Planck 2013 results. XIV. Zodiacal emission
Planck 2013 results. XIV. Zodiacal emission
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普朗克 2013 年结果。
DOI：
10.1051/0004-6361/201321562
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发表时间：
2013
期刊：
影响因子：
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通讯作者：
A. Zonca
中科院分区：
文献类型：
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作者：
P. Ade;N. Aghanim;C. Armitage;M. Arnaud;M. Ashdown;F. Atrio;J. Aumont;C. Baccigalupi;A. Banday;R. B. Barreiro;J. G. Bartlett;E. Battaner;K. Benabed;A. Benoit;A. Benoit;J. Bernard;M. Bersanelli;P. Bielewicz;J. Bobin;J. Bock;A. Bonaldi;J. Bond;J. Borrill;F. Bouchet;F. Boulanger;M. Bridges;M. Bucher;C. Burigana;R. Butler;J. Cardoso;A. Catalano;A. Chamballu;R. Chary;X. Chen;H. Chiang;L. Chiang;P. Christensen;S. Church;D. Clements;J. Colley;S. Colombi;L. Colombo;F. Couchot;A. Coulais;B. Crill;A. Curto;F. Cuttaia;L. Danese;R. Davies;P. De Bernardis;A. de Rosa;G. De Zotti;J. Delabrouille;J. Delouis;F. Désert;C. Dickinson;J. M. Diego;H. Dole;S. Donzelli;O. Doré;M. Douspis;X. Dupac;G. Efstathiou;T. Ensslin;H. Eriksen;F. Finelli;O. Forni;M. Frailis;A. Fraisse;E. Franceschi;S. Galeotta;K. Ganga;M. Giard;Y. Giraud;J. González;K. Górski;S. Gratton;A. Gregorio;A. Gruppuso;F. Hansen;D. Hanson;D. Harrison;G. Helou;S. Henrot;C. Hernández;D. Herranz;S. Hildebrandt;E. Hivon;M. Hobson;W. Holmes;A. Hornstrup;W. Hovest;K. Huffenberger;A. Jaffe;T. R. Jaffe;W. Jones;M. Juvela;E. Keihänen;R. Keskitalo;T. Kisner;R. Kneissl;J. Knoche;L. Knox;M. Kunz;H. Kurki;G. Lagache;A. Lähteenmäki;J. Lamarre;A. Lasenby;R. Laureijs;C. Lawrence;R. Leonardi;J. Lesgourgues;M. Liguori;P. Lilje;M. Linden;M. López;P. Lubin;J. Macı́as;B. Maffei;D. Maino;N. Mandolesi;M. Maris;D. Marshall;P. Martin;E. Martinez;S. Masi;M. Massardi;S. Matarrese;F. Matthai;P. Mazzotta;P. Meinhold;A. Melchiorri;L. Mendes;A. Mennella;M. Migliaccio;S. Mitra;M. Miville;A. Moneti;L. Montier;G. Morgante;D. Mortlock;S. Mottet;D. Munshi;J. A. Murphy;P. Naselsky;F. Nati;P. Natoli;C. Netterfield;H. Nørgaard;F. Noviello;D. Novikov;I. Novikov;S. Osborne;C. O'Sullivan;C. A. Oxborrow;F. Paci;L. Pagano;F. Pajot;R. Paladini;D. Paoletti;F. Pasian;G. Patanchon;O. Perdereau;L. Perotto;F. Perrotta;F. Piacentini;M. Piat;E. Pierpaoli;D. Pietrobon;S. Plaszczynski;E. Pointecouteau;A. Polegre;G. Polenta;N. Ponthieu;L. Popa;T. Poutanen;G. Pratt;G. Prézeau;S. Prunet;J. Puget;J. Rachen;W. Reach;R. Rebolo;M. Reinecke;M. Remazeilles;C. Renault;S. Ricciardi;T. Riller;I. Ristorcelli;G. Rocha;C. Rosset;G. Roudier;M. Rowan;B. Rusholme;M. Sandri;D. Santos;G. Savini;D. Scott;M. Seiffert;E. Shellard;G. Smoot;L. Spencer;J. Starck;V. Stolyarov;R. Stompor;R. Sudiwala;F. Sureau;D. Sutton;A.;J. Sygnet;J. Tauber;D. Tavagnacco;L. Terenzi;L. Toffolatti;M. Tomasi;M. Tristram;M. Tucci;J. Tuovinen;G. Umana;L. Valenziano;J. Valiviita;B. van Tent;P. Vielva;F. Villa;N. Vittorio;L. Wade;B. Wandelt;D. Yvon;A. Zacchei;A. Zonca
普朗克卫星在30 GHz到857 GHz的9个频率上提供了一组全天地图。行星、小天体和弥漫的行星际尘埃排放(IPD)都被观测到。IPD可以与银河系和其他排放物分开，因为普朗克通过IPD的不同列多次查看天球上的一个给定点。我们使用普朗克数据来研究整个天空亚毫米和毫米波长黄道辐射的行为。我们对普朗克数据进行了拟合，以求出COBE黄道带模型的各个组成部分的发射率--扩散云、三个小行星尘埃带、一个绕太阳的环和一个地球拖尾特征。漫射云的发射率随着波长的增加而降低，正如早期分析所预期的那样。然而，尘埃带的发射率下降得不那么快，这表明尘埃带中的颗粒的性质与漫射云中的不同。我们符合通过望远镜远旁瓣观测到的少量银河辐射，并限制了黄道和远旁瓣辐射对CMB可能造成的污染。必要时，结果将用于普朗克管道，以制作去除黄道发射和远旁瓣的地图。我们表明，与普朗克CMB温度功率谱相比，CMB图的黄道校正较小，并给出了小型太阳系天体的通量密度列表。
The Planck satellite provides a set of all-sky maps at nine frequencies from 30 GHz to 857 GHz. Planets, minor bodies, and diffuse 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 different 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 diffuse 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 different from those in the diffuse cloud. We fit the small amount of Galactic emission seen through the telescope's far sidelobes, and place limits on possible contamination of the 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.