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This paper characterizes the effective beams, the effective beam window functions and the associated errors for the Planck High Frequency Instrument (HFI) detectors. The effective beam is theangular response including the effect of the optics, detectors, data processing and the scan strategy. The window function is the representation of this beam in the harmonic domain which is required to recover an unbiased measurement of the cosmic microwave background angular power spectrum. The HFI is a scanning instrument and its effective beams are the convolution of: a) the optical response of the telescope and feeds; b) the processing of the time-ordered data and deconvolution of the bolometric and electronic transfer function; and c) the merging of several surveys to produce maps. The time response transfer functions are measured using observations of Jupiter and Saturn and by minimizing survey difference residuals. The scanning beam is the post-deconvolution angular response of the instrument, and is characterized with observations of Mars. The main beam solid angles are determined to better than 0.5% at each HFI frequency band. Observations of Jupiter and Saturn limit near sidelobes (within 5°) to about 0.1% of the total solid angle. Time response residuals remain as long tails in the scanning beams, but contribute less than 0.1% of the total solid angle. The bias and uncertainty in the beam products are estimated using ensembles of simulated planet observations that include the impact of instrumental noise and known systematic effects. The correlation structure of these ensembles is well-described by five error eigenmodes that are sub-dominant to sample variance and instrumental noise in the harmonic domain. A suite of consistency tests provide confidence that the error model represents a sufficient description of the data. The total error in the effective beam window functions is below 1% at 100 GHz up to multipole ℓ ~ 1500, and below 0.5% at 143 and 217 GHz up to ℓ ~ 2000.
Tauber, J., Ade, P., Aghanim, N., Armitage Caplan, C., Arnaud, M., Ashdown, M., et al. (2014). Planck 2013 results. VII. HFI time response and beams. ASTRONOMY & ASTROPHYSICS, 571, 1-31 [10.1051/0004-6361/201321535].
Planck 2013 results. VII. HFI time response and beams
Tauber, Jan;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.;Battaner, E.;Benabed, K.;Benoît, A.;Benoit Lévy, A.;Bernard, J. P.;Bersanelli, M.;Bielewicz, P.;Bobin, J.;Bock, J. J.;Bond, J. R.;Borrill, J.;Bouchet, F. R.;Bowyer, J. W.;Bridges, M.;Bucher, M;Burigana, C.;Cardoso, J. F.;Catalano, A.;Challinor, A.;Chamballu, A.;Chary, R. R.;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.;Curto, A.;Cuttaia, F.;Danese, L.;Davies, R. D.;DE BERNARDIS, Paolo;De Rosa, A.;De Zotti, G.;Delabrouille, J.;Delouis, J. M.;Désert, F. X.;Diego, J. M.;Dole, H.;Donzelli, S.;Doré, O.;Douspis, M.;Dunkley, J.;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.;Gudmundsson, J. E.;Haissinski, J.;Hansen, F. K.;Hanson, D.;Harrison, D.;Henrot Versillé, S.;Hernández Monteagudo, C.;Herranz, D.;Hildebrandt, S. R.;Hivon, E.;Hobson, M.;Holmes, W. A.;Hornstrup, A.;Hou, Z.;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.;Lamarre, J. M.;Lasenby, A.;Laureijs, R. J.;Lawrence, C. R.;Leonardi, R.;Leroy, C.;Lesgourgues, J.;Liguori, M.;Lilje, P. B.;Linden Vørnle, M.;López Caniego, M.;Lubin, P. M.;MacIás Pérez, J. F.;Mactavish, C. J.;Maffei, B.;Mandolesi, N.;Maris, M.;Marshall, D. J.;Martin, P. G.;Martínez González, E.;MASI, Silvia;Massardi, M.;Matarrese, S.;Matsumura, T.;Matthai, F.;Mazzotta, P.;Mcgehee, P.;MELCHIORRI, Alessandro;Mendes, L.;Mennella, A.;Migliaccio, M.;Mitra, S.;Miville Deschênes, M. A.;Moneti, A.;Montier, L.;Morgante, G.;Mortlock, D.;Munshi, D.;Murphy, J. A.;Naselsky, P.;NATI, FEDERICO;Natoli, P.;Netterfield, C. B.;Nørgaard Nielsen, H. U.;Noviello, F.;Novikov, D.;Novikov, I.;Osborne, S.;Oxborrow, C. A.;Paci, F.;PAGANO, LUCA;Pajot, F.;Paoletti, D.;Pasian, F.;Patanchon, G.;Perdereau, O.;Perotto, L.;Perrotta, F.;PIACENTINI, Francesco;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.;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.;Sauvé, A.;Savini, G.;Scott, D.;Shellard, E. P. S.;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.;Tomasi, M.;Tristram, M.;Tucci, M.;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.;Zonca, A.
2014
Abstract
This paper characterizes the effective beams, the effective beam window functions and the associated errors for the Planck High Frequency Instrument (HFI) detectors. The effective beam is theangular response including the effect of the optics, detectors, data processing and the scan strategy. The window function is the representation of this beam in the harmonic domain which is required to recover an unbiased measurement of the cosmic microwave background angular power spectrum. The HFI is a scanning instrument and its effective beams are the convolution of: a) the optical response of the telescope and feeds; b) the processing of the time-ordered data and deconvolution of the bolometric and electronic transfer function; and c) the merging of several surveys to produce maps. The time response transfer functions are measured using observations of Jupiter and Saturn and by minimizing survey difference residuals. The scanning beam is the post-deconvolution angular response of the instrument, and is characterized with observations of Mars. The main beam solid angles are determined to better than 0.5% at each HFI frequency band. Observations of Jupiter and Saturn limit near sidelobes (within 5°) to about 0.1% of the total solid angle. Time response residuals remain as long tails in the scanning beams, but contribute less than 0.1% of the total solid angle. The bias and uncertainty in the beam products are estimated using ensembles of simulated planet observations that include the impact of instrumental noise and known systematic effects. The correlation structure of these ensembles is well-described by five error eigenmodes that are sub-dominant to sample variance and instrumental noise in the harmonic domain. A suite of consistency tests provide confidence that the error model represents a sufficient description of the data. The total error in the effective beam window functions is below 1% at 100 GHz up to multipole ℓ ~ 1500, and below 0.5% at 143 and 217 GHz up to ℓ ~ 2000.
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Utilizza questo identificativo per citare o creare un link a questo documento: https://hdl.handle.net/10281/405710
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simulazione ASN
Il report seguente simula gli indicatori relativi alla propria produzione scientifica in relazione alle soglie ASN 2023-2025 del proprio SC/SSD. Si ricorda che il superamento dei valori soglia (almeno 2 su 3) è requisito necessario ma non sufficiente al conseguimento dell'abilitazione. La simulazione si basa sui dati IRIS e sugli indicatori bibliometrici alla data indicata e non tiene conto di eventuali periodi di congedo obbligatorio, che in sede di domanda ASN danno diritto a incrementi percentuali dei valori. La simulazione può differire dall'esito di un’eventuale domanda ASN sia per errori di catalogazione e/o dati mancanti in IRIS, sia per la variabilità dei dati bibliometrici nel tempo. Si consideri che Anvur calcola i valori degli indicatori all'ultima data utile per la presentazione delle domande.
La presente simulazione è stata realizzata sulla base delle specifiche raccolte sul tavolo ER del Focus Group IRIS coordinato dall’Università di Modena e Reggio Emilia e delle regole riportate nel DM 598/2018 e allegata Tabella A. Cineca, l’Università di Modena e Reggio Emilia e il Focus Group IRIS non si assumono alcuna responsabilità in merito all’uso che il diretto interessato o terzi faranno della simulazione. Si specifica inoltre che la simulazione contiene calcoli effettuati con dati e algoritmi di pubblico dominio e deve quindi essere considerata come un mero ausilio al calcolo svolgibile manualmente o con strumenti equivalenti.
