Logo
ScienceStack
Table of Contents
Fetching ...
Sign In

Planck 2013 results. XIV. Zodiacal emission

Planck Collaboration, P. A. R. Ade, N. Aghanim, C. Armitage-Caplan, M. Arnaud, M. Ashdown, F. Atrio-Barandela, J. Aumont, C. Baccigalupi, A. J. Banday, R. B. Barreiro, J. G. Bartlett, E. Battaner, K. Benabed, A. Benoît, A. Benoit-Lévy, J. -P. Bernard, M. Bersanelli, P. Bielewicz, J. Bobin, J. J. Bock, A. Bonaldi, J. R. Bond, J. Borrill, F. R. Bouchet, F. Boulanger, M. Bridges, M. Bucher, C. Burigana, R. C. Butler, J. -F. Cardoso, A. Catalano, A. Chamballu, R. -R. Chary, X. Chen, H. C. Chiang, L. -Y Chiang, P. R. Christensen, S. Church, D. L. Clements, J. -M. Colley, S. Colombi, L. P. L. Colombo, F. Couchot, A. Coulais, B. P. Crill, A. Curto, F. Cuttaia, L. Danese, R. D. Davies, P. de Bernardis, A. de Rosa, G. de Zotti, J. Delabrouille, J. -M. Delouis, F. -X. Désert, C. Dickinson, J. M. Diego, H. Dole, S. Donzelli, O. Doré, M. Douspis, X. Dupac, G. Efstathiou, T. A. Enßlin, H. K. Eriksen, F. Finelli, O. Forni, M. Frailis, A. A. Fraisse, E. Franceschi, S. Galeotta, K. Ganga, M. Giard, Y. Giraud-Héraud, J. González-Nuevo, K. M. Górski, S. Gratton, A. Gregorio, A. Gruppuso, F. K. Hansen, D. Hanson, D. Harrison, G. Helou, S. Henrot-Versillé, C. Hernández-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. Keihänen, R. Keskitalo, T. S. Kisner, R. Kneissl, J. Knoche, L. Knox, M. Kunz, H. Kurki-Suonio, G. Lagache, A. Lähteenmäki, J. -M. Lamarre, A. Lasenby, R. J. Laureijs, C. R. Lawrence, R. Leonardi, J. Lesgourgues, M. Liguori, P. B. Lilje, M. Linden-Vørnle, M. López-Caniego, P. M. Lubin, J. F. Macías-Pérez, B. Maffei, D. Maino, N. Mandolesi, M. Maris, D. J. Marshall, P. G. Martin, E. Martínez-González, S. Masi, M. Massardi, S. Matarrese, F. Matthai, P. Mazzotta, P. R. Meinhold, A. Melchiorri, L. Mendes, A. Mennella, M. Migliaccio, S. Mitra, M. -A. Miville-Deschênes, 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. Nørgaard-Nielsen, 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. M. Polegre, G. Polenta, N. Ponthieu, L. Popa, T. Poutanen, G. W. Pratt, G. Prézeau, S. Prunet, J. -L. Puget, J. P. Rachen, W. T. Reach, R. Rebolo, M. Reinecke, M. Remazeilles, C. Renault, S. Ricciardi, T. Riller, I. Ristorcelli, G. Rocha, C. Rosset, G. Roudier, M. Rowan-Robinson, B. Rusholme, M. Sandri, D. Santos, G. Savini, D. Scott, M. D. Seiffert, E. P. S. Shellard, G. F. Smoot, L. D. Spencer, J. -L. Starck, V. Stolyarov, R. Stompor, R. Sudiwala, F. Sureau, D. Sutton, A. -S. Suur-Uski, J. -F. Sygnet, J. A. 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. A. Wade, B. D. Wandelt, D. Yvon, A. Zacchei, A. Zonca

Abstract

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.

Planck 2013 results. XIV. Zodiacal emission

Abstract

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.

Paper Structure

This paper contains 7 sections, 17 equations, 5 figures, 3 tables.

Table of Contents

  1. Introduction
  2. The Planck Mission
  3. Orbit, Scanning Strategy, and Dates of Observation
  4. Circumsolar Ring and Earth-Trailing Feature
  5. Integrated Emission
  6. Galactic Emission Seen Through Sidelobes
  7. Spectrum

Figures (5)

  • Figure 5: Origin of far sidelobes. The "SR Spillover" (for Secondary Reflector Spillover; the lowest set of rays on the left of the figure) arrives at the focal plane from outside the secondary mirror, directly from the sky. The "PR Spillover" (for Primary Reflector Spillover), arrives at the focal plane from above the primary mirror and reflects off the secondary to arrive at the focal plane. The set of rays between these two contributions represents the main beam. The "baffle" contribution, light reaching the focal plane after reflecting from the inner sides of the baffles, is not shown here. It is often included as part of the SR Spillover. Adopted from tauber2010b.
  • Figure 6: Templates of the dipole and the Galaxy, in MJy/sr, seen through our far sidelobes for Surveys 1 (left) and 2 (centre), and for the difference in these two (right). Row 1: dipole seen through the direct SR contribution. Row 2: dipole seen through the PR contribution. Row 3: dipole seen through the baffle SR contribution. Row 4: Galaxy seen through the direct SR contribution. Row 5: Galaxy seen through the PR contribution. Row 6: Galaxy seen through the baffle SR contribution. The simulations in Rows 4--6 are made using 857GHz data passed through the far sidelobe calculation described in Sect. \ref{['subsec:galFSL']}. The scales are different for the top and bottom three rows, and for the first two and the last columns.
  • Figure 7: Sequence of maps in MJy/sr, each building upon that above, designed to show the relative contributions of the various templates in Figs. \ref{['fig:zodiMaps']} and \ref{['fig:FSLs']}. Row 1: the sum of the last three templates in Fig. \ref{['fig:FSLs']}. Row 2: Row 1 plus Dust band 1. Row 3: Row 2 plus Dust band 2. Row 4: Row 3 plus Dust band 3. Row 5: Row 4 plus the Circumsolar Ring and Earth-Trailing Feature. Row 6: The far sidelobes and all zodiacal components. Left: Survey 1. Centre: Survey 2. Right: Survey 2 minus Survey 1. Note that the amplitudes used are only approximate, the figure being for illustrative purposes only. The scales change between the first and second rows, and between the fifth and sixth rows, as well as between the second and third column.
  • Figure 8: Emissivities of components from fits at 857GHz. Fits to the first year of Planck observations are in red, divided into Survey 1 (circles) and Survey 2 (squares). Fits to the second year are in blue, divided into Survey 3 (circles) and Survey 4 (squares). Absent time variability of the zodiacal emission, little difference would be expected between corresponding red and blue symbols. Agreement or disagreement between squares and circles gives some indication of systematic errors in the data and the correctness of the templates. The average of all measurements for each horn is shown as a black square, and the average and standard errors for the entire frequency, is given by the horizontal grey band. Dotted lines mark zero levels where appropriate. Similar plots for all HFI frequencies can be found in the Planck Explanatory Supplement planck2013-p28.
  • Figure 9: Emissivities of components of the K98 zodiacal emission model obtained from Planck/HFI ($\lambda > 250$m$$μ$m$) and COBE/DIRBE ($\lambda \le 250$m$$μ$m$, grey shading; K98). The Diffuse Cloud is shown as blue squares. For DIRBE, all dust bands (red, left-pointing triangles) were assumed have the same emissivity. For HFI, the bands (red, up-pointing triangles for Dust Band 1; pink, right-pointing triangles for Dust Band 2; and orange, down-pointing triangles for Dust Band 3) were allowed to have different emissivities. Similarly, K98 assumed that the Circumsolar Ring and Earth-Trailing Feature (green circles) had the same emissivities. For Planck the Circumsolar Ring (green hexagons) and Earth-Trailing Feature (yellow hexagons) were allowed to be different. Planck values were obtained by fitting an amplitude to each component, as well as the Galaxy seen through the sidelobes. All other parameters in the model were fixed at their K98 values. Each point is the average of the corresponding values obtained for all individual horns and Surveys at the given frequency, over the first two years of HFI data (grey-shaded regions in each panel of Fig. \ref{['fig:fit857']}. Error bars give the standard errors of these different measures. Numerical values are given in Table \ref{['tab:fullFit']}. Note that a few Cloud, Circumsolar Ring, and Earth-Trailing Feature values are negative, and so do not appear in this log--log plot. In such cases, the upper limit will appear as a short horizontal line. The dotted line indicates an emissivity of unity at all wavelengths, and the dashed line indicates an emissivity that is unity at wavelengths below 150μ$m$$\mu$m and proportional to $\lambda^{-2}$ at longer wavelengths.