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- W2964461154 abstract "Context. Accurate radial velocities ( v rad ) of Cepheids are mandatory within the context of Cepheid distance measurements using the Baade-Wesselink technique. The most common v rad derivation method consists in cross-correlating the observed stellar spectra with a binary template and measuring a velocity on the resulting mean profile. Nevertheless, for Cepheids and other pulsating stars, the spectral lines selected within the template as well as the way of fitting the cross-correlation function (CCF) have a direct and significant impact on the measured v rad . Aims. Our first aim is to detail the steps to compute consistent CCFs and v rad of Cepheids. Next, this study aims at characterising the impact of Cepheid spectral properties and v rad computation methods on the resulting line profiles and v rad time series. Methods. We collected more than 3900 high-resolution spectra from seven different spectrographs of 64 Classical Milky Way (MW) Cepheids. These spectra were normalised and standardised using a single custom-made process on pre-defined wavelength ranges. We built six tailored correlation templates selecting unblended spectral lines of different depths based on a synthetic Cepheid spectrum, on three different wavelength ranges from 3900 to 8000 Å. Each observed spectrum was cross-correlated with these templates to build the corresponding CCFs, adopted as the proxy for the spectrum mean line profile. We derived a set of line profile observables as well as three different v rad measurements from each CCF and two custom proxies for the CCF quality and amount of signal. Results. This study presents a large catalogue of consistent Cepheid CCFs and v rad time series. It confirms that each step of the process has a significant impact on the deduced v rad : the wavelength, the template line depth and width, and the v rad computation method. The way towards more robust Cepheid v rad time series seems to go through steps that minimise the asymmetry of the line profile and its impact on the v rad . Centroid or first-moment v rad , that exhibit slightly smaller amplitudes but significantly smaller scatter than Gaussian or biGaussian v rad , should therefore be favoured. Stronger or deeper spectral lines also tend to be less asymmetric and lead to more robust v rad than weaker lines." @default.
- W2964461154 created "2019-08-13" @default.
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- W2964461154 date "2019-10-16" @default.
- W2964461154 modified "2023-10-15" @default.
- W2964461154 title "Consistent radial velocities of classical Cepheids from the cross-correlation technique" @default.
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- W2964461154 doi "https://doi.org/10.1051/0004-6361/201935622" @default.
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