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TRIDENT: An Infrared Differential Imaging Camera Optimized for the Detection of Methanated Substellar Companions
We describe a near-infrared camera in use at the Canada-France-HawaiiTelescope (CFHT) and at the 1.6 m telescope of the Observatoire du montMégantic (OMM). The camera is based on a Hawaii-1 1024 ×1024 HgCdTe array detector. Its main feature is the acquisition of threesimultaneous images at three wavelengths across the methane absorptionbandhead at 1.6 μm, enabling, in theory, an accurate subtraction ofthe stellar point-spread function (PSF) and the detection of faintclose, methanated companions. The instrument has no coronagraph andfeatures fast data acquisition, yielding high observing efficiency onbright stars. The performance of the instrument is described, and it isillustrated by laboratory tests and CFHT observations of the nearbystars GL 526, υ And, and χ And. TRIDENT can detect (6 σ)a methanated companion with ΔH=9.5 at 0.5" separation from thestar in 1 hr of observing time. Non-common-path aberrations andamplitude modulation differences between the three optical paths arelikely to be the limiting factors preventing further PSF attenuation.Instrument rotation and reference-star subtraction improve the detectionlimit by a factor of 2 and 4, respectively. A PSF noise attenuationmodel is presented to estimate the non-common-path wave-front differenceeffect on PSF subtraction performance.Based on observations obtained at the Canada-France-Hawaii Telescope(CFHT), which is operated by the National Research Council of Canada,the Institut National des Science de l'Univers of the Centre National dela Recherche Scientifique of France, and the University of Hawaii.
| A preliminary compilation of DS-programme star positions
A catalog is presented of the double-star-program (DS-program) starpositions, listing right ascensions for 930 DSs and declinations for1225 DSs of the program. The positions were compiled from the observedvalues obtained between 1980 and 1987 with the meridian circles of sixUSSR observatories (the Moscow, Kazan', Kiev, Khar'kov, Odessa, andTashkent Observatories) and the Belgrade Observatory. The measurementsand the treatment of the observational material were performed using therelative method, and the FK-4 system stars were used as reference stars.
| A second list of wide visual binaries
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| A second list of wide visual binaries
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| Mesures d'etoiles doubles faites a Nice.
Abstract image available at:http://adsabs.harvard.edu/cgi-bin/nph-bib_query?1978A&AS...33..275M&db_key=AST
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