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1. Intermediate resolution H-beta spectroscopy and photometric monitoring of 3C 390.3 I. Further evidence of a nuclear accretion disk

Author

Shapovalova, A. I., Burenkov, A. N., Carrasco, L., Chavushyan, V. H., Doroshenko, V. T., Dumont, A. M., Lyuty, V. M., Valdes, J. R., Vlasuyk, V. V., Bochkarev, N. G., Collin, S., Legrand, F., Mikhailov, V. P., Spiridonova, O. I., Kurtanidze, O., and Nikolashvili, M. G.

Subjects
Astrophysics
Abstract

We have monitored the AGN 3C390.3 between 1995 and 2000.Two large amplitude outbursts, of different duration, in continuum and H beta light were observed ie.: in October 1994 a brighter flare that lasted about 1000 days and in July 1997 another one that lasted about 700 days were detected. The flux in the H beta wings and line core vary simultaneously, a behavior indicative of predominantly circular motions in the BLR.Important changes of the Hbeta emission profiles were detected: at times, we found profiles with prominent asymmetric wings, as those normaly seen in Sy1s, while at other times, we observe profiles with weak almost symmetrical wings, similar to those seen in Sy1.8s. We found that the radial velocity difference between the red and blue bumps is anticorrelated with the light curves of H beta and continuum radiation.e found that the radial velocity difference between the red and blue bumps is anticorrelated with the light curves of H-beta and continuum radiation. Theoretical H-beta profiles were computed for an accretion disk, the observed profiles are best reproduced by an inclined disk (25 deg) whose region of maximum emission is located roughly at 200 Rg. The mass of the black hole in 3C 390.3, estimated from the reverberation analysis is Mrev = 2.1 x 10^9 Msun, ie. 5 times larger than previous estimates, Comment: 18 pages, 13 figures, 4 tables. to appear in Astronomy and Astrophysics

Published
2001
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2. A continuous low star formation rate in IZw 18 ?

Author

Legrand, F., Kunth, D., Roy, J. -R., Mas-Hesse, J. M., and Walsh, J. R.

Subjects
Astrophysics
Abstract

Deep long-slit spectroscopic observations of the blue compact galaxy IZw 18 obtained with the CFH 3.6 m Telescope are presented. The very low value of oxygen abundance previously reported is confirmed and a very homogeneous abundance distribution is found (no variation larger than 0.05 dex) over the whole ionized region. We concur with Tenorio-Tagle (1996) and Devost et al. (1997) that the observed abundance level cannot result from the material ejected by the stars formed in the current burst, and propose that the observed metals were formed in a previous star formation episode. Metals ejected in the current burst of star formation remain most probably hidden in a hot phase and are undetectable using optical spectroscopy. We discuss different scenarios of star formation in IZw 18. Combining various observational facts, for instance the faint star formation rate observed in low surface brightness galaxies van Zee et al. (1997), it is proposed that a low and continuous rate of star formation occurring during quiescent phases between bursts could be a significant source of metal enrichment of the interstellar medium., Comment: 10 pages, 4 Postscript figures, to be published in Astronomy and Astrophysics main journal

Published
2000

3. On the star formation history of IZw 18

Author

Legrand, F.

Subjects
Astrophysics
Abstract

It has been suggested that a continuous low star formation rate has been the dominant regime in IZw 18 and in dwarf galaxies for the lifetime of these objects (Legrand et al. 1999). Here, we discuss and model various star-forming histories for IZw 18. Particularly, we show that if the metallicity observed in IZw 18 results from starburst events only, the observed colors constrain the fraction of the metals ejected from the galaxy to be less than 50-70 %. We demonstrate that the continuous star formation scenario reproduces the observed parameters of IZw 18. A continuous star formation rate (SFR) of about 10E-4 Msol/yr during 14 Gyr reproduces precisely the observed abundances. This SFR is comparable with the lowest SFR observed in low surface brightness galaxies (van Zee et al. 1997). Generalized to all galaxies, the low continuous SFR scenario accounts for various facts: the presence of star formation in quiescent dwarfs and LSBG, the metallicity increase with time in the most underabundant DLA systems, and the metal content extrapolations to the outskirts of spiral galaxies. Also the apparent absence of galaxies with a metallicity lower than IZw 18, the apparent absence of HI clouds without optical counterparts, and the homogeneity of abundances in dwarfs galaxies are natural outcomes of the scenario. This implies that, even if starbursts are strong and important events in the life of galaxies, their more subdued but continuous star formation regime cannot be ignored when accounting for their chemical evolution., Comment: 10 pages, 5 postscript figures. Accepted for publication in Astronomy and Astrophysics main journal

Published
1999

4. Low Rate Star Formation Activity During Quiescent Phases in Dwarf Galaxies

Author

Legrand, F. and Kunth, D.

Subjects
Astrophysics
Abstract

Observations of quiescent dwarfs and low surface brightness galaxies suggest that continuous low rate star formation is likely to occur, during the quiescent phases between bursts, in dwarf galaxies. We thus have used a spectrophotometric model to reproduce the observed abundances in IZw 18, assuming only a low constant star formation rate. We conclude that such a continuous low star formation rate cannot be neglected, especially when considering the chemical evolution of very metal poor objects., Comment: figure 2 modified due to an error in the metallicity used to compute the spectra. 4 pages, 2 postscript figures, To appear in "Dwarf Galaxies and Cosmology" proceedings of the XVIIIth Moriond astrophysics meeting, Les Arcs, March 1998

Published
1998

5. Abundance profile and stellar content of IZw18

Author

Legrand, F.

Subjects
Astrophysics
Abstract

New spectroscopic observations of the metal poor galaxy IZw 18 are discussed. Wolf-Rayet stars of WC type have been detected in the NW-HII region contrary to evolutionary synthesis model predictions. Implications on the mass loss rate and on the formation processes of WR stars are discussed. A very homogeneous metal abundance is observed within the HII region. This emphasizes the problem of the dispersal and mixing of new synthesized element in a starburst. Different scenarios are discussed, showing that metals remain most likely hidden in a hot phase and that the observed present metallicity is the result of a previous star formation event., Comment: 4 pages, 2 postscript figures, To appear in "Abundance Profiles: Diagnostic Tools for Galaxy History" proceedings from workshop at U. Laval, October 1997

Published
1997

6. Detection of WR stars in the metal-poor starburst galaxy IZw 18

Author

Legrand, F., Kunth, D., Roy, J. -R., Mas-Hesse, J. M., and Walsh, J. R.

Subjects
Astrophysics
Abstract

Wolf-Rayet stars (WR) have been detected in the NW region of the metal-poor starburst galaxy IZw 18. The integrated luminosity and FWHM of the bumps at 4650 A and 5808 A are consistent with the presence of a few individual stars of WC4 or WC5 type. Evolutionary synthesis models predict few WRs in this galaxy, but only of WN type. The presence of WC stars at such low metallicity could however be explained by high mass loss rates, which would constrain the IMF upper mass cut-off in IZw 18 to be higher than 80 Msol or alternatively favor a binary channel for WR formation. WC stars could also explain the strong and narrow HeII 4686 A emission line which peaks co-spatially with the WR bump emission, as suggested by Schaerer (1996). This detection shows that WR stars, even of WC type, are formed at metallicities below 1/40th solar., Comment: 4 pages, 2 postscript figures A&A in press

Published
1997

7. Evidences for an expanding shell in the Blue Compact Dwarf Galaxy Haro 2

Author

Legrand, F., Kunth, D., Mas-Hesse, J. M., and Lequeux, J.

Subjects
Astrophysics
Abstract

Long-slit observations of the blue compact galaxy Haro 2 have been performed to detect the Halpha emission originating in the partially ionized wind outflowing at 200 km/s, that had been previously detected with the Hubble Space Telescope. A shallow broadening of the Halpha line wings has been observed, consistent with the existence of an expanding shell. The rotation curve shows two dips at the same systemic velocity as the nucleus. At the positions of the dips the Halpha line is clearly broadened with respect to the central core. This broadening is produced by the outer layers of the expanding shell. From the position of these dips we estimate the size of the shell to be around 20'' in diameter, with a corresponding kinematical age between 5 and 6 Myr. A comparison of the Halpha and Ly_alpha profiles shows that Ly_alpha is significantly broader than Halpha, with an additional emission in the red wing. We interpret this redshifted source of Ly_alpha emission as line photons backscattered by the receding part of the expanding shell. These observations outline the extremely high sensitivity of the Ly_alpha line to the structure and kinematics of the interstellar medium., Comment: 8 pages, 5 postscript figures. To be published in Astronomy & Astrophysics

Published
1997

8. Detection of WR stars in the metal-poor starburst galaxy IZw 18

Author

Legrand, F., Kunth, D., Roy, J. -R, J. Miguel Mas-Hesse, and Walsh, J. R.

Subjects
Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract

Wolf-Rayet stars (WR) have been detected in the NW region of the metal-poor starburst galaxy IZw 18. The integrated luminosity and FWHM of the bumps at 4650 A and 5808 A are consistent with the presence of a few individual stars of WC4 or WC5 type. Evolutionary synthesis models predict few WRs in this galaxy, but only of WN type. The presence of WC stars at such low metallicity could however be explained by high mass loss rates, which would constrain the IMF upper mass cut-off in IZw 18 to be higher than 80 Msol or alternatively favor a binary channel for WR formation. WC stars could also explain the strong and narrow HeII 4686 A emission line which peaks co-spatially with the WR bump emission, as suggested by Schaerer (1996). This detection shows that WR stars, even of WC type, are formed at metallicities below 1/40th solar., Comment: 4 pages, 2 postscript figures A&A in press

9. Planck pre-launch status: The Planck mission

Author

J. A. Tauber1, N. Mandolesi2, J.-L. Puget3, T. Banos4, M. Bersanelli5, F. R. Bouchet6, R. C. Butler2, J. Charra3, G. Crone7, J. Dodsworth8, G. Efstathiou9, R. Gispert3, G. Guyot3, A. Gregorio10, J. J. Juillet4, J.-M. Lamarre11, R. J. Laureijs1, C. R. Lawrence12, H. U. Nørgaard-Nielsen13, T. Passvogel7, J. M. Reix4, D. Texier14, L. Vibert3, A. Zacchei15, P. A. R. Ade16, N. Aghanim3, B. Aja17, E. Alippi18, L. Aloy7, P. Armand4, M. Arnaud19, A. Arondel3, A. Arreola-Villanueva12, E. Artal17, E. Artina18, A. Arts7, M. Ashdown20, J. Aumont21, M. Azzaro22, A. Bacchetta23, C. Baccigalupi24, M. Baker7, M. Balasini18, A. Balbi25, A. J. Banday26, G. Barbier28, R. B. Barreiro29, M. Bartelmann26, P. Battaglia18, E. Battaner31, K. Benabed6, J.-L. Beney32, R. Beneyton6, K. Bennett1, A. Benoit28, J.-P. Bernard27, P. Bhandari12, R. Bhatia12, M. Biggi33, R. Biggins8, G. Billig8, Y. Blanc34, H. Blavot3, J. J. Bock12, A. Bonaldi35, R. Bond36, J. Bonis32, J. Borders12, J. Borrill37, L. Boschini18, F. Boulanger3, J. Bouvier28, M. Bouzit3, R. Bowman12, E. Bréelle38, T. Bradshaw39, M. Braghin7, M. Bremer1, D. Brienza40, D. Broszkiewicz38, C. Burigana2, M. Burkhalter41, P. Cabella25, T. Cafferty12, M. Cairola23, S. Caminade3, P. Camus42, C. M. Cantalupo43, B. Cappellini5, J.-F. Cardoso38, R. Carr14, A. Catalano38, L. Cayón44, M. Cesa23, M. Chaigneau3, A. Challinor9, A. Chamballu45, J. P. Chambelland4, M. Charra3, L.-Y. Chiang46, G. Chlewicki23, P. R. Christensen47, S. Church48, E. Ciancietta23, M. Cibrario23, R. Cizeron32, D. Clements45, B. Collaudin4, J.-M. Colley38, 6, S. Colombi6, A. Colombo7, F. Colombo18, O. Corre4, F. Couchot32, B. Cougrand3, A. Coulais11, P. Couzin4, B. Crane3, B. Crill12, M. Crook39, D. Crumb12, F. Cuttaia2, U. Dörl26, P. da Silva6, R. Daddato7, C. Damasio7, L. Danese24, G. d'Aquino7, O. D'Arcangelo49, K. Dassas3, R. D. Davies50, W. Davies41, R. J. Davis50, P. De Bernardis40, D. de Chambure7, G. de Gasperis25, M. L. De la Fuente17, P. De Paco51, A. De Rosa2, G. De Troia25, G. De Zotti35, M. Dehamme32, J. Delabrouille38, J.-M. Delouis6, F.-X. Désert28, G. di Girolamo8, C. Dickinson50, E. Doelling8, K. Dolag26, I. Domken52, M. Douspis3, D. Doyle7, S. Du32, D. Dubruel4, C. Dufour38, C. Dumesnil3, X. Dupac14, P. Duret3, C. Eder32, A. Elfving7, T. A. Enßlin26, P. Eng3, K. English12, H. K. Eriksen53, P. Estaria7, M. C. Falvella55, F. Ferrari18, F. Finelli2, A. Fishman12, S. Fogliani15, S. Foley8, A. Fonseca12, G. Forma4, O. Forni27, P. Fosalba56, J.-J. Fourmond3, M. Frailis15, C. Franceschet5, E. Franceschi2, S. François3, M. Frerking12, M. F. Gómez-Reñasco57, K. M. Górski12, T. C. Gaier12, S. Galeotta58, K. Ganga38, J. García Lázaro14, A. Garnica12, M. Gaspard32, E. Gavila4, M. Giard27, G. Giardino1, G. Gienger8, Y. Giraud-Heraud38, J.-M. Glorian27, M. Griffin16, A. Gruppuso2, L. Guglielmi38, D. Guichon4, B. Guillaume7, P. Guillouet38, J. Haissinski32, F. K. Hansen53, J. Hardy12, D. Harrison9, A. Hazell59, M. Hechler8, V. Heckenauer3, D. Heinzer8, R. Hell26, S. Henrot-Versillé32, C. Hernández-Monteagudo26, D. Herranz29, J. M. Herreros57, V. Hervier3, A. Heske7, A. Heurtel32, S. R. Hildebrandt57, R. Hills20, E. Hivon6, M. Hobson20, D. Hollert12, W. Holmes12, A. Hornstrup13, W. Hovest26, R. J. Hoyland57, G. Huey12, K. M. Huffenberger60, N. Hughes61, U. Israelsson12, B. Jackson7, A. Jaffe45, T. R. Jaffe50, T. Jagemann14, N. C. Jessen13, J. Jewell12, W. Jones62, M. Juvela63, J. Kaplan38, P. Karlman12, F. Keck8, E. Keihänen64, M. King12, T. S. Kisner43, P. Kletzkine7, R. Kneissl26, J. Knoche26, L. Knox65, T. Koch12, M. Krassenburg7, H. Kurki-Suonio64, A. Lähteenmäki67, G. Lagache3, E. Lagorio28, P. Lami3, J. Lande27, A. Lange12, F. Langlet3, R. Lapini33, M. Lapolla18, A. Lasenby20, M. Le Jeune38, J. P. Leahy50, M. Lefebvre3, F. Legrand6, G. Le Meur32, R. Leonardi68, B. Leriche3, C. Leroy3, P. Leutenegger18, S. M. Levin12, P. B. Lilje53, C. Lindensmith12, M. Linden-Vørnle69, A. Loc12, Y. Longval3, P. M. Lubin68, T. Luchik12, I. Luthold7, J. F. Macias-Perez70, T. Maciaszek34, C. MacTavish45, S. Madden7, B. Maffei50, C. Magneville71, D. Maino5, A. Mambretti18, B. Mansoux32, D. Marchioro18, M. Maris15, F. Marliani7, J.-C. Marrucho32, J. Martí-Canales7, E. Martínez-González29, A. Martín-Polegre7, P. Martin4, C. Marty27, W. Marty27, S. Masi40, M. Massardi35, S. Matarrese72, F. Matthai26, P. Mazzotta25, A. McDonald8, P. McGrath12, A. Mediavilla17, P. R. Meinhold68, J.-B. Mélin71, F. Melot70, L. Mendes14, A. Mennella5, C. Mervier3, L. Meslier3, M. Miccolis18, M.-A. Miville-Deschenes3, A. Moneti6, D. Montet4, L. Montier27, J. Mora12, G. Morgante2, G. Morigi2, G. Morinaud3, N. Morisset73, D. Mortlock9, S. Mottet6, J. Mulder12, D. Munshi9, A. Murphy74, P. Murphy12, P. Musi23, J. Narbonne27, P. Naselsky47, A. Nash12, F. Nati40, P. Natoli25, B. Netterfield36, J. Newell12, M. Nexon27, C. Nicolas3, P. H. Nielsen75, N. Ninane52, F. Noviello3, D. Novikov45, I. Novikov47, I. J. O'Dwyer12, P. Oldeman7, P. Olivier7, L. Ouchet4, C. A. Oxborrow13, L. Pérez-Cuevas7, L. Pagan18, C. Paine12, F. Pajot3, R. Paladini76, F. Pancher28, J. Panh34, G. Parks12, P. Parnaudeau6, B. Partridge77, B. Parvin12, J. P. Pascual17, F. Pasian15, D. P. Pearson12, T. Pearson12, M. Pecora18, O. Perdereau32, L. Perotto70, F. Perrotta24, F. Piacentini40, M. Piat38, E. Pierpaoli78, O. Piersanti7, E. Plaige32, S. Plaszczynski32, P. Platania49, E. Pointecouteau27, G. Polenta79, N. Ponthieu3, L. Popa80, G. Poulleau3, T. Poutanen64, G. Prézeau12, L. Pradell81, M. Prina12, S. Prunet6, J. P. Rachen26, D. Rambaud27, F. Rame23, I. Rasmussen7, J. Rautakoski7, W. T. Reach82, R. Rebolo57, M. Reinecke26, J. Reiter12, C. Renault70, S. Ricciardi83, P. Rideau4, T. Riller26, I. Ristorcelli27, J. B. Riti4, G. Rocha12, Y. Roche4, R. Pons27, R. Rohlfs73, D. Romero12, S. Roose52, C. Rosset32, S. Rouberol6, M. Rowan-Robinson45, J. A. Rubiño-Martín57, P. Rusconi18, B. Rusholme82, M. Salama12, E. Salerno84, M. Sandri2, D. Santos70, J. L. Sanz29, L. Sauter6, F. Sauvage4, G. Savini85, M. Schmelzel12, A. Schnorhk7, W. Schwarz12, D. Scott86, M. D. Seiffert12, P. Shellard20, C. Shih12, M. Sias23, J. I. Silk87, R. Silvestri18, R. Sippel88, G. F. Smoot89, J.-L. Starck71, P. Stassi70, J. Sternberg1, F. Stivoli83, V. Stolyarov9, R. Stompor38, L. Stringhetti2, D. Strommen12, T. Stute88, R. Sudiwala16, R. Sugimura12, R. Sunyaev26, J.-F. Sygnet6, M. Türler73, E. Taddei18, J. Tallon12, C. Tamiatto3, M. Taurigna32, D. Taylor14, L. Terenzi2, S. Thuerey7, J. Tillis12, G. Tofani90, L. Toffolatti91, E. Tommasi55, M. Tomasi5, E. Tonazzini84, J.-P. Torre3, S. Tosti3, F. Touze32, M. Tristram32, J. Tuovinen92, M. Tuttlebee8, G. Umana93, L. Valenziano2, D. Vallée38, M. van der Vlis7, F. Van Leeuwen9, J.-C. Vanel38, B. Van-Tent6, J. Varis92, E. Vassallo8, C. Vescovi28, F. Vezzu28, D. Vibert6, P. Vielva29, J. Vierra12, F. Villa2, N. Vittorio25, C. Vuerli15, L. A. Wade12, A. R. Walker86, B. D. Wandelt94, C. Watson8, D. Werner8, M. White95, S. D. M. White26, A. Wilkinson50, P. Wilson12, A. Woodcraft16, B. Yoffo38, M. Yun12, V. Yurchenko74, D. Yvon71, B. Zhang12, O. Zimmermann28, A. Zonca58, D. Zorita96, Universitat Politècnica de Catalunya. Departament de Teoria del Senyal i Comunicacions, Universitat Politècnica de Catalunya. RF&MW - Grup de Recerca de sistemes, dispositius i materials de RF i microones, TAUBER J., A, Mandolesi, N, PUGET J., L, Banos, T, Bersanelli, M, BOUCHET F., R, BUTLER C., R, Charra, J, Crone, G, Dodsworth, J, Efstathiou, G, Gispert, R, Guyot, G, Gregorio, Anna, JUILLET J., J, LAMARRE J., M, LAUREIJS R., J, LAWRENCE C., R, NØRGAARD NIELSEN H., U, Passvogel, T, REIX J., M, Texier, D, Vibert, L, Zacchei, A, ADE P. A., R, Aghanim, N, Aja, B, Alippi, E, Aloy, L, Armand, P, Arnaud, M, Arondel, A, ARREOLA VILLANUEVA, A, Artal, E, Artina, E, Arts, A, Ashdown, M, Aumont, J, Azzaro, M, Bacchetta, A, Baccigalupi, C, Baker, M, Balasini, M, Balbi, A, BANDAY A., J, Barbier, G, BARREIRO R., B, Bartelmann, M, Battaglia, P, Battaner, E, Benabed, K, BENEY J., L, Beneyton, R, Bennett, K, Benoit, A, BERNARD J., P, Bhandari, P, Bhatia, R, Biggi, M, Biggins, R, Billig, G, Blanc, Y, Blavot, H, BOCK J., J, Bonaldi, A, Bond, R, Bonis, J, Borders, J, Borrill, J, Boschini, L, Boulanger, F, Bouvier, J, Bouzit, M, Bowman, R, Brelle, E, Bradshaw, T, Braghin, M, Bremer, M, Brienza, D, Broszkiewicz, D, Burigana, C, Burkhalter, M, Cabella, P, Cafferty, T, Cairola, M, Caminade, S, Camus, P, CANTALUPO C., M, Cappellini, B, CARDOSO J., F, Carr, R, Catalano, A, Cayon, L, Cesa, M, Chaigneau, M, Challinor, A, Chamballu, A, CHAMBELLAND J., P, Charra, M, CHIANG L., Y, Chlewicki, G, CHRISTENSEN P., R, Church, S, Ciancietta, E, Cibrario, M, Cizeron, R, Clements, D, Collaudin, B, COLLEY J., M, Colombi, S, Colombo, A, Colombo, F, Corre, O, Couchot, F, Cougrand, B, Coulais, A, Couzin, P, Crane, B, Crill, B, Crook, M, Crumb, D, Cuttaia, F, Dorl, U, DA SILVA, P, Daddato, R, Damasio, C, Danese, L, Daquino, G, Darcangelo, O, Dassas, K, DAVIES R., D, Davies, W, DAVIS R., J, DE BERNARDIS, P, DE CHAMBURE, D, DE GASPERIS, G, DE LA FUENTA M., L, DE PACO, P, DE ROSA, A, DE TROIA, G, DE ZOTTI, G, Dehamme, M, Delabrouille, J, DELOUIS J., M, DESERT F., X, DI GIROLAMO, G, Dickinson, C, Doelling, E, Dolag, K, Domken, I, Douspis, M, Doyle, D, Du, S, Dubruel, D, Dufour, C, Dumesnil, C, Dupac, X, Duret, P, Eder, C, Elfving, A, ENLIN T., A, Eng, P, English, K, ERIKSEN H., K, Estaria, P, FALVELLA M., C, Ferrari, F, Finelli, F, Fishman, A, Fogliani, S, Foley, S, Fonseca, A, Forma, G, Forni, O, Fosalba, P, ., ., Universidad de Cantabria, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Institut d'Astrophysique de Paris (IAP), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-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), Laboratoire de l'Accélérateur Linéaire (LAL), 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), AstroParticule et Cosmologie (APC (UMR_7164)), 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), APC - Gravitation (APC-Gravitation), 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)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, APC - Cosmologie, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), 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), PLANCK, Tauber, J, Puget, J, Bouchet, F, Butler, R, Gregorio, A, Juillet, J, Lamarre, J, Laureijs, R, Lawrence, C, NØRGAARD NIELSEN, H, Reix, J, Ade, P, Banday, A, Barreiro, R, Beney, J, Bernard, J, Bock, J, Bréelle, E, Cantalupo, C, Cardoso, J, Cayón, L, Chambelland, J, Chiang, L, Christensen, P, Colley, J, Dörl, U, D'Aquino, G, D'Arcangelo, O, Davies, R, Davis, R, DE LA FUENTE, M, Delouis, J, Désert, F, Enlin, T, Eriksen, H, Falvella, M, Fourmond, J, Frailis, M, Franceschet, C, Franceschi, E, François, S, Frerking, M, GÓMEZ REÑASCO, M, Górski, K, Gaier, T, Galeotta, S, Ganga, K, GARCÍA LÁZARO, J, Garnica, A, Gaspard, M, Gavila, E, Giard, M, Giardino, G, Gienger, G, GIRAUD HERAUD, Y, Glorian, J, Griffin, M, Gruppuso, A, Guglielmi, L, Guichon, D, Guillaume, B, Guillouet, P, Haissinski, J, Hansen, F, Hardy, J, Harrison, D, Hazell, A, Hechler, M, Heckenauer, V, Heinzer, D, Hell, R, HENROT VERSILLÉ, S, HERNÁNDEZ MONTEAGUDO, C, Herranz, D, Herreros, J, Hervier, V, Heske, A, Heurtel, A, Hildebrandt, S, Hills, R, Hivon, E, Hobson, M, Hollert, D, Holmes, W, Hornstrup, A, Hovest, W, Hoyland, R, Huey, G, Huffenberger, K, Hughes, N, Israelsson, U, Jackson, B, Jaffe, A, Jaffe, T, Jagemann, T, Jessen, N, Jewell, J, Jones, W, Juvela, M, Kaplan, J, Karlman, P, Keck, F, Keihänen, E, King, M, Kisner, T, Kletzkine, P, Kneissl, R, Knoche, J, Knox, L, Koch, T, Krassenburg, M, KURKI SUONIO, H, Lähteenmäki, A, Lagache, G, Lagorio, E, Lami, P, Lande, J, Lange, A, Langlet, F, Lapini, R, Lapolla, M, Lasenby, A, LE JEUNE, M, Leahy, J, Lefebvre, M, Legrand, F, LE MEUR, G, Leonardi, R, Leriche, B, Leroy, C, Leutenegger, P, Levin, S, Lilje, P, Lindensmith, C, LINDEN VØRNLE, M, Loc, A, Longval, Y, Lubin, P, Luchik, T, Luthold, I, MACIAS PEREZ, J, Maciaszek, T, Mactavish, C, Madden, S, Maffei, B, Magneville, C, Maino, D, Mambretti, A, Mansoux, B, Marchioro, D, Maris, M, Marliani, F, Marrucho, J, MARTÍ CANALES, J, MARTÍNEZ GONZÁLEZ, E, MARTÍN POLEGRE, A, Martin, P, Marty, C, Marty, W, Masi, S, Massardi, M, Matarrese, S, Matthai, F, Mazzotta, P, Mcdonald, A, Mcgrath, P, Mediavilla, A, Meinhold, P, Mélin, J, Melot, F, Mendes, L, Mennella, A, Mervier, C, Meslier, L, Miccolis, M, MIVILLE DESCHENES, M, Moneti, A, Montet, D, Montier, L, Mora, J, Morgante, G, Morigi, G, Morinaud, G, Morisset, N, Mortlock, D, Mottet, S, Mulder, J, Munshi, D, Murphy, A, Murphy, P, Musi, P, Narbonne, J, Naselsky, P, Nash, A, Nati, F, Natoli, P, Netterfield, B, Newell, J, Nexon, M, Nicolas, C, Nielsen, P, Ninane, N, Noviello, F, Novikov, D, Novikov, I, O'Dwyer, I, Oldeman, P, Olivier, P, Ouchet, L, Oxborrow, C, PÉREZ CUEVAS, L, Pagan, L, Paine, C, Pajot, F, Paladini, R, Pancher, F, Panh, J, Parks, G, Parnaudeau, P, Partridge, B, Parvin, B, Pascual, J, Pasian, F, Pearson, D, Pearson, T, Pecora, M, Perdereau, O, Perotto, L, Perrotta, F, Piacentini, F, Piat, M, Pierpaoli, E, Piersanti, O, Plaige, E, Plaszczynski, S, Platania, P, Pointecouteau, E, Polenta, G, Ponthieu, N, Popa, L, Poulleau, G, Poutanen, T, Prézeau, G, Pradell, L, Prina, M, Prunet, S, Rachen, J, Rambaud, D, Rame, F, Rasmussen, I, Rautakoski, J, Reach, W, Rebolo, R, Reinecke, M, Reiter, J, Renault, C, Ricciardi, S, Rideau, P, Riller, T, Ristorcelli, I, Riti, J, Rocha, G, Roche, Y, Pons, R, Rohlfs, R, Romero, D, Roose, S, Rosset, C, Rouberol, S, ROWAN ROBINSON, M, RUBIÑO MARTÍN, J, Rusconi, P, Rusholme, B, Salama, M, Salerno, E, Sandri, M, Santos, D, Sanz, J, Sauter, L, Sauvage, F, Savini, G, Schmelzel, M, Schnorhk, A, Schwarz, W, Scott, D, Seiffert, M, Shellard, P, Shih, C, Sias, M, Silk, J, Silvestri, R, Sippel, R, Smoot, G, Starck, J, Stassi, P, Sternberg, J, Stivoli, F, Stolyarov, V, Stompor, R, Stringhetti, L, Strommen, D, Stute, T, Sudiwala, R, Sugimura, R, Sunyaev, R, Sygnet, J, Türler, M, Taddei, E, Tallon, J, Tamiatto, C, Taurigna, M, Taylor, D, Terenzi, L, Thuerey, S, Tillis, J, Tofani, G, Toffolatti, L, Tommasi, E, Tomasi, M, Tonazzini, E, Torre, J, Tosti, S, Touze, F, Tristram, M, Tuovinen, J, Tuttlebee, M, Umana, G, Valenziano, L, Vallée, D, VAN DER VLIS, M, VAN LEEUWEN, F, Vanel, J, VAN TENT, B, Varis, J, Vassallo, E, Vescovi, C, Vezzu, F, Vibert, D, Vielva, P, Vierra, J, Villa, F, Vittorio, N, Vuerli, C, Wade, L, Walker, A, Wandelt, B, Watson, C, Werner, D, White, M, White, S, Wilkinson, A, Wilson, P, Woodcraft, A, Yoffo, B, Yun, M, Yurchenko, V, Yvon, D, Zhang, B, Zimmermann, O, Zonca, A, Zorita, D, Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS Paris)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), 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), 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), 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)), 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, 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), Department of Physics, Helsinki Institute of Physics, Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), École normale supérieure - Paris (ENS Paris), 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), 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), 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)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), and 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)

Subjects
[SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astrophysics, general [Submillimeter], 7. Clean energy, 01 natural sciences, DESIGN, Aeronautics, CMB physics, SPACE, Space vehicles: instruments, Instrumentation: detectors, 010303 astronomy & astrophysics, detectors [Instrumentation], QB, CALIBRATION, Physics, Planck ESA mission, general [Radio continuum], Astrophysics::Instrumentation and Methods for Astrophysics, space vehicles: instrument, MICROWAVE BACKGROUND ANISOTROPY, instrumentation: polarimeter, HIGH-FREQUENCY INSTRUMENT, cosmic microwave background, Submillimeter: general, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Cosmic microwawe background, education, Astrophysics::Cosmology and Extragalactic Astrophysics, instrumentation: detector, Instrumentation: polarimeters, Cosmic microwave background, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], instruments [Space vehicles], Radio continuum: general, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, polarimeters [Instrumentation], 010308 nuclear & particles physics, Astronomy and Astrophysics, Space vehicles, PERFORMANCE, 115 Astronomy, Space science, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], space vehicles: instruments, instrumentation: detectors, instrumentation: polarimeters, submillimeter: general, radio continuum: general, CMB EXPERIMENTS, 13. Climate action, Space and Planetary Science, Astronautics, Aeronàutica i espai::Astronàutica [Àrees temàtiques de la UPC], Instruments, Astronàutica
Abstract

22 páginas, 16 figuras, 6 tablas.-- Planck Science Team: et al., The European Space Agency's Planck satellite, launched on 14 May 2009, is the third-generation space experiment in the field of cosmic microwave background (CMB) research. It will image the anisotropies of the CMB over the whole sky, with unprecedented sensitivity ( ~ 2 × 10-6) and angular resolution (~5 arcmin). Planck will provide a major source of information relevant to many fundamental cosmological problems and will test current theories of the early evolution of the Universe and the origin of structure. It will also address a wide range of areas of astrophysical research related to the Milky Way as well as external galaxies and clusters of galaxies. The ability of Planck to measure polarization across a wide frequency range (30-350 GHz), with high precision and accuracy, and over the whole sky, will provide unique insight, not only into specific cosmological questions, but also into the properties of the interstellar medium. This paper is part of a series which describes the technical capabilities of the Planck scientific payload. It is based on the knowledge gathered during the on-ground calibration campaigns of the major subsystems, principally its telescope and its two scientific instruments, and of tests at fully integrated satellite level. It represents the best estimate before launch of the technical performance that the satellite and its payload will achieve in flight. In this paper, we summarise the main elements of the payload performance, which is described in detail in the accompanying papers. In addition, we describe the satellite performance elements which are most relevant for science, and provide an overview of the plans for scientific operations and data analysis.

Published
2010
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