Orbital elements of 9 visual double stars

Alzner, A.

doi:10.1051/aas:1998292

Cited by 23 publications

(3 citation statements)

References 3 publications

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“…Nonetheless, the level of internal consistency between different values of position angle and separation is very high. In addition, BU 151 and BU 1295AB have well-determined orbits (Alzner 1998;Hartkopf et al 1996), and the separation and position angle Table 2 are consistent with the orbit ephemerides for the observation epochs in question, given our lack of precision at this point in the scale determination. The magnitude differences listed in Table 2 also have a high degree of internal consistency, on the level of a few hundredths of a magnitude for observations of the same object taken in the same filter.…”

Section: Initial Resultssupporting

confidence: 63%

RYTSI: The Rochester Institute of Technology–Yale Tip‐Tilt Speckle Imager

Meyer

Horch

Ninkov

et al. 2006

PUBL ASTRON SOC PAC

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We have constructed a new speckle imaging system that collects a large number of speckle patterns on the detector area of a large-format CCD. The system is called the RIT-Yale Tip-tilt Speckle Imager (RYTSI) because it uses two galvanometric scanning mirrors to tip and tilt each speckle pattern to a different location on the CCD chip. It therefore solves the bandwidth problem of using CCDs in speckle imaging in a unique way: the mirrors direct speckle patterns across the chip with millisecond accuracy, and the CCD is read out only when the chip is filled with patterns. The instrument was designed to accommodate a variety of detector formats, readout systems, and telescope plate scales; it was initially used at the WIYN Observatory in conjunction with an RIT (Rochester Institute of Technology) 2048 2 CCD. We present the design of the instrument and a sample of first results, which indicate that the instrument can be expected to recover, with high precision, both astrometric and photometric information for binary and multiple stars.

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Section: Initial Resultssupporting

confidence: 63%

RYTSI: The Rochester Institute of Technology–Yale Tip‐Tilt Speckle Imager

Meyer

Horch

Ninkov

et al. 2006

PUBL ASTRON SOC PAC

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“… Orbit references in Column 12: Alz1998a =Alzner (1998a), Baz1976 =Baize (1976), Baz1980a =Baize (1980a), Baz1987b =Baize (1987b), Cou1999b =Couteau (1999b), Cve2006e =Cvetkovic & Novakovic (2006e), Cve2008a =Cvetkovic, Novakovic & Todorovic (2008a), Doc1984b =Docobo & Costa (1984b), Doc1985c =Docobo & Costa (1985c), Doc1987b =Docobo & Costa (1987b), Doc1990a =Docobo & Costa (1990a), Doc1997b =Docobo & Ling (1997b), Doc2004a =Docobo & Ling (2004a), Doc2007e =Docobo et al (2007e), Doc2008f =Docobo & Ling (2008f), Fei1969 =Feierman (1969), Ge1954 =Gasteyer (1954), Gon2002b =Gontcharov & Kiyaeva (2002b), Hei1966 =Heintz (1966), Hei1975b =Heintz (1975b), Hei1981b =Heintz (1981b), Hei1984b =Heintz (1984b), Hei1988a =Heintz (1988a), Hei1988d =Heintz (1988d), Hei1991 =Heintz (1991), Hei1994a =Heintz (1994a), Hei1995 =Heintz (1995), Hei1996a =Heintz (1996a), Hei1996c =Heintz (1996c), Hei1997 =Heintz (1997), Hei1998 =Heintz (1998), Hei2001 =Heintz (2001), Hop1964b =Hopmann (1964b), Hop1971 =Hopmann (1971), Hop1973b =Hopmann (1973b), Hou1987 =Houser (1987), Hrt1989 =Hartkopf, McAlister & Franz (1989), Hrt2000b =Hartkopf (2000b), Hrt2001a =Hartkopf & Mason (2001a), Hrt2009 =Hartkopf & Mason (2009), Lin1985c =Ling (1985c), Lin2007b =Ling (2007b), Lmp2001a =Lampens & Strigachev (2001a), Luy1934a =Luyten (1934a), Msn1999a =Mason, Douglass & Hartkopf (1999a), Msn2001c =Mason & Hartkopf (2001c), Nov2006e =Novakovic & Todorovic (2006e), Nov2007d =Novakovic (2007d), Ole1990 =Olevic & Catovic (1990), Ole2001 =Olevic & Jovanovic (2001), Ole2003b =Olevic & Cvetkovic (2003b), Pal2005b =Pavlovic & Todorovic (2005b), Pbx2000b =Pourbaix (2000b), Pop1987 =Popovic (1987), Pop1995d =Popovic & Pavlovic (1995d), Pop1996b =Popovic & Pavlovic (1996b), Pru2009 =Prieur et al (2009) Sca1981f =Scardia (1981f), Sca1983a =…”

Section: Astrometric Measurementsmentioning

confidence: 99%

Speckle observations with PISCO in Merate - IX. Astrometric measurements of visual binaries in 2008

Prieur¹,

Scardia²,

Pansecchi³

et al. 2010

Monthly Notices of the Royal Astronomical Society

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We present relative astrometric measurements of visual binaries, made in 2008 with the Pupil Interferometry Speckle camera and Coronagraph (PISCO) at the 102 cm Zeiss telescope of Brera Astronomical Observatory, in Merate. Our sample contains orbital couples as well as binaries whose motion is still uncertain. We obtained 240 new measurements of 237 objects with angular separations in the range 0.15-4.6 arcsec, and an average accuracy of 0.014 arcsec. The mean error on the position angles is 0. • 6. Most of the position angles were determined without the usual 180 • ambiguity with the application of triple-correlation techniques and/or by inspection of the long integration files.We have found a new component in ADS 11074. This component was not fully resolved in our previous observations of 2006, but it was clearly separated with the observations presented here.We also present the new revised orbits we have computed for ADS 11468, 13850 and 16057, for which our measurements lead to large residuals with the last published orbits. For ADS 13850, we propose to extend the quadrant correction that was previously used by the other authors to the first measurements made before 1930. In this way, we obtain an orbit with a longer period which leads to a much more plausible value for the total mass of the system.

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“…As mentioned above, this system consists of two evolved stars, allowing for a relatively precise age determination from both CTIO and WIYN data. The orbit of Alzner (1998) is of excellent quality, easily grade 1 in the Sixth Orbit Catalog, and was produced from high-quality speckle data spanning over a full orbit. This represents one of the most interesting tests of our method, since the uncertainty in the dynamical mass sum is only about three tenths of a solar mass, and the components are evolved.…”

Section: Notes On Specific Systemsmentioning

confidence: 99%

A Photometric Analysis of Seventeen Binary Stars Using Speckle Imaging

Davidson

Baptista

Horch

et al. 2009

The Astronomical Journal

199

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Magnitude differences obtained from speckle imaging are used in combination with other data in the literature to place the components of binary star systems on the H-R diagram. Isochrones are compared with the positions obtained, and a best-fit isochrone is determined for each system, yielding both masses of the components as well as an age range consistent with the system parameters. Seventeen systems are studied, 12 of which were observed with the 0.6 m Lowell-Tololo Telescope at Cerro Tololo Inter-American Observatory and six of which were observed with the WIYN 3.5 m Telescope (The WIYN Observatory is a joint facility of the University of Wisconsin-Madison, Indiana University, Yale University, and the National Optical Astronomy Observatories) at Kitt Peak. One system was observed from both sites. In comparing photometric masses to mass information from orbit determinations, we find that the photometric masses agree very well with the dynamical masses, and are generally more precise. For three systems, no dynamical masses exist at present, and therefore the photometrically determined values are the first mass estimates derived for these components.

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Orbital elements of 9 visual double stars

Abstract: Abstract. Orbital elements and ephemerides for 9 visual double stars are given.

Cited by 23 publications

References 3 publications

RYTSI: The Rochester Institute of Technology–Yale Tip‐Tilt Speckle Imager

RYTSI: The Rochester Institute of Technology–Yale Tip‐Tilt Speckle Imager

Speckle observations with PISCO in Merate - IX. Astrometric measurements of visual binaries in 2008

A Photometric Analysis of Seventeen Binary Stars Using Speckle Imaging

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