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

P. A.R. Ade; N. Aghanim; R. Ansari; M. Arnaud; M. Ashdown; J. Aumont; A. J. Banday; M. Bartelmann; J. G. Bartlett; E. Battaner; K. Benabed; A. Benoît; J. P. Bernard; M. Bersanelli; R. Bhatia; J. J. Bock; J. R. Bond; J. Borrill; F. R. Bouchet; F. Boulanger; T. Bradshaw; E. Bréelle; M. Bucher; P. Camus; J. F. Cardoso; A. Catalano; A. Challinor; A. Chamballu; J. Charra; M. Charra; R. R. Chary; C. Chiang; S. Church; D. L. Clements; S. Colombi; F. Couchot; A. Coulais; C. Cressiot; B. P. Crill; M. Crook; P. De Bernardis; J. Delabrouille; J. M. Delouis; F. X. Désert; K. Dolag; H. Dole; O. Doré; M. Douspis; G. Efstathiou; P. Eng; C. Filliard; O. Forni; P. Fosalba; J. J. Fourmond; K. Ganga; M. Giard; D. Girard; Y. Giraud-Héraud; R. Gispert; K. M. Górski; S. Gratton; M. Griffin; G. Guyot; J. Haissinski; D. Harrison; G. Helou; S. Henrot-Versillé; C. Hernández-Monteagudo; S. R. Hildebrandt; R. Hills; E. Hivon; M. Hobson; W. A. Holmes; K. M. Huffenberger; A. H. Jaffe; W. C. Jones; J. Kaplan; R. Kneissl; L. Knox; G. Lagache; J. M. Lamarre; P. Lami; A. E. Lange; A. Lasenby; A. Lavabre; C. R. Lawrence; B. Leriche; C. Leroy; Y. Longval; J. F. MacÍas-Pérez; T. MacIaszek; C. J. MacTavish; B. Maffei; N. Mandolesi; R. Mann; B. Mansoux; S. Masi; T. Matsumura; P. McGehee; J. B. Melin

doi:10.1051/0004-6361/201116487

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

P. A.R. Ade, N. Aghanim, R. Ansari, M. Arnaud, M. Ashdown, J. Aumont, A. J. Banday, M. Bartelmann, J. G. Bartlett, E. Battaner, K. Benabed, A. Benoît, J. P. Bernard, M. Bersanelli, R. Bhatia, J. J. Bock, J. R. Bond, J. Borrill, F. R. Bouchet, F. BoulangerT. Bradshaw, E. Bréelle, M. Bucher, P. Camus, J. F. Cardoso, A. Catalano, A. Challinor, A. Chamballu, J. Charra, M. Charra, R. R. Chary, C. Chiang, S. Church, D. L. Clements, S. Colombi, F. Couchot, A. Coulais, C. Cressiot, B. P. Crill, M. Crook, P. De Bernardis, J. Delabrouille, J. M. Delouis, F. X. Désert, K. Dolag, H. Dole, O. Doré, M. Douspis, G. Efstathiou, P. Eng, C. Filliard, O. Forni, P. Fosalba, J. J. Fourmond, K. Ganga, M. Giard, D. Girard, Y. Giraud-Héraud, R. Gispert, K. M. Górski, S. Gratton, M. Griffin, G. Guyot, J. Haissinski, D. Harrison, G. Helou, S. Henrot-Versillé, C. Hernández-Monteagudo, S. R. Hildebrandt, R. Hills, E. Hivon, M. Hobson, W. A. Holmes, K. M. Huffenberger, A. H. Jaffe, W. C. Jones, J. Kaplan, R. Kneissl, L. Knox, G. Lagache, J. M. Lamarre, P. Lami, A. E. Lange, A. Lasenby, A. Lavabre, C. R. Lawrence, B. Leriche, C. Leroy, Y. Longval, J. F. MacÍas-Pérez, T. MacIaszek, C. J. MacTavish, B. Maffei, N. Mandolesi, R. Mann, B. Mansoux, S. Masi, T. Matsumura, P. McGehee, J. B. Melin

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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
Article number	A4
Journal	Astronomy and Astrophysics
Volume	536
DOIs	https://doi.org/10.1051/0004-6361/201116487
Publication status	Published - 12 Dec 2011

Keywords

Cosmic background radiation
Cosmology
data analysis
detectors
Instrumentation
Methods
observations
photometers

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10.1051/0004-6361/201116487

Cite this

Ade, P. A. R., Aghanim, N., Ansari, R., Arnaud, M., Ashdown, M., Aumont, J., Banday, A. J., Bartelmann, M., Bartlett, J. G., Battaner, E., Benabed, K., Benoît, A., Bernard, J. P., Bersanelli, M., Bhatia, R., Bock, J. J., Bond, J. R., Borrill, J., Bouchet, F. R., ... Melin, J. B. (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{5510195222884b15a677c20bbfcb72f2,

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.",

keywords = "Cosmic background radiation, Cosmology, data analysis, detectors, Instrumentation, Methods, observations, photometers",

author = "Ade, {P. A.R.} and N. Aghanim and R. Ansari and M. Arnaud and M. Ashdown and J. Aumont and Banday, {A. J.} and M. Bartelmann and Bartlett, {J. G.} and E. Battaner and K. Benabed and A. Beno{\^i}t and Bernard, {J. P.} and M. Bersanelli and R. Bhatia and Bock, {J. J.} and Bond, {J. R.} and J. Borrill and Bouchet, {F. R.} and F. Boulanger and T. Bradshaw and E. Br{\'e}elle and M. Bucher and P. Camus and Cardoso, {J. F.} and A. Catalano and A. Challinor and A. Chamballu and J. Charra and M. Charra and Chary, {R. R.} and C. Chiang and S. Church and Clements, {D. L.} and S. Colombi and F. Couchot and A. Coulais and C. Cressiot and Crill, {B. P.} and M. Crook and {De Bernardis}, P. and J. Delabrouille and Delouis, {J. M.} and D{\'e}sert, {F. X.} and K. Dolag and H. Dole and O. Dor{\'e} and M. Douspis and G. Efstathiou and P. Eng and C. Filliard and O. Forni and P. Fosalba and Fourmond, {J. J.} and K. Ganga and M. Giard and D. Girard and Y. Giraud-H{\'e}raud and R. Gispert and G{\'o}rski, {K. M.} and S. Gratton and M. Griffin and G. Guyot and J. Haissinski and D. Harrison and G. Helou and S. Henrot-Versill{\'e} and C. Hern{\'a}ndez-Monteagudo and Hildebrandt, {S. R.} and R. Hills and E. Hivon and M. Hobson and Holmes, {W. A.} and Huffenberger, {K. M.} and Jaffe, {A. H.} and Jones, {W. C.} and J. Kaplan and R. Kneissl and L. Knox and G. Lagache and Lamarre, {J. M.} and P. Lami and Lange, {A. E.} and A. Lasenby and A. Lavabre and Lawrence, {C. R.} and B. Leriche and C. Leroy and Y. Longval and Mac{\'I}as-P{\'e}rez, {J. F.} and T. MacIaszek and MacTavish, {C. J.} and B. Maffei and N. Mandolesi and R. Mann and B. Mansoux and S. Masi and T. Matsumura and P. McGehee and Melin, {J. B.}",

year = "2011",

month = dec,

day = "12",

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

language = "English",

volume = "536",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

}

Ade, PAR, Aghanim, N, Ansari, R, Arnaud, M, Ashdown, M, Aumont, J, Banday, AJ, Bartelmann, M, Bartlett, JG, Battaner, E, Benabed, K, Benoît, A, Bernard, JP, Bersanelli, M, Bhatia, R, Bock, JJ, Bond, JR, Borrill, J, Bouchet, FR, Boulanger, F, Bradshaw, T, Bréelle, E, Bucher, M, Camus, P, Cardoso, JF, Catalano, A, Challinor, A, Chamballu, A, Charra, J, Charra, M, Chary, RR, Chiang, C, Church, S, Clements, DL, Colombi, S, Couchot, F, Coulais, A, Cressiot, C, Crill, BP, Crook, M, De Bernardis, P, Delabrouille, J, Delouis, JM, Désert, FX, Dolag, K, Dole, H, Doré, O, Douspis, M, Efstathiou, G, Eng, P, Filliard, C, Forni, O, Fosalba, P, Fourmond, JJ, Ganga, K, Giard, M, Girard, D, Giraud-Héraud, Y, Gispert, R, Górski, KM, Gratton, S, Griffin, M, Guyot, G, Haissinski, J, Harrison, D, Helou, G, Henrot-Versillé, S, Hernández-Monteagudo, C, Hildebrandt, SR, Hills, R, Hivon, E, Hobson, M, Holmes, WA, Huffenberger, KM, Jaffe, AH, Jones, WC, Kaplan, J, Kneissl, R, Knox, L, Lagache, G, Lamarre, JM, Lami, P, Lange, AE, Lasenby, A, Lavabre, A, Lawrence, CR, Leriche, B, Leroy, C, Longval, Y, MacÍas-Pérez, JF, MacIaszek, T, MacTavish, CJ, Maffei, B, Mandolesi, N, Mann, R, Mansoux, B, Masi, S, Matsumura, T, McGehee, P & Melin, JB 2011, 'Planck early results. IV. First assessment of the High Frequency Instrument in-flight performance', Astronomy and Astrophysics, vol. 536, 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 - Ade, P. A.R.

AU - Aghanim, N.

AU - Ansari, R.

AU - Arnaud, M.

AU - Ashdown, M.

AU - Aumont, J.

AU - Banday, A. J.

AU - Bartelmann, M.

AU - Bartlett, J. G.

AU - Battaner, E.

AU - Benabed, K.

AU - Benoît, A.

AU - Bernard, J. P.

AU - Bersanelli, M.

AU - Bhatia, R.

AU - Bock, J. J.

AU - Bond, J. R.

AU - Borrill, J.

AU - Bouchet, F. R.

AU - Boulanger, F.

AU - Bradshaw, T.

AU - Bréelle, E.

AU - Bucher, M.

AU - Camus, P.

AU - Cardoso, J. F.

AU - Catalano, A.

AU - Challinor, A.

AU - Chamballu, A.

AU - Charra, J.

AU - Charra, M.

AU - Chary, R. R.

AU - Chiang, C.

AU - Church, S.

AU - Clements, D. L.

AU - Colombi, S.

AU - Couchot, F.

AU - Coulais, A.

AU - Cressiot, C.

AU - Crill, B. P.

AU - Crook, M.

AU - De Bernardis, P.

AU - Delabrouille, J.

AU - Delouis, J. M.

AU - Désert, F. X.

AU - Dolag, K.

AU - Dole, H.

AU - Doré, O.

AU - Douspis, M.

AU - Efstathiou, G.

AU - Eng, P.

AU - Filliard, C.

AU - Forni, O.

AU - Fosalba, P.

AU - Fourmond, J. J.

AU - Ganga, K.

AU - Giard, M.

AU - Girard, D.

AU - Giraud-Héraud, Y.

AU - Gispert, R.

AU - Górski, K. M.

AU - Gratton, S.

AU - Griffin, M.

AU - Guyot, G.

AU - Haissinski, J.

AU - Harrison, D.

AU - Helou, G.

AU - Henrot-Versillé, S.

AU - Hernández-Monteagudo, C.

AU - Hildebrandt, S. R.

AU - Hills, R.

AU - Hivon, E.

AU - Hobson, M.

AU - Holmes, W. A.

AU - Huffenberger, K. M.

AU - Jaffe, A. H.

AU - Jones, W. C.

AU - Kaplan, J.

AU - Kneissl, R.

AU - Knox, L.

AU - Lagache, G.

AU - Lamarre, J. M.

AU - Lami, P.

AU - Lange, A. E.

AU - Lasenby, A.

AU - Lavabre, A.

AU - Lawrence, C. R.

AU - Leriche, B.

AU - Leroy, C.

AU - Longval, Y.

AU - MacÍas-Pérez, J. F.

AU - MacIaszek, T.

AU - MacTavish, C. J.

AU - Maffei, B.

AU - Mandolesi, N.

AU - Mann, R.

AU - Mansoux, B.

AU - Masi, S.

AU - Matsumura, T.

AU - McGehee, P.

AU - Melin, J. B.

PY - 2011/12/12

Y1 - 2011/12/12

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.

KW - Cosmic background radiation

KW - Cosmology

KW - data analysis

KW - detectors

KW - Instrumentation

KW - Methods

KW - observations

KW - photometers

U2 - 10.1051/0004-6361/201116487

DO - 10.1051/0004-6361/201116487

M3 - Article

SN - 0004-6361

VL - 536

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A4

ER -

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

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Keywords

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