<i>Planck</i>early results. III. First assessment of the Low Frequency Instrument in-flight performance

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, Stuart; 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.; Väliviita, J.; Villa, F.; Watson, R. A.; 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. P. L.; Cruz, M.; Danese, L.; D'Arcangelo, O.; Davies, R. D.; Gasperis, G. de; Rosa, A. de; Zotti, G. de; 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.; Génova-Santos, R. T.; George, Danielle; Gomez, F.; González‐Nuevo, J.; Górski, K. M.; Gruppuso, A.; Hansen, F. K.; Herranz, D.; Herreros, J. M.; Hoyland, R. J.; Hughes, N.; Jewell, Jeffrey; Jukkala, P.; Juvela, M.; Kangaslahti, Pekka; Keihänen, E.; Keskitalo, R.; Kilpiä, 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, Domenico; 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.W.; Prézeau, G.; Prina, M.; Procopio, P.; Puget, J.‐L.; Quercellini, Claudia; Rachen, J. P.; Реболо, Р.; Reinecke, M.; Ricciardi, S.; Robbers, Georg; Rocha, G.; Roddis, N.; no-Martín, Jose Alberto Rubi; Савелайнен, М.; Scott, D.; Silvestri, R.; Simonetto, A.; Sjoman, P.; Smoot, George 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, Simon D. M.; Winder, F.

doi:10.1051/0004-6361/201116480

Cited by 114 publications

(49 citation statements)

References 56 publications

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“…Planck observes the sky in nine frequency bands covering 30-857 GHz, with high sensitivity and angular resolution from 31 to 5 arcmin. The Low Frequency Instrument (LFI; Bersanelli et al 2010;Mandolesi et al 2010;Mennella et al 2011) covers the 30, 44, and 70 GHz bands with amplifiers cooled to 20 K. The High Frequency Instrument (HFI; Lamarre et al 2010; Planck HFI Core Team 2011a) covers the 100, 143, 217, 353, 545, and 857 GHz bands with bolometers cooled to 0.1 K. Early astrophysics results, based on data taken between 13 August 2009 and 7 June 2010 (Planck HFI Core Team 2011b; Zacchei et al 2011), are given in Planck Collaboration VIII-XXVI 2011. Intermediate astrophysics results are now based on data taken between 13 August 2009 and 27 November 2010.…”

Section: The Planck Missionmentioning

confidence: 99%

Clusters of galaxies in the Planck survey

Pointecouteau

2013

Astron Nachr

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The Planck satellite has surveyed the whole sky more than four times. The nominal mission of two all-sky surveys will be released to the public in 2013. From the first all-sky survey, we have demonstrated the ability to detect clusters via the Sunyaev-Zel'dovich effect with high reliability and out to large redshifts. We have released the first large sample of 189 high signal-to-noise SZ clusters. We also presented the detection of 45 new Planck clusters, confirmed in X-ray with the XMM-Newton satellite. The Planck collaboration is engaged in a massive identification and follow-up programme of its SZ sources at X-ray, optical, and SZ wavelengths. Dedicated cluster studies are also conducted by the consortium in order to better constrain the scaling and structural properties of the cluster population. We have thus provided high precision calibration of scaling relation between the SZ signal and the clusters physical quantities. The excellent agreement found between SZ and X-ray measurements have demonstrated our good understanding of the hot intra-cluster gas at least within R500. These results together with those from other operating SZ instruments are shading new light on our understanding of the most massive bound structure of the Universe. With its whole sky reach and unprecedented frequency coverage, the Planck mission is a crucial asset to these endeavours.

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Section: The Planck Missionmentioning

confidence: 99%

Clusters of galaxies in the Planck survey

Pointecouteau

2013

Astron Nachr

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“…( 3.12) where FWHM is the full width at half-maximum of the channel beams in arcmin. We illustrate our method on a Planck-like case taking the beams and noise characteristics from Planck HFI Core Team (2011) and Mennella et al (2011). Moreover, the noise has been divided by 2 to account for the approved extension of the mission.…”

Section: E T H O D O L O G Ymentioning

confidence: 99%

“…Planck channel performance characteristics(Mennella et al 2011; Planck HFI Core Team 2011) for the nominal mission.…”

mentioning

confidence: 99%

A multifrequency approach of the cosmological parameter estimation in the presence of extragalactic point sources

Paoletti

Aghanim

Douspis

et al. 2012

Monthly Notices of the Royal Astronomical Society

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We present a multifrequency approach which optimizes the constraints on cosmological parameters with respect to extragalactic point source and secondary anisotropy contamination on small scales. We model with a minimal number of parameters the expected dominant contaminations in intensity, such as unresolved point sources and the thermal Sunyaev-Zel'dovich effect. The model for unresolved point sources, either Poisson distributed or clustered, uses data from Planck early results. The method presented is the first one where the models of the point-source contributions are based on the Planck early data. To reduce the number of parameters necessary to characterize the residuals, the method uses the knowledge of the frequency dependences of the residual signals coming from the data. The dependences are directly included in the parametrizations, allowing us to reduce the number of the residual parameters to the minimum of three. The overall three amplitudes of the residual contributions are included in a Markov chain Monte Carlo analysis for the estimate of cosmological parameters. We show that our method is robust: as long as the main contaminants are taken into account, the constraints on the cosmological parameters are unbiased regardless of the realistic uncertainties on the contaminants. Although general, the method is applied only to Planck.

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“…The other acronyms here used are: N of R (or B) = number of radiometers (or bolometers), EB = effective bandwidth (in GHz). Adapted from [6,7] and consistent with [3,4]. Note that at 100 GHz all bolometers are polarized and the equivalent temperature value is obtained by combining polarization measurements.…”

Section: The Esa Planck Mission: Overviewmentioning

confidence: 99%

“…The spacecraft accumulated data with its two instruments, the High Frequency Instrument (HFI) [3], based on bolometers working between 100 and 857 GHz, and the Low Frequency Instrument (LFI) [4], based on radiometers working between 30 and 70 GHz, up to the consumption of the cryogenic liquids on January 2012, achieving ≃ 29.5 months of integration, corresponding to about five complete sky surveys. A further 12 months extension is on-going for observations with LFI only, cooled down with the cryogenic system provided by HFI.…”

Section: Introductionmentioning

confidence: 99%