Planck 2013 results. XIV. Zodiacal emission

Ade, P.A.R.; Wade, L.A.; Stolyarov, V.; Knoche, J.; Giard, M.; Dupac, X.; Liguori, M.; Matarrese, S.; Kurki-Suonio, H.; Mazzotta, P.; Mottet, S.; Coulais, A.; Tristram, M.; Smoot, G.F.; Bucher, M.; Mitra, S.; Umana, G.; de Zotti, G.; Leonardi, R.; Netterfield, C.B.; Martínez-González, E.; Paladini, R.; Mortlock, D.; Perotto, L.; Nørgaard-Nielsen, H.U.; Franceschi, E.; Roudier, G.; Pajot, F.; Santos, D.; Maris, M.; Colley, J. -M.; Nati, F.; Chiang, H.C.; Plaszczynski, S.; Crill, B.P.; Tuovinen, J.; Galeotta, S.; Reinecke, M.; Danese, L.; Puget, J. -L.; Christensen, P.R.; Poutanen, T.; Wandelt, B.D.; Gratton, S.; Dickinson, C.; Natoli, P.; Rusholme, B.; Meinhold, P.R.; Macías-Pérez, J.F.; Diego, J.M.; Remazeilles, M.; Giraud-Héraud, Y.; Villa, F.; Reach, W.T.; Battaner, E.; Tauber, J.A.; Riller, T.; Atrio-Barandela, F.; Starck, J. -L.; Miville-Deschênes, M. -A.; López-Caniego, M.; Sandri, M.; Efstathiou, G.; Paoletti, D.; Bock, J.J.; Bernard, J. -P.; Benabed, K.; Delabrouille, J.; Lesgourgues, J.; Martin, P.G.; Linden-Vørnle, M.; Vittorio, N.; Jaffe, T.R.; Mennella, A.; Church, S.; Valenziano, L.; Osborne, S.; Maino, D.; Savini, G.; Dole, H.; Perrotta, F.; Pasian, F.; Douspis, M.; Pratt, G.W.; Polenta, G.; Zonca, A.; Perdereau, O.; Chen, X.; Henrot-Versillé, S.; Bonaldi, A.; Ponthieu, N.; Cuttaia, F.; Moneti, A.; Pointecouteau, E.; Hobson, M.; Piacentini, F.; Bobin, J.; Munshi, D.; Tomasi, M.; Lamarre, J. -M.; Lilje, P.B.; Enßlin, T.A.; Montier, L.; Hivon, E.; Sureau, F.; Davies, R.D.; Cardoso, J. -F.; Marshall, D.J.; Stompor, R.; Ganga, K.; Rebolo, R.; Juvela, M.; Bartlett, J.G.; Baccigalupi, C.; Pierpaoli, E.; Oxborrow, C.A.; Rowan-Robinson, M.; González-Nuevo, J.; Shellard, E.P.S.; Knox, L.; Pietrobon, D.; Benoît, A.; Ricciardi, S.; Keihänen, E.; Mendes, L.; Chary, R. -R.; Lawrence, C.R.; Clements, D.L.; Ashdown, M.; Suur-Uski, A. -S.; Curto, A.; Scott, D.; Mandolesi, N.; Novikov, I.; Bersanelli, M.; Barreiro, R.B.; Hornstrup, A.; Popa, L.; Lagache, G.; Harrison, D.; Kisner, T.S.; Holmes, W.A.; Melchiorri, A.; Chamballu, A.; Rachen, J.P.; Hanson, D.; Frailis, M.; Hildebrandt, S.R.; Murphy, J.A.; Seiffert, M.D.; Delouis, J. -M.; Van Tent, B.; Gruppuso, A.; Donzelli, S.; Lähteenmäki, A.; Spencer, L.D.; Kneissl, R.; Górski, K.M.; Keskitalo, R.; Jones, W.C.; Zacchei, A.; Finelli, F.; Colombo, L.P.L.; Rocha, G.; Noviello, F.; Burigana, C.; Pagano, L.; Prézeau, G.; Naselsky, P.; Polegre, A.M.; Migliaccio, M.; Bouchet, F.R.; Kunz, M.; Masi, S.; Lubin, P.M.; Paci, F.; Sudiwala, R.; Yvon, D.; Novikov, D.; Bielewicz, P.; Patanchon, G.; Désert, F. -X.; Boulanger, F.; Armitage-Caplan, C.; Doré, O.; Valiviita, J.; Vielva, P.; Lasenby, A.; Hansen, F.K.; Sygnet, J. -F.; Prunet, S.; Terenzi, L.; Couchot, F.; de Rosa, A.; Bond, J.R.; Matthai, F.; Hernández-Monteagudo, C.; Jaffe, A.H.; Butler, R.C.; Laureijs, R.J.; Toffolatti, L.; Aumont, J.; Herranz, D.; Aghanim, N.; Eriksen, H.K.; Maffei, B.; Sutton, D.; Tucci, M.; Colombi, S.; Fraisse, A.A.; Tavagnacco, D.; de Bernardis, P.; Morgante, G.; O'Sullivan, C.; Arnaud, M.; Forni, O.; Rosset, C.; Chiang, L. -Y; Catalano, A.; Renault, C.; Piat, M.; Bridges, M.; Helou, G.; Ristorcelli, I.; Banday, A.J.; Borrill, J.; Hovest, W.; Huffenberger, K.M.; Benoit-Lévy, A.; Gregorio, A.
doi:10.1051/0004-6361/201321562
001530684 001__ 1530684
001530684 003__ SzGeCERN
001530684 005__ 20230312215011.0
001530684 0247_ $$2DOI$$a10.1051/0004-6361/201321562
001530684 0248_ $$aoai:cds.cern.ch:1530684$$pcerncds:FULLTEXT$$pcerncds:CERN:FULLTEXT$$pcerncds:CERN
001530684 035__ $$9arXiv$$aoai:arXiv.org:1303.5074
001530684 035__ $$9Inspire$$a1224739
001530684 037__ $$9arXiv$$aarXiv:1303.5074$$castro-ph.CO
001530684 037__ $$aCERN-PH-TH-2013-127
001530684 041__ $$aeng
001530684 084__ $$2CERN Librairy$$aTH-2013-127
001530684 088__ $$aCERN-PH-TH-2013-127
001530684 084__ $$2CERN Library$$aTH-2013-127
001530684 100__ $$aAde, P.A.R.
001530684 245__ $$aPlanck 2013 results. XIV. Zodiacal emission
001530684 260__ $$c2014-10-29
001530684 269__ $$c22 Mar 2013
001530684 300__ $$a25 p
001530684 520__ $$aThe 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.
001530684 520__ $$9arXiv$$aThe 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.
001530684 540__ $$3Preprint$$aCC-BY-3.0
001530684 542__ $$3Preprint$$dCERN$$g2013
001530684 595__ $$agiva a faire
001530684 595__ $$aLANL EDS
001530684 595__ $$aCERN-TH
001530684 595__ $$aNot for annual report
001530684 65017 $$2arXiv$$aAstrophysics and Astronomy
001530684 690C_ $$aARTICLE
001530684 690C_ $$aCERN
001530684 695__ $$9LANL EDS$$aastro-ph.CO
001530684 693__ $$ePLANCK RE24
001530684 700__ $$aAghanim, N.
001530684 700__ $$aArmitage-Caplan, C.
001530684 700__ $$aArnaud, M.
001530684 700__ $$aAshdown, M.
001530684 700__ $$aAtrio-Barandela, F.
001530684 700__ $$aAumont, J.
001530684 700__ $$aBaccigalupi, C.
001530684 700__ $$aBanday, A.J.
001530684 700__ $$aBarreiro, R.B.
001530684 700__ $$aBartlett, J.G.
001530684 700__ $$aBattaner, E.
001530684 700__ $$aBenabed, K.
001530684 700__ $$aBenoît, A.
001530684 700__ $$aBenoit-Lévy, A.
001530684 700__ $$aBernard, J. -P.
001530684 700__ $$aBersanelli, M.
001530684 700__ $$aBielewicz, P.
001530684 700__ $$aBobin, J.
001530684 700__ $$aBock, J.J.
001530684 700__ $$aBonaldi, A.
001530684 700__ $$aBond, J.R.
001530684 700__ $$aBorrill, J.
001530684 700__ $$aBouchet, F.R.
001530684 700__ $$aBoulanger, F.
001530684 700__ $$aBridges, M.
001530684 700__ $$aBucher, M.
001530684 700__ $$aBurigana, C.
001530684 700__ $$aButler, R.C.
001530684 700__ $$aCardoso, J. -F.
001530684 700__ $$aCatalano, A.
001530684 700__ $$aChamballu, A.
001530684 700__ $$aChary, R. -R.
001530684 700__ $$aChen, X.
001530684 700__ $$aChiang, L. -Y
001530684 700__ $$aChiang, H.C.
001530684 700__ $$aChristensen, P.R.
001530684 700__ $$aChurch, S.
001530684 700__ $$aClements, D.L.
001530684 700__ $$aColley, J. -M.
001530684 700__ $$aColombi, S.
001530684 700__ $$aColombo, L.P.L.
001530684 700__ $$aCouchot, F.
001530684 700__ $$aCoulais, A.
001530684 700__ $$aCrill, B.P.
001530684 700__ $$aCurto, A.
001530684 700__ $$aCuttaia, F.
001530684 700__ $$aDanese, L.
001530684 700__ $$aDavies, R.D.
001530684 700__ $$ade Bernardis, P.
001530684 700__ $$ade Rosa, A.
001530684 700__ $$ade Zotti, G.
001530684 700__ $$aDelabrouille, J.
001530684 700__ $$aDelouis, J. -M.
001530684 700__ $$aDésert, F. -X.
001530684 700__ $$aDickinson, C.
001530684 700__ $$aDiego, J.M.
001530684 700__ $$aDole, H.
001530684 700__ $$aDonzelli, S.
001530684 700__ $$aDoré, O.
001530684 700__ $$aDouspis, M.
001530684 700__ $$aDupac, X.
001530684 700__ $$aEfstathiou, G.
001530684 700__ $$aEnßlin, T.A.
001530684 700__ $$aEriksen, H.K.
001530684 700__ $$aFinelli, F.
001530684 700__ $$aForni, O.
001530684 700__ $$aFrailis, M.
001530684 700__ $$aFraisse, A.A.
001530684 700__ $$aFranceschi, E.
001530684 700__ $$aGaleotta, S.
001530684 700__ $$aGanga, K.
001530684 700__ $$aGiard, M.
001530684 700__ $$aGiraud-Héraud, Y.
001530684 700__ $$aGonzález-Nuevo, J.
001530684 700__ $$aGórski, K.M.
001530684 700__ $$aGratton, S.
001530684 700__ $$aGregorio, A.
001530684 700__ $$aGruppuso, A.
001530684 700__ $$aHansen, F.K.
001530684 700__ $$aHanson, D.
001530684 700__ $$aHarrison, D.
001530684 700__ $$aHelou, G.
001530684 700__ $$aHenrot-Versillé, S.
001530684 700__ $$aHernández-Monteagudo, C.
001530684 700__ $$aHerranz, D.
001530684 700__ $$aHildebrandt, S.R.
001530684 700__ $$aHivon, E.
001530684 700__ $$aHobson, M.
001530684 700__ $$aHolmes, W.A.
001530684 700__ $$aHornstrup, A.
001530684 700__ $$aHovest, W.
001530684 700__ $$aHuffenberger, K.M.
001530684 700__ $$aJaffe, T.R.
001530684 700__ $$aJaffe, A.H.
001530684 700__ $$aJones, W.C.
001530684 700__ $$aJuvela, M.
001530684 700__ $$aKeihänen, E.
001530684 700__ $$aKeskitalo, R.
001530684 700__ $$aKisner, T.S.
001530684 700__ $$aKneissl, R.
001530684 700__ $$aKnoche, J.
001530684 700__ $$aKnox, L.
001530684 700__ $$aKunz, M.
001530684 700__ $$aKurki-Suonio, H.
001530684 700__ $$aLagache, G.
001530684 700__ $$aLähteenmäki, A.
001530684 700__ $$aLamarre, J. -M.
001530684 700__ $$aLasenby, A.
001530684 700__ $$aLaureijs, R.J.
001530684 700__ $$aLawrence, C.R.
001530684 700__ $$aLeonardi, R.
001530684 700__ $$aLesgourgues, J.
001530684 700__ $$aLiguori, M.
001530684 700__ $$aLilje, P.B.
001530684 700__ $$aLinden-Vørnle, M.
001530684 700__ $$aLópez-Caniego, M.
001530684 700__ $$aLubin, P.M.
001530684 700__ $$aMacías-Pérez, J.F.
001530684 700__ $$aMaffei, B.
001530684 700__ $$aMaino, D.
001530684 700__ $$aMandolesi, N.
001530684 700__ $$aMaris, M.
001530684 700__ $$aMarshall, D.J.
001530684 700__ $$aMartin, P.G.
001530684 700__ $$aMartínez-González, E.
001530684 700__ $$aMasi, S.
001530684 700__ $$aMatarrese, S.
001530684 700__ $$aMatthai, F.
001530684 700__ $$aMazzotta, P.
001530684 700__ $$aMeinhold, P.R.
001530684 700__ $$aMelchiorri, A.
001530684 700__ $$aMendes, L.
001530684 700__ $$aMennella, A.
001530684 700__ $$aMigliaccio, M.
001530684 700__ $$aMitra, S.
001530684 700__ $$aMiville-Deschênes, M. -A.
001530684 700__ $$aMoneti, A.
001530684 700__ $$aMontier, L.
001530684 700__ $$aMorgante, G.
001530684 700__ $$aMortlock, D.
001530684 700__ $$aMottet, S.
001530684 700__ $$aMunshi, D.
001530684 700__ $$aMurphy, J.A.
001530684 700__ $$aNaselsky, P.
001530684 700__ $$aNati, F.
001530684 700__ $$aNatoli, P.
001530684 700__ $$aNetterfield, C.B.
001530684 700__ $$aNørgaard-Nielsen, H.U.
001530684 700__ $$aNoviello, F.
001530684 700__ $$aNovikov, D.
001530684 700__ $$aNovikov, I.
001530684 700__ $$aOsborne, S.
001530684 700__ $$aO'Sullivan, C.
001530684 700__ $$aOxborrow, C.A.
001530684 700__ $$aPaci, F.
001530684 700__ $$aPagano, L.
001530684 700__ $$aPajot, F.
001530684 700__ $$aPaladini, R.
001530684 700__ $$aPaoletti, D.
001530684 700__ $$aPasian, F.
001530684 700__ $$aPatanchon, G.
001530684 700__ $$aPerdereau, O.
001530684 700__ $$aPerotto, L.
001530684 700__ $$aPerrotta, F.
001530684 700__ $$aPiacentini, F.
001530684 700__ $$aPiat, M.
001530684 700__ $$aPierpaoli, E.
001530684 700__ $$aPietrobon, D.
001530684 700__ $$aPlaszczynski, S.
001530684 700__ $$aPointecouteau, E.
001530684 700__ $$aPolegre, A.M.
001530684 700__ $$aPolenta, G.
001530684 700__ $$aPonthieu, N.
001530684 700__ $$aPopa, L.
001530684 700__ $$aPoutanen, T.
001530684 700__ $$aPratt, G.W.
001530684 700__ $$aPrézeau, G.
001530684 700__ $$aPrunet, S.
001530684 700__ $$aPuget, J. -L.
001530684 700__ $$aRachen, J.P.
001530684 700__ $$aReach, W.T.
001530684 700__ $$aRebolo, R.
001530684 700__ $$aReinecke, M.
001530684 700__ $$aRemazeilles, M.
001530684 700__ $$aRenault, C.
001530684 700__ $$aRicciardi, S.
001530684 700__ $$aRiller, T.
001530684 700__ $$aRistorcelli, I.
001530684 700__ $$aRocha, G.
001530684 700__ $$aRosset, C.
001530684 700__ $$aRoudier, G.
001530684 700__ $$aRowan-Robinson, M.
001530684 700__ $$aRusholme, B.
001530684 700__ $$aSandri, M.
001530684 700__ $$aSantos, D.
001530684 700__ $$aSavini, G.
001530684 700__ $$aScott, D.
001530684 700__ $$aSeiffert, M.D.
001530684 700__ $$aShellard, E.P.S.
001530684 700__ $$aSmoot, G.F.
001530684 700__ $$aSpencer, L.D.
001530684 700__ $$aStarck, J. -L.
001530684 700__ $$aStolyarov, V.
001530684 700__ $$aStompor, R.
001530684 700__ $$aSudiwala, R.
001530684 700__ $$aSureau, F.
001530684 700__ $$aSutton, D.
001530684 700__ $$aSuur-Uski, A. -S.
001530684 700__ $$aSygnet, J. -F.
001530684 700__ $$aTauber, J.A.
001530684 700__ $$aTavagnacco, D.
001530684 700__ $$aTerenzi, L.
001530684 700__ $$aToffolatti, L.
001530684 700__ $$aTomasi, M.
001530684 700__ $$aTristram, M.
001530684 700__ $$aTucci, M.
001530684 700__ $$aTuovinen, J.
001530684 700__ $$aUmana, G.
001530684 700__ $$aValenziano, L.
001530684 700__ $$aValiviita, J.
001530684 700__ $$aVan Tent, B.
001530684 700__ $$aVielva, P.
001530684 700__ $$aVilla, F.
001530684 700__ $$aVittorio, N.
001530684 700__ $$aWade, L.A.
001530684 700__ $$aWandelt, B.D.
001530684 700__ $$aYvon, D.
001530684 700__ $$aZacchei, A.
001530684 700__ $$aZonca, A.
001530684 710__ $$gPlanck Collaboration
001530684 773__ $$cA14$$pAstron. Astrophys.$$v571$$y2014
001530684 8564_ $$uhttp://arxiv.org/pdf/1303.5074.pdf$$yPreprint
001530684 8564_ $$uhttp://www.aanda.org/articles/aa/pdf/2014/11/aa21562-13.pdf$$yEDP Sciences Free Access article
001530684 8564_ $$82431939$$s18378652$$uhttps://cds.cern.ch/record/1530684/files/arXiv:1303.5074.pdf
001530684 8564_ $$82431898$$s69243$$uhttps://cds.cern.ch/record/1530684/files/Z545SurveyJackknifeWiZodi.png$$y00063 Survey 2 minus Survey 1 difference maps, before (left) and after (right) zodiacal emission removal. The top two rows, for 857 and 545\,GHz, are in units MJy\,sr$^{-1}$, while the bottom row, for 353\,GHz, is in units of $\mu\mathrm{K}_\mathrm{CMB}$.
001530684 8564_ $$82431899$$s220373$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_survey1_Galactic_baffle.png$$y00040 Templates of the dipole and the Galaxy, in MJy/sr, seen through our far sidelobes for Surveys 1 (left) and 2 (centre), and for the difference in these two (right). Row~1: dipole seen through the direct SR contribution. Row~2: dipole seen through the PR contribution. Row~3: dipole seen through the baffle SR contribution. Row~4: Galaxy seen through the direct SR contribution. Row~5: Galaxy seen through the PR contribution. Row~6: Galaxy seen through the baffle SR contribution. The simulations in Rows~4--6 are made using 857\,GHz data passed through the far sidelobe calculation described in Sect.~\ref{subsec:galFSL}. The scales are different for the top and bottom three rows, and for the first two and the last columns.
001530684 8564_ $$82431900$$s265389$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_surveyD_tblob.png$$y00020 Estimated 857\,GHz zodiacal emission templates, in MJy/sr, based on the model of~K98, in Galactic coordinates, for Survey~1 (left), Survey~2 (center), and Survey~2 minus Survey~1 (right). From top to bottom we show Dust Band~1, Dust Band~2, Dust Band~3, the Circumsolar Ring, the Earth-Trailing Feature, and finally the Diffuse Cloud. Note that the scales for the right-hand column are different from those of the left-hand and centre columns, and that the scale for the bottom row is different from that of the others.
001530684 8564_ $$82431901$$s237068$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_survey1_Dipolar_secondary.png$$y00028 Templates of the dipole and the Galaxy, in MJy/sr, seen through our far sidelobes for Surveys 1 (left) and 2 (centre), and for the difference in these two (right). Row~1: dipole seen through the direct SR contribution. Row~2: dipole seen through the PR contribution. Row~3: dipole seen through the baffle SR contribution. Row~4: Galaxy seen through the direct SR contribution. Row~5: Galaxy seen through the PR contribution. Row~6: Galaxy seen through the baffle SR contribution. The simulations in Rows~4--6 are made using 857\,GHz data passed through the far sidelobe calculation described in Sect.~\ref{subsec:galFSL}. The scales are different for the top and bottom three rows, and for the first two and the last columns.
001530684 8564_ $$82431902$$s284110$$uhttps://cds.cern.ch/record/1530684/files/857-1_W_TauDeconv_survey2_I.png$$y00004 Single-Survey maps in Galactic coordinates for the 857-1 detector. \emph{Top:} Survey 1 map. \emph{Middle:} Survey 2 map. \emph{Bottom:} Survey 2 minus Survey 1 difference map. This bottom image shows the zodiacal emission and the residual Galactic emission effects that are discussed in the text. The units are MJy\,sr$^{-1}$, assuming a spectrum inversely proportional to frequency. Undefined pixels are shown in grey. These occur in pixels that either have not been observed during the Survey, were observed during the passage of a planet, or for a small number of other events. In the top two plots, pixels that were observed over periods longer than a week were not masked, and thus the masked regions are smaller in the top two images than that in the difference (bottom) panel. The units are MJy/sr.
001530684 8564_ $$82431903$$s265663$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_survey1_cloud.png$$y00021 Estimated 857\,GHz zodiacal emission templates, in MJy/sr, based on the model of~K98, in Galactic coordinates, for Survey~1 (left), Survey~2 (center), and Survey~2 minus Survey~1 (right). From top to bottom we show Dust Band~1, Dust Band~2, Dust Band~3, the Circumsolar Ring, the Earth-Trailing Feature, and finally the Diffuse Cloud. Note that the scales for the right-hand column are different from those of the left-hand and centre columns, and that the scale for the bottom row is different from that of the others.
001530684 8564_ $$82431904$$s70020$$uhttps://cds.cern.ch/record/1530684/files/Z100SurveyJackknifeNoZodi.png$$y00072 Survey 2 minus Survey 1 difference maps before (left) and after (right) zodiacal emission removal. The rows, from top to bottom, are for 217, 143, and 100\,GHz. All maps are in units of $\mu\mathrm{K}_\mathrm{CMB}$.
001530684 8564_ $$82431905$$s204034$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_survey1_Galactic_secondary.png$$y00037 Templates of the dipole and the Galaxy, in MJy/sr, seen through our far sidelobes for Surveys 1 (left) and 2 (centre), and for the difference in these two (right). Row~1: dipole seen through the direct SR contribution. Row~2: dipole seen through the PR contribution. Row~3: dipole seen through the baffle SR contribution. Row~4: Galaxy seen through the direct SR contribution. Row~5: Galaxy seen through the PR contribution. Row~6: Galaxy seen through the baffle SR contribution. The simulations in Rows~4--6 are made using 857\,GHz data passed through the far sidelobe calculation described in Sect.~\ref{subsec:galFSL}. The scales are different for the top and bottom three rows, and for the first two and the last columns.
001530684 8564_ $$82431906$$s242266$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_surveyD_band1.png$$y00014 Estimated 857\,GHz zodiacal emission templates, in MJy/sr, based on the model of~K98, in Galactic coordinates, for Survey~1 (left), Survey~2 (center), and Survey~2 minus Survey~1 (right). From top to bottom we show Dust Band~1, Dust Band~2, Dust Band~3, the Circumsolar Ring, the Earth-Trailing Feature, and finally the Diffuse Cloud. Note that the scales for the right-hand column are different from those of the left-hand and centre columns, and that the scale for the bottom row is different from that of the others.
001530684 8564_ $$82431907$$s254215$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_surveyD_band2.png$$y00011 Estimated 857\,GHz zodiacal emission templates, in MJy/sr, based on the model of~K98, in Galactic coordinates, for Survey~1 (left), Survey~2 (center), and Survey~2 minus Survey~1 (right). From top to bottom we show Dust Band~1, Dust Band~2, Dust Band~3, the Circumsolar Ring, the Earth-Trailing Feature, and finally the Diffuse Cloud. Note that the scales for the right-hand column are different from those of the left-hand and centre columns, and that the scale for the bottom row is different from that of the others.
001530684 8564_ $$82431908$$s241699$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_surveyD_band3.png$$y00008 Estimated 857\,GHz zodiacal emission templates, in MJy/sr, based on the model of~K98, in Galactic coordinates, for Survey~1 (left), Survey~2 (center), and Survey~2 minus Survey~1 (right). From top to bottom we show Dust Band~1, Dust Band~2, Dust Band~3, the Circumsolar Ring, the Earth-Trailing Feature, and finally the Diffuse Cloud. Note that the scales for the right-hand column are different from those of the left-hand and centre columns, and that the scale for the bottom row is different from that of the others.
001530684 8564_ $$82431909$$s215527$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_survey2_Galactic_secondary.png$$y00038 Templates of the dipole and the Galaxy, in MJy/sr, seen through our far sidelobes for Surveys 1 (left) and 2 (centre), and for the difference in these two (right). Row~1: dipole seen through the direct SR contribution. Row~2: dipole seen through the PR contribution. Row~3: dipole seen through the baffle SR contribution. Row~4: Galaxy seen through the direct SR contribution. Row~5: Galaxy seen through the PR contribution. Row~6: Galaxy seen through the baffle SR contribution. The simulations in Rows~4--6 are made using 857\,GHz data passed through the far sidelobe calculation described in Sect.~\ref{subsec:galFSL}. The scales are different for the top and bottom three rows, and for the first two and the last columns.
001530684 8564_ $$82431910$$s228963$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_survey1_6.png$$y00046 Sequence of maps in MJy/sr, each building upon that above, designed to show the relative contributions of the various templates in Figs.~\ref{fig:zodiMaps} and~\ref{fig:FSLs}. Row 1: the sum of the last three templates in Fig.~\ref{fig:FSLs}. Row 2: Row 1 plus Dust band~1. Row 3: Row 2 plus Dust band~2. Row 4: Row 3 plus Dust band~3. Row 5: Row 4 plus the Circumsolar Ring and Earth-Trailing Feature. Row 6: The far sidelobes and all zodiacal components. \emph{Left}: Survey 1. \emph{Centre}: Survey 2. \emph{Right}: Survey 2 minus Survey 1. Note that the amplitudes used are only approximate, the figure being for illustrative purposes only. The scales change between the first and second rows, and between the fifth and sixth rows, as well as between the second and third column.
001530684 8564_ $$82431911$$s259650$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_survey1_Dipolar_baffle.png$$y00031 Templates of the dipole and the Galaxy, in MJy/sr, seen through our far sidelobes for Surveys 1 (left) and 2 (centre), and for the difference in these two (right). Row~1: dipole seen through the direct SR contribution. Row~2: dipole seen through the PR contribution. Row~3: dipole seen through the baffle SR contribution. Row~4: Galaxy seen through the direct SR contribution. Row~5: Galaxy seen through the PR contribution. Row~6: Galaxy seen through the baffle SR contribution. The simulations in Rows~4--6 are made using 857\,GHz data passed through the far sidelobe calculation described in Sect.~\ref{subsec:galFSL}. The scales are different for the top and bottom three rows, and for the first two and the last columns.
001530684 8564_ $$82431912$$s293301$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_surveyD_Galactic_baffle.png$$y00042 Templates of the dipole and the Galaxy, in MJy/sr, seen through our far sidelobes for Surveys 1 (left) and 2 (centre), and for the difference in these two (right). Row~1: dipole seen through the direct SR contribution. Row~2: dipole seen through the PR contribution. Row~3: dipole seen through the baffle SR contribution. Row~4: Galaxy seen through the direct SR contribution. Row~5: Galaxy seen through the PR contribution. Row~6: Galaxy seen through the baffle SR contribution. The simulations in Rows~4--6 are made using 857\,GHz data passed through the far sidelobe calculation described in Sect.~\ref{subsec:galFSL}. The scales are different for the top and bottom three rows, and for the first two and the last columns.
001530684 8564_ $$82431913$$s256536$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_survey1_8.png$$y00052 Sequence of maps in MJy/sr, each building upon that above, designed to show the relative contributions of the various templates in Figs.~\ref{fig:zodiMaps} and~\ref{fig:FSLs}. Row 1: the sum of the last three templates in Fig.~\ref{fig:FSLs}. Row 2: Row 1 plus Dust band~1. Row 3: Row 2 plus Dust band~2. Row 4: Row 3 plus Dust band~3. Row 5: Row 4 plus the Circumsolar Ring and Earth-Trailing Feature. Row 6: The far sidelobes and all zodiacal components. \emph{Left}: Survey 1. \emph{Centre}: Survey 2. \emph{Right}: Survey 2 minus Survey 1. Note that the amplitudes used are only approximate, the figure being for illustrative purposes only. The scales change between the first and second rows, and between the fifth and sixth rows, as well as between the second and third column.
001530684 8564_ $$82431914$$s242352$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_survey1_7.png$$y00049 Sequence of maps in MJy/sr, each building upon that above, designed to show the relative contributions of the various templates in Figs.~\ref{fig:zodiMaps} and~\ref{fig:FSLs}. Row 1: the sum of the last three templates in Fig.~\ref{fig:FSLs}. Row 2: Row 1 plus Dust band~1. Row 3: Row 2 plus Dust band~2. Row 4: Row 3 plus Dust band~3. Row 5: Row 4 plus the Circumsolar Ring and Earth-Trailing Feature. Row 6: The far sidelobes and all zodiacal components. \emph{Left}: Survey 1. \emph{Centre}: Survey 2. \emph{Right}: Survey 2 minus Survey 1. Note that the amplitudes used are only approximate, the figure being for illustrative purposes only. The scales change between the first and second rows, and between the fifth and sixth rows, as well as between the second and third column.
001530684 8564_ $$82431915$$s225433$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_survey1_5.png$$y00043 Sequence of maps in MJy/sr, each building upon that above, designed to show the relative contributions of the various templates in Figs.~\ref{fig:zodiMaps} and~\ref{fig:FSLs}. Row 1: the sum of the last three templates in Fig.~\ref{fig:FSLs}. Row 2: Row 1 plus Dust band~1. Row 3: Row 2 plus Dust band~2. Row 4: Row 3 plus Dust band~3. Row 5: Row 4 plus the Circumsolar Ring and Earth-Trailing Feature. Row 6: The far sidelobes and all zodiacal components. \emph{Left}: Survey 1. \emph{Centre}: Survey 2. \emph{Right}: Survey 2 minus Survey 1. Note that the amplitudes used are only approximate, the figure being for illustrative purposes only. The scales change between the first and second rows, and between the fifth and sixth rows, as well as between the second and third column.
001530684 8564_ $$82431916$$s285280$$uhttps://cds.cern.ch/record/1530684/files/857-1_W_TauDeconv_survey1_I.png$$y00003 Single-Survey maps in Galactic coordinates for the 857-1 detector. \emph{Top:} Survey 1 map. \emph{Middle:} Survey 2 map. \emph{Bottom:} Survey 2 minus Survey 1 difference map. This bottom image shows the zodiacal emission and the residual Galactic emission effects that are discussed in the text. The units are MJy\,sr$^{-1}$, assuming a spectrum inversely proportional to frequency. Undefined pixels are shown in grey. These occur in pixels that either have not been observed during the Survey, were observed during the passage of a planet, or for a small number of other events. In the top two plots, pixels that were observed over periods longer than a week were not masked, and thus the masked regions are smaller in the top two images than that in the difference (bottom) panel. The units are MJy/sr.
001530684 8564_ $$82431917$$s256666$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_survey2_Dipolar_baffle.png$$y00032 Templates of the dipole and the Galaxy, in MJy/sr, seen through our far sidelobes for Surveys 1 (left) and 2 (centre), and for the difference in these two (right). Row~1: dipole seen through the direct SR contribution. Row~2: dipole seen through the PR contribution. Row~3: dipole seen through the baffle SR contribution. Row~4: Galaxy seen through the direct SR contribution. Row~5: Galaxy seen through the PR contribution. Row~6: Galaxy seen through the baffle SR contribution. The simulations in Rows~4--6 are made using 857\,GHz data passed through the far sidelobe calculation described in Sect.~\ref{subsec:galFSL}. The scales are different for the top and bottom three rows, and for the first two and the last columns.
001530684 8564_ $$82431918$$s256265$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_survey2_Dipolar_direct.png$$y00026 Templates of the dipole and the Galaxy, in MJy/sr, seen through our far sidelobes for Surveys 1 (left) and 2 (centre), and for the difference in these two (right). Row~1: dipole seen through the direct SR contribution. Row~2: dipole seen through the PR contribution. Row~3: dipole seen through the baffle SR contribution. Row~4: Galaxy seen through the direct SR contribution. Row~5: Galaxy seen through the PR contribution. Row~6: Galaxy seen through the baffle SR contribution. The simulations in Rows~4--6 are made using 857\,GHz data passed through the far sidelobe calculation described in Sect.~\ref{subsec:galFSL}. The scales are different for the top and bottom three rows, and for the first two and the last columns.
001530684 8564_ $$82431919$$s304975$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_surveyD_7.png$$y00051 Sequence of maps in MJy/sr, each building upon that above, designed to show the relative contributions of the various templates in Figs.~\ref{fig:zodiMaps} and~\ref{fig:FSLs}. Row 1: the sum of the last three templates in Fig.~\ref{fig:FSLs}. Row 2: Row 1 plus Dust band~1. Row 3: Row 2 plus Dust band~2. Row 4: Row 3 plus Dust band~3. Row 5: Row 4 plus the Circumsolar Ring and Earth-Trailing Feature. Row 6: The far sidelobes and all zodiacal components. \emph{Left}: Survey 1. \emph{Centre}: Survey 2. \emph{Right}: Survey 2 minus Survey 1. Note that the amplitudes used are only approximate, the figure being for illustrative purposes only. The scales change between the first and second rows, and between the fifth and sixth rows, as well as between the second and third column.
001530684 8564_ $$82431920$$s300626$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_surveyD_6.png$$y00048 Sequence of maps in MJy/sr, each building upon that above, designed to show the relative contributions of the various templates in Figs.~\ref{fig:zodiMaps} and~\ref{fig:FSLs}. Row 1: the sum of the last three templates in Fig.~\ref{fig:FSLs}. Row 2: Row 1 plus Dust band~1. Row 3: Row 2 plus Dust band~2. Row 4: Row 3 plus Dust band~3. Row 5: Row 4 plus the Circumsolar Ring and Earth-Trailing Feature. Row 6: The far sidelobes and all zodiacal components. \emph{Left}: Survey 1. \emph{Centre}: Survey 2. \emph{Right}: Survey 2 minus Survey 1. Note that the amplitudes used are only approximate, the figure being for illustrative purposes only. The scales change between the first and second rows, and between the fifth and sixth rows, as well as between the second and third column.
001530684 8564_ $$82431921$$s291606$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_surveyD_5.png$$y00045 Sequence of maps in MJy/sr, each building upon that above, designed to show the relative contributions of the various templates in Figs.~\ref{fig:zodiMaps} and~\ref{fig:FSLs}. Row 1: the sum of the last three templates in Fig.~\ref{fig:FSLs}. Row 2: Row 1 plus Dust band~1. Row 3: Row 2 plus Dust band~2. Row 4: Row 3 plus Dust band~3. Row 5: Row 4 plus the Circumsolar Ring and Earth-Trailing Feature. Row 6: The far sidelobes and all zodiacal components. \emph{Left}: Survey 1. \emph{Centre}: Survey 2. \emph{Right}: Survey 2 minus Survey 1. Note that the amplitudes used are only approximate, the figure being for illustrative purposes only. The scales change between the first and second rows, and between the fifth and sixth rows, as well as between the second and third column.
001530684 8564_ $$82431922$$s262914$$uhttps://cds.cern.ch/record/1530684/files/jd_h857-1_s1_d07_v53.png$$y00002 Julian date of observation of pixels on the sky during Survey 1, for a single detector, in Galactic coordinates. There are only very small differences between maps for different detectors. The grid lines show ecliptic coordinates, with the darker lines representing the ecliptic plane and the line of zero ecliptic longitude. Undefined pixels, which were either not observed at all, or which were observed multiple times over a period that spanned more than one week and are thus not used in this analysis, are shown as the uniform grey band.
001530684 8564_ $$82431923$$s261704$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_surveyD_cloud.png$$y00023 Estimated 857\,GHz zodiacal emission templates, in MJy/sr, based on the model of~K98, in Galactic coordinates, for Survey~1 (left), Survey~2 (center), and Survey~2 minus Survey~1 (right). From top to bottom we show Dust Band~1, Dust Band~2, Dust Band~3, the Circumsolar Ring, the Earth-Trailing Feature, and finally the Diffuse Cloud. Note that the scales for the right-hand column are different from those of the left-hand and centre columns, and that the scale for the bottom row is different from that of the others.
001530684 8564_ $$82431924$$s70107$$uhttps://cds.cern.ch/record/1530684/files/Z100SurveyJackknifeWiZodi.png$$y00071 Survey 2 minus Survey 1 difference maps before (left) and after (right) zodiacal emission removal. The rows, from top to bottom, are for 217, 143, and 100\,GHz. All maps are in units of $\mu\mathrm{K}_\mathrm{CMB}$.
001530684 8564_ $$82431925$$s268137$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_surveyD_Dipolar_secondary.png$$y00030 Templates of the dipole and the Galaxy, in MJy/sr, seen through our far sidelobes for Surveys 1 (left) and 2 (centre), and for the difference in these two (right). Row~1: dipole seen through the direct SR contribution. Row~2: dipole seen through the PR contribution. Row~3: dipole seen through the baffle SR contribution. Row~4: Galaxy seen through the direct SR contribution. Row~5: Galaxy seen through the PR contribution. Row~6: Galaxy seen through the baffle SR contribution. The simulations in Rows~4--6 are made using 857\,GHz data passed through the far sidelobe calculation described in Sect.~\ref{subsec:galFSL}. The scales are different for the top and bottom three rows, and for the first two and the last columns.
001530684 8564_ $$82431926$$s267625$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_survey1_11.png$$y00058 Sequence of maps in MJy/sr, each building upon that above, designed to show the relative contributions of the various templates in Figs.~\ref{fig:zodiMaps} and~\ref{fig:FSLs}. Row 1: the sum of the last three templates in Fig.~\ref{fig:FSLs}. Row 2: Row 1 plus Dust band~1. Row 3: Row 2 plus Dust band~2. Row 4: Row 3 plus Dust band~3. Row 5: Row 4 plus the Circumsolar Ring and Earth-Trailing Feature. Row 6: The far sidelobes and all zodiacal components. \emph{Left}: Survey 1. \emph{Centre}: Survey 2. \emph{Right}: Survey 2 minus Survey 1. Note that the amplitudes used are only approximate, the figure being for illustrative purposes only. The scales change between the first and second rows, and between the fifth and sixth rows, as well as between the second and third column.
001530684 8564_ $$82431927$$s63204$$uhttps://cds.cern.ch/record/1530684/files/Z353SurveyJackknifeWiZodi.png$$y00065 Survey 2 minus Survey 1 difference maps, before (left) and after (right) zodiacal emission removal. The top two rows, for 857 and 545\,GHz, are in units MJy\,sr$^{-1}$, while the bottom row, for 353\,GHz, is in units of $\mu\mathrm{K}_\mathrm{CMB}$.
001530684 8564_ $$82431928$$s68878$$uhttps://cds.cern.ch/record/1530684/files/Z217SurveyJackknifeNoZodi.png$$y00068 Survey 2 minus Survey 1 difference maps before (left) and after (right) zodiacal emission removal. The rows, from top to bottom, are for 217, 143, and 100\,GHz. All maps are in units of $\mu\mathrm{K}_\mathrm{CMB}$.
001530684 8564_ $$82431929$$s214969$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_survey2_cring.png$$y00016 Estimated 857\,GHz zodiacal emission templates, in MJy/sr, based on the model of~K98, in Galactic coordinates, for Survey~1 (left), Survey~2 (center), and Survey~2 minus Survey~1 (right). From top to bottom we show Dust Band~1, Dust Band~2, Dust Band~3, the Circumsolar Ring, the Earth-Trailing Feature, and finally the Diffuse Cloud. Note that the scales for the right-hand column are different from those of the left-hand and centre columns, and that the scale for the bottom row is different from that of the others.
001530684 8564_ $$82431930$$s214276$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_survey1_Galactic_direct.png$$y00034 Templates of the dipole and the Galaxy, in MJy/sr, seen through our far sidelobes for Surveys 1 (left) and 2 (centre), and for the difference in these two (right). Row~1: dipole seen through the direct SR contribution. Row~2: dipole seen through the PR contribution. Row~3: dipole seen through the baffle SR contribution. Row~4: Galaxy seen through the direct SR contribution. Row~5: Galaxy seen through the PR contribution. Row~6: Galaxy seen through the baffle SR contribution. The simulations in Rows~4--6 are made using 857\,GHz data passed through the far sidelobe calculation described in Sect.~\ref{subsec:galFSL}. The scales are different for the top and bottom three rows, and for the first two and the last columns.
001530684 8564_ $$82431931$$s65834$$uhttps://cds.cern.ch/record/1530684/files/Z143SurveyJackknifeNoZodi.png$$y00070 Survey 2 minus Survey 1 difference maps before (left) and after (right) zodiacal emission removal. The rows, from top to bottom, are for 217, 143, and 100\,GHz. All maps are in units of $\mu\mathrm{K}_\mathrm{CMB}$.
001530684 8564_ $$82431932$$s228777$$uhttps://cds.cern.ch/record/1530684/files/Rays-sketch-2.png$$y00024 Origin of far sidelobes. The ``SR Spillover'' (for Secondary Reflector Spillover; the lowest set of rays on the left of the figure) arrives at the focal plane from outside the secondary mirror, directly from the sky. The ``PR Spillover'' (for Primary Reflector Spillover), arrives at the focal plane from above the primary mirror and reflects off the secondary to arrive at the focal plane. The set of rays between these two contributions represents the main beam. The ``baffle'' contribution, light reaching the focal plane after reflecting from the inner sides of the baffles, is not shown here. It is often included as part of the SR Spillover. Adopted from~\cite{tauber2010b}.
001530684 8564_ $$82431933$$s234126$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_survey2_Dipolar_secondary.png$$y00029 Templates of the dipole and the Galaxy, in MJy/sr, seen through our far sidelobes for Surveys 1 (left) and 2 (centre), and for the difference in these two (right). Row~1: dipole seen through the direct SR contribution. Row~2: dipole seen through the PR contribution. Row~3: dipole seen through the baffle SR contribution. Row~4: Galaxy seen through the direct SR contribution. Row~5: Galaxy seen through the PR contribution. Row~6: Galaxy seen through the baffle SR contribution. The simulations in Rows~4--6 are made using 857\,GHz data passed through the far sidelobe calculation described in Sect.~\ref{subsec:galFSL}. The scales are different for the top and bottom three rows, and for the first two and the last columns.
001530684 8564_ $$82431934$$s274358$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_survey1_10.png$$y00055 Sequence of maps in MJy/sr, each building upon that above, designed to show the relative contributions of the various templates in Figs.~\ref{fig:zodiMaps} and~\ref{fig:FSLs}. Row 1: the sum of the last three templates in Fig.~\ref{fig:FSLs}. Row 2: Row 1 plus Dust band~1. Row 3: Row 2 plus Dust band~2. Row 4: Row 3 plus Dust band~3. Row 5: Row 4 plus the Circumsolar Ring and Earth-Trailing Feature. Row 6: The far sidelobes and all zodiacal components. \emph{Left}: Survey 1. \emph{Centre}: Survey 2. \emph{Right}: Survey 2 minus Survey 1. Note that the amplitudes used are only approximate, the figure being for illustrative purposes only. The scales change between the first and second rows, and between the fifth and sixth rows, as well as between the second and third column.
001530684 8564_ $$82431935$$s279365$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_survey2_10.png$$y00056 Sequence of maps in MJy/sr, each building upon that above, designed to show the relative contributions of the various templates in Figs.~\ref{fig:zodiMaps} and~\ref{fig:FSLs}. Row 1: the sum of the last three templates in Fig.~\ref{fig:FSLs}. Row 2: Row 1 plus Dust band~1. Row 3: Row 2 plus Dust band~2. Row 4: Row 3 plus Dust band~3. Row 5: Row 4 plus the Circumsolar Ring and Earth-Trailing Feature. Row 6: The far sidelobes and all zodiacal components. \emph{Left}: Survey 1. \emph{Centre}: Survey 2. \emph{Right}: Survey 2 minus Survey 1. Note that the amplitudes used are only approximate, the figure being for illustrative purposes only. The scales change between the first and second rows, and between the fifth and sixth rows, as well as between the second and third column.
001530684 8564_ $$82431936$$s212312$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_survey2_Galactic_direct.png$$y00035 Templates of the dipole and the Galaxy, in MJy/sr, seen through our far sidelobes for Surveys 1 (left) and 2 (centre), and for the difference in these two (right). Row~1: dipole seen through the direct SR contribution. Row~2: dipole seen through the PR contribution. Row~3: dipole seen through the baffle SR contribution. Row~4: Galaxy seen through the direct SR contribution. Row~5: Galaxy seen through the PR contribution. Row~6: Galaxy seen through the baffle SR contribution. The simulations in Rows~4--6 are made using 857\,GHz data passed through the far sidelobe calculation described in Sect.~\ref{subsec:galFSL}. The scales are different for the top and bottom three rows, and for the first two and the last columns.
001530684 8564_ $$82431937$$s65952$$uhttps://cds.cern.ch/record/1530684/files/Z143SurveyJackknifeWiZodi.png$$y00069 Survey 2 minus Survey 1 difference maps before (left) and after (right) zodiacal emission removal. The rows, from top to bottom, are for 217, 143, and 100\,GHz. All maps are in units of $\mu\mathrm{K}_\mathrm{CMB}$.
001530684 8564_ $$82431938$$s275591$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_surveyD_11.png$$y00060 Sequence of maps in MJy/sr, each building upon that above, designed to show the relative contributions of the various templates in Figs.~\ref{fig:zodiMaps} and~\ref{fig:FSLs}. Row 1: the sum of the last three templates in Fig.~\ref{fig:FSLs}. Row 2: Row 1 plus Dust band~1. Row 3: Row 2 plus Dust band~2. Row 4: Row 3 plus Dust band~3. Row 5: Row 4 plus the Circumsolar Ring and Earth-Trailing Feature. Row 6: The far sidelobes and all zodiacal components. \emph{Left}: Survey 1. \emph{Centre}: Survey 2. \emph{Right}: Survey 2 minus Survey 1. Note that the amplitudes used are only approximate, the figure being for illustrative purposes only. The scales change between the first and second rows, and between the fifth and sixth rows, as well as between the second and third column.
001530684 8564_ $$82431940$$s214017$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_survey1_tblob.png$$y00018 Estimated 857\,GHz zodiacal emission templates, in MJy/sr, based on the model of~K98, in Galactic coordinates, for Survey~1 (left), Survey~2 (center), and Survey~2 minus Survey~1 (right). From top to bottom we show Dust Band~1, Dust Band~2, Dust Band~3, the Circumsolar Ring, the Earth-Trailing Feature, and finally the Diffuse Cloud. Note that the scales for the right-hand column are different from those of the left-hand and centre columns, and that the scale for the bottom row is different from that of the others.
001530684 8564_ $$82431941$$s43717$$uhttps://cds.cern.ch/record/1530684/files/Z143Correction.png$$y00076 Survey 2 minus survey 1 difference maps before (left) and after (center) Zodiacal emission removal, as well as the total (i.e., not differenced) Zodiacal emission removed from the nominal mission HFI maps (right). The rows, from top to bottom, are for 857, 545, 353, 217, 143, and 100\,GHz. The top two rows, for 857 and 545\,GHz, are in units MJy/sr, while the other frequencies are in units of $\mu\mathrm{K}_\mathrm{CMB}$. Note that while these images are presented together for compactness, they are different, as some are differences and some or not.
001530684 8564_ $$82431942$$s219886$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_survey2_Galactic_baffle.png$$y00041 Templates of the dipole and the Galaxy, in MJy/sr, seen through our far sidelobes for Surveys 1 (left) and 2 (centre), and for the difference in these two (right). Row~1: dipole seen through the direct SR contribution. Row~2: dipole seen through the PR contribution. Row~3: dipole seen through the baffle SR contribution. Row~4: Galaxy seen through the direct SR contribution. Row~5: Galaxy seen through the PR contribution. Row~6: Galaxy seen through the baffle SR contribution. The simulations in Rows~4--6 are made using 857\,GHz data passed through the far sidelobe calculation described in Sect.~\ref{subsec:galFSL}. The scales are different for the top and bottom three rows, and for the first two and the last columns.
001530684 8564_ $$82431943$$s300524$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_surveyD_10.png$$y00057 Sequence of maps in MJy/sr, each building upon that above, designed to show the relative contributions of the various templates in Figs.~\ref{fig:zodiMaps} and~\ref{fig:FSLs}. Row 1: the sum of the last three templates in Fig.~\ref{fig:FSLs}. Row 2: Row 1 plus Dust band~1. Row 3: Row 2 plus Dust band~2. Row 4: Row 3 plus Dust band~3. Row 5: Row 4 plus the Circumsolar Ring and Earth-Trailing Feature. Row 6: The far sidelobes and all zodiacal components. \emph{Left}: Survey 1. \emph{Centre}: Survey 2. \emph{Right}: Survey 2 minus Survey 1. Note that the amplitudes used are only approximate, the figure being for illustrative purposes only. The scales change between the first and second rows, and between the fifth and sixth rows, as well as between the second and third column.
001530684 8564_ $$82431944$$s52370$$uhttps://cds.cern.ch/record/1530684/files/Scan_a.png$$y00000 Schematic representation of the geometry of \Planck's measurements, which shows that it can view different amounts of zodiacal emission while looking at the same point on the distant sky. Observations of two points on the sky are shown, each with two measurements of the given point. The plane of the Ecliptic is in the plane of the diagram. The Sun is in the centre of each panel. The solid black ring represents the orbit of the Earth and \Planck. The orange circle represents the IPD cloud, cut off at the orbit of Jupiter, beyond which we assume there is no contribution to the zodiacal emission. {\it Left\/}: Case where the phase of the scan cycloid and the location of the observed point on the sky (towards the right of the page in this case) yield two measurements for which the lines of sight through the IPD are roughly equal, and the same zodiacal signal is seen. {\it Right\/}: Case where the phase of the scan cycloid and the location of the observed point on the sky (now towards the top of the page) yield different total columns of IPD along the lines of sight, and thus a different zodiacal signal. \textit{Note that this figure is highly stylized and not to scale.}
001530684 8564_ $$82431945$$s53475$$uhttps://cds.cern.ch/record/1530684/files/Scan_b.png$$y00001 Schematic representation of the geometry of \Planck's measurements, which shows that it can view different amounts of zodiacal emission while looking at the same point on the distant sky. Observations of two points on the sky are shown, each with two measurements of the given point. The plane of the Ecliptic is in the plane of the diagram. The Sun is in the centre of each panel. The solid black ring represents the orbit of the Earth and \Planck. The orange circle represents the IPD cloud, cut off at the orbit of Jupiter, beyond which we assume there is no contribution to the zodiacal emission. {\it Left\/}: Case where the phase of the scan cycloid and the location of the observed point on the sky (towards the right of the page in this case) yield two measurements for which the lines of sight through the IPD are roughly equal, and the same zodiacal signal is seen. {\it Right\/}: Case where the phase of the scan cycloid and the location of the observed point on the sky (now towards the top of the page) yield different total columns of IPD along the lines of sight, and thus a different zodiacal signal. \textit{Note that this figure is highly stylized and not to scale.}
001530684 8564_ $$82431946$$s262006$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_surveyD_Dipolar_direct.png$$y00027 Templates of the dipole and the Galaxy, in MJy/sr, seen through our far sidelobes for Surveys 1 (left) and 2 (centre), and for the difference in these two (right). Row~1: dipole seen through the direct SR contribution. Row~2: dipole seen through the PR contribution. Row~3: dipole seen through the baffle SR contribution. Row~4: Galaxy seen through the direct SR contribution. Row~5: Galaxy seen through the PR contribution. Row~6: Galaxy seen through the baffle SR contribution. The simulations in Rows~4--6 are made using 857\,GHz data passed through the far sidelobe calculation described in Sect.~\ref{subsec:galFSL}. The scales are different for the top and bottom three rows, and for the first two and the last columns.
001530684 8564_ $$82431947$$s210960$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_survey2_band2.png$$y00010 Estimated 857\,GHz zodiacal emission templates, in MJy/sr, based on the model of~K98, in Galactic coordinates, for Survey~1 (left), Survey~2 (center), and Survey~2 minus Survey~1 (right). From top to bottom we show Dust Band~1, Dust Band~2, Dust Band~3, the Circumsolar Ring, the Earth-Trailing Feature, and finally the Diffuse Cloud. Note that the scales for the right-hand column are different from those of the left-hand and centre columns, and that the scale for the bottom row is different from that of the others.
001530684 8564_ $$82431948$$s203974$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_survey2_band3.png$$y00007 Estimated 857\,GHz zodiacal emission templates, in MJy/sr, based on the model of~K98, in Galactic coordinates, for Survey~1 (left), Survey~2 (center), and Survey~2 minus Survey~1 (right). From top to bottom we show Dust Band~1, Dust Band~2, Dust Band~3, the Circumsolar Ring, the Earth-Trailing Feature, and finally the Diffuse Cloud. Note that the scales for the right-hand column are different from those of the left-hand and centre columns, and that the scale for the bottom row is different from that of the others.
001530684 8564_ $$82431949$$s261278$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_surveyD_cring.png$$y00017 Estimated 857\,GHz zodiacal emission templates, in MJy/sr, based on the model of~K98, in Galactic coordinates, for Survey~1 (left), Survey~2 (center), and Survey~2 minus Survey~1 (right). From top to bottom we show Dust Band~1, Dust Band~2, Dust Band~3, the Circumsolar Ring, the Earth-Trailing Feature, and finally the Diffuse Cloud. Note that the scales for the right-hand column are different from those of the left-hand and centre columns, and that the scale for the bottom row is different from that of the others.
001530684 8564_ $$82431950$$s204414$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_survey2_band1.png$$y00013 Estimated 857\,GHz zodiacal emission templates, in MJy/sr, based on the model of~K98, in Galactic coordinates, for Survey~1 (left), Survey~2 (center), and Survey~2 minus Survey~1 (right). From top to bottom we show Dust Band~1, Dust Band~2, Dust Band~3, the Circumsolar Ring, the Earth-Trailing Feature, and finally the Diffuse Cloud. Note that the scales for the right-hand column are different from those of the left-hand and centre columns, and that the scale for the bottom row is different from that of the others.
001530684 8564_ $$82431951$$s268381$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_survey2_11.png$$y00059 Sequence of maps in MJy/sr, each building upon that above, designed to show the relative contributions of the various templates in Figs.~\ref{fig:zodiMaps} and~\ref{fig:FSLs}. Row 1: the sum of the last three templates in Fig.~\ref{fig:FSLs}. Row 2: Row 1 plus Dust band~1. Row 3: Row 2 plus Dust band~2. Row 4: Row 3 plus Dust band~3. Row 5: Row 4 plus the Circumsolar Ring and Earth-Trailing Feature. Row 6: The far sidelobes and all zodiacal components. \emph{Left}: Survey 1. \emph{Centre}: Survey 2. \emph{Right}: Survey 2 minus Survey 1. Note that the amplitudes used are only approximate, the figure being for illustrative purposes only. The scales change between the first and second rows, and between the fifth and sixth rows, as well as between the second and third column.
001530684 8564_ $$82431952$$s70449$$uhttps://cds.cern.ch/record/1530684/files/Z857SurveyJackknifeWiZodi.png$$y00061 Survey 2 minus Survey 1 difference maps, before (left) and after (right) zodiacal emission removal. The top two rows, for 857 and 545\,GHz, are in units MJy\,sr$^{-1}$, while the bottom row, for 353\,GHz, is in units of $\mu\mathrm{K}_\mathrm{CMB}$.
001530684 8564_ $$82431953$$s205386$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_survey1_band1.png$$y00012 Estimated 857\,GHz zodiacal emission templates, in MJy/sr, based on the model of~K98, in Galactic coordinates, for Survey~1 (left), Survey~2 (center), and Survey~2 minus Survey~1 (right). From top to bottom we show Dust Band~1, Dust Band~2, Dust Band~3, the Circumsolar Ring, the Earth-Trailing Feature, and finally the Diffuse Cloud. Note that the scales for the right-hand column are different from those of the left-hand and centre columns, and that the scale for the bottom row is different from that of the others.
001530684 8564_ $$82431954$$s337865$$uhttps://cds.cern.ch/record/1530684/files/survey_jack_857-1_year1.png$$y00005 Single-Survey maps in Galactic coordinates for the 857-1 detector. \emph{Top:} Survey 1 map. \emph{Middle:} Survey 2 map. \emph{Bottom:} Survey 2 minus Survey 1 difference map. This bottom image shows the zodiacal emission and the residual Galactic emission effects that are discussed in the text. The units are MJy\,sr$^{-1}$, assuming a spectrum inversely proportional to frequency. Undefined pixels are shown in grey. These occur in pixels that either have not been observed during the Survey, were observed during the passage of a planet, or for a small number of other events. In the top two plots, pixels that were observed over periods longer than a week were not masked, and thus the masked regions are smaller in the top two images than that in the difference (bottom) panel. The units are MJy/sr.
001530684 8564_ $$82431955$$s204495$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_survey1_band3.png$$y00006 Estimated 857\,GHz zodiacal emission templates, in MJy/sr, based on the model of~K98, in Galactic coordinates, for Survey~1 (left), Survey~2 (center), and Survey~2 minus Survey~1 (right). From top to bottom we show Dust Band~1, Dust Band~2, Dust Band~3, the Circumsolar Ring, the Earth-Trailing Feature, and finally the Diffuse Cloud. Note that the scales for the right-hand column are different from those of the left-hand and centre columns, and that the scale for the bottom row is different from that of the others.
001530684 8564_ $$82431956$$s213087$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_survey1_band2.png$$y00009 Estimated 857\,GHz zodiacal emission templates, in MJy/sr, based on the model of~K98, in Galactic coordinates, for Survey~1 (left), Survey~2 (center), and Survey~2 minus Survey~1 (right). From top to bottom we show Dust Band~1, Dust Band~2, Dust Band~3, the Circumsolar Ring, the Earth-Trailing Feature, and finally the Diffuse Cloud. Note that the scales for the right-hand column are different from those of the left-hand and centre columns, and that the scale for the bottom row is different from that of the others.
001530684 8564_ $$82431957$$s437266$$uhttps://cds.cern.ch/record/1530684/files/Z_Corrections_combined.png$$y00073 Difference maps (uncorrected for zodiacal emission minus corrected) showing the zodiacal corrections calculated in this paper. Units are MJy/sr for 857 and 545\,GHz, $\mu\mathrm{K}_\mathrm{CMB}$ for the other frequencies.
001530684 8564_ $$82431958$$s212796$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_survey1_cring.png$$y00015 Estimated 857\,GHz zodiacal emission templates, in MJy/sr, based on the model of~K98, in Galactic coordinates, for Survey~1 (left), Survey~2 (center), and Survey~2 minus Survey~1 (right). From top to bottom we show Dust Band~1, Dust Band~2, Dust Band~3, the Circumsolar Ring, the Earth-Trailing Feature, and finally the Diffuse Cloud. Note that the scales for the right-hand column are different from those of the left-hand and centre columns, and that the scale for the bottom row is different from that of the others.
001530684 8564_ $$82431959$$s23096$$uhttps://cds.cern.ch/record/1530684/files/Asts.png$$y00075 \textit{Top}: ratio of $f\,s^{1/2}$ of the first and subsequent measurements for those Solar System objects that were detected in more than one Survey. Measurements at 857\,GHz are shown in blue, measurements at 545\,GHz are shown in green, and measurements at 353\,GHz are shown in red. The grey line shows $\left(d/d_0\right)^{-2}$, which one would expect for Rayleigh-Jeans objects. \textit{Bottom}: spectral index for those asteroids detected in multiple frequency bands for a given Survey, defined as $\log\left(I_{545}/I_{857}\right)/\log\left(545/857\right)$. Juno and Vesta are shown in brown and yellow, to indicate that they have different spectral classifications than Ceres, Pallas, Hygiea and Europa, shown in shades of blue. The white symbols show the corresponding values for 353--545\,GHz, where they exist. For both panels, the symbols used for each object are: 1\,Ceres --- circles; 2\,Pallas --- squares; 3\,Juno --- diamonds; 4\,Vesta --- hexagons; 6\,Hebe --- +; 8\,Flora --- $\times$; 9\,Metis -- upward-pointing triangle; 10\,Hygiea -- right-pointing triangles; 19\,Fortuna -- vertical lines; 45\,Eugenia -- downward-pointing triangles; 52\,Europa -- stars; 324\,Bamberga -- left-pointing triangle; and 704\,Interamnia -- horizontal lines.
001530684 8564_ $$82431960$$s62672$$uhttps://cds.cern.ch/record/1530684/files/Z353SurveyJackknifeNoZodi.png$$y00066 Survey 2 minus Survey 1 difference maps, before (left) and after (right) zodiacal emission removal. The top two rows, for 857 and 545\,GHz, are in units MJy\,sr$^{-1}$, while the bottom row, for 353\,GHz, is in units of $\mu\mathrm{K}_\mathrm{CMB}$.
001530684 8564_ $$82431961$$s283453$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_surveyD_Galactic_secondary.png$$y00039 Templates of the dipole and the Galaxy, in MJy/sr, seen through our far sidelobes for Surveys 1 (left) and 2 (centre), and for the difference in these two (right). Row~1: dipole seen through the direct SR contribution. Row~2: dipole seen through the PR contribution. Row~3: dipole seen through the baffle SR contribution. Row~4: Galaxy seen through the direct SR contribution. Row~5: Galaxy seen through the PR contribution. Row~6: Galaxy seen through the baffle SR contribution. The simulations in Rows~4--6 are made using 857\,GHz data passed through the far sidelobe calculation described in Sect.~\ref{subsec:galFSL}. The scales are different for the top and bottom three rows, and for the first two and the last columns.
001530684 8564_ $$82431962$$s243128$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_survey2_5.png$$y00044 Sequence of maps in MJy/sr, each building upon that above, designed to show the relative contributions of the various templates in Figs.~\ref{fig:zodiMaps} and~\ref{fig:FSLs}. Row 1: the sum of the last three templates in Fig.~\ref{fig:FSLs}. Row 2: Row 1 plus Dust band~1. Row 3: Row 2 plus Dust band~2. Row 4: Row 3 plus Dust band~3. Row 5: Row 4 plus the Circumsolar Ring and Earth-Trailing Feature. Row 6: The far sidelobes and all zodiacal components. \emph{Left}: Survey 1. \emph{Centre}: Survey 2. \emph{Right}: Survey 2 minus Survey 1. Note that the amplitudes used are only approximate, the figure being for illustrative purposes only. The scales change between the first and second rows, and between the fifth and sixth rows, as well as between the second and third column.
001530684 8564_ $$82431963$$s251145$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_survey2_7.png$$y00050 Sequence of maps in MJy/sr, each building upon that above, designed to show the relative contributions of the various templates in Figs.~\ref{fig:zodiMaps} and~\ref{fig:FSLs}. Row 1: the sum of the last three templates in Fig.~\ref{fig:FSLs}. Row 2: Row 1 plus Dust band~1. Row 3: Row 2 plus Dust band~2. Row 4: Row 3 plus Dust band~3. Row 5: Row 4 plus the Circumsolar Ring and Earth-Trailing Feature. Row 6: The far sidelobes and all zodiacal components. \emph{Left}: Survey 1. \emph{Centre}: Survey 2. \emph{Right}: Survey 2 minus Survey 1. Note that the amplitudes used are only approximate, the figure being for illustrative purposes only. The scales change between the first and second rows, and between the fifth and sixth rows, as well as between the second and third column.
001530684 8564_ $$82431964$$s238457$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_survey2_6.png$$y00047 Sequence of maps in MJy/sr, each building upon that above, designed to show the relative contributions of the various templates in Figs.~\ref{fig:zodiMaps} and~\ref{fig:FSLs}. Row 1: the sum of the last three templates in Fig.~\ref{fig:FSLs}. Row 2: Row 1 plus Dust band~1. Row 3: Row 2 plus Dust band~2. Row 4: Row 3 plus Dust band~3. Row 5: Row 4 plus the Circumsolar Ring and Earth-Trailing Feature. Row 6: The far sidelobes and all zodiacal components. \emph{Left}: Survey 1. \emph{Centre}: Survey 2. \emph{Right}: Survey 2 minus Survey 1. Note that the amplitudes used are only approximate, the figure being for illustrative purposes only. The scales change between the first and second rows, and between the fifth and sixth rows, as well as between the second and third column.
001530684 8564_ $$82431965$$s74738$$uhttps://cds.cern.ch/record/1530684/files/ZCorrectionCls.png$$y00074 Power spectra of the zodiacal correction maps shown in Fig.~\ref{fig:MapCorrections}. Black plus signs = 857\,GHz; grey crosses = 545\,GHz; cyan triangles = 353\,GHz; orange diamonds = 217\,GHz; blue circles = 143\,GHz; and red squares = 100\,GHz. For the ``CMB channels'' 100--353\,GHz, even multipoles are shown with filled symbols, odd multipoles with empty symbols. The ``even-odd'' pattern is a consequence of the symmetry around the ecliptic plane -- odd multipoles are almost absent, as they would indicate structure in the maps that was anti-symmetric about the ecliptic plane. The best-fit $\Lambda$CDM CMB temperature anisotropy spectrum using the ``Planck+WP+highL+BAO'' data combination from~\cite{planck2013-p11}, is shown as the solid line roughly half-way down the plot, orders of magnitude above the zodiacal spectrum in the \Planck\ CMB channels.
001530684 8564_ $$82431966$$s265893$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_survey2_8.png$$y00053 Sequence of maps in MJy/sr, each building upon that above, designed to show the relative contributions of the various templates in Figs.~\ref{fig:zodiMaps} and~\ref{fig:FSLs}. Row 1: the sum of the last three templates in Fig.~\ref{fig:FSLs}. Row 2: Row 1 plus Dust band~1. Row 3: Row 2 plus Dust band~2. Row 4: Row 3 plus Dust band~3. Row 5: Row 4 plus the Circumsolar Ring and Earth-Trailing Feature. Row 6: The far sidelobes and all zodiacal components. \emph{Left}: Survey 1. \emph{Centre}: Survey 2. \emph{Right}: Survey 2 minus Survey 1. Note that the amplitudes used are only approximate, the figure being for illustrative purposes only. The scales change between the first and second rows, and between the fifth and sixth rows, as well as between the second and third column.
001530684 8564_ $$82431967$$s46980$$uhttps://cds.cern.ch/record/1530684/files/Z100Correction.png$$y00077 Survey 2 minus survey 1 difference maps before (left) and after (center) Zodiacal emission removal, as well as the total (i.e., not differenced) Zodiacal emission removed from the nominal mission HFI maps (right). The rows, from top to bottom, are for 857, 545, 353, 217, 143, and 100\,GHz. The top two rows, for 857 and 545\,GHz, are in units MJy/sr, while the other frequencies are in units of $\mu\mathrm{K}_\mathrm{CMB}$. Note that while these images are presented together for compactness, they are different, as some are differences and some or not.
001530684 8564_ $$82431968$$s263839$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_surveyD_Dipolar_baffle.png$$y00033 Templates of the dipole and the Galaxy, in MJy/sr, seen through our far sidelobes for Surveys 1 (left) and 2 (centre), and for the difference in these two (right). Row~1: dipole seen through the direct SR contribution. Row~2: dipole seen through the PR contribution. Row~3: dipole seen through the baffle SR contribution. Row~4: Galaxy seen through the direct SR contribution. Row~5: Galaxy seen through the PR contribution. Row~6: Galaxy seen through the baffle SR contribution. The simulations in Rows~4--6 are made using 857\,GHz data passed through the far sidelobe calculation described in Sect.~\ref{subsec:galFSL}. The scales are different for the top and bottom three rows, and for the first two and the last columns.
001530684 8564_ $$82431969$$s257470$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_survey1_Dipolar_direct.png$$y00025 Templates of the dipole and the Galaxy, in MJy/sr, seen through our far sidelobes for Surveys 1 (left) and 2 (centre), and for the difference in these two (right). Row~1: dipole seen through the direct SR contribution. Row~2: dipole seen through the PR contribution. Row~3: dipole seen through the baffle SR contribution. Row~4: Galaxy seen through the direct SR contribution. Row~5: Galaxy seen through the PR contribution. Row~6: Galaxy seen through the baffle SR contribution. The simulations in Rows~4--6 are made using 857\,GHz data passed through the far sidelobe calculation described in Sect.~\ref{subsec:galFSL}. The scales are different for the top and bottom three rows, and for the first two and the last columns.
001530684 8564_ $$82431970$$s52628$$uhttps://cds.cern.ch/record/1530684/files/Z545Correction.png$$y00067 Survey 2 minus survey 1 difference maps before (left) and after (center) Zodiacal emission removal, as well as the total (i.e., not differenced) Zodiacal emission removed from the nominal mission HFI maps (right). The rows, from top to bottom, are for 857, 545, 353, 217, 143, and 100\,GHz. The top two rows, for 857 and 545\,GHz, are in units MJy/sr, while the other frequencies are in units of $\mu\mathrm{K}_\mathrm{CMB}$. Note that while these images are presented together for compactness, they are different, as some are differences and some or not.
001530684 8564_ $$82431971$$s304725$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_surveyD_8.png$$y00054 Sequence of maps in MJy/sr, each building upon that above, designed to show the relative contributions of the various templates in Figs.~\ref{fig:zodiMaps} and~\ref{fig:FSLs}. Row 1: the sum of the last three templates in Fig.~\ref{fig:FSLs}. Row 2: Row 1 plus Dust band~1. Row 3: Row 2 plus Dust band~2. Row 4: Row 3 plus Dust band~3. Row 5: Row 4 plus the Circumsolar Ring and Earth-Trailing Feature. Row 6: The far sidelobes and all zodiacal components. \emph{Left}: Survey 1. \emph{Centre}: Survey 2. \emph{Right}: Survey 2 minus Survey 1. Note that the amplitudes used are only approximate, the figure being for illustrative purposes only. The scales change between the first and second rows, and between the fifth and sixth rows, as well as between the second and third column.
001530684 8564_ $$82431972$$s265381$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_survey2_cloud.png$$y00022 Estimated 857\,GHz zodiacal emission templates, in MJy/sr, based on the model of~K98, in Galactic coordinates, for Survey~1 (left), Survey~2 (center), and Survey~2 minus Survey~1 (right). From top to bottom we show Dust Band~1, Dust Band~2, Dust Band~3, the Circumsolar Ring, the Earth-Trailing Feature, and finally the Diffuse Cloud. Note that the scales for the right-hand column are different from those of the left-hand and centre columns, and that the scale for the bottom row is different from that of the others.
001530684 8564_ $$82431973$$s210389$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_survey2_tblob.png$$y00019 Estimated 857\,GHz zodiacal emission templates, in MJy/sr, based on the model of~K98, in Galactic coordinates, for Survey~1 (left), Survey~2 (center), and Survey~2 minus Survey~1 (right). From top to bottom we show Dust Band~1, Dust Band~2, Dust Band~3, the Circumsolar Ring, the Earth-Trailing Feature, and finally the Diffuse Cloud. Note that the scales for the right-hand column are different from those of the left-hand and centre columns, and that the scale for the bottom row is different from that of the others.
001530684 8564_ $$82431974$$s71900$$uhttps://cds.cern.ch/record/1530684/files/Z857SurveyJackknifeNoZodi.png$$y00062 Survey 2 minus Survey 1 difference maps, before (left) and after (right) zodiacal emission removal. The top two rows, for 857 and 545\,GHz, are in units MJy\,sr$^{-1}$, while the bottom row, for 353\,GHz, is in units of $\mu\mathrm{K}_\mathrm{CMB}$.
001530684 8564_ $$82431975$$s273657$$uhttps://cds.cern.ch/record/1530684/files/Z857JackSim_surveyD_Galactic_direct.png$$y00036 Templates of the dipole and the Galaxy, in MJy/sr, seen through our far sidelobes for Surveys 1 (left) and 2 (centre), and for the difference in these two (right). Row~1: dipole seen through the direct SR contribution. Row~2: dipole seen through the PR contribution. Row~3: dipole seen through the baffle SR contribution. Row~4: Galaxy seen through the direct SR contribution. Row~5: Galaxy seen through the PR contribution. Row~6: Galaxy seen through the baffle SR contribution. The simulations in Rows~4--6 are made using 857\,GHz data passed through the far sidelobe calculation described in Sect.~\ref{subsec:galFSL}. The scales are different for the top and bottom three rows, and for the first two and the last columns.
001530684 8564_ $$82431976$$s55763$$uhttps://cds.cern.ch/record/1530684/files/Z857Correction.png$$y00064 Survey 2 minus survey 1 difference maps before (left) and after (center) Zodiacal emission removal, as well as the total (i.e., not differenced) Zodiacal emission removed from the nominal mission HFI maps (right). The rows, from top to bottom, are for 857, 545, 353, 217, 143, and 100\,GHz. The top two rows, for 857 and 545\,GHz, are in units MJy/sr, while the other frequencies are in units of $\mu\mathrm{K}_\mathrm{CMB}$. Note that while these images are presented together for compactness, they are different, as some are differences and some or not.
001530684 916__ $$sn$$w201311
001530684 960__ $$a13
001530684 980__ $$aARTICLE
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