The transformation of the coordinates of a gamma burst source to a star catalogue

1981 ◽  
Vol 75 (1) ◽  
pp. 219-224 ◽  
Author(s):  
G. S. Bisnovaty-Kogan ◽  
I. V. Estulin ◽  
N. G. Havenson ◽  
V. G. Kurt ◽  
G. A. Mersov ◽  
...  
1981 ◽  
Vol 30 (1-4) ◽  
pp. 467-470 ◽  
Author(s):  
G. Pizzichini ◽  
J. Danziger ◽  
P. Grosb� ◽  
M. Tarenghi ◽  
T. L. Cline ◽  
...  

2000 ◽  
pp. 327-459
Author(s):  
Patrick Moore
Keyword(s):  

1981 ◽  
pp. 467-470
Author(s):  
G. Pizzichini ◽  
J. Danziger ◽  
P. Grosbøl ◽  
M. Tarenghi ◽  
T. L. Cline ◽  
...  

1983 ◽  
Vol 62 ◽  
pp. 73-90

The catalogue is divided into three sections: bright stars with magnitudes less than or equal to 6.7: other stars having numbers in the Smithsonian Astrophysical Star Catalogue with magnitudes greater than 6.7: and other stars with no SAO numbers, usually faint and with often only fragmentary information concerning their magnitudes or spectra.Each section has the following columns: SAO number, other name, magnitude, spectral type, run number of the observation, date in obvious coded form, grade — grade zero indicates no duplicity, grade 1 possible duplicity, grade 2 probable duplicity, and grade 3 certain duplicity. Grades are based on statements by observers. For grades other than zero the vector separation and its computed error are given in arc milliseconds. P.A. denotes the direction in which the vector separation is measured, that is the position angle on the lunar limb as modified by the slope deduced in favorable cases from the spacing of the diffraction bands on the occultation trace. The next column gives the limb slope and its error.


2001 ◽  
Vol 200 ◽  
pp. 84-92 ◽  
Author(s):  
Andrei Tokovinin

The available information on the statistics of high multiplicity (3–6 components) systems is reviewed. The ratio of triple to binary systems is f3 ≍ 0.11, while fn ≍ 0.25 for higher n. Despite selection effects in the multiple star catalogue, the signatures of formation mechanisms are found in the distributions of period ratios and mass ratios. For example, the frequent occurrence of close sub-systems with periods less than 6 days can be explained by tidal dissipation in a 3-body system. In triple stars the angular momentum vectors of inner orbits are inclined to those of outer orbits by an average angle of 50°, hence the orbital spins are neither co-aligned nor completely random. Close binaries have a tendency to be found in higher-multiplicity systems, showing that close and wide binarity is statistically related. Future theoretical and observational studies are outlined.


1997 ◽  
Vol 165 ◽  
pp. 547-550
Author(s):  
M. Assafin ◽  
R. Vieira Martins ◽  
A.H. Andrei

AbstractWe present results of CCD observations for 85 quasars with −80° ≤ δ ≤ +20° declination, belonging to the International Celestial Reference System (ICRS). The positions are referred to the Carlsberg Series (CAMC) and PPM catalogues. We discuss a method which allows one to obtain precise positions based only on CCD observations, on the use of the Digitized Sky Survey of ST ScI and on the Guide Star Catalogue. The results are compared with the VLBI positions.


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