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1. Planck Intermediate Results. IX. Detection of the Galactic haze with Planck

Author: Planck Collaboration, Ade, P. A. R., Aghanim, N., Arnaud, M., Ashdown, M., Atrio-Barandela, F., 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., Bonaldi, A., Bond, J. R., Borrill, J., Bouchet, F. R., Burigana, C., Cabella, P., Cardoso, J. -F., Catalano, A., Cayón, L., Chary, R. -R., Chiang, L. -Y, Christensen, P. R., Clements, D. L., Colombo, L. P. L., Coulais, A., Crill, B. P., Cuttaia, F., Danese, L., D'Arcangelo, O., Davis, R. J., de Bernardis, P., de Gasperis, G., de Rosa, A., de Zotti, G., Delabrouille, J., Dickinson, C., Diego, J. M., Dobler, G., Dole, H., Donzelli, S., Doré, O., Dörl, U., Douspis, M., Dupac, X., Efstathiou, G., Enßlin, T. A., Eriksen, H. K., Finelli, F., Forni, O., Frailis, M., Franceschi, E., Galeotta, S., Ganga, K., Giard, M., Giardino, G., González-Nuevo, J., Górski, K. M., Gratton, S., Gregorio, A., Gruppuso, A., Hansen, F. K., Harrison, D., Helou, G., Henrot-Versillé, S., Hernández-Monteagudo, C., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hornstrup, A., Hovest, W., Huffenberger, K. M., Jaffe, T. R., Jagemann, T., Jones, W. C., Juvela, M., Keihänen, E., Knoche, J., Knox, L., Kunz, M., Kurki-Suonio, H., Lagache, G., Lähteenmäki, A., Lamarre, J. -M., Lasenby, A., Lawrence, C. R., Leach, S., Leonardi, R., Lilje, P. B., Linden-Vørnle, M., López-Caniego, M., Lubin, P. M., Macías-Pérez, J. F., Maffei, B., Maino, D., Mandolesi, N., Maris, M., Martin, P. G., Martínez-González, E., Masi, S., Massardi, M., Matarrese, S., Matthai, F., Mazzotta, P., Meinhold, P. R., Melchiorri, A., Mendes, L., Mennella, A., Mitra, S., Miville-Deschênes, M. -A., Moneti, A., Montier, L., Morgante, G., Munshi, D., Murphy, J. A., Naselsky, P., Natoli, P., Nørgaard-Nielsen, H. U., Noviello, F., Osborne, S., Pajot, F., Paladini, R., Paoletti, D., Partridge, B., Pearson, T. J., Perdereau, O., 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., Prunet, S., Puget, J. -L., Rachen, J. P., Rebolo, R., Reinecke, M., Renault, C., Ricciardi, S., Riller, T., Rocha, G., Rosset, C., Rubiño-Martín, J. A., Rusholme, B., Sandri, M., Savini, G., Schaefer, B. M., Scott, D., Smoot, G. F., Stivoli, F., Sudiwala, R., Suur-Uski, A. -S., Sygnet, J. -F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Türler, M., Umana, G., Valenziano, L., Van Tent, B., Vielva, P., Villa, F., Vittorio, N., Wade, L. A., Wandelt, B. D., White, M., Yvon, D., Zacchei, A., and Zonca, A.
Subjects: Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Using precise full-sky observations from Planck, and applying several methods of component separation, we identify and characterize the emission from the Galactic "haze" at microwave wavelengths. The haze is a distinct component of diffuse Galactic emission, roughly centered on the Galactic centre, and extends to |b| ~35 deg in Galactic latitude and |l| ~15 deg in longitude. By combining the Planck data with observations from the WMAP we are able to determine the spectrum of this emission to high accuracy, unhindered by the large systematic biases present in previous analyses. The derived spectrum is consistent with power-law emission with a spectral index of -2.55 +/- 0.05, thus excluding free-free emission as the source and instead favouring hard-spectrum synchrotron radiation from an electron population with a spectrum (number density per energy) dN/dE ~ E^-2.1. At Galactic latitudes |b|<30 deg, the microwave haze morphology is consistent with that of the Fermi gamma-ray "haze" or "bubbles," indicating that we have a multi-wavelength view of a distinct component of our Galaxy. Given both the very hard spectrum and the extended nature of the emission, it is highly unlikely that the haze electrons result from supernova shocks in the Galactic disk. Instead, a new mechanism for cosmic-ray acceleration in the centre of our Galaxy is implied., Comment: 15 pages, 9 figures, submitted to Astronomy and Astrophysics
Published: 2012
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2. Planck intermediate results. X. Physics of the hot gas in the Coma cluster

Author: Planck Collaboration, Ade, P. A. R., Aghanim, N., Arnaud, M., Ashdown, M., Atrio-Barandela, F., 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., Bikmaev, I., Böhringer, H., Bonaldi, A., Bond, J. R., Borrill, J., Bouchet, F. R., Bourdin, H., Brown, M. L., Brown, S. D., Burenin, R., Burigana, C., Cabella, P., Cardoso, J. -F., Carvalho, P., Catalano, A., Cayón, L., Chiang, L. -Y, Chon, G., Christensen, P. R., Churazov, E., Clements, D. L., Colafrancesco, S., Colombo, L. P. L., Coulais, A., Crill, B. P., Cuttaia, F., Da Silva, A., Dahle, H., Danese, L., Davis, R. J., de Bernardis, P., de Gasperis, G., de Rosa, A., de Zotti, G., Delabrouille, J., Démoclès, J., Désert, F. -X., Dickinson, C., Diego, J. M., Dolag, K., Dole, H., Donzelli, S., Doré, O., Dörl, U., Douspis, M., Dupac, X., Enßlin, T. A., Eriksen, H. K., Finelli, F., Flores-Cacho, I., Forni, O., Frailis, M., Franceschi, E., Frommert, M., Galeotta, S., Ganga, K., Génova-Santos, R. T., Giard, M., Gilfanov, M., González-Nuevo, J., Górski, K. M., Gregorio, A., Gruppuso, A., Hansen, F. K., Harrison, D., Henrot-Versillé, S., Hernández-Monteagudo, C., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hornstrup, A., Hovest, W., Huffenberger, K. M., Hurier, G., Jaffe, T. R., Jagemann, T., Jones, W. C., Juvela, M., Keihänen, E., Khamitov, I., Kneissl, R., Knoche, J., Knox, L., Kunz, M., Kurki-Suonio, H., Lagache, G., Lähteenmäki, A., Lamarre, J. -M., Lasenby, A., Lawrence, C. R., Jeune, M. Le, Leonardi, R., Lilje, P. B., Linden-Vørnle, M., López-Caniego, M., Lubin, P. M., Macías-Pérez, J. F., Maffei, B., Maino, D., Mandolesi, N., Maris, M., Marleau, F., Martínez-González, E., Masi, S., Massardi, M., Matarrese, S., Matthai, F., Mazzotta, P., Mei, S., Melchiorri, A., Melin, J. -B., Mendes, L., Mennella, A., Mitra, S., Miville-Deschênes, M. -A., Moneti, A., Montier, L., Morgante, G., Munshi, D., Murphy, J. A., Naselsky, P., Natoli, P., Nørgaard-Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., Osborne, S., Pajot, F., Paoletti, D., Perdereau, O., Perrotta, F., Piacentini, F., Piat, M., Pierpaoli, E., Piffaretti, R., Plaszczynski, S., Pointecouteau, E., Polenta, G., Ponthieu, N., Popa, L., Poutanen, T., Pratt, G. W., Prunet, S., Puget, J. -L., Rachen, J. P., Rebolo, R., Reinecke, M., Remazeilles, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Roman, M., Rosset, C., Rossetti, M., Rubiño-Martín, J. A., Rudnick, L., Rusholme, B., Sandri, M., Savini, G., Schaefer, B. M., Scott, D., Smoot, G. F., Stivoli, F., Sudiwala, R., Sunyaev, R., Sutton, D., Suur-Uski, A. -S., Sygnet, J. -F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tuovinen, J., Türler, M., Umana, G., Valenziano, L., Van Tent, B., Varis, J., Vielva, P., Villa, F., Vittorio, N., Wade, L. A., Wandelt, B. D., Welikala, N., White, S. D. M., Yvon, D., Zacchei, A., Zaroubi, S., and Zonca, A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present an analysis of Planck satellite data on the Coma Cluster observed via the Sunyaev-Zeldovich effect. Planck is able, for the first time, to detect SZ emission up to r ~ 3 X R_500. We test previously proposed models for the pressure distribution in clusters against the azimuthally averaged data. We find that the Arnaud et al. universal pressure profile does not fit Coma, and that their pressure profile for merging systems provides a good fit of the data only at rR_500 than the mean pressure profile predicted by the simulations. The Planck image shows significant local steepening of the y profile in two regions about half a degree to the west and to the south-east of the cluster centre. These features are consistent with the presence of shock fronts at these radii, and indeed the western feature was previously noticed in the ROSAT PSPC mosaic as well as in the radio. Using Planck y profiles extracted from corresponding sectors we find pressure jumps of 4.5+0.4-0.2 and 5.0+1.3-0.1 in the west and southeast, respectively. Assuming Rankine-Hugoniot pressure jump conditions, we deduce that the shock waves should propagate with Mach number M_w=2.03+0.09-0.04 and M_se=2.05+0.25-0.02 in the West and Southeast, respectively. Finally, we find that the y and radio-synchrotron signals are quasi-linearly correlated on Mpc scales with small intrinsic scatter. This implies either that the energy density of cosmic-ray electrons is relatively constant throughout the cluster, or that the magnetic fields fall off much more slowly with radius than previously thought., Comment: 20 pages, 18 figure, accepted by A&A, replaced to match published version
Published: 2012
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3. Planck Intermediate Results. IV. The XMM-Newton validation programme for new Planck galaxy clusters

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., Bikmaev, I., Böhringer, H., Bonaldi, A., Bond, J. R., Borgani, S., Borrill, J., Bouchet, F. R., Brown, M. L., Burigana, C., Butler, R. C., Cabella, P., Carvalho, P., Catalano, A., Cayón, L., Chamballu, A., Chary, R. -R., Chiang, L. -Y, Chon, G., Christensen, P. R., Clements, D. L., Colafrancesco, S., Colombi, S., Coulais, A., Crill, B. P., Cuttaia, F., Da Silva, A., Dahle, H., Davis, R. J., de Bernardis, P., de Gasperis, G., de Zotti, G., Delabrouille, J., Démoclès, J., Désert, F. -X., Diego, J. M., Dolag, K., Dole, H., Donzelli, S., Doré, O., Douspis, M., Dupac, X., Enßlin, T. A., Eriksen, H. K., Finelli, F., Flores-Cacho, I., Forni, O., Frailis, M., Franceschi, E., Frommert, M., Galeotta, S., Ganga, K., Génova-Santos, R. T., Giraud-Héraud, Y., González-Nuevo, J., González-Riestra, R., Górski, K. M., Gregorio, A., Gruppuso, A., Hansen, F. K., Harrison, D., Hempel, A., 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., Hurier, G., Jaffe, A. H., Jagemann, T., Jones, W. C., Juvela, M., Kneissl, R., Knoche, J., Knox, L., Kunz, M., Kurki-Suonio, H., Lagache, G., Lamarre, J. -M., Lasenby, A., Lawrence, C. R., Jeune, M. Le, Leach, S., Leonardi, R., Liddle, A., Lilje, P. B., Linden-Vørnle, M., López-Caniego, M., Luzzi, G., Macías-Pérez, J. F., Maino, D., Mandolesi, N., Mann, R., Maris, M., Marleau, F., Marshall, D. J., Martínez-González, E., Masi, S., Massardi, M., Matarrese, S., Mazzotta, P., Mei, S., Meinhold, P. R., Melchiorri, A., Melin, J. -B., Mendes, L., Mennella, A., Mitra, S., Miville-Deschênes, M. -A., Moneti, A., Morgante, G., Mortlock, D., Munshi, D., Naselsky, P., Nati, F., Natoli, P., Nørgaard-Nielsen, H. U., Noviello, F., Osborne, S., Pajot, F., Paoletti, D., Perdereau, O., Perrotta, F., Piacentini, F., Piat, M., Pierpaoli, E., Piffaretti, R., Plaszczynski, S., Platania, P., Pointecouteau, E., Polenta, G., Popa, L., Poutanen, T., Pratt, G. W., Prunet, S., Puget, J. -L., Reinecke, M., Remazeilles, M., Renault, C., Ricciardi, S., Rocha, G., Rosset, C., Rossetti, M., Rubiño-Martín, J. A., Rusholme, B., Sandri, M., Savini, G., Scott, D., Smoot, G. F., Stanford, A., Stivoli, F., Sudiwala, R., Sunyaev, R., Sutton, D., Suur-Uski, A. -S., Sygnet, J. -F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Valenziano, L., Van Tent, B., Vielva, P., Villa, F., Vittorio, N., Wade, L. A., Wandelt, B. D., Welikala, N., Weller, J., White, S. D. M., Yvon, D., Zacchei, A., and Zonca, A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present the final results from the XMM-Newton validation follow-up of new Planck galaxy cluster candidates. We observed 15 new candidates, detected with signal-to-noise ratios between 4.0 and 6.1 in the 15.5-month nominal Planck survey. The candidates were selected using ancillary data flags derived from the ROSAT All Sky Survey (RASS) and Digitized Sky Survey all-sky maps, with the aim of pushing into the low SZ flux, high-z regime and testing RASS flags as indicators of candidate reliability. 14 new clusters were detected by XMM, including 2 double systems. Redshifts lie in the range 0.2 to 0.9, with 6 clusters at z>0.5. Estimated M500 range from 2.5 10^14 to 8 10^14 Msun. We discuss our results in the context of the full XMM validation programme, in which 51 new clusters have been detected. This includes 4 double and 2 triple systems, some of which are chance projections on the sky of clusters at different z. We find that association with a RASS-BSC source is a robust indicator of the reliability of a candidate, whereas association with a FSC source does not guarantee that the SZ candidate is a bona fide cluster. Nevertheless, most Planck clusters appear in RASS maps, with a significance greater than 2 sigma being a good indication that the candidate is a real cluster. The full sample gives a Planck sensitivity threshold of Y500 ~ 4 10^-4 arcmin^2, with indication for Malmquist bias in the YX-Y500 relation below this level. The corresponding mass threshold depends on z. Systems with M500 > 5 10^14 Msun at z > 0.5 are easily detectable with Planck. The newly-detected clusters follow the YX-Y500 relation derived from X-ray selected samples. Compared to X-ray selected clusters, the new SZ clusters have a lower X-ray luminosity on average for their mass. There is no indication of departure from standard self-similar evolution in the X-ray versus SZ scaling properties. (abridged), Comment: accepted by A&A
Published: 2012
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4. Planck intermediate results. III. The relation between galaxy cluster mass and Sunyaev-Zeldovich signal

Author: Planck Collaboration, Ade, P. A. R., Aghanim, N., Arnaud, M., Ashdown, M., Atrio-Barandela, F., Aumont, J., Baccigalupi, C., Balbi, A., Banday, A. J., Barreiro, R. B., Bartlett, J. G., Battaner, E., Battye, R., Benabed, K., Bernard, J. -P., Bersanelli, M., Bhatia, R., Bikmaev, I., Böhringer, H., Bonaldi, A., Bond, J. R., Borgani, S., Borrill, J., Bouchet, F. R., Bourdin, H., Brown, M. L., Bucher, M., Burenin, R., Burigana, C., Butler, R. C., Cabella, P., Cardoso, J. -F., Carvalho, P., Chamballu, A., Chiang, L. -Y, Chon, G., Clements, D. L., Colafrancesco, S., Coulais, A., Cuttaia, F., Da Silva, A., Dahle, H., Davis, R. J., de Bernardis, P., de Gasperis, G., Delabrouille, J., Démoclès, J., Désert, F. -X., Diego, J. M., Dolag, K., Dole, H., Donzelli, S., Doré, O., Douspis, M., Dupac, X., Efstathiou, G., Enßlin, T. A., Eriksen, H. K., Finelli, F., Flores-Cacho, I., Forni, O., Frailis, M., Franceschi, E., Frommert, M., Galeotta, S., Ganga, K., Génova-Santos, R. T., Giard, M., Giraud-Héraud, Y., González-Nuevo, J., Górski, K. M., Gregorio, A., Gruppuso, A., Hansen, F. K., Harrison, D., Hernández-Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Huffenberger, K. M., Hurier, G., Jagemann, T., Juvela, M., Keihänen, E., Khamitov, I., Kneissl, R., Knoche, J., Kunz, M., Kurki-Suonio, H., Lagache, G., Lamarre, J. -M., Lasenby, A., Lawrence, C. R., Jeune, M. Le, Leach, S., Leonardi, R., Liddle, A., Lilje, P. B., Linden-Vørnle, M., López-Caniego, M., Luzzi, G., Macías-Pérez, J. F., Maino, D., Mandolesi, N., Maris, M., Marleau, F., Marshall, D. J., Martínez-González, E., Masi, S., Matarrese, S., Matthai, F., Mazzotta, P., Meinhold, P. R., Melchiorri, A., Melin, J. -B., Mendes, L., Mitra, S., Miville-Deschênes, M. -A., Montier, L., Morgante, G., Munshi, D., Natoli, P., Nørgaard-Nielsen, H. U., Noviello, F., Osborne, S., Pajot, F., Paoletti, D., Partridge, B., Pearson, T. J., Perdereau, O., Perrotta, F., Piacentini, F., Piat, M., Pierpaoli, E., Piffaretti, R., Platania, P., Pointecouteau, E., Polenta, G., Ponthieu, N., Popa, L., Poutanen, T., Pratt, G. W., Prunet, S., Puget, J. -L., Rachen, J. P., Rebolo, R., Reinecke, M., Remazeilles, M., Renault, C., Ricciardi, S., Ristorcelli, I., Rocha, G., Rosset, C., Rossetti, M., Rubiño-Martín, J. A., Rusholme, B., Sandri, M., Savini, G., Scott, D., Starck, J. -L., Stivoli, F., 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., Valenziano, L., Van Tent, B., Vielva, P., Villa, F., Vittorio, N., Wandelt, B. D., Weller, J., White, S. D. M., Yvon, D., Zacchei, A., and Zonca, A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We examine the relation between the galaxy cluster mass M and Sunyaev-Zeldovich (SZ) effect signal D_A^2 Y for a sample of 19 objects for which weak lensing (WL) mass measurements obtained from Subaru Telescope data are available in the literature. Hydrostatic X-ray masses are derived from XMM-Newton archive data and the SZ effect signal is measured from Planck all-sky survey data. We find an M_WL-D_A^2 Y relation that is consistent in slope and normalisation with previous determinations using weak lensing masses; however, there is a normalisation offset with respect to previous measures based on hydrostatic X-ray mass-proxy relations. We verify that our SZ effect measurements are in excellent agreement with previous determinations from Planck data. For the present sample, the hydrostatic X-ray masses at R_500 are on average ~ 20 per cent larger than the corresponding weak lensing masses, at odds with expectations. We show that the mass discrepancy is driven by a difference in mass concentration as measured by the two methods, and, for the present sample, the mass discrepancy and difference in mass concentration is especially large for disturbed systems. The mass discrepancy is also linked to the offset in centres used by the X-ray and weak lensing analyses, which again is most important in disturbed systems. We outline several approaches that are needed to help achieve convergence in cluster mass measurement with X-ray and weak lensing observations., Comment: 19 pages, 9 figures, matches accepted version
Published: 2012
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5. Planck Intermediate Results II: Comparison of Sunyaev-Zeldovich measurements from Planck and from the Arcminute Microkelvin Imager for 11 galaxy clusters

Author: Planck, Collaborations, AMI, Aghanim, N., Arnaud, M., Ashdown, M., Aumont, J., Baccigalupi, C., Balbi, A., Banday, A. J., Barreiro, R. B., Battaner, E., Battye, R., Benabed, K., Benoît, A., Bernard, J. -P., Bersanelli, M., Bhatia, R., Bikmaev, I., Böhringer, H., Bonaldi, A., Bond, J. R., Borrill, J., Bouchet, F. R., Bourdin, H., Brown, M. L., Bucher, M., Burenin, R., Burigana, C., Butler, R. C., Cabella, P., Carvalho, P., Catalano, A., Cayón, L., Chamballu, A., Chary, R. -R., Chiang, L. -Y, Chon, G., Clements, D. L., Colafrancesco, S., Colombi, S., Crill, B. P., Cuttaia, F., Da Silva, A., Dahle, H., Davies, R. D., Davis, R. J., de Bernardis, P., de Gasperis, G., de Rosa, A., de Zotti, G., Delabrouille, J., Démoclès, J., Dickinson, C., Diego, J. M., Dolag, K., Dole, H., Donzelli, S., Doré, O., Douspis, M., Dupac, X., Enßlin, T. A., Eriksen, H. K., Feroz, F., Finelli, F., Flores-Cacho, I., Forni, O., Fosalba, P., Frailis, M., Franceschi, E., Fromenteau, S., Galeotta, S., Ganga, K., Génova-Santos, R. T., Giard, M., Giraud-Héraud, Y., González-Nuevo, J., Górski, K. M., Grainge, K. J. B., Gregorio, A., Gruppuso, A., Hansen, F. K., Harrison, D., Henrot-Versillé, S., Hernández-Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Huffenberger, K. M., Hurier, G., Hurley-Walker, N., Jagemann, T., Juvela, M., Keihänen, E., Khamitov, I., Kneissl, R., Knoche, J., Kunz, M., Kurki-Suonio, H., Lagache, G., Lamarre, J. -M., Lasenby, A., Lawrence, C. R., Jeune, M. Le, Leach, S., Leonardi, R., Liddle, A., Lilje, P. B., Linden-Vørnle, M., López-Caniego, M., Luzzi, G., Macías-Pérez, J. F., MacTavish, C. J., Maino, D., Mandolesi, N., Maris, M., Marleau, F., Marshall, D. J., Martínez-González, E., Masi, S., Massardi, M., Matarrese, S., Matthai, F., Mazzotta, P., Melchiorri, A., Melin, J. -B., Mendes, L., Mennella, A., Mitra, S., Miville-Deschênes, M. -A., Montier, L., Morgante, G., Munshi, D., Naselsky, P., Natoli, P., Noviello, F., Olamaie, M., Osborne, S., Pajot, F., Paoletti, D., Pasian, F., Patanchon, G., Pearson, T. J., Perdereau, O., Perrott, Y. C., Perrotta, F., Piacentini, F., Pierpaoli, E., Platania, P., Pointecouteau, E., Polenta, G., Popa, L., Poutanen, T., Pratt, G. W., Puget, J. -L., Rachen, J. P., Rebolo, R., Reinecke, M., Remazeilles, M., Renault, C., Ricciardi, S., Ristorcelli, I., Rocha, G., Rodríguez-Gonzálvez, C., Rosset, C., Rossetti, M., Rubiño-Martín, J. A., Rusholme, B., Saunders, R. D. E., Savini, G., Schammel, M. P., Scott, D., Shimwell, T. W., Smoot, G. F., Starck, J. -L., Stivoli, F., Stolyarov, V., Sunyaev, R., Sutton, D., Suur-Uski, A. -S., Sygnet, J. -F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Valenziano, L., Van Tent, B., Vielva, P., Villa, F., Vittorio, N., Wade, L. A., Wandelt, B. D., Yvon, D., Zacchei, A., and Zonca, A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: A comparison is presented of Sunyaev-Zeldovich measurements for 11 galaxy clusters as obtained by Planck and by the ground-based interferometer, the Arcminute Microkelvin Imager. Assuming a universal spherically-symmetric Generalised Navarro, Frenk & White (GNFW) model for the cluster gas pressure profile, we jointly constrain the integrated Compton-Y parameter (Y_500) and the scale radius (theta_500) of each cluster. Our resulting constraints in the Y_500-theta_500 2D parameter space derived from the two instruments overlap significantly for eight of the clusters, although, overall, there is a tendency for AMI to find the Sunyaev-Zeldovich signal to be smaller in angular size and fainter than Planck. Significant discrepancies exist for the three remaining clusters in the sample, namely A1413, A1914, and the newly-discovered Planck cluster PLCKESZ G139.59+24.18. The robustness of the analysis of both the Planck and AMI data is demonstrated through the use of detailed simulations, which also discount confusion from residual point (radio) sources and from diffuse astrophysical foregrounds as possible explanations for the discrepancies found. For a subset of our cluster sample, we have investigated the dependence of our results on the assumed pressure profile by repeating the analysis adopting the best-fitting GNFW profile shape which best matches X-ray observations. Adopting the best-fitting profile shape from the X-ray data does not, in general, resolve the discrepancies found in this subset of five clusters. Though based on a small sample, our results suggest that the adopted GNFW model may not be sufficiently flexible to describe clusters universally., Comment: update to metadata author list only
Published: 2012
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6. Planck Intermediate Results. I. Further validation of new Planck clusters with XMM-Newton

Author: The Planck Collaboration, Aghanim, N., Arnaud, M., Ashdown, M., Atrio-Barandela, F., Aumont, J., Baccigalupi, C., Balbi, A., Banday, A. J., Barreiro, R. B., Bartlett, J. G., Battaner, E., Benabed, K., Bernard, J. -P., Bersanelli, M., Böhringer, H., Bonaldi, A., Bond, J. R., Borrill, J., Bouchet, F. R., Bourdin, H., Brown, M. L., Burigana, C., Butler, R. C., Cabella, P., Cardoso, J. -F., Carvalho, P., Catalano, A., Cayón, L., Chamballu, A., Chary, R. -R., Chiang, L. -Y, Chon, G., Christensen, P. R., Clements, D. L., Colafrancesco, S., Colombi, S., Coulais, A., Crill, B. P., Cuttaia, F., Da Silva, A., Dahle, H., Davis, R. J., de Bernardis, P., de Gasperis, G., de Zotti, G., Delabrouille, J., Démoclès, J., Désert, F. -X., Diego, J. M., Dolag, K., Dole, H., Donzelli, S., Doré, O., Douspis, M., Dupac, X., Enßlin, T. A., Eriksen, H. K., Finelli, F., Flores-Cacho, I., Forni, O., Fosalba, P., Frailis, M., Fromenteau, S., Galeotta, S., Ganga, K., Génova-Santos, R. T., Giard, M., González-Nuevo, J., González-Riestra, R., Górski, K. M., Gregorio, A., Gruppuso, A., Hansen, F. K., Harrison, D., Hempel, A., Hernández-Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hornstrup, A., Huffenberger, K. M., Hurier, G., Jagemann, T., Jasche, J., Juvela, M., Keihänen, E., Keskitalo, R., Kisner, T. S., Kneissl, R., Knoche, J., Knox, L., Kurki-Suonio, H., Lagache, G., Lähteenmäki, A., Lamarre, J. -M., Lasenby, A., Lawrence, C. R., Leach, S., Leonardi, R., Liddle, A., Lilje, P. B., López-Caniego, M., Luzzi, G., Macías-Pérez, J. F., Maino, D., Mandolesi, N., Mann, R., Marleau, F., Marshall, D. J., Martínez-González, E., Masi, S., Massardi, M., Matarrese, S., Matthai, F., Mazzotta, P., Meinhold, P. R., Melchiorri, A., Melin, J. -B., Mendes, L., Mennella, A., Miville-Deschênes, M. -A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Naselsky, P., Natoli, P., Nørgaard-Nielsen, H. U., Noviello, F., Osborne, S., Pasian, F., Patanchon, G., Perdereau, O., Perrotta, F., Piacentini, F., Pierpaoli, E., Plaszczynski, S., Platania, P., Pointecouteau, E., Polenta, G., Ponthieu, N., Popa, L., Poutanen, T., Pratt, G. W., Puget, J. -L., Rachen, J. P., Rebolo, R., Reinecke, M., Remazeilles, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Rossetti, M., Rubiño-Martín, J. A., Rusholme, B., Sandri, M., Savini, G., Schaefer, B. M., Scott, D., Smoot, G. F., Starck, J. -L., Stivoli, F., Sunyaev, R., Sutton, D., Sygnet, J. -F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Valenziano, L., Van Tent, B., Vielva, P., Villa, F., Vittorio, N., Wandelt, B. D., Weller, J., White, S. D. M., Yvon, D., Zacchei, A., and Zonca, A.
Subjects: Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract: We present further results from the ongoing XMM-Newton validation follow-up of Planck cluster candidates, detailing X-ray observations of eleven candidates detected at a signal-to-noise ratio of 4.5
Published: 2011
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7. Estimating the tensor-to-scalar ratio and the effect of residual foreground contamination

Author

Fantaye, Y., Stivoli, F., Grain, J., Leach, S. M., Tristram, M., Baccigalupi, C., and Stompor, R.

Subjects

Astrophysics - Cosmology and Extragalactic Astrophysics

Abstract

We consider future balloon-borne and ground-based suborbital experiments designed to search for inflationary gravitational waves, and investigate the impact of residual foregrounds that remain in the estimated cosmic microwave background maps. This is achieved by propagating foreground modelling uncertainties from the component separation, under the assumption of a spatially uniform foreground frequency scaling, through to the power spectrum estimates, and up to measurement of the tensor to scalar ratio in the parameter estimation step. We characterize the error covariance due to subtracted foregrounds, and find it to be subdominant compared to instrumental noise and sample variance in our simulated data analysis. We model the unsubtracted residual foreground contribution using a two-parameter power law and show that marginalization over these foreground parameters is effective in accounting for a bias due to excess foreground power at low $\ell$. We conclude that, at least in the suborbital experimental setups we have simulated, foreground errors may be modeled and propagated up to parameter estimation with only a slight degradation of the target sensitivity of these experiments derived neglecting the presence of the foregrounds., Comment: 19 pages, 12 figures, accepted for publication in JCAP

Published

2011

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8. Planck early results. XV. Spectral energy distributions and radio continuum spectra of northern extragalactic radio sources

Author

Planck Collaboration, Aatrokoski, J., Ade, P. A. R., Aghanim, N., Aller, H. D., Aller, M. F., Angelakis, E., 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., Berdyugin, A., Bernard, J. -P., Bersanelli, M., Bhatia, R., Bonaldi, A., Bonavera, L., Bond, J. R., Borrill, J., Bouchet, F. R., Bucher, M., Burigana, C., Burrows, D. N., Cabella, P., Capalbi, M., Cappellini, B., Cardoso, J. -F., Catalano, A., Cavazzuti, E., Cayón, L., Challinor, A., Chamballu, A., Chary, R. -R., Chiang, L. -Y, Christensen, P. R., Clements, D. L., Colafrancesco, S., Colombi, S., Couchot, F., Coulais, A., Cutini, S., 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., Dickinson, C., Dole, H., Donzelli, S., Doré, O., Dörl, U., Douspis, M., Dupac, X., Efstathiou, G., Enßlin, T. A., Finelli, F., Forni, O., Frailis, M., Franceschi, E., Fuhrmann, L., Galeotta, S., Ganga, K., Gargano, F., Gasparrini, D., Gehrels, N., Giard, M., Giardino, G., Giglietto, N., Giommi, P., Giordano, F., Giraud-Héraud, Y., González-Nuevo, J., Górski, K. M., Gratton, S., Gregorio, A., Gruppuso, A., Harrison, D., 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., Juvela, M., Keihänen, E., Keskitalo, R., King, O., Kisner, T. S., Kneissl, R., Knox, L., Krichbaum, T. P., Kurki-Suonio, H., Lagache, G., Lähteenmäki, A., Lamarre, J. -M., Lasenby, A., Laureijs, R. J., Lavonen, N., Lawrence, C. R., Leach, S., Leonardi, R., León-Tavares, J., Linden-Vørnle, M., Lindfors, E., López-Caniego, M., Lubin, P. M., Macías-Pérez, J. F., Maffei, B., Maino, D., Mandolesi, N., Mann, R., Maris, M., Martínez-González, E., Masi, S., Massardi, M., Matarrese, S., Matthai, F., Max-Moerbeck, W., Mazziotta, M. N., Mazzotta, P., Melchiorri, A., Mendes, L., Mennella, A., Michelson, P. F., Mingaliev, M., Mitra, S., Miville-Deschênes, M. -A., Moneti, A., Monte, C., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, A., Naselsky, P., Natoli, P., Nestoras, I., Netterfield, C. B., Nieppola, E., Nilsson, K., Nørgaard-Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., O'Dwyer, I. J., Osborne, S., Pajot, F., Partridge, B., Pasian, F., Patanchon, G., Pavlidou, V., Pearson, T. J., Perdereau, O., Perotto, L., Perri, M., Perrotta, F., Piacentini, F., Piat, M., Plaszczynski, S., Platania, P., Pointecouteau, E., Polenta, G., Ponthieu, N., Poutanen, T., Prézeau, G., Procopio, P., Prunet, S., Puget, J. -L., Rachen, J. P., Rainò, S., Reach, W. T., Readhead, A., Rebolo, R., Reeves, R., Reinecke, M., Reinthal, R., Renault, C., Ricciardi, S., Richards, J., Riller, T., Riquelme, D., Ristorcelli, I., Rocha, G., Rosset, C., Rowan-Robinson, M., Rubiño-Martín, J. A., Rusholme, B., Saarinen, J., Sandri, M., Savolainen, P., Scott, D., Seiffert, M. D., Sievers, A., Sillanpää, A., Smoot, G. F., Sotnikova, Y., Starck, J. -L., Stevenson, M., Stivoli, F., Stolyarov, V., Sudiwala, R., Sygnet, J. -F., Takalo, L., Tammi, J., Tauber, J. A., Terenzi, L., Thompson, D. J., Toffolatti, L., Tomasi, M., Tornikoski, M., Torre, J. -P., Tosti, G., Tramacere, A., Tristram, M., Tuovinen, J., Türler, M., Turunen, M., Umana, G., Ungerechts, H., Valenziano, L., Valtaoja, E., Varis, J., Verrecchia, F., Vielva, P., Villa, F., Vittorio, N., Wandelt, B. D., Wu, J., Yvon, D., Zacchei, A., Zensus, J. A., Zhou, X., and Zonca, A.

Subjects

Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics

Abstract

Spectral energy distributions (SEDs) and radio continuum spectra are presented for a northern sample of 104 extragalactic radio sources, based on the Planck Early Release Compact Source Catalogue (ERCSC) and simultaneous multifrequency data. The nine Planck frequencies, from 30 to 857 GHz, are complemented by a set of simultaneous observations ranging from radio to gamma-rays. This is the first extensive frequency coverage in the radio and millimetre domains for an essentially complete sample of extragalactic radio sources, and it shows how the individual shocks, each in their own phase of development, shape the radio spectra as they move in the relativistic jet. The SEDs presented in this paper were fitted with second and third degree polynomials to estimate the frequencies of the synchrotron and inverse Compton (IC) peaks, and the spectral indices of low and high frequency radio data, including the Planck ERCSC data, were calculated. SED modelling methods are discussed, with an emphasis on proper, physical modelling of the synchrotron bump using multiplecomponents. Planck ERCSC data also suggest that the original accelerated electron energy spectrum could be much harder than commonly thought, with power-law index around 1.5 instead of the canonical 2.5. The implications of this are discussed for the acceleration mechanisms effective in blazar shock. Furthermore in many cases the Planck data indicate that gamma-ray emission must originate in the same shocks that produce the radio emission., Comment: High-resolution figures will be posted at http://www.rssd.esa.int (TBC). Accepted version updated, Published version updated

Published

2011

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9. Planck Early Results: Statistical properties of extragalactic radio sources in the Planck Early Release Compact Source Catalogue

Author

Planck Collaboration, Ade, P. A. R., Aghanim, N., Argüeso, F., Arnaud, M., Ashdown, M., Aumont, J., Baccigalupi, C., Balbi, A., Banday, A. J., Barreiro, R. B., Bartlett, J. G., Battaner, E., Benabed, K., Bernard, J. -P., Bersanelli, M., Bhatia, R., Bonaldi, A., Bonavera, L., Bond, J. R., Borrill, J., Bouchet, F. R., Bucher, M., Burigana, C., Cabella, P., Cappellini, B., Cardoso, J. -F., Catalano, A., Cayón, L., Challinor, A., Chamballu, A., Chary, R. -R., Chen, X., Chiang, L. -Y, Christensen, P. R., Clements, D. L., Colafrancesco, S., Colombi, S., Couchot, F., 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., Dole, H., Donzelli, S., Doré, O., Dörl, U., Douspis, M., Dupac, X., Efstathiou, G., Enßlin, T. A., Eriksen, H. K., 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., 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., Juvela, M., Keihänen, E., Keskitalo, R., Kisner, T. S., Kneissl, R., Knox, L., Kurki-Suonio, H., Lagache, G., Lähteenmäki, A., Lasenby, A., Laureijs, R. J., Lawrence, C. R., Leach, S., Leahy, J. P., Leonardi, R., Lilje, P. B., Linden-Vørnle, M., López-Caniego, M., Lubin, P. M., Macías-Pérez, J. F., Maffei, B., Magliocchetti, M., Maino, D., Mandolesi, N., Mann, R., Maris, M., Martínez-González, E., Masi, S., Massardi, M., Matarrese, S., Matthai, F., Mazzotta, P., Meinhold, P. R., Melchiorri, A., Mendes, L., Mennella, A., Miville-Deschênes, M. -A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, A., Naselsky, P., Natoli, P., Netterfield, C. B., Nørgaard-Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., O'Dwyer, I. J., Osborne, S., Pajot, F., Paladini, R., Partridge, B., Pasian, F., Patanchon, G., Pearson, T. J., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Pierpaoli, E., Plaszczynski, S., Platania, P., Pointecouteau, E., Polenta, G., Ponthieu, N., Poutanen, T., Prézeau, G., Prunet, S., Puget, J. -L., Rachen, J. P., Rebolo, R., Reinecke, M., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Rowan-Robinson, M., Rubiño-Martín, J. A., Rusholme, B., Sajina, A., Sandri, M., Scott, D., Seiffert, M. D., Serjeant, S., Shellard, P., Smoot, G. F., Starck, J. -L., Stivoli, F., Stolyarov, V., Stompor, R., Sudiwala, R., Sygnet, J. -F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Torre, J. -P., Tristram, M., Tuovinen, J., Türler, M., Umana, G., Valenziano, L., Varis, J., Vielva, P., Villa, F., Vittorio, N., Wade, L. A., Wandelt, B. D., Wilkinson, A., Yvon, D., Zacchei, A., and Zonca, A.

Subjects

Astrophysics - Cosmology and Nongalactic Astrophysics

Abstract

The data reported in Planck's Early Release Compact Source Catalogue (ERCSC) are exploited to measure the number counts (dN/dS) of extragalactic radio sources at 30, 44, 70, 100, 143 and 217 GHz. Due to the full-sky nature of the catalogue, this measurement extends to the rarest and brightest sources in the sky. At lower frequencies (30, 44, and 70 GHz) our counts are in very good agreement with estimates based on WMAP data, being somewhat deeper at 30 and 70 GHz, and somewhat shallower at 44 GHz. Planck's source counts at 143 and 217 GHz join smoothly with the fainter ones provided by the SPT and ACT surveys over small fractions of the sky. An analysis of source spectra, exploiting Planck's uniquely broad spectral coverage, finds clear evidence of a steepening of the mean spectral index above about 70 GHz. This implies that, at these frequencies, the contamination of the CMB power spectrum by radio sources below the detection limit is significantly lower than previously estimated., Comment: Planck Collaboration 2011i, A&A accepted, 11 pages, 7 figures

Published

2011

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10. Planck Early Results: Thermal dust in Nearby Molecular Clouds

Author

Planck Collaboration, Abergel, A., 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., Cardoso, J. -F., Catalano, A., Cayón, L., Challinor, A., Chamballu, A., Chiang, L. -Y, Chiang, C., 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., Eriksen, H. K., 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., Guillet, V., Hansen, F. K., Harrison, D., 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., Jones, A., 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., Masi, S., Matarrese, S., Matthai, F., Mazzotta, P., McGehee, P., Meinhold, P. R., 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., 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., 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., Rubiño-Martín, J. A., Rusholme, B., Sandri, M., Santos, D., Savini, G., Scott, D., Seiffert, M. D., Shellard, P., 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., Tristram, M., Tuovinen, J., Umana, G., Valenziano, L., Verstraete, L., Vielva, P., Villa, F., Vittorio, N., Wade, L. A., Wandelt, B. D., Yvon, D., Zacchei, A., and Zonca, A.

Subjects

Astrophysics - Astrophysics of Galaxies

Abstract

Planck allows unbiased mapping of Galactic sub-millimetre and millimetre emission from the most diffuse regions to the densest parts of molecular clouds. We present an early analysis of the Taurus molecular complex, on line-of-sight-averaged data and without component separation. The emission spectrum measured by Planck and IRAS can be fitted pixel by pixel using a single modified blackbody. Some systematic residuals are detected at 353 GHz and 143 GHz, with amplitudes around -7 % and +13 %, respectively, indicating that the measured spectra are likely more complex than a simple modified blackbody. Significant positive residuals are also detected in the molecular regions and in the 217 GHz and 100 GHz bands, mainly caused by to the contribution of the J=2-1 and J=1-0 12CO and 13CO emission lines. We derive maps of the dust temperature T, the dust spectral emissivity index beta, and the dust optical depth at 250 microns tau. The temperature map illustrates the cooling of the dust particles in thermal equilibrium with the incident radiation field, from 16-17 K in the diffuse regions to 13-14 K in the dense parts. The distribution of spectral indices is centred at 1.78, with a standard deviation of 0.08 and a systematic error of 0.07. We detect a significant T-beta anti-correlation. The dust optical depth map reveals the spatial distribution of the column density of the molecular complex from the densest molecular regions to the faint diffuse regions. We use near-infrared extinction and HI data at 21-cm to perform a quantitative analysis of the spatial variations of the measured dust optical depth at 250 microns per hydrogen atom tau/NH. We report an increase of tau/NH by a factor of about 2 between the atomic phase and the molecular phase, which has a strong impact on the equilibrium temperature of the dust particles., Comment: Planck early paper accepted for publication in Astronomy & Astrophysics, 18 pages

Published

2011

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11. Planck Early Results: The submillimetre properties of a sample of Galactic cold clumps

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., 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., de Bernardis, P., de Gasperis, G., de Rosa, A., de Zotti, G., Delabrouille, J., Delouis, J. -M., Désert, F. -X., Dickinson, C., Doerl, U., Doi, Y., Donzelli, S., Doré, O., 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., Ikeda, N., Jaffe, A. H., Jones, W. C., Juvela, M., Keihänen, E., Keskitalo, R., Kisner, T. S., Kitamura, Y., 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., Malinen, J., Mandolesi, N., Mann, R., Maris, M., Marshall, D. J., Martin, P., Martínez-González, E., Masi, S., Matarrese, S., Matthai, F., Mazzotta, P., McGehee, P., Melchiorri, A., Mendes, L., Mennella, A., Meny, C., 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., Pagani, L., Pajot, F., Paladini, R., Pasian, F., Patanchon, G., 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., and Zonca, A.

Subjects

Astrophysics - Astrophysics of Galaxies

Abstract

(abridged) We perform a detailed investigation of sources from the Cold Cores Catalogue of Planck Objects (C3PO). Our goal is to probe the reliability of the detections, validate the separation between warm and cold dust emission components, provide the first glimpse at the nature, internal morphology and physical characterictics of the Planck-detected sources. We focus on a sub-sample of ten sources from the C3PO list, selected to sample different environments, from high latitude cirrus to nearby (150pc) and remote (2kpc) molecular complexes. We present Planck surface brightness maps and derive the dust temperature, emissivity spectral index, and column densities of the fields. With the help of higher resolution Herschel and AKARI continuum observations and molecular line data, we investigate the morphology of the sources and the properties of the substructures at scales below the Planck beam size., Comment: This paper is part of a package of papers describing first results of the Planck mission, to be published together in a special issue of A&A. Corresponding author: Isabelle.Ristorcelli@cesr.fr. Full resolution version available from http://www.sciops.esa.int/index.php?project=PLANCK&page=Planck_Published_Papers

Published

2011

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12. Planck early results. XX. New light on anomalous microwave emission from spinning dust grains

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., Cappellini, B., Cardoso, J. -F., Casassus, S., Catalano, A., Cayón, L., Challinor, A., Chamballu, A., Chary, R. -R., Chen, X., Chiang, L. -Y, Chiang, C., Christensen, P. R., Clements, D. L., Colombi, S., Couchot, F., Coulais, A., Crill, B. P., Cuttaia, F., Danese, L., Davies, R. D., Davis, R. J., de Bernardis, P., de Gasperis, G., de Rosa, A., de Zotti, G., Delabrouille, J., Delouis, J. -M., Dickinson, C., Donzelli, S., Doré, O., Dörl, U., Douspis, M., Dupac, X., Efstathiou, G., Enßlin, T. A., Eriksen, H. K., Finelli, F., Forni, O., Frailis, M., Franceschi, E., Galeotta, S., Ganga, K., Génova-Santos, R. T., 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, T. R., Jaffe, A. H., Jones, W. C., Juvela, M., Keihänen, E., Keskitalo, R., Kisner, T. S., Kneissl, R., Knox, L., Kurki-Suonio, H., Lagache, G., Lähteenmäki, A., Lamarre, J. -M., Lasenby, A., Laureijs, R. J., Lawrence, C. R., Leach, S., Leonardi, R., Lilje, P. B., Linden-Vørnle, M., López-Caniego, M., Lubin, P. M., Macías-Pérez, J. F., MacTavish, C. J., Maffei, B., Maino, D., Mandolesi, N., Mann, R., Maris, M., Marshall, D. J., Martínez-González, E., Masi, S., Matarrese, S., Matthai, F., Mazzotta, P., McGehee, P., Meinhold, P. R., 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., Natoli, P., Netterfield, C. B., Nørgaard-Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., O'Dwyer, I. J., Osborne, S., Pajot, F., Paladini, R., Partridge, B., Pasian, F., Patanchon, G., Pearson, T. J., Peel, M., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Plaszczynski, S., Platania, P., Pointecouteau, E., Polenta, G., Ponthieu, N., Poutanen, T., Prézeau, G., Procopio, P., Prunet, S., Puget, J. -L., Reach, W. T., Rebolo, R., Reich, W., 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., Shellard, P., Smoot, G. F., Starck, J. -L., Stivoli, F., Stolyarov, V., Stompor, R., Sudiwala, R., Sygnet, J. -F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Torre, J. -P., Tristram, M., Tuovinen, J., Umana, G., Valenziano, L., Varis, J., Verstraete, L., Vielva, P., Villa, F., Vittorio, N., Wade, L. A., Wandelt, B. D., Watson, R., Wilkinson, A., Ysard, N., Yvon, D., Zacchei, A., and Zonca, A.

Subjects

Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics

Abstract

Anomalous microwave emission (AME) has been observed by numerous experiments in the frequency range ~10-60 GHz. Using Planck maps and multi-frequency ancillary data, we have constructed spectra for two known AME regions: the Perseus and Rho Ophiuchi molecular clouds. The spectra are well fitted by a combination of free-free radiation, cosmic microwave background, thermal dust, and electric dipole radiation from small spinning dust grains. The spinning dust spectra are the most precisely measured to date, and show the high frequency side clearly for the first time. The spectra have a peak in the range 20-40 GHz and are detected at high significances of 17.1 sigma for Perseus and 8.4 sigma for Rho Ophiuchi. In Perseus, spinning dust in the dense molecular gas can account for most of the AME; the low density atomic gas appears to play a minor role. In Rho Ophiuchi, the ~30 GHz peak is dominated by dense molecular gas, but there is an indication of an extended tail at frequencies 50-100 GHz, which can be accounted for by irradiated low density atomic gas. The dust parameters are consistent with those derived from other measurements. We have also searched the Planck map at 28.5 GHz for candidate AME regions, by subtracting a simple model of the synchrotron, free-free, and thermal dust. We present spectra for two of the candidates; S140 and S235 are bright HII regions that show evidence for AME, and are well fitted by spinning dust models., Comment: 17 pages, 14 figures, published in A&A as a special issue for Planck early papers. Final version and high-resolution figures, as well as a list of the members of the Planck collaboration can be obtained from http://www.rssd.esa.int or from the A&A webpage: http://www.aanda.org/index.php?option=com_toc&url=%2Farticles%2Faa%2Fabs%2F2011%2F12%2Fcontents%2Fcontents.html&lang=en_GB.utf8%2C+en_GB.UT

Published

2011

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13. Planck Early Results. X. Statistical analysis of Sunyaev-Zeldovich scaling relations for X-ray galaxy clusters

Author

Planck Collaboration, Aghanim, N., Arnaud, M., Ashdown, M., Aumont, J., Baccigalupi, C., Balbi, A., Banday, A. J., Barreiro, R. B., Bartelmann, M., 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., Brown, M. L., Bucher, M., Burigana, C., Cabella, P., Cardoso, J. -F., Catalano, A., Cayón, L., Challinor, A., Chamballu, A., Chary, R. -R., Chiang, L. -Y, Chiang, C., Chon, G., Christensen, P. R., Churazov, E., Clements, D. L., Colafrancesco, S., Colombi, S., Couchot, F., Coulais, A., Crill, B. P., Cuttaia, F., Da Silva, A., Dahle, H., Danese, L., de Bernardis, P., de Gasperis, G., de Rosa, A., de Zotti, G., Delabrouille, J., Delouis, J. -M., Désert, F. -X., Diego, J. M., Dolag, K., Donzelli, S., Doré, O., Dörl, U., Douspis, M., Dupac, X., Efstathiou, G., Enßlin, T. A., Finelli, F., Flores, I., Forni, O., Frailis, M., Franceschi, E., Fromenteau, S., Galeotta, S., Ganga, K., Génova-Santos, R. T., Giard, M., Giardino, G., Giraud-Héraud, Y., González-Nuevo, J., Górski, K. M., Gratton, S., Gregorio, A., Gruppuso, A., Harrison, D., Henrot-Versillé, S., Hernández-Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hovest, W., Hoyland, R. J., Huffenberger, K. M., Jaffe, A. H., Jones, W. C., Juvela, M., Keihänen, E., Keskitalo, R., Kisner, T. S., Kneissl, R., Knox, L., Kurki-Suonio, H., Lagache, G., Lamarre, J. -M., Lasenby, A., Laureijs, R. J., Lawrence, C. R., Leach, S., Leonardi, R., Linden-Vørnle, M., López-Caniego, M., Lubin, P. M., Macías-Pérez, J. F., MacTavish, C. J., Maffei, B., Maino, D., Mandolesi, N., Mann, R., Maris, M., Marleau, F., Martínez-González, E., Masi, S., Matarrese, S., Matthai, F., Mazzotta, P., Melchiorri, A., Melin, J. -B., Mendes, L., Mennella, A., Mitra, S., Miville-Deschênes, M. -A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, A., Naselsky, P., Natoli, P., Netterfield, C. B., Nørgaard-Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., Osborne, S., Pajot, F., Pasian, F., Patanchon, G., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Pierpaoli, E., Piffaretti, R., Plaszczynski, S., Pointecouteau, E., Polenta, G., Ponthieu, N., Poutanen, T., Pratt, G. W., Prézeau, G., Prunet, S., Puget, J. -L., Rebolo, R., Reinecke, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Rubiño-Martín, J. A., Rusholme, B., Sandri, M., Santos, D., Schaefer, B. M., Scott, D., Seiffert, M. D., Smoot, G. F., Starck, J. -L., Stivoli, F., Stolyarov, V., Sunyaev, R., Sygnet, J. -F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tuovinen, J., Valenziano, L., Vibert, L., Vielva, P., Villa, F., Vittorio, N., Wandelt, B. D., White, S. D. M., White, M., Yvon, D., Zacchei, A., and Zonca, A.

Subjects

Astrophysics - Cosmology and Nongalactic Astrophysics

Abstract

All-sky data from the Planck survey and the Meta-Catalogue of X-ray detected Clusters of galaxies (MCXC) are combined to investigate the relationship between the thermal Sunyaev-Zeldovich (SZ) signal and X-ray luminosity. The sample comprises ~ 1600 X-ray clusters with redshifts up to ~ 1 and spans a wide range in X-ray luminosity. The SZ signal is extracted for each object individually, and the statistical significance of the measurement is maximised by averaging the SZ signal in bins of X-ray luminosity, total mass, or redshift. The SZ signal is detected at very high significance over more than two decades in X-ray luminosity (10^43 erg/s < L_500 E(z)^-7/3 < 2 X 10^45 erg/s). The relation between intrinsic SZ signal and X-ray luminosity is investigated and the measured SZ signal is compared to values predicted from X-ray data. Planck measurements and X-ray based predictions are found to be in excellent agreement over the whole explored luminosity range. No significant deviation from standard evolution of the scaling relations is detected. For the first time the intrinsic scatter in the scaling relation between SZ signal and X-ray luminosity is measured and found to be consistent with the one in the luminosity -- mass relation from X-ray studies. There is no evidence of any deficit in SZ signal strength in Planck data relative to expectations from the X-ray properties of clusters, underlining the robustness and consistency of our overall view of intra-cluster medium properties., Comment: Final version accepted for publication in A&A. Also available from this http://www.rssd.esa.int/

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2011

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14. Planck Early Results: The Planck View of Nearby Galaxies

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., Bucher, M., Burigana, C., Cabella, P., 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., Dole, H., Donzelli, S., Doré, O., Dörl, U., Douspis, M., Dupac, X., Efstathiou, G., Enßlin, T. A., 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., Jones, W. C., Juvela, M., Keihänen, E., Keskitalo, R., Kisner, T. S., Kneissl, R., Knox, L., Kurki-Suonio, H., Lagache, G., Lähteenmäki, A., Lamarre, J. -M., Lasenby, A., Laureijs, R. J., Lawrence, C. R., Leach, S., Leonardi, R., Linden-Vørnle, M., López-Caniego, M., Lubin, P. M., Macías-Pérez, J. F., MacTavish, C. J., Madden, S., Maffei, B., Maino, D., Mandolesi, N., Mann, R., Maris, M., Martínez-González, E., Masi, S., Matarrese, S., Matthai, F., Mazzotta, P., Melchiorri, A., Mendes, L., Mennella, A., Miville-Deschênes, M. -A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, A., Naselsky, P., Natoli, P., Netterfield, C. B., Nørgaard-Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., Osborne, S., Pajot, F., Partridge, B., Pasian, F., Patanchon, G., Peel, 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., Savini, G., Scott, D., Seiffert, M. D., Shellard, P., 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., Tristram, M., Tuovinen, J., Türler, M., Umana, G., Valenziano, L., Varis, J., Vielva, P., Villa, F., Vittorio, N., Wade, L. A., Wandelt, B. D., Yvon, D., Zacchei, A., and Zonca, A.

Subjects

Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies

Abstract

The all-sky coverage of the Planck Early Release Compact Source Catalogue (ERCSC) provides an unsurpassed survey of galaxies at submillimetre (submm) wavelengths, representing a major improvement in the numbers of galaxies detected, as well as the range of far-IR/submm wavelengths over which they have been observed. We here present the first results on the properties of nearby galaxies using these data. We match the ERCSC catalogue to IRAS-detected galaxies in the Imperial IRAS Faint Source Redshift Catalogue (IIFSCz), so that we can measure the spectral energy distributions (SEDs) of these objects from 60 to 850 microns. This produces a list of 1717 galaxies with reliable associations between Planck and IRAS, from which we select a subset of 468 for SED studies, namely those with strong detections in the three highest frequency Planck bands and no evidence of cirrus contamination. The SEDs are fitted using parametric dust models to determine the range of dust temperatures and emissivities. We find evidence for colder dust than has previously been found in external galaxies, with T<20K. Such cold temperatures are found using both the standard single temperature dust model with variable emissivity beta, or a two dust temperature model with beta fixed at 2. We also compare our results to studies of distant submm galaxies (SMGs) which have been claimed to contain cooler dust than their local counterparts. We find that including our sample of 468 galaxies significantly reduces the distinction between the two populations. Fits to SEDs of selected objects using more sophisticated templates derived from radiative transfer models confirm the presence of the colder dust found through parameteric fitting. We thus conclude that cold (T<20K) dust is a significant and largely unexplored component of many nearby galaxies., Comment: 16 pages, 14 figures

Published

2011

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15. Planck Early Results: Origin of the submm excess dust emission in the Magellanic Clouds

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., Bot, C., Bouchet, F. R., Boulanger, F., Bucher, M., Burigana, C., Cabella, P., Cardoso, J. -F., Catalano, A., Cayón, L., Challinor, A., Chamballu, A., Chiang, L. -Y, Chiang, C., 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., Doerl, U., Donzelli, S., Doré, O., Douspis, M., Dupac, X., Efstathiou, G., Enßlin, T. A., Finelli, F., Forni, O., Frailis, M., Franceschi, E., Fukui, Y., Galeotta, S., Ganga, K., Giard, M., Giardino, G., Giraud-Héraud, Y., González-Nuevo, J., Górski, K. M., Gratton, S., Gregorio, A., Gruppuso, A., 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., Jones, W. C., Juvela, M., Kawamura, A., Keihänen, E., Keskitalo, R., Kisner, T. S., Kneissl, R., Knox, L., Kurki-Suonio, H., Lagache, G., Lähteenmäki, A., Lamarre, J. -M., Lasenby, A., Laureijs, R. J., Lawrence, C. R., Leach, S., Leonardi, R., Leroy, C., Linden-Vørnle, M., López-Caniego, M., Lubin, P. M., Macías-Pérez, J. F., MacTavish, C. J., Madden, S., Maffei, B., Mandolesi, N., Mann, R., Maris, M., Martínez-González, E., Masi, S., Matarrese, S., Matthai, F., Mazzotta, P., Meinhold, P. R., Melchiorri, A., Mendes, L., Mennella, A., 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., Onishi, T., Osborne, S., Pajot, F., Paladini, R., Paradis, D., Pasian, F., Patanchon, G., 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., 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., Tristram, M., Tuovinen, J., Umana, G., Valenziano, L., Varis, J., Vielva, P., Villa, F., Vittorio, N., Wade, L. A., Wandelt, B. D., Ysard, N., Yvon, D., Zacchei, A., and Zonca, A.

Subjects

Astrophysics - Cosmology and Nongalactic Astrophysics

Abstract

The integrated Spectral Energy Distributions of the Large and Small Magellanic Cloud appear significantly flatter than expected from dust models based on their FIR and radio emission. The origin of this millimetre excess is still unexplained, and is here investigated using the Planck data. The background CMB contribution is subtracted using an ILC method performed locally around the galaxies. The foreground emission from the Milky Way is subtracted. After subtraction, the emission of both galaxies correlates closely with the gas emission of the LMC and SMC. The millimetre excess in the LMC can be explained by CMB fluctuations, but a significant excess is still present in the SMC SED. The Planck and IRIS data at 100 micron are combined to produce thermal dust temperature and optical depth maps of the two galaxies. The LMC temperature map shows the presence of a warm inner arm already found with the Spitzer data, but also shows the existence of a previously unidentified cold outer arm. Several cold regions are found along this arm, some of which are associated with known molecular clouds. The average emissivity spectral index is found to be consistent with beta=1.5 and beta=1.2 below 500 microns for the LMC and SMC respectively, significantly flatter than the values observed in the Milky Way. Furthermore, there is evidence in the SMC for a further flattening of the SED in the sub-mm. The spatial distribution of the millimetre dust excess in the SMC follows the gas and thermal dust distribution. Different models are explored in order to fit the dust emission in the SMC. It is concluded that the millimetre excess is unlikely to be caused by very cold dust emission and that it could be due to a combination of spinning dust. emission and thermal dust emission by more amorphous dust grains than those present in our Galaxy., Comment: 17 pages, 14 Figures

Published

2011

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16. Planck Early Results. VII. The Early Release Compact Source Catalog

Author

Planck Collaboration, Ade, P. A. R., Aghanim, N., Arnaud, M., Ashdown, M., Aumont, J., Baccigalupi, C., Balbi, A., Banday, A. J., Barreiro, R. B., Bartlett, J. G., Battaner, E., Benabed, K., Benoît, A., Bernard, J. -P., Bersanelli, M., Bhatia, R., Bonaldi, A., Bonavera, L., Bond, J. R., Borrill, J., Bouchet, F. R., Bucher, M., Burigana, C., Butler, R. C., Cabella, P., Cantalupo, C. M., Cappellini, B., Cardoso, J. -F., Carvalho, P., Catalano, A., Cayón, L., Challinor, A., Chamballu, A., Chary, R. -R., Chen, X., Chiang, L. -Y, Chiang, C., Christensen, P. R., Clements, D. L., Colombi, S., Couchot, F., Coulais, A., Crill, B. P., Cuttaia, F., Danese, L., Davis, R. J., de Bernardis, P., de Rosa, A., de Zotti, G., Delabrouille, J., Delouis, J. -M., Désert, F. -X., Dickinson, C., Diego, J. M., Dolag, K., Dole, H., Donzelli, S., Doré, O., Dörl, U., Douspis, M., Dupac, X., Efstathiou, G., Enßlin, T. A., Eriksen, H. K., Finelli, F., Forni, O., Fosalba, P., Frailis, M., Franceschi, E., Galeotta, S., Ganga, K., Giard, M., Giraud-Héraud, Y., González-Nuevo, J., Górski, K. M., Gratton, S., Gregorio, A., Gruppuso, A., Haissinski, J., Hansen, F. K., Harrison, D., Helou, G., Henrot-Versillé, S., Hernández-Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hornstrup, A., Hovest, W., Hoyland, R. J., Huffenberger, K. M., Huynh, M., Jaffe, A. H., Jones, W. C., Juvela, M., Keihänen, E., Keskitalo, R., Kisner, T. S., Kneissl, R., Knox, L., Kurki-Suonio, H., Lagache, G., Lähteenmäki, A., Lamarre, J. -M., Lasenby, A., Laureijs, R. J., Lawrence, C. R., Leach, S., Leahy, J. P., Leonardi, R., León-Tavares, J., Leroy, C., Lilje, P. B., Linden-Vørnle, M., López-Caniego, M., Lubin, P. M., Macías-Pérez, J. F., MacTavish, C. J., Maffei, B., Maggio, G., Maino, D., Mandolesi, N., Mann, R., Maris, M., Marleau, F., Marshall, D. J., Martínez-González, E., Masi, S., Massardi, M., Matarrese, S., Matthai, F., Mazzotta, P., McGehee, P., Meinhold, P. R., Melchiorri, A., Melin, J. -B., Mendes, L., Mennella, A., Mitra, S., Miville-Deschênes, M. -A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, A., Naselsky, P., Natoli, P., Netterfield, C. B., Nørgaard-Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., O'Dwyer, I. J., Osborne, S., Pajot, F., Paladini, R., Partridge, B., Pasian, F., Patanchon, G., Pearson, T. J., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Piffaretti, R., Plaszczynski, S., Platania, P., Pointecouteau, E., Polenta, G., Ponthieu, N., Poutanen, T., Pratt, G. W., Prézeau, G., Prunet, S., Puget, J. -L., Rachen, J. P., Reach, W. T., Rebolo, R., Reinecke, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Rowan-Robinson, M., Rubiño-Martín, J. A., Rusholme, B., Sajina, A., Sandri, M., Santos, D., Savini, G., Schaefer, B. M., Scott, D., Seiffert, M. D., Shellard, P., Smoot, G. F., Starck, J. -L., Stivoli, F., Stolyarov, V., Sudiwala, R., Sunyaev, R., Sygnet, J. -F., Tauber, J. A., Tavagnacco, D., Terenzi, L., Toffolatti, L., Tomasi, M., Torre, J. -P., Tristram, M., Tuovinen, J., Türler, M., Umana, G., Valenziano, L., Valiviita, J., Varis, J., Vielva, P., Villa, F., Vittorio, N., Wade, L. A., Wandelt, B. D., White, S. D. M., Wilkinson, A., Yvon, D., Zacchei, A., and Zonca, A.

Subjects

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

Abstract

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

Published

2011

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17. Planck Early Results. V. The Low Frequency Instrument data processing

Author

Zacchei, A., Maino, D., Baccigalupi, C., Bersanelli, M., Bonaldi, A., Bonavera, L., Burigana, C., Butler, R. C., Cuttaia, F., de Zotti, G., Dick, J., Frailis, M., Galeotta, S., González-Nuevo, J., Górski, K. M., Gregorio, A., Keihänen, E., Keskitalo, R., Knoche, J., Kurki-Suonio, H., Lawrence, C. R., Leach, S., Leahy, J. P., López-Caniego, M., Mandolesi, N., Maris, M., Matthai, F., Meinhold, P. R., Mennella, A., Morgante, G., Morisset, N., Natoli, P., Pasian, F., Perrotta, F., Polenta, G., Poutanen, T., Reinecke, M., Ricciardi, S., Rohlfs, R., Sandri, M., Suur-Uski, A. -S., Tauber, J. A., Tavagnacco, D., Terenzi, L., Tomasi, M., Valiviita, J., Villa, F., Zonca, A., Banday, A. J., Barreiro, R. B., Bartlett, J. G., Bartolo, N., Bedini, L., Bennett, K., Binko, P., Borrill, J., Bouchet, F. R., Bremer, M., Cabella, P., Cappellini, B., Chen, X., Colombo, L., Cruz, M., Curto, A., Danese, L., Davies, R. D., Davis, R. J., de Gasperis, G., de Rosa, A., de Troia, G., Dickinson, C., Diego, J. M., Donzelli, S., Dörl, U., Efstathiou, G., Enßlin, T. A., Eriksen, H. K., Falvella, M. C., Finelli, F., Franceschi, E., Gaier, T. C., Gasparo, F., Génova-Santos, R. T., Giardino, G., Gómez, F., Gruppuso, A., Hansen, F. K., Hell, R., Herranz, D., Hovest, W., Huynh, M., Jewell, J., Juvela, M., Kisner, T. S., Knox, L., Lähteenmäki, A., Lamarre, J. -M., Leonardi, R., León-Tavares, J., Lilje, P. B., Lubin, P. M., Maggio, G., Marinucci, D., Martínez-González, E., Massardi, M., Matarrese, S., Meharga, M. T., Melchiorri, A., Migliaccio, M., Mitra, S., Moss, A., Nørgaard-Nielsen, H. U., Pagano, L., Paladini, R., Paoletti, D., Partridge, B., Pearson, D., Pettorino, V., Pietrobon, D., Prézeau, G., Procopio, P., Puget, J. -L., Quercellini, C., Rachen, J. P., Rebolo, R., Robbers, G., Rocha, G., Rubiño-Martín, J. A., Salerno, E., Savelainen, M., Scott, D., Seiffert, M. D., Silk, J. I., Smoot, G. F., Sternberg, J., Stivoli, F., Stompor, R., Tofani, G., Toffolatti, L., Tuovinen, J., Türler, M., Umana, G., Vielva, P., Vittorio, N., Vuerli, C., Wade, L. A., Watson, R., White, S. D. M., and Wilkinson, A.

Subjects

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

Abstract

We describe the processing of data from the Low Frequency Instrument (LFI) used in production of the Planck Early Release Compact Source Catalogue (ERCSC). In particular, we discuss the steps involved in reducing the data from telemetry packets to cleaned, calibrated, time-ordered data (TOD) and frequency maps. Data are continuously calibrated using the modulation of the temperature of the cosmic microwave background radiation induced by the motion of the spacecraft. Noise properties are estimated from TOD from which the sky signal has been removed using a generalized least square map-making algorithm. Measured 1/f noise knee-frequencies range from 100mHz at 30GHz to a few tens of mHz at 70GHz. A destriping code (Madam) is employed to combine radiometric data and pointing information into sky maps, minimizing the variance of correlated noise. Noise covariance matrices required to compute statistical uncertainties on LFI and Planck products are also produced. Main beams are estimated down to the approx -10dB level using Jupiter transits, which are also used for geometrical calibration of the focal plane., Comment: A&A Volume 536, December 2011 Planck early results

Published

2011

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18. Planck Early Results XXIV: Dust in the diffuse interstellar medium and the Galactic halo

Author

Planck Collaboration, Abergel, A., 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., Benoit, A., Bernard, J. -P., Bersanelli, M., Bhatia, R., Blagrave, K., 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., Cayon, L., Challinor, A., Chamballu, A., Chiang, L. -Y, Chiang, C., 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., Desert, F. -X., Dickinson, C., Donzelli, S., Dore, O., Dorl, U., Douspis, M., Dupac, X., Efstathiou, G., Ensslin, T. A., Eriksen, H. K., Finelli, F., Forni, O., Frailis, M., Franceschi, E., Galeotta, S., Ganga, K., Giard, M., Giardino, G., Giraud-Heraud, Y., Gonzalez-Nuevo, J., Gorski, K. M., Gratton, S., Gregorio, A., Gruppuso, A., Hansen, F. K., Harrison, D., Helou, G., Henrot-Versille, 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, A., Jones, W. C., Juvela, M., Keihanen, 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-Vornle, M., Lockman, F. J., Lopez-Caniego, M., Lubin, P. M., Macias-Perez, J. F., MacTavish, C. J., Maffei, B., Maino, D., Mandolesi, N., Mann, R., Maris, M., Marshall, D. J., Martin, P., Martinez-Gonzalez, E., Masi, S., Matarrese, S., Matthai, F., Mazzotta, P., McGehee, P., Meinhold, P. R., Melchiorri, A., Mendes, L., Mennella, A., Miville-Deschenes, M. -A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, A., Naselsky, P., Nati, F., Natoli, P., Netterfield, C. B., Norgaard-Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., O'Dwyer, I. J., Osborne, S., Pajot, F., Paladini, R., Pasian, F., Patanchon, G., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Goncalves, D. Pinheiro, Plaszczynski, S., Pointecouteau, E., Polenta, G., Ponthieu, N., Poutanen, T., Prezeau, G., Prunet, S., Puget, J. -L., Rachen, J. P., Reach, W. T., Reinecke, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Rowan-Robinson, M., Rubino-Martin, J. A., Rusholme, B., Sandri, M., Santos, D., Savini, G., Scott, D., Seiffert, M. D., Shellard, P., Smoot, G. F., Starck, J. -L., Stivoli, F., Stolyarov, V., Stompor, R., Sudiwala, R., Sygnet, J. -F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Torre, J. -P., Tristram, M., Tuovinen, J., Umana, G., Valenziano, L., Vielva, P., Villa, F., Vittorio, N., Wade, L. A., Wandelt, B. D., Wilkinson, A., Yvon, D., Zacchei, A., and Zonca, A.

Subjects

Astrophysics - Astrophysics of Galaxies

Abstract

This paper presents the first results of comparison of Planck along with IRAS data with Green Bank Telescope 21-cm observations in 14 fields covering more than 800 square degrees at high Galactic latitude. Galactic dust emission for fields with average HI column density lower than 2 x 10^20 cm^-2 is well correlated with 21-cm emission. The residual emission in these fields, once the HI-correlated emission is removed, is consistent with the expected statistical properties of the cosmic infrared background fluctuations. Fields with larger column densities show significant excess dust emission compared to the HI column density. Regions of excess lie in organized structures that suggest the presence of hydrogen in molecular form, though they are not always correlated with CO emission. Dust emission from intermediate-velocity clouds is detected with high significance. Its spectral properties are consistent with, compared to the local ISM values, significantly hotter dust (T~20 K), lower sub-millimeter dust opacity, and a relative abundance of very small grains to large grains about four times higher. These results are compatible with expectations for clouds that are part of the Galactic fountain in which there is dust shattering and fragmentation. Correlated dust emission in HVCs is not detected; the average of the 99.9% confidence upper limits to the emissivity is 0.15 times the local ISM value at 857 and 3000 GHz, in accordance with gas phase evidence for lower metallicity and depletion in these clouds. Unexpected anti-correlated variations of the dust temperature and emission cross-section per H atom are identified in the local ISM and IVCs, a trend that continues into molecular environments. This suggests that dust growth through aggregation, seen in molecular clouds, is active much earlier in the cloud condensation and star formation processes., Comment: 30 pages, 22 figures, accepted for publication in A&A as a special issue for Planck early papers

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2011

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19. Planck early results. XXI. Properties of the interstellar medium in the Galactic plane

Author

Planck Collaboration, Abergel, A., 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., Benoit, 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., Cardoso, J. -F., Catalano, A., Cayon, L., Challinor, A., Chamballu, A., Chiang, L. -Y, Chiang, C., Christensen, P. R., Colombi, S., Couchot, F., Coulais, A., Crill, B. P., Cuttaia, F., Dame, T., 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., Desert, F. -X., Dickinson, C., Donzelli, S., Dore, O., Dorl, U., Douspis, M., Dupac, X., Efstathiou, G., Ensslin, T. A., Finelli, F., Forni, O., Frailis, M., Franceschi, E., Galeotta, S., Ganga, K., Giard, M., Giardino, G., Giraud-Heraud, Y., Gonzalez-Nuevo, J., Gorski, K. M., Gratton, S., Gregorio, A., Grenier, I. A., Gruppuso, A., Hansen, F. K., Harrison, D., Henrot-Versille, S., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hovest, W., Hoyland, R. J., Huffenberger, K. M., Jaffe, T. R., Jaffe, A. H., Jones, W. C., Juvela, M., Keihanen, E., Keskitalo, R., Kisner, T. S., Kneissl, R., Knox, L., Kurki-Suonio, H., Lagache, G., Lahteenmaki, A., Lamarre, J. -M., Lasenby, A., Laureijs, R. J., Lawrence, C. R., Leach, S., Leonardi, R., Leroy, C., Lilje, P. B., Linden-Vornle, M., Lopez-Caniego, M., Lubin, P. M., Macias-Perez, J. F., MacTavish, C. J., Maffei, B., Mandolesi, N., Mann, R., Maris, M., Marshall, D. J., Martinez-Gonzalez, E., Masi, S., Matarrese, S., Matthai, F., Mazzotta, P., McGehee, P., Meinhold, P. R., Melchiorri, A., Mendes, L., Mennella, A., Miville-Deschenes, M. -A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, A., Naselsky, P., Natoli, P., Netterfield, C. B., Norgaard-Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., Osborne, S., Pajot, F., Paladini, R., Pasian, F., Patanchon, G., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Plaszczynski, S., Pointecouteau, E., Polenta, G., Ponthieu, N., Poutanen, T., Prezeau, G., Prunet, S., Puget, J. -L., Rachen, J. P., Reach, W. T., Rebolo, R., Reich, W., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Rubino-Martin, J. A., Rusholme, B., Sandri, M., Santos, D., Savini, G., Scott, D., Seiffert, M. D., Shellard, P., Smoot, G. F., Starck, J. -L., Stivoli, F., Stolyarov, V., Stompor, R., Sudiwala, R., Sygnet, J. -F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Torre, J. -P., Tristram, M., Tuovinen, J., Umana, G., Valenziano, L., Varis, J., Vielva, P., Villa, F., Vittorio, N., Wade, L. A., Wandelt, B. D., Wilkinson, A., Ysard, N., Yvon, D., Zacchei, A., and Zonca, A.

Subjects

Astrophysics - Astrophysics of Galaxies

Abstract

(abridged) Planck has observed the entire sky from 30 GHz to 857GHz. The observed foreground emission contains contributions from different phases of the interstellar medium (ISM). We have separated the observed Galactic emission into the different gaseous components (atomic, molecular and ionised) in each of a number of Galactocentric rings. Templates are created for various Galactocentric radii using velocity information from atomic (neutral hydrogen) and molecular (12CO) observations. The ionised template is assumed to be traced by free-free emission as observed by WMAP, while 408 MHz emission is used to trace the synchrotron component. Gas emission not traced by the above templates, namely "ark gas", as evidenced using Planck data, is included as an additional template, the first time such a component has been used in this way. These templates are then correlated with each of the Planck frequency bands, as well as other ancillary data. The emission per column density of the gas templates allows us to create distinct spectral energy distributions (SEDs) per Galactocentric ring and in each of the gaseous tracers from 1.4 GHz to 25 THz (12\mu m). Apart from the thermal dust and free-free emission, we have probed the Galaxy for anomalous (e.g., spinning) dust as well as synchrotron emission. We show that anomalous dust emission is present in the atomic, molecular and dark gas phases throughout the Galactic disk. The derived dust propeties associated with the dark gas phase are derived but do not allow us to reveal the nature of this phase. For all environments, the anomalous emission is consistent with rotation from polycyclic aromatic hydrocarbons (PAHs) and, according to our simple model, accounts for $(25\pm5)%$ (statistical) of the total emission at 30 GHz., Comment: Accepted for publication. This paper is part of a package of papers describing first results of the Planck mission, to be published together in a special issue of A&A. Corresponding author: Douglas Marshall : douglas.marshall@cesr.fr. Full resolution version available from http://www.sciops.esa.int/index.php?project=PLANCK&page=Planck_Published_Papers

Published

2011

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20. 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., and Zonca, A.

Subjects

Astrophysics - Astrophysics of Galaxies

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)

Published

2011

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21. Planck early results. IX. XMM-Newton follow-up for validation of Planck cluster candidates

Author

Planck Collaboration, Aghanim, N., Arnaud, M., Ashdown, M., Aumont, J., Baccigalupi, C., Balbi, A., Banday, A. J., Barreiro, R. B., Bartelmann, M., 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., Brown, M. L., Bucher, M., Burigana, C., Cabella, P., Cardoso, J. -F., Catalano, A., Cayòn, L., Challinor, A., Chamballu, A., Chary, R. R., Chiang, L. Y, Chiang, C., Chon, G., Christensen, P. R., Churazov, E., Clements, D. L., Colafrancesco, S., Colombi, S., Couchot, F., Coulais, A., Crill, B. P., Cuttaia, F., Da Silva, A., Dahle, H., Danese, L., de Bernardis, P., de Gasperis, G., de Rosa, A., de Zotti, G., Delabrouille, J., Delouis, J. -M., Désert, F. -X., Diego, J. M., Dolag, K., Donzelli, S., Doré, O., Dörl, U., Douspis, M., Dupac, X., Efstathiou, G., Ensslin, T. A., Finelli, F., Flores, I., Forni, O., Frailis, M., Franceschi, E., Fromenteau, S., Galeotta, S., Ganga, K., Génova-Santos, R. T., Giard, M., Giardino, G., Giraud-Héraud, Y., González-Nuevo, J., Górski, K. M., Gratton, S., Gregorio, A., Gruppuso, A., Harrison, D., Henrot-Versillé, S., Hernández-Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hovest, W., Hoyland, R. J., Huffenberger, K. M., Jaffe, A. H., Jones, W. C., Juvela, M., Keihänen, E., Keskitalo, R., Kisner, T. S., Kneissl, R., Knox, L., Kurki-Suonio, H., Lagache, G., Lamarre, J. -M., Lasenby, A., Laureijs, R. J., Lawrence, C. R., Leach, S., Leonardi, R., Linden-Vornle, M., López-Caniego, M., Lubin, P. M., Macías-Pérez, J. -F., MacTavish, C. J., Maffei, B., Maino, D., Mandolesi, N., Mann, R., Maris, M., Marleau, F., Martínez-González, E., Masi, S., Matarrese, S., Matthai, F., Mazzotta, P., Melchiorri, A., Melin, J. -B., Mendes, L., Mennella, A., Mitra, S., Miville-Deschênes, M. -A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, A., Naselsky, P., Natoli, P., Netterfield, C. B., Norgaard-Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., Osborne, S., Pajot, F., Pasian, F., Patanchon, G., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Pierpaoli, E., Piffaretti, R., Plaszczynski, S., Pointecouteau, E., Polenta, G., Ponthieu, N., Poutanen, T., Pratt, G. W., Prézeau, G., Prunet, S., Puget, J. -L., Rebolo, R., Reinecke, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Rubiõo-Martín, J. A., Rusholme, B., Sandri, M., Santos, D., Schaefer, B. M., Scott, D., Seiffert, M. D., Smoot, G. F., Starck, J. -L., Stivoli, F., Stolyarov, V., Sunyaev, R., Sygnet, J. -F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tuovinen, J., Valenziano, L., Vibert, L., Vielva, P., Villa, F., Vittorio, N., Wandelt, B. D., White, S. D. M., White, M., Yvon, D., Zacchei, A., and Zonca, A.

Subjects

Astrophysics - Cosmology and Nongalactic Astrophysics

Abstract

We present the XMM-Newton follow-up for confirmation of Planck cluster candidates. Twenty-five candidates have been observed to date using snapshot (~10 ksec) exposures, ten as part of a pilot programme to sample a low range of signal-to-noise ratios (45 candidates. The sensitivity and spatial resolution of XMM-Newton allows unambiguous discrimination between clusters and false candidates. The 4 false candidates have S/N <= 4.1. A total of 21 candidates are confirmed as extended X-ray sources. Seventeen are single clusters, the majority of which are found to have highly irregular and disturbed morphologies (about ~70%). The remaining four sources are multiple systems, including the unexpected discovery of a supercluster at z=0.45. For 20 sources we are able to derive a redshift estimate from the X-ray Fe K line (albeit of variable quality). The new clusters span the redshift range 0.09 <= z <= 0.54, with a median redshift of z~0.37. A first determination is made of their X-ray properties including the characteristic size, which is used to improve the estimate of the SZ Compton parameter, Y_SZ. The follow-up validation programme has helped to optimise the Planck candidate selection process. It has also provided a preview of the X-ray properties of these newly-discovered clusters, allowing comparison with their SZ properties, and to the X-ray and SZ properties of known clusters observed in the Planck survey. Our results suggest that Planck may have started to reveal a non-negligible population of massive dynamically perturbed objects that is under-represented in X-ray surveys. However, despite their particular properties, these new clusters appear to follow the Y_SZ-Y_X relation established for X-ray selected objects, where Y_X is the product of the gas mass and temperature., Comment: 21 pages, 16 figures (some low resolution), final version accepted for publication in A&A

Published

2011

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22. Planck Early Results XVIII: The power spectrum of cosmic infrared background anisotropies

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., Blagrave, K., Bock, J. J., Bonaldi, A., Bonavera, L., Bond, J. R., Borrill, J., Bouchet, F. R., Bucher, M., Burigana, C., Cabella, P., Cardoso, J. -F., Catalano, A., Cayón, L., Challinor, A., Chamballu, A., Chiang, L. -Y, Chiang, C., 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., Dole, H., Donzelli, S., Doré, O., Dörl, U., Douspis, M., Dupac, X., Efstathiou, G., Enßlin, T. A., Eriksen, H. K., Finelli, F., Forni, O., Fosalba, P., Frailis, M., Franceschi, E., Galeotta, S., Ganga, K., Giard, M., Giardino, G., Giraud-Héraud, Y., González-Nuevo, J., Górski, K. M., Grain, J., 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., 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., Lilje, P. B., Linden-Vørnle, M., Lockman, F. J., López-Caniego, M., Lubin, P. M., Macías-Pérez, J. F., MacTavish, C. J., Maffei, B., Maino, D., Mandolesi, N., Mann, R., Maris, M., Martin, P., Martínez-González, E., Masi, S., Matarrese, S., Matthai, F., Mazzotta, 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., Natoli, P., Netterfield, C. B., Nørgaard-Nielsen, H. U., Novikov, D., Novikov, I., O'Dwyer, I. J., Oliver, S., Osborne, S., Pajot, F., Pasian, F., Patanchon, G., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Gonçalves, D. Pinheiro, Plaszczynski, S., Pointecouteau, E., Polenta, G., Ponthieu, N., Poutanen, T., Prézeau, G., Prunet, S., Puget, J. -L., Rachen, J. P., Reach, W. T., Reinecke, M., Remazeilles, 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., Shellard, P., Smoot, G. F., Starck, J. -L., Stivoli, F., Stolyarov, V., Stompor, R., Sudiwala, R., Sunyaev, R., Sygnet, J. -F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Torre, J. -P., Tristram, M., Tuovinen, J., Umana, G., Valenziano, L., Vielva, P., Villa, F., Vittorio, N., Wade, L. A., Wandelt, B. D., White, M., Yvon, D., Zacchei, A., and Zonca, A.

Subjects

Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - Astrophysics of Galaxies

Abstract

Using Planck maps of six regions of low Galactic dust emission with a total area of about 140 square degrees, we determine the angular power spectra of cosmic infrared background (CIB) anisotropies from multipole l = 200 to l = 2000 at 217, 353, 545 and 857 GHz. We use 21-cm observations of HI as a tracer of thermal dust emission to reduce the already low level of Galactic dust emission and use the 143 GHz Planck maps in these fields to clean out cosmic microwave background anisotropies. Both of these cleaning processes are necessary to avoid significant contamination of the CIB signal. We measure correlated CIB structure across frequencies. As expected, the correlation decreases with increasing frequency separation, because the contribution of high-redshift galaxies to CIB anisotropies increases with wavelengths. We find no significant difference between the frequency spectrum of the CIB anisotropies and the CIB mean, with Delta I/I=15% from 217 to 857 GHz. In terms of clustering properties, the Planck data alone rule out the linear scale- and redshift-independent bias model. Non-linear corrections are significant. Consequently, we develop an alternative model that couples a dusty galaxy, parametric evolution model with a simple halo-model approach. It provides an excellent fit to the measured anisotropy angular power spectra and suggests that a different halo occupation distribution is required at each frequency, which is consistent with our expectation that each frequency is dominated by contributions from different redshifts. In our best-fit model, half of the anisotropy power at l=2000 comes from redshifts z<0.8 at 857 GHz and z<1.5 at 545 GHz, while about 90% come from redshifts z>2 at 353 and 217 GHz, respectively., Comment: Final A&A version. Few typos corrected

Published

2011

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23. Planck Early Results: All sky temperature and dust optical depth from Planck and IRAS: Constraints on the 'dark gas' in our galaxy

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., Cardoso, J. -F., Catalano, A., Cayón, L., Challinor, A., Chamballu, A., Chiang, L. -Y, Chiang, C., Christensen, P. R., Clements, D. L., Colombi, S., Couchot, F., Coulais, A., Crill, B. P., Cuttaia, F., Dame, T., 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., Doerl, U., Donzelli, S., Doré, O., Douspis, M., Dupac, X., Efstathiou, G., Enßlin, T. A., Eriksen, H. K., Finelli, F., Forni, O., Fosalba, P., Frailis, M., Franceschi, E., Fukui, Y., Galeotta, S., Ganga, K., Giard, M., Giardino, G., Giraud-Héraud, Y., González-Nuevo, J., Górski, K. M., Gratton, S., Gregorio, A., Grenier, I. 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., Jones, W. C., Juvela, M., Kawamura, A., 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., Lilje, P. B., Linden-Vørnle, M., López-Caniego, M., Lubin, P. M., Macías-Pérez, J. F., MacTavish, C. J., Maffei, B., Maino, D., Mandolesi, N., Mann, R., Maris, M., Martin, P., Martínez-González, E., Masi, S., Matarrese, S., Matthai, F., Mazzotta, P., McGehee, P., Meinhold, P. R., Melchiorri, A., Mendes, L., Mennella, A., Miville-Deschênes, M. -A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, A., Naselsky, P., Natoli, P., Netterfield, C. B., Nørgaard-Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., O'Dwyer, I. J., Onishi, T., Osborne, S., Pajot, F., Paladini, R., Paradis, D., Pasian, F., Patanchon, G., 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., 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., Shellard, P., Smoot, G. F., Starck, J. -L., Stivoli, F., Stolyarov, V., Stompor, R., Sudiwala, R., Sygnet, J. -F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Torre, J. -P., Tristram, M., Tuovinen, J., Umana, G., Valenziano, L., Vielva, P., Villa, F., Vittorio, N., Wade, L. A., Wandelt, B. D., Wilkinson, A., Yvon, D., Zacchei, A., and Zonca, A.

Subjects

Astrophysics - Astrophysics of Galaxies

Abstract

We construct an all-sky map of the apparent temperature and optical depth of thermal dust emission using the Planck-HFI and IRAS data. The optical depth maps are correlated to tracers of the atomic and molecular gas. The correlation is linear in the lowest column density regions at high galactic latitudes. At high NH, the correlation is consistent with that of the lowest NH. In the intermediate NH range, we observe departure from linearity, with the dust optical depth in excess to the correlation. We attribute this excess emission to thermal emission by dust associated with a Dark-Gas phase, undetected in the available HI and CO measurements. We show the 2D spatial distribution of the Dark-Gas in the solar neighborhood and show that it extends around known molecular regions traced by CO. The average dust emissivity in the HI phase in the solar neighborhood follows roughly a power law distribution with beta = 1.8 all the way down to 3 mm, although the SED flattens slightly in the millimetre. The threshold for the existence of the Dark-Gas is found at NH = (8.0\pm 0.58) 10^{20} Hcm-2. Assuming the same dust emissivity at high frequencies for the dust in the atomic and molecular phases leads to an average XCO = (2.54\pm0.13) 10^{20} H2cm-2/(K km s-1). The mass of Dark-Gas is found to be 28% of the atomic gas and 118% of the CO emitting gas in the solar neighborhood. A possible origin for the Dark-Gas is the existence of a dark molecular phase, where H2 survives photodissociation but CO does not. The observed transition for the onset of this phase in the solar neighborhood (AV = 0.4 mag) appears consistent with recent theoretical predictions. We also discuss the possibility that up to half of the Dark-Gas could be in atomic form, due to optical depth effects in the HI measurements., Comment: 16 pages, 10 figures

Published

2011

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24. Planck Early Results XI: Calibration of the local galaxy cluster Sunyaev-Zeldovich scaling relations

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., Bartelmann, M., 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., Bourdin, H., Brown, M. L., Bucher, M., Burigana, C., Cabella, P., Cardoso, J. -F., Catalano, A., Cayón, L., Challinor, A., Chamballu, A., Chiang, L. -Y, Chiang, C., Chon, G., Christensen, P. R., Churazov, E., Clements, D. L., Colafrancesco, S., Colombi, S., Couchot, F., Coulais, A., Crill, B. P., Cuttaia, F., Da Silva, A., Dahle, H., Danese, L., de Bernardis, P., de Gasperis, G., de Rosa, A., de Zotti, G., Delabrouille, J., Delouis, J. -M., Désert, F. -X., Diego, J. M., Dolag, K., Donzelli, S., Doré, O., Dörl, U., Douspis, M., Dupac, X., Efstathiou, G., Enßlin, T. A., Finelli, F., Flores, I., Forni, O., Frailis, M., Franceschi, E., Fromenteau, S., Galeotta, S., Ganga, K., Génova-Santos, R. T., Giard, M., Giardino, G., Giraud-Héraud, Y., González-Nuevo, J., Górski, K. M., Gratton, S., Gregorio, A., Gruppuso, A., Harrison, D., Henrot-Versillé, S., Hernández-Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hovest, W., Hoyland, R. J., Huffenberger, K. M., Jaffe, A. H., Jones, W. C., Juvela, M., Keihänen, E., Keskitalo, R., Kisner, T. S., Kneissl, R., Knox, L., Kurki-Suonio, H., Lagache, G., Lamarre, J. -M., Lanoux, J., Lasenby, A., Laureijs, R. J., Lawrence, C. R., Leach, S., Leonardi, R., Liddle, A., Lilje, P. B., Linden-Vørnle, M., López-Caniego, M., Lubin, P. M., Macías-Pérez, J. F., MacTavish, C. J., Maffei, B., Maino, D., Mandolesi, N., Mann, R., Maris, M., Marleau, F., Martínez-González, E., Masi, S., Matarrese, S., Matthai, F., Mazzotta, P., Melchiorri, A., Melin, J. -B., Mendes, L., Mennella, A., Mitra, S., Miville-Deschênes, M. -A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, A., Naselsky, P., Natoli, P., Netterfield, C. B., Nørgaard-Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., Osborne, S., Pajot, F., Pasian, F., Patanchon, G., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Pierpaoli, E., Piffaretti, R., Plaszczynski, S., Pointecouteau, E., Polenta, G., Ponthieu, N., Poutanen, T., Pratt, G. W., Prézeau, G., Prunet, S., Puget, J. -L., Rachen, J. P., Rebolo, R., Reinecke, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Rubiño-Martín, J. A., Rusholme, B., Sandri, M., Santos, D., Savini, G., Schaefer, B. M., Scott, D., Seiffert, M. D., Shellard, P., Smoot, G. F., Starck, J. -L., Stivoli, F., Stolyarov, V., Sudiwala, R., Sunyaev, R., Sygnet, J. -F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Torre, J. -P., Tristram, M., Tuovinen, J., Valenziano, L., Vibert, L., Vielva, P., Villa, F., Vittorio, N., Wade, L. A., Wandelt, B. D., White, S. D. M., White, M., Yvon, D., Zacchei, A., and Zonca, A.

Subjects

Astrophysics - Cosmology and Nongalactic Astrophysics

Abstract

We present precise Sunyaev-Zeldovich (SZ) effect measurements in the direction of 62 nearby galaxy clusters (z <0.5) detected at high signal-to-noise in the first Planck all-sky dataset. The sample spans approximately a decade in total mass, 10^14 < M_500 < 10^15, where M_500 is the mass corresponding to a total density contrast of 500. Combining these high quality Planck measurements with deep XMM-Newton X-ray data, we investigate the relations between D_A^2 Y_500, the integrated Compton parameter due to the SZ effect, and the X-ray-derived gas mass M_g,500, temperature T_X, luminosity L_X, SZ signal analogue Y_X,500 = M_g,500 * T_X, and total mass M_500. After correction for the effect of selection bias on the scaling relations, we find results that are in excellent agreement with both X-ray predictions and recently-published ground-based data derived from smaller samples. The present data yield an exceptionally robust, high-quality local reference, and illustrate Planck's unique capabilities for all-sky statistical studies of galaxy clusters., Comment: 14 pages, 6 figures, to appear in A&A; final version corrects values for A1413 and A3921 in Table 1

Published

2011

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25. Planck early results: Cluster Sunyaev-Zeldovich optical scaling relations

Author

Planck Collaboration, Aghanim, N., Arnaud, M., Ashdown, M., Aumont, J., Baccigalupi, C., Balbi, A., Banday, A. J., Barreiro, R. B., Bartelmann, M., 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., Brown, M. L., Bucher, M., Burigana, C., Cabella, P., Cardoso, J. -F., Catalano, A., Cayón, L., Challinor, A., Chamballu, A., Chiang, L. -Y, Chiang, C., Chon, G., Christensen, P. R., Churazov, E., Clements, D. L., Colafrancesco, S., Colombi, S., Couchot, F., Coulais, A., Crill, B. P., Cuttaia, F., Da Silva, A., Dahle, H., Danese, L., Davis, R. J., de Bernardis, P., de Gasperis, G., de Rosa, A., de Zotti, G., Delabrouille, J., Delouis, J. -M., Désert, F. -X., Diego, J. M., Dolag, K., Donzelli, S., Doré, O., Dörl, U., Douspis, M., Dupac, X., Efstathiou, G., Enßlin, T. A., Finelli, F., Flores, I., Forni, O., Frailis, M., Franceschi, E., Fromenteau, S., Galeotta, S., Ganga, K., Génova-Santos, R. T., Giard, M., Giardino, G., Giraud-Héraud, Y., González-Nuevo, J., Górski, K. M., Gratton, S., Gregorio, A., Gruppuso, A., Harrison, D., Henrot-Versillé, S., Hernández-Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hovest, W., Hoyland, R. J., Huffenberger, K. M., Jaffe, A. H., Jones, W. C., Juvela, M., Keihänen, E., Keskitalo, R., Kisner, T. S., Kneissl, R., Knox, L., Kurki-Suonio, H., Lagache, G., Lamarre, J. -M., Lasenby, A., Laureijs, R. J., Lawrence, C. R., Leach, S., Leonardi, R., Linden-Vørnle, M., López-Caniego, M., Lubin, P. M., Macías-Pérez, J. F., MacTavish, C. J., Maffei, B., Maino, D., Mandolesi, N., Mann, R., Maris, M., Marleau, F., Martínez-González, E., Masi, S., Matarrese, S., Matthai, F., Mazzotta, P., Mei, S., Melchiorri, A., Melin, J. -B., Mendes, L., Mennella, A., Mitra, S., Miville-Deschênes, M. -A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, A., Naselsky, P., Natoli, P., Netterfield, C. B., Nørgaard-Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., O'Dwyer, I. J., Osborne, S., Pajot, F., Pasian, F., Patanchon, G., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Pierpaoli, E., Piffaretti, R., Plaszczynski, S., Pointecouteau, E., Polenta, G., Ponthieu, N., Poutanen, T., Pratt, G. W., Prézeau, G., Prunet, S., Puget, J. -L., Rebolo, R., Reinecke, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Rubiño-Martín, J. A., Rusholme, B., Sandri, M., Savini, G., Schaefer, B. M., Scott, D., Seiffert, M. D., Shellard, P., Smoot, G. F., Starck, J. -L., Stivoli, F., Stolyarov, V., Sudiwala, R., Sunyaev, R., Sygnet, J. -F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Torre, J. -P., Tristram, M., Tuovinen, J., Valenziano, L., Vibert, L., Vielva, P., Villa, F., Vittorio, N., Wandelt, B. D., White, S. D. M., White, M., Yvon, D., Zacchei, A., and Zonca, A.

Subjects

Astrophysics - Cosmology and Nongalactic Astrophysics

Abstract

We present the Sunyaev-Zeldovich (SZ) signal-to-richness scaling relation (Y500-N200) for the MaxBCG cluster catalogue. Employing a multi-frequency matched filter on the Planck sky maps, we measure the SZ signal for each cluster by adapting the filter according to weak-lensing calibrated mass-richness relations (N200-M500). We bin our individual measurements and detect the SZ signal down to the lowest richness systems (N200=10) with high significance, achieving a detection of the SZ signal in systems with mass as low as M500~5e13 Msolar. The observed Y500-N200 relation is well modeled by a power law over the full richness range. It has a lower normalisation at given N200 than predicted based on X-ray models and published mass-richness relations. An X-ray subsample, however, does conform to the predicted scaling, and model predictions do reproduce the relation between our measured bin-average SZ signal and measured bin-average X-ray luminosities. At fixed richness, we find an intrinsic dispersion in the Y500-N200 relation of 60% rising to of order 100% at low richness. Thanks to its all-sky coverage, Planck provides observations for more than 13,000 MaxBCG clusters and an unprecedented SZ/optical data set, extending the list of known cluster scaling laws to include SZ-optical properties. The data set offers essential clues for models of galaxy formation. Moreover, the lower normalisation of the SZ-mass relation implied by the observed SZ-richness scaling has important consequences for cluster physics and cosmological studies with SZ clusters., Comment: Also available from this URL: http://www.rssd.esa.int

Published

2011

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26. Planck Early Results VIII: The all-sky Early Sunyaev-Zeldovich cluster sample

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., Bartelmann, M., Bartlett, J. G., Battaner, E., Battye, R., Benabed, K., Benoît, A., Bernard, J. -P., Bersanelli, M., Bhatia, R., Bock, J. J., Bonaldi, A., Bond, J. R., Borrill, J., Bouchet, F. R., Brown, M. L., Bucher, M., Burigana, C., Cabella, P., Cantalupo, C. M., Cardoso, J. -F., Carvalho, P., Catalano, A., Cayón, L., Challinor, A., Chamballu, A., Chary, R. -R., Chiang, L. -Y, Chiang, C., Chon, G., Christensen, P. R., Churazov, E., Clements, D. L., Colafrancesco, S., Colombi, S., Couchot, F., Coulais, A., Crill, B. P., Cuttaia, F., Da Silva, A., Dahle, H., Danese, L., 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., Diego, J. M., Dolag, K., Dole, H., Donzelli, S., Doré, O., Dörl, U., Douspis, M., Dupac, X., Efstathiou, G., Eisenhardt, P., Enßlin, T. A., Feroz, F., Finelli, F., Flores, I., Forni, O., Fosalba, P., Frailis, M., Franceschi, E., Fromenteau, S., Galeotta, S., Ganga, K., Génova-Santos, R. T., Giard, M., Giardino, G., Giraud-Héraud, Y., González-Nuevo, J., González-Riestra, R., Górski, K. M., Grainge, K. J. B., Gratton, S., Gregorio, A., Gruppuso, A., Harrison, D., Heinämäki, P., Henrot-Versillé, S., Hernández-Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hovest, W., Hoyland, R. J., Huffenberger, K. M., Hurier, G., Hurley-Walker, N., Jaffe, A. H., 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., Jeune, M. Le, Leach, S., Leonardi, R., Li, C., Liddle, A., Lilje, P. B., Linden-Vørnle, M., López-Caniego, M., Lubin, P. M., Macías-Pérez, J. F., MacTavish, C. J., Maffei, B., Maino, D., Mandolesi, N., Mann, R., Maris, M., Marleau, F., Martínez-González, E., Masi, S., Matarrese, S., Matthai, F., Mazzotta, P., Mei, S., Meinhold, P. R., Melchiorri, A., Melin, J. -B., Mendes, L., Mennella, A., Mitra, S., Miville-Deschênes, M. -A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, A., Naselsky, P., Nati, F., Natoli, P., Netterfield, C. B., Nørgaard-Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., Olamie, M., Osborne, S., Pajot, F., Pasian, F., Patanchon, G., Pearson, T. J., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Pierpaoli, E., Piffaretti, R., Plaszczynski, S., Pointecouteau, E., Polenta, G., Ponthieu, N., Poutanen, T., Pratt, G. W., Prézeau, G., Prunet, S., Puget, J. -L., Rachen, J. P., Reach, W. T., Rebolo, R., Reinecke, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Rubiño-Martín, J. A., Rusholme, B., Saar, E., Sandri, M., Santos, D., Saunders, R. D. E., Savini, G., Schaefer, B. M., Scott, D., Seiffert, M. D., Shellard, P., Smoot, G. F., Stanford, A., Starck, J. -L., Stivoli, F., Stolyarov, V., Stompor, R., Sudiwala, R., Sunyaev, R., Sutton, D., Sygnet, J. -F., Taburet, N., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Torre, J. -P., Tristram, M., Tuovinen, J., Valenziano, L., Vibert, L., Vielva, P., Villa, F., Vittorio, N., Wade, L. A., Wandelt, B. D., Weller, J., White, S. D. M., White, M., Yvon, D., Zacchei, A., and Zonca, A.

Subjects

Astrophysics - Cosmology and Nongalactic Astrophysics

Abstract

We present the first all-sky sample of galaxy clusters detected blindly by the Planck satellite through the Sunyaev-Zeldovich (SZ) effect from its six highest frequencies. This early SZ (ESZ) sample is comprised of 189 candidates, which have a high signal-to-noise ratio ranging from 6 to 29. Its high reliability (purity above 95%) is further ensured by an extensive validation process based on Planck internal quality assessments and by external cross-identification and follow-up observations. Planck provides the first measured SZ signal for about 80% of the 169 previously-known ESZ clusters. Planck furthermore releases 30 new cluster candidates, amongst which 20 meet the ESZ signal-to-noise selection criterion. At the submission date, twelve of the 20 ESZ candidates were confirmed as new clusters, with eleven confirmed using XMM-Newton snapshot observations, most of them with disturbed morphologies and low luminosities. The ESZ clusters are mostly at moderate redshifts (86% with z below 0.3) and span more than a decade in mass, up to the rarest and most massive clusters with masses above 10^15 Msol., Comment: Accepted for publication in a special issue of A&A, 26 pages, this paper is part of a package of papers describing first results of the Planck mission

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2011

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27. Planck Early Results. II. The thermal performance of Planck

Author

Planck Collaboration, Ade, P. A. R., Aghanim, N., Arnaud, M., Ashdown, M., Aumont, J., Baccigalupi, C., Baker, M., Balbi, A., Banday, A. J., Barreiro, R. B., Battaner, E., Benabed, K., Benoit, A., Bernard, J. P., Bersanelli, M., Bhandari, P., Bhatia, R., Bock, J. J., Bonaldi, A., Bond, J. R., Borders, J., Borrill, J., Bouchet, F. R., Bowman, B., Bradshaw, T., Breelle, E., Bucher, M., Burigana, C., Butler, R. C., Cabella, P., Camus, P., Cantalupo, C. M., Cappellini, B., Cardoso, J. F., Catalano, A., Cayon, L., Challinor, A., Chamballu, A., Chambelland, J. P., Charra, J., Charra, M., Chiang, L. Y, Chiang, C., Christensen, P. R., Clements, D. L., Collaudin, B., Colombi, S., Couchot, F., Coulais, A., Crill, B. P., Crook, M., Cuttaia, F., Damasio, C., Danese, L., Davies, R. D., Davis, R. J., de Bernardis, P., de Gasperis, G., de Rosa, A., Delabrouille, J., Delouis, J. M., Desert, F. -X., Doerl, U., Dolag, K., Donzelli, S., Dore, O., Douspis, M., Dupac, X., Efstathiou, G., Enslin, T. A., Eriksen, H. K., Finelli, F., Foley, S., Forni, O., Fosalba, P., Fourmond, J. J., Frailis, M., Franceschi, E., Galeotta, S., Ganga, K., Gavila, E., Giard, M., Giardino, G., Giraud-Heraud, Y., Gonzalez-Nuevo, J., Gorski, K. M., Gratton, S., Gregorio, A., Gruppuso, A., Guyot, G., Harrison, D., Helou, G., Henrot-Versille, S., Hernandez-Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hornstrup, A., Hovest, W., Hoyland, R. J., Huffenberger, K. M., Israelsson, U., Jaffe, A. H., Jones, W. C., Juvela, M., Keihanen, E., Keskitalo, R., Kisner, T. S., Kneissl, R., Knox, L., Kurki-Suonio, H., Lagache, G., Lamarre, J. M., Lami, P., Lasenby, A., Laureijs, R. J., Lawrence, C. R., Leach, S., Leonardi, R., Leroy, C., Lilje, P. B., Lopez-Caniego, M., Lubin, P. M., Macias-Perez, J. F., Maciaszek, T., MacTavish, C. J., Maffei, B., Maino, D., Mandolesi, N., Mann, R., Maris, M., Martinez-Gonzalez, E., Masi, S., Matarrese, S., Matthai, F., Mazzotta, P., McGehee, P., Meinhold, P. R., Melchiorri, A., Melot, F., Mendes, L., Mennella, A., Miville-Deschenes, M. -A., Moneti, A., Montier, L., Mora, J., Morgante, G., Morisset, N., Mortlock, D., Munshi, D., Murphy, A., Naselsky, P., Nash, A., Natoli, P., Netterfield, C. B., Novikov, D., Novikov, I., O'Dwyer, I. J., Osborne, S., Pajot, F., Pasian, F., Patanchon, G., Pearson, D., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Plaszczynski, S., Platania, P., Pointecouteau, E., Polenta, G., Ponthieu, N., Poutanen, T., Prezeau, G., Prina, M., Prunet, S., Puget, J. L., Rachen, J. P., Rebolo, R., Reinecke, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rosset, C., Rubiino-Martin, J. A., Rusholme, B., Sandri, M., Santos, D., Schaefer, B. M., Scott, D., Seiffert, M. D., Shellard, P., Smoot, G. F., Starck, J. -L., Stassi, P., Stivoli, F., Stolyarov, V., Stompor, R., Sudiwala, R., Sygnet, J. -F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Torre, J. -P., Tristram, M., Tuovinen, J., Valenziano, L., Vibert, L., Vielva, P., Villa, F., Vittorio, N., Wade, L. A., Wandelt, B. D., Watson, C., White, S. D. M., Wilkinson, A., Wilson, P., Yvon, D., Zacchei, A., Zhang, B., and Zonca, A.

Subjects

Astrophysics - Instrumentation and Methods for Astrophysics

Abstract

The performance of the Planck instruments in space is enabled by their low operating temperatures, 20K for LFI and 0.1K for HFI, achieved through a combination of passive radiative cooling and three active mechanical coolers. The scientific requirement for very broad frequency coverage led to two detector technologies with widely different temperature and cooling needs. Active coolers could satisfy these needs; a helium cryostat, as used by previous cryogenic space missions (IRAS, COBE, ISO, Spitzer, AKARI), could not. Radiative cooling is provided by three V-groove radiators and a large telescope baffle. The active coolers are a hydrogen sorption cooler (<20K), a 4He Joule-Thomson cooler (4.7K), and a 3He-4He dilution cooler (1.4K and 0.1K). The flight system was at ambient temperature at launch and cooled in space to operating conditions. The HFI bolometer plate reached 93mK on 3 July 2009, 50 days after launch. The solar panel always faces the Sun, shadowing the rest of Planck, andoperates at a mean temperature of 384K. At the other end of the spacecraft, the telescope baffle operates at 42.3K and the telescope primary mirror operates at 35.9K. The temperatures of key parts of the instruments are stabilized by both active and passive methods. Temperature fluctuations are driven by changes in the distance from the Sun, sorption cooler cycling and fluctuations in gas-liquid flow, and fluctuations in cosmic ray flux on the dilution and bolometer plates. These fluctuations do not compromise the science data., Comment: Accepted by A&A. Also available at http://www.rssd.esa.int

Published

2011

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28. Planck Early Results: The Planck mission

Author

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

Subjects

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

Abstract

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

Published

2011

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29. Planck early results XIV: ERCSC validation and extreme radio sources

Author

Planck Collaboration, Ade, P. A. R., Aghanim, N., Angelakis, E., Arnaud, M., Ashdown, M., Aumont, J., Baccigalupi, C., Balbi, A., Banday, A. J., Barreiro, R. B., Bartlett, J. G., Battaner, E., Benabed, K., Benoît, A., Bernard, J. P., Bersanelli, M., Bhatia, R., Bonaldi, A., Bonavera, L., Bond, J. R., Borrill, J., Bouchet, F. R., Bucher, M., Burigana, C., Cabella, P., Cappellini, B., Cardoso, J. F., Catalano, A., Cayón, L., Challinor, A., Chamballu, A., Chary, R. R., Chen, X., 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., Donzelli, S., Doré, O., Dörl, U., Douspis, M., Dupac, X., Efstathiou, G., Ensslin, T. A., Finelli, F., Forni, O., Frailis, M., Franceschi, E., Fuhrmann, L., Galeotta, S., Ganga, K., Giard, M., Giardino, G., Giraud-Héraud, Y., González-Nuevo, J., Górski, K. M., Gratton, S., Gregorio, A., Gruppuso, A., Harrison, D., Henrot-Versillé, S., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hovest, W., Hoyland, R. J., Huffenberger, K. M., Huynh, M., Jaffe, A. H., Juvela, M., Keihänen, E., Keskitalo, R., Kisner, T. S., Kneissl, R., Knox, L., Krichbaum, T. P., Kurki-Suonio, H., Lagache, G., Lähteenmäki, A., Lamarre, J. M., Lasenby, A., Laureijs, R. J., Lavonen, N., Lawrence, C. R., Leach, S., Leahy, J. P., Leonardi, R., Linden-Vørnle, M., López-Caniego, M., Lubin, P. M., Macías-Pérez, J. F., Maffei, B., Maino, D., Mandolesi, N., Mann, R., Maris, M., Marleau, F., Martínez-González, E., Masi, S., Massardi, M., Matarrese, S., Matthai, F., Mazzotta, P., Meinhold, P. R., Melchiorri, A., Mendes, L., Mennella, A., Mingaliev, M., Miville-Deschênes, M. A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, A., Naselsky, P., Natoli, P., Nestoras, I., Netterfield, C. B., Nieppola, E., Nørgaard-Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., Osborne, S., Pajot, F., Partridge, B., Pasian, F., Patanchon, G., Pearson, T. J., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Pierpaoli, E., Plaszczynski, S., Platania, P., Pointecouteau, E., Polenta, G., Ponthieu, N., Poutanen, T., Prézeau, G., Procopio, P., Prunet, S., Puget, J. L., Rachen, J. P., Reach, W. T., Rebolo, R., Reinecke, M., Renault, C., Ricciardi, S., Riller, T., Riquelme, D., Ristorcelli, I., Rocha, G., Rosset, C., Seiffert, D., Sievers, A., Smoot, G. F., Sotnikova, Y., Starck, J. L., Stivoli, F., Stolyarov, V., Sudiwala, R., Sygnet, J. F., Tammi, J., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Tornikoski, M., Torre, J. P., Tristram, M., Tuovinen, J., Türler, M., Turunen, M., Umana, G., Ungerechts, H., Valenziano, L., Varis, J., Vielva, P., Villa, F., Vittorio, N., Wade, L. A., Wandelt, B. D., Wilkinson, A., Yvon, D., Zacchei, A., Zensus, J. A., and Zonca, A.

Subjects

Astrophysics - Cosmology and Nongalactic Astrophysics

Abstract

Planck's all sky surveys at 30-857 GHz provide an unprecedented opportunity to follow the radio spectra of a large sample of extragalactic sources to frequencies 2-20 times higher than allowed by past, large area, ground-based surveys. We combine the results of the Planck Early Release Compact Source Catalog (ERCSC) with quasi-simultaneous ground-based observations, as well as archival data, at frequencies below or overlapping Planck frequency bands, to validate the astrometry and photometry of the ERCSC radio sources and study the spectral features shown in this new frequency window opened by Planck. The ERCSC source positions and flux density scales are found to be consistent with the ground-based observations. We present and discuss the spectral energy distributions (SEDs) of a sample of "extreme" radio sources to illustrate the richness of the ERCSC for the study of extragalactic radio sources. Variability is found to play a role in the unusual spectral features of some of these sources., Comment: Revised to accommodate referee's comments. Changes made to sections 5.1 and 5.4. No change in figures or scientific conclusions

Published

2011

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30. Maximum likelihood, parametric component separation and CMB B-mode detection in suborbital experiments

Author

Stivoli, F., Grain, J., Leach, S. M., Tristram, M., Baccigalupi, C., and Stompor, R.

Subjects

Astrophysics - Cosmology and Extragalactic Astrophysics

Abstract

We investigate the performance of the parametric Maximum Likelihood component separation method in the context of the CMB B-mode signal detection and its characterization by small-scale CMB suborbital experiments. We consider high-resolution (FWHM=8') balloon-borne and ground-based observatories mapping low dust-contrast sky areas of 400 and 1000 square degrees, in three frequency channels, 150, 250, 410 GHz, and 90, 150, 220 GHz, with sensitivity of order 1 to 10 micro-K per beam-size pixel. These are chosen to be representative of some of the proposed, next-generation, bolometric experiments. We study the residual foreground contributions left in the recovered CMB maps in the pixel and harmonic domain and discuss their impact on a determination of the tensor-to-scalar ratio, r. In particular, we find that the residuals derived from the simulated data of the considered balloon-borne observatories are sufficiently low not to be relevant for the B-mode science. However, the ground-based observatories are in need of some external information to permit satisfactory cleaning. We find that if such information is indeed available in the latter case, both the ground-based and balloon-borne experiments can detect the values of r as low as ~0.04 at 95% confidence level. The contribution of the foreground residuals to these limits is found to be then subdominant and these are driven by the statistical uncertainty due to CMB, including E-to-B leakage, and noise. We emphasize that reaching such levels will require a sufficient control of the level of systematic effects present in the data., Comment: 18 pages, 12 figures, 6 tables

Published

2010

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31. Planck pre-launch status: the Planck-LFI programme

Author

Mandolesi, N., Bersanelli, M., Butler, R. C., Artal, E., Baccigalupi, C., Balbi, A., Banday, A. J., Barreiro, R. B., Bartelmann, M., Bennett, K., Bhandari, P., Bonaldi, A., Borrill, J., Bremer, M., Burigana, C., Bowman, R. C., Cabella, P., Cantalupo, C., Cappellini, B., Courvoisier, T., Crone, G., Cuttaia, F., Danese, L., D'Arcangelo, O., Davies, R. D., Davis, R. J., De Angelis, L., de Gasperis, G., De Rosa, A., De Troia, G., de Zotti, G., Dick, J., Dickinson, C., Diego, J. M., Donzelli, S., Dörl, U., Dupac, X., Enßlin, T. A., Eriksen, H. K., Falvella, M. C., Finelli, F., Frailis, M., Franceschi, E., Gaier, T., Galeotta, S., Gasparo, F., Giardino, G., Gomez, F., Gonzalez-Nuevo, J., Górski, K. M., Gregorio, A., Gruppuso, A., Hansen, F., Hell, R., Herranz, D., Herreros, J. M., Hildebrandt, S., Hovest, W., Hoyland, R., Huffenberger, K., Janssen, M., Jaffe, T., Keihänen, E., Keskitalo, R., Kisner, T., Kurki-Suonio, H., Lähteenmäki, A., Lawrence, C. R., Leach, S. M., Leahy, J. P., Leonardi, R., Levin, S., Lilje, P. B., López-Caniego, M., Lowe, S. R., Lubin, P. M., Maino, D., Malaspina, M., Maris, M., Marti-Canales, J., Martinez-Gonzalez, E., Massardi, M., Matarrese, S., Matthai, F., Meinhold, P., Melchiorri, A., Mendes, L., Mennella, A., Morgante, G., Morigi, G., Morisset, N., Moss, A., Nash, A., Natoli, P., Nesti, R., Paine, C., Partridge, B., Pasian, F., Passvogel, T., Pearson, D., Pérez-Cuevas, L., Perrotta, F., Polenta, G., Popa, L. A., Poutanen, T., Prezeau, G., Prina, M., Rachen, J. P., Rebolo, R., Reinecke, M., Ricciardi, S., Riller, T., Rocha, G., Roddis, N., Rohlfs, R., Rubiño-Martin, J. A., Salerno, E., Sandri, M., Scott, D., Seiffert, M., Silk, J., Simonetto, A., Smoot, G. F., Sozzi, C., Sternberg, J., Stivoli, F., Stringhetti, L., Tauber, J., Terenzi, L., Tomasi, M., Tuovinen, J., Türler, M., Valenziano, L., Varis, J., Vielva, P., Villa, F., Vittorio, N., Wade, L., White, M., White, S., Wilkinson, A., Zacchei, A., and Zonca, A.

Subjects

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

Abstract

This paper provides an overview of the Low Frequency Instrument (LFI) programme within the ESA Planck mission. The LFI instrument has been developed to produce high precision maps of the microwave sky at frequencies in the range 27-77 GHz, below the peak of the cosmic microwave background (CMB) radiation spectrum. The scientific goals are described, ranging from fundamental cosmology to Galactic and extragalactic astrophysics. The instrument design and development are outlined, together with the model philosophy and testing strategy. The instrument is presented in the context of the Planck mission. The LFI approach to ground and inflight calibration is described. We also describe the LFI ground segment. We present the results of a number of tests demonstrating the capability of the LFI data processing centre (DPC) to properly reduce and analyse LFI flight data, from telemetry information to calibrated and cleaned time ordered data, sky maps at each frequency (in temperature and polarization), component emission maps (CMB and diffuse foregrounds), catalogs for various classes of sources (the Early Release Compact Source Catalogue and the Final Compact Source Catalogue). The organization of the LFI consortium is briefly presented as well as the role of the core team in data analysis and scientific exploitation. All tests carried out on the LFI flight model demonstrate the excellent performance of the instrument and its various subunits. The data analysis pipeline has been tested and its main steps verified. In the first three months after launch, the commissioning, calibration, performance, and verification phases will be completed, after which Planck will begin its operational life, in which LFI will have an integral part., Comment: 25 pages, 16 figures. In press on Astronomy and Astrophysics

Published

2010

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32. Component separation methods for the Planck mission

Author

Leach, S. M., Cardoso, J. -F., Baccigalupi, C., Barreiro, R. B., Betoule, M., Bobin, J., Bonaldi, A., Delabrouille, J., de Zotti, G., Dickinson, C., Eriksen, H. K., González-Nuevo, J., Hansen, F. K., Herranz, D., LeJeune, M., López-Caniego, M., Martinez-González, E., Massardi, M., Melin, J. -B., Miville-Deschênes, M. -A., Patanchon, G., Prunet, S., Ricciardi, S., Salerno, E., Sanz, J. L., Starck, J. -L., Stivoli, F., Stolyarov, V., Stompor, R., and Vielva, P.

Subjects

Astrophysics

Abstract

The Planck satellite will map the full sky at nine frequencies from 30 to 857 GHz. The CMB intensity and polarization that are its prime targets are contaminated by foreground emission. The goal of this paper is to compare proposed methods for separating CMB from foregrounds based on their different spectral and spatial characteristics, and to separate the foregrounds into components of different physical origin. A component separation challenge has been organized, based on a set of realistically complex simulations of sky emission. Several methods including those based on internal template subtraction, maximum entropy method, parametric method, spatial and harmonic cross correlation methods, and independent component analysis have been tested. Different methods proved to be effective in cleaning the CMB maps from foreground contamination, in reconstructing maps of diffuse Galactic emissions, and in detecting point sources and thermal Sunyaev-Zeldovich signals. The power spectrum of the residuals is, on the largest scales, four orders of magnitude lower than that of the input Galaxy power spectrum at the foreground minimum. The CMB power spectrum was accurately recovered up to the sixth acoustic peak. The point source detection limit reaches 100 mJy, and about 2300 clusters are detected via the thermal SZ effect on two thirds of the sky. We have found that no single method performs best for all scientific objectives. We foresee that the final component separation pipeline for Planck will involve a combination of methods and iterations between processing steps targeted at different objectives such as diffuse component separation, spectral estimation and compact source extraction., Comment: Matches version accepted by A&A. A version with high resolution figures is available at http://people.sissa.it/~leach/compsepcomp.pdf

Published

2008

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33. Maximum Likelihood algorithm for parametric component separation in CMB experiments

Author

Stompor, R., Leach, S., Stivoli, F., and Baccigalupi, C.

Subjects

Astrophysics

Abstract

We discuss an approach to the component separation of microwave, multi-frequency sky maps as those typically produced from Cosmic Microwave Background (CMB) Anisotropy data sets. The algorithm is based on the two step, parametric, likelihood-based technique recently elaborated on by Eriksen et al., (2006), where the foreground spectral parameters are estimated prior to the actual separation of the components. In contrast with the previous approaches, we accomplish the former task with help of an analytically-derived likelihood function for the spectral parameters, which, we show, yields estimates equal to the maximum likelihood values of the full multi-dimensional data problem. We then use these estimates to perform the second step via the standard, generalized-least-square-like procedure. We demonstrate that the proposed approach is equivalent to a direct maximization of the full data likelihood, which is recast in a computationally tractable form. We use the corresponding curvature matrices to characterize statistical properties of the recovered parameters. We incorporate in the formalism some of the essential features of the CMB data sets, such as inhomogeneous pixel domain noise, unknown map offsets as well as calibration errors and study their consequences for the separation. We find that the calibration is likely to have a dominant effect on the precision of the spectral parameter determination for a realistic CMB experiment. We apply the algorithm to simulated data and discuss the results. Our focus is on partial-sky, total-intensity and polarization, CMB experiments such as planned balloon-borne and ground-based efforts, however, the techniques presented here should be also applicable to the full-sky data as for instance, those produced by WMAP and anticipated from Planck., Comment: 18 pages, 8 figures, minor changes to match the published version

Published

2008

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34. WMAP 3yr data with the CCA: anomalous emission and impact of component separation on the CMB power spectrum

Author

Bonaldi, A., Ricciardi, S., Leach, S., Stivoli, F., Baccigalupi, C., and De Zotti, G.

Subjects

Astrophysics

Abstract

The Correlated Component Analysis (CCA) allows us to estimate how the different diffuse emissions mix in CMB experiments, exploiting also complementary information from other surveys. It is especially useful to deal with possible additional components. An application of CCA to WMAP maps assuming that only the canonical Galactic emissions are present, highlights the widespread presence of a spectrally flat "synchrotron" component, largely uncorrelated with the synchrotron template, suggesting that an additional foreground is indeed required. We have tested various spectral shapes for such component, namely a power law as expected if it is flat synchrotron, and two spectral shapes that may fit the spinning dust emission: a parabola in the logS - log(frequency) plane, and a grey body. Quality tests applied to the reconstructed CMB maps clearly disfavour two of the models. The CMB power spectra, estimated from CMB maps reconstructed exploiting the three surviving foreground models, are generally consistent with the WMAP ones, although at least one of them gives a significantly higher quadrupole moment than found by the WMAP team. Taking foreground modeling uncertainties into account, we find that the mean quadrupole amplitude for the three "good" models is less than 1 sigma below the expectation from the standard LambdaCDM model. Also the other reported deviations from model predictions are found not to be statistically significant, except for the excess power at l~40. We confirm the evidence for a marked North-South asymmetry in the large scale (l < 20) CMB anisotropies. We also present a first, albeit preliminary, all-sky map of the "anomalous" component., Comment: 14 pages, 17 figures, submitted to MNRAS, references added

Published

2007

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35. CMB signal in WMAP 3yr data with FastICA

Author

Maino, D., Donzelli, S., Banday, A. J., Stivoli, F., and Baccigalupi, C.

Subjects

Astrophysics

Abstract

We present an application of the fast Independent Component Analysis (FastICA) to the WMAP 3yr data with the goal of extracting the CMB signal. We evaluate the confidence of our results by means of Monte Carlo simulations including CMB, foreground contaminations and instrumental noise specific of each WMAP frequency band. We perform a complete analysis involving all or a subset of the WMAP channels in order to select the optimal combination for CMB extraction, using the frequency scaling of the reconstructed component as a figure of merit. We found that the combination KQVW provides the best CMB frequency scaling, indicating that the low frequency foreground contamination in Q, V and W bands is better traced by the emission in the K band. The CMB angular power spectrum is recovered up to the degree scale, it is consistent within errors for all WMAP channel combination considered, and in close agreement with the WMAP 3yr results. We perform a statistical analysis of the recovered CMB pattern, and confirm the sky asymmetry reported in several previous works with independent techniques., Comment: 10 pages, 7 figures, submitted to MNRAS

Published

2006

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35 results on '"Stivoli, F"'

1. Planck Intermediate Results. IX. Detection of the Galactic haze with Planck

2. Planck intermediate results. X. Physics of the hot gas in the Coma cluster

3. Planck Intermediate Results. IV. The XMM-Newton validation programme for new Planck galaxy clusters

4. Planck intermediate results. III. The relation between galaxy cluster mass and Sunyaev-Zeldovich signal

5. Planck Intermediate Results II: Comparison of Sunyaev-Zeldovich measurements from Planck and from the Arcminute Microkelvin Imager for 11 galaxy clusters

6. Planck Intermediate Results. I. Further validation of new Planck clusters with XMM-Newton

7. Estimating the tensor-to-scalar ratio and the effect of residual foreground contamination

8. Planck early results. XV. Spectral energy distributions and radio continuum spectra of northern extragalactic radio sources

9. Planck Early Results: Statistical properties of extragalactic radio sources in the Planck Early Release Compact Source Catalogue

10. Planck Early Results: Thermal dust in Nearby Molecular Clouds

11. Planck Early Results: The submillimetre properties of a sample of Galactic cold clumps

12. Planck early results. XX. New light on anomalous microwave emission from spinning dust grains

13. Planck Early Results. X. Statistical analysis of Sunyaev-Zeldovich scaling relations for X-ray galaxy clusters

14. Planck Early Results: The Planck View of Nearby Galaxies

15. Planck Early Results: Origin of the submm excess dust emission in the Magellanic Clouds

16. Planck Early Results. VII. The Early Release Compact Source Catalog

17. Planck Early Results. V. The Low Frequency Instrument data processing

18. Planck Early Results XXIV: Dust in the diffuse interstellar medium and the Galactic halo

19. Planck early results. XXI. Properties of the interstellar medium in the Galactic plane

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

21. Planck early results. IX. XMM-Newton follow-up for validation of Planck cluster candidates

22. Planck Early Results XVIII: The power spectrum of cosmic infrared background anisotropies

23. Planck Early Results: All sky temperature and dust optical depth from Planck and IRAS: Constraints on the 'dark gas' in our galaxy

24. Planck Early Results XI: Calibration of the local galaxy cluster Sunyaev-Zeldovich scaling relations

25. Planck early results: Cluster Sunyaev-Zeldovich optical scaling relations

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27. Planck Early Results. II. The thermal performance of Planck

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29. Planck early results XIV: ERCSC validation and extreme radio sources

30. Maximum likelihood, parametric component separation and CMB B-mode detection in suborbital experiments

31. Planck pre-launch status: the Planck-LFI programme

32. Component separation methods for the Planck mission

33. Maximum Likelihood algorithm for parametric component separation in CMB experiments

34. WMAP 3yr data with the CCA: anomalous emission and impact of component separation on the CMB power spectrum

35. CMB signal in WMAP 3yr data with FastICA

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