排序方式： 共有14条查询结果，搜索用时 31 毫秒
1.
A. S. Shugarov N. V. Chupina A. E. Piskunov N. V. Kharchenko 《Astrophysics and Space Science》2011,335(1):317-321
Precise pointing and stabilization of the T-170M telescope (World Space Observatory Ultraviolet, WSO-UV project) is provided
by the Fine Guidance System (FGS) that uses a guide star catalogue (Master Catalogue). To verify the photometric system of
the Master Catalogue we have carried out ground based observations with a CCD-camera in a spectral band, close to that of
FGS. We have found, that the photometric quality of the Master Catalogue is sufficient for FGS operations. The mean photometric
error in the range of 14–17 mag is ±0.23 mag; its variation over the sky does not exceed the factor of two. 2% of stars from
the Master Catalogue have photometric errors higher than 2 mag. We have also found a correlation between large photometric
errors and the Master Catalogue flags. 相似文献
2.
Astronomy Reports - On the basis of the Gaia data, we analyze the formation pattern of peripherical structures of planetary systems, the elements of which are dust, asteroids, comets, and unbound... 相似文献
3.
Vereshchagin S. V. Tutukov A. V. Chupina N. V. Postnikova E. S. Sizova M. D. 《Astronomy Reports》2022,66(5):361-386
Astronomy Reports - The aim of this study is to search for close binary gravitationally bound pairs of open star clusters (CBOCs). We divided the observed pairs of clusters into visual binaries... 相似文献
4.
2MASS is the most complete, homogeneous, and least contaminated catalog among the deep all-sky catalogs of stellar data produced to date. These qualities allow it to be successfully used not only for astrophysical studies, but also for solving various problems of all-sky astrometry and for operational support of automated telescopes. However, the lack of optical photometry in the catalog prevents its potential from being completely unveiled. To overcome this shortcoming, we have developed a procedure for transforming the 2MASS near-infrared magnitudes to optical magnitudes R J relative to the UCAC2 magnitudes R U . As a result of applying this procedure, all 2MASS objects have gotten optical magnitudes with effective wavelengths between the V and R bands of the Johnson system. The resulting transformation accuracy \(\varepsilon _{R_J } \) < 0 . m 5). We also give a brief overview of the present-day all-sky catalogs with emphasis on their photometric properties and completeness. 相似文献
5.
A test of the photometric calibration accuracy for the guide-star catalog (Master Catalog) of the Spectrum-UV project (World
Space Observatory—Ultraviolet) has been performed using CCD observations in a spectral band close to that of the guide sensor
system of the T-170M space telescope. The mean photometric uncertainty of the Master Catalog at 14
m
–17
m
is 0.23
m
; variations in this uncertainty over the sky are within a factor of two. About 2% of the stars in the Master Catalog were
found to have photometric errors in excess of 2
m
. We analyze the correspondence of large photometric errors to flags of the Master Catalog. 相似文献
6.
Six Tautenburg astrograph plates have been used to derive proper motions for 12 740 stars in the region of the Great Nebula
in Orion. The Oricat catalog of proper motions and B and R photometry has been compiled, incorporating as well data from other published catalogs. The proper motions presented in different
catalogs are compared. The Oricat catalog is useful for studies of features of the structure and kinematics of star clusters
and groups. 相似文献
7.
We consider kinematic inhomogeneities (stellar groups) in the corona of the Ursa Major flow. We show that the orientation of the major axis of the error ellipse for each star is defined by its position relative to its own apex. We apply the AD-diagram method suggested by us earlier; a statistical analysis confirms the existence of stellar groups in the corona of the Ursa Major flow. 相似文献
8.
Data from the Hipparcos catalog are used to study the internal kinematics of the Hyades cluster. Cluster members whose proper motions and parallaxes are known with precisions not less than 5 mas/yr and 3 mas were used. The proper motions were reduced to the cluster center. A correlation between a component of the tangential velocity and the parallax provides evidence for possible rotation of the cluster. The total velocity gradient is 0.04±0.03 km s?1 pc?1. The rotation axis is located perpendicular to the direction to the Hyades apex on the celestial sphere. 相似文献
9.
W. H. Elsanhoury E. S. Postnikova N. V. Chupina S. V. Vereshchagin Devesh P. Sariya R. K. S. Yadav Ing-Guey Jiang 《Astrophysics and Space Science》2018,363(3):58
A study of cluster characteristics and internal kinematical structure of the middle-aged Pleiades open star cluster is presented. The individual star apexes and various cluster kinematical parameters including the velocity ellipsoid parameters are determined using both Hipparcos and Gaia data. Modern astrometric parameters were taken from the Gaia Data Release 1 (DR1) in combination with the Radial Velocity Experiment Fifth Data Release (DR5). The necessary set of parameters including parallaxes, proper motions and radial velocities are used for \(n=17\) stars from Gaia DR1+RAVE DR5 and for \(n=19\) stars from the Hipparcos catalog using SIMBAD data base. Single stars are used to improve accuracy by eliminating orbital movements. RAVE DR5 measurements were taken only for the stars with the radial velocity errors not exceeding \(2~\mbox{km}/\mbox{s}\). For the Pleiades stars taken from Gaia, we found mean heliocentric distance as \(136.8 \pm 6.4\) pc, and the apex position is calculated as: \(A_{CP}=92^{\circ }.52\pm 1^{\circ }.72\), \(D_{CP}=-42^{\circ }.28\pm 2^{\circ }.56\) by the convergent point method and \(A_{0}=95^{\circ }.59\pm 2^{\circ }.30\) and \(D_{0}=-50^{\circ }.90\pm 2^{\circ }.04\) using AD-diagram method (\(n=17\) in both cases). The results are compared with those obtained historically before the Gaia mission era. 相似文献
10.
The internal kinematics of the Ursa Majoris stellar flow is considered. The details of the flow structure are considered, and new candidate members are searched for using high-precision Gaia DR1 TGAS data. The flow structure is studied using apex diagrams, which have been shown to be effective in studies of open clusters. To select member-stars of the flow, a chain of filters was applied to the spatial coordinates and velocities, photometric data, and elemental abundances of potential members. The nonuniform kinematic structure of the flow, manifest through its separation into different velocity directions for the core and three groups in the corona, is confirmed. Several filters were used to identify three candidate members. These included apex diagrams, MV?(B?V)0 diagrams, and the abundances of Fe, Mg, Al, Si, Ti, and Ni. 相似文献