Author name code: shinoda ADS astronomy entries on 2022-09-14 author:"Shinoda, Kazuya" ------------------------------------------------------------------------ Title: Development of Fast and Precise Scan Mirror Mechanism for an Airborne Solar Telescope Authors: Oba, Takayoshi; Shimizu, Toshifumi; Katsukawa, Yukio; Kubo, Masahito; Kawabata, Yusuke; Hara, Hirohisa; Uraguchi, Fumihiro; Tsuzuki, Toshihiro; Tamura, Tomonori; Shinoda, Kazuya; Kodeki, Kazuhide; Fukushima, Kazuhiko; Morales Fernández, José Miguel; Sánchez Gómez, Antonio; Balaguer Jimenéz, María; Hernández Expósito, David; Gandorfer, Achim Bibcode: 2022arXiv220713864O Altcode: We developed a scan mirror mechanism (SMM) that enable a slit-based spectrometer or spectropolarimeter to precisely and quickly map an astronomical object. The SMM, designed to be installed in the optical path preceding the entrance slit, tilts a folding mirror and then moves the reflected image laterally on the slit plane, thereby feeding a different one-dimensional image to be dispersed by the spectroscopic equipment. In general, the SMM is required to scan quickly and broadly while precisely placing the slit position across the field-of-view (FOV). These performances are highly in demand for near-future observations, such as studies on the magnetohydrodynamics of the photosphere and the chromosphere. Our SMM implements a closed-loop control system by installing electromagnetic actuators and gap-based capacitance sensors. Our optical test measurements confirmed that the SMM fulfils the following performance criteria: i) supreme scan-step uniformity (linearity of 0.08%) across the wide scan range (${\pm}$1005 arcsec), ii) high stability (3${\sigma}$ = 0.1 arcsec), where the angles are expressed in mechanical angle, and iii) fast stepping speed (26 ms). The excellent capability of the SMM will be demonstrated soon in actual use by installing the mechanism for a near-infrared spectropolarimeter onboard the balloon-borne solar observatory for the third launch, Sunrise III. Title: SUNRISE Chromospheric Infrared spectroPolarimeter (SCIP) for SUNRISE III: Scan mirror mechanism Authors: Oba, Takayoshi; Shimizu, Toshifumi; Katsukawa, Yukio; Kubo, Masahito; Uraguchi, Fumihiro; Tsuzuki, Toshihiro; Tamura, Tomonori; Shinoda, Kazuya; Kodeki, Kazuhide; Fukushima, Kazuhiko; Gandorfer, Achim; del Toro Iniesta, Jose Carlos Bibcode: 2020SPIE11445E..4FO Altcode: The SUNRISE Chromospheric Infrared spectroPolarimeter (SCIP) is a balloon-borne long-slit spectrograph for SUNRISE III to precisely measure magnetic fields in the solar atmosphere. The scan mirror mechanism (SMM) is installed in the optical path to the entrance slit of the SCIP to move solar images focused on the slit for 2-dimensional mapping. The SMM is required to have (1) the tilt stability better than 0.035″ (3σ) on the sky angle for the diffraction-limited spatial resolution of 0.2″, (2) step response shorter than 32 msec for rapid scanning observations, and (3) good linearity (i.e. step uniformity) over the entire field-of-view (60″x60″). To achieve these performances, we have developed a flight-model mechanism and its electronics, in which the mirror tilt is controlled by electromagnetic actuators with a closed-loop feedback logic with tilt angles from gap-based capacitance sensors. Several optical measurements on the optical bench verified that the mechanism meets the requirements. In particular, the tilt stability achives better than 0.012″ (3σ). Thermal cycling and thermal vacuum tests have been completed to demonstrate the performance in the vacuum and the operational temperature range expected in the balloon flight. We found a small temperature dependence in the step uniformity and this dependence will be corrected to have 2-demensional maps with the sub-arcsec spatial accuracy in the data post-processing. Title: Sunrise Chromospheric Infrared spectroPolarimeter (SCIP) for SUNRISE III: polarization modulation unit Authors: Kubo, Masahito; Shimizu, Toshifumi; Katsukawa, Yukio; Kawabata, Yusuke; Anan, Tetsu; Ichimoto, Kiyoshi; Shinoda, Kazuya; Tamura, Tomonori; Nodomi, Yoshifumi; Nakayama, Satoshi; Yamada, Takuya; Tajima, Takao; Nakata, Shimpei; Nakajima, Yoshihito; Okutani, Kousei; Feller, Alex; del Toro Iniesta, Jose Carlos Bibcode: 2020SPIE11447E..A3K Altcode: Polarization measurements of the solar chromospheric lines at high precision are key to present and future solar telescopes for understanding magnetic field structures in the chromosphere. The Sunrise Chromospheric Infrared spectroPolarimeter (SCIP) for Sunrise III is a spectropolarimeter with a polarimetric precision of 0.03 % (1 σ). The key to high-precision polarization measurements using SCIP is a polarization modulation unit that rotates a waveplate continuously at a constant speed. The rotating mechanism is a DC brushless motor originally developed for a future space mission, and its control logic was originally developed for the sounding rocket experiment CLASP. Because of our requirement on a speed of rotation (0.512 s/rotation) that was 10 times faster than that of CLASP, we optimized the control logic for the required faster rotation. Fast polarization modulation is essential for investigating the fine-scale magnetic field structures related to the dynamical chromospheric phenomena. We have verified that the rotation performance can achieve the polarization precision of 0.03 % (1 σ) required by SCIP and such a significant rotation performance is maintained under thermal vacuum conditions by simulating the environment of the Sunrise III balloon flight. The waveplate was designed as a pair of two birefringent plates made of quartz and sapphire to achieve a constant retardation in a wide wavelength range. We have confirmed that the retardation is almost constant in the 770 nm and 850nm wavelength bands of SCIP under the operational temperature conditions. Title: Sunrise Chromospheric Infrared SpectroPolarimeter (SCIP) for sunrise III: system design and capability Authors: Katsukawa, Y.; del Toro Iniesta, J. C.; Solanki, S. K.; Kubo, M.; Hara, H.; Shimizu, T.; Oba, T.; Kawabata, Y.; Tsuzuki, T.; Uraguchi, F.; Nodomi, Y.; Shinoda, K.; Tamura, T.; Suematsu, Y.; Ishikawa, R.; Kano, R.; Matsumoto, T.; Ichimoto, K.; Nagata, S.; Quintero Noda, C.; Anan, T.; Orozco Suárez, D.; Balaguer Jiménez, M.; López Jiménez, A. C.; Cobos Carrascosa, J. P.; Feller, A.; Riethmueller, T.; Gandorfer, A.; Lagg, A. Bibcode: 2020SPIE11447E..0YK Altcode: The Sunrise balloon-borne solar observatory carries a 1 m aperture optical telescope and provides us a unique platform to conduct continuous seeing-free observations at UV-visible-IR wavelengths from an altitude of higher than 35 km. For the next flight planned for 2022, the post-focus instrumentation is upgraded with new spectro- polarimeters for the near UV (SUSI) and the near-IR (SCIP), whereas the imaging spectro-polarimeter Tunable Magnetograph (TuMag) is capable of observing multiple spectral lines within the visible wavelength. A new spectro-polarimeter called the Sunrise Chromospheric Infrared spectroPolarimeter (SCIP) is under development for observing near-IR wavelength ranges of around 770 nm and 850 nm. These wavelength ranges contain many spectral lines sensitive to solar magnetic fields and SCIP will be able to obtain magnetic and velocity structures in the solar atmosphere with a sufficient height resolution by combining spectro-polarimetric data of these lines. Polarimetric measurements are conducted using a rotating waveplate as a modulator and polarizing beam splitters in front of the cameras. The spatial and spectral resolutions are 0.2" and 2 105, respectively, and a polarimetric sensitivity of 0.03 % (1σ) is achieved within a 10 s integration time. To detect minute polarization signals with good precision, we carefully designed the opto-mechanical system, polarization optics and modulation, and onboard data processing. Title: Infrared spectro-polarimeter on the Solar Flare Telescope at NAOJ/Mitaka Authors: Sakurai, Takashi; Hanaoka, Yoichiro; Arai, Takehiko; Hagino, Masaoki; Kawate, Tomoko; Kitagawa, Naomasa; Kobiki, Toshihiko; Miyashita, Masakuni; Morita, Satoshi; Otsuji, Ken'ichi; Shinoda, Kazuya; Suzuki, Isao; Yaji, Kentaro; Yamasaki, Takayuki; Fukuda, Takeo; Noguchi, Motokazu; Takeyama, Norihide; Kanai, Yoshikazu; Yamamuro, Tomoyasu Bibcode: 2018PASJ...70...58S Altcode: 2018PASJ..tmp...63S; 2018PASJ..tmp...82S An infrared spectro-polarimeter installed on the Solar Flare Telescope at the Mitaka headquarters of the National Astronomical Observatory of Japan is described. The new spectro-polarimeter observes the full Sun via slit scans performed at two wavelength bands, one near 1565 nm for a Zeeman-sensitive spectral line of Fe I and the other near 1083 nm for He I and Si I lines. The full Stokes profiles are recorded; the Fe I and Si I lines give information on photospheric vector magnetic fields, and the helium line is suitable for deriving chromospheric magnetic fields. The infrared detector we are using is an InGaAs camera with 640 × 512 pixels and a read-out speed of 90 frames s-1. The solar disk is covered by two swaths (the northern and southern hemispheres) of 640 pixels each. The final magnetic maps are made of 1200 × 1200 pixels with a pixel size of 1{^''.}8. We have been carrying out regular observations since 2010 April, and have provided full-disk, full-Stokes maps, at the rate of a few maps per day, on the internet. Title: Wavefront error measurements and alignment of CLASP2 telescope with a dual-band pass cold mirror coated primary mirror Authors: Yoshida, Masaki; Song, Donguk; Ishikawa, Ryoko; Kano, Ryouhei; Katsukawa, Yukio; Suematsu, Yoshinori; Narukage, Noriyuki; Kubo, Masahito; Shinoda, Kazuya; Okamoto, Takenori J.; McKenzie, David E.; Rachmeler, Laurel A.; Auchère, Frédéric; Trujillo Bueno, Javier Bibcode: 2018SPIE10699E..30Y Altcode: "Chromospheric LAyer Spectro-Polarimeter (CLASP2)" is the next sounding rocket experiment of the "Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP)" that succeeded in observing for the first time the linear polarization spectra in the hydrogen Lyman-α line (121.6 nm) and is scheduled to be launched in 2019. In CLASP2, we will carry out full Stokes-vector spectropolarimetric observations in the Mg ii h and k lines near 280 nm with the spectro-polarimeter (SP), while imaging observations in the Lyman-α line will be conducted with the slitjaw optics (SJ). For the wavelength selection of CLASP2, the primary mirror of the telescope uses a new dual-band pass cold mirror coating targeting both at 121.6 nm and 280 nm. Therefore, we have to perform again the alignment of the telescope after the installation of the recoated primary mirror. Before unmounting the primary mirror from the telescope structure, we measured the wave-front error (WFE) of the telescope. The measured WFE map was consistent with what we had before the CLASP flight, clearly indicating that the telescope alignment has been maintained even after the flight. After the re-coated primary mirror was installed the WFE was measured, and coma aberration was found to be larger. Finally, the secondary mirror shim adjustments were carried out based on the WFE measurements. In CLASP2 telescope, we improved a fitting method of WFE map (applying 8th terms circular Zernike polynomial fitting instead of 37th terms circular Zernike fitting) and the improved method enables to achieve better performance than CLASP telescope. Indeed, WFE map obtained after the final shim adjustment indicated that the required specification (< 5.5 μm RMS spot radius) that is more stringent than CLASP telescope was met. Title: Optical alignment of the high-precision UV spectro-polarimeter (CLASP2) Authors: Song, Donguk; Ishikawa, Ryohko; Kano, Ryouhei; Yoshida, Masaki; Tsuzuki, Toshihiro; Uraguchi, Fumihiro; Shinoda, Kazuya; Hara, Hirohisa; Okamoto, Takenori J.; Auchère, Frédéric; McKenzie, David E.; Rachmeler, Laurel A.; Trujillo Bueno, Javier Bibcode: 2018SPIE10699E..2WS Altcode: Chromospheric LAyer Spectro-Polarimeter (CLASP2) is our next sounding rocket experiment after the success of Chromospheric Lyman-Alpha Spectro-Polarimeter (CLASP1). CLASP2 is scheduled to launch in 2019, and aims to achieve high precision measurements (< 0.1 %) of the linear and circular polarizations in the Mg ii h and k lines near the 280 nm, whose line cores originate in the upper solar chromosphere. The CLASP2 spectro-polarimeter follows very successful design concept of the CLASP1 instrument with the minimal modification. A new grating was fabricated with the same radius of curvature as the CLASP1 grating, but with a different ruling density. This allows us to essentially reuse the CLASP1 mechanical structures and layout of the optics. However, because the observing wavelength of CLASP2 is twice longer than that of CLASP1, a magnifier optical system was newly added in front of the cameras to double the focal length of CLASP2 and to maintain the same wavelength resolution as CLASP1 (0.01 nm). Meanwhile, a careful optical alignment of the spectro-polarimeter is required to reach the 0.01 nm wavelength resolution. Therefore, we established an efficient alignment procedure for the CLASP2 spectro-polarimeter based on an experience of CLASP1. Here, we explain in detail the methods for achieving the optical alignment of the CLASP2 spectro-polarimeter and discuss our results by comparing with the performance requirements. Title: Development of the Universal Tunable Filter and High-resolution Imaging Observation with the Fuxian Solar Observatory Authors: Hagino, M.; Ichimoto, K.; Ueno, S.; Kimura, G.; Otsuji, K.; Kitai, R.; Zhong, L.; Xu, Z.; Shinoda, K.; Hara, H.; Suematsu, Y.; Shimizu, T. Bibcode: 2016ASPC..504..103H Altcode: We have developed a new narrow-band universal tunable filter to perform imaging spectroscopy of the solar chromosphere. The development stage of the filter has been almost finished and we shifted to the scientific observation phase by using large grand-based telescopes. Using the filter, a series of high-resolution images were obtained with the 1m vacuum solar telescope at the Fuxian Solar Observatory. We succeeded in observing several flares and fine structures of the chromospheric layer. Title: Development of a universal tunable filter for future solar observations Authors: Hagino, M.; Ichimoto, K.; Kimura, G.; Nakatani, Y.; Kawate, T.; Shinoda, K.; Suematsu, Y.; Hara, H.; Shimizu, T. Bibcode: 2014SPIE.9151E..5VH Altcode: We have developed a new narrowband tunable filter to perform imaging spectroscopy of the solar chromosphere. Using Liquid Crystal Variable Retarders (LCVRs) as the tuning elements for wavelength, wide-band polarizers and super achromatic half-wave plates, it is possible to make high speed tuning (about 0.1Sec), to exclude mechanical drives (and oil tank), and to cover a wide wavelength range (510-100nm). This filter builds up with seven stages each consisting of a pair of calcites, LCVR, half-wave plates and linear polarizer. The full width at half maximum (FWHM) of the filter transmission is about 0.025nm at 656.3nm.We demonstrate that the concept of the universal tunable filter using the LCVR's as tuning elements is highly promising for future application to space mission and ground based observations. Title: Integral Field Spectroscopy of the Sun with Microlens Array and Liquid Crystal Retarders Authors: Suematsu, Y.; Shinoda, K.; Sano, I.; Kobiki, T. Bibcode: 2011AGUFMSH13B1947S Altcode: Simultaneous spectrographic observations over extended solar structures, at a high spatial resolution and temporal cadence, are important to track and understand the physics of transient phenomena such as Ellerman bombs, flare kernels, prominences/filaments and spicules. With two-dimensional (2-D) field spectral data, we can make monochromatic images at a given wavelength in a designed passband and line profile analysis to derive 2-D distribution of atmospheric parameters. One technique to produce a spectrum of each spatial elements in an extended two-dimensional field is to use a micro-lens array. Replacing a slit of a conventional spectrograph with a micro-lens array then helps to capture two-dimensionally distributed short spectra from 2-D field using additional optics inserted, a bandpass filter and a large format detector. For observations of magnetic field, we can add polarization modulator made of liquid crystal retarders which give a sequence of alternative orthogonal polarization states with time. We describe a design concept and limitations for observations with the micro-lens array spectrograph and an initial result applied for a few existing solar telescopes at NAOJ and Hida Observatory, Kyoto University. Title: Infrared Stokes Spectro-Polarimeter at the National Astronomical Observatory of Japan Authors: Hanaoka, Y.; Sakurai, T.; Shinoda, K.; Noguchi, M.; Miyashita, M.; Fukuda, T.; Suzuki, I.; Hagino, M.; Arai, T.; Yamasaki, T.; Takeyama, N. Bibcode: 2011ASPC..437..371H Altcode: We are now constructing an infrared spectro-polarimeter for the Solar Flare Telescope of NAOJ. It observes the full Sun in two wavelength bands, one near 1.56 μm for highly Zeeman-sensitive spectral lines of Fe I and the other near 10830 Å for He I and Si I lines. The instrument records full Stokes profiles, and a Stokes inversion process will give information on the strength and orientation of the magnetic field vector for both of the photosphere and the chromosphere. The infrared detector we are using is an InGaAs camera manufactured by a Belgian company Xenics. Its format is 640×512 pixels and its read-out speed is 90 frames s-1. The solar disk will be covered by two swaths (the northern and southern hemispheres) of 640 pixels each. The final magnetic maps will be made of 1200×1200 pixels with a pixel size of 1.8 arcsec. Now we are operating regular observations and generate full-disk, full-Stokes maps (a few maps per day). Our ultimate goal is to derive the distribution of magnetic helicity over the whole surface of the Sun, not only in sunspots and active regions. Title: Polarization Calibration of the Solar Optical Telescope onboard Hinode Authors: Ichimoto, K.; Lites, B.; Elmore, D.; Suematsu, Y.; Tsuneta, S.; Katsukawa, Y.; Shimizu, T.; Shine, R.; Tarbell, T.; Title, A.; Kiyohara, J.; Shinoda, K.; Card, G.; Lecinski, A.; Streander, K.; Nakagiri, M.; Miyashita, M.; Noguchi, M.; Hoffmann, C.; Cruz, T. Bibcode: 2008SoPh..249..233I Altcode: 2008SoPh..tmp...69I The Solar Optical Telescope (SOT) onboard Hinode aims to obtain vector magnetic fields on the Sun through precise spectropolarimetry of solar spectral lines with a spatial resolution of 0.2 - 0.3 arcsec. A photometric accuracy of 10−3 is achieved and, after the polarization calibration, any artificial polarization from crosstalk among Stokes parameters is required to be suppressed below the level of the statistical noise over the SOT's field of view. This goal was achieved by the highly optimized design of the SOT as a polarimeter, extensive analyses and testing of optical elements, and an end-to-end calibration test of the entire system. In this paper we review both the approach adopted to realize the high-precision polarimeter of the SOT and its final polarization characteristics. Title: Photopolarimetric measurement system of Mueller matrix with dual rotating waveplates Authors: Ichimoto, Kiyoshi; Shinoda, Kazuya; Yamamoto, Tetsuya; Kiyohara, Junko Bibcode: 2006PNAOJ...9...11I Altcode: A new photopolarimetric measurement system of Mueller matrix of optical elements is developed using dual rotating waveplates. The waveplates in polarization generator and analyzer rotate continuously with a constant ratio of revolution speed, and the Mueller matrix of a sample can be obtained in a few seconds. General principle of such measurement and the optimization of operation parameters are discussed, followed by detailed descriptions of the constructed system. Some examples of its application are also demonstrated. The system is sensitive to <10-3 for each Mueller matrix element for weak polarization elements. Title: Flexible prism used as an image stabilizer Authors: Sakurai, Takashi; Noguchi, Motokazu; Shinoda, Kazuya; Tanaka, Nobuyuki Bibcode: 2003naoj.book...35S Altcode: No abstract at ADS Title: Observations of the Mie scattered light intensities around the Sun with a portable coronagraph Authors: Tanaka, Nobuyuki; Kobiki, Toshihiko; Saito, Moriya; Shinoda, Kazuya; Irie, Makoto Bibcode: 2002RNAOJ...6...11T Altcode: Measurements of Mie scattering intensites around the Sun have been carried out by using a 5 cm coronagraph at (1) Chichijima, Ogasawara Islands, (2) Shiiba, Miyazaki prefecture, (3) Kitadaito Island, Okinawa, (4) Hateruma Islands, Okinawa, and (5) Saku Island, Aichi prefecture. Although our observations were limited in time for only a few days, the results indicate that the solar corona may be observable even at an altitude of 1,000m or less (for example at Shiiba, Miyazaki) where the intensity of scattered light is eventually less than 100 μIo (here Io is the intensity of the solar disk center, and μIo means Io×10-6). Comparison among the tested sites is diffucult because the measurements were done in various seasons in the year; and monitoring over longer time period is necessary to derive definite conclusions. However, the sites where the scattered light intensity is stable and less than 100 μIo, could be a good site for the observations of the Sun considering the transparency of the sky. Title: Two nakhlites from Antarctica: Y000593 and Y000749. Authors: Imae, N.; Ikeda, Y.; Shinoda, K.; Kojima, H.; Iwata, N. Bibcode: 2002anme...27...45I Altcode: No abstract at ADS Title: A Flexible Prism used as an Image Stabilizer Authors: Sakurai, T.; Noguchi, M.; Shinoda, K.; Tanaka, N.; Aoki, K.; Hagino, M.; Mochizuki, H. Bibcode: 2002SoPh..205..201S Altcode: An image stabilizer was constructed by making use of a flexible prism, which is widely used as an anti-vibration mechanism in handheld video cameras. The prism responds to frequencies up to 20 Hz, and can be simply inserted into existing optics. The performance of the prism has been confirmed by observing the Sun through it. Title: A universal polarimeter using liquid crystal variable retarders at the Norikura Solar Observatory Authors: Shinoda, Kazuya; Ichimoto, Kiyoshi; Fukuda, Takeo; Shin, Junho Bibcode: 2001RNAOJ...5...97S Altcode: A universal Stokes polarimeter was developed for the 25-cm coronagraph of the Norikura Solar Observatory. The polarimeter utilizes two liquid crystal variable retarders (LCVR) as the polarization modulator and a Savart plate as the polarization analyser. By controlling the voltages applied to LCVRs, modulations of the polarization states are achieved more flexibly and efficiently in a wavelength range of 450-1,600 nm. The polarimeter is installed at the primary focus of the coronagraph to minimize the instrumental polarization caused by optics. Two orthogonal polarization states are measured simultaneously to minimize the effect of guiding errors and seeing effects. Combined with the coronagraph and the high resolution spectrograph at the coude focus, the polarimeter enables us not only observations of photospheric Zeeman effect but also various types of diagnostics of the solar atmosphere, including coronal Zeeman effect, Hanle effect, impact polarization, and Stark effect. Title: An imaging system of coronal green-line with a Lyot filter. Authors: Imai, H.; Nishino, Y.; Shinoda, K.; Ichimoto, K. Bibcode: 1999RNAOJ...4..157I Altcode: An experimental observation system for taking coronal images in the green line (Fe XIV 5303 Å) was constructed on the 25 cm coronagraph of the Norikura Solar Observatory. By re-arranging the birefringent elements and equipping rotating waveplates on a Lyot filter, the authors were able to obtain images in coronal green-line and sky continuum with a high time cadence. It is shown that this system can provide a powerful tool for diagnosing the physical processes in coronal transient phenomena. Title: A New Imaging System of the Corona at Norikura Authors: Ichimoto, Kiyoshi; Noguchi, Motokazu; Tanaka, Nobuyuki; Kumagai, Kazuyoshi; Shinoda, Kazuya; Nishino, Tetsuo; Fukuda, Takeo; Sakurai, Takashi; Takeyama, Norihide Bibcode: 1999PASJ...51..383I Altcode: A new imaging system of the coronal green line (Fe XIV 5303 Angstroms) was constructed at the Norikura Solar Observatory. The system consists of a 10-cm coronagraph, a tunable Lyot filter, and a cooled CCD camera. The transmission curve of the Lyot filter can be modulated by two liquid-crystal variable retarders. This scheme provides quick wavelength tuning and efficient subtraction of sky background. Two-dimensional distributions of the intensity and Doppler shift of the coronal green line can be obtained within 30 seconds with accuracies of better than 10-6I_Solar and 1 km s-1. Regular operation was started in 1997 September. The aim of the new system is to investigate plasma motions associated with the magnetic field reconnection and waves in the solar corona. Title: An Experimental Study of Hydrous Mineral Formation Reaction Between Enstatite and Water Vapor Authors: Imae, N.; Shinoda, K. Bibcode: 1998M&PSA..33...73I Altcode: No abstract at ADS Title: Solar Flare Telescope at Mitaka Authors: Sakurai, Takashi; Ichimoto, Kiyoshi; Nishino, Yohei; Shinoda, Kazuya; Noguchi, Motokazu; Hiei, Eijiro; Li, Ting; He, Fengbao; Mao, Weijun; Lu, Haitian; Ai, Guoxiang; Zhao, Zhaowang; Kawakami, Singo; Chae, Jong-Chul Bibcode: 1995PASJ...47...81S Altcode: A new solar telescope constructed recently at Mitaka, Tokyo, is described. This instrument, called the Solar Flare Telescope, comprises four telescopes which respectively perform: (1) magnetic-field vector measurements, (2) Doppler-velocity measurements, (3) Hα observations, and (4) continuum observations. The instrument has been operated as a ground-based support for the X-ray satellite Yohkoh launched in 1991 August. Title: Optical and SXT Observations of the x9 Flare of Nov. 1992 Authors: Ichimoto, K.; Sakurai, T.; Nishino, Y.; Noguchi, M.; Shinoda, K.; Yamaguchi, A.; Kumagai, K.; Hirayama, T.; Tsuneta, S.; Acton, L. Bibcode: 1994xspy.conf..259I Altcode: No abstract at ADS Title: Solar Flare Telescope project. Authors: Ichimoto, K.; Sakurai, T.; Hiei, E.; Nishino, Y.; Shinoda, K.; Noguchi, M.; Imai, H.; Irie, M.; Miyashita, M.; Tanaka, N.; Kumagai, K.; Sano, I.; Suematsu, Y.; Okamoto, T.; Miyazaki, H.; Fukushima, H.; Yose, Y.; Zhao, Z. W. Bibcode: 1993RNAOJ...1..375I Altcode: 1993RNOAJ...1..375I The Solar Flare Telescope was built at Mitaka in 1989. This instrument comprises four telescopes which observe (1) Hα images, (2) continuum images, (3) vector magnetic fields, and (4) Doppler velocities, respectively. The instrument aims at the study of energy build-up and energy release in solar flares, in cooperation with the Solar-A satellite (Yohkoh). The Solar Flare Telescope has been in operation since 1990 December. Title: Magnetic Field Observation with the Solar Flare Telescope Authors: Ichimoto, K.; Sakurai, T.; Nishino, Y.; Shinoda, K.; Noguchi, M.; Kumagai, K.; Imai, H.; Irie, M.; Miyashita, M.; Tanaka, N.; Sano, I.; Suematsu, Y.; Hiei, E. Bibcode: 1993ASPC...46..166I Altcode: 1993IAUCo.141..166I; 1993mvfs.conf..166I No abstract at ADS Title: White-Light Flares of 1991 June in the NOAA Region 6659 Authors: Sakurai, Takashi; Ichimoto, Kiyoshi; Hiei, Eijiro; Irie, Makoto; Kumagai, Kazuyoshi; Miyashita, Masakuni; Nishino, Yohei; Yamaguchi, Kisuke; Fang, Geng; Kambry, Maspul Aini; Zhao, Zhaowang; Shinoda, Kazuya Bibcode: 1992PASJ...44L...7S Altcode: We report on observations of flare activities in an active region NOAA 6659, which appeared on the sun in 1991 June. Among six X-class flares in this region, we observed three flares (June 4, 9, and 11), all of which were white-light flares. A detailed discussion is given concerning a particularly interesting white-light flare which occurred on June 11. Title: GINGA observation of the X-ray pulsar 1E 2259+586 in the supernova remnant G 109.1-1.0 Authors: Koyama, K.; Nagase, F.; Ogawara, Y.; Shinoda, K.; Kawai, N.; Jones, M. H.; Williams, O. R.; Watson, M. G.; Makishima, K.; Ohashi, T. Bibcode: 1989PASJ...41..461K Altcode: The X-ray pulsar 1E 2259+586 in the supernova remnant G109.1-1.0 was observed with the Ginga satellite from June 21 to 23, 1987. The heliocentric pulse period is found to be 6.978759 + or - 0.000002 s, confirming a secular spin down rate of 6.2 x 10 to the -13th s/s. The pulsation was observed to have asymmetric double peaks in the energy range from 1 keV to 10 keV. The upper limit on the projected semimajor axis is 0.08 1t-s (3sigma) throughout the period range searched. The constraint on the binary system is discussed in the light of this new upper limit. The energy spectrum of 1E 2259+586 does not show a single power law spectrum but exhibits a complex structure which mimics an emission line at 7.2 keV. An attempt to ascribe the structure to a cyclotron line feature is presented. This interpretation implies a weak magnetic field of 5 x 10 to the 11th G at the neutron star surface of 1E 2259+586. Title: Ginga observation of the X-ray pulsar 1E2259+586 in the supernova remnant G109.1-1.0. Authors: Shinoda, K.; Koyama, K.; Nagase, F.; Ogawara, Y.; Kawai, N. Bibcode: 1988pnsb.conf...67S Altcode: 1988pbsb.conf...67S The authors observed 1E 2259+586 on June 21-23, 1987 with the Ginga satellite. In this paper they report briefly the pulse profile, the pulse period and energy spectrum observed.