Author: "Joncas, G." / Language: undetermined - Searchworks@Jio Institute Digital Library Search Results

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21 results on '"Joncas, G."'

1. Properties of Hi-GAL clumps in the inner Galaxy]{The Hi-GAL compact source catalogue. I. The physical properties of the clumps in the inner Galaxy ($-71.0^{\circ}< \ell < 67.0^{\circ}$)

Author: Elia, D., Molinari, S., Schisano, E., Pestalozzi, M., Pezzuto, S., Merello, M., Noriega-Crespo, A., Moore, T. J. T., Russeil, D., Mottram, J. C., Paladini, R., Strafella, F., Benedettini, M., Bernard, J. P., Di Giorgio, A., Eden, D. J., Fukui, Y., Plume, R., Bally, J., Martin, P. G., Ragan, S. E., Jaffa, S. E., Motte, F., Olmi, L., Schneider, N., Testi, L., Wyrowski, F., Zavagno, A., Calzoletti, L., Faustini, F., Natoli, P., Palmerim, P., Piacentini, F., Piazzo, L., Pilbratt, G. L., Polychroni, D., Baldeschi, A., Beltr��n, M. T., Billot, N., Cambr��sy, L., Cesaroni, R., Garc��a-Lario, P., Hoare, M. G., Huang, M., Joncas, G., Liu, S. J., Maiolo, B. M. T., Marsh, K. A., Maruccia, Y., M��ge, P., Peretto, N., Rygl, K. L. J., Schilke, P., Thompson, M. A., Traficante, A., Umana, G., Veneziani, M., Ward-Thompson, D., Whitworth, A. P., Arab, H., Bandieramonte, M., Becciani, U., Brescia, M., Buemi, C., Bufano, F., Butora, R., Cavuoti, S., Costa, A., Fiorellino, E., Hajnal, A., Hayakawa, T., Kacsuk, P., Leto, P., Causi, G. Li, Marchili, N., Martinavarro-Armengol, S., Mercurio, A., Molinaro, M., Riccio, G., Sano, H., Sciacca, E., Tachihara, K., Torii, K., Trigilio, C., Vitello, F., and Yamamoto, H.
Subjects: Astrophysics of Galaxies (astro-ph.GA), Astrophysics::Solar and Stellar Astrophysics, FOS: Physical sciences, Astrophysics::Earth and Planetary Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Galaxy Astrophysics
Abstract: Hi-GAL is a large-scale survey of the Galactic plane, performed with Herschel in five infrared continuum bands between 70 and 500 $��$m. We present a band-merged catalogue of spatially matched sources and their properties derived from fits to the spectral energy distributions (SEDs) and heliocentric distances, based on the photometric catalogs presented in Molinari et al. (2016a), covering the portion of Galactic plane $-71.0^{\circ}< \ell < 67.0^{\circ}$. The band-merged catalogue contains 100922 sources with a regular SED, 24584 of which show a 70 $��$m counterpart and are thus considered proto-stellar, while the remainder are considered starless. Thanks to this huge number of sources, we are able to carry out a preliminary analysis of early stages of star formation, identifying the conditions that characterise different evolutionary phases on a statistically significant basis. We calculate surface densities to investigate the gravitational stability of clumps and their potential to form massive stars. We also explore evolutionary status metrics such as the dust temperature, luminosity and bolometric temperature, finding that these are higher in proto-stellar sources compared to pre-stellar ones. The surface density of sources follows an increasing trend as they evolve from pre-stellar to proto-stellar, but then it is found to decrease again in the majority of the most evolved clumps. Finally, we study the physical parameters of sources with respect to Galactic longitude and the association with spiral arms, finding only minor or no differences between the average evolutionary status of sources in the fourth and first Galactic quadrants, or between "on-arm" and "inter-arm" positions., Accepted by MNRAS
Published: 2017
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2. Hi-GAL, the Herschel infrared Galactic Plane Survey: photometric maps and compact source catalogues. First data release for Inner Milky Way: +68��> l > -70��

Author: Molinari, S., Schisano, E., Elia, D., Pestalozzi, M., Traficante, A., Pezzuto, S., Swinyard, B. M., Noriega-Crespo, A., Bally, J., Moore, T. J. T., Plume, R., Zavagno, A., di Giorgio, A. M., Liu, S. J., Pilbratt, G. L., Mottram, J. C., Russeil, D., Piazzo, L., Veneziani, M., Benedettini, M., Calzoletti, L., Faustini, F., Natoli, P., Piacentini, F., Merello, M., Palmese, A., Del Grande, R., Polychroni, D., Rygl, K. L. J., Polenta, G., Barlow, M. J., Bernard, J. -P., Martin, P. G., Testi, L., Ali, B., Andr��, P., Beltr��n, M. T., Billot, N., Brunt, C., Carey, S., Cesaroni, R., Compi��gne, M., Eden, D., Fukui, Y., Garcia-Lario, P., Hoare, M. G., Huang, M., Joncas, G., Lim, T. L., Lord, S. D., Martinavarro-Armengol, S., Motte, F., Paladini, R., Paradis, D., Peretto, N., Robitaille, T., Schilke, P., Schneider, N., Schulz, B., Sibthorpe, B., Strafella, F., Thompson, M. A., Umana, G., Ward-Thompson, D., and Wyrowski, F.
Subjects: Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences
Abstract: (Abridged) We present the first public release of high-quality data products (DR1) from Hi-GAL, the {\em Herschel} infrared Galactic Plane Survey. Hi-GAL is the keystone of a suite of continuum Galactic Plane surveys from the near-IR to the radio, and covers five wavebands at 70, 160, 250, 350 and 500 micron, encompassing the peak of the spectral energy distribution of cold dust for 8 < T < 50K. This first Hi-GAL data release covers the inner Milky Way in the longitude range 68�� > l > -70�� in a |b, Astronomy & Astrophysics, accepted
Published: 2016
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3. Planck 2013 results. XI. All-sky model of thermal dust emission

Author: Tauber, Jan, Abergel, A., Ade, P. A. R., Aghanim, N., Alves, M. I. R., Aniano, G., Armitage Caplan, C., Arnaud, M., Ashdown, M., Atrio Barandela, F., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Bartlett, J. G., Battaner, E., Benabed, K., Benoît, A., Benoit Lévy, A., Bernard, J. P., Bersanelli, M., Bielewicz, P., Bobin, J., Bock, J. J., Bonaldi, A., Bond, J. R., Borrill, J., Bouchet, F. R., Boulanger, F., Bridges, M., Bucher, M., Burigana, C., Butler, R. C., Cardoso, J. F., Catalano, A., Chamballu, A., Chary, R. R., Chiang, H. C., Chiang, L. Y., Christensen, P. R., Church, S., Clemens, M., Clements, D. L., Colombi, S., Colombo, L. P. L., Combet, C., Couchot, F., Coulais, A., Crill, B. P., Curto, A., Cuttaia, F., Danese, L., Davies, R. D., Davis, R. J., DE BERNARDIS, Paolo, De Rosa, A., De Zotti, G., Delabrouille, J., Delouis, J. M., Désert, F. X., Dickinson, C., Diego, J. M., Dole, H., Donzelli, S., Doré, O., Douspis, M., Draine, B. T., Dupac, X., Efstathiou, G., Enßlin, T. A., Eriksen, H. K., Falgarone, E., Finelli, F., Forni, O., Frailis, M., Fraisse, A. A., Franceschi, E., Galeotta, S., Ganga, K., Ghosh, T., Giard, M., Giardino, G., Giraud Héraud, Y., González Nuevo, J., Górski, K. M., Gratton, S., Gregorio, A., Grenier, I. A., Gruppuso, A., Guillet, V., Hansen, F. K., Hanson, D., Harrison, D. L., Helou, G., Henrot Versillé, S., Hernández Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hornstrup, A., Hovest, W., Huffenberger, K. M., Jaffe, A. H., Jaffe, T. R., Jewell, J., Joncas, G., Jones, W. C., Juvela, M., Keihänen, E., Keskitalo, R., Kisner, T. S., Knoche, J., Knox, L., Kunz, M., Kurki Suonio, H., Lagache, G., Lähteenmäki, A., Lamarre, J. M., Lasenby, A., Laureijs, R. J., Lawrence, C. R., Leonardi, R., León Tavares, J., Lesgourgues, J., Levrier, F., Liguori, M., Lilje, P. B., Linden Vørnle, M., López Caniego, M., Lubin, P. M., Maciás Pérez, J. F., Maffei, B., Maino, D., Mandolesi, N., Maris, M., Marshall, D. J., Martin, P. G., Martínez González, E., MASI, Silvia, Massardi, M., Matarrese, S., Matthai, F., Mazzotta, P., Mcgehee, P., MELCHIORRI, Alessandro, Mendes, L., Mennella, A., Migliaccio, M., Mitra, S., Miville Deschênes, M. A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, J. A., Naselsky, P., NATI, FEDERICO, Natoli, P., Netterfield, C. B., Nørgaard Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., Osborne, S., Oxborrow, C. A., Paci, F., PAGANO, LUCA, Pajot, F., Paladini, R., Paoletti, D., Pasian, F., Patanchon, G., Perdereau, O., Perotto, L., Perrotta, F., PIACENTINI, Francesco, Piat, M., Pierpaoli, E., Pietrobon, D., Plaszczynski, S., Pointecouteau, E., Polenta, G., Ponthieu, N., Popa, L., Poutanen, T., Pratt, G. W., Prézeau, G., Prunet, S., Puget, J. L., Rachen, J. P., Reach, W. T., Rebolo, R., Reinecke, M., Remazeilles, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Roudier, G., Rowan Robinson, M., Rubinõ Martín, J. A., Rusholme, B., Sandri, M., Santos, D., Savini, G., Scott, D., Seiffert, M. D., Shellard, E. P. S., Spencer, L. D., Starck, J. L., Stolyarov, V., Stompor, R., Sudiwala, R., Sunyaev, R., Sureau, F., Sutton, D., Suur Uski, A. S., Sygnet, J. F., Tauber, J. A., Tavagnacco, D., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Tuovinen, J., Türler, M., Umana, G., Valenziano, L., Valiviita, J., Van Tent, B., Verstraete, L., Vielva, P., Villa, F., Vittorio, N., Wade, L. A., Wandelt, B. D., Welikala, N., Ysard, N., Yvon, D., Zacchei, A., Zonca, A., Department of Physics, Helsinki Institute of Physics, Universidad de Cantabria, Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-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), Institut Néel (NEEL), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Etude du Rayonnement et de la Matière en Astrophysique (LERMA), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Pierre et Marie Curie - Paris 6 (UPMC)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université de Cergy Pontoise (UCP), Université Paris-Seine-Université Paris-Seine-Centre National de la Recherche Scientifique (CNRS), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), APC - Gravitation (APC-Gravitation), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, PLANCK, Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Hélium : du fondamental aux applications (HELFA), Institut 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), École normale supérieure - Paris (ENS Paris), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), 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), 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)-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)-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)-Centre National de la Recherche Scientifique (CNRS), HELFA - Hélium : du fondamental aux applications, Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), 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), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), European Commission, European Research Council, Alfred P. Sloan Foundation, Science and Technology Facilities Council (STFC), Science and Technology Facilities Council [2006-2012], Tauber, Jan, Abergel, A., Ade, P. A. R., Aghanim, N., Alves, M. I. R., Aniano, G., Armitage Caplan, C., Arnaud, M., Ashdown, M., Atrio Barandela, F., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Bartlett, J. G., Battaner, E., Benabed, K., Benoît, A., Benoit Lévy, A., Bernard, J. P., Bersanelli, M., Bielewicz, P., Bobin, J., Bock, J. J., Bonaldi, A., Bond, J. R., Borrill, J., Bouchet, F. R., Boulanger, F., Bridges, M., Bucher, M., Burigana, C., Butler, R. C., Cardoso, J. F., Catalano, A., Chamballu, A., Chary, R. R., Chiang, H. C., Chiang, L. Y., Christensen, P. R., Church, S., Clemens, M., Clements, D. L., Colombi, S., Colombo, L. P. L., Combet, C., Couchot, F., Coulais, A., Crill, B. P., Curto, A., Cuttaia, F., Danese, L., Davies, R. D., Davis, R. J., De Bernardis, P., De Rosa, A., De Zotti, G., Delabrouille, J., Delouis, J. M., Désert, F. X., Dickinson, C., Diego, J. M., Dole, H., Donzelli, S., Doré, O., Douspis, M., Draine, B. T., Dupac, X., Efstathiou, G., Enßlin, T. A., Eriksen, H. K., Falgarone, E., Finelli, F., Forni, O., Frailis, M., Fraisse, A. A., Franceschi, E., Galeotta, S., Ganga, K., Ghosh, T., Giard, M., Giardino, G., Giraud Héraud, Y., González Nuevo, J., Górski, K. M., Gratton, S., Gregorio, Anna, Grenier, I. A., Gruppuso, A., Guillet, V., Hansen, F. K., Hanson, D., Harrison, D. L., Helou, G., Henrot Versillé, S., Hernández Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hornstrup, A., Hovest, W., Huffenberger, K. M., Jaffe, A. H., Jaffe, T. R., Jewell, J., Joncas, G., Jones, W. C., Juvela, M., Keihänen, E., Keskitalo, R., Kisner, T. S., Knoche, J., Knox, L., Kunz, M., Kurki Suonio, H., Lagache, G., Lähteenmäki, A., Lamarre, J. M., Lasenby, A., Laureijs, R. J., Lawrence, C. R., Leonardi, R., León Tavares, J., Lesgourgues, J., Levrier, F., Liguori, M., Lilje, P. B., Linden Vørnle, M., López Caniego, M., Lubin, P. M., Maciás Pérez, J. F., Maffei, B., Maino, D., Mandolesi, N., Maris, M., Marshall, D. J., Martin, P. G., Martínez González, E., Masi, S., Massardi, M., Matarrese, S., Matthai, F., Mazzotta, P., Mcgehee, P., Melchiorri, A., Mendes, L., Mennella, A., Migliaccio, M., Mitra, S., Miville Deschênes, M. A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Natoli, P., Netterfield, C. B., Nørgaard Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., Osborne, S., Oxborrow, C. A., Paci, F., Pagano, L., Pajot, F., Paladini, R., Paoletti, D., Pasian, F., Patanchon, G., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Pierpaoli, E., Pietrobon, D., Plaszczynski, S., Pointecouteau, E., Polenta, G., Ponthieu, N., Popa, L., Poutanen, T., Pratt, G. W., Prézeau, G., Prunet, S., Puget, J. L., Rachen, J. P., Reach, W. T., Rebolo, R., Reinecke, M., Remazeilles, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Roudier, G., Rowan Robinson, M., Rubinõ Martín, J. A., Rusholme, B., Sandri, M., Santos, D., Savini, G., Scott, D., Seiffert, M. D., Shellard, E. P. S., Spencer, L. D., Starck, J. L., Stolyarov, V., Stompor, R., Sudiwala, R., Sunyaev, R., Sureau, F., Sutton, D., Suur Uski, A. S., Sygnet, J. F., Tauber, J. A., Tavagnacco, Daniele, Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Tuovinen, J., Türler, M., Umana, G., Valenziano, L., Valiviita, J., Van Tent, B., Verstraete, L., Vielva, P., Villa, F., Vittorio, N., Wade, L. A., Wandelt, B. D., Welikala, N., Ysard, N., Yvon, D., Zacchei, A., Zonca, A., Tauber, J, Abergel, A, Ade, P, Aghanim, N, Alves, M, Aniano, G, Armitage Caplan, C, Arnaud, M, Ashdown, M, Atrio Barandela, F, Aumont, J, Baccigalupi, C, Banday, A, Barreiro, R, Bartlett, J, Battaner, E, Benabed, K, Benoît, A, Benoit Lévy, A, Bernard, J, Bersanelli, M, Bielewicz, P, Bobin, J, Bock, J, Bonaldi, A, Bond, J, Borrill, J, Bouchet, F, Boulanger, F, Bridges, M, Bucher, M, Burigana, C, Butler, R, Cardoso, J, Catalano, A, Chamballu, A, Chary, R, Chiang, H, Chiang, L, Christensen, P, Church, S, Clemens, M, Clements, D, Colombi, S, Colombo, L, Combet, C, Couchot, F, Coulais, A, Crill, B, Curto, A, Cuttaia, F, Danese, L, Davies, R, Davis, R, DE BERNARDIS, P, De Rosa, A, De Zotti, G, Delabrouille, J, Delouis, J, Désert, F, Dickinson, C, Diego, J, Dole, H, Donzelli, S, Doré, O, Douspis, M, Draine, B, Dupac, X, Efstathiou, G, Enßlin, T, Eriksen, H, Falgarone, E, Finelli, F, Forni, O, Frailis, M, Fraisse, A, Franceschi, E, Galeotta, S, Ganga, K, Ghosh, T, Giard, M, Giardino, G, Giraud Héraud, Y, González Nuevo, J, Górski, K, Gratton, S, Gregorio, A, Grenier, I, Gruppuso, A, Guillet, V, Hansen, F, Hanson, D, Harrison, D, Helou, G, Henrot Versillé, S, Hernández Monteagudo, C, Herranz, D, Hildebrandt, S, Hivon, E, Hobson, M, Holmes, W, Hornstrup, A, Hovest, W, Huffenberger, K, Jaffe, A, Jaffe, T, Jewell, J, Joncas, G, Jones, W, Juvela, M, Keihänen, E, Keskitalo, R, Kisner, T, Knoche, J, Knox, L, Kunz, M, Kurki Suonio, H, Lagache, G, Lähteenmäki, A, Lamarre, J, Lasenby, A, Laureijs, R, Lawrence, C, Leonardi, R, León Tavares, J, Lesgourgues, J, Levrier, F, Liguori, M, Lilje, P, Linden Vørnle, M, López Caniego, M, Lubin, P, Maciás Pérez, J, Maffei, B, Maino, D, Mandolesi, N, Maris, M, Marshall, D, Martin, P, Martínez González, E, Masi, S, Massardi, M, Matarrese, S, Matthai, F, Mazzotta, P, Mcgehee, P, Melchiorri, A, Mendes, L, Mennella, A, Migliaccio, M, Mitra, S, Miville Deschênes, M, Moneti, A, Montier, L, Morgante, G, Mortlock, D, Munshi, D, Murphy, J, Naselsky, P, Nati, F, Natoli, P, Netterfield, C, Nørgaard Nielsen, H, Noviello, F, Novikov, D, Novikov, I, Osborne, S, Oxborrow, C, Paci, F, Pagano, L, Pajot, F, Paladini, R, Paoletti, D, Pasian, F, Patanchon, G, Perdereau, O, Perotto, L, Perrotta, F, Piacentini, F, Piat, M, Pierpaoli, E, Pietrobon, D, Plaszczynski, S, Pointecouteau, E, Polenta, G, Ponthieu, N, Popa, L, Poutanen, T, Pratt, G, Prézeau, G, Prunet, S, Puget, J, Rachen, J, Reach, W, Rebolo, R, Reinecke, M, Remazeilles, M, Renault, C, Ricciardi, S, Riller, T, Ristorcelli, I, Rocha, G, Rosset, C, Roudier, G, Rowan Robinson, M, Rubinõ Martín, J, Rusholme, B, Sandri, M, Santos, D, Savini, G, Scott, D, Seiffert, M, Shellard, E, Spencer, L, Starck, J, Stolyarov, V, Stompor, R, Sudiwala, R, Sunyaev, R, Sureau, F, Sutton, D, Suur Uski, A, Sygnet, J, Tavagnacco, D, Terenzi, L, Toffolatti, L, Tomasi, M, Tristram, M, Tucci, M, Tuovinen, J, Türler, M, Umana, G, Valenziano, L, Valiviita, J, Van Tent, B, Verstraete, L, Vielva, P, Villa, F, Vittorio, N, Wade, L, Wandelt, B, Welikala, N, Ysard, N, Yvon, D, Zacchei, A, and Zonca, A
Subjects: SOLAR NEIGHBORHOOD, [SDU.ASTR.CO]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Astronomy, Astrophysics, 7. Clean energy, 01 natural sciences, Dust, extinction, Infrared: ISM, ISM: general, Methods: data analysis, Opacity, Submillimeter: ISM, Astronomy and Astrophysics, Space and Planetary Science, Luminosity, 7TH DATA RELEASE, INTERSTELLAR MOLECULAR-HYDROGEN, Astrophysics::Solar and Stellar Astrophysics, HIGH GALACTIC LATITUDES, data analysis [Methods], 010303 astronomy & astrophysics, Optical depth, Physics, infrared: ISM, Spectral index, general [ISM], extinction, 4. Education, ISM [Submillimeter], Astrophysics::Instrumentation and Methods for Astrophysics, Dust, Extinction, Computer Science::Computers and Society, CIRRUS CLOUDS, Physical Sciences, Physics::Space Physics, astro-ph.CO, ComputingMethodologies_DOCUMENTANDTEXTPROCESSING, submillimeter: ISM, dust, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Astrophysics::Earth and Planetary Astrophysics, dust, extinction, Astrophysics - Cosmology and Nongalactic Astrophysics, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Astrophysics::High Energy Astrophysical Phenomena, astro-ph.GA, INFRARED-EMISSION, ISM [Infrared], Extinction (astronomy), education, Data analysis, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, SPECTRAL ENERGY-DISTRIBUTIONS, Astronomy & Astrophysics, Computer Science::Digital Libraries, NO, [PHYS.ASTR.CO]Physics [physics]/Astrophysics [astro-ph]/Cosmology and Extra-Galactic Astrophysics [astro-ph.CO], Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Astrophysics::Galaxy Astrophysics, Science & Technology, 010308 nuclear & particles physics, Molecular cloud, opacity, Quasar, Astronomy and Astrophysic, 115 Astronomy, Space science, Astrophysics - Astrophysics of Galaxies, methods: data analysis, data analysi [Methods], Interstellar medium, 0201 Astronomical And Space Sciences, [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Astrophysics of Galaxies (astro-ph.GA), ULTRAVIOLET EXTINCTION, PROTOPLANETARY DISKS, Methods: data analysi, H-I
Abstract: The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, JA and RES (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php? project=planck&page=Planck_Collaboration. The research leading to these results has received funding from the European Research Council under the European Union’s Seventh Framework Programme (FP7/2007-2013)/ERC grant agreement No. 267934. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the US Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbuk agakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS web site is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-PlanckInstitute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington. Some of the results in this paper have been derived using the HEALPix package., This paper presents an all-sky model of dust emission from the Planck 353, 545, and 857 GHz, and IRAS 100 µm data. Using a modified blackbody fit to the data we present all-sky maps of the dust optical depth, temperature, and spectral index over the 353–3000 GHz range. This model is a good representation of the IRAS and Planck data at 50 between 353 and 3000 GHz (850 and 100 µm). It shows variations of the order of 30% compared with the widely-used model of Finkbeiner, Davis, and Schlegel. The Planck data allow us to estimate the dust temperature uniformly over the whole sky, down to an angular resolution of 50 , providing an improved estimate of the dust optical depth compared to previous all-sky dust model, especially in high-contrast molecular regions where the dust temperature varies strongly at small scales in response to dust evolution, extinction, and/or local production of heating photons. An increase of the dust opacity at 353 GHz, τ353/NH, from the diffuse to the denser interstellar medium (ISM) is reported. It is associated with a decrease in the observed dust temperature, Tobs, that could be due at least in part to the increased dust opacity. We also report an excess of dust emission at H  column densities lower than 1020 cm−2 that could be the signature of dust in the warm ionized medium. In the diffuse ISM at high Galactic latitude, we report an anticorrelation between τ353/NH and Tobs while the dust specific luminosity, i.e., the total dust emission integrated over frequency (the radiance) per hydrogen atom, stays about constant, confirming one of the Planck Early Results obtained on selected fields. This effect is compatible with the view that, in the diffuse ISM, Tobs responds to spatial variations of the dust opacity, due to variations of dust properties, in addition to (small) variations of the radiation field strength. The implication is that in the diffuse high-latitude ISM τ353 is not as reliable a tracer of dust column density as we conclude it is in molecular clouds where the correlation of τ353 with dust extinction estimated using colour excess measurements on stars is strong. To estimate Galactic E(B − V) in extragalactic fields at high latitude we develop a new method based on the thermal dust radiance, instead of the dust optical depth, calibrated to E(B−V) using reddening measurements of quasars deduced from Sloan Digital Sky Survey data., Planck (http://www.esa.int/Planck) is a project of the European Space Agency (ESA) with instruments provided by two scientific consortia funded by ESA member states (in particular the lead countries France and Italy), with contributions from NASA (USA) and telescope reflectors provided by a collaboration between ESA and a scientific consortium led and funded by Denmark.
Published: 2014
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4. Planck intermediate results: XVII. Emission of dust in the diffuse interstellar medium from the far-infrared to microwave frequencies

Author: Abergel, A, Ade, PAR, Aghanim, N, Alves, MIR, Aniano, G, Arnaud, M, Ashdown, M, Aumont, J, Baccigalupi, C, Banday, AJ, Barreiro, RB, Bartlett, JG, Battaner, E, Benabed, K, Benoit-Lévy, A, Bernard, JP, Bersanelli, M, Bielewicz, P, Bobin, J, Bonaldi, A, Bond, JR, Bouchet, FR, Boulanger, F, Burigana, C, Cardoso, JF, Catalano, A, Chamballu, A, Chiang, HC, Christensen, PR, Clements, DL, Colombi, S, Colombo, LPL, Couchot, F, Crill, BP, Cuttaia, F, Danese, L, Davis, RJ, De Bernardis, P, De Rosa, A, De Zotti, G, Delabrouille, J, Désert, FX, Dickinson, C, Diego, JM, Dole, H, Donzelli, S, Doré, O, Douspis, M, Dupac, X, Efstathiou, G, Enßlin, TA, Eriksen, HK, Falgarone, E, Finelli, F, Forni, O, Frailis, M, Franceschi, E, Galeotta, S, Ganga, K, Ghosh, T, Giard, M, Giraud-Héraud, Y, González-Nuevo, J, Górski, KM, Gregorio, A, Gruppuso, A, Guillet, V, Hansen, FK, Harrison, D, Helou, G, Henrot-Versillé, S, Hernández-Monteagudo, C, Herranz, D, Hildebrandt, SR, Hivon, E, Hobson, M, Holmes, WA, Hornstrup, A, Hovest, W, Huffenberger, KM, Jaffe, AH, Jaffe, TR, Joncas, G, Jones, A, Jones, WC, Juvela, M, Kalberla, P, Keihänen, E, Kerp, J, Keskitalo, R, Kisner, TS, Kneissl, R, Knoche, J, Kunz, M, Kurki-Suonio, H, Lagache, G, Lähteenmäki, A, Lamarre, JM, Lasenby, A, and Lawrence, CR
Subjects: extinction, Astrophysics::High Energy Astrophysical Phenomena, astro-ph.GA, Astrophysics::Cosmology and Extragalactic Astrophysics, cosmic background radiation, Astronomy & Astrophysics, diffuse background [infrared], Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Earth and Planetary Astrophysics, dust, ISM [submillimeter], Astrophysics::Galaxy Astrophysics, local insterstellar matter, Astronomical and Space Sciences
Abstract: The dust-Hi correlation is used to characterize the emission properties of dust in the diffuse interstellar medium (ISM) from far infrared wavelengths to microwave frequencies. The field of this investigation encompasses the part of the southern sky best suited to study the cosmic infrared and microwave backgrounds. We cross-correlate sky maps from Planck, the Wilkinson Microwave Anisotropy Probe (WMAP), and the diffuse infrared background experiment (DIRBE), at 17 frequencies from 23 to 3000 GHz, with the Parkes survey of the 21 cm line emission of neutral atomic hydrogen, over a contiguous area of 7500 deg2 centred on the southern Galactic pole. We present a general methodology to study the dust-H i correlation over the sky, including simulations to quantify uncertainties. Our analysis yields four specific results. (1) We map the temperature, submillimetre emissivity, and opacity of the dust per H-atom. The dust temperature is observed to be anti-correlated with the dust emissivity and opacity. We interpret this result as evidence of dust evolution within the diffuse ISM. The mean dust opacity is measured to be (7.1 ± 0.6) × 10-27 cm2 H-1 × (v/353 GHz) 1.53 ± 0.03for 100 ≤ v ≤ 353 GHz. This is a reference value to estimate hydrogen column densities from dust emission at submillimetre and millimetre wavelengths. (2) We map the spectral index βmm of dust emission at millimetre wavelengths (defined here as v ≤ 353GHz), and find it to be remarkably constant at βmm = 1.51 ± 0.13. We compare it with the far infrared spectral index βFIR derived from greybody fits at higher frequencies, and find a systematic difference, βmm -βFIR = -0.15, which suggests that the dust spectral energy distribution (SED) flattens at v ≤ 353 GHz. (3) We present spectral fits of the microwave emission correlated with Hi from 23 to 353 GHz, which separate dust and anomalous microwave emission (AME). We show that the flattening of the dust SED can be accounted for with an additional component with a blackbody spectrum. This additional component, which accounts for (26 ± 6)% of the dust emission at 100GHz, could represent magnetic dipole emission. Alternatively, it could account for an increasing contribution of carbon dust, or a flattening of the emissivity of amorphous silicates, at millimetre wavelengths. These interpretations make different predictions for the dust polarization SED. (4) We analyse the residuals of the dust-Hi correlation. We identify a Galactic contribution to these residuals, which we model with variations of the dust emissivity on angular scales smaller than that of our correlation analysis. This model of the residuals is used to quantify uncertainties of the CIB power spectrum in a companion Planck paper.© ESO 2014.
Published: 2014

5. The Canadian Galactic Plane Survey

Author: Gibson, S., Taylor, A. R., Leahy, A., Dougherty, S., Carignan, C., St -Louis, N., Fich, M., Ghazzali, N., Joncas, G., Pineault, S., Normandeau, M., Heiles, C., Irwin, J., English, J., Martin, P., Johnstone, D., Basu, S., Mccutcheon, W., Routledge, D., Vaneldik, F., Dewdney, P., Galt, J., Gray, A., Higgs, L., Lewis Knee, Landecker, T., Purton, C., Roger, R. S., Tapping, K., Willis, T., Moriarty-Schieven, G., Beichman, C., Terebey, S., Duric, N., Green, D., Heyer, M., Wendker, H., and Zhang, Xizhen

6. Physical conditions of star forming sites in the S247/252 molecular complex

Author: Koempe, C., Joncas, G., Jan Wouterloot, and Meyerdierks, H.
Subjects: Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics::Earth and Planetary Astrophysics, General Medicine, Astrophysics::Galaxy Astrophysics
Abstract: By now, it is well established that massive stars form in giant molecular clouds. Numerous studies have shown that star formation, instead of being spread uniformly throughout molecular clouds, occurs in dense condensations located within these clouds. The physical conditions in these condensations are therefore critical input parameters for any theory of star formation.

7. VizieR Online Data Catalog: JCMT Gould Belt Survey: dense cores in Orion B (Kirk+, 2016)

Author: Kirk, H., Di Francesco, J., Doug Johnstone, Duarte-Cabral, A., Sadavoy, S., Hatchell, J., Mottram, J. C., Buckle, J., Berry, D. S., Broekhoven-Fiene, H., Currie, M. J., Fich, M., Jenness, T., Nutter, D., Pattle, K., Pineda, J. E., Quinn, C., Salji, C., Tisi, S., Hogerheijde, M. R., Ward-Thompson, D., Bastien, P., Bresnahan, D., Butner, H., Chen, M., Chrysostomou, A., Coude, S., Davis, C. J., Drabek-Maunder, E., Fiege, J., Friberg, P., Friesen, R., Fuller, G. A., Graves, S., Greaves, J., Gregson, J., Holland, W., Joncas, G., Kirk, J. M., Knee, L. B. G., Mairs, S., Marsh, K., Matthews, B. C., Moriarty-Schieven, G., Mowat, C., Rawlings, J., Richer, J., Robertson, D., Rosolowsky, E., Rumble, D., Thomas, H., Tothill, N., Viti, S., White, G. J., Wouterloot, J., Yates, J., and Zhu, M.

8. Planck Early Results: The Galactic Cold Core Population revealed by the first all-sky survey

Author: Planck Collaboration, Ade, P. A. R., Aghanim, N., Arnaud, M., Ashdown, M., Aumont, J., Baccigalupi, C., Balbi, A., Banday, A. J., Barreiro, R. B., Bartlett, J. G., Battaner, E., Benabed, K., Benoît, A., Bernard, J. -P., Bersanelli, M., Bhatia, R., Bock, J. J., Bonaldi, A., Bond, J. R., Borrill, J., Bouchet, F. R., Boulanger, F., Bucher, M., Burigana, C., Cabella, P., Cantalupo, C. M., Cardoso, J. -F., Catalano, A., Cayón, L., Challinor, A., Chamballu, A., Chary, R. -R., Chiang, L. -Y, Christensen, P. R., Clements, D. L., Colombi, S., Couchot, F., Coulais, A., Crill, B. P., Cuttaia, F., Danese, L., Davies, R. D., Davis, R. J., de Bernardis, P., de Gasperis, G., de Rosa, A., de Zotti, G., Delabrouille, J., Delouis, J. -M., Désert, F. -X., Dickinson, C., Dobashi, K., Donzelli, S., Doré, O., Dörl, U., Douspis, M., Dupac, X., Efstathiou, G., Enßlin, T. A., Falgarone, E., Finelli, F., Forni, O., Frailis, M., Franceschi, E., Galeotta, S., Ganga, K., Giard, M., Giardino, G., Giraud-Héraud, Y., González-Nuevo, J., Górski, K. M., Gratton, S., Gregorio, A., Gruppuso, A., Hansen, F. K., Harrison, D., Helou, G., Henrot-Versillé, S., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hovest, W., Hoyland, R. J., Huffenberger, K. M., Jaffe, A. H., Joncas, G., Jones, W. C., Juvela, M., Keihänen, E., Keskitalo, R., Kisner, T. S., Kneissl, R., Knox, L., Kurki-Suonio, H., Lagache, G., Lamarre, J. -M., Lasenby, A., Laureijs, R. J., Lawrence, C. R., Leach, S., Leonardi, R., Leroy, C., Linden-Vørnle, M., López-Caniego, M., Lubin, P. M., Macías-Pérez, J. F., MacTavish, C. J., Maffei, B., Mandolesi, N., Mann, R., Maris, M., Marshall, D. J., Martin, P., Martínez-González, E., Marton, G., Masi, S., Matarrese, S., Matthai, F., Mazzotta, P., McGehee, P., Melchiorri, A., Mendes, L., Mennella, A., Mitra, S., Miville-Deschênes, M. -A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, A., Naselsky, P., Nati, F., Natoli, P., Netterfield, C. B., Nørgaard-Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., Osborne, S., Pajot, F., Paladini, R., Pasian, F., Patanchon, G., Pearson, T. J., Pelkonen, V. -M., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Plaszczynski, S., Pointecouteau, E., Polenta, G., Ponthieu, N., Poutanen, T., Prézeau, G., Prunet, S., Puget, J. -L., Reach, W. T., Rebolo, R., Reinecke, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Rowan-Robinson, M., Rubiño-Martín, J. A., Rusholme, B., Sandri, M., Santos, D., Savini, G., Scott, D., Seiffert, M. D., Smoot, G. F., Starck, J. -L., Stivoli, F., Stolyarov, V., Sudiwala, R., Sygnet, J. -F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Torre, J. -P., Toth, V., Tristram, M., Tuovinen, J., Umana, G., Valenziano, L., Vielva, P., Villa, F., Vittorio, N., Wade, L. A., Wandelt, B. D., Ysard, N., Yvon, D., Zacchei, A., Zahorecz, S., Zonca, A., APC - Cosmologie, Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), AstroParticule et Cosmologie (APC (UMR_7164)), Laboratoire de l'Accélérateur Linéaire (LAL), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), APC - Gravitation (APC-Gravitation), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), Max-Planck-Gesellschaft-Max-Planck-Gesellschaft, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA), PLANCK, 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), 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), 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), 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), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Hélium : du fondamental aux applications (NEEL - HELFA), 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), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Max-Planck-Institut für Gravitationsphysik ( Albert-Einstein-Institut ) (AEI), and Université Joseph Fourier - Grenoble 1 (UJF)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Institut Polytechnique de Grenoble - Grenoble Institute of Technology-Centre National de la Recherche Scientifique (CNRS)
Subjects: [PHYS.ASTR.GA]Physics [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Astrophysics of Galaxies (astro-ph.GA), FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, [SDU.ASTR.GA]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Galactic Astrophysics [astro-ph.GA], Astrophysics - Astrophysics of Galaxies, Astrophysics::Galaxy Astrophysics
Abstract: We present the statistical properties of the first version of the Cold Core Catalogue of Planck Objects (C3PO), in terms of their spatial distribution, temperature, distance, mass, and morphology. We also describe the statistics of the Early Cold Core Catalogue (ECC, delivered with the Early Release Compact Source Catalogue, ERCSC) that is the subset of the 915 most reliable detections of the complete catalogue. We have used the CoCoCoDeT algorithm to extract 10783 cold sources. Temperature and dust emission spectral index {\beta} values are derived using the fluxes in the IRAS 100 \mum band and the three highest frequency Planck bands. Temperature spans from 7K to 17K, and peaks around 13K. Data are not consistent with a constant value of {\beta} over the all temperature range. {\beta} ranges from 1.4 to 2.8 with a mean value around 2.1, and several possible scenarios are possible, including {\beta}(T) and the effect of multiple T components folded into the measurements. For one third of the objects the distances are obtained. Most of the detections are within 2 kpc in the Solar neighbourhood, but a few are at distances greater than 4 kpc. The cores are distributed from the deep Galactic plane, despite the confusion, to high latitudes (>30$^{\circle}$). The associated mass estimates range from 1 to $10^5$ solar masses. Using their physical properties these cold sources are shown to be cold clumps, defined as the intermediate cold sub-structures between clouds and cores. These cold clumps are not isolated but mostly organized in filaments associated with molecular clouds. The Cold Core Catalogue of Planck Objects (C3PO) is the first unbiased all-sky catalogue of cold objects. It gives an unprecedented statistical view to the properties of these potential pre-stellar clumps and offers a unique possibility for their classification in terms of their intrinsic properties and environment., Comment: This paper is part of package of Planck early papers, labelled in their title by "Planck Early results:..." Corresponding Author: L. Montier (Ludovic.Montier@cesr.fr)
Full Text: View/download PDF

9. The Canadian Galactic plane survey

Author: Taylor, A. R., Gibson, S., Leahy, D., Peracaula, M., Dougherty, S., Carignan, C., St-Louis, N., Fich, M., Ghazzali, N., Joncas, G., Pineault, S., Mashchenko, S., Irwin, J., English, J., Heiles, C., Normandeau, M., Martin, P., Johnstone, D., Basu, S., Mccutcheon, W., Routledge, D., Vaneldik, F., Dewdney, P., Galt, J., Gray, A., Higgs, L., Lewis Knee, Landecker, T., Purton, C., Roger, R. S., Tapping, K., Wallace, B., Willis, T., Beichman, C., Duric, N., Green, D., Heyer, M., Wendker, H., and Zhang, Xizhen

10. VizieR Online Data Catalog: JCMT Plane Survey: l=30° field (Moore+, 2015)

Author: Moore, T. J. T., Plume, R., Thompson, M. A., Parsons, H., Urquhart, J. S., Eden, D. J., Dempsey, J. T., Morgan, L. K., Thomas, H. S., Buckle, J., Brunt, C. M., Butner, H., Carretero, D., Chrysostomou, A., Devilliers, H. M., Fich, M., Hoare, M. G., Manser, G., Mottram, J. C., Natario, C., Olguin, F., Peretto, N., Polychroni, D., Redman, R. O., Rigby, A. J., Salji, C., Summers, L. J., Berry, D., Currie, M. J., Jenness, T., Pestalozzi, M., Traficante, A., Bastien, P., Difrancesco, J., Davis, C. J., Evans, A., Friberg, P., Fuller, G. A., Gibb, A. G., Gibson, S., Hill, T., Doug Johnstone, Joncas, G., Longmore, S. N., Lumsden, S. L., Martin, P. G., Nguyen Luong, Q., Pineda, J. E., Purcell, C., Richer, J. S., Schieven, G. H., Shipman, R., Spaans, M., Taylor, A. R., Viti, S., Weferling, B., White, G. J., and Zhu, M.

11. GHIGLS: H I MAPPING AT INTERMEDIATE GALACTIC LATITUDE USING THE GREEN BANK TELESCOPE

Author: Martin, P., Lockman, Felix, Goncalves, D., Boothroyd, A., Joncas, G., Miville-Deschenes, M., Stephan, G., Martin, Peter, Blagrave, K., Miville-Deschênes, M.-A., and Gonçalves, D.
Subjects: Physics, Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Green Bank Telescope, FOS: Physical sciences, Astronomy, Astronomy and Astrophysics, Astrophysics - Astrophysics of Galaxies, Galaxy, Latitude
Abstract: This paper introduces the data cubes from GHIGLS, deep Green Bank Telescope surveys of the 21-cm line emission of HI in 37 targeted fields at intermediate Galactic latitude. The GHIGLS fields together cover over 1000 square degrees at 9.55' spatial resolution. The HI spectra have an effective velocity resolution about 1.0 km/s and cover at least -450 < v < +250 km/s. GHIGLS highlights that even at intermediate Galactic latitude the interstellar medium is very complex. Spatial structure of the HI is quantified through power spectra of maps of the column density, NHI. For our featured representative field, centered on the North Ecliptic Pole, the scaling exponents in power-law representations of the power spectra of NHI maps for low, intermediate, and high velocity gas components (LVC, IVC, and HVC) are -2.86 +/- 0.04, -2.69 +/- 0.04, and -2.59 +/- 0.07, respectively. After Gaussian decomposition of the line profiles, NHI maps were also made corresponding to the narrow-line and broad-line components in the LVC range; for the narrow-line map the exponent is -1.9 +/- 0.1, reflecting more small scale structure in the cold neutral medium (CNM). There is evidence that filamentary structure in the HI CNM is oriented parallel to the Galactic magnetic field. The power spectrum analysis also offers insight into the various contributions to uncertainty in the data. The effect of 21-cm line opacity on the GHIGLS NHI maps is estimated., Accepted for publication in The Astrophysical Journal, 2015 July 16. 32 pages, 21 figures (Fig. 10 new). Minor revisions from review, particularly Section 8 and Appendix C; results unchanged. Additional surveys added and made available; new Appendix B. Added descriptions of available FITS files and links to four illustrative movies on enhanced GHIGLS archive (www.cita.utoronto.ca/GHIGLS/)

12. ASKAP and MeerKAT surveys of the magellanic clouds

Author: Loon, J. Th, Arce, H., Bailey, A., Bains, I., Begum, A., Bekki, K., Bekhti, N. B., Bland-Hawthorn, J., Brooks, K., Brunt, C., Burton, M., Caswell, J., Cunningham, M., Dickey, J., Douglas, K., Ellingsen, S., English, J., Estalella, R., Ford, A., Foster, T., Gaensler, B., Gallagher, J., Gibson, S., Girart, J., Goldsmith, P., Gómez, J. F., Gómez, Y., Green, A., Green, J., Haffner, M., Heiles, C., Heitsch, F., Hennebelle, P., Hirota, T., Hoare, M., Imai, H., Izumiura, H., Joncas, G., Jones, P., Kalberla, P., Kang, J. -H, Kawamura, A., Kerp, J., Kerton, C., Koo, B. -C, Kothes, R., Kurtz, S., Masa Lakicevic, Landecker, T., Lazarian, A., Lo, N., Lockman, F., Magnani, L., Mcclure-Griffiths, N., Menten, K., Migenes, V., Miville-Deschênes, M. -A, Muller, E., Nakagawa, A., Nakanishi, H., Nakashima, J. -I, Nidever, D., Nigra, L., Peek, J., Pérez-Torres, M., Phillips, C., Putman, M., Remijan, A., Richter, P., Schilke, P., Sofue, Y., Stanimirović, S., Tafoya, D., Taylor, R., Tian, W. -W, Uscanga, L., Loon, J., Voronkov, M., Wakker, B., Walsh, A., Westmeier, T., Winkel, B., Zweibel, E., Bagheri, G., Barway, S., Beletsky, Y., Bernard, J. -P, Bietenholz, M., Booth, R., Bot, C., Brinks, E., Cioni, M. -R, Blok, E., Evans, C., Gibson, B., Goedhart, S., Gómez, J., Gordon, K., Haverkorn, M., Holwerda, B., Indebetouw, R., Israel, F., Koribalski, B., Krumholz, M., Lakićević, M., Meixner, M., Oliveira, J., Sarre, P., Sewiło, M., Sibbons, L., Smith, K., Vlemmings, W., Walter, F., Whitelock, P., and Zijlstra, A.
Abstract: The Magellanic Clouds are a stepping stone from the overwhelming detail of the Milky Way in which we are immersed, to the global characteristics of galaxies both in the nearby and distant universe. They are interacting, gas-rich dwarf galaxies of sub-solar metallicity, not unlike the building blocks that assembled the large galaxies that dominate groups and clusters, and representative of the conditions at the height of cosmic star formation. The Square Kilometre Array (SKA) can make huge strides in understanding galactic metabolism and the ecological processes that govern star formation, by observations of the Magellanic Clouds and other, nearby Magellanic-type irregular galaxies. Two programmes with SKA Pathfinders attempt to pave the way: the approved Galactic ASKAP Spectral Line Survey (GASKAP) includes a deep survey in H I and OH of the Magellanic Clouds, whilst MagiKAT is proposed to perform more detailed studies of selected regions within the Magellanic Clouds - also including Faraday rotation measurements and observations at higher frequencies. These surveys also close the gap with the revolutionizing surveys at far-IR wavelengths with the Spitzer Space Telescope and Herschel Space Observatory.

13. VizieR Online Data Catalog: JCMT Gould Belt Survey: Serpens MWC 297 (Rumble+, 2015)

Author: Rumble, D., Hatchell, J., Gutermuth, R. A., Kirk, H., Buckle, J., Beaulieu, S. F., Berry, D. S., Broekhoven-Fiene, H., Currie, M. J., Fich, M., Jenness, T., Johnstone, D., Mottram, J. C., Nutter, D., Pattle, K., Pineda, J. E., Quinn, C., Salji, C., Tisi, S., Walker-Smith, S., Di, Francesco J., Hogerheijde, M. R., Ward-Thompson, D., Allen, L. E., Cieza, L. A., Dunham, M. M., Harvey, P. M., Stapelfeldt, K. R., Bastien, P., Butner, H., Chen, M., Chrysostomou, A., Coude, S., Davis, C. J., Drabek-Maunder, E., Duarte-Cabral, A., Fiege, J., Friberg, P., Friesen, R., Fuller, G. A., Graves, S., Greaves, J., Gregson, J., Holland, W., Joncas, G., Kirk, J. M., Knee, L. B. G., Mairs, S., Marsh, K., Matthews, B. C., Moriarty-Schieven, G., Rawlings, J., Richer, J., Robertson, D., Rosolowsky, E., Sadavoy, S., Holly Thomas, Tothill, N., Viti, S., White, G. J., Wilson, C. D., Wouterloot, J., Yates, J., and Zhu, M.

14. Large SCUBA images of the Rho Ophiuchi and Orion B molecular clouds

Author: Mitchell, G., Avery, L., Knee, L., Matthews, H., Moriarty-Schieven, G., Basu, S., Fiege, J., Matthews, B., Pudritz, R., Wilson, C., Fich, M., Doug Johnstone, and Joncas, G.

15. ISOCAM mapping of the Whirlpool galaxy M 51

Author: Sauvage, M., Blommaert, J., Boulanger, F., Cesarsky, Cj, Cesarsky, Da, Desert, Fx, Elbaz, D., Gallais, P., Joncas, G., Metcalfe, L., Okumura, K., Ott, S., Siebenmorgen, R., Jean-Luc Starck, Tran, D., and Vigroux, L.

16. The SCUBA-2 'All-Sky' Survey

Author: Thompson, M. A., Serjeant, S., Jenness, T., Scott, D., Ashdown, M., Brunt, C., Butner, H., Chapin, E., Chrysostomou, A. C., Clark, J. S., Clements, D., Collett, J. L., Coppin, K., Coulson, I. M., Dent, W. R. F., Economou, F., Evans, A., Friberg, P., Fuller, G. A., Gibb, A. G., Greaves, J., Hatchell, J., Holland, W. S., Mike Hudson, Ivison, R. J., Jaffe, A., Joncas, G., Jones, H. R. A., Knapen, J. H., Leech, J., Mann, R., Matthews, H. E., Moore, T. J. T., Mortier, A., Negrello, M., Nutter, D., Pestalozzi, M. P., Pope, A., Richer, J., Shipman, R., Urquhart, J. S., Vaccari, M., Waerbeke, L., Viti, S., Weferling, B., White, G. J., Wouterloot, J., and Zhu, M.
Subjects: Astrophysics (astro-ph), FOS: Physical sciences, Astrophysics
Abstract: The sub-millimetre wavelength regime is perhaps the most poorly explored over large areas of the sky, despite the considerable effort that has been expended in making deep maps over small regions. As a consequence the properties of the sub-millimetre sky as a whole, and of rare bright objects in particular, remains largely unknown. Here we describe a forthcoming survey (the SCUBA-2 ``All-Sky'' Survey, or SASSy) designed to address this issue by making a large-area map of approximately one-fifth of the sky visible from the JCMT (4800 square degrees) down to a 1 sigma noise level of 30 mJy/beam. This map forms the pilot for a much larger survey, which will potentially map the remaining sky visible from the JCMT, with the region also visible to ALMA as a priority. SASSy has been awarded 500 hours for the 4800 square degree pilot phase and will commence after the commissioning of SCUBA-2, expected in early 2008., 26 pages, 5 figures. In referee's format. Submitted to PASP. Figs 1-3 are missing due to file size constraints. A full version of the paper may be found at http://star-www.herts.ac.uk/~mat/sassy_pasp.pdf Version 2 fixes author list and link to full version of paper

17. The Canadian Galactic Plane Survey - Phase 2

Author: Landecker, T. L., Lewis Knee, Brunt, C., Dewdney, P. E., Dougherty, S. M., Galt, J. A., Gray, A. D., Higgs, L. A., Kothes, R., Purton, C. R., Roger, R. S., Tapping, K., Wallace, B. J., Willis, A. G., Brown, J. C., Gibson, S. J., Leahy, D. A., Peracaula, M., Taylor, A. R., Wilder, S., Foster, T., Routledge, D., Vaneldik, J. F., Mccutcheon, W. H., Basu, S., Johnstone, D. I., Kerton, C., Martin, P. G., Cazzolato, F., Gagnon, E., Germain, S., Ghazzali, N., Godbout, S., Joncas, G., Maschenko, S. Y., Miville-Deschènes, M. -A, Pineault, S., Carignan, C., St-Louis, N., Christie, R. A., Irwin, J. A., Brar, R., Fich, M., Zhang, X. -Z, Heiles, C. E., Normandeau, M., Tereby, S., Heyer, M. H., Wendker, H. J., Beichman, C. A., Moriarty-Schieven, G. H., Green, D. A., Duric, N., and English, J.

18. VizieR Online Data Catalog: JCMT Gould Belt Survey: W40 complex (Rumble+, 2016)

Author: Rumble, D., Hatchell, J., Pattle, K., Kirk, H., Wilson, T., Buckle, J., Berry, D. S., Broekhoven-Fiene, H., Currie, M. J., Fich, M., Jenness, T., Doug Johnstone, Mottram, J. C., Nutter, D., Pineda, J. E., Quinn, C., Salji, C., Tisi, S., Walker-Smith, S., Di, Francesco J., Hogerheijde, M. R., Ward-Thompson, D., Bastien, P., Bresnahan, D., Butner, H., Chen, M., Chrysostomou, A., Coude, S., Davis, C. J., Drabek-Maunder, E., Duarte-Cabral, A., Fiege, J., Friberg, P., Friesen, R., Fuller, G. A., Graves, S., Greaves, J., Gregson, J., Holland, W., Joncas, G., Kirk, J. M., Knee, L. B. G., Mairs, S., Marsh, K., Matthews, B. C., Moriarty-Schieven, G., Mowat, C., Rawlings, J., Richer, J., Robertson, D., Rosolowsky, E., Sadavoy, S., Thomas, H., Tothill, N., Viti, S., White, G. J., Wouterloot, J., Yates, J., and Zhu, M.

19. Clouds, filaments, and protostars: The Herschel Hi-GAL Milky Way

Author: J. A. Rodón, K. Ganga, M. Pomarès, Friedrich Wyrowski, Mika Juvela, F. Piacentini, Melvin Hoare, William T. Reach, Stefano Pezzuto, A. Roy, Jean-Paul Baluteau, Marc-Antoine Miville-Deschenes, Russell H. Taylor, Pierre Royer, Alessio Traficante, Peter Schilke, D. Paradis, Glenn J. White, Cara Battersby, Alberto Noriega-Crespo, Harriet Parsons, M. Veneziani, Dimitrios Stamatellos, Vincent Minier, Lorenzo Piazzo, Guy S. Stringfellow, Michael G. Burton, L. K. Morgan, Frederic Schuller, F. Faustini, P. Saraceno, S. D. Lord, Jason Glenn, E. Sturm, Michael D. Smith, G. Joncas, A. M. di Giorgio, D. Polychroni, L. Montier, D. J. Marshall, N. Billot, José Cernicharo, F. Boulanger, M. T. Beltrán, Paul Martin, Matthew Joseph Griffin, B. Swinyard, Guilaine Lagache, Serena Viti, Mathieu Compiegne, Derek Ward-Thompson, P. de Bernardis, Frédérique Motte, B. Sibthorpe, Sukanya Chakrabarti, Nicolas Flagey, Christopher M. Brunt, Maggie A. Thompson, Qizhou Zhang, J.-P. Bernard, Annie Zavagno, Jean-François Robitaille, L. Spinoglio, Marc Sauvage, D. Russeil, Paolo Natoli, A. Abergel, Babar Ali, Davide Elia, D. Ikhenaode, Gary A. Fuller, C. Joblin, G. de Gasperis, Eugenio Schisano, Pedro García-Lario, Jin-Zeng Li, Isabelle Ristorcelli, Sergio Molinari, Luca Calzoletti, M. R. Pestalozzi, Nicolas Peretto, Thomas P. Robitaille, Mikako Matsuura, Riccardo Cesaroni, Rene Plume, Jan Brand, Paul F. Goldsmith, Leonardo Testi, Joseph C. Mottram, H. W. Yorke, Cristina Popescu, Martin Cohen, M. Benedettini, M. J. Barlow, Antonio Chrysostomou, Paola Caselli, Luca Olmi, Maohai Huang, Massimo Marengo, R. Paladini, Fabrizio Massi, L. A. Wilcock, Grazia Umana, Francesco Strafella, Toby J. T. Moore, Benjamin L. Schulz, R. Vavrek, T. Mueller, John Bally, J. A. D. L. Blommaert, L. D. Anderson, C. Waelkens, T. L. Lim, Richard J. Tuffs, Sean Carey, Yasuo Fukui, J. Neves, Nicola Schneider, Jason M. Kirk, Silvia Masi, Pascal André, Howard A. Smith, Luca Valenziano, Sylvain Bontemps, Istituto di Fisica dello Spazio Interplanetario (IFSI), National Research Council of Italy | Consiglio Nazionale delle Ricerche (CNR), Centre d'étude spatiale des rayonnements (CESR), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut d'astrophysique spatiale (IAS), Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), CITA, University of Toronto, European Southern Observatory (ESO), Laboratoire d'Astrophysique de Marseille (LAM), Aix Marseille Université (AMU)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS), Observatoire Astronomique de Marseille Provence (OAMP), Université de Provence - Aix-Marseille 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Laboratory of Comparative Carcinogenesis (LABORATORY OF COMPARATIVE CARCINOGENESIS), National Cancer Institute [Bethesda] (NCI-NIH), National Institutes of Health [Bethesda] (NIH)-National Institutes of Health [Bethesda] (NIH), Laboratoire d'Informatique de Nantes Atlantique (LINA), Mines Nantes (Mines Nantes)-Université de Nantes (UN)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Grenoble (LAOG), Université Joseph Fourier - 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Osservatorio Astrofisico di Arcetri (OAA), Istituto Nazionale di Astrofisica (INAF), Centro de Investigaciones Biológicas (CSIC), Consejo Superior de Investigaciones Científicas [Madrid] (CSIC), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, APC - Cosmologie, AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-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), ISO Data Centre (ESA - Espagne), Agence Spatiale Européenne = European Space Agency (ESA), Herschel Science Centre (ESA Espagne), National Astronomical Observatories [Beijing] (NAOC), Chinese Academy of Sciences [Beijing] (CAS), STFC Rutherford Appleton Laboratory (RAL), Science and Technology Facilities Council (STFC), Universiti Brunei Darussalam, Biology Department, Universitii Brunei Darussalam, Università degli Studi di Roma Tor Vergata [Roma], University of Manchester [Manchester], Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Tenovus Centre for Cancer Research, Welsh School of Pharmacy, Antarctic Research a European Network for Astrophysics (ARENA), Commissariat à l'énergie atomique et aux énergies alternatives (CEA), Inter University Accelerator Centre, Aruna Asaf Ali Marg, LEOSPHERE France, LEOSPHERE, Max-Planck-Institut für Radioastronomie (MPIFR), Laboratoire de Radioastronomie (LRA), Fédération de recherche du Département de physique de l'Ecole Normale Supérieure - ENS Paris (FRDPENS), École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS-PSL), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Royal Observatory Edinburgh (ROE), University of Edinburgh, Atmospheric Sciences Division [Hampton], NASA Langley Research Center [Hampton] (LaRC), School of Physics and Astronomy [Cardiff], Cardiff University, Shanghai Inst Opt & Fine Mech, Key Lab Mat Sci & Technol High Power Lasers, Molinari, S., Swinyard, B., Bally, J., Barlow, M., Bernard, J. P., Martin, P., Moore, T., Noriega Crespo, A., Plume, R., Testi, L., Zavagno, A., Abergel, A., Ali, B., Anderson, L., Andre, P., Baluteau, J. P., Battersby, C., Beltrán, M. T., Benedettini, M., Billot, N., Blommaert, J., Bontemps, S., Boulanger, F., Brand, J., Brunt, C., Burton, M., Calzoletti, L., Carey, S., Caselli, P., Cesaroni, R., Cernicharo, J., Chakrabarti, S., Chrysostomou, A., Cohen, M., Compiegne, M., de Bernardis, P., de Gasperis, G., di Giorgio, A. M., Elia, Davide Quintino, Faustini, F., Flagey, N., Fukui, Y., Fuller, G. A., Ganga, K., Garcia Lario, P., Glenn, J., Goldsmith, P. F., Griffin, M., Hoare, M., Huang, M., Ikhenaode, D., Joblin, C., Joncas, G., Juvela, M., Kirk, J. M., Lagache, G., Li, J. Z., Lim, T. L., Lord, S. D., Marengo, M., Marshall, D. J., Masi, S., Massi, F., Matsuura, M., Minier, V., Miville Deschênes, M. A., Montier, L. A., Morgan, L., Motte, F., Mottram, J. C., Müller, T. G., Natoli, P., Neves, J., Olmi, L., Paladini, R., Paradis, D., Parsons, H., Peretto, N., Pestalozzi, M., Pezzuto, S., Piacentini, F., Piazzo, L., Polychroni, D., Pomarès, M., Popescu, C. C., Reach, W. T., Ristorcelli, I., Robitaille, J. F., Robitaille, T., Rodón, J. A., Roy, A., Royer, P., Russeil, D., Saraceno, P., Sauvage, M., Schilke, P., Schisano, E., Schneider, N., Schuller, F., Schulz, B., Sibthorpe, B., Smith, H. A., Smith, M. D., Spinoglio, L., Stamatellos, D., Strafella, Francesco, Stringfellow, G. S., Sturm, E., Taylor, R., Thompson, M. A., Traficante, A., Tuffs, R. J., Umana, G., Valenziano, L., Vavrek, R., Veneziani, M., Viti, S., Waelkens, C., Ward Thompson, D., White, G., Wilcock, L. A., Wyrowski, F., Yorke, H. W., Zhang, Q., Consiglio Nazionale delle Ricerche (CNR), Observatoire Midi-Pyrénées (OMP), 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)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées, Université Paris-Sud - Paris 11 (UP11)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), 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), Centre National de la Recherche Scientifique (CNRS)-Mines Nantes (Mines Nantes)-Université de Nantes (UN), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Observatoire aquitain des sciences de l'univers (OASU), Université Sciences et Technologies - Bordeaux 1-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Centre National de la Recherche Scientifique (CNRS)-Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), 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), European Space Agency (ESA), Dipartimento di Fisica, Universita` di Roma Tor Vergata, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Consejo Superior de Investigaciones Científicas [Spain] (CSIC), Physique Corpusculaire et Cosmologie - Collège de France (PCC), Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Collège de France (CdF)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-AstroParticule et Cosmologie (APC (UMR_7164)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire des Sciences du Climat et de l'Environnement [Gif-sur-Yvette] (LSCE), Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université de Versailles Saint-Quentin-en-Yvelines (UVSQ)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris)-Centre National de la Recherche Scientifique (CNRS)-École normale supérieure - Paris (ENS Paris), ITA, USA, GBR, FRA, DEU, and ESP
Subjects: 010504 meteorology & atmospheric sciences, Field (physics), Milky Way, stars: formation, ISM: structure, ISM: clouds, Galaxy: general, FOS: Physical sciences, ism: structure, ism: clouds, galaxy: general, Astrophysics, 01 natural sciences, Protein filament, Settore FIS/05 - Astronomia e Astrofisica, 0103 physical sciences, Protostar, Infrared dark cloud, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Physics, [SDU.ASTR.SR]Sciences of the Universe [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astronomy and Astrophysics, Galactic plane, [PHYS.ASTR.SR]Physics [physics]/Astrophysics [astro-ph]/Solar and Stellar Astrophysics [astro-ph.SR], Astrophysics - Astrophysics of Galaxies, Core (optical fiber), Space and Planetary Science, Astrophysics of Galaxies (astro-ph.GA), Magnetohydrodynamics
Abstract: We present the first results from the science demonstration phase for the Hi-GAL survey, the Herschel key-project that will map the inner Galactic Plane of the Milky Way in 5 bands. We outline our data reduction strategy and present some science highlights on the two observed 2{\deg} x 2{\deg} tiles approximately centered at l=30{\deg} and l=59{\deg}. The two regions are extremely rich in intense and highly structured extended emission which shows a widespread organization in filaments. Source SEDs can be built for hundreds of objects in the two fields, and physical parameters can be extracted, for a good fraction of them where the distance could be estimated. The compact sources (which we will call 'cores' in the following) are found for the most part to be associated with the filaments, and the relationship to the local beam-averaged column density of the filament itself shows that a core seems to appear when a threshold around A_V of about 1 is exceeded for the regions in the l=59{\deg} field; a A_V value between 5 and 10 is found for the l=30{\deg} field, likely due to the relatively larger distances of the sources. This outlines an exciting scenario where diffuse clouds first collapse into filaments, which later fragment to cores where the column density has reached a critical level. In spite of core L/M ratios being well in excess of a few for many sources, we find core surface densities between 0.03 and 0.5 g cm-2. Our results are in good agreement with recent MHD numerical simulations of filaments forming from large-scale converging flows., Comment: A&A, accepted
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20. Direct estimate of cirrus noise in Herschel Hi-GAL images

Author: Christopher M. Brunt, Marc-Antoine Miville-Deschênes, Francesco Strafella, Alberto Noriega-Crespo, Jean-François Robitaille, Sergio Molinari, Peter G. Martin, A. M. DiGiorgio, M. Veneziani, Paolo Natoli, Davide Elia, A. Roy, F. Faustini, G. Joncas, Joseph C. Mottram, L. Calzoletti, Roberta Paladini, J.-P. Bernard, N. Billot, Alessio Traficante, Martin, P. G., Miville Deschênes, M. A., Roy, A., Bernard, J. P., Molinari, S., Billot, N., Brunt, C., Calzoletti, L., Di Giorgio, A. M., Elia, Davide Quintino, Faustini, F., Joncas, G., Mottram, J. C., Natoli, P., Noriega Crespo, A., Paladini, R., Robitaille, J. F., Strafella, Francesco, Traficante, A., and Veneziani, M.
Subjects: Physics, Brightness, Astrophysics::High Energy Astrophysical Phenomena, Spectral density, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galactic plane, Astrophysics - Astrophysics of Galaxies, submillimetrico [protostelle], formazione stellare, infrarosso [mezzo interstellare], Amplitude, Space and Planetary Science, struttura [mezzo interstellare], Astrophysics of Galaxies (astro-ph.GA), Spectral energy distribution, Cirrus, Surface brightness, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM), Noise (radio), Astrophysics::Galaxy Astrophysics
Abstract: In Herschel images of the Galactic plane and many star forming regions, a major factor limiting our ability to extract faint compact sources is cirrus confusion noise, operationally defined as the "statistical error to be expected in photometric measurements due to confusion in a background of fluctuating surface brightness". The histogram of the flux densities of extracted sources shows a distinctive faint-end cutoff below which the catalog suffers from incompleteness and the flux densities become unreliable. This empirical cutoff should be closely related to the estimated cirrus noise and we show that this is the case. We compute the cirrus noise directly, both on Herschel images from which the bright sources have been removed and on simulated images of cirrus with statistically similar fluctuations. We connect these direct estimates with those from power spectrum analysis, which has been used extensively to predict the cirrus noise and provides insight into how it depends on various statistical properties and photometric operational parameters. We report multi-wavelength power spectra of diffuse Galactic dust emission from Hi-GAL observations at 70 to 500 microns within Galactic plane fields at l= 30 degrees and l= 59 degrees. We find that the exponent of the power spectrum is about -3. At 250 microns, the amplitude of the power spectrum increases roughly as the square of the median brightness of the map and so the expected cirrus noise scales linearly with the median brightness. Generally, the confusion noise will be a worse problem at longer wavelengths, because of the combination of lower angular resolution and the rising power spectrum of cirrus toward lower spatial frequencies, but the photometric signal to noise will also depend on the relative spectral energy distribution of the source compared to the cirrus., Comment: 4 pages (in journal), 3 figures, Astronomy and Astrophysics, accepted for publication 13 May 2010

21. [Post-encephalitic sequels in a congenital syphilitic].

Author: JONCAS G and DAGENAIS-PERUSSE P
Subjects: Humans, Encephalitis, Syphilis, Syphilis, Congenital
Published: 1951

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21 results on '"Joncas, G."'

1. Properties of Hi-GAL clumps in the inner Galaxy]{The Hi-GAL compact source catalogue. I. The physical properties of the clumps in the inner Galaxy ($-71.0^{\circ}< \ell < 67.0^{\circ}$)

2. Hi-GAL, the Herschel infrared Galactic Plane Survey: photometric maps and compact source catalogues. First data release for Inner Milky Way: +68��> l > -70��

3. Planck 2013 results. XI. All-sky model of thermal dust emission

4. Planck intermediate results: XVII. Emission of dust in the diffuse interstellar medium from the far-infrared to microwave frequencies

5. The Canadian Galactic Plane Survey

6. Physical conditions of star forming sites in the S247/252 molecular complex

7. VizieR Online Data Catalog: JCMT Gould Belt Survey: dense cores in Orion B (Kirk+, 2016)

8. Planck Early Results: The Galactic Cold Core Population revealed by the first all-sky survey

9. The Canadian Galactic plane survey

10. VizieR Online Data Catalog: JCMT Plane Survey: l=30° field (Moore+, 2015)

11. GHIGLS: H I MAPPING AT INTERMEDIATE GALACTIC LATITUDE USING THE GREEN BANK TELESCOPE

12. ASKAP and MeerKAT surveys of the magellanic clouds

13. VizieR Online Data Catalog: JCMT Gould Belt Survey: Serpens MWC 297 (Rumble+, 2015)

14. Large SCUBA images of the Rho Ophiuchi and Orion B molecular clouds

15. ISOCAM mapping of the Whirlpool galaxy M 51

16. The SCUBA-2 'All-Sky' Survey

17. The Canadian Galactic Plane Survey - Phase 2

18. VizieR Online Data Catalog: JCMT Gould Belt Survey: W40 complex (Rumble+, 2016)

19. Clouds, filaments, and protostars: The Herschel Hi-GAL Milky Way

20. Direct estimate of cirrus noise in Herschel Hi-GAL images

21. [Post-encephalitic sequels in a congenital syphilitic].

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