Planck 2013 results. X. HFI energetic particle effects: characterization, removal, and simulation
Articolo
Data di Pubblicazione:
2014
Abstract:
We describe the detection, interpretation, and removal of the signal
resulting from interactions of high energy particles with the Planck
High Frequency Instrument (HFI). There are two types of interactions:
heating of the 0.1 K bolometer plate; and glitches in each detector time
stream. The transientresponses to detector glitch shapes are not simple
single-pole exponential decays and fall into three families. The glitch
shape for each family has been characterized empirically in flight data
and these shapes have been used to remove glitches from the detector
time streams. The spectrum of the count rate per unit energy is computed
for each family and a correspondence is made to the location on the
detector of the particle hit. Most of the detected glitches are from
Galactic protons incident on the die frame supporting the micro-machined
bolometric detectors. In the Planck orbit at L2, the particle flux is
around 5 cm-2 s-1 and is dominated by protons
incident on the spacecraft with energy >39 MeV, at a rate of
typically one event per second per detector. Different categories of
glitches have different signatures in the time stream. Two of the glitch
types have a low amplitude component that decays over nearly 1 s. This
component produces excess noise if not properly removed from the
time-ordered data. We have used a glitch detection and subtraction
method based on the joint fit of population templates. The application
of this novel glitch subtraction method removes excess noise from the
time streams. Using realistic simulations, we find that this method does
not introduce signal bias into the Planck data.
resulting from interactions of high energy particles with the Planck
High Frequency Instrument (HFI). There are two types of interactions:
heating of the 0.1 K bolometer plate; and glitches in each detector time
stream. The transientresponses to detector glitch shapes are not simple
single-pole exponential decays and fall into three families. The glitch
shape for each family has been characterized empirically in flight data
and these shapes have been used to remove glitches from the detector
time streams. The spectrum of the count rate per unit energy is computed
for each family and a correspondence is made to the location on the
detector of the particle hit. Most of the detected glitches are from
Galactic protons incident on the die frame supporting the micro-machined
bolometric detectors. In the Planck orbit at L2, the particle flux is
around 5 cm-2 s-1 and is dominated by protons
incident on the spacecraft with energy >39 MeV, at a rate of
typically one event per second per detector. Different categories of
glitches have different signatures in the time stream. Two of the glitch
types have a low amplitude component that decays over nearly 1 s. This
component produces excess noise if not properly removed from the
time-ordered data. We have used a glitch detection and subtraction
method based on the joint fit of population templates. The application
of this novel glitch subtraction method removes excess noise from the
time streams. Using realistic simulations, we find that this method does
not introduce signal bias into the Planck data.
Tipologia CRIS:
1.1 Articolo in rivista
Keywords:
cosmic background radiation; cosmology: observations; instrumentation: detectors; space vehicles: instruments; methods: data analysis
Elenco autori:
P., Collaboration; P. A., R.; 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., Beno�t; A., Benoit L�vy; J., Bernard; M., Bersanelli; P., Bielewicz; J., Bobin; J. J., Bock; J. R., Bond; J., Borrill; F. R., Bouchet; M., Bridges; M., Bucher; C., Burigana; J., Cardoso; A., Catalano; A., Challinor; A., Chamballu; H. C., Chiang; L., Chiang; P. R., Christensen; S., Church; D. L., Clements; S., Colombi; L. P., L.; F., Couchot; A., Coulais; B. P., Crill; A., Curto; F., Cuttaia; L., Danese; R. D., Davies; P. d., Bernardis; A. d., Rosa; G. d., Zotti; J., Delabrouille; J., Delouis; F., D�sert; J. M., Diego; H., Dole; S., Donzelli; O., Dor�; M., Douspis; X., Dupac; G., Efstathiou; T. A., En�lin; H. K., Eriksen; F., Finelli; O., Forni; M., Frailis; E., Franceschi; S., Galeotta; K., Ganga; M., Giard; D., Girard; Y., Giraud H�raud; J., Gonz�lez Nuevo; K. M., G�rski; S., Gratton; A., Gregorio; A., Gruppuso; F. K., Hansen; D., Hanson; D., Harrison; S., Henrot Versill�; C., Hern�ndez Monteagudo; D., Herranz; S. R., Hildebrandt; E., Hivon; M., Hobson; W. A., Holmes; A., Hornstrup; W., Hovest; K. M., Huffenberger; A. H., Jaffe; T. R., Jaffe; W. C., Jones; M., Juvela; E., Keih�nen; R., Keskitalo; T. S., Kisner; R., Kneissl; J., Knoche; L., Knox; M., Kunz; H., Kurki Suonio; G., Lagache; J., Lamarre; A., Lasenby; R. J., Laureijs; C. R., Lawrence; R., Leonardi; C., Leroy; J., Lesgourgues; M., Liguori; P. B., Lilje; M., Linden V�rnle; M., L�pez Caniego; P. M., Lubin; J. F., Mac�as P�rez; N., Mandolesi; M., Maris; D. J., Marshall; P. G., Martin; E., Mart�nez Gonz�lez; S., Masi; M., Massardi; S., Matarrese; F., Matthai; P., Mazzotta; P., Mcgehee; A., Melchiorri; L., Mendes; A., Mennella; M., Migliaccio; A., Miniussi; S., Mitra; M., Miville Desch�nes; A., Moneti; L., Montier; G., Morgante; D., Mortlock; S., Mottet; D., Munshi; J. A., Murphy; P., Naselsky; F., Nati; P., Natoli; C. B., Netterfield; H. U., N�rgaard 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; G., Polenta; N., Ponthieu; L., Popa; T., Poutanen; G. W., Pratt; G., Pr�zeau; S., Prunet; J., Puget; J. P., Rachen; B., Racine; M., Reinecke; M., Remazeilles; C., Renault; S., Ricciardi; T., Riller; I., Ristorcelli; G., Rocha; C., Rosset; G., Roudier; B., Rusholme; L., Sanselme; D., Santos; A., Sauv�; G., Savini; D., Scott; E. P., S.; L. D., Spencer; J., Starck; V., Stolyarov; R., Stompor; R., Sudiwala; F., Sureau; D., Sutton; A., Suur Uski; J., Sygnet; J. A., Tauber; D., Tavagnacco; Terenzi, Luca; L., Toffolatti; M., Tomasi; M., Tristram; M., Tucci; G., Umana; L., Valenziano; J., Valiviita; B. V., Tent; P., Vielva; F., Villa; N., Vittorio; L. A., Wade; B. D., Wandelt; D., Yvon; A., Zacchei; A., Zonca
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