A1 Refereed original research article in a scientific journal
Planck 2013 results. XI. All-sky model of thermal dust emission
Authors: Abergel A, Ade PAR, Aghanim N, Alves MIR, Aniano G, Armitage-Caplan C, Arnaud M, Ashdown M, Atrio-Barandela F, Aumont J, Baccigalupi C, Banday AJ, Barreiro RB, Bartlett JG, Battaner E, Benabed K, Benoit A, Benoit-Levy A, Bernard JP, Bersanelli M, Bielewicz P, Bobin J, Bock JJ, Bonaldi A, Bond JR, Borrill J, Bouchet FR, Boulanger F, Bridges M, Bucher M, Burigana C, Butler RC, Cardoso JF, Catalano A, Chamballu A, Chary RR, Chiang HC, Chiang LY, Christensen PR, Church S, Clemens M, Clements DL, Colombi S, Colombo LPL, Combet C, Couchot F, Coulais A, Crill BP, Curto A, Cuttaia F, Danese L, Davies RD, Davis RJ, de Bernardis P, de Rosa A, de Zotti G, Delabrouille J, Delouis JM, Desert FX, Dickinson C, Diego JM, Dole H, Donzelli S, Dore O, Douspis M, Draine BT, Dupac X, Efstathiou G, Ensslin TA, Eriksen HK, Falgarone E, Finelli F, Forni O, Frailis M, Fraisse AA, Franceschi E, Galeotta S, Ganga K, Ghosh T, Giard M, Giardino G, Giraud-Heraud Y, Gonzalez-Nuevo J, Gorski KM, Gratton S, Gregorio A, Grenier IA, Gruppuso A, Guillet V, Hansen FK, Hanson D, Harrison DL, Helou G, Henrot-Versille S, Hernandez-Monteagudo C, Herranz D, Hildebrandt SR, Hivon E, Hobson M, Holmes WA, Hornstrup A, Hovest W, Huffenberger KM, Jaffe AH, Jaffe TR, Jewell J, Joncas G, Jones WC, Juvela M, Keihanen E, Keskitalo R, Kisner TS, Knoche J, Knox L, Kunz M, Kurki-Suonio H, Lagache G, Lahteenmaki A, Lamarre JM, Lasenby A, Laureijs RJ, Lawrence CR, Leonardi R, Leon-Tavares J, Lesgourgues J, Levrier F, Liguori M, Lilje PB, Linden-Vornle M, Lopez-Caniego M, Lubin PM, Macias-Perez JF, Maffei B, Maino D, Mandolesi N, Maris M, Marshall DJ, Martin PG, Martinez-Gonzalez E, Masi S, Massardi M, Matarrese S, Matthai F, Mazzotta P, McGehee P, Melchiorri A, Mendes L, Mennella A, Migliaccio M, Mitra S, Miville-Deschenes MA, Moneti A, Montier L, Morgante G, Mortlock D, Munshi D, Murphy JA, Naselsky P, Nati F, Natoli P, Netterfield CB, Norgaard-Nielsen HU, Noviello F, Novikov D, Novikov I, Osborne S, Oxborrow CA, Paci F, Pagano L, Pajot F, Paladini R, Paoletti D, Pasian F, Patanchon G, Perdereau O, Perotto L, Perrotta F, Piacentini F, Piat M, Pierpaoli E, Pietrobon D, Plaszczynski S, Pointecouteau E, Polenta G, Ponthieu N, Popa L, Poutanen T, Pratt GW, Prezeau G, Prunet S, Puget JL, Rachen JP, Reach WT, Rebolo R, Reinecke M, Remazeilles M, Renault C, Ricciardi S, Riller T, Ristorcelli I, Rocha G, Rosset C, Roudier G, Rowan-Robinson M, Rubino-Martin JA, Rusholme B, Sandri M, Santos D, Savini G, Scott D, Seiffert MD, Shellard EPS, Spencer LD, Starck JL, Stolyarov V, Stompor R, Sudiwala R, Sunyaev R, Sureau F, Sutton D, Suur-Uski AS, Sygnet JF, Tauber JA, Tavagnacco D, Terenzi L, Toffolatti L, Tomasi M, Tristram M, Tucci M, Tuovinen J, Turler M, Umana G, Valenziano L, Valiviita J, Van Tent B, Verstraete L, Vielva P, Villa F, Vittorio N, Wade LA, Wandelt BD, Welikala N, Ysard N, Yvon D, Zacchei A, Zonca A
Publisher: EDP SCIENCES S A
Publication year: 2014
Journal: Astronomy and Astrophysics
Journal name in source: ASTRONOMY & ASTROPHYSICS
Journal acronym: ASTRON ASTROPHYS
Article number: ARTN A11
Volume: 571
Number of pages: 37
ISSN: 1432-0746
DOI: https://doi.org/10.1051/0004-6361/201323195
This paper presents an all-sky model of dust emission from the Planck 353, 545, and 857 GHz, and IRAS 100 mu m data. Using a modified blackbody fit to the data we present all-sky maps of the dust optical depth, temperature, and spectral index over the 353-3000 GHz range. This model is a good representation of the IRAS and Planck data at 5 0 between 353 and 3000 GHz (850 and 100 mu m). It shows variations of the order of 30% compared with the widely-used model of Finkbeiner, Davis, and Schlegel. The Planck data allow us to estimate the dust temperature uniformly over the whole sky, down to an angular resolution of 5 0, providing an improved estimate of the dust optical depth compared to previous all-sky dust model, especially in high-contrast molecular regions where the dust temperature varies strongly at small scales in response to dust evolution, extinction, and/or local production of heating photons. An increase of the dust opacity at 353 GHz, tau(353)/N-H, from the diffuse to the denser interstellar medium (ISM) is reported. It is associated with a decrease in the observed dust temperature, T-obs, that could be due at least in part to the increased dust opacity. We also report an excess of dust emission at HI column densities lower than 10(20) cm(-2) that could be the signature of dust in the warm ionized medium. In the diffuse ISM at high Galactic latitude, we report an anticorrelation between tau(353)/N-H and T-obs while the dust specific luminosity, i.e., the total dust emission integrated over frequency (the radiance) per hydrogen atom, stays about constant, confirming one of the Planck Early Results obtained on selected fields. This e ff ect is compatible with the view that, in the diffuse ISM, Tobs responds to spatial variations of the dust opacity, due to variations of dust properties, in addition to (small) variations of the radiation field strength. The implication is that in the di ff use high-latitude ISM tau(353) is not as reliable a tracer of dust column density as we conclude it is in molecular clouds where the correlation of tau(353) with dust extinction estimated using colour excess measurements on stars is strong. To estimate Galactic E(B-V) in extragalactic fields at high latitude we develop a new method based on the thermal dust radiance, instead of the dust optical depth, calibrated to E(B-V) using reddening measurements of quasars deduced from Sloan Digital Sky Survey data.
