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19 results on '"Lanoux, J."'

1. A Bcool magnetic snapshot survey of solar-type stars

Author

Marsden, S. C., Petit, P., Jeffers, S. V., Morin, J., Fares, R., Reiners, A., Nascimento Jr., J. D. do, Auriere, M., Bouvier, J., Carter, B. D., Catala, C., Dintrans, B., Donati, J. -F., Gastine, T., Jardine, M., Konstantinova-Antova, R., Lanoux, J., Lignieres, F., Morgenthaler, A., Ramirez-Velez, J. C., Theado, S., Van Grootel, V., and Collaboration, the Bcool

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

Stellar magnetic field measurements obtained from spectropolarimetry offer key data for activity and dynamo studies, and we present the results of a major high-resolution spectropolarimetric Bcool project magnetic snapshot survey of 170 solar-type stars from observations with the Telescope Bernard Lyot and the Canada-France-Hawaii Telescope. For each target star a high signal-to-noise circularly polarised Stokes V profile has been obtained using Least-Squares Deconvolution, and used to detect surface magnetic fields and measure the corresponding mean surface longitudinal magnetic field ($B_{l}$). Chromospheric activity indicators were also measured. Surface magnetic fields were detected for 67 stars, with 21 of these stars classified as mature solar-type stars, a result that increases by a factor of four the number of mature solar-type stars on which magnetic fields have been observed. In addition, a magnetic field was detected for 3 out of 18 of the subgiant stars surveyed. For the population of K-dwarfs the mean value of $B_{l}$ ($|B_{l}|_{mean}$) was also found to be higher (5.7 G) than $|B_{l}|_{mean}$ measured for the G-dwarfs (3.2 G) and the F-dwarfs (3.3 G). For the sample as a whole $|B_{l}|_{mean}$ increases with rotation rate and decreases with age, and the upper envelope for $|B_{l}|$ correlates well with the observed chromospheric emission. Stars with a chromospheric S-index greater than about 0.2 show a high magnetic field detection rate and so offer optimal targets for future studies. This survey constitutes the most extensive spectropolarimetric survey of cool stars undertaken to date, and suggests that it is feasible to pursue magnetic mapping of a wide range of moderately active solar-type stars to improve understanding of their surface fields and dynamos., Comment: 36 pages, 26 figures, 7 tables, submitted to MNRAS

Published
2013
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2. Long-term magnetic field monitoring of the Sun-like star \xi Bootis A

Author

Morgenthaler, A., Petit, P., Saar, S., Solanki, S. K., Morin, J., Marsden, S. C., Auriere, M., Dintrans, B., Fares, R., Gastine, T., Lanoux, J., Lignieres, F., Paletou, F., Velez, J. C. Ramirez, Theado, S., and Van Grootel, V.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

Aims. We aim to investigate the long-term temporal evolution of the magnetic field of the solar-type star \xi Bootis A, both from direct magnetic field measurements and from the simultaneous estimate of indirect activity indicators. Methods. We obtained seven epochs of high-resolution, circularly-polarized spectra from the NARVAL spectropolarimeter between 2007 and 2011, for a total of 76 spectra. Using approximately 6,100 photospheric spectral lines covering the visible domain, we employed a cross-correlation procedure to compute a mean polarized line profile from each spectrum. The large-scale photospheric magnetic field of the star was then modelled by means of Zeeman-Doppler Imaging, allowing us to follow the year-to-year evolution of the reconstructed magnetic topology. Simultaneously, we monitored the width of several magnetically sensitive spectral lines, the radial velocity, the line asymmetry of intensity line profiles, and the chromospheric emission in the cores of the Ca II H and Halpha lines. Results. During the highest observed activity states, in 2007 and 2011, the large-scale field of \xi Boo A is almost completely axisymmetric and is dominated by its toroidal component. The magnetic topologies reconstructed for these activity maxima are very similar, suggesting a form of short cyclicity in the large-scale field distribution. Correlated temporal evolution, due to both rotational modulation and seasonal variability, is observed between the Ca II emission, the Halpha emission and the width of magnetically sensitive lines. When measurable, the differential rotation reveals a strong latitudinal shear in excess of 0.2 rad/d., Comment: 16 pages, 8 figures, accepted for publication in A&A, abstract shortened to respect the 1920 characters required

Published
2011
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3. A statistical investigation of the radio emission of clusters : role of AGNs

Author

Lanoux, J., Pointecouteau, E., and Giard, M.

Subjects
Astrophysics - Cosmology and Extragalactic Astrophysics
Abstract

Radio emission in the direction of galaxy clusters is due to the individual emission of AGNs, and to the diffuse non-thermal emission of the intracluster medium (ICM). The population of AGNs in clusters is correlated to the overall halo properties, and likely impacts their evolutions. In order to better understand this connection (which will also leads to constraints on the non-thermal ICMemission for lower mass systems), we are conducting a statistical analysis of the radio emission in the direction of a large number of X-ray clusters. By means of their stacked radio emission, we are investigating the radio luminosities in clusters of galaxies with respect to their mass, with the goal to better understand their link to and their imprint on the intra-cluster gas physics., Comment: 2 pages, 2 figures, to appear in proceedings of the conference "Non-thermal phenomena in colliding galaxy clusters" (Nice, France, Nov 2010)

Published
2011

4. Planck Early Results XI: Calibration of the local galaxy cluster Sunyaev-Zeldovich scaling relations

Author

Planck Collaboration, Ade, P. A. R., Aghanim, N., Arnaud, M., Ashdown, M., Aumont, J., Baccigalupi, C., Balbi, A., Banday, A. J., Barreiro, R. B., Bartelmann, M., Bartlett, J. G., Battaner, E., Benabed, K., Benoît, A., Bernard, J. -P., Bersanelli, M., Bhatia, R., Bock, J. J., Bonaldi, A., Bond, J. R., Borrill, J., Bouchet, F. R., Bourdin, H., Brown, M. L., Bucher, M., Burigana, C., Cabella, P., Cardoso, J. -F., Catalano, A., Cayón, L., Challinor, A., Chamballu, A., Chiang, L. -Y, Chiang, C., Chon, G., Christensen, P. R., Churazov, E., Clements, D. L., Colafrancesco, S., Colombi, S., Couchot, F., Coulais, A., Crill, B. P., Cuttaia, F., Da Silva, A., Dahle, H., Danese, L., de Bernardis, P., de Gasperis, G., de Rosa, A., de Zotti, G., Delabrouille, J., Delouis, J. -M., Désert, F. -X., Diego, J. M., Dolag, K., Donzelli, S., Doré, O., Dörl, U., Douspis, M., Dupac, X., Efstathiou, G., Enßlin, T. A., Finelli, F., Flores, I., Forni, O., Frailis, M., Franceschi, E., Fromenteau, S., Galeotta, S., Ganga, K., Génova-Santos, R. T., Giard, M., Giardino, G., Giraud-Héraud, Y., González-Nuevo, J., Górski, K. M., Gratton, S., Gregorio, A., Gruppuso, A., Harrison, D., Henrot-Versillé, S., Hernández-Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hovest, W., Hoyland, R. J., Huffenberger, K. M., Jaffe, A. H., Jones, W. C., Juvela, M., Keihänen, E., Keskitalo, R., Kisner, T. S., Kneissl, R., Knox, L., Kurki-Suonio, H., Lagache, G., Lamarre, J. -M., Lanoux, J., Lasenby, A., Laureijs, R. J., Lawrence, C. R., Leach, S., Leonardi, R., Liddle, A., Lilje, P. B., Linden-Vørnle, M., López-Caniego, M., Lubin, P. M., Macías-Pérez, J. F., MacTavish, C. J., Maffei, B., Maino, D., Mandolesi, N., Mann, R., Maris, M., Marleau, F., Martínez-González, E., Masi, S., Matarrese, S., Matthai, F., Mazzotta, P., Melchiorri, A., Melin, J. -B., Mendes, L., Mennella, A., Mitra, S., Miville-Deschênes, M. -A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, A., Naselsky, P., Natoli, P., Netterfield, C. B., Nørgaard-Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., Osborne, S., Pajot, F., Pasian, F., Patanchon, G., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Pierpaoli, E., Piffaretti, R., Plaszczynski, S., Pointecouteau, E., Polenta, G., Ponthieu, N., Poutanen, T., Pratt, G. W., Prézeau, G., Prunet, S., Puget, J. -L., Rachen, J. P., Rebolo, R., Reinecke, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Rubiño-Martín, J. A., Rusholme, B., Sandri, M., Santos, D., Savini, G., Schaefer, B. M., Scott, D., Seiffert, M. D., Shellard, P., Smoot, G. F., Starck, J. -L., Stivoli, F., Stolyarov, V., Sudiwala, R., Sunyaev, R., Sygnet, J. -F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Torre, J. -P., Tristram, M., Tuovinen, J., Valenziano, L., Vibert, L., Vielva, P., Villa, F., Vittorio, N., Wade, L. A., Wandelt, B. D., White, S. D. M., White, M., Yvon, D., Zacchei, A., and Zonca, A.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present precise Sunyaev-Zeldovich (SZ) effect measurements in the direction of 62 nearby galaxy clusters (z <0.5) detected at high signal-to-noise in the first Planck all-sky dataset. The sample spans approximately a decade in total mass, 10^14 < M_500 < 10^15, where M_500 is the mass corresponding to a total density contrast of 500. Combining these high quality Planck measurements with deep XMM-Newton X-ray data, we investigate the relations between D_A^2 Y_500, the integrated Compton parameter due to the SZ effect, and the X-ray-derived gas mass M_g,500, temperature T_X, luminosity L_X, SZ signal analogue Y_X,500 = M_g,500 * T_X, and total mass M_500. After correction for the effect of selection bias on the scaling relations, we find results that are in excellent agreement with both X-ray predictions and recently-published ground-based data derived from smaller samples. The present data yield an exceptionally robust, high-quality local reference, and illustrate Planck's unique capabilities for all-sky statistical studies of galaxy clusters., Comment: 14 pages, 6 figures, to appear in A&A; final version corrects values for A1413 and A3921 in Table 1

Published
2011
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5. Long-term magnetic field monitoring of the Sun-like star Ksi Bootis A

Author

Morgenthaler, A., Petit, P., Auriere, M., Dintrans, B., Fares, R., Gastine, T., Lanoux, J., Lignieres, F., Morin, J., Ramirez, J., Saar, S., Solanki, S. K., Theado, S., and Van Grootel, V.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

Phase-resolved observations of the solar-type star Ksi Bootis A were obtained using the NARVAL spectropolarimeter at the Telescope Bernard Lyot (Pic du Midi, France) during years 2007, 2008, 2009 and 2010. The data sets enable us to study both the rotational modulation and the long-term evolution of various magnetic and activity tracers. Here, we focus on the large-scale photospheric magnetic field (reconstructed by Zeeman-Doppler Imaging), the Zeeman broadening of the FeI 846.84 nm magnetic line, and the chromospheric CaII H and H alpha emission., Comment: 6 pages, 4 figures, Cool Stars 16 proceeding

Published
2010

6. Exploring the magnetic topologies of cool stars

Author

Morin, J., Donati, J. -F., Petit, P., Albert, L., Auriere, M., Cabanac, R., Catala, C., Delfosse, X., Dintrans, B., Fares, R., Forveille, T., Gastine, T., Jardine, M., Konstantinova-Antova, R., Lanoux, J., Lignieres, F., Morgenthaler, A., Paletou, F., Velez, J. C. Ramirez, Solanki, S. K., Theado, S., and Van Grootel, V.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

Magnetic fields of cool stars can be directly investigated through the study of the Zeeman effect on photospheric spectral lines using several approaches. With spectroscopic measurement in unpolarised light, the total magnetic flux averaged over the stellar disc can be derived but very little information on the field geometry is available. Spectropolarimetry provides a complementary information on the large-scale component of the magnetic topology. With Zeeman-Doppler Imaging (ZDI), this information can be retrieved to produce a map of the vector magnetic field at the surface of the star, and in particular to assess the relative importance of the poloidal and toroidal components as well as the degree of axisymmetry of the field distribution. The development of high-performance spectropolarimeters associated with multi-lines techniques and ZDI allows us to explore magnetic topologies throughout the Hertzsprung-Russel diagram, on stars spanning a wide range of mass, age and rotation period. These observations bring novel constraints on magnetic field generation by dynamo effect in cool stars. In particular, the study of solar twins brings new insight on the impact of rotation on the solar dynamo, whereas the detection of strong and stable dipolar magnetic fields on fully convective stars questions the precise role of the tachocline in this process., Comment: 6 pages, 2 figures, IAU Symposium 273 "Physics of Sun and Star Spots", 22-26 August 2010

Published
2010
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7. The rapid rotation and complex magnetic field geometry of Vega

Author

Petit, P., Lignières, F., Wade, G. A., Aurière, M., Böhm, T., Bagnulo, S., Dintrans, B., Fumel, A., Grunhut, J., Lanoux, J., Morgenthaler, A., and Van Grootel, V.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

The recent discovery of a weak surface magnetic field on the normal intermediate-mass star Vega raises the question of the origin of this magnetism in a class of stars that was not known to host magnetic fields. We aim to confirm the field detection and provide additional observational constraints about the field characteristics, by modelling the magnetic geometry of the star and by investigating the seasonal variability of the reconstructed field. We analyse a total of 799 circularly-polarized spectra collected with the NARVAL and ESPaDOnS spectropolarimeters during 2008 and 2009. We employ a cross-correlation procedure to compute, from each spectrum, a mean polarized line profile with a signal-to-noise ratio of about 20,000. The technique of Zeeman-Doppler Imaging is then used to determine the rotation period of the star and reconstruct the large-scale magnetic geometry of Vega at two different epochs. We confirm the detection of circularly polarized signatures in the mean line profiles. The amplitude of the signatures is larger when spectral lines of higher magnetic sensitivity are selected for the analysis, as expected for a signal of magnetic origin. The short-term evolution of polarized signatures is consistent with a rotational period of 0.732 \pm 0.008 d. The reconstructed magnetic topology unveils a magnetic region of radial field orientation, closely concentrated around the rotation pole. This polar feature is accompanied by a small number of magnetic patches at lower latitudes. No significant variability in the field structure is observed over a time span of one year. The repeated observation of a weak photospheric magnetic field on Vega suggests that a previously unknown type of magnetic stars exists in the intermediate-mass domain. Vega may well be the first confirmed member of a much larger, as yet unexplored, class of weakly-magnetic stars., Comment: Accepted by Astronomy & Astrophysics. Abstract shortened to respect the arXiv limit of 1920 characters

Published
2010
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8. A polarity reversal in the large-scale magnetic field of the rapidly rotating Sun HD 190771

Author

Petit, P., Dintrans, B., Morgenthaler, A., Van Grootel, V., Morin, J., Lanoux, J., Auriere, M., and Konstantinova-Antova, R.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

Aims. We investigate the long-term evolution of the large-scale photospheric magnetic field geometry of the solar-type star HD 190771. With fundamental parameters very close to those of the Sun except for a shorter rotation period of 8.8 d, HD 190771 provides us with a first insight into the specific impact of the rotation rate in the dynamo generation of magnetic fields in 1 $M_\odot$ stars. Methods. We use circularly polarized, high-resolution spectra obtained with the NARVAL spectropolarimeter (Observatoire du Pic du Midi, France) and compute cross-correlation line profiles with high signal-to-noise ratio to detect polarized Zeeman signatures. From three phase-resolved data sets collected during the summers of 2007, 2008, and 2009, we model the large-scale photospheric magnetic field of the star by means of Zeeman-Doppler imaging and follow its temporal evolution. Results. The comparison of the magnetic maps shows that a polarity reversal of the axisymmetric component of the large-scale magnetic field occurred between 2007 and 2008, this evolution being observed in both the poloidal and toroidal magnetic components. Between 2008 and 2009, another type of global evolution occured, characterized by a sharp decrease of the fraction of magnetic energy stored in the toroidal component. These changes were not accompanied by significant evolution in the total photospheric magnetic energy. Using our spectra to perform radial velocity measurements, we also detect a very low-mass stellar companion to HD 190771., Comment: Accepted by Astronomy and Astrophysics (Letter to the Editor)

Published
2009
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9. Simulating the impact of dust cooling on the statistical properties of the intracluster medium

Author

Pointecouteau, E., Da Silva, A., Catalano, A., Montier, L., Lanoux, J., Roncarelli, M., and Giard, M.

Subjects
Astrophysics - Cosmology and Extragalactic Astrophysics
Abstract

From the first stages of star and galaxy formation, non-gravitational processes such as ram pressure stripping, SNs, galactic winds, AGNs, galaxy-galaxy mergers, etc... lead to the enrichment of the IGM in stars, metals as well as dust, via the ejection of galactic material into the IGM. We know now that these processes shape, side by side with gravitation, the formation and the evolution of structures. We present here hydrodynamic simulations of structure formation implementing the effect of the cooling by dust on large scale structure formation. We focus on the scale of galaxy clusters and study the statistical properties of clusters. Here we present our results on the $T_X-M$ and the $L_X-M$ scaling relations which exhibit changes on both the slope and normalization when adding cooling by dust to the standard radiative cooling model. For example, the normalization of the $T_X-M$ relation changes only by a maximum of 2% at $M=10^{14}$ M$_\odot$ whereas the normalization of the $L_X-T_X$ changes by as much as 10% at $T_X=1$ keV for models that including dust cooling. Our study shows that the dust is an added non-gravitational process that contributes shaping the thermodynamical state of the hot ICM gas., Comment: 11 pages, 4 figures, ASR in press

Published
2009
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10. Planck early results. XI. Calibration of the local galaxy cluster Sunyaev-Zeldovich scaling relations

Author

Poutanen, T., Natoli, P., Polenta, G., Bartlett, J.G., Bucher, M., Cardoso, J.-F., Catalano, A., Delabrouille, J., Fromenteau, S., Ganga, K., Giraud-Héraud, Y., Patanchon, G., Piat, M., Rosset, C., Smoot, G.F., Ashdown, M., Brown, M.L., Chon, G., Hobson, M., Lasenby, A., Stolyarov, V., Bhatia, R., Kneissl, R., Bond, J.R., Miville-Deschênes, M.-A., Banday, A.J., Bernard, J.-P., Forni, O., Giard, M., Lanoux, J., Montier, L., Pointecouteau, E., Ristorcelli, I., Bock, J.J., Doré, O., Hildebrandt, S.R., Prézeau, G., Rocha, G., Seiffert, M.D., Dahle, H., Lilje, P.B., Da Silva, A., Challinor, A., Shellard, P., Melin, J.-B., Piffaretti, R., Starck, J.-L., Yvon, D., Linden-Vørnle, Michael, Nørgaard-Nielsen, Hans Ulrik, Toffolatti, L., Marleau, F., Netterfield, C.B., Scott, D., Pierpaoli, E., Liddle, A., Juvela, M., Keihänen, E., Keskitalo, R., Kurki-Suonio, H., Chiang, C., Jones, W.C., Cayón, L., White, M., Knox, L., Leonardi, R., Lubin, P.M., Zonca, A., Wandelt, B.D., Matarrese, S., De Bernardis, P., Masi, S., Melchiorri, A., Piacentini, F., Bersanelli, M., Maino, D., Mennella, A., Tomasi, M., Gregorio, A., Balbi, A., Bourdin, H., Cabella, P., De Gasperis, G., Mazzotta, P., Vittorio, N., Christensen, P.R., Naselsky, P., Flores-Cacho, I., Génova-Santos, R.T., Rebolo, R., Rubiño-Martín, J.A., Dupac, X., Mendes, L., Giardino, G., Laureijs, R.J., Tauber, J.A., Bonaldi, A., De Zotti, G., Colafrancesco, S., Frailis, M., Galeotta, S., Maris, M., Pasian, F., Zacchei, A., Burigana, C., Cuttaia, F., De Rosa, A., Finelli, F., Franceschi, E., Gruppuso, A., Mandolesi, N., Morgante, G., Ricciardi, S., Sandri, M., Terenzi, L., Valenziano, L., Villa, F., Donzelli, S., Stivoli, F., Désert, F.-X., Chamballu, A., Clements, D.L., Jaffe, A.H., Mortlock, D., Novikov, D., Rusholme, B., Benoît, A., Aghanim, N., Aumont, J., Douspis, M., Lagache, G., Noviello, F., Pajot, F., Ponthieu, N., Puget, J.-L., Torre, J.-P., Vibert, L., Benabed, K., Bouchet, F.R., Colombi, S., Delouis, J.-M., Hivon, E., Moneti, A., Prunet, S., Sygnet, J.-F., Chiang, L.-Y., Efstathiou, G., Gratton, S., Harrison, D., Munshi, D., Hoyland, R.J., Barreiro, R.B., Diego, J.M., Herranz, D., López-Caniego, M., Martínez-González, E., Vielva, P., Crill, B.P., Górski, K.M., Holmes, W.A., Lawrence, C.R., Mitra, S., Wade, L.A., Maffei, B., MacTavish, C.J., Coulais, A., Lamarre, J.-M., Arnaud, M., Pratt, G.W., MacÍas-Pérez, J.F., Perotto, L., Renault, C., Santos, D., Couchot, F., Henrot-Versillé, S., Perdereau, O., Plaszczynski, S., Tristram, M., Borrill, J., Kisner, T.S., Bartelmann, M., Churazov, E., Dolag, K., Dörl, U., Enßlin, T.A., Hernández-Monteagudo, C., Hovest, W., Matthai, F., Rachen, J.P., Reinecke, M., Riller, T., Sunyaev, R., White, S.D.M., Tuovinen, J., Murphy, A., Novikov, I., Savini, G., Baccigalupi, C., Danese, L., González-Nuevo, J., Leach, S., Perrotta, F., Mann, R., Ade, P.A.R., Sudiwala, R., Osborne, S., Schaefer, B.M., Battaner, E., Huffenberger, K.M., Department of Physics, Helsinki Institute of Physics, Universidad de Cantabria, APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Hélium : du fondamental aux applications (HELFA), Institut Néel (NEEL), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), APC - Gravitation (APC-Gravitation), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), PLANCK, Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Hélium : du fondamental aux applications (NEEL - HELFA), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS), Ade, P. A. R., Aghanim, N., Arnaud, M., Ashdown, M., Aumont, J., Baccigalupi, C., Balbi, A., Banday, A. J., Barreiro, R. B., Bartelmann, M., Bartlett, J. G., Battaner, E., Benabed, K., Benoît, A., Bernard, J. P., Bersanelli, M., Bhatia, R., Bock, J. J., Bonaldi, A., Bond, J. R., Borrill, J., Bouchet, F. R., Bourdin, H., Brown, M. L., Bucher, M., Burigana, C., Cabella, P., Cardoso, J. F., Catalano, A., Cayón, L., Challinor, A., Chamballu, A., Chiang, L. Y, Chiang, C., Chon, G., Christensen, P. R., Churazov, E., Clements, D. L., Colafrancesco, S., Colombi, S., Couchot, F., Coulais, A., Crill, B. P., Cuttaia, F., Da Silva, A., Dahle, H., Danese, L., de Bernardis, P., de Gasperis, G., de Rosa, A., de Zotti, G., Delabrouille, J., Delouis, J. M., Désert, F. X., Diego, J. M., Dolag, K., Donzelli, S., Doré, O., Dörl, U., Douspis, M., Dupac, X., Efstathiou, G., Ensslin, T. A., Finelli, F., Flores, I., Forni, O., Frailis, M., Franceschi, E., Fromenteau, S., Galeotta, S., Ganga, K., Génova Santos, R. T., Giard, M., Giardino, G., Giraud Héraud, Y., González Nuevo, J., Górski, K. M., Gratton, S., Gregorio, Anna, Gruppuso, A., Harrison, D., Henrot Versillé, S., Hernández Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hovest, W., Hoyland, R. J., Huffenberger, K. M., Jaffe, A. H., Jones, W. C., Juvela, M., Keihänen, E., Keskitalo, R., Kisner, T. S., Kneissl, R., Knox, L., Kurki Suonio, H., Lagache, G., Lamarre, J. M., Lanoux, J., Lasenby, A., Laureijs, R. J., Lawrence, C. R., Leach, S., Leonardi, R., Liddle, A., Lilje, P. B., Linden Vornle, M., López Caniego, M., Lubin, P. M., Macías Pérez, J. F., Mactavish, C. J., Maffei, B., Maino, D., Mandolesi, N., Mann, R., Maris, M., Marleau, F., Martínez González, E., Masi, S., Matarrese, S., Matthai, F., Mazzotta, P., Melchiorri, A., Melin, J. B., Mendes, L., Mennella, A., Mitra, S., Miville Deschênes, M. A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, A., Naselsky, P., Natoli, P., Netterfield, C. B., Norgaard Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., Osborne, S., Pajot, F., Pasian, F., Patanchon, G., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Pierpaoli, E., Piffaretti, R., Plaszczynski, S., Pointecouteau, E., Polenta, G., Ponthieu, N., Poutanen, T., Pratt, G. W., Prézeau, G., Prunet, S., Puget, J. L., Rachen, J. P., Rebolo, R., Reinecke, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Rubiño Martín, J. A., Rusholme, B., Sandri, M., Santos, D., Savini, G., Schaefer, B. M., Scott, D., Seiffert, M. D., Shellard, P., Smoot, G. F., Starck, J. L., Stivoli, F., Stolyarov, V., Sudiwala, R., Sunyaev, R., Sygnet, J. F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Torre, J. P., Tristram, M., Tuovinen, J., Valenziano, L., Vibert, L., Vielva, P., Villa, F., Vittorio, N., Wade, L. A., Wandelt, B. D., White, S. D. M., White, M., Yvon, D., Zacchei, A., Zonca, A., Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), HELFA - Hélium : du fondamental aux applications, Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), and Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)

Subjects
Experimental Physics, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics, 01 natural sciences, 7. Clean energy, Luminosity, CMB physic, CMB physics, galaxies, clusters, observations [Cosmology], 010303 astronomy & astrophysics, QB, Physics, Planck ESA mission, Cosmology: observations, Cosmology, observations, Early results, galaxies: clusters: interacluster medium – X-rays: galaxies: clusters – cosmology: observations, symbols, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, education, x-rays, cosmology: observations, interacluster medium, x-rays: galaxies: clusters, cosmology, galaxies: clusters: interacluster medium, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, clusters: interacluster medium [Galaxies], [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], symbols.namesake, Settore FIS/05 - Astronomia e Astrofisica, clusters: interacluster medium – X-rays: galaxies: clusters – cosmology: observations [galaxies], X-rays, 0103 physical sciences, Calibration, Planck, Density contrast, Scaling, Galaxy cluster, 010308 nuclear & particles physics, Astronomy and Astrophysics, Galaxies, 115 Astronomy, Space science, Galaxies: clusters: interacluster medium, Space and Planetary Science, X-rays: galaxies: clusters, galaxies: clusters [X-rays]
Abstract

14 páginas, 6 figuras, 2 tablas.-- Planck Collaboration: et al., We present precise Sunyaev-Zeldovich (SZ) effect measurements in the direction of 62 nearby galaxy clusters (z < 0.5) detected at high signal-to-noise in the first Planck all-sky data set. The sample spans approximately a decade in total mass, 2 × 1014 M⊙ < M500 < 2 × 1015 M⊙, where M500 is the mass corresponding to a total density contrast of 500. Combining these high quality Planck measurements with deep XMM-Newton X-ray data, we investigate the relations between DA2 Y500, the integrated Compton parameter due to the SZ effect, and the X-ray-derived gas mass Mg,500, temperature TX, luminosity LX,500, SZ signal analogue YX,500 = Mg,500 × TX, and total mass M500. After correction for the effect of selection bias on the scaling relations, we find results that are in excellent agreement with both X-ray predictions and recently-published ground-based data derived from smaller samples. The present data yield an exceptionally robust, high-quality local reference, and illustrate Planck’s unique capabilities for all-sky statistical studies of galaxy clusters., The Planck Collaboration acknowledges the support of: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN and JA (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and DEISA (EU).

Published
2011

11. Long-term magnetic field monitoring of the Sun-like star ��Bootis A

Author

Morgenthaler, A., Petit, P., Saar, S., Solanki, S. K., Morin, J., Marsden, S. C., Auriere, M., Dintrans, B., Fares, R., Gastine, T., Lanoux, J., Lignieres, F., Paletou, F., Velez, J. C. Ramirez, Theado, S., and Van Grootel, V.

Subjects
Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Solar and Stellar Astrophysics (astro-ph.SR)
Abstract

Aims. We aim to investigate the long-term temporal evolution of the magnetic field of the solar-type star ��Bootis A, both from direct magnetic field measurements and from the simultaneous estimate of indirect activity indicators. Methods. We obtained seven epochs of high-resolution, circularly-polarized spectra from the NARVAL spectropolarimeter between 2007 and 2011, for a total of 76 spectra. Using approximately 6,100 photospheric spectral lines covering the visible domain, we employed a cross-correlation procedure to compute a mean polarized line profile from each spectrum. The large-scale photospheric magnetic field of the star was then modelled by means of Zeeman-Doppler Imaging, allowing us to follow the year-to-year evolution of the reconstructed magnetic topology. Simultaneously, we monitored the width of several magnetically sensitive spectral lines, the radial velocity, the line asymmetry of intensity line profiles, and the chromospheric emission in the cores of the Ca II H and Halpha lines. Results. During the highest observed activity states, in 2007 and 2011, the large-scale field of ��Boo A is almost completely axisymmetric and is dominated by its toroidal component. The magnetic topologies reconstructed for these activity maxima are very similar, suggesting a form of short cyclicity in the large-scale field distribution. Correlated temporal evolution, due to both rotational modulation and seasonal variability, is observed between the Ca II emission, the Halpha emission and the width of magnetically sensitive lines. When measurable, the differential rotation reveals a strong latitudinal shear in excess of 0.2 rad/d., 16 pages, 8 figures, accepted for publication in A&A, abstract shortened to respect the 1920 characters required

Published
2011
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13. Long-term magnetic field monitoring of the Sun-like starξBootis A

Author

Morgenthaler, A., primary, Petit, P., additional, Saar, S., additional, Solanki, S. K., additional, Morin, J., additional, Marsden, S. C., additional, Aurière, M., additional, Dintrans, B., additional, Fares, R., additional, Gastine, T., additional, Lanoux, J., additional, Lignières, F., additional, Paletou, F., additional, Ramírez Vélez, J. C., additional, Théado, S., additional, and Van Grootel, V., additional

Published
2012
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14. The rapid rotation and complex magnetic field geometry of Vega

Author

Petit, P., primary, Lignières, F., additional, Wade, G. A., additional, Aurière, M., additional, Böhm, T., additional, Bagnulo, S., additional, Dintrans, B., additional, Fumel, A., additional, Grunhut, J., additional, Lanoux, J., additional, Morgenthaler, A., additional, and Van Grootel, V., additional

Published
2010
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15. Exploring the magnetic topologies of cool stars

Author

Morin, J., primary, Donati, J.-F., additional, Petit, P., additional, Albert, L., additional, Auriére, M., additional, Cabanac, R., additional, Catala, C., additional, Delfosse, X., additional, Dintrans, B., additional, Fares, R., additional, Forveille, T., additional, Gastine, T., additional, Jardine, M., additional, Konstantinova-Antova, R., additional, Lanoux, J., additional, Lignires, F., additional, Morgenthaler, A., additional, Paletou, F., additional, Velez, J.C. Ramirez, additional, Solanki, S.K., additional, Thado, S., additional, and Van Grootel, V., additional

Published
2010
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17. A BCool magnetic snapshot survey of solar-type stars.

Author

Marsden, S. C., Petit, P., Jeffers, S. V., Morin, J., Fares, R., Reiners, A., do Nascimento, J.-D., Aurière, M., Bouvier, J., Carter, B. D., Catala, C., Dintrans, B., Donati, J.-F., Gastine, T., Jardine, M., Konstantinova-Antova, R., Lanoux, J., Lignières, F., Morgenthaler, A., and Ramìrez-Vèlez, J. C.

Subjects
MAGNETIC fields, SOLAR system, HIGH resolution imaging, SPECTROPOLARIMETERS, ROTATIONAL motion, SOLAR chromosphere
Abstract

We present the results of a major high-resolution spectropolarimetric BCool project magnetic survey of 170 solar-type stars. Surface magnetic fields were detected on 67 stars, with 21 classified as mature solar-type stars, a result that increases by a factor of 4 the number of mature solar-type stars on which magnetic fields have been observed. In addition, a magnetic field was detected for 3 out of 18 of the subgiant stars surveyed. For the population of K-dwarfs, the mean value of |Bl| (|Bl|mean) was also found to be higher (5.7 G) than |Bl|mean measured for the G-dwarfs (3.2 G) and the F-dwarfs (3.3 G). For the sample as a whole, |Bl|mean increases with rotation rate and decreases with age, and the upper envelope for |Bl| correlates well with the observed chromospheric emission. Stars with a chromospheric S-index greater than about 0.2 show a high magnetic field detection rate and so offer optimal targets for future studies. This survey constitutes the most extensive spectropolarimetric survey of cool stars undertaken to date, and suggests that it is feasible to pursue magnetic mapping of a wide range of moderately active solar-type stars to improve our understanding of their surface fields and dynamos. [ABSTRACT FROM AUTHOR]

Published
2014

18. VizieR Online Data Catalog: BCool survey of solar-type stars (Marsden+ 2014)

Author

Marsden, S. C., Petit, P., Jeffers, S. V., Morin, J., Rim Fares, Reiners, A., Do Nascimento, J. -D, Auriere, M., Bouvier, J., Carter, B. D., Catala, C., Dintrans, B., Donati, J. -F, Gastine, T., Jardine, M., Konstantinova-Antova, R., Lanoux, J., Lignieres, F., Morgenthaler, A., Ramirez-Velez, J. C., Theado, S., Grootel, V., and BCool Collaboration

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