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Start Over Author "WIESEMEYER, H." Publisher edp sciences
128 results on '"WIESEMEYER, H."'

2. NIKA 150 GHz polarization observations of the Crab nebula and its spectral energy distribution (Corrigendum)

Author

Ritacco, A., primary, Macías-Pérez, J. F., additional, Ponthieu, N., additional, Adam, R., additional, Ade, P., additional, André, P., additional, Aumont, J., additional, Beelen, A., additional, Benoît, A., additional, Bideaud, A., additional, Billot, N., additional, Bourrion, O., additional, Bracco, A., additional, Calvo, M., additional, Catalano, A., additional, Coiffard, G., additional, Comis, B., additional, D’Addabbo, A., additional, De Petris, M., additional, Désert, F.-X., additional, Doyle, S., additional, Goupy, J., additional, Kramer, C., additional, Lagache, G., additional, Leclercq, S., additional, Lestrade, J.-F., additional, Mauskopf, P., additional, Mayet, F., additional, Maury, A., additional, Monfardini, A., additional, Pajot, F., additional, Pascale, E., additional, Perotto, L., additional, Pisano, G., additional, Rebolo-Iglesias, M., additional, Revéret, V., additional, Rodriguez, L., additional, Romero, C., additional, Roussel, H., additional, Ruppin, F., additional, Schuster, K., additional, Sievers, A., additional, Siringo, G., additional, Thum, C., additional, Triqueneaux, S., additional, Tucker, C., additional, Wiesemeyer, H., additional, and Zylka, R., additional

Published
2022
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7. Anatomy of the massive star-forming region S106

Author

Schneider, N., primary, Röllig, M., additional, Simon, R., additional, Wiesemeyer, H., additional, Gusdorf, A., additional, Stutzki, J., additional, Güsten, R., additional, Bontemps, S., additional, Comerón, F., additional, Csengeri, T., additional, Adams, J. D., additional, and Richter, H., additional

Published
2018
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8. Magnetic field in a young circumbinary disk

Author

Alves, F. O., primary, Girart, J. M., additional, Padovani, M., additional, Galli, D., additional, Franco, G. A. P., additional, Caselli, P., additional, Vlemmings, W. H. T., additional, Zhang, Q., additional, and Wiesemeyer, H., additional

Published
2018
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9. NIKA 150 GHz polarization observations of the Crab nebula and its spectral energy distribution

Author

Ritacco, A., primary, Macías-Pérez, J. F., additional, Ponthieu, N., additional, Adam, R., additional, Ade, P., additional, André, P., additional, Aumont, J., additional, Beelen, A., additional, Benoît, A., additional, Bideaud, A., additional, Billot, N., additional, Bourrion, O., additional, Bracco, A., additional, Calvo, M., additional, Catalano, A., additional, Coiffard, G., additional, Comis, B., additional, D’Addabbo, A., additional, De Petris, M., additional, Désert, F.-X., additional, Doyle, S., additional, Goupy, J., additional, Kramer, C., additional, Lagache, G., additional, Leclercq, S., additional, Lestrade, J.-F., additional, Mauskopf, P., additional, Mayet, F., additional, Maury, A., additional, Monfardini, A., additional, Pajot, F., additional, Pascale, E., additional, Perotto, L., additional, Pisano, G., additional, Rebolo-Iglesias, M., additional, Revéret, V., additional, Rodriguez, L., additional, Romero, C., additional, Roussel, H., additional, Ruppin, F., additional, Schuster, K., additional, Sievers, A., additional, Siringo, G., additional, Thum, C., additional, Triqueneaux, S., additional, Tucker, C., additional, Wiesemeyer, H., additional, and Zylka, R., additional

Published
2018
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11. Unveiling the chemistry of interstellar CH

Author

Wiesemeyer, H., primary, Güsten, R., additional, Menten, K.M., additional, Durán, C.A., additional, Csengeri, T., additional, Jacob, A.M., additional, Simon, R., additional, Stutzki, J., additional, and Wyrowski, F., additional

Published
2018
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14. Nature of shocks revealed by SOFIA OI observations in the Cepheus E protostellar outflow

Author

Gusdorf, A., primary, Anderl, S., additional, Lefloch, B., additional, Leurini, S., additional, Wiesemeyer, H., additional, Güsten, R., additional, Benedettini, M., additional, Codella, C., additional, Godard, B., additional, Gómez-Ruiz, A. I., additional, Jacobs, K., additional, Kristensen, L. E., additional, Lesaffre, P., additional, Pineau des Forêts, G., additional, and Lis, D. C., additional

Published
2017
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17. Planck intermediate results XXXII. The relative orientation between the magnetic field and structures traced by interstellar dust

Author

Adam, R., Ade, P.A.R., Aghanim, N., Alves, M.I.R., Arnaud, M., Arzoumanian, D., Ashdown, M., Aumont, J., Baccigalupi, C., Banday, A.J., Barreiro, R.B., Bartolo, N., Battaner, E., Benabed, K., Benoit-Lévy, A., Bernard, J.-P., Bersanelli, M., Bielewicz, P., Bonaldi, A., Bonavera, L., Bond, J.R., Borrill, J., Bouchet, F.R., Boulanger, F., Bracco, A., Burigana, C., Butler, R.C., Calabrese, E., Cardoso, J.-F., Catalano, A., Chamballu, A., Chiang, H.C., Christensen, P.R., Colombi, S., Colombo, L.P.L., Combet, C., Couchot, F., Crill, B.P., Curto, A., Cuttaia, F., Danese, L., Davies, R.D., Davis, R.J., De Bernardis, P., de Rosa, A., de Zotti, G., Delabrouille, J., Dickinson, C., Diego, J.M., Dole, H., Donzelli, S., Dore, O., Douspis, M., Ducout, A., Dupac, X., Efstathiou, G., Elsner, F., Enßlin, T.A., Eriksen, H.K., Falgarone, E., Ferrière, K., Finelli, F., Forni, O., Frailis, M., Fraisse, A.A., Franceschi, E., Frejsel, A., Galeotta, S., Galli, S., Ganga, K., Ghosh, T., Giard, M., Gjerløw, E., Gonzalez-Nuevo, J., Gorski, K.M., Gregorio, A., Gruppuso, A., Guillet, V., Hansen, F.K., Hanson, D., Harrison, D., Henrot-Versille, S., Hernandez-Monteagudo, C., Herranz, D., Hildebrandt, S.R., Hivon, E., Hobson, M., Holmes, W.A., Hovest, W., Huffenberger, K.M., Hurier, G., Jaffe, A.H., Jaffe, T.R., Jones, W.C., Juvela, M., Keihanen, E., Keskitalo, R., Kisner, T.S., Kneissl, R., Knoche, J., Kunz, M., Kurki-Suonio, H., Lagache, G., Lamarre, J.-M., Lasenby, A., Lattanzi, M., Lawrence, C.R., Leonardi, R., Levrier, F., Liguori, M., Lilje, P.B., Linden-Vornle, M., Lopez-Caniego, M., Lubin, P.M., Macias-Perez, J.F., Maffei, B., Maino, D., Mandolesi, N., Maris, M., Marshall, D.J., Martin, P.G., Martinez-Gonzalez, E., Masi, S., Matarrese, S., Mazzotta, P., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Miville-Deschenes, M.-A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, J.Anthony, Naselsky, P., Natoli, P., Norgaard-Nielsen, H.U., Noviello, F., Novikov, D., Novikov, I., Oppermann, N., Oxborrow, C.A., Pagano, L., Pajot, F., Paoletti, D., Pasian, F., Perdereau, O., Perotto, L., Perrotta, F., Pettorino, V., Piacentini, F., Piat, M., Plaszczynski, S., Pointecouteau, E., Polenta, G., Ponthieu, N., Popa, L., Pratt, G.W., Prunet, S., Puget, J.-L., Rachen, J.P., Reach, W.T., Reinecke, M., Remazeilles, M., Renault, C., Ristorcelli, I., Rocha, G., Roudier, G., Rubino-Martin, J.A., Rusholme, B., Sandri, M., Santos, D., Savini, G., Scott, D., Soler, J.D., Spencer, L., Stolyarov, V., Sudiwala, R., Sunyaev, R., Sutton, D., Suur-Uski, A.-S., Sygnet, J.-F., Tauber, J.A., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Umana, G., Valenziano, L., Valiviita, J., Van Tent, B., Vielva, P., Villa, F., Wade, L.A., Wandelt, B.D., Wehus, I., Wiesemeyer, H., Yvon, D., Zacchei, A., Zonca, A., Adam, R., Ade, P.A.R., Aghanim, N., Alves, M.I.R., Arnaud, M., Arzoumanian, D., Ashdown, M., Aumont, J., Baccigalupi, C., Banday, A.J., Barreiro, R.B., Bartolo, N., Battaner, E., Benabed, K., Benoit-Lévy, A., Bernard, J.-P., Bersanelli, M., Bielewicz, P., Bonaldi, A., Bonavera, L., Bond, J.R., Borrill, J., Bouchet, F.R., Boulanger, F., Bracco, A., Burigana, C., Butler, R.C., Calabrese, E., Cardoso, J.-F., Catalano, A., Chamballu, A., Chiang, H.C., Christensen, P.R., Colombi, S., Colombo, L.P.L., Combet, C., Couchot, F., Crill, B.P., Curto, A., Cuttaia, F., Danese, L., Davies, R.D., Davis, R.J., De Bernardis, P., de Rosa, A., de Zotti, G., Delabrouille, J., Dickinson, C., Diego, J.M., Dole, H., Donzelli, S., Dore, O., Douspis, M., Ducout, A., Dupac, X., Efstathiou, G., Elsner, F., Enßlin, T.A., Eriksen, H.K., Falgarone, E., Ferrière, K., Finelli, F., Forni, O., Frailis, M., Fraisse, A.A., Franceschi, E., Frejsel, A., Galeotta, S., Galli, S., Ganga, K., Ghosh, T., Giard, M., Gjerløw, E., Gonzalez-Nuevo, J., Gorski, K.M., Gregorio, A., Gruppuso, A., Guillet, V., Hansen, F.K., Hanson, D., Harrison, D., Henrot-Versille, S., Hernandez-Monteagudo, C., Herranz, D., Hildebrandt, S.R., Hivon, E., Hobson, M., Holmes, W.A., Hovest, W., Huffenberger, K.M., Hurier, G., Jaffe, A.H., Jaffe, T.R., Jones, W.C., Juvela, M., Keihanen, E., Keskitalo, R., Kisner, T.S., Kneissl, R., Knoche, J., Kunz, M., Kurki-Suonio, H., Lagache, G., Lamarre, J.-M., Lasenby, A., Lattanzi, M., Lawrence, C.R., Leonardi, R., Levrier, F., Liguori, M., Lilje, P.B., Linden-Vornle, M., Lopez-Caniego, M., Lubin, P.M., Macias-Perez, J.F., Maffei, B., Maino, D., Mandolesi, N., Maris, M., Marshall, D.J., Martin, P.G., Martinez-Gonzalez, E., Masi, S., Matarrese, S., Mazzotta, P., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Miville-Deschenes, M.-A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, J.Anthony, Naselsky, P., Natoli, P., Norgaard-Nielsen, H.U., Noviello, F., Novikov, D., Novikov, I., Oppermann, N., Oxborrow, C.A., Pagano, L., Pajot, F., Paoletti, D., Pasian, F., Perdereau, O., Perotto, L., Perrotta, F., Pettorino, V., Piacentini, F., Piat, M., Plaszczynski, S., Pointecouteau, E., Polenta, G., Ponthieu, N., Popa, L., Pratt, G.W., Prunet, S., Puget, J.-L., Rachen, J.P., Reach, W.T., Reinecke, M., Remazeilles, M., Renault, C., Ristorcelli, I., Rocha, G., Roudier, G., Rubino-Martin, J.A., Rusholme, B., Sandri, M., Santos, D., Savini, G., Scott, D., Soler, J.D., Spencer, L., Stolyarov, V., Sudiwala, R., Sunyaev, R., Sutton, D., Suur-Uski, A.-S., Sygnet, J.-F., Tauber, J.A., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Umana, G., Valenziano, L., Valiviita, J., Van Tent, B., Vielva, P., Villa, F., Wade, L.A., Wandelt, B.D., Wehus, I., Wiesemeyer, H., Yvon, D., Zacchei, A., and Zonca, A.

Abstract

The role of the magnetic field in the formation of the filamentary structures observed in the interstellar medium (ISM) is a debated topic owing to the paucity of relevant observations needed to test existing models. The Planck all-sky maps of linearly polarized emission from dust at 353 GHz provide the required combination of imaging and statistics to study the correlation between the structures of the Galactic magnetic field and of interstellar matter over the whole sky, both in the diffuse ISM and in molecular clouds. The data reveal that structures, or ridges, in the intensity map have counterparts in the Stokes Q and/or U maps. We focus our study on structures at intermediate and high Galactic latitudes, which cover two orders of magnitude in column density, from 1020 to 1022 cm-2. We measure the magnetic field orientation on the plane ofthe sky from the polarization data, and present an algorithm to estimate the orientation of the ridges from the dust intensity map. We use analytical models to account for projection effects. Comparing polarization angles on and off the structures, we estimate the mean ratio between the strengths of the turbulent and mean components of the magnetic field to be between 0.6 and 1.0, with a preferred value of 0.8. We find that the ridges are usually aligned with the magnetic field measured on the structures. This statistical trend becomes more striking for increasing polarization fraction and decreasing column density. There is no alignment for the highest column density ridges. We interpret the increase in alignment with polarization fraction as a consequence of projection effects. We present maps to show that the decrease in alignment for high column density is not due to a loss of correlation between the distribution of matter and the geometry of the magnetic field. In molecular complexes, we also observe structures perpendicular to the magnetic field, which, statistically, cannot be accounted for by projection effects. This fi

Published
2016

18. SOFIA follow-ups of massive clumps from the ATLASGAL galactic plane survey

Author

Wyrowski, F., Güsten, R., Menten, K.M., Wiesemeyer, H., Csengeri, T., König, C., Urquhart, J.S., Wyrowski, F., Güsten, R., Menten, K.M., Wiesemeyer, H., Csengeri, T., König, C., and Urquhart, J.S.

Abstract

With the GREAT receiver at the Stratospheric Observatory for Infrared Astronomy (SOFIA) we started a concerted observing effort towards a well selected sample of clumps with high masses covering a range of evolutionary stages based on their infrared properties. The sources were selected from the ATLASGAL sub-millimeter dust continuum survey of our Galaxy. The goal is threefold: (i) SOFIA/GREAT allows to study the cooling budget of the clumps, in particular with observations of the CII and OI cooling lines. (ii) With SOFIA/GREAT high-J CO lines can be observed to measure in combination with ground based data the CO SEDs of the sources. (iii) Using rotational transitions of ammonia at THz frequencies the kinematics of the clumps can be probed with absorption spectroscopy to search for infall. Here we will describe these efforts and in particular report new results from the ammonia 32+-22- (1.8 THz) observing program. © 2016 EAS, EDP Sciences.

Published
2016

19. Infall through the evolution of high-mass star-forming clumps

Author

Wyrowski, F., Güsten, R., Menten, K.M., Wiesemeyer, H., Csengeri, T., Heyminck, S., Klein, B., König, C., Urquhart, J.S., Wyrowski, F., Güsten, R., Menten, K.M., Wiesemeyer, H., Csengeri, T., Heyminck, S., Klein, B., König, C., and Urquhart, J.S.

Abstract

With the GREAT receiver at the Stratospheric Observatory for Infrared Astronomy (SOFIA), nine massive molecular clumps have been observed in the ammonia 32+?22? line at 1.8 THz in a search for signatures of infall. The sources were selected from the ATLASGAL submillimeter dust continuum survey of our Galaxy. Clumps with high masses covering a range of evolutionary stages based on their infrared properties were chosen. The ammonia line was detected in all sources, leading to five new detections and one confirmation of a previous detection of redshifted absorption in front of their strong THz continuum as a probe of infall in the clumps. These detections include two clumps embedded in infrared dark clouds. The measured velocity shifts of the absorptions compared to optically thin C17O (3–2) emission are 0.3–2.8 km?s-1, corresponding to fractions of 3% to 30% of the free-fall velocities of the clumps. The ammonia infall signature is compared with complementary data of different transitions of HCN, HNC, CS, and HCO+, which are often used to probe infall because of their blue-skewed line profiles. The best agreement with the ammonia results is found for the HCO+ (4–3) transitions, but the latter is still strongly blended with emission from associated outflows. This outflow signature is far less prominent in the THz ammonia lines, which confirms it as a powerful probe of infall in molecular clumps. Infall rates in the range from 0.3 to 16 × 10-3 M?/yr were derived with a tentative correlation with the virial parameters of the clumps. The new observations show that infall on clump scales is ubiquitous through a wide range of evolutionary stages, from L/M covering about ten to several hundreds.

Published
2016

20. Planck early results. VI. The High Frequency Instrument data processing

Author

Colley, J.-M., Bartlett, J.G., Bucher, M., Cardoso, J.-F., Castex, G., Catalano, A., Cressiot, C., Delabrouille, J., Ganga, K., Giraud-Héraud, Y., Kaplan, J., Le Jeune, M., Patanchon, G., Piat, M., Remazeilles, M., Rosset, C., Roudier, G., Stompor, R., Ashdown, M., Hills, R., Hobson, M., Lasenby, A., Stolyarov, V., Kneissl, R., Bond, J.R., Miville-Deschênes, M.-A., Banday, A.J., Bernard, J.-P., Forni, O., Giard, M., Leroy, C., Marshall, D.J., Montier, L., Pointecouteau, E., Ristorcelli, I., Bock, J.J., Doré, O., Helou, G., Hildebrandt, S.R., Matsumura, T., Pearson, T.J., Prézeau, G., Rocha, G., Challinor, A., Shellard, P., Melin, J.-B., Starck, J.-L., Yvon, D., Nørgaard-Nielsen, Hans Ulrik, Kunz, M., Marleau, F., Netterfield, C.B., Chiang, C., Jones, W.C., Knox, L., Wandelt, B.D., Dunkley, J., De Bernardis, P., Masi, S., Nati, F., Piacentini, F., Bersanelli, M., Tauber, J.A., Zacchei, A., Mandolesi, N., Guyot, G., Désert, F.-X., Chamballu, A., Clements, D.L., Jaffe, A.H., Mortlock, D., Novikov, D., Rowan-Robinson, M., Chary, R.-R., Chen, X., Lange, A.E., McGehee, P., Rusholme, B., Benoît, A., Aghanim, N., Aumont, J., Boulanger, F., Dole, H., Douspis, M., Gispert, R., Lagache, G., Mercier, C., Noviello, F., Pajot, F., Ponthieu, N., Puget, J.-L., Torre, J.-P., Vibert, L., Benabed, K., Bouchet, F.R., Colombi, S., Delouis, J.-M., Hivon, E., Lesgourgues, J., Moneti, A., Prunet, S., Riazuelo, A., Sygnet, J.-F., Fosalba, P., Wiesemeyer, H., Thum, C., Efstathiou, G., Gratton, S., Harrison, D., Sutton, D., Van Leeuwen, F., Crill, B.P., Górski, K.M., Holmes, W.A., Lawrence, C.R., Mitra, S., Saha, R., Wade, L.A., Maffei, B., MacTavish, C.J., Coulais, A., Lamarre, J.-M., Arnaud, M., Vibert, D., Girard, D., MacÍas-Pérez, J.F., Perotto, L., Renault, C., Santos, D., Ansari, R., Couchot, F., Filliard, C., Haissinski, J., Henrot-Versillé, S., Lavabre, A., Perdereau, O., Plaszczynski, S., Touze, F., Tristram, M., Borrill, J., Bartelmann, M., Dolag, K., Hernández-Monteagudo, C., Sunyaev, R., White, S.D.M., McAuley, I., Murphy, A., Peacocke, T., Yurchenko, V., Savini, G., Bradshaw, T., Crook, M., Mann, R., Ade, P.A.R., Griffin, M., North, C., Spencer, L., Sudiwala, R., Woodcraft, A., Church, S., Osborne, S., Schaefer, B.M., Reach, W.T., Battaner, E., Huffenberger, K.M., Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo-France -Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Institut d'Astrophysique de Paris (IAP), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Pierre et Marie Curie - Paris 6 (UPMC), Hélium : du fondamental aux applications (HELFA), Institut Néel (NEEL), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS), Laboratoire Traitement et Communication de l'Information (LTCI), Télécom ParisTech-Institut Mines-Télécom [Paris] (IMT)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), APC - Gravitation (APC-Gravitation), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, Institut de Planétologie et d'Astrophysique de Grenoble (IPAG ), Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry]), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS), Département de Physique des Particules (ex SPP) (DPP), Institut de RadioAstronomie Millimétrique (IRAM), Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Marseille (LAM), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Aix Marseille Université (AMU)-Centre National d'Études Spatiales [Toulouse] (CNES), PLANCK, Hfi Core Team, P, Ade, P, Aghanim, N, Ansari, R, Arnaud, M, Ashdown, M, Aumont, J, Banday, A, Bartelmann, M, Bartlett, J, Battaner, E, Benabed, K, Benoit, A, Bernard, J, Bersanelli, M, Bock, J, Bond, J, Borrill, J, Bouchet, F, Boulanger, F, Bradshaw, T, Bucher, M, Cardoso, J, Castex, G, Catalano, A, Challinor, A, Chamballu, A, Chary, R, Chen, X, Chiang, C, Church, S, Clements, D, Colley, J, Colombi, S, Couchot, F, Coulais, A, Cressiot, C, Crill, B, Crook, M, De Bernardis, P, Delabrouille, J, Delouis, J, Desert, F, Dolag, K, Dole, H, Dore, O, Douspis, M, Dunkley, J, Efstathiou, G, Filliard, C, Forni, O, Fosalba, P, Ganga, K, Giard, M, Girard, D, Giraud-Heraud, Y, Gispert, R, Gorski, K, Gratton, S, Griffin, M, Guyot, G, Haissinski, J, Harrison, D, Helou, G, Henrot-Versille, S, Hernandez-Monteagudo, C, Hildebrandt, S, Hills, R, Hivon, E, Hobson, M, Holmes, W, Huffenberger, K, Jaffe, A, Jones, W, Kaplan, J, Kneissl, R, Knox, L, Kunz, M, Lagache, G, Lamarre, J, Lange, A, Lasenby, A, Lavabre, A, Lawrence, C, Le Jeune, M, Leroy, C, Lesgourgues, J, Macias-Perez, J, Mactavish, C, Maffei, B, Mandolesi, N, Mann, R, Marleau, F, Marshall, D, Masi, S, Matsumura, T, Mcauley, I, Mcgehee, P, Melin, J, Mercier, C, Mitra, S, Miville-Deschenes, M, Moneti, A, Montier, L, Mortlock, D, Murphy, A, Nati, F, Netterfield, C, Nørgaard-Nielsen, H, Norgaard-Nielsen, H, North, C, Noviello, F, Novikov, D, Osborne, S, Pajot, F, Patanchon, G, Peacocke, T, Pearson, T, Perdereau, O, Perotto, L, Piacentini, F, Piat, M, Plaszczynski, S, Pointecouteau, E, Ponthieu, N, Prezeau, G, Prunet, S, Puget, J, Reach, W, Remazeilles, M, Renault, C, Riazuelo, A, Ristorcelli, I, Rocha, G, Rosset, C, Roudier, G, Rowan-Robinson, M, Rusholme, B, Saha, R, Santos, D, Savini, G, Schaefer, B, Shellard, P, Spencer, L, Starck, J, Stolyarov, V, Stompor, R, Sudiwala, R, Sunyaev, R, Sutton, D, Sygnet, J, Tauber, J, Thum, C, Torre, J, Touze, F, Tristram, M, Van Leeuwen, F, Vibert, L, Vibert, D, Wade, L, Wandelt, B, White, S, Wiesemeyer, H, Woodcraft, A, Yurchenko, V, Yvon, D, Zacchei, A, Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Hélium : du fondamental aux applications (NEEL - HELFA), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Centre National de la Recherche Scientifique (CNRS), Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), HELFA - Hélium : du fondamental aux applications, Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS Paris)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université de Cergy Pontoise (UCP), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Science and Technology Facilities Council (STFC), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), École normale supérieure - Paris (ENS Paris), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, and PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI)

Subjects
Experimental Physics, Cosmic microwave background, Astrophysics, cosmic background radiation, 01 natural sciences, NOISE, MICROWAVE, 010303 astronomy & astrophysics, media_common, QB, MISSION, Physics, CALIBRATION, Data processing, POWER SPECTRA, White noise, observations, SKY MAPS, Physical Sciences, symbols, astro-ph.CO, method, Astrophysics - Instrumentation and Methods for Astrophysics, methods: data analysi, Astrophysics - Cosmology and Nongalactic Astrophysics, data analysi, Cosmology and Nongalactic Astrophysics (astro-ph.CO), COMPONENT SEPARATION, [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], media_common.quotation_subject, astro-ph.GA, FOS: Physical sciences, Astronomy & Astrophysics, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], symbols.namesake, Quality (physics), surveys, 0103 physical sciences, 0201 Astronomical and Space Sciences, methods, data analysis, cosmology: observations, methods: data analysis, cosmology, PRE-LAUNCH STATUS, Angular resolution, survey, Planck, Instrumentation and Methods for Astrophysics (astro-ph.IM), Science & Technology, cosmology: observation, 010308 nuclear & particles physics, Instrument Data, Astronomy and Astrophysics, IN-FLIGHT PERFORMANCE, Astrophysics - Astrophysics of Galaxies, [SDU.ASTR.IM]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], Space and Planetary Science, Sky, Astrophysics of Galaxies (astro-ph.GA), MAP-MAKING METHOD, astro-ph.IM
Abstract

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

Published
2011

21. The upGREAT 1.9 THz multi-pixel high resolution spectrometer for the SOFIA Observatory

Author

Risacher, C., primary, Güsten, R., additional, Stutzki, J., additional, Hübers, H.-W., additional, Bell, A., additional, Buchbender, C., additional, Büchel, D., additional, Csengeri, T., additional, Graf, U. U., additional, Heyminck, S., additional, Higgins, R. D., additional, Honingh, C. E., additional, Jacobs, K., additional, Klein, B., additional, Okada, Y., additional, Parikka, A., additional, Pütz, P., additional, Reyes, N., additional, Ricken, O., additional, Riquelme, D., additional, Simon, R., additional, and Wiesemeyer, H., additional

Published
2016
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24. On the radiation driven alignment of dust grains: Detection of the polarization hole in a starless core (Corrigendum)

Author

Alves, Felipe de O., Frau, Pau, Girart, Josep Miquel, Franco, Gabriel A. P., Santos, F. P., Wiesemeyer, H., Alves, Felipe de O., Frau, Pau, Girart, Josep Miquel, Franco, Gabriel A. P., Santos, F. P., and Wiesemeyer, H.

Abstract

Figure 2 in the original manuscript displays the polarization efficiency for the optical, near infrared and sub-millimeter (submm) polarimetric data as P/AV, where P is the polarization degree and AV is the visual extinction traced by the data. However, the polarization efficiency for the submm data should be simply P. By dividing P by AV, we obtain a steeper and wrong slope for the decrease in polarization efficiency. The suitable form for Fig. 2 of the original document is exhibited in Fig. 1 of the present corrigendum. The submm polarization efficiency decreases as ~−1.0 with respect to AV, instead of the originally published ~−2.0. Although the decrease in polarization efficiency at the submm regime is shallower than originally proposed, our modelling of the polarization degree with respect to the relative intensity, I/Imax, still predicts the detection of a polarization hole (Sect. 3 of the published manuscript). Therefore, the main conclusions are unchanged.

Published
2015

26. Challenging shock models with SOFIA OH observations in the high-mass star-forming region Cepheus A

Author

Gusdorf, A., primary, Güsten, R., additional, Menten, K. M., additional, Flower, D. R., additional, Pineau des Forêts, G., additional, Codella, C., additional, Csengeri, T., additional, Gómez-Ruiz, A. I., additional, Heyminck, S., additional, Jacobs, K., additional, Kristensen, L. E., additional, Leurini, S., additional, Requena-Torres, M. A., additional, Wampfler, S. F., additional, Wiesemeyer, H., additional, and Wyrowski, F., additional

Published
2015
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27. Planck early results. IV. First assessment of the High Frequency Instrument in-flight performance

Author

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

Subjects
Experimental Physics, Astrophysics::Instrumentation and Methods for Astrophysics
Abstract

The Planck High Frequency Instrument (HFI) is designed to measure the temperature and polarization anisotropies of the cosmic microwave background and Galactic foregrounds in six ∼30% bands centered at 100, 143, 217, 353, 545, and 857 GHz at an angular resolution of 10 (100 GHz), 7 (143 GHz), and 5 (217 GHz and higher). HFI has been operating flawlessly since launch on 14 May 2009, with the bolometers reaching 100 mK the first week of July. The settings of the readout electronics, including bolometer bias currents, that optimize HFI’s noise performance on orbit are nearly the same as the ones chosen during ground testing. Observations of Mars, Jupiter, and Saturn have confirmed that the optical beams and the time responses of the detection chains are in good agreement with the predictions of physical optics modeling and pre-launch measurements. The Detectors suffer from a high flux of cosmic rays due to historically low levels of solar activity. As a result of the redundancy of Planck’s observation strategy, the removal of a few percent of data contaminated by glitches does not significantly affect the instrumental sensitivity. The cosmic ray flux represents a significant and variable heat load on the sub-Kelvin stage. Temporal variation and the inhomogeneous distribution of the flux results in thermal fluctuations that are a probable source of low frequency noise. The removal of systematic effects in the time ordered data provides a signal with an average noise equivalent power that is 70% of the goal in the 0.6−2.5 Hz range. This is slightly higher than was achieved during the pre-launch characterization but better than predicted in the early phases of the project. The improvement over the goal is a result of the low level of instrumental background loading achieved by the optical and thermal design of the HFI.

Published
2011

31. Sulphur-bearing molecules in diffuse molecular clouds: new results from SOFIA/GREAT and the IRAM 30 m telescope

Author

Neufeld, D. A., primary, Godard, B., additional, Gerin, M., additional, Pineau des Forêts, G., additional, Bernier, C., additional, Falgarone, E., additional, Graf, U. U., additional, Güsten, R., additional, Herbst, E., additional, Lesaffre, P., additional, Schilke, P., additional, Sonnentrucker, P., additional, and Wiesemeyer, H., additional

Published
2015
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36. Performance and Science Opportunities with the upGREAT Spectrometer onboard of SOFIA

Author

Güsten, R., primary, Wiesemeyer, H., additional, Risacher, C., additional, Stutzki, J., additional, Hübers, H.-W., additional, Bell, A., additional, Buchbender, C., additional, Büchel, D., additional, Chambers, E., additional, Csengeri, T., additional, Graf, U., additional, Heyminck, S., additional, Honingh, C., additional, Jacobs, K., additional, Klein, B., additional, Klein, T., additional, Leinz, C., additional, Okada, Y., additional, Pütz, P., additional, Requena, M., additional, Reyes, N., additional, Richter, H., additional, Ricken, O., additional, Riquelme, D., additional, Simon, R., additional, and Wunsch, A., additional

Published
2015
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38. On the radiation driven alignment of dust grains: Detection of the polarization hole in a starless core

Author

Conselho Nacional de Desenvolvimento Científico e Tecnológico (Brasil), Federal Ministry of Education and Research (Germany), Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (Brasil), Fundação de Amparo à Pesquisa do Estado de São Paulo Minas Gerais, Ministerio de Ciencia e Innovación (España), Ministerio de Economía y Competitividad (España), Generalitat de Catalunya, Alves, Felipe de O., Frau, Pau, Girart, Josep Miquel, Franco, Gabriel A. P., Santos, F. P., Wiesemeyer, H., Conselho Nacional de Desenvolvimento Científico e Tecnológico (Brasil), Federal Ministry of Education and Research (Germany), Coordenação de Aperfeiçoamento de Pessoal de Nível Superior (Brasil), Fundação de Amparo à Pesquisa do Estado de São Paulo Minas Gerais, Ministerio de Ciencia e Innovación (España), Ministerio de Economía y Competitividad (España), Generalitat de Catalunya, Alves, Felipe de O., Frau, Pau, Girart, Josep Miquel, Franco, Gabriel A. P., Santos, F. P., and Wiesemeyer, H.

Abstract

[Aims] We aim to investigate the polarization properties of a starless core in an early evolutionary stage. Linear polarization data reveal the properties of the dust grains in the distinct phases of the interstellar medium. Our goal is to investigate how the polarization degree and angle correlate with the cloud and core gas., [Methods] We use optical, near infrared, and submillimeter polarization observations on the starless object Pipe-109 in the Pipe nebula. Our data cover a physical scale range of 0.08 to 0.4 pc, comprising the dense gas, envelope, and the surrounding cloud., [Results] The cloud polarization is well traced by the optical data. The near infrared polarization is produced by a mixed population of grains from the core border and the cloud gas. The optical and near infrared polarization toward the cloud reaches the maximum possible value and saturates with respect to the visual extinction. The core polarization is predominantly traced by the submillimeter data and has a steep decrease with respect to the visual extinction. Modeling of the submillimeter polarization indicates a magnetic field main direction projected onto the plane-of-sky and loss of grain alignment for densities higher than 6 × 104 cm-3 (or AV> 30 mag)., [Conclusions] The object is immersed in a magnetized medium with a very ordered magnetic field. The absence of internal source of radiation significantly affects the polarization efficiencies in the core, creating a polarization hole at the center of the starless core. This result supports the theory of dust grain alignment via radiative torques.

Published
2014

39. Oxygen budget in low-mass protostars: the NGC 1333-IRAS4A R1 shock observed in [O i] at 63 µm with SOFIA-GREAT.

Author

Kristensen, L. E., Gusdorf, A., Mottram, J. C., Karska, A., Visser, R., Wiesemeyer, H., Güsten, R., and Simon, R.

Subjects
PROTOSTARS, MECHANICAL shock, OXYGEN, STELLAR magnitudes, RADIATIVE transfer
Abstract

In molecular outflows from forming low-mass protostars, most oxygen is expected to be locked up in water. However, Herschel observations have shown that typically an order of magnitude or more of the oxygen is still unaccounted for. To test if the oxygen is instead in atomic form, SOFIA-GREAT observed the R1 position of the bright molecular outflow from NGC 1333-IRAS4A. The [O i] 63 µm line is detected and spectrally resolved. From an intensity peak at +15 km s-1, the intensity decreases until +50 km s-1. The profile is similar to that of high-velocity (HV) H2O and CO 16-15, the latter observed simultaneously with [O i]. A radiative transfer analysis suggests that ~15% of the oxygen is in atomic form toward this shock position. The CO abundance is inferred to be ~10-4 by a similar analysis, suggesting that this is the dominant oxygen carrier in the HV component. These results demonstrate that a large portion of the observed [O i] emission is part of the outflow. Further observations are required to verify whether this is a general trend. [ABSTRACT FROM AUTHOR]

Published
2017
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43. Planck early results. VI. The High Frequency Instrument data processing

Author

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

Abstract

We describe the processing of the 336 billion raw data samples from the High Frequency Instrument (HFI) which we performed to produce six temperature maps from the first 295 days of Planck-HFI survey data. These maps provide an accurate rendition of the sky emission at 100, 143, 217, 353, 545 and 857GHz with an angular resolution ranging from 9.9 to 4.4'. The white noise level is around 1.5 mu K degree or less in the 3 main CMB channels (100-217 GHz). The photometric accuracy is better than 2% at frequencies between 100 and 353 GHz and around 7% at the two highest frequencies. The maps created by the HFI Data Processing Centre reach our goals in terms of sensitivity, resolution, and photometric accuracy. They are already sufficiently accurate and well-characterised to allow scientific analyses which are presented in an accompanying series of early papers. At this stage, HFI data appears to be of high quality and we expect that with further refinements of the data processing we should be able to achieve, or exceed, the science goals of the Planck project.

Published
2011

44. Planck early results. IV. First assessment of the High Frequency Instrument in-flight performance

Author

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

Abstract

The Planck High Frequency Instrument (HFI) is designed to measure the temperature and polarization anisotropies of the cosmic microwave background and Galactic foregrounds in six ~30% bands centered at 100, 143, 217, 353, 545, and 857 GHz at an angular resolution of 10′ (100 GHz), 7′ (143 GHz), and 5′ (217 GHz and higher). HFI has been operating flawlessly since launch on 14 May 2009, with the bolometers reaching 100 mK the first week of July. The settings of the readout electronics, including bolometer bias currents, that optimize HFI's noise performance on orbit are nearly the same as the ones chosen during ground testing. Observations of Mars, Jupiter, and Saturn have confirmed that the optical beams and the time responses of the detection chains are in good agreement with the predictions of physical optics modeling and pre-launch measurements. The Detectors suffer from a high flux of cosmic rays due to historically low levels of solar activity. As a result of the redundancy of Planck's observation strategy, theremoval of a few percent of data contaminated by glitches does not significantly affect the instrumental sensitivity. The cosmic ray flux represents a significant and variable heat load on the sub-Kelvin stage. Temporal variation and the inhomogeneous distribution of the flux results in thermal fluctuations that are a probable source of low frequency noise. The removal of systematic effects in the time ordered data provides a signal with an average noise equivalent power that is 70% of the goal in the 0.6-2.5 Hz range. This is slightly higher than was achieved during the pre-launch characterization but better than predicted in the early phases of the project. The improvement over the goal is a result of the low level of instrumental background loading achieved by the optical and thermal design of the HFI.

Published
2011

47. GREAT/SOFIA atmospheric calibration

Author

Guan, X., primary, Stutzki, J., additional, Graf, U. U., additional, Güsten, R., additional, Okada, Y., additional, Requena-Torres, M. A., additional, Simon, R., additional, and Wiesemeyer, H., additional

Published
2012
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50. The ionized and hot gas in M17 SW

Author

Pérez-Beaupuits, J. P., primary, Wiesemeyer, H., additional, Ossenkopf, V., additional, Stutzki, J., additional, Güsten, R., additional, Simon, R., additional, Hübers, H.-W., additional, and Ricken, O., additional

Published
2012
Full Text
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