

Sodium Beaconsexploit a layer ofsodium vapor in the

upper atmosphere ndash 10W LASER at 589nm

ndash Excites sodium atoms90 to 92 km in altitude

Photo - The Sodium laser launching

from the side of the LickObservatory 120 ShaneTelescope This is a 10 minute timeexposure - note the star trails

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1926

Artificial Guide Stars

Natural guide starrequired for tiltcorrection

Limiting magnitude forguide star is about 20

Result is nearly 100

sky coverage

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2026

IR Stellar imaging from Lick

Observatory

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2126

Upper Left Io imagetaken with Keckadaptive optics K-band 22 micron

Upper Right Io imagebased on visible lighttaken with Galileospacecraft orbiter

Lower Left Io imagetaken with Keckadaptive optics L-band35micron

Lower Right Io imagetaken without Keckadaptive optics

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2226

The Lick Observatory CIS

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2326

Non-Astronomical Applications

Most of the current AOtechnology wasdeveloped by DARPA

during the Cold War toimage and shoot downsatellites with LASERweapons

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2426

Retinal Imaging

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2526

References

Carroll Joseph Daniel C Gray Austin Roorda David R Williams ldquoRecent Advances inRetinal Imaging with Adaptive Opticsrdquo Optics and Photonics News Jan 2005 p 36-42

Chaisson Eric and Steve McMillan Astronomy Today 4th Edition Prentice Hall UpperSaddle River NJ 2002

Florence Ronald The Perfect Machine Harper Collins New York NY 1994

Hardy John W Adaptive Optics for Astronomical Telescopes Oxford University PressNew York NY 1998

Hardy John W ldquoAdaptive Opticsrdquo Scientific American June 1994 p 60-65

Hecht Eugene Optics 4th Edition Addison-Wesley Reading MA 2002

Tyson Robert K Principles of Adaptive Optics 2nd Edition Academic Press San DiegoCA 1998

AdaptiveOpticscom 2002 Adaptive Optics Associates Inc httpwwwaoainccom Center for Adaptive Optics 2005 University of California Santa Cruz

httpcfaoucolickorg

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2626

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 726

How does it work

Two Basic Functions

ndash Wavefront sensing

Shack-Hartmann wavefront sensor

Shearing interferometer

ndash Wavefront correction

Tip-tilt optical element

Deformable optical element

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 826

Wavefront Sensing

Shack-HartmannSensor

ndash Has become the

standard type of sensor ndash Uses an array of

spherical ldquolenseletsrdquo

ndash Focuses wavefronts

onto a CCD array ndash (b) is a plane wave

ndash (c) is a distorted wave

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 926

Wavefront Sensing

ShearingInterferometer

ndash Distorted wavefronts

result in phase shiftedoutput signals betweenthe detector arrays

ndash Two interferometers are

required for correctionin the x-y plane

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1026

Wavefront Correction

High speed tip-tiltmirror reduces overallwavefront tilt

Deformable mirror(monolithic orsegmented) correctswavefront shape

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1126

Wavefront Correction Monolithic Deformable Mirror

ndash Reflective face cast on a solid piezoelectric backing (14um)

ndash Thin face supported by an array of electro-mechanical actuators (+- 30um) ndash Thin face supported by an array of piezoelectric actuators (50um)

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1226

Wavefront Correction

Segmented Mirrors

ndash Capable of largercorrections than

monolithic types ndash Requires frequent

calibration

ndash Diffraction due to gaps

between segments

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1326

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1426

Some Definitions

Apparent or VisualMagnitude ndash The relativebrightness of a star asseen by an observer on

Earth Guide Star ndash A sufficiently

bright star to use as areference for imagecompensation The

required magnitude variesas a function of the desiredobservation wavelength

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1526

Limitations of Image Compensation

Compensation in visible wavelengths (05um)requires a guide star of magnitude 10 or brighter

Compensation in infrared wavelengths (22um)

allows guide stars down to magnitude 14

Small isoplanatic region around the guide starlimits total observation area

ndash Visual ndash 1100000 of the sky ndash IR ndash 11000 of the sky

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1626

Guide Stars

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1726

Artificial Guide Stars

The area of sky coverage can beexpanded using artificial guide stars

Created using a LASER aligned withthe telescope optics

Rayleigh beacons take advantage ofRayleigh scattering in theatmosphere ndash Useful for telescopes with apertures lt 2m

ndash Creates a 1 to 2 arc second guide star 5 to

10km in altitude ndash 100W LASER

ndash LASER is pulsed so that backscatter can beeliminated by range gating

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1826

Artificial Guide Stars

Sodium Beaconsexploit a layer ofsodium vapor in the

upper atmosphere ndash 10W LASER at 589nm

ndash Excites sodium atoms90 to 92 km in altitude

Photo - The Sodium laser launching

from the side of the LickObservatory 120 ShaneTelescope This is a 10 minute timeexposure - note the star trails

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1926

Artificial Guide Stars

Natural guide starrequired for tiltcorrection

Limiting magnitude forguide star is about 20

Result is nearly 100

sky coverage

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2026

IR Stellar imaging from Lick

Observatory

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2126

Upper Left Io imagetaken with Keckadaptive optics K-band 22 micron

Upper Right Io imagebased on visible lighttaken with Galileospacecraft orbiter

Lower Left Io imagetaken with Keckadaptive optics L-band35micron

Lower Right Io imagetaken without Keckadaptive optics

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2226

The Lick Observatory CIS

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2326

Non-Astronomical Applications

Most of the current AOtechnology wasdeveloped by DARPA

during the Cold War toimage and shoot downsatellites with LASERweapons

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2426

Retinal Imaging

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2526

References

Carroll Joseph Daniel C Gray Austin Roorda David R Williams ldquoRecent Advances inRetinal Imaging with Adaptive Opticsrdquo Optics and Photonics News Jan 2005 p 36-42

Chaisson Eric and Steve McMillan Astronomy Today 4th Edition Prentice Hall UpperSaddle River NJ 2002

Florence Ronald The Perfect Machine Harper Collins New York NY 1994

Hardy John W Adaptive Optics for Astronomical Telescopes Oxford University PressNew York NY 1998

Hardy John W ldquoAdaptive Opticsrdquo Scientific American June 1994 p 60-65

Hecht Eugene Optics 4th Edition Addison-Wesley Reading MA 2002

Tyson Robert K Principles of Adaptive Optics 2nd Edition Academic Press San DiegoCA 1998

AdaptiveOpticscom 2002 Adaptive Optics Associates Inc httpwwwaoainccom Center for Adaptive Optics 2005 University of California Santa Cruz

httpcfaoucolickorg

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2626

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 826

Wavefront Sensing

Shack-HartmannSensor

ndash Has become the

standard type of sensor ndash Uses an array of

spherical ldquolenseletsrdquo

ndash Focuses wavefronts

onto a CCD array ndash (b) is a plane wave

ndash (c) is a distorted wave

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 926

Wavefront Sensing

ShearingInterferometer

ndash Distorted wavefronts

result in phase shiftedoutput signals betweenthe detector arrays

ndash Two interferometers are

required for correctionin the x-y plane

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1026

Wavefront Correction

High speed tip-tiltmirror reduces overallwavefront tilt

Deformable mirror(monolithic orsegmented) correctswavefront shape

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1126

Wavefront Correction Monolithic Deformable Mirror

ndash Reflective face cast on a solid piezoelectric backing (14um)

ndash Thin face supported by an array of electro-mechanical actuators (+- 30um) ndash Thin face supported by an array of piezoelectric actuators (50um)

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1226

Wavefront Correction

Segmented Mirrors

ndash Capable of largercorrections than

monolithic types ndash Requires frequent

calibration

ndash Diffraction due to gaps

between segments

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1326

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1426

Some Definitions

Apparent or VisualMagnitude ndash The relativebrightness of a star asseen by an observer on

Earth Guide Star ndash A sufficiently

bright star to use as areference for imagecompensation The

required magnitude variesas a function of the desiredobservation wavelength

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1526

Limitations of Image Compensation

Compensation in visible wavelengths (05um)requires a guide star of magnitude 10 or brighter

Compensation in infrared wavelengths (22um)

allows guide stars down to magnitude 14

Small isoplanatic region around the guide starlimits total observation area

ndash Visual ndash 1100000 of the sky ndash IR ndash 11000 of the sky

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1626

Guide Stars

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1726

Artificial Guide Stars

The area of sky coverage can beexpanded using artificial guide stars

Created using a LASER aligned withthe telescope optics

Rayleigh beacons take advantage ofRayleigh scattering in theatmosphere ndash Useful for telescopes with apertures lt 2m

ndash Creates a 1 to 2 arc second guide star 5 to

10km in altitude ndash 100W LASER

ndash LASER is pulsed so that backscatter can beeliminated by range gating

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1826

Artificial Guide Stars

Sodium Beaconsexploit a layer ofsodium vapor in the

upper atmosphere ndash 10W LASER at 589nm

ndash Excites sodium atoms90 to 92 km in altitude

Photo - The Sodium laser launching

from the side of the LickObservatory 120 ShaneTelescope This is a 10 minute timeexposure - note the star trails

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1926

Artificial Guide Stars

Natural guide starrequired for tiltcorrection

Limiting magnitude forguide star is about 20

Result is nearly 100

sky coverage

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2026

IR Stellar imaging from Lick

Observatory

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2126

Upper Left Io imagetaken with Keckadaptive optics K-band 22 micron

Upper Right Io imagebased on visible lighttaken with Galileospacecraft orbiter

Lower Left Io imagetaken with Keckadaptive optics L-band35micron

Lower Right Io imagetaken without Keckadaptive optics

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2226

The Lick Observatory CIS

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2326

Non-Astronomical Applications

Most of the current AOtechnology wasdeveloped by DARPA

during the Cold War toimage and shoot downsatellites with LASERweapons

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2426

Retinal Imaging

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2526

References

Carroll Joseph Daniel C Gray Austin Roorda David R Williams ldquoRecent Advances inRetinal Imaging with Adaptive Opticsrdquo Optics and Photonics News Jan 2005 p 36-42

Chaisson Eric and Steve McMillan Astronomy Today 4th Edition Prentice Hall UpperSaddle River NJ 2002

Florence Ronald The Perfect Machine Harper Collins New York NY 1994

Hardy John W Adaptive Optics for Astronomical Telescopes Oxford University PressNew York NY 1998

Hardy John W ldquoAdaptive Opticsrdquo Scientific American June 1994 p 60-65

Hecht Eugene Optics 4th Edition Addison-Wesley Reading MA 2002

Tyson Robert K Principles of Adaptive Optics 2nd Edition Academic Press San DiegoCA 1998

AdaptiveOpticscom 2002 Adaptive Optics Associates Inc httpwwwaoainccom Center for Adaptive Optics 2005 University of California Santa Cruz

httpcfaoucolickorg

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2626

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 926

Wavefront Sensing

ShearingInterferometer

ndash Distorted wavefronts

result in phase shiftedoutput signals betweenthe detector arrays

ndash Two interferometers are

required for correctionin the x-y plane

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1026

Wavefront Correction

High speed tip-tiltmirror reduces overallwavefront tilt

Deformable mirror(monolithic orsegmented) correctswavefront shape

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1126

Wavefront Correction Monolithic Deformable Mirror

ndash Reflective face cast on a solid piezoelectric backing (14um)

ndash Thin face supported by an array of electro-mechanical actuators (+- 30um) ndash Thin face supported by an array of piezoelectric actuators (50um)

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1226

Wavefront Correction

Segmented Mirrors

ndash Capable of largercorrections than

monolithic types ndash Requires frequent

calibration

ndash Diffraction due to gaps

between segments

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1326

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1426

Some Definitions

Apparent or VisualMagnitude ndash The relativebrightness of a star asseen by an observer on

Earth Guide Star ndash A sufficiently

bright star to use as areference for imagecompensation The

required magnitude variesas a function of the desiredobservation wavelength

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1526

Limitations of Image Compensation

Compensation in visible wavelengths (05um)requires a guide star of magnitude 10 or brighter

Compensation in infrared wavelengths (22um)

allows guide stars down to magnitude 14

Small isoplanatic region around the guide starlimits total observation area

ndash Visual ndash 1100000 of the sky ndash IR ndash 11000 of the sky

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1626

Guide Stars

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1726

Artificial Guide Stars

The area of sky coverage can beexpanded using artificial guide stars

Created using a LASER aligned withthe telescope optics

Rayleigh beacons take advantage ofRayleigh scattering in theatmosphere ndash Useful for telescopes with apertures lt 2m

ndash Creates a 1 to 2 arc second guide star 5 to

10km in altitude ndash 100W LASER

ndash LASER is pulsed so that backscatter can beeliminated by range gating

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1826

Artificial Guide Stars

Sodium Beaconsexploit a layer ofsodium vapor in the

upper atmosphere ndash 10W LASER at 589nm

ndash Excites sodium atoms90 to 92 km in altitude

Photo - The Sodium laser launching

from the side of the LickObservatory 120 ShaneTelescope This is a 10 minute timeexposure - note the star trails

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1926

Artificial Guide Stars

Natural guide starrequired for tiltcorrection

Limiting magnitude forguide star is about 20

Result is nearly 100

sky coverage

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2026

IR Stellar imaging from Lick

Observatory

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2126

Upper Left Io imagetaken with Keckadaptive optics K-band 22 micron

Upper Right Io imagebased on visible lighttaken with Galileospacecraft orbiter

Lower Left Io imagetaken with Keckadaptive optics L-band35micron

Lower Right Io imagetaken without Keckadaptive optics

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2226

The Lick Observatory CIS

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2326

Non-Astronomical Applications

Most of the current AOtechnology wasdeveloped by DARPA

during the Cold War toimage and shoot downsatellites with LASERweapons

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2426

Retinal Imaging

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2526

References

Carroll Joseph Daniel C Gray Austin Roorda David R Williams ldquoRecent Advances inRetinal Imaging with Adaptive Opticsrdquo Optics and Photonics News Jan 2005 p 36-42

Chaisson Eric and Steve McMillan Astronomy Today 4th Edition Prentice Hall UpperSaddle River NJ 2002

Florence Ronald The Perfect Machine Harper Collins New York NY 1994

Hardy John W Adaptive Optics for Astronomical Telescopes Oxford University PressNew York NY 1998

Hardy John W ldquoAdaptive Opticsrdquo Scientific American June 1994 p 60-65

Hecht Eugene Optics 4th Edition Addison-Wesley Reading MA 2002

Tyson Robert K Principles of Adaptive Optics 2nd Edition Academic Press San DiegoCA 1998

AdaptiveOpticscom 2002 Adaptive Optics Associates Inc httpwwwaoainccom Center for Adaptive Optics 2005 University of California Santa Cruz

httpcfaoucolickorg

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2626

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1026

Wavefront Correction

High speed tip-tiltmirror reduces overallwavefront tilt

Deformable mirror(monolithic orsegmented) correctswavefront shape

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1126

Wavefront Correction Monolithic Deformable Mirror

ndash Reflective face cast on a solid piezoelectric backing (14um)

ndash Thin face supported by an array of electro-mechanical actuators (+- 30um) ndash Thin face supported by an array of piezoelectric actuators (50um)

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1226

Wavefront Correction

Segmented Mirrors

ndash Capable of largercorrections than

monolithic types ndash Requires frequent

calibration

ndash Diffraction due to gaps

between segments

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1326

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1426

Some Definitions

Apparent or VisualMagnitude ndash The relativebrightness of a star asseen by an observer on

Earth Guide Star ndash A sufficiently

bright star to use as areference for imagecompensation The

required magnitude variesas a function of the desiredobservation wavelength

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1526

Limitations of Image Compensation

Compensation in visible wavelengths (05um)requires a guide star of magnitude 10 or brighter

Compensation in infrared wavelengths (22um)

allows guide stars down to magnitude 14

Small isoplanatic region around the guide starlimits total observation area

ndash Visual ndash 1100000 of the sky ndash IR ndash 11000 of the sky

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1626

Guide Stars

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1726

Artificial Guide Stars

The area of sky coverage can beexpanded using artificial guide stars

Created using a LASER aligned withthe telescope optics

Rayleigh beacons take advantage ofRayleigh scattering in theatmosphere ndash Useful for telescopes with apertures lt 2m

ndash Creates a 1 to 2 arc second guide star 5 to

10km in altitude ndash 100W LASER

ndash LASER is pulsed so that backscatter can beeliminated by range gating

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1826

Artificial Guide Stars

Sodium Beaconsexploit a layer ofsodium vapor in the

upper atmosphere ndash 10W LASER at 589nm

ndash Excites sodium atoms90 to 92 km in altitude

Photo - The Sodium laser launching

from the side of the LickObservatory 120 ShaneTelescope This is a 10 minute timeexposure - note the star trails

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1926

Artificial Guide Stars

Natural guide starrequired for tiltcorrection

Limiting magnitude forguide star is about 20

Result is nearly 100

sky coverage

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2026

IR Stellar imaging from Lick

Observatory

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2126

Upper Left Io imagetaken with Keckadaptive optics K-band 22 micron

Upper Right Io imagebased on visible lighttaken with Galileospacecraft orbiter

Lower Left Io imagetaken with Keckadaptive optics L-band35micron

Lower Right Io imagetaken without Keckadaptive optics

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2226

The Lick Observatory CIS

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2326

Non-Astronomical Applications

Most of the current AOtechnology wasdeveloped by DARPA

during the Cold War toimage and shoot downsatellites with LASERweapons

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2426

Retinal Imaging

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2526

References

Carroll Joseph Daniel C Gray Austin Roorda David R Williams ldquoRecent Advances inRetinal Imaging with Adaptive Opticsrdquo Optics and Photonics News Jan 2005 p 36-42

Chaisson Eric and Steve McMillan Astronomy Today 4th Edition Prentice Hall UpperSaddle River NJ 2002

Florence Ronald The Perfect Machine Harper Collins New York NY 1994

Hardy John W Adaptive Optics for Astronomical Telescopes Oxford University PressNew York NY 1998

Hardy John W ldquoAdaptive Opticsrdquo Scientific American June 1994 p 60-65

Hecht Eugene Optics 4th Edition Addison-Wesley Reading MA 2002

Tyson Robert K Principles of Adaptive Optics 2nd Edition Academic Press San DiegoCA 1998

AdaptiveOpticscom 2002 Adaptive Optics Associates Inc httpwwwaoainccom Center for Adaptive Optics 2005 University of California Santa Cruz

httpcfaoucolickorg

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2626

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1126

Wavefront Correction Monolithic Deformable Mirror

ndash Reflective face cast on a solid piezoelectric backing (14um)

ndash Thin face supported by an array of electro-mechanical actuators (+- 30um) ndash Thin face supported by an array of piezoelectric actuators (50um)

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1226

Wavefront Correction

Segmented Mirrors

ndash Capable of largercorrections than

monolithic types ndash Requires frequent

calibration

ndash Diffraction due to gaps

between segments

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1326

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1426

Some Definitions

Apparent or VisualMagnitude ndash The relativebrightness of a star asseen by an observer on

Earth Guide Star ndash A sufficiently

bright star to use as areference for imagecompensation The

required magnitude variesas a function of the desiredobservation wavelength

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1526

Limitations of Image Compensation

Compensation in visible wavelengths (05um)requires a guide star of magnitude 10 or brighter

Compensation in infrared wavelengths (22um)

allows guide stars down to magnitude 14

Small isoplanatic region around the guide starlimits total observation area

ndash Visual ndash 1100000 of the sky ndash IR ndash 11000 of the sky

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1626

Guide Stars

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1726

Artificial Guide Stars

The area of sky coverage can beexpanded using artificial guide stars

Created using a LASER aligned withthe telescope optics

Rayleigh beacons take advantage ofRayleigh scattering in theatmosphere ndash Useful for telescopes with apertures lt 2m

ndash Creates a 1 to 2 arc second guide star 5 to

10km in altitude ndash 100W LASER

ndash LASER is pulsed so that backscatter can beeliminated by range gating

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1826

Artificial Guide Stars

Sodium Beaconsexploit a layer ofsodium vapor in the

upper atmosphere ndash 10W LASER at 589nm

ndash Excites sodium atoms90 to 92 km in altitude

Photo - The Sodium laser launching

from the side of the LickObservatory 120 ShaneTelescope This is a 10 minute timeexposure - note the star trails

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1926

Artificial Guide Stars

Natural guide starrequired for tiltcorrection

Limiting magnitude forguide star is about 20

Result is nearly 100

sky coverage

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2026

IR Stellar imaging from Lick

Observatory

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2126

Upper Left Io imagetaken with Keckadaptive optics K-band 22 micron

Upper Right Io imagebased on visible lighttaken with Galileospacecraft orbiter

Lower Left Io imagetaken with Keckadaptive optics L-band35micron

Lower Right Io imagetaken without Keckadaptive optics

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2226

The Lick Observatory CIS

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2326

Non-Astronomical Applications

Most of the current AOtechnology wasdeveloped by DARPA

during the Cold War toimage and shoot downsatellites with LASERweapons

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2426

Retinal Imaging

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2526

References

Carroll Joseph Daniel C Gray Austin Roorda David R Williams ldquoRecent Advances inRetinal Imaging with Adaptive Opticsrdquo Optics and Photonics News Jan 2005 p 36-42

Chaisson Eric and Steve McMillan Astronomy Today 4th Edition Prentice Hall UpperSaddle River NJ 2002

Florence Ronald The Perfect Machine Harper Collins New York NY 1994

Hardy John W Adaptive Optics for Astronomical Telescopes Oxford University PressNew York NY 1998

Hardy John W ldquoAdaptive Opticsrdquo Scientific American June 1994 p 60-65

Hecht Eugene Optics 4th Edition Addison-Wesley Reading MA 2002

Tyson Robert K Principles of Adaptive Optics 2nd Edition Academic Press San DiegoCA 1998

AdaptiveOpticscom 2002 Adaptive Optics Associates Inc httpwwwaoainccom Center for Adaptive Optics 2005 University of California Santa Cruz

httpcfaoucolickorg

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2626

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1226

Wavefront Correction

Segmented Mirrors

ndash Capable of largercorrections than

monolithic types ndash Requires frequent

calibration

ndash Diffraction due to gaps

between segments

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1326

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1426

Some Definitions

Apparent or VisualMagnitude ndash The relativebrightness of a star asseen by an observer on

Earth Guide Star ndash A sufficiently

bright star to use as areference for imagecompensation The

required magnitude variesas a function of the desiredobservation wavelength

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1526

Limitations of Image Compensation

Compensation in visible wavelengths (05um)requires a guide star of magnitude 10 or brighter

Compensation in infrared wavelengths (22um)

allows guide stars down to magnitude 14

Small isoplanatic region around the guide starlimits total observation area

ndash Visual ndash 1100000 of the sky ndash IR ndash 11000 of the sky

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1626

Guide Stars

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1726

Artificial Guide Stars

The area of sky coverage can beexpanded using artificial guide stars

Created using a LASER aligned withthe telescope optics

Rayleigh beacons take advantage ofRayleigh scattering in theatmosphere ndash Useful for telescopes with apertures lt 2m

ndash Creates a 1 to 2 arc second guide star 5 to

10km in altitude ndash 100W LASER

ndash LASER is pulsed so that backscatter can beeliminated by range gating

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1826

Artificial Guide Stars

Sodium Beaconsexploit a layer ofsodium vapor in the

upper atmosphere ndash 10W LASER at 589nm

ndash Excites sodium atoms90 to 92 km in altitude

Photo - The Sodium laser launching

from the side of the LickObservatory 120 ShaneTelescope This is a 10 minute timeexposure - note the star trails

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1926

Artificial Guide Stars

Natural guide starrequired for tiltcorrection

Limiting magnitude forguide star is about 20

Result is nearly 100

sky coverage

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2026

IR Stellar imaging from Lick

Observatory

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2126

Upper Left Io imagetaken with Keckadaptive optics K-band 22 micron

Upper Right Io imagebased on visible lighttaken with Galileospacecraft orbiter

Lower Left Io imagetaken with Keckadaptive optics L-band35micron

Lower Right Io imagetaken without Keckadaptive optics

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2226

The Lick Observatory CIS

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2326

Non-Astronomical Applications

Most of the current AOtechnology wasdeveloped by DARPA

during the Cold War toimage and shoot downsatellites with LASERweapons

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2426

Retinal Imaging

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2526

References

Carroll Joseph Daniel C Gray Austin Roorda David R Williams ldquoRecent Advances inRetinal Imaging with Adaptive Opticsrdquo Optics and Photonics News Jan 2005 p 36-42

Chaisson Eric and Steve McMillan Astronomy Today 4th Edition Prentice Hall UpperSaddle River NJ 2002

Florence Ronald The Perfect Machine Harper Collins New York NY 1994

Hardy John W Adaptive Optics for Astronomical Telescopes Oxford University PressNew York NY 1998

Hardy John W ldquoAdaptive Opticsrdquo Scientific American June 1994 p 60-65

Hecht Eugene Optics 4th Edition Addison-Wesley Reading MA 2002

Tyson Robert K Principles of Adaptive Optics 2nd Edition Academic Press San DiegoCA 1998

AdaptiveOpticscom 2002 Adaptive Optics Associates Inc httpwwwaoainccom Center for Adaptive Optics 2005 University of California Santa Cruz

httpcfaoucolickorg

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2626

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1326

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1426

Some Definitions

Apparent or VisualMagnitude ndash The relativebrightness of a star asseen by an observer on

Earth Guide Star ndash A sufficiently

bright star to use as areference for imagecompensation The

required magnitude variesas a function of the desiredobservation wavelength

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1526

Limitations of Image Compensation

Compensation in visible wavelengths (05um)requires a guide star of magnitude 10 or brighter

Compensation in infrared wavelengths (22um)

allows guide stars down to magnitude 14

Small isoplanatic region around the guide starlimits total observation area

ndash Visual ndash 1100000 of the sky ndash IR ndash 11000 of the sky

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1626

Guide Stars

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1726

Artificial Guide Stars

The area of sky coverage can beexpanded using artificial guide stars

Created using a LASER aligned withthe telescope optics

Rayleigh beacons take advantage ofRayleigh scattering in theatmosphere ndash Useful for telescopes with apertures lt 2m

ndash Creates a 1 to 2 arc second guide star 5 to

10km in altitude ndash 100W LASER

ndash LASER is pulsed so that backscatter can beeliminated by range gating

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1826

Artificial Guide Stars

Sodium Beaconsexploit a layer ofsodium vapor in the

upper atmosphere ndash 10W LASER at 589nm

ndash Excites sodium atoms90 to 92 km in altitude

Photo - The Sodium laser launching

from the side of the LickObservatory 120 ShaneTelescope This is a 10 minute timeexposure - note the star trails

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1926

Artificial Guide Stars

Natural guide starrequired for tiltcorrection

Limiting magnitude forguide star is about 20

Result is nearly 100

sky coverage

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2026

IR Stellar imaging from Lick

Observatory

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2126

Upper Left Io imagetaken with Keckadaptive optics K-band 22 micron

Upper Right Io imagebased on visible lighttaken with Galileospacecraft orbiter

Lower Left Io imagetaken with Keckadaptive optics L-band35micron

Lower Right Io imagetaken without Keckadaptive optics

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2226

The Lick Observatory CIS

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2326

Non-Astronomical Applications

Most of the current AOtechnology wasdeveloped by DARPA

during the Cold War toimage and shoot downsatellites with LASERweapons

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2426

Retinal Imaging

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2526

References

Carroll Joseph Daniel C Gray Austin Roorda David R Williams ldquoRecent Advances inRetinal Imaging with Adaptive Opticsrdquo Optics and Photonics News Jan 2005 p 36-42

Chaisson Eric and Steve McMillan Astronomy Today 4th Edition Prentice Hall UpperSaddle River NJ 2002

Florence Ronald The Perfect Machine Harper Collins New York NY 1994

Hardy John W Adaptive Optics for Astronomical Telescopes Oxford University PressNew York NY 1998

Hardy John W ldquoAdaptive Opticsrdquo Scientific American June 1994 p 60-65

Hecht Eugene Optics 4th Edition Addison-Wesley Reading MA 2002

Tyson Robert K Principles of Adaptive Optics 2nd Edition Academic Press San DiegoCA 1998

AdaptiveOpticscom 2002 Adaptive Optics Associates Inc httpwwwaoainccom Center for Adaptive Optics 2005 University of California Santa Cruz

httpcfaoucolickorg

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2626

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1426

Some Definitions

Apparent or VisualMagnitude ndash The relativebrightness of a star asseen by an observer on

Earth Guide Star ndash A sufficiently

bright star to use as areference for imagecompensation The

required magnitude variesas a function of the desiredobservation wavelength

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1526

Limitations of Image Compensation

Compensation in visible wavelengths (05um)requires a guide star of magnitude 10 or brighter

Compensation in infrared wavelengths (22um)

allows guide stars down to magnitude 14

Small isoplanatic region around the guide starlimits total observation area

ndash Visual ndash 1100000 of the sky ndash IR ndash 11000 of the sky

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1626

Guide Stars

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1726

Artificial Guide Stars

The area of sky coverage can beexpanded using artificial guide stars

Created using a LASER aligned withthe telescope optics

Rayleigh beacons take advantage ofRayleigh scattering in theatmosphere ndash Useful for telescopes with apertures lt 2m

ndash Creates a 1 to 2 arc second guide star 5 to

10km in altitude ndash 100W LASER

ndash LASER is pulsed so that backscatter can beeliminated by range gating

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1826

Artificial Guide Stars

Sodium Beaconsexploit a layer ofsodium vapor in the

upper atmosphere ndash 10W LASER at 589nm

ndash Excites sodium atoms90 to 92 km in altitude

Photo - The Sodium laser launching

from the side of the LickObservatory 120 ShaneTelescope This is a 10 minute timeexposure - note the star trails

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1926

Artificial Guide Stars

Natural guide starrequired for tiltcorrection

Limiting magnitude forguide star is about 20

Result is nearly 100

sky coverage

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2026

IR Stellar imaging from Lick

Observatory

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2126

Upper Left Io imagetaken with Keckadaptive optics K-band 22 micron

Upper Right Io imagebased on visible lighttaken with Galileospacecraft orbiter

Lower Left Io imagetaken with Keckadaptive optics L-band35micron

Lower Right Io imagetaken without Keckadaptive optics

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2226

The Lick Observatory CIS

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2326

Non-Astronomical Applications

Most of the current AOtechnology wasdeveloped by DARPA

during the Cold War toimage and shoot downsatellites with LASERweapons

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2426

Retinal Imaging

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2526

References

Carroll Joseph Daniel C Gray Austin Roorda David R Williams ldquoRecent Advances inRetinal Imaging with Adaptive Opticsrdquo Optics and Photonics News Jan 2005 p 36-42

Chaisson Eric and Steve McMillan Astronomy Today 4th Edition Prentice Hall UpperSaddle River NJ 2002

Florence Ronald The Perfect Machine Harper Collins New York NY 1994

Hardy John W Adaptive Optics for Astronomical Telescopes Oxford University PressNew York NY 1998

Hardy John W ldquoAdaptive Opticsrdquo Scientific American June 1994 p 60-65

Hecht Eugene Optics 4th Edition Addison-Wesley Reading MA 2002

Tyson Robert K Principles of Adaptive Optics 2nd Edition Academic Press San DiegoCA 1998

AdaptiveOpticscom 2002 Adaptive Optics Associates Inc httpwwwaoainccom Center for Adaptive Optics 2005 University of California Santa Cruz

httpcfaoucolickorg

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2626

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1526

Limitations of Image Compensation

Compensation in visible wavelengths (05um)requires a guide star of magnitude 10 or brighter

Compensation in infrared wavelengths (22um)

allows guide stars down to magnitude 14

Small isoplanatic region around the guide starlimits total observation area

ndash Visual ndash 1100000 of the sky ndash IR ndash 11000 of the sky

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1626

Guide Stars

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1726

Artificial Guide Stars

The area of sky coverage can beexpanded using artificial guide stars

Created using a LASER aligned withthe telescope optics

Rayleigh beacons take advantage ofRayleigh scattering in theatmosphere ndash Useful for telescopes with apertures lt 2m

ndash Creates a 1 to 2 arc second guide star 5 to

10km in altitude ndash 100W LASER

ndash LASER is pulsed so that backscatter can beeliminated by range gating

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1826

Artificial Guide Stars

Sodium Beaconsexploit a layer ofsodium vapor in the

upper atmosphere ndash 10W LASER at 589nm

ndash Excites sodium atoms90 to 92 km in altitude

Photo - The Sodium laser launching

from the side of the LickObservatory 120 ShaneTelescope This is a 10 minute timeexposure - note the star trails

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1926

Artificial Guide Stars

Natural guide starrequired for tiltcorrection

Limiting magnitude forguide star is about 20

Result is nearly 100

sky coverage

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2026

IR Stellar imaging from Lick

Observatory

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2126

Upper Left Io imagetaken with Keckadaptive optics K-band 22 micron

Upper Right Io imagebased on visible lighttaken with Galileospacecraft orbiter

Lower Left Io imagetaken with Keckadaptive optics L-band35micron

Lower Right Io imagetaken without Keckadaptive optics

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2226

The Lick Observatory CIS

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2326

Non-Astronomical Applications

Most of the current AOtechnology wasdeveloped by DARPA

during the Cold War toimage and shoot downsatellites with LASERweapons

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2426

Retinal Imaging

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2526

References

Carroll Joseph Daniel C Gray Austin Roorda David R Williams ldquoRecent Advances inRetinal Imaging with Adaptive Opticsrdquo Optics and Photonics News Jan 2005 p 36-42

Chaisson Eric and Steve McMillan Astronomy Today 4th Edition Prentice Hall UpperSaddle River NJ 2002

Florence Ronald The Perfect Machine Harper Collins New York NY 1994

Hardy John W Adaptive Optics for Astronomical Telescopes Oxford University PressNew York NY 1998

Hardy John W ldquoAdaptive Opticsrdquo Scientific American June 1994 p 60-65

Hecht Eugene Optics 4th Edition Addison-Wesley Reading MA 2002

Tyson Robert K Principles of Adaptive Optics 2nd Edition Academic Press San DiegoCA 1998

AdaptiveOpticscom 2002 Adaptive Optics Associates Inc httpwwwaoainccom Center for Adaptive Optics 2005 University of California Santa Cruz

httpcfaoucolickorg

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2626

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1626

Guide Stars

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1726

Artificial Guide Stars

The area of sky coverage can beexpanded using artificial guide stars

Created using a LASER aligned withthe telescope optics

Rayleigh beacons take advantage ofRayleigh scattering in theatmosphere ndash Useful for telescopes with apertures lt 2m

ndash Creates a 1 to 2 arc second guide star 5 to

10km in altitude ndash 100W LASER

ndash LASER is pulsed so that backscatter can beeliminated by range gating

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1826

Artificial Guide Stars

Sodium Beaconsexploit a layer ofsodium vapor in the

upper atmosphere ndash 10W LASER at 589nm

ndash Excites sodium atoms90 to 92 km in altitude

Photo - The Sodium laser launching

from the side of the LickObservatory 120 ShaneTelescope This is a 10 minute timeexposure - note the star trails

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1926

Artificial Guide Stars

Natural guide starrequired for tiltcorrection

Limiting magnitude forguide star is about 20

Result is nearly 100

sky coverage

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2026

IR Stellar imaging from Lick

Observatory

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2126

Upper Left Io imagetaken with Keckadaptive optics K-band 22 micron

Upper Right Io imagebased on visible lighttaken with Galileospacecraft orbiter

Lower Left Io imagetaken with Keckadaptive optics L-band35micron

Lower Right Io imagetaken without Keckadaptive optics

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2226

The Lick Observatory CIS

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2326

Non-Astronomical Applications

Most of the current AOtechnology wasdeveloped by DARPA

during the Cold War toimage and shoot downsatellites with LASERweapons

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2426

Retinal Imaging

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2526

References

Carroll Joseph Daniel C Gray Austin Roorda David R Williams ldquoRecent Advances inRetinal Imaging with Adaptive Opticsrdquo Optics and Photonics News Jan 2005 p 36-42

Chaisson Eric and Steve McMillan Astronomy Today 4th Edition Prentice Hall UpperSaddle River NJ 2002

Florence Ronald The Perfect Machine Harper Collins New York NY 1994

Hardy John W Adaptive Optics for Astronomical Telescopes Oxford University PressNew York NY 1998

Hardy John W ldquoAdaptive Opticsrdquo Scientific American June 1994 p 60-65

Hecht Eugene Optics 4th Edition Addison-Wesley Reading MA 2002

Tyson Robert K Principles of Adaptive Optics 2nd Edition Academic Press San DiegoCA 1998

AdaptiveOpticscom 2002 Adaptive Optics Associates Inc httpwwwaoainccom Center for Adaptive Optics 2005 University of California Santa Cruz

httpcfaoucolickorg

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2626

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1726

Artificial Guide Stars

The area of sky coverage can beexpanded using artificial guide stars

Created using a LASER aligned withthe telescope optics

Rayleigh beacons take advantage ofRayleigh scattering in theatmosphere ndash Useful for telescopes with apertures lt 2m

ndash Creates a 1 to 2 arc second guide star 5 to

10km in altitude ndash 100W LASER

ndash LASER is pulsed so that backscatter can beeliminated by range gating

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1826

Artificial Guide Stars

Sodium Beaconsexploit a layer ofsodium vapor in the

upper atmosphere ndash 10W LASER at 589nm

ndash Excites sodium atoms90 to 92 km in altitude

Photo - The Sodium laser launching

from the side of the LickObservatory 120 ShaneTelescope This is a 10 minute timeexposure - note the star trails

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1926

Artificial Guide Stars

Natural guide starrequired for tiltcorrection

Limiting magnitude forguide star is about 20

Result is nearly 100

sky coverage

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2026

IR Stellar imaging from Lick

Observatory

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2126

Upper Left Io imagetaken with Keckadaptive optics K-band 22 micron

Upper Right Io imagebased on visible lighttaken with Galileospacecraft orbiter

Lower Left Io imagetaken with Keckadaptive optics L-band35micron

Lower Right Io imagetaken without Keckadaptive optics

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2226

The Lick Observatory CIS

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2326

Non-Astronomical Applications

Most of the current AOtechnology wasdeveloped by DARPA

during the Cold War toimage and shoot downsatellites with LASERweapons

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2426

Retinal Imaging

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2526

References

Carroll Joseph Daniel C Gray Austin Roorda David R Williams ldquoRecent Advances inRetinal Imaging with Adaptive Opticsrdquo Optics and Photonics News Jan 2005 p 36-42

Chaisson Eric and Steve McMillan Astronomy Today 4th Edition Prentice Hall UpperSaddle River NJ 2002

Florence Ronald The Perfect Machine Harper Collins New York NY 1994

Hardy John W Adaptive Optics for Astronomical Telescopes Oxford University PressNew York NY 1998

Hardy John W ldquoAdaptive Opticsrdquo Scientific American June 1994 p 60-65

Hecht Eugene Optics 4th Edition Addison-Wesley Reading MA 2002

Tyson Robert K Principles of Adaptive Optics 2nd Edition Academic Press San DiegoCA 1998

AdaptiveOpticscom 2002 Adaptive Optics Associates Inc httpwwwaoainccom Center for Adaptive Optics 2005 University of California Santa Cruz

httpcfaoucolickorg

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2626

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1826

Artificial Guide Stars

Sodium Beaconsexploit a layer ofsodium vapor in the

upper atmosphere ndash 10W LASER at 589nm

ndash Excites sodium atoms90 to 92 km in altitude

Photo - The Sodium laser launching

from the side of the LickObservatory 120 ShaneTelescope This is a 10 minute timeexposure - note the star trails

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1926

Artificial Guide Stars

Natural guide starrequired for tiltcorrection

Limiting magnitude forguide star is about 20

Result is nearly 100

sky coverage

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2026

IR Stellar imaging from Lick

Observatory

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2126

Upper Left Io imagetaken with Keckadaptive optics K-band 22 micron

Upper Right Io imagebased on visible lighttaken with Galileospacecraft orbiter

Lower Left Io imagetaken with Keckadaptive optics L-band35micron

Lower Right Io imagetaken without Keckadaptive optics

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2226

The Lick Observatory CIS

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2326

Non-Astronomical Applications

Most of the current AOtechnology wasdeveloped by DARPA

during the Cold War toimage and shoot downsatellites with LASERweapons

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2426

Retinal Imaging

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2526

References

Carroll Joseph Daniel C Gray Austin Roorda David R Williams ldquoRecent Advances inRetinal Imaging with Adaptive Opticsrdquo Optics and Photonics News Jan 2005 p 36-42

Chaisson Eric and Steve McMillan Astronomy Today 4th Edition Prentice Hall UpperSaddle River NJ 2002

Florence Ronald The Perfect Machine Harper Collins New York NY 1994

Hardy John W Adaptive Optics for Astronomical Telescopes Oxford University PressNew York NY 1998

Hardy John W ldquoAdaptive Opticsrdquo Scientific American June 1994 p 60-65

Hecht Eugene Optics 4th Edition Addison-Wesley Reading MA 2002

Tyson Robert K Principles of Adaptive Optics 2nd Edition Academic Press San DiegoCA 1998

AdaptiveOpticscom 2002 Adaptive Optics Associates Inc httpwwwaoainccom Center for Adaptive Optics 2005 University of California Santa Cruz

httpcfaoucolickorg

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2626

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 1926

Artificial Guide Stars

Natural guide starrequired for tiltcorrection

Limiting magnitude forguide star is about 20

Result is nearly 100

sky coverage

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2026

IR Stellar imaging from Lick

Observatory

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2126

Upper Left Io imagetaken with Keckadaptive optics K-band 22 micron

Upper Right Io imagebased on visible lighttaken with Galileospacecraft orbiter

Lower Left Io imagetaken with Keckadaptive optics L-band35micron

Lower Right Io imagetaken without Keckadaptive optics

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2226

The Lick Observatory CIS

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2326

Non-Astronomical Applications

Most of the current AOtechnology wasdeveloped by DARPA

during the Cold War toimage and shoot downsatellites with LASERweapons

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2426

Retinal Imaging

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2526

References

Carroll Joseph Daniel C Gray Austin Roorda David R Williams ldquoRecent Advances inRetinal Imaging with Adaptive Opticsrdquo Optics and Photonics News Jan 2005 p 36-42

Chaisson Eric and Steve McMillan Astronomy Today 4th Edition Prentice Hall UpperSaddle River NJ 2002

Florence Ronald The Perfect Machine Harper Collins New York NY 1994

Hardy John W Adaptive Optics for Astronomical Telescopes Oxford University PressNew York NY 1998

Hardy John W ldquoAdaptive Opticsrdquo Scientific American June 1994 p 60-65

Hecht Eugene Optics 4th Edition Addison-Wesley Reading MA 2002

Tyson Robert K Principles of Adaptive Optics 2nd Edition Academic Press San DiegoCA 1998

AdaptiveOpticscom 2002 Adaptive Optics Associates Inc httpwwwaoainccom Center for Adaptive Optics 2005 University of California Santa Cruz

httpcfaoucolickorg

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2626

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2026

IR Stellar imaging from Lick

Observatory

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2126

Upper Left Io imagetaken with Keckadaptive optics K-band 22 micron

Upper Right Io imagebased on visible lighttaken with Galileospacecraft orbiter

Lower Left Io imagetaken with Keckadaptive optics L-band35micron

Lower Right Io imagetaken without Keckadaptive optics

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2226

The Lick Observatory CIS

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2326

Non-Astronomical Applications

Most of the current AOtechnology wasdeveloped by DARPA

during the Cold War toimage and shoot downsatellites with LASERweapons

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2426

Retinal Imaging

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2526

References

Carroll Joseph Daniel C Gray Austin Roorda David R Williams ldquoRecent Advances inRetinal Imaging with Adaptive Opticsrdquo Optics and Photonics News Jan 2005 p 36-42

Chaisson Eric and Steve McMillan Astronomy Today 4th Edition Prentice Hall UpperSaddle River NJ 2002

Florence Ronald The Perfect Machine Harper Collins New York NY 1994

Hardy John W Adaptive Optics for Astronomical Telescopes Oxford University PressNew York NY 1998

Hardy John W ldquoAdaptive Opticsrdquo Scientific American June 1994 p 60-65

Hecht Eugene Optics 4th Edition Addison-Wesley Reading MA 2002

Tyson Robert K Principles of Adaptive Optics 2nd Edition Academic Press San DiegoCA 1998

AdaptiveOpticscom 2002 Adaptive Optics Associates Inc httpwwwaoainccom Center for Adaptive Optics 2005 University of California Santa Cruz

httpcfaoucolickorg

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2626

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2126

Upper Left Io imagetaken with Keckadaptive optics K-band 22 micron

Upper Right Io imagebased on visible lighttaken with Galileospacecraft orbiter

Lower Left Io imagetaken with Keckadaptive optics L-band35micron

Lower Right Io imagetaken without Keckadaptive optics

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2226

The Lick Observatory CIS

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2326

Non-Astronomical Applications

Most of the current AOtechnology wasdeveloped by DARPA

during the Cold War toimage and shoot downsatellites with LASERweapons

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2426

Retinal Imaging

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2526

References

Carroll Joseph Daniel C Gray Austin Roorda David R Williams ldquoRecent Advances inRetinal Imaging with Adaptive Opticsrdquo Optics and Photonics News Jan 2005 p 36-42

Chaisson Eric and Steve McMillan Astronomy Today 4th Edition Prentice Hall UpperSaddle River NJ 2002

Florence Ronald The Perfect Machine Harper Collins New York NY 1994

Hardy John W Adaptive Optics for Astronomical Telescopes Oxford University PressNew York NY 1998

Hardy John W ldquoAdaptive Opticsrdquo Scientific American June 1994 p 60-65

Hecht Eugene Optics 4th Edition Addison-Wesley Reading MA 2002

Tyson Robert K Principles of Adaptive Optics 2nd Edition Academic Press San DiegoCA 1998

AdaptiveOpticscom 2002 Adaptive Optics Associates Inc httpwwwaoainccom Center for Adaptive Optics 2005 University of California Santa Cruz

httpcfaoucolickorg

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2626

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2226

The Lick Observatory CIS

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2326

Non-Astronomical Applications

Most of the current AOtechnology wasdeveloped by DARPA

during the Cold War toimage and shoot downsatellites with LASERweapons

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2426

Retinal Imaging

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2526

References

Carroll Joseph Daniel C Gray Austin Roorda David R Williams ldquoRecent Advances inRetinal Imaging with Adaptive Opticsrdquo Optics and Photonics News Jan 2005 p 36-42

Chaisson Eric and Steve McMillan Astronomy Today 4th Edition Prentice Hall UpperSaddle River NJ 2002

Florence Ronald The Perfect Machine Harper Collins New York NY 1994

Hardy John W Adaptive Optics for Astronomical Telescopes Oxford University PressNew York NY 1998

Hardy John W ldquoAdaptive Opticsrdquo Scientific American June 1994 p 60-65

Hecht Eugene Optics 4th Edition Addison-Wesley Reading MA 2002

Tyson Robert K Principles of Adaptive Optics 2nd Edition Academic Press San DiegoCA 1998

AdaptiveOpticscom 2002 Adaptive Optics Associates Inc httpwwwaoainccom Center for Adaptive Optics 2005 University of California Santa Cruz

httpcfaoucolickorg

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2626

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2326

Non-Astronomical Applications

Most of the current AOtechnology wasdeveloped by DARPA

during the Cold War toimage and shoot downsatellites with LASERweapons

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2426

Retinal Imaging

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2526

References

Carroll Joseph Daniel C Gray Austin Roorda David R Williams ldquoRecent Advances inRetinal Imaging with Adaptive Opticsrdquo Optics and Photonics News Jan 2005 p 36-42

Chaisson Eric and Steve McMillan Astronomy Today 4th Edition Prentice Hall UpperSaddle River NJ 2002

Florence Ronald The Perfect Machine Harper Collins New York NY 1994

Hardy John W Adaptive Optics for Astronomical Telescopes Oxford University PressNew York NY 1998

Hardy John W ldquoAdaptive Opticsrdquo Scientific American June 1994 p 60-65

Hecht Eugene Optics 4th Edition Addison-Wesley Reading MA 2002

Tyson Robert K Principles of Adaptive Optics 2nd Edition Academic Press San DiegoCA 1998

AdaptiveOpticscom 2002 Adaptive Optics Associates Inc httpwwwaoainccom Center for Adaptive Optics 2005 University of California Santa Cruz

httpcfaoucolickorg

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2626

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2426

Retinal Imaging

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2526

References

Carroll Joseph Daniel C Gray Austin Roorda David R Williams ldquoRecent Advances inRetinal Imaging with Adaptive Opticsrdquo Optics and Photonics News Jan 2005 p 36-42

Chaisson Eric and Steve McMillan Astronomy Today 4th Edition Prentice Hall UpperSaddle River NJ 2002

Florence Ronald The Perfect Machine Harper Collins New York NY 1994

Hardy John W Adaptive Optics for Astronomical Telescopes Oxford University PressNew York NY 1998

Hardy John W ldquoAdaptive Opticsrdquo Scientific American June 1994 p 60-65

Hecht Eugene Optics 4th Edition Addison-Wesley Reading MA 2002

Tyson Robert K Principles of Adaptive Optics 2nd Edition Academic Press San DiegoCA 1998

AdaptiveOpticscom 2002 Adaptive Optics Associates Inc httpwwwaoainccom Center for Adaptive Optics 2005 University of California Santa Cruz

httpcfaoucolickorg

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2626

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2526

References

Carroll Joseph Daniel C Gray Austin Roorda David R Williams ldquoRecent Advances inRetinal Imaging with Adaptive Opticsrdquo Optics and Photonics News Jan 2005 p 36-42

Chaisson Eric and Steve McMillan Astronomy Today 4th Edition Prentice Hall UpperSaddle River NJ 2002

Florence Ronald The Perfect Machine Harper Collins New York NY 1994

Hardy John W Adaptive Optics for Astronomical Telescopes Oxford University PressNew York NY 1998

Hardy John W ldquoAdaptive Opticsrdquo Scientific American June 1994 p 60-65

Hecht Eugene Optics 4th Edition Addison-Wesley Reading MA 2002

Tyson Robert K Principles of Adaptive Optics 2nd Edition Academic Press San DiegoCA 1998

AdaptiveOpticscom 2002 Adaptive Optics Associates Inc httpwwwaoainccom Center for Adaptive Optics 2005 University of California Santa Cruz

httpcfaoucolickorg

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2626

822019 Rahul Krishnan Seminar Adaopt

httpslidepdfcomreaderfullrahul-krishnan-seminar-adaopt 2626


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