Search

We have determined the isotopic abundance ratio of 7Li/6Li in the interstellar media (ISMs) along lines of sight to HD169454 and HD250290 using the High-Dispersion Spectrograph on the Subaru Telescope. We also observed ζ Oph for comparison with previous data. The observed abundance ratios were 7Li/6Li = 8.1+3.6 –1.8 and 6.3+3.0 –1.7 for HD169454 and HD250290, respectively. These values are in reasonable agreement with those observed previously in the solar neighborhood ISMs within ±2σ error bars and are also consistent with our measurement of 7Li/6Li = 7.1+2.9 –1.6 for a cloud along the line of sight to ζ Oph. This is good evidence for homogeneous mixing and instantaneous recycling of the gas component in the Galactic disk. We also discuss several source compositions of 7Li, Galactic cosmic-ray interactions, stellar nucleosynthesis, and big bang nucleosynthesis.

An overview of the current status of the 8.2 m Subaru Telescope constructed and operated at Mauna Kea, Hawaii, by the National Astronomical Observatory of Japan is presented. The basic design concept and the verified performance of the telescope system are described. Also given are the status of the instrument package offered to the astronomical community, the status of operation, and some of the future plans. The status of the telescope reported in a number of SPIE papers as of the summer of 2002 are incorporated with some updates included as of 2004 February. However, readers are encouraged to check the most updated status of the telescope through the home page, http://subarutelescope.org/index.html, and/or the direct contact with the observatory staff., Comment: 18 pages (17 pages in published version), 29 figures (GIF format), This is the version before the galley proof

We present high spatial resolution images of the gravitational-lens system PG 1115+080 taken with the near-infrared camera (CISCO) on the Subaru telescope. The FWHM of the combined image is $0.''32$ in the $K'$-band, yielding spatial resolution of $0.''14$ after a deconvolution procedure. This is a first detection of an extended emission adjacent to the A1/A2 components, indicating the presence of a fairly bright emission region with a characteristic angular radius of $\sim$ 5 mas (40 pc). The near-infrared image of the Einstein ring was extracted in both the $J$ and $K'$ bands. The $J-K'$ color is found to be significantly redder than that of a synthetic model galaxy with an age of 3 Gyr, the age of the universe at the quasar redshift., 11 pages, 6 figures. Accepted for publication in PASJ(2000)

The Japan National Large Telescope (SUBARU) is an 8.2 m optical-infrared telescope to be installed on top of Mauna Kea in Hawaii, to be operational in 1998. The control system for the SUBARU telescope is now in the design phase. The control system consists of distributed workstations, local processors, and data acquisition computers, which are interconnected by control LANs and data LANs. The control software uses message-based communication. Two key processes, a scheduler and a status logger cooperating with any other processes, are designed to ensure efficiency and security in observation processes. The main concept and functions of the control system for the SUBARU telescope are described.

Balmer and Paschen continuum emission as well as Balmer series lines of P Cygni-type profile from H_gamma through H_23 are revealed in the violet spectra of BM Gem, a carbon star associated with an oxygen-rich circumstellar shell (`silicate carbon star') observed with the high dispersion spectrograph (HDS) on the Subaru telescope. The blue-shifted absorption in the Balmer lines indicates the presence of an outflow, the line of sight velocity of which is at least 400 km s^-1, which is the highest outflow velocity observed to date in a carbon star. We argue that the observed unusual features in BM Gem are strong evidence for the presence of a companion, which should form an accretion disk that gives rise to both an ionized gas region and a high velocity, variable outflow. The estimated luminosity of ~0.2 (0.03-0.6) L_sun for the ionized gas can be maintained by a mass accretion rate to a dwarf companion of ~10^-8 M_sun yr^-1, while ~10^-10 M_sun yr^-1 is sufficient for accretion to a white dwarf companion. These accretion rates are feasible for some detached binary configurations on the basis of the Bond-Hoyle type accretion process. We concluded that the carbon star BM Gem is in a detached binary system with a companion of low mass and low luminosity. However, we are unable to determine whether this companion object is a dwarf or a white dwarf. The upper limits for binary separation are 210 AU and 930 AU for a dwarf and a white dwarf, respectively. We also note that the observed features of BM Gem mimic those of Mira (omi Cet), which may suggest actual similarities in their binary configurations and circumstellar structures., Comment: 11 pages, 2 figures, 1 table, accepted for publication in ApJ

The Subaru Telescope has been stably operated with high image quality since common use began in December2000. We have updated the following items in order to achieve further improvement of observation eciency,image quality, and tracking. 1. High re”ectivity of mirrors. The re”ectivity of the primary mirror has beenmaintained, yielding 84% at 670 nm by regular CO 2 cleaning (every two to three weeks). We successfully carriedout the silver coating of the Infrared secondary mirror in April 2003 without over-coating. The re”ectivity hasbeen maintained at greater 98% at 1,300 nm. 2. Image Quality. Subaru telescope delivers exceptional imagequality a median image size of 0.6 arc-second FWHM in the R -band as taken by Auto-Guider Cameras atall four foci; Prime, Cassegrain, and two Nasmyth. We optimized parameters of the servo control system ofthe Elevation servo, reducing the amplitude of 3 8 Hz vibration mode of the telescope and improving imagequality when using the Adaptive Optics (AO) system. 3. Acquisition Guiding. Dithering time was shortened byupdating the control software. The slit viewer camera for HDS and the “ber bundle for FMOS are available foracquisition guiding in addition to Auto-Guider Cameras. 4. New instruments. We are developing a new primefocus unit for FMOS and will start functional tests in 2005. Moreover, we have started to prepare new interfacesand facilities for FMOS and the new 188 element AO natural/laser guide star system. The focus switching timewill be shortened by updating the hardware of the IR and Cassegrain Optical secondary mirrors from September2004, reducing it to 10 minutes to switch the focus between Cassegrain and Nasmyth foci.Keywords: Subaru Telescope, Ground based Large Telescope, Astronomy

We report current status of active mirror support of Subaru telescope. Total wavefront error we provide for observation is 150-300 nm rms . Elevation dependency of the shape of the primary mirror and wind buffeting effect are shown. We also show a procedure for SH measurements at prime focus with half-cut (D-shape) pick-up mirror.

Accepted: 2014-08-29, 資料番号: SA1005003000

This paper describes a high dispersion spectrograph (HDS) now under construction towards the first-light phase of Subaru Telescope. It is located at a Nasmyth focus. HDS is an echelle spectrograph with grating as a post-disperser. The collimated beam size is 272 mm, and the echelle is 300 mm by 840 mm in total size (31.6 gr/mm, R-2.8). The overall throughput (resolution X slit width product) achieved is 38,000 arcseconds. HDS has two cross-dispersers (400 gr/mm, 250 gr/mm) which are optimized for blue- and red-wavelength regions, respectively. The camera is of catadioptric type system, consisting of three correctors and a mirror. It spans the entire chromatic range from 0.30 to 2.0 micrometer. It delivers 10-micrometer images on average within a flat 60 mm- diameter focal plane area in the wavelength range from 0.3 to 1.1 micrometer, without refocusing. This image quality corresponds to typical limiting spectral resolutions well above 300,000 though the resolution will generally be limited to less than this by the entrance slit width and finite CCD pixel sizes. The detector will be a 2 X 1 mosaic of 2k X 4k CCD's with 15-micrometer pixels. Typical limiting spectral resolution will be 100,000.© (1998) COPYRIGHT SPIE--The International Society for Optical Engineering. Downloading of the abstract is permitted for personal use only.

We adopt the hierarchy structure for the telescope control system of the Subaru Telescope. The system is made up of a TSC, three TWSs, three DCMOMs, three MLPs, and many LCUs. All devices are connected through local network each other.© (1998) COPYRIGHT SPIE--The International Society for Optical Engineering. Downloading of the abstract is permitted for personal use only.

The overall updated plan for constructing 7 scientific instruments and 3 baseline programs for the 8 m Subaru telescope is shown. Somewhat detailed descriptions are given further for projects to develop large format CCDs, faint object camera and spectrograph (FOCAS), high dispersion spectrograph (HDS), Subaru prime focus camera (Suprime-Cam), and Cassegrain adaptive optics system (AO).

An engineering prototype with a 62 cm thin meniscus mirror to investigate the practical problems of the JNLT active optics system has been constructed. The structure and the performance of the prototype and the basis for the control algorithms are described. The stiffness of the mirror and the purity of figure control for the correction of lower order Zernike modes were measured for this system. The results of experiments to control the surface figure of the mirror under varying elevation angle of the telescope or under external force load are reported. The thermal effects on this system were also evaluated.

Night airglow of oxygen 130.4 and 135.6 nm emissions was measured by a spectrophotometer aborad an S520 sounding rocket, launched at 19:50 JST (10:50 UT) on 14 February, 1982 from Kagoshima, Japan. The altitude variation of the emissions was obtained from 110 to 266 km at zenith angles of 35.5°±4°. The emission intensity around 260 km was about 160R and is roughly compatible with model calculations taking account of O++e − radiative recombination as well as O+−O− mutual neutralization. Some excess of about 50R, compared to the model calculation, was observed around 200 km. Possible explanations of the excess are: (i) remnant oxygen ions during the transition period from day to night and (ii) diffuse radiation from the background sky. Model calculations taking account of remnant oxygen ions were also performed by adding an excess electron density to the original density profile. However, it was found that an unreasonably large electron density is required around 200 km (∼5×105 cm−3) to produce the observed intensity. It is also probable that some contribution from the background sky is present in the observed intensity.