Image quality on the NASA Infrared Telescope Facility (IRTF) is currently limited by telescope-induced aberrations when seeing is good. We have measured telescope image quality as a function of telescope pointing over several recent epochs to quantify these aberrations. Using the measured aberrations and seeing, we “Donut” modeled the expected image quality improvements through applications of the soon-to-be commissioned off-axis Shack-Hartmann (S-H) wavefront sensor and CCD camera, FELIX. The average telescope-induced wavefront error without defocus is 0.7 ± 0.04μm RMS, the largest contributor being astigmatism (∼0.21μm RMS). Uncorrected images would require ∼ 2 times longer integration times to compensate for light loss through seeing-limited slits. Our models indicate that active control of the hexapod-mounted secondary mirror by a 2x2 S-H in FELIX can accurately correct the largest current aberration (defocus). However, a 3x3 S-H is needed to correct higher-order telescope aberrations using the proposed Adaptive Secondary Mirror (ASM).
We performed closed-loop lab testing of large-format deformable mirrors (DMs) with hybrid variable reluctance actuators. TNO has been developing the hybrid variable reluctance actuators in support for a new generation of adaptive secondary mirrors (ASMs), which aim to be more robust and reliable. Compared to the voice coil actuators, this new actuator technology has a higher current to force efficiency, and thus can support DMs with thicker facesheets. Before putting this new technology on-sky, it is necessary to understand how to control it and how it behaves in closed-loop. We performed closed-loop tests with the Shack-Hartmann wavefront sensor with three large-format deformable mirrors that use the TNO actuators: DM3, FLASH, and IRTF-ASM-1 ASM. The wavefront sensor and the real-time control systems were developed for the NASA Infrared Telescope Facility (IRTF) and the UH 2.2-meter telescope ASMs. We tested IRTF-ASM-1 on-sky and proved that it meets all of our performance requirements. This work presents our lab setup for the experiments, the techniques we have employed to drive these new ASMs, the results of our closed-loop lab tests for FLASH and IRTF-ASM-1, and the on-sky closed-loop results of IRTF-ASM-1 ASM.
We are developing an adaptive secondary mirror (ASM) that uses a new actuator technology created by the Netherlands Organization for Applied Scientific Research (TNO). The TNO hybrid variable reluctance actuators have more than an order of magnitude better efficiency over the traditional voice coil actuators that have been used on existing ASMs and show potential for improving the long-term robustness and reliability of ASMs. To demonstrate the performance, operations, and serviceability of TNO’s actuators in an observatory, we have developed a 36-actuator prototype ASM for the NASA Infrared Telescope Facility (IRTF) called IRTF-ASM-1. IRTF-ASM-1 provides the first on-sky demonstration of this approach and will help us evaluate the long-term performance and use of this technology in an astronomical facility environment. We present calibration and performance results with the ASM in a Meniscus Hindle Sphere lens setup as well as preliminary on-sky results on IRTF. IRTF-ASM-1 achieved stable closed-loop performance on-sky with H-band Strehl ratios of 35-40% in long-exposure images under a variety of seeing conditions.
TNO and partners at University of Hawai’i (UH), the NASA InfraRed Telescope Facility (IRTF), and the Center for Adaptive Optics (CfAO) at UCSC have been working on the realization of a 244 mm Adaptive Secondary Mirror (ASM) for the NASA IRTF called the IRTF-ASM-1. After successful performance testing of several laboratory prototypes, this project provided the first on-sky demonstration of TNO’s ASM technology at M2 location with an optically powered mirror shell.
The ASM is designed to retrofit the current passive M2. The ASM consists of a 244mm-diameter slumped convex aspherical mirror shell, manipulated by 36 hybrid variable reluctance actuators mounted on a light-weighted backing structure. The mirror shell is manufactured to the required accuracy at reduced cost through slumping by UCSC. The mirror shell is finished to final figure with Magnetorheological Finishing (MRF) by TNO before it was coated.
The ASM was shipped to UH in Hilo in February 2024, where performance was tested in the lab. The IRTF ASM saw ‘first light’ on telescope on the 23rd of April, already achieving stable closed-loop performance that was diffraction limited at the H-band (1.62 microns) with a long-exposure Strehl ratio of 35%-40% in sub-arcsecond seeing during the first night.
This paper will report on the status and first results of the IRTF ASM, including the latest status of the deformable mirror technology at TNO and an outlook to a second generation IRTF ASM with improved dynamic performance and increased actuator count.
SPECTRE is a proposed 0.4-4.2 µm low-resolution spectrograph being developed for the NASA Infrared Telescope Facility. Dispersion is accomplished using prisms to optimize throughput, resulting in a mean resolving power of R=160. SPECTRE has an image-slicer integral field unit with a 7.2′′ field of view to remove slit losses, reduce mechanical complexity, and enable precision spectrophotometry. Dichroics are used to divide the light into three spectroscopic channels, each with optimized optics and its own detector. We will use a 2K frame transfer CCD for the optical channel, and an H2RG in each of the two infrared channels. SPECTRE is a single mode instrument: there are no moving optics and the spectral format is fixed, making for a simple and rigid instrument. Guiding will be done by a co-mounted visible light camera with a 3′ field of view.
‘Opihi is a 0.43 m, 32′ field of view (FOV) finder scope that rides along with the NASA Infrared Telescope Facility (IRTF), a 3.2 m infrared-optimized telescope near the summit of Mauna Kea, Hawai‘i. The main purpose of ‘Opihi is to recover Near-Earth Objects (NEOs) with positional uncertainties larger than can feasibly be found with the 1 ′ FOV of IRTF. Automated data collection with ‘Opihi will be useful for bootstrap photometry and can provide general context observing images. We present the design and commissioning process for ‘Opihi, including its photometric performance and first asteroid detection results
We are building a next-generation laser adaptive optics system, Robo-AO-2, for the UH 2.2-m telescope that will deliver robotic, diffraction-limited observations at visible and near-infrared wavelengths in unprecedented numbers. The superior Maunakea observing site, expanded spectral range and rapid response to high-priority events represent a significant advance over the prototype. Robo-AO-2 will include a new reconfigurable natural guide star sensor for exquisite wavefront correction on bright targets and the demonstration of potentially transformative hybrid AO techniques that promise to extend the faintness limit on current and future exoplanet adaptive optics systems.
iSHELL is 1.10-5.3 μm high spectral resolution spectrograph being built for the NASA Infrared Telescope Facility on Maunakea, Hawaii. Dispersion is accomplished with a silicon immersion grating in order to keep the instrument small enough to be mounted at the Cassegrain focus of the telescope. The white pupil spectrograph produces resolving powers of up to R=75,000. Cross-dispersing gratings mounted in a tilt-able mechanism allow observers to select different wavelength ranges and, in combination with a slit wheel and Dekker mechanism, slit lengths ranging from 5ʺ″ to 25ʺ″. One Teledyne 2048x2048 Hawaii 2RG array is used in the spectrograph, and one Raytheon 512x512 Aladdin 2 array is used in a slit viewer for object acquisition and guiding. First light is expected in mid-2016. In this paper we discuss details of the construction, assembly and laboratory testing.
The prototype Robo-AO system at the Palomar Observatory 1.5-m telescope is the world's first fully automated laser adaptive optics instrument. Scientific operations commenced in June 2012 and more than 12,000 observations have since been performed at the ~0.12" visible-light diffraction limit. Two new infrared cameras providing high-speed tip-tilt sensing and a 2' field-of-view will be integrated in 2014. In addition to a Robo-AO clone for the 2-m IGO and the natural guide star variant KAPAO at the 1-m Table Mountain telescope, a second generation of facility-class Robo-AO systems are in development for the 2.2-m University of Hawai'i and 3-m IRTF telescopes which will provide higher Strehl ratios, sharper imaging, ~0.07", and correction to λ = 400 nm.
Direct imaging of extrasolar planets in visible light, and Earth-like planets in particular, is an exciting but difficult problem requiring a telescope imaging system with 10-10 contrast at separations of 100mas and less. Furthermore, only a small 1-2m space telescope may be realistic for a mission in the foreseeable future, which puts strong demands on the performance of the imaging instrument. Fortunately, an efficient coronagraph called the Phase Induced Amplitude Apodization (PIAA) coronagraph may enable Earth-like planet imaging for such small telescopes if any exist around the nearest stars. In this paper, we report on the latest results from a testbed at the NASA Ames Research Center focused on testing the PIAA coronagraph. This laboratory facility was built in 2008 and is designed to be flexible, operated in a highly stabilized air environment, and to complement efforts at NASA JPL's High Contrast Imaging Testbed. For our wavefront control we are focusing on using small Micro-Electro-Mechanical-System deformable mirrors (MEMS DMs), which promises to reduce the size of the beam and overall instrument, a consideration that becomes very important for small telescopes. In this paper, we briefly describe our lab and methods, including the new active thermal control system, and report the demonstration of 5.4×10-8 average raw contrast in a dark zone from 2.0 - 5.2 λ/D. In addition, we present an analysis of our current limits and solutions to overcome them.
Direct imaging of extrasolar planets, and Earth-like planets in particular, is an exciting but difficult problem requiring a
telescope imaging system with 1010 contrast at separations of 100mas and less. Furthermore, the current NASA science
budget may only allow for a small 1-2m space telescope for this task, which puts strong demands on the performance of
the imaging instrument. Fortunately, an efficient coronagraph called the Phase Induced Amplitude Apodization (PIAA)
coronagraph has been maturing and may enable Earth-like planet imaging for such small telescopes. In this paper, we
report on the latest results from a new testbed at NASA Ames focused on testing the PIAA coronagraph. This laboratory
facility was built in 2008 and is designed to be flexible, operated in a highly stabilized air environment, and to
complement existing efforts at NASA JPL. For our wavefront control we are focusing on using small Micro-Electro-
Mechanical-System deformable mirrors (MEMS DMs), which promises to reduce the size of the beam and overall
instrument, a consideration that becomes very important for small telescopes. At time of this writing, we are operating a
refractive PIAA system and have achieved contrasts of about 1.2x10-7 in a dark zone from 2.0 to 4.8 λ/D (with 6.6x10-8
in selected regions). In this paper, we present these results, describe our methods, present an analysis of current limiting
factors, and solutions to overcome them.
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