Author: "Perdereau, O." / Database: Supplemental Index - Searchworks@Jio Institute Digital Library Search Results

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41 results on '"Perdereau, O."'

1. Thermal architecture for the QUBIC cryogenic receiver

Author: Zmuidzinas, Jonas, Gao, Jian-Rong, May, A. J., Chapron, C., Coppi, G., D'Alessandro, G., de Bernardis, P., Masi, S., Melhuish, S., Piat, M., Piccirillo, L., Schillaci, A., Thermeau, J.-P., Ade, P., Amico, G., Auguste, D., Aumont, J., Banfi, S., Barbarán, G., Battaglia, P., Battistelli, E., Baù, A., Bélier, B., Bennett, D., Bergé, L., Bernard, J.-Ph., Bersanelli, M., Bigot-Sazy, M.-A., Bleurvacq, N., Bonaparte, J., Bonis, J., Bordier, G., Bréelle, E., Bunn, E., Burke, D., Buzi, D., Buzzelli, A., Cavaliere, F., Chanial, P., Charlassier, R., Columbro, F., Coppolecchia, A., Couchot, F., D'Agostino, R., De Gasperis, G., De Leo, M., De Petris, M., Di Donato, A., Dumoulin, L., Etchegoyen, A., Fasciszewski, A., Franceschet, C., Gamboa Lerena, M. M., García, B., Garrido, X., Gaspard, M., Gault, A., Gayer, D., Gervasi, M., Giard, M., Giraud-Héraud, Y., Gómez Berisso, M., González, M., Gradziel, M., Grandsire, L., Guerrard, E., Hamilton, J.-Ch., Harari, D., Haynes, V., Henrot-Versillé, S., Hoang, D. T., Incardona, F., Jules, E., Kaplan, J., Korotkov, A., Kristukat, C., Lamagna, L., Loucatos, S., Louis, T., Lowitz, A., Lukovic, V., Luterstein, R., Maffei, B., Marnieros, S., Mattei, A., McCulloch, M. A., Medina, M. C., Mele, L., Mennella, A., Montier, L., Mundo, L. M., Murphy, J. A., Murphy, J. D., O'Sullivan, C., Olivieri, E., Paiella, A., Pajot, F., Passerini, A., Pastoriza, H., Pelosi, A., Perbost, C., Perdereau, O., Pezzotta, F., Piacentini, F., Pisano, G., Polenta, G., Prêle, D., Puddu, R., Rambaud, D., Ringegni, P., Romero, G. E., Salatino, M., Scóccola, C. G., Scully, S., Spinelli, S., Stolpovskiy, M., Suarez, F., Tartari, A., Timbie, P., Torchinsky, S. A., Tristram, M., Truongcanh, V., Tucker, C., Tucker, G., Vanneste, S., Viganó, D., Vittorio, N., Voisin, F., Watson, B., Wicek, F., Zannoni, M., and Zullo, A.
Published: 2018
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2. Simulations and performance of the QUBIC optical beam combiner

Author: Zmuidzinas, Jonas, Gao, Jian-Rong, O'Sullivan, C., Burke, D., Gayer, D., Murphy, J. D., Scully, S., De Leo, M., De Petris, M., Mattei, A., Zullo, A., Mennella, A., Zannoni, M., Bleurvacq, N., Chapron, C., Hamilton, J.-Ch., Piat, M., Ade, P., Amico, G., Auguste, D., Aumont, J., Banfi, S., Barbarán, G., Battaglia, P., Battistelli, E., Baù, A., Bélier, B., Bennett, D., Bergé, L., Bernard, J.-Ph., Bersanelli, M., Bigot-Sazy, M.-A., Bonaparte, J., Bonis, J., Bordier, G., Bréelle, E., Bunn, E., Buzi, D., Buzzelli, A., Cavaliere, F., Chanial, P., Charlassier, R., Columbro, F., Coppi, G., Coppolecchia, A., Couchot, F., D'Agostino, R., D’Alessandro, G., de Bernardis, P., De Gasperis, G., Di Donato, A., Dumoulin, L., Etchegoyen, A., Fasciszewski, A., Franceschet, C., Gamboa Lerena, M. M., García, B., Garrido, X., Gaspard, M., Gault, A., Gervasi, M., Giard, M., Giraud-Héraud, Y., Gómez Berisso, M., González, M., Gradziel, M., Grandsire, L., Guerrard, E., Harari, D., Haynes, V., Henrot-Versillé, S., Hoang, D. T., Incardona, F., Jules, E., Kaplan, J., Korotkov, A., Kristukat, C., Lamagna, L., Loucatos, S., Louis, T., Lowitz, A., Lukovic, V., Luterstein, R., Maffei, B., Marnieros, S., Masi, S., May, A., McCulloch, M., Medina, M. C., Mele, L., Melhuish, S., Montier, L., Mundo, L. M., Murphy, J. A., Olivieri, E., Paiella, A., Pajot, F., Passerini, A., Pastoriza, H., Pelosi, A., Perbost, C., Perdereau, O., Pezzotta, F., Piacentini, F., Piccirillo, L., Pisano, G., Polenta, G., Prêle, D., Puddu, R., Rambaud, D., Ringegni, P., Romero, G. E., Salatino, M., Schillaci, A., Scóccola, C. G., Spinelli, S., Stolpovskiy, M., Suarez, F., Tartari, A., Thermeau, J.-P., Timbie, P., Torchinsky, S. A., Tristram, M., Truongcanh, V., Tucker, C., Tucker, G., Vanneste, S., Viganò, D., Vittorio, N., Voisin, F., Watson, B., and Wicek, F.
Published: 2018
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3. QUBIC: the Q and U bolometric interferometer for cosmology

Author: Zmuidzinas, Jonas, Gao, Jian-Rong, O'Sullivan, C., Ade, P., Amico, G., Auguste, D., Aumont, J., Banfi, S., Barbarán, G., Battaglia, P., Battistelli, E., Baù, A., Bélier, B., Bennett, D., Bergé, L., Bernard, J.-Ph., Bersanelli, M., Bigot-Sazy, M.-A., Bleurvacq, N., Bonaparte, J., Bonis, J., Bordier, G., Bréelle, E., Bunn, E., Burke, D., Buzi, D., Buzzelli, A., Cavaliere, F., Chanial, P., Chapron, C., Charlassier, R., Columbro, F., Coppi, G., Coppolecchia, A., Couchot, F., D'Agostino, R., D’Alessandro, G., de Bernardis, P., de Gasperis, G., De Leo, M., De Petris, M., Di Donato, A., Dumoulin, L., Etchegoyen, A., Fasciszewski, A., Franceschet, C., Gamboa Lerena, M. M., García, B., Garrido, X., Gaspard, M., Gault, A., Gayer, D., Gervasi, M., Giard, M., Giraud-Héraud, Y., Gómez Berisso, M., González, M., Gradziel, M., Grandsire, L., Guerrard, E., Hamilton, J.-Ch., Harari, D., Haynes, V., Henrot-Versillé, S., Hoang, D. T., Incardona, F., Jules, E., Kaplan, J., Korotkov, A., Kristukat, C., Lamagna, L., Loucatos, S., Louis, T., Lowitz, A., Lukovic, V., Luterstein, R., Maffei, B., Marnieros, S., Masi, S., Mattei, A., May, A., McCulloch, M., Medina, M. C., Mele, L., Melhuish, S., Mennella, A., Montier, L., Mundo, L. M., Murphy, J. A., Murphy, J. D., Olivieri, E., Paiella, A., Pajot, F., Passerini, A., Pastoriza, H., Pelosi, A., Perbost, C., Perdereau, O., Pezzotta, F., Piacentini, F., Piat, M., Piccirillo, L., Pisano, G., Polenta, G., Prêle, D., Puddu, R., Rambaud, D., Ringegni, P., Romero, G. E., Salatino, M., Schillaci, A., Scóccola, C. G., Scully, S., Spinelli, S., Stolpovskiy, M., Suarez, F., Tartari, A., Thermeau, J.-P., Timbie, P., Torchinsky, S. A., Tristram, M., Truongcanh, V., Tucker, C., Tucker, G., Vanneste, S., Viganò, D., Vittorio, N., Voisin, F., Watson, B., Wicek, F., Zannoni, M., and Zullo, A.
Published: 2018
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4. Optical modelling and analysis of the Q and U bolometric interferometer for cosmology

Author: Sadwick, Laurence P., Yang, Tianxin, Burke, D., Gayer, D., Kalinauskaite, E., O'Sullivan, C., Murphy, J. D., Scully, S. P., De Petris, M., De Leo, M., Mennella, A., Torchinsky, S. A., Zannoni, M., Amico, G., Auguste, D., Aumont, J., Banfi, S., Barbarán, G., Battaglia, P., Battistelli, E., Baù, A., Bélier, B., Bennett, D. G., Bergé, L., Bernard, J.-Ph., Bersanelli, M., Bigot-Sazy, M.-A., Bleurvac, N., Bonaparte, J., Bonis, J., Bordier, G., Bréelle, E., Bunn, E. F., Buzi, D., Buzzelli, A., Cavaliere, F., Chanial, P., Chapron, C., Charlassier, R., Columbro, F., Coppi, G., Coppolecchia, A., Couchot, F., D’Alessandro, G., D'Agostino, R., de Bernardis, P., De Gasperis, G., Di Donato, A., Drilien, A.-A., Dumoulin, Louis, Etchegoyen, A., Fasciszewski, A., Franceschet, C., Gamboa-Lerena, M., García, B., Garrido, X., Gaspard, M., Gault, A., Gervasi, M., Giard, M., Giraud-Héraud, Y., Gómez Berisso, M., González, M., Gradziel, M. L., Grandsire, L., Guerrard, E., Hamilton, J.-Ch., Harari, D., Haynes, V., Henrot-Versillé, S., Hoang, D. T., Holtzer, N., Incardona, F., Jules, E., Kaplan, J., Korotkov, A. L., Kristukat, C., Lamagna, L., Lande, J., Loucatos, S., Louis, T., Lowitz, A., Lukovic, V., Luterstein, R., Maffei, Bruno, Marnieros, S., Masi, S., Mattei, A., May, A. J., McCulloch, M. A., Medina, M. C., Mele, L., Melhuish, S. J., Mundo, L., Montier, L., Murphy, J. A., Néel, D., Olivieri, E., Paiella, A., Pajot, F., Passerini, A., Pastoriza, H., Pelosi, A., Perbost, C., Perdereau, O., Pezzotta, F., Piacentini, F., Piat, M. R., Piccirillo, L., Pisano, G., Polenta, G., Prêle, D., Puddu, R., Rambaud, D., Rigaut, O., Ringegni, P., Romero, G. E., Salatino, M., Schillaci, A., Scóccola, C. G., Spinelli, S. M., Stolpovskiy, M., Suarez, F., Tartari, A., Thermeau, J.-P., Timbie, P. T., Tristram, M., Truongcanh, V., Tucker, G. S., Tucker, C. E., Viganò, D., Vittorio, N., Voisin, F., Watson, B., Wicek, F., and Zullo, A.
Published: 2018
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5. 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, É., 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., Haïssinski, J., Hamadache, C., de Kat, J., Lesquoy, É., Loup, C., Le Guillou, L., Magneville, C., Mansoux, B., Marquette, J.-B., Maurice, É., Maury, A., Milsztajn, A., Moniez, M., Palanque-Delabrouille, N., Perdereau, O., Rahvar, S., Rich, J., Spiro, M., Tisserand, P., Vidal-Madjar, A., Rahal, Y. R., Afonso, C., Albert, J.-N., Andersen, J., Ansari, R., Aubourg, É., 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., Haïssinski, J., Hamadache, C., de Kat, J., Lesquoy, É., Loup, C., Le Guillou, L., Magneville, C., Mansoux, B., Marquette, J.-B., Maurice, É., Maury, A., Milsztajn, A., Moniez, M., Palanque-Delabrouille, N., Perdereau, O., Rahvar, S., Rich, J., Spiro, M., Tisserand, P., and Vidal-Madjar, A.
Abstract: Aims. 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.
Published: 2009
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6. The beat Cepheids in the Magellanic Clouds: an analysis from the EROS-2 database ***

Author: Marquette, J. B., Beaulieu, J. P., Buchler, J. R., Szabó, R., Tisserand, P., Belghith, S., Fouqué, P., Lesquoy, É., Milsztajn, A., Schwarzenberg-Czerny, A., Afonso, C., Albert, J. N., Andersen, J., Ansari, R., Aubourg, É., Bareyre, P., Charlot, X., Coutures, C., Ferlet, R., Glicenstein, J. F., Goldman, B., Gould, A., Graff, D., Gros, M., Haïssinski, J., Hamadache, C., de Kat, J., Le Guillou, L., Loup, C., Magneville, C., Maurice, É., Maury, A., Moniez, M., Palanque-Delabrouille, N., Perdereau, O., Rahal, Y. R., Rich, J., Spiro, M., Vidal-Madjar, A., Marquette, J. B., Beaulieu, J. P., Buchler, J. R., Szabó, R., Tisserand, P., Belghith, S., Fouqué, P., Lesquoy, É., Milsztajn, A., Schwarzenberg-Czerny, A., Afonso, C., Albert, J. N., Andersen, J., Ansari, R., Aubourg, É., Bareyre, P., Charlot, X., Coutures, C., Ferlet, R., Glicenstein, J. F., Goldman, B., Gould, A., Graff, D., Gros, M., Haïssinski, J., Hamadache, C., de Kat, J., Le Guillou, L., Loup, C., Magneville, C., Maurice, É., Maury, A., Moniez, M., Palanque-Delabrouille, N., Perdereau, O., Rahal, Y. R., Rich, J., Spiro, M., and Vidal-Madjar, A.
Abstract: Context. 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.
Published: 2009
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7. Discovery of a peculiar Cepheid-like star towards the northern edge of the Small Magellanic Cloud ***

Author: Marquette, J. B., Tisserand, P., François, P., Beaulieu, J. P., Doublier, V., Lesquoy, É., Milsztajn, A., Pritchard, J., Schwarzenberg-Czerny, A., Afonso, C., Albert, J. N., Andersen, J., Ansari, R., Aubourg, É., Bareyre, 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., Le Guillou, L., Loup, C., Magneville, C., Maurice, É., Maury, A., Moniez, M., Palanque-Delabrouille, N., Perdereau, O., Rahal, Y. R., Rich, J., Spiro, M., Vidal-Madjar, A., Zylberajch, S., Marquette, J. B., Tisserand, P., François, P., Beaulieu, J. P., Doublier, V., Lesquoy, É., Milsztajn, A., Pritchard, J., Schwarzenberg-Czerny, A., Afonso, C., Albert, J. N., Andersen, J., Ansari, R., Aubourg, É., Bareyre, 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., Le Guillou, L., Loup, C., Magneville, C., Maurice, É., Maury, A., Moniez, M., Palanque-Delabrouille, N., Perdereau, O., Rahal, Y. R., Rich, J., Spiro, M., Vidal-Madjar, A., and Zylberajch, S.
Abstract: Context. 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.
Published: 2008
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8. R Coronae Borealis stars in the Galactic bulge discovered by EROS-2 *

Author: Tisserand, P., Marquette, J. B., Wood, P. R., Lesquoy, É., Beaulieu, J. P., Milsztajn, A., Hamadache, C., Afonso, C., Albert, J. N., Andersen, J., Ansari, R., Aubourg, É., Bareyre, P., Charlot, X., Coutures, C., Ferlet, R., Fouqué, P., Glicenstein, J. F., Goldman, B., Gould, A., Gros, M., Haissinski, J., de Kat, J., Le Guillou, L., Loup, C., Magneville, C., Maurice, É., Maury, A., Moniez, M., Palanque-Delabrouille, N., Perdereau, O., Rahal, Y., Rich, J., Spiro, M., Vidal-Madjar, A., Zylberajch, S., Tisserand, P., Marquette, J. B., Wood, P. R., Lesquoy, É., Beaulieu, J. P., Milsztajn, A., Hamadache, C., Afonso, C., Albert, J. N., Andersen, J., Ansari, R., Aubourg, É., Bareyre, P., Charlot, X., Coutures, C., Ferlet, R., Fouqué, P., Glicenstein, J. F., Goldman, B., Gould, A., Gros, M., Haissinski, J., de Kat, J., Le Guillou, L., Loup, C., Magneville, C., Maurice, É., Maury, A., Moniez, M., Palanque-Delabrouille, N., Perdereau, O., Rahal, Y., Rich, J., Spiro, M., Vidal-Madjar, A., and Zylberajch, S.
Abstract: Context. Rare types of variable stars may provide 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 such rare variable stars. One example is the R Coronae Borealis (RCB) stars, a rare type of evolved carbon-rich supergiant.
Published: 2008
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9. Limits on the Macho content of the Galactic Halo from the EROS-2 Survey of the Magellanic Clouds ***

Author: Tisserand, P., Le Guillou, L., Afonso, C., Albert, J. N., Andersen, J., Ansari, R., Aubourg, É., 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, É., Loup, C., Magneville, C., Marquette, J. B., Maurice, É., Maury, A., Milsztajn, A., Moniez, M., Palanque-Delabrouille, N., Perdereau, O., Rahal, Y. R., Rich, J., Spiro, M., Vidal-Madjar, A., Vigroux, L., Tisserand, P., Le Guillou, L., Afonso, C., Albert, J. N., Andersen, J., Ansari, R., Aubourg, É., 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, É., Loup, C., Magneville, C., Marquette, J. B., Maurice, É., Maury, A., Milsztajn, A., Moniez, M., Palanque-Delabrouille, N., Perdereau, O., Rahal, Y. R., Rich, J., Spiro, M., Vidal-Madjar, A., and Vigroux, L.
Abstract: Aims.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.
Published: 2007
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10. Archeops in-flight performance, data processing, and map making

Author: Macías-Pérez, J. F., Lagache, G., Maffei, B., Ganga, K., Bourrachot, A., Ade, P., Amblard, A., Ansari, R., Aubourg, E., Aumont, J., Bargot, S., Bartlett, J., Benoît, A., Bernard, J.-Ph., Bhatia, R., Blanchard, A., Bock, J. J., Boscaleri, A., Bouchet, F. R., Camus, P., Cardoso, J.-F., Couchot, F., de Bernardis, P., Delabrouille, J., Désert, F.-X., Doré, O., Douspis, M., Dumoulin, L., Dupac, X., Filliatre, Ph., Fosalba, P., Gannaway, F., Gautier, B., Giard, M., Giraud-Héraud, Y., Gispert, R., Guglielmi, L., Hamilton, J.-Ch., Hanany, S., Henrot-Versillé, S., Hristov, V., Kaplan, J., Lamarre, J.-M., Lange, A. E., Madet, K., Magneville, Ch., Marrone, D. P., Masi, S., Mayet, F., Murphy, J. A., Naraghi, F., Nati, F., Patanchon, G., Perdereau, O., Perrin, G., Plaszczynski, S., Piat, M., Ponthieu, N., Prunet, S., Puget, J.-L., Renault, C., Rosset, C., Santos, D., Starobinsky, A., Strukov, I., Sudiwala, R. V., Teyssier, R., Tristram, M., Tucker, C., Vanel, J.-Ch., Vibert, D., Wakui, E., Yvon, D., Macías-Pérez, J. F., Lagache, G., Maffei, B., Ganga, K., Bourrachot, A., Ade, P., Amblard, A., Ansari, R., Aubourg, E., Aumont, J., Bargot, S., Bartlett, J., Benoît, A., Bernard, J.-Ph., Bhatia, R., Blanchard, A., Bock, J. J., Boscaleri, A., Bouchet, F. R., Camus, P., Cardoso, J.-F., Couchot, F., de Bernardis, P., Delabrouille, J., Désert, F.-X., Doré, O., Douspis, M., Dumoulin, L., Dupac, X., Filliatre, Ph., Fosalba, P., Gannaway, F., Gautier, B., Giard, M., Giraud-Héraud, Y., Gispert, R., Guglielmi, L., Hamilton, J.-Ch., Hanany, S., Henrot-Versillé, S., Hristov, V., Kaplan, J., Lamarre, J.-M., Lange, A. E., Madet, K., Magneville, Ch., Marrone, D. P., Masi, S., Mayet, F., Murphy, J. A., Naraghi, F., Nati, F., Patanchon, G., Perdereau, O., Perrin, G., Plaszczynski, S., Piat, M., Ponthieu, N., Prunet, S., Puget, J.-L., Renault, C., Rosset, C., Santos, D., Starobinsky, A., Strukov, I., Sudiwala, R. V., Teyssier, R., Tristram, M., Tucker, C., Vanel, J.-Ch., Vibert, D., Wakui, E., and Yvon, D.
Abstract: Aims.Archeops is a balloon-borne experiment inspired by the Planck satellite and its high frequency instrument (HFI). It is designed to measure the cosmic microwave background (CMB) temperature anisotropies at high angular resolution (~12 arcmin) over a large fraction of the sky (around 30%) at 143, 217, 353, and 545 GHz. The Archeops 353 GHz channel consists of three pairs of polarized sensitive bolometers designed to detect the polarized diffuse emission of Galactic dust.
Published: 2007
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11. Galactic Bulge microlensing optical depth from EROS-2

Author: Hamadache, C., Le Guillou, L., Tisserand, P., Afonso, C., Albert, J. N., Andersen, J., Ansari, R., Aubourg, É., 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, É., Loup, C., Magneville, C., Marquette, J. B., Maurice, É., Maury, A., Milsztajn, A., Moniez, M., Palanque-Delabrouille, N., Perdereau, O., Rahal, Y. R., Rich, J., Spiro, M., Vidal-Madjar, A., Vigroux, L., Zylberajch, S., Hamadache, C., Le Guillou, L., Tisserand, P., Afonso, C., Albert, J. N., Andersen, J., Ansari, R., Aubourg, É., 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, É., Loup, C., Magneville, C., Marquette, J. B., Maurice, É., 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.
Abstract: Aims.We present a new EROS-2 measurement of the microlensing optical depth toward the Galactic Bulge.
Published: 2006
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12. The OGLE-II event sc5_2859: a classical nova outburst?

Author: Afonso, C., Glicenstein, J. F., Gould, A., Smith, M. C., Wagner, R. M., Albert, J. N., Andersen, J., Ansari, R., Aubourg, É., Bareyre, P., Beaulieu, J. P., Blanc, G., Charlot, X., Coutures, C., Ferlet, R., Fouqué, P., Goldman, B., Graff, D., Gros, M., Haissinski, J., Hamadache, C., de Kat, J., LeGuillou, L., Lesquoy, É., Loup, C., Magneville, C., Marquette, J. B., Maurice, É., Maury, A., Milsztajn, A., Moniez, M., Palanque-Delabrouille, N., Perdereau, O., Prévot, L., Rahal, Y. R., Rich, J., Spiro, M., Tisserand, P., Vidal-Madjar, A., Vigroux, L., Zylberajch, S., Afonso, C., Glicenstein, J. F., Gould, A., Smith, M. C., Wagner, R. M., Albert, J. N., Andersen, J., Ansari, R., Aubourg, É., Bareyre, P., Beaulieu, J. P., Blanc, G., Charlot, X., Coutures, C., Ferlet, R., Fouqué, P., Goldman, B., Graff, D., Gros, M., Haissinski, J., Hamadache, C., de Kat, J., LeGuillou, L., Lesquoy, É., Loup, C., Magneville, C., Marquette, J. B., Maurice, É., Maury, A., Milsztajn, A., Moniez, M., Palanque-Delabrouille, N., Perdereau, O., Prévot, L., Rahal, Y. R., Rich, J., Spiro, M., Tisserand, P., Vidal-Madjar, A., Vigroux, L., and Zylberajch, S.
Abstract: Context.The OGLE-II event sc5_2859 was previously identified as the third longest microlensing event ever observed.Aims.Additional photometric observations from the EROS (Expérience de Recherche d'Objets Sombres) survey and spectroscopic observations of the candidate star are used to test the microlensing hypothesis.Methods.The combined OGLE and EROS data provide a high quality coverage of the light curve. The colour of the sc5_2859 event is seen to change with time. A spectrum taken in 2003 exhibits a strong Hαemission line.Results.The additionnal data show that the OGLE-II sc5_2859 event is actually a classical nova outburst.
Published: 2006
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13. The CMB temperature power spectrum from an improved analysis of the Archeops data

Author: Tristram, M., Patanchon, G., Macías-Pérez, J. F., Ade, P., Amblard, A., Ansari, R., Aubourg, É., Benoît, A., Bernard, J.-Ph., Blanchard, A., Bock, J. J., Bouchet, F. R., Bourrachot, A., Camus, P., Cardoso, J.-F., Couchot, F., de Bernardis, P., Delabrouille, J., Désert, F.-X., Douspis, M., Dumoulin, L., Filliatre, Ph., Fosalba, P., Giard, M., Giraud-Héraud, Y., Gispert†, R., Guglielmi, L., Hamilton, J.-Ch., Hanany, S., Henrot-Versillé, S., Kaplan, J., Lagache, G., Lamarre, J.-M., Lange, A. E., Madet, K., Maffei, B., Magneville, Ch., Masi, S., Mayet, F., Nati, F., Perdereau, O., Plaszczynski, S., Piat, M., Ponthieu, N., Prunet, S., Renault, C., Rosset, C., Santos, D., Vibert, D., Yvon, D., Tristram, M., Patanchon, G., Macías-Pérez, J. F., Ade, P., Amblard, A., Ansari, R., Aubourg, É., Benoît, A., Bernard, J.-Ph., Blanchard, A., Bock, J. J., Bouchet, F. R., Bourrachot, A., Camus, P., Cardoso, J.-F., Couchot, F., de Bernardis, P., Delabrouille, J., Désert, F.-X., Douspis, M., Dumoulin, L., Filliatre, Ph., Fosalba, P., Giard, M., Giraud-Héraud, Y., Gispert†, R., Guglielmi, L., Hamilton, J.-Ch., Hanany, S., Henrot-Versillé, S., Kaplan, J., Lagache, G., Lamarre, J.-M., Lange, A. E., Madet, K., Maffei, B., Magneville, Ch., Masi, S., Mayet, F., Nati, F., Perdereau, O., Plaszczynski, S., Piat, M., Ponthieu, N., Prunet, S., Renault, C., Rosset, C., Santos, D., Vibert, D., and Yvon, D.
Abstract: We present improved results on the measurement of the angular power spectrum of the Cosmic Microwave Background (CMB) temperature anisotropies using the data from the last Archeopsflight. This refined analysis is obtained by using the 6 most sensitive photometric pixels in the CMB bands centered at 143 and 217 GHz and 20% of the sky, mostly clear of foregrounds. Using two different cross-correlation methods, we obtain very similar results for the angular power spectrum. Consistency checks are performed to test the robustness of these results paying particular attention to the foreground contamination level which remains well below the statistical uncertainties. The multipole range from $\ell=10$to $\ell=700$is covered with 25 bins, confirming strong evidence for a plateau at large angular scales (the Sachs-Wolfe plateau) followed by two acoustic peaks centered around $\ell=220$and $\ell=550$respectively. These data provide an independent confirmation, obtained at different frequencies, of the Wmapfirst year results.
Published: 2005
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14. EROS 2 photometry of probable R Coronae Borealis stars in the Small Magellanic Cloud*

Author: Tisserand, P., Marquette, J. B., Beaulieu, J. P., de Laverny, P., Lesquoy, É., Milsztajn, A., Afonso, C., Albert, J. N., Andersen, J., Ansari, R., Aubourg, É., Bareyre, P., Bauer, F., Blanc, G., Charlot, X., 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., Lasserre, T., Le Guillou, L., Loup, C., Magneville, C., Mansoux, B., Maurice, É., Maury, A., Moniez, M., Palanque-Delabrouille, N., Perdereau, O., Prévot, L., Rahal, Y., Regnault, N., Rich, J., Spiro, M., Vidal-Madjar, A., Vigroux, L., Zylberajch, S., Tisserand, P., Marquette, J. B., Beaulieu, J. P., de Laverny, P., Lesquoy, É., Milsztajn, A., Afonso, C., Albert, J. N., Andersen, J., Ansari, R., Aubourg, É., Bareyre, P., Bauer, F., Blanc, G., Charlot, X., 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., Lasserre, T., Le Guillou, L., Loup, C., Magneville, C., Mansoux, B., Maurice, É., Maury, A., Moniez, M., Palanque-Delabrouille, N., Perdereau, O., Prévot, L., Rahal, Y., Regnault, N., Rich, J., Spiro, M., Vidal-Madjar, A., Vigroux, L., and Zylberajch, S.
Abstract: EROS 2 (Expérience de Recherche d'Objets Sombres) conducted a survey of the SMC between July 1996 and February 2003 in two EROS broad-band colours, VEand RE. The photometric data of 4.2 million stars have been searched for behaviour typical of R Coronae Borealis (RCB) candidates such as drastic changes in magnitude. Five objects have been found, four of them being catalogued in the Simbad database as RAW 21, RAW 233, RAW 476, and [MH95] 431with confirmed carbon-rich atmospheres, characteristic of RCB. From the EROS 2 light curve of RAW 21and its spectrum reported by [CITE], we confirm that it is the first RCB to be found in the SMC. The other objects are new RCB candidates with absolute luminosity and colour close to those found for RCBs in the LMC. We propose that 2 of them are DY Per-like RCBs.
Published: 2004
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15. 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, É., Balland, C., Bareyre, P., Beaulieu, J. P., Charlot, X., Conley, A., Coutures, C., Dahlén, T., Derue, F., Fan, X., Ferlet, R., Folatelli, G., Fouqué, 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., de Kat, J., Kent, S., Kim, A., Lasserre, T., Le Guillou, L., Lesquoy, É., Loup, C., Magneville, C., Marquette, J. B., Maurice, É., Maury, A., Milsztajn, A., Moniez, M., Mouchet, M., Newberg, H., Nobili, S., Palanque-Delabrouille, N., Perdereau, O., Prévot, L., Rahal, Y. R., Regnault, N., Rich, J., Ruiz-Lapuente, P., Spiro, M., Tisserand, P., Vidal-Madjar, A., Vigroux, L., Walton, N. A., Zylberajch, S., Blanc, G., Afonso, C., Alard, C., Albert, J. N., Aldering, G., Amadon, A., Andersen, J., Ansari, R., Aubourg, É., Balland, C., Bareyre, P., Beaulieu, J. P., Charlot, X., Conley, A., Coutures, C., Dahlén, T., Derue, F., Fan, X., Ferlet, R., Folatelli, G., Fouqué, 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., de Kat, J., Kent, S., Kim, A., Lasserre, T., Le Guillou, L., Lesquoy, É., Loup, C., Magneville, C., Marquette, J. B., Maurice, É., Maury, A., Milsztajn, A., Moniez, M., Mouchet, M., Newberg, H., Nobili, S., Palanque-Delabrouille, N., Perdereau, O., Prévot, 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.
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 / $10^{10}\ {L}_{\odot}^B$/ century. This value is compatible with the previous EROS measurement [CITE], 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.
Published: 2004
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16. Study of a strategy for parallax microlensing detection towards the Magellanic Clouds

Author: Rahvar, S., Moniez, M., Ansari, R., Perdereau, O., Rahvar, S., Moniez, M., Ansari, R., and Perdereau, O.
Abstract: In this article, we have investigated the possibility to distinguish between different galactic models through microlensing parallax studies. We show that a systematic search for parallax effects can be done using the currently running alert systems and complementary photometric telescopes, to distinguish between different lens distance distributions. We have considered two galactic dark compact object distributions, with total optical depths corresponding to the EROS current upper limits. These models correspond to two extreme hypotheses on a three component galactic structure made of a thin disk, a thick disk, and a spherically symmetric halo. Our study shows that for sub-solar mass lenses, an exposure of $8\times 10^7$star $\times$yr toward the LMC should allow one to distinguish between these two extreme models. In addition, the self-lensing hypothesis (lensing by LMC objects) can efficiently be tested through the method proposed here.
Published: 2003
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17. Bulge microlensing optical depth from EROS 2 observations $^{\bullet}$*

Author: Afonso, C., Albert, J. N., Alard, C., 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., Fouqué, P., Glicenstein, J. F., Goldman, B., Gould, A., Graff, D., Gros, M., Haissinski, J., Hamadache, C., 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., Maury, A., Milsztajn, A., Moniez, M., Palanque-Delabrouille, N., Perdereau, O., Prévot, L., Regnault, N., Rich, J., Spiro, M., Tisserand, P., Vidal-Madjar, A., Vigroux, L., Zylberajch, S., Afonso, C., Albert, J. N., Alard, C., 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., Fouqué, P., Glicenstein, J. F., Goldman, B., Gould, A., Graff, D., Gros, M., Haissinski, J., Hamadache, C., 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., Maury, A., Milsztajn, A., Moniez, M., Palanque-Delabrouille, N., Perdereau, O., Prévot, L., Regnault, N., Rich, J., Spiro, M., Tisserand, P., Vidal-Madjar, A., Vigroux, L., and Zylberajch, S.
Abstract: We present a measurement of the microlensing optical depth toward the Galactic bulge based on the analysis of 15 contiguous $1\,\rm deg^2$fields centered on $(l=2.\hskip-2pt^\circ 5, b=-4.\hskip-2pt^\circ 0)$and containing $N_*=1.42\times 10^{6}$clump-giant stars (belonging to the extended clump area) monitored during almost three bulge seasons by EROS (Expérience de Recherche d'Objets Sombres). We find $\tau_{\rm bulge}=0.94\pm 0.29\times 10^{-6}$averaged over all fields, based on 16 microlensing events with clump giants as sources. This value is substantially below several other determinations by the MACHO and OGLE groups and is more in agreement with what is expected from axisymmetric and non-axisymmetric bulge models.
Published: 2003
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18. Optical design and modelling of the QUBIC instrument, a next-generation quasi-optical bolometric interferometer for cosmology

Author: Holland, Wayne S., Zmuidzinas, Jonas, Scully, S., Burke, D., O'Sullivan, C., Gayer, D., Gradziel, M., Murphy, J. A., De Petris, M., Buzi, D., Zannoni, M., Mennella, A, Gervasi, M., Tartari, A., Maffei, B., Aumont, J., Banfi, S., Battaglia, P., Battistelli, E. S., Baù, A., Bélier, B., Bennet, D., Bergé, L., Bernard, J.-Ph., Bersanelli, M., Bigot-Sazy, M.-A., Bleurvacq, N., Bordier, G., Brossard, J., Bunn, E. F., Cammileri, D., Cavaliere, F., Chanial, P., Chapron, C., Coppolecchia, A., Couchot, F., D'Alessandro, G., De Bernardis, P., Decourcelle, T., Del Torto, F., Dumoulin, L., Franceschet, C., Gault, A., Ghribi, A., Giard, M., Giraud-Héraud, Y., Grandsire, L., Hamilton, J. C., Haynes, V., Henrot-Versillé, S., Holtzer, N., Kaplan, J., Korotkov, A., Lande, J., Lowitz, A., Marnieros, S., Martino, J., Masi, S., McCulloch, Mark, Melhuish, Simon, Montier, L., Néel, D., Ng, M. W., Pajot, F., Passerini, A., Perbost, C., Perdereau, O., Piacentini, F., Piat, M., Piccirillo, L., Pisano, G., Prêle, D., Puddu, R., Rambaud, D., Rigaut, O., Salatino, M., Schillaci, A., Stolpovskiy, M., Timbie, P., Tristram, M., Tucker, G., Viganò, D., Voisin, F., and Watson, B.
Published: 2016
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19. Limits on Galactic dark matter with 5 years of EROS SMC data*

Author: Afonso, C., Albert, J. N., Andersen, J., Ansari, R., Aubourg, É., Bareyre, P., Beaulieu, J. P., Blanc, G., Charlot, X., Couchot, F., 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., Le Guillou, L., Lesquoy, É., Loup, C., Magneville, C., Marquette, J. B., Maurice, É., Maury, A., Milsztajn, A., Moniez, M., Palanque-Delabrouille, N., Perdereau, O., Prévot, L., Rahal, Y. R., Rich, J., Spiro, M., Tisserand, P., Vidal-Madjar, A., Vigroux, L., Zylberajch, S., Afonso, C., Albert, J. N., Andersen, J., Ansari, R., Aubourg, É., Bareyre, P., Beaulieu, J. P., Blanc, G., Charlot, X., Couchot, F., 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., Le Guillou, L., Lesquoy, É., Loup, C., Magneville, C., Marquette, J. B., Maurice, É., Maury, A., Milsztajn, A., Moniez, M., Palanque-Delabrouille, N., Perdereau, O., Prévot, L., Rahal, Y. R., Rich, J., Spiro, M., Tisserand, P., Vidal-Madjar, A., Vigroux, L., and Zylberajch, S.
Abstract: Five years of erosdata towards the Small Magellanic Cloud have been searched for gravitational microlensing events, using a new, more accurate method to assess the impact of stellar blending on the efficiency. Four long-duration candidates have been found which, if they are microlensing events, hint at a non-halo population of lenses. Combined with results from other erosobservation programs, this analysis yields strong limits on the amount of Galactic dark matter made of compact objects. Less than 25% of a standard halo can be composed of objects with a mass between $2\times10^{-7}~M_\odot$and 1 $M_\odot$at the 95% C.L.
Published: 2003
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20. 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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21. EROS 2 proper motion survey: Constraints on the halo white dwarfs*

Author: Goldman, B., Afonso, C., Alard, Ch., Albert, J.-N., Amadon, A., Andersen, J., Ansari, R., Aubourg, É., Bareyre, P., Bauer, F., Beaulieu, J.-Ph., Blanc, G., Bouquet, A., Charlot, X., Couchot, F., Coutures, Ch., Derue, F., Ferlet, R., Fouqué, P., Glicenstein, J.-F., Gould, A., Graff, D., Gros, M., Haïssinski, J., Hamadache, C., Hamilton, J.-Ch., Hardin, D., de Kat, J., Kim, A., Lasserre, Th., Le Guillou, L., Lesquoy, É., Loup, C., Magneville, Ch., Mansoux, B., Marquette, J.-B., Maurice, É., Maury, A., Milsztajn, A., Moniez, M., Palanque-Delabrouille, N., Perdereau, O., Prévot, L., Regnault, N., Rich, J., Spiro, M., Tisserand, P., Vidal-Madjar, A., Vigroux, L., Zylberajch, S., Goldman, B., Afonso, C., Alard, Ch., Albert, J.-N., Amadon, A., Andersen, J., Ansari, R., Aubourg, É., Bareyre, P., Bauer, F., Beaulieu, J.-Ph., Blanc, G., Bouquet, A., Charlot, X., Couchot, F., Coutures, Ch., Derue, F., Ferlet, R., Fouqué, P., Glicenstein, J.-F., Gould, A., Graff, D., Gros, M., Haïssinski, J., Hamadache, C., Hamilton, J.-Ch., Hardin, D., de Kat, J., Kim, A., Lasserre, Th., Le Guillou, L., Lesquoy, É., Loup, C., Magneville, Ch., Mansoux, B., Marquette, J.-B., Maurice, É., Maury, A., Milsztajn, A., Moniez, M., Palanque-Delabrouille, N., Perdereau, O., Prévot, L., Regnault, N., Rich, J., Spiro, M., Tisserand, P., Vidal-Madjar, A., Vigroux, L., and Zylberajch, S.
Abstract: We are conducting a $377^{\circ 2}$proper motion survey in the ~Vand Ibands in order to determine the cool white dwarf contribution to the Galactic dark matter. Using the $250^{\circ 2}$for which we possess three epochs, and applying selection criteria designed to isolate halo-type objects, we find no candidates in a $5500\,{\rm pc}^3$effective volume for old, fast MV=17 white dwarfs. We check the detection efficiency by cross-matching our catalogue with Luyten's NLTT catalogue. The halo white dwarf contribution cannot exceed 5% (95% C.L.) for objects with and . The same conclusion applies to a 14 Gyr halo composed of white dwarfs with hydrogen atmosphere, as modeled by Chabrier.
Published: 2002
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22. Blue irregular variable stars in the Small Magellanic Cloud from EROS2: Herbig Ae/Be or classical Be stars?*

Author: Beaulieu, J.-P., de Wit, W. J., Lamers, H. J. G. L. M., Marquette, J.-B., Coutures, C., Leisy, P., Totor, S., Palanque-Delabrouille, N., Afonso, C., Alard, C., Albert, J. N., Andersen, J., Ansari, R., Aubourg, É., Bareyre, P., Bauer, F., Blanc, G., Charlot, X., Couchot, F., Derue, F., Ferlet, R., Fouqué, P., Glicenstein, J. F., Goldman, B., Graff, D., Gros, M., Haissinski, J., Hamilton, J. C., Hardin, D., de Kat, J., Lasserre, T., Lesquoy, É., Loup, C., Magneville, C., Mansoux, B., Maurice, É., Milsztajn, A., Moniez, M., Perdereau, O., Prévot, L., Regnault, N., Rich, J., Spiro, M., Vidal-Madjar, A., Vigroux, L., Zylberajch, S., Beaulieu, J.-P., de Wit, W. J., Lamers, H. J. G. L. M., Marquette, J.-B., Coutures, C., Leisy, P., Totor, S., Palanque-Delabrouille, N., Afonso, C., Alard, C., Albert, J. N., Andersen, J., Ansari, R., Aubourg, É., Bareyre, P., Bauer, F., Blanc, G., Charlot, X., Couchot, F., Derue, F., Ferlet, R., Fouqué, P., Glicenstein, J. F., Goldman, B., Graff, D., Gros, M., Haissinski, J., Hamilton, J. C., Hardin, D., de Kat, J., Lasserre, T., Lesquoy, É., Loup, C., Magneville, C., Mansoux, B., Maurice, É., Milsztajn, A., Moniez, M., Perdereau, O., Prévot, L., Regnault, N., Rich, J., Spiro, M., Vidal-Madjar, A., Vigroux, L., and Zylberajch, S.
Abstract: Using data from the EROS2 microlensing survey, we report the discovery of two blue objects with irregular photometric behaviour of $\Delta V \sim 0.1$-0.4 mag on time scales of 20 to 200 days. They show a bluer when fainter behaviour. Subsequent spectra taken with the ESO 3.6 m telescope show spectral type B4eIII and B2eIV-V with strong ${\rm H} \alpha$emission. These objects resemble the Herbig AeBe but also classical Be stars. At this stage, it is not possible to distinguish unambiguously between pre-main sequence and classical Be nature. If we favour the pre-main sequence interpretation, they are more luminous than the luminosity upper limit for Galactic HAeBe stars. The same was found for the HAeBe candidates in the LMC. This might be due to a shorter accretion time scale ($\tau = M_*/\dot{M}$), or the smaller dust content during the pre-main sequence evolution of SMC and LMC stars. Further studies on a larger scale of the environment and IR properties of the stars are needed.
Published: 2001
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23. 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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24. Observation of microlensing toward the galactic spiral arms. EROS II 3 year survey *

Author: Derue, F., Afonso, C., Alard, C., Albert, J.-N., 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., 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., Derue, F., Afonso, C., Alard, C., Albert, J.-N., 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., 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., and Zylberajch, S.
Abstract: We present an analysis of the light curves of 9.1 million stars observed during three seasons by EROS(Expérience de Recherche d'Objets Sombres), in the Galactic plane away from the bulge. Seven stars exhibit luminosity variations compatible with gravitational microlensing effects due to unseen objects. The corresponding optical depth, averaged over four directions, is $\bar\tau = 0.43 \pm 0.2 \times 10^{-6}$. While this value is compatible with expectations from simple Galactic models under reasonable assumptions on the target star distances, we find an excess of events with short timescales toward the direction closest to the Galactic centre. We discuss a possible interpretation involving the contribution of an elongated bar.
Published: 2001
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25. AGAPEROS: Searching for microlensing in the LMC with the pixel method

Author: Melchior, A.-L., Afonso, C., Ansari, R., Aubourg, É., Baillon, P., Bareyre, P., Bauer, F., Beaulieu, J.-Ph., Bouquet, A., Brehin, S., Cavalier, F., Char, S., Couchot, F., Coutures, C., Ferlet, R., Fernandez, J., Gaucherel, C., Giraud-Héraud, Y., Glicenstein, J.-F., Goldman, B., Gondolo, P., Gros, M., Guibert, J., Hardin, D., Kaplan, J., de Kat, J., Lachièze-Rey, M., Laurent, B., Lesquoy, É., Magneville, Ch., Mansoux, B., Marquette, J.-B., Maurice, E., Milsztajn, A., Moniez, M., Moreau, O., Moscoso, L., Palanque-Delabrouille, N., Perdereau, O., Prévôt, L., Renault, C., Queinnec, F., Rich, J., Spiro, M., Vidal-Madjar, A., Vigroux, L., Zylberajch, S., Melchior, A.-L., Afonso, C., Ansari, R., Aubourg, É., Baillon, P., Bareyre, P., Bauer, F., Beaulieu, J.-Ph., Bouquet, A., Brehin, S., Cavalier, F., Char, S., Couchot, F., Coutures, C., Ferlet, R., Fernandez, J., Gaucherel, C., Giraud-Héraud, Y., Glicenstein, J.-F., Goldman, B., Gondolo, P., Gros, M., Guibert, J., Hardin, D., Kaplan, J., de Kat, J., Lachièze-Rey, M., Laurent, B., Lesquoy, É., Magneville, Ch., Mansoux, B., Marquette, J.-B., Maurice, E., Milsztajn, A., Moniez, M., Moreau, O., Moscoso, L., Palanque-Delabrouille, N., Perdereau, O., Prévôt, L., Renault, C., Queinnec, F., Rich, J., Spiro, M., Vidal-Madjar, A., Vigroux, L., and Zylberajch, S.
Abstract: Recent surveys monitoring millions of light curves of resolved stars in the LMC have discovered several microlensing events. Unresolved stars could however significantly contribute to the microlensing rate towards the LMC. Monitoring pixels, as opposed to individual stars, should be able to detect stellar variability as a variation of the pixel flux. We present a first application of this new type of analysis (Pixel Method) to the LMC Bar. We describe the complete procedure applied to the EROS 91-92 data (one tenth of the existing CCD data set) in order to monitor pixel fluxes. First, geometric and photometric alignments are applied to each image. Averaging the images of each night reduces significantly the noise level. Second, one light curve for each of the $2.1~10^6$pixels is built and pixels are lumped into 3.6″ × 3.6″ super-pixels, one for each elementary pixel. An empirical correction is then applied to account for seeing variations. We find that the final super-pixel light curves fluctuate at a level of 1.8% of the flux in blue and 1.3% in red. We show that this noise level corresponds to about twice the expected photon noise and confirms previous assumptions used for the estimation of the contribution of unresolved stars. We also demonstrate our ability to correct very efficiently for seeing variations affecting each pixel flux. The technical results emphasised here show the efficacy of the Pixel Method and allow us to study luminosity variations due to possible microlensing events and variable stars in two companion papers.
Published: 1999
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26. New Magellanic Cloud R Coronae Borealis and DY Persei type stars from the EROS-2 database: the connection between RCBs, DYPers, and ordinary carbon stars

Author: Tisserand, P., Wood, P., Marquette, J., Afonso, C., Albert, J., Andersen, J., Ansari, R., Aubourg, ?., Bareyre, P., Beaulieu, J., Charlot, X., Coutures, C., Ferlet, R., Fouqu?, P., Glicenstein, J., Goldman, B., Gould, A., Gros, M., de Kat, J., Lesquoy, ?., Loup, C., Magneville, C., Maurice, ?., Maury, A., Milsztajn, A., Moniez, M., Palanque-Delabrouille, N., Perdereau, O., Rich, J., Schwemling, P., Spiro, M., and Vidal-Madjar, A.
Abstract: Context. R Coronae Borealis stars (RCB) are a rare type of evolved carbon-rich supergiant stars that are increasingly thought to result from the merger of two white dwarfs, called the Double degenerate scenario. This scenario is also studied as a source, at higher mass, of type Ia Supernovae (SnIa) explosions. Therefore a better understanding of RCBs composition would help to constrain simulations of such events.Aims. We searched for and studied RCB stars in the EROS Magellanic Clouds database. We also extended our research to DY?Per?type stars (DYPers) that are expected to be cooler RCBs (T ?3500?K) and much more numerous than their hotter counterparts. With the aim of studying possible evolutionary connections between RCBs and DYPers, and also ordinary carbon stars, we compared their publically available broad band photometry in the optical, near, and mid-infrared.Methods. The light curves of ~70?millions stars, monitored for 6.7?years (from July 1996 to February 2003), have been analysed to search for the main signature of RCBs and DYPers: a large (up to 9?mag) drop in luminosity. Carbon stars with fading episodes were also found by inspecting numerous light curves of objects that presented an infrared excess in the 2MASS and Spitzer- SAGE and S3MC databases. Follow-up optical spectroscopy was used to confirm each photometric candidate found.Results. We have discovered and confirmed 6?new Magellanic Cloud RCB stars and 7?new DYPers, but also listed new candidates: 3?RCBs and 14?DYPers. Optical and infrared colour magnitude diagrams that give new insights into these two sets of stars are discussed. We estimated a range of Magellanic RCB shell temperatures between 360 and 600?K.Conclusions. We confirm the wide range of absolute luminosity known for RCB?stars, MV?-5.2 to ?2.6. Our study further shows that mid-infrared surveys are ideal to search for RCB stars, since they have thinner and cooler circumstellar shells than classical post-AGB stars. In addition, by increasing the number of known DYPers by ~400%, we have been able to shed light on the similarities in the spectral energy distribution between DYPers and ordinary carbon stars. We also observed that DYPer circumstellar shells are fainter and hotter than those of RCBs. This suggests that DYPers may simply be ordinary carbon stars with ejection events, but more abundance analysis is necessary to give a status on a possible evolutionnary connexion between RCBs and DYPers.
Published: 2009

27. Measurement of the branching ratio of the double Dalitz decayKL→e+e−e+e− and the CP parity of theKL-meson

Author: Barr, G. D., Buchholz, P., Cundy, D., Doble, N., Gatignon, L., Grafström, P., Hagelberg, R., Wahl, H., Peach, K. J., Beier, T., Blümer, H., Coward, D., Heinz, R., Kleinknecht, K., Leber, F., Mayer, P., Renk, B., Rohrer, H., Sander, H. G., Scheidt, J., Staeck, J., Wagner, A., Augé, E., Fournier, D., Iconomidou-Fayard, L., Perdereau, O., Schaffer, A. C., Serin, L., Bertanza, L., Calafiura, P., Calvetti, M., Carosi, R., Casali, R., Cerri, C., Mannelli, I., Marzulli, V. M., Nappi, A., Pierazzini, G. M., Holder, M., Kreutz, A., Rost, M., and Werthenbach, R.
Abstract: Data from the NA31 experiment at CERN have been used to measure the branching ratio of the double Dalitz decay of the long-lived neutral kaon. Eight events have been found with negligible background. The measured distribution of the angle between the planes of the two e+e−-pairs favours aCP=−1 state for the long-lived neutral kaon.
Published: 1995
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28. Determination of the atmospheric neutrino spectra with the Fréjus detector

Author: Daum, K., Rhode, W., Bareyre, P., Barloutaud, R., Chardin, G., Degrange, B., Ernwein, J., Kuznik, B., Meyer, H., Mosca, L., Moscoso, L., Perdereau, O., Schubnell, M., Tisserant, S., and Wei, Y.
Abstract: The combined analysis of the final event set of data on neutrino interactions inside the detector, upward going stopping muons and horizontal muons recorded in the Fréjus experiment is presented. The absolute atmospheric neutrino spectra in the energy range for electron neutrinos and for muon neutrinos are determined. Based on the parameterization of Volkova for thevµ a spectral index of ?=2.66±0.05 is obtained from the ratio of horizontal muons over upward going stopping muons and from the measurement of the energy loss of horizontal muons inside the detector. The neutrino spectra are compared with various flux calculations. They do not show any evidence for neutrino oscillations in agreement with earlier analyses of the Fréjus data.
Published: 1995
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29. Determination of the branching ratiosΓ(KL→3π0)/Γ(KL→π+-0) andΓ(KL→3π0)/Γ(KL→πev)

Author: Kreutz, A., Holder, M., Rost, M., Werthenbach, R., Peach, K. J., Blümer, H., Heinz, R., Kleinknecht, K., Mayer, P., Panzer, B., Renk, B., Rohrer, H., Wagner, A., Augé, E., Fournier, D., Iconomidou-Fayard, L., Perdereau, O., Schaffer, A. C., Serin, L., Bertanza, L., Bigi, A., Calafiura, P., Calvetti, M., Carosi, R., Casali, R., Cerri, C., Mannelli, I., Marzulli, V., Nappi, A., and Pierazzini, G. M.
Abstract: Improved branching ratios were measured for theKL→3π0 decay in a neutral beam at the CERN SPS with the NA31 detector: $$\Gamma ({\rm K}_L \to 3\pi ^0 )/\Gamma ({\rm K}_L \to \pi ^ + \pi ^ - \pi ^0 ) = 1.611 \pm 0.037$$ and $$\Gamma ({\rm K}_L \to 3\pi ^0 )/\Gamma ({\rm K}_L \to \pi ev) = 0.545 \pm 0.010.$$ From the first number an upper limit for ΔI=5/2 and ΔI=7/2 transitions in neutral kaon decay is derived. Using older results for the Ke3/Kμ3 fraction, the 3π0 branching ratio is found to beΓ(KL→3π0)/Γtot=(0.211±0.003), about a factor three more precise than from previous experiments.
Published: 1995
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30. Results from the Fréjus experiment on nucleon decay modes with charged leptons

Author: Berger, Ch., Fröhlich, M., Mönch, H., Nisius, R., Raupach, F., Schleper, P., Benadjal, Y., Blum, D., Bourdarios, C., Dudelzak, B., Eschstruth, P., Jullian, S., Lalanne, D., Laplanche, F., Longuemare, C., Paulot, C., Perdereau, O., Roy, Ph., Szklarz, G., Behr, L., Degrange, B., Nguyen-Khac, U., Tisserant, S., Arpesella, C., Bareyre, P., Barloutaud, R., Borg, A., Chardin, G., Ernwein, J., Glicenstein, J. F., Mosca, L., Moscoso, L., Becker, J., Becker, K. H., Daum, H. J., Jacobi, B., Kuznik, B., Löffler, J., Meyer, H., Möller, R., Schubnell, M., Wei, Y., and Wintgen, P.
Abstract: Lower limits on the nucleon lifetime in channels containing at least one positron or muon are given. The analysis is based on 4 years of data taking with the Fréjus detector. Various approaches to determine the background from atmospheric neutrinos are discussed and two different nuclear models are used in event simulations. The limits obtained range from 1031 years forp?e+K*0 to 1.5·1032 years forp?e+K*0 to 1.5·1032 years forp?µ+?.
Published: 1991
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31. A search for high energy neutrinos from SN 1987A, the Carb, Hercules X-1, and Cygnus X-3 with the Fréjus detector

Author: Berger, Ch., Fröhlich, M., Mönch, H., Nisius, R., Raupach, F., Benadjal, Y., Blum, D., Bourdarios, C., Dudelzak, B., Eschstruth, P., Jullian, S., Lalanne, D., Laplanche, F., Longuemare, C., Paulot, C., Perdereau, O., Roy, Ph., Szklarz, G., Behr, L., Degrange, B., Minet, Y., Nguyen-Khac, U., Tisserant, S., Arpesella, C., Bareyre, P., Barloutaud, R., Borg, A., Chardin, G., Ernwein, J., Glicenstein, J. F., Mosca, L., Moscoso, L., Becker, J., Becker, K. H., Daum, H. J., Jacobi, B., Kuznik, B., Meyer, H., Möller, R., Schubnell, M., and Wei, Y.
Abstract: With the Fréjus detector we studied four astrophysical point-like sources by using and interactions in the detector and interactions in the surrounding rock. No excess of events was found. Therefore upper limits of neutrino fluxes and source luminositics are quoted. These limits confirm results from other experiments. In addition new limits are presented for spectral indices above 3.
Published: 1990
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32. Performance of NbSi transition-edge sensors readout with a 128 MUX factor for the QUBIC experiment

Author: Zmuidzinas, Jonas, Gao, Jian-Rong, Salatino, M., Bélier, B., Chapron, C., Hoang, D. T., Maestre, S., Marnieros, S., Marty, W., Montier, L., Piat, M., Prêle, D., Rambaud, D., Thermeau, J. P., Torchinsky, S. A., Henrot-Versillé, S., Voisin, F., Ade, P., Amico, G., Auguste, D., Aumont, J., Banfi, S., Barbarán, G., Battaglia, P., Battistelli, E., Baù, A., Bennett, D., Bergé, L., Bernard, J.-Ph., Bersanelli, M., Bigot-Sazy, M.-A., Bleurvacq, N., Bonaparte, J., Bonis, J., Bordier, G., Bréelle, E., Bunn, E., Burke, D., Buzi, D., Buzzelli, A., Cavaliere, F., Chanial, P., Charlassier, R., Columbro, F., Coppi, G., Coppolecchia, A., Couchot, F., D'Agostino, R., D’Alessandro, G., de Bernardis, P., De Gasperis, G., De Leo, M., De Petris, M., Di Donato, A., Dumoulin, L., Etchegoyen, A., Fasciszewski, A., Franceschet, C., Gamboa Lerena, M. M., García, B., Garrido, X., Gaspard, M., Gault, A., Gayer, D., Gervasi, M., Giard, M., Giraud-Héraud, Y., Gómez Berisso, M., González, M., Gradziel, M., Grandsire, L., Guerrard, E., Hamilton, J.-Ch., Harari, D., Haynes, V., Incardona, F., Jules, E., Kaplan, J., Korotkov, A., Kristukat, C., Lamagna, L., Loucatos, S., Louis, T., Lowitz, A., Lukovic, V., Luterstein, R., Maffei, B., Masi, S., Mattei, A., May, A. J., McCulloch, M. A., Medina, M. C., Mele, L., Melhuish, S., Mennella, A., Mundo, L. M., Murphy, J. A., Murphy, J. D., O'Sullivan, C., Olivieri, E., Paiella, A., Pajot, F., Passerini, A., Pastoriza, H., Pelosi, A., Perbost, C., Perdereau, O., Pezzotta, F., Piacentini, F., Piccirillo, L., Pisano, G., Polenta, G., Puddu, R., Ringegni, P., Romero, G. E., Schillaci, A., Scóccola, C. G., Scully, S., Spinelli, S., Stolpovskiy, M., Suarez, F., Tartari, A., Timbie, P., Tristram, M., Truongcanh, V., Tucker, C., Tucker, G., Vanneste, S., Viganò, D., Vittorio, N., Watson, B., Wicek, F., Zannoni, M., and Zullo, A.
Published: 2018
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33. Iterative destriping and photometric calibration for Planck-HFI, polarized, multi-detector map-making

Author: Tristram, M., Filliard, C., Perdereau, O., Plaszczynski, S., Stompor, R., and Touze, F.
Abstract: We present an iterative scheme designed to recover calibrated I, Q, and Umaps from Planck-HFI data using the orbital dipole due to the satellite motion with respect to the Solar System frame. It combines a map reconstruction, based on a destriping technique, juxtaposed with an absolute calibration algorithm. We evaluate systematic and statistical uncertainties incurred during both these steps with the help of realistic, Planck-like simulations containing CMB, foreground components and instrumental noise, and assess the accuracy of the sky map reconstruction by considering the maps of the residuals and their spectra. In particular, we discuss destriping residuals for polarization sensitive detectors similar to those of Planck-HFI under different noise hypotheses and show that these residuals are negligible (for intensity maps) or smaller than the white noise level (for Qand UStokes maps), for ℓ> 50. We also demonstrate that the combined level of residuals of this scheme remains comparable to those of the destriping-only case except at very low ℓwhere residuals from the calibration appear. For all the considered noise hypotheses, the relative calibration precision is on the order of a few 10-4, with a systematic bias of the same order of magnitude.
Published: 2011
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34. Planckpre-launch status: The Planckmission

Author: Tauber, J. A., Mandolesi, N., Puget, J.-L., Banos, T., Bersanelli, M., Bouchet, F. R., Butler, R. C., Charra, J., Crone, G., Dodsworth, J., Efstathiou, G., Gispert, R., Guyot, G., Gregorio, A., Juillet, J. J., Lamarre, J.-M., Laureijs, R. J., Lawrence, C. R., Nørgaard-Nielsen, H. U., Passvogel, T., Reix, J. M., Texier, D., Vibert, L., Zacchei, A., Ade, P. A. R., Aghanim, N., Aja, B., Alippi, E., Aloy, L., Armand, P., Arnaud, M., Arondel, A., Arreola-Villanueva, A., Artal, E., Artina, E., Arts, A., Ashdown, M., Aumont, J., Azzaro, M., Bacchetta, A., Baccigalupi, C., Baker, M., Balasini, M., Balbi, A., Banday, A. J., Barbier, G., Barreiro, R. B., Bartelmann, M., Battaglia, P., Battaner, E., Benabed, K., Beney, J.-L., Beneyton, R., Bennett, K., Benoit, A., Bernard, J.-P., Bhandari, P., Bhatia, R., Biggi, M., Biggins, R., Billig, G., Blanc, Y., Blavot, H., Bock, J. J., Bonaldi, A., Bond, R., Bonis, J., Borders, J., Borrill, J., Boschini, L., Boulanger, F., Bouvier, J., Bouzit, M., Bowman, R., Bréelle, E., Bradshaw, T., Braghin, M., Bremer, M., Brienza, D., Broszkiewicz, D., Burigana, C., Burkhalter, M., Cabella, P., Cafferty, T., Cairola, M., Caminade, S., Camus, P., Cantalupo, C. M., Cappellini, B., Cardoso, J.-F., Carr, R., Catalano, A., Cayón, L., Cesa, M., Chaigneau, M., Challinor, A., Chamballu, A., Chambelland, J. P., Charra, M., Chiang, L.-Y., Chlewicki, G., Christensen, P. R., Church, S., Ciancietta, E., Cibrario, M., Cizeron, R., Clements, D., Collaudin, B., Colley, J.-M., Colombi, S., Colombo, A., Colombo, F., Corre, O., Couchot, F., Cougrand, B., Coulais, A., Couzin, P., Crane, B., Crill, B., Crook, M., Crumb, D., Cuttaia, F., Dörl, U., da Silva, P., Daddato, R., Damasio, C., Danese, L., d'Aquino, G., D'Arcangelo, O., Dassas, K., Davies, R. D., Davies, W., Davis, R. J., De Bernardis, P., de Chambure, D., de Gasperis, G., De la Fuente, M. L., De Paco, P., De Rosa, A., De Troia, G., De Zotti, G., Dehamme, M., Delabrouille, J., Delouis, J.-M., Désert, F.-X., di Girolamo, G., Dickinson, C., Doelling, E., Dolag, K., Domken, I., Douspis, M., Doyle, D., Du, S., Dubruel, D., Dufour, C., Dumesnil, C., Dupac, X., Duret, P., Eder, C., Elfving, A., Enßlin, T. A., Eng, P., English, K., Eriksen, H. K., Estaria, P., Falvella, M. C., Ferrari, F., Finelli, F., Fishman, A., Fogliani, S., Foley, S., Fonseca, A., Forma, G., Forni, O., Fosalba, P., Fourmond, J.-J., Frailis, M., Franceschet, C., Franceschi, E., François, S., Frerking, M., Gómez-Reñasco, M. F., Górski, K. M., Gaier, T. C., Galeotta, S., Ganga, K., García Lázaro, J., Garnica, A., Gaspard, M., Gavila, E., Giard, M., Giardino, G., Gienger, G., Giraud-Heraud, Y., Glorian, J.-M., Griffin, M., Gruppuso, A., Guglielmi, L., Guichon, D., Guillaume, B., Guillouet, P., Haissinski, J., Hansen, F. K., Hardy, J., Harrison, D., Hazell, A., Hechler, M., Heckenauer, V., Heinzer, D., Hell, R., Henrot-Versillé, S., Hernández-Monteagudo, C., Herranz, D., Herreros, J. M., Hervier, V., Heske, A., Heurtel, A., Hildebrandt, S. R., Hills, R., Hivon, E., Hobson, M., Hollert, D., Holmes, W., Hornstrup, A., Hovest, W., Hoyland, R. J., Huey, G., Huffenberger, K. M., Hughes, N., Israelsson, U., Jackson, B., Jaffe, A., Jaffe, T. R., Jagemann, T., Jessen, N. C., Jewell, J., Jones, W., Juvela, M., Kaplan, J., Karlman, P., Keck, F., Keihänen, E., King, M., Kisner, T. S., Kletzkine, P., Kneissl, R., Knoche, J., Knox, L., Koch, T., Krassenburg, M., Kurki-Suonio, H., Lähteenmäki, A., Lagache, G., Lagorio, E., Lami, P., Lande, J., Lange, A., Langlet, F., Lapini, R., Lapolla, M., Lasenby, A., Le Jeune, M., Leahy, J. P., Lefebvre, M., Legrand, F., Le Meur, G., Leonardi, R., Leriche, B., Leroy, C., Leutenegger, P., Levin, S. M., Lilje, P. B., Lindensmith, C., Linden-Vørnle, M., Loc, A., Longval, Y., Lubin, P. M., Luchik, T., Luthold, I., Macias-Perez, J. F., Maciaszek, T., MacTavish, C., Madden, S., Maffei, B., Magneville, C., Maino, D., Mambretti, A., Mansoux, B., Marchioro, D., Maris, M., Marliani, F., Marrucho, J.-C., Martí-Canales, J., Martínez-González, E., Martín-Polegre, A., Martin, P., Marty, C., Marty, W., Masi, S., Massardi, M., Matarrese, S., Matthai, F., Mazzotta, P., McDonald, A., McGrath, P., Mediavilla, A., Meinhold, P. R., Mélin, J.-B., Melot, F., Mendes, L., Mennella, A., Mervier, C., Meslier, L., Miccolis, M., Miville-Deschenes, M.-A., Moneti, A., Montet, D., Montier, L., Mora, J., Morgante, G., Morigi, G., Morinaud, G., Morisset, N., Mortlock, D., Mottet, S., Mulder, J., Munshi, D., Murphy, A., Murphy, P., Musi, P., Narbonne, J., Naselsky, P., Nash, A., Nati, F., Natoli, P., Netterfield, B., Newell, J., Nexon, M., Nicolas, C., Nielsen, P. H., Ninane, N., Noviello, F., Novikov, D., Novikov, I., O'Dwyer, I. J., Oldeman, P., Olivier, P., Ouchet, L., Oxborrow, C. A., Pérez-Cuevas, L., Pagan, L., Paine, C., Pajot, F., Paladini, R., Pancher, F., Panh, J., Parks, G., Parnaudeau, P., Partridge, B., Parvin, B., Pascual, J. P., Pasian, F., Pearson, D. P., Pearson, T., Pecora, M., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Pierpaoli, E., Piersanti, O., Plaige, E., Plaszczynski, S., Platania, P., Pointecouteau, E., Polenta, G., Ponthieu, N., Popa, L., Poulleau, G., Poutanen, T., Prézeau, G., Pradell, L., Prina, M., Prunet, S., Rachen, J. P., Rambaud, D., Rame, F., Rasmussen, I., Rautakoski, J., Reach, W. T., Rebolo, R., Reinecke, M., Reiter, J., Renault, C., Ricciardi, S., Rideau, P., Riller, T., Ristorcelli, I., Riti, J. B., Rocha, G., Roche, Y., Pons, R., Rohlfs, R., Romero, D., Roose, S., Rosset, C., Rouberol, S., Rowan-Robinson, M., Rubiño-Martín, J. A., Rusconi, P., Rusholme, B., Salama, M., Salerno, E., Sandri, M., Santos, D., Sanz, J. L., Sauter, L., Sauvage, F., Savini, G., Schmelzel, M., Schnorhk, A., Schwarz, W., Scott, D., Seiffert, M. D., Shellard, P., Shih, C., Sias, M., Silk, J. I., Silvestri, R., Sippel, R., Smoot, G. F., Starck, J.-L., Stassi, P., Sternberg, J., Stivoli, F., Stolyarov, V., Stompor, R., Stringhetti, L., Strommen, D., Stute, T., Sudiwala, R., Sugimura, R., Sunyaev, R., Sygnet, J.-F., Türler, M., Taddei, E., Tallon, J., Tamiatto, C., Taurigna, M., Taylor, D., Terenzi, L., Thuerey, S., Tillis, J., Tofani, G., Toffolatti, L., Tommasi, E., Tomasi, M., Tonazzini, E., Torre, J.-P., Tosti, S., Touze, F., Tristram, M., Tuovinen, J., Tuttlebee, M., Umana, G., Valenziano, L., Vallée, D., van der Vlis, M., Van Leeuwen, F., Vanel, J.-C., Van-Tent, B., Varis, J., Vassallo, E., Vescovi, C., Vezzu, F., Vibert, D., Vielva, P., Vierra, J., Villa, F., Vittorio, N., Vuerli, C., Wade, L. A., Walker, A. R., Wandelt, B. D., Watson, C., Werner, D., White, M., White, S. D. M., Wilkinson, A., Wilson, P., Woodcraft, A., Yoffo, B., Yun, M., Yurchenko, V., Yvon, D., Zhang, B., Zimmermann, O., Zonca, A., and Zorita, D.
Abstract: The European Space Agency's Plancksatellite, launched on 14 May 2009, is the third-generation space experiment in the field of cosmic microwave background (CMB) research. It will image the anisotropies of the CMB over the whole sky, with unprecedented sensitivity (${{\Delta T}\over T}$~ 2 × 10-6) and angular resolution (~5 arcmin). Planckwill provide a major source of information relevant to many fundamental cosmological problems and will test current theories of the early evolution of the Universe and the origin of structure. It will also address a wide range of areas of astrophysical research related to the Milky Way as well as external galaxies and clusters of galaxies. The ability of Planckto measure polarization across a wide frequency range (30-350 GHz), with high precision and accuracy, and over the whole sky, will provide unique insight, not only into specific cosmological questions, but also into the properties of the interstellar medium. This paper is part of a series which describes the technical capabilities of the Planckscientific payload. It is based on the knowledge gathered during the on-ground calibration campaigns of the major subsystems, principally its telescope and its two scientific instruments, and of tests at fully integrated satellite level. It represents the best estimate before launch of the technical performance that the satellite and its payload will achieve in flight. In this paper, we summarise the main elements of the payload performance, which is described in detail in the accompanying papers. In addition, we describe the satellite performance elements which are most relevant for science, and provide an overview of the plans for scientific operations and data analysis.
Published: 2010

35. Planckpre-launch status: HFI ground calibration

Author: Pajot, F., Ade, P. A. R., Beney, J.-L., Bréelle, E., Broszkiewicz, D., Camus, P., Carabétian, C., Catalano, A., Chardin, A., Charra, M., Charra, J., Cizeron, R., Couchot, F., Coulais, A., Crill, B. P., Dassas, K., Daubin, J., de Bernardis, P., de Marcillac, P., Delouis, J.-M., Désert, F.-X., Duret, P., Eng, P., Evesque, C., Fourmond, J.-J., François, S., Giard, M., Giraud-Héraud, Y., Guglielmi, L., Guyot, G., Haissinski, J., Henrot-Versillé, S., Hervier, V., Holmes, W., Jones, W. C., Lamarre, J.-M., Lami, P., Lange, A. E., Lefebvre, M., Leriche, B., Leroy, C., Macias-Perez, J., Maciaszek, T., Maffei, B., Mahendran, A., Mansoux, B., Marty, C., Masi, S., Mercier, C., Miville-Deschenes, M.-A., Montier, L., Nicolas, C., Noviello, F., Perdereau, O., Piacentini, F., Piat, M., Plaszczynski, S., Pointecouteau, E., Pons, R., Ponthieu, N., Puget, J.-L., Rambaud, D., Renault, C., Renault, J.-C., Rioux, C., Ristorcelli, I., Rosset, C., Savini, G., Sudiwala, R., Torre, J.-P., Tristram, M., Vallée, D., Veneziani, M., and Yvon, D.
Abstract: Context. The Plancksatellite was successfully launched on May 14th 2009. We have completed the pre-launch calibration measurements of the High Frequency Instrument (HFI) on board Planckand their processing.Aims. We present the results ot the pre-launch calibration of HFI in which we have multiple objectives. First, we determine instrumental parameters that cannot be measured in-flight and predict parameters that can. Second, we take the opportunity to operate and understand the instrument under a wide range of anticipated operating conditions. Finally, we estimate the performance of the instrument built.Methods. We obtained our pre-launch calibration results by characterising the component and subsystems, then by calibrating the focal plane at IAS (Orsay) in the Saturne simulator, and later from the tests at the satellite level carried out in the CSL (Liège) cryogenic vacuum chamber. We developed models to estimate the instrument pre-launch parameters when no measurement could be performed.Results. We reliably measure the Planck-HFI instrument characteristics and behaviour, and determine the flight nominal setting of all parameters. The expected in-flight performance exceeds the requirements and is close or superior to the goal specifications.
Published: 2010

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

Author: Rosset, C., Tristram, M., Ponthieu, N., Ade, P., Aumont, J., 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.
Abstract: The High Frequency Instrument of Planckwill map the entire sky in the millimeter and sub-millimeter domain from 100 to 857 GHz with unprecedented sensitivity to polarization (ΔP/Tcmb~ 4 × 10-6for Peither Qor Uand Tcmb$\simeq$2.7 K) 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. Planckwill make high resolution measurements of the E-mode spectrum (up to $\ell$~ 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° respectively. Pre-launch ground measurements reported in this paper already fulfill these requirements.
Published: 2010

37. Planckpre-launch status: The HFI instrument, from specification to actual performance

Author: Lamarre, J.-M., Puget, J.-L., Ade, P. A. R., Bouchet, F., Guyot, G., Lange, A. E., Pajot, F., Arondel, A., Benabed, K., Beney, J.-L., Benoît, A., Bernard, J.-Ph., Bhatia, R., Blanc, Y., Bock, J. J., Bréelle, E., Bradshaw, T. W., Camus, P., Catalano, A., Charra, J., Charra, M., Church, S. E., Couchot, F., Coulais, A., Crill, B. P., Crook, M. R., Dassas, K., de Bernardis, P., Delabrouille, J., de Marcillac, P., Delouis, J.-M., Désert, F.-X., Dumesnil, C., Dupac, X., Efstathiou, G., Eng, P., Evesque, C., Fourmond, J.-J., Ganga, K., Giard, M., Gispert, R., Guglielmi, L., Haissinski, J., Henrot-Versillé, S., Hivon, E., Holmes, W. A., Jones, W. C., Koch, T. C., Lagardère, H., Lami, P., Landé, J., Leriche, B., Leroy, C., Longval, Y., Macías-Pérez, J. F., Maciaszek, T., Maffei, B., Mansoux, B., Marty, C., Masi, S., Mercier, C., Miville-Deschênes, M.-A., Moneti, A., Montier, L., Murphy, J. A., Narbonne, J., Nexon, M., Paine, C. G., Pahn, J., Perdereau, O., Piacentini, F., Piat, M., Plaszczynski, S., Pointecouteau, E., Pons, R., Ponthieu, N., Prunet, S., Rambaud, D., Recouvreur, G., Renault, C., Ristorcelli, I., Rosset, C., Santos, D., Savini, G., Serra, G., Stassi, P., Sudiwala, R. V., Sygnet, J.-F., Tauber, J. A., Torre, J.-P., Tristram, M., Vibert, L., Woodcraft, A., Yurchenko, V., and Yvon, D.
Abstract: Context. The High Frequency Instrument (HFI) is one of the two focal instruments of the Planckmission. It will observe the whole sky in six bands in the 100 GHz–1 THz range.Aims. The HFI instrument is designed to measure the cosmic microwave background (CMB) with a sensitivity limited only by fundamental sources: the photon noise of the CMB itself and the residuals left after the removal of foregrounds. The two high frequency bands will provide full maps of the submillimetre sky, featuring mainly extended and point source foregrounds. Systematic effects must be kept at negligible levels or accurately monitored so that the signal can be corrected. This paper describes the HFI design and its characteristics deduced from ground tests and calibration.Methods. The HFI instrumental concept and architecture are feasible only by pushing new techniques to their extreme capabilities, mainly: (i) bolometers working at 100 mK and absorbing the radiation in grids; (ii) a dilution cooler providing 100 mK in microgravity conditions; (iii) a new type of AC biased readout electronics and (iv) optical channels using devices inspired from radio and infrared techniques.Results. The Planck-HFI instrument performance exceeds requirements for sensitivity and control of systematic effects. During ground-based calibration and tests, it was measured at instrument and system levels to be close to or better than the goal specification.
Published: 2010

38. Planckpre-launch status: The Planckmission

Author: Tauber, J. A., Mandolesi, N., Puget, J.-L., Banos, T., Bersanelli, M., Bouchet, F. R., Butler, R. C., Charra, J., Crone, G., Dodsworth, J., Efstathiou, G., Gispert, R., Guyot, G., Gregorio, A., Juillet, J. J., Lamarre, J.-M., Laureijs, R. J., Lawrence, C. R., Nørgaard-Nielsen, H. U., Passvogel, T., Reix, J. M., Texier, D., Vibert, L., Zacchei, A., Ade, P. A. R., Aghanim, N., Aja, B., Alippi, E., Aloy, L., Armand, P., Arnaud, M., Arondel, A., Arreola-Villanueva, A., Artal, E., Artina, E., Arts, A., Ashdown, M., Aumont, J., Azzaro, M., Bacchetta, A., Baccigalupi, C., Baker, M., Balasini, M., Balbi, A., Banday, A. J., Barbier, G., Barreiro, R. B., Bartelmann, M., Battaglia, P., Battaner, E., Benabed, K., Beney, J.-L., Beneyton, R., Bennett, K., Benoit, A., Bernard, J.-P., Bhandari, P., Bhatia, R., Biggi, M., Biggins, R., Billig, G., Blanc, Y., Blavot, H., Bock, J. J., Bonaldi, A., Bond, R., Bonis, J., Borders, J., Borrill, J., Boschini, L., Boulanger, F., Bouvier, J., Bouzit, M., Bowman, R., Bréelle, E., Bradshaw, T., Braghin, M., Bremer, M., Brienza, D., Broszkiewicz, D., Burigana, C., Burkhalter, M., Cabella, P., Cafferty, T., Cairola, M., Caminade, S., Camus, P., Cantalupo, C. M., Cappellini, B., Cardoso, J.-F., Carr, R., Catalano, A., Cayón, L., Cesa, M., Chaigneau, M., Challinor, A., Chamballu, A., Chambelland, J. P., Charra, M., Chiang, L.-Y., Chlewicki, G., Christensen, P. R., Church, S., Ciancietta, E., Cibrario, M., Cizeron, R., Clements, D., Collaudin, B., Colley, J.-M., Colombi, S., Colombo, A., Colombo, F., Corre, O., Couchot, F., Cougrand, B., Coulais, A., Couzin, P., Crane, B., Crill, B., Crook, M., Crumb, D., Cuttaia, F., Dörl, U., da Silva, P., Daddato, R., Damasio, C., Danese, L., d'Aquino, G., D'Arcangelo, O., Dassas, K., Davies, R. D., Davies, W., Davis, R. J., De Bernardis, P., de Chambure, D., de Gasperis, G., De la Fuente, M. L., De Paco, P., De Rosa, A., De Troia, G., De Zotti, G., Dehamme, M., Delabrouille, J., Delouis, J.-M., Désert, F.-X., di Girolamo, G., Dickinson, C., Doelling, E., Dolag, K., Domken, I., Douspis, M., Doyle, D., Du, S., Dubruel, D., Dufour, C., Dumesnil, C., Dupac, X., Duret, P., Eder, C., Elfving, A., Enßlin, T. A., Eng, P., English, K., Eriksen, H. K., Estaria, P., Falvella, M. C., Ferrari, F., Finelli, F., Fishman, A., Fogliani, S., Foley, S., Fonseca, A., Forma, G., Forni, O., Fosalba, P., Fourmond, J.-J., Frailis, M., Franceschet, C., Franceschi, E., François, S., Frerking, M., Gómez-Reñasco, M. F., Górski, K. M., Gaier, T. C., Galeotta, S., Ganga, K., García Lázaro, J., Garnica, A., Gaspard, M., Gavila, E., Giard, M., Giardino, G., Gienger, G., Giraud-Heraud, Y., Glorian, J.-M., Griffin, M., Gruppuso, A., Guglielmi, L., Guichon, D., Guillaume, B., Guillouet, P., Haissinski, J., Hansen, F. K., Hardy, J., Harrison, D., Hazell, A., Hechler, M., Heckenauer, V., Heinzer, D., Hell, R., Henrot-Versillé, S., Hernández-Monteagudo, C., Herranz, D., Herreros, J. M., Hervier, V., Heske, A., Heurtel, A., Hildebrandt, S. R., Hills, R., Hivon, E., Hobson, M., Hollert, D., Holmes, W., Hornstrup, A., Hovest, W., Hoyland, R. J., Huey, G., Huffenberger, K. M., Hughes, N., Israelsson, U., Jackson, B., Jaffe, A., Jaffe, T. R., Jagemann, T., Jessen, N. C., Jewell, J., Jones, W., Juvela, M., Kaplan, J., Karlman, P., Keck, F., Keihänen, E., King, M., Kisner, T. S., Kletzkine, P., Kneissl, R., Knoche, J., Knox, L., Koch, T., Krassenburg, M., Kurki-Suonio, H., Lähteenmäki, A., Lagache, G., Lagorio, E., Lami, P., Lande, J., Lange, A., Langlet, F., Lapini, R., Lapolla, M., Lasenby, A., Le Jeune, M., Leahy, J. P., Lefebvre, M., Legrand, F., Le Meur, G., Leonardi, R., Leriche, B., Leroy, C., Leutenegger, P., Levin, S. M., Lilje, P. B., Lindensmith, C., Linden-Vørnle, M., Loc, A., Longval, Y., Lubin, P. M., Luchik, T., Luthold, I., Macias-Perez, J. F., Maciaszek, T., MacTavish, C., Madden, S., Maffei, B., Magneville, C., Maino, D., Mambretti, A., Mansoux, B., Marchioro, D., Maris, M., Marliani, F., Marrucho, J.-C., Martí-Canales, J., Martínez-González, E., Martín-Polegre, A., Martin, P., Marty, C., Marty, W., Masi, S., Massardi, M., Matarrese, S., Matthai, F., Mazzotta, P., McDonald, A., McGrath, P., Mediavilla, A., Meinhold, P. R., Mélin, J.-B., Melot, F., Mendes, L., Mennella, A., Mervier, C., Meslier, L., Miccolis, M., Miville-Deschenes, M.-A., Moneti, A., Montet, D., Montier, L., Mora, J., Morgante, G., Morigi, G., Morinaud, G., Morisset, N., Mortlock, D., Mottet, S., Mulder, J., Munshi, D., Murphy, A., Murphy, P., Musi, P., Narbonne, J., Naselsky, P., Nash, A., Nati, F., Natoli, P., Netterfield, B., Newell, J., Nexon, M., Nicolas, C., Nielsen, P. H., Ninane, N., Noviello, F., Novikov, D., Novikov, I., O'Dwyer, I. J., Oldeman, P., Olivier, P., Ouchet, L., Oxborrow, C. A., Pérez-Cuevas, L., Pagan, L., Paine, C., Pajot, F., Paladini, R., Pancher, F., Panh, J., Parks, G., Parnaudeau, P., Partridge, B., Parvin, B., Pascual, J. P., Pasian, F., Pearson, D. P., Pearson, T., Pecora, M., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Pierpaoli, E., Piersanti, O., Plaige, E., Plaszczynski, S., Platania, P., Pointecouteau, E., Polenta, G., Ponthieu, N., Popa, L., Poulleau, G., Poutanen, T., Prézeau, G., Pradell, L., Prina, M., Prunet, S., Rachen, J. P., Rambaud, D., Rame, F., Rasmussen, I., Rautakoski, J., Reach, W. T., Rebolo, R., Reinecke, M., Reiter, J., Renault, C., Ricciardi, S., Rideau, P., Riller, T., Ristorcelli, I., Riti, J. B., Rocha, G., Roche, Y., Pons, R., Rohlfs, R., Romero, D., Roose, S., Rosset, C., Rouberol, S., Rowan-Robinson, M., Rubiño-Martín, J. A., Rusconi, P., Rusholme, B., Salama, M., Salerno, E., Sandri, M., Santos, D., Sanz, J. L., Sauter, L., Sauvage, F., Savini, G., Schmelzel, M., Schnorhk, A., Schwarz, W., Scott, D., Seiffert, M. D., Shellard, P., Shih, C., Sias, M., Silk, J. I., Silvestri, R., Sippel, R., Smoot, G. F., Starck, J.-L., Stassi, P., Sternberg, J., Stivoli, F., Stolyarov, V., Stompor, R., Stringhetti, L., Strommen, D., Stute, T., Sudiwala, R., Sugimura, R., Sunyaev, R., Sygnet, J.-F., Türler, M., Taddei, E., Tallon, J., Tamiatto, C., Taurigna, M., Taylor, D., Terenzi, L., Thuerey, S., Tillis, J., Tofani, G., Toffolatti, L., Tommasi, E., Tomasi, M., Tonazzini, E., Torre, J.-P., Tosti, S., Touze, F., Tristram, M., Tuovinen, J., Tuttlebee, M., Umana, G., Valenziano, L., Vallée, D., van der Vlis, M., Van Leeuwen, F., Vanel, J.-C., Van-Tent, B., Varis, J., Vassallo, E., Vescovi, C., Vezzu, F., Vibert, D., Vielva, P., Vierra, J., Villa, F., Vittorio, N., Vuerli, C., Wade, L. A., Walker, A. R., Wandelt, B. D., Watson, C., Werner, D., White, M., White, S. D. M., Wilkinson, A., Wilson, P., Woodcraft, A., Yoffo, B., Yun, M., Yurchenko, V., Yvon, D., Zhang, B., Zimmermann, O., Zonca, A., and Zorita, D.
Abstract: The European Space Agency's Plancksatellite, launched on 14 May 2009, is the third-generation space experiment in the field of cosmic microwave background (CMB) research. It will image the anisotropies of the CMB over the whole sky, with unprecedented sensitivity (${{\Delta T}\over T}$~ 2 × 10-6) and angular resolution (~5 arcmin). Planckwill provide a major source of information relevant to many fundamental cosmological problems and will test current theories of the early evolution of the Universe and the origin of structure. It will also address a wide range of areas of astrophysical research related to the Milky Way as well as external galaxies and clusters of galaxies. The ability of Planckto measure polarization across a wide frequency range (30-350 GHz), with high precision and accuracy, and over the whole sky, will provide unique insight, not only into specific cosmological questions, but also into the properties of the interstellar medium. This paper is part of a series which describes the technical capabilities of the Planckscientific payload. It is based on the knowledge gathered during the on-ground calibration campaigns of the major subsystems, principally its telescope and its two scientific instruments, and of tests at fully integrated satellite level. It represents the best estimate before launch of the technical performance that the satellite and its payload will achieve in flight. In this paper, we summarise the main elements of the payload performance, which is described in detail in the accompanying papers. In addition, we describe the satellite performance elements which are most relevant for science, and provide an overview of the plans for scientific operations and data analysis.
Published: 2010
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39. Planckpre-launch status: The HFI instrument, from specification to actual performance

Author: Lamarre, J.-M., Puget, J.-L., Ade, P. A. R., Bouchet, F., Guyot, G., Lange, A. E., Pajot, F., Arondel, A., Benabed, K., Beney, J.-L., Benoît, A., Bernard, J.-Ph., Bhatia, R., Blanc, Y., Bock, J. J., Bréelle, E., Bradshaw, T. W., Camus, P., Catalano, A., Charra, J., Charra, M., Church, S. E., Couchot, F., Coulais, A., Crill, B. P., Crook, M. R., Dassas, K., de Bernardis, P., Delabrouille, J., de Marcillac, P., Delouis, J.-M., Désert, F.-X., Dumesnil, C., Dupac, X., Efstathiou, G., Eng, P., Evesque, C., Fourmond, J.-J., Ganga, K., Giard, M., Gispert, R., Guglielmi, L., Haissinski, J., Henrot-Versillé, S., Hivon, E., Holmes, W. A., Jones, W. C., Koch, T. C., Lagardère, H., Lami, P., Landé, J., Leriche, B., Leroy, C., Longval, Y., Macías-Pérez, J. F., Maciaszek, T., Maffei, B., Mansoux, B., Marty, C., Masi, S., Mercier, C., Miville-Deschênes, M.-A., Moneti, A., Montier, L., Murphy, J. A., Narbonne, J., Nexon, M., Paine, C. G., Pahn, J., Perdereau, O., Piacentini, F., Piat, M., Plaszczynski, S., Pointecouteau, E., Pons, R., Ponthieu, N., Prunet, S., Rambaud, D., Recouvreur, G., Renault, C., Ristorcelli, I., Rosset, C., Santos, D., Savini, G., Serra, G., Stassi, P., Sudiwala, R. V., Sygnet, J.-F., Tauber, J. A., Torre, J.-P., Tristram, M., Vibert, L., Woodcraft, A., Yurchenko, V., and Yvon, D.
Abstract: Context. The High Frequency Instrument (HFI) is one of the two focal instruments of the Planckmission. It will observe the whole sky in six bands in the 100 GHz–1 THz range.
Published: 2010
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40. Planckpre-launch status: HFI ground calibration

Author: Pajot, F., Ade, P. A. R., Beney, J.-L., Bréelle, E., Broszkiewicz, D., Camus, P., Carabétian, C., Catalano, A., Chardin, A., Charra, M., Charra, J., Cizeron, R., Couchot, F., Coulais, A., Crill, B. P., Dassas, K., Daubin, J., de Bernardis, P., de Marcillac, P., Delouis, J.-M., Désert, F.-X., Duret, P., Eng, P., Evesque, C., Fourmond, J.-J., François, S., Giard, M., Giraud-Héraud, Y., Guglielmi, L., Guyot, G., Haissinski, J., Henrot-Versillé, S., Hervier, V., Holmes, W., Jones, W. C., Lamarre, J.-M., Lami, P., Lange, A. E., Lefebvre, M., Leriche, B., Leroy, C., Macias-Perez, J., Maciaszek, T., Maffei, B., Mahendran, A., Mansoux, B., Marty, C., Masi, S., Mercier, C., Miville-Deschenes, M.-A., Montier, L., Nicolas, C., Noviello, F., Perdereau, O., Piacentini, F., Piat, M., Plaszczynski, S., Pointecouteau, E., Pons, R., Ponthieu, N., Puget, J.-L., Rambaud, D., Renault, C., Renault, J.-C., Rioux, C., Ristorcelli, I., Rosset, C., Savini, G., Sudiwala, R., Torre, J.-P., Tristram, M., Vallée, D., Veneziani, M., and Yvon, D.
Abstract: Context. The Plancksatellite was successfully launched on May 14th 2009. We have completed the pre-launch calibration measurements of the High Frequency Instrument (HFI) on board Planckand their processing.
Published: 2010
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41. Planckpre-launch status: High Frequency Instrument polarization calibration

Author: Rosset, C., Tristram, M., Ponthieu, N., Ade, P., Aumont, J., 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.
Abstract: The High Frequency Instrument of Planckwill map the entire sky in the millimeter and sub-millimeter domain from 100 to 857 GHz with unprecedented sensitivity to polarization (ΔP/Tcmb~ 4 × 10-6for Peither Qor Uand Tcmb$\simeq$2.7 K) 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. Planckwill make high resolution measurements of the E-mode spectrum (up to $\ell$~ 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° respectively. Pre-launch ground measurements reported in this paper already fulfill these requirements.
Published: 2010
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