The Superconducting Submillimeter-Wave Limb-Emission Sounder-2 (SMILES-2) is a satellite mission for observation of the stratosphere, mesosphere, and lower thermosphere with superconducting submillimeter-wave receivers, being proposed to the announcement of opportunity for M-class missions run by the Japan Aerospace Exploration Agency (JAXA). The SMILES-2 notable features are extremely high sensitivity and observation capability of atmospheric diurnal cycles. Those are requested from a scientific requirement for the investigation of the 4-D space-time structure of diurnal variations in the whole atmosphere. Such features require SMILES-2 to have 4–K cooled superconducting devices for high sensitivity and to be aboard a satellite platform on a non-sunsynchronous orbit. The mechanical 4–K cooling system is a power consuming instrument. Satellite on a non- sunsynchronous orbit gets a large sun-shade ratio in most of season, and has limitations of power supply to the mission instrument. The issue of the SMILES-2 mission design is mainly to fit the 4–K cooling system to the limited power resource of M-class satellite. This paper discusses our development status on designing the SMILES-2 mission payload. SMILES-2 will be proposed to JAXA in the beginning of the next year.

The Superconducting Submillimeter- Wave Limb-Emission Sounder 2 (SMILES-2) is a satellite mission to observe the stratosphere, mesosphere, and lower thermosphere with superconducting submillimeter receivers. SMILES-2 aims at studying the dynamical, chemical, and electromagnetic coupling of the middle and upper atmosphere with an unprecedented high-precision observations of multiple atmospheric parameters from a platform on a non-sunsynchronous orbit. SMILES-2 consists of superconducting receivers at frequencies between 619 GHz and 2.06 THz. The GHz receivers observe mainly the temperature, wind, and chemical compositions in the stratosphere and mesosphere. The frequency band of 640 GHz receiver includes the band investigated by JEM/SMILES mission, which was operated during the period from 2009 to 2010. The THz receiver, a new channel of SMILES-2, is devoted to measurement of atomic oxygen for observation of the lower thermospheric temperature and wind. The SIS mixer of GHz receiver and HEB mixer of THz receiver are cooled down to around 4 K by a mechanical cryocooler, which is designed to have 3 year lifetime and 5 year goal. The SMILES-2 payload is estimated to be less than 200 kg and consume power of 300 to 400 W. SMILES-2 is proposed for a mission installed on 500 kg size satellite of the Japan Aerospace Exploration Agency (JAXA).

Superconducting devices were used to make atmospheric limb observations from space for the first time. The Superconducting Submillimeter-Wave Limb-Emission Sounder (SMILES) is a superconductor-insulator-superconductor (SIS) receiver in frequency bands of 625 and 650 GHz. SMILES was deployed on the International Space Station. SMILES observed atmospheric limb spectra for six months from October 2009 to April 2010. The sensitivity of the receiver is the most important performance parameter for microwave atmospheric limb observation, in which the receiver measures, sometimes very weak, thermal line emissions. The SMILES SIS receivers demonstrated limb observations with a sensitivity more than one order of magnitude better than that of conventional limb sensors. The sensitivity of the SMILES receivers in space was 315 K-322 K in a definition of single-sideband system noise temperature at the antenna; this met the instrument requirement with a large margin. The SMILES-receiver stability also met the requirement; the stability time of the receiver was 8 s (and 500 s for spectroscopic data) in a frequency resolution of about 1.1 MHz. Although the stability time is shorter than the calibration period (53 s) in operational observation, the variance increment by the drift noise is found to be insignificant. The temperature resolution for the continuum signal is estimated to be better than 0.27 K. There was no evidence that the stability of the SIS receiver was influenced by the temperature fluctuation of the 4-K cooling system, which consists of a two-stage Stirling cooler and a Joule-Thomson cycle cooler. The suppression of baseline ripples is another important performance parameter of the receiver for spectral measurement like the SMILES receivers. As a result of our design of low-standing-wave optics, we found no baseline ripple in the observed spectra of SMILES in practical level.

Superconducting Submillimeter-Wave Limb-Emission Sounder (SMILES) has been operated on orbit since late September 2009. The on-orbit performance of the SMILES submillimeter receiver satisfied the specifications and demonstrated a high capability of superconducting technology for atmospheric science by providing an invaluable low-noise atmospheric limb-emission spectral data in 640-GHz band. The accuracy of the limb spectral data are going to be improved by radiometric calibration based on the instrumental knowledge measured on the ground and measurements on orbit. The observation by SMILES was unfortunately halted because of a failure of the submillimeter-wave local oscillator on 21 April 2010.

A balloon-borne superconducting submillimeter-wave limb-emission sounder (BSMILES) was developed to observe thermal emission lines from stratospheric minor constituents. BSMILES carries a 300-mm-diameter offset parabolic antenna, a 624-639-GHz superconductor-insulator-superconductor (SIS) receiver, a three-axis fiber-optical gyroscope, and an acousto-optical spectrometer. BSMILES was launched from the Pacific Coast of Japan. All systems operated properly and emission line spectra of stratospheric gases, such as O/sub 3/, HCl, HO/sub 2/, and O/sub 3/ isotopes were measured. The system noise temperature in double sideband (DSB) during the flight was less than 460 K over the observing bandwidth with a best value of 330 K that is 11 times as large as the quantum limit (11h/spl nu//k/sub B/). After the observation, the gondola splashed down in the Pacific Ocean and was retrieved. Almost all instruments were waterproofed, and it has been proved that they are reusable.

We have developed a balloon-borne superconducting submillimeter-wave limb-emission sounder (BSMILES) to determine vertical profiles of stratospheric minor constituents like ozone and a number of key species related to ozone destruction by observing thermal emission lines from these molecules. BSMILES carries a 624-652 GHz superconductor-insulator-superconductor (SIS) receiver with the system noise temperature of 330-460 K in double sideband (DSB) during the flight. BSMILES flight experiments were conducted on August 30, 2003 and September 7, 2004 from the Pacific Coast of Japan. The system operated properly and spectra of O/sub 3/, ClO, HCl, HO/sub 2/, O/sub 3/ isotopes were successfully measured. After the observation, the gondola splashed down in the Pacific Ocean and was retrieved.

Stratospheric O/sub 3/ and ClO were simultaneously observed off the northeastern coast of Japan by the Balloon-Borne Superconducting Submillimeter-Wave Limb-Emission Sounder (BSMILES) developed at National Institute of Information and Communications Technology. BSMILES is a highly sensitive submillimeter radiometer that exploits the superconductor-insulator-superconductor (SIS) technology for atmospheric research. This paper presents the first BSMILES spectra, and describes the details of the calibration process. The vertical profiles of O/sub 3/ and ClO have been also retrieved. In spite of some calibration uncertainties the obtained profiles are in relatively good agreement with previous and other available measurements.

A new 17-GHz radio interferometer dedicated for solar observations was constructed in two years at Nobeyama, Nagano. It consists of eighty-four 80-cm-diameter antennas arranged in a tee-shaped array extending 490 m in east-west and 220 m in north-south directions. Since late June of 1992, radio full-disk images of the Sun have been observed for 8 h every day. The spatial resolution is 10" and the temporal resolution is 1 s and also 50 ms for selected events. Every 10 s correlator data are synthesized into images in real time and displayed on a monitor screen. The array configuration is optimized to observe the whole Sun with high spatial and temporal resolution and a high dynamic range of images. Image quality of better than 20 dB is realized by incorporation of technical advances in hardware and software, such as (1) low-loss phase-stable optical-fiber cables for local reference signal and IF signals, (2) newly developed phase-stable local oscillators, (3) custom CMOS gate-array LSTs of 1-b quadraphase correlators for 4/spl times/4 combinations, and (4) new image processing techniques to suppress large sidelobe effects due to the solar disk and extended sources.>