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1. SPIDAST: a new modular software to process spectro-interferometric measurements

Author

Cruzalèbes, Pierre, Rabbia, Yves, Jorissen, Alain, Spang, Alain, Sacuto, Stéphane, Pasquato, Ester, Chiavassa, Andrea, Chesneau, Olivier, and Fréville, Patrick

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

Extracting stellar fundamental parameters from SPectro-Interferometric (SPI) data requires reliable estimates of observables and with robust uncertainties (visibility, triple product, phase closure). A number of fine calibration procedures is necessary throughout the reduction process. Testing departures from centro-symmetry of brightness distributions is a useful complement. Developing a set of automatic routines, called SPIDAST (made available to the community) to reduce, calibrate and interpret raw data sets of instantaneous spectro-interferograms at the spectral channel level, we complement (and in some respects improve) the ones contained in the amdlib Data Reduction Software. Our new software SPIDAST is designed to work in an automatic mode, free from subjective choices, while being versatile enough to suit various processing strategies. SPIDAST performs the following automated operations: weighting of non-aberrant SPI data (visibility, triple product), fine spectral calibration (sub-pixel level), accurate and robust determinations of stellar diameters for calibrator sources (and their uncertainties as well), correction for the degradations of the interferometer response in visibility and triple product, calculation of the Centro-Symmetry Parameter (CSP) from the calibrated triple product, fit of parametric chromatic models on SPI observables, to extract model parameters. SPIDAST is currently applied to the scientific study of 18 cool giant and supergiant stars, observed with the VLTI/AMBER facility at medium resolution in the K band. Because part of their calibrators have no diameter in the current catalogs, SPIDAST provides new determinations of the angular diameters of all calibrators. Comparison of SPIDAST final calibrated observables with amdlib determinations shows good agreement, under good and poor seeing conditions., Comment: 14 pages, 15 figures, 3 tables

Published
2013
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2. Limits in astrometric accuracy induced by surface brightness asymmetries in red supergiant stars

Author

Pasquato, Ester, Pourbaix, Dimitri, and Jorissen, Alain

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

Surface brightness asymmetries are a very common feature of stars. Among other effects they cause a difference between the projected barycentre and photocentre. The evolution of those surface features makes this difference time-dependent. In some cases, e. g. for supergiant stars, the displacement can be a non-negligible fraction of the star radius R, and if R>1 AU, of the parallax. We investigate the impact of surface brightness asymmetries on both the Gaia astrometric solution and the data processing flow with a theoretical approach. We show that when the amplitude of the displacement is comparable to the epoch astrometric precision, the resulting astrometric solution of a genuine single star may be, in some cases, of low quality (with some parameters up to 10 sigma off). In this case, we provide an analytical prediction of the impact of the photocentre motion on both chi squared and the uncertainty in the astrometric parameters. Non-single star solutions are found, if allowed for the closest stars. A closer look at the parameters of the orbital solutions reveals however that they are spurious (since the semi-major axis is smaller than either its error or the stellar radius). It is thus possible to filter out those spurious orbital solutions. Interestingly, for the stocastic solutions, the stochastic noise appears to be a good estimate of the photocentric noise., Comment: Accepted for publication on Astronomy and Astrophysics

Published
2011
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3. Effects of stellar surface inhomogeneities on astrometric accuracy / Effets des inhomogénéités de surface stellaire sur la précision astrométrique

Author

Pasquato, Ester, Clerbaux, Barbara, De Mol, Christine, Bruss, Thomas, Turon, Catherine, Lennart, Lindegren, Jorissen, Alain, and Pourbaix, Dimitri

Subjects
convective cells, magnetic spots, astrometry, Gaia, red supergiants
Abstract

Surface brightness asymmetries are a very common feature of stars. Among other effects they cause a difference between the projected centre of mass and the photocentre. The evolution of those surface features makes this difference time-dependent. In some cases the displacement can be a non-negligible fraction of the star radius R, and if R>1 AU, of the parallax. We investigate the impact of surface brightness asymmetries on the Gaia astrometric solution and on the data processing flow. In particular we derive analytical expressions for the change in the derived astrometric parameters for a single-star, with respect to the parameters for a uniformly-bright star, as a function of the characteristics of the surface brightness asymmetries. These predictions are confirmed by the results of the processing of simulated astrometric Gaia data where a photocentre motion caused by surface brightness asymmetries has been added using a Gaussian Markovian model. In the case of a red supergiant star, the average photocentre shift is about 0.1 AU. Such a photocentric noise translates in a 10% inaccuracy on the parallax (independently of the distance), which becomes larger than the statistical error on the parallax derived from the data reduction for stars that are up to about 4 kpc away. For the most nearby stars, we derive an inaccuracy on the parallax that can be 10 times its statistical error. Finally we estimate that up to about 4000 stars among red supergiants and bright giants may have astrometric parameters that are inaccurate at levels bigger than expected because of the surface brightness asymmetries. In the determination of this number, a crucial role is played by the Gaia observable magnitude range. The fact that Gaia will not observe stars brighter than 5.6 in the Gaia G band means that the closest stars will not be observed. Yet, the impact of the surface brightness asymmetries is proportional to their angular size, meaning that the stars whose astrometric accuracy would be most affected are not observed. Various non-Gaussian spot models (as applicable in the case of magnetic spots) have been implemented and analytical predictions for the effects of such magnetic spots are computed for the most representative classes of magnetic stars. Another effect of the presence of surface brightness asymmetries is their impact on Gaia data processing flow. The quality of the fit of the data is evaluated with the F2 parameter that is a transformation of χ2 such that it has a unit normal distribution when the model is adequate and it is independent of the number of measurements. If the goodness-of-fit F2 of the single-star solution is not good enough (F2>3), a chain of solution of growing complexity is tried until a satisfactory one (with F21 UA, de la parallaxe. Nous examinons l'impact des asymétries de brillance de surface sur la solution astrométrique de Gaia et sur le processus de traitement des données. En particulier nous dérivons des expressions analytiques pour le changement des paramètres astrométriques déerivées pour une étoile simple, par rapport aux paramètres pour une étoile uniformément lumineuse, en fonction des caractéristiques des asymétries de brillance de surface. Ces prévisions sont confirmées par les résultats de simulations du traitement des données astrométriques de Gaia, auxquelles des mouvements du photocentre causés par des asymétries de brillance de surface ont été ajoutés en utilisant un modèle gaussien markovien. Dans le cas d'une étoile super-géante rouge, le décalage moyen du photocentre est d'environ 0.1 UA. Un bruit photocentrique de cette amplitude se traduit dans une imprécision de 10% sur la parallaxe (indépendamment de la distance), qui peut devenir plus grande que l'erreur statistique sur la parallaxe déerivée par la réduction des données, pour les étoiles plus proches d'environ 4 kpc. Pour les étoiles les plus proches, nous évaluons une imprécision sur la parallaxe qui peut être 10 fois leur erreur statistique. Finalement, nous estimons que jusqu'à environ 4000 étoiles parmi les super-géantes rouges et géantes brillantes peuvent avoir des paramètres astrométriques inexactes à des niveaux plus grands que prévu en raison des asymétries de brillance de surface. Dans la détermination de ce nombre, la gamme de magnitudes observables par Gaia joue un rôle crucial. Le fait que Gaia n'observera pas les étoiles plus brillantes que 5.6 mag (en bande Gaia) signifie que les étoiles les plus proches ne seront pas observées. Pourtant, l'impact des asymétries de brillance de surface est proportionnel à leur taille angulaire, ce qui signifie que les étoiles dont la précision astrométrique seraient la plus affecté ne seront pas observées. Différents modèles de taches ont été réalisés et des prédictions analytiques pour les effets de ces taches magnétiques sont calculés pour les classes les plus représentatives des étoiles magnétiques. Un autre effet de la présence des asymétries de brillance de surface est leur impact sur le traitement des données de Gaia. La qualité de l'ajustement des données est évaluée avec le paramètre F2 qui est une transformation de χ2 telle qu'il ait une distribution normale lorsque le modèle est adéquat. Si la qualité de l'ajustement F2 de la solution étoile-simple n'est pas acceptable (F2>3), une chaîne de solutions de complexité croissante est essayée jusqu'à ce qu'une solution satisfaisante (avec F2, Doctorat en Sciences, info:eu-repo/semantics/published

Published
2011

4. Effets des inhomogénéités de surface stellaire sur la précision astrométrique

Author

Pasquato, Ester, Jorissen, Alain, Pourbaix, Dimitri, Clerbaux, Barbara, De Mol, Christine, Bruss, F Thomas, Turon, Catherine, and Lennart, Lindegren

Subjects
Etoiles magnétiques, convective cells, Physique, Astrométrie, Géantes rouges, Gaia, Astrometry, red supergiants, Red giants, Stars -- Observations, magnetic spots, Etoiles -- Observations, Sciences exactes et naturelles, Magnetic stars
Abstract

Surface brightness asymmetries are a very common feature of stars. Among other effects they cause a difference between the projected centre of mass and the photocentre. The evolution of those surface features makes this difference time-dependent. In some cases the displacement can be a non-negligible fraction of the star radius R, and if R>1 AU, of the parallax. We investigate the impact of surface brightness asymmetries on the Gaia astrometric solution and on the data processing flow. In particular we derive analytical expressions for the change in the derived astrometric parameters for a single-star, with respect to the parameters for a uniformly-bright star, as a function of the characteristics of the surface brightness asymmetries. These predictions are confirmed by the results of the processing of simulated astrometric Gaia data where a photocentre motion caused by surface brightness asymmetries has been added using a Gaussian Markovian model.In the case of a red supergiant star, the average photocentre shift is about 0.1 AU. Such a photocentric noise translates in a 10% inaccuracy on the parallax (independently of the distance), which becomes larger than the statistical error on the parallax derived from the data reduction for stars that are up to about 4 kpc away. For the most nearby stars, we derive an inaccuracy on the parallax that can be 10 times its statistical error. Finally we estimate that up to about 4000 stars among red supergiants and bright giants may have astrometric parameters that are inaccurate at levels bigger than expected because of the surface brightness asymmetries. In the determination of this number, a crucial role is played by the Gaia observable magnitude range. The fact that Gaia will not observe stars brighter than 5.6 in the Gaia G band means that the closest stars will not be observed. Yet, the impact of the surface brightness asymmetries is proportional to their angular size, meaning that the stars whose astrometric accuracy would be most affected are not observed.Various non-Gaussian spot models (as applicable in the case of magnetic spots) have been implemented and analytical predictions for the effects of such magnetic spots are computed for the most representative classes of magnetic stars.Another effect of the presence of surface brightness asymmetries is their impact on Gaia data processing flow. The quality of the fit of the data is evaluated with the F2 parameter that is a transformation of χ2 such that it has a unit normal distribution when the model is adequate and it is independent of the number of measurements. If the goodness-of-fit F2 of the single-star solution is not good enough (F2>3), a chain of solution of growing complexity is tried until a satisfactory one (with F2/Les asymétries de brillance de surface sont une caractéristique commune des étoiles. Parmi d'autres effets, elles provoquent une différence entre la projection du centre de masse et le photocentre. L'évolution de ces structures de surface rend cette différence variable avec le temps. Dans certains cas, le déplacement du photocentre peut être une fraction non négligeable du rayon de l'étoile R et, si R>1 UA, de la parallaxe. Nous examinons l'impact des asymétries de brillance de surface sur la solution astrométrique de Gaia et sur le processus de traitement des données. En particulier nous dérivons des expressions analytiques pour le changement des paramètres astrométriques déerivées pour une étoile simple, par rapport aux paramètres pour une étoile uniformément lumineuse, en fonction des caractéristiques des asymétries de brillance de surface. Ces prévisions sont confirmées par les résultats de simulations du traitement des données astrométriques de Gaia, auxquelles des mouvements du photocentre causés par des asymétries de brillance de surface ont été ajoutés en utilisant un modèle gaussien markovien.Dans le cas d'une étoile super-géante rouge, le décalage moyen du photocentre est d'environ 0.1 UA. Un bruit photocentrique de cette amplitude se traduit dans une imprécision de 10% sur la parallaxe (indépendamment de la distance), qui peut devenir plus grande que l'erreur statistique sur la parallaxe déerivée par la réduction des données, pour les étoiles plus proches d'environ 4 kpc. Pour les étoiles les plus proches, nous évaluons une imprécision sur la parallaxe qui peut être 10 fois leur erreur statistique. Finalement, nous estimons que jusqu'à environ 4000 étoiles parmi les super-géantes rouges et géantes brillantes peuvent avoir des paramètres astrométriques inexactes à des niveaux plus grands que prévu en raison des asymétries de brillance de surface. Dans la détermination de ce nombre, la gamme de magnitudes observables par Gaia joue un rôle crucial. Le fait que Gaia n'observera pas les étoiles plus brillantes que 5.6 mag (en bande Gaia) signifie que les étoiles les plus proches ne seront pas observées. Pourtant, l'impact des asymétries de brillance de surface est proportionnel à leur taille angulaire, ce qui signifie que les étoiles dont la précision astrométrique seraient la plus affecté ne seront pas observées.Différents modèles de taches ont été réalisés et des prédictions analytiques pour les effets de ces taches magnétiques sont calculés pour les classes les plus représentatives des étoiles magnétiques. Un autre effet de la présence des asymétries de brillance de surface est leur impact sur le traitement des données de Gaia. La qualité de l'ajustement des données est évaluée avec le paramètre F2 qui est une transformation de χ2 telle qu'il ait une distribution normale lorsque le modèle est adéquat. Si la qualité de l'ajustement F2 de la solution étoile-simple n'est pas acceptable (F2>3), une chaîne de solutions de complexité croissante est essayée jusqu'à ce qu'une solution satisfaisante (avec F2, Doctorat en Sciences, info:eu-repo/semantics/nonPublished

Published
2011

5. Fundamental parameters of 16 late-type stars derived from their angular diameter measured with VLTI/AMBER

Author

Cruzalèbes, Pierre, Jorissen, Alain, Rabbia, Yves, Sacuto, Stéphane, Chiavassa, Andréa, Pasquato, Ester, Plez, B., Eriksson, Karl Martin, Spang, A., Chesneau, Olivier, Cruzalèbes, Pierre, Jorissen, Alain, Rabbia, Yves, Sacuto, Stéphane, Chiavassa, Andréa, Pasquato, Ester, Plez, B., Eriksson, Karl Martin, Spang, A., and Chesneau, Olivier

Abstract

info:eu-repo/semantics/published

Published
2013

6. SPIDAST: a new modular software to process spectrointerferometric measurements

Author

Cruzalèbes, Pierre, Rabbia, Yves, Jorissen, Alain, Spang, A., Sacuto, Stéphane, Pasquato, Ester, Chiavassa, Andréa, Chesneau, Olivier, Fréville, P., Cruzalèbes, Pierre, Rabbia, Yves, Jorissen, Alain, Spang, A., Sacuto, Stéphane, Pasquato, Ester, Chiavassa, Andréa, Chesneau, Olivier, and Fréville, P.

Abstract

Extracting stellar fundamental parameters from Spectrointerferometric (SPI) data requires reliable estimates of observables and with robust uncertainties (visibility, triple product, phase closure). A number of fine calibration procedures are necessary throughout the reduction process. Testing departures from centrosymmetry of brightness distributions is a useful complement. Developing a set of automatic routines called SPIDAST (made available to the community) to reduce, calibrate and interpret raw data sets of instantaneous spectrointerferograms at the spectral channel level, we complement (and in some respects improve) the ones contained in the AMDLIB Data Reduction Software. Our new software SPIDAST is designed to work in an automatic mode, free from subjective choices, while being versatile enough to suit various processing strategies. SPIDAST performs the following automated operations: weighting of nonaberrant SPI data (visibility, triple product), fine spectral calibration (subpixel level), accurate and robust determinations of stellar diameters for calibrator sources (and their uncertainties as well), correction for the degradations of the interferometer response in visibility and triple product, calculation of the centrosymmetry parameter from the calibrated triple product, fit of parametric chromatic models on SPI observables, to extract model parameters. SPIDAST is currently applied to the scientific study of 18 cool giant and supergiant stars, observed with the VLTI/AMBER facility at medium resolution in the K band. Because part of their calibrators have no diameter in the current catalogues, SPIDAST provides new determinations of the angular diameters of all calibrators. Comparison of SPIDAST final calibrated observables with AMDLIB determinations shows good agreement, under good and poor seeing conditions. © 2013 The Authors. Published by Oxford University Press on behalf of the Royal Astronomical Society., SCOPUS: ar.j, info:eu-repo/semantics/published

Published
2013

7. Effects of stellar surface inhomogeneities on astrometric accuracy

Author

Jorissen, Alain, Pourbaix, Dimitri, Clerbaux, Barbara, De Mol, Christine, Bruss, F Thomas, Turon, Catherine, Lennart, Lindegren, Pasquato, Ester, Jorissen, Alain, Pourbaix, Dimitri, Clerbaux, Barbara, De Mol, Christine, Bruss, F Thomas, Turon, Catherine, Lennart, Lindegren, and Pasquato, Ester

Abstract

Surface brightness asymmetries are a very common feature of stars. Among other effects they cause a difference between the projected centre of mass and the photocentre. The evolution of those surface features makes this difference time-dependent. In some cases the displacement can be a non-negligible fraction of the star radius R, and if R>1 AU, of the parallax. We investigate the impact of surface brightness asymmetries on the Gaia astrometric solution and on the data processing flow. In particular we derive analytical expressions for the change in the derived astrometric parameters for a single-star, with respect to the parameters for a uniformly-bright star, as a function of the characteristics of the surface brightness asymmetries. These predictions are confirmed by the results of the processing of simulated astrometric Gaia data where a photocentre motion caused by surface brightness asymmetries has been added using a Gaussian Markovian model.In the case of a red supergiant star, the average photocentre shift is about 0.1 AU. Such a photocentric noise translates in a 10% inaccuracy on the parallax (independently of the distance), which becomes larger than the statistical error on the parallax derived from the data reduction for stars that are up to about 4 kpc away. For the most nearby stars, we derive an inaccuracy on the parallax that can be 10 times its statistical error. Finally we estimate that up to about 4000 stars among red supergiants and bright giants may have astrometric parameters that are inaccurate at levels bigger than expected because of the surface brightness asymmetries. In the determination of this number, a crucial role is played by the Gaia observable magnitude range. The fact that Gaia will not observe stars brighter than 5.6 in the Gaia G band means that the closest stars will not be observed. Yet, the impact of the surface brightness asymmetries is proportional to their angular size, meaning that the stars whose astrometric accuracy w, Doctorat en Sciences, info:eu-repo/semantics/nonPublished

Published
2011

8. Chemically tagging the Hyades stream: does it partly originate from the Hyades cluster?

Author

Pompéia, L., Masseron, Thomas, Famaey, Benoît, Van Eck, Sophie, Jorissen, Alain, Minchev, I., Siebert, Arnaud, Sneden, C., Lépine, J.R.D., Siopis, Christos, Gentile, Gianfranco, Dermine, Tijl, Pasquato, Ester, Van Winckel, Hans, Waelkens, Ch, Raskin, Gert, Prins, S., Pessemier, W., Hensberge, Herman, Frémat, Yves, Dumortier, L., Bienaymé, Olivier, Pompéia, L., Masseron, Thomas, Famaey, Benoît, Van Eck, Sophie, Jorissen, Alain, Minchev, I., Siebert, Arnaud, Sneden, C., Lépine, J.R.D., Siopis, Christos, Gentile, Gianfranco, Dermine, Tijl, Pasquato, Ester, Van Winckel, Hans, Waelkens, Ch, Raskin, Gert, Prins, S., Pessemier, W., Hensberge, Herman, Frémat, Yves, Dumortier, L., and Bienaymé, Olivier

Abstract

The Hyades stream has long been thought to be a dispersed vestige of the Hyades cluster. However, recent analyses of the parallax distribution, of the mass function, and of the action-space distribution of stream stars have shown it to be rather composed of orbits trapped at a resonance of a density disturbance. This resonant scenario should leave a clearly different signature in the element abundances of stream stars than the dispersed cluster scenario, since the Hyades cluster is chemically homogeneous. Here, we study the metallicity as well as the element abundances of Li, Na, Mg, Fe, Zr, Ba, La, Ce, Nd and Eu for a random sample of stars belonging to the Hyades stream, and compare them with those of stars from the Hyades cluster. From this analysis: (i) we independently confirm that the Hyades stream cannot be solely composed of stars originating in the Hyades cluster; (ii) we show thatsomestars (namely 2/21) from the Hyades stream nevertheless have abundances compatible with an origin in the cluster; (iii) we emphasize that the use of Li as a chemical tag of the cluster origin of main-sequence stars is very efficient in the range 5500K ≤Teff≤ 6200K, since the Li sequence in the Hyades cluster is very tight, while at the same time spanning a large abundance range; (iv) we show that, while this evaporated population has a metallicity excess of ~0.2 dex with respect to the local thin-disc population, identical to that of the Hyades cluster, the remainder of the Hyades stream population has still a metallicity excess of ~0.06-0.15 dex, consistent with an origin in the inner Galaxy and (v) we show that the Hyades stream can be interpreted as an inner 4:1 resonance of the spiral pattern: this then also reproduces an orbital family compatible with the Sirius stream, and places the origin of the Hyades stream up to 1kpc inwards from the solar radius, which might explain the observed metallicity excess of the stream population. © 2011 The Authors Monthly Notices of the, SCOPUS: ar.j, info:eu-repo/semantics/published

Published
2011

9. Radiative hydrodynamic simulations of red supergiant stars. III. Spectro-photocentric variability, photometric variability, and consequences on Gaia measurements

Author

Chiavassa, Andréa, Pasquato, Ester, Jorissen, Alain, Sacuto, Stéphane, Babusiaux, Carine, Freytag, B., Ludwig, Hans Günter, Cruzalèbes, Pierre, Rabbia, Yves, Spang, A., Chesneau, Olivier, Chiavassa, Andréa, Pasquato, Ester, Jorissen, Alain, Sacuto, Stéphane, Babusiaux, Carine, Freytag, B., Ludwig, Hans Günter, Cruzalèbes, Pierre, Rabbia, Yves, Spang, A., and Chesneau, Olivier

Abstract

Context. It has been shown that convection in red supergiant stars (RSG) gives rise to large granules that cause surface inhomogeneities and shock waves in the photosphere. The resulting motion of the photocentre (on time scales ranging from months to years) could possibly have adverse effects on the parallax determination with Gaia. Aims. We explore the impact of the granulation on the photocentric and photometric variability. We quantify these effects in order to better characterise the error that could possibly alter the parallax. Methods. We use 3D radiative-hydrodynamics (RHD) simulations of convection with CO5BOLD and the post-processing radiative transfer code Optim3D to compute intensity maps and spectra in the Gaia G band [325-1030 nm]. Results. We provide astrometric and photometric predictions from 3D simulations of RSGs that are used to evaluate the possible degradation of the astrometric parameters of evolved stars derived by Gaia. We show in particular from RHD simulations that a supergiant like Betelgeuse exhibits a photocentric noise characterised by a standard deviation of the order of 0.1 AU. The number of bright giant and supergiant stars whose Gaia parallaxes will be altered by the photocentric noise ranges from a few tens to several thousands, depending on the poorly known relation between the size of the convective cells and the atmospheric pressure scale height of supergiants, and to a lower extent, on the adopted prescription for galactic extinction. In the worst situation, the degradation of the astrometric fit caused by this photocentric noise will be noticeable up to about 5 kpc for the brightest supergiants. Moreover, parallaxes of Betelgeuse-like supergiants are affected by an error of the order of a few percents. We also show that the photocentric noise, as predicted by the 3D simulation, does account for a substantial part of the supplementary "cosmic noise" that affects Hipparcos measurements of Betelgeuse and Antares. © 2011 ESO ., SCOPUS: ar.j, info:eu-repo/semantics/published

Published
2011

11. Interferometric Constraints on Surface Brightness Asymmetries in Long-Period Variable Stars. A Threat to Accurate Gaia Parallaxes

Author

Proceedings - Workshop "Why Galaxies Care About AGB Stars II" (16-20 August 2010: Vienna), Sacuto, Stéphane, Jorissen, Alain, Cruzalèbes, Pierre, Pasquato, Ester, Chiavassa, Andréa, Proceedings - Workshop "Why Galaxies Care About AGB Stars II" (16-20 August 2010: Vienna), Sacuto, Stéphane, Jorissen, Alain, Cruzalèbes, Pierre, Pasquato, Ester, and Chiavassa, Andréa

Abstract

0, info:eu-repo/semantics/nonPublished

Published
2010

12. Photocentric and photometric variability of Red Supergiant stars

Author

Proceedings-Workshop "Why galaxies care About AGB Stars II" (16-20 August 2010: Vienna), Chiavassa, Andréa, Pasquato, Ester, Jorissen, Alain, Proceedings-Workshop "Why galaxies care About AGB Stars II" (16-20 August 2010: Vienna), Chiavassa, Andréa, Pasquato, Ester, and Jorissen, Alain

Abstract

0, info:eu-repo/semantics/nonPublished

Published
2010

13. Three-dimensional hydrodynamical simulations of red giant stars: semi-global models for interpreting interferometric observations

Author

Chiavassa, Andréa, Pasquato, Ester, Jorissen, Alain, Sacuto, Stéphane, Babusiaux, Carine, Freytag, B., Ludwig, Hans Günter, Cruzalèbes, Pierre, Rabbia, Yves, Spang, A., Chesneau, Olivier, Chiavassa, Andréa, Pasquato, Ester, Jorissen, Alain, Sacuto, Stéphane, Babusiaux, Carine, Freytag, B., Ludwig, Hans Günter, Cruzalèbes, Pierre, Rabbia, Yves, Spang, A., and Chesneau, Olivier

Abstract

info:eu-repo/semantics/published

Published
2010

14. Photocentric variability of red supergiant stars and consequences on Gaia measurements

Author

Chiavassa, Andréa, Pasquato, Ester, Jorissen, Alain, Sacuto, Stéphane, Babusiaux, Carine, Freytag, B., Ludwig, Hans Günter, Cruzalèbes, Pierre, Rabbia, Yves, Spang, A., Chesneau, Olivier, Chiavassa, Andréa, Pasquato, Ester, Jorissen, Alain, Sacuto, Stéphane, Babusiaux, Carine, Freytag, B., Ludwig, Hans Günter, Cruzalèbes, Pierre, Rabbia, Yves, Spang, A., and Chesneau, Olivier

Abstract

info:eu-repo/semantics/published

Published
2010

15. Imaging simulations of selected science with the Magdalena Ridge Observatory Interferometer

Author

Chiavassa, Andréa, Pasquato, Ester, Jorissen, Alain, Sacuto, Stéphane, Babusiaux, Carine, Freytag, B., Ludwig, Hans Günter, Cruzalèbes, Pierre, Rabbia, Yves, Spang, A., Chesneau, Olivier, Chiavassa, Andréa, Pasquato, Ester, Jorissen, Alain, Sacuto, Stéphane, Babusiaux, Carine, Freytag, B., Ludwig, Hans Günter, Cruzalèbes, Pierre, Rabbia, Yves, Spang, A., and Chesneau, Olivier

Abstract

info:eu-repo/semantics/published

Published
2010

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