Planck 2013 results. XI. All-sky model of thermal dust emission

Planck Collaboration; A Abergel; P A R Ade; N Aghanim; M I R Alves; G Aniano; 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 Beno??t; A Benoit-L??vy; 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; H C Chiang; L-Y Chiang; P R Christensen; S Church; M Clemens; D L Clements; S Colombi; L P L Colombo; C Combet; F Couchot; A Coulais; B P Crill; A Curto; F Cuttaia; L Danese; R D Davies; R J Davis; P de Bernardis; A de Rosa; G de Zotti; J Delabrouille; J-M Delouis; F-X D??sert; C Dickinson; J M Diego; H Dole; S Donzelli; O Dor??; M Douspis; B T Draine; X Dupac; G Efstathiou; T A En??lin; H K Eriksen; E Falgarone; F Finelli; O Forni; M Frailis; A A Fraisse; E Franceschi; S Galeotta; K Ganga; T Ghosh; M Giard; G Giardino; Y Giraud-H??raud; J Gonz??lez-Nuevo; K M G??rski; S Gratton; A Gregorio; I A Grenier; A Gruppuso; V Guillet; F K Hansen; D Hanson; D L Harrison; G Helou; S Henrot-Versill??; C Hern??ndez-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; J Jewell; G Joncas; W C Jones; M Juvela; E Keih??nen; R Keskitalo; T S Kisner; J Knoche; L Knox; M Kunz; H Kurki-Suonio; G Lagache; A L??hteenm??ki; J-M Lamarre; A Lasenby; R J Laureijs; C R Lawrence; R Leonardi; J Le??n-Tavares; J Lesgourgues; F Levrier; M Liguori; P B Lilje; M Linden-V??rnle; M L??pez-Caniego; P M Lubin; J F Mac??as-P??rez; B Maffei; D Maino; N Mandolesi; M Maris; D J Marshall; P G Martin; E Mart??nez-Gonz??lez; S Masi; M Massardi; S Matarrese; F Matthai; P Mazzotta; P McGehee; A Melchiorri; L Mendes; A Mennella; M Migliaccio; S Mitra; M-A Miville-Desch??nes; A Moneti; L Montier; G Morgante; D Mortlock; D Munshi; J A Murphy; P Naselsky; F Nati; P Natoli; C B Netterfield; H U N??rgaard-Nielsen; F Noviello; D Novikov; I Novikov; S Osborne; 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; G Polenta; N Ponthieu; L Popa; T Poutanen; G W Pratt; G Pr??zeau; 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; J A Rubi??o-Mart??n; B Rusholme; M Sandri; D Santos; G Savini; D Scott; M D Seiffert; E P S Shellard; L D Spencer; J-L Starck; V Stolyarov; R Stompor; R Sudiwala; R Sunyaev; 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; M T??rler; G Umana; L Valenziano; J Valiviita; B Van Tent; L Verstraete; P Vielva; F Villa; N Vittorio; L A Wade; B D Wandelt; N Welikala; N Ysard; D Yvon; A Zacchei; A Zonca

doi:10.1051/0004-6361/201323195

Planck 2013 results. XI. All-sky model of thermal dust emission

Planck Collaboration, A Abergel, P A R Ade, N Aghanim, M I R Alves, G Aniano, 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 Beno??t, A Benoit-L??vy, J-P BernardM 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, H C Chiang, L-Y Chiang, P R Christensen, S Church, M Clemens, D L Clements, S Colombi, L P L Colombo, C Combet, F Couchot, A Coulais, B P Crill, A Curto, F Cuttaia, L Danese, R D Davies, R J Davis, P de Bernardis, A de Rosa, G de Zotti, J Delabrouille, J-M Delouis, F-X D??sert, C Dickinson, J M Diego, H Dole, S Donzelli, O Dor??, M Douspis, B T Draine, X Dupac, G Efstathiou, T A En??lin, H K Eriksen, E Falgarone, F Finelli, O Forni, M Frailis, A A Fraisse, E Franceschi, S Galeotta, K Ganga, T Ghosh, M Giard, G Giardino, Y Giraud-H??raud, J Gonz??lez-Nuevo, K M G??rski, S Gratton, A Gregorio, I A Grenier, A Gruppuso, V Guillet, F K Hansen, D Hanson, D L Harrison, G Helou, S Henrot-Versill??, C Hern??ndez-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, J Jewell, G Joncas, W C Jones, M Juvela, E Keih??nen, R Keskitalo, T S Kisner, J Knoche, L Knox, M Kunz, H Kurki-Suonio, G Lagache, A L??hteenm??ki, J-M Lamarre, A Lasenby, R J Laureijs, C R Lawrence, R Leonardi, J Le??n-Tavares, J Lesgourgues, F Levrier, M Liguori, P B Lilje, M Linden-V??rnle, M L??pez-Caniego, P M Lubin, J F Mac??as-P??rez, B Maffei, D Maino, N Mandolesi, M Maris, D J Marshall, P G Martin, E Mart??nez-Gonz??lez, S Masi, M Massardi, S Matarrese, F Matthai, P Mazzotta, P McGehee, A Melchiorri, L Mendes, A Mennella, M Migliaccio, S Mitra, M-A Miville-Desch??nes, A Moneti, L Montier, G Morgante, D Mortlock, D Munshi, J A Murphy, P Naselsky, F Nati, P Natoli, C B Netterfield, H U N??rgaard-Nielsen, F Noviello, D Novikov, I Novikov, S Osborne, 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, G Polenta, N Ponthieu, L Popa, T Poutanen, G W Pratt, G Pr??zeau, 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, J A Rubi??o-Mart??n, B Rusholme, M Sandri, D Santos, G Savini, D Scott, M D Seiffert, E P S Shellard, L D Spencer, J-L Starck, V Stolyarov, R Stompor, R Sudiwala, R Sunyaev, 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, M T??rler, G Umana, L Valenziano, J Valiviita, B Van Tent, L Verstraete, P Vielva, F Villa, N Vittorio, L A Wade, B D Wandelt, N Welikala, N Ysard, D Yvon, A Zacchei, A Zonca

Research output: Contribution to journal › Article › peer-review

Abstract

This paper presents an all-sky model of dust emission from the Planck 353, 545, and 857 {GHz}, and {IRAS} 100 mum data. Using a modifiedblackbody 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' between 353 and 3000 {GHz} (850 and 100 mum). 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', 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},tau353/{NH}, from the diffuse to the denserinterstellar medium ({ISM}) is reported. It is associated with a decrease in the observed dust temperature, Tobs, that could be due at least in part to the increased dust opacity. We also report an excess of dust emission at H i column densities lower than 1020 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 tau353/{NH} andTobs 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 effect 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 diffuse high-latitude {ISM} tau353 is not as reliable a tracer of dust column density as we conclude it is in molecular clouds where the correlation of tau353 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) usingreddening measurements of quasars deduced from Sloan Digital Sky Survey data.

Original language	English
Journal	Astronomy and Astrophysics
Volume	571
DOIs	https://doi.org/10.1051/0004-6361/201323195
Publication status	Published - Nov 2014

Keywords

dust
extinction
infrared: ISM
{ISM}: general
methods: data analysis
opacity
submillimeter: ISM

Access to Document

10.1051/0004-6361/201323195

http://adsabs.harvard.edu/abs/2014A%26A...571A..11P

Cite this

Collaboration, P., Abergel, A., Ade, P. A. R., Aghanim, N., Alves, M. I. R., Aniano, G., Armitage-Caplan, C., Arnaud, M., Ashdown, M., Atrio-Barandela, F., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Bartlett, J. G., Battaner, E., Benabed, K., Beno??t, A., Benoit-L??vy, A., ... Zonca, A. (2014). Planck 2013 results. XI. All-sky model of thermal dust emission. Astronomy and Astrophysics, 571. https://doi.org/10.1051/0004-6361/201323195

@article{4f2270bac81d4efd92bfd24c0e2d4f4e,

title = "Planck 2013 results. XI. All-sky model of thermal dust emission",

abstract = "This paper presents an all-sky model of dust emission from the Planck 353, 545, and 857 {GHz}, and {IRAS} 100 mum data. Using a modifiedblackbody 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' between 353 and 3000 {GHz} (850 and 100 mum). 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', 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},tau353/{NH}, from the diffuse to the denserinterstellar medium ({ISM}) is reported. It is associated with a decrease in the observed dust temperature, Tobs, that could be due at least in part to the increased dust opacity. We also report an excess of dust emission at H i column densities lower than 1020 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 tau353/{NH} andTobs 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 effect 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 diffuse high-latitude {ISM} tau353 is not as reliable a tracer of dust column density as we conclude it is in molecular clouds where the correlation of tau353 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) usingreddening measurements of quasars deduced from Sloan Digital Sky Survey data.",

keywords = "dust, extinction, infrared: ISM, {ISM}: general, methods: data analysis, opacity, submillimeter: ISM",

author = "Planck Collaboration and A Abergel and Ade, {P A R} and N Aghanim and Alves, {M I R} and G Aniano and C Armitage-Caplan and M Arnaud and M Ashdown and F Atrio-Barandela and J Aumont and C Baccigalupi and Banday, {A J} and Barreiro, {R B} and Bartlett, {J G} and E Battaner and K Benabed and A Beno??t and A Benoit-L??vy and J-P Bernard and M Bersanelli and P Bielewicz and J Bobin and Bock, {J J} and A Bonaldi and Bond, {J R} and J Borrill and Bouchet, {F R} and F Boulanger and M Bridges and M Bucher and C Burigana and Butler, {R C} and J-F Cardoso and A Catalano and A Chamballu and R-R Chary and Chiang, {H C} and L-Y Chiang and Christensen, {P R} and S Church and M Clemens and Clements, {D L} and S Colombi and Colombo, {L P L} and C Combet and F Couchot and A Coulais and Crill, {B P} and A Curto and F Cuttaia and L Danese and Davies, {R D} and Davis, {R J} and {de Bernardis}, P and {de Rosa}, A and {de Zotti}, G and J Delabrouille and J-M Delouis and F-X D??sert and C Dickinson and Diego, {J M} and H Dole and S Donzelli and O Dor?? and M Douspis and Draine, {B T} and X Dupac and G Efstathiou and En??lin, {T A} and Eriksen, {H K} and E Falgarone and F Finelli and O Forni and M Frailis and Fraisse, {A A} and E Franceschi and S Galeotta and K Ganga and T Ghosh and M Giard and G Giardino and Y Giraud-H??raud and J Gonz??lez-Nuevo and G??rski, {K M} and S Gratton and A Gregorio and Grenier, {I A} and A Gruppuso and V Guillet and Hansen, {F K} and D Hanson and Harrison, {D L} and G Helou and S Henrot-Versill?? and C Hern??ndez-Monteagudo and D Herranz and Hildebrandt, {S R} and E Hivon and M Hobson and Holmes, {W A} and A Hornstrup and W Hovest and Huffenberger, {K M} and Jaffe, {A H} and Jaffe, {T R} and J Jewell and G Joncas and Jones, {W C} and M Juvela and E Keih??nen and R Keskitalo and Kisner, {T S} and J Knoche and L Knox and M Kunz and H Kurki-Suonio and G Lagache and A L??hteenm??ki and J-M Lamarre and A Lasenby and Laureijs, {R J} and Lawrence, {C R} and R Leonardi and J Le??n-Tavares and J Lesgourgues and F Levrier and M Liguori and Lilje, {P B} and M Linden-V??rnle and M L??pez-Caniego and Lubin, {P M} and Mac??as-P??rez, {J F} and B Maffei and D Maino and N Mandolesi and M Maris and Marshall, {D J} and Martin, {P G} and E Mart??nez-Gonz??lez and S Masi and M Massardi and S Matarrese and F Matthai and P Mazzotta and P McGehee and A Melchiorri and L Mendes and A Mennella and M Migliaccio and S Mitra and M-A Miville-Desch??nes and A Moneti and L Montier and G Morgante and D Mortlock and D Munshi and Murphy, {J A} and P Naselsky and F Nati and P Natoli and Netterfield, {C B} and N??rgaard-Nielsen, {H U} and F Noviello and D Novikov and I Novikov and S Osborne and Oxborrow, {C A} and F Paci and L Pagano and F Pajot and R Paladini and D Paoletti and F Pasian and G Patanchon and O Perdereau and L Perotto and F Perrotta and F Piacentini and M Piat and E Pierpaoli and D Pietrobon and S Plaszczynski and E Pointecouteau and G Polenta and N Ponthieu and L Popa and T Poutanen and Pratt, {G W} and G Pr??zeau and S Prunet and J-L Puget and Rachen, {J P} and Reach, {W T} and R Rebolo and M Reinecke and M Remazeilles and C Renault and S Ricciardi and T Riller and I Ristorcelli and G Rocha and C Rosset and G Roudier and M Rowan-Robinson and Rubi??o-Mart??n, {J A} and B Rusholme and M Sandri and D Santos and G Savini and D Scott and Seiffert, {M D} and Shellard, {E P S} and Spencer, {L D} and J-L Starck and V Stolyarov and R Stompor and R Sudiwala and R Sunyaev and F Sureau and D Sutton and A-S Suur-Uski and J-F Sygnet and Tauber, {J A} and D Tavagnacco and L Terenzi and L Toffolatti and M Tomasi and M Tristram and M Tucci and J Tuovinen and M T??rler and G Umana and L Valenziano and J Valiviita and {Van Tent}, B and L Verstraete and P Vielva and F Villa and N Vittorio and Wade, {L A} and Wandelt, {B D} and N Welikala and N Ysard and D Yvon and A Zacchei and A Zonca",

year = "2014",

month = nov,

doi = "10.1051/0004-6361/201323195",

language = "English",

volume = "571",

journal = "Astronomy and Astrophysics",

issn = "1432-0746",

publisher = "EDP Sciences",

}

Collaboration, P, 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, Beno??t, A, Benoit-L??vy, A, Bernard, J-P, 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, J-F, Catalano, A, Chamballu, A, Chary, R-R, Chiang, HC, Chiang, L-Y, 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, J-M, D??sert, F-X, Dickinson, C, Diego, JM, Dole, H, Donzelli, S, Dor??, O, Douspis, M, Draine, BT, Dupac, X, Efstathiou, G, En??lin, 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-H??raud, Y, Gonz??lez-Nuevo, J, G??rski, KM, Gratton, S, Gregorio, A, Grenier, IA, Gruppuso, A, Guillet, V, Hansen, FK, Hanson, D, Harrison, DL, Helou, G, Henrot-Versill??, S, Hern??ndez-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, Keih??nen, E, Keskitalo, R, Kisner, TS, Knoche, J, Knox, L, Kunz, M, Kurki-Suonio, H, Lagache, G, L??hteenm??ki, A, Lamarre, J-M, Lasenby, A, Laureijs, RJ, Lawrence, CR, Leonardi, R, Le??n-Tavares, J, Lesgourgues, J, Levrier, F, Liguori, M, Lilje, PB, Linden-V??rnle, M, L??pez-Caniego, M, Lubin, PM, Mac??as-P??rez, JF, Maffei, B, Maino, D, Mandolesi, N, Maris, M, Marshall, DJ, Martin, PG, Mart??nez-Gonz??lez, E, Masi, S, Massardi, M, Matarrese, S, Matthai, F, Mazzotta, P, McGehee, P, Melchiorri, A, Mendes, L, Mennella, A, Migliaccio, M, Mitra, S, Miville-Desch??nes, M-A, Moneti, A, Montier, L, Morgante, G, Mortlock, D, Munshi, D, Murphy, JA, Naselsky, P, Nati, F, Natoli, P, Netterfield, CB, N??rgaard-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, Pr??zeau, G, Prunet, S, Puget, J-L, 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, Rubi??o-Mart??n, JA, Rusholme, B, Sandri, M, Santos, D, Savini, G, Scott, D, Seiffert, MD, Shellard, EPS, Spencer, LD, Starck, J-L, Stolyarov, V, Stompor, R, Sudiwala, R, Sunyaev, R, Sureau, F, Sutton, D, Suur-Uski, A-S, Sygnet, J-F, Tauber, JA, Tavagnacco, D, Terenzi, L, Toffolatti, L, Tomasi, M, Tristram, M, Tucci, M, Tuovinen, J, T??rler, 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 2014, 'Planck 2013 results. XI. All-sky model of thermal dust emission', Astronomy and Astrophysics, vol. 571. https://doi.org/10.1051/0004-6361/201323195

TY - JOUR

T1 - Planck 2013 results. XI. All-sky model of thermal dust emission

AU - Collaboration, Planck

AU - Abergel, A

AU - Ade, P A R

AU - Aghanim, N

AU - Alves, M I R

AU - Aniano, G

AU - Armitage-Caplan, C

AU - Arnaud, M

AU - Ashdown, M

AU - Atrio-Barandela, F

AU - Aumont, J

AU - Baccigalupi, C

AU - Banday, A J

AU - Barreiro, R B

AU - Bartlett, J G

AU - Battaner, E

AU - Benabed, K

AU - Beno??t, A

AU - Benoit-L??vy, A

AU - Bernard, J-P

AU - Bersanelli, M

AU - Bielewicz, P

AU - Bobin, J

AU - Bock, J J

AU - Bonaldi, A

AU - Bond, J R

AU - Borrill, J

AU - Bouchet, F R

AU - Boulanger, F

AU - Bridges, M

AU - Bucher, M

AU - Burigana, C

AU - Butler, R C

AU - Cardoso, J-F

AU - Catalano, A

AU - Chamballu, A

AU - Chary, R-R

AU - Chiang, H C

AU - Chiang, L-Y

AU - Christensen, P R

AU - Church, S

AU - Clemens, M

AU - Clements, D L

AU - Colombi, S

AU - Colombo, L P L

AU - Combet, C

AU - Couchot, F

AU - Coulais, A

AU - Crill, B P

AU - Curto, A

AU - Cuttaia, F

AU - Danese, L

AU - Davies, R D

AU - Davis, R J

AU - de Bernardis, P

AU - de Rosa, A

AU - de Zotti, G

AU - Delabrouille, J

AU - Delouis, J-M

AU - D??sert, F-X

AU - Dickinson, C

AU - Diego, J M

AU - Dole, H

AU - Donzelli, S

AU - Dor??, O

AU - Douspis, M

AU - Draine, B T

AU - Dupac, X

AU - Efstathiou, G

AU - En??lin, T A

AU - Eriksen, H K

AU - Falgarone, E

AU - Finelli, F

AU - Forni, O

AU - Frailis, M

AU - Fraisse, A A

AU - Franceschi, E

AU - Galeotta, S

AU - Ganga, K

AU - Ghosh, T

AU - Giard, M

AU - Giardino, G

AU - Giraud-H??raud, Y

AU - Gonz??lez-Nuevo, J

AU - G??rski, K M

AU - Gratton, S

AU - Gregorio, A

AU - Grenier, I A

AU - Gruppuso, A

AU - Guillet, V

AU - Hansen, F K

AU - Hanson, D

AU - Harrison, D L

AU - Helou, G

AU - Henrot-Versill??, S

AU - Hern??ndez-Monteagudo, C

AU - Herranz, D

AU - Hildebrandt, S R

AU - Hivon, E

AU - Hobson, M

AU - Holmes, W A

AU - Hornstrup, A

AU - Hovest, W

AU - Huffenberger, K M

AU - Jaffe, A H

AU - Jaffe, T R

AU - Jewell, J

AU - Joncas, G

AU - Jones, W C

AU - Juvela, M

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PY - 2014/11

Y1 - 2014/11

N2 - This paper presents an all-sky model of dust emission from the Planck 353, 545, and 857 {GHz}, and {IRAS} 100 mum data. Using a modifiedblackbody 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' between 353 and 3000 {GHz} (850 and 100 mum). 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', 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},tau353/{NH}, from the diffuse to the denserinterstellar medium ({ISM}) is reported. It is associated with a decrease in the observed dust temperature, Tobs, that could be due at least in part to the increased dust opacity. We also report an excess of dust emission at H i column densities lower than 1020 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 tau353/{NH} andTobs 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 effect 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 diffuse high-latitude {ISM} tau353 is not as reliable a tracer of dust column density as we conclude it is in molecular clouds where the correlation of tau353 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) usingreddening measurements of quasars deduced from Sloan Digital Sky Survey data.

AB - This paper presents an all-sky model of dust emission from the Planck 353, 545, and 857 {GHz}, and {IRAS} 100 mum data. Using a modifiedblackbody 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' between 353 and 3000 {GHz} (850 and 100 mum). 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', 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},tau353/{NH}, from the diffuse to the denserinterstellar medium ({ISM}) is reported. It is associated with a decrease in the observed dust temperature, Tobs, that could be due at least in part to the increased dust opacity. We also report an excess of dust emission at H i column densities lower than 1020 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 tau353/{NH} andTobs 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 effect 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 diffuse high-latitude {ISM} tau353 is not as reliable a tracer of dust column density as we conclude it is in molecular clouds where the correlation of tau353 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) usingreddening measurements of quasars deduced from Sloan Digital Sky Survey data.

KW - dust

KW - extinction

KW - infrared: ISM

KW - {ISM}: general

KW - methods: data analysis

KW - opacity

KW - submillimeter: ISM

U2 - 10.1051/0004-6361/201323195

DO - 10.1051/0004-6361/201323195

M3 - Article

SN - 1432-0746

SN - 2329-1265

VL - 571

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

ER -

Planck 2013 results. XI. All-sky model of thermal dust emission

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