MICADO will enable the ELT to perform diffraction limited near-infrared observations at first light. The instrument’s capabilities focus on imaging (including astrometric and high contrast) as well as single object spectroscopy. This contribution looks at how requirements from the observing modes have driven the instrument design and functionality. Using examples from specific science cases, and making use of the data simulation tool, an outline is presented of what we can expect the instrument to achieve.
MICADO, the Multi-AO-Imaging-Camera and Spectrometer for Deep Observations, is one of the first light instruments for the future 40 m class Extremely Large Telescope (ELT). MICADO utilizes the advanced laser guide star multiconjugate adaptive optics system MCAO developed by the MAORY consortium and the jointly developed singleconjugate adaptive optics system (SCAO). We present an overview on the conceptual design of the MICADO Cold Optical Instrument (COI) which comprises the infrared focal plane imager with its 3 x 3 4k2 HgCdTe detector array and a compact cross-dispersing slit spectrometer operating in the spectral range of 0.8 to 2.4 μm. High contrast imaging is enabled via a classical configuration of coronagraph and Lyot stops. The paper summarizes the MICADO COI interchangeable optics, its cryogenic implementation together with the modular opto-mechanical configuration of the cryo-mechanisms and the cryo-vacuum cooling system, which consists of a continuous LN2 flow cryostat.
The GeMS/GSAOI pair has been in regular science operation since 2013 at the Gemini South telescope and regularly delivers close to diffraction limited imaging in the NIR bands over a wide field of view of 85" square. Although the original GeMS/GSAOI science cases intentionally did not specify any astrometric performance, the Gemini users community expressed a large interest into using it with this purpose. Both instruments are subject to gravity-induced flexures. GSAOI is often dismounted from the telescope in instrument exchanges, making a regular on-sky calibration strategy time prohibitive. In 2017, we installed a new GeMS calibration focal plane
mask offering ~1600 pinhole sources with a position accuracy of ±25 μm equivalent to ±0.4 mas, which can be used to deliver distortion calibration. We evaluate the flexure effect in the GeMS/GSAOI pair and discuss how to
facilitate the mask to calibrate intra-night distortion drifts.
Sodium guide star technologies for Adaptive Optics (AO) have been around for over 20 years. During this time, the technologies for the lasers used to excite the mesospheric sodium have been in constant development, with the goals being not only to excite as much sodium as possible, but to do so efficiently, while producing a round guide star, and while offering a reliable facility. The first lasers in use were dye lasers with a liquid gain medium, while these lasers were able to produce sodium guide stars, the liquid dye used was toxic and flammable. The second generation of guide star lasers used sum-frequency-mixed solid-state lasers. These lasers provided excellent return but were notoriously difficult to calibrate and maintain, requiring a full-time laser engineer on staff. The current third generation of sodium guide star lasers use Raman fiber amplification to generate a laser that is very efficient at exciting sodium with a good spot profile and offer a high degree of reliability. The Gemini South observatory for the last few years has been in the process of obtaining one of these third-generation lasers, a Toptica Sodium Star 20/2 while maintaining its second-generation Lockheed Martin Coherent Technologies (LMCT) 50W CW Mode-locked laser. In October of 2017 successful on-sky commissioning of the Toptica laser was executed while the LMCT laser was still active and in operations. During the course of the commissioning run both lasers were used on sky in close in time in possible. We present a comparative study of the performance of each laser.
Adaptive Optics (AO) systems aim at detecting and correcting for optical distortions induced by atmospheric turbulences. The Gemini Multi Conjugated AO System GeMS is operational and regularly used for science observations since 2013 delivering close to diffraction limit resolution over a large field of view. GeMS entered this year into a new era. The laser system has been upgraded from the old 50W Lockheed Martin Coherent Technologies (LMCT) pulsed laser to the Toptica 20/2W CW SodiumStar laser. The laser has been successfully commissioned and is now used regularly in operation. In this paper we first review the performance obtained with the instrument. I will go then into the details of the commissioning of the Toptica laser and show the improvements obtained in term of acquisition, stability, reliability and performance.
AO systems aim at detecting and correcting for optical distortions induced by atmospheric turbulences. They are also extremely sensitive to extraneous sources of perturbation such as vibrations, which degrade the performance. The Gemini South telescope has currently two main AO systems: the Gemini Multi Conjugated AO System GeMS and the Gemini Planet Imager GPI. GeMS is operational and regularly used for science observation delivering close to diffraction limit resolution over a large field of view (85×85 arcsec2). Performance limitation due to the use of an integrator for tip-tilt control is here explored. In particular, this type of controller does not allow for the mitigation of vibrations with an arbitrary natural frequency. We have thus implemented a tip-tilt Linear Quadratic Gaussian (LQG) controller with different underlying perturbation models: (i) a sum of autoregressive models of order 2 identified from an estimated power spectrum density (s-AR2) of the perturbation,1 already tested on CANARY2 and routinely used on SPHERE;3 (ii) cascaded ARMA models of order 2 identified using prediction error minimization (c-PEM) as proposed in.4, 5 Both s-AR2 and c-PEM were parameterized to produce tip or tilt state-space models up to order 20 and 30 respectively. We discuss the parallelized implementation in the real time computer and the expected performance. On-sky tests are scheduled during the November 2016 run or the January 2017 run.
ELTs equipped with MCAO systems will be powerful astrometric tools in the next two decades. With sparse-field precisions exceeding 30 uas for V > 18, the ELTs will surpass even GAIA's per-epoch precision for faint stars (V > 12). We present results from an ongoing astrometry program with Gemini GeMS and discuss synergies with WFIRST and GAIA. First, we present a fit to the relative orbit of the individual L/T components of Luhman16 AB, the nearest brown dwarf binary known. Exploiting GeMS' wide field of view to image reference stars, we are able to track the relative motion to better than 0.2 mas. We find that a mutual Keplerian orbit with no perturbing planets fits the binary separation to within the measurement errors, ruling out companions down to 14 earth masses for certain orbits and periods.
AutoCAD, Zemax Optic Studio 15, and Interactive Data Language (IDL) with the Proper Library are used to computationally model and test a diffractive mask (DiM) suitable for use in the Gemini Multi-Conjugate Adaptive Optics System (GeMS) on the Gemini South Telescope. Systematic errors in telescope imagery are produced when the light travels through the adaptive optics system of the telescope. DiM is a transparent, flat optic with a pattern of miniscule dots lithographically applied to it. It is added ahead of the adaptive optics system in the telescope in order to produce diffraction spots that will encode systematic errors in the optics after it. Once these errors are encoded, they can be corrected for. DiM will allow for more accurate measurements in astrometry and thus improve exoplanet detection. The mechanics and physical attributes of the DiM are modeled in AutoCAD. Zemax models the ray propagation of point sources of light through the telescope. IDL and Proper simulate the wavefront and image results of the telescope. Aberrations are added to the Zemax and IDL models to test how the diffraction spots from the DiM change in the final images. Based on the Zemax and IDL results, the diffraction spots are able to encode the systematic aberrations.
GeMS, the Gemini South MCAO System, has now been in operation for 3 years with the near infrared imager GSAOI. We first review the performance obtained by the system, the science cases and the current operational model. In the very near future, GeMS will undergo a profound metamorphosis, as we will integrate a new NGS wavefront sensor, replace the current 50W laser with a more robust one and prepare for a new operational model where operations will shift from the mountain to the base facility. Along this major evolution, we are also presenting several improvements on the loop control, calibrations and automatization of this complex system. We discuss here the progress of the different upgrades and what we expect in terms of performance improvements and operational efficiency.
NGS2 is an upgrade for the multi-natural guide star tip-tilt & plate scale wavefront sensor for GeMS (Gemini Multi-Conjugate Adaptive Optics system). It uses a single Nüvü HNü-512 Electron-Multiplied CCD array that spans the entire GeMS wavefront sensor focal plane. Multiple small regions-of-interest are used to enable frame rates up to 800Hz. This set up will improve the optical throughput with respect to the current wavefront sensor, as well as streamline acquisition and allow for distortion compensation.
The Beam Transfer Optics (BTO) is a sub-system of the Gemini Multi-Conjugate Adaptive Optics System (GeMS). The main purpose of the BTO is to relay the laser light from the laser service enclosure up to the Laser Launch Telescope (LLT), located behind the telescope secondary mirror, where the five laser beams are propagated to the sky. Other functionalities besides relaying the laser light from the laser to the LLT, is the laser polarization control, which is crucial to any AO related system. The polarization state of the laser output beam influences the photon return flux. It is proven that the backscattering efficiency is higher when exciting the sodium layer with a circular polarized beam than one with linear polarization. For this reason circular polarization of our five laser beams that exit the LLT is desired for any telescope position. The paper reviews the current status of the Gemini South Beam Transfer Optics polarization and its control scheme. It reports on the improvements already done on the polarization control and measurement data of the polarization state at different BTO sections. In addition we discuss further optimization and upgrade ideas of the system.
Multiple sodium laser beacons are a crucial development in multi-conjugate adaptive optics systems that offers wide-field diffraction limited adaptive optics correction to the astronomical community. This correction is strongly dependent on the laser beam power and quality, so a beam shaping concept is currently being developed to speed-up calibration and alignment of the laser before every run. A method previously reported, has now been implemented on a laboratory bench using MEMS deformable mirrors. Necessary calibration and characterization of the deformable mirrors are described and the results for experimental amplitude correction are presented.
The Gemini Multi-conjugate adaptive optics System (GeMS) at the Gemini South telescope in Cerro Pachon is the first sodium Laser Guide Star (LGS) adaptive optics (AO) system with multiple guide stars. It uses five LGSs and two deformable mirrors (DMs) to measure and compensate for distortions induced by atmospheric turbulence. After its 2012 commissioning phase, it is now transitioning into regular operations. Although GeMS has unique scientific capabilities, it remains a challenging instrument to maintain, operate and upgrade. In this paper, we summarize the latest news and results. First, we describe the engineering work done this past year, mostly during our last instrument shutdown in 2013 austral winter, covering many subsystems: an erroneous reconjugation of the Laser guide star wavefront sensor, the correction of focus field distortion for the natural guide star wavefront sensor and engineering changes dealing with our laser and its beam transfer optics. We also describe our revamped software, developed to integrate the instrument into the Gemini operational model, and the new optimization procedures aiming to reduce GeMS time overheads. Significant software improvements were achieved on the acquisition of natural guide stars by our natural guide star wavefront sensor, on the automation of tip-tilt and higher-order loop optimization, and on the tomographic non-common path aberration compensation. We then go through the current operational scheme and present the plan for the next years. We offered 38 nights in our last semester. We review the current system efficiency in term of raw performance, completed programs and time overheads. We also present our current efforts to merge GeMS into the Gemini base facility project, where night operations are all reliably driven from our La Serena headquarter, without the need for any spotter. Finally we present the plan for the future upgrades, mostly dedicated toward improving the performance and reliability of the system. Our first upgrade called NGS2, a project lead by the Australian National University, based a focal plane camera will replace the current low throughput natural guide wavefront sensor. On a longer term, we are also planning the (re-)integration of our third deformable mirror, lost during the early phase of commissioning. Early plans to improve the reliability of our laser will be presented.
We measure the long-term systematic component of the astrometric error in the GeMS MCAO system as a function of field radius and Ks magnitude. The experiment uses two epochs of observations of NGC 1851 separated by one month. The systematic component is estimated for each of three field of view cases (15'' radius, 30'' radius, and full field) and each of three distortion correction schemes: 8 DOF/chip + local distortion correction (LDC), 8 DOF/chip with no LDC, and 4 DOF/chip with no LDC. For bright, unsaturated stars with 13 < Ks < 16, the systematic component is < 0.2, 0.3, and 0.4 mas, respectively, for the 15'' radius, 30'' radius, and full field cases, provided that an 8 DOF/chip distortion correction with LDC (for the full-field case) is used to correct distortions. An 8 DOF/chip distortion-correction model always outperforms a 4 DOF/chip model, at all field positions and magnitudes and for all field-of-view cases, indicating the presence of high-order distortion changes. Given the order of the models needed to correct these distortions (~8 DOF/chip or 32 degrees of freedom total), it is expected that at least 25 stars per square arcminute would be needed to keep systematic errors at less than 0.3 milliarcseconds for multi-year programs. We also estimate the short-term astrometric precision of the newly upgraded Shane AO system with undithered M92 observations. Using a 6-parameter linear transformation to register images, the system delivers ~0.3 mas astrometric error over short-term observations of 2-3 minutes.
During the 2012 commissioning of the Gemini MCAO System (GeMS) in Gemini South Observatory, we briefly explored the performance improvement brought by pairing GeMS with the Gemini Multi-Object Spectrograph (GMOS), compared to GMOS in natural seeing mode. GMOS is an instrument sensitive in the visible band with imaging and spectroscopic capabilities, hence pushing MCAO toward the visible, a mode for which it was not specifically designed.
We report in this paper the first results obtained with the GeMS +GMOS pair. Several globular clusters were observed in imaging mode only. We have derived performance in term of FWHM and determined the improvement against natural seeing. We also obtain photometric, relative and absolute astrometric precision for the AO enhanced images. We also studied the influence of the NGS constellation on the photometric performance.
Finally, we also looked at the expected performance of the GeMS+GMOS system once the CCD upgrade, scheduled during 2014, will occur.
The Subaru adaptive optics system (AO188) is a 188-element curvature sensor adaptive optics system that is operated in both natural and laser guide star modes. AO188 is installed at Nasmyth platform of the 8m Subaru telescope as a facility AO system. The laser guide star mode for AO188 has been commissioned and offered for use in science operation since 2011. The performance of AO188 in the laser guide star mode has been well verified from on-sky data obtained with the infrared camera and spectrograph (IRCS). In this paper, we describe the operation procedure and observing efficiency for the laser guide star mode. We also show the result of the on-sky performance evaluation of AO188 in the laser guide star mode and the characterization of the laser guide star, together with the obtained science results.
In 2009 our group started the integration of the SCExAO project, a highly flexible, open platform for high
contrast imaging at the highest angular resolution, inserted between the coronagraphic imaging camera HiCIAO
and the 188-actuator AO system of Subaru. In its first version, SCExAO combines a MEMS-based wavefront
control system feeding a high performance PIAA-based coronagraph. This paper presents some of the images
obtained during the first engineering observations conducted with SCExAO in 2011: diffraction limited imaging
in the visible as well as PIAA coronagraphy in the near infrared; along with the wavefront control strategies to
be tested on sky during the next round of SCExAO observations, scheduled in the Fall 2012.
In this paper we explain why a non-linear curvature wavefront sensor (nlCWFS) is more sensitive
than conventional wavefront sensors such as the Shack Hartmann wavefront sensor (SHWFS) and
the conventional curvature wavefront sensor (cCWFS) for sensing mV < 14 natural guide stars.
The non-linear approach builds on the successful curvature wavefront sensing concept but uses a
non-linear Gerchberg-Saxton (GS) phase diversity algorithm to reconstruct the wavefront. The nonlinear
reconstruction algorithm is an advantage for sensitivity but a challenge for fast computation.
The current speed is a factor of 10 to 100 times slower than needed for high performance groundbased
AO. We present a two step strategy to increase the speed of the algorithm. In the last
paper3 we presented laboratory results obtained with a monochromatic source, here we extend our
experiment to incorporate a broadband source. The sensitivity of the nlCWFS depends on the
ability to extract wavefront phase from diffraction limited speckles therefore it is essential that
the speckles do not suffer from chromatic aberration when used with a polychromatic source. We
discuss the design for the chromatic re-imaging optics, which through chromatic compensation,
allow us to obtain diffraction limited speckles in Fresnel propagated planes on either side of the
pupil plane.
The Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) system uses advanced coronagraphic technique
for high contrast imaging of exoplanets and disks as close as 1 lambda/D from the host star. In addition
to unusual optics, achieving high contrast at this small angular separation requires a wavefront sensing and
control architecture which is optimized for exquisite control and calibration of low order aberrations. The
SCExAO system was thus designed to include the wavefront sensors required for bias-free high sensitivity and
high speed wavefront measurements. Information is combined from two infrared wavefront sensors and a fast
visible wavefront sensors to drive a single MEMS type deformable mirror mounted on a tip-tilt mount. The
wavefront sensing and control architecture is highly integrated with the coronagraph system.
The Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) system is an instrument designed to be inserted
between the Subaru AO188 system and the infrared HiCIAO camera in order to greatly improve the contrast in
the very close (less than 0.5") neighbourhood of stars.Next to the infrared coronagraphic path, a visible scientific
path, based on a EMCCD camera, has been implemented. Benefiting from both AO correction and new data
processing techniques, it is a powerful tool for high angular resolution imaging and opens numerous new science
opportunities. A factor 2 to 3 in Strehl ratio is obtained compared to the AO long exposure time: up to 25% Strehl
in the 650nm wavelength, depending on the image processing algorithm used and the seeing conditions. The
system is able to deliver diffraction limited images at 650 nm (17 mas FWHM). Our baseline image processing
algorithm is based on the selection of the best signal for each spatial frequency. We demonstrate that this
approach offers significantly better results than the classical select, shift and add approach (lucky imaging).
In 2009 our group started the integration of the SCExAO project, a highly flexible, open platform for high
contrast imaging at the highest angular resolution, inserted between the coronagraphic imaging camera HiCIAO
and the 188-actuator AO system of Subaru. In its first version, SCExAO combines a MEMS-based wavefront
control system feeding a high performance PIAA-based coronagraph. It also includes a coronagraphic low-order
wavefront sensor, a non-redundant aperture mask and a visible imaging mode, all of them designed to take full
advantage of the angular resolution that an 8-meter telescope has to offer. SCExAO is currently undergoing
commissioning, and this paper presents the first on-sky results acquired in August 2011, using together Subaru's
AO system, SCExAO and HiCIAO.
The Subaru laser guide star adaptive optics system (AO188) was installed at the Nasmyth focus of the Subaru
Telescope on October 2006 and it is in operation with the natural guide star (NGS) mode. The operation of
the laser guide star (LGS) mode started on January 2010. A visible low-order wavefront sensor (LOWFS) was
built to measure tip-tilt and defocus terms of wavefront by using a single NGS within a 2.7 arcmin diameter field
when an LGS is used for high-order wavefront sensing with the 188-element curvature based wavefront sensor.
This LOWFS is a 2 × 2 sub-aperture Shack-Hartmann sensor with 16 photon-counting avalanche photodiode
(APD) modules. A 4×4-element lenslet array is located after the 2 × 2 sub-aperture Shack-Hartmann lenslet
array and it is coupled with the APD modules through optical fibers. The field of view of the LOWFS is 4 arcsec
in diameter. It has own guide star acquisition unit, acquisition and pupil cameras, and atmospheric dispersion
corrector. We describe the design, construction, and integration of this low-order wavefront sensor.
KEYWORDS: Telescopes, Mirrors, Adaptive optics, Telecommunications, Secondary tip-tilt mirrors, Infrared telescopes, Digital signal processing, Control systems, Infrared radiation, Data conversion
A tip/tilt off-load function from AO188 deformable mirror mount to Subaru telescope infrared secondary mirror
has been implemented and tested. The function is effective to reduce the influence of strong background pattern
at thermal infrared wavelengths. We describe the function and report the test results in this paper.
The Subaru Coronagraphic Extreme Adaptive Optics (SCExAO) system is an instrument designed to be inserted
between the Subaru AO188 system and the infrared HiCIAO camera in order to greatly improve the contrast
in the very close (less than 0.5") neighbourhood of stars. Next to the infrared coronagraphic path, a visible
scientific path, based on a EMCCD camera, has been implemented. Benefiting from both Adaptive Optics (AO)
correction and new data processing techniques, it is a powerful tool for high angular resolution imaging and
opens numerous new science opportunities. We propose here a new image processing algorithm, based on the
selection of the best signal for each spatial frequency. A factor 2 to 3 in Strehl ratio is obtained compared to
the AO long exposure time depending on the image processing algorithm used and the seeing conditions. The
system is able to deliver diffraction limited images at 650 nm (17 mas FWHM).We also demonstrate that this
approach offers significantly better results than the classical select, shift and add approach (lucky imaging).
Subaru adaptive optics system (AO188) is an 188-elements curvature sensor adaptive optics system that is operated
in both natural and laser guide star modes. AO188 was installed at Nasmyth platform of the Subaru
telescope and it has been successfully operating in the natural guide star mode since October 2008. The performance
of AO188 in the natural guide star mode has been well verified from on-sky data obtained with the infrared
camera and spectrograph (IRCS). Under normal seeing condition, AO188 achieves K-band Strehl ratio between
60% and 70% using R = 9.0 magnitude natural guide stars and it works well with faint guide stars down to
R = 16.5 magnitude. We measured the FWHM and Strehl ratio of stellar images in globular clusters and found
that the isoplanatic angle is approximately 30 arcsec. In this paper, we describe an overview of the operation
procedure for AO188, as well as its performance such as angular resolution, Strehl ration, and sensitivity gain
for detecting faint objects.
We are developing a laser guide star (LGS) system for the
188-elements Adaptive Optics system (AO188) of the
Subaru telescope. In this paper we describe the results of the performance tests of the LGS system. The beam
that excites sodium atoms at 90 km altitude of the LGS is generated by the following sequence. The source
of the beam is a quasi-CW mode locked sum-frequency generating 589 nm laser. This laser beam propagates
through a diagnostics system for measuring the wavelength and the beam quality. Then it couples into a solidcore
photonic crystal fiber cable for transmitting the beam to a telescope for launching the beam (LLT: Laser
Launching Telescope). The output beam from this fiber cable is collimated by the optics mounted on the
LLT. This collimated beam is expanded by the LLT and launched into the sky. We executed several engineering
observations of the LGS system from 2009 for confirming the performance of all the components in this sequence.
We also report the quality of the LGS.
We report recent development in real time control system of Subaru adaptive optics system. The main topic is
modification of the real time control system for laser guide star operation. The primary change is appending lower order
wave-front sensor. And also, an auxiliary tip-tilt and focus control are appended before higher order waver-front sensor
to absorb the perturbation of the laser beam and height of sodium layer. Our implementations using the control gain
matrix are introduced thoroughly from the basis of the system design and down to the details. Also, other new function
and prospects in the near future will be presented for the cascaded average monitor and the time domain over sampling.
The Subaru Coronagraphic Extreme AO project (SCExAO) is a high performance coronagraph designed to
deliver high contrast at small angular separation. For the detection of structures near the diffraction limit, an
accurate control of low order wavefront aberrations - tip-tilt and focus - is essential as these aberrations create
light leaks that are the source of confusion in the final science image. To address this major difficulty, we have
equipped SCExAO with a specially designed Coronagraphic Low Order WaveFront Sensor (CLOWFS) using
defocused images of a reflective ring located in the focal plane, that can track tip-tilt errors as small as 10-3λ/D.
CLOWFS was originally designed to drive actuators in a closed-loop. Here, we show that it can also be used in
post-processing to efficiently subtract the tip-tilt induced coronagraphic leaks in the final science image.
The current status of commissioning and recent results in performance of Subaru laser guide star adaptive optics
system is presented. After the first light using natural guide stars with limited configuration of the system in
October 2006, we concentrated to complete a final configuration for a natural guide star to serve AO188 to an
open use observation. On sky test with full configurations using natural guide star started in August 2008, and
opened to a public one month later. We continuously achieved around 0.6 to 0.7 of Strehl ratio at K band using
a bright guide star around 9th to 10th magnitude in R band. We found an unexpectedly large wavefront error
in our laser launching telescope. The modification to fix this large wavefront error was made and we resumed
the characterization of a laser guide star in February 2009. Finally we obtained a round-shaped laser guide star,
whose image size is about 1.2 to 1.6 arcsec under the typical seeing condition. We are in the final phase of
commissioning. A diffraction limited image by our AO system using a laser guide star will be obtained in the
end of 2010. An open use observation with laser guide star system will start in the middle of 2011.
In this paper we show why a non-linear curvature wavefront sensor (nlCWFS) is superior to both
Shack-Hartmann wavefront sensor (SHWFS) and conventional curvature wavefront sensor (cCWFS)
for sensing mV < 15 natural guide stars. We have developed an experimental setup aimed at
comparing the the rms wavefront error obtained with the nlCWFS and the SHWFS. We describe
our experimental setup and present results from the laboratory demonstration of the nlCWFS. The
non-linear approach builds on the successful curvature wavefront sensing concept. The wavefront
is reconstructed from the defocused pupil images using the
Gerchberg-Saxton (GS) phase diversity
algorithm. We compare results obtained from reconstructing the wavefront using a Shack-Hartmann
wavefront sensor (SHWFS) and a nlCWFS for a monochromatic source. We discuss approaches
to overcome non-linearity issues and discuss the challenge of using two WFSs in the same spatiotemporal
control regime and the implementation of the nlCWFS on the 6.5 m MMT.
The image derotator is an integral part of the AO188 System at Subaru Telescope. In this article software control,
characterization and integration issues of the image derotator for AO188 System presented. Physical limitations of the
current hardware reviewed. Image derotator synchronization, tracking accuracy, and problem solving strategies to
achieve requirements presented. It's use in different observation modes for various instruments and interaction with the
telescope control system provides status and control functionality. We describe available observation modes along with
integration issues. Technical solutions with results of the image derotator performance presented. Further improvements
and control software for on-sky observations discussed based on the results obtained during engineering observations.
An overview of the requirements, the final control method, and the structure of its control software is shown. Control
limitations and accepted solutions that might be useful for development of other instrument's image derotators presented.
An eight-octant phase-mask (EOPM) coronagraph is one of the highest performance coronagraphic concepts, and attains
simultaneously high throughput, small inner working angle, and large discovery space. However, its application to
ground-based telescopes such as the Subaru Telescope is challenging due to pupil geometry (thick spider vanes and large
central obstruction) and residual tip-tilt errors. We show that the Subaru Coronagraphic Extreme Adaptive Optics
(SCExAO) system, scheduled to be installed onto the Subaru Telescope, includes key technologies which can solve these
problems. SCExAO uses a spider removal plate which translates four parts of the pupil with tilted plane parallel plates.
The pupil central obstruction can be removed by a pupil remapping system similar to the PIAA optics already in the
SCExAO system, which could be redesigned with no amplitude apodization. The EOPM is inserted in the focal plane to
divide a stellar image into eight-octant regions, and introduces a π-phase difference between adjacent octants. This
causes a self-destructive interference inside the pupil area on a following reimaged pupil plane. By using a reflective
mask instead of a conventional opaque Lyot stop, the stellar light diffracted outside the pupil can be used for a
coronagraphic low-order wave-front sensor to accurately measure and correct tip-tilt errors. A modified inverse-PIAA
system, located behind the reimaged pupil plane, is used to remove off-axis aberrations and deliver a wide field of view.
We show that this EOPM coronagraph architecture enables high contrast imaging at small working angle on the Subaru
Telescope. Our approach could be generalized to other phase-mask type coronagraphs and other ground-based telescopes.
The Subaru Coronagraphic Extreme-AO (SCExAO) system is designed for high contrast coronagraphic imaging at small angular separations, and is scheduled to see first light on the Subaru Telescope in early 2011. The wavefront control architecture for SCExAO is optimized for scattered light control and calibration at small angular separations, and is described in this paper. Key subsystems for the SCExAO wavefront control architecture have been successfully demonstrated, and we report results from these tests and discuss their role in the SCExAO system. Among these subsystems, a technique which can calibrate and remove static and slow speckles which traditionally limit high contrast detections is discussed. A visible light lab prototype system at Subaru Telescope recently demonstrated speckle halo reduction to 2e-7 contrast within 2 2λ/D, and removal of static coherent speckles to 3e-9 contrast.
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