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October 2013 (v1)Journal articleUploaded on: December 4, 2022
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December 2017 (v1)Journal article
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...
Uploaded on: December 4, 2022 -
May 14, 2019 (v1)Conference paper
Cepheids are the keystone of the extragalactic distance ladder since their pulsation periods correlate directly with their luminosity, through the Period-Luminosity (PL) relation (Leavitt & Pickering 1912). The discovery of the accelerated expansion of the Universe (Riess et al. 1998; 2011 Nobel prize) is largely based on the Cepheid distance...
Uploaded on: December 4, 2022 -
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 -
December 2019 (v1)Journal article
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Uploaded on: December 3, 2022 -
June 2015 (v1)Journal article
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January 2016 (v1)Journal article
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2020 (v1)Journal article
Context. It has recently been shown that the infrared (IR) emission of Cepheids, constant over the pulsation cycle, might be due to a pulsating shell of ionized gas with a radius of about 15% of that of the star radius, which could be attributed to the chromospheric activity of Cepheids. Aims. The aim of this paper is to investigate the...
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December 2015 (v1)Journal article
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Uploaded on: December 4, 2022 -
May 2012 (v1)Journal article
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November 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 -
2017 (v1)Journal article
Context. The projection factor p is the key quantity used in the Baade-Wesselink (BW) method for distance determination; it converts radial velocities into pulsation velocities. Several methods are used to determine p, such as geometrical and hydrodynamical models or the inverse BW approach when the distance is known. Aims. We analyze new...
Uploaded on: December 4, 2022 -
October 2019 (v1)Publication
Our sample is made up of 64 Classical Galactic Cepheids with pulsation periods in the range 2 to 68 days. We provide the full details of our sample in Table A.1. We present both the six correlation templates built to derive tailored cross-correlation functions (CCFs), the CCFs themselves, and the derived radial velocity and line profile...
Uploaded on: December 4, 2022 -
July 5, 2016 (v1)Journal article
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Uploaded on: December 3, 2022 -
2020 (v1)Journal article
Context. The surface brightness – color relationship (SBCR) is a poweful tool for determining the angular diameter of stars from photometry. It was for instance used to derive the distance of eclipsing binaries in the Large Magellanic Cloud (LMC), which led to its distance determination with an accuracy of 1%.Aims. We calibrate the SBCR for red...
Uploaded on: December 4, 2022 -
August 2018 (v1)Journal article
Context. The dynamical structure of the atmosphere of Cepheids has been well studied in the optical. Several authors have found very interesting spectral features in the J band, but little data have been secured beyond 1.6 μm. However, such observations can probe different radial velocities and line asymmetry regimes, and are able to provide...
Uploaded on: December 4, 2022 -
July 2015 (v1)Journal article
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Uploaded on: December 4, 2022