scholarly journals Automated Proper Motion Survey: Data Reduction and Initial System Performance

1970 ◽  
Vol 7 ◽  
pp. 26-47 ◽  
Author(s):  
A. E. La Bonte
Keyword(s):  
Data Reduction ◽  
Proper Motion ◽  
System Performance ◽  
Processing Time ◽  
The Other ◽  
Photographic Emulsion ◽  
Proper Motions ◽  
Plate Material ◽  
Schmidt Telescope ◽  
Plate Center

The Automated Proper Motion Survey (APMS) has three broad goals-accuracy, completeness, and efficiency in the discovery and measurement of stellar proper motions on pairs of red-sensitive photographic star plates taken with the forty-eight inch Schmidt telescope. The specific range of motions sought is from 0.1 to 2.5 seconds-of-arc per year. The lower limit of 0.1 arc sec/year is consistent with the inherent uncertainties in the photographic emulsion and the typical epoch difference between plate exposures. At the opposite end of the scale, extension of the search radius beyond that corresponding to 2.5 arc sec/year would result in a prohibitively large number of spurious matches and a significant increase in processing time while yielding extremely few (though individually interesting) additional stellar motions. The specific range of stellar magnitudes sought is from 12 to 19 red. Significant motions for stars brighter than the limit mred = 12 are already fairly well documented and the corresponding bright Schmidt images begin to show extensive contamination from diffraction spikes, “blazes” radially away from the plate center, and photographic “bloom”. At the other limit, although images of stars fainter than mred = 19 are visually discernible on the plates (the plate limit is typically mred= 20), inspection of the faintest images reveals that they are amorphous and often quite asymmetric clusters of photographic grain. Thus, both the motion limits and the magnitude limits for the survey have been selected to cover the range of reliable and largely unexplored data on the plate material. The implementation of APMS, then, is tailored to these goals and ranges.

scholarly journals Proper Motions Referred to Faint Galaxies

1986 ◽  
Vol 7 ◽  
pp. 89-92
Author(s):  
W. F. van Altena ◽  
T. Girard ◽  
C. E. López ◽  
A. R. Klemola ◽  
B. F. Jones ◽  
...  
Keyword(s):  
Proper Motion ◽  
Reference Frames ◽  
Photographic Plate ◽  
Proper Motions ◽  
Plate Material ◽  
Present Epoch ◽  
Magnitude Range ◽  
Large Numbers ◽  
Material Forming ◽  
Partial Extension

The Lick Northern Proper Motion (NPM) and the Yale-San Juan Southern Proper Motion (SPM) programs have been described on several occasions (Wright 1950; Deutsch and Klemola 1974; Vasilevskis 1973; and Wesselink 1974). The two programs represent an attempt to measure the coordinates and proper motions, with respect to the extragalactic reference frames, for large numbers of stars representing most of the astrophysically-recognized classes. The photographic plate material forming the basis of the NPM program derives from the first (1947-1954) and second (1970-present) epoch phases for 1246 fields with the Lick 51 cm Carnegie double-astrograph for centers at -20° and northward (Shane and Wirtanen 1967). A southern supplement of 144 additional fields takes the program to -30°. The SPM consists of 632 fields with centers at -20° and southward. The first epoch plates were taken between 1965 and 1974 and a partial extension of 72 fields to more northerly declinations is essentially complete. One short and one long exposure permit the measurement of positions and approximate photometry for selected stars and reference galaxies over the blue magnitude range from about 8 to 17-18.

scholarly journals The Tautenburg Schmidt Telescope and Galactic Proper Motion Studies

1995 ◽  
Vol 148 ◽  
pp. 267-270 ◽  
Author(s):  
E. Schilbach ◽  
R.-D. Scholz ◽  
S. Hirte
Keyword(s):  
Proper Motion ◽  
Galactic Plane ◽  
Proper Motions ◽  
Schmidt Telescope ◽  
Automatic Measuring ◽  
Wide Range ◽  
Motion Studies ◽  
Photographic Photometry ◽  
Better Than

AbstractThe combination of Tautenburg plates and automatic measuring machines provides a powerful tool to obtain photometry and proper motions of a great number of stars for statistical investigations of our Galaxy. Photographic photometry with an accuracy of about 0.07 mag can be obtained provided two plates of the same colour and a sufficient number of photometric standards are available. With two plate pairs and a 20 years baseline, a proper motion accuracy better than 4 mas/year can be achieved for stars over a wide range of magnitudes. Outside the Galactic plane proper motions are determined with respect to hundreds of background galaxies.

scholarly journals Proper Motions with respect to Galaxies (Invited Paper)

1974 ◽  
Vol 61 ◽  
pp. 193-200
Author(s):  
A. N. Deutsch ◽  
A. R. Klemola
Keyword(s):  
Southern Hemisphere ◽  
Proper Motion ◽  
Second Phase ◽  
Proper Motions ◽  
Schmidt Telescope ◽  
Complete Coverage ◽  
Physical Interest ◽  
Zone Of Avoidance

At Lick the second phase of the proper motion program is in progress. In addition to generally selected stars, as was done for the first phase, so far over 30000 stars of special types of astro-physical interest and about 29000 AGK3 stars have been selected for measurement.In accordance with the Pulkovo program, second-epoch photography with galaxies is being continued at Pulkovo, Moscow and Tashkent, and proper motions with reference to galaxies are derived.Analyses of proper motions at Pulkovo and Lick show agreement in some instances and disagreement in others. The same applies to comparisons with fundamental catalogues. The analyses suffer to some extent from absence of proper motions in the zone of avoidance and in the southern part of the sky.In the southern hemisphere, first-epoch photography of 164 fields with galaxies has been completed using the Maksutov double-meniscus telescope at Cerro El Roble in Chile, and a complete coverage of the sky has been started with the same telescope; this work is being done jointly by the Soviet and Chilean astronomers. On the Yale-Columbia southern program, the first-epoch photography is nearly completed with the double astrograph at Leoncito in Argentina. There are plans at Lohrmann Institute, Dresden, to take photographs with the 2-m Schmidt telescope at Tautenburg, thus providing first-epoch plates for proper motions with reference to galaxies.

scholarly journals Proper Motions in the Bulge: Looking Through Plaut's Low Extinction Window

1998 ◽  
Vol 179 ◽  
pp. 223-224
Author(s):  
R.A. Méndez ◽  
R.M. Rich ◽  
W.F. Van Altena ◽  
T.M. Girard ◽  
S. Van Den Bergh ◽  
...  
Keyword(s):  
Proper Motion ◽  
Main Sequence ◽  
Proper Motions ◽  
Galactic Bulge ◽  
Plate Material

We are conducting the deepest and largest photographic proper-motion survey ever undertaken of the Galactic bulge. Our first-epoch plate material (from 1972-3) goes deep enough (Vlim ∼ 22) to reach below the bulge main-sequence turnoff. These plates cover an area of approximately 25′ × 25′ of the bulge in the low-extinction (Av ∼ 0.8 mag) Plaut field at l= 0°, b= −8°, approximately 1 kpc south of the nucleus. This is the point at which the transition between bulge and halo populations likely occurs and is, therefore, an excellent location to study the interface between the dense metal-rich bulge and the metal-poor halo.

scholarly journals Measurement of the absolute proper motions of the Magellanic Clouds

1991 ◽  
Vol 148 ◽  
pp. 491-492 ◽  
Author(s):  
H.-J. Tucholke ◽  
M. Hiesgen
Keyword(s):  
Proper Motion ◽  
Independent Study ◽  
Magellanic Clouds ◽  
Proper Motions ◽  
Schmidt Telescope ◽  
Large Numbers ◽  
The Absolute

Currently, we are measuring the absolute proper motions of the Magellanic Clouds relative to background galaxies, using plates taken with the ESO Schmidt Telescope. In spite of the small epoch difference of about 15 years, an accuracy of 0.5-1.0 milliarcsecs (mas) may be achieved using large numbers of stars and galaxies. Measurement and reduction procedures are presented; a preliminary solution for the absolute proper motion of the LMC from the measurements of three plates gives a result similar to the independent study of Jones et al. (1989).

scholarly journals Statistical HR Diagrams for One Hundred and Fifteen Thousand Proper-Motion Stars

1978 ◽  
Vol 80 ◽  
pp. 63-64
Author(s):  
Willem J. Luyten
Keyword(s):  
Proper Motion ◽  
Tangential Velocity ◽  
Complete Data ◽  
The Other ◽  
Proper Motions ◽  
Real Situation ◽  
The Real ◽  
Using Data ◽  
The One ◽  
Hr Diagram

Since regular HR diagrams require apparent magnitudes, colors or spectra, and parallaxes, and such complete data are available for relatively few stars, there may be some advantage in making up diagrams which utilize proper motions instead of parallaxes, and are thus statistically similar to an HR diagram. The reduced proper motion, first used by Hertzsprung, is defined as H = m + 5 + 5log μ, but may also be written as H = M + 5log T, where T is the tangential velocity, and is expressed in astronomical units per year. A diagram plotting H against color will thus contain the considerable dispersion in tangential velocity which is a serious disadvantage. However, this is outweighed by two practical advantages. First the one and the same person who does the proper motion survey can, and does also determine the other two quantities needed. Second, when using data obtained from such a proper motion survey one deals, statistically, with all the stars within a given distance and the results, therefore, are much more representative of the real situation in space than many HR diagrams which often contain an unrealistic preponderance of giants.

scholarly journals The Determination of the Proper Motions of X-Ray Sources

1970 ◽  
Vol 7 ◽  
pp. 164-166
Author(s):  
Heinrich Eichhorn ◽  
George D. Gatewood ◽  
Sabatino Sofia
Keyword(s):  
Neutron Star ◽  
Neutron Stars ◽  
Proper Motion ◽  
South Florida ◽  
The Other ◽  
Proper Motions ◽  
X Ray ◽  
Other Information ◽  
The University

At the University of South Florida Observatory, a program is under way to determine the proper motions of the star-like objects which are possibly or probably associated with X-Ray sources. The objects under study are Sco X-l, and objects believed to be identical with Cen X-2, Cyg X-2, and Co D -32° 1057. Since it has been speculated that these might be neutron stars, an effort was made to study not only their proper motions but also those of other stars in the neighborhood to ascertain membership of any moving cluster with known age and distance, whereby their own ages and distances might become known. These efforts were successful so far in the case of ScoX-1 (Sofia, Eichhorn and Gatewood, 1969), whose proper motion is virtually identical to that which a member of theScorpio-Centaurus Association would have at this position, so that the membership of Sco X-l in this association becomes highly probable. On the basis of this and other information, Gatewood and Sofia (1969) conclude that Sco X-l is quite likely a neutron star. The reduction was described in detail by Gatewood (1968). No definitive results are available yet for the other three objects.

scholarly journals The New Catalogue of Positions and Proper Motions of 5115 Bright Stars Compiled as the Result of the International “Bright Stars” Program

1995 ◽  
Vol 166 ◽  
pp. 353-353
Author(s):  
O.A. Molotaj ◽  
V.V. Tel'Nyuk-Adamchuk ◽  
N.A. Chernega ◽  
N.D. Kanivec'
Keyword(s):  
Proper Motion ◽  
The Other ◽  
Standard Errors ◽  
Star System ◽  
Proper Motions ◽  
International Program ◽  
Motion System ◽  
Stellar Astronomy ◽  
The Mean ◽  
The One

At Kyiv University Observatory, in accordance with IAU resolution, the Combined Catalogue of Positions and Proper Motions of 5115 Bright Stars in the FK5 system for Epoch and Equinox J2000.0 (BSC, see reference) has been compiled using 20 source catalogues obtained within the framework of ‘Bright Stars’ International Program. The source catalogs are Bordeaux-66, Bucharest-65, Bucharest-68, Belgrade-79, Cape-68, Kharkiv-70n, Kharkiv-70s, Kyiv-66, Kyiv-73, El Leoncito-70, Moscow-76, Mykolaiv-65, Perth-70, Perth-75, Santiago-65, Santiago-67, Strasbourg-65, Tashkent-64, Tokyo-68, Washington-66. The BSC accumulates around 30,000 source catalogue positions observed within 1960-1980. The standard errors of BSC do not exceed 0.1 arcsec and 0.25 arcsec/cy for positions and proper motions, respectively. The systematic differences between BSC and FK5 in positions for the mean BSC epoch 1970 as a rule do not exceed several hundredths of arcsec. A comparison of the BSC with the PPM catalogue indicates that in the latter the accuracy of positions and proper motions of the ordinary bright stars is slightly worse than that of average values given by the authors of the PPM. It is important to note that the comparison of the BSC with PPM for various star subsets shows deviations of both the HPS bright star system and the rest of the PPM bright stars, on the one hand, from the stars of the FK5 Extension contained in the PPM on the other hand. To examine the BSC proper motion system the stellar astronomy constants and correction to precession have been determined using the BSC proper motions. The parameters obtained agree with the standard ones. But the Oort constants are slightly smaller than those of standard.The BSC catalogue as a whole is acceptable for astrometry usage with respect to both accidental and systematic accuracy.

scholarly journals The Tautenburg Part Of The Programme Studying The Main Meridional Section Of The Galaxy

1988 ◽  
Vol 133 ◽  
pp. 451-454
Author(s):  
E. Schilbach
Keyword(s):  
Proper Motion ◽  
Proper Motions ◽  
Schmidt Telescope ◽  
Meridional Section ◽  
Mean Error ◽  
The Galaxy ◽  
The Mean

The programme for the determination of proper motions with reference to galaxies for 6000 stars on 17 fields near the main meridional section of the Galaxy is presented. For each field there are 2 or 3 first-epoch plates taken with the Tautenburg Schmidt-telescope before 1970. In preliminary investigations the mean error of an individual proper motion was found to be per century both for bright (8m–12m) and for faint (16m–18m) stars.

scholarly journals Maintenance and densification: current proper-motion catalogs

2007 ◽  
Vol 3 (S248) ◽  
pp. 303-309
Author(s):  
T. M. Girard
Keyword(s):  
Proper Motion ◽  
Reference System ◽  
Milky Way ◽  
Raw Material ◽  
Proper Motions ◽  
Schmidt Telescope ◽  
Large Area ◽  
Milky Way Galaxy ◽  
Celestial Reference System

AbstractAn overview of currently available, large-area, proper-motion catalogs is presented. These include the well-known catalogs based on historical Schmidt-telescope surveys as well as other projects that make use of observational material the primary purpose of which, from inception, was the determination of proper motions. The various catalogs are characterized and compared, with an emphasis on their limitations and their appropriateness for various astrophysical uses.In addition to allowing for the maintenance of a practical celestial reference system, absolute proper-motion surveys provide the raw material from which a better understanding of our Galaxy's structure and kinematics can be built. Several examples will be cited in which large proper-motion surveys are used to probe and describe the distinct stellar components that comprise our Milky Way Galaxy.

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