Context. The Baade-Wesselink (BW) method, which combines linear and angular diameter variations, is the most common method to determine the distances to pulsating stars. However, the projection factor, p-factor, used to convert radial velocities into pulsation velocities, is still poorly calibrated. This parameter is critical on the use of this...
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December 2017 (v1)Journal articleUploaded on: December 4, 2022
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July 2021 (v1)Journal article
Aims. We aim to investigate the infrared excess of 45 Milky Way (MW) Cepheids combining different observables in order to constrain the presence of circumstellar envelopes (CSEs). Methods. We used the SpectroPhoto-Interferometry of Pulsating Stars (SPIPS) algorithm, a robust implementation of the parallaxof-pulsation method that combines...
Uploaded on: December 3, 2022 -
August 2018 (v1)Journal article
Observations of 48 red-clump stars were obtained in the H band with the PIONIER instrument installed at the Very Large Telescope Interferometer. Limb-darkened angular diameters were measured by fitting radial intensity profile I(r) to square visibility measurements. Half the angular diameters determined have formal errors better than 1.2%,...
Uploaded on: December 4, 2022 -
July 2015 (v1)Journal article
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July 5, 2016 (v1)Journal article
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December 2019 (v1)Journal article
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Uploaded on: December 3, 2022 -
January 2020 (v1)Journal article
Context. The infrared (IR) excess of classical Cepheids is seldom studied and poorly understood despite observational evidence and the potential for its contribution to induce systematics on the period-luminosity (PL) relation used in the calibration of the extragalactic distance scale. Aims: This study aims to understand the physical origin of...
Uploaded on: December 4, 2022 -
November 2019 (v1)Journal article
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Uploaded on: December 3, 2022 -
December 1, 2019 (v1)Journal article
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Uploaded on: December 4, 2022 -
July 2015 (v1)Journal article
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March 2, 2023 (v1)Journal article
Context. The Baade-Wesselink (BW) method of distance determination of Cepheids is used to calibrate the distance scale. Various versions of this method are mainly based on interferometry and/or the surface-brightness color relation (SBCR). Aims. We quantify the impact of the SBCR, its slope, and its zero point on the projection factor. This...
Uploaded on: November 30, 2023 -
April 2013 (v1)Journal article
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Uploaded on: December 4, 2022 -
October 2022 (v1)Journal article
Aims. Surface brightness – colour relations (SBCRs) are very useful tools for predicting the angular diameters of stars. They offer the possibility to calculate very precise spectrophotometric distances by the eclipsing binary method or the Baade-Wesselink method. Double-lined Detached Eclipsing Binary stars (SB2 DEBs) with precisely known...
Uploaded on: December 4, 2022 -
December 2018 (v1)Journal article
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March 2020 (v1)Publication
In the last 20 years, over the course of the Araucaria project, we have studied 20 very special eclipsing binary systems in the Large Magellanic Cloud (LMC). Based on these systems and our newly calibrated surface brightness-colour relation we have measured a distance to the LMC that is accurate to 1%. This is currently the best benchmark for...
Uploaded on: December 4, 2022 -
March 2019 (v1)Journal article
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Uploaded on: December 4, 2022 -
October 2014 (v1)Journal article
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Uploaded on: December 3, 2022