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1. Planck 2013 results. XVI. Cosmological parameters

Author

Planck Collaboration, Ade, P. A. R., Aghanim, N., Armitage-Caplan, C., Arnaud, M., Ashdown, M., Atrio-Barandela, F., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Bartlett, J. G., Battaner, E., Benabed, K., Benoît, A., Benoit-Lévy, A., Bernard, J. -P., Bersanelli, M., Bielewicz, P., Bobin, J., Bock, J. J., Bonaldi, A., Bond, J. R., Borrill, J., Bouchet, F. R., Bridges, M., Bucher, M., Burigana, C., Butler, R. C., Calabrese, E., Cappellini, B., Cardoso, J. -F., Catalano, A., Challinor, A., Chamballu, A., Chary, R. -R., Chen, X., Chiang, H. C., Chiang, L. -Y, Christensen, P. R., Church, S., Clements, D. L., Colombi, S., Colombo, L. P. L., Couchot, F., Coulais, A., Crill, B. P., Curto, A., Cuttaia, F., Danese, L., Davies, R. D., Davis, R. J., de Bernardis, P., de Rosa, A., de Zotti, G., Delabrouille, J., Delouis, J. -M., Désert, F. -X., Dickinson, C., Diego, J. M., Dolag, K., Dole, H., Donzelli, S., Doré, O., Douspis, M., Dunkley, J., Dupac, X., Efstathiou, G., Elsner, F., Enßlin, T. A., Eriksen, H. K., Finelli, F., Forni, O., Frailis, M., Fraisse, A. A., Franceschi, E., Gaier, T. C., Galeotta, S., Galli, S., Ganga, K., Giard, M., Giardino, G., Giraud-Héraud, Y., Gjerløw, E., González-Nuevo, J., Górski, K. M., Gratton, S., Gregorio, A., Gruppuso, A., Gudmundsson, J. E., Haissinski, J., Hamann, J., Hansen, F. K., Hanson, D., Harrison, D., Henrot-Versillé, S., Hernández-Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hornstrup, A., Hou, Z., Hovest, W., Huffenberger, K. M., Jaffe, A. H., Jaffe, T. R., Jewell, J., Jones, W. C., Juvela, M., Keihänen, E., Keskitalo, R., Kisner, T. S., Kneissl, R., Knoche, J., Knox, L., Kunz, M., Kurki-Suonio, H., Lagache, G., Lähteenmäki, A., Lamarre, J. -M., Lasenby, A., Lattanzi, M., Laureijs, R. J., Lawrence, C. R., Leach, S., Leahy, J. P., Leonardi, R., León-Tavares, J., Lesgourgues, J., Lewis, A., Liguori, M., Lilje, P. B., Linden-Vørnle, M., López-Caniego, M., Lubin, P. M., Macías-Pérez, J. F., Maffei, B., Maino, D., Mandolesi, N., Maris, M., Marshall, D. J., Martin, P. G., Martínez-González, E., Masi, S., Massardi, M., Matarrese, S., Matthai, F., Mazzotta, P., Meinhold, P. R., Melchiorri, A., Melin, J. -B., Mendes, L., Menegoni, E., Mennella, A., Migliaccio, M., Millea, M., Mitra, S., Miville-Deschênes, M. -A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Moss, A., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Natoli, P., Netterfield, C. B., Nørgaard-Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., O'Dwyer, I. J., Osborne, S., Oxborrow, C. A., Paci, F., Pagano, L., Pajot, F., Paoletti, D., Partridge, B., Pasian, F., Patanchon, G., Pearson, D., Pearson, T. J., Peiris, H. V., Perdereau, O., Perotto, L., Perrotta, F., Pettorino, V., Piacentini, F., Piat, M., Pierpaoli, E., Pietrobon, D., Plaszczynski, S., Platania, P., Pointecouteau, E., Polenta, G., Ponthieu, N., Popa, L., Poutanen, T., Pratt, G. W., Prézeau, G., Prunet, S., Puget, J. -L., Rachen, J. P., Reach, W. T., Rebolo, R., Reinecke, M., Remazeilles, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Roudier, G., Rowan-Robinson, M., Rubiño-Martín, J. A., Rusholme, B., Sandri, M., Santos, D., Savelainen, M., Savini, G., Scott, D., Seiffert, M. D., Shellard, E. P. S., Spencer, L. D., Starck, J. -L., Stolyarov, V., Stompor, R., Sudiwala, R., Sunyaev, R., Sureau, F., Sutton, D., Suur-Uski, A. -S., Sygnet, J. -F., Tauber, J. A., Tavagnacco, D., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Tuovinen, J., Türler, M., Umana, G., Valenziano, L., Valiviita, J., Van Tent, B., Vielva, P., Villa, F., Vittorio, N., Wade, L. A., Wandelt, B. D., Wehus, I. K., White, M., White, S. D. M., Wilkinson, A., Yvon, D., Zacchei, A., and Zonca, A.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

We present the first results based on Planck measurements of the CMB temperature and lensing-potential power spectra. The Planck spectra at high multipoles are extremely well described by the standard spatially-flat six-parameter LCDM cosmology. In this model Planck data determine the cosmological parameters to high precision. We find a low value of the Hubble constant, H0=67.3+/-1.2 km/s/Mpc and a high value of the matter density parameter, Omega_m=0.315+/-0.017 (+/-1 sigma errors) in excellent agreement with constraints from baryon acoustic oscillation (BAO) surveys. Including curvature, we find that the Universe is consistent with spatial flatness to percent-level precision using Planck CMB data alone. We present results from an analysis of extensions to the standard cosmology, using astrophysical data sets in addition to Planck and high-resolution CMB data. None of these models are favoured significantly over standard LCDM. The deviation of the scalar spectral index from unity is insensitive to the addition of tensor modes and to changes in the matter content of the Universe. We find a 95% upper limit of r<0.11 on the tensor-to-scalar ratio. There is no evidence for additional neutrino-like relativistic particles. Using BAO and CMB data, we find N_eff=3.30+/-0.27 for the effective number of relativistic degrees of freedom, and an upper limit of 0.23 eV for the summed neutrino mass. Our results are in excellent agreement with big bang nucleosynthesis and the standard value of N_eff=3.046. We find no evidence for dynamical dark energy. Despite the success of the standard LCDM model, this cosmology does not provide a good fit to the CMB power spectrum at low multipoles, as noted previously by the WMAP team. While not of decisive significance, this is an anomaly in an otherwise self-consistent analysis of the Planck temperature data., Comment: 69 pages. Matches version to appear in Astronomy & Astrophysics

Published
2013
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2. Planck 2013 results. VII. HFI time response and beams

Author

Planck Collaboration, Ade, P. A. R., Aghanim, N., Armitage-Caplan, C., Arnaud, M., Ashdown, M., Atrio-Barandela, F., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Battaner, E., Benabed, K., Benoît, A., Benoit-Lévy, A., Bernard, J. -P., Bersanelli, M., Bielewicz, P., Bobin, J., Bock, J. J., Bond, J. R., Borrill, J., Bouchet, F. R., Bowyer, J. W., Bridges, M., Bucher, M., Burigana, C., Cardoso, J. -F., Catalano, A., Challinor, A., Chamballu, A., Chary, R. -R., Chiang, H. C., Chiang, L. -Y, Christensen, P. R., Church, S., Clements, D. L., Colombi, S., Colombo, L. P. L., Couchot, F., Coulais, A., Crill, B. P., Curto, A., Cuttaia, F., Danese, L., Davies, R. D., de Bernardis, P., de Rosa, A., de Zotti, G., Delabrouille, J., Delouis, J. -M., Désert, F. -X., Diego, J. M., Dole, H., Donzelli, S., Doré, O., Douspis, M., Dunkley, J., Dupac, X., Efstathiou, G., Enßlin, T. A., Eriksen, H. K., Finelli, F., Forni, O., Frailis, M., Fraisse, A. A., Franceschi, E., Galeotta, S., Ganga, K., Giard, M., Giraud-Héraud, Y., González-Nuevo, J., Górski, K. M., Gratton, S., Gregorio, A., Gruppuso, A., Gudmundsson, J. E., Haissinski, J., Hansen, F. K., Hanson, D., Harrison, D., Henrot-Versillé, S., Hernández-Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hornstrup, A., Hou, Z., Hovest, W., Huffenberger, K. M., Jaffe, A. H., Jaffe, T. R., Jones, W. C., Juvela, M., Keihänen, E., Keskitalo, R., Kisner, T. S., Kneissl, R., Knoche, J., Knox, L., Kunz, M., Kurki-Suonio, H., Lagache, G., Lamarre, J. -M., Lasenby, A., Laureijs, R. J., Lawrence, C. R., Leonardi, R., Leroy, C., Lesgourgues, J., Liguori, M., Lilje, P. B., Linden-Vørnle, M., López-Caniego, M., Lubin, P. M., Macías-Pérez, J. F., MacTavish, C. J., Maffei, B., Mandolesi, N., Maris, M., Marshall, D. J., Martin, P. G., Martínez-González, E., Masi, S., Massardi, M., Matarrese, S., Matsumura, T., Matthai, F., Mazzotta, P., McGehee, P., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Mitra, S., Miville-Deschênes, M. -A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Natoli, P., Netterfield, C. B., Nørgaard-Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., Osborne, S., Oxborrow, C. A., Paci, F., Pagano, L., Pajot, F., Paoletti, D., Pasian, F., Patanchon, G., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Pierpaoli, E., Pietrobon, D., Plaszczynski, S., Pointecouteau, E., Polegre, A. M., Polenta, G., Ponthieu, N., Popa, L., Poutanen, T., Pratt, G. W., Prézeau, G., Prunet, S., Puget, J. -L., Rachen, J. P., Reinecke, M., Remazeilles, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Roudier, G., Rowan-Robinson, M., Rusholme, B., Sandri, M., Santos, D., Sauvé, A., Savini, G., Scott, D., Shellard, E. P. S., Spencer, L. D., Starck, J. -L., Stolyarov, V., Stompor, R., Sudiwala, R., Sureau, F., Sutton, D., Suur-Uski, A. -S., Sygnet, J. -F., Tauber, J. A., Tavagnacco, D., Terenzi, L., Tomasi, M., Tristram, M., Tucci, M., Umana, G., Valenziano, L., Valiviita, J., Van Tent, B., Vielva, P., Villa, F., Vittorio, N., Wade, L. A., Wandelt, B. D., Yvon, D., Zacchei, A., and Zonca, A.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

This paper characterizes the effective beams,the effective beam window functions and the associated errors for the Planck HFI detectors. The effective beam is the angular response including the effect of the optics,detectors,data processing and the scan strategy. The window function is the representation of this beam in the harmonic domain which is required to recover an unbiased measurement of the CMB angular power spectrum. The HFI is a scanning instrument and its effective beams are the convolution of: (a) the optical response of the telescope and feeds;(b)the processing of the time-ordered data and deconvolution of the bolometric and electronic time response; and (c) the merging of several surveys to produce maps. The time response functions are measured using observations of Jupiter and Saturn and by minimizing survey difference residuals. The scanning beam is the post-deconvolution angular response of the instrument, and is characterized with observations of Mars. The main beam solid angles are determined to better than 0.5% at each HFI frequency band. Observations of Jupiter and Saturn limit near sidelobes (within 5deg) to about 0.1% of the total solid angle. Time response residuals remain as long tails in the scanning beams, but contribute less than 0.1% of the total. The bias and uncertainty in the beam products are estimated using ensembles of simulated planet observations that include the impact of instrumental noise and known systematic effects.The correlation structure of these ensembles is well-described by five error eigenmodes that are sub-dominant to sample variance and instrumental noise in the harmonic domain. A suite of consistency tests provide confidence that the error model represents a sufficient description of the data. The total error in the effective beam window functions is below 1% at 100GHz up to ell~1500$,and below 0.5% at 143 and 217GHz up to ~2000.

Published
2013
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3. Planck 2013 results. I. Overview of products and scientific results

Author

Planck Collaboration, Ade, P. A. R., Aghanim, N., Alves, M. I. R., Armitage-Caplan, C., Arnaud, M., Ashdown, M., Atrio-Barandela, F., Aumont, J., Aussel, H., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Barrena, R., Bartelmann, M., Bartlett, J. G., Bartolo, N., Basak, S., Battaner, E., Battye, R., Benabed, K., Benoît, A., Benoit-Lévy, A., Bernard, J. -P., Bersanelli, M., Bertincourt, B., Bethermin, M., Bielewicz, P., Bikmaev, I., Blanchard, A., Bobin, J., Bock, J. J., Böhringer, H., Bonaldi, A., Bonavera, L., Bond, J. R., Borrill, J., Bouchet, F. R., Boulanger, F., Bourdin, H., Bowyer, J. W., Bridges, M., Brown, M. L., Bucher, M., Burenin, R., Burigana, C., Butler, R. C., Calabrese, E., Cappellini, B., Cardoso, J. -F., Carr, R., Carvalho, P., Casale, M., Castex, G., Catalano, A., Challinor, A., Chamballu, A., Chary, R. -R., Chen, X., Chiang, H. C., Chiang, L. -Y, Chon, G., Christensen, P. R., Churazov, E., Church, S., Clemens, M., Clements, D. L., Colombi, S., Colombo, L. P. L., Combet, C., Comis, B., Couchot, F., Coulais, A., Crill, B. P., Cruz, M., Curto, A., Cuttaia, F., Da Silva, A., Dahle, H., Danese, L., Davies, R. D., Davis, R. J., de Bernardis, P., de Rosa, A., de Zotti, G., Déchelette, T., Delabrouille, J., Delouis, J. -M., Démoclès, J., Désert, F. -X., Dick, J., Dickinson, C., Diego, J. M., Dolag, K., Dole, H., Donzelli, S., Doré, O., Douspis, M., Ducout, A., Dunkley, J., Dupac, X., Efstathiou, G., Elsner, F., Enßlin, T. A., Eriksen, H. K., Fabre, O., Falgarone, E., Falvella, M. C., Fantaye, Y., Fergusson, J., Filliard, C., Finelli, F., Flores-Cacho, I., Foley, S., Forni, O., Fosalba, P., Frailis, M., Fraisse, A. A., Franceschi, E., Freschi, M., Fromenteau, S., Frommert, M., Gaier, T. C., Galeotta, S., Gallegos, J., Galli, S., Gandolfo, B., Ganga, K., Gauthier, C., Génova-Santos, R. T., Ghosh, T., Giard, M., Giardino, G., Gilfanov, M., Girard, D., Giraud-Héraud, Y., Gjerløw, E., González-Nuevo, J., Górski, K. M., Gratton, S., Gregorio, A., Gruppuso, A., Gudmundsson, J. E., Haissinski, J., Hamann, J., Hansen, F. K., Hansen, M., Hanson, D., Harrison, D. L., Heavens, A., Helou, G., Hempel, A., Henrot-Versillé, S., Hernández-Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Ho, S., Hobson, M., Holmes, W. A., Hornstrup, A., Hou, Z., Hovest, W., Huey, G., Huffenberger, K. M., Hurier, G., Ilić, S., Jaffe, A. H., Jaffe, T. R., Jasche, J., Jewell, J., Jones, W. C., Juvela, M., Kalberla, P., Kangaslahti, P., Keihänen, E., Kerp, J., Keskitalo, R., Khamitov, I., Kiiveri, K., Kim, J., Kisner, T. S., Kneissl, R., Knoche, J., Knox, L., Kunz, M., Kurki-Suonio, H., Lacasa, F., Lagache, G., Lähteenmäki, A., Lamarre, J. -M., Langer, M., Lasenby, A., Lattanzi, M., Laureijs, R. J., Lavabre, A., Lawrence, C. R., Jeune, M. Le, Leach, S., Leahy, J. P., Leonardi, R., León-Tavares, J., Leroy, C., Lesgourgues, J., Lewis, A., Li, C., Liddle, A., Liguori, M., Lilje, P. B., Linden-Vørnle, M., Lindholm, V., López-Caniego, M., Lowe, S., Lubin, P. M., Macías-Pérez, J. F., MacTavish, C. J., Maffei, B., Maggio, G., Maino, D., Mandolesi, N., Mangilli, A., Marcos-Caballero, A., Marinucci, D., Maris, M., Marleau, F., Marshall, D. J., Martin, P. G., Martínez-González, E., Masi, S., Massardi, M., Matarrese, S., Matsumura, T., Matthai, F., Maurin, L., Mazzotta, P., McDonald, A., McEwen, J. D., McGehee, P., Mei, S., Meinhold, P. R., Melchiorri, A., Melin, J. -B., Mendes, L., Menegoni, E., Mennella, A., Migliaccio, M., Mikkelsen, K., Millea, M., Miniscalco, R., Mitra, S., Miville-Deschênes, M. -A., Molinari, D., Moneti, A., Montier, L., Morgante, G., Morisset, N., Mortlock, D., Moss, A., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Natoli, P., Negrello, M., Nesvadba, N. P. H., Netterfield, C. B., Nørgaard-Nielsen, H. U., North, C., Noviello, F., Novikov, D., Novikov, I., O'Dwyer, I. J., Orieux, F., Osborne, S., O'Sullivan, C., Oxborrow, C. A., Paci, F., Pagano, L., Pajot, F., Paladini, R., Pandolfi, S., Paoletti, D., Partridge, B., Pasian, F., Patanchon, G., Paykari, P., Pearson, D., Pearson, T. J., Peel, M., Peiris, H. V., Perdereau, O., Perotto, L., Perrotta, F., Pettorino, V., Piacentini, F., Piat, M., Pierpaoli, E., Pietrobon, D., Plaszczynski, S., Platania, P., Pogosyan, D., Pointecouteau, E., Polenta, G., Ponthieu, N., Popa, L., Poutanen, T., Pratt, G. W., Prézeau, G., Prunet, S., Puget, J. -L., Pullen, A. R., Rachen, J. P., Racine, B., Rahlin, A., Räth, C., Reach, W. T., Rebolo, R., Reinecke, M., Remazeilles, M., Renault, C., Renzi, A., Riazuelo, A., Ricciardi, S., Riller, T., Ringeval, C., Ristorcelli, I., Robbers, G., Rocha, G., Roman, M., Rosset, C., Rossetti, M., Roudier, G., Rowan-Robinson, M., Rubiño-Martín, J. A., Ruiz-Granados, B., Rusholme, B., Salerno, E., Sandri, M., Sanselme, L., Santos, D., Savelainen, M., Savini, G., Schaefer, B. M., Schiavon, F., Scott, D., Seiffert, M. D., Serra, P., Shellard, E. P. S., Smith, K., Smoot, G. F., Souradeep, T., Spencer, L. D., Starck, J. -L., Stolyarov, V., Stompor, R., Sudiwala, R., Sunyaev, R., Sureau, F., Sutter, P., Sutton, D., Suur-Uski, A. -S., Sygnet, J. -F., Tauber, J. A., Tavagnacco, D., Taylor, D., Terenzi, L., Texier, D., Toffolatti, L., Tomasi, M., Torre, J. -P., Tristram, M., Tucci, M., Tuovinen, J., Türler, M., Tuttlebee, M., Umana, G., Valenziano, L., Valiviita, J., Van Tent, B., Varis, J., Vibert, L., Viel, M., Vielva, P., Villa, F., Vittorio, N., Wade, L. A., Wandelt, B. D., Watson, C., Watson, R., Wehus, I. K., Welikala, N., Weller, J., White, M., White, S. D. M., Wilkinson, A., Winkel, B., Xia, J. -Q., Yvon, D., Zacchei, A., Zibin, J. P., and Zonca, A.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The ESA's Planck satellite, dedicated to studying the early Universe and its subsequent evolution, was launched 14 May 2009 and has been scanning the microwave and submillimetre sky continuously since 12 August 2009. This paper gives an overview of the mission and its performance, the processing, analysis, and characteristics of the data, the scientific results, and the science data products and papers in the release. The science products include maps of the CMB and diffuse extragalactic foregrounds, a catalogue of compact Galactic and extragalactic sources, and a list of sources detected through the SZ effect. The likelihood code used to assess cosmological models against the Planck data and a lensing likelihood are described. Scientific results include robust support for the standard six-parameter LCDM model of cosmology and improved measurements of its parameters, including a highly significant deviation from scale invariance of the primordial power spectrum. The Planck values for these parameters and others derived from them are significantly different from those previously determined. Several large-scale anomalies in the temperature distribution of the CMB, first detected by WMAP, are confirmed with higher confidence. Planck sets new limits on the number and mass of neutrinos, and has measured gravitational lensing of CMB anisotropies at greater than 25 sigma. Planck finds no evidence for non-Gaussianity in the CMB. Planck's results agree well with results from the measurements of baryon acoustic oscillations. Planck finds a lower Hubble constant than found in some more local measures. Some tension is also present between the amplitude of matter fluctuations derived from CMB data and that derived from SZ data. The Planck and WMAP power spectra are offset from each other by an average level of about 2% around the first acoustic peak.

Published
2013
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4. Planck early results. VI. The High Frequency Instrument data processing

Author

Planck HFI Core Team, Ade, P. A. R., Aghanim, N., Ansari, R., Arnaud, M., Ashdown, M., Aumont, J., Banday, A. J., Bartelmann, M., Bartlett, J. G., Battaner, E., Benabed, K., Benoît, A., Bernard, J. -P., Bersanelli, M., Bock, J. J., Bond, J. R., Borrill, J., Bouchet, F. R., Boulanger, F., Bradshaw, T., Bucher, M., Cardoso, J. -F., Castex, G., Catalano, A., Challinor, A., Chamballu, A., Chary, R. -R., Chen, X., Chiang, C., Church, S., Clements, D. L., Colley, J. -M., Colombi, S., Couchot, F., Coulais, A., Cressiot, C., Crill, B. P., Crook, M., de Bernardis, P., Delabrouille, J., Delouis, J. -M., Désert, F. -X., Dolag, K., Dole, H., Doré, O., Douspis, M., Dunkley, J., Efstathiou, G., Filliard, C., Forni, O., Fosalba, P., Ganga, K., Giard, M., Girard, D., Giraud-Héraud, Y., Gispert, R., Górski, K. M., Gratton, S., Griffin, M., Guyot, G., Haissinski, J., Harrison, D., Helou, G., Henrot-Versillé, S., Hernández-Monteagudo, C., Hildebrandt, S. R., Hills, R., Hivon, E., Hobson, M., Holmes, W. A., Huffenberger, K. M., Jaffe, A. H., Jones, W. C., Kaplan, J., Kneissl, R., Knox, L., Kunz, M., Lagache, G., Lamarre, J. -M., Lange, A. E., Lasenby, A., Lavabre, A., Lawrence, C. R., Jeune, M. Le, Leroy, C., Lesgourgues, J., Lewis, A., Macías-Pérez, J. F., MacTavish, C. J., Maffei, B., Mandolesi, N., Mann, R., Marleau, F., Marshall, D. J., Masi, S., Matsumura, T., McAuley, I., McGehee, P., Melin, J. -B., Mercier, C., Mitra, S., Miville-Deschênes, M. -A., Moneti, A., Montier, L., Mortlock, D., Murphy, A., Nati, F., Netterfield, C. B., Nørgaard-Nielsen, H. U., North, C., Noviello, F., Novikov, D., Osborne, S., Pajot, F., Patanchon, G., Peacocke, T., Pearson, T. J., Perdereau, O., Perotto, L., Piacentini, F., Piat, M., Plaszczynski, S., Pointecouteau, E., Ponthieu, N., Prézeau, G., Prunet, S., Puget, J. -L., Reach, W. T., Remazeilles, M., Renault, C., Riazuelo, A., Ristorcelli, I., Rocha, G., Rosset, C., Roudier, G., Rowan-Robinson, M., Rusholme, B., Saha, R., Santos, D., Savini, G., Schaefer, B. M., Shellard, P., Spencer, L., Starck, J. -L., Stolyarov, V., Stompor, R., Sudiwala, R., Sunyaev, R., Sutton, D., Sygnet, J. -F., Tauber, J. A., Thum, C., Torre, J. -P., Touze, F., Tristram, M., Van Leeuwen, F., Vibert, L., Vibert, D., Wandelt, B. D., White, S. D. M., Wiesemeyer, H., Woodcraft, A., Yurchenko, V., Yvon, D., and Zacchei, A.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We describe the processing of the 336 billion raw data samples from the High Frequency Instrument (HFI) which we performed to produce six temperature maps from the first 295 days of Planck-HFI survey data. These maps provide an accurate rendition of the sky emission at 100, 143, 217, 353, 545 and 857 GHz with an angular resolution ranging from 9.9 to 4.4^2. The white noise level is around 1.5 {\mu}K degree or less in the 3 main CMB channels (100--217GHz). The photometric accuracy is better than 2% at frequencies between 100 and 353 GHz and around 7% at the two highest frequencies. The maps created by the HFI Data Processing Centre reach our goals in terms of sensitivity, resolution, and photometric accuracy. They are already sufficiently accurate and well-characterised to allow scientific analyses which are presented in an accompanying series of early papers. At this stage, HFI data appears to be of high quality and we expect that with further refinements of the data processing we should be able to achieve, or exceed, the science goals of the Planck project., Comment: Replaced by the accepted version for publication, as part of a package of papers describing first results of the Planck mission The paper with figures at full resolution and full color tables can also be downloaded from the ESA site http://www.rssd.esa.int/Planck

Published
2011
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5. Planck Early Results. VII. The Early Release Compact Source Catalog

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., Bartlett, J. G., Battaner, E., Benabed, K., Benoît, A., Bernard, J. -P., Bersanelli, M., Bhatia, R., Bonaldi, A., Bonavera, L., Bond, J. R., Borrill, J., Bouchet, F. R., Bucher, M., Burigana, C., Butler, R. C., Cabella, P., Cantalupo, C. M., Cappellini, B., Cardoso, J. -F., Carvalho, P., Catalano, A., Cayón, L., Challinor, A., Chamballu, A., Chary, R. -R., Chen, X., Chiang, L. -Y, Chiang, C., Christensen, P. R., Clements, D. L., Colombi, S., Couchot, F., Coulais, A., Crill, B. P., Cuttaia, F., Danese, L., Davis, R. J., de Bernardis, P., de Rosa, A., de Zotti, G., Delabrouille, J., Delouis, J. -M., Désert, F. -X., Dickinson, C., Diego, J. M., Dolag, K., Dole, H., Donzelli, S., Doré, O., Dörl, U., Douspis, M., Dupac, X., Efstathiou, G., Enßlin, T. A., Eriksen, H. K., Finelli, F., Forni, O., Fosalba, P., Frailis, M., Franceschi, E., Galeotta, S., Ganga, K., Giard, M., Giraud-Héraud, Y., González-Nuevo, J., Górski, K. M., Gratton, S., Gregorio, A., Gruppuso, A., Haissinski, J., Hansen, F. K., Harrison, D., Helou, G., Henrot-Versillé, S., Hernández-Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hornstrup, A., Hovest, W., Hoyland, R. J., Huffenberger, K. M., Huynh, 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., Lähteenmäki, A., Lamarre, J. -M., Lasenby, A., Laureijs, R. J., Lawrence, C. R., Leach, S., Leahy, J. P., Leonardi, R., León-Tavares, J., Leroy, C., Lilje, P. B., Linden-Vørnle, M., López-Caniego, M., Lubin, P. M., Macías-Pérez, J. F., MacTavish, C. J., Maffei, B., Maggio, G., Maino, D., Mandolesi, N., Mann, R., Maris, M., Marleau, F., Marshall, D. J., Martínez-González, E., Masi, S., Massardi, M., Matarrese, S., Matthai, F., Mazzotta, P., McGehee, P., Meinhold, P. R., 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., O'Dwyer, I. J., Osborne, S., Pajot, F., Paladini, R., Partridge, B., Pasian, F., Patanchon, G., Pearson, T. J., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Piffaretti, R., Plaszczynski, S., Platania, P., Pointecouteau, E., Polenta, G., Ponthieu, N., Poutanen, T., Pratt, G. W., Prézeau, G., Prunet, S., Puget, J. -L., Rachen, J. P., Reach, W. T., Rebolo, R., Reinecke, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Rowan-Robinson, M., Rubiño-Martín, J. A., Rusholme, B., Sajina, A., 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., Tavagnacco, D., Terenzi, L., Toffolatti, L., Tomasi, M., Torre, J. -P., Tristram, M., Tuovinen, J., Türler, M., Umana, G., Valenziano, L., Valiviita, J., Varis, J., Vielva, P., Villa, F., Vittorio, N., Wade, L. A., Wandelt, B. D., White, S. D. M., Wilkinson, A., Yvon, D., Zacchei, A., and Zonca, A.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Solar and Stellar Astrophysics
Abstract

(Abridged) A brief description of the methodology of construction, contents and usage of the Planck Early Release Compact Source Catalogue (ERCSC), including the Early Cold Cores (ECC) and the Early Sunyaev-Zeldovich (ESZ) cluster catalogue is provided. The catalogue is based on data that consist of mapping the entire sky once and 60% of the sky a second time by Planck, thereby comprising the first high sensitivity radio/submillimetre observations of the entire sky. A Monte-Carlo algorithm based on the injection and extraction of artificial sources into the Planck maps was implemented to select reliable sources among all extracted candidates such that the cumulative reliability of the catalogue is >=90%. The 10sigma photometric flux density limit of the catalogue at |b|>30 deg is 0.49, 1.0, 0.67, 0.5, 0.33, 0.28, 0.25, 0.47 and 0.82 Jy at each of the nine frequencies between 30 and 857 GHz. Sources which are up to a factor of ~2 fainter than this limit, and which are present in "clean" regions of the Galaxy where the sky background due to emission from the interstellar medium is low, are included in the ERCSC if they meet the high reliability criterion. The Planck ERCSC sources have known associations to stars with dust shells, stellar cores, radio galaxies, blazars, infrared luminous galaxies and Galactic interstellar medium features. A significant fraction of unclassified sources are also present in the catalogs. In addition, two early release catalogs that contain 915 cold molecular cloud core candidates and 189 SZ cluster candidates that have been generated using multi-frequency algorithms are presented. The entire source list, with more than 15000 unique sources, is ripe for follow-up characterisation with Herschel, ATCA, VLA, SOFIA, ALMA and other ground-based observing facilities., Comment: Updated to match A&A press version

Published
2011
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6. Planck early results: first assessment of the High Frequency Instrument in-flight performance

Author

Planck HFI Core Team, Ade, P. A. R., Aghanim, N., Ansari, R., Arnaud, M., Ashdown, M., Aumont, J., Banday, A. J., Bartelmann, M., Bartlett, J. G., Battaner, E., Benabed, K., Benot, A., Bernard, J. -P., Bersanelli, M., Bhatia, R., Bock, J. J., Bond, J. R., Borrill, J., Bouchet, F. R., Boulanger, F., Bradshaw, T., Brelle, E., Bucher, M., Camus, P., Cardoso, J. -F., Catalano, A., Challinor, A., Chamballu, A., Charra, J., Charra, M., Chary, R. -R., Chiang, C., Church, S., Clements, D. L., Colombi, S., Couchot, F., Coulais, A., Cressiot, C., Crill, B. P., Crook, M., de Bernardis, P., Delabrouille, J., Delouis, J. -M., Désert, F. -X., Dolag, K., Dole, H., Doré, O., Douspis, M., Efstathiou, G., Eng, P., Filliard, C., Forni, O., Fosalba, P., Fourmond, J. -J., Ganga, K., Giard, M., Girard, D., Giraud-Héraud, Y., Gispert, R., Gorski, K. M., Gratton, S., Griffin, M., Guyot, G., Haissinski, J., Harrison, D., Helou, G., Henrot-Versillé, S., Hernandez-Monteagudo, C., Hildebrandt, S. R., Hills, R., Hivon, E., Hobson, M., Holmes, W. A., Huenberger, K. M., Jae, A. H., Jones, W. C., Kaplan, J., Kneissl, R., Knox, L., Lagache, G., Lamarre, J. -M., Lami, P., Lange, A. E., Lasenby, A., Lavabre, A., Lawrence, C. R., Leriche, B., Leroy, C., Longval, Y., Macas-Perez, J. F., Maciaszek, T., MacTavish, C. J., Maei, B., Mandolesi, N., Mann, R., Mansoux, B., Masi, S., Matsumura, T., McGehee, P., Melin, J. -B., Mercier, C., Miville-Deschnes, M. -A., Moneti, A., Montier, L., Mortlock, D., Murphy, A., Nati, F., Nettereld, C. B., Norgaard-Nielsen, H. U., North, C., Noviello, F., Novikov, D., Osborne, S., Paine, C., Pajot, F., Patanchon, G., Peacocke, T., Pearson, T. J., Perdereau, O., Perotto, L., Piacentini, F., Piat, M., Plaszczynski, S., Pointecouteau, E., Pons, R., Ponthieu, N., Prezeau, G., Prunet, S., Puget, J. -L., Reach, W. T., Renault, C., Ristorcelli, I., Rocha, G., Rosset, C., Roudier, G., Rowan-Robinson, M., Rusholme, B., Santos, D., Savini, G., Schaefer, B. M., Shellard, P., Spencer, L., Starck, J. -L., Stassi, P., Stolyarov, V., Stompor, R., Sudiwala, R., Sunyaev, R., Sygnet, J. -F., Tauber, J. A., Thum, C., Torre, J. -P., Touze, F., Tristram, M., Van Leeuwen, F., Vibert, L., Vibert, D., Wade, L. A., Wandelt, B. D., White, S. D. M., Wiesemeyer, H., Woodcraft, A., Yurchenko, V., Yvon, D., and Zacchei, A.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The Planck High Frequency Instrument (HFI) is designed to measure the temperature and polarization anisotropies of the Cosmic Microwave Background and galactic foregrounds in six wide bands centered at 100, 143, 217, 353, 545 and 857 GHz at an angular resolution of 10' (100 GHz), 7' (143 GHz), and 5' (217 GHz and higher). HFI has been operating flawlessly since launch on 14 May 2009. The bolometers cooled to 100 mK as planned. The settings of the readout electronics, such as the bolometer bias current, that optimize HFI's noise performance on orbit are nearly the same as the ones chosen during ground testing. Observations of Mars, Jupiter, and Saturn verified both the optical system and the time response of the detection chains. The optical beams are close to predictions from physical optics modeling. The time response of the detection chains is close to pre-launch measurements. The detectors suffer from an unexpected high flux of cosmic rays related to low solar activity. Due to the redundancy of Planck's observations strategy, the removal of a few percent of data contaminated by glitches does not affect significantly the sensitivity. The cosmic rays heat up significantly the bolometer plate and the modulation on periods of days to months of the heat load creates a common drift of all bolometer signals which do not affect the scientific capabilities. Only the high energy cosmic rays showers induce inhomogeneous heating which is a probable source of low frequency noise., Comment: Submitted to A&A. 22 pages, 6 tables, 21 figures. One of a set of simultaneous papers for the Planck Mission

Published
2011
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7. Planck Early Results: The Planck mission

Author

Planck Collaboration, Ade, P. A. R., Aghanim, N., Arnaud, M., Ashdown, M., Aumont, J., Baccigalupi, C., Baker, M., Balbi, A., Banday, A. J., Barreiro, R. B., Bartlett, J. G., Battaner, E., Benabed, K., Bennett, K., Benoît, A., Bernard, J. -P., Bersanelli, M., Bhatia, R., Bock, J. J., Bonaldi, A., Bond, J. R., Borrill, J., Bouchet, F. R., Bradshaw, T., Bremer, M., Bucher, M., Burigana, C., Butler, R. C., Cabella, P., Cantalupo, C. M., Cappellini, B., Cardoso, J. -F., Carr, R., Casale, M., Catalano, A., Cayón, L., Challinor, A., Chamballu, A., Charra, J., Chary, R. -R., Chiang, L. -Y, Chiang, C., Christensen, P. R., Clements, D. L., Colombi, S., Couchot, F., Coulais, A., Crill, B. P., Crone, G., Crook, M., Cuttaia, F., Danese, L., D'Arcangelo, O., Davies, R. D., Davis, R. J., de Bernardis, P., de Bruin, J., de Gasperis, G., de Rosa, A., de Zotti, G., Delabrouille, J., Delouis, J. -M., Dèsert, F. -X., Dick, J., Dickinson, C., Dolag, K., Dole, H., Donzelli, S., Dorè, O., Dörl, U., Douspis, M., Dupac, X., Efstathiou, G., Enfllin, T. A., Eriksen, H. K., Finelli, F., Foley, S., Forni, O., Fosalba, P., Frailis, M., Franceschi, E., Freschi, M., Gaier, T. C., Galeotta, S., Gallegos, J., Gandolfo, B., Ganga, K., Giard, M., Giardino, G., Gienger, G., Giraud-Hèraud, Y., González, J., González-Nuevo, J., Górski, K. M., Gratton, S., Gregorio, A., Gruppuso, A., Guyot, G., Haissinski, J., Hansen, F. K., Harrison, D., Helou, G., Henrot-Versillè, S., Hernández-Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hornstrup, A., Hovest, W., Hoyland, R. J., Huffenberger, K. M., Jaffe, A. H., Jagemann, T., Jones, W. C., Juillet, J. J., Juvela, M., Kangaslahti, P., Keihänen, E., Keskitalo, R., Kisner, T. S., Kneissl, R., Knox, L., Krassenburg, M., Kurki-Suonio, H., Lagache, G., Lähteenmäki, A., Lamarre, J. -M., Lange, A. E., Lasenby, A., Laureijs, R. J., Lawrence, C. R., Leach, S., Leahy, J. P., Leonardi, R., Leroy, C., Lilje, P. B., Linden-Vørnle, M., López-Caniego, M., Lowe, S., Lubin, P. M., Macìas-Pèrez, J. F., Maciaszek, T., MacTavish, C. J., Maffei, B., Maino, D., Mandolesi, N., Mann, R., Maris, M., Martìnez-González, E., Masi, S., Massardi, M., Matarrese, S., Matthai, F., Mazzotta, P., McDonald, A., McGehee, P., Meinhold, P. R., Melchiorri, A., Melin, J. -B., Mendes, L., Mennella, A., Mevi, C., Miniscalco, R., Mitra, S., Miville-Deschínes, M. -A., Moneti, A., Montier, L., Morgante, G., Morisset, N., Mortlock, D., Munshi, D., Murphy, A., Naselsky, P., Natoli, P., Netterfield, C. B., Nørgaard-Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., O'Dwyer, I. J., Ortiz, I., Osborne, S., Osuna, P., Oxborrow, C. A., Pajot, F., Paladini, R., Partridge, B., Pasian, F., Passvogel, T., Patanchon, G., Pearson, D., Pearson, T. J., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Pierpaoli, E., Plaszczynski, S., Platania, P., Pointecouteau, E., Polenta, G., Ponthieu, N., Popa, L., Poutanen, T., Prèzeau, G., Prunet, S., Puget, J. -L., Rachen, J. P., Reach, W. T., Rebolo, R., Reinecke, M., Reix, J. -M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Rowan-Robinson, M., Rubiñ-Martìn, J. A., Rusholme, B., Salerno, E., Sandri, M., Santos, D., Savini, G., Schaefer, B. M., Scott, D., Seiffert, M. D., Shellard, P., Simonetto, A., Smoot, G. F., Sozzi, C., Starck, J. -L., Sternberg, J., Stivoli, F., Stolyarov, V., Stompor, R., Stringhetti, L., Sudiwala, R., Sunyaev, R., Sygnet, J. -F., Tapiador, D., Tauber, J. A., Tavagnacco, D., Taylor, D., Terenzi, L., Texier, D., Toffolatti, L., Tomasi, M., Torre, J. -P., Tristram, M., Tuovinen, J., Türler, M., Tuttlebee, M., Umana, G., Valenziano, L., Valiviita, J., Varis, J., Vibert, L., Vielva, P., Villa, F., Vittorio, N., Wade, L. A., Wandelt, B. D., Watson, C., White, S. D. M., White, M., Wilkinson, A., Yvon, D., Zacchei, A., and Zonca, A.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies
Abstract

The European Space Agency's Planck satellite was launched on 14 May 2009, and has been surveying the sky stably and continuously since 13 August 2009. Its performance is well in line with expectations, and it will continue to gather scientific data until the end of its cryogenic lifetime. We give an overview of the history of Planck in its first year of operations, and describe some of the key performance aspects of the satellite. This paper is part of a package submitted in conjunction with Planck's Early Release Compact Source Catalogue, the first data product based on Planck to be released publicly. The package describes the scientific performance of the Planck payload, and presents results on a variety of astrophysical topics related to the sources included in the Catalogue, as well as selected topics on diffuse emission., Comment: This is part of a package of Planck papers labelled in their titles as "Planck Early Results". The whole package can also be downloaded from http://www.rssd.esa.int/Planck. This paper was accepted by Astronomy & Astrophysics on 31 May 2011

Published
2011
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8. Planck pre-launch status: High Frequency Instrument polarization calibration

Author

Rosset, C., Tristram, M., Ponthieu, N., Ade, P., Catalano, A., Conversi, L., Couchot, F., Crill, B. P., Désert, F. -X., Ganga, K., Giard, M., Giraud-Héraud, Y., Haïssinski, J., Henrot-Versillé, S., Holmes, W., Jones, W. C., Lamarre, J. -M., Lange, A., Leroy, C., Macías-Pérez, J., Maffei, B., de Marcillac, P., Miville-Deschênes, M. -A., Montier, L., Noviello, F., Pajot, F., Perdereau, O., Piacentini, F., Piat, M., Plaszczynski, S., Pointecouteau, E., Puget, J. -L., Ristorcelli, I., Savini, G., Sudiwala, R., Veneziani, M., and Yvon, D.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

The High Frequency Instrument of Planck will map the entire sky in the millimeter and sub-millimeter domain from 100 to 857 GHz with unprecedented sensitivity to polarization ($\Delta P/T_{\tiny cmb} \sim 4\cdot 10^{-6}$) at 100, 143, 217 and 353 GHz. It will lead to major improvements in our understanding of the Cosmic Microwave Background anisotropies and polarized foreground signals. Planck will make high resolution measurements of the $E$-mode spectrum (up to $\ell \sim 1500$) and will also play a prominent role in the search for the faint imprint of primordial gravitational waves on the CMB polarization. This paper addresses the effects of calibration of both temperature (gain) and polarization (polarization efficiency and detector orientation) on polarization measurements. The specific requirements on the polarization parameters of the instrument are set and we report on their pre-flight measurement on HFI bolometers. We present a semi-analytical method that exactly accounts for the scanning strategy of the instrument as well as the combination of different detectors. We use this method to propagate errors through to the CMB angular power spectra in the particular case of Planck-HFI, and to derive constraints on polarization parameters. We show that in order to limit the systematic error to 10% of the cosmic variance of the $E$-mode power spectrum, uncertainties in gain, polarization efficiency and detector orientation must be below 0.15%, 0.3% and 1\deg\ respectively. Pre-launch ground measurements reported in this paper already fulfill these requirements., Comment: accepted by Astronomy&Astrophysics

Published
2010
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9. The EROS2 search for microlensing events towards the spiral arms: the complete seven season results

Author

Rahal, Y. R., Afonso, C., Albert, J. -N., Andersen, J., Ansari, R., Aubourg, E., Bareyre, P., Beaulieu, J. -P., Charlot, X., Couchot, F., Coutures, C., Derue, F., Ferlet, R., Fouqué, P., Glicenstein, J. -F., Goldman, B., Gould, A., Graff, D., Gros, M., Haissinski, J., Hamadache, C., de Kat, J., Lesquoy, E., Loup, C., Guillou, L. Le, Magneville, C., Mansoux, B., Marquette, J. -B., Maurice, E., Maury, A., Milsztajn, A., Moniez, M., Palanque-Delabrouille, N., Perdereau, O., Rahvar, S., Rich, J., Spiro, M., Tisserand, P., and Vidal-Madjar, A.

Subjects
Astrophysics - Astrophysics of Galaxies
Abstract

The EROS-2 project has been designed to search for microlensing events towards any dense stellar field. The densest parts of the Galactic spiral arms have been monitored to maximize the microlensing signal expected from the stars of the Galactic disk and bulge. 12.9 million stars have been monitored during 7 seasons towards 4 directions in the Galactic plane, away from the Galactic center. A total of 27 microlensing event candidates have been found. Estimates of the optical depths from the 22 best events are provided. A first order interpretation shows that simple Galactic models with a standard disk and an elongated bulge are in agreement with our observations. We find that the average microlensing optical depth towards the complete EROS-cataloged stars of the spiral arms is $\bar{\tau} =0.51\pm .13\times 10^{-6}$, a number that is stable when the selection criteria are moderately varied. As the EROS catalog is almost complete up to $I_C=18.5$, the optical depth estimated for the sub-sample of bright target stars with $I_C<18.5$ ($\bar{\tau}=0.39\pm >.11\times 10^{-6}$) is easier to interpret. The set of microlensing events that we have observed is consistent with a simple Galactic model. A more precise interpretation would require either a better knowledge of the distance distribution of the target stars, or a simulation based on a Galactic model. For this purpose, we define and discuss the concept of optical depth for a given catalog or for a limiting magnitude., Comment: 22 pages submitted to Astronomy & Astrophysics

Published
2009
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10. The beat Cepheids in the Magellanic Clouds: an analysis from the EROS-2 database

Author

Marquette, J. B., Beaulieu, J. P., Buchler, J. R., Szabo, R., Tisserand, P., Belghith, S., Fouque, P., Lesquoy, E., Milsztajn, A., Schwarzenberg-Czerny, A., Afonso, C., Albert, J. N., Andersen, J., Ansari, R., Aubourg, E., Bareyre, P., Charlot, X., Coutures, C., Ferlet, R., Glicenstein, J. F., Goldman, B., Gould, A., Graff, D., Gros, M., Haissinski, J., Hamadache, C., de Kat, J., Guillou, L. Le, Loup, C., Magneville, C., Maurice, E., Maury, A., Moniez, M., Palanque-Delabrouille, N., Perdereau, O., Rahal, Y. R., Rich, J., Spiro, M., and Vidal-Madjar, A.

Subjects
Astrophysics - Solar and Stellar Astrophysics
Abstract

A number of microlensing dark-matter surveys have produced tens of millions of light curves of individual background stars. These data provide an unprecedented opportunity for systematic studies of whole classes of variable stars and their host galaxies. We aim to use the EROS-2 survey of the Magellanic Clouds to detect and study the population of beat Cepheids (BCs) in both Clouds. BCs pulsating simultaneously in the first overtone and fundamental modes (FO/F) or in the second and first overtone modes (SO/FO) are of particular interest. Using special software designed to search for periodic variables, we have scanned the EROS-2 data base for variables in the typical period range of Cepheids. Metallicities of FO/F objects were then calculated from linear nonadiabatic convective stellar models. We identify 74 FO/F BCs in the LMC and 41 in the SMC, and 173 and 129 SO/FO pulsators in the LMC and SMC, respectively; 185 of these stars are new discoveries. For nearly all the FO/F objects we determine minimum, mean, and maximum values of the metallicity. The EROS data have expanded the samples of known BCs in the LMC by 31%, in the SMC by 110%. The FO/F objects provide independent measures of metallicities in these galaxies. The mean value of metallicity is 0.0045 in the LMC and 0.0018 in the SMC., Comment: 10 pages, 7 figures, accepted for publication in A&A

Published
2009
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11. Discovery of a peculiar Cepheid-like star towards the northern edge of the Small Magellanic Cloud

Author

Marquette, J. B., Tisserand, P., Francois, P., Beaulieu, J. P., Doublier, V., Lesquoy, E., Milsztajn, A., Pritchard, J., Schwarzenberg-Czerny, A., Afonso, C., Albert, J. N., Andersen, J., Ansari, R., Aubourg, E., Bareyre, P., Charlot, X., Coutures, C., Ferlet, R., Fouque, P., Glicenstein, J. F., Goldman, B., Gould, A., Graff, D., Gros, M., Haissinski, J., Hamadache, C., de Kat, J., Guillou, L. Le, Loup, C., Magneville, C., Maurice, E., Maury, A., Moniez, M., Palanque-Delabrouille, N., Perdereau, O., Rahal, Y. R., Rich, J., Spiro, M., Vidal-Madjar, A., and Zylberajch, S.

Subjects
Astrophysics
Abstract

For seven years, the EROS-2 project obtained a mass of photometric data on variable stars. We present a peculiar Cepheid-like star, in the direction of the Small Magellanic Cloud, which demonstrates unusual photometric behaviour over a short time interval. We report on data of the photometry acquired by the MARLY telescope and spectroscopy from the EFOSC instrument for this star, called EROS2 J005135-714459(sm0060n13842), which resembles the unusual Cepheid HR 7308. The light curve of our target is analysed using the Analysis of Variance method to determine a pulsational period of 5.5675 days. A fit of time-dependent Fourier coefficients is performed and a search for proper motion is conducted. The light curve exhibits a previously unobserved and spectacular change in both mean magnitude and amplitude, which has no clear theoretical explanation. Our analysis of the spectrum implies a radial velocity of 104 km s$^{-1}$ and a metallicity of -0.4$\pm$0.2 dex. In the direction of right ascension, we measure a proper motion of 17.4$\pm$6.0 mas yr$^{-1}$ using EROS astrometry, which is compatible with data from the NOMAD catalogue. The nature of EROS2 J005135-714459(sm0060n13842) remains unclear. For this star, we may have detected a non-zero proper motion for this star, which would imply that it is a foreground object. Its radial velocity, pulsational characteristics, and photometric data, however, suggest that it is instead a Cepheid-like object located in the SMC. In such a case, it would present a challenge to conventional Cepheid models., Comment: Correction of typos in the abstract

Published
2008
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12. Improved Cosmological Constraints from New, Old and Combined Supernova Datasets

Author

Kowalski, M., Rubin, D., Aldering, G., Agostinho, R. J., Amadon, A., Amanullah, R., Balland, C., Barbary, K., Blanc, G., Challis, P. J., Conley, A., Connolly, N. V., Covarrubias, R., Dawson, K. S., Deustua, S. E., Ellis, R., Fabbro, S., Fadeyev, V., Fan, X., Farris, B., Folatelli, G., Frye, B. L., Garavini, G., Gates, E. L., Germany, L., Goldhaber, G., Goldman, B., Goobar, A., Groom, D. E., Haissinski, J., Hardin, D., Hook, I., Kent, S., Kim, A. G., Knop, R. A., Lidman, C., Linder, E. V., Mendez, J., Meyers, J., Miller, G. J., Moniez, M., Mourao, A. M., Newberg, H., Nobili, S., Nugent, P. E., Pain, R., Perdereau, O., Perlmutter, S., Phillips, M. M., Prasad, V., Quimby, R., Regnault, N., Rich, J., Rubenstein, E. P., Ruiz-Lapuente, P., Santos, F. D., Schaefer, B. E., Schommer, R. A., Smith, R. C., Soderberg, A. M., Spadafora, A. L., Strolger, L. -G., Strovink, M., Suntzeff, N. B., Suzuki, N., Thomas, R. C., Walton, N. A., Wang, L., Wood-Vasey, W. M., and Yun, J. L.

Subjects
Astrophysics
Abstract

We present a new compilation of Type Ia supernovae (SNe Ia), a new dataset of low-redshift nearby-Hubble-flow SNe and new analysis procedures to work with these heterogeneous compilations. This ``Union'' compilation of 414 SN Ia, which reduces to 307 SNe after selection cuts, includes the recent large samples of SNe Ia from the Supernova Legacy Survey and ESSENCE Survey, the older datasets, as well as the recently extended dataset of distant supernovae observed with HST. A single, consistent and blind analysis procedure is used for all the various SN Ia subsamples, and a new procedure is implemented that consistently weights the heterogeneous data sets and rejects outliers. We present the latest results from this Union compilation and discuss the cosmological constraints from this new compilation and its combination with other cosmological measurements (CMB and BAO). The constraint we obtain from supernovae on the dark energy density is $\Omega_\Lambda= 0.713^{+0.027}_{-0.029} (stat)}^{+0.036}_{-0.039} (sys)}$, for a flat, LCDM Universe. Assuming a constant equation of state parameter, $w$, the combined constraints from SNe, BAO and CMB give $w=-0.969^{+0.059}_{-0.063}(stat)^{+0.063}_{-0.066} (sys)$. While our results are consistent with a cosmological constant, we obtain only relatively weak constraints on a $w$ that varies with redshift. In particular, the current SN data do not yet significantly constrain $w$ at $z>1$. With the addition of our new nearby Hubble-flow SNe Ia, these resulting cosmological constraints are currently the tightest available., Comment: 49 pages, 17 figures; accepted for publication in Astrophysical Journal. For data tables, code for cosmological analysis and full-resolution figures, see http://supernova.lbl.gov/Union

Published
2008
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13. R Coronae Borealis stars in the Galactic Bulge discovered by EROS-2

Author

Tisserand, P., Marquette, J. B., Wood, P. R., Lesquoy, E., Beaulieu, J. P., Milsztajn, A., Hamadache, C., Afonso, C., Albert, J. N., Andersen, J., Ansari, R., Aubourg, E., Bareyre, P., Charlot, X., Coutures, C., Ferlet, R., Fouqué, P., Glicenstein, J. F., Goldman, B., Gould, A., Gros, M., Haissinski, J., de Kat, J., Guillou, L. Le, Loup, C., Magneville, C., Maurice, E., Maury, A., Moniez, M., Palanque-Delabrouille, N., Perdereau, O., Rahal, Y., Rich, J., Spiro, M., Vidal-Madjar, A., and Zylberajch, S.

Subjects
Astrophysics
Abstract

Rare types of variable star may give unique insight into short-lived stages of stellar evolution. The systematic monitoring of millions of stars and advanced light curve analysis techniques of microlensing surveys make them ideal for discovering also such rare variable stars. One example is the R Coronae Borealis (RCB) stars, a rare type of evolved carbon-rich supergiant. We have conducted a systematic search of the EROS-2 database for the Galactic catalogue Bulge and spiral arms to find Galactic RCB stars. The light curves of $\sim$100 million stars, monitored for 6.7 years (from July 1996 to February 2003), have been analysed to search for the main signature of RCB stars, large and rapid drops in luminosity. Follow-up spectroscopy has been used to confirm the photometric candidates. We have discovered 14 new RCB stars, all in the direction of the Galactic Bulge, bringing the total number of confirmed Galactic RCB stars to about 51. After reddening correction, the colours and absolute magnitudes of at least 9 of the stars are similar to those of Magellanic RCB stars. This suggests that these stars are in fact located in the Galactic Bulge, making them the first RCB stars discovered in the Bulge. The localisation of the 5 remaining RCBs is more uncertain: 4 are either located behind the Bulge at an estimated maximum distance of 14 kpc or have an unusual thick circumstellar shell; the other is a DY Per RCB which may be located in the Bulge, even if it is fainter than the known Magellanic DY Per. From the small scale height found using the 9 new Bulge RCBs, $61

Published
2008
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14. About the connection between vacuum birefringence and the light-light scattering amplitude

Author

Haissinski, J., Dagoret, S., Urban, M., and Zomer, F.

Subjects
Physics - General Physics
Abstract

Birefringence phenomena stemming from vacuum polarization are revisited in the framework of coherent scattering. Based on photon-photon scattering, our analysis brings out the direct connection between this process and vacuum birefringence. We show how this procedure can be extended to the Kerr and the Cotton-Mouton birefringences in vacuum, thus providing a unified treatment of various polarization schemes, including those involving static fields.

Published
2006
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15. Limits on the Macho Content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds

Author

Tisserand, P., Guillou, L. Le, Afonso, C., Albert, J. N., Andersen, J., Ansari, R., Aubourg, E., Bareyre, P., Beaulieu, J. P., Charlot, X., Coutures, C., Ferlet, R., Fouqué, P., Glicenstein, J. F., Goldman, B., Gould, A., Graff, D., Gros, M., Haissinski, J., Hamadache, C., de Kat, J., Lasserre, T., Lesquoy, E., Loup, C., Magneville, C., Marquette, J. B., Maurice, E., Maury, A., Milsztajn, A., Moniez, M., Palanque-Delabrouille, N., Perdereau, O., Rahal, Y. R., Rich, J., Spiro, M., Vidal-Madjar, A., Vigroux, L., and Zylberajch, S.

Subjects
Astrophysics
Abstract

The EROS-2 project was designed to test the hypothesis that massive compact halo objects (the so-called ``machos'') could be a major component of the dark matter halo of the Milky Way galaxy. To this end, EROS-2 monitored over 6.7 years $33\times10^6$ stars in the Magellanic clouds for microlensing events caused by such objects. In this work, we use only a subsample of $7\times10^6$ bright stars spread over $84 \deg^2$ of the LMC and $9 \deg^2$ of the SMC. The strategy of using only bright stars helps to discriminate against background events due to variable stars and allows a simple determination of the effects of source confusion (blending). The use of a large solid angle makes the survey relatively insensitive to effects that could make the optical depth strongly direction dependent. Using this sample of bright stars, only one candidate event was found, whereas $\sim39$ events would have been expected if the Halo were entirely populated by objects of mass $M\sim0.4M_{\odot}$. Combined with the results of EROS-1, this implies that the optical depth toward the Large Magellanic Cloud (\object{LMC}) due to such lenses is $\tau<0.36\times10^{-7}$ (95%CL), corresponding to a fraction of the halo mass of less than 8%. This optical depth is considerably less than that measured by the MACHO collaboration in the central region of the LMC. More generally, machos in the mass range $0.6\times10^{-7}M_\odot

Published
2006
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16. Galactic Bulge Microlensing Optical Depth from EROS-2

Author

Hamadache, C., Guillou, L. Le, Tisserand, P., Afonso, C., Albert, J. N., Andersen, J., Ansari, R., Aubourg, E., Bareyre, P., Beaulieu, J. P., Charlot, X., Coutures, C., Ferlet, R., Fouqué, P., Glicenstein, J. F., Goldman, B., Gould, A., Graff, D., Gros, M., Haissinski, J., de Kat, J., Lesquoy, E., Loup, C., Magneville, C., Marquette, J. B., Maurice, E., Maury, A., Milsztajn, A., Moniez, M., Palanque-Delabrouille, N., Perdereau, O., Rahal, Y. R., Rich, J., Spiro, M., Vidal-Madjar, A., Vigroux, L., and Zylberajch, S.

Subjects
Astrophysics
Abstract

We present a new EROS-2 measurement of the microlensing optical depth toward the Galactic Bulge. Light curves of $5.6\times 10^{6}$ clump-giant stars distributed over $66 \deg^2$ of the Bulge were monitored during seven Bulge seasons. 120 events were found with apparent amplifications greater than 1.6 and Einstein radius crossing times in the range $5 {\rm d}

Published
2006
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17. Spectroscopic Observations and Analysis of the Unusual Type Ia SN 1999ac

Author

Project, The Supernova Cosmology, Garavini, G., Aldering, G., Amadon, A., Amanullah, R., Astier, P., Balland, C., Blanc, G., Conley, A., Dahlen, T., Deustua, S. E., Fabbro, R. Ellis S., Fadeyev, V., Fan, X., Folatelli, G., Frye, B., Gates, E. L., Gibbons, R., Goldhaber, G., Goldman, B., Goobar, A., Groom, D. E., Haissinski, J., Hardin, D., Hook, I., Howell, D. A., Kent, S., Kim, A. G., Knop, R. A., Kowalski, M., Kuznetsova, N., Lidman, B. C. Lee C., Mendez, J., Miller, G. J., Moniez, M., Mouchet, M., Mourao, A., Newberg, H., Nobili, S., Nugent, P. E., Pain, R., Perdereau, O., Perlmutter, S., Quimby, R., Regnault, N., Rich, J., Richards, G. T., Ruiz-Lapuente, P., Schaefer, B. E., Schahmaneche, K., Smith, E., Spadafora, A. L., Stanishev, V., Thomas, R. C., Walton, N. A., Wang, L., and Wood-Vasey, W. M.

Subjects
Astrophysics
Abstract

We present optical spectra of the peculiar Type Ia supernova (SN Ia) 1999ac. The data extend from -15 to +42 days with respect to B-band maximum and reveal an event that is unusual in several respects. Prior to B-band maximum, the spectra resemble those of SN 1999aa, a slowly declining event, but possess stronger SiII and CaII signatures (more characteristic of a spectroscopically normal SN). Spectra after B-band maximum appear more normal. The expansion velocities inferred from the Iron lines appear to be lower than average; whereas, the expansion velocity inferred from Calcium H and K are higher than average. The expansion velocities inferred from SiII are among the slowest ever observed, though SN 1999ac is not particularly dim. The analysis of the parameters v_10, R(SiII), dv(SiII)/dt, and d_m15 further underlines the unique characteristics of SN 1999ac. We find convincing evidence of CII 6580 in the day -15 spectrum with ejection velocity v > 16,000 km/s, but this signature disappears by day -9. This rapid evolution at early times highlights the importance of extremely early-time spectroscopy., Comment: 40 pages, 24 figures, accepted for publication in The Astronomical Journal

Published
2005
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18. Type Ia supernova rate at a redshift of ~ 0.1

Author

Blanc, G., Afonso, C., Alard, C., Albert, J. N., Aldering, G., Amadon, A., Andersen, J., Ansari, R., Aubourg, E., Balland, C., Bareyre, P., Beaulieu, J. P., Charlot, X., Conley, A., Coutures, C., Dahlen, T., Derue, F., Fan, X., Ferlet, R., Folatelli, G., Fouque, P., Garavini, G., Glicenstein, J. F., Goldman, B., Goobar, A., Gould, A., Graff, D., Gros, M., Haissinski, J., Hamadache, C., Hardin, D., Hook, I. M., deKat, J., Kent, S., Kim, A., Lasserre, T., LeGuillou, L., Lesquoy, E., Loup, C., Magneville, C., Marquette, J. B., Maurice, E., Maury, A., Milsztajn, A., Moniez, M., Mouchet, M., Newberg, H., Nobili, S., Palanque-Delabrouille, N., Perdereau, O., Prevot, L., Rahal, Y. R., Regnault, N., Rich, J., Ruiz-Lapuente, P., Spiro, M., Tisserand, P., Vidal-Madjar, A., Vigroux, L., Walton, N. A., and Zylberajch, S.

Subjects
Astrophysics
Abstract

We present the type Ia rate measurement based on two EROS supernova search campaigns (in 1999 and 2000). Sixteen supernovae identified as type Ia were discovered. The measurement of the detection efficiency, using a Monte Carlo simulation, provides the type Ia supernova explosion rate at a redshift ~ 0.13. The result is $0.125^{+0.044+0.028}_{-0.034-0.028} h_{70}^2$ SNu where 1 SNu = 1 SN / $10^{10} L_{sun}^B$ / century. This value is compatible with the previous EROS measurement (Hardin et al. 2000), done with a much smaller sample, at a similar redshift. Comparison with other values at different redshifts suggests an evolution of the type Ia supernova rate., Comment: Accepted for publication in Astronomy & Astrophysics (15 pages, 16 figures)

Published
2004
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19. Spectroscopic Observations and Analysis of the Peculiar SN 1999aa

Author

Garavini, G., Folatelli, G., Goobar, A., Nobili, S., Aldering, G., Amadon, A., Amanullah, R., Astier, P., Balland, C., Blanc, G., Burns, M. S., Conley, A., Dahlen, T., Deustua, S. E., Ellis, R., Fabbro, S., Fan, X., Frye, B., Gates, E. L., Gibbons, R., Goldhaber, G., Goldman, B., Groom, D. E., Haissinski, J., Hardin, D., Hook, I. M., Howell, D. A., Kasen, D., Kent, S., Kim, A. G., Knop, R. A., Lee, B. C., Lidman, C., Mendez, J., Miller, G. J., Moniez, M., Mourao, A., Newberg, H., Nugent, P. E., Pain, R., Perdereau, O., Perlmutter, S., Prasad, V., Quimby, R., Raux, J., Regnault, N., Rich, J., Richards, G. T., Ruiz-Lapuente, P., Sainton, G., Schaefer, B. E., Schahmaneche, K., Smith, E., Spadafora, A. L., Stanishev, V., Walton, N. A., Wang, L., and Wood-Vasey, W. M.

Subjects
Astrophysics
Abstract

We present an extensive new time-series of spectroscopic data of the peculiar SN 1999aa in NGC 2595. Our data set includes 25 optical spectra between -11 and +58 days with respect to B-band maximum light, providing an unusually complete time history. The early spectra resemble those of a SN 1991T-like object but with a relatively strong Ca H&K absorption feature. The first clear sign of Si II 6355, characteristic of Type Ia supernovae, is found at day -7 and its velocity remains constant up to at least the first month after B-band maximum light. The transition to normal-looking spectra is found to occur earlier than in SN 1991T suggesting SN 1999aa as a possible link between SN 1991T-like and Branch-normal supernovae. Comparing the observations with synthetic spectra, doubly ionized Fe, Si and Ni are identified at early epochs. These are characteristic of SN 1991T-like objects. Furthermore, in the day -11 spectrum, evidence is found for an absorption feature which could be identified as high velocity C II 6580 or H-alpha. At the same epoch C III 4648.8 at photospheric velocity is probably responsible for the absorption feature at 4500 A. High velocity Ca is found around maximum light together with Si II and Fe II confined in a narrow velocity window. Implied constraints on supernovae progenitor systems and explosion hydrodynamical models are briefly discussed., Comment: 46 pages including 23 figures. Accepted for publication by AJ. For full-resolution figures see http://www.physto.se/~gabri/sn99aa/

Published
2004
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20. About the connection between the $C_{\ell}$ power spectrum of the Cosmic Microwave Background and the $\Gamma_{m}$ Fourier spectrum of rings on the sky

Author

Ansari, R., Bargot, S., Bourrachot, A., Couchot, F., Haïssinski, J., Henrot-Versillé, S., Meur, G. Le, Perdereau, O., Piat, M., Plaszczynski, S., and Touze, F.

Subjects
Astrophysics
Abstract

In this article we present and study a scaling law of the $m\Gamma_m$ CMB Fourier spectrum on rings which allows us (i) to combine spectra corresponding to different colatitude angles (e.g. several detectors at the focal plane of a telescope), and (ii) to recover the $C_l$ power spectrum once the $\Gamma_m$ coefficients have been measured. This recovery is performed numerically below the 1% level for colatitudes $\Theta> 80^\circ$ degrees. In addition, taking advantage of the smoothness of the $C_l$ and of the $\Gamma_m$, we provide analytical expressions which allow to recover one of the spectrum at the 1% level, the other one being known., Comment: 8 pages, 8 figures

Published
2003
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21. Type Ia supernova rate at $z \sim 0.1$

Author

Hardin, D., Afonso, C., Alard, C., Albert, J. N., Amadon, A., Andersen, J., Ansari, R., Aubourg, É., Bareyre, P., Bauer, F., Beaulieu, J. P., Blanc, G., Bouquet, A., Char, S., Charlot, X., Couchot, F., Coutures, C., Derue, F., Ferlet, R., Glicenstein, J. F., Goldman, B., Gould, A., Graff, D., Gros, M., Haissinski, J., Hamilton, J. C., de Kat, J., Kim, A., Lasserre, T., Lesquoy, É., Loup, C., Magneville, C., Mansoux, B., Marquette, J. B., Maurice, É., Milsztajn, A., Moniez, M., Palanque-Delabrouille, N., Perdereau, O., Prévot, L., Regnault, N., Rich, J., Spiro, M., Vidal-Madjar, A., Vigroux, L., Zylberajch, S., and collaboration, The EROS

Subjects
Astrophysics
Abstract

We present the EROS nearby supernova ($z \sim 0.02 - 0.2$) search and the analysis of the first year of data (1997). A total of 80 square degrees were surveyed. Eight supernov{\ae} were detected, four of which were spectroscopically identified as type Ia supernov{\ae}. The search efficiency was determined with a Monte-Carlo simulation taking into account the efficiencies for both supernova detection and host galaxy identification. Assuming that for a given galaxy the supernova rate is proportional to the galactic luminosity, we compute a type Ia supernova explosion rate of: ${\cal R} = 0.44 {}_{-0.21}^{+0.35} {}_{-0.07}^{+0.13} h^2: / 10^{10} \lbsun / 100 {\rm yrs}$ at an average redshift of $\sim 0.1$ where the errors are respectively statistical and systematic (type misidentification included)., Comment: 8 pages, 6 figures, accepted in A&A

Published
2000

22. The LAL Compton program

Author

Variola, A., Brasile, J.P., Bruni, C., Chehab, R., Chiche, R., Cizeron, R., Couchot, F., Fedala, Y., Haissinski, J., Jacquet, M., Jehanno, D., Lacroix, M., Lepercq, P., Mouton, B., Roux, R., Soskov, V., Vivoli, A., and Zomer, F.

Published
2009
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23. γ, γ Physics at D.C.I.

Author

Brossard, M., Falvard, A., Jousset, J., Michel, B., Montarou, G., Montret, J. C., Reichstadt, P., Courau, A., Haissinski, J., Ehlers, J., editor, Hepp, K., editor, Kippenhahn, R., editor, Weidenmüller, H. A., editor, Zittartz, J., editor, Beiglböck, W., editor, Cochard, Gérard, editor, and Kessler, Paul, editor

Published
1980
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25. An experimental study ofe + e − annihilation into four leptons at $$\sqrt S \geqq 35$$ GeVGeV

Author

Behrend, H. -J., Criegee, L., Dainton, J. B., Field, J. H., Franke, G., Jung, H., Meyer, J., Schröder, V., Winter, G. G., Bussey, P. J., Buttar, C., Campbell, A. J., Hendry, D., McCurrach, G., Scarr, J. M., Skillicorn, I. O., Smith, K. M., Ahme, J., Blobel, V., Brehm, W., Feindt, M., Fenner, H., Harjes, J., Peters, J. H., Podobrin, O., Spitzer, H., Apel, W. -D., Engler, J., Flügge, G., Fries, D. C., Fuster, J., Gabriel, P., Gamerdinger, K., Grosse-Wiesmann, P., Hahn, M., Hädinger, U., Hansmeyer, J., Küster, H., Müller, H., Ranitzsch, K. H., Schneider, H., Seufert, R., de Boer, W., Buschhorn, G., Grindhammer, G., Gunderson, B., Kiesling, Ch., Kotthaus, R., Kroha, H., Lüers, D., Oberlack, H., Schacht, P., Scholz, S., Shooshtari, G., Wiedenmann, W., Davier, M., Fournier, D., Grivaz, J. F., Haïssinski, J., Janot, P., Journé, V., Kim, D. W., Le Diberder, F., Veillet, J. -J., Blohm, K., George, R., Goldberg, M., Hamon, O., Kapusta, F., Poggioli, L., Rivoal, M., D'Agostini, G., Ferrarotto, F., Iacovacci, M., Stella, B., Aleksan, R., Cozzika, G., Ducros, Y., Pierre, F., Alexander, G., Beck, A., Bella, G., Grunhaus, J., Klatchko, A., Levy, A., Milstène, C., and CELLO Collaboration

Published
1989
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26. Photometric constraints on microlens spectroscopy of EROS-BLG-2000-5

Author

Alfonso, C., Albert, J. N., Andersen, J., Ansari, R., Aubourg, É, Bareyre, P., Bauer, F., Blanc, G., Bouquet, A., Char, S., Charlot, X., Couchot, F., Coutures, C., Derue, F., Ferlet, R., Fouqué, P., Glicenstein, J. F., Goldman, B., Gould, A., Graff, D., Gros, M., Haïssinski, J., Hamilton, J. C., Hardin, D., Kat, J., Kim, A., Lasserre, T., Leguillou, L., Lesquoy, É, Loup, C., Magneville, C., Mansoux, B., Marquette, J. B., Maurice, É, Milsztajn, A., Moniez, M., Nathalie Palanque-Delabrouille, Perdereau, O., Prévot, L., Regnault, N., Rich, J., Spiro, M., Vidal-Madjar, A., Vigroux, L., Zylberajch, S., Département d'Astrophysique, de physique des Particules, de physique Nucléaire et de l'Instrumentation Associée (DAPNIA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), 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), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF (institution))-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Departement de recherche SPAtiale (DESPA), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), EROS, 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 Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), and Fouqué, Pascal

Subjects
Physics, Microlens, Photosphere, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], 010308 nuclear & particles physics, Astrophysics (astro-ph), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Radius, Atmospheric model, [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], 01 natural sciences, Spectral line, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 13. Climate action, Space and Planetary Science, [PHYS.ASTR.CO] Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], 0103 physical sciences, Absorption (electromagnetic radiation), Spectroscopy, 010303 astronomy & astrophysics, Chromosphere
Abstract

We apply EROS photometric data to interpret previously published Keck and VLT spectra of the binary-microlens caustic-crossing event EROS-BLG-2000-5. We show that the VLT data imply that the outer 4 % of the limb of the K3-giant source is strongly in emission in Halpha, in contradiction to available models of the photosphere. This conflict could be resolved if the integrated Halpha emission from the chromosphere were equal to 8 % of the integrated Halpha absorption from the source as a whole. These conclusions regarding the extreme limb are almost completely model-independent. We also present a general method for using the photometric data to facilitate direct comparison between the atmospheric model and the spectroscopic data. While this method has some model-dependent features, it is fairly robust and can serve to guide the analysis of spectra while more detailed models of the lens geometry are being developed. In addition, we find that the color of the limb of the source (outer 5.5 % by radius) is Delta(V-I) = 0.37 redder than the source as a whole, so that it has the color of a M0 giant., Comment: 7 figures, 1 table

Published
2001

27. Observation of Microlensing towards the Galactic Spiral Arms: EROS II 3 year survey

Author

Derue, F, Afonso, C, Alard, C, Albert, J N, Andersen, J, Ansari, R, Aubourg, E, Bareyre, P, Bauer, F, Beaulieu, J P, Blanc, G, Bouquet, A, Char, S, Charlot, X, Couchot, F, Coutures, C, Ferlet, R, Fouqué, P, Glicenstein, J F, Goldman, B, Gould, A, Graff, D, Gros, M H, Haïssinski, J, Hamilton, J C, Hardin, D, De Kat, J, Kim, A, Lasserre, T, Le Guillou, Laurent, Lesquoy, E, Loup, C, Magneville, C, Mansoux, B, Marquette, J B, Maurice, E, Milsztajn, A, Moniez, M, Palanque-Delabrouille, Nathalie, Perdereau, O, Prévot, L, Regnault, N, Rich, J, Spiro, Michel, Vidal-Madjar, A, Vigroux, L, and Zylberajch, S

Subjects
Astrophysics and Astronomy
Published
2000

29. Planckpre-launch status: High Frequency Instrument polarization calibration

Author

Rosset, C., primary, Tristram, M., additional, Ponthieu, N., additional, Ade, P., additional, Aumont, J., additional, Catalano, A., additional, Conversi, L., additional, Couchot, F., additional, Crill, B. P., additional, Désert, F.-X., additional, Ganga, K., additional, Giard, M., additional, Giraud-Héraud, Y., additional, Haïssinski, J., additional, Henrot-Versillé, S., additional, Holmes, W., additional, Jones, W. C., additional, Lamarre, J.-M., additional, Lange, A., additional, Leroy, C., additional, Macías-Pérez, J., additional, Maffei, B., additional, de Marcillac, P., additional, Miville-Deschênes, M.-A., additional, Montier, L., additional, Noviello, F., additional, Pajot, F., additional, Perdereau, O., additional, Piacentini, F., additional, Piat, M., additional, Plaszczynski, S., additional, Pointecouteau, E., additional, Puget, J.-L., additional, Ristorcelli, I., additional, Savini, G., additional, Sudiwala, R., additional, Veneziani, M., additional, and Yvon, D., additional

Published
2010
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30. The beat Cepheids in the Magellanic Clouds: an analysis from the EROS-2 database

Author

Marquette, J. B., primary, Beaulieu, J. P., additional, Buchler, J. R., additional, Szabó, R., additional, Tisserand, P., additional, Belghith, S., additional, Fouqué, P., additional, Lesquoy, É., additional, Milsztajn, A., additional, Schwarzenberg-Czerny, A., additional, Afonso, C., additional, Albert, J. N., additional, Andersen, J., additional, Ansari, R., additional, Aubourg, É., additional, Bareyre, P., additional, Charlot, X., additional, Coutures, C., additional, Ferlet, R., additional, Glicenstein, J. F., additional, Goldman, B., additional, Gould, A., additional, Graff, D., additional, Gros, M., additional, Haïssinski, J., additional, Hamadache, C., additional, de Kat, J., additional, Le Guillou, L., additional, Loup, C., additional, Magneville, C., additional, Maurice, É., additional, Maury, A., additional, Moniez, M., additional, Palanque-Delabrouille, N., additional, Perdereau, O., additional, Rahal, Y. R., additional, Rich, J., additional, Spiro, M., additional, and Vidal-Madjar, A., additional

Published
2009
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32. PHASEFIX - correcting the tunes of the SLC arcs

Author

Haïssinski, J, Bambade, P, Brown, K L, Burke, D L, Fieguth, T H, Hutton, A M, Mattison, T S, Murray, J J, Phinney, N, Placidi, Massimo, Sands, M, Sheppard, J C, Toge, N, and Weinstein, A

Subjects
Accelerators and Storage Rings
Published
1990

34. EROS 2 proper motion survey: Constraints on the halo white dwarfs

Author

Goldman, B., primary, Afonso, C., additional, Alard, Ch., additional, Albert, J.-N., additional, Amadon, A., additional, Andersen, J., additional, Ansari, R., additional, Aubourg, É., additional, Bareyre, P., additional, Bauer, F., additional, Beaulieu, J.-Ph., additional, Blanc, G., additional, Bouquet, A., additional, Charlot, X., additional, Couchot, F., additional, Coutures, Ch., additional, Derue, F., additional, Ferlet, R., additional, Fouqué, P., additional, Glicenstein, J.-F., additional, Gould, A., additional, Graff, D., additional, Gros, M., additional, Haïssinski, J., additional, Hamadache, C., additional, Hamilton, J.-Ch., additional, Hardin, D., additional, de Kat, J., additional, Kim, A., additional, Lasserre, Th., additional, Le Guillou, L., additional, Lesquoy, É., additional, Loup, C., additional, Magneville, Ch., additional, Mansoux, B., additional, Marquette, J.-B., additional, Maurice, É., additional, Maury, A., additional, Milsztajn, A., additional, Moniez, M., additional, Palanque-Delabrouille, N., additional, Perdereau, O., additional, Prévot, L., additional, Regnault, N., additional, Rich, J., additional, Spiro, M., additional, Tisserand, P., additional, Vidal-Madjar, A., additional, Vigroux, L., additional, and Zylberajch, S., additional

Published
2002
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35. Observation of microlensing toward the galactic spiral arms. EROS II 3 year survey

Author

Derue, F., primary, Afonso, C., additional, Alard, C., additional, Albert, J.-N., additional, Andersen, J., additional, Ansari, R., additional, Aubourg, É., additional, Bareyre, P., additional, Bauer, F., additional, Beaulieu, J.-P., additional, Blanc, G., additional, Bouquet, A., additional, Char, S., additional, Charlot, X., additional, Couchot, F., additional, Coutures, C., additional, Ferlet, R., additional, Fouqué, P., additional, Glicenstein, J.-F., additional, Goldman, B., additional, Gould, A., additional, Graff, D., additional, Gros, M., additional, Haïssinski, J., additional, Hamilton, J.-C., additional, Hardin, D., additional, de Kat, J., additional, Kim, A., additional, Lasserre, T., additional, Le Guillou, L., additional, Lesquoy, É., additional, Loup, C., additional, Magneville, C., additional, Mansoux, B., additional, Marquette, J.-B., additional, Maurice, É., additional, Milsztajn, A., additional, Moniez, M., additional, Palanque-Delabrouille, N., additional, Perdereau, O., additional, Prévot, L., additional, Regnault, N., additional, Rich, J., additional, Spiro, M., additional, Vidal-Madjar, A., additional, Vigroux, L., additional, and Zylberajch, S., additional

Published
2001
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36. Observation of periodic variable stars towards the Galactic spiral arms by EROS II ******

Author

Derue, F., Marquette, J.-B., Lupone, S., Afonso, C., Alard, C., Albert, J.-N., Amadon, A., Andersen, J., Ansari, R., Aubourg, É., Bareyre, P., Bauer, F., Beaulieu, J.-P., Blanc, G., Bouquet, A., Char, S., Charlot, X., Couchot, F., Coutures, C., Ferlet, R., Fouqué, P., Glicenstein, J.-F., Goldman, B., Gould, A., Graff, D., Gros, M., Haïssinski, J., Hamilton, J.-C., Hardin, D., de Kat, J., Kim, A., Lasserre, T., Le Guillou, L., Lesquoy, É., Loup, C., Magneville, C., Mansoux, B., Maurice, É., Milsztajn, A., Moniez, M., Palanque-Delabrouille, N., Perdereau, O., Prévot, L., Regnault, N., Rich, J., Spiro, M., Vidal-Madjar, A., Vigroux, L., Zylberajch, S., Derue, F., Marquette, J.-B., Lupone, S., Afonso, C., Alard, C., Albert, J.-N., Amadon, A., Andersen, J., Ansari, R., Aubourg, É., Bareyre, P., Bauer, F., Beaulieu, J.-P., Blanc, G., Bouquet, A., Char, S., Charlot, X., Couchot, F., Coutures, C., Ferlet, R., Fouqué, P., Glicenstein, J.-F., Goldman, B., Gould, A., Graff, D., Gros, M., Haïssinski, J., Hamilton, J.-C., Hardin, D., de Kat, J., Kim, A., Lasserre, T., Le Guillou, L., Lesquoy, É., Loup, C., Magneville, C., Mansoux, B., Maurice, É., Milsztajn, A., Moniez, M., Palanque-Delabrouille, N., Perdereau, O., Prévot, L., Regnault, N., Rich, J., Spiro, M., Vidal-Madjar, A., Vigroux, L., and Zylberajch, S.

Abstract

We present the results of a massive variability search based on a photometric survey of a six square degree region along the Galactic plane at ($l = 305^\circ$, $b = -0.8^\circ$) and ($l = 330^\circ$, $b = -2.5^\circ$). This survey was performed in the framework of the EROS II(Expérience de Recherche d'Objets Sombres) microlensing program. The variable stars were found among 1 913 576 stars that were monitored between April and June 1998 in two passbands, with an average of 60 measurements. A new period-search technique is proposed which makes use of a statistical variable that characterizes the overall regularity of the flux versus phase diagram. This method is well suited when the photometric data are unevenly distributed in time, as is our case. 1362 objects whose luminosity varies were selected. Among them we identified 9 Cepheids, 19 RR Lyræ, 34 Miras, 176 eclipsing binaries and 266 Semi-Regular stars. Most of them are newly identified objects. The cross-identification with known catalogues has been performed. The mean distance of the RR Lyræ is estimated to be ~$ 4.9 \pm 0.3$kpc undergoing an average absorption of ~$ 3.4 \pm 0.2$mag. This distance is in good agreement with that of disc stars that contribute to the microlensing source star population. Our catalogue and light curves are available electronically from the CDS, Strasbourg and from our Web site.

Published
2002
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37. Photometric constraints on microlens spectroscopy of EROS-BLG-2000-5

Author

Afonso, C., Albert, J. N., Andersen, J., Ansari, R., Aubourg, É., Bareyre, P., Bauer, F., Blanc, G., Bouquet, A., Char, S., Charlot, X., Couchot, F., Coutures, C., Derue, F., Ferlet, R., Fouqué, P., Glicenstein, J. F., Goldman, B., Gould, A., Graff, D., Gros, M., Haïssinski, J., Hamilton, J. C., Hardin, D., de Kat, J., Kim, A., Lasserre, T., LeGuillou, L., Lesquoy, É., Loup, C., Magneville, C., Mansoux, B., Marquette, J. B., Maurice, É., Milsztajn, A., Moniez, M., Palanque-Delabrouille, N., Perdereau, O., Prévot, L., Regnault, N., Rich, J., Spiro, M., Vidal-Madjar, A., Vigroux, L., Afonso, C., Albert, J. N., Andersen, J., Ansari, R., Aubourg, É., Bareyre, P., Bauer, F., Blanc, G., Bouquet, A., Char, S., Charlot, X., Couchot, F., Coutures, C., Derue, F., Ferlet, R., Fouqué, P., Glicenstein, J. F., Goldman, B., Gould, A., Graff, D., Gros, M., Haïssinski, J., Hamilton, J. C., Hardin, D., de Kat, J., Kim, A., Lasserre, T., LeGuillou, L., Lesquoy, É., Loup, C., Magneville, C., Mansoux, B., Marquette, J. B., Maurice, É., Milsztajn, A., Moniez, M., Palanque-Delabrouille, N., Perdereau, O., Prévot, L., Regnault, N., Rich, J., Spiro, M., Vidal-Madjar, A., and Vigroux, L.

Abstract

We apply EROS photometric data to interpret previously published Keck and VLT spectra of the binary-microlens caustic-crossing event EROS-BLG-2000-5. We show that the VLT data imply that the outer ${\sim} 4\%$of the limb of the K3-giant source is strongly in emission in Hα, in contradiction to available models of the photosphere. This conflict could be resolved if the integrated Hαemission from the chromosphere were equal to 8% of the integrated Hαabsorption from the source as a whole. These conclusions regarding the extreme limb are almost completely model-independent. We also present a general method for using the photometric data to facilitate direct comparison between the atmospheric model and the spectroscopic data. While this method has some model-dependent features, it is fairly robust and can serve to guide the analysis of spectra while more detailed models of the lens geometry are being developed. In addition, we find that the color of the limb of the source (outer 5.5% by radius) is $\Delta(V-I)\sim 0.37$redder than the source as a whole, so that it has the color of a M0 giant.

Published
2001
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38. Concerning the connection between the C ℓ power spectrum of the cosmic microwave background and the <MATH>Γ m </MATH> Fourier spectrum of rings on the sky.

Author

Ansari, R., Bargot, S., Bourrachot, A., Couchot, F., Haïssinski, J., Henrot-Versillé, S., Le Meur, G., Perdereau, O., Piat, M., Plaszczynski, S., and Touze, F.

Subjects
COSMIC background radiation, POWER spectra
Abstract

ABSTRACT In this article we present and study a scaling law of the mΓ[sub m] cosmic microwave background Fourier spectrum on rings that allows us to (i) combine spectra corresponding to different colatitude angles (e.g. several detectors at the focal plane of a telescope) and (ii) recover the C[sub ℓ] power spectrum once the Γ[sub m] coefficients have been measured. This recovery is performed numerically below the 1 per cent level for colatitudes Θ > 80° . In addition, taking advantage of the smoothness of C[sub ℓ] and of Γ[sub m] , we provide analytical expressions that allow the recovery of one of the spectra at the 1 per cent level, the other one being known. [ABSTRACT FROM AUTHOR]

Published
2003
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39. Lepton and pion pair production in γγ collisions measured near the threshold at DCI

Author

Courau, A., Falvard, A., Haïssinski, J., Jousset, J., Michel, B., Montret, J.C., Cordier, A., Delcourt, B., and Mane, F.

Abstract

This paper reports a complete analysis of data taken at DCI to measure lepton and pion pair production close to the threshold in two-photon processes: e+e−→ e+e−(e+e−, μ+μ−, π+π−). Preliminary results have been previously published including one-half of the total statistics. Final results presented here are in good agreement with QED for lepton pair production. The measured cross section for pion pair production is twice as large as that expected from Born terms only — a two standard deviation effect.

Published
1986
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40. An experimental study ofe+e− annihilation into four leptons at <img src="/fulltext-image.asp?format=htmlnonpaginated&src=W580H72401T887W1_html\10052_2006_Article_BF02430605_TeX2GIFIE1.gif" border="0" alt=" $$\sqrt S \geqq 35$$ " /> GeVGeV

Author

Behrend, H., Criegee, L., Dainton, J., Field, J., Franke, G., Jung, H., Meyer, J., Schröder, V., Winter, G., Bussey, P., Buttar, C., Campbell, A., Hendry, D., McCurrach, G., Scarr, J., Skillicorn, I., Smith, K., Ahme, J., Blobel, V., Brehm, W., Feindt, M., Fenner, H., Harjes, J., Peters, J., Podobrin, O., Spitzer, H., Apel, W., Engler, J., Flügge, G., Fries, D., Fuster, J., Gabriel, P., Gamerdinger, K., Grosse-Wiesmann, P., Hahn, M., Hädinger, U., Hansmeyer, J., Küster, H., Müller, H., Ranitzsch, K., Schneider, H., Seufert, R., de Boer, W., Buschhorn, G., Grindhammer, G., Gunderson, B., Kiesling, Ch., Kotthaus, R., Kroha, H., Lüers, D., Oberlack, H., Schacht, P., Scholz, S., Shooshtari, G., Wiedenmann, W., Davier, M., Fournier, D., Grivaz, J., Haïssinski, J., Janot, P., Journé, V., Kim, D., Le Diberder, F., Veillet, J., Blohm, K., George, R., Goldberg, M., Hamon, O., Kapusta, F., Poggioli, L., Rivoal, M., D'Agostini, G., Ferrarotto, F., Iacovacci, M., Stella, B., Aleksan, R., Cozzika, G., Ducros, Y., Pierre, F., Alexander, G., Beck, A., Bella, G., Grunhaus, J., Klatchko, A., Levy, A., and Milstène, C.

Abstract

Abstract: The three reactionse +e−→e +e−e+e−,e + e -→e + e -μ+μ- ande + e -→μ+μ-μ+ μ- have been studied using the CELLO detector at PETRA. The data correspond to 130 pb−1 collected at energies ranging from 35 GeV to 46.8 GeV. A detailed analysis of the distribution of the observed events in phase space shows good agreement with QED to order α4.

Published
1989
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42. Observation of microlensing towards the galactic spiral arms EROS II. 2 year survey

Author

Derue, F., Afonso, C., Alard, C., Albert, J. -N, Alexis Amadon, Andersen, J., Ansari, R., Aubourg, É, Bareyre, P., Bauer, F., Beaulieu, J. -P, Bouquet, A., Char, S., Charlot, X., Couchot, F., Coutures, C., Ferlet, R., Glicenstein, J. -F, Goldman, B., Gould, A., Graff, D., Gras, M., Haïssinski, J., Hamilton, J. -C, Hardin, D., Kat, J., Kim, A., Lasserre, T., Lesquoy, É, Loup, C., Magneville, C., Mansoux, B., Marquette, J. -B, Maurice, E., Milsztajn, A., Moniez, M., Palanque-Delabrouille, N., Perdereau, O., Prévot, L., Regnault, N., Rich, J., Spiro, M., Vidal-Madjar, A., Vigroux, L., and Zylberajch, S.

43. Determination of the radiative widths of the η′ and A2 from two-photon exchange production

Author

Behrend, H.J., primary, Chen, Ch., additional, Fenner, H., additional, Field, J.H., additional, Schröder, V., additional, Sindt, H., additional, D'Agostini, G., additional, Apel, W.-D., additional, Banerjee, S., additional, Bodenkamp, J., additional, Chrobaczek, D., additional, Engler, J., additional, Flügge, G., additional, Fries, D.C., additional, Fues, W., additional, Gamerdinger, K., additional, Hopp, G., additional, Küster, H., additional, Müller, H., additional, Randoll, H., additional, Schmidt, G., additional, Schneider, H., additional, De Boer, W., additional, Buschhorn, G., additional, Grindhammer, G., additional, Grosse-Wiesmann, P., additional, Gunderson, B., additional, Kiesling, C., additional, Kotthaus, R., additional, Kruse, U., additional, Lierl, H., additional, Lüers, D., additional, Meyer, T., additional, Oberlack, H., additional, Schacht, P., additional, Schachter, M.J., additional, Snyder, A., additional, Steiner, H., additional, Carnesecchi, G., additional, Colas, P., additional, Cordier, A., additional, Davier, M., additional, Fournier, D., additional, Grivaz, J.F., additional, Haïssinski, J., additional, Journé, V., additional, Klarsfeld, A., additional, Laplanche, F., additional, Le Diberder, F., additional, Mallik, U., additional, Veillet, J.J., additional, George, R., additional, Goldberg, M., additional, Grossetête, B., additional, Hamon, O., additional, Kapusta, F., additional, Kovacs, F., additional, London, G., additional, Poggioli, L., additional, Rivoal, M., additional, Aleksan, R., additional, Bouchez, J., additional, Cozzika, G., additional, Ducros, Y., additional, Gaidot, A., additional, Jadach, S., additional, Lavagne, Y., additional, Pamela, J., additional, Pansart, J.P., additional, and Pierre, F., additional

Published
1982
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44. A zero-degree tagging system used for photon-photon experiments at DCI

Author

Brossard, M., primary, Falvard, A., additional, Jousset, J., additional, Michel, B., additional, Montarou, G., additional, Montret, J.C., additional, Reichstadt, P., additional, Bertin, P.Y., additional, Fournier, G., additional, Vialatte, M.C., additional, Buon, J., additional, Courau, A., additional, Haïssinski, J., additional, Marx, J.P., additional, and Souchet, R., additional

Published
1980
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46. Scalar lepton search with the CELLO detector at PETRA

Author

Behrend, H.J., primary, Chen, Ch., additional, Fenner, H., additional, Field, J.H., additional, Schröder, V., additional, Sindt, H., additional, D'Agostini, G., additional, Apel, W.D., additional, Banerjee, S., additional, Bodenkamp, J., additional, Chrobaczek, D., additional, Engler, J., additional, Flügge, G., additional, Fries, D.C., additional, Fues, W., additional, Gamerdinger, K., additional, Hopp, G., additional, Küster, H., additional, Müller, H., additional, Randoll, H., additional, Schmidt, G., additional, Schneider, H., additional, De Boer, W., additional, Buschhorn, G., additional, Grindhammer, G., additional, Grosse-Wiesmann, P., additional, Gunderson, B., additional, Kiesling, C., additional, Kotthaus, R., additional, Kruse, U., additional, Lierl, H., additional, Lüers, D., additional, Meyer, T., additional, Oberlack, H., additional, Schacht, P., additional, Schachter, M.J., additional, Snyder, A., additional, Carnesecchi, G., additional, Colas, P., additional, Cordier, A., additional, Davier, M., additional, Fournier, D., additional, Grivaz, J.F., additional, Haïssinski, J., additional, Journé, V., additional, Klarsfeld, A., additional, Laplanche, F., additional, Le Diberder, F., additional, Mallik, U., additional, Veillet, J.J., additional, George, R., additional, Goldberg, M., additional, Grossetête, B., additional, Hamon, O., additional, Kapusta, F., additional, Kovacs, F., additional, London, G., additional, Poggioli, L., additional, Rivoal, M., additional, Aleksan, R., additional, Bouchez, J., additional, Cozzika, G., additional, Ducros, Y., additional, Gaidot, A., additional, Jadach, S., additional, Lavagne, Y., additional, Pamela, J., additional, Pansart, J.P., additional, and Pierre, F., additional

Published
1982
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47. Observation of topologically isolated energetic electrons in e+e− interactions

Author

Behrend, H.-J., primary, Chen, C., additional, Fenner, H., additional, Schachter, M.J., additional, Schröder, V., additional, Sindt, H., additional, D'Agostini, G., additional, Apel, W.D., additional, Banerjee, S., additional, Bodenkamp, J., additional, Chrobaczek, D., additional, Engler, J., additional, Flügge, G., additional, Fries, D.C., additional, Fues, W., additional, Gamerdinger, K., additional, Hopp, G., additional, Küster, H., additional, Müller, H., additional, Randoll, H., additional, Schmidt, G., additional, Schneider, H., additional, De Boer, W., additional, Buschhorn, G., additional, Grindhammer, G., additional, Grosse-Wiesmann, P., additional, Gunderson, B., additional, Kiesling, C., additional, Kotthaus, R., additional, Kruse, U., additional, Lierl, H., additional, Lüers, D., additional, Oberlack, H., additional, Schacht, P., additional, Colas, P., additional, Cordier, A., additional, Davier, M., additional, Fournier, D., additional, Grivaz, J.F., additional, Haïssinski, J., additional, Journé, V., additional, Klarsfeld, A., additional, Laplanche, F., additional, Le Diberder, F., additional, Mallik, U., additional, Viellet, J.J., additional, Field, J.H., additional, George, R., additional, Goldberg, M., additional, Grossetête, B., additional, Hamon, O., additional, Kapusta, F., additional, Kovacs, F., additional, London, G., additional, Poggioli, L., additional, Rivoal, M., additional, Aleksan, R., additional, Bouchez, J., additional, Carnesecchi, G., additional, Cozzika, G., additional, Ducros, Y., additional, Gaidot, A., additional, Jadach, S., additional, Lavagne, Y., additional, Pamela, J., additional, Pansart, J.P., additional, and Pierre, F., additional

Published
1982
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48. An analysis of the charged and neutral energy flow in e+e− hadronic annihilation at 34 GeV, and a determination of the QCD effective coupling constant

Author

Behrend, H.J., primary, Chen, Ch., additional, Fenner, H., additional, Field, J.H., additional, Schröder, V., additional, Sindt, H., additional, D'Agostini, G., additional, Apel, W.D., additional, Banerjee, S., additional, Bodenkamp, J., additional, Chrobaczek, D., additional, Engler, J., additional, Flügge, G., additional, Fries, D.C., additional, Fues, W., additional, Gamerdinger, K., additional, Hopp, G., additional, Küster, H., additional, Müller, H., additional, Randoll, H., additional, Schmidt, G., additional, Schneider, H., additional, de Boer, W., additional, Buschhorn, G., additional, Grindhammer, G., additional, Grosse-Wiesmann, P., additional, Gunderson, B., additional, Kiesling, C., additional, Kotthaus, R., additional, Kruse, U., additional, Lierl, H., additional, Lüers, D., additional, Meyer, T., additional, Oberlack, H., additional, Schacht, P., additional, Schachter, M.J., additional, Snyder, A., additional, Carnesecchi, G., additional, Colas, P., additional, Cordier, A., additional, Davier, M., additional, Fournier, D., additional, Grivaz, J.F., additional, Haïssinski, J., additional, Journé, V., additional, Klarsfeld, A., additional, Laplanche, F., additional, Le Diberder, F., additional, Mallik, U., additional, Veillet, J.J., additional, George, R., additional, Goldberg, M., additional, Grossetěte, B., additional, Hamon, O., additional, Kapusta, F., additional, Kovacs, F., additional, London, G., additional, Poggioli, L., additional, Rivoal, M., additional, Aleksan, R., additional, Bouchez, J., additional, Cozzika, G., additional, Ducros, Y., additional, Gaidot, A., additional, Jadach, S., additional, Lavagne, Y., additional, Pamela, J., additional, Pansart, J.P., additional, and Pierre, F., additional

Published
1982
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49. Measurement of e+e−→τ+τ− at high energy and properties of the τ lepton

Author

Behrend, H.J., primary, Chen, Ch., additional, Fenner, H., additional, Field, J.H., additional, Schröder, V., additional, Sindt, H., additional, D'Agostini, G., additional, Apel, W.D., additional, Banerjee, S., additional, Bodenkamp, J., additional, Chrobaczek, D., additional, Engler, J., additional, Flügge, G., additional, Fries, D.C., additional, Fues, W., additional, Gamerdinger, K., additional, Hopp, G., additional, Küster, H., additional, Müller, H., additional, Randoll, H., additional, Schmidt, G., additional, Schneider, H., additional, de Boer, W., additional, Buschhorn, G., additional, Grindhammer, G., additional, Grosse-Wiesmann, P., additional, Gunderson, B., additional, Kiesling, C., additional, Kotthaus, R., additional, Kruse, U., additional, Lierl, H., additional, Luers, D., additional, Meyer, T., additional, Oberlack, H., additional, Schacht, P., additional, Schachter, M.J., additional, Snyder, A., additional, Carnesecchi, G., additional, Colas, P., additional, Cordier, A., additional, Davier, M., additional, Fournier, D., additional, Grivaz, J.F., additional, Haïssinski, J., additional, Journé, V., additional, Klarsfeld, A., additional, Laplanche, F., additional, le Diberder, F., additional, Mallik, U., additional, Veillet, J.J., additional, George, R., additional, Goldberg, M., additional, Grossetête, B., additional, Hamon, O., additional, Kapusta, F., additional, Kovacs, F., additional, London, G., additional, Poggioli, L., additional, Rivoal, M., additional, Aleksan, R., additional, Bouchez, J., additional, Cozzika, G., additional, Ducros, Y., additional, Gaidot, A., additional, Jadach, S., additional, Lavagne, Y., additional, Pamela, J., additional, Pansart, J.P., additional, and Pierre, F., additional

Published
1982
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50. τ Branching ratios and polarization limits in e+e− interaction at √s=34GeV

Author

Behrend, H.J., primary, Chen, Ch., additional, Fenner, H., additional, Gümpel, U., additional, Schachter, M.-J., additional, Schröder, V., additional, Sindt, H., additional, D'Agostini, G., additional, Apel, W.-D., additional, Banerjee, S., additional, Bodenkamp, J., additional, Engler, J., additional, Flügge, G., additional, Fries, D.C., additional, Fues, W., additional, Gamerdinger, K., additional, Hopp, G., additional, Küster, H., additional, Müller, H., additional, Randoll, H., additional, Schmidt, G., additional, Schneider, H., additional, de Boer, W., additional, Buschhorn, G., additional, Grindhammer, G., additional, Grosse-Wiesmann, P., additional, Gunderson, B., additional, Kiesling, C., additional, Kotthaus, R., additional, Kruse, U., additional, Lierl, H., additional, Lüers, D., additional, Oberlack, H., additional, Schacht, P., additional, Colas, P., additional, Cordier, A., additional, Davier, M., additional, Fournier, D., additional, Grivaz, J.F., additional, Haïssinski, J., additional, Journé, V., additional, Klarsfeld, A., additional, Laplanche, F., additional, Mallik, U., additional, Veillet, J.-J., additional, Field, J.H., additional, George, R., additional, Goldberg, M., additional, Grossettête, B., additional, Hamon, O., additional, Kapusta, F., additional, Kovacs, F., additional, London, G., additional, Poggioli, L., additional, Rivoal, M., additional, Aleksan, R., additional, Bouchez, J., additional, Carnesecchi, G., additional, Cozzika, G., additional, Ducros, Y., additional, Gaidot, A., additional, Lavagne, Y., additional, Pamela, J., additional, Pansart, J.P., additional, and Pierre, F., additional

Published
1983
Full Text
View/download PDF

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