Planck early results. IV. First assessment of the High Frequency Instrument in-flight performance

J.G. Bartlett; E. Bréelle; M. Bucher; J.-F. Cardoso; A. Catalano; C. Cressiot; J. Delabrouille; K. Ganga; Y. Giraud-Héraud; J. Kaplan; G. Patanchon; M. Piat; C. Rosset; G. Roudier; R. Stompor; M. Ashdown; R. Hills; M. Hobson; A. Lasenby; V. Stolyarov; R. Bhatia; R. Kneissl; J.R. Bond; M.-A. Miville-Deschênes; T. MacIaszek; A.J. Banday; J.-P. Bernard; O. Forni; M. Giard; C. Leroy; L. Montier; E. Pointecouteau; R. Pons; I. Ristorcelli; J.J. Bock; O. Doré; G. Helou; S.R. Hildebrandt; T. Matsumura; T.J. Pearson; G. Prézeau; G. Rocha; A. Challinor; P. Shellard; J.-B. Melin; J.-L. Starck; D. Yvon; Hans Ulrik Nørgaard-Nielsen; C.B. Netterfield; C. Chiang; W.C. Jones; L. Knox; B.D. Wandelt; P. De Bernardis; S. Masi; F. Nati; F. Piacentini; M. Bersanelli; R. Kneissl; J.A. Tauber; A. Zacchei; N. Mandolesi; M. Bersanelli; G. Guyot; F.-X. Désert; A. Chamballu; D.L. Clements; A.H. Jaffe; D. Mortlock; D. Novikov; M. Rowan-Robinson; R.-R. Chary; K. Ganga; A.E. Lange; P. McGehee; T.J. Pearson; B. Rusholme; A. Benoît; P. Camus; N. Aghanim; J. Aumont; F. Boulanger; J. Charra; M. Charra; H. Dole; M. Douspis; P. Eng; J.-J. Fourmond; R. Gispert; G. Lagache; P. Lami; B. Leriche; C. Leroy; Y. Longval; C. Mercier; M.-A. Miville-Deschênes; F. Noviello; F. Pajot; N. Ponthieu; J.-L. Puget; J.-P. Torre; L. Vibert; K. Benabed; F.R. Bouchet; J.-F. Cardoso; S. Colombi; J.-M. Delouis; E. Hivon; A. Moneti; S. Prunet; J.-F. Sygnet; B.D. Wandelt; P. Fosalba; H. Wiesemeyer; C. Thum; A. Challinor; G. Efstathiou; S. Gratton; D. Harrison; F. Van Leeuwen; S.R. Hildebrandt; J.G. Bartlett; J.J. Bock; B.P. Crill; O. Doré; K.M. Górski; W.A. Holmes; C.R. Lawrence; C. Paine; G. Prézeau; G. Rocha; L.A. Wade; B. Maffei; M. Ashdown; A. Challinor; S. Gratton; D. Harrison; A. Lasenby; C.J. MacTavish; A. Catalano; A. Coulais; J.-M. Lamarre; M. Arnaud; J.-L. Starck; J.-F. Cardoso; D. Vibert; D. Girard; S.R. Hildebrandt; J.F. MacÍas-Pérez; L. Perotto; C. Renault; D. Santos; P. Stassi; R. Ansari; F. Couchot; C. Filliard; J. Haissinski; S. Henrot-Versillé; A. Lavabre; B. Mansoux; O. Perdereau; S. Plaszczynski; F. Touze; M. Tristram; J. Borrill; A.J. Banday; M. Bartelmann; K. Dolag; C. Hernández-Monteagudo; R. Sunyaev; S.D.M. White; A. Murphy; T. Peacocke; V. Yurchenko; B.P. Crill; G. Savini; T. Bradshaw; M. Crook; R. Mann; P.A.R. Ade; M. Griffin; C. North; L. Spencer; R. Sudiwala; A. Woodcraft; R. Sunyaev; J. Borrill; S. Church; S. Osborne; M. Bartelmann; B.M. Schaefer; A.J. Banday; J.-P. Bernard; O. Forni; M. Giard; C. Leroy; L. Montier; E. Pointecouteau; R. Pons; I. Ristorcelli; W.T. Reach; E. Battaner; K.M. Huffenberger; K.M. Górski

doi:10.1051/0004-6361/201116487

Planck early results. IV. First assessment of the High Frequency Instrument in-flight performance

J.G. Bartlett, E. Bréelle, M. Bucher, J.-F. Cardoso, A. Catalano, C. Cressiot, J. Delabrouille, K. Ganga, Y. Giraud-Héraud, J. Kaplan, G. Patanchon, M. Piat, C. Rosset, G. Roudier, R. Stompor, M. Ashdown, R. Hills, M. Hobson, A. Lasenby, V. StolyarovR. Bhatia, R. Kneissl, J.R. Bond, M.-A. Miville-Deschênes, T. MacIaszek, A.J. Banday, J.-P. Bernard, O. Forni, M. Giard, C. Leroy, L. Montier, E. Pointecouteau, R. Pons, I. Ristorcelli, J.J. Bock, O. Doré, G. Helou, S.R. Hildebrandt, T. Matsumura, T.J. Pearson, G. Prézeau, G. Rocha, A. Challinor, P. Shellard, J.-B. Melin, J.-L. Starck, D. Yvon, Hans Ulrik Nørgaard-Nielsen, C.B. Netterfield, C. Chiang, W.C. Jones, L. Knox, B.D. Wandelt, P. De Bernardis, S. Masi, F. Nati, F. Piacentini, M. Bersanelli, R. Kneissl, J.A. Tauber, A. Zacchei, N. Mandolesi, M. Bersanelli, G. Guyot, F.-X. Désert, A. Chamballu, D.L. Clements, A.H. Jaffe, D. Mortlock, D. Novikov, M. Rowan-Robinson, R.-R. Chary, K. Ganga, A.E. Lange, P. McGehee, T.J. Pearson, B. Rusholme, A. Benoît, P. Camus, N. Aghanim, J. Aumont, F. Boulanger, J. Charra, M. Charra, H. Dole, M. Douspis, P. Eng, J.-J. Fourmond, R. Gispert, G. Lagache, P. Lami, B. Leriche, C. Leroy, Y. Longval, C. Mercier, M.-A. Miville-Deschênes, F. Noviello, F. Pajot, N. Ponthieu, J.-L. Puget, J.-P. Torre, L. Vibert, K. Benabed, F.R. Bouchet, J.-F. Cardoso, S. Colombi, J.-M. Delouis, E. Hivon, A. Moneti, S. Prunet, J.-F. Sygnet, B.D. Wandelt, P. Fosalba, H. Wiesemeyer, C. Thum, A. Challinor, G. Efstathiou, S. Gratton, D. Harrison, F. Van Leeuwen, S.R. Hildebrandt, J.G. Bartlett, J.J. Bock, B.P. Crill, O. Doré, K.M. Górski, W.A. Holmes, C.R. Lawrence, C. Paine, G. Prézeau, G. Rocha, L.A. Wade, B. Maffei, M. Ashdown, A. Challinor, S. Gratton, D. Harrison, A. Lasenby, C.J. MacTavish, A. Catalano, A. Coulais, J.-M. Lamarre, M. Arnaud, J.-L. Starck, J.-F. Cardoso, D. Vibert, D. Girard, S.R. Hildebrandt, J.F. MacÍas-Pérez, L. Perotto, C. Renault, D. Santos, P. Stassi, R. Ansari, F. Couchot, C. Filliard, J. Haissinski, S. Henrot-Versillé, A. Lavabre, B. Mansoux, O. Perdereau, S. Plaszczynski, F. Touze, M. Tristram, J. Borrill, A.J. Banday, M. Bartelmann, K. Dolag, C. Hernández-Monteagudo, R. Sunyaev, S.D.M. White, A. Murphy, T. Peacocke, V. Yurchenko, B.P. Crill, G. Savini, T. Bradshaw, M. Crook, R. Mann, P.A.R. Ade, M. Griffin, C. North, L. Spencer, R. Sudiwala, A. Woodcraft, R. Sunyaev, J. Borrill, S. Church, S. Osborne, M. Bartelmann, B.M. Schaefer, A.J. Banday, J.-P. Bernard, O. Forni, M. Giard, C. Leroy, L. Montier, E. Pointecouteau, R. Pons, I. Ristorcelli, W.T. Reach, E. Battaner, K.M. Huffenberger, K.M. Górski

Research output: Contribution to journal › Journal article › Research › peer-review

291 Downloads (Pure)

Abstract

The Planck High Frequency Instrument (HFI) is designed to measure the temperature and polarization anisotropies of the cosmic microwave background and Galactic foregrounds in six ~30% bands centered at 100, 143, 217, 353, 545, and 857 GHz at an angular resolution of 10′ (100 GHz), 7′ (143 GHz), and 5′ (217 GHz and higher). HFI has been operating flawlessly since launch on 14 May 2009, with the bolometers reaching 100 mK the first week of July. The settings of the readout electronics, including bolometer bias currents, that optimize HFI's noise performance on orbit are nearly the same as the ones chosen during ground testing. Observations of Mars, Jupiter, and Saturn have confirmed that the optical beams and the time responses of the detection chains are in good agreement with the predictions of physical optics modeling and pre-launch measurements. The Detectors suffer from a high flux of cosmic rays due to historically low levels of solar activity. As a result of the redundancy of Planck's observation strategy, theremoval of a few percent of data contaminated by glitches does not significantly affect the instrumental sensitivity. The cosmic ray flux represents a significant and variable heat load on the sub-Kelvin stage. Temporal variation and the inhomogeneous distribution of the flux results in thermal fluctuations that are a probable source of low frequency noise. The removal of systematic effects in the time ordered data provides a signal with an average noise equivalent power that is 70% of the goal in the 0.6-2.5 Hz range. This is slightly higher than was achieved during the pre-launch characterization but better than predicted in the early phases of the project. The improvement over the goal is a result of the low level of instrumental background loading achieved by the optical and thermal design of the HFI. © ESO, 2011.

Original language	English
Journal	Astronomy and Astrophysics
Volume	536
Pages (from-to)	A4
ISSN	0004-6361
DOIs	https://doi.org/10.1051/0004-6361/201116487
Publication status	Published - 2011

Access to Document

10.1051/0004-6361/201116487

Aa16487-11Final published version, 4.47 MB

OpenUrl availability

Full text

Cite this

Bartlett, J. G., Bréelle, E., Bucher, M., Cardoso, J-F., Catalano, A., Cressiot, C., Delabrouille, J., Ganga, K., Giraud-Héraud, Y., Kaplan, J., Patanchon, G., Piat, M., Rosset, C., Roudier, G., Stompor, R., Ashdown, M., Hills, R., Hobson, M., Lasenby, A., ... Górski, K. M. (2011). Planck early results. IV. First assessment of the High Frequency Instrument in-flight performance. Astronomy and Astrophysics, 536, A4. https://doi.org/10.1051/0004-6361/201116487

@article{4ba4513aec8d4f69a340428b95f2c96c,

title = "Planck early results. IV. First assessment of the High Frequency Instrument in-flight performance",

abstract = "The Planck High Frequency Instrument (HFI) is designed to measure the temperature and polarization anisotropies of the cosmic microwave background and Galactic foregrounds in six ~30% bands centered at 100, 143, 217, 353, 545, and 857 GHz at an angular resolution of 10′ (100 GHz), 7′ (143 GHz), and 5′ (217 GHz and higher). HFI has been operating flawlessly since launch on 14 May 2009, with the bolometers reaching 100 mK the first week of July. The settings of the readout electronics, including bolometer bias currents, that optimize HFI's noise performance on orbit are nearly the same as the ones chosen during ground testing. Observations of Mars, Jupiter, and Saturn have confirmed that the optical beams and the time responses of the detection chains are in good agreement with the predictions of physical optics modeling and pre-launch measurements. The Detectors suffer from a high flux of cosmic rays due to historically low levels of solar activity. As a result of the redundancy of Planck's observation strategy, theremoval of a few percent of data contaminated by glitches does not significantly affect the instrumental sensitivity. The cosmic ray flux represents a significant and variable heat load on the sub-Kelvin stage. Temporal variation and the inhomogeneous distribution of the flux results in thermal fluctuations that are a probable source of low frequency noise. The removal of systematic effects in the time ordered data provides a signal with an average noise equivalent power that is 70% of the goal in the 0.6-2.5 Hz range. This is slightly higher than was achieved during the pre-launch characterization but better than predicted in the early phases of the project. The improvement over the goal is a result of the low level of instrumental background loading achieved by the optical and thermal design of the HFI. {\textcopyright} ESO, 2011.",

author = "J.G. Bartlett and E. Br{\'e}elle and M. Bucher and J.-F. Cardoso and A. Catalano and C. Cressiot and J. Delabrouille and K. Ganga and Y. Giraud-H{\'e}raud and J. Kaplan and G. Patanchon and M. Piat and C. Rosset and G. Roudier and R. Stompor and M. Ashdown and R. Hills and M. Hobson and A. Lasenby and V. Stolyarov and R. Bhatia and R. Kneissl and J.R. Bond and M.-A. Miville-Desch{\^e}nes and T. MacIaszek and A.J. Banday and J.-P. Bernard and O. Forni and M. Giard and C. Leroy and L. Montier and E. Pointecouteau and R. Pons and I. Ristorcelli and J.J. Bock and O. Dor{\'e} and G. Helou and S.R. Hildebrandt and T. Matsumura and T.J. Pearson and G. Pr{\'e}zeau and G. Rocha and A. Challinor and P. Shellard and J.-B. Melin and J.-L. Starck and D. Yvon and N{\o}rgaard-Nielsen, {Hans Ulrik} and C.B. Netterfield and C. Chiang and W.C. Jones and L. Knox and B.D. Wandelt and {De Bernardis}, P. and S. Masi and F. Nati and F. Piacentini and M. Bersanelli and R. Kneissl and J.A. Tauber and A. Zacchei and N. Mandolesi and M. Bersanelli and G. Guyot and F.-X. D{\'e}sert and A. Chamballu and D.L. Clements and A.H. Jaffe and D. Mortlock and D. Novikov and M. Rowan-Robinson and R.-R. Chary and K. Ganga and A.E. Lange and P. McGehee and T.J. Pearson and B. Rusholme and A. Beno{\^i}t and P. Camus and N. Aghanim and J. Aumont and F. Boulanger and J. Charra and M. Charra and H. Dole and M. Douspis and P. Eng and J.-J. Fourmond and R. Gispert and G. Lagache and P. Lami and B. Leriche and C. Leroy and Y. Longval and C. Mercier and M.-A. Miville-Desch{\^e}nes and F. Noviello and F. Pajot and N. Ponthieu and J.-L. Puget and J.-P. Torre and L. Vibert and K. Benabed and F.R. Bouchet and J.-F. Cardoso and S. Colombi and J.-M. Delouis and E. Hivon and A. Moneti and S. Prunet and J.-F. Sygnet and B.D. Wandelt and P. Fosalba and H. Wiesemeyer and C. Thum and A. Challinor and G. Efstathiou and S. Gratton and D. Harrison and {Van Leeuwen}, F. and S.R. Hildebrandt and J.G. Bartlett and J.J. Bock and B.P. Crill and O. Dor{\'e} and K.M. G{\'o}rski and W.A. Holmes and C.R. Lawrence and C. Paine and G. Pr{\'e}zeau and G. Rocha and L.A. Wade and B. Maffei and M. Ashdown and A. Challinor and S. Gratton and D. Harrison and A. Lasenby and C.J. MacTavish and A. Catalano and A. Coulais and J.-M. Lamarre and M. Arnaud and J.-L. Starck and J.-F. Cardoso and D. Vibert and D. Girard and S.R. Hildebrandt and J.F. Mac{\'I}as-P{\'e}rez and L. Perotto and C. Renault and D. Santos and P. Stassi and R. Ansari and F. Couchot and C. Filliard and J. Haissinski and S. Henrot-Versill{\'e} and A. Lavabre and B. Mansoux and O. Perdereau and S. Plaszczynski and F. Touze and M. Tristram and J. Borrill and A.J. Banday and M. Bartelmann and K. Dolag and C. Hern{\'a}ndez-Monteagudo and R. Sunyaev and S.D.M. White and A. Murphy and T. Peacocke and V. Yurchenko and B.P. Crill and G. Savini and T. Bradshaw and M. Crook and R. Mann and P.A.R. Ade and M. Griffin and C. North and L. Spencer and R. Sudiwala and A. Woodcraft and R. Sunyaev and J. Borrill and S. Church and S. Osborne and M. Bartelmann and B.M. Schaefer and A.J. Banday and J.-P. Bernard and O. Forni and M. Giard and C. Leroy and L. Montier and E. Pointecouteau and R. Pons and I. Ristorcelli and W.T. Reach and E. Battaner and K.M. Huffenberger and K.M. G{\'o}rski",

year = "2011",

doi = "10.1051/0004-6361/201116487",

language = "English",

volume = "536",

pages = "A4",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

publisher = "EDP Sciences",

}

Bartlett, JG, Bréelle, E, Bucher, M, Cardoso, J-F, Catalano, A, Cressiot, C, Delabrouille, J, Ganga, K, Giraud-Héraud, Y, Kaplan, J, Patanchon, G, Piat, M, Rosset, C, Roudier, G, Stompor, R, Ashdown, M, Hills, R, Hobson, M, Lasenby, A, Stolyarov, V, Bhatia, R, Kneissl, R, Bond, JR, Miville-Deschênes, M-A, MacIaszek, T, Banday, AJ, Bernard, J-P, Forni, O, Giard, M, Leroy, C, Montier, L, Pointecouteau, E, Pons, R, Ristorcelli, I, Bock, JJ, Doré, O, Helou, G, Hildebrandt, SR, Matsumura, T, Pearson, TJ, Prézeau, G, Rocha, G, Challinor, A, Shellard, P, Melin, J-B, Starck, J-L, Yvon, D, Nørgaard-Nielsen, HU, Netterfield, CB, Chiang, C, Jones, WC, Knox, L, Wandelt, BD, De Bernardis, P, Masi, S, Nati, F, Piacentini, F, Bersanelli, M, Kneissl, R, Tauber, JA, Zacchei, A, Mandolesi, N, Bersanelli, M, Guyot, G, Désert, F-X, Chamballu, A, Clements, DL, Jaffe, AH, Mortlock, D, Novikov, D, Rowan-Robinson, M, Chary, R-R, Ganga, K, Lange, AE, McGehee, P, Pearson, TJ, Rusholme, B, Benoît, A, Camus, P, Aghanim, N, Aumont, J, Boulanger, F, Charra, J, Charra, M, Dole, H, Douspis, M, Eng, P, Fourmond, J-J, Gispert, R, Lagache, G, Lami, P, Leriche, B, Leroy, C, Longval, Y, Mercier, C, Miville-Deschênes, M-A, Noviello, F, Pajot, F, Ponthieu, N, Puget, J-L, Torre, J-P, Vibert, L, Benabed, K, Bouchet, FR, Cardoso, J-F, Colombi, S, Delouis, J-M, Hivon, E, Moneti, A, Prunet, S, Sygnet, J-F, Wandelt, BD, Fosalba, P, Wiesemeyer, H, Thum, C, Challinor, A, Efstathiou, G, Gratton, S, Harrison, D, Van Leeuwen, F, Hildebrandt, SR, Bartlett, JG, Bock, JJ, Crill, BP, Doré, O, Górski, KM, Holmes, WA, Lawrence, CR, Paine, C, Prézeau, G, Rocha, G, Wade, LA, Maffei, B, Ashdown, M, Challinor, A, Gratton, S, Harrison, D, Lasenby, A, MacTavish, CJ, Catalano, A, Coulais, A, Lamarre, J-M, Arnaud, M, Starck, J-L, Cardoso, J-F, Vibert, D, Girard, D, Hildebrandt, SR, MacÍas-Pérez, JF, Perotto, L, Renault, C, Santos, D, Stassi, P, Ansari, R, Couchot, F, Filliard, C, Haissinski, J, Henrot-Versillé, S, Lavabre, A, Mansoux, B, Perdereau, O, Plaszczynski, S, Touze, F, Tristram, M, Borrill, J, Banday, AJ, Bartelmann, M, Dolag, K, Hernández-Monteagudo, C, Sunyaev, R, White, SDM, Murphy, A, Peacocke, T, Yurchenko, V, Crill, BP, Savini, G, Bradshaw, T, Crook, M, Mann, R, Ade, PAR, Griffin, M, North, C, Spencer, L, Sudiwala, R, Woodcraft, A, Sunyaev, R, Borrill, J, Church, S, Osborne, S, Bartelmann, M, Schaefer, BM, Banday, AJ, Bernard, J-P, Forni, O, Giard, M, Leroy, C, Montier, L, Pointecouteau, E, Pons, R, Ristorcelli, I, Reach, WT, Battaner, E, Huffenberger, KM & Górski, KM 2011, 'Planck early results. IV. First assessment of the High Frequency Instrument in-flight performance', Astronomy and Astrophysics, vol. 536, pp. A4. https://doi.org/10.1051/0004-6361/201116487

TY - JOUR

T1 - Planck early results. IV. First assessment of the High Frequency Instrument in-flight performance

AU - Bartlett, J.G.

AU - Bréelle, E.

AU - Bucher, M.

AU - Cardoso, J.-F.

AU - Catalano, A.

AU - Cressiot, C.

AU - Delabrouille, J.

AU - Ganga, K.

AU - Giraud-Héraud, Y.

AU - Kaplan, J.

AU - Patanchon, G.

AU - Piat, M.

AU - Rosset, C.

AU - Roudier, G.

AU - Stompor, R.

AU - Ashdown, M.

AU - Hills, R.

AU - Hobson, M.

AU - Lasenby, A.

AU - Stolyarov, V.

AU - Bhatia, R.

AU - Kneissl, R.

AU - Bond, J.R.

AU - Miville-Deschênes, M.-A.

AU - MacIaszek, T.

AU - Banday, A.J.

AU - Bernard, J.-P.

AU - Forni, O.

AU - Giard, M.

AU - Leroy, C.

AU - Montier, L.

AU - Pointecouteau, E.

AU - Pons, R.

AU - Ristorcelli, I.

AU - Bock, J.J.

AU - Doré, O.

AU - Helou, G.

AU - Hildebrandt, S.R.

AU - Matsumura, T.

AU - Pearson, T.J.

AU - Prézeau, G.

AU - Rocha, G.

AU - Challinor, A.

AU - Shellard, P.

AU - Melin, J.-B.

AU - Starck, J.-L.

AU - Yvon, D.

AU - Nørgaard-Nielsen, Hans Ulrik

AU - Netterfield, C.B.

AU - Chiang, C.

AU - Jones, W.C.

AU - Knox, L.

AU - Wandelt, B.D.

AU - De Bernardis, P.

AU - Masi, S.

AU - Nati, F.

AU - Piacentini, F.

AU - Bersanelli, M.

AU - Kneissl, R.

AU - Tauber, J.A.

AU - Zacchei, A.

AU - Mandolesi, N.

AU - Bersanelli, M.

AU - Guyot, G.

AU - Désert, F.-X.

AU - Chamballu, A.

AU - Clements, D.L.

AU - Jaffe, A.H.

AU - Mortlock, D.

AU - Novikov, D.

AU - Rowan-Robinson, M.

AU - Chary, R.-R.

AU - Ganga, K.

AU - Lange, A.E.

AU - McGehee, P.

AU - Pearson, T.J.

AU - Rusholme, B.

AU - Benoît, A.

AU - Camus, P.

AU - Aghanim, N.

AU - Aumont, J.

AU - Boulanger, F.

AU - Charra, J.

AU - Charra, M.

AU - Dole, H.

AU - Douspis, M.

AU - Eng, P.

AU - Fourmond, J.-J.

AU - Gispert, R.

AU - Lagache, G.

AU - Lami, P.

AU - Leriche, B.

AU - Leroy, C.

AU - Longval, Y.

AU - Mercier, C.

AU - Miville-Deschênes, M.-A.

AU - Noviello, F.

AU - Pajot, F.

AU - Ponthieu, N.

AU - Puget, J.-L.

AU - Torre, J.-P.

AU - Vibert, L.

AU - Benabed, K.

AU - Bouchet, F.R.

AU - Cardoso, J.-F.

AU - Colombi, S.

AU - Delouis, J.-M.

AU - Hivon, E.

AU - Moneti, A.

AU - Prunet, S.

AU - Sygnet, J.-F.

AU - Wandelt, B.D.

AU - Fosalba, P.

AU - Wiesemeyer, H.

AU - Thum, C.

AU - Challinor, A.

AU - Efstathiou, G.

AU - Gratton, S.

AU - Harrison, D.

AU - Van Leeuwen, F.

AU - Hildebrandt, S.R.

AU - Bartlett, J.G.

AU - Bock, J.J.

AU - Crill, B.P.

AU - Doré, O.

AU - Górski, K.M.

AU - Holmes, W.A.

AU - Lawrence, C.R.

AU - Paine, C.

AU - Prézeau, G.

AU - Rocha, G.

AU - Wade, L.A.

AU - Maffei, B.

AU - Ashdown, M.

AU - Challinor, A.

AU - Gratton, S.

AU - Harrison, D.

AU - Lasenby, A.

AU - MacTavish, C.J.

AU - Catalano, A.

AU - Coulais, A.

AU - Lamarre, J.-M.

AU - Arnaud, M.

AU - Starck, J.-L.

AU - Cardoso, J.-F.

AU - Vibert, D.

AU - Girard, D.

AU - Hildebrandt, S.R.

AU - MacÍas-Pérez, J.F.

AU - Perotto, L.

AU - Renault, C.

AU - Santos, D.

AU - Stassi, P.

AU - Ansari, R.

AU - Couchot, F.

AU - Filliard, C.

AU - Haissinski, J.

AU - Henrot-Versillé, S.

AU - Lavabre, A.

AU - Mansoux, B.

AU - Perdereau, O.

AU - Plaszczynski, S.

AU - Touze, F.

AU - Tristram, M.

AU - Borrill, J.

AU - Banday, A.J.

AU - Bartelmann, M.

AU - Dolag, K.

AU - Hernández-Monteagudo, C.

AU - Sunyaev, R.

AU - White, S.D.M.

AU - Murphy, A.

AU - Peacocke, T.

AU - Yurchenko, V.

AU - Crill, B.P.

AU - Savini, G.

AU - Bradshaw, T.

AU - Crook, M.

AU - Mann, R.

AU - Ade, P.A.R.

AU - Griffin, M.

AU - North, C.

AU - Spencer, L.

AU - Sudiwala, R.

AU - Woodcraft, A.

AU - Sunyaev, R.

AU - Borrill, J.

AU - Church, S.

AU - Osborne, S.

AU - Bartelmann, M.

AU - Schaefer, B.M.

AU - Banday, A.J.

AU - Bernard, J.-P.

AU - Forni, O.

AU - Giard, M.

AU - Leroy, C.

AU - Montier, L.

AU - Pointecouteau, E.

AU - Pons, R.

AU - Ristorcelli, I.

AU - Reach, W.T.

AU - Battaner, E.

AU - Huffenberger, K.M.

AU - Górski, K.M.

PY - 2011

Y1 - 2011

N2 - The Planck High Frequency Instrument (HFI) is designed to measure the temperature and polarization anisotropies of the cosmic microwave background and Galactic foregrounds in six ~30% bands centered at 100, 143, 217, 353, 545, and 857 GHz at an angular resolution of 10′ (100 GHz), 7′ (143 GHz), and 5′ (217 GHz and higher). HFI has been operating flawlessly since launch on 14 May 2009, with the bolometers reaching 100 mK the first week of July. The settings of the readout electronics, including bolometer bias currents, that optimize HFI's noise performance on orbit are nearly the same as the ones chosen during ground testing. Observations of Mars, Jupiter, and Saturn have confirmed that the optical beams and the time responses of the detection chains are in good agreement with the predictions of physical optics modeling and pre-launch measurements. The Detectors suffer from a high flux of cosmic rays due to historically low levels of solar activity. As a result of the redundancy of Planck's observation strategy, theremoval of a few percent of data contaminated by glitches does not significantly affect the instrumental sensitivity. The cosmic ray flux represents a significant and variable heat load on the sub-Kelvin stage. Temporal variation and the inhomogeneous distribution of the flux results in thermal fluctuations that are a probable source of low frequency noise. The removal of systematic effects in the time ordered data provides a signal with an average noise equivalent power that is 70% of the goal in the 0.6-2.5 Hz range. This is slightly higher than was achieved during the pre-launch characterization but better than predicted in the early phases of the project. The improvement over the goal is a result of the low level of instrumental background loading achieved by the optical and thermal design of the HFI. © ESO, 2011.

AB - The Planck High Frequency Instrument (HFI) is designed to measure the temperature and polarization anisotropies of the cosmic microwave background and Galactic foregrounds in six ~30% bands centered at 100, 143, 217, 353, 545, and 857 GHz at an angular resolution of 10′ (100 GHz), 7′ (143 GHz), and 5′ (217 GHz and higher). HFI has been operating flawlessly since launch on 14 May 2009, with the bolometers reaching 100 mK the first week of July. The settings of the readout electronics, including bolometer bias currents, that optimize HFI's noise performance on orbit are nearly the same as the ones chosen during ground testing. Observations of Mars, Jupiter, and Saturn have confirmed that the optical beams and the time responses of the detection chains are in good agreement with the predictions of physical optics modeling and pre-launch measurements. The Detectors suffer from a high flux of cosmic rays due to historically low levels of solar activity. As a result of the redundancy of Planck's observation strategy, theremoval of a few percent of data contaminated by glitches does not significantly affect the instrumental sensitivity. The cosmic ray flux represents a significant and variable heat load on the sub-Kelvin stage. Temporal variation and the inhomogeneous distribution of the flux results in thermal fluctuations that are a probable source of low frequency noise. The removal of systematic effects in the time ordered data provides a signal with an average noise equivalent power that is 70% of the goal in the 0.6-2.5 Hz range. This is slightly higher than was achieved during the pre-launch characterization but better than predicted in the early phases of the project. The improvement over the goal is a result of the low level of instrumental background loading achieved by the optical and thermal design of the HFI. © ESO, 2011.

U2 - 10.1051/0004-6361/201116487

DO - 10.1051/0004-6361/201116487

M3 - Journal article

SN - 0004-6361

VL - 536

SP - A4

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

ER -

Planck early results. IV. First assessment of the High Frequency Instrument in-flight performance

Abstract

Access to Document

OpenUrl availability

Fingerprint

Cite this