共查询到20条相似文献，搜索用时 15 毫秒
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2.
G. I. Pinigin 《Astrophysics and Space Science》1991,177(1-2):225-227
Observing programs are discussed for the Pulkovo automatic horizontal meridian circle. The instrument is highly efficient and yields precise and accurate positions. We prepare an observing program of faint FK5 stars with the aim of improving on the system of this catalogue and also prepare a program of observations of IRS reference catalogue stars. 相似文献
3.
The catalogue of positions and stellar V magnitudes of up to 17 m stars in the declination zone from 2° to 5.5° has been compiled. The catalogue includes 2.05 × 106 stars and is based on the observations performed in 2010–2015 on the meridian axial circle (MAC) of GAO NAN Ukraine and the Astronomical Observatory of Taras Shevchenko National University. The errors of the positions and photometry for stars of 11–14 magnitude are 0.06″–0.08″ and 0.04 m –0.08 m , respectively. 相似文献
4.
A new list of reference stars for differential meridian observations is proposed. The list inclides 905 stars of stellar magnitude 7–9 with 3–5 stars in each area of 252 compact extragalactic radio sources, available for high precision measurements in radio and optics. 相似文献
5.
Abstract— Infrared spectra of mineral grains from primitive meteorites could be useful for comparison with astronomical infrared spectra since some of their grains might be similar to those formed in the planet‐forming disks around young stars or in the envelopes surrounding late‐type stars. To assess the usefulness of meteorite spectra, olivine grains separated from primitive meteorites have been analyzed using FTIR microscope techniques in the 2–16 μm wavelength range. The sub‐micron sizes of the grains made a complex preparation process necessary. Five characteristic bands were measured near 11.9, 11.2, 10.4, 10.1, and 10.0 μm. The results of 59 analyses allow the calculation of band positions for meteoritic olivines as a function of their iron and magnesium contents. Comparison of the meteoritic results with astronomical data for comets and dust around young and old stars, which exhibit bands similar to the strongest infrared bands observed in the grains (at 11.2 μm), show that the spectral resolution of the astronomical observations is too low to ascertain the exact iron and magnesium (Mg: Fe) ratio of the dust in the 8–13 μm wavelength range. 相似文献
6.
P. F. Lazorenko V. L. Karbovs’kyi O. V. Denysiuk Yu. G. Babenko M. I. Buroms’kyi S. I. Kas’ian O. M. Koval’chuk 《Kinematics and Physics of Celestial Bodies》2007,23(5):221-226
We describe the modifications made in the design of the Kyiv meridian axial circle (MAC) and in the observation technique after the instrument was equipped with a CCD camera with an array of 1040×1160 pixels. The observations are performed in the drift-scan mode (time-delay imaging) with an effective exposure time of 108 s for equatorial stars. The MAC photometric system reproduces the standard V system; the limiting magnitude is V = 17 m . The observations made with the modified MAC in 2001–2003 served as the basis for the KMAC1 catalog which contains positions, proper motions, and magnitudes B, V, R, r′, J for 100 000 stars in the sky areas with the ICRF objects. The errors of positions and V magnitudes in the catalog are 50–90 mas and 0.1 m , respectively, for stars with V = 15 m . Stars in the equatorial sky areas and radio stars are presently observed with the aim to determine their exact positions, proper motions, and magnitudes. The catalogs are available in the data base of the Centre de Données Astronomiques de Strasbourg (ftp.cdsarc.u-strasbg.fr) and on the site of the Main Astronomical Observatory (http://www.mao.kiev.ua). 相似文献
7.
利用北京天文台具有ＣＣＤ终端的６０ｃｍ光学望远镜（Ｖ波段）观测射电源的光学对应体，得到了０７１６＋７１４和０８３９＋１８７精确的光学位置。参考星表采用拉帕尔玛（ＬａＰａｌｍａ）的１８ｃｍ全自动子午环观测资料编制的ＣＡＭＣ星表，该星表是ＦＫ５星表系统。两颗源位置的内符精度约为０．″１９，与其他作者给出的光学和射电位置观测结果分别进行了比较 相似文献
8.
The paper deals with the method based on treating the axial meridian circle and a long-focus light mark in the prime vertical as a single virtual instrument that has properties of meridian circle. A horizontal axis, a sighting line, and a micrometer cross-wire of the instrument are created by optical means. The key function here is performed by the light mark that ensures a reference direction used for formation of instrumental principal planes and directions. Stability of instrumental azimuth, inclination, and collimation is expected to be about ±0.″01. Besides, an accuracy of observations is not affected by any temperature and weight deformations of telescope mechanics. Owing to the last circumstance, the design is cheap and the telescope aperture may be increased significantly, to about 1m. An estimate of accuracy of observations depends on the adopted model of image motion, and for sites with excellent seeing and bright stars is ±0.″03 to ±0.″05 (rms). 相似文献
9.
Peng Qing-yu Mao Wei 《紫金山天文台台刊》1998,(2)
This paper presents a new method to determine precisely the barycentric positions of the outer planets(Saturn - Neptune)by optical observations. It requires the CCD observations from a long focal distance telescope which is used to observe a planet and its satellites and ones from a meridian circle when it works in a CCD drift scanning manner. The key part of the method is tested by the observations with 1 meter telescope of Yunnan Observatory. The result shows that the new method is feasible to carry out. 相似文献
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V. L. Karbovs’ky P. F. Lazorenko V. N. Andruk V. V. Kleshchenok M. O. Litvin K. O. Bogatyrev E. V. Denisyuk 《Kinematics and Physics of Celestial Bodies》2011,27(4):204-210
Specifications of a new Apogee Alta U47 CCD camera mounted at the Kyiv meridian axial circle (MAC) are presented. The camera
is based on the 1024 × 1024 pxl e2v CCD47-10 with pixel sizes of 13 × 13 μm. Observations are carried out in the scan-drift
mode with an effective exposure time of 77 s for equatorial stars. The MAC photometric system answers the standard Johnson
V band, the MAC limiting magnitude V is 17
m
. The test MAC observations of 2009 give positional accuracy and V magnitude errors equal to approximately 0.1″ and 0.09
m
, respectively, for Tycho-2 stars. The telescope is used for observations of equatorial stars with the purpose of detecting
their positions, proper motion, and brightness. 相似文献
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N. V. Maigurova M. V. Martynov G. I. Pinigin 《Kinematics and Physics of Celestial Bodies》2013,29(1):44-51
On the base of CCD-observations made with the axial meridian circle of the Nikolaev Observatory from 2008 to 2009, we compiled a catalogue for astrometric positions and proper motions for 140321 stars located in an ecliptic zone and around high proper motion stars. The root-meansquare error for a star position is 20–65 mas in right ascension and 30–70 mas in declination. The UCAC2 catalogue is used as a reference for astrometric reductions. To derive stars’ proper motion and to estimate systematic errors of the compiled catalogue, cross-identification of the obtained data with modern astronomic catalogues Tycho2, 2MASS, CMC14, LSPM, PPMX, USNO-A2, and XPM-1.0 is performed. In addition to star position and proper motion, our catalogue contains photometric values B, V, r’, J, H, and K taken from other catalogues. 相似文献
14.
V. P. Ryl’kov N. V. Narizhnaya A. A. Dement’eva G. I. Pinigin N. V. Maigurova M. V. Martynov 《Kinematics and Physics of Celestial Bodies》2011,27(6):299-303
A compiled catalogue of 21 440 stars with magnitudes between 10 and 17 is prepared from original observations made at the end of the 20th century to the beginning of the 21st century. The catalogue contains 227 fields of the celestial sphere centered at ICRF extragalactic radio sources with declinations of ?17 to +89°. The field size is 40′ for both right ascension and declination. The internal accuracy of positions for both coordinates is no worse than 0.1″. A comparison of the stellar positions with the UCAC2 and CMC13 catalogues shows that the average external accuracy is approximately 0.05–0.15″. The positions of 10 795 stars with declinations to +50° are given for the epoch and equinox of J2000.0, whereas the positions of other stars are given for the epoch of observation. 相似文献
15.
T. S. Bastian 《Solar physics》1990,130(1-2):265-294
Observations of radio emission from flare stars are reviewed, including surveys of flare stars in the solar neighborhood and in stellar associations, studies of quiescent emission, and continuum and spectral studies of radio burst emission. The radio observations are placed in an observational context provided by soft X-ray, UV, and optical observations. It is stressed that, as is the case for the latter wavelength regimes, observations of rado bursts on flare stars are qualitatively similar to those on the Sun, albeit in a dramatically scaled-up fashion. 相似文献
16.
C. de Vegt J. A. Hughes D. Jauncey G. White K. J. Johnston J. Russell G. Nicholson 《Astrophysics and Space Science》1991,177(1-2):199-202
An observational pilot program is described which provides a first step towards the construction of an inertial extragalactic reference frame from optical and radio measurements. Candidate objects will be selected from extragalactic compact radio sources which display optical counterparts. Galactic radio stars will be secondary reference objects. The reference frame will be defined by the radio positions of the extragalactic objects. Based on a coordinated effort in both hemispheres, a global homogeneous net of about 400 quasars and 100 radio stars is expected to result from a five year campaign. 相似文献
17.
Presented is a method of global adjustment of stars' right ascensions for the compilation of an independent catalog obtained with a meridian circle. The concept of the problem is shown first, in which corrections to the catalog positions of observed stars can be determined directly by solving a set of observation equations constructed over many of nights. Some parameters such as clock correction, azimuth of artificial azimuth marks, and the correction to an adopted value of the latitude are assumed to vary regularly over the observation period. The present method is applied to the determination of the absolute azimuth of the Tokyo PMC by using upper and lower transits of azimuth stars. 相似文献
18.
F. G. Ajupov R. I. Gumerov V. B. Kapkov B. K. Bagildinsky V. N. Ershov K. N. Naumov O. Yu. Nikiforova T. R. Kirijan Yu. G. Ostrensky Yu. S. Streletsky B. N. Smirnov A. A. Pozhalov V. D. Shkutov G. I. Pinigin A. V. Sergeev O. E. Shornikov 《Astrophysics and Space Science》1991,177(1-2):219-223
The results of investigations and observations with classical meridian circle MK-200 and photographic vertical circle (PVC) after its modernization and automation are discussed. The data concerning the stability of the instrumental system and the flexure of the Pulkovo Horizontal meridian circle (HMC) are given. New work on the establishment of in axial meridian circle in Nikolaev, Ecker meridian circle and reflecting one in Pulkovo is mentioned. 相似文献
19.
Graeme L. White David L. Jauncey Bruce R. Harvey Ann Savage Samuel Gulkis Robert A. Preston Bruce A. Peterson John E. Reynolds George D. Nicolson D. F. Malin 《Astrophysics and Space Science》1991,177(1-2):79-83
An overview is presented of a number of astrometry and astrophysics programs based on radio sources from the Parkes 2.7 GHz catalogues. The programs cover the optical identification and spectroscopy of flat-spectrum Parkes sources and the determination of their milliarc-second radio structures and positions. Work is also in progress to tie together the radio and Hipparcos positional reference frames. A parallel program of radio and optical astrometry of southern radio stars is also under way. 相似文献
20.
Determination of the azimuth error of the transit instrument by means of prime vertical observations
《Chinese Astronomy and Astrophysics》1984,8(1):8-13
We present the principle and some test results of determining the instrumental azimuth by measuring the times of passage of the same stars through the meridian and the prime vertical. The test measurements were made on a reconstructed Zeiss transit instrument, equipped with four supporting pillars. The results of the test (TABLE 1) show that the method is successful. Applied to the meridian circle, this method replaces the traditional method of determining the absolute azimuth by observing circumpolar stars and thereby by-passes the difficulties inherant therein and the errors involved in the method of transfer via the azimuth mark. 相似文献