scholarly journals Double Star Astrometry with the Hipparcos Data

1995 ◽  
Vol 166 ◽  
pp. 69-76
Author(s):  
F. Mignard
Keyword(s):  
Position Angle ◽  
Double Star ◽  
Recognition Procedure ◽  
Double Stars ◽  
Multiple Stars ◽  
Relative Coordinates ◽  
Double And Multiple Stars

As we approach the final processing of the observations carried out by HIPPARCOS, in particular for the double and multiple stars, it is possible to provide reliable statistics on the number of such objects detected and on the quality of the relative and absolute astrometry and photometry. About 24 000 stars have been recognized as non-single, including 11 000 already known as double and multiple before the mission and 13000 discovered by Hipparcos. Also, a subset of 16 000 stars among the 24 000 have been successfully solved for their relative coordinates (position angle and separation) with an accuracy in the range of 3 to 30 mas, including 7000 new double stars. I outline in this paper the principle of the internal recognition procedure and present some statistics on the solution.

scholarly journals HIPPARCOS First Results in the Double Star Processing by the FAST Consortium

1992 ◽  
Vol 135 ◽  
pp. 403-411
Author(s):  
F. Mignard ◽  
M. Badiali ◽  
P.L. Bernacca ◽  
H. Bernstein ◽  
D. Cardini ◽  
...  
Keyword(s):  
Position Angle ◽  
Double Star ◽  
Double Stars ◽  
Multiple Stars ◽  
Relative Coordinates ◽  
First Results ◽  
Double And Multiple Stars ◽  
Quantitative Results ◽  
One Year

AbstractAfter the processing of one year of observations carried out by HIPPARCOS it is possible to provide quantitative results as to the number of new double and multiple stars to be detected and the real capacity of this mission to perform relative astrometry on double stars. We present and discuss the methods developed to this end and include the first results concerning the detection statistics and the determination of separation and position angle for double stars. About 16,000 stars have been recognized as non-single, including 9,000 already known as double and mutliple before the mission. Also, a subset of 10,500 stars have been successfully solved for their relative coordinates with an accuracy in the range of 3 to 10 mas.

scholarly journals Double Star Recognition

1992 ◽  
Vol 9 ◽  
pp. 423-423
Author(s):  
M. Frœschle ◽  
F. Mignard ◽  
J.L. Falin
Keyword(s):  
Statistical Tests ◽  
Real Data ◽  
Double Star ◽  
Field Of View ◽  
Double Stars ◽  
Signal Parameters ◽  
Multiple Stars ◽  
Double And Multiple Stars ◽  
Stellar Source

AbstractHipparcos observations provide a wealthy source of discovery of new double and multiple stars. We have developed adequate procedures to recognize in the signal parameters the multiplicity of the stellar source passing through the Hipparcos field of view. These procedures are outlined together with the design of the statistical tests employed. Sampling on real data indicates that about 6000 new double stars will be detected at the mission completion.

scholarly journals Relative-coordinate determination for visual double stars by applying Fourier transforms

2013 ◽  
pp. 65-76
Author(s):  
Viktor Radovic ◽  
R. Pavlovic ◽  
Zorica Cvetkovic
Keyword(s):  
Fourier Transforms ◽  
Position Angle ◽  
Double Stars ◽  
Coordinate Determination ◽  
Relative Coordinate ◽  
Visual Double Stars ◽  
Multiple Stars ◽  
Relative Coordinates

We discuss the software developed for the purpose of determining the relative coordinates (position angle ? and separation ?) for visual double or multiple stars. It is based on application of Fourier transforms in treating CCD frames of these systems. The objective was to determine the relative coordinates automatically to an extent as large as possible. In this way the time needed for the reduction of many CCD frames becomes shorter. The capabilities and limitations of the software are examined. Besides, the possibility of improving is also considered. The software has been tested and checked on a sample consisting of CCD frames of 165 double or multiple stars obtained with the 2m telescope at NAO Rozhen in Bulgaria in October 2011. The results have been compared with the corresponding results obtained by applying different software and the agreement is found to be very good.

scholarly journals Classical Observations of Visual Binary and Multiple Stars

2006 ◽  
Vol 2 (S240) ◽  
pp. 88-96
Author(s):  
Brian D. Mason
Keyword(s):  
Field Work ◽  
Speckle Interferometry ◽  
Double Star ◽  
The Past ◽  
Multiple Stars ◽  
Successful Work ◽  
Different Types ◽  
Star Database ◽  
Double And Multiple Stars ◽  
Types Of Information

AbstractChanges in the double star database are highlighted, describing various methods of observation (both historically and those of the past few years) and their effectiveness in different regimes of separation space. The various niches for wide- and narrow-field work as they apply to double and multiple stars are examined and the different types of information which each can provide are described. Despite the significant growth of the double star database, much can still be done, such as finding lost pairs, filling in missing parameters so that observing programs can select all stars appropriate to their capabilities, or providing at least gross kinematic descriptions. After more than 20 years of successful work, speckle interferometry and conventional CCD astrometry have replaced filar micrometry and photography as preferred classical techniques. Indeed, most work in filar micrometry is now being done by amateurs. Work on pairs described as neglected in the last major WDS data release (2001) is given as a specific example. Finally, the continued need to publish data in classical double star parameters is also discussed.

scholarly journals Dynamic study of possible host stars for extrasolar planetary systems

2014 ◽  
Vol 9 (S310) ◽  
pp. 104-105 ◽  
Author(s):  
N. A. Shakht ◽  
L. G. Romanenko ◽  
D. L. Gorshanov ◽  
O. O. Vasilkova
Keyword(s):  
Planetary Systems ◽  
Dynamic Study ◽  
Stellar Systems ◽  
The Sun ◽  
Solar Mass ◽  
Double Stars ◽  
Multiple Stars ◽  
Double And Multiple Stars ◽  
Host Stars

AbstractWe present the stellar systems which consist of double and multiple stars with distances 3.5 ÷ 25 pc from the Sun, belonging to spectral classes F, G, K, M, having masses from 0.3 to 1.5 solar mass and can, in principle, possess planetary systems. On the basis of observations with Pulkovo 65 cm refractor the relative positions of double stars, the parameters of motion, the orbits and also the ephemeris for the nearest epochs have been computed.

scholarly journals Focal length determination for the 60cm telescope at Astronomical station Vidojevica

2012 ◽  
pp. 97-104 ◽  
Author(s):  
Z. Cvetkovic ◽  
G. Damljanovic ◽  
R. Pavlovic ◽  
O. Vince ◽  
I.S. Milic ◽  
...  
Keyword(s):  
Focal Length ◽  
Ccd Camera ◽  
Angular Separation ◽  
Multiple Stars ◽  
Relative Coordinates ◽  
Double And Multiple Stars ◽  
Positional Angle ◽  
Length Determination ◽  
Optical Wavelengths ◽  
Astronomical Station

The focal length of a telescope is an important parameter in determining the angular pixel size. This parameter is used for the purpose of determining the relative coordinates (angular separation and positional angle) of double and multiple stars, and the precise coordinates of extragalactic radio sources (ERS) that are visible at optical wavelengths. At the Astronomical Station Vidojevica we have collected observations of these objects using two CCD cameras, Apogee Alta U42 and SBIG ST-10ME, attached to the 60 cm telescope. Its nominal focal length is 600 cm as given by the manufacturer. To determine the telescope focal length more precisely for both attached detectors, we used angular-separation measurements from CCD images taken at Astronomical Station Vidojevica. The obtained focal lengths are: F42 = (5989 ? 7) mm using the CCD camera Apogee Alta U42 attached to the telescope, and F10 = (5972 ? 4) mm with the CCD camera SBIG ST-10ME attached to the telescope.

scholarly journals The Catalogue of the Components of Double and Multiple Stars (CCDM) - First Edition

1995 ◽  
Vol 166 ◽  
pp. 395-395 ◽  
Author(s):  
J. Dommanget ◽  
O. Nys
Keyword(s):  
Data Base ◽  
Multiple Star ◽  
Multiple Systems ◽  
Double Stars ◽  
Multiple Stars ◽  
Double And Multiple Stars ◽  
General Data ◽  
Input Catalogue ◽  
Better Than

The Hipparcos mission required the realisation of an Input Catalogue giving the positions of 100.000 stars (single or components of double and multiple systems) to an accuracy better than 1″5. At the start of this work (1981) no specific catalogue of double and multiple stars provided these data. The only general data base on double stars available to us, giving positions to ±1′, was the Index (1961,0) updated at the USNO by C. E. Worley till 1976,5 and of which a copy was communicated by P. Muller of the Observatoire de Meudon. It has then been decided to reformat this Catalogue in such a way as to allow the introduction of all necessary information for the mission. This permitted a correct cross-identification with the Hipparcos Input Catalogue (of finally 118.000 stars). It was later called: the Catalogue of the Components of Double and Multiple stars (CCDM). Since then, it has been developed and its aim remains to furnish the best accurate locations and descriptions of the double and multiple systems on the sky for all double and multiple star research.

scholarly journals The Discovery of Double Stars at Occultations

1983 ◽  
Vol 62 ◽  
pp. 63-72 ◽  
Author(s):  
David S. Evans
Keyword(s):  
Position Angle ◽  
Visual Observation ◽  
Double Star ◽  
Double Stars ◽  
Photoelectric Observations ◽  
Vector Separation ◽  
Successful Observation

When systematic photoelectric observations of occultations were started some dozen years ago it was realised that they yielded a significant crop of double star discoveries and observations. The limitations of the method were well recognised: only about ten percent of the area of the sky would ever be available and one could not choose which stars to be observed. Moreover the data obtained from a successful observation of a double star are less comprehensive than the normal visual observation. The result is the vector separation or the true separation projected along a line perpendicular to the actual lunar limb, that is the position angle of the point of occultation modified by the slope of the limb at that point.

scholarly journals How Double Star Astronomy May Develop After HIPPARCOS

1992 ◽  
Vol 135 ◽  
pp. 435-438
Author(s):  
J. Dommanget ◽  
P. Lampens
Keyword(s):  
Double Star ◽  
Multiple Stars ◽  
Hipparcos Catalogue ◽  
Double And Multiple Stars ◽  
Celestial Bodies ◽  
Input Catalogue

AbstractNow that the HIPPARCOS satellite safely revolves on its “degraded” orbit — after the exploit of the ESA technicians to rescue it from the faulty ignition of its apogeum boost motor — and regularly provides the information expected for reaching the initial aim of the project, one may turn to examine the possible exploitation of the final HIPPARCOS Catalogue.In the present paper, we describe how double and multiple stars have been introduced in the Input Catalogue and what may be expected from their observation. We also try to evaluate how much the final HIPPARCOS data may influence future researches on these celestial bodies and what kind of ground–based observation programmes should be conducted in order to support the space results.

scholarly journals A Very Special Catalogue: The Hipparcos Input Catalogue

1988 ◽  
Vol 133 ◽  
pp. 245-257
Author(s):  
C. Turon
Keyword(s):  
Observational Constraints ◽  
List Type ◽  
Type Number ◽  
Multiple Stars ◽  
Final Data ◽  
Double And Multiple Stars ◽  
Input Catalogue

The various characteristics of the HIPPARCOS Input Catalogue are described:–How to select 110 000 stars for HIPPARCOS observation from the 210 000 proposed stars, taking into account the following sometimes conflicting requirements : satisfy a maximum of scientific programmes and respect the observational constraints inherent in the HIPPARCOS satellite operation ?–What are the present results regarding the principal astrometric programmes ?–How to process the specific problems which are raised by the HIPPARCOS observation of double and multiple stars and of stars in dense areas ?–Which compilations and observations have been undertaken and are in progress within the frame of the Input Catalogue preparation ? What will be the quality of the final data ?Finally, the contents of the catalogues and annexes that will be published are briefly presented.

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