Planck 2013 results. XIV. Zodiacal emission

被引：78

作者：

Ade, P. A. R. ^{[89
]}

Aghanim, N. ^{[61
]}

Armitage-Caplan, C. ^{[93
]}

Arnaud, M. ^{[74
]}

Ashdown, M. ^{[6
,71
]}

Atrio-Barandela, F. ^{[19
]}

Aumont, J.

Baccigalupi, C. ^{[88
]}

Banday, A. J. ^{[10
,96
]}

Barreiro, R. B. ^{[68
]}

Bartlett, J. G. ^{[1
]}

Battaner, E. ^{[98
]}

Benabed, K. ^{[62
,95
]}

Benoit, A. ^{[59
]}

Benoit-Levy, A. ^{[26
,62
,95
]}

Bernard, J. -P. ^{[10
,96
]}

Bersanelli, M. ^{[37
,52
]}

Bielewicz, P. ^{[10
,88
,96
]}

Bobin, J. ^{[74
]}

Bock, J. J. ^{[11
]}

Bonaldi, A. ^{[69
,70
]}

Bond, J. R. ^{[9
]}

Borrill, J. ^{[14
,90
]}

Bouchet, F. R. ^{[62
,95
]}

Boulanger, F. ^{[61
]}

Bridges, M. ^{[6
,65
,71
]}

Bucher, M. ^{[1
]}

Burigana, C. ^{[35
,51
]}

Butler, R. C. ^{[51
]}

Cardoso, J. -F. ^{[1
,62
,75
,76
]}

Catalano, A. ^{[73
,77
]}

Chamballu, A. ^{[16
,61
,74
]}

Chary, R. -R. ^{[58
]}

Chen, X. ^{[58
]}

Chiang, H. C. ^{[7
,29
]}

Chiang, L. -Y ^{[64
]}

Christensen, P. R. ^{[40
,84
]}

Church, S. ^{[92
]}

Clements, D. L. ^{[57
]}

Colley, J. -M. ^{[1
,62
]}

Colombi, S. ^{[95
]}

Colombo, L. P. L. ^{[25
]}

Couchot, F. ^{[72
]}

Coulais, A. ^{[73
]}

Crill, B. P. ^{[85
]}

Curto, A. ^{[6
,68
]}

Cuttaia, F. ^{[51
]}

Danese, L. ^{[88
]}

Davies, R. D. ^{[69
,70
]}

de Bernardis, P. ^{[36
]}

机构：

[1] Univ Paris Diderot, Observ Paris, Sorbonne Paris Cite, CNRS IN2P3 CEA Irfu,APC, 10 Rue Alice Domon & Leonie Duquet, F-75205 Paris 13, France

[2] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland

[3] African Inst Math Sci, ZA-7945 Cape Town, South Africa

[4] Agenzia Spaziale Italiana, Sci Data Ctr, I-00133 Rome, Italy

[5] Agenzia Spaziale Italiana, I-00198 Rome, Italy

[6] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England

[7] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4000 Durban, South Africa

[8] ALMA Santiago Cent Off, Santiago 7630355, Chile

[9] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada

[10] CNRS, IRAP, F-31028 Toulouse 4, France

[11] CALTECH, Pasadena, CA 91125 USA

[12] Univ Cambridge, DAMTP, Ctr Theoret Cosmol, Cambridge CB3 0WA, England

[13] Ctr Estudios Fis Cosmos Aragon, Teruel 44001, Spain

[14] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA

[15] CSIC, E-28006 Madrid, Spain

[16] CEA Saclay, DSM Irfu SPP, F-91191 Gif Sur Yvette, France

[17] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark

[18] Univ Geneva, Dept Phys Theor, CH-1211 Geneva 4, Switzerland

[19] Univ Salamanca, Fac Ciencias, Dept Fis Fundamental, E-37008 Salamanca, Spain

[20] Univ Oviedo, Dept Fis, E-33007 Oviedo, Spain

[21] Univ Toronto, Dept Astron & Astrophys, Toronto, ON, Canada

[22] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands

[23] Univ Calif Berkeley, Dept Elect Engn & Comp Sci, Berkeley, CA 94720 USA

[24] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada

[25] Univ So Calif, Dept Phys & Astron, Dana & David Dornsife Coll Letter Arts & Sci, Los Angeles, CA 90089 USA

[26] UCL, Dept Phys & Astron, London WC1E 6BT, England

[27] Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA

[28] Univ Helsinki, Dept Phys, FIN-00014 Helsinki, Finland

[29] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA

[30] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA

[31] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA

[32] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA

[33] Univ Illinois UrbanaChampaign, Dept Phys, Urbana, IL USA

[34] Univ Padua, Dipartimento Fis & Astron G Galilei, I-35131 Padua, Italy

[35] Univ Ferrara, Dipartimento Fis & Sci Terra, I-44122 Ferrara, Italy

[36] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy

[37] Univ Milan, Dipartimento Fis, I-20133 Milan, Italy

[38] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy

[39] Univ Roma Tor Vergata, Dipartmento Fis, I-00133 Rome, Italy

[40] Niels Bohr Inst, Discovery Ctr, DK-2100 Copenhagen, Denmark

[41] Univ La Laguna, Dept Astrofis, Tenerife 38206, Spain

[42] European So Observ, ESO Vitacura, Santiago 19001, Chile

[43] European Space Agcy, ESAC, Planck Sci Off, Madrid 28692, Spain

[44] European Space Agcy, Estec, NL-2201 AZ Noordwijk, Netherlands

[45] Aalto Univ, Univ Helsinki, Helsinki Inst Phys, FIN-00014 Helsinki, Finland

[46] Osserv Astrofis Catania, INAF, I-95123 Catania, Italy

[47] Osserv Astron Padova, INAF, I-35122 Padua, Italy

[48] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy

[49] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy

[50] INAF Ist Radioastron, I-40129 Bologna, Italy

来源：

ASTRONOMY & ASTROPHYSICS | 2014年 / 571卷

关键词：

zodiacal dust; interplanetary medium; cosmic background radiation; DUST BANDS; IRAS OBSERVATIONS; ORIGIN; COBE; CLOUD; MODEL; COMETARY; SPECTRUM; LIGHT;

D O I：

10.1051/0004-6361/201321562

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The Planck satellite provides a set of all-sky maps at nine frequencies from 30 GHz to 857 GHz. Planets, minor bodies, and di ff use interplanetary dust emission (IPD) are all observed. The IPD can be separated from Galactic and other emissions because Planck views a given point on the celestial sphere multiple times, through di ff erent columns of IPD. We use the Planck data to investigate the behaviour of zodiacal emission over the whole sky at sub-millimetre and millimetre wavelengths. We fit the Planck data to find the emissivities of the various components of the COBE zodiacal model -a di ff use cloud, three asteroidal dust bands, a circumsolar ring, and an Earth-trailing feature. The emissivity of the diffuse cloud decreases with increasing wavelength, as expected from earlier analyses. The emissivities of the dust bands, however, decrease less rapidly, indicating that the properties of the grains in the bands are di ff erent from those in the di ff use cloud. We fit the small amount of Galactic emission seen through the telescope's far sidelobes, and place limits on possible contamination of the cosmic microwave background (CMB) results from both zodiacal and far-sidelobe emission. When necessary, the results are used in the Planck pipeline to make maps with zodiacal emission and far sidelobes removed. We show that the zodiacal correction to the CMB maps is small compared to the Planck CMB temperature power spectrum and give a list of flux densities for small solar system bodies.

引用

页数：25

共 75 条

[41] HEALPix:: A framework for high-resolution discretization and fast analysis of data distributed on the sphere
Górski, KM
Hivon, E
Banday, AJ
Wandelt, BD
Hansen, FK
Reinecke, M
Bartelmann, M
[J]. ASTROPHYSICAL JOURNAL, 2005, 622 (02) : 759 - 771
[42] The size-frequency distribution of the zodiacal cloud: Evidence from the solar system dust bands
Grogan, K
Dermott, SF
Durda, DD
[J]. ICARUS, 2001, 152 (02) : 251 - 267
[43] Can residuals of the solar system foreground explain low multipole anomalies of the CMB?
Hansen, M.
Kim, J.
Frejsel, A. M.
Ramazanov, S.
Naselsky, P.
Zhao, W.
Burigana, C.
[J]. JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS, 2012, (10):
[44] IRAS OBSERVATIONS OF THE DIFFUSE INFRARED BACKGROUND
HAUSER, MG
GILLETT, FC
LOW, FJ
GAUTIER, TN
BEICHMAN, CA
NEUGEBAUER, G
AUMANN, HH
BAUD, B
BOGGESS, N
EMERSON, JP
HOUCK, JR
SOIFER, BT
WALKER, RG
[J]. ASTROPHYSICAL JOURNAL, 1984, 278 (01) : L15 - L18
[45] A PHYSICAL MODEL FOR THE IRAS ZODIACAL DUST BANDS
JONES, MH
ROWANROBINSON, M
[J]. MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY, 1993, 264 (01) : 237 - 247
[46] A polarization sensitive bolometric receiver for observations of the cosmic microwave background
Jones, WC
Bhatia, RS
Bock, JJ
Lange, AE
[J]. MILLIMETER AND SUBMILLIMETER DETECTORS FOR ASTRONOMY, 2003, 4855 : 227 - 238
[47] The COBE Diffuse Infrared Background Experiment search for the cosmic infrared background.: II.: Model of the interplanetary dust cloud
Kelsall, T
Weiland, JL
Franz, BA
Reach, WT
Arendt, RG
Dwek, E
Freudenreich, HT
Hauser, MG
Moseley, SH
Odegard, NP
Silverberg, RF
Wright, EL
[J]. ASTROPHYSICAL JOURNAL, 1998, 508 (01) : 44 - 73
[48] Accretion of interplanetary dust particles by the Earth
Kortenkamp, SJ
Dermott, SF
[J]. ICARUS, 1998, 135 (02) : 469 - 495
[49] Planck pre-launch status: The HFI instrument, from specification to actual performance
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.
Benoit, A.
Bernard, J. -Ph.
Bhatia, R.
Blanc, Y.
Bock, J. J.
Breelle, E.
Bradshaw, T. W.
Camus, P.
Catalano, A.
Charra, J.
Charra, M.
Church, S. E.
Couchot, F.
Coulais, A.
Crill, B. P.
Crook, M. R.
Dassas, K.
de Bernardis, P.
Delabrouille, J.
de Marcillac, P.
Delouis, J. -M.
Desert, F. -X.
Dumesnil, C.
Dupac, X.
Efstathiou, G.
Eng, P.
Evesque, C.
Fourmond, J. -J.
Ganga, K.
Giard, M.
Gispert, R.
Guglielmi, L.
Haissinski, J.
Henrot-Versille, S.
Hivon, E.
Holmes, W. A.
Jones, W. C.
Koch, T. C.
Lagardere, H.
Lami, P.
[J]. ASTRONOMY & ASTROPHYSICS, 2010, 520
[50] Leinert C., 1997, VIZIER ONLINE DATA C

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