Speckle observations of binary systems measured 
by Hipparcos

Prieur, Jean‐Louis; Oblak, E.; Lampens, P.; Kurpińska-Winiarska, M.; Aristidi, Éric; Koechlin, Laurent; Ruymaekers, G.

doi:10.1051/0004-6361:20000550

Cited by 16 publications

(18 citation statements)

References 22 publications

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“…There exist a number of inconsistencies and uncertainties with this visual and spectroscopic binary in the literature. Thus, the radial velocities by Duquennoy & Mayor (1991) led them to conclude that HR 7637 has an eccentric orbit with a period of less than 5 yr. From the visual observations Baize (1992) and Hartkopf, Mason & McAlister (1996) both found instead a circular orbit with a semimajor axis a = 0.23 arcsec and an orbital period P = 9.7 yr. As briefly discussed in Prieur et al (2001) this discrepancy arises from a quadrant ambiguity of the relative positions, but it would appear that the circular orbit is the correct one. Yet, the relative Doppler velocity predicted by Hartkopf et al (1996, their fig.…”

Section: The Volume‐complete Samplementioning

confidence: 98%

Nearby stars of the Galactic disc and halo - V

Fuhrmann¹

2011

Monthly Notices of the Royal Astronomical Society

155

115

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This fifth in a series of papers finishes the model atmosphere analyses of an unbiased, volumecomplete sample of more than 300 nearby solar-type stars. The sample first disintegrates into thick-disc and thin-disc stars on account of their different distributions in the [Mg/H]-[Fe/Mg] chemical abundance plane. Detailed stellar age-datings of the locally few, but very relevant, subgiants show this map to be the sequel of a major star formation gap and hence the legacy for the two stellar populations. Among the stars of the thin disc the subgiant 70 Vir with τ = 8.1 ± 0.6 Gyr remains the best case to constrain the age of this comparatively young population. Uncertainties for the existing thick-disc subgiants are about twice as much, but they consistently promote ages of 12-13 Gyr. The unbiased thin-disc metallicity distribution functions of magnesium and iron average at [Mg/H] = −0.009 ± 0.012 dex and [Fe/H] = −0.034 ± 0.015 dex, thereby demonstrating that the Sun is a typical thin-disc star in terms of these two elements. The small but likewise unbiased sample of thick-disc stars leads to [Mg/H] = −0.207 ± 0.049 dex and [Fe/H] = −0.584 ± 0.057 dex, which implies that about two-thirds of the α-element magnesium was already synthesized in the early Milky Way. Similarly, the age-metallicity relations for the thin disc result in [Mg/H] = +0.006 dex Gyr −1 and [Fe/H] = +0.017 dex Gyr −1 and lead to the conclusion that a similar percentage of iron was synthesized before the birth of the thin disc. In comparison with the considerable metallicity dispersions σ [Mg/H] = 0.151 dex and σ [Fe/H] = 0.191 dex for the stars of the thin disc, this immediately explains the coexistence of old, metal rich as well as young, fairly metal poor stars within this stellar population. The stellar multiplicities of the solar-type thin-disc stars show a minority of less than 47 per cent to be single and at least 15 per cent to belong to triple and higher level systems. More concisely, in terms of the primary masses there is a clear correlation with mass with a cross-over of preferentially single to binary stars at M 1.25 M and a fraction of 21 per cent of triple and higher level systems at this particular mass. The steady record of new discoveries of nearby companion stars renders these numbers, however, as yet provisional, with an ever-decreasing fraction of single objects. For the thick disc the multiplicity statistics are necessarily weak, yet tentatively imply even less single stars and eventually more triple or higher level systems. Most importantly, and as already addressed in the previous papers of this series, the rigorous census of the long-lived stars of the sample uncovers the thick disc as a massive, dark population with a 20 per cent local normalization, and, on account of its larger scaleheight, a mass comparable to that of the thin disc. With the ages of its stars at or above 12 Gyr the thick-disc epoch then leads to a very different star formation rate and qualifies this stellar population as a single-burst component, much at ...

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Section: The Volume‐complete Samplementioning

confidence: 98%

Nearby stars of the Galactic disc and halo - V

Fuhrmann¹

2011

Monthly Notices of the Royal Astronomical Society

155

115

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“…For each observing sequence, we give the epoch of observation (Column 4) in fraction of Besselian years (2004+), the filter (Column 5) (whose characteristics are listed in table 1 of Paper I), the focal length of the eyepiece used for magnifying the image (Column 6), the angular separation ρ (Column 7) and its error (Column 8) in arcsec and the position angle θ (Column 9) and its error (Column 10) in degrees. The errors were estimated by quadratically adding the calibration errors (see Paper I) to the standard deviation of a series (from 4 to 8) of independent measurements obtained with the same data set (see Prieur et al 2001). This procedure generally leads to good error estimates, but may underestimate the errors on θ in the case of diffuse autocorrelation peaks.…”

Section: Astrometric Measurementsmentioning

confidence: 99%

Speckle observations with PISCO in Merate - II. Astrometric measurements of visual binaries in 2004

Scardia¹,

Prieur²,

Pansecchi³

et al. 2006

Monthly Notices of the Royal Astronomical Society

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International audienceWe present relative astrometric measurements of visual binaries taken during the second semester of 2004 with the Pupil Interferometry Speckle camera and Coronagraph (PISCO) at the 1-m Zeiss telescope of the Brera Astronomical Observatory, in Merate, Italy. We performed 207 new observations of 194 objects with angular separations in the range 0.1-4.0 arcsec and an accuracy better than ~0.01 arcsec. Our sample contains orbital couples as well as binaries whose motion is still uncertain. Our purpose is to improve the accuracy of the orbits and constrain the masses of the components. Those measurements show that the orbit of ADS 15115 needs to be revised; we propose a new orbit for this object

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“…A specially designed program (by JLP), can control a videotape recorder and a digitizing board, thus allowing fully automatic processing of these tapes (Prieur et al 2001). The first step of the data reduction consists of computing the autocorrelation of the elementary frames, using the method described by Worden et al (1977).…”

Section: Observations and Data Reductionmentioning

confidence: 99%

“…This procedure allows the removal of the background of the mean autocorrelation and nicely increases the contrast of the secondary peaks of binary stars. Astrometry parameters are then derived from this autocorrelation, by carefully measuring the location of the secondary peaks, following the procedure described in Prieur et al (2001).…”

Section: Observations and Data Reductionmentioning

confidence: 99%

“…For each observing sequence, we give the epoch of observation (column 4) in a fraction of Besselian years (2004+), the filter (column 5) whose characteristics are listed in Table 1, the angular separation ρ (column 6) and its error (column 7) in arcseconds, and the position angle θ (column 8) and its error (column 9) in degrees. The errors were estimated by adding quadratically the calibration errors (see ) to the standard deviation of a series (from 4 to 8) of independent measurements obtained with the same data set (see Prieur et al 2001). This procedure generally leads to good error estimates, but can underestimate the errors on θ in the case of very diffuse fringes (see ).…”

Section: Astrometric Measurementsmentioning

confidence: 99%

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Speckle observations with PISCO in Merate -- I. Astrometric measurements of visual binaries in 2004

Scardia

Prieur

Sala

et al. 2005

Monthly Notices of the Royal Astronomical Society

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We present relative astrometric measurements of visual binaries made with the Pupil Interferometry Speckle camera and Coronagraph (PISCO) at the 1‐m Zeiss telescope of Brera Astronomical Observatory, in Merate. We provide 135 new observations of 103 objects, with angular separations in the range 0.1–4.0 arcsec and with an accuracy better than ∼0.01 arcsec. Our sample is made of orbital couples as well as binaries whose motion is still uncertain. Our purpose is to improve the accuracy of the orbits and constrain the masses of the components. This work already leads to the revision of the orbits of three systems (ADS 5447, 8035 and 8739).

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Speckle observations of binary systems measured by Hipparcos

Cited by 16 publications

References 22 publications

Nearby stars of the Galactic disc and halo - V

Nearby stars of the Galactic disc and halo - V

Speckle observations with PISCO in Merate - II. Astrometric measurements of visual binaries in 2004

Speckle observations with PISCO in Merate -- I. Astrometric measurements of visual binaries in 2004

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