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Vol. 71

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http://www.astron.kharkov.ua/dip/maindep.htm

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sensor are dominated by mechanical vibration and pointing errors. The tip-tilt signal is used to drive the laser system
uplink tip-tilt mirror, thus keeping the Shack-Hartmann pattern centered on the wavefront sensor.
The high-order wavefront corrector within Robo-AO is a micro-electro-mechanical-systems (MEM
deformable mirror16 (Boston Micromachines Multi-DM). Robo-AO uses 120 of the 140 actuators to adjust
illuminated surface of the mirror, sufficient in spatial resolution to accurately fit the calculated correcting shape. T
actuators have a maximum surface deviation amplitude of 3.5 ȝm which corresponds to optical phase compensation
up to 7 ȝm. In typical seeing at Palomar observatory (median ~1.1"), this compensation length is greater than 5-sigma
the amplitude of the turbulence induced optical error and therefore results in significant correction headroo
Furthermore, the deformable mirror is used to compensate for static optical errors arising from the instrument atelescope at the cost of reduced dynamic range.

• Robo-AO (http://www.ifa.hawaii.edu/Robo-AO/)– ;þĻĘĕLæ
– ƫưƄưŽŷƒƅƇƏơ– ĹlŚï12

Baranec et al 2012 SPIE

Figure 1.The Robo-AO laser adaptive-optics system. The adaptive optics and science instruments are installed at theCassegrain focus of the robotic 60-inch telescope at Palomar Observatory. The laser system and support electronics areattached to opposite sides of the telescope tube for balance.
Figure 2. The Robo-AO adaptive optics system and science instruments. Light focused from the telescope secondary mirror
enters through a small hole at the center of the instrument before being reflected by 90 degrees by the first fold mirror
towards anflexure.
off-axis parabolic (OAP) mirror. This mirror images the telescope pupil on the deformable mirror surface. Afterand an uplink tip-tilt mirror to both stabilize the apparent laser beam position on sky and to correct for telescopereflection from the deformable mirror, an UV dichroic splits off the laser light (violet) and directs it to the laser wavefrontadaptive optics.
4.2 Synergistic projects

4.3 OutreachWe have established an educational collaboration with Pomona College which has proven to be particularly fruitful. This
collaboration inspired the creation of a new AO lab atPomona
aimed collaboration
at hands-on educationof undergraduates,
anddetailingtheTheRobo-AO
has publisheda web sitethe goals, science
deployment of a natural-guide-star version of Robo-AO
on
their1-m
telescopeatTableMountain.
Aspartofthegeared towards accessibility to the general public: http://www.astro.caltech.edu
ongoing collaboration, the Robo-AO has supplied the Pomona AO system with the full real-time Robo-AO software
highlighting major project milestones.
engine. The prototype Pomona system, dubbed ꞌKAPAO-Alphaꞌ, which demonstrates the basic operation of a natural
20
Disseminationof results
resultshaveto thebroader
interpretation ofguide star adaptive optics system has recently closed the AO loop
on-sky and theirrecentlybeenpublic,reportedincluding.
society,aremadeto simultaneous
thepublicPalomarO
The final KAPAO system (no ꞌAlphaꞌ), which will
be a remote-accesssystem offeringdual-band, bydiffraction-limited imaging at visible and near-infrared
wavelengths, delivering an order-of-magnitude improvementin(http://www.astro.caltech.edu/palomar/exhibits/)
which draws
over 100,000 visi
point source sensitivity and angular resolution relative
to the currenthighlighting
seeing limits adaptive
is in development
and is expectedtopresentationoptics science
is on display
in the Visitor Cen
be deployed in the near future21. Beyond the expanded
scientificcapabilities
enabledbyAO-enhanced
resolutionandobservatory has also embraced other online social media, and the results Robo-A
sensitivity, the interdisciplinary nature of the instrument development effort provides an exceptional opportunity to train
Palomar Observatory’s blog and Facebook page.
a broad range of undergraduate STEM students in AO technologies and techniques. The Pomona Table Mountain AO
Robo-AO
has recently
been augmented
with an eyepiece fosystem is an exciting example of how Robo-AO can expandIntheaddition,interaction
between researchand learning
through
adaptiveoptics
corrected
astronomicalobjects
(Fig.
7).
Theeyepieceis fed by a sel
adaptive optics.

ôÒØ• Robo-AO (http://www.ifa.hawaii.edu/Robo-AO/)

mounted on a removable kinematic base between the visible dichroic and vis– ƃŷźƮƇƀưƇ4.3 Outreach
simultaneous imaging with the visible camera. While access is currently limited, w
observing
astronomyclasses details
from Caltechand Pomona College.
The Robo-AO collaboration has published a web sitedetailing bythevisiting
goals, scienceand technicalof the project,geared towards accessibility to the general public: http://www.astro.caltech.edu/Robo-AO/. Updates are provided,– ŵŸƑƩưƍ
highlighting major project milestones.
Dissemination of results to the broader public, including interpretation of science discovery and its impact onsociety,aremadeto
thepublicbyPalomar
Observatory’sVisitor
Center(http://www.astro.caltech.edu/palomar/exhibits/) which draws over 100,000 visitors annually. A web-based kioskpresentation highlighting adaptive optics science is on display in the Visitor Center and available on the web. The
observatory has also embraced other online social media, and the results Robo-AO commissioning have appeared on
Palomar Observatory’s blog and Facebook page.
In addition, Robo-AO has recently been augmented with an eyepiece for the direct viewing of visible-light
adaptive optics corrected astronomical objects (Fig. 7). The eyepiece is fed by a selectable visible beam splitting mirror
mounted on a removable kinematic base between the visible dichroic and visible filter wheels. This allows for
simultaneous imaging with the visible camera. While access is currently limited, we intend to support future eyepieceobserving by visiting astronomy classes from Caltech and Pomona College.

Figure 7. Members of the Robo-AO team observing Mars with the eyepiece attached toband images of Mars captured without adaptive optics correction (middle) and with the5. FUTURE WORK
5.1 Infrared camera upgrade

The Robo-AO collaboration is currently in the process of upgrading the infrared igrade camera to a low-noise wide-field imager using a 2.5 μm cutoff Teledyne HAWRG). The science grade H2-RG detector has ~ 0.01 e-/sec dark current, < 5 equantum efficiency than the InGaAs, offering 45-80 times more sensitivity (TableZiegler+16Figure 7. Members of the Robo-AO team observing Mars with the eyepiece attached to Robo-AO (left). Simultaneous iband images of Mars captured without adaptive optics correction (middle) and with the Robo-AO system running (right).
Kepler áLyøŜƚŻƬưŵƎƜBranec+125. FUTURE WORKôÒØ• Robo-AO(http://www.ifa.hawaii.edu/Robo-AO/)– ƂƙưµŜ7À1→ŉŰųēŔŖŅŖÿÁÎÍńĜ}ŊŰŰŞŐŰŗòŀ
Robo-AO

http://www.ifa.hawaii.edu/Robo-AO/team.html

ŗŨłĹŀŴŗŋūŁƺ– AO÷çŘŋŖŜ ÜõńnĉŤŔŖŀů– `¢ĞĤŗŨ÷çƜƬƆŹžƑŘŋŖŝO ńĩŲů#ņ>ŌŉŘųÎ²śħËŋŖŨŚĿ

Robo-AO

http://www.ifa.hawaii.edu/Robo-AO/team.htm

The Robo-AO Team (Palomar 2009-2015)
Principal Investigator
Project Scientist
Co-Investigator
Software Lead

Christoph Baranec (U. Hawai'i)
Nicholas Law (UNC Chapel Hill)
A. N. Ramaprakash (IUCAA)
Reed Riddle (Caltech)

The Robo-AO Kitt Peak Team (2015-)
Principal Investigator
Project Scientist
Data Scientist
Robo-AO PI/Inst. Scientist
Robo-AO PS

Shri Kulkarni (Caltech)
Reed Riddle (Caltech)
Dmitry Duev (Caltech)
Christoph Baranec (U. Hawai'i)
Nicholas Law (UNC Chapel Hill)

Students
Graduate

Rachel Bowens-Rubin (U. Hawai'i)*Maïssa Salama (U. Hawai'i)*
Rebecca Jensen-Clem (Caltech)*Dani Atkinson (U. Hawai'i)*Carl Ziegler (UNC Chapel Hill)*
Larissa Nofi (U. Hawai'i)
Amy Ray (Mississippi State)
Gina Duggan (Caltech)
Avinash Surendran (IUCAA)
Kristina Hogstrom (Caltech)
Shriharsh Tendulkar (Caltech)
Undergraduate Jessica Schonhut (U. Hertfordshire/U. Hawaii, '17)*Celia Zhang (Caltech '18)*
Bianca Avalani (Caltech '17)
Rachel Thorp (Caltech '16)
Chatarin "Mee" Wong-u-railertkun (Caltech '14)
Dan Filler (Univ. of Utah '13)
Corinne Vassallo (Carnegie Mellon '13)
Victoria "Ashley" Villar (MIT '14)
Athanasios Papadopoulos (Aristotle U., Thessaloniki '13)
Ankit Arya (Mississippi State '12)
Alexander Rudy (Pomona '11)
Marland Sitt (Caltech '11)

Christoph Baranec
Rebecca Jensen-Clem
Nicholas Law
Morgan Bonnet

Reed Riddle
Dmitry Duev
Michael Feeney

Observing team (Kitt Peak)
Amy Ray
Mark TruebloodMegan Nieberding

Science team (Palomar)
Christoph Baranec
John Johnson
Shri Kulkarni
Timothy Morton
A. N. Ramaprakash
Shriharsh Tendulkar
Sergi Hildebrandt
Michał Drahus

Richard Dekany
Mansi Kasliwal
Nicholas Law
Eran Ofek
Reed Riddle
Lynne Hillenbrand
Gregg Hallinan
Leon Harding

Technical team (Palomar)
Christoph Baranec
Mahesh Burse
Hillol Das
Ernest Croner
Jason Fucik
Sujit Punnadi
Reed Riddle
Shriharsh Tendulkar
Kristina Hogstrom
Gina Duggan

Khanh Bui
Pravin Chordia
Jack Davis
Richard Dekany
Nicholas Law
A. N. Ramaprakash
Roger Smith
Jeff Zolkower
Dani Atkinson
Avinash Surendran(* currently active students on project)

Science team (Kitt Peak - under construction)
Shri Kulkarni
Nicholas Law
Rebecca Jensen-Clem

Christoph Baranec
Reed Riddle
Dmitry Duev

Technical team (Kitt Peak - under construction)

Original CAMERA concept and testbed team
Matthew Britton
Viswa Velur
Dan Beeler (Pomona '09)

Nicholas Law
Lothar Ratschbacher (U. of Vienna '08)
Wojciech Makowiecki (Jagiellonian U. '08)(c) 2009-2015 Robo-AO Collaboration.

`¢ĞĤÉAOĈĸ÷çŜħË• ĽõYĆľśÎ²ų'Xé– ƫưƄưŽŷƒŝ¶ŜƇƏƎƜŗ• ŤŎŝĽũŔŖťůľ– AOƅƇƏơ#ñśŲŒůG¥õŜêsĽÕľųċŴœœňŗġÆŝŗŅŚŀAOïƵčĻĖ·Ļ¢ĞĤ8ĻÿÁĴĻPT• VŗĽĳŚľAO÷ç
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AO instrument with a laser-guide star system, is mounted on the Palomar observatory 60-inch telescope and the Kitt-Peak
2.1-m telescope and used for research in astronomy.
We started the development of the AO systems for small telescopes, and now we made a compact optical AO instrument
to demonstrate the AO capability. The engineering observation was successfully done in Japan, however, the seeing was
not good. The best performance will be achieved when it is mounted on a telescope at a good seeing site like observatories
in Chile, and we hope to mount it on the 1-m telescope in La Silla observatory to demonstrate the AO capability of 0.1-0.2
arcsec angular resolution. We will briefly overview our AO instrument and show its performance in the engineeringobservation.

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2.1 Instrument overview– ąăĻùƳƱú¦ùƴ
The AO instrument we have developed is a demonstrator of the AO capability for small telescopes in optical wavelength.
A bright star is used as the natural guide star for the measurement of the atmospheric wavefront distortion, and it is also
the target, which is–observedby the integrated science camera (SC) to measure the point-spread function (PSF) after the,tƊƚƑòĻYĸĻwîćƳ©OTğÈ4¯ÒØČĶƴAO system. We adopt a refractive optics using ready-made commercial lenses by limiting the observing wavelength to the2. A COMPACT AO INSTRUMENT FOR SMALL TELESCOPESoptical. Affordable cameras are used for the WFS and the SC, because modest sensitivity is enough to demonstrate andexamine the AO performance. The control PC is a usual desktop PC operated by Windows 7. Accordingly, our AO
instrument becomes a compact and inexpensive system with a simple optics. Based on these concepts, we contracted withNishimura Co. Ltd. (Kyoto, Japan) for the design and fabrication. The external and internal views of our AO instrument
are shown in Figure 3.

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