First speckle interferometric measurements of binary stars at the Observatorio Astrofísico Guillermo Haro

ABSTRACT In this paper, we present the first multiband speckle interferometric measurements of binary stars performed using the 2.1 m telescope of the Observatorio Astrofísico Guillermo Haro, Cananea, Sonora, México. We describe here FICCO: Fast Imaging Camera for Cananea Observatory, a new instrument developed to perform speckle observations from the Northern Hemisphere. We tested this new instrument with objects from the Washington Double Star Catalog, that were observed during three runs allocated in 2019. We report 480 astrometric measurements of 138 pairs, with angular separations ranging from 0.06 to 5.76 arcsec, including 347 measurements with separations smaller than 1 arcsec. We estimated a mean error in separation of 14 mas, 1.6° in position angle, and 0.45 mag for the magnitude difference. We confirmed 12 double stars discovered by Hipparcos. Finally, we present a correction to four previously published orbital solutions of visual binaries.

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U.S. Naval Observatory Double Star CD 2006.5

Proceedings of the International Astronomical Union ◽

10.1017/s1743921307006333 ◽

2006 ◽

Vol 2 (S240) ◽

pp. 575-580 ◽

Cited By ~ 1

Author(s):

Brian D. Mason ◽

William I. Hartkopf

Keyword(s):

Binary Stars ◽

Double Star ◽

List Type ◽

Star Catalog ◽

Naval Observatory ◽

Scale Calibration ◽

Linear Elements ◽

Visual Binary Stars ◽

Star Catalogs ◽

Magnitude Difference

AbstractThe U.S. Naval Observatory has produced its second CDROM of double star catalogs. This successor to the 2001.0 CDROM includes the latest versions (June 30 2006) of four major double star catalogs maintained at the USNO: •Washington Double Star Catalog (WDS),•Second Photometric Magnitude Difference Catalog,•Fourth Catalog of Interferometric Measurements of Binary Stars, and•Sixth Catalog of Orbits of Visual Binary Stars.Each of these catalogs had seen significant changes during the past six years; for example, the WDS has grown by over 150,000 measures and the number of systems in the Interferometric Catalog has nearly doubled. Other improvements include precise coordinates for the vast majority of systems, as well as new observing lists for tens of thousands of “neglected” doubles.Also included on this CDROM is a Catalog of Linear Elements for several hundred optical pairs. These elements should prove useful for improving the components' proper motions, as well as providing scale calibration out to several tens of arcseconds.As was done with its predecessor, the new CDROM is automatically distributed free of charge to members of the double star community and to astronomy libraries. Others may receive a complementary copy upon request.

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SUSI’s Potential for Double Star Research

International Astronomical Union Colloquium ◽

10.1017/s0252921100007041 ◽

1992 ◽

Vol 135 ◽

pp. 521-526

Author(s):

John Davis

Keyword(s):

Angular Resolution ◽

Double Star ◽

Double Stars ◽

Stellar Interferometer ◽

New Instrument

AbstractThe Sydney University Stellar Interferometer (SUSI) is currently undergoing commissioning and will soon commence its astronomical program in which observations of double stars will form a major component. With its 640-m long North–South array of input siderostats, the new instrument will have unprecedented angular resolution.

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The New Index Catalog of Visual Double Stars-WDS

Symposium - International Astronomical Union ◽

10.1017/s0074180900077159 ◽

1986 ◽

Vol 109 ◽

pp. 649-651

Author(s):

Charles E. Worley ◽

Geoffrey G. Douglass

Keyword(s):

Double Star ◽

Star Catalog ◽

Star Data ◽

Double Stars ◽

Visual Double Stars

A new index catalog of visual double stars, the Washington Double Star Catalog (WDS), 1984.0, is now available in tape form. All of the double star data has been updated, as well as the notes to the catalog. This report summarizes the contents of the WDS and describes its compilation.

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The Discovery of Double Stars at Occultations

International Astronomical Union Colloquium ◽

10.1017/s0252921100009842 ◽

1983 ◽

Vol 62 ◽

pp. 63-72 ◽

Cited By ~ 1

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.

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Systematic Errors in Double Star Observations

International Astronomical Union Colloquium ◽

10.1017/s0252921100006631 ◽

1992 ◽

Vol 135 ◽

pp. 311-313 ◽

Cited By ~ 1

Author(s):

Geoffrey G. Douglass ◽

Charles E. Worley

Keyword(s):

Root Mean Square ◽

Proximity Effect ◽

Position Angle ◽

Systematic Errors ◽

Double Star ◽

Mean Square ◽

Double Stars ◽

Visual Double Stars ◽

Systematic Effects

AbstractWe have examined the visual and speckle observations of visual double stars made by 31 experienced observers in order to evaluate possible systematic errors in these series. Using 57 “definitive” orbits, we find no appreciable errors in position angle. We do find systematic effects in separation for some observers, and, in particular, a “proximity” effect for measurements of pairs closer than 0″.5.Root-mean-square residuals are:

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HIPPARCOS First Results in the Double Star Photometry

International Astronomical Union Colloquium ◽

10.1017/s0252921100006904 ◽

1992 ◽

Vol 135 ◽

pp. 421-428

Author(s):

F. Mignard ◽

J.L. Falin ◽

M. Froeschlé

Keyword(s):

Double Star ◽

Multiple Systems ◽

Double Stars ◽

Multiple Stars ◽

Accuracy And Precision ◽

First Results ◽

Main Detector ◽

Input Catalogue ◽

Magnitude Difference ◽

Better Than

AbstractIn addition to its astrometric capabilities the HIPPARCOS main detector proves to be a good phototometer. The main features of the photometric reduction applied to double stars are outlined. We show how it is possible to discriminate single stars from multiple stars from the photometric signal. Results presented are based on about 16000 stars recognized as non-single, of which 8000 were not known to be double in the HIPPARCOS Input Catalogue. Magnitudes for multiple systems as a whole are derived with a precision usually better than 0.005 mag while the magnitude of each component is recovered up to magnitude difference of 3 mag, but with less accuracy and precision.

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Detection of Double Stars with the Two-Color Refractometer

International Astronomical Union Colloquium ◽

10.1017/s0252921100009775 ◽

1983 ◽

Vol 62 ◽

pp. 28-35 ◽

Cited By ~ 1

Author(s):

James W. Christy ◽

Dennis D. Wellnitz ◽

Douglas G. Currie

Keyword(s):

Position Angle ◽

Angular Distance ◽

Double Star ◽

Measured Quantity ◽

University Of Maryland ◽

Additional Information ◽

Double Stars ◽

Color Differences ◽

Nearby Stars ◽

The University

AbstractAttempts to detect double stars are being made with the Two-Color Refractometer (TCR). The refractometer is an instrument developed by the Quantum Electronics Group of the University of Maryland to measure atmospheric refraction.During check-out observations using the U.S. Naval Observatory’s (USNO’s) 24“ reflecting telescope, the refractometer is being used to detect the astrometric separation of the ultraviolet and red photocenters of the combined light from a double star, differentially referenced to nearby stars. The refractometer contains two dispersive wedges which null the incoming dispersion; the positions of the wedges then provide a measure of the dispersion of the incoming light. The angular part of this measure immediately gives the position angle of the double. The angular distance between the two components of the pair is a combined function of the measured quantity and of the magnitude and color differences of the components of the double star, and is therefore obtainable only with additional information.

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Double Star Astrometry with the Hipparcos Data

Symposium - International Astronomical Union ◽

10.1017/s0074180900227861 ◽

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.

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

International Astronomical Union Colloquium ◽

10.1017/s0252921100006886 ◽

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.

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A Mass Estimate in a Sample of Double Stars

Proceedings of the International Astronomical Union ◽

10.1017/s1743921307006394 ◽

2006 ◽

Vol 2 (S240) ◽

pp. 631-633

Author(s):

S. Ninković ◽

Z. Cvetković

Keyword(s):

Binary Stars ◽

Main Sequence ◽

Apparent Magnitude ◽

Orbital Elements ◽

Double Stars ◽

Trigonometric Parallax ◽

Hipparcos Catalogue ◽

Mass Estimate ◽

Visual Binary Stars ◽

Magnitude Difference

AbstractThe total masses of binaries are calculated on the basis of their orbital elements from the Sixth Catalog of Orbits of Visual Binary Stars. They are then compared with the values resulted from the mass-luminosity relation for the Main Sequence where as the input data are used: trigonometric parallax, total apparent magnitude of the pair (source Hipparcos Catalogue) and magnitude difference (source Hipparcos Catalogue and Photometric Magnitude Difference Catalog). It seems that for the pairs indicated as having qualitative orbital elements the agreement between the total-mass values obtained in these two ways is satisfactory.

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