We are carrying out a 1.8-m aperture off-axis telescope project PLANETS. The PLANETS telescope is characterized by using an off-axis mirror to enable us high-contrast imaging and spectroscopy with low-scattering in the optical system. Our major scientific goal is to observe faint emission around a bright body, such as gases surrounding planets and satellites in the solar system (e.g., Jovian satellite Europa’s water plume) as well as exoplanets. Using a new technology of mirror polishing with a robot arm and 3-point drag probe, we performed the polishing of the off-axis primary mirror. We also developed the whiffletree support with warping harness for the primary mirror support. We will assemble the whole PLANETS telescope system and conduct the first light of stars as technical demonstration in Japan within a year. We have begun coordinating with several high-altitude observatory sites in which the PLANETS telescope will be installed after the technical demonstration in Japan.
KEYWORDS: Tunable filters, Feedback control, Control systems, Digital signal processing, Electronic filtering, Repetition frequency, Signal processing, Mirrors
In ground-based mid-infrared observations the background radiation must be removed. Chopping is a background removal method requiring fast switching of the observation field. For MIMIZUKU, the mid-infrared instrument for the TAO telescope, we have developed a cold chopper which switches the observing field by tilting a movable mirror inside MIMIZUKU, instead of tilting the large secondary mirror.
We require a short transition time, sufficient amplitude, high frequency and steadyness for observation in the chopper movement.
With Repetitive Control we significantly increase performance by iteratively improving a feedforward trajectory and continously adapting to changes in the nonlinear dynamics.
This allows for much shorter transition time (<30 ms) and more freedom in the design of a feedback controller. Furthermore, repetitive disturbances originating from the cryo-cooler can be countered thus improving stability on sky.
Controller design, stabilisation, choice of reference trajectory, real-time computability and performance trade-offs are subjects in this research.
MIMIZUKU, the mid-infrared instrument for the 6.5-m telescope at the University of Tokyo Atacama Observatory (TAO), employs a cold chopper to perform chopping, which tilts a mirror placed on the internal cold optics at about 30 K. The mirror rotates around two orthogonal axes, and its tilt angle is controlled by the balance between the restoring force of the flexural pivots and the magnetic force driven by the coils in the system. In this study, we developed a final-product model of the chopper and tested its onboard performance in MIMIZUKU. This experiment showed that the mirror could be operated with a stability of 3.83×10−4 and 3.29×10−4 degrees, and a transition time of 31.2 and 32.2 milliseconds for each rotation, when both rotations were driven at 5 Hz with an amplitude of 0.59 degrees, satisfying the performance requirements.
JAXA recently selected LAPYUTA (Life-environmentology, Astronomy, and PlanetarY Ultraviolet Telescope Assembly) as a candidate for JAXA's Small Scale Program No. 6 to be launched by Epsilon in ~2032. We will accomplish the following four objectives: #1 Solar System, #2 Exoplanets, #3 Galaxies, #4 the origin of heavy elements. To achieve these scientific objectives, LAPYUTA aims to carry out spectroscopy with a large effective area (>300 cm2) and a high spatial resolution (0.1 arc-sec) and imaging in far ultraviolet spectral range (110-190 nm). A high dispersion spectrograph with a spectral resolution of > 40000 is required, especially for observing exospheres of terrestrial (Earth-like) exoplanets. We are considering the design of the Spectrograph with High dispersion Echelle grating for the Terrestrial (exo-)planetary Atmosphere (SHETA) as an instrument. In this presentation, we introduce the scientific objective and the conceptual design of the SHETA instrument.
Ultraviolet (UV) spectroscopy is one of the most powerful tools used in a wide range of scientific fields from planetary science to astronomy. We propose a future UV space telescope, LAPYUTA (Life-environmentology, Astronomy, and PlanetarY Ultraviolet Telescope Assembly), selected as a candidate for JAXA’s 6th M-class mission in 2023. Launch is planned for the early 2030s. LAPYUTA will accomplish the following four objectives related to two scientific goals: understanding (1) the habitable environment and (2) the origin of structure and matter in the universe. Objective 1 focuses on the subsurface ocean environments of Jupiter's icy moons and the atmospheric evolution of terrestrial planets. Objective 2 characterizes the atmosphere of the exoplanets around the habitable zone and estimates their surface environment by detecting their exospheric atmosphere. In cosmology and astronomy, Objective 3 tests whether the structures of presentday galaxies contain ubiquitous Ly-α halos and reveals the physical origins of Ly-α halos. Objective 4 elucidates the synthesis process of heavy elements based on observations of ultraviolet radiation from hot gas immediately after neutronstar mergers. LAPYUTA will perform spectroscopic and imaging observations in the far-UV range of 110-190 nm with an effective area of >300 cm2 and a high spatial resolution of 0.1 arcsec. The apogee is 2,000 km, and the perigee is 1,000 km to avoid the influence of the geocorona when observing oxygen and hydrogen atoms and the Earth's radiation belt.
We present a comparative study of optical designs of ultraviolet (UV) spectrometers onboard spaceborne telescopes. Such spectrometers provide unique findings for the space sciences that cannot be obtained via ground-based observation due to the atmospheric opacity in this wavelength region. Instruments for observing in the UV wavelength range should have as few reflective surfaces as possible to maintain a high throughput. For instance, the Hisaki spectrometer uses simple optics, consisting of only one toroidal grating. However, in this case, the spot qualities produced by optics onto detectors have room for improvement. In this study, we present several optical designs with improved spot qualities by adding one or a few reflective surfaces, and compare them. We also discuss optical designs that is potentially useful for the proposed Life-environmentology, Astronomy, and Planetary Ultraviolet Telescope Assembly (LAPYUTA) mission.
We have developed a new coronagraph using digital micromirror device (DMD) to observe faint emissions close to a bright objects in our solar system such as water plumes on Europa and Enceladus, plasma emissions in giant planet’s magnetospheres, escaping plasma and neutrals from Venus and Mars, and so on. The focal plane DMD mask enables us to occult planet’s disks and their moons even when their angular dimeter and geometry vary with time. The coronagraph composed of a DMD as an occulting mask on a telescope focal plane, a pupil stop, a narrow-band filter, and others. The DMD located at the focal plane produces color dispersion of entrance aperture on a pupil plane for an extended lightsource. Thus, we designed a proper shape of pupil mask to reduce remaining from the occulted light-source considering wavelength and bandwidth of observations. The coronagraph was installed on a Cassegrain focus of the Tohoku 60-cm telescope at Haleakala observatory in Hawaii. We have been using the coronagraph for observing sulfur ion emissions [SII] 671.6 and 673.1 nm from Io plasma torus since 2018. The DMD occultation reduces light from Jupiter disk and Galilean moons by 2.6×10-3. The system throughput is 56 % of a previous conventional coronagraph. In observation of Io plasma torus, north-south position of [SII] brightness peak shifted by 0.07 jovian radii toward the magnetic equator during three days. Increase of flesh pickup ion possibly makes higher anisotropy or higher ion perpendicular temperature causing the observed magnetic-equatorward shift of the plasma torus.
PLANETS will be a 1.8-m off-axis telescope combined with contrast enhancement techniques, enabling us to observe faint emissions in the vicinity of bright objects. This “high dynamic-range” capability is largely dependent upon precision of telescope optics as well as atmospheric distortion. We present feasibility study of monitoring water plumes on Europa, neutral torus close to Enceladus, and ionosphere on Mars using PLANETS telescope. To test feasibility of high dynamic-range observation under actual conditions of wavefront error, we modeled propagation of light though the system based on Fraunhofer calculation taking into account for wavefront error made by atmospheric distortion and by primary mirror figure error. Then point spread function is calculated for several cases of figure errors under use of adaptive optics. The modeling result predicts that the moderate or high-precision primary mirror is mandatory to accomplish the high dynamic-range observation. We also present the latest design of PLANETS, especially focus on the support structures of primary mirror. We employ 36-point whiffletrees with 33 warping harnesses for axial support, and 24-point Schwesinger support for lateral support. The active support system is expected to reduce pre-polished RMS error from 1.51 μm to 0.66 μm corresponding to 70% reduction in total volume of final polish. The laboratory experiment using one third part of prototype whiffletrees shows supporting force RMS repeatability < 0.005 kgf, and drive hysteresis < 0.7% of load range, which are precise enough to control or to keep the primary mirror figure.
We report the current status of small-telescope activities and the 1.8-m aperture telescope PLANETS project at Haleakala dedicated to planetary and exoplanetary observations. Continuous monitoring is essential to understand the planetary atmospheric phenomena, and therefore, own facilities with even small- and medium sized telescopes and instruments are important. On the summit of Mt. Haleakala, Hawaii, we are operating a 40 cm (T40) and 60 cm (T60) telescopes for measuring faint atmospheric features such as Io torus, Mercury, and so on. It has uniquely provided long-term Io torus activities for more than ten years. T60 is now observing planetary atmospheres in visible and infrared ranges. The polarization imager DIPOL-2 is also installed to measure the weak polarization of exoplanetary light. In addition, we are carrying out a 1.8-m off-axis telescope project PLANETS at Haleakala. This project is managed by the PLANETS Foundation (www.planets.life) is an international collaboration of several institutes from Japan, USA, Germany, Brazil, and France. This off-axis optical system enables very low-stray light contamination and high-contrast in data, i.e., "high dynamic range". It will achieve unrivaled scientific capabilities on coronagraphy and polarimetry, aimed at detecting exoplanet reflected light and tenuous planetary exo-atmospheres in the Solar system. The main mirror is Clearceram ZHS with a diameter of 1850 mm, which is now on the final polishing process. We completed the telescope design and wind analysis of the mechanical support and tracking. The "split-ring" mount is so stiff that it has a first vibration mode above 50 Hz.
We report the development of infrared Echelle spectrograph covering 1 - 4 micron and mid-infrared heterodyne
spectrometer around 10 micron installed on the 60-cm telescope at the summit of Haleakala, Hawaii (alt.=3000m). It is
essential to carry out continuous measurement of planetary atmosphere, such as the Jovian infrared aurora and the
volcanoes on Jovian satellite Io, to understand its time and spatial variations. A compact and easy-to-use high resolution
infrared spectrometer provide the good opportunity to investigate these objects continuously. We are developing an
Echelle spectrograph called ESPRIT: Echelle Spectrograph for Planetary Research In Tohoku university. The main
target of ESPRIT is to measure the Jovian H3+ fundamental line at 3.9 micron, and H2 nu=1 at 2.1 micron. The 256x256
pixel CRC463 InSb array is used. An appropriate Echelle grating is selected to optimize at 3.9 micron and 2.1 micron for
the Jovian infrared auroral observations. The pixel scale corresponds to the atmospheric seeing (0.3 arcsec/pixel). This
spectrograph is characterized by a long slit field-of-view of ~ 50 arcsec with a spectral resolution is over 20,000. In
addition, we recently developed a heterodyne spectrometer called MILAHI on the 60 cm telescope. MILAHI is
characterized by super high-resolving power (more than 1,500,000) covering from 7 - 13 microns. Its sensitivity is 2400
K at 9.6 micron with a MCT photo diode detector of which bandwidth of 3000 MHz. ESPRIT and MILAHI is planned to
be installed on 60 cm telescope is planned in 2014.
The extreme ultraviolet (EUV) telescope EXCEED (Extreme Ultraviolet Spectroscope for Exospheric
Dynamics) onboard the Japan's small satellite SPRINT-A will be launched in August 2013. The EXCEED instrument
will observe tenuous gases and plasmas around the planets in the solar system (e.g., Mercury, Venus, Mars, Jupiter, and
Saturn). The EXCEED instrument is designed to have a spectral range of 60-145 nm with a spectral resolution of 0.4-1.0
nm. The instrument has a field of view of 400” x 140” (maximum), and the attitude fluctuations are stabilized within ±5".
The optics of the instrument consists of an entrance mirror with a diameter of 200 mm, three types of slits, two types of
filters, a laminar type grating, and a 5-stage microchannel plate assembly with a resistive anode encoder. In this paper,
we report the general mission overview, the instrumentations, and the results of ground calibrations.
EXtreme ultraviolet spectrosCope for ExosphEric Dynamics (EXCEED) will carry out the extreme ultraviolet
(EUV) spectroscopic imaging observations from earth orbit. It clarifies the plasma distributions and compositions around
the various planets and examines the interactions with the solar wind. Observations should be carried out at high altitude
so that the earth's atmospheric absorption is free. Our spectral range is from 60 to 145 nm and the spectral resolution is
0.3 to 1 nm (FWHM). The mission is planned to be launched in 2013, beginning of the next period of solar maximum. In
this paper, we will introduce the general mission overview, scientific objectives and development of instrument.
EXtreme ultraviolet spectrosCope for ExosphEric Dynamics (EXCEED) will carry out the extreme ultraviolet
(EUV) spectroscopic imaging observations from earth orbit. It clarifies the plasma distributions and compositions around
the various planets and examines the interactions with the solar wind. Observations should be carried out at high altitude
so that the earth's atmospheric absorption is free. Our spectral range is from 60 to 145 nm and the spectral resolution is
0.2 to 0.5 nm (FWHM). The mission is planned to be launched in 2013, beginning of the next period of solar maximum.
In this paper, we will introduce the general mission overview, scientific objectives and development of instrument.
EXtreme ultraviolet spectrosCope for ExosphEric Dynamics (EXCEED) is the earth-orbiting Extreme
Ultraviolet (EUV) spectroscope mission which dedicates to the planetary space science. Our mission will carry out the
EUV spectroscopic imaging which clarifies the plasma distributions and compositions around the planets and examines
the interaction with the solar wind. Orbital altitude should be enough high so that the earth's atmospheric absorption is
free. The spectral range of the mission is from 60 to 145 nm and the resolution is 0.2 to 0.5 nm FWHM. The mission is
planned to be launched in 2013, beginning of the next period of solar maximum. In this paper, we will introduce the
general mission overview, its instrument and its scientific targets.
EXtreme ultraviolet spectrosCope for ExosphEric Dynamics (EXCEED) is an earth-orbiting space Extreme
Ultraviolet (EUV) telescope mission. The satellite will be launched in 2012 by a Japanese new solid propulsion rocket
and injected into the elliptic orbit around the earth. The orbital altitude is 900 to 1200 km for perigee and apogee
respectively. EXCEED will make EUV spectroscopic and imaging observations of plasma space around various planets
in our solar system. The wavelength range is from 60 to 145 nm and the resolution is 0.2 to 0.5 nm FWHM. It enables us
to study Io plasma torus of Jupiter, and interaction of the solar wind with the upper atmosphere of the terrestrial planets
and their escape. In this paper, we will introduce the mission overview and its instrument especially for holographic
grating which is coated by Chemical vapor deposited silicon carbide.
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