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857 results on '"SMOOT, G. F."'

1. A uniform stellar origin for binary black holes revealed by lensing

Author

Broadhurst, T., Diego, J. M., and Smoot, G. F.

Subjects
Astrophysics - Astrophysics of Galaxies, Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, General Relativity and Quantum Cosmology
Abstract

Although most gravitational wave events are claimed to be mergers of unusually massive, $25-65M_\odot$, black holes, it is now clear that 20\% of all reported events comprise modest mass black holes, $5-15M_\odot$, like the stellar black holes in the Milky Way. We show that such stellar mass black hole binaries (BBH) if magnified by lensing galaxies can be detected at high redshift, 1$< $z$ <$5, with chirp masses increased by $1+z$, accounting for the majority of apparently high mass BBH events. This simple lensing explanation is manifested by the evident bimodality of BBH chirp masses now visible, with 80\% of BBH events in a broad peak centered on $m_{chirp} \simeq 35M_\odot$, and 20\% of BBH events in a narrow, low mass peak at $m_{chirp} \simeq 8.5M_\odot$, matching well our prediction for lensed and unlensed events respectively. This lensing interpretation is reinforced by the "graveyard plot" when ranked by chirp mass, revealing a jump in chirp mass at $m_{chirp} \simeq 10M_\odot$ that we show is caused by the large redshift difference between unlensed events with $z<0.3$ and lensed events above $z>1$. Furthermore, nearly all BBH events are seen to share a component mass ratio of $m_1/m_2=1.45\pm0.03$, indicating a common stellar origin for BBH events across all chirp masses. This observed component mass uniformity implies most binary black holes seldom pair up by random capture, instead we may conclude that massive progenitor stars of BBH black holes typically formed in-situ, in a well defined way over the full span of cosmic time accessed through gravitational lensing., Comment: 7 pages, 5 figures

Published
2022

2. A Distant Origin For Magnified LIGO/Virgo Black Holes Implied By Binary Component Masses

Author

Broadhurst, T., Diego, J. M., and Smoot, G. F.

Subjects
General Relativity and Quantum Cosmology, Astrophysics - High Energy Astrophysical Phenomena
Abstract

The primary and secondary masses of the binary black holes (BBH) reported by LIGO/Virgo are correlated with a narrow dispersion that appears to increase in proportion to mass. The mean binary mass ratio $1.45\pm0.07$ we show is consistent with pairs drawn randomly from the mass distribution of black holes in our Galaxy. However, BBH masses are concentrated around $\simeq 30M_\odot$, whereas black holes in our Galaxy peak at $\simeq 10M_\odot$. This mass difference can be reconciled by gravitational lensing magnification which allows distant events to be detected with typically $z\simeq 2$, so the waveform is reduced in frequency by $1+z$, and hence the measured chirp masses appear 3 times larger than their intrinsic values. This redshift enhancement also accounts for the dispersion of primary and secondary masses, both of which should increase as $1+z$, thereby appearing to scale with mass, in agreement with the data. Thus the BBH component masses provide independent support for lensing, implying most high chirp mass events have intrinsic masses like the stellar mass black holes in our Galaxy, coalescing at $z>1$, with only two low mass BBH detections, of $\simeq 10M_\odot$ as expected for unlensed events in the local Universe, $z\simeq 0.1$. This lensing solution requires a rapidly declining BBH event rate below $z<1$, which together with the observed absence of BBH spin suggests most events originate within young globular clusters at $z>1$, via efficient binary capture of stellar mass black holes with randomly oriented spins., Comment: 2 figures

Published
2020

3. Observational signatures of microlensing in gravitational waves at LIGO/Virgo frequencies

Author

Diego, J. M., Hannuksela, O. A., Kelly, P. L., Broadhurst, T., Kim, K., Li, T. G. F., and Smoot, G. F.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

Microlenses with typical stellar masses (a few ${\rm M}_{\odot}$) have traditionally been disregarded as potential sources of gravitational lensing effects at LIGO/Virgo frequencies, since the time delays are often much smaller than the inverse of the frequencies probed by LIGO/Virgo, resulting in negligible interference effects at LIGO/Virgo frequencies. While this is true for isolated microlenses in this mass regime, we show how, under certain circumstances and for realistic scenarios, a population of microlenses (for instance stars and remnants from a galaxy halo or from the intracluster medium) embedded in a macromodel potential (galaxy or cluster) can conspire together to produce time delays of order one millisecond which would produce significant interference distortions in the observed strains. At sufficiently large magnification factors (of several hundred), microlensing effects should be common in gravitationally lensed gravitational waves. We explore the regime where the predicted signal falls in the frequency range probed by LIGO/Virgo. We find that stellar mass microlenses, permeating the lens plane, and near critical curves, can introduce interference distortions in strongly lensed gravitational waves. For those lensed events with negative parity, (or saddle points, never studied before in the context of gravitational waves), and that take place near caustics of macromodels, they are more likely to produce measurable interference effects at LIGO/Virgo frequencies. This is the first study that explores the effect of a realistic population of microlenses, plus a macromodel, on strongly lensed gravitational waves., Comment: 16 pages

Published
2019
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4. Hydrodynamic simulations of the interaction of supernova shock waves with a clumpy environment: the case of the RX J0852.0-4622 (Vela Jr) supernova remnant

Author

Obergaulinger, M., Iyudin, A., Müller, E., and Smoot, G. F.

Subjects
Astrophysics - Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

Observations in all electromagnetic bands show that many supernova remnants (SNRs) have a very aspherical shape. This can be the result of asymmetries in the supernova explosion or a clumpy circumstellar medium. We study the generation of inhomogeneities and the mixing of elements arising from these two sources in multidimensional hydrodynamic simulations of the propagation of a supernova blast wave into a cloudy environment. We model a specific SNR, Vela Jr (RX J0852.0-4622). By comparing our results with recent observations, we can constrain the properties of the explosion. We find that a very energetic explosion of several 10^{51} erg occurring roughly about 800 years ago is consistent with the shape and emission of the SNR, as well as a supernova with an energy closer to the canonical value of 10^{51} erg a few thousand years ago., Comment: 18 pages, 13 figures

Published
2014
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5. Planck 2013 results. XIV. Zodiacal emission

Author

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

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The Planck satellite provides a set of all-sky maps at nine frequencies from 30 GHz to 857 GHz. Planets, minor bodies, and diffuse interplanetary dust emission (IPD) are all observed. The IPD can be separated from Galactic and other emissions because Planck views a given point on the celestial sphere multiple times, through different columns of IPD. We use the Planck data to investigate the behaviour of zodiacal emission over the whole sky at sub-millimetre and millimetre wavelengths. We fit the Planck data to find the emissivities of the various components of the COBE zodiacal model -- a diffuse cloud, three asteroidal dust bands, a circumsolar ring, and an Earth-trailing feature. The emissivity of the diffuse cloud decreases with increasing wavelength, as expected from earlier analyses. The emissivities of the dust bands, however, decrease less rapidly, indicating that the properties of the grains in the bands are different from those in the diffuse cloud. We fit the small amount of Galactic emission seen through the telescope's far sidelobes, and place limits on possible contamination of the CMB results from both zodiacal and far-sidelobe emission. When necessary, the results are used in the Planck pipeline to make maps with zodiacal emission and far sidelobes removed. We show that the zodiacal correction to the CMB maps is small compared to the Planck CMB temperature power spectrum and give a list of flux densities for small Solar System bodies.

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

Author

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

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

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

Published
2013
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7. Feasibility of a Small, Rapid Optical-to-IR Response, Next Generation Gamma Ray Burst Mission

Author

Grossan, B., Smoot, G. F., Bogomolov, V. V., Svertilov, S. I., Vedenkin, N. N., Panasyuk, M., Goncharov, B., Rozhkov, G., Saleev, K., Grobovskoj, E., Krasnov, A. S., Morozenko, V. S., Osedlo, V. I., Rogkov, E., Vachenko, T. V., and Linder, E. V.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

We present motivations for and study feasibility of a small, rapid optical to IR response gamma ray burst (GRB) space observatory. By analyzing existing GRB data, we give realistic detection rates for X-ray and optical/IR instruments of modest size under actual flight conditions. Given new capabilities of fast optical/IR response (about 1 s to target) and simultaneous multi-band imaging, such an observatory can have a reasonable event rate, likely leading to new science. Requiring a Swift-like orbit, duty cycle, and observing constraints, a Swift-BAT scaled down to 190 square cm of detector area would still detect and locate about 27 GRB per yr. for a trigger threshold of 6.5 sigma. About 23 percent of X-ray located GRB would be detected optically for a 10 cm diameter instrument (about 6 per yr. for the 6.5 sigma X-ray trigger)., Comment: Elaborated text version of a poster presented at 2012 Malaga/Marbella symposium

Published
2012
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8. Planck intermediate results. VIII. Filaments between interacting clusters

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., Bhatia, R., Bikmaev, I., Böhringer, H., Bonaldi, A., Bond, J. R., Borrill, J., Bouchet, F. R., Bourdin, H., Burenin, R., Burigana, C., Cabella, P., Cardoso, J. -F., Castex, G., Catalano, A., Cayón, L., Chamballu, A., Chary, R. -R., Chiang, L. -Y, Chon, G., Christensen, P. R., Clements, D. L., Colafrancesco, S., Colombo, L. P. L., Comis, B., Coulais, A., Crill, B. P., Cuttaia, F., Da Silva, A., Dahle, H., Danese, L., 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., Dörl, U., 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., Gilfanov, M., Giraud-Héraud, Y., González-Nuevo, J., 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., Hovest, W., Hurier, G., Jaffe, T. R., Jaffe, A. H., Jagemann, T., Jones, W. C., Juvela, M., Khamitov, I., Kisner, T. S., Kneissl, R., Knoche, J., Knox, L., Kunz, M., Kurki-Suonio, H., Lagache, G., 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., Luzzi, G., Macías-Pérez, J. F., Maffei, B., Maino, D., Mandolesi, N., Maris, M., Marleau, F., Marshall, D. J., 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., Nati, F., Natoli, P., Nørgaard-Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., Osborne, S., Pajot, F., Paoletti, D., 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., 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., Rusholme, B., Sandri, M., Savini, G., Schaefer, B. M., Scott, D., Smoot, G. F., Starck, J. -L., 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., White, S. D. M., Yvon, D., Zacchei, A., and Zonca, A.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

About half of the baryons of the Universe are expected to be in the form of filaments of hot and low density intergalactic medium. Most of these baryons remain undetected even by the most advanced X-ray observatories which are limited in sensitivity to the diffuse low density medium. The Planck satellite has provided hundreds of detections of the hot gas in clusters of galaxies via the thermal Sunyaev-Zel'dovich (tSZ) effect and is an ideal instrument for studying extended low density media through the tSZ effect. In this paper we use the Planck data to search for signatures of a fraction of these missing baryons between pairs of galaxy clusters. Cluster pairs are good candidates for searching for the hotter and denser phase of the intergalactic medium (which is more easily observed through the SZ effect). Using an X-ray catalogue of clusters and the Planck data, we select physical pairs of clusters as candidates. Using the Planck data we construct a local map of the tSZ effect centered on each pair of galaxy clusters. ROSAT data is used to construct X-ray maps of these pairs. After having modelled and subtracted the tSZ effect and X-ray emission for each cluster in the pair we study the residuals on both the SZ and X-ray maps. For the merging cluster pair A399-A401 we observe a significant tSZ effect signal in the intercluster region beyond the virial radii of the clusters. A joint X-ray SZ analysis allows us to constrain the temperature and density of this intercluster medium. We obtain a temperature of kT = 7.1 +- 0.9, keV (consistent with previous estimates) and a baryon density of (3.7 +- 0.2)x10^-4, cm^-3. The Planck satellite mission has provided the first SZ detection of the hot and diffuse intercluster gas., Comment: Accepted by A&A

Published
2012
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9. 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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10. 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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11. A next generation Ultra-Fast Flash Observatory (UFFO-100) for IR/optical observations of the rise phase of gamma-ray bursts

Author

Grossan, B., Park, I. H., Ahmad, S., Ahn, K. B., Barrillon, P., Brandt, S., Budtz-Jørgensen, C., Castro-Tirado, A. J., Chen, P., Choi, H. S., Choi, Y. J., Connell, P., Dagoret-Campagne, S., De La Taille, C., Eyles, C., Hermann, I., Huang, M. -H. A., Jung, A., Jeong, S., Kim, J. E., Kim, M., Kim, S. -W., Kim, Y. W., Lee, J., Lim, H., Linder, E. V., Liu, T. -C., Lund, N., Min, K. W., Na, G. W., Nam, J. W., Panasyuk, M. I., Ripa, J., Reglero, V., Rodrigo, J. M., Smoot, G. F., Suh, J. E., Svertilov, S., Vedenkin, N., Wang, M. -Z., Yashin, I., and Zhao, M. H.

Subjects
Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

The Swift Gamma-ray Burst (GRB) observatory responds to GRB triggers with optical observations in ~ 100 s, but cannot respond faster than ~ 60 s. While some ground-based telescopes respond quickly, the number of sub-60 s detections remains small. In mid- to late-2013, the Ultra-Fast Flash Observatory-Pathfinder is to be launched on the Lomonosov spacecraft to investigate early optical GRB emission. This pathfinder mission is necessarily limited in sensitivity and event rate; here we discuss a next generation rapid-response space observatory. We list science topics motivating our instruments, those that require rapid optical-IR GRB response, including: A survey of GRB rise shapes/times, measurements of optical bulk Lorentz factors, investigation of magnetic dominated (vs. non-magnetic) jet models, internal vs. external shock origin of prompt optical emission, the use of GRBs for cosmology, and dust evaporation in the GRB environment. We also address the impacts of the characteristics of GRB observing on our instrument and observatory design. We describe our instrument designs and choices for a next generation observatory as a second instrument on a low-earth orbit spacecraft, with a 120 kg instrument mass budget. Restricted to relatively modest mass and power, we find that a coded mask X-ray camera with 1024 cm2 of detector area could rapidly locate about 64 GRB triggers/year. Responding to the locations from the X-ray camera, a 30 cm aperture telescope with a beam-steering system for rapid (~ 1 s) response and a near-IR camera should detect ~ 29 GRB, given Swift GRB properties. Am additional optical camera would give a broadband optical-IR slope, allowing dynamic measurement of dust extinction at the source, for the first time., Comment: 12 pages, 11 figures, submitted to SPIE 2012 Amsterdam conference proceedings

Published
2012
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12. Planck intermediate results. VII. Statistical properties of infrared and radio extragalactic sources from the Planck Early Release Compact Source Catalogue at frequencies between 100 and 857 GHz

Author

Planck Collaboration, Ade, P. A. R., Aghanim, N., Argüeso, F., Arnaud, M., Ashdown, M., Atrio-Barandela, F., Aumont, J., Baccigalupi, C., Balbi, A., Banday, A. J., Barreiro, R. B., Battaner, E., Benabed, K., Benoît, A., Bernard, J. -P., Bersanelli, M., Bethermin, M., Bhatia, R., Bonaldi, A., Bond, J. R., Borrill, J., Bouchet, F. R., Burigana, C., Cabella, P., Cardoso, J. -F., Catalano, A., Cayón, L., Chamballu, A., Chary, R. -R., Chen, X., Chiang, L. -Y, Christensen, P. R., Clements, D. L., Colafrancesco, S., Colombi, S., Colombo, L. P. L., Coulais, A., Crill, B. P., Cuttaia, F., Danese, L., Davis, R. J., de Bernardis, P., de Gasperis, G., de Zotti, G., Delabrouille, J., Dickinson, C., Diego, J. M., 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., 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., Jaffe, T. R., Jaffe, A. H., Jagemann, T., Jones, W. C., Juvela, M., Keihänen, E., Kisner, T. S., Kneissl, R., Knoche, J., Knox, L., Kunz, M., Kurinsky, N., Kurki-Suonio, H., Lagache, G., Lähteenmäki, A., Lamarre, J. -M., Lasenby, A., Lawrence, C. R., Leonardi, R., Lilje, P. B., López-Caniego, M., Macías-Pérez, J. F., Maino, D., Mandolesi, N., Maris, M., Marshall, D. J., Martínez-González, E., Masi, S., Massardi, M., Matarrese, S., 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, J. A., Naselsky, P., Nati, F., Natoli, P., Nørgaard-Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., Osborne, S., Pajot, F., Paladini, R., Paoletti, D., Partridge, B., Pasian, F., Patanchon, G., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Piat, M., Pierpaoli, E., Plaszczynski, S., Pointecouteau, E., Polenta, G., Ponthieu, N., Popa, L., Poutanen, T., Pratt, G. W., 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., Savini, G., Scott, D., Smoot, G. F., Starck, J. -L., Sudiwala, R., Suur-Uski, A. -S., Sygnet, J. -F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Tucci, M., Türler, M., 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 - Cosmology and Nongalactic Astrophysics
Abstract

(abridged for arXiv) We make use of the Planck all-sky survey to derive number counts and spectral indices of extragalactic sources -- infrared and radio sources -- from the Planck Early Catalogue (ERCSC) at 100 to 857GHz. Our sample contains, after the 80% completeness cut, between 122 and 452 and sources, with flux densities above 0.3 and 1.9Jy at 100 and 857GHz, over about 31 to 40% of the sky. Using Planck HFI, all the sources have been classified as either dust-dominated or synchrotron-dominated on the basis of their spectral energy distributions (SED). Our sample is thus complete, flux-limited and color-selected to differentiate between the two populations. We find an approximately equal number of synchrotron and dusty sources between 217 and 353GHz; at 353GHz or higher (or 217GHz and lower) frequencies, the number is dominated by dusty (synchrotron) sources, as expected. For most of the sources, the spectral indices are also derived. We provide for the first time counts of bright sources from 353 to 857GHz and the contributions from dusty and synchrotron sources at all HFI frequencies in the key spectral range where these spectra are crossing. The observed counts are in the Euclidean regime. The number counts are compared to previously published data (earlier Planck, Herschel, BLAST, SCUBA, LABOCA, SPT, and ACT) and models taking into account both radio or infrared galaxies. We derive the multi-frequency Euclidean level and compare it to WMAP, Spitzer and IRAS results. The submillimetre number counts are not well reproduced by current evolution models of dusty galaxies, whereas the millimetre part appears reasonably well fitted by the most recent model for synchrotron-dominated sources. Finally we provide estimates of the local luminosity density of dusty galaxies, providing the first such measurements at 545 and 857GHz., Comment: in press, A&A, 2013 -- matches published version (updated text for clarity after referee's report; conclusions unchanged) 20 pages (2 column), 14 figs (+3 in appendix), 9 tables

Published
2012
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13. Planck Intermediate Results. V. Pressure profiles of galaxy clusters from the Sunyaev-Zeldovich effect

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., Benoit, A., Bernard, J. -P., Bersanelli, M., Bhatia, R., Bikmaev, I., Boehringer, H., Bonaldi, A., Bond, J. R., Borgani, S., Borrill, J., Bouchet, F. R., Bourdin, H., Brown, M. L., Burenin, R., Burigana, C., Cabella, P., Cardoso, J. -F., Carvalho, P., Castex, G., Catalano, A., Cayon, L., Chamballu, A., Chiang, L. -Y, Chon, G., Christensen, P. R., Churazov, E., Clements, D. L., Colafrancesco, S., Colombi, S., Colombo, L. P. L., Comis, B., Coulais, A., Crill, B. P., Cuttaia, F., Da Silva, A., Dahle, H., Danese, L., Davis, R. J., de Bernardis, P., de Gasperis, G., de Zotti, G., Delabrouille, J., Democles, J., Desert, F. -X., Diego, J. M., Dolag, K., Dole, H., Donzelli, S., Dore, O., Dorl, U., Douspis, M., Dupac, X., Efstathiou, G., Ensslin, T. A., Eriksen, H. K., Finelli, F., Flores-Cacho, I., Forni, O., Fosalba, P., Frailis, M., Franceschi, E., Frommert, M., Galeotta, S., Ganga, K., Genova-Santos, R. T., Giard, M., Giraud-Heraud, Y., Gonzalez-Nuevo, J., Gorski, K. M., Gregorio, A., Gruppuso, A., Hansen, F. K., Harrison, D., Hempel, A., Henrot-Versille, S., Hernandez-Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hurier, G., Jaffe, T. R., Jaffe, A. H., Jagemann, T., Jones, W. C., Juvela, M., Keihanen, E., Khamitov, I., Kisner, T. S., Kneissl, R., Knoche, J., Knox, L., Kunz, M., Kurki-Suonio, H., Lagache, G., Lahteenmaki, A., Lamarre, J. -M., Lasenby, A., Lawrence, C. R., Jeune, M. Le, Leonardi, R., Liddle, A., Lilje, P. B., Lopez-Caniego, M., Luzzi, G., Macias-Perez, J. F., Maino, D., Mandolesi, N., Maris, M., Marleau, F., Marshall, D. J., Martinez-Gonzalez, E., Masi, S., Massardi, M., Matarrese, S., Mazzotta, P., Mei, S., Melchiorri, A., Melin, J. -B., Mendes, L., Mennella, A., Mitra, S., Miville-Deschaines, M. -A., Moneti, A., Montier, L., Morgante, G., Mortlock, D., Munshi, D., Murphy, J. A., Naselsky, P., Nati, F., Natoli, P., Norgaard-Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., Osborne, S., Pajot, F., Paoletti, D., 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., Popa, L., Poutanen, T., Pratt, G. W., Prunet, S., Puget, J. -L., Rachen, J. P., Reach, W. T., Rebolo, R., Reinecke, M., Remazeilles, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Roman, M., Rosset, C., Rossetti, M., Rubino-Martin, J. A., Rusholme, B., Sandri, M., Savini, G., Scott, D., Smoot, G. F., Starck, J. -L., 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., 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., White, M., Yvon, D., Zacchei, A., and Zonca, A.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

Taking advantage of the all-sky coverage and broad frequency range of the Planck satellite, we study the Sunyaev-Zeldovich (SZ) and pressure profiles of 62 nearby massive clusters detected at high significance in the 14-month nominal survey. Careful reconstruction of the SZ signal indicates that most clusters are individually detected at least out to R500. By stacking the radial profiles, we have statistically detected the radial SZ signal out to 3 x R500, i.e., at a density contrast of about 50-100, though the dispersion about the mean profile dominates the statistical errors across the whole radial range. Our measurement is fully consistent with previous Planck results on integrated SZ fluxes, further strengthening the agreement between SZ and X-ray measurements inside R500. Correcting for the effects of the Planck beam, we have calculated the corresponding pressure profiles. This new constraint from SZ measurements is consistent with the X-ray constraints from XMM-Newton in the region in which the profiles overlap (i.e., [0.1-1]R500), and is in fairly good agreement with theoretical predictions within the expected dispersion. At larger radii the average pressure profile is slightly flatter than most predictions from numerical simulations. Combining the SZ and X-ray observed profiles into a joint fit to a generalised pressure profile gives best-fit parameters [P0, c500, gamma, alpha, beta] = [6.41, 1.81, 0.31, 1.33, 4.13]. Using a reasonable hypothesis for the gas temperature in the cluster outskirts we reconstruct from our stacked pressure profile the gas mass fraction profile out to 3 x R500. Within the temperature driven uncertainties, our Planck constraints are compatible with the cosmic baryon fraction and expected gas fraction in halos., Comment: 24 pages, 15 figures, accepted for publication in A&A

Published
2012
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14. Planck intermediate results. VI: The dynamical structure of PLCKG214.6+37.0, a Planck discovered triple system of galaxy clusters

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., Bhatia, R., Böhringer, H., Bonaldi, A., Bond, J. R., Borrill, J., Bouchet, F. R., Bourdin, H., Burigana, C., Cabella, P., Cardoso, J. -F., Castex, G., Catalano, A., Cayón, L., Chamballu, A., Chiang, L. -Y, Chon, G., Christensen, P. R., Clements, D. L., Colafrancesco, S., Colombi, S., Colombo, L. P. L., Comis, B., Coulais, A., Crill, B. P., Cuttaia, F., Da Silva, A., Dahle, H., Danese, L., Davis, R. J., de Bernardis, P., de Gasperis, G., de Zotti, G., Delabrouille, J., 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., Flores-Cacho, I., Forni, O., Frailis, M., Franceschi, E., Frommert, M., Galeotta, S., Ganga, K., Génova-Santos, R. T., Giard, M., Gilfanov, M., Giraud-Héraud, Y., González-Nuevo, J., Górski, K. M., Gregorio, A., Gruppuso, A., Hansen, F. K., Harrison, D., Heinämäki, P., Hempel, A., Henrot-Versillé, S., Hernández-Monteagudo, C., Herranz, D., Hildebrandt, S. R., Hivon, E., Hobson, M., Holmes, W. A., Hurier, G., Jaffe, T. R., Jaffe, A. H., Jagemann, T., Jones, W. C., Juvela, M., Keihänen, E., Kisner, T. S., 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., 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., Massardi, M., Matarrese, S., 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, J. A., Naselsky, P., Nati, F., Natoli, P., Nørgaard-Nielsen, H. U., Noviello, F., Osborne, S., Pajot, F., Paoletti, D., 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., 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., Rusholme, B., Sandri, M., Savini, G., Scott, D., Smoot, G. F., Starck, J. -L., 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., Valenziano, L., Van Tent, B., Vielva, P., Villa, F., Vittorio, N., Wade, L. A., Wandelt, B. D., Welikala, N., Yvon, D., Zacchei, A., Zaroubi, S., and Zonca, A.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The survey of galaxy clusters performed by Planck through the Sunyaev-Zeldovich effect has already discovered many interesting objects, thanks to the whole coverage of the sky. One of the SZ candidates detected in the early months of the mission near to the signal to noise threshold, PLCKG214.6+37.0, was later revealed by XMM-Newton to be a triple system of galaxy clusters. We have further investigated this puzzling system with a multi-wavelength approach and we present here the results from a deep XMM-Newton re-observation. The characterisation of the physical properties of the three components has allowed us to build a template model to extract the total SZ signal of this system with Planck data. We partly reconciled the discrepancy between the expected SZ signal from X-rays and the observed one, which are now consistent at less than 1.2 sigma. We measured the redshift of the three components with the iron lines in the X-ray spectrum, and confirmed that the three clumps are likely part of the same supercluster structure. The analysis of the dynamical state of the three components, as well as the absence of detectable excess X-ray emission, suggest that we are witnessing the formation of a massive cluster at an early phase of interaction., Comment: Submitted to Astronomy & Astrophysics

Published
2012
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15. 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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16. 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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17. 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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18. The UFFO (Ultra Fast Flash Observatory) Pathfinder: Science and Mission

Author

Chen, P., Ahmad, S., Ahn, K., Barrillon, P., Blin-Bondil, S., Brandt, S., Budtz-Jorgensen, C., Castro-Tirado, A. J., Choi, H. S., Choi, Y. J., Connell, P., Dagoret-Campagne, S., De La Taille, C., Eyles, C., Grossan, B., Hermann, I., Huang, M. -H. A., Jeong, S., Jung, A., Kim, J. E., Kim, S. H., Kim, Y. W., Lee, J., Lim, H., Linder, E. V., Liu, T. -C., Lund, Niels, Min, K. W., Na, G. W., Nam, J. W., Nam, K., Panayuk, M. I., Park, I. H., Re-Glero, V., Rodrigo, J. M., Smoot, G. F., Suh, Y. D., Svelitov, S., Vedenken, N., Wang, M. -Z, Yashin, I., and Zhao, M. H.

Subjects
Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract

Hundreds of gamma-ray burst (GRB) optical light curves have been measured since the discovery of optical afterglows. However, even after nearly 7 years of operation of the Swift Observatory, only a handful of measurements have been made soon (within a minute) after the gamma ray signal. This lack of early observations fails to address burst physics at short time scales associated with prompt emissions and progenitors. Because of this lack of sub-minute data, the characteristics of the rise phase of optical light curve of short-hard type GRB and rapid-rising GRB, which may account for ~30% of all GRB, remain practically unknown. We have developed methods for reaching sub-minute and sub-second timescales in a small spacecraft observatory. Rather than slewing the entire spacecraft to aim the optical instrument at the GRB position, we use rapidly moving mirror to redirect our optical beam. As a first step, we employ motorized slewing mirror telescope (SMT), which can point to the event within 1s, in the UFFO Pathfinder GRB Telescope onboard the Lomonosov satellite to be launched in Nov. 2011. UFFO's sub-minute measurements of the optical emission of dozens of GRB each year will result in a more rigorous test of current internal shock models, probe the extremes of bulk Lorentz factors, provide the first early and detailed measurements of fast-rise GRB optical light curves, and help verify the prospect of GRB as a new standard candle. We will describe the science and the mission of the current UFFO Pathfinder project, and our plan of a full-scale UFFO-100 as the next step., Comment: 4 pages, 5 figures, to appear in the 32nd International Conference on Cosmic Rays (ICRC), Beijing, August 11-18, 2011

Published
2011
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19. Implementation of the readout system in the UFFO Slewing Mirror Telescope

Author

Kim, J. E., Lim, H., Jung, A., Ahn, K. -B, Choi, H. S., Choi, Y. J., Grossan, B., Hermann, I., Jeong, S., Kim, S. -W., Kim, Y. W., Lee, J., Linder, E. V., Min, K. W., Na, G. W., Nam, J. W., Nam, K. H., Panayuk, M. I., Park, I. H., Smoot, G. F., Suh, Y. D., Svelitov, S., Vedenken, N., Yashin, I., and Zhao, M. H.

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

The Ultra-Fast Flash Observatory (UFFO) is a new space-based experiment to observe Gamma-Ray Bursts (GRBs). GRBs are the most luminous electromagnetic events in the universe and occur randomly in any direction. Therefore the UFFO consists of two telescopes; UFFO Burst Alert & Trigger Telescope (UBAT) to detect GRBs using a wide field-of-view (FOV), and a Slewing Mirror Telescope (SMT) to observe UV/optical events rapidly within the narrow, targeted FOV. The SMT is a Ritchey-Chretien telescope that uses a motorized mirror system and an Intensified Charge-Coupled Device (ICCD). When the GRB is triggered by the UBAT, the SMT receives the position information and rapidly tilts the mirror to the target. The ICCD start to take the data within a second after GRB is triggered. Here we give the details about the SMT readout electronics that deliver the data.

Published
2011
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20. Optical Performances of Slewing Mirror Telescope for UFFO-Pathfinder

Author

Jeong, S., Ahn, K. -B., Nam, J. W., Park, I. H., Kim, S. -W., Choi, H. S., Grossan, B., Hermann, I., Jung, A., Kim, Y. W., Kim, J. E., Linder, E. V., Lee, J., Lim, H., Min, K. W., Na, G. W., Nam, K. H., Panasyuk, M. I., Smoot, G. F., Svertilov, S., Suh, Y. D., Vedenkin, N., Yashin, I., and Zhao, M. H.

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

The Ultra-Fast Flash Observatory-Pathfinder (UFFO-P) is to be launched onboard Lomonosov spacecraft in November 2011. It is to measure early UV/Optical photons from Gamma Ray Bursts (GRBs). Slewing Mirror Telescope (SMT) is one of two instruments designed for detection of UV/Optical images of the GRBs. SMT is a Ritchey-Chr\'etien telescope of 100 mm in diameter with a motorized slewing mirror at the entrance providing 17\times17 arcmin2 in Field of View (FOV) and 4 arcsec in pixel resolution. Its sky coverage can be further expanded up to 35 degrees in FOV by tilting a motorized slewing mirror. All mirrors were fabricated to about RMS 0.02 waves in wave front error (WFE) and 84.7% (in average reflectivity) over 200nm~650nm range. SMT was aligned to RMS 0.05 waves in WFE (test wavelength 632.8nm). From the static gravity test result, SMT optics system is expected to survive during launch. The technical details of SMT assembly and laboratory performance test results are reported., Comment: 4 pages, 6 figures, proceeding paper for the 32nd International Conference on Cosmic Rays (ICRC), Beijing, August 11-18, 2011

Published
2011
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21. Design and Fabrication of Detector Module for UFFO Burst Alert & Trigger Telescope

Author

Jung, A., Ahmad, S., Ahn, K. -B., Barrillon, P., Blin-Bondil, S., Brandt, S., Budtz-JØRgensen, C., CaStro-Tirado, A. J., Chen, P., Choi, H. S., Choi, Y. J., Connell, P., Dagoret-Campagne, S., De La Taille, C., Eyles, C., Grossan, B., Hermann, I., Huang, M. -H. A., Jeong, S., Kim, J. E., Kim, S. -W., Kim, Y. W., Lee, J., Lim, H., Linder, E. V., Liu, T. -C., Lund, N., Min, K. W., Na, G. W., Nam, J. W., Nam, K. H., Panasyuk, M. I., Park, I. H., Reglero, V., Rodrigo, J. M., Smoot, G. F., Suh, Y. D., Svertilov, S., Vedenkin, N., Wang, M. -Z, Yashin, I., and Zhao, M. H.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics
Abstract

The Ultra-Fast Flash Observatory (UFFO) pathfinder is a space mission devoted to the measurement of Gamma-Ray Bursts (GRBs), especially their early light curves which will give crucial information on the progenitor stars and central engines of the GRBs. It consists of two instruments: the UFFO Burst Alert & Trigger telescope (UBAT) for the detection of GRB locations and the Slewing Mirror Telescope (SMT) for the UV/optical afterglow observations, upon triggering by UBAT. The UBAT employs a coded-mask {\gamma}/X-ray camera with a wide field of view (FOV), and is comprised of three parts: a coded mask, a hopper, and a detector module (DM). The UBAT DM consists of a LYSO scintillator crystal array, multi-anode photo multipliers, and analog and digital readout electronics. We present here the design and fabrication of the UBAT DM, as well as its preliminary test results., Comment: 4 pages, 7 figures, 3 tables, ICRC conference proceeding paper; Beijing, August 11-18, 2011

Published
2011
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22. Data Acquisition System for the UFFO Pathfinder

Author

Na, G. W., Ahn, K. -B., Choi, H. S., Choi, Y. J., Grossan, B., Hermann, I., Jeong, S., Jung, A., Kim, J. E., Kim, S. -W., Kim, Y. W., Lee, J., Lim, H., Linder, E. V., Min, K. W., Nam, J. W., Nam, K. H., Panasyuk, M. I., Park, I. H., Smoot, G. F., Suh, Y. D., Svertilov, S., Vedenkin, N., Yashin, I., and Zhao, M. H.

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

The Ultra-Fast Flash Observatory (UFFO) Pathfinder is a payload on the Russian Lomonosov satellite, scheduled to be launched in November 2011. The Observatory is designed to detect early UV/Optical photons from Gamma-Ray Bursts (GRBs). There are two telescopes and one main data acquisition system: the UFFO Burst Alert & Trigger Telescope (UBAT), the Slewing Mirror Telescope (SMT), and the UFFO Data Acquisition (UDAQ) system. The UDAQ controls and manages the operation and communication of each telescope, and is also in charge of the interface with the satellite. It will write the data taken by each telescope to the NOR flash memory and sends them to the satellite via the Bus-Interface system (BI). It also receives data from the satellite including the coordinates and time of an external trigger from another payload, and distributes them to two telescopes. These functions are implemented in field programmable gates arrays (FPGA) for low power consumption and fast processing without a microprocessor. The UDAQ architecture, control of the system, and data flow will be presented., Comment: 4 pages, 7 figures, 2 tables, proceeding paper for the 32nd International Conference on Cosmic Rays (ICRC), Beijing, August 11-18, 2011

Published
2011
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23. Planck Early Results XXVI: Detection with Planck and confirmation by XMM-Newton of PLCK G266.6-27.3, an exceptionally X-ray luminous and massive galaxy cluster at z~1

Author

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., Benoît, A., Bernard, J. -P., Bersanelli, M., Bhatia, R., Böhringer, H., Bonaldi, A., Bond, J. R., Borgani, S., Borrill, J., Bouchet, F. R., Brown, M. L., Burigana, C., Cabella, P., Cantalupo, C. M., Cappellini, B., Carvalho, P., Catalano, A., Cayón, L., Chiang, L. -Y, Chiang, C., Chon, G., Christensen, P. R., Churazov, E., Clements, D. L., Colafrancesco, S., Colombi, S., Crill, B. P., Cuttaia, F., Da Silva, A., Dahle, H., Danese, L., D'Arcangelo, O., Davis, R. J., de Bernardis, P., de Gasperis, G., de Zotti, G., Delabrouille, J., Delouis, J. -M., Démoclès, J., Désert, F. -X., Dickinson, C., Diego, J. M., 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., Fosalba, P., Frailis, M., Franceschi, E., 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., Heinämäki, P., Hernández-Monteagudo, C., Hildebrandt, S. R., Hivon, E., Hobson, M., Hurier, G., Jaffe, A. H., Jones, W. C., Juvela, M., Keihänen, E., Keskitalo, R., Kisner, T. S., Kneissl, R., Kurki-Suonio, H., Lagache, G., Lähteenmäki, A., Lamarre, J. -M., Lasenby, A., Lawrence, C. R., Jeune, M. Le, Leach, S., Leonardi, R., Leroy, C., Liddle, A., Lilje, P. B., López-Caniego, M., Luzzi, G., Macías-Pérez, J. F., Maino, D., Mandolesi, N., Marleau, F., Martínez-González, E., Masi, S., Matarrese, S., 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., Nevalainen, J., Nørgaard-Nielsen, H. U., Noviello, F., Novikov, D., Novikov, I., O'Dwyer, I. J., Osborne, S., Paladini, R., Pasian, F., Patanchon, G., Pearson, T. J., Perdereau, O., Perotto, L., Perrotta, F., Piacentini, F., Pierpaoli, E., Piffaretti, R., Platania, P., Pointecouteau, E., Polenta, G., Ponthieu, N., Popa, L., Poutanen, T., Pratt, G. W., Prézeau, G., Prunet, S., Puget, J. -L., Rachen, J. P., Rebolo, R., Reinecke, M., Renault, C., Ricciardi, S., Riller, T., Ristorcelli, I., Rocha, G., Rubiño-Martín, J. A., Saar, E., Sandri, M., Savini, G., Schaefer, B. M., Scott, D., Smoot, G. F., Starck, J. -L., Sutton, D., Sygnet, J. -F., Tauber, J. A., Terenzi, L., Toffolatti, L., Tomasi, M., Tristram, M., Türler, M., Valenziano, 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 first results on PLCK G266.6-27.3, a galaxy cluster candidate detected at a signal-to-noise ratio of 5 in the Planck All Sky survey. An XMM-Newton validation observation has allowed us to confirm that the candidate is a bona fide galaxy cluster. With these X-ray data we measure an accurate redshift, z = 0.94 +/- 0.02, and estimate the cluster mass to be M_500 = (7.8 +/- 0.8)e+14 solar masses. PLCK G266.6-27.3 is an exceptional system: its luminosity of L_X(0.5-2.0 keV)=(1.4 +/- 0.05)e+45 erg/s, equals that of the two most luminous known clusters in the z > 0.5 universe, and it is one of the most massive clusters at z~1. Moreover, unlike the majority of high-redshift clusters, PLCK G266.6-27.3 appears to be highly relaxed. This observation confirms Planck's capability of detecting high-redshift, high-mass clusters, and opens the way to the systematic study of population evolution in the exponential tail of the mass function., Comment: 6 pages, 3 figures; final version accepted for publication in A&A ; minor changes in Sec.2.,3.2 and 4.1; Table 1: misprint on R500 error corrected; abundance value added

Published
2011
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24. 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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25. 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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26. 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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27. 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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28. 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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29. 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/

Published
2011
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30. Planck early results. III. First assessment of the Low Frequency Instrument in-flight performance

Author

Mennella, A., Bersanelli, M., Butler, R. C., Curto, A., Cuttaia, F., Davis, R. J., Dick, J., Frailis, M., Galeotta, S., Gregorio, A., Kurki-Suonio, H., Lawrence, C. R., Leach, S., Leahy, J. P., Lowe, S., Maino, D., Mandolesi, N., Maris, M., Martínez-González, E., Meinhold, P. R., Morgante, G., Pearson, D., Perrotta, F., Polenta, G., Poutanen, T., Sandri, M., Seiffert, M. D., Suur-Uski, A. -S., Tavagnacco, D., Terenzi, L., Tomasi, M., Valiviita, J., Villa, F., Watson, R., Wilkinson, A., Zacchei, A., Zonca, A., Aja, B., Artal, E., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Bartlett, J. G., Bartolo, N., Battaglia, P., Bennett, K., Bonaldi, A., Bonavera, L., Borrill, J., Bouchet, F. R., Burigana, C., Cabella, P., Cappellini, B., Chen, X., Colombo, L., Cruz, M., Danese, L., D'Arcangelo, O., Davies, R. D., de Gasperis, G., de Rosa, A., de Zotti, G., Dickinson, C., Diego, J. M., Donzelli, S., Efstathiou, G., Enßlin, T. A., Eriksen, H. K., Falvella, M. C., Finelli, F., Foley, S., Franceschet, C., Franceschi, E., Gaier, T. C., Génova-Santos, R. T., George, D., Gómez, F., González-Nuevo, J., Górski, K. M., Gruppuso, A., Hansen, F. K., Herranz, D., Herreros, J. M., Hoyland, R. J., Hughes, N., Jewell, J., Jukkala, P., Juvela, M., Kangaslahti, P., Keihänen, E., Keskitalo, R., Kilpia, V. -H., Kisner, T. S., Knoche, J., Knox, L., Laaninen, M., Lähteenmäki, A., Lamarre, J. -M., Leonardi, R., León-Tavares, J., Leutenegger, P., Lilje, P. B., López-Caniego, M., Lubin, P. M., Malaspina, M., Marinucci, D., Massardi, M., Matarrese, S., Matthai, F., Melchiorri, A., Mendes, L., Miccolis, M., Migliaccio, M., Mitra, S., Moss, A., Natoli, P., Nesti, R., Nørgaard-Nielsen, H. U., Pagano, L., Paladini, R., Paoletti, D., Partridge, B., Pasian, F., Pettorino, V., Pietrobon, D., Pospieszalski, M., Prézeau, G., Prina, M., Procopio, P., Puget, J. -L., Quercellini, C., Rachen, J. P., Rebolo, R., Reinecke, M., Ricciardi, S., Robbers, G., Rocha, G., Roddis, N., Rubiño-Martín, J. A., Savelainen, M., Scott, D., Silvestri, R., Simonetto, A., Sjoman, P., Smoot, G. F., Sozzi, C., Stringhetti, L., Tauber, J. A., Tofani, G., Toffolatti, L., Tuovinen, J., Türler, M., Umana, G., Valenziano, L., Varis, J., Vielva, P., Vittorio, N., Wade, L. A., Watson, C., White, S. D. M., and Winder, F.

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

The scientific performance of the Planck Low Frequency Instrument (LFI) after one year of in-orbit operation is presented. We describe the main optical parameters and discuss photometric calibration, white noise sensitivity, and noise properties. A preliminary evaluation of the impact of the main systematic effects is presented. For each of the performance parameters, we outline the methods used to obtain them from the flight data and provide a comparison with pre-launch ground assessments, which are essentially confirmed in flight., Comment: Published version

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2011
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31. 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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32. 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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33. 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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34. 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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35. 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

Published
2011
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36. 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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37. 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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38. 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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39. 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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40. 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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41. 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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42. 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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43. 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

Published
2011
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44. 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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45. 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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46. 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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47. Search for Cosmic Strings in the COSMOS Survey

Author

Christiansen, J. L., Albin, E., Fletcher, T., Goldman, J., Teng, I. P. W., Foley, M., and Smoot, G. F.

Subjects
Astrophysics - Cosmology and Extragalactic Astrophysics
Abstract

We search the COSMOS survey for pairs of galaxies consistent with the gravitational lensing signature of a cosmic string. The COSMOS survey imaged 1.64 square degrees using the Advanced Camera for Surveys (ACS) aboard the Hubble Space Telescope (HST). Our technique includes estimates of the efficiency for finding the lensed galaxy pair. We find no evidence for cosmic strings with a mass per unit length of G mu/c^2 < 3.0E-7 out to redshifts greater than 0.6 and set 95% upper limits. This corresponds to a global 95% upper limit of Omega_string<0.0028.

Published
2010
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48. Probing Cosmic Strings with Satellite CMB measurements

Author

Jeong, E., Baccigalupi, Carlo, and Smoot, G. F.

Subjects
Astrophysics - Cosmology and Nongalactic Astrophysics, High Energy Physics - Phenomenology, High Energy Physics - Theory
Abstract

We study the problem of searching for cosmic string signal patterns in the present high resolution and high sensitivity observations of the Cosmic Microwave Background (CMB). This article discusses a technique capable of recognizing Kaiser-Stebbins effect signatures in total intensity anisotropy maps, and shows that the biggest factor that produces confusion is represented by the acoustic oscillation features of the scale comparable to the size of horizon at recombination. Simulations show that the distribution of null signals for pure Gaussian maps converges to a $\chi^2$ distribution, with detectability threshold corresponding to a string induced step signal with an amplitude of about 100 $\muK$ which corresponds to a limit of roughly $G\mu < 1.5\times 10^{-6}$. We study the statistics of spurious detections caused by extra-Galactic and Galactic foregrounds. For diffuse Galactic foregrounds, which represents the dominant source of contamination, we derive sky masks outlining the available region of the sky where the Galactic confusion is sub-dominant, specializing our analysis to the case represented by the frequency coverage and nominal sensitivity and resolution of the Planck experiment., Comment: 14 pages, 3 figures, to be published in JCAP

Published
2010
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49. Planck pre-launch status: Design and description of the Low Frequency Instrument

Author

Bersanelli, M., Mandolesi, N., Butler, R. C., Mennella, A., Villa, F., Aja, B., Artal, E., Artina, E., Baccigalupi, C., Balasini, M., Baldan, G., Banday, A., Bastia, P., Battaglia, P., Bernardino, T., Blackhurst, E., Boschini, L., Burigana, C., Cafagna, G., Cappellini, B., Cavaliere, F., Colombo, F., Crone, G., Cuttaia, F., D'Arcangelo, O., Danese, L., Davies, R. D., Davis, R. J., De Angelis, L., De Gasperis, G. C., De La Fuente, L., De Rosa, A., De Zotti, G., Falvella, M. C., Ferrari, F., Ferretti, R., Figini, L., Fogliani, S., Franceschet, C., Franceschi, E., Gaier, T., Garavaglia, S., Gomez, F., Gorski, K., Gregorio, A., Guzzi, P., Herreros, J. M., Hildebrandt, S. R., Hoyland, R., Hughes, N., Janssen, M., Jukkala, P., Kettle, D., Kilpia, V. H., Laaninen, M., Lapolla, P. M., Lawrence, C. R., Leahy, J. P., Leonardi, R., Leutenegger, P., Levin, S., Lilje, P. B., Lowe, S. R., Lubin, D. Lawson P. M., Maino, D., Malaspina, M., Maris, M., Marti-Canales, J., Martinez-Gonzalez, E., Mediavilla, A., Meinhold, P., Miccolis, M., Morgante, G., Natoli, P., Nesti, R., Pagan, L., Paine, C., Partridge, B., Pascual, J. P., Pasian, F., Pearson, D., Pecora, M., Perrotta, F., Platania, P., Pospieszalski, M., Poutanen, T., Prina, M., Rebolo, R., Roddis, N., Rubino-Martin, J. A., Salmon, n M. J., Sandri, M., Seiffert, M., Silvestri, R., Simonetto, A., Sjoman, P., Smoot, G. F., Sozzi, C., Stringhetti, L., Taddei, E., Tauber, J., Terenzi, L., Tomasi, M., Tuovinen, J., Valenziano, L., Varis, J., Vittorio, N., Wade, L. A., Wilkinson, A., Winder, F., Zacchei, A., and Zonca, A.

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

In this paper we present the Low Frequency Instrument (LFI), designed and developed as part of the Planck space mission, the ESA program dedicated to precision imaging of the cosmic microwave background (CMB). Planck-LFI will observe the full sky in intensity and polarisation in three frequency bands centred at 30, 44 and 70 GHz, while higher frequencies (100-850 GHz) will be covered by the HFI instrument. The LFI is an array of microwave radiometers based on state-of-the-art Indium Phosphide cryogenic HEMT amplifiers implemented in a differential system using blackbody loads as reference signals. The front-end is cooled to 20K for optimal sensitivity and the reference loads are cooled to 4K to minimise low frequency noise. We provide an overview of the LFI, discuss the leading scientific requirements and describe the design solutions adopted for the various hardware subsystems. The main drivers of the radiometric, optical and thermal design are discussed, including the stringent requirements on sensitivity, stability, and rejection of systematic effects. Further details on the key instrument units and the results of ground calibration are provided in a set of companion papers., Comment: 23 pages, 31 figures, accepted by Astronomy and Astrophysics, Planck LFI technical papers published by JINST: http://www.iop.org/EJ/journal/-page=extra.proc5/1748-0221

Published
2010
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50. 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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