Planck has produced detailed all-sky observations over nine frequency bands between 30 and 857 GHz. These observations allow robust reconstruction of the primordial cosmic microwave background (CMB) temperature fluctuations over nearly the full sky, as well as new constraints on Galactic foregrounds, including thermal dust and line emission from molecular carbon monoxide (CO). This paper describes the component separation framework adopted by Planck for many cosmological analyses, including CMB power spectrum determination and likelihood construction on large angular scales, studies of primordial non-Gaussianity and statistical isotropy, the integrated Sachs-Wolfe effect, gravitational lensing, and searches for topological defects. We test four foreground-cleaned CMB maps derived using qualitatively different component separation algorithms. The quality of our reconstructions is evaluated through detailed simulations and internal comparisons, and shown through various tests to be internally consistent and robust for CMB power spectrum and cosmological parameter estimation up to l = 2000. The parameter constraints on ACDM cosmologies derived from these maps are consistent with those presented in the cross-spectrum based Planck likelihood analysis. We choose two of the CMB maps for specific scientific goals. We also present maps and frequency spectra of the Galactic low-frequency, CO, and thermal dust emission. The component maps are found to provide a faithful representation of the sky, as evaluated by simulations, with the largest bias seen in the CO component at 3%. For the low-frequency component, the spectral index varies widely over the sky, ranging from about beta = 4 to -2. Considering both morphology and prior knowledge of the low frequency components, the index map allows us to associate a steep spectral index (beta < -3.2) with strong anomalous microwave emission, corresponding to a spinning dust spectrum peaking below 20 GHz, a flat index of beta > -2.3 with strong free-free emission, and intermediate values with synchrotron emission. © 2014 ESO.

Planck 2013 results. XII. Diffuse component separation / Ade, P. A. R.; Aghanim, N.; Armitage Caplan, C.; Arnaud, M.; Ashdown, M.; Atrio Barandela, F.; Aumont, J.; Baccigalupi, Carlo; Banday, A. J.; Barreiro, R. B.; Bartlett, J. G.; Battaner, E.; Benabed, K.; Benoît, A.; Benoit Lévy, A.; Bernard, J. P.; Bersanelli, Marco Rinaldo Fedele; Bielewicz, Pawel; Bobin, J.; Bock, J. J.; Bonaldi, Anna Valentina; Bonavera, Laura; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Boulanger, Francois Bernard Marie; Bridges, M.; Bucher, M.; Burigana, Carlo; Butler, R. C.; Cardoso, J. F.; Castex, Guillaume Jean Serge; Catalano, A.; Challinor, A.; Chamballu, A.; Chary, R. R.; Chen, X.; Chiang, H. C.; Chiang, L. Y.; Christensen, P. R.; Church, S.; Clements, D. L.; Colombi, S.; Colombo, L. P. L.; Couchot, F.; Coulais, A.; Crill, B. P.; Cruz, M.; Curto, A.; Cuttaia, F.; Danese, Luigi; Davies, R. D.; Davis, R. J.; De Bernardis, P.; De Rosa, A.; De Zotti, Gianfranco; Delabrouille, J.; Delouis, J. M.; Désert, F. X.; Dickinson, C.; Diego, J. M.; Dobler, G.; Dole, H.; Donzelli, Simona; Doré, O.; Douspis, M.; Dunkley, J.; Dupac, X.; Efstathiou, G.; Enßlin, T. A.; Eriksen, H. K.; Falgarone, E.; Finelli, F.; Forni, O.; Frailis, M.; Fraisse, A. A.; Franceschi, E.; Galeotta, S.; Ganga, K.; Giard, M.; Giardino, G.; Giraud Héraud, Y.; González Nuevo, J.; Górski, K. M.; Gratton, S.; Gregorio, Anna; Gruppuso, A.; Hansen, F. K.; Hanson, D.; Harrison, D. L.; Helou, G.; Henrot Versillé, S.; Hernández Monteagudo, C.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hornstrup, A.; Hovest, W.; Huey, G.; Huffenberger, K. M.; Jaffe, Andrew Howard; Jaffe, T. R.; Jewell, J.; 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.; Le Jeune, M.; Leach, Samuel Michael; Leahy, J. P.; Leonardi, R.; Lesgourgues, J.; Liguori, M.; Lilje, P. B.; Linden Vørnle, M.; López Caniego, M.; Lubin, P. M.; Maciás Pérez, J. F.; Maffei, B.; Maino, Davide; Mandolesi, N.; Marcos Caballero, A.; Maris, M.; Marshall, D. J.; Martin, P. G.; Martínez González, E.; Masi, S.; Massardi, Marcella; Matarrese, Sabino; Matthai, F.; Mazzotta, P.; Meinhold, P. R.; Melchiorri, A.; Mendes, L.; Mennella, Aniello; Migliaccio, M.; Mikkelsen, K.; Mitra, S.; Miville Deschênes, M. A.; Molinari, D.; Moneti, A.; Montier, L.; Morgante, G.; Mortlock, D.; Moss, A.; Munshi, D.; Murphy, J. A.; Naselsky, P.; Nati, F.; Natoli, P.; Netterfield, C. B.; Nørgaard Nielsen, H. U.; Noviello, F.; Novikov, D.; Novikov, I.; O'Dwyer, I. J.; Osborne, S.; Oxborrow, C. A.; Paci, Francesco; Pagano, L.; Pajot, F.; Paladini, Roberta; Paoletti, D.; Partridge, B.; Pasian, Fabio; Patanchon, G.; Pearson, T. J.; Perdereau, O.; Perotto, L.; Perrotta, Francesca; Pettorino, Valeria; Piacentini, Francesco; Piat, M.; Pierpaoli, Elena Maria; Pietrobon, D.; Plaszczynski, S.; 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.; Reach, W. T.; Rebolo, R.; Reinecke, M.; Remazeilles, M.; Renault, C.; Renzi, Alessandro; Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha, G.; Roman, M.; Rosset, C.; Roudier, G.; Rowan Robinson, M.; Rubinõ Martín, J. A.; Rusholme, B.; Salerno, E.; Sandri, Matteo; Santos, D.; Savini, G.; Schiavon, F.; Scott, D.; Seiffert, M. D.; Shellard, E. P. S.; Spencer, L. D.; Starck, J. L.; Stompor, R.; Sudiwala, R.; Sunyaev, R.; Sureau, F.; Sutton, D.; Suur Uski, A. S.; Sygnet, J. F.; Tauber, J. A.; Tavagnacco, D.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram, M.; Tucci, M.; Tuovinen, J.; Türler, M.; Umana, G.; Valenziano, L.; Valiviita, J.; Van Tent, B.; Varis, J.; Viel, Matteo; Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt, B. D.; Wehus, I. K.; Wilkinson, A.; Xia, J. Q.; Yvon, D.; Zacchei, A.; Zonca, A.. - In: ASTRONOMY & ASTROPHYSICS. - ISSN 0004-6361. - 571:Nov(2014), pp. A12.1-A12.31. [10.1051/0004-6361/201321580]

Planck 2013 results. XII. Diffuse component separation

Baccigalupi, Carlo;Bersanelli, Marco Rinaldo Fedele;Bielewicz, Pawel;Bonaldi, Anna Valentina;Bonavera, Laura;Boulanger, Francois Bernard Marie;Bucher, M.;Burigana, Carlo;Castex, Guillaume Jean Serge;Danese, Luigi;De Zotti, Gianfranco;Donzelli, Simona;Gregorio, Anna;Jaffe, Andrew Howard;Leach, Samuel Michael;Maino, Davide;Massardi, Marcella;Matarrese, Sabino;Mennella, Aniello;Natoli, P.;Paci, Francesco;Paladini, Roberta;Pasian, Fabio;Perrotta, Francesca;Pettorino, Valeria;Piacentini, Francesco;Pierpaoli, Elena Maria;Renzi, Alessandro;Sandri, Matteo;Stompor, R.;Viel, Matteo;
2014-01-01

Abstract

Planck has produced detailed all-sky observations over nine frequency bands between 30 and 857 GHz. These observations allow robust reconstruction of the primordial cosmic microwave background (CMB) temperature fluctuations over nearly the full sky, as well as new constraints on Galactic foregrounds, including thermal dust and line emission from molecular carbon monoxide (CO). This paper describes the component separation framework adopted by Planck for many cosmological analyses, including CMB power spectrum determination and likelihood construction on large angular scales, studies of primordial non-Gaussianity and statistical isotropy, the integrated Sachs-Wolfe effect, gravitational lensing, and searches for topological defects. We test four foreground-cleaned CMB maps derived using qualitatively different component separation algorithms. The quality of our reconstructions is evaluated through detailed simulations and internal comparisons, and shown through various tests to be internally consistent and robust for CMB power spectrum and cosmological parameter estimation up to l = 2000. The parameter constraints on ACDM cosmologies derived from these maps are consistent with those presented in the cross-spectrum based Planck likelihood analysis. We choose two of the CMB maps for specific scientific goals. We also present maps and frequency spectra of the Galactic low-frequency, CO, and thermal dust emission. The component maps are found to provide a faithful representation of the sky, as evaluated by simulations, with the largest bias seen in the CO component at 3%. For the low-frequency component, the spectral index varies widely over the sky, ranging from about beta = 4 to -2. Considering both morphology and prior knowledge of the low frequency components, the index map allows us to associate a steep spectral index (beta < -3.2) with strong anomalous microwave emission, corresponding to a spinning dust spectrum peaking below 20 GHz, a flat index of beta > -2.3 with strong free-free emission, and intermediate values with synchrotron emission. © 2014 ESO.
2014
571
Nov
1
31
A12
10.1051/0004-6361/201321580
http://adsabs.harvard.edu/abs/2014A%26A...571A..12P
https://arxiv.org/abs/1301.5839
http://inspirehep.net/record/1224737
Ade, P. A. R.; Aghanim, N.; Armitage Caplan, C.; Arnaud, M.; Ashdown, M.; Atrio Barandela, F.; Aumont, J.; Baccigalupi, Carlo; Banday, A. J.; Barreiro, R. B.; Bartlett, J. G.; Battaner, E.; Benabed, K.; Benoît, A.; Benoit Lévy, A.; Bernard, J. P.; Bersanelli, Marco Rinaldo Fedele; Bielewicz, Pawel; Bobin, J.; Bock, J. J.; Bonaldi, Anna Valentina; Bonavera, Laura; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Boulanger, Francois Bernard Marie; Bridges, M.; Bucher, M.; Burigana, Carlo; Butler, R. C.; Cardoso, J. F.; Castex, Guillaume Jean Serge; Catalano, A.; Challinor, A.; Chamballu, A.; Chary, R. R.; Chen, X.; Chiang, H. C.; Chiang, L. Y.; Christensen, P. R.; Church, S.; Clements, D. L.; Colombi, S.; Colombo, L. P. L.; Couchot, F.; Coulais, A.; Crill, B. P.; Cruz, M.; Curto, A.; Cuttaia, F.; Danese, Luigi; Davies, R. D.; Davis, R. J.; De Bernardis, P.; De Rosa, A.; De Zotti, Gianfranco; Delabrouille, J.; Delouis, J. M.; Désert, F. X.; Dickinson, C.; Diego, J. M.; Dobler, G.; Dole, H.; Donzelli, Simona; Doré, O.; Douspis, M.; Dunkley, J.; Dupac, X.; Efstathiou, G.; Enßlin, T. A.; Eriksen, H. K.; Falgarone, E.; Finelli, F.; Forni, O.; Frailis, M.; Fraisse, A. A.; Franceschi, E.; Galeotta, S.; Ganga, K.; Giard, M.; Giardino, G.; Giraud Héraud, Y.; González Nuevo, J.; Górski, K. M.; Gratton, S.; Gregorio, Anna; Gruppuso, A.; Hansen, F. K.; Hanson, D.; Harrison, D. L.; Helou, G.; Henrot Versillé, S.; Hernández Monteagudo, C.; Herranz, D.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hornstrup, A.; Hovest, W.; Huey, G.; Huffenberger, K. M.; Jaffe, Andrew Howard; Jaffe, T. R.; Jewell, J.; 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.; Le Jeune, M.; Leach, Samuel Michael; Leahy, J. P.; Leonardi, R.; Lesgourgues, J.; Liguori, M.; Lilje, P. B.; Linden Vørnle, M.; López Caniego, M.; Lubin, P. M.; Maciás Pérez, J. F.; Maffei, B.; Maino, Davide; Mandolesi, N.; Marcos Caballero, A.; Maris, M.; Marshall, D. J.; Martin, P. G.; Martínez González, E.; Masi, S.; Massardi, Marcella; Matarrese, Sabino; Matthai, F.; Mazzotta, P.; Meinhold, P. R.; Melchiorri, A.; Mendes, L.; Mennella, Aniello; Migliaccio, M.; Mikkelsen, K.; Mitra, S.; Miville Deschênes, M. A.; Molinari, D.; Moneti, A.; Montier, L.; Morgante, G.; Mortlock, D.; Moss, A.; Munshi, D.; Murphy, J. A.; Naselsky, P.; Nati, F.; Natoli, P.; Netterfield, C. B.; Nørgaard Nielsen, H. U.; Noviello, F.; Novikov, D.; Novikov, I.; O'Dwyer, I. J.; Osborne, S.; Oxborrow, C. A.; Paci, Francesco; Pagano, L.; Pajot, F.; Paladini, Roberta; Paoletti, D.; Partridge, B.; Pasian, Fabio; Patanchon, G.; Pearson, T. J.; Perdereau, O.; Perotto, L.; Perrotta, Francesca; Pettorino, Valeria; Piacentini, Francesco; Piat, M.; Pierpaoli, Elena Maria; Pietrobon, D.; Plaszczynski, S.; 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.; Reach, W. T.; Rebolo, R.; Reinecke, M.; Remazeilles, M.; Renault, C.; Renzi, Alessandro; Ricciardi, S.; Riller, T.; Ristorcelli, I.; Rocha, G.; Roman, M.; Rosset, C.; Roudier, G.; Rowan Robinson, M.; Rubinõ Martín, J. A.; Rusholme, B.; Salerno, E.; Sandri, Matteo; Santos, D.; Savini, G.; Schiavon, F.; Scott, D.; Seiffert, M. D.; Shellard, E. P. S.; Spencer, L. D.; Starck, J. L.; Stompor, R.; Sudiwala, R.; Sunyaev, R.; Sureau, F.; Sutton, D.; Suur Uski, A. S.; Sygnet, J. F.; Tauber, J. A.; Tavagnacco, D.; Terenzi, L.; Toffolatti, L.; Tomasi, M.; Tristram, M.; Tucci, M.; Tuovinen, J.; Türler, M.; Umana, G.; Valenziano, L.; Valiviita, J.; Van Tent, B.; Varis, J.; Viel, Matteo; Vielva, P.; Villa, F.; Vittorio, N.; Wade, L. A.; Wandelt, B. D.; Wehus, I. K.; Wilkinson, A.; Xia, J. Q.; Yvon, D.; Zacchei, A.; Zonca, A.
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