Search

Your search keyword '"Bonhomme, S."' showing total 234 results
Start Over Author "Bonhomme, S."
234 results on '"Bonhomme, S."'

1. Four winters of photometry with ASTEP South at Dome C, Antarctica

Author

Crouzet, N., Chapellier, E., Guillot, T., Mékarnia, D., Agabi, A., Fanteï-Caujolle, Y., Abe, L., Rivet, J. -P., Schmider, F. -X., Fressin, F., Bondoux, E., Challita, Z., Pouzenc, C., Valbousquet, F., Bayliss, D., Bonhomme, S., Daban, J. -B., Gouvret, C., and Blazit, A.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

Dome C in Antarctica is a promising site for photometric observations thanks to the continuous night during the Antarctic winter and favorable weather conditions. We developed instruments to assess the quality of this site for photometry in the visible and to detect and characterize variable objects through the Antarctic Search for Transiting ExoPlanets (ASTEP) project. We present the full analysis of four winters of data collected with ASTEP South, a 10 cm refractor pointing continuously toward the celestial south pole. We improved the instrument over the years and developed specific data reduction methods. We achieved nearly continuous observations over the winters. We measure an average sky background of 20 mag arcsec$^{-2}$ in the 579-642 nm bandpass. We built the lightcurves of 6000 stars and developed a model to infer the photometric quality of Dome C from the lightcurves themselves. The weather is photometric $67.1\pm4.2$ % of the time and veiled $21.8\pm2.0$ % of the time. The remaining time corresponds to poor quality data or winter storms. We analyzed the lightcurves of $\sigma$ Oct and HD 184465 and find that the amplitude of their main frequency varies by a factor of 3.5 and 6.7 over the four years, respectively. We also identify 34 new variable stars and eight new eclipsing binaries with periods ranging from 0.17 to 81 days. The phase coverage that we achieved with ASTEP South is exceptional for a ground-based instrument and the data quality enables the detection and study of variable objects. These results demonstrate the high quality of Dome C for photometry in the visible and for time series observations in general., Comment: 23 pages, 23 figures, A&A in press

Published
2018
Full Text
View/download PDF

3. Six winters of photometry from Dome C, Antarctica: challenges, improvements, and results from the ASTEP experiment

Author

Crouzet, N., Mékarnia, D., Guillot, T., Abe, L., Agabi, A., Rivet, J. -P., Gonçalves, I., Schmider, F. -X., Daban, J. -B., Fanteï-Caujolle, Y., Gouvret, C., Bayliss, D. D. R., Zhou, G., Aristidi, E., Fruth, T., Erikson, A., Rauer, H., Szulágyi, J., Bondoux, E., Challita, Z., Pouzenc, C., Fressin, F., Valbousquet, F., Barbieri, M., Blazit, A., Bonhomme, S., Bouchy, F., Gerakis, J., and Bouchez, G.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

ASTEP (Antarctica Search for Transiting ExoPlanets) is a pilot project that aims at searching and characterizing transiting exoplanets from Dome C in Antarctica and to qualify this site for photometry in the visible. Two instruments were installed at Dome C and ran for six winters in total. The analysis of the collected data is nearly complete. We present the operation of the instruments, and the technical challenges, limitations, and possible solutions in light of the data quality. The instruments performed continuous observations during the winters. Human interventions are required mainly for regular inspection and ice dust removal. A defrosting system is efficient at preventing and removing ice on the mirrors. The PSF FWHM is 4.5 arcsec on average which is 2.5 times larger than the specification, and is highly variable; the causes are the poor ground-level seeing, the turbulent plumes generated by the heating system, and to a lower extent the imperfect optical alignment and focusing, and some astigmatism. We propose solutions for each of these aspects that would largely increase the PSF stability. The astrometric and guiding precisions are satisfactory and would deserve only minor improvements. Major issues are encountered with the camera shutter which did not close properly after two winters; we minimized this issue by heating the shutter and by developing specific image calibration algorithms. Finally, we summarize the site testing and science results obtained with ASTEP. Overall, the ASTEP experiment will serve as a basis to design and operate future optical and near-infrared telescopes in Antarctica., Comment: 10 pages, 6 figures, SPIE conference proceedings, Ground-based and Airborne Instrumentation for Astronomy VI, 2016

Published
2016
Full Text
View/download PDF

5. The secondary eclipses of WASP-19b as seen by the ASTEP 400 telescope from Antarctica

Author

Abe, L., Gonçalves, I., Agabi, A., Alapini, A., Guillot, T., Mékarnia, D., Rivet, J. -P., Schmider, F. -X., Crouzet, N., Fortney, J., Pont, F., Barbieri, M., Daban, J. -B., Fanteï-Caujolle, Y., Gouvret, C., Bresson, Y., Roussel, A., Bonhomme, S., Robini, A., Dugué, M., Bondoux, E., Péron, S., Petit, P. -Y., Szulágyi, J., Fruth, T., Erikson, A., Rauer, H., Fressin, F., Valbousquet, F., Blanc, P. -E., van Suu, A. Le, and Aigrain, S.

Subjects
Astrophysics - Earth and Planetary Astrophysics
Abstract

The ASTEP (Antarctica Search for Transiting ExoPlanets) program was originally aimed at probing the quality of the Dome C, Antarctica for the discovery and characterization of exoplanets by photometry. In the first year of operation of the 40 cm ASTEP 400 telescope (austral winter 2010), we targeted the known transiting planet WASP-19b in order to try to detect its secondary transits in the visible. This is made possible by the excellent sub-millimagnitude precision of the binned data. The WASP-19 system was observed during 24 nights in May 2010. The photometric variability level due to starspots is about 1.8% (peak-to-peak), in line with the SuperWASP data from 2007 (1.4%) and larger than in 2008 (0.07%). We find a rotation period of WASP-19 of 10.7 +/- 0.5 days, in agreement with the SuperWASP determination of 10.5 +/- 0.2 days. Theoretical models show that this can only be explained if tidal dissipation in the star is weak, i.e. the tidal dissipation factor Q'star > 3.10^7. Separately, we find evidence for a secondary eclipse of depth 390 +/- 190 ppm with a 2.0 sigma significance, a phase consistent with a circular orbit and a 3% false positive probability. Given the wavelength range of the observations (420 to 950 nm), the secondary transit depth translates into a day side brightness temperature of 2690(-220/+150) K, in line with measurements in the z' and K bands. The day side emission observed in the visible could be due either to thermal emission of an extremely hot day side with very little redistribution of heat to the night side, or to direct reflection of stellar light with a maximum geometrical albedo Ag=0.27 +/- 0.13. We also report a low-frequency oscillation well in phase at the planet orbital period, but with a lower-limit amplitude that could not be attributed to the planet phase alone, and possibly contaminated with residual lightcurve trends., Comment: Accepted for publication in Astronomy and Astrophysics, 13 pages, 13 figures

Published
2013
Full Text
View/download PDF

6. ASTEP South: a first photometric analysis

Author

Crouzet, N., Guillot, T., Mékarnia, D., Szulágyi, J., Abe, L., Agabi, A., Fanteï-Caujolle, Y., Gonçalves, I., Barbieri, M., Schmider, F. -X., Rivet, J. -P., Bondoux, E., Challita, Z., Pouzenc, C., Fressin, F., Valbousquet, F., Blazit, A., Bonhomme, S., Daban, J. -B., Gouvret, C., Bayliss, D., Zhou, G., and team, the ASTEP

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Earth and Planetary Astrophysics
Abstract

The ASTEP project aims at detecting and characterizing transiting planets from Dome C, Antarctica, and qualifying this site for photometry in the visible. The first phase of the project, ASTEP South, is a fixed 10 cm diameter instrument pointing continuously towards the celestial South pole. Observations were made almost continuously during 4 winters, from 2008 to 2011. The point-to-point RMS of 1-day photometric lightcurves can be explained by a combination of expected statistical noises, dominated by the photon noise up to magnitude 14. This RMS is large, from 2.5 mmag at R=8 to 6% at R=14, because of the small size of ASTEP South and the short exposure time (30 s). Statistical noises should be considerably reduced using the large amount of collected data. A 9.9-day period eclipsing binary is detected, with a magnitude R=9.85. The 2-season lightcurve folded in phase and binned into 1000 points has a RMS of 1.09 mmag, for an expected photon noise of 0.29 mmag. The use of the 4 seasons of data with a better detrending algorithm should yield a sub-millimagnitude precision for this folded lightcurve. Radial velocity follow-up observations are conducted and reveal a F-M binary system. The detection of this 9.9-day period system with a small instrument such as ASTEP South and the precision of the folded lightcurve show the quality of Dome C for continuous photometric observations, and its potential for the detection of planets with orbital period longer than those usually detected from the ground., Comment: 5 pages, 3 figures, IAUS 288 conference proceedings

Published
2012
Full Text
View/download PDF

7. Direct constraint on the distance of y2 Velorum from AMBER/VLTI observations

Author

Millour, F., Petrov, R. G., Chesneau, O., Bonneau, D., Dessart, L., Bechet, C., Tallon-Bosc, I., Tallon, M., Thiébaut, E., Vakili, F., Malbet, F., Mourard, D., Zins, G., Roussel, A., Robbe-Dubois, S., Puget, P., Perraut, K., Lisi, F., Coarer, E. Le, Lagarde, S., Kern, P., Glück, L., Duvert, G., Chelli, A., Bresson, Y., Beckmann, U., Antonelli, P., Weigelt, G., Ventura, N., Vannier, M., Valtier, J. -C., Testi, L., Tatulli, E., Tasso, D., Stefanini, P., Stee, P., Solscheid, W., Schertl, D., Salinari, P., Sacchettini, M., Richichi, A., Reynaud, F., Rebattu, S., Rabbia, Y., Preibisch, T., Perrier, C., Pacini, F., Ohnaka, K., Nussbaum, E., Mouillet, D., Monin, J. -L., Mège, P., Mathias, P., Martinot-Lagarde, G., Mars, G., Marconi, A., Magnard, Y., Lopez, B., Contel, D. Le, Contel, J. -M. Le, Kraus, S., Kamm, D., Hofmann, K. -H., Utrera, O. Hernandez, Heininger, M., Heiden, M., Gil, C., Giani, E., Glentzlin, A., Gennari, S., Gallardo, A., Fraix-Burnet, D., Foy, R., Fossat, E., Forveille, T., Ferruzzi, D., Feautrier, P., Dugué, M., Driebe, T., De Souza, A. Domiciano, Delboulbé, A., Connot, C., Colin, J., Clausse, J. -M., Cassaing, F., Busoni, S., Bonhomme, S., Blöcker, T., Behrend, J., Baffa, C., Aristidi, E., Arezki, B., Agabi, K., Acke, B., Accardo, M., Kiekebusch, M., Rantakyrö, F., and Schoeller, Markus

Subjects
Astrophysics
Abstract

In this work, we present the first AMBER observations, of the Wolf-Rayet and O (WR+O) star binary system y2 Velorum. The AMBER instrument was used with the telescopes UT2, UT3, and UT4 on baselines ranging from 46m to 85m. It delivered spectrally dispersed visibilities, as well as differential and closure phases, with a resolution R = 1500 in the spectral band 1.95-2.17 micron. We interpret these data in the context of a binary system with unresolved components, neglecting in a first approximation the wind-wind collision zone flux contribution. We show that the AMBER observables result primarily from the contribution of the individual components of the WR+O binary system. We discuss several interpretations of the residuals, and speculate on the detection of an additional continuum component, originating from the free-free emission associated with the wind-wind collision zone (WWCZ), and contributing at most to the observed K-band flux at the 5% level. The expected absolute separation and position angle at the time of observations were 5.1±0.9mas and 66±15° respectively. However, we infer a separation of 3.62+0.11-0.30 mas and a position angle of 73+9-11°. Our analysis thus implies that the binary system lies at a distance of 368+38-13 pc, in agreement with recent spectrophotometric estimates, but significantly larger than the Hipparcos value of 258+41-31 pc.

Published
2006
Full Text
View/download PDF

8. First AMBER/VLTI observations of hot massive stars

Author

Petrov, R. G., Millour, F., Chesneau, O., Weigelt, G., Bonneau, D., Stee, Ph., Kraus, S., Mourard, D., Meilland, A., Malbet, F., Lisi, F., Kern, P., Beckmann, U., Lagarde, S., Gennari, S., Lecoarer, E., Driebe, Th., Accardo, M., Robbe-Dubois, S., Ohnaka, K., Busoni, S., Roussel, A., Zins, G., Behrend, J., Ferruzi, D., Bresson, Y., Duvert, G., Nussbaum, E., Marconi, A., Feautrier, Ph., Dugué, M., Chelli, A., Tatulli, E., Heininger, M., Delboulbé, A., Bonhomme, S., Schertl, D., Testi, L., Mathias, Ph., Monin, J. -L., Gluck, L., Hofmann, K. H., Salinari, P., Puget, P., Clausse, J. -M., Fraix-Burnet, D., Foy, R., and Isella, A.

Subjects
Astrophysics
Abstract

AMBER is the first near infrared focal instrument of the VLTI. It combines three telescopes and produces spectrally resolved interferometric measures. This paper discusses some preliminary results of the first scientific observations of AMBER with three Unit Telescopes at medium (1500) and high (12000) spectral resolution. We derive a first set of constraints on the structure of the circumstellar material around the Wolf Rayet Gamma2 Velorum and the LBV Eta Carinae.

Published
2005
Full Text
View/download PDF

13. Developmental Regulation of Co-suppression In Petunia hybrida

Author

Flavell, R. B., O’Dell, M., Metzlaff, M., Bonhomme, S., Cluster, P. D., Capron, A., editor, Compans, R. W., editor, Cooper, M., editor, Koprowski, H., editor, McConnell, I., editor, Melchers, F., editor, Oldstone, M., editor, Olsnes, S., editor, Potter, M., editor, Saedler, H., editor, Vogt, P. K., editor, Wagner, H., editor, Wilson, I., editor, and Meyer, Peter, editor

Published
1995
Full Text
View/download PDF

21. Four winters of photometry with ASTEP South at Dome C, Antarctica

Author

Crouzet, N., primary, Chapellier, E., additional, Guillot, T., additional, Mékarnia, D., additional, Agabi, A., additional, Fanteï-Caujolle, Y., additional, Abe, L., additional, Rivet, J.-P., additional, Schmider, F.-X., additional, Fressin, F., additional, Bondoux, E., additional, Challita, Z., additional, Pouzenc, C., additional, Valbousquet, F., additional, Bayliss, D., additional, Bonhomme, S., additional, Daban, J.-B., additional, Gouvret, C., additional, and Blazit, A., additional

Published
2018
Full Text
View/download PDF

22. Non-parametric estimation of finite mixtures from repeated measurements

Author

Bonhomme, S, Jochmans, K, Robin, JM, Jochmans, Koen [0000-0002-3090-3003], and Apollo - University of Cambridge Repository

Subjects
Finite mixture, Reweighting, Two-step estimation, Repeated measurement data
Abstract

Summary This paper provides methods to estimate finite mixtures from data with repeated measurements non-parametrically. We present a constructive identification argument and use it to develop simple two-step estimators of the component distributions and all their functionals. We discuss a computationally efficient method for estimation and derive asymptotic theory. Simulation experiments suggest that our theory provides confidence intervals with good coverage in small samples.

Published
2016

31. Six winters of photometry from Dome C, Antarctica: challenges, improvements, and results from the ASTEP experiment

Author

Crouzet, N., additional, Mékarnia, D., additional, Guillot, T., additional, Abe, L., additional, Agabi, A., additional, Rivet, J.-P., additional, Gonçalves, I., additional, Schmider, F.-X., additional, Daban, J.-B., additional, Fanteï-Caujolle, Y., additional, Gouvret, C., additional, Bayliss, D. D. R., additional, Zhou, G., additional, Aristidi, E., additional, Fruth, T., additional, Erikson, A., additional, Rauer, H., additional, Szulágyi, J., additional, Bondoux, E., additional, Challita, Z., additional, Pouzenc, C., additional, Fressin, F., additional, Valbousquet, F., additional, Barbieri, M., additional, Blazit, A., additional, Bonhomme, S., additional, Bouchy, F., additional, Gerakis, J., additional, and Bouchez, G., additional

Published
2016
Full Text
View/download PDF

38. Generalized non-parametric deconvolution with an application to earnings dynamics

Author

Bonhomme, S. and Robin, J. -M

Abstract

In this paper, we construct a non-parametric estimator of the distributions of latent factors in linear independent multi-factor models under the assumption that factor loadings are known. Our approach allows estimation of the distributions of up to L(L+ 1)/2 factors given L measurements. The estimator uses empirical characteristic functions, like many available deconvolution estimators. We show that it is consistent, and derive asymptotic convergence rates. Monte Carlo simulations show good finite-sample performance, less so if distributions are highly skewed or leptokurtic. We finally apply the generalized deconvolution procedure to decompose individual log earnings from the panel study of income dynamics (PSID) into permanent and transitory components.

Published
2010

41. Une thrombose veineuse hyperalgique

Author

Fourgeaud, C., primary, Benzimra, M., additional, Michon Pasturel, U., additional, Bonhomme, S., additional, Marteau, V., additional, Daneshvar, M., additional, Soury, P., additional, and Priollet, P., additional

Published
2015
Full Text
View/download PDF

42. An asymmetry detected in the disk of Kappa CMa with the AMBER/VLTI

Author

Meilland, Anthony, Millour, Florentin, Stee, Philippe, Domiciano De Souza, Armando, Petrov, Romain, Mourard, Denis, Jankov, Slobodan, Robbe-Dubois, Sylvie, Spang, Alain, Arisitidi, Eric, Antonelli, P., Beckmann, U., Bresson, Y., Chelli, A., Dugué, M., Duvert, G., Glück, L., Kern, P., Lagarde, S., Le Coarer, E., Lisi, F., Malbet, F., Perraut, K., Puget, P., Robbe-Dubois, S., Weigelt, G., Zins, G., Accardo, M., Acke, B., Agabi, K., Arezki, B., Altariba, E., Baffa, C., Behrend, J., Blöcker, T., Bonhomme, S., Busoni, S., Cassaing, F., Clausse, J.-M., Connot, C., Delboulbé, A., Domicinano De Souza, A., Driebe, T., Feautrier, P., Ferruzzi, D., Forveille, T., Fossat, E., Foy, R., Fraix-Burnet, D., Gallardo, A., Gennari, S., Glentzlin, A., Giani, E., Gilinst, C., Heiden, M., Heininger, M., Hernandez, O., Hofmann, K.-H., Kamm, D., Kraus, S., Le Contel, D., Le Contel, J.-M., Lopez, B., Magnard, Y., Marconi, A., Mars, G., Martinot-Lagarde, G., Mathias, P., Millour, F., Monin, J.-L., Mouillet, D., Mourard, D., Mège, P., Nussbaum, E., Ohnaka, K., Pacini, F., Perrier, C., Rabbia, Y., Rebattu, S., Reynaud, F., Richichi, A., Roussel, A., Sacchettini, M., Salinari, P., Schertl, D., Solscheid, W., Stee, P., Stefanini, P., Tallon, M., Tallon-Bosc, I., Tasso, D., Tatulli, E., Testi, L., Valtier, J.-C., Vannier, M., Ventura, N., Kiekebusch, M., Schöller, M., Laboratoire Gemini (LG), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Universitaire d'Astrophysique de Nice (LUAN), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Centre National de la Recherche Scientifique (CNRS), and COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
[SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Stars: emission-line, Astrophysics (astro-ph), Stars: individual (kappa CMa), FOS: Physical sciences, Be, Astrophysics, Techniques: high angular resolution, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Stars: Keplerian rotation, Techniques: interferometric, Stars: circumstellar matter, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

International audience; Aims. We study the geometry and kinematics of the circumstellar environment of the Be star Kappa CMa in the Br gamma emission line and its nearby continuum. Methods. We use the VLTI/AMBER instrument operating in the K band which provides a spatial resolution of about 6 mas with a spectral resolution of 1500 to study the kinematics within the disk and to infer its rotation law. In order to obtain more kinematical constraints we also use an high spectral resolution Pa beta line profile obtain in December 2005 at the Observatorio do Pico do Dios, Brazil and we compile V/R line profile variations and spectral energy distribution data points from the literature. Results. Using differential visibilities and differential phases across the Br gamma line we detect an asymmetry in the disk. Moreover, we found that kappa CMa seems difficult to fit within the classical scenario for Be stars, illustrated recently by alpha Arae observations, i.e. a fast rotating B star close to its breakup velocity surrounded by a Keplerian circumstellar disk with an enhanced polar wind. Finally we discuss the possibility for kappa CMa to be a critical rotator with a Keplerian rotating disk and try to see if the detected asymmetry can be interpreted within the "one-armed" viscous disk framework.

Published
2006
Full Text
View/download PDF

43. First AMBER/VLTI Observations of Hot Massive Stars

Author

Romain Petrov, Millour, F., Chesneau, O., Weigelt, G., Bonneau, D., Ph. Stee, Kraus, S., Mourard, D., Meilland, A., Vannier, M., Malbet, F., Lisi, F., Antonelli, P., Kern, P., Beckmann, U., Lagarde, S., Perraut, K., Gennari, S., Le Coarer, E., Th. Driebe, Accardo, M., Robbe-Dubois, S., Ohnaka, K., Busoni, S., Roussel, A., Zins, G., Behrend, J., Ferruzi, D., Bresson, Y., Duvert, G., Nussbaum, E., Marconi, A., Ph. Feautrier, Dugué, M., Chelli, A., Tatulli, E., Heininger, M., Delboulbe, A., Bonhomme, S., Schertl, D., Testi, L., Ph. Mathias, L Monin, J., Gluck, L., Hofmann, K. H., Salinari, P., Puget, P., Clausse, J. M., Didier Fraix-Burnet, D., Renaud Foy, Isella, A., Laboratoire Universitaire d'Astrophysique de Nice (LUAN), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Astronomie (MPIA), Max-Planck-Gesellschaft, Laboratoire Gemini (LG), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Radioastronomie (MPIFR), European Southern Observatory (ESO), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), Centre de Recherche Astrophysique de Lyon (CRAL), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Université Nice Sophia Antipolis (1965 - 2019) (UNS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)

Subjects
[PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

8 pages; International audience; AMBER is the first near infrared focal instrument of the VLTI. It combines three telescopes and produces spectrally resolved interferometric measures. This paper discusses some preliminary results of the first scientific observations of AMBER with three Unit Telescopes at medium (1500) and high (12000) spectral resolution. We derive a first set of constraints on the structure of the circumstellar material around the Wolf Rayet gamma2 Velorum and the LBV eta Carinae.

Published
2005

44. Disk and wind interaction in the young stellar object MWC 297 spatially resolved with VLTI/AMBER

Author

Malbet, F., Benisty, M., de Wit, W.J., Kraus, S., Meilland, A., Millour, F., Tatulli, E., Berger, J.P., Chesneau, O., Hofmann, K.H., Isella, A., Natta, A., Petrov, R., Preibisch, T., Stee, P., Testi, L., Weigelt, G., Antonelli, P., Beckmann, U., Bresson, Y., Chelli, A., Duvert, G., Glück, L., Kern, P., Lagarde, S., Le Coarer, E., Lisi, F., Perraut, K., Robbe-Dubois, S., Roussel, A., Zins, G., Accardo, M., Acke, B., Agabi, K., Arezki, B., Aristidi, E., Baffa, C., Behrend, J., Blöcker, T., Bonhomme, S., Busoni, S., Cassaing, F., Clausse, J.-M., Colin, J., Connot, C., Delboulbé, A., Driebe, T., Dugué, M., Feautrier, P., Ferruzzi, D., Forveille, T., Fossat, E., Foy, Renaud, Fraix-Burnet, D., Gallardo, A., Gennari, S., Glentzlin, A., Giani, E., Gil, C., Heiden, M., Heininger, M., Kamm, D., Le Contel, D., Le Contel, J.-M., Lopez, B., Magnard, Y., Marconi, A., Mars, G., Martinot-Lagarde, G., Mathias, P., Monin, J.-L., Mouillet, D., Mourard, D., Mège, P., Nussbaum, E., Ohnaka, K., Pacheco, J., Pacini, F., Perrier, C., Puget, P., Rabbia, Y., Rebattu, S., Reynaud, François, Richichi, A., Sacchettini, M., Salinari, P., Schertl, D., Solscheid, W., Stefanini, P., Tallon, Michel, Tallon-Bosc, Isabelle, Tasso, D., Valtier, J.-C., Vannier, M., Ventura, N., Kiekebusch, M., Rantakyrö, F., Schöller, M., Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Max-Planck-Institut für Radioastronomie (MPIFR), Laboratoire Gemini (LG), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de la Côte d'Azur, Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Universitaire d'Astrophysique de Nice (LUAN), Université Nice Sophia Antipolis (... - 2019) (UNS), Université Côte d'Azur (UCA)-Université Côte d'Azur (UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), INAF - Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), ONERA - The French Aerospace Lab [Châtillon], ONERA, Centre de Recherche Astrophysique de Lyon (CRAL), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-École normale supérieure - Lyon (ENS Lyon), Division technique INSU/SDU (DTI), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), PHOTONIQUE, XLIM (XLIM), Université de Limoges (UNILIM)-Centre National de la Recherche Scientifique (CNRS)-Université de Limoges (UNILIM)-Centre National de la Recherche Scientifique (CNRS), European Southern Observatory (ESO), AMBER, Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Centre National de la Recherche Scientifique (CNRS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), ONERA-Université Paris Saclay (COmUE), École normale supérieure - Lyon (ENS Lyon)-Université Claude Bernard Lyon 1 (UCBL), Université de Lyon-Université de Lyon-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS), COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-COMUE Université Côte d'Azur (2015-2019) (COMUE UCA)-Université Côte d'Azur (UCA)-Centre National de la Recherche Scientifique (CNRS), Université Nice Sophia Antipolis (1965 - 2019) (UNS), École normale supérieure de Lyon (ENS de Lyon)-Université Claude Bernard Lyon 1 (UCBL), and Université de Lyon-Université de Lyon-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Protoplanetary disks, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics::High Energy Astrophysical Phenomena, Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, Pre-main-sequence stars, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Planetary systems, Early-type stars, Emission-line stars, Accretion disks, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, Infrared, Interferometric Techniques, Astrophysics::Galaxy Astrophysics
Abstract

The young stellar object MWC 297 has been observed with the VLT interferometer equipped with the AMBER instrument. MWC 297 has been spatially resolved in the continuum with a visibility of 0.50 as well as in the Br gamma emission line where the visibility decrease to a lower value of 0.33. This change in the visibility with the wavelength can be interpreted by the presence of an optically thick disk responsible for the visibility in the continuum and of a stellar wind traced by Br gamma and whose apparent size is 40% larger. We validate this interpretation by building a model of the stellar environment that combines a geometrically thin, optically thick accretion disk model consisting of gas and dust, and a latitude-dependent stellar wind outflowing above the disk surface. The continuum emission and visibilities obtained from this model are fully consistent with the interferometric AMBER data. They agree also with existing optical, near-infrared spectra and other broad-band near-infrared interferometric visibilities. A picture emerges in which MWC 297 is surrounded by an equatorial flat disk that is possibly still accreting and an outflowing wind which has a much higher velocity in the polar region than at the equator. [abridged], Comment: 13 pages; to be published in A&A; Acceptance day: 11/10/2005

Published
2005
Full Text
View/download PDF

45. First AMBER/VLTI Observations of Hot Massive Stars

Author

Petrov, R. G., primary, Millour, F., additional, Chesneau, O., additional, Weigelt, G., additional, Bonneau, D., additional, Stee, Ph., additional, Kraus, S., additional, Mourard, D., additional, Meilland, A., additional, Vannier, M., additional, Malbet, F., additional, Lisi, F., additional, Antonelli, P., additional, Kern, P., additional, Beckmann, U., additional, Lagarde, S., additional, Perraut, K., additional, Gennari, S., additional, Coarer, E. Le, additional, Driebe, Th., additional, Accardo, M., additional, Robbe-Dubois, S., additional, Ohnaka, K., additional, Busoni, S., additional, Roussel, A., additional, Zins, G., additional, Behrend, J., additional, Ferruzi, D., additional, Bresson, Y., additional, Duvert, G., additional, Nussbaum, E., additional, Marconi, A., additional, Feautrier, Ph., additional, Dugué, M., additional, Chelli, A., additional, Tatulli, E., additional, Heininger, M., additional, Delboulbe, A., additional, Bonhomme, S., additional, Schertl, D., additional, Testi, L., additional, Mathias, Ph., additional, Monin, J. -L., additional, Gluck, L., additional, Hofmann, K. H., additional, Salinari, P., additional, Puget, P., additional, Clausse, J. M., additional, Fraix-Burnet, D., additional, Foy, R., additional, and Isella, A., additional

Full Text
View/download PDF

46. MATISSE status report and science forecast

Author

Lopez, B., additional, Lagarde, S., additional, Jaffe, W., additional, Petrov, R., additional, Schöller, M., additional, Antonelli, P., additional, Beckman, U., additional, Bério, Ph., additional, Bettonvil, F., additional, Graser, U., additional, Millour, F., additional, Robbe-Dubois, S., additional, Venema, L., additional, Wolf, S., additional, Bristow, P., additional, Glindemann, A., additional, Gonzalez, J.-C., additional, Lanz, Th., additional, Henning, T., additional, Weigelt, G., additional, Agócs, T., additional, Augereau, J.-C., additional, Ávila, G., additional, Bailet, C., additional, Behrend, J., additional, Berger, J.-P., additional, von Boekel, Roy, additional, Bonhomme, S., additional, Bourget, P., additional, Brast, R., additional, Bresson, Y., additional, Clausse, J. M., additional, Chesneau, O., additional, Csépány, G., additional, Connot, C., additional, Crida, A., additional, Danchi, W. C., additional, Delbo, M., additional, Delplancke, F., additional, Dominik, C., additional, Dugué, M., additional, Elswijk, E., additional, Fanteï, Y., additional, Finger, G., additional, Gabasch, A., additional, Girard, P., additional, Girault, V., additional, Gitton, P., additional, Glazenborg, A., additional, Gonté, F., additional, Guitton, F., additional, Guniat, S., additional, De Haan, M., additional, Haguenauer, P., additional, Hanenburg, H., additional, Heininger, M., additional, Hofmann, K.-H., additional, Hogerheijde, M., additional, ter Horst, R., additional, Hron, J., additional, Hughes, Y., additional, Ives, D., additional, Jakob, G., additional, Jaskó, A., additional, Jolley, P., additional, Kragt, J., additional, Köhler, R., additional, Kroener, T., additional, Kroes, G., additional, Labadie, L., additional, Laun, W., additional, Lehmitz, M., additional, Leinert, Ch., additional, Lizon, J. L., additional, Lucuix, Ch., additional, Marcotto, A., additional, Martinache, F., additional, Matter, A., additional, Martinot-Lagarde, G., additional, Mauclert, N., additional, Mehrgan, L., additional, Meilland, A., additional, Mellein, M., additional, Ménardi, S., additional, Menut, J. L., additional, Meisenheimer, K., additional, Morel, S., additional, Mosoni, L., additional, Navarro, R., additional, Neumann, U., additional, Nussbaum, E., additional, Ottogalli, S., additional, Palsa, R., additional, Panduro, J., additional, Pantin, E., additional, Percheron, I., additional, Duc, T. Phan, additional, Pott, J.-U., additional, Pozna, Eszter, additional, Przygodda, F., additional, Richichi, A., additional, Rigal, F., additional, Rupprecht, G., additional, Schertl, D., additional, Stegmeier, J., additional, Thiam, L., additional, Tromp, N., additional, Vannier, M., additional, Vakili, F., additional, van Belle, G., additional, Wagner, K., additional, and Woillez, J., additional

Published
2014
Full Text
View/download PDF

Catalog

Books, media, physical & digital resources
See catalog results