共查询到10条相似文献，搜索用时 593 毫秒
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光电测微器是中－丹水平子午环最关键的部分．本文介绍了数据采集系统的设计思想．根据长期对仪器的测试和观测结果分析，表明系统完全达到设计要求，同时为下一步改装成ＣＣＤ终端，观测极限星等达１７ｍ．５提供了可行的方案． 相似文献
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Erik Høg 《Astrophysics and Space Science》1991,177(1-2):203-208
The flexure term and a correction to the atmospheric refraction constant calculated from meteorological data may be determined from the zenith distances of FK5 stars observed each night on a meridian circle. All such determinations on meridian circles and vertical circles have been corrupted-and in fact dominated-byinternal refraction which is often larger than 1" and quite variable. After removing internal refraction by a simple equipment at the CAMC on La Palma, it became apparent that the true flexure and the true correction to the calculated refraction constant vary by less than 0."09 (rms) from night to night. This is a reduction of the estimated uncertainty of these quantities by a factor of about four. This improvement is expected at any meridian circle which is equipped with sufficiently precise (photoelectric) micrometers if internal refraction were removed.Alternative forms of the observation equation for declinations are discussed. Observations over a period of two months may be solved in oneglobal least-squares solution keeping the refraction and the flexure terms constant. Furthermore, one per star is obtained, instead of a different each night for each star. 相似文献
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The long term evolution of the metallic divided circle mounted on the Bordeaux meridian instrument is presented. Results of three independent determinations carried out in 1987 with different ambient temperatures show deviations the major part of which could be due to small malfunction of the photoelectric reading microscopes. The importance of a regular monitoring of the division errors is stressed. 相似文献
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We have measured the spectrum of Titan near 5 micrometers and have found it to be dominated by absorption from the carbon monoxide 1-0 vibration-rotation band. The position of the band edge allows us to constrain the abundance of CO in the atmosphere and/or the location of the reflecting layer in the atmosphere. In the most likely case, 5 micrometers radiation is reflected from the surface and the mole fraction of CO in the atmosphere is qCO=10(+10/-5) ppm, significantly lower than previous estimates for tropospheric CO. The albedo of the reflecting layer is approximately 0.07(+0.02/-0.01) in the 5 micrometers continuum outside the CO band. The 5 micrometers albedo is consistent with a surface of mixed ice and silicates similar to the icy Galilean satellites. Organic solids formed in simulated Titan conditions can also produce similar albedos at 5 micrometers. 相似文献
6.
Bregman JD Campins H Witteborn FC Wooden DH Rank DM Allamandola LJ Cohen M Tielens AG 《Astronomy and Astrophysics》1987,187(1-2):616-620
Spectrophotometry from 5-10 micrometers (delta lambda/lambda approximately 0.02) of comet Halley was obtained from the Kuiper Airborne Observatory on 1985 December 12.1 and 1986 April 8.6 and 10.5, UT. 8-13 micrometers data were obtained on 17.2 December 1985 from the Nickel Telescope at Lick Observatory. The spectra show a strong broad emission band at 10 micrometers and a weak feature at 6.8 micrometers. We do not confirm the strong 7.5 micrometers emission feature observed by the Vega 1 spacecraft. The 10 micrometers band, identified with silicate materials, has substructure indicative of crystalline material. The band can be fitted by combining spectra data from a sample of interplanetary dust particles. The primary component of the silicate emission is due to olivine. The 6.8 micrometers emission feature can be due either to carbonates or the C-H deformation mode in organic molecules. The lack of other emission bands is used to place limits on the types of organic molecules responsible for the emission observed by others at 3.4 micrometers. Color temperatures significantly higher than the equilibrium blackbody temperature indicate that small particles are abundant in the coma. Significant spatial and temporal variations in the spectrum have been observed and show trends similar to those observed by the spacecraft and from the ground. Temporal variability of the silicate emission relative to the 5-8 micrometers continuum suggests that there are at least two physically separated components of the dust. 相似文献
7.
Bregman JD Allamandola LJ Tielens AG Geballe TR Witteborn FC 《The Astrophysical journal》1989,344(2):791-798
We have studied the spectral and spatial distribution across the Orion Bar of the 3-14 micrometers emission, including hydrogen Brackett alpha and 12.8 micrometers [Ne II] emission lines and several "dust" emission features. The data indicate that the "dust" consists of three components; (1) "classical" dust with a temperature of approximately 60 K accounting for emission longward of 20 micrometers, (2) amorphous carbon particles or polycyclic aromatic hydrocarbon (PAH) clusters (approximately 400 C atoms) which produce broad emission features in the 6-9 and 11-13 micrometers bands, and (3) free PAHs which emit in sharper bands (most strongly at 3.3, 6.2, 7.7, 8.6, and 11.3 micrometers). The 3.3 and 11.3 micrometers features, which are due to C-H modes, are well correlated spatially, while the 7.7 micrometers band, due to C=C modes, has a different distribution than the 3.3 and 11.3 micrometers bands. We conclude that the sharp emission bands arise in the photodissociation transition region between the H II region and the molecular cloud and are not present in the H II region. The broad continuum feature extending from 11-13 micrometers is strong in both regions. Previous broad-band observations of the 10 and 20 micrometers flux distributions, which show that the 10 micrometers radiation extends farther into the neutral gas to the south than the 20 micrometers radiation, suggest that some of the 10 micrometers flux is supplied via a nonthermal mechanism, such as fluorescence. 相似文献
8.
《Chinese Astronomy and Astrophysics》1984,8(1):54-62
The General Catalogue of Photoelectric Astrolabe Stars (GCPA) based on the Chinese photoelectric astrolabe system is described. It is a combined system of right ascension and declination synthesized from four primitive star catalogues' obtained with the photoelectric astrolabe. Four other primitive catalogues obtained with the Danjon astrolabe are reduced to the combined system and added to it. GCPA contains 1579 stars, 1541 Δα values and 1131 Δδ values. The overall average accuracy is ±3.3 ms in Δα, and ±0″.058 in Δδ; for the FK4 stars, the corresponding values are ±2.3 ms and ±0″.042. FK4 stars observed by two or more instruments gave 485 Δα values and 349 Δδ values, with external accuracies ±3.8 ms and ±0″.041. Corrections to the FK4 system as determined by GCPA are given and a comparison with the relevant catalogues is presented. 相似文献
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R. F. Griffin 《Journal of Astrophysics and Astronomy》2001,22(2-3):187-211
The four stars treated in this paper have been under observation with photoelectric radial-velocity spectrometers for many
years. They have proved to be binaries with periods of 30, 1828, 1514 and 822 days respectively; the orbits are of modest
eccentricity apart from that of HD 110743 which is indistinguishable from a circle. The mass functions are small, and no companion
has been observed for any of the stars. HD 110743, a K dwarf, is much the nearest of the four, and its orbit is of short enough
period for the photocentric motion to have been recognized byHipparcos. An eleventh-magnitude star rather more than 1≈ away from HD 106104 is shown to be a genuine physical companion, with practically
identical radial velocity, proper motion and distance modulus, although the projected separation is about 13,000 AU. 相似文献
10.
Since 1983, a TI 800×800 CCD has been routinely used on the 1.5-m astrometric reflector during dark time to measure parallaxes of faint (V16.0) stars. The rest of the time remains devoted to the fine grain (Kodak type IIIa emulsions) photographic parallax program, which now uses magnitude compensating filters to extend the range of the program to V=0. Sufficient data are now available to evaluate the precisions of these programs. For CCD fields, the mean error for the relative parallax ranges from ±0".0025 for fields with relatively few observations to ±0".0005 for intensively observed fields such as vB10. The photographic program is now producing relative parallaxes with average mean errors of ±0".0026 compared to ±0".0038 previously obtained with coarse grain emulsions. 相似文献