The UK FMOS spectrograph forms part of Subaru's FMOS multi-object infrared spectroscopy facility. The spectrograph
was shipped to Hilo in component form in August of 2007. We describe the integration sequence for the spectrograph,
the results of cooldown tests using a new chiller unit fitted to the spectrograph at the telescope, and alignment tests of the
spectrograph, gratings and OH-suppression masks. We present the first-light observations for the spectrograph from May
FMOS: the Fiber Multiple-Object Spectrograph is the next common-use instrument of the Subaru Telescope,
having a capability of 400 targets multiplicity in the near-infrared 0.9-1.8μm wavelength range with a field
coverage of 30' diameter. FMOS consists of three units: 1) the prime focus unit including the corrector lenses,
the Echidna fiber positioner, and the instrument-bay to adjust the instrument focus and shift the axis of the
corrector lens system, 2) the fiber bundle unit equipping two fiber slits on one end and a fiber connector box with
the back-illumination mechanism on the other end on the bundle, 3) the two infrared spectrographs (IRS1 and
IRS2) to obtain 2×200 spectra simultaneously. After all the components were installed in the telescope at the
end of 2007, the total performance was checked through various tests and engineering observations. We report
the results of these tests and demonstrate the performance of FMOS.
We describe the build phase of the UK FMOS spectrograph, a 200 fibre cooled OH Suppression infrared spectrograph
being constructed as part of Subaru's Fibre Multi Object Spectroscopy facility. Here we describe recent UK activities
within the FMOS programme and the likely schedule for commissioning at Subaru.
The GLAS (Ground-layer Laser Adaptive-optics System) project is to construct a common-user Rayleigh laser beacon that will work in conjunction with the existing NAOMI adaptive optics system, instruments (near IR imager INGRID, optical integral field spectrograph OASIS, coronagraph OSCA) and infrastructure at the 4.2-m William Herschel Telescope (WHT) on La Palma. The laser guide star system will increase sky coverage available to high-order adaptive optics from ~1% to approaching 100% and will be optimized for scientific exploitation of the OASIS integral-field spectrograph at optical wavelengths. Additionally GLAS will be used in on-sky experiments for the application of laser beacons to ELTs. This paper describes the full range of engineering of the project ranging through the laser launch system, wavefront sensors, computer control, mechanisms, diagnostics, CCD detectors and the safety system. GLAS is a fully funded project, with final design completed and all equipment ordered, including the laser. Integration has started on the WHT and first light is expected summer 2006.
We present results from cryogenic tests of a Volume-Phase Holographic
(VPH) grating at 200 K measured at near-infrared wavelengths. The aims
of these tests were to see whether the diffraction efficiency and
angular dispersion of a VPH grating are significantly different at a low temperature from those at a room temperature, and to see how many
cooling and heating cycles the grating can withstand. We have completed 5 cycles between room temperature and 200 K, and find that the performance is nearly independent of temperature, at least over the temperature range which we are investigating. In future, we will not only try more cycles between these temperatures but also perform
measurements at a much lower temperature (e.g., ~80 K).
Control software for astronomy matches the ever increasing complexity of new large instrumentation projects. In order to speed the development cycle, object-oriented techniques have been used to generate loosely coupled software objects and larger scale components that can be reused in future projects. Such object-oriented systems provide for short development cycles which can respond to changing requirements and allow for extension. The Unified Modeling Language (UML) has been used for the analysis, design and implementation of this software. A distributed system is supported by the use of an object broker such as CORBA. These techniques are being applied to the development of an instrument control system for the UK spectrograph within FMOS (Fiber-fed Multi-Object Spectrograph). This is a second generation instrument for the Subaru Telescope of the National Astronomical Observatory of Japan.