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Background Excessive alcohol consumption is a social problem. According to the World Health Organization, approximately three million deaths were attributed to alcohol consumption, which is 5.3% of all deaths. Despite this high mortality, only a small number of alcoholics receive alcoholism treatment, and many do not receive it. The reason for the lack of progress in the treatment of alcohol dependence or alcohol use disorders (AUD) has been that the goal of sobriety is a hurdle for alcoholics. Abstinence is a common therapeutic goal, but the perception that abstinence is the only treatment goal may discourage treatment-seeking. Recently, it was reported that the prognosis at one year was the same for both abstinence and moderation use goals in the treatment of alcohol dependence and that it was important for patients to choose their own treatment goal of abstinence or reduction in alcohol consumption to continue treatment. Therefore, medication to reduce drinking is used for patients whose treatment goal is to reduce drinking. In the past, a network meta-analysis (NMA) of pharmacologically controlled drinking in the treatment of alcoholism or AUD has been reported. The review summarizes existing data from randomized controlled trials up to June 2016. However, in recent years, there have been several reports that there are some drugs that can be expected to reduce alcohol consumption including anticonvulsants, and some RCTs of drugs to reduce alcohol consumption have been reported. This systematic review and NMA aimed to summarize and critically appraise all existing evidence on the efficacy and safety of drug therapy for reducing alcohol consumption in the treatment of alcohol dependence or AUD. Purpose The purpose of this study is to conduct an updated review of efficacy and safety of drug therapy aimed at reducing alcohol consumption in the treatment of alcohol dependence or AUD. Method and analysis [Part 1] Updated review of drug therapy aimed at reducing alcohol consumption in the treatment of alcohol dependence or AUD (clinical definition) The purpose of our review is to update efficacy and safety of drug therapy aimed at reducing alcohol consumption in the treatment of alcohol dependence or AUD. We describe this protocol that follows the Cochrane Handbook for Systematic Reviews of Interventions and the PRISMA extension statement for reporting of systematic reviews. [Part 2] Systematic review and meta-analysis of drug therapy aimed at reducing alcohol consumption in the treatment of alcohol dependence or AUD Based on the updated review above, we will design PICO and conduct a systematic review and meta-analysis to examine the efficacy and safety of drug therapy aimed at reducing alcohol consumption in the treatment of alcohol dependence or AUD. We used a systematic review protocol template (dx.doi.org/10.17504/protocols.io.bu4qnyvw). We followed the Preferred reporting items for systematic review and meta-analysis protocols (PRISMA extension statement for reporting of systematic reviews) 2015 for preparing this protocol. Ethics and dissemination In this systematic review, only data from previously conducted studies will be analyzed. We will publish this systematic review in peer-reviewed journals.

The Simultaneous-color Wide-field Infrared Multi-object Spectrograph (SWIMS) is one of the 1st generation facility instruments for the University of Tokyo Atacama Observatory (TAO) 6.5 m telescope currently being constructed at the summit of Cerro Chajnantor (5,640 m altitude) in northern Chile. SWIMS has two optical arms, the blue arm covering 0.9–1.4 µm and the red 1.4–2.5 µm, by inserting a dichroic mirror into the collimated beam, and thus is capable of taking images in two filter-bands simultaneously in imaging mode, or whole nearinfrared (0.9–2.5 µm) low-to-medium resolution multi-object spectra in spectroscopy (MOS) mode, both with a single exposure. SWIMS was carried into Subaru Telescope in 2017 for performance evaluation prior to completion of the construction of the 6.5 m telescope, and successfully saw the imaging first light in May 2018 and MOS first light in Jan 2019. After three engineering runs including the first light observations, SWIMS has been accepted as a new PI instrument for Subaru Telescope from the semester S21A until S22B. In this paper, we report on details of on-sky performance of the instrument evaluated during the engineering observations for a total of 7.5 nights.

Since the University of Tokyo Atacama Observatory (TAO) is located in extremely high altitude (5,640 m.a.s.l.), safety management is one of the most important issues for the project. We have developed safety management program for work at the site in order to prevent medical illness for humans. In this program all staff have to take medical examinations such as Electrocardiogram and Hipobaria before their work starts. The results are reviewed by medical doctor. Only authorized staff can be permitted to work at the site. During stay in site, all staff need to always use oxygen supply because there is only half of the oxygen at the site. It is also important to understand physical workload at the site. Our safety staff reviews it and determines necessary resting time for each worker, e.g. great load works need to work 50 minutes and rest 10 minutes. In addition to low air pressure, very low temperature, extremely high UV radiation, and extremely dry atmosphere should be concerned. Our program requests all staff to use winter clothes, sunblock and UV protection sunglasses and a lot of potable water consumption. Keep communication is also very important to secure the safety. Normal telephone communication is not available as well as internet connectivity. We have established satellite communication as well as UHF internal communication for general works and safety coordination with other observatories in Atacama area.

The telescope of the University of Tokyo Atacama Observatory has a primary mirror with a diameter in 6.5m. In order to fabricate the reflecting film initially on the mirror surface and to maintain its optical performance over a long period, a mirror{coating facility will be installed in operation building beside enclosure of the telescope at the summit of Co. Chajnantor (5,640m). The facility consists of mirror coating chamber, cleaning unit for stripping off the old film and clean-up the mirror, and a cart with a lifter for handling the primary mirror cell. Almost all equipment, including the main chamber, was completed by early 2020 and engaged as a mirror coating facility. In order to optimize the coating parameters, comprehensive performance tests were carried out (without primary mirror cell which plays a role of a part of chamber). The evaluation items are how long it takes to reach the target vacuum level and parameters of the current, voltage, and application time during ion bombardment and aluminization. Through iterating test, we were able to obtain each parameter that ultimately met the requirements of the TAO telescope mirror.

One of remarkable features of the University of Tokyo Atacama Observatory (TAO) is an altitude of the site (5,640 m.a.s.l.) While this provides us an excellent condition for astronomical observations, the site development is attended with difficulty due to the hard conditions such as low pressure, low temperature, and limited access. Site preparation for the TAO 6.5 m telescope started in Apr. 2018. Firstly, we have constructed an access road from Pampa la bola plateau (~ 5,000 m.a.s.l) to the summit. It has a width of < 6.5 meter for transportation of telescope parts including the 6.5meter mirror. In order to prevent collapse, angle of side slope is carefully determined based on ground condition and frozen soils. All workers always use oxygen during their work as a measure against hypobaropathy. Since the site temperature in night is lower than 0 degree even in the summer season, it is difficult to ensure quality of foundation concrete if we cast it in-situ. We use pre-cast concrete for the foundation of the telescope, the enclosure, and the support building. The biggest part is the telescope foundation. It has a weight of 600 ton. Considering the transportation to the summit, it is divided into 43 parts and unified at the summit. This is a new trial to make a massive foundation for a large telescope with pre-cast concrete.

The Near-Infrared Cross-dispersed Echelle spectrograph (NICE) is a first light instrument for the TAO 6.5 m telescope. The instrument covers a wavelength range of 0.9 to 2.4 µm and has a resolving power of λ/∆λ ~2,600. NICE was first used on the 1.5 m infrared telescope at the National Astronomical Observatory of Japan from 2001 to 2005 and on the 1.6 m Pirka telescope in Japan from 2009 to 2018. We are now upgrading the cryogenics and computer system for the installation of NICE on the TAO telescope. Here we report on the current status and future schedules of instrumentation updates, control system, and modified specifications of NICE for its transfer to the TAO 6.5 m telescope.

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 (

Ice rich permafrost is observed at Chajnantor volcano (5,640m a.s.l.) on the University of Tokyo Atacama Observatory (TAO) site. Presence or absence of the permafrost is considered to be requested quite different engineering skills for their infrastructures. Lower altitude boundary is reported to be above 5,079m a.s.l. and maximum active (thawing) layer is 14cm. Minimal seasonal temperature variation, small active layer thickness as the consequences of low numbers of thawing and freezing degree days. Diurnal amplitude results in freeze-thaw cycles only near the surface. Severe frost shattering occurs near the ground surface, producing a dusty, fine-material horizon called a hyper-cryogenic layer. The importance of the snow-covered season for providing great protection for surface energy penetration. Many permafrost hazards are expecting in this construction site such as frost heaving, subsiding, mass movements, erosion, chemical weathering, frost shattering, embankment instability, and

The University of Tokyo Atacama Observatory Project is to construct a 6.5 m infrared-optimized telescope at the summit of Co. Chajnantor (5640 m altitude) in northern Chile. The telescope optics uses a Ritchey-Chretien type layout, with an under-sized secondary mirror to reduce stray light caused by thermal emission from the telescope structure. The primary mirror is a F/1.25 lightweight borosilicate glass (Ohara E6) mirror with honeycomb structure, which is developed by Steward Observatory Richard F. Caris Mirror Lab. The telescope has two Nasmyth foci and two folded-Cassegrain foci, which can be switched by rotating a tertiary mirror. The final focal ratio is 12.2 with a field of view of 25 arcmin in diameter. The telescope mount is a tripod-disk alt-azimuth mount. Both the azimuth and elevation axes are supported by and run on hydrostatic bearings, and they are driven by friction drives with servo motors, which are controlled by the telescope control system. It also controls the hexapod mount of the secondary mirror and the pneumatic actuators of the primary mirror support to keep good image quality during the observation. An off-axis Shack-Hartmann sensor installed in each focus measures the wavefront aberration of the telescope optics, then the misalignment between the secondary and primary mirrors is corrected by adjusting the hexapod mount while other aberrations are corrected by the deformation of the primary mirror. The force distribution of the actuators for correction will be calculated by fitting the wave-front errors with a series of bending modes of the primary mirror.

Institute of Astronomy, Graduate School of Science, the University of Tokyo is promoting the University of Tokyo Atacama Observatory Project, which is to construct an infrared-optimized 6.5m telescope at the summit of Co. Chajnantor (5640m altitude) in northern Chile. The high altitude and dry climate (PWV-0.5mm) realize transparent atmosphere in the infrared wavelength. The project is now approaching the final phase of the construction. Production of major components are almost completed: Production and preassembly test of a telescope mount and dome enclosure have been completed in Japan, and they are being transported to Chile. Three mirrors, the 6.5m primary, 0.9m secondary, and 1.1m-0.75m tertiary mirrors and their support systems have been all completed and tested in the USA. An aluminizing chamber have been fabricated in China, and its tests have been carried out in Japan. Development of two facility instruments, SWIMS and MIMIZUKU, are also completed. They were transported to the Subaru telescope, successfully saw the first light in 2018, and are confirmed to have the performance as designed. On-site construction work at the summit is now underway. Expansion of a summit access road from the ALMA concession was completed in 2019. Installation of foundation will follow, and then erection of the dome enclosure and a control building. The construction works are delayed by COVID-19, and we expect to complete the dome enclosure by Q3 of 2021. The telescope will be installed inside the dome and see the engineering first light by early 2022.

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.

Kenji Washida,1,2 Toshihiko Takeda,2 Toshiaki Habara,2 Soichiro Sato,2 Takuro Oka,2 Masuo Tanaka,2 Yusaku Yoshimura,2 Shozo Aoki11Department of Psychiatry, Kawasaki Medical Graduate School, Kurashiki, Japan; 2Zikei Hospital, Okayama, JapanAim: The aim of this study was to examine the speed of response, doses, and safety of treatment with second-generation antipsychotics (SGAs) in patients at ultra-high risk (UHR) compared to those with schizophrenia.Methods: A 12-week open-label, prospective study of SGAs was performed in UHR patients and those with first-episode schizophrenia (FES) and multi-episode schizophrenia (MES). The subjects were 14–30 years old and were recruited at Zikei Hospital, Okayama, Japan from December 1, 2006 to December 1, 2011. Treatment was carried out in a natural setting in an open-label format, but clinical evaluation was performed blind. The clinical rating scales include the Global Assessment of Functioning (GAF), the Positive and Negative Syndrome Scale (PANSS), and the Clinical Global Impression-Severity scale (CGI-S).Results: UHR (n = 17), FES (n = 23), and MES (n = 21) patients all showed significant improvements on the GAF, PANSS, and CGI-S. However, the UHR patients showed significantly greater improvement on the GAF at weeks 4, 8, and 12 compared to the other groups, and a significantly lower modal dose of SGAs (chlorpromazine equivalent: 183 [201.1] mg/day, mean [SD]) was needed for improvement in the UHR group. Each group was also prescribed anticholinergic agents during the study period and the UHR group had significantly fewer extrapyramidal symptoms (only 6%) compared with the FES group.Conclusion: Our findings suggest that UHR patients have a better response to SGAs compared to patients with schizophrenia, and that these drugs can be given safely by minimizing the dosage of SGAs and using anticholinergic agents.Keywords: ultra-high risk, second-generation antipsychotics, schizophrenia

Simultaneous-color Wide-field Infrared Multi-object Spectrograph, SWIMS, is one of the first generation instruments for University of Tokyo Atacama Observatory 6.5m Telescope where almost continuous atmospheric window from 0.9 to 2.5μm appears, thanks to the high altitude and dry climate of the site. To utilize this excellent condition, SWIMS is capable of simultaneous two-color imaging with a field of view of 9’. in diameter and λ/Δλ ~1000 multi-object spectroscopy at 0.9–2.5μm in a single exposure, utilizing a dichroic mirror inserted in the collimated beam. Here, we overview the instrument, report results of its full-assembly tests in the laboratory and present the future plan.

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.

We present results on the computational fluid dynamics (CFD) numerical simulations as well as the wind tunnel experiments for the observation facilities of the University of Tokyo Atacama Observatory 6.5m Telescope being constructed at the summit of Co. Chajnantor in northern Chile. Main purpose of this study starting with the baseline design reported in 2014 is to analyze topographic effect on the wind behavior, and to evaluate the wind pressure, the air turbulence, and the air change (ventilation) efficiency in the enclosure. The wind velocity is found to be accelerated by a factor of ~ 1.2 to reach the summit (78 m sec-1 expected at a maximum), and the resulting wind pressure (3,750 N m-2) is used for the framework design of the facilities. The CFD data reveals that the open space below the floor of the facilities works efficiently to drift away the air turbulence near the ground level which could significantly affect the dome seeing. From comparisons of the wind velocity field obtained from the CFD simulation for three configurations of the ventilation windows, we find that the windows at a level of the telescope secondary mirror have less efficiency of the air change than those at lower levels. Considering the construction and maintenance costs, and operation procedures, we finally decide to allocate 13 windows at a level of the observing floor, 12 at a level of the primary mirror, and 2 at the level of the secondary mirror. The opening area by those windows accounts for about 14% of the total interior surface of the enclosure. Typical air change rate of 20-30 per hour is expected at the wind velocity of 1 m sec-1.

The telescope of the University of Tokyo Atacama Observatory has a primary mirror with a diameter in 6.5m. In order to fabricate the reflecting film initially on the mirror surface and to maintain its optical performance over a long period, we have a mirror-coating facility being installed at the summit of Co. Chajnantor (5,640m). The facility consists of a clean booth for stripping off the old film, a mirror coating chamber, and a cart with a lifter for handling the primary mirror. A conventional evaporation system with a metal pre-wetted filament array is adopted for achieving various optical requests. Among the many development items, the fabrication of the transportation and lifting cart has been already completed. It has efficient performance in load capacity (>60 tons) and maximum lifting height (1,750 mm). A cleaning machine having injection nozzles that can realize an efficient and safe cleaning sequence also been completed. A test of the evaporation system using dedicated filaments and filament boxes, which are customized to the TAO's requirements, has shown a uniform coating on a test mirror. An array pattern of the filaments has also been decided based on the coating tests to satisfy the optical specification of the telescope. A detailed design of the main chamber has been almost completed, it is only waiting for the production in the near future.

We made spectroscopic monitoring observations of the three yellow hypergiants ( Cassiopeia, HR 8752, and IRC+10420) in the 0.9–2.4 m wavelength range with a resolution of 2600 over a fifteen month period. The spectra of HR 8752 and IRC+10420 showed no time variations. On the other hand, those of Cas showed just a series of time variation in 2.3 m CO features from nondetection to absorption through emission during 2002–2004. We interpret this variation as being a result of an expanding gas shell whose excitation temperature was being cooled down to 800 K. The CO column densities were estimated from the CO absorption depths. Moreover, assuming spherical symmetry of the expanding shell with a constant expansion velocity of 35 km s , a stellar effective temperature of 7000 K, a stellar radius of 400 Rˇ, solar abundance, and all carbon atoms forming CO molecules, we estimated the mass of the shell to be 2 10 Mˇ for a model with a single shell expanding from the photosphere, or 5 10 Mˇ for another model with an expanding shell and a static envelope. These estimates of the released mass strongly depend on assumptions of the expansion velocity, the abundance, and the dissociation of the CO molecules.

Near-infrared spectra of 29 carbon stars in the 0.9–2.4 � m range were obtained by using a cross-dispersed echelle spectrograph. The target stars, which were classified into C-H, C-R, C-J, and C-N types, were selected from an atlas of Barnbaum, Stone, and Keenan (1996, ApJS, 105, 419). Because the stars are non long-period variables, the phase differences of the light curves do not strongly affect the spectra. The effective temperatures (Teff) of the carbon stars were estimated with errors of ˙ 200 K by fitting our spectra at wavelengths of 1.35, 1.74, and 2.29 � m, with simple

We developed a Near-Infrared Cross-dispersed Echelle spectrograph, “NICE”, which covers the wavelength range from 0.9 m to 2.4 m with four exposures, and has a wavelength resolution of =i 2600. These capabilities enable us to simultaneously evaluate the continuum level and intensity of various lines of a spectrum with high accuracy over a wide wavelength range. Since NICE is designed to be compact, by adopting a “white pupil” configuration and fully refractive lenses, we can carry out observations with small telescopes.

著者人数: 38名, Accepted: 2014-10-06, 資料番号: SA1150065000

著者人数: 36名, Accepted: 2014-12-10, 資料番号: SA1150021000

The effects of repeated prenatal stress with different severity (restraint and immobilization) on Fos expression in the maternal and fetal hypothalamic paraventricular nucleus (PVN) were examined in rats. Acute stress treatment was performed for 30 min on gestational day 21, and repeated stress treatment for 30 min daily for 5 days from gestational days 17-21. In the parvocellular region of the maternal PVN, the stress-induced increases in the number of Fos-immunoreactive neurons were smaller in the repeated stress groups than the acute stress groups, indicating an adaptation of Fos expression to repeated stress. The attenuated Fos expression observed in the maternal PVN following repeated mild stress did not occur in the fetal PVN. In contrast, repeated immobilization stress caused a much smaller increase in Fos expression in the fetal PVN than did acute immobilization stress. The reduced Fos expression in the fetal PVN following repeated severe stress was thought to be due to cell death, since the fetal PVN in the chronic immobilization group revealed a reduction in the total number of cells and an increase in the number of apoptotic cells. In the female but not male fetuses, repeated restraint stress induced a significant increase in the number of apoptotic cells in the PVN. These findings suggest that the fetal PVN shows no adaptation of Fos expression to repeated maternal stress, but great vulnerability to cell death, including apoptosis. In addition, stress-induced apoptosis may more easily occur in the fetal PVN in females than males.

The present experiments were performed to clarify the brain sites whose activity is affected exclusively by cortical spreading depression (CoSD). For this purpose, Fos protein, a product of an immediate early gene, was used as a marker of neuronal activation. Because Fos can be induced by many manipulations such as stress stimuli, we verified CoSD-induced Fos expression by excluding the influence of other factors such as anaesthesia and surgical manipulation. CoSD was induced by applying a KCl solution directly to the dura mater over the cerebral cortex, and Fos expression in the brain was assessed by immunohistochemistry using antibodies against Fos protein. We found that during CoSD, Fos expression was increased specifically in the magnocellular region of the hypothalamic paraventricular nucleus (PVN), as well as in the ipsilateral cortex, whereas reduced Fos expression was observed in both the parvocellular region of the PVN and the whole cortex contralateral to the CoSD site. Consistent with the reduced Fos expression, approximately 40% of neurons in the contralateral cortex revealed a suppression of electrical activity during CoSD. These results suggest that in addition to the ipsilateral cortex, CoSD affects Fos expression exclusively in the PVN and the contralateral cortex.

The [Fe II] 1.257 μm and He I 1.083 μm emission lines were observed in the central 6' × 8' region of the Orion Nebula, and their excitation in the photoionized H II region, HH flows, jets, and proplyds is investigated. Observations were carried out using the imaging Fabry-Perot spectrometer MUSE at the National Astronomical Observatory of Japan 1.5 m infrared telescope, which provides a 4' × 4' field of view and a spectral resolution λ/δλ of ~2000 at the observed wavelengths. The [Fe II] images exhibit (1) filamentary structures and diffuse emission, which presumably arise from ionization fronts of the photoionized H II region, and (2) a number of knots, some of which are newly identified. Centroidal velocities in most of the knots are negative relative to those in the ionization fronts by up to -60 km s-1, and observed line profiles in the bright knots exhibit blueshifted wings, agreeing with bow shock models. The He I 1.083 μm emission in the observed region is dominated by the photoionized H II region, and its distribution reflects the complicated nature of the excitation. The He I images also contain blueshifted emission from several HH flows and jets and redshifted emission associated with proplyds. Our results for the shocks suggest that the [Fe II] 1.257 μm and He I 1.083 μm emission reflects the ionization of the preshock gas: the [Fe II] 1.257 μm emission is prominent in shocks propagating in molecular/atomic gas, while the He I 1.083 μm is prominent in shocks in the photoionized H II region. Different line excitation in these shocks can be explained by the following physical properties and processes: (1) difference of the excitation energies from the ground state (1 and 20 eV for the [Fe II] and He I lines, respectively), (2) resonance scattering and collisional excitation from the metastable state, enhancing the He I 1.083 μm line in shocks in the photoionized H II region, (3) a large photoionization cross section of Fe+, causing the absence of the [Fe II] emission in the same shocks, and possibly (4) charge exchange reactions of Fe, which could enhance the [Fe II] emission in neutral gas.

The Simultaneous-color Wide-field Infrared Multi-object Spectrograph, SWIMS, is a first-generation near-infrared instrument for the University of Tokyo Atacama Observatory (TAO) 6.5m Telescope now being constructed in northern Chile. To utilize the advantage of the site that almost continuous atmospheric window appears from 0.9 to 2.5 μm, the instrument is capable of simultaneous two-color imaging with a field-of-view of 9.′6 in diameter or λ/uλ 1000 multi-object spectroscopy at 0.9–2.5 μm in a single exposure. The instrument has been trans- ported in 2017 to the Subaru Telescope as a PI-type instrument for carrying out commissioning observations before starting science operation on the 6.5m telescope. In this paper, we report the latest updates on the instrument and present preliminary results from the on-sky performance verification observations.

The telescope of the University of Tokyo Atacama Observatory has a 6.5-m primary mirror in diameter. In order to fabricate the reflecting film initially and to maintain its performance over a long period, we have mirror coating facility on site. We have chosen to leave the primary mirror in its cell with the mirror support system intact. Two major advantages of leaving the mirror in its cell are that the mirror does not have to be lifted or handled and the support system does not have to be removed or reinstalled for coating. The facility consists of a clean booth for stripping of the old film, an evaporation coating chamber, and a cart with a lifter for handling the primary mirror. A conventional evaporation system with a metal pre-wetted filament array is adopted for achieving various optical requests. The coating equipment has also a function of fabrication for film on secondary and tertiary mirrors.

We here summarize the design and the current fabrication status for the University of Tokyo Atacama Observatory (TAO) 6.5-m telescope. The TAO telescope is operated at one of the best sites for infrared observations, at the summit of Co. Chajnantor in Chile, and is optimized for infrared observations. The telescope mount, mirrors, and mirror support systems are now at the final design phase. The mechanical and optical designs are done by following and referring to those of the Magellan telescopes, MMT, and Large Binocular Telescope. The final focal ratio is 12.2. The field-of-view is as wide as 25 arcmin in diameter and the plate scale is 2.75 arcsec mm −1 . The F/1.25 light-weighted borosilicate (Ohara E6) honeycomb primary mirror is adopted and being fabricated by the Steward Observatory Mirror Laboratory. The primary mirror is supported by 104 loadspreaders bonded to the back surface of the mirror and 6 adjustable hardpoints. The mirror is actively controlled by adjusting the actuator forces based on the realtime wavefront measurement. The actuators are optimized for operation at high altitude of the site, 5640-m above the sea level, by considering the low temperature and low air pressure. The mirror is held in the primary mirror cell which is used as a part of the vacuum chamber when the mirror surface is aluminized without being detached from the cell. The pupil is set at the secondary mirror to minimize infrared radiation into instruments. The telescope has two Nasmyth foci for near-infrared and mid-infrared facility instruments (SWIMS and MIMIZUKU, respectively) and one folded-Caseggrain focus for carry-in instruments. At each focus, autoguider and wavefront measurement systems are attached to achieve seeing-limited image quality. The telescope mount is designed as a tripod-disk type alt-azimuth mount. Both the azimuthal and elevation axes are supported by and run on the hydrostatic bearings. Friction drives are selected for these axis drives. The telescope mount structure and primary mirror support as well as the mirrors are under thermal control and maintained at ambient air temperature to minimize the mirror seeing.

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.

Near-infrared (NIR) monitoring observations of asymptotic giant branch stars exciting bright SiO masers have been made with the 1 m telescope of Kagoshima University. In order to investigate the properties of these stars and their envelopes, we combined our NIR photometric data with mid- and far-infrared flux data obtained by the IRAS satellite, SiO maser flux data provided by the Nobeyama Radio Observatory, visual magnitude data provided by the AAVSO, and the reported data on the expansion velocities of the circumstellar envelopes. The absolute magnitudes at the K-band and the distances are estimated using the period–luminosity relation of Mira variables determined by Feast et al. Then, mass-loss rates and isotropic luminosities of an SiO maser are estimated. The mass-loss rates range from approximately 10−8 to over 10−5 . We found that the NIR pulsation amplitudes are correlated with the pulsation periods and the observed wavelengths. We also found correlations of the isotropic luminosities of SiO masers with the mass-loss rates and absolute magnitudes at the K-band. These results will help us to understand the pumping mechanism of SiO masers. We measured, for the first time, the periods and/or NIR magnitudes of TX Cam, BW Cam, IRAS 06297+4045, IRAS 18387–0423, and RT Cep.

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

SWIMS (Simultaneous-color Wide-field Infrared Multi-object Spectrograph) is one of the first-generation instruments for the University of Tokyo Atacama Observatory (TAO; P.I.: Yuzuru Yoshii) 6.5-m telescope which is planned to be constructed at the world's highest site, the summit of Cerro Chajnantor (an altitude of 5,640 m or 18,500 ft) in northern Chile. By placing a dichroic mirror into the collimated beam, SWIMS is capable of wide-field (φ 9'.6 with 0".126 pixel-1) two-color simultaneous imaging as well as multi-object spectroscopy (MOS) using cooled multi-slit masks covering the entire near-infrared spectra between 0.9 and 2.5 μm in a single exposure with low-to-medium spectral resolutions. Up to 20 user-defined slit masks as well as long slit masks are available. The field of view is covered with four 2048 x 2048 pixel HgCdTe focal plane arrays (HAWAII-2RG). Tests of the MOS slit mask exchanger motions have been completed successfully without any trouble under cryogenic environment. Further MOS tests will be performed at various tilt and rotation angles of the instrument using a telescope simulator. Also, a conceptual study of a compact and cryogenic wide-field integral field spectroscopy unit handled by the slit mask exchanger is now being carried out. The part of the current designs is optimized for installation on the Subaru Telescope for performance verification and early scientific observations prior to the construction of the TAO 6.5-m telescope. In this paper, we present the design and development status of the instrument.

ANIR (Atacama Near InfraRed camera) is a near infrared camera for the University of Tokyo Atacama 1.0m telescope installed at the summit of Co. Chajnantor (5640m altitude) in northern Chile. The high altitude and the extremely low water vapor (precipitable water vapor:PWV=0.5mm) of the site enables us to perform observation of hydrogen Paschen alpha (Paα) emission line at 1.8751 μm. Since the first light observation in June 2009, we have succesfully obtained Paα narrow-band images of Galactic objects and near-by Galaxies. However, as there are many atmospheric absorption features within the wavelength range of the narrow-band filters which vary temporally due to change of PWV, it is difficult to calibrate the emission line flux accurately. Therefore, we have developed a new method to restore Paα emission-line flux from ground-based narrow-band filter imaging observations. First, average atmospheric transmittance within the narrow-band filter is derived using 2MASS stars in a image. Second, PWV is then estimated by comparing the transmittance with that calculated by atmospheric transmittance model software, ATRAN. Finally, the atmospheric transmittance at the wavelength of Paα emission-line is obtained from the model atmosphere corresponding to the obtained PWV. By applying this method to the data of nearby Luminous Infrared Galaxies obtained by ANIR, the emission line strength is estimated within the accuracy of 10% relative to that observed by HST/NICMOS. In this paper, we describe details of the calibration method and its accuracy.

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.

Thirty micron has remained one of unexplored frontiers of ground-based astronomical observations. Recent developments of extreme high sites including the Chajnantor TAO site (5,640m) enable us to access the this wavelengths from the ground. The expected transmittance seems clear enough for astronomical observations, but practical evaluations based on astronomical data has not been carried out yet. We have analyzed images obtained at the 31.7 micron with a mid-infrared camera MAX38 attached on a mini-TAO 1.0-meter telescope. 109 images of a star IRC+10420 and 11,114 images of the sky have been reduced. Clear relationship between the measured photocurrents and the perceptible water vapor has been found. Simple estimation of the photocurrents with of the ATRAN model gives good agreements with the measurements, indicating that the ATRAN model reproduce the atmospheric transmittance reasonably well. This also supports our assumption that the scaling factor 0.85 of the PVW at the Chajnantor TAO site to the PWV at the APEX. The average transmittance in the 31.7 micron is achieved to be over 20% when the PWV below 0.6 mm. In some cases clear degradation up to 10% in the transmittance is found. It may be caused by droplets of liquid or iced water with a size over 10 micron although the causes are not exactly specified. Diurnal time variations of the sky photocurrents are also investigated. The sky is sometimes bright and usually unstable in the twilight time. On the other hand the sky around the noontime does not show clear difference from the night sky. It may suggest that the observing condition at the thirty micron windows remain good even in the daytime.

Aim Japanese psychiatrists have increasingly reported patients with depression that does not seem to fit the criteria of the ICD-10 and the DSM-IV, and which has recently been called modern type depression (MTD). We explored whether MTD is frequently seen in Japan and also in other countries, and if so, how patients with MTD are diagnosed and treated. Methods The questionnaires, with two case vignettes (traditional type depression (TTD) and MTD), were sent to psychiatrists in Australia, Bangladesh, India, Iran, Japan, Korea, Taiwan, Thailand and the USA. Participants rated their opinions about each case's prevalence in their country, etiology, diagnosis, suicide risk, and treatment using Likert scales. Results Out of 247 responses (123 from Japan and 124 from other countries), two hundred thirty-nine valid responses were received. MTD was recognized in all participating countries, and especially in urban areas. Generally, the factor of personality was regarded as the most probable cause of MTD. Whereas about 90% of Japanese psychiatrists applied the ICD/DSM criteria to TTD, only about 60% applied the criteria to MTD. Conclusion Our results indicate that Japan's MTD seems to be occurring in many other countries, and that the present ICD/DSM criteria may not be sufficient to diagnose MTD. Therefore, it could be an important candidate for a new international diagnostic criterion as a subtype of depression. A clear diagnostic framework and consensus on the interventions to treat MTD would be valuable. Further clinical, psychopathological and international epidemiological studies are needed to confirm our preliminary findings of MTD.

We describe the design and current status of a near-infrared multi-object spectrograph for the University of Tokyo Atacama Observatory (TAO) project, which is to construct a 6.5m infrared telescope on the summit of Co. Chajnantor (altitude of 5,460m) in the northern Chile. The instrument, named SWIMS (Simultaneous-color Wide-field Infrared Multi-object Spectrograph), covers a wavelength range from 0.9 to 2.5 μm with a field of view of 9.6 in diameter using 4096 × 4096 pixels with a pixel scale of 0.13 pixel-1. It has two observation modes: a wide-field imager and a multi-object spectrograph (MOS). The MOS mode adopts cooled multi-slit masks with 30 slits at a maximum, and achieves a spectral resolution of λ/uλ~ 1000. Up to 20 masks can be installed in a mask storage dewar. In both modes, two wavelength ranges of 0.9-1.4 μm and 1.4-2.5 μm are observed simultaneously with a dichroic mirror placed in the collimated beam. This will provide us data covering the wide spectral range under same conditions such as weather, telescope pointing, and so on. Such data are important not only for redshift surveys of distant galaxies but also for rapidly time-variable events such as gamma-ray bursts. As SWIMS is expected to be completed before the construction of the 6.5m telescope, we plan to carry out performance verification and early scientific observations on the Subaru Telescope at Hawaii.

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.

We have developed a near infrared camera called ANIR (Atacama Near InfraRed camera) for the University of Tokyo Atacama 1.0m telescope installed at the summit of Co. Chajnantor (5640m altitude) in northern Chile. The camera is based on a PACE HAWAII-2 array with an Offner relay optics for re-imaging, and field of view is 5. 3 × 5. 3 with pixel scale of 0. 31/pix. It is also capable of optical/infrared simultaneous imaging by inserting a dichroic mirror before the focal plane. The high altitude and extremely low water vapor (PWV=0.5mm) of the site enables us to perform observation of hydrogen Paschenα (Paα) emission line at 1.8751 μm. The first light observation was carried out in July 2009, and we have successfully obtained Paα images of the Galactic center using the N1875 narrow-band filter. This is the first success of Paα imaging of a Galactic object from a ground based telescope. System efficiencies for the broad-band filters are measured to be 15% at the J-band and 30% at Ks, while that of the N1875 narrow-band filter, corresponding to Paα; wavelength, varies from 8 to 15%, which may be caused by fluctuation of the atmospheric transmittance. ATRAN simulation suggests that this corresponds to PWV of 0.3 - 1.5mm, consistent with previous results of the site testing. Measured seeing size is median ~0. 8, corresponding to the real seeing value of 0. 6 - 0. 8. These results demonstrates the excellent capability of the site for infrared observations.

The University of Tokyo Atacama Observatory (TAO) is a project to construct a 6.5m infrared-optimized telescope at the summit of Co. Chajnantor, 5,640 m altitude, in northern Chile, promoted by Institute of Astronomy, University of Tokyo. Thanks to the high altitude and low water vapor, continuous window from 0.9 to 2.5μm as well as new windows at wavelength longer than 25μm appears. The site shows extremely low precipitable water vapor of 0.5mm (25 percentile), and fraction of usable night is more than 80%. Measured median seeing is 0".69, which is comparable or better than major observatories over the world. Prior to the 6.5m telescope, a 1m pathfinder telescope called miniTAO is installed and started observations in 2009. Its successes of Paschen α imaging at 1.875 μm and mid-infrared observations at 30μm confirm promising capabilities of the site. The 6.5m telescope is now at a design phase, and two facility instruments are now being constructed, which are a near-infrared imager/multi-object spectrograph with a field of view of 9'.6 and a mid-infrared imager/spectrograph for observations in 2 to 38μm.

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.

We present the current status of the University of Tokyo Atacama 1.0-m telescope constructed at the summit of Co. Chajnantor (5,640 m) in Atacama, Chile, which is an optical/infrared telescope at the world's highest site. The telescope is an f/12 Ritchey-Chretien type with a field of view of 10 arcmin. It is installed in a 6-m dome and is controlled from the operation room in a container separated from the dome. The engineering first light observation was carried out in March 2009, and the astronomical observations have been carried out since June 2009. The pointing of the telescope is as accurate as 2.4 arcsec (RMS), showing good tracking accuracy of 0.2 arcsec for 60-s observation without guiding. The Hartmann constant is 0.19 arcsec and the image quality of the telescope is satisfactory for scientific observations. The best PSF obtained is 0.5 arcsec (FWHM) in optical, which demonstrates that the summit of Co. Chajnantor is one of the best seeing site in the world. Also the excellent atmospheric transmission in infrared wavelength at the site is proved by successful observations carried out by the ANIR near-infrared camera and the MAX38 mid-infrared instrument. In the near future, the operation room will be connected to the base support facility at San Pedro de Atacama for remote observation.

Early follow‐up observations of gamma‐ray bursts (GRBs) in wide wavelength range, especially from the optical to the near infrared (NIR) bands, are crucial for search of high‐redshift GRBs by detecting their Lyman limit break. For this purpose, we have developed a NIR/optical simultaneous imager called ANIR (Atacama Near InfraRed camera) for the University of Tokyo Atacama 1.0 m telescope. Installed at the summit of Co. Chajnantor (5640 m altitude) in northern Chile, this telescope is the world’s highest optical/NIR observatory. ANIR saw the first light in June 2009, and several observing runs have been carried out for performance verification as well as scientific observations. During the run, we have successfully detected an optical/NIR afterglow of GRB091018. Thanks to the excellent seeing (median ∼0″.8), 5σ limiting magnitudes reach 23.3, 20.6, and 20.8 mag(AB) in the B, J and Ks bands, respectively, with 600 sec exposure.

Because of the high transparency in infrared wavelength, Co. Chajnantor (5,650m altitude) at Atacama, Chile, is one of the most promising sites for infrared astronomy in the world. For evaluating the site condition quantitatively we carried out weather and cloud emissivity monitoring campaign from April 2006 to April 2007. The ground-level condition such as wind direction, wind speed, air temperature, and humidity was monitored by a weather station installed at the summit. Cloud emissivity was estimated by mid-infrared sky images taken by a whole-sky infrared camera every five minutes for 24 hours a day, every day. Results are summarized as followings. 1) The weather condition at the summit is slightly harsher than the condition at the Pampa la Bola plateau. Maximum speed of the wind is 35m/s, and minimum temperature is about -10 degree. 2) Fraction of "clear+usable" weather (which is defined as the cloud emissivity < 10%)" is 82% in a year. The fraction decrease to 40-50% on Bolivian winter season, and increases to over 90% from April to July. This is comparable or even better than the other astronomical sites.