Planck 2013 results. VII. HFI time response and beams

P. A.R. Ade; N. Aghanim; C. Armitage-Caplan; M. Arnaud; M. Ashdown; F. Atrio-Barandela; J. Aumont; C. Baccigalupi; A. J. Banday; R. B. Barreiro; E. Battaner; K. Benabed; A. Benoît; A. Benoit-Lévy; J. P. Bernard; M. Bersanelli; P. Bielewicz; J. Bobin; J. J. Bock; J. R. Bond; J. Borrill; F. R. Bouchet; J. W. Bowyer; M. Bridges; M. Bucher; C. Burigana; J. F. Cardoso; A. Catalano; A. Challinor; A. Chamballu; R. R. Chary; H. C. Chiang; L. Y. Chiang; P. R. Christensen; S. Church; D. L. Clements; S. Colombi; L. P.L. Colombo; F. Couchot; A. Coulais; B. P. Crill; A. Curto; F. Cuttaia; L. Danese; R. D. Davies; P. De Bernardis; A. De Rosa; G. De Zotti; J. Delabrouille; J. M. Delouis; F. X. Désert; J. M. Diego; H. Dole; S. Donzelli; O. Doré; M. Douspis; J. Dunkley; X. Dupac; G. Efstathiou; T. A. Enßlin; H. K. Eriksen; F. Finelli; O. Forni; M. Frailis; A. A. Fraisse; E. Franceschi; S. Galeotta; K. Ganga; M. Giard; Y. Giraud-Héraud; J. González-Nuevo; K. M. Górski; S. Gratton; A. Gregorio; A. Gruppuso; J. E. Gudmundsson; J. Haissinski; F. K. Hansen; D. Hanson; D. Harrison; S. Henrot-Versillé; C. Hernández-Monteagudo; D. Herranz; S. R. Hildebrandt; E. Hivon; M. Hobson; W. A. Holmes; A. Hornstrup; Z. Hou; W. Hovest; K. M. Huffenberger; A. H. Jaffe; T. R. Jaffe; W. C. Jones; M. Juvela; E. Keihänen; R. Keskitalo; T. S. Kisner; R. Kneissl; J. Knoche; L. Knox; M. Kunz; H. Kurki-Suonio; G. Lagache; J. M. Lamarre; A. Lasenby; R. J. Laureijs; C. R. Lawrence; R. Leonardi; C. Leroy; J. Lesgourgues; M. Liguori; P. B. Lilje; M. Linden-Vørnle; M. López-Caniego; P. M. Lubin; J. F. MacIás-Pérez; C. J. MacTavish; B. Maffei; N. Mandolesi; M. Maris; D. J. Marshall; P. G. Martin; E. Martínez-González; S. Masi; M. Massardi; S. Matarrese; T. Matsumura; F. Matthai; P. Mazzotta; P. McGehee; A. Melchiorri; L. Mendes; A. Mennella; M. Migliaccio; S. Mitra; M. A. Miville-Deschênes; A. Moneti; L. Montier; G. Morgante; D. Mortlock; D. Munshi; J. A. Murphy; P. Naselsky; F. Nati; P. Natoli; C. B. Netterfield; H. U. Nørgaard-Nielsen; F. Noviello; D. Novikov; I. Novikov; S. Osborne; C. A. Oxborrow; F. Paci; L. Pagano; F. Pajot; D. Paoletti; F. Pasian; G. Patanchon; O. Perdereau; L. Perotto; F. Perrotta; F. Piacentini; M. Piat; E. Pierpaoli; D. Pietrobon; S. Plaszczynski; E. Pointecouteau; A. M. Polegre; G. Polenta; N. Ponthieu; L. Popa; T. Poutanen; G. W. Pratt; G. Prézeau; S. Prunet; J. L. Puget; J. P. Rachen; M. Reinecke; M. Remazeilles; C. Renault; S. Ricciardi; T. Riller; I. Ristorcelli; G. Rocha; C. Rosset; G. Roudier; M. Rowan-Robinson; B. Rusholme; M. Sandri; D. Santos; A. Sauvé; G. Savini; D. Scott; E. P.S. Shellard; L. D. Spencer; J. L. Starck; V. Stolyarov; R. Stompor; R. Sudiwala; F. Sureau; D. Sutton; A. S. Suur-Uski; J. F. Sygnet; J. A. Tauber; D. Tavagnacco; L. Terenzi; M. Tomasi; M. Tristram; M. Tucci; G. Umana; L. Valenziano; J. Valiviita; B. Van Tent; P. Vielva; F. Villa; N. Vittorio; L. A. Wade; B. D. Wandelt; D. Yvon; A. Zacchei; A. Zonca

doi:10.1051/0004-6361/201321535

Planck 2013 results. VII. HFI time response and beams

P. A.R. Ade, N. Aghanim, C. Armitage-Caplan, M. Arnaud, M. Ashdown, F. Atrio-Barandela, J. Aumont, C. Baccigalupi, A. J. Banday, R. B. Barreiro, E. Battaner, K. Benabed, A. Benoît, A. Benoit-Lévy, J. P. Bernard, M. Bersanelli, P. Bielewicz, J. Bobin, J. J. Bock, J. R. BondJ. Borrill, F. R. Bouchet, J. W. Bowyer, M. Bridges, M. Bucher, C. Burigana, J. F. Cardoso, A. Catalano, A. Challinor, A. Chamballu, R. R. Chary, H. C. Chiang, L. Y. Chiang, P. R. Christensen, S. Church, D. L. Clements, S. Colombi, L. P.L. Colombo, F. Couchot, A. Coulais, B. P. Crill, A. Curto, F. Cuttaia, L. Danese, R. D. Davies, P. De Bernardis, A. De Rosa, G. De Zotti, J. Delabrouille, J. M. Delouis, F. X. Désert, J. M. Diego, H. Dole, S. Donzelli, O. Doré, M. Douspis, J. Dunkley, X. Dupac, G. Efstathiou, T. A. Enßlin, H. K. Eriksen, F. Finelli, O. Forni, M. Frailis, A. A. Fraisse, E. Franceschi, S. Galeotta, K. Ganga, M. Giard, Y. Giraud-Héraud, J. González-Nuevo, K. M. Górski, S. Gratton, A. Gregorio, A. Gruppuso, J. E. Gudmundsson, J. Haissinski, F. K. Hansen, D. Hanson, D. Harrison, S. Henrot-Versillé, C. Hernández-Monteagudo, D. Herranz, S. R. Hildebrandt, E. Hivon, M. Hobson, W. A. Holmes, A. Hornstrup, Z. Hou, W. Hovest, K. M. Huffenberger, A. H. Jaffe, T. R. Jaffe, W. C. Jones, M. Juvela, E. Keihänen, R. Keskitalo, T. S. Kisner, R. Kneissl, J. Knoche, L. Knox, M. Kunz, H. Kurki-Suonio, G. Lagache, J. M. Lamarre, A. Lasenby, R. J. Laureijs, C. R. Lawrence, R. Leonardi, C. Leroy, J. Lesgourgues, M. Liguori, P. B. Lilje, M. Linden-Vørnle, M. López-Caniego, P. M. Lubin, J. F. MacIás-Pérez, C. J. MacTavish, B. Maffei, N. Mandolesi, M. Maris, D. J. Marshall, P. G. Martin, E. Martínez-González, S. Masi, M. Massardi, S. Matarrese, T. Matsumura, F. Matthai, P. Mazzotta, P. McGehee, A. Melchiorri, L. Mendes, A. Mennella, M. Migliaccio, S. Mitra, M. A. Miville-Deschênes, A. Moneti, L. Montier, G. Morgante, D. Mortlock, D. Munshi, J. A. Murphy, P. Naselsky, F. Nati, P. Natoli, C. B. Netterfield, H. U. Nørgaard-Nielsen, F. Noviello, D. Novikov, I. Novikov, S. Osborne, C. A. Oxborrow, F. Paci, L. Pagano, F. Pajot, D. Paoletti, F. Pasian, G. Patanchon, O. Perdereau, L. Perotto, F. Perrotta, F. Piacentini, M. Piat, E. Pierpaoli, D. Pietrobon, S. Plaszczynski, E. Pointecouteau, A. M. Polegre, G. Polenta, N. Ponthieu, L. Popa, T. Poutanen, G. W. Pratt, G. Prézeau, S. Prunet, J. L. Puget, J. P. Rachen, M. Reinecke, M. Remazeilles, C. Renault, S. Ricciardi, T. Riller, I. Ristorcelli, G. Rocha, C. Rosset, G. Roudier, M. Rowan-Robinson, B. Rusholme, M. Sandri, D. Santos, A. Sauvé, G. Savini, D. Scott, E. P.S. Shellard, L. D. Spencer, J. L. Starck, V. Stolyarov, R. Stompor, R. Sudiwala, F. Sureau, D. Sutton, A. S. Suur-Uski, J. F. Sygnet, J. A. Tauber, D. Tavagnacco, L. Terenzi, M. Tomasi, M. Tristram, M. Tucci, G. Umana, L. Valenziano, J. Valiviita, B. Van Tent, P. Vielva, F. Villa, N. Vittorio, L. A. Wade, B. D. Wandelt, D. Yvon, A. Zacchei, A. Zonca

Physics

Research output: Contribution to journal › Article › peer-review

16 Scopus citations

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 â.," ~ 1500, and below 0.5% at 143 and 217 GHz up to ~ 2000.

Original language	English (US)
Article number	A7
Journal	Astronomy and Astrophysics
Volume	571
DOIs	https://doi.org/10.1051/0004-6361/201321535
State	Published - Nov 1 2014

All Science Journal Classification (ASJC) codes

Astronomy and Astrophysics
Space and Planetary Science

Keywords

Cosmic background radiation
Cosmology: observations
Instrumentation: detectors
Surveys

Access to Document

10.1051/0004-6361/201321535

Cite this

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., ... Zonca, A. (2014). Planck 2013 results. VII. HFI time response and beams. Astronomy and Astrophysics, 571, Article A7. https://doi.org/10.1051/0004-6361/201321535

@article{0742241387a0442990976812b2dcb7e1,

title = "Planck 2013 results. VII. HFI time response and beams",

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 {\^a}.,{"} ~ 1500, and below 0.5% at 143 and 217 GHz up to ~ 2000.",

keywords = "Cosmic background radiation, Cosmology: observations, Instrumentation: detectors, Surveys",

author = "Ade, {P. A.R.} and N. Aghanim and C. Armitage-Caplan and M. Arnaud and M. Ashdown and F. Atrio-Barandela and J. Aumont and C. Baccigalupi and Banday, {A. J.} and Barreiro, {R. B.} and E. Battaner and K. Benabed and A. Beno{\^i}t and A. Benoit-L{\'e}vy and Bernard, {J. P.} and M. Bersanelli and P. Bielewicz and J. Bobin and Bock, {J. J.} and Bond, {J. R.} and J. Borrill and Bouchet, {F. R.} and Bowyer, {J. W.} and M. Bridges and M. Bucher and C. Burigana and Cardoso, {J. F.} and A. Catalano and A. Challinor and A. Chamballu and Chary, {R. R.} and Chiang, {H. C.} and Chiang, {L. Y.} and Christensen, {P. R.} and S. Church and Clements, {D. L.} and S. Colombi and Colombo, {L. P.L.} and F. Couchot and A. Coulais and Crill, {B. P.} and A. Curto and F. Cuttaia and L. Danese and Davies, {R. D.} and {De Bernardis}, P. and {De Rosa}, A. and {De Zotti}, G. and J. Delabrouille and Delouis, {J. M.} and D{\'e}sert, {F. X.} and Diego, {J. M.} and H. Dole and S. Donzelli and O. Dor{\'e} and M. Douspis and J. Dunkley and X. Dupac and G. Efstathiou and En{\ss}lin, {T. A.} and Eriksen, {H. K.} and F. Finelli and O. Forni and M. Frailis and Fraisse, {A. A.} and E. Franceschi and S. Galeotta and K. Ganga and M. Giard and Y. Giraud-H{\'e}raud and J. Gonz{\'a}lez-Nuevo and G{\'o}rski, {K. M.} and S. Gratton and A. Gregorio and A. Gruppuso and Gudmundsson, {J. E.} and J. Haissinski and Hansen, {F. K.} and D. Hanson and D. Harrison and S. Henrot-Versill{\'e} and C. Hern{\'a}ndez-Monteagudo and D. Herranz and Hildebrandt, {S. R.} and E. Hivon and M. Hobson and Holmes, {W. A.} and A. Hornstrup and Z. Hou and W. Hovest and Huffenberger, {K. M.} and Jaffe, {A. H.} and Jaffe, {T. R.} and Jones, {W. C.} and M. Juvela and E. Keih{\"a}nen and R. Keskitalo and Kisner, {T. S.} and R. Kneissl and J. Knoche and L. Knox and M. Kunz and H. Kurki-Suonio and G. Lagache and Lamarre, {J. M.} and A. Lasenby and Laureijs, {R. J.} and Lawrence, {C. R.} and R. Leonardi and C. Leroy and J. Lesgourgues and M. Liguori and Lilje, {P. B.} and M. Linden-V{\o}rnle and M. L{\'o}pez-Caniego and Lubin, {P. M.} and MacI{\'a}s-P{\'e}rez, {J. F.} and MacTavish, {C. J.} and B. Maffei and N. Mandolesi and M. Maris and Marshall, {D. J.} and Martin, {P. G.} and E. Mart{\'i}nez-Gonz{\'a}lez and S. Masi and M. Massardi and S. Matarrese and T. Matsumura and F. Matthai and P. Mazzotta and P. McGehee and A. Melchiorri and L. Mendes and A. Mennella and M. Migliaccio and S. Mitra and Miville-Desch{\^e}nes, {M. A.} and A. Moneti and L. Montier and G. Morgante and D. Mortlock and D. Munshi and Murphy, {J. A.} and P. Naselsky and F. Nati and P. Natoli and Netterfield, {C. B.} and N{\o}rgaard-Nielsen, {H. U.} and F. Noviello and D. Novikov and I. Novikov and S. Osborne and Oxborrow, {C. A.} and F. Paci and L. Pagano and F. Pajot and D. Paoletti and F. Pasian and G. Patanchon and O. Perdereau and L. Perotto and F. Perrotta and F. Piacentini and M. Piat and E. Pierpaoli and D. Pietrobon and S. Plaszczynski and E. Pointecouteau and Polegre, {A. M.} and G. Polenta and N. Ponthieu and L. Popa and T. Poutanen and Pratt, {G. W.} and G. Pr{\'e}zeau and S. Prunet and Puget, {J. L.} and Rachen, {J. P.} and M. Reinecke and M. Remazeilles and C. Renault and S. Ricciardi and T. Riller and I. Ristorcelli and G. Rocha and C. Rosset and G. Roudier and M. Rowan-Robinson and B. Rusholme and M. Sandri and D. Santos and A. Sauv{\'e} and G. Savini and D. Scott and Shellard, {E. P.S.} and Spencer, {L. D.} and Starck, {J. L.} and V. Stolyarov and R. Stompor and R. Sudiwala and F. Sureau and D. Sutton and Suur-Uski, {A. S.} and Sygnet, {J. F.} and Tauber, {J. A.} and D. Tavagnacco and L. Terenzi and M. Tomasi and M. Tristram and M. Tucci and G. Umana and L. Valenziano and J. Valiviita and {Van Tent}, B. and P. Vielva and F. Villa and N. Vittorio and Wade, {L. A.} and Wandelt, {B. D.} and D. Yvon and A. Zacchei and A. Zonca",

note = "Funding Information: The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, JA and RES (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php?project=planck&page=Planck_Collaboration . Publisher Copyright: {\textcopyright} 2014 ESO.",

year = "2014",

month = nov,

day = "1",

doi = "10.1051/0004-6361/201321535",

language = "English (US)",

volume = "571",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

}

Ade, PAR, Aghanim, N, Armitage-Caplan, C, Arnaud, M, Ashdown, M, Atrio-Barandela, F, Aumont, J, Baccigalupi, C, Banday, AJ, Barreiro, RB, Battaner, E, Benabed, K, Benoît, A, Benoit-Lévy, A, Bernard, JP, Bersanelli, M, Bielewicz, P, Bobin, J, Bock, JJ, Bond, JR, Borrill, J, Bouchet, FR, Bowyer, JW, Bridges, M, Bucher, M, Burigana, C, Cardoso, JF, Catalano, A, Challinor, A, Chamballu, A, Chary, RR, Chiang, HC, Chiang, LY, Christensen, PR, Church, S, Clements, DL, Colombi, S, Colombo, LPL, Couchot, F, Coulais, A, Crill, BP, Curto, A, Cuttaia, F, Danese, L, Davies, RD, De Bernardis, P, De Rosa, A, De Zotti, G, Delabrouille, J, Delouis, JM, Désert, FX, Diego, JM, Dole, H, Donzelli, S, Doré, O, Douspis, M, Dunkley, J, Dupac, X, Efstathiou, G, Enßlin, TA, Eriksen, HK, Finelli, F, Forni, O, Frailis, M, Fraisse, AA, Franceschi, E, Galeotta, S, Ganga, K, Giard, M, Giraud-Héraud, Y, González-Nuevo, J, Górski, KM, Gratton, S, Gregorio, A, Gruppuso, A, Gudmundsson, JE, Haissinski, J, Hansen, FK, Hanson, D, Harrison, D, Henrot-Versillé, S, Hernández-Monteagudo, C, Herranz, D, Hildebrandt, SR, Hivon, E, Hobson, M, Holmes, WA, Hornstrup, A, Hou, Z, Hovest, W, Huffenberger, KM, Jaffe, AH, Jaffe, TR, Jones, WC, Juvela, M, Keihänen, E, Keskitalo, R, Kisner, TS, Kneissl, R, Knoche, J, Knox, L, Kunz, M, Kurki-Suonio, H, Lagache, G, Lamarre, JM, Lasenby, A, Laureijs, RJ, Lawrence, CR, Leonardi, R, Leroy, C, Lesgourgues, J, Liguori, M, Lilje, PB, Linden-Vørnle, M, López-Caniego, M, Lubin, PM, MacIás-Pérez, JF, MacTavish, CJ, Maffei, B, Mandolesi, N, Maris, M, Marshall, DJ, Martin, PG, Martínez-González, E, Masi, S, Massardi, M, Matarrese, S, Matsumura, T, Matthai, F, Mazzotta, P, McGehee, P, Melchiorri, A, Mendes, L, Mennella, A, Migliaccio, M, Mitra, S, Miville-Deschênes, MA, Moneti, A, Montier, L, Morgante, G, Mortlock, D, Munshi, D, Murphy, JA, Naselsky, P, Nati, F, Natoli, P, Netterfield, CB, Nørgaard-Nielsen, HU, Noviello, F, Novikov, D, Novikov, I, Osborne, S, Oxborrow, CA, Paci, F, Pagano, L, Pajot, F, 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, AM, Polenta, G, Ponthieu, N, Popa, L, Poutanen, T, Pratt, GW, Prézeau, G, Prunet, S, Puget, JL, Rachen, JP, 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, EPS, Spencer, LD, Starck, JL, Stolyarov, V, Stompor, R, Sudiwala, R, Sureau, F, Sutton, D, Suur-Uski, AS, Sygnet, JF, Tauber, JA, 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, LA, Wandelt, BD, Yvon, D, Zacchei, A & Zonca, A 2014, 'Planck 2013 results. VII. HFI time response and beams', Astronomy and Astrophysics, vol. 571, A7. https://doi.org/10.1051/0004-6361/201321535

TY - JOUR

T1 - Planck 2013 results. VII. HFI time response and beams

AU - Ade, P. A.R.

AU - Aghanim, N.

AU - Armitage-Caplan, C.

AU - Arnaud, M.

AU - Ashdown, M.

AU - Atrio-Barandela, F.

AU - Aumont, J.

AU - Baccigalupi, C.

AU - Banday, A. J.

AU - Barreiro, R. B.

AU - Battaner, E.

AU - Benabed, K.

AU - Benoît, A.

AU - Benoit-Lévy, A.

AU - Bernard, J. P.

AU - Bersanelli, M.

AU - Bielewicz, P.

AU - Bobin, J.

AU - Bock, J. J.

AU - Bond, J. R.

AU - Borrill, J.

AU - Bouchet, F. R.

AU - Bowyer, J. W.

AU - Bridges, M.

AU - Bucher, M.

AU - Burigana, C.

AU - Cardoso, J. F.

AU - Catalano, A.

AU - Challinor, A.

AU - Chamballu, A.

AU - Chary, R. R.

AU - Chiang, H. C.

AU - Chiang, L. Y.

AU - Christensen, P. R.

AU - Church, S.

AU - Clements, D. L.

AU - Colombi, S.

AU - Colombo, L. P.L.

AU - Couchot, F.

AU - Coulais, A.

AU - Crill, B. P.

AU - Curto, A.

AU - Cuttaia, F.

AU - Danese, L.

AU - Davies, R. D.

AU - De Bernardis, P.

AU - De Rosa, A.

AU - De Zotti, G.

AU - Delabrouille, J.

AU - Delouis, J. M.

AU - Désert, F. X.

AU - Diego, J. M.

AU - Dole, H.

AU - Donzelli, S.

AU - Doré, O.

AU - Douspis, M.

AU - Dunkley, J.

AU - Dupac, X.

AU - Efstathiou, G.

AU - Enßlin, T. A.

AU - Eriksen, H. K.

AU - Finelli, F.

AU - Forni, O.

AU - Frailis, M.

AU - Fraisse, A. A.

AU - Franceschi, E.

AU - Galeotta, S.

AU - Ganga, K.

AU - Giard, M.

AU - Giraud-Héraud, Y.

AU - González-Nuevo, J.

AU - Górski, K. M.

AU - Gratton, S.

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N1 - Funding Information: The development of Planck has been supported by: ESA; CNES and CNRS/INSU-IN2P3-INP (France); ASI, CNR, and INAF (Italy); NASA and DoE (USA); STFC and UKSA (UK); CSIC, MICINN, JA and RES (Spain); Tekes, AoF and CSC (Finland); DLR and MPG (Germany); CSA (Canada); DTU Space (Denmark); SER/SSO (Switzerland); RCN (Norway); SFI (Ireland); FCT/MCTES (Portugal); and PRACE (EU). A description of the Planck Collaboration and a list of its members, including the technical or scientific activities in which they have been involved, can be found at http://www.sciops.esa.int/index.php?project=planck&page=Planck_Collaboration . Publisher Copyright: © 2014 ESO.

PY - 2014/11/1

Y1 - 2014/11/1

N2 - 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 â.," ~ 1500, and below 0.5% at 143 and 217 GHz up to ~ 2000.

AB - 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 â.," ~ 1500, and below 0.5% at 143 and 217 GHz up to ~ 2000.

KW - Cosmic background radiation

KW - Cosmology: observations

KW - Instrumentation: detectors

KW - Surveys

UR - http://www.scopus.com/inward/record.url?scp=84908664266&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=84908664266&partnerID=8YFLogxK

U2 - 10.1051/0004-6361/201321535

DO - 10.1051/0004-6361/201321535

M3 - Article

AN - SCOPUS:84908664266

SN - 0004-6361

VL - 571

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A7

ER -

Planck 2013 results. VII. HFI time response and beams

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