We conducted the evaluation testing of the InGaAs image sensor for the future JASMINE mission. The InGaAs image sensor, which is manufactured by Hamamatsu Photonics K.K., has been updated with substrate removal to avoid fluorescence caused by cosmic rays. We introduce preliminary performance reports of the 128×128 arrayed small prototype at 170K, assuming space use, including dark current and relative quantum efficiency in the near-infrared. Notably, we confirmed that fluorescence is significantly mitigated with an exposure of about 10 minutes. Furthermore, the relative quantum efficiency in the visible wavelength is enhanced compared to previous evaluations in the literature. These results provide a good configuration for the test of the sensor for deployment and play an important role in the future development of infrared astronomical instruments.
Structural, Thermal and Optical Performance (STOP) analysis is performed to investigate the stability of the telescope to be onboard the Japan Astrometry Satellite Mission for INfrared Exploration (JASMINE). In order to perform one of the prime science objectives, high-precision astrometric observations in the wavelength range of 1.0–1.6 µm toward the Galactic center to reveal its central core structure and formation history, the JASMINE telescope is requested to be highly stable with an orbital change in the image distortion pattern being less than a few 10 µas after low-order correction. The JASMINE telescope tried to satisfy this requirement by adopting two design concepts. Firstly, the mirror and their support structures are made of extremely low coefficientof-thermal-expansion materials. Secondly, their temperatures are highly stabilized with an orbital variation of less the 0.1 ◦C by the unique thermal control idea. Through the preliminary STOP analysis, the structural and thermal structural feasibility of the JASMINE telescope is considered. By combining the results of the structural and thermal design, its thermal deformation is estimated. The optical performance of the JASMINE telescope after the thermal deformation is numerically evaluated. It is found that the thermal displacement of the mirrors in the current structural thermal design produces a slightly large focus-length change. As far as the focus adjustment is adequately applied, the orbital variation of the image distortion pattern is suggested to become acceptable after the low-order correction.
JASMINE is a Japanese near-infrared space mission with the scientific objectives of ultra-high-precision astrometric observations of stars in the central region of the Galaxy and exploration of terrestrial exoplanets around M-type stars. To achieve these scientific objectives, we are developing a 36-cm aperture diffraction-limited telescope with an emphasis on ultra-low stable telescope structure. The telescope will be equipped with an infrared detector and a bandpass filter for the wavelength range of 1000-1600 nm. For the astrometry, the telescope will have a high optical performance: the Strehl ratio larger than 0.9 at near-infrared wavelengths and is required to have a stable image distortion of less than a few tens micro arcsec during a low Earth sun-synchronous orbital motion. The telescope has an axisymmetric Korsch-type optical system which is easy to be designed to have the high optical performance over a large field-of-view. We present the progress of the telescope optics design, optics alignment/adjustment procedures, and telescope optics evaluation and verification procedures.
To investigate the evolution of our Galaxy, we plan to measure the distances and motions of stars in the Galactic center region. Additionally, our goal is to detect planets within the habitable zone around mid-M-type stars using transit phenomena. To achieve these objectives, we initiated the Japan Astrometry Satellite Mission for Infrared Exploration (JASMINE) project, targeting a 40 microarcsecond annual parallax measurement and aiming photometric accuracy of less than 0.3% for mid-M-type stars. A conceptual study of the observation instrument was conducted. As a result, the telescope is designed with high stability in orbit through carefully chosen materials and a special thermal design. A three-year operation is planned to collect sufficient data for annual parallax measurements. The telescope, with a diameter of 36 cm, covers wavelengths from 1.0 to 1.6 microns using InGaAs detectors. This paper will detail how instrument parameters were selected based on scientific objectives.
JASMINE is a Japanese planned space mission that aims to reveal the formation history of our Galaxy and discover habitable exoEarths. For these objectives, the JASMINE satellite performs high-precision astrometric observations of the Galactic bulge and high-precision transit monitoring of M-dwarfs in the near-infrared (1.0—1.6 µm in wavelength). For feasibility studies, we develop an image simulation software named JASMINE-imagesim, which produces realistic observation images. This software takes into account various factors such as the optical point spread function (PSF), telescope jitter caused by the satellite’s attitude control error (ACE), detector flat patterns, exposure timing differences between detector pixels, and various noise factors. As an example, we report a simulation for the feasibility study of astrometric observations using JASMINE-imagesim. The simulation confirms that the required position measurement accuracy of 4 milliarcseconds for a single exposure of 12.5-mag objects is achievable if the telescope pointing jitter uniformly dilutes the PSF across all stars in the field of view. On the other hand, the simulation also demonstrates that the combination of realistic pointing jitter and exposure timing differences in the detector can significantly degrade accuracy and prevent achieving the requirement. This means that certain countermeasures against this issue must be developed. This result implies that this kind of simulation is important for mission planning and advanced developments to realize more realistic simulations help us to identify critical issues and also devise effective solutions.
MIMIZUKU is the first-generation mid-infrared instrument for the TAO 6.5-m telescope. It has three internal optical channels to cover a wide wavelength range from 2 to 38 µm. Of the three channels, the NIR channel is responsible for observations in the shortest wavelength range, shorter than 5.3 µm. The performance of the NIR channel is evaluated in the laboratory. Through the tests, we confirm the followings: 1) the detector (HAWAII 1RG with 5.3-µm cutoff) likely achieves ∼80% quantum efficiency; 2) imaging performance is sufficient to achieve seeing-limit spatial resolution; 3) system efficiencies in imaging mode are 2.4–31%; and 4) the system efficiencies in spectroscopic modes is 5–18%. These results suggest that the optical performance of the NIR channel is achieved as expected from characteristics of the optical components. However, calculations of the background levels and on-sky sensitivity based on these results suggest that neutral density (ND) filters are needed to avoid saturation in L ′ - and M′ -band observations and that the ND filters and the entrance window, made of chemical-vapor-deposition (CVD) diamond, significantly degrade the sensitivity in these bands. This means that the use of different window materials and improvements of the detector readout speed are required to achieve both near-infrared and long-wavelength mid-infrared (>30 µm) observations.
We have developed a prototype half-wave plate (HWP) based polarization modulator (PMU) for Cosmic Microwave Background polarization measurement experiments. We built a 1/10 scaled PMU that consists of a 50 mm diameter five-layer achromatic HWP with a moth-eye broadband anti-reflection sub-wavelength structure mounted on a superconducting magnetic bearing. The entire system has cooled below 20 K in a cryostat chamber that has two millimeter-wave transparent windows. A coherent source and the diode detector are placed outside of the cryostat and the millimeter-wave goes through the PMU in the cryostat. We have measured the modulated signal by the PMU, analyzed the spectral signatures, and extracted the modulation efficiency over the frequency coverage of 34-161 GHz. We identified the peaks in the optical data, which are synchronous to the rotational frequency. We also identified the peaks that are originated from the resonance frequency of the levitating system. We also recovered the modulation efficiency as a function of the incident electromagnetic frequency and the data agrees to the predicted curves within uncertainties of the input parameters, i.e. the indices of refraction, thickness, and angle alignment. Finally, we discuss the implication of the results when this is applied to the LiteBIRD low-frequency telescope.
Although astronomers have confirmed the existence of 4,000 exoplanets to date, it is still difficult to directly compare exoplanets with the planets in our solar system because most of the known transiting exoplanets have an orbital period shorter than 1 year. Recent analyses of the 4-year data from the Kepler spacecraft revealed dozens of long-period transiting exoplanets and showed that their abundance is of order unity around Sun-like stars. However, the stars targeted by Kepler are too faint to conduct follow-up observations. The on-going all-sky survey mission TESS, with four 10.5 cm cameras with a field of view of 24 deg x 24 deg, is finding nearby transiting planets; however, the nominal observation period (1 month{1 year) is too short to find long-period planets with au-scale orbits. Herein, we propose using the LOng-period Transiting exoplanet sUrvey Satellite (LOTUS) mission, which employs a 7.5 cm wide-field (33 deg x 33 deg) camera placed on a nanosatellite, to continuously monitor the same sky region and find long-period planets transiting nearby bright stars. We present a conceptual design for the optics and bus system of LOTUS. Our optical system has a uniform point spread function over the entire field of view and a wide wavelength range (0.5{1.0 um). The bus system is designed to ensure that the pointing precision is sufficient to achieve the sub-percent photometry required for the detection of transiting exoplanets.
The Mid-Infrared Multi-field Imager for gaZing at the UnKnown Universe (MIMIZUKU) is developed as the first-generation mid-infrared instrument for the University of Tokyo Atacama Observatory (TAO) 6.5-m telescope. MIMIZUKU performs medium-band imaging and low-resolution spectroscopy in 2-38 microns and enables highest-spatial-resolution observations in the long-wavelength mid-infrared beyond 25 microns. In addition, MIMIZUKU has a unique opto-mechanical device called ‘Field Stacker’, which enables us to observe a distant (<25 arcminutes) pair of target and reference objects simultaneously and improves accuracy of atmospheric calibration. This function is expected to improve photometric accuracy and quality of spectroscopic data even in the long-wavelength mid-infrared regions, where the atmospheric absorption is severe. In 2018, engineering observations of MIMIZUKU were carried out at the Subaru telescope, and its first-light was successfully achieved. In the engineering observations, the imaging and spectroscopic functions in the mid-infrared wavelengths (7.6-25 microns) were confirmed to be working almost as expected, although the sensitivity is still worse than the background-limited performance by a factor of a few due to high readout noise. The Field Stacker was also confirmed to be working as expected. It is confirmed that the photometric instability can be reduced to a few percent by using Field Stacker even when the atmospheric transmittance varies by 10% in time. It is also confirmed that spectroscopic observations can be performed not only in 10-micron band but also in 20-micron band, where the spectroscopic observations are difficult even at the Mauna Kea site. We report the results of these on-sky performance evaluations.
With the imminent launch of the JWST, the field of thermal-infrared (TIR) astronomy will enjoy a revolution. It is easy to imagine that all areas of infrared (IR) astronomy will be greatly advanced, but perhaps impossible to conceive of the new vistas that will be opened. To allow both follow-up JWST observations and a continuance of work started on the ground-based 8m’s, we continue to plan the science cases and instrument design for a TIR imager and spectrometer for early operation on the TMT. We present the current status of our science cases and the instrumentation plans, harnessing expertise across the TMT partnership. This instrument will be proposed by the MICHI team as a second-generation instrument in any upcoming calls for proposals.
We present our design and development of a polarization modulator unit (PMU) for LiteBIRD space mission. LiteBIRD is a next generation cosmic microwave background (CMB) polarization satellite to measure the primordial B-mode. The science goal of LiteBIRD is to measure the tensor-to-scalar ratio with the sensitivity of δr < 10-3. The baseline design of LiteBIRD is to employ the PMU based on a continuous rotating half-wave plate (HWP) at a telescope aperture with a diameter of 400 mm. It is an essential for LiteBIRD to achieve the science goal because it significantly reduces detector noise and systematic uncertainties. The LiteBIRD PMU consists of a multi-layered sapphire as a broadband achromatic HWP and a mechanism to continuously rotate it at 88 rpm. The whole system is maintained at below 10K to minimize the thermal emission from the HWP. In this paper, we discuss the current development status of the broadband achromatic HWP and the cryogenic rotation mechanism.
The Mid-Infrared Multi-field Imager for gaZing at the UnKnown Universe (MIMIZUKU) is a mid-infrared camera and spectrograph developed as a first-generation instrument on the University of Tokyo Atacama Observatory (TAO) 6.5-m telescope. MIMIZUKU covers a wide wavelength range from 2 to 38 μm and has a unique optical device called Field Stacker which realizes accurate calibration of variable atmospheric transmittance with a few percent accuracy. By utilizing these capabilities, MIMIZUKU realizes mid-infrared long-term monitoring, which has not been challenged well. MIMIZUKU has three optical channels, called NIR, MIR-S, and MIR-L, to realize the wide wavelength coverage. The MIR-S channel, which covers 6.8–26 μm, has been completed by now. We are planning to perform engineering observations with this channel at the Subaru telescope before the completion of the TAO 6.5-m telescope. In this paper, we report the results of the laboratory tests to evaluate the optical and detector performances of the MIR-S channel. As a result, we confirmed a pixel scale of 0.12 arcsec/pix and a vignetting- free field of view of 2./0 1./8. The instrument throughputs for imaging modes are measured to be 20–30%. Those for N - and Q -band spectroscopy modes are 17 and 5%, respectively. As for the detector performance, we derived the quantum efficiency to be 40–50% in the mid-infrared wavelength region and measured the readout noise to be 3000–6000 electrons, which are larger than the spec value. It was found that this large readout noise degrades the sensitivity of MIMIZUKU by a factor of two.
The Space Infrared Telescope for Cosmology and Astrophysics (SPICA) mission is a Japanese astronomical infrared satellite project optimized for mid' to far-infrared observatories. It will be launched at ambient temperature and cooled down on orbit by mechanical coolers on board with an efficient radiative cooling system, which allow us to have a 3.5m cooled (4.5K) telescope in space. SPICA will answer a number of important problems in present-day astronomy, ranging from the star-formation history of the universe to the formation of planets, owing to its high spatial resolution and unprecedented sensitivity in the mid- to far-infrared. The large aperture mirror for cryogenically use in space, however, demand a challenging development for the telescope system. A single aperture design of the primary mirror will be adopted for the SPICA telescope rather than deployable mirror designs to avoid further complexity and ensure the feasibility. The number of actuators for the primary mirror, if needed, will be minimized. Silicon carbide and carbon-filter reinforced silicon carbide are extensively investigated at present as the prime candidate materials for the SPICA primary mirror. This presentation reports the current status of the SPICA telescope system development.
SPICA (Space Infrared Telescope for Cosmology and Astrophysics) is an astronomical mission optimized for mid-and far-infrared astronomy with a cryogenically cooled 3-m class telescope, envisioned for launch in early 2020s. Mid-infrared Camera and Spectrometer (MCS) is a focal plane instrument for SPICA with imaging and spectroscopic observing capabilities in the mid-infrared wavelength range of 5-38μm. MCS consists of two relay optical modules and following four scientific optical modules of WFC (Wide Field Camera; 5'x 5' field of view, f/11.7 and f/4.2 cameras), LRS (Low Resolution Spectrometer; 2'.5 long slits, prism dispersers, f/5.0 and f/1.7 cameras, spectral resolving power R ∼ 50-100), MRS (Mid Resolution Spectrometer; echelles, integral field units by image slicer, f/3.3 and f/1.9 cameras, R ∼ 1100-3000) and HRS (High Resolution Spectrometer; immersed echelles, f/6.0 and f/3.6 cameras, R ∼ 20000-30000). Here, we present optical design and expected optical performance of MCS. Most parts of MCS optics adopt off-axis reflective system for covering the wide wavelength range of 5-38μm without chromatic aberration and minimizing problems due to changes in shapes and refractive indices of materials from room temperature to cryogenic temperature. In order to achieve the high specification requirements of wide field of view, small F-number and large spectral resolving power with compact size, we employed the paraxial and aberration analysis of off-axial optical systems (Araki 2005 [1]) which is a design method using free-form surfaces for compact reflective optics such as head mount displays. As a result, we have successfully designed compact reflective optics for MCS with as-built performance of diffraction-limited image resolution.
MIMIZUKU is the first-generation mid-infrared instrument for the university of Tokyo Atacama Observatory (TAO) 6.5-m telescope. MIMIZUKU provides imaging and spectroscopic monitoring capabilities in a wide wavelength range from 2 to 38 μm, including unique bands like 2.7-μm and 30-μm band. Recently, we decided to add spectroscopic functions, KL-band mode (λ= 2.1-4.0 μm; R =λ/Δλ ~ 210) and 2.7-μm band mode ( λ= 2.4-2.95 μm; R ~ 620), and continuous spectroscopic coverage from 2.1 to 26 μm is realized by this update. Their optical designing is completed, and fabrications of optical elements are ongoing. As recent progress, we also report the completion of the cryogenic system and optics. The cryogenic system has been updated by changing materials and structures of thermal links, and the temperatures of the optical bench and detector mounting stages finally achieved required temperatures. Their stability against instrument attitude is also confirmed through an inclination test. As for the optics, its gold-plated mirrors have been recovered from galvanic corrosion by refabrication and reconstruction. Enough image quality and stability are confirmed by room-temperature tests. MIMIZUKU is intended to be completed in this autumn, and commissioning at the Subaru telescope and scientific operations on the TAO telescope are planned in 2017 and around 2019, respectively. In this paper, these development activities and future prospects of MIMIZUKU are reported.
A cold chopper is a key device for next generation mid-infrared instruments such as TMT/MICHI. It should achieve fast and accurate position switching with a large chopping throw at cryogenic temperature. To satisfy the requirements, voice coil motors using superconducting MgB2 wire have been developed. We have made a first prototype of the VCM and carried out its performance measurements such as a transition temperature, transfer functions, and power dissipation in the laboratory. The results are almost consistent with the expectations and the calculations, but some show significant inconsistency. We have also made a next prototype which is small to fit the size of the MICHI chopper. This will be installed to a developing mid-infrared instrument MIMIZUKU and used for actual observations.
We have carried out a trial production of the large-format (n=11) image slicer unit for a possible future mid-infrared instrument on the TMT aiming to verify its technical feasibility. The key elements in our trial production are the monolithic large-format slice mirrors and the monolithic large-format pupil mirrors. The results of our trial production of those key elements based on the ultra high-precision cutting techniques and the assembly of the large-format image slicer unit are presented in this paper.
We present the concept, design, fabrication, and evaluation of a new deformable mirror (DM), which is latchable, compact, and designed to be applicable for cryogenic environments. The main body of a prototype DM was fabricated from a monolithic cuboid of aluminum using wire electrical discharge machining (EDM). A flexible structure was constructed inside the block by 3-dimensionally crossed hollowing using the EDM. The prototype has 6 × 6 channels, and its volume is 27 mm × 27 mm × 30 mm. The mirror was formed on the surface of the aluminum block using a highprecision NC lathe. The surface figure of the mirror was evaluated and 34 nm rms was obtained. The evaluated surface roughness for the center and off-center areas of the mirror was 9.2 nm rms and 7.6 nm rms, respectively Screws set at the back of the block deform the mirror via springs and the internal flexible structure. We present our first demonstration of deformation of the mirror carried out at ambient temperature. The relationship between the displacement of the screws and the deformation of the mirror was evaluated. Consequently, a linear relationship was confirmed, and no significant hysteresis was found. The application of such mirrors to telescopes used for various different objectives is discussed. We conclude that a DM based on our concept can be used for wavefront correction of space-borne telescopes, especially in the infrared wavelength region.
SPICA (Space Infrared Telescope for Cosmology and Astrophysics) is an astronomical mission optimized for mid- and far-infrared astronomy with a 3-m class telescope which is cryogenically cooled to be less than 6 K. The SPICA mechanical cooling system is indispensable for the mission but, generates micro-vibrations which could affect to the pointing stability performances. Activities to be undertaken during a risk mitigation phase (RMP) include consolidation of micro-vibration control design for the satellite, as well as a number of breadboarding activities centered on technologies that are critical to the success of the mission. This paper presents the RMP activity results on the microvibration control design.
We have carried out the trial production of small format (n=5) image slicer aiming to obtain the technical verification of the Integral Field Unit (IFU) that can be equipped to the next generation infrared instruments such as TMT/MICHI and SPICA/SMI. Our goal is to achieve stable pseudo slit image with high efficiency. Here we report the results of the assembly of the image slicer unit and the non-cryogenic evaluation system of the pseudo slit image quality in the infrared.
We report the restraint deformation and the corrosion protection of gold deposited aluminum mirrors for mid-infrared
instruments. To evaluate the deformation of the aluminum mirrors by thermal shrinkage, monitoring measurement of the
surface of a mirror has been carried out in the cooling cycles from the room temperature to 100 K. The result showed
that the effect of the deformation was reduced to one fourth if the mirror was screwed with spring washers.
We have explored an effective way to prevent the mirror from being galvanically corroded. A number of samples have
been prepared by changing the coating conditions, such as inserting an insulation layer, making a multi-layer and overcoating
water blocking layer, or carrying out precision cleaning before coating. Precision cleaning before the deposition
and protecting coat with SiO over the gold layer seemed to be effective in blocking corrosion of the aluminum. The SiO
over-coated mirror has survived the cooling test for the mid-infrared use and approximately 1 percent decrease in the
reflectance has been detected at 6-25 microns compared to gold deposited mirror without coating.
The MIMIZUKU is the first-generation mid-infrared instrument for the TAO 6.5-m telescope. It challenges to prove the origin of dust and the formation of planets with its unique capabilities, wide wavelength coverage and precise calibration capability. The wide wavelength coverage (2-38 μm) is achieved by three switchable cameras, NIR, MIR-S, and MIR-L. The specifications of the cameras are revised. A 5μm-cutoff HAWAII-1RG is decided to be installed in the NIR camera. The optical design of the MIR-L camera is modified to avoid detector saturation.
Its final F-number is extended from 5.2 to 10.5. With these modifications, the field of view of the NIR and MIR-L camera becomes 1.2’ × 1.2’ and 31” × 31”, respectively. The sensitivity of each camera is estimated based on the
revised specifications. The precise calibration is achieved by the “Field Stacker” mechanism, which enables the simultaneous observation of the target and the calibration object in different fields. The up-and-down motion
of the cryostat (~ 1 t), critical for the Field Stacker, is confirmed to have enough speed (4 mm/s) and position accuracy (~ 50 μm). A control panel for the Field Stacker is completed, and its controllers are successfully
installed. The current specifications and the development status are reported.
An image slicer is highly in demand for an integral field unit (IFU) spectrograph of the next generation infrared
telescopes. This paper reports the results of the trial production of three key optical elements for a small format (number
of slice; n=5) image slicer, i.e. monolithic slice mirrors, monolithic pupil mirrors and monolithic pseudo slit mirrors. We
have demonstrated that sufficiently high processing accuracy and mirror surface accuracy for infrared observations are
achieved for each optical element based on our super precision cutting techniques.
TAO (The University of Tokyo Atacama Observatory) is planned to be constructed at the summit of Co. Chajnantor (5640 m altitude) in Chile. MIMIZUKU (Mid-Infrared Multi-field Imager for gaZing at the UnKnown Universe) is a mid-infrared imager (Field of View: 1' x 1'- 2' x 2') and spectrometer (Δλ/λ: 60-230) for the 6.5-m TAO telescope, covering the wavelength range of 2-38 μm. The MIMIZUKU has a unique equipment called Field Stacker (FS) which enables the simultaneous observation of target and reference object. The simultaneity is expected to improve photometric accuracy and to realize long-term monitoring observations. The development status of the MIMIZUKU is reported in this paper. The FS and the cryostat of the MIMIZUKU have been fabricated and under testing. The cold optics (550 mm x 750 mm x 2 floors) with 28 mirrors has been constructed. The mirrors were aligned with the positional precision of 0.1 mm and the angular precision of 0.1 deg. The evaluated optical performance is that the diffraction-limited image at λ <8 μm and the enough compact image (r <2 pix=0.22") at 2 λ ~2μm can be obtained. In the cold optics, the drive systems with backlash-less gears are employed and work well even in cryogenic environment. The grisms made with silicon and germanium have been fabricated by ultraprecision cutting. It was found that their surface roughness, grating constant, and blaze angle almost measure up to the designed values.
A mid-infrared (MIR) imager and spectrometer is being investigated for possible construction in the early operation of the Thirty Meter Telescope (TMT). Combined with the MIR adaptive optics (AO) system (MIRAO), the instrument will afford ~15 times higher sensitivity and ~4 times better spatial resolution (0.07”) at 10μm compared to 8m-class telescopes. Additionally, through exploiting the large collection area of the TMT, the high-dispersion spectroscopy mode will be unrivaled by other ground- and space-based facilities. These combined capabilities offer the possibility for breakthrough science, as well as ‘workhorse’ observing modes of imaging and low/moderate spectral resolution. In this paper we summarize the primary science drivers that are guiding the instrument design.
We have evaluated on-sky performances of a mid-infrared camera MAX38 (Mid-infrared Astronomical eXploerer)
on the miniTAO 1-meter telescope. A Strehl ratio at the N-band is estimated to be 0.7-0.8, and it reaches to 0.9
at the 37.7 micron, indicating that diffraction limited angular resolution is almost achieved at the wavelength
range from 8 to 38 micron. System efficiencies at the N and the Q-band are estimated with photometry of
standard stars. The sensitivity at the 30 micron cannot be exactly estimated because there are no standard stars
bright enough. We use the sky brightness instead. The estimated efficiencies at the 8.9, 18.7, and 31.7 micron
are 4%, 3%, 15% , respectively. One-sigma sensitivity in 1 sec integration of each filter is also evaluated. These
give good agreements with the designed values. Preliminary scientific results are briefly reported.
SPICA (Space Infrared Telescope for Cosmology and Astrophysics) is an astronomical mission optimized for
mid- and far-infrared astronomy, envisioned for launch in early 2020s. The core wavelength coverage of this
mission is 5 to 200 micron. Mid-infrared Camera and Spectrometer (MCS) will provide imaging and spectroscopic
observing capabilities in the mid-infrared region with 4 modules. WFC (Wide Field Camera) has two 5
arcminutes square field of view and covers the wavelength range from 5 to 38 micron. MRS (Mid Resolution
Spectrometer) has integral field units by image slicer and covers the wavelength range from 12.2 to 37.5 micron
simultaneously using dichroic filter and two sets of spectrometers. HRS (High Resolution Spectrometer) covers
the wavelength range from 12 to 18 micron with resolving power 20000 to 30000, and it has optional short
wavelength channel which covers from 4 to 8 micron with resolving power 30000. LRS (Low Resolution Spectrometer)
adopts prism disperser and covers the wavelength range from 5 to 38 micron with resolving power 50
to 100. Here, we present detailed specifications of MCS, optical design, and estimated performance on orbit.
Mid-infrared Medium Resolution Spectrometer (MRS) is one of the key spectroscopic modules of Mid-
Infrared Camera and Spectrometers (MCS) that will be onboard SPICA. MRS is an Echelle Grating
spectrometer designed to observe a number of fine structure lines of ions and atoms, molecular lines, and
band features stemming from solid particles and dust grains of the interstellar and circumstellar
medium in the mid-infrared wavelength range. MRS consists of two channels; the shorter wavelength
channel (MRS-S) covers the spectral range from 12.2 to 23.0 micron with a spectral resolution power of
R~1900-3000 and the longer wavelength channel (MRS-L) covers from 23.0 to 37.5 micron with
R~1100-1500 on the basis of the latest results of the optical design. The distinctive functions of the
MRS are (1) a dichroic beam splitter equipped in the fore-optics, by which the same field of view is
shared between the two channels, and (2) the small format image slicer as the integral field unit
installed in each channel. These functions enable us to collect continuous 12-38 micron spectra of both
the point-like and diffuse sources reliably with a single exposure pointed observation. In this paper, the
specifications and the expected performance of the MRS are summarized on the basis of the latest
results of the optical design. The latest progress in the development of the key technological elements,
such as the Dichroic Beam Splitter and the Small Format Monolithic Slice Mirrors, are also reported.
We present the current status of the development of the SPICA Coronagraph Instrument (SCI). SPICA is a next-generation
3-meter class infrared telescope, which will be launched in 2022. SCI is high-contrast imaging, spectroscopic
instrument mainly for direct detection and spectroscopy of extra-solar planets in the near-to-mid infrared wavelengths to
characterize their atmospheres, physical parameters and evolutionary scenarios. SCI is now under the international
review process. In this paper, we present a science case of SCI. The main targets of SCI, not only for direct imaging but
also for spectroscopy, are young to matured giant planets. We will also show that some of known exoplanets by ground-based
direct detection are good targets for SCI, and a number of direct detection planets that are suitable for SCI will be
significantly increased in the next decade. Second, a general design of SCI and a key technology including a new high-throughput
binary mask coronagraph, will be presented. Furthermore, we will show that SCI is potentially capable of
achieving 10-6 contrast by a PSF subtraction method, even with a telescope pointing error. This contrast enhancement
will be important to characterize low-mass and cool planets.
We present the Prototype-testbed for Infrared Optics and Coronagraphs (PINOCO) which is a large, multi-purpose
cryogenic chamber. At present, the priority for PINOCO is to evaluate binary pupil mask coronagraphs in the mid-infrared
wavelength region, which are planned to be adopted for the SPICA coronagraph instrument. In addition, various
other experiments are possible using PINOCO: testing diverse high dynamic-range techniques, mirrors, active optics,
infrared detectors, filters and spectral dispersion devices, the mechanics of the instruments, measurement of material
properties, and so on. PINOCO provides a work space of 1m × 1m × 0.3m, of which inside is cooled to <5K.
Flexible access to the work surface is possible by removing detachable plates at the four sides and on the top of the
chamber. At the interface to the exterior, PINOCO is currently equipped with an optical window, electric
connectors, and an interferometer stage. PINOCO is cooled by two GM-cycle cryo-coolers, so no cryogen is
needed. A cooling test of PINOCO was successfully completed.
Mid-infrared Camera and Spectrometer (MCS) is one of focal plane instruments for SPICA (Space Infrared
Telescope for Cosmology and Astrophysics), which have 3 m class 6 K cooled telescope. MCS will provide wide
field imaging and low-, medium-, and high-resolution spectroscopic observing capabilities with 7 detectors in the
wavelength range from 5 to 38 micron. Large format array detectors are required in order to realize wide field of
view in imaging and wide spectral coverage in spectroscopy. We are planning to cover the wavelength range of
5-26 micron by Si:As IBC 2K x 2K and 20-38 micron by Si:Sb BIB 1K x 1K. The development status and their
design including the electrical and thermal design are described.
We describe the principles and potential of Color-Differential Astrometry (CDA), a high-resolution technique easily
implementable on the Science Coronographic Instrument (SCI) of the SPICA satellite, and aimed here at the direct
detection and spectroscopy of giant Extrasolar Planets (ESP). By measuring the photocentre of the source diffraction
pattern relatively between dispersed spectral channels, CDA gives access to flux ratio and angular information well
beyond the telescope resolution limit. Applied to known ESPs, it can yield the inclination (thus the mass) and spectrum
of the planet. Our estimates show that low-resolution spectroscopy of Jupiter-radius ESP can be measured within a few
hours for planets at orbital distances ranging from 0.05 AU to a few AUs, thus complementing the detection range
expected using the coronographic measurements. More generally, it may also apply to any unresolved source with some
wavelength-dependent asymmetry.
In addition to the ESP cases considered for the scientific signal and to their associated fundamental noises, we also
present the instrumental effects and a dedicated optical testbench. The combined effects of several instrumental noise
sources can be introduced into our numerical model (pointing errors, beam tip-tilt, optical aberations, variations of the
detector gain table), and then confronted to measurements from the experimental testbench.
We have been developing an immersion grating for high-resolution spectroscopy in the mid-infrared (MIR)
wavelength region. A MIR (12-18 µm) high-resolution (R = 20,000-30,000) spectrograph with the immersion
grating is proposed for SPICA, Japanese next-generation space telescope. The instrument will be the world's first
high-resolution spectrograph in space, and it would make great impacts on infrared astronomy. To realize a high-efficiency immersion grating, optical properties and machinability of bulk materials are the critical issues. There
are three candidate materials with good MIR transmittance; CdTe (n = 2.65), CdZnTe (n = 2.65), and KRS5 (n
= 2.30). From measurements of transmittance with FTIR and of homogeneity with phase-shifting interferometry
at 1.55 μm, we confirmed that CdZnTe is the best material that satisfies all the optical requirements. As for
machinability, by applying Canon's diamond cutting (planing) technique, fine grooves that meet our requirement
were successfully cut on flats for all the materials. We also managed to fabricate a small CdZnTe immersion
grating, which shows a high grating efficiency from the air. For the reflective metal coating, we tried Au (with
thin underlying layer of Cr) and Al on CdZnTe flats both by sputter deposition and vapor deposition. All samples
are found to be robust under 77 K and some of them achieve required reflectivity. Despite several remaining
technical issues, the fabrication of CdZnTe immersion grating appears to be sound.
SPICA (Space Infrared Telescope for Cosmology and Astrophysics) is an astronomical mission optimized for
mid- and far-infrared astronomy, envisioned for launch in 2018. Mid-infrared instruments for SPICA are
required to have three basic capabilities; a wide-field imaging, spectroscopic capability, and coronagraphic
capability as an option. First two capabilities are implemented by three instruments; MIRACLE(Mid-infRAred
Camera w/o Lens), MIRMES(Mid-IR Medium-resolution Echelle Spectrometer), and MIRHES(Mid-IR High-resolution
Echelle Spectrometer). Here, we present an optical architecture of the union of MIRACLE, MIRMES,
and MIRHES. MIRACLE has two channels (-S for short wavelength and -L for long wavelength) to cover the
wavelength range 5 to 40 micron. MIRACLE-L and MIRMES are packaged into one unit with common optical
bench and MIRACLE-S and MIRHES are packaged into another unit. Two units are independent with each
other and occupy different field of view of the SPICA telescope. Each unit has common fore-optics shared by
MIRACLE and MIR(M/H)ES. This fore-optics is designed using reflective mirror optics only, and has wide
filed of view(FOV). Most of the FOV is used by MIRACLE and small part of the FOV is used by MIRMES
or MIRHES. This structure of the instruments reduces the size and weight of the instruments. This benefit
outweigh the complexity of the instruments.
S. Oyabu, I. Yamamura, C. Alfageme, P. Barthel, A. Cassatella, M. Cohen, N. Cox, E. Figueredo, H. Fujiwara, N. Ikeda, D. Ishihara, W.-S. Jeong, H. Kataza, Do Kester, H. M. Lee, S. Makiuti, T. Mueller, T. Nakagawa, S. Takita, S. H. Oh, S. Oliver, C. Pearson, N. Rahman, M. Rowan-Robinson, A. Salama, R. Savage, S. Serjeant, G. J. White, C. Yamauchi
Bright source catalogues based on the new mid- and far-infrared all-sky survey by the infrared astronomical
satellite AKARI were released into the public domain in March 2010. The mid-infrared catalogue contains
more than 870 thousand sources observed at 9 and 18 μm, and the far-infrared catalogue provides information
of about 427 thousand sources at 65, 90, 140, and 160 μm. The AKARI catalogues will take over the IRAS
catalogues and will become one of the most important catalogues in astronomy. We present the characteristics
of the AKARI infrared source catalogues as well as current activity for the future versions.
The Mid-Infrared Medium-Resolution Eschelle Spectrometer (MIRMES) is one of the focal-plane instrument onboard
SPICA mission proposed in the pre-project phase. It is designed for measuring the strengths and the profiles of lines and
bands emitted from various phases of materials including ionized gas, gas-phase molecules, solid-phase molecules and
dust particles in the wavelengths from 10 to 40μm. The MIRMES provides a medium resolution (R=700-1500)
spectroscopic capability in the mid-infrared spectral range (10-36μm) with integrated field units of a field-of-view of
about 12"×6" for shorter wavelength range (10-20μm) and 12"×12".5 for longer wavelength range (20-36μm). The
science targets of the MIRMES and the results of the concept study on its optical design and the expected performance
are described.
Mid-InfRAred Camera w/o LEns (MIRACLE) is a focal plane instrument for the future JAXA/ESA infrared
astronomical mission, SPICA. MIRACLE is designed for wide field imaging (5' × 5') and low-resolution spectroscopic
observations (R~100) over a wide spectral range in the mid-infrared wavelengths (5-38μm). Thanks
to the SPICA's large aperture (3-m class) and cold (<6K) telescope, MIRACLE has a better sensitivity than
JWST/MIRI at the wavelength over 20μm (3.5 μJy at 20μm, R=5, S/N=5, 3600 seconds) and its wider field
of view (FOV) provides a faster mapping speed in its full spectral range for point sources. Confocal off-axis
reflective imaging system provides a wide FOV with diffraction limited image quality over wide spectral range.
MIRACLE consists of two channels: MIRACLE-S and MIRACLE-L, which are optimized for 5-26μm and 20-
38μm, respectively. Each of them consists of a fore-optics and a rear-optics, each of which has a pupil position
equipped with a filter wheel and a grating wheel, respectively. A field stop wheel, which provides optimal slits in
the spectroscopic mode and a wide FOV in the imaging mode, is installed at the focal plane of the fore-optics.
A large format array detector (Si:As 2K×2K for MIRACLE-S and Si:Sb 1K×1K for MIRACLE-L) is installed at
the focal plane of the rear-optics in order to achieve Nyquist sampling of the point spread function. Contiguous
wavelength coverage is considered in choice of the filter bands from the experiences in the Spitzer and AKARI
observations. We will present the results of conceptual design study including sensitivity analysis.
We successfully carried out 30-micron observations from the ground-based telescope for the first time with our newly
developed mid-infrared instrument, MAX38, which is mounted on the University of Tokyo Atacama 1.0-m telescope
(miniTAO telescope). Thanks to the high altitude of the miniTAO (5,640m) and dry weather condition of the Atacama
site, we can access the 30-micron wavelength region from ground-based telescopes. To achieve the observation at 30-
micron wavelength, remarkable devices are employed in MAX38. First, a Si:Sb 128x128 array detector is installed
which can detect long mid-infrared light up to 38-micron. Second, we developed metal mesh filters for 30-micron region
band-pass filter, which are composed of several gold thin-films with cross-shaped holes. Third, a cold chopper, a 6-cm
square plane mirror controlled by a piezoelectric actuator, is built into the MAX38 optics for canceling out the
atmospheric turbulence noise. It enables square-wave chopping with a 50-arcsecound throw at a frequency more than 5-
Hz. Finally, a low-dispersion grism spectrometer (R~50) will provide information on the transmission spectrum of the
terrestrial atmosphere in 20 to 40 micron. In this observation, we clearly demonstrated that the atmospheric windows
around 30-micron can be used for the astronomical observations at the miniTAO site.
A mid-infrared (MIR) imager and spectrometer is being investigated for possible consideration for construction
in the early operation of the Thirty Meter Telescope (TMT). Combined with adaptive optics for the MIR, the
instrument will afford 15 times higher sensitivity (0.1mJy as 5 sigma detection in 1hour integration in the N-band
imaging) and 4 times better spatial resolution (0.08") at 10μm compared to 8m-class telescopes. In addition, its
large light-gathering power allows high-dispersion spectroscopy in the MIR that will be unrivaled by any other
facility. We, a collaborating team of Japanese and US MIR astronomers, have carefully considered the science
drivers for the TMT MIR instrument. Such an instrument would offer both broad and potentially transformative
science. Furthering the science cases for the MIRES1, where high-dispersion spectroscopy was emphasized, we
discuss additional capabilities for the instrument drawn from the enlarged science cases. The science cases include
broader areas of astronomical fields: star and planet formation, solar system bodies, evolved stars, interstellar
medium (ISM), extragalaxies, and cosmology. Based on these science drivers, essential instrument capabilities
and key enhancement are discussed (see the companion paper Tokunaga et al. 20102): specifically imaging, lowand
high-spectral resolution modes, integral field spectroscopy, and polarimetry.
Ground-based mid-infrared observations have two distinct advantages over space observations despite relatively lower
sensitivity. One is the high spatial resolution and the other is the monitoring capability. These advantages can be
emphasized particularly for the next coming ground-based infrared project University of Tokyo Atacama Observatory
(TAO). Thanks to the low water vapor of the TAO site (5,640m) and the large aperture of the telescope (6.5meter), we
can observe at 30 micron with a spatial resolution of 1 arcsec. It is about ten times higher than that of current space
telescopes. The TAO is also useful for monitoring observations because of the ample observing time.
To take these advantages we are now developing a new mid-infrared infrared instrument for the TAO 6.5-meter
telescope. This covers a wide wavelength range from 2 to 38 micron with three detectors (Si:As, Si:Sb, and InSb).
Diffraction limited spatial resolution can be achieved at wavelengths longer than 7 micron. Low-resolution spectroscopy
can also be carried out with grisms. This instrument equips a newly invented "field stacker" for monitoring observations.
It is an optical system that consists of two movable pick-up mirrors and a triangle shaped mirror, and combine two
discrete fields of the telescope into camera's field of view. It will enable us to apply a differential photometry method
and dramatically improve the accuracy and increase the feasibility of the monitoring observations at the mid-infrared
wavelengths.
A mid-infrared imager and spectrometer is under consideration for construction in the first decade of the Thirty-
Meter Telescope (TMT) operation (see the companion paper by Okamoto). MIRES, a mid-infrared high-spectral
resolution optimized instrument, was previously proposed to provide these capabilities to the TMT community.
We have revised the design in order to provide an improved optical design for the high-spectral resolution
mode with R=120,000, improved imaging with sky chopping, low-spectral resolution mode with an integral
field spectrograph, and polarimetry. In this paper we describe the optical design concepts currently under
consideration.
We have developed a cold chopper system for mid-infrared observations. This system is installed into the newly
developing mid-infrared instrument, MAX38, for the University of Tokyo Atacama 1.0-m telescope. It is cooled to about
9K. The cold chopper mirror is controlled by a piezoelectric actuator with a flexure hinge lever, and enables square-wave
chopping at a frequency up to 7.8 Hz. At the moment, the maximum throw of the chopper is 30 arcseconds on the sky.
This cooled chopping mirror system can also be applied to the tip-tilt mirror for SPICA infrared space telescope. We
carried out the first light with Kanata 1.5-m telescope at Higashi-Hiroshima Observatory (Hiroshima, Japan) in June
2007 and March 2008. In this observation, we demonstrated that the cold chopper could cancel out the atmospheric
turbulence noise of a frequency of 5 Hz at 8.9 micron.
We have developed bandpass filters for long mid-infrared astronomy in 25 to 40μm. Most of materials become opaque in
wavelengths longer than 25μm. We have applied the metal mesh method to make filters of non-transparent materials.
The mesh patterns are designed based on the FDTD calculations and fabricated by the photolithography method.
Measured transmittances of the fabricated filters agree with model calculations. The mesh filter has leakage in
wavelengths shorter than the peak wavelength in principle. The most effective way to achieve a high stopband rejection
is to stack several identical mesh filters incoherently. A narrow bandwidth fitted to atmospheric windows is required in
the ground-based 30μm observations. We have fabricated a thick mesh filter without dielectric substrate, which is main
source of internal absorption. The thick mesh leads to narrowing of the bandwidth due to the waveguide effect. The
fabricated non-coated thick mesh filter has a peak transmittance of 0.8 and a bandwidth of λ/dλ=8.3 at 4 K. When
stacking four of these mesh filters, it is expected to achieve a stopband rejection over 50dB, a peak transmittance of 0.41,
and a bandwidth of λ=/dλ=17.5.
KEYWORDS: Clocks, Fiber reinforced polymers, Digital signal processing, Signal processing, Infrared radiation, Operating systems, Data processing, Control systems, Field programmable gate arrays, Cameras
Real-time capabilities are required for a controller of a large format array to reduce a dead-time attributed by readout and
data transfer. The real-time processing has been achieved by dedicated processors including DSP, CPLD, and FPGA
devices. However, the dedicated processors have problems with memory resources, inflexibility, and high cost.
Meanwhile, a recent PC has sufficient resources of CPUs and memories to control the infrared array and to process a
large amount of frame data in real-time. In this study, we have developed an infrared array controller with a software
real-time operating system (RTOS) instead of the dedicated processors. A Linux PC equipped with a RTAI extension
and a dual-core CPU is used as a main computer, and one of the CPU cores is allocated to the real-time processing. A
digital I/O board with DMA functions is used for an I/O interface. The signal-processing cores are integrated in the OS
kernel as a real-time driver module, which is composed of two virtual devices of the clock processor and the frame
processor tasks. The array controller with the RTOS realizes complicated operations easily, flexibly, and at a low cost.
The present status of the development of an extrinsic photoconductor based on a high-purity GaAs is reported. This
photoconductor utilizing the shallow donor levels in GaAs and is highly sensitive for incident terahertz photons in the
wavelength range 150 to 300 micron. The n-type GaAs crystal has been growth by liquid phase epitaxial (LPE) method,
which is suitable to obtain thick and high-purity GaAs. The impurity concentration in GaAs layer has been decreased to
the order of 1013 atoms/cm-3. By doping the donors lightly in the LPE growth process, C/Si, (background doped) Se and
Te doped GaAs layers has been fabricated. The GaAs photoconductors using these crystals are sensitive in longer
wavelength region than Ge:Ga photoconductors used in the past far-infrared astronomical observations. The most
sensitive detector is obtained with C or Si background doped GaAs, of which NEP is reached to 3×10-16 W/Hz0.5 at the
temperature of 1.5 K, at 290 micron, the peak of its responsivity spectrum.
A balloon-borne telescope utilizing our GaAs photoconductors, Tera-GATE (THz observation with GaAs
photoconductors and a balloon-borne Telescope) is now under development. The Tera-GATE is a 69 cm diameter
telescope. On its focal plane, a photoconductor array with Winston cone has 2-mm entrance aperture and leads the
incident photons to a cavity where 0.5-mm size photoconductor is installed. Measured optical efficiency of the
cone/cavity system is in an acceptable range ~40 percent.
We describe the balloon-borne telescope (69cm aperture) for the project Tera-GATE (THz observation with GaAs photoconductors and a balloon-borne TElescope) aiming at the THz astronomical observations. THz region is the last frontier left not well explored and we are planning to have multiband photometric observations covering the wavelength from 50 to 300 microns and get completed SED data for some Young Stellar Objects in this band. The telescope, we are constructing, has image stabilizing system which cancels out pointing error (up to about 0.3 degrees) of the balloon gondola, and enables us to take a long exposure needed for highly sensitive observations. We will show the structure of the telescope, cold stop design, and characteristics of the image stabilizing system.
Infrared Camera (IRC) onboard AKARI satellite has carried out more than 4000 pointed observations during the phases
1 and 2, a significant amount of which were performed in the spectroscopic mode. In this paper, we investigate the
properties of the spectroscopic data taken with MIR-S channel and propose a new data reduction procedure for slit-less
spectroscopy of sources embedded in complicated diffuse background structures. The relative strengths of the 0th to 1st
order light as well as the efficiency profiles of the 2nd order light are examined for various objects taken with MIR-S
dispersers. The boundary shapes of the aperture mask are determined by using the spectroscopic data of uniform zodiacal
emission. Based on these results, if the appropriate template spectra of zodiacal light emission and the diffuse
background emission are prepared and the geometries of the diffuse structures are obtained by the imaging data, we can
reproduce the slit-less spectroscopic patterns made by a uniform zodiacal emission and the diffuse background emission
by a convolution of those template profiles. This technique enables us to obtain the spectra of infrared sources in highly
complicated diffuse background and/or foreground structures, such as in the Galactic plane and in nearby galaxies.
The Infrared Camera (IRC) is one of two focal-plane instruments on the AKARI satellite. It is designed for
wide-field deep imaging and low-resolution spectroscopy in the near- to mid-infrared (1.8-26.5 micron) in the
pointed observation mode of AKARI. The IRC is also operated in the survey mode to make an All-Sky Survey
at 9 and 18 microns. The IRC is composed of three channels. The NIR channel (1.8-5.5 micron) employs
a 512x412 InSb photodiode array, whereas both the MIR-S (4.6-13.4 micron) and MIR-L (12.6-26.5 micron)
channels use 256x256 Si:As impurity band conduction (IBC) arrays. Each of the three channels has a field-ofview
of approximately 10x10 arcmin., and they are operated simultaneously. The NIR and MIR-S channels share
the same field-of-view by virtue of a beam splitter. The MIR-L observes the sky about 25 arcmin. away from the
NIR/MIR-S field-of-view. The in-flight performance of the IRC has been confirmed to be in agreement with the
pre-flight expectation. More than 4000 pointed observations dedicated for the IRC are successfully completed,
and more than 90% of the sky are covered by the all-sky survey before the exhaustion of the Akari's cryogen. The
focal-plane instruments are currently cooled by the mechanical cooler and only the NIR channel is still working
properly. Brief introduction, in-flight performance and scientific highlights from the IRC cool mission, together
with the result of performance test in the warm mission, are presented.
AKARI is the first Japanese astronomical infrared satellite mission orbiting around the Earth in a sun-synchronous
polar orbit at the altitude of 700 km. One of the major observation programs of the AKARI is an all-sky survey in the
mid- to far-infrared spectral regions with 6 photometric bands. The mid-infrared part of the AKARI All-Sky Survey was
carried out with the Infrared Camera (IRC) at the 9 and 18 µm bands with the sensitivity of about 50 and 120 mJy (5σ
per scan), respectively. The spatial resolution is about 9.4" at both bands. AKARI mid-infrared (MIR) all-sky survey
substantially improves the MIR dataset of the IRAS survey of two decades ago and provides a significant database for
studies of various fields of astronomy ranging from star-formation and debris disk systems to cosmology. This paper
describes the current status of the data reduction and the characteristics of the AKARI MIR all-sky survey data.
We present a preliminary optical design and layout for the mid-infrared (4-18 μm) high-resolution spectrograph for
SPICA, Japanese next-generation space IR observatory with 3.5 m telescope. MIR high-resolution spectroscopy
is a powerful probe to study gas-phase molecules/atoms in a variety of astronomical objects. Space observation
provides a great opportunity to study many molecular lines especially in between the atmospheric windows.
SPICA gives us a chance to realize MIR high-resolution spectroscopy from space with the large telescope aperture.
The major technical challenge is the size of the spectrograph, which tends to be too large for space. We hope to
overcome this problem with a novel MIR immersion grating, which can make the instrument smaller by a factor
of the refractive index of the grating material. We plan to fabricate a large pitch ZnSe (n = 2.4) immersion
grating with the fly-cutting technique at LLNL (see Poster paper 7018-183 by Ikeda et al.1 and 7018-181 by
Kuzmenko et al.2 in the proceedings of this conference). We show our preliminary spectrograph designs with
a spectral resolution of ~30,000 in 4-8 μm (short mode) and 12-18 μm (long mode). The instrument size can
be as small as 200 × 400 mm thanks to the MIR immersion gratings. With unprecedented spectral resolution
in space, which is 10-times higher than ISO-SWS, the high-resolution spectrograph for SPICA (SPICA-HIRES)
could be a unique instrument that can provide most sensitive and clear spectra of this kind.
The SPace Infrared telescope for Cosmology and Astrophysics (SPICA) is a infrared space-borne telescope mission of
the next generation following AKARI. SPICA will carry a telescope with a 3.5 m diameter monolithic primary mirror
and the whole telescope will be cooled to 5 K. SPICA is planned to be launched in 2017, into the sun-earth L2 libration
halo orbit by an H II-A rocket and execute infrared observations at wavelengths mainly between 5 and 200 micron. The
large telescope aperture, the simple pupil shape, the capability of infrared observations from space, and the early launch
gives us with the SPICA mission a unique opportunity for coronagraphic observation. We have started development of a
coronagraphic instrument for SPICA. The primary target of the SPICA coronagraph is direct observation of extra-solar
Jovian planets. The main wavelengths of observation, the required contrast and the inner working angle (IWA) of the
SPICA coronagraph are set to be 5-27 micron (3.5-5 micron is optional), 10-6, and a few λ/D (and as small as possible),
respectively, in which λ is the observation wavelength and D is the diameter of the telescope aperture (3.5m). For our
laboratory demonstration, we focused first on a coronagraph with a binary shaped pupil mask as the primary candidate
for SPICA because of its feasibility. In an experiment with a binary shaped pupil coronagraph with a He-Ne laser
(λ=632.8nm), the achieved raw contrast was 6.7×10-8, derived from the average measured in the dark region without
active wavefront control. On the other hand, a study of Phase Induced Amplitude Apodization (PIAA) was initiated in an
attempt to achieve better performance, i.e., smaller IWA and higher throughput. A laboratory experiment was performed
using a He-Ne laser with active wavefront control, and a raw contrast of 6.5×10-7 was achieved. We also present recent
progress made in the cryogenic active optics for SPICA. Prototypes of cryogenic deformable by Micro Electro
Mechanical Systems (MEMS) techniques were developed and a first demonstration of the deformation of their surfaces
was performed with liquid nitrogen cooling. Experiments with piezo-actuators for a cryogenic tip-tilt mirror are also
ongoing.
The SPICA, Japanese next generation infrared space telescope with a cooled 3.5 m primary mirror, will be a quite unique
observatory in the mid and far-infrared with unprecedented sensitivity and the spatial resolving power. Here we briefly
describe the key scientific objectives which can be performed only with SPICA, based on its unique design concepts. We
then describe the scientific requirements for the focal plane instruments, and summarize the constraints on the various
resources available for the focal plane instruments, derived from the spacecraft system design. We also outline the
concept of the planned focal plane instruments, and the future development plan.
Within the focal-plane instrument space (2.5m diameter, 0.5m height), two major instruments are so far planned to be
equipped: one is a mid-infrared instrument, consisting of a mid-infrared camera, mid-infrared spectrometers, and a midinfrared
coronagraph, while the another is a far-infrared camera and spectrometer. The mid-infrared camera will consist
of four channels covering 5-38 μm with approximately 25-40 square arcminutes, while the mid-infrared spectrometer
will have high-dispersion (R=30000) channels at 4-18 μm and moderate-dispersion (R=3000) channels at 16-38 μm.
The mid-infrared coronagraph will have both imaging and spectroscopic capability at 5-27 μm, with the contrast higher
than 10-6. As for the far-infrared camera and spectrometer, a Fourier-type imaging spectrometer covering 30-210 μm is
proposed and extensively studied by the European consortium (SAFARI consortium). A far-infrared and sub-millimeter
grating spectrometer instrument is also under consideration by the US SPICA team.
We describe the optical design of balloon-borne telescope with an image stabilizing secondary mirror which correct the
pointing error of the attitude control system and enable a long-time exposure. We adopted a Cassegrain-like two-mirror
system, and investigated the best mirror surface figure by surveying Conic constant (K) of the primary mirror from -1 to
0, where the secondary mirror is a high order aspheric surface to cancel spherical aberration at each K. In the small
pointing error region, the classical Cassegrain system (K=-1) provides a wide field of view. However, in the large
pointing error region, systems with large K provide a wide FOV. For λt (target wavelength) =50µm and 69cm aperture, a
spherical primary system has acceptable optical performances when we assume the pointing error around 0.3 degree.
Mid-Infrared Spectrometer with an Image Slicer (MIRSIS) is a 10micron band spectrometer for ground-based
observations. Based on the optical design reported in Okamoto et al. (2006), we recently developed most of
optical elements and their mounts. There, we adopted designs based on an ultra-precision cut for the slice mirrors
and the pupil mirrors. We also designed and partly manufactured the optical parts with switching/adjusting
mechanism with cryogenic step motors. Since MIRSIS has a very complicated stereoscopic configuration of
optical elements, we developed a method to adjust the optical alignment where relative positional markers and
a three-dimensional measuring system are combined. We confirmed that we can achieve position and angular
adjustment with error down to 0.1mm and 0.05degree through alignment test with a pair of mirrors.
Mid Infrared Spectrometer with an Image Slicer (MIRSIS) is a compact mid-infrared spectrometer with an image slicer
as a testbed of techniques for efficient observations with next generation telescopes. MIRSIS is a 10-micron band
spectrometer for ground-based observations. Optics of MIRSIS is mostly composed of reflective ones. A key point of the
development of MIRSIS is a fabrication of slicer optics, which consists of slice mirrors, pupil mirrors and pseudo slit
mirrors. It is necessary to develop fabrication technique of slicer optics, because shapes and alignment of these mirrors
are special. Here it is also important to choose the design matched to the processing method. In this paper, we report our
fabrication of the slicer optics elements in detail. As a result, we achieved the slice mirror with the micro-roughness of
RMS 12nm and the angle accuracy of under 0.0041deg, the pupil mirror with the micro-roughness of RMS 20nm and
the shape accuracy of PV 3micron, and the pseudo slit mirror with the angle accuracy of 0.02deg. All of the parts
fabricated satisfy the required specification.
We are developing a new infrared camera MAX38 (Mid-infrared Astronomical eXplorer) for long mid-infrared (25-40
micron) astronomy for the Univ. of Tokyo Atacama 1.0-meter telescope which is the world highest infrared telescope at
5,640m altitude. Thanks to the high altitude and dry weather condition of the Atacama site we can access the 30-micron
wavelength region from ground-based telescopes for the first time in the world. We employ a Si:Sb 128×128 array
detector to cover the wide mid-infrared wavelength range from 8 to 38 micron.
The development of the MAX38 has been almost completed. Test observations in N-band wavelength at Hiroshima
Kanata telescope (Hiroshima, Japan) was successfully carried out on June 2007 and March 2008. The first 30-micron
observation at Atacama is scheduled in the spring of 2009.
KEYWORDS: Coronagraphy, Cameras, Point spread functions, Data modeling, Glasses, Microscopes, Space telescopes, Absorbance, Numerical simulations, Signal attenuation
Prolate (Pupil) Apodized Lyot Coronagraphs (PPALC) are known to offer optimal performances for a Lyot-type
Coronagraph configuration, i.e. with an opaque occulting focal mask. One additional benefit of PPALC is its possible
use in a multi-stage configuration. In theory, the coronagraphic performance can be QN, where Q is the energy rejection
factor of one stage (the first one), and N the number of stages. Several ground-based telescopes are considering PPALC
as an option for their high-contrast instrumentation (e.g. Gemini/GPI, EELT/EPICS, Subaru HiCIAO). Although the
PPALC suffers from several limitations, several works are currently focused on fabricating entrance pupil apodizers and
trying to find ways to overcome chromatism issues. In this work, we present the first experimental results from Multi-Stage PPALC (MS-PPALC) that was done in the context of the Japanese space telescope SPICA coronagraph project.
Our entrance pupil apodizers use small diameter High Energy Beam Sensitive glass (HEBS-glass) from Canyon
Materials Inc. The current results show modest coronagraphic performance due to uncompensated phase aberrations
inherent to HEBS-glass material. In addition, and due to these uncompensated phase aberrations, the present optical
configuration is an altered version of the originally planned set-up. However, we can demonstrate the validity the MS-PPALC
concept and compare it to numerical simulations.
KEYWORDS: Coronagraphy, Space telescopes, Telescopes, Point spread functions, Mirrors, Infrared telescopes, Binary data, James Webb Space Telescope, Photomasks, Wavefronts
We present the status of the development of a coronagraph for the Space Infrared telescope for Cosmology and
Astrophysics (SPICA). SPICA is the next generation of infrared space-borne telescope missions following to AKARI,
led by Japan. SPICA will carry a telescope that has a 3.5 m diameter monolithic primary mirror and the whole telescope
will be cooled to 4.5 K. It is planned to launch SPICA into the sun-earth L2 libration halo orbit using H II-A rocket in the
middle of the 2010s and execute infrared observations at wavelengths mainly between 5 and 200 micron. The SPICA
mission gives us a unique opportunity for coronagraph observations, because of the large telescope aperture, the simple
pupil shape, the capability of infrared observations from space, and the early launch. We have started development of the
SPICA coronagraph in which the primary target is direct observation of extra-solar Jovian planets. The main
wavelengths of observation, the required contrast and the inner working angle (IWA) of the SPICA coronagraph
instrument are set to be 5-27 micron, 10-6, and a few λ/D (and as small as possible), respectively, in which λ is the
observation wavelength and D is the diameter of the telescope aperture (3.5m). We focused on a coronagraph with a
binary shaped pupil mask as the primary candidate for SPICA because of its feasibility. Nano-fabrication technology
using electron beam lithography was applied to manufacture a high precision mask and a laboratory experiment with a
He-Ne laser (λ=632.8nm) was performed in air without active wavefront control. The raw contrast derived from the
average measured in the dark region reached 6.7×10-8. On the other hand, a study of Phase Induced Amplitude
Apodization (PIAA) was started in an attempt to achieve higher performance, i.e., smaller IWA and higher throughput. A
hybrid solution using PIAA and a shaped pupil mask was proposed. A laboratory experiment was performed using a He-
Ne laser with active wavefront control via a 32×32 channel deformable mirror. A raw contrast of 6.5×10-7 was achieved.
Designs of binary shaped pupil mask are presented for the actual SPICA pupil which is obstructed by the telescope's
secondary mirror and its support. Subtraction of point spread function (PSF) was also evaluated.
KEYWORDS: Mirrors, Space telescopes, Telescopes, Silicon carbide, Cryogenics, Infrared telescopes, James Webb Space Telescope, Space mirrors, Composites, Astronomy
SPICA (Space Infrared Telescope for Cosmology and Astrophysics) is a Japanese astronomical infrared satellite project
with a 3.5-m telescope. The target year for launch is 2017. The telescope is cooled down to 4.5 K in space by a
combination of newly-developed mechanical coolers with an efficient radiative cooling system at the L2 point. The
SPICA telescope has requirements for its total weight to be lighter than 700 kg and for the imaging performance to be
diffraction-limited at 5 μm at 4.5 K. Material for the SPICA telescope mirrors is silicon carbide (SiC). Among various
types of SiC, primary candidates comprise normally-sintered SiC, reaction-sintered SiC, and carbon-fiber-reinforced
SiC; the latter two have been being developed in Japan. This paper reports the current design and status of the SPICA
telescope along with our recent activities on the cryogenic optical testing of SiC and C/SiC composite mirrors, including
the development of an innovative support mechanism for cryogenic mirrors, which are based on lessons learned from a
SiC 70 cm telescope onboard the previous Japanese infrared astronomical mission AKARI.
We present our high spectral resolution tandem Fabry-Perot (FP) spectrometer for detecting the pure rotational
transition line of molecular Hydrogen S (1) at 17.035 μm. It is designed to be attached to a new dedicated 1
m telescope planned to be put at a dry and high-altitude site. The spectrometer has two sequentially placed
FP units (order 1000 and 99 with finesse >50) consisting of ZnSe etalons and one narrow band filter. We will
be able to obtain high spectral resolution of R=50,000 at 17.035 μm. The ZnSe etalons of 110mm diameter
with >94% reflectance are to be provided from Barr Associates. The interval and tilt of etalons are sensed and
regulated by piezo actuators and newly-developed capacitance sensors, which resolve 100nm in vacuum and 30K
environment. By changing the interval, we change the wavelength of transmission up to 17.2 μm, corresponding
toν = 3000 km/s. We adopt an on-axis catadioptric system, in which the two FP units are placed. The focal
plane detector is a Raytheon SB-774, 320×240 pixel array of Si:As, yielding 9.1 × 6.8 arcmin2 field of view with
1.7 arcsec pixel scale. To suppress the thermal background radiation and dark current of the Si:As detector, the
system is cooled down to 6K at the detector and 35K for the whole optical system by two refrigerators. The
development of spectrometer will be completed in 2007.
A spectrometer with integral field units on large optical/infrared telescopes enables efficient spectroscopy of moderately extended objects. In future mid-infrared observations with 30m class telescopes, where circumstellar disks larger than the spatial resolution will be major targets, such efficient observations are strongly desirable. Here we present an optical design of our new N-band image slicing spectrometer to test basic techniques for future image slicing spectrometers on larger telescopes. Our prototype image slicer follows the idea of the advanced image slicer considering not only object images but also pupil images and is optimized for the N-band (10 micron atmospheric window). Five slicing mirrors and five pupil mirrors are used to slice the field of view and make a rearranged pseudo slit image. The pseudo slit image is collimated, dispersed by a grating, and imaged on a Si:As 320x240 array. For the slicing mirrors, we plan to use polished stainless mirrors of 300 micron width. The spectral resolution is set as about 200. We plan to put an imaging optics module for target aquisition in addition to the simple image slicer module. The whole optics is designed to be compact (about 600mm x 450mm x 300 mm), which will allow us to make test observations easily with various telescopes.
We present the status of the development of a coronagraph for the Space Infrared telescope for Cosmology and
Astrophysics (SPICA). SPICA is the next generation infrared space-borne telescope missions led by Japan. The SPICA
satellite will be equipped with a telescope that has a 3.5 m diameter monolithic primary mirror and the whole telescope
will be cooled to 4.5 K. The satellite is planed be launched early in the 2010s into the sun-earth L2 libration halo orbit
and execute infrared observations at wavelengths mainly between 5 and 200 micron. The SPICA mission gives us a
unique opportunity for coronagraph observations, because of the large telescope aperture, a simple pupil shape,
capability of infrared observations from space and the early launch. We have started development of the SPICA
coronagraph in which the primary target is direct observation of extra-solar Jovian planets. The main wavelengths of
observation, the required contrast and the inner working angle (IWA) of the SPICA coronagraph instrument are set to be
5-20 micron, 106, and approximately 5 λ/D respectively, whereλ is the observation wavelength and D is the diameter of
the telescope aperture. Coronagraphs using a checkerboard mask and a concentric ring mask have been investigated. We
found some solutions for the SPICA pupil, which has a large obstruction due to the secondary mirror and its supports.
We carried out laboratory experiments to examine coronagraphs obtained using checkerboard-type pupil masks with a
central obstruction. Nano-fabrication technology with electron beam was applied to manufacture a high precision mask
consisting of a patterned aluminum film on a glass substrate and its performance was confirmed by experiments with
visible light. Contrast higher than 106 was achieved. In the future, we will be developing a cryogenic mid-infrared
test-bed to investigate the SPICA coronagraphs.
KEYWORDS: Space telescopes, Telescopes, Mirrors, Silicon carbide, Infrared telescopes, Cryogenics, James Webb Space Telescope, Optical instrument design, Silicon, Far infrared
The Space Infrared Telescope for Cosmology and Astrophysics (SPICA) mission is the third Japanese astronomical infrared satellite project of a 3.5m cooled telescope optimized for mid- to far-infrared observations, following the Infrared Telescope in Space (IRTS) and the ASTRO-F missions. It will employ mechanical coolers and an efficient radiative cooling system, which allow us to have a cooled (4.5K) telescope of the aperture much larger than previous missions in space. The SPICA will attack a number of key problems in present-day astrophysics, ranging from the origin of the universe to the formation of planetary systems, owing to its high spatial resolution and unprecedented sensitivity in the mid- to far-infrared. The large aperture size for cryogenically use is, however, a great challenge and demands substantial technology developments for the telescope system. We adopt monolithic mirror design in the baseline model because of the technical feasibility and reliability. We set the optical performance requirement as being diffraction limited at 5μm at the operating temperature of 4.5K. The total weight attributed to the telescope system is 700kg, which requires a very light 3.5m primary mirror together with the mirror support structure. At present we are working on two candidate materials for the SPICA telescope: silicon carbide (SiC) and carbon-fiber reinforced silicon carbide (C/SiC). This presentation gives a general overview of the SPICA mission and reports the current design and status of the SPICA telescope system, including recent progress of the development of C/SiC mirrors.
The MIR-L is the mid-IR (12-26 μm) instrument for Japanese infrared astronomical satellite, the ASTRO-F. The instrument has 2 observing modes: a wide field imaging mode with a field of view of 10.7 × 10.2 arcmin2 and a low resolution spectroscopic mode with a spectral resolution R = λ/Δλ about 20. The spectroscopic mode provides with not only slit-spectroscopy for extended sources but also slitless-spectroscopy for point sources. We describe here the design, manufacturing, and performance evaluation of the cryogenic optical system of the MIR-L. The concept of the optical system design is to realize wide field observations with a compact size. The instrument employs a refractive optics of 5 lenses (CsI - CsI - KRS-5 - CsI - KRS-5) with a 256×256 pixel Si:As IBC array detector, 3 filters, and 2 grisms. The refractive indices of CsI and KRS-5 at the operating temperature of about 6 K have ambiguities because of the difficulty of the measurements. We therefore designed the MIR-L optics with tolerances for the uncertainties of the indices. Since both CsI and KRS-5 have the fragility and the large thermal expansion, we designed a specialized mounting architecture to prevent from making damages and/or decentrations of the lenses at cryogenic temperatures under the serious vibration during the launch. As a result, the optical system of the MIR-L has passed both vibration and thermal cycle tests without damage and performance degradation, and achieved diffraction limited performance over its full wavelength range at the operating temperature.
The ASTRO-F is an on-going infrared satellite mission covering 2-200 μm infrared wavelengths. Not only the all-sky survey in the mid-IR and far-IR, but also deep pointing observations are planned especially at 2-26 μm. In this paper, we focus on the near-infrared (NIR) channel of the infrared camera (IRC) on board ASTRO-F, and describe its design, and results of the imaging mode performance evaluation as a single component. The NIR consists of 4 lenses (Silicon - Silicon - Germanium - Silicon) with a 412 * 512 In:Sb detector. Three broad-band filters, and two spectroscopic elements are installed covering 2-5 μm wavelengths. Since the ASTRO-F telescope and the focal plane are cooled to 6 K, the evaluation of adjustment of the focus and the end-to-end test of the whole NIR camera assembly have to be done at cryogenic temperature. As a result of measurements, we found that the transverse magnification and distortion are well matched with the specification value (1 versus 1.017 and 1 %), while the chromatic aberration, point spread function, and encircled energy are slightly degraded from the specification (300 μm from 88 μm, > 1pixel from ~ 1pixel, 80 % encircled energy radius > 1pixel from ~ 1pixel). However, with these three measured values, in-flight simulations show the same quality as specification without degradation. In addition to the image quality, we also verified the ghost image generated from the optical element (1 % energy fraction to the original image) and the slightly narrowed field of view (10' * 9.5' from 10' * 10'). For the responsivity, the NIR shows expected response. Totally, the NIR imaging mode shows satisfactory results for the expected in-flight performance.
An all-sky survey in two mid-infrared bands which cover wavelengths of 5-12um and 12-26μm with a spatial resolution of ~9" is planned to be performed with the Infrared Camera (IRC) on board the ASTRO-F infrared astronomical satellite. The expected detection limits for point sources are few tens mJy. The all-sky survey will provide the data with sensitivities more than one order of magnitude deeper and with spatial resolutions an order of magnitude higher than the Infrared Astronomical Satellite (IRAS) survey.
The IRC is optimally designed for deep imaging in pointing observations. It employs 256x256 Si:As IBC infrared focal plane arrays (FPA) for the two mid-infrared channels. In order to make observations with the IRC during the survey mode of the ASTRO-F, a new operation method for the arrays has been developed - the scan mode operation. In the scan mode, only 256 pixels in a single row aligned in the cross-scan direction on the array are used as the scan detector and sampled every 44ms. Special cares have been made to stabilize the temperature of the array in the scan mode, which enables to achieve a low readout noise compatible with the imaging mode (~30 e-). The flux calibration method in the scan mode observation is also investigated. The performance of scan mode observations has been examined in computer simulations as well as
in laboratory simulations by using the flight model camera and moving artificial point sources. In this paper we present the scan mode operation method of the array, the results of laboratory performance tests, the results of the computer simulation, and the expected performance of the IRC all-sky survey observations.
The SPICA (Space Infrared Telescope for Cosmology and Astrophysics), which is a Japanese astronomical infrared satellite project with a 3.5-m telescope, is scheduled for launch in early 2010s. The telescope is cooled down to 4.5 K in space by a combination of mechanical coolers with an efficient radiative cooling system. The SPICA telescope has requirements for its total weight to be lighter than 700 kg and for the imaging performance to be diffraction-limited at 5 µm at 4.5 K. Two candidate materials, silicon carbide (SiC) and carbon-fiber-reinforced SiC (C/SiC composite), are currently under investigation for the primary mirror. A monolithic mirror design will be adopted in both cases because of the technical feasibility and reliability. This paper reports the current design and status of the SPICA telescope together with some of our recent results on laboratory cryogenic tests for the SiC and C/SiC composite mirrors.
The Infrared Camera (IRC) is one of the focal-plane instruments on board the Japanese infrared astronomical space mission ASTRO-F. It will make wide-field deep imaging and low-resolution spectroscopic observations over a wide spectral range in the near- to mid-infrared (2-26um) in the pointed observation mode of the ASTRO-F. The IRC will also be operated in the survey mode and make an all-sky survey at mid-infrared wavelengths. It comprises three channels. The NIR channel (2-5um) employs a 512x412 InSb array, whereas both the MIR-S (5-12um) and the MIR-L (12-26um) channels use 256x256 Si:As impurity band conduction (IBC) arrays. The three channels will be operated simultaneously. All the channels have 10'x10' fields of view with nearly diffraction-limited spatial resolutions. The NIR and MIR-S share the same field of view, while the MIR-L will observe the sky about 25' away from the NIR/MIR-S field of view. The IRC will give us deep insights into the formation and evolution of galaxies, the properties of brown dwarfs, the evolution of planetary disks, the process of star-formation, the properties of the interstellar medium under various physical environments, as well as the nature and evolution of solar system objects. This paper summarizes the latest laboratory measurements as well as the expected performance of the IRC.
We report the surface structure and roughness of the mirrors made of carbon fiber reinforced silicon carbide (C/SiC) composite improved for the SPICA (Space Infrared telescope for Cosmology and Astrophysics) mission. The improved C/SiC is a candidate of material for the SPICA light weight mirrors because of its superior properties: high toughness, high stiffness, small thermal deformation, feasibility to make large single dish mirror, low cost, and short term for production. The surface of the bare C/SiC composite consists of carbon fiber, silicon carbide and silicon, each of which has different hardness, so it is difficult to polish this surface smoothly. Our improved polishing technique achieved the surface roughness of better than 20nm RMS for the C/SiC composite flat mirror, which satisfies the requirement of the SPICA mission. For curved bare surface of the C/SiC mirror, the roughness is larger than 30 nm and now under improving. The Change of Bidirectional reflectance distribution function (BRDF) of the bare C/SiC composite at cryogenic temperature was measured with 632.8nm lasar. No significant difference was found between the BRDFs at 95K and that at room temperature. In order to improve surface roughness further, we are planning to apply the SiSiC slurry coating on the surface of the improved C/SiC composite. This combination can realize the surface roughness well enough to be applied even for optical telescopes.
MIR-L is a 12-26μm channel of Infrared Camera(IRC) onboard ASTRO-F. The camera employs a refractive optics which consists of 5 lenses (CsI - CsI - KRS-5 - CsI - KRS-5) and a large format Si:As IBC array detector (256 x 256 pixels). The design concept is to realize a wide field of view with a compact size. It has 2 observing modes: a wide field imaging with a field of view of 10.7 x 10.2arcmin2 or a pixel resolution of 2.5 x 2.4arcsec2/pixel in 3 bands (12.5-18μm, 14-26μm, 22-26μm), and low resolution spectroscopy with a spectral resolution R = λ/Δλ
≈40 in 2 bands 11-19μm,18-26μm). It also has a small slit to adapt for spectroscopic observations of extended sources. We describe the current design of the optics and the mounting architecture of MIR-L and evaluation of the optical performance at cryogenic temperatures.
We developed a new data acquisition device for COMICS, a mid
infrared instrument of the Subaru telescope. The new device was
installed in place of our previous data acquisition device with a lower data transfer speed. The new device is 32 bit PCI bus and PC Linux based and provides bus-master DMA transfer function. It consists of a clock pattern generator, frame memories, and an image co-adder. In order to achieve high operational efficiency for mid infrared instruments, the data handling speed is essential as well as the speed of A/D converter. The data transfer to the hard disk drive on the PC is made during acquiring the data at the rate
higher than the data generation rate. As a result, we succeeded
to reduce the dead time due to the data transfer procedure from
60 sec to less than 1 sec for 200 frames (64M bytes). Furthermore
by replacing the host computer by a higher performance PC, the
observation efficiency of COMICS was improved from 44% to 74%
in the imaging mode. This PCI based data acquisition device can
also be applied to the other instruments that have fast data rates.
COMICS is an observatory and mid-infrared instrument for the 8.2 m Subaru Telescope. It is designed for imaging and spectroscopic observations in the N- (8-13 micron) and Q-bands (16-25 micron) atmospheric windows. The design and very preliminary performances at the first light observations in December 1999 were reported at the SPIE meeting in 2000. We describe here the improved performances of COMICS and capability of high spectral resolution spectrocopy which became available from December 2001. We will also briefly report preliminary scientific results.
The infrared camera(IRC) onboard ASTRO-F is designed for wide-field imaging and spectroscopic observations at near- and mid-infrared wavelengths. The IRC consists of three channels; NIR, MIR-S and MIR-L, each of which covers wavelengths of 2-5, 5-12 and 12-26 micron, respectively. All channels adopt compact refractive optical designs. Large format array detectors (InSb 512x412 and Si:As IBC 256x256) are employed. Each channel has 10x10 arcmin wide FOV with diffraction-limited angular resolution of the 67cm telescope of ASTRO-F at wavelengths over 5 micron. A 6-position filter wheel is placed at the
aperture stop in each channel, and has three band-pass filters, two grisms/prisms and a mask for dark current measurements. The 5 sigma sensitivity of one pointed observation is estimated to be 2, 11 and 62 micro-Jy at 4, 9, 20 micron bands, respectively. Because ASTRO-F is a low-earth orbiting satellite, the observing duration of each pointing is limited to 500 seconds. In addition to pointed observations, we plan to perform mid-infrared scanning observation.
Fabrications of the flight-model of NIR, MIR-S, and the warm electronics have been mostly completed, while that of MIR-L is underway. The performance evaluation of the IRC in the first end-to-end test (including the satellite system) is presented.
We report on the extensive tests to characterize the performance of the infrared detector arrays for the Infrared Camera (IRC) on board the next Japanese infrared astronomical satellite, ASTRO-F. The ASTRO-Fwill be launched early 2004 and the IRC is one of the focal plane instruments to make observations in 2-26μm. For the near-infrared observations of 2-5μm, a 512x412 InSb array will be employed, while two 256x256 Si:As arrays will be used for the observations of 5-26μum in the IRC. Both arrays are manufactured by Raytheon.
To maximize the advantage of the cooled telescope and extremely low background radiation conditions in space, the dark current and readout noise must be minimized. The heat dissipation of the arrays also has to be minimized. To meet these requirements and achieve the best performance of the arrays, we optimized the array driving clocks, the bias voltage, and the supply currents, and evaluated the temperature dependence of the performance. In particular, we found that the voltage between the gate and source of the FET of the multiplexer SBRC-189 had a strong dependence on temperature. This effect becomes a dominant source for the noise unless the temperature
is kept within 20mK. We have achieved the readout noises of about 30e- and 40e- with the correlated double sampling for the flight model readout circuits of the InSb and Si:As arrays, respectively. These noises ensure that the background-limited performance can be achieved for the observations of IRC in the 4-26μm range in the current observing scheme.
In addition, we are now planning to make scan mode observations by IRC. We have developed a new operation way of the arrays to achieve the stable response and low readout noise in the scanning operation for the first time.
The IRC is now installed in the flight model cryostat and the first
end-to-end test has just been completed. We report on the expected performance of the IRC together with the array test results.
We have developed the mid-IR Camera and Spectrometer (MICS), which optimized for ground based observations in the N-band atmospheric window. The MICS has two observing capabilities, imaging and long slit low-resolution spectroscopy. The major characteristics of the MICS are nearly diffraction-limited performance, both in imaging and in spectroscopy and the capability to take a spectrum of the whole N-band range with a spectral resolving power of 100 under one exposure. The MICS employs a 2D array of 128 by 128 Si:As BIB detector, an aberration-corrected concave grating, and a high-speed read out system of a compact design with high sensitivity. In mid-IR observations form the ground, there is a large background radiation from the telescope and the sky. The fluctuation of the background radiation is not well understood so far. We measured the sky fluctuation in the N- band region with the MICS on the UKIRT. These measurements have revealed that (1) the sky noise was dominant below 0.5 Hz when the sky condition was good, and (2) the sky noise has strong excess at the positions of atmospheric water vapor lines than those without water vapor lines. In this paper, we describe the design of the MICS, including optics, cryogenics, and electronics, and its performance when used on the UKIRT. We also discuss sky noise measured by the MICS in the N-band region.
In this paper, we present the design and test performance of the COMICS, the mid-IR instrument for the 8.2 m Subaru Telescope at Mauna Kea. The instrument has both imaging and long slit grating spectroscopy capabilities in the 8-26 micrometers wavelength range. In the camera section, there are selectable three sets of lens assembly, one for the 10 micrometers imaging, another for the 20 micrometers imaging, and the other for the 10 micrometers pupil imaging. This camera section has an SBRC 320 X 240 Si:As IBC array and serves as a slit viewer and as a camera pixel scale of 0.130 arcsec. The spectrograph section is designed to have fiber SBRC 320 X 240 Si:As IBC arrays. Five arrays will cover 8-13 micrometers wavelength range in two positions of the grating with resolving power around 2500. So far, two arrays are installed for the spectrograph section and full spectral region is covered with tilting the grating. Selectable four sets of gratings provide spectral resolution ranging from 250 to 10000 in the N band and around 2500 in the Q band.
The infrared instrumentation plan for the Subaru telescope is described. Four approved infrared instruments and one test observation system are now in the construction phase. They are coronagraph imager using adaptive optics (CIAO), cooled mid- infrared camera and spectrograph (COMICS), infrared camera and spectrograph (IRCS), OH-airglow suppressor spectrograph (OHS) and mid-infrared test observation system (MIRTOS). Their performance goals and construction schedules are summarized. The plan for procurement and evaluation of infrared arrays required by these instruments is briefly described.
We have constructed a near-infrared camera with a 1040 by 1040 PtSi CSD array for astronomical use. The camera is attached to the prime focus (f/3.1) of the 105 cm Schmidt telescope at Kiso observatory. The field of view is 18.4 by 18.4 arcmin2 and the spatial resolution is 1.06 by 1.06 arcsec2/pixel. The camera can be used mainly in J ((lambda) eff equals 1.25 micrometer), H (1.65 micrometer), and K' (2.15 micrometer) bands. Since thermal emissions from the atmosphere and room-temperature bodies are main background noise sources in the near-infrared, we designed a cold baffle inside the camera to minimize the effect of the thermal radiation from the telescope. Both the charge transfer efficiency and the dark current of PtSi arrays are sensitive to the array temperature. Therefore we carefully control the temperature at 60 +/- 0.05 K by using a refrigerator and a temperature controller. The readout noise was reduced to 70 e by adopting a correlated multiple sampling technique. The array response was linear within 0.7% accuracy below 25% of the full well capacity (< 4.0 X 105 e).
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