Planck pre-launch status: The HFI instrument, from specification to actual performance

J. M. Lamarre; J. L. Puget; P. A R Ade; F. Bouchet; G. Guyot; A. E. Lange; F. Pajot; A. Arondel; K. Benabed; J. L. Beney; A. Benoît; J. Ph Bernard; R. Bhatia; Y. Blanc; J. J. Bock; E. Bréelle; T. W. Bradshaw; P. Camus; A. Catalano; J. Charra; M. Charra; S. E. Church; F. Couchot; A. Coulais; B. P. Crill; M. R. Crook; K. Dassas; P. De Bernardis; J. Delabrouille; P. De Marcillac; J. M. Delouis; F. X. Désert; C. Dumesnil; X. Dupac; G. Efstathiou; P. Eng; C. Evesque; J. J. Fourmond; K. Ganga; M. Giard; R. Gispert; L. Guglielmi; J. Haissinski; S. Henrot-Versillé; E. Hivon; W. A. Holmes; W. C. Jones; T. C. Koch; H. Lagardère; P. Lami; J. Landé; B. Leriche; C. Leroy; Y. Longval; J. F. MacÍas-Pérez; T. MacIaszek; B. Maffei; B. Mansoux; C. Marty; S. Masi; C. Mercier; M. A. Miville-Deschênes; A. Moneti; L. Montier; J. A. Murphy; J. Narbonne; M. Nexon; C. G. Paine; J. Pahn; O. Perdereau; F. Piacentini; M. Piat; S. Plaszczynski; E. Pointecouteau; R. Pons; N. Ponthieu; S. Prunet; D. Rambaud; G. Recouvreur; C. Renault; I. Ristorcelli; C. Rosset; D. Santos; G. Savini; G. Serra; P. Stassi; R. V. Sudiwala; J. F. Sygnet; J. A. Tauber; J. P. Torre; M. Tristram; L. Vibert; A. Woodcraft; V. Yurchenko; D. Yvon

doi:10.1051/0004-6361/200912975

Planck pre-launch status: The HFI instrument, from specification to actual performance

J. M. Lamarre, J. L. Puget, P. A R Ade, F. Bouchet, G. Guyot, A. E. Lange, F. Pajot, A. Arondel, K. Benabed, J. L. Beney, A. Benoît, J. Ph Bernard, R. Bhatia, Y. Blanc, J. J. Bock, E. Bréelle, T. W. Bradshaw, P. Camus, A. Catalano, J. CharraM. Charra, S. E. Church, F. Couchot, A. Coulais, B. P. Crill, M. R. Crook, K. Dassas, P. De Bernardis, J. Delabrouille, P. De Marcillac, J. M. Delouis, F. X. Désert, C. Dumesnil, X. Dupac, G. Efstathiou, P. Eng, C. Evesque, J. J. Fourmond, K. Ganga, M. Giard, R. Gispert, L. Guglielmi, J. Haissinski, S. Henrot-Versillé, E. Hivon, W. A. Holmes, W. C. Jones, T. C. Koch, H. Lagardère, P. Lami, J. Landé, B. Leriche, C. Leroy, Y. Longval, J. F. MacÍas-Pérez, T. MacIaszek, B. Maffei, B. Mansoux, C. Marty, S. Masi, C. Mercier, M. A. Miville-Deschênes, A. Moneti, L. Montier, J. A. Murphy, J. Narbonne, M. Nexon, C. G. Paine, J. Pahn, O. Perdereau, F. Piacentini, M. Piat, S. Plaszczynski, E. Pointecouteau, R. Pons, N. Ponthieu, S. Prunet, D. Rambaud, G. Recouvreur, C. Renault, I. Ristorcelli, C. Rosset, D. Santos, G. Savini, G. Serra, P. Stassi, R. V. Sudiwala, J. F. Sygnet, J. A. Tauber, J. P. Torre, M. Tristram, L. Vibert, A. Woodcraft, V. Yurchenko, D. Yvon

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

Abstract

Context. The High Frequency Instrument (HFI) is one of the two focal instruments of the Planck mission. It will observe the whole sky in six bands in the 100 GHz-1 THz range. Aims. The HFI instrument is designed to measure the cosmic microwave background (CMB) with a sensitivity limited only by fundamental sources: the photon noise of the CMB itself and the residuals left after the removal of foregrounds. The two high frequency bands will provide full maps of the submillimetre sky, featuring mainly extended and point source foregrounds. Systematic effects must be kept at negligible levels or accurately monitored so that the signal can be corrected. This paper describes the HFI design and its characteristics deduced from ground tests and calibration. Methods. The HFI instrumental concept and architecture are feasible only by pushing new techniques to their extreme capabilities, mainly: (i) bolometers working at 100 mK and absorbing the radiation in grids; (ii) a dilution cooler providing 100 mK in microgravity conditions; (iii) a new type of AC biased readout electronics and (iv) optical channels using devices inspired from radio and infrared techniques. Results. The Planck-HFI instrument performance exceeds requirements for sensitivity and control of systematic effects. During ground-based calibration and tests, it was measured at instrument and system levels to be close to or better than the goal specification. © ESO, 2010.

Original language	English
Article number	aa12975-09
Journal	Astronomy and Astrophysics
Volume	520
Issue number	1
DOIs	https://doi.org/10.1051/0004-6361/200912975
Publication status	Published - 15 Sept 2010

Keywords

cosmic microwave background
space vehicles: instruments
submillimeter: general
techniques: photometric
techniques: polarimetric

Access to Document

10.1051/0004-6361/200912975

http://adsabs.harvard.edu/abs/2010A%26A...520A...9L

Cite this

Lamarre, J. M., Puget, J. L., Ade, P. A. R., Bouchet, F., Guyot, G., Lange, A. E., Pajot, F., Arondel, A., Benabed, K., Beney, J. L., Benoît, A., Bernard, J. P., Bhatia, R., Blanc, Y., Bock, J. J., Bréelle, E., Bradshaw, T. W., Camus, P., Catalano, A., ... Yvon, D. (2010). Planck pre-launch status: The HFI instrument, from specification to actual performance. Astronomy and Astrophysics, 520(1), Article aa12975-09. https://doi.org/10.1051/0004-6361/200912975

@article{430655f76ed44f67bf121755e14473dc,

title = "Planck pre-launch status: The HFI instrument, from specification to actual performance",

abstract = "Context. The High Frequency Instrument (HFI) is one of the two focal instruments of the Planck mission. It will observe the whole sky in six bands in the 100 GHz-1 THz range. Aims. The HFI instrument is designed to measure the cosmic microwave background (CMB) with a sensitivity limited only by fundamental sources: the photon noise of the CMB itself and the residuals left after the removal of foregrounds. The two high frequency bands will provide full maps of the submillimetre sky, featuring mainly extended and point source foregrounds. Systematic effects must be kept at negligible levels or accurately monitored so that the signal can be corrected. This paper describes the HFI design and its characteristics deduced from ground tests and calibration. Methods. The HFI instrumental concept and architecture are feasible only by pushing new techniques to their extreme capabilities, mainly: (i) bolometers working at 100 mK and absorbing the radiation in grids; (ii) a dilution cooler providing 100 mK in microgravity conditions; (iii) a new type of AC biased readout electronics and (iv) optical channels using devices inspired from radio and infrared techniques. Results. The Planck-HFI instrument performance exceeds requirements for sensitivity and control of systematic effects. During ground-based calibration and tests, it was measured at instrument and system levels to be close to or better than the goal specification. {\textcopyright} ESO, 2010.",

keywords = "cosmic microwave background, space vehicles: instruments, submillimeter: general, techniques: photometric, techniques: polarimetric",

author = "Lamarre, {J. M.} and Puget, {J. L.} and Ade, {P. A R} and F. Bouchet and G. Guyot and Lange, {A. E.} and F. Pajot and A. Arondel and K. Benabed and Beney, {J. L.} and A. Beno{\^i}t and Bernard, {J. Ph} and R. Bhatia and Y. Blanc and Bock, {J. J.} and E. Br{\'e}elle and Bradshaw, {T. W.} and P. Camus and A. Catalano and J. Charra and M. Charra and Church, {S. E.} and F. Couchot and A. Coulais and Crill, {B. P.} and Crook, {M. R.} and K. Dassas and {De Bernardis}, P. and J. Delabrouille and {De Marcillac}, P. and Delouis, {J. M.} and D{\'e}sert, {F. X.} and C. Dumesnil and X. Dupac and G. Efstathiou and P. Eng and C. Evesque and Fourmond, {J. J.} and K. Ganga and M. Giard and R. Gispert and L. Guglielmi and J. Haissinski and S. Henrot-Versill{\'e} and E. Hivon and Holmes, {W. A.} and Jones, {W. C.} and Koch, {T. C.} and H. Lagard{\`e}re and P. Lami and J. Land{\'e} and B. Leriche and C. Leroy and Y. Longval and Mac{\'I}as-P{\'e}rez, {J. F.} and T. MacIaszek and B. Maffei and B. Mansoux and C. Marty and S. Masi and C. Mercier and Miville-Desch{\^e}nes, {M. A.} and A. Moneti and L. Montier and Murphy, {J. A.} and J. Narbonne and M. Nexon and Paine, {C. G.} and J. Pahn and O. Perdereau and F. Piacentini and M. Piat and S. Plaszczynski and E. Pointecouteau and R. Pons and N. Ponthieu and S. Prunet and D. Rambaud and G. Recouvreur and C. Renault and I. Ristorcelli and C. Rosset and D. Santos and G. Savini and G. Serra and P. Stassi and Sudiwala, {R. V.} and Sygnet, {J. F.} and Tauber, {J. A.} and Torre, {J. P.} and M. Tristram and L. Vibert and A. Woodcraft and V. Yurchenko and D. Yvon",

note = "DOI: 10.1051/0004-6361/200912975",

year = "2010",

month = sep,

day = "15",

doi = "10.1051/0004-6361/200912975",

language = "English",

volume = "520",

journal = "Astronomy and Astrophysics",

issn = "0004-6361",

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Lamarre, JM, Puget, JL, Ade, PAR, Bouchet, F, Guyot, G, Lange, AE, Pajot, F, Arondel, A, Benabed, K, Beney, JL, Benoît, A, Bernard, JP, Bhatia, R, Blanc, Y, Bock, JJ, Bréelle, E, Bradshaw, TW, Camus, P, Catalano, A, Charra, J, Charra, M, Church, SE, Couchot, F, Coulais, A, Crill, BP, Crook, MR, Dassas, K, De Bernardis, P, Delabrouille, J, De Marcillac, P, Delouis, JM, Désert, FX, Dumesnil, C, Dupac, X, Efstathiou, G, Eng, P, Evesque, C, Fourmond, JJ, Ganga, K, Giard, M, Gispert, R, Guglielmi, L, Haissinski, J, Henrot-Versillé, S, Hivon, E, Holmes, WA, Jones, WC, Koch, TC, Lagardère, H, Lami, P, Landé, J, Leriche, B, Leroy, C, Longval, Y, MacÍas-Pérez, JF, MacIaszek, T, Maffei, B, Mansoux, B, Marty, C, Masi, S, Mercier, C, Miville-Deschênes, MA, Moneti, A, Montier, L, Murphy, JA, Narbonne, J, Nexon, M, Paine, CG, Pahn, J, Perdereau, O, Piacentini, F, Piat, M, Plaszczynski, S, Pointecouteau, E, Pons, R, Ponthieu, N, Prunet, S, Rambaud, D, Recouvreur, G, Renault, C, Ristorcelli, I, Rosset, C, Santos, D, Savini, G, Serra, G, Stassi, P, Sudiwala, RV, Sygnet, JF, Tauber, JA, Torre, JP, Tristram, M, Vibert, L, Woodcraft, A, Yurchenko, V & Yvon, D 2010, 'Planck pre-launch status: The HFI instrument, from specification to actual performance', Astronomy and Astrophysics, vol. 520, no. 1, aa12975-09. https://doi.org/10.1051/0004-6361/200912975

TY - JOUR

T1 - Planck pre-launch status: The HFI instrument, from specification to actual performance

AU - Lamarre, J. M.

AU - Puget, J. L.

AU - Ade, P. A R

AU - Bouchet, F.

AU - Guyot, G.

AU - Lange, A. E.

AU - Pajot, F.

AU - Arondel, A.

AU - Benabed, K.

AU - Beney, J. L.

AU - Benoît, A.

AU - Bernard, J. Ph

AU - Bhatia, R.

AU - Blanc, Y.

AU - Bock, J. J.

AU - Bréelle, E.

AU - Bradshaw, T. W.

AU - Camus, P.

AU - Catalano, A.

AU - Charra, J.

AU - Charra, M.

AU - Church, S. E.

AU - Couchot, F.

AU - Coulais, A.

AU - Crill, B. P.

AU - Crook, M. R.

AU - Dassas, K.

AU - De Bernardis, P.

AU - Delabrouille, J.

AU - De Marcillac, P.

AU - Delouis, J. M.

AU - Désert, F. X.

AU - Dumesnil, C.

AU - Dupac, X.

AU - Efstathiou, G.

AU - Eng, P.

AU - Evesque, C.

AU - Fourmond, J. J.

AU - Ganga, K.

AU - Giard, M.

AU - Gispert, R.

AU - Guglielmi, L.

AU - Haissinski, J.

AU - Henrot-Versillé, S.

AU - Hivon, E.

AU - Holmes, W. A.

AU - Jones, W. C.

AU - Koch, T. C.

AU - Lagardère, H.

AU - Lami, P.

AU - Landé, J.

AU - Leriche, B.

AU - Leroy, C.

AU - Longval, Y.

AU - MacÍas-Pérez, J. F.

AU - MacIaszek, T.

AU - Maffei, B.

AU - Mansoux, B.

AU - Marty, C.

AU - Masi, S.

AU - Mercier, C.

AU - Miville-Deschênes, M. A.

AU - Moneti, A.

AU - Montier, L.

AU - Murphy, J. A.

AU - Narbonne, J.

AU - Nexon, M.

AU - Paine, C. G.

AU - Pahn, J.

AU - Perdereau, O.

AU - Piacentini, F.

AU - Piat, M.

AU - Plaszczynski, S.

AU - Pointecouteau, E.

AU - Pons, R.

AU - Ponthieu, N.

AU - Prunet, S.

AU - Rambaud, D.

AU - Recouvreur, G.

AU - Renault, C.

AU - Ristorcelli, I.

AU - Rosset, C.

AU - Santos, D.

AU - Savini, G.

AU - Serra, G.

AU - Stassi, P.

AU - Sudiwala, R. V.

AU - Sygnet, J. F.

AU - Tauber, J. A.

AU - Torre, J. P.

AU - Tristram, M.

AU - Vibert, L.

AU - Woodcraft, A.

AU - Yurchenko, V.

AU - Yvon, D.

N1 - DOI: 10.1051/0004-6361/200912975

PY - 2010/9/15

Y1 - 2010/9/15

N2 - Context. The High Frequency Instrument (HFI) is one of the two focal instruments of the Planck mission. It will observe the whole sky in six bands in the 100 GHz-1 THz range. Aims. The HFI instrument is designed to measure the cosmic microwave background (CMB) with a sensitivity limited only by fundamental sources: the photon noise of the CMB itself and the residuals left after the removal of foregrounds. The two high frequency bands will provide full maps of the submillimetre sky, featuring mainly extended and point source foregrounds. Systematic effects must be kept at negligible levels or accurately monitored so that the signal can be corrected. This paper describes the HFI design and its characteristics deduced from ground tests and calibration. Methods. The HFI instrumental concept and architecture are feasible only by pushing new techniques to their extreme capabilities, mainly: (i) bolometers working at 100 mK and absorbing the radiation in grids; (ii) a dilution cooler providing 100 mK in microgravity conditions; (iii) a new type of AC biased readout electronics and (iv) optical channels using devices inspired from radio and infrared techniques. Results. The Planck-HFI instrument performance exceeds requirements for sensitivity and control of systematic effects. During ground-based calibration and tests, it was measured at instrument and system levels to be close to or better than the goal specification. © ESO, 2010.

AB - Context. The High Frequency Instrument (HFI) is one of the two focal instruments of the Planck mission. It will observe the whole sky in six bands in the 100 GHz-1 THz range. Aims. The HFI instrument is designed to measure the cosmic microwave background (CMB) with a sensitivity limited only by fundamental sources: the photon noise of the CMB itself and the residuals left after the removal of foregrounds. The two high frequency bands will provide full maps of the submillimetre sky, featuring mainly extended and point source foregrounds. Systematic effects must be kept at negligible levels or accurately monitored so that the signal can be corrected. This paper describes the HFI design and its characteristics deduced from ground tests and calibration. Methods. The HFI instrumental concept and architecture are feasible only by pushing new techniques to their extreme capabilities, mainly: (i) bolometers working at 100 mK and absorbing the radiation in grids; (ii) a dilution cooler providing 100 mK in microgravity conditions; (iii) a new type of AC biased readout electronics and (iv) optical channels using devices inspired from radio and infrared techniques. Results. The Planck-HFI instrument performance exceeds requirements for sensitivity and control of systematic effects. During ground-based calibration and tests, it was measured at instrument and system levels to be close to or better than the goal specification. © ESO, 2010.

KW - cosmic microwave background

KW - space vehicles: instruments

KW - submillimeter: general

KW - techniques: photometric

KW - techniques: polarimetric

U2 - 10.1051/0004-6361/200912975

DO - 10.1051/0004-6361/200912975

M3 - Article

SN - 0004-6361

VL - 520

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

IS - 1

M1 - aa12975-09

ER -

Planck pre-launch status: The HFI instrument, from specification to actual performance

Abstract

Keywords

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