<i>SearchCal</i>: a Virtual Observatory tool for searching calibrators in optical long-baseline interferometry

Bonneau, D.; Delfosse, X.; Mourard, D.; Lafrasse, S.; Mella, Guillaume; Cetre, Sylvain; Clausse, J. M.; Zins, G.

doi:10.1051/0004-6361/201015124

Cited by 80 publications

(84 citation statements)

References 29 publications

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“…The calibrators, listed in Table 3, were selected using the SearchCal 1 software (Bonneau et al 2006(Bonneau et al , 2011 provided by the Jean-Marie Mariotti Center (JMMC).…”

Section: Interferometric Observationsmentioning

confidence: 99%

The Araucaria Project: High-precision orbital parallax and masses of the eclipsing binary TZ Fornacis

Gallenne

Pietrzyński

Graczyk

et al. 2016

A&A

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Context. Independent distance estimates are particularly useful to check the precision of other distance indicators, while accurate and precise masses are necessary to constrain evolution models. Aims. The goal is to measure the masses and distance of the detached eclipsing-binary TZ For with a precision level lower than 1% using a fully geometrical and empirical method. Methods. We obtained the first interferometric observations of TZ For with the VLTI/PIONIER combiner, which we combined with new and precise radial velocity measurements to derive its three-dimensional orbit, masses, and distance. Results. The system is well resolved by PIONIER at each observing epoch, which allowed a combined fit with eleven astrometric positions. Our derived values are in a good agreement with previous work, but with an improved precision. We measured the mass of both components to be M 1 = 2.057 ± 0.001 M and M 2 = 1.958 ± 0.001 M . The comparison with stellar evolution models gives an age of the system of 1.20 ± 0.10 Gyr. We also derived the distance to the system with a precision level of 1.1%: d = 185.9 ± 1.9 pc. Such precise and accurate geometrical distances to eclipsing binaries provide a unique opportunity to test the absolute calibration of the surface brightness-colour relation for late-type stars, and will also provide the best opportunity to check on the future Gaia measurements for possible systematic errors.

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“…The calibrators, listed in Table 3, were selected using the SearchCal 1 software (Bonneau et al 2006(Bonneau et al , 2011 provided by the Jean-Marie Mariotti Center (JMMC).…”

Section: Interferometric Observationsmentioning

confidence: 99%

The Araucaria Project: High-precision orbital parallax and masses of the eclipsing binary TZ Fornacis

Gallenne

Pietrzyński

Graczyk

et al. 2016

A&A

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“…The longest baseline between UT1 and UT4 is nominally 130 m in length. A single observation of the science target was sandwiched between two calibrator observations, one of HD 34137 and the other of HD 36059, with diameters of 0.73 ± 0.02 mas and 0.51 ± 0.01 mas, respectively (Bonneau et al 2006(Bonneau et al , 2011. The data were reduced using the amdlib pipeline (Tatulli et al 2007;Chelli et al 2009) but only the top 30% visibility data in terms of signal-to-noise ratio were used to reduce the influence of periods of poor group-delay fringe tracking.…”

Section: Vlti Observations and Data Reductionmentioning

confidence: 99%

Orbits, Distance, and Stellar Masses of the Massive Triple Star Σ Orionis

Schaefer¹,

Hummel²,

Gies³

et al. 2016

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We present interferometric observations of the σ Orionis triple system using the CHARA Array, NPOI, and VLTI. Using these measurements, we spatially resolve the orbit of the close spectroscopic binary (Aa,Ab) for the first time and present a revised orbit for the wide pair (A,B). Combining the visual orbits with previously published radial velocity measurements and new radial velocities measured at CTIO, we derive dynamical masses for the three massive stars in the system of M Aa = 16.99 ± 0.20 M ⊙ , M Ab = 12.81 ± 0.18 M ⊙ , and M B = 11.5 ± 1.2 M ⊙ . The inner and outer orbits in the triple are not coplanar, with a relative inclination of 120• -127• . The orbital parallax provides a precise distance of 387.5 ± 1.3 pc to the system. This is a significant improvement over previous estimates of the distance to the young σ Orionis cluster.

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“…Two different calibrators were used for the VEGA observations: HD 3360 and HD 25642. They were identified using the SearchCal service 3 (Bonneau et al 2006(Bonneau et al , 2011 and the CDS Astronomical Databases SIMBAD and VIZIER 4 . We used the SearchCal spectrophotometric uniform disk angular diameter determinations in the R and H bands, which led to θ UD−R = 0.284 ± 0.020 mas and θ UD−H = 0.287 ± 0.020 mas for HD 3360 and to θ UD−R = 0.439 ± 0.031 mas and θ UD−H = 0.447±0.031 mas for HD 25642.…”

Section: Interferometric Observations and Data Analysis Principlesmentioning

confidence: 99%

Spectral and spatial imaging of the Be+sdO binaryϕPersei

Mourard

Monnier

Meilland

et al. 2015

A&A

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Aims. The rapidly rotating Be star ϕ Persei was spun up by mass and angular momentum transfer from a now stripped-down, hot subdwarf companion. Here we present the first high angular resolution images of ϕ Persei made possible by new capabilities in longbaseline interferometry at near-IR and visible wavelengths. We analyzed these images to search for the companion, to determine the binary orbit, stellar masses, and fluxes, and to examine the geometrical and kinematical properties of the outflowing disk surrounding the Be star. Methods. We observed ϕ Persei with the MIRC and VEGA instruments of the CHARA Array. MIRC was operated in six-telescope mode, whereas VEGA was configured in four-telescope mode with a change of quadruplets of telescopes during two nights to improve the (u, v) plane coverage. Additional MIRC-only observations were performed to track the orbital motion of the companion, and these were fit together with new and existing radial velocity measurements of both stars to derive the complete orbital elements and distance. We also used the MIRC data to reconstruct an image of the Be disk in the near-IR H-band. VEGA visible broadband and spectro-interferometric Hα observations were fit with analytical models for the Be star and disk, and image reconstruction was performed on the spectrally resolved Hα emission line data. Results. The hot subdwarf companion is clearly detected in the near-IR data at each epoch of observation with a flux contribution of 1.5% in the H band, and restricted fits indicate that its flux contribution rises to 3.3% in the visible. A new binary orbital solution is determined by combining the astrometric and radial velocity measurements. The derived stellar masses are 9.6 ± 0.3 M and 1.2 ± 0.2 M for the Be primary and subdwarf secondary, respectively. The inferred distance (186 ± 3 pc), kinematical properties, and evolutionary state are consistent with membership of ϕ Persei in the α Per cluster. From the cluster age we deduce significant constraints on the initial masses and evolutionary mass transfer processes that transformed the ϕ Persei binary system. The interferometric data place strong constraints on the Be disk elongation, orientation, and kinematics, and the disk angular momentum vector is coaligned with and has the same sense of rotation as the orbital angular momentum vector. The VEGA visible continuum data indicate an elongated shape for the Be star itself, due to the combined effects of rapid rotation, partial obscuration of the photosphere by the circumstellar disk, and flux from the bright inner disk.

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SearchCal: a Virtual Observatory tool for searching calibrators in optical long-baseline interferometry

Cited by 80 publications

References 29 publications

The Araucaria Project: High-precision orbital parallax and masses of the eclipsing binary TZ Fornacis

The Araucaria Project: High-precision orbital parallax and masses of the eclipsing binary TZ Fornacis

Orbits, Distance, and Stellar Masses of the Massive Triple Star Σ Orionis

Spectral and spatial imaging of the Be+sdO binaryϕPersei

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