The angular sizes of dwarf stars and subgiants

Kervella, P.; Thévenin, F.; Folco, E. Di; Ségransan, D.

doi:10.1051/0004-6361:20035930

Cited by 496 publications

(594 citation statements)

References 63 publications

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“…The jktabsdim does not work on brightnesses in Kepler band, so, unless stated otherwise, for the distance estimation we used B, V, J, H and K-band entries from Simbad (Wenger et al 2000). As the final value of distance we adopt a weighted average of five values, calculated for each band from the surface brightness-T e f f relations of Kervella et al (2004). For the majority of distance calculations, we used temperatures found from isochrone fitting (Sect.…”

Section: Light Curve Solutions and Absolute Parametersmentioning

confidence: 99%

HIDES spectroscopy of bright detached eclipsing binaries from the Kepler field – II. Double- and triple-lined objects

Hełminiak

Ukita

Kambe

et al. 2017

Monthly Notices of the Royal Astronomical Society

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We present the results of our spectroscopic observations of eight detached eclipsing binaries (DEBs), selected from the Kepler Eclipsing Binary Catalog. Radial velocities (RVs) were calculated from high resolution spectra obtained with the HIDES spectrograph, attached to the 1.88-m telescope of the Okayama Astrophysical Observatory, and were used to characterize the targets in combination with the Kepler light curves. For each binary we obtained a full set of orbital and physical parameters, reaching precision below 3% in masses and radii for 5 pairs. By comparing our results with theoretical models, we assess the distance, age and evolutionary status of the researched objects. We also study eclipse timing variations of selected objects, and identify a new system with a γDor pulsator. Two systems are triples, and show lines coming from three components. In one case the motion of the outer star and the perturbation in the RVs of the inner binary are clearly visible and periodical, which allows us to directly calculate the mass of the third star, and inclination of the outer orbit. In the second case we only see a clear motion of the tertiary, and investigate two scenarios: that it is a linear trend coming from the orbital motion around the inner binary, and that it is caused by a planetary mass companion. When possible, we also compare our results with the literature, and conclude that only by combining photometry with RVs it is possible to obtain correct physical parameters of both components of a DEB.

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Section: Light Curve Solutions and Absolute Parametersmentioning

confidence: 99%

HIDES spectroscopy of bright detached eclipsing binaries from the Kepler field – II. Double- and triple-lined objects

Hełminiak

Ukita

Kambe

et al. 2017

Monthly Notices of the Royal Astronomical Society

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“…Using this and the measurements reported above, we derive [(V−I), I] 0,s =(0.77±0.04, 19.35±0.05). Using the VIK color-color relations of Bessell & Brett (1988) and the color/surface-brightness relations of Kervella et al (2004), this yields (e.g., Yoo et al 2004)…”

Section: Cmd and Spitzer-ground Color-color Relationmentioning

confidence: 99%

OGLE-2016-BLG-1190Lb: The First Spitzer Bulge Planet Lies Near the Planet/Brown-dwarf Boundary

Ryu¹,

Yee²,

Udalski³

et al. 2017

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We report the discovery of OGLE-2016-BLG-1190Lb, which is likely to be the first Spitzer microlensing planet in the Galactic bulge/bar, an assignation that can be confirmed by two epochs of high-resolution imaging of the combined source-lens baseline object. The planet's mass, M p =13.4±0.9 M J , places it right at the deuteriumburning limit, i.e., the conventional boundary between "planets" and "brown dwarfs." Its existence raises the question of whether such objects are really "planets" (formed within the disks of their hosts) or "failed stars" (lowmass objects formed by gas fragmentation). This question may ultimately be addressed by comparing disk and bulge/bar planets, which is a goal of the Spitzer microlens program. The host is a G dwarf, M host =0.89±0.07 M e , and the planet has a semimajor axis a∼2.0 au. We use Kepler K2 Campaign 9 microlensing data to break the lens-mass degeneracy that generically impacts parallax solutions from Earth-Spitzer observations alone, which is the first successful application of this approach. The microlensing data, derived primarily from near-continuous, ultradense survey observations from OGLE, MOA, and three KMTNet telescopes, contain more orbital information than for any previous microlensing planet, but not quite enough to accurately specify the full orbit. However, these data do permit the first rigorous test of microlensing orbital-motion measurements, which are typically derived from data taken over <1% of an orbital period.

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“…4.4) and angular resolution of VEGA/CHARA gives access to a broad range of stellar properties. Based on the Hipparcos catalogue V band photometry, K band magnitudes from 2MASS, and (V, V − K) surface brightness color relations from Kervella et al (2004), we computed the limb-darkened angular diameter of all stars brighter than m V = 6.5. We then estimated the accuracy we can obtain on the measurement of their angular diameter with VEGA/CHARA, and selected only the stars for which the accuracy is better than 2%.…”

Section: Fundamental Stellar Parametersmentioning

confidence: 99%

“…Long-baseline interferometers currently provide a new quasi-geometrical way to calibrate the Cepheid periodluminosity relation; indeed it is now possible to determine the distance of galactic Cepheids up to 1 kpc using the Interferometric Baade-Wesselink method (Kervella et al 2004;Sasselov & Karovska 1994;Davis et al 2009). Interferometric measurements lead to angular diameter estimations over the whole pulsation period, while the stellar radius variations can be obtained from the integration of the pulsation velocity curve deduced from line profiles by the so-called projection factor p.…”

Section: Fundamental Stellar Parametersmentioning

confidence: 99%

VEGA: Visible spEctroGraph and polArimeter for the CHARA array: principle and performance

Mourard

Clausse

Marcotto

et al. 2009

A&A

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140

183

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Context. Among optical stellar interferometers, the CHARA Array located at Mt Wilson in California offers the potential of very long baselines (up to 330 m) and the prospect of coupling multiple beam combiners. This paper presents the principle and the measured performance of VEGA, Visible spEctroGraph and polArimeter installed in September 2007 at the coherent focus of the array. Aims. With 0.3 ms of arc of spatial resolution and up to 30 000 of spectral resolution, VEGA intends to measure fundamental parameters of stars, to study stellar activities and to image and analyze circumstellar environments. We describe the observing modes that have been implemented for this spectro-polarimeter and show actual performances measured on the sky during the first observing runs. Methods. The astrophysical programs are described in relation to the observing modes of the instrument, the presentation of the spectrograph and of the interface table is shown and finally the data is presented. We discuss the perspectives of further development in the framework of the CHARA Array. Results. We show that VEGA/CHARA is fully operational. The current limiting magnitude is nearly 7 but the results depend on the observing conditions (seeing, spectral resolution, etc.). We have validated the stability of the instrumental visibility at the level of 1 to 2% over half an hour and of the instrumental polarization for various declinations. Some examples of squared visibility and differential visibility are presented. Conclusions. The spectro-polarimeter VEGA has been installed and successfully tested on CHARA. It will permit stellar physics studies at unprecedented spectral and spatial resolutions.

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The angular sizes of dwarf stars and subgiants

Cited by 496 publications

References 63 publications

HIDES spectroscopy of bright detached eclipsing binaries from the Kepler field – II. Double- and triple-lined objects

HIDES spectroscopy of bright detached eclipsing binaries from the Kepler field – II. Double- and triple-lined objects

OGLE-2016-BLG-1190Lb: The First Spitzer Bulge Planet Lies Near the Planet/Brown-dwarf Boundary

VEGA: Visible spEctroGraph and polArimeter for the CHARA array: principle and performance

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