Planck intermediate results. XXV. The Andromeda galaxy as seen by Planck

Planck Collaboration; P A R Ade; N Aghanim; M Arnaud; M Ashdown; J Aumont; C Baccigalupi; A J Banday; R B Barreiro; N Bartolo; E Battaner; Richard A Battye; K Benabed; G J Bendo; A Benoit-L??vy; J-P Bernard; M Bersanelli; P Bielewicz; A Bonaldi; L Bonavera; J R Bond; J Borrill; F R Bouchet; C Burigana; R C Butler; E Calabrese; J-F Cardoso; A Catalano; A Chamballu; R-R Chary; X Chen; H C Chiang; P R Christensen; D L Clements; 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; C Dickinson; J M Diego; H Dole; S Donzelli; O Dor??; M Douspis; A Ducout; X Dupac; G Efstathiou; F Elsner; T A En??lin; H K Eriksen; F Finelli; O Forni; M Frailis; A A Fraisse; E Franceschi; A Frejsel; S Galeotta; K Ganga; M Giard; Y Giraud-H??raud; E Gjerl??w; J Gonz??lez-Nuevo; K M G??rski; A Gregorio; A Gruppuso; F K Hansen; D Hanson; D L Harrison; 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; G Hurier; F P Israel; A H Jaffe; T R Jaffe; W C Jones; M Juvela; E Keih??nen; R Keskitalo; T S Kisner; R Kneissl; J Knoche; M Kunz; H Kurki-Suonio; G Lagache; A L??hteenm??ki; J-M Lamarre; A Lasenby; M Lattanzi; C R Lawrence; R Leonardi; F Levrier; M Liguori; P B Lilje; M Linden-V??rnle; M L??pez-Caniego; P M Lubin; J F Mac??as-P??rez; S Madden; B Maffei; D Maino; N Mandolesi; M Maris; P G Martin; E Mart??nez-Gonz??lez; S Masi; S Matarrese; P Mazzotta; L Mendes; A Mennella; M Migliaccio; M-A Miville-Desch??nes; A Moneti; L Montier; G Morgante; D Mortlock; D Munshi; J A Murphy; P Naselsky; F Nati; P Natoli; H U N??rgaard-Nielsen; F Noviello; D Novikov; I Novikov; C A Oxborrow; L Pagano; F Pajot; R Paladini; D Paoletti; B Partridge; F Pasian; T J Pearson; Michael Peel; O Perdereau; F Perrotta; V Pettorino; F Piacentini; M Piat; E Pierpaoli; D Pietrobon; S Plaszczynski; E Pointecouteau; G Polenta; L Popa; G W Pratt; S Prunet; J-L Puget; J P Rachen; M Reinecke; M Remazeilles; C Renault; S Ricciardi; I Ristorcelli; G Rocha; C Rosset; M Rossetti; G Roudier; J A Rubi??o-Mart??n; B Rusholme; M Sandri; G Savini; D Scott; L D Spencer; V Stolyarov; R Sudiwala; D Sutton; A-S Suur-Uski; J-F Sygnet; J A Tauber; L Terenzi; L Toffolatti; M Tomasi; M Tristram; M Tucci; G Umana; L Valenziano; J Valiviita; B Van Tent; P Vielva; F Villa; L A Wade; B D Wandelt; R Watson; I K Wehus; D Yvon; A Zacchei; A Zonca; A. Benoit-Lévy; O. Doré; T. A. Enßlin; Y. Giraud-Héraud; E. Gjerløw; J. González-Nuevo; K. M. Górski; S. Henrot-Versillé; C. Hernández-Monteagudo; E. Keihänen; A. Lähteenmäki; M. Linden-Vørnle; M. López-Caniego; J. F. Macías-Pérez; E. Martínez-González; M.-A. Miville-Deschênes; H. U. Nørgaard-Nielsen; J. A. Rubiño-Martín

doi:10.1051/0004-6361/201424643

Planck intermediate results. XXV. The Andromeda galaxy as seen by Planck

Planck Collaboration, P A R Ade, N Aghanim, M Arnaud, M Ashdown, J Aumont, C Baccigalupi, A J Banday, R B Barreiro, N Bartolo, E Battaner, Richard A Battye, K Benabed, G J Bendo, A Benoit-L??vy, J-P Bernard, M Bersanelli, P Bielewicz, A Bonaldi, L BonaveraJ R Bond, J Borrill, F R Bouchet, C Burigana, R C Butler, E Calabrese, J-F Cardoso, A Catalano, A Chamballu, R-R Chary, X Chen, H C Chiang, P R Christensen, D L Clements, 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, C Dickinson, J M Diego, H Dole, S Donzelli, O Dor??, M Douspis, A Ducout, X Dupac, G Efstathiou, F Elsner, T A En??lin, H K Eriksen, F Finelli, O Forni, M Frailis, A A Fraisse, E Franceschi, A Frejsel, S Galeotta, K Ganga, M Giard, Y Giraud-H??raud, E Gjerl??w, J Gonz??lez-Nuevo, K M G??rski, A Gregorio, A Gruppuso, F K Hansen, D Hanson, D L Harrison, 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, G Hurier, F P Israel, A H Jaffe, T R Jaffe, W C Jones, M Juvela, E Keih??nen, R Keskitalo, T S Kisner, R Kneissl, J Knoche, M Kunz, H Kurki-Suonio, G Lagache, A L??hteenm??ki, J-M Lamarre, A Lasenby, M Lattanzi, C R Lawrence, R Leonardi, F Levrier, M Liguori, P B Lilje, M Linden-V??rnle, M L??pez-Caniego, P M Lubin, J F Mac??as-P??rez, S Madden, B Maffei, D Maino, N Mandolesi, M Maris, P G Martin, E Mart??nez-Gonz??lez, S Masi, S Matarrese, P Mazzotta, L Mendes, A Mennella, M Migliaccio, M-A Miville-Desch??nes, A Moneti, L Montier, G Morgante, D Mortlock, D Munshi, J A Murphy, P Naselsky, F Nati, P Natoli, H U N??rgaard-Nielsen, F Noviello, D Novikov, I Novikov, C A Oxborrow, L Pagano, F Pajot, R Paladini, D Paoletti, B Partridge, F Pasian, T J Pearson, Michael Peel, O Perdereau, F Perrotta, V Pettorino, F Piacentini, M Piat, E Pierpaoli, D Pietrobon, S Plaszczynski, E Pointecouteau, G Polenta, L Popa, G W Pratt, S Prunet, J-L Puget, J P Rachen, M Reinecke, M Remazeilles, C Renault, S Ricciardi, I Ristorcelli, G Rocha, C Rosset, M Rossetti, G Roudier, J A Rubi??o-Mart??n, B Rusholme, M Sandri, G Savini, D Scott, L D Spencer, V Stolyarov, R Sudiwala, D Sutton, A-S Suur-Uski, J-F Sygnet, J A Tauber, L Terenzi, L Toffolatti, M Tomasi, M Tristram, M Tucci, G Umana, L Valenziano, J Valiviita, B Van Tent, P Vielva, F Villa, L A Wade, B D Wandelt, R Watson, I K Wehus, D Yvon, A Zacchei, A Zonca, A. Benoit-Lévy, O. Doré, T. A. Enßlin, Y. Giraud-Héraud, E. Gjerløw, J. González-Nuevo, K. M. Górski, S. Henrot-Versillé, C. Hernández-Monteagudo, E. Keihänen, A. Lähteenmäki, M. Linden-Vørnle, M. López-Caniego, J. F. Macías-Pérez, E. Martínez-González, M.-A. Miville-Deschênes, H. U. Nørgaard-Nielsen, J. A. Rubiño-Martín

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

Abstract

The Andromeda galaxy (M 31) is one of a few galaxies that has sufficient angular size on the sky to be resolved by the Planck satellite. Planck has detected M 31 in all of its frequency bands, and has mapped out the dust emission with the High Frequency Instrument, clearly resolving multiple spiralarms and sub-features. We examine the morphology of this long-wavelength dust emission as seen by Planck, including a study of its outermost spiral arms, and investigate the dust heating mechanism across M 31. We find that dust dominating the longer wavelength emission (‚â≥0.3 mm) is heated by the diffuse stellar population (as traced by 3.6 Œºm emission), with the dust dominating the shorter wavelength emission heated by a mix of the old stellar population and star-forming regions (as traced by 24 Œºm emission). We also fit spectral energy distributions for individual 5' pixels and quantify the dust properties across the galaxy, taking into account these different heating mechanisms, finding that there is a linear decrease in temperature with galactocentric distance for dust heated by the old stellar population, as would be expected, with temperatures ranging from around 22 K in the nucleus to 14 K outside of the 10 kpc ring. Finally, we measure the integrated spectrum of the whole galaxy, which we find to be well-fitted with a global dust temperature of (18.2 ¬± 1.0) K with a spectral index of 1.62 ¬± 0.11 (assuming a single modified blackbody), and a significant amount of free-free emission at intermediate frequencies of 20-60 GHz, which corresponds to a star formation rate of around 0.12 M_‚äô yr^-1. We find a 2.3œÉ detection of the presence of spinning dust emission, with a 30 GHz amplitude of 0.7 ¬± 0.3 Jy, which is in line with expectations from our Galaxy.

Original language	English
Article number	A28
Number of pages	23
Journal	Astronomy and Astrophysics
Volume	582
DOIs	https://doi.org/10.1051/0004-6361/201424643
Publication status	Published - Oct 2015

Keywords

galaxies: individual: Messier 31
galaxies: ISM
galaxies: structure
radio continuum: galaxies
submillimeter: galaxies

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10.1051/0004-6361/201424643

Cite this

Collaboration, P., Ade, P. A. R., Aghanim, N., Arnaud, M., Ashdown, M., Aumont, J., Baccigalupi, C., Banday, A. J., Barreiro, R. B., Bartolo, N., Battaner, E., Battye, R. A., Benabed, K., Bendo, G. J., Benoit-L??vy, A., Bernard, J.-P., Bersanelli, M., Bielewicz, P., Bonaldi, A., ... Rubiño-Martín, J. A. (2015). Planck intermediate results. XXV. The Andromeda galaxy as seen by Planck. Astronomy and Astrophysics, 582, Article A28. https://doi.org/10.1051/0004-6361/201424643

@article{0a849d7a14f241d0b5a3f8cf1e8f2079,

title = "Planck intermediate results. XXV. The Andromeda galaxy as seen by Planck",

abstract = "The Andromeda galaxy (M 31) is one of a few galaxies that has sufficient angular size on the sky to be resolved by the Planck satellite. Planck has detected M 31 in all of its frequency bands, and has mapped out the dust emission with the High Frequency Instrument, clearly resolving multiple spiralarms and sub-features. We examine the morphology of this long-wavelength dust emission as seen by Planck, including a study of its outermost spiral arms, and investigate the dust heating mechanism across M 31. We find that dust dominating the longer wavelength emission (‚{\^a}≥0.3 mm) is heated by the diffuse stellar population (as traced by 3.6 {\OE}ºm emission), with the dust dominating the shorter wavelength emission heated by a mix of the old stellar population and star-forming regions (as traced by 24 {\OE}ºm emission). We also fit spectral energy distributions for individual 5' pixels and quantify the dust properties across the galaxy, taking into account these different heating mechanisms, finding that there is a linear decrease in temperature with galactocentric distance for dust heated by the old stellar population, as would be expected, with temperatures ranging from around 22 K in the nucleus to 14 K outside of the 10 kpc ring. Finally, we measure the integrated spectrum of the whole galaxy, which we find to be well-fitted with a global dust temperature of (18.2 ¬± 1.0) K with a spectral index of 1.62 ¬± 0.11 (assuming a single modified blackbody), and a significant amount of free-free emission at intermediate frequencies of 20-60 GHz, which corresponds to a star formation rate of around 0.12 M‚{\"a}{\^o} yr-1. We find a 2.3{\oe}{\'E} detection of the presence of spinning dust emission, with a 30 GHz amplitude of 0.7 ¬± 0.3 Jy, which is in line with expectations from our Galaxy.",

keywords = "galaxies: individual: Messier 31, galaxies: ISM, galaxies: structure, radio continuum: galaxies, submillimeter: galaxies",

author = "Planck Collaboration and Ade, {P A R} and N Aghanim and M Arnaud and M Ashdown and J Aumont and C Baccigalupi and Banday, {A J} and Barreiro, {R B} and N Bartolo and E Battaner and Battye, {Richard A} and K Benabed and Bendo, {G J} and A Benoit-L??vy and J-P Bernard and M Bersanelli and P Bielewicz and A Bonaldi and L Bonavera and Bond, {J R} and J Borrill and Bouchet, {F R} and C Burigana and Butler, {R C} and E Calabrese and J-F Cardoso and A Catalano and A Chamballu and R-R Chary and X Chen and Chiang, {H C} and Christensen, {P R} and Clements, {D L} 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 C Dickinson and Diego, {J M} and H Dole and S Donzelli and O Dor?? and M Douspis and A Ducout and X Dupac and G Efstathiou and F Elsner and En??lin, {T A} and Eriksen, {H K} and F Finelli and O Forni and M Frailis and Fraisse, {A A} and E Franceschi and A Frejsel and S Galeotta and K Ganga and M Giard and Y Giraud-H??raud and E Gjerl??w and J Gonz??lez-Nuevo and G??rski, {K M} and A Gregorio and A Gruppuso and Hansen, {F K} and D Hanson and Harrison, {D L} 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 G Hurier and Israel, {F P} and Jaffe, {A H} and Jaffe, {T R} and Jones, {W C} and M Juvela and E Keih??nen and R Keskitalo and Kisner, {T S} and R Kneissl and J Knoche and M Kunz and H Kurki-Suonio and G Lagache and A L??hteenm??ki and J-M Lamarre and A Lasenby and M Lattanzi and Lawrence, {C R} and R Leonardi 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 S Madden and B Maffei and D Maino and N Mandolesi and M Maris and Martin, {P G} and E Mart??nez-Gonz??lez and S Masi and S Matarrese and P Mazzotta and L Mendes and A Mennella and M Migliaccio 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 N??rgaard-Nielsen, {H U} and F Noviello and D Novikov and I Novikov and Oxborrow, {C A} and L Pagano and F Pajot and R Paladini and D Paoletti and B Partridge and F Pasian and Pearson, {T J} and Michael Peel and O Perdereau and F Perrotta and V Pettorino and F Piacentini and M Piat and E Pierpaoli and D Pietrobon and S Plaszczynski and E Pointecouteau and G Polenta and L Popa and Pratt, {G W} and S Prunet and J-L Puget and Rachen, {J P} and M Reinecke and M Remazeilles and C Renault and S Ricciardi and I Ristorcelli and G Rocha and C Rosset and M Rossetti and G Roudier and Rubi??o-Mart??n, {J A} and B Rusholme and M Sandri and G Savini and D Scott and Spencer, {L D} and V Stolyarov and R Sudiwala and D Sutton and A-S Suur-Uski and J-F Sygnet and Tauber, {J A} and L Terenzi and L Toffolatti and M Tomasi and M Tristram and M Tucci and G Umana and L Valenziano and J Valiviita and {Van Tent}, B and P Vielva and F Villa and Wade, {L A} and Wandelt, {B D} and R Watson and Wehus, {I K} and D Yvon and A Zacchei and A Zonca and A. Benoit-L{\'e}vy and O. Dor{\'e} and En{\ss}lin, {T. A.} and Y. Giraud-H{\'e}raud and E. Gjerl{\o}w and J. Gonz{\'a}lez-Nuevo and G{\'o}rski, {K. M.} and S. Henrot-Versill{\'e} and C. Hern{\'a}ndez-Monteagudo and E. Keih{\"a}nen and A. L{\"a}hteenm{\"a}ki and M. Linden-V{\o}rnle and M. L{\'o}pez-Caniego and Mac{\'i}as-P{\'e}rez, {J. F.} and E. Mart{\'i}nez-Gonz{\'a}lez and M.-A. Miville-Desch{\^e}nes and N{\o}rgaard-Nielsen, {H. U.} and Rubi{\~n}o-Mart{\'i}n, {J. A.}",

year = "2015",

month = oct,

doi = "10.1051/0004-6361/201424643",

language = "English",

volume = "582",

journal = "Astronomy and Astrophysics",

issn = "1432-0746",

publisher = "EDP Sciences",

}

Collaboration, P, Ade, PAR, Aghanim, N, Arnaud, M, Ashdown, M, Aumont, J, Baccigalupi, C, Banday, AJ, Barreiro, RB, Bartolo, N, Battaner, E, Battye, RA, Benabed, K, Bendo, GJ, Benoit-L??vy, A, Bernard, J-P, Bersanelli, M, Bielewicz, P, Bonaldi, A, Bonavera, L, Bond, JR, Borrill, J, Bouchet, FR, Burigana, C, Butler, RC, Calabrese, E, Cardoso, J-F, Catalano, A, Chamballu, A, Chary, R-R, Chen, X, Chiang, HC, Christensen, PR, Clements, DL, 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, Dickinson, C, Diego, JM, Dole, H, Donzelli, S, Dor??, O, Douspis, M, Ducout, A, Dupac, X, Efstathiou, G, Elsner, F, En??lin, TA, Eriksen, HK, Finelli, F, Forni, O, Frailis, M, Fraisse, AA, Franceschi, E, Frejsel, A, Galeotta, S, Ganga, K, Giard, M, Giraud-H??raud, Y, Gjerl??w, E, Gonz??lez-Nuevo, J, G??rski, KM, Gregorio, A, Gruppuso, A, Hansen, FK, Hanson, D, Harrison, DL, Henrot-Versill??, S, Hern??ndez-Monteagudo, C, Herranz, D, Hildebrandt, SR, Hivon, E, Hobson, M, Holmes, WA, Hornstrup, A, Hovest, W, Huffenberger, KM, Hurier, G, Israel, FP, Jaffe, AH, Jaffe, TR, Jones, WC, Juvela, M, Keih??nen, E, Keskitalo, R, Kisner, TS, Kneissl, R, Knoche, J, Kunz, M, Kurki-Suonio, H, Lagache, G, L??hteenm??ki, A, Lamarre, J-M, Lasenby, A, Lattanzi, M, Lawrence, CR, Leonardi, R, Levrier, F, Liguori, M, Lilje, PB, Linden-V??rnle, M, L??pez-Caniego, M, Lubin, PM, Mac??as-P??rez, JF, Madden, S, Maffei, B, Maino, D, Mandolesi, N, Maris, M, Martin, PG, Mart??nez-Gonz??lez, E, Masi, S, Matarrese, S, Mazzotta, P, Mendes, L, Mennella, A, Migliaccio, M, Miville-Desch??nes, M-A, Moneti, A, Montier, L, Morgante, G, Mortlock, D, Munshi, D, Murphy, JA, Naselsky, P, Nati, F, Natoli, P, N??rgaard-Nielsen, HU, Noviello, F, Novikov, D, Novikov, I, Oxborrow, CA, Pagano, L, Pajot, F, Paladini, R, Paoletti, D, Partridge, B, Pasian, F, Pearson, TJ, Peel, M, Perdereau, O, Perrotta, F, Pettorino, V, Piacentini, F, Piat, M, Pierpaoli, E, Pietrobon, D, Plaszczynski, S, Pointecouteau, E, Polenta, G, Popa, L, Pratt, GW, Prunet, S, Puget, J-L, Rachen, JP, Reinecke, M, Remazeilles, M, Renault, C, Ricciardi, S, Ristorcelli, I, Rocha, G, Rosset, C, Rossetti, M, Roudier, G, Rubi??o-Mart??n, JA, Rusholme, B, Sandri, M, Savini, G, Scott, D, Spencer, LD, Stolyarov, V, Sudiwala, R, Sutton, D, Suur-Uski, A-S, Sygnet, J-F, Tauber, JA, Terenzi, L, Toffolatti, L, Tomasi, M, Tristram, M, Tucci, M, Umana, G, Valenziano, L, Valiviita, J, Van Tent, B, Vielva, P, Villa, F, Wade, LA, Wandelt, BD, Watson, R, Wehus, IK, Yvon, D, Zacchei, A, Zonca, A, Benoit-Lévy, A, Doré, O, Enßlin, TA, Giraud-Héraud, Y, Gjerløw, E, González-Nuevo, J, Górski, KM, Henrot-Versillé, S, Hernández-Monteagudo, C, Keihänen, E, Lähteenmäki, A, Linden-Vørnle, M, López-Caniego, M, Macías-Pérez, JF, Martínez-González, E, Miville-Deschênes, M-A, Nørgaard-Nielsen, HU & Rubiño-Martín, JA 2015, 'Planck intermediate results. XXV. The Andromeda galaxy as seen by Planck', Astronomy and Astrophysics, vol. 582, A28. https://doi.org/10.1051/0004-6361/201424643

TY - JOUR

T1 - Planck intermediate results. XXV. The Andromeda galaxy as seen by Planck

AU - Collaboration, Planck

AU - Ade, P A R

AU - Aghanim, N

AU - Arnaud, M

AU - Ashdown, M

AU - Aumont, J

AU - Baccigalupi, C

AU - Banday, A J

AU - Barreiro, R B

AU - Bartolo, N

AU - Battaner, E

AU - Battye, Richard A

AU - Benabed, K

AU - Bendo, G J

AU - Benoit-L??vy, A

AU - Bernard, J-P

AU - Bersanelli, M

AU - Bielewicz, P

AU - Bonaldi, A

AU - Bonavera, L

AU - Bond, J R

AU - Borrill, J

AU - Bouchet, F R

AU - Burigana, C

AU - Butler, R C

AU - Calabrese, E

AU - Cardoso, J-F

AU - Catalano, A

AU - Chamballu, A

AU - Chary, R-R

AU - Chen, X

AU - Chiang, H C

AU - Christensen, P R

AU - Clements, D L

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 - Dickinson, C

AU - Diego, J M

AU - Dole, H

AU - Donzelli, S

AU - Dor??, O

AU - Douspis, M

AU - Ducout, A

AU - Dupac, X

AU - Efstathiou, G

AU - Elsner, F

AU - En??lin, T A

AU - Eriksen, H K

AU - Finelli, F

AU - Forni, O

AU - Frailis, M

AU - Fraisse, A A

AU - Franceschi, E

AU - Frejsel, A

AU - Galeotta, S

AU - Ganga, K

AU - Giard, M

AU - Giraud-H??raud, Y

AU - Gjerl??w, E

AU - Gonz??lez-Nuevo, J

AU - G??rski, K M

AU - Gregorio, A

AU - Gruppuso, A

AU - Hansen, F K

AU - Hanson, D

AU - Harrison, D L

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 - Hurier, G

AU - Israel, F P

AU - Jaffe, A H

AU - Jaffe, T R

AU - Jones, W C

AU - Juvela, M

AU - Keih??nen, E

AU - Keskitalo, R

AU - Kisner, T S

AU - Kneissl, R

AU - Knoche, J

AU - Kunz, M

AU - Kurki-Suonio, H

AU - Lagache, G

AU - L??hteenm??ki, A

AU - Lamarre, J-M

AU - Lasenby, A

AU - Lattanzi, M

AU - Lawrence, C R

AU - Leonardi, R

AU - Levrier, F

AU - Liguori, M

AU - Lilje, P B

AU - Linden-V??rnle, M

AU - L??pez-Caniego, M

AU - Lubin, P M

AU - Mac??as-P??rez, J F

AU - Madden, S

AU - Maffei, B

AU - Maino, D

AU - Mandolesi, N

AU - Maris, M

AU - Martin, P G

AU - Mart??nez-Gonz??lez, E

AU - Masi, S

AU - Matarrese, S

AU - Mazzotta, P

AU - Mendes, L

AU - Mennella, A

AU - Migliaccio, M

AU - Miville-Desch??nes, M-A

AU - Moneti, A

AU - Montier, L

AU - Morgante, G

AU - Mortlock, D

AU - Munshi, D

AU - Murphy, J A

AU - Naselsky, P

AU - Nati, F

AU - Natoli, P

AU - N??rgaard-Nielsen, H U

AU - Noviello, F

AU - Novikov, D

AU - Novikov, I

AU - Oxborrow, C A

AU - Pagano, L

AU - Pajot, F

AU - Paladini, R

AU - Paoletti, D

AU - Partridge, B

AU - Pasian, F

AU - Pearson, T J

AU - Peel, Michael

AU - Perdereau, O

AU - Perrotta, F

AU - Pettorino, V

AU - Piacentini, F

AU - Piat, M

AU - Pierpaoli, E

AU - Pietrobon, D

AU - Plaszczynski, S

AU - Pointecouteau, E

AU - Polenta, G

AU - Popa, L

AU - Pratt, G W

AU - Prunet, S

AU - Puget, J-L

AU - Rachen, J P

AU - Reinecke, M

AU - Remazeilles, M

AU - Renault, C

AU - Ricciardi, S

AU - Ristorcelli, I

AU - Rocha, G

AU - Rosset, C

AU - Rossetti, M

AU - Roudier, G

AU - Rubi??o-Mart??n, J A

AU - Rusholme, B

AU - Sandri, M

AU - Savini, G

AU - Scott, D

AU - Spencer, L D

AU - Stolyarov, V

AU - Sudiwala, R

AU - Sutton, D

AU - Suur-Uski, A-S

AU - Sygnet, J-F

AU - Tauber, J A

AU - Terenzi, L

AU - Toffolatti, L

AU - Tomasi, M

AU - Tristram, M

AU - Tucci, M

AU - Umana, G

AU - Valenziano, L

AU - Valiviita, J

AU - Van Tent, B

AU - Vielva, P

AU - Villa, F

AU - Wade, L A

AU - Wandelt, B D

AU - Watson, R

AU - Wehus, I K

AU - Yvon, D

AU - Zacchei, A

AU - Zonca, A

AU - Benoit-Lévy, A.

AU - Doré, O.

AU - Enßlin, T. A.

AU - Giraud-Héraud, Y.

AU - Gjerløw, E.

AU - González-Nuevo, J.

AU - Górski, K. M.

AU - Henrot-Versillé, S.

AU - Hernández-Monteagudo, C.

AU - Keihänen, E.

AU - Lähteenmäki, A.

AU - Linden-Vørnle, M.

AU - López-Caniego, M.

AU - Macías-Pérez, J. F.

AU - Martínez-González, E.

AU - Miville-Deschênes, M.-A.

AU - Nørgaard-Nielsen, H. U.

AU - Rubiño-Martín, J. A.

PY - 2015/10

Y1 - 2015/10

N2 - The Andromeda galaxy (M 31) is one of a few galaxies that has sufficient angular size on the sky to be resolved by the Planck satellite. Planck has detected M 31 in all of its frequency bands, and has mapped out the dust emission with the High Frequency Instrument, clearly resolving multiple spiralarms and sub-features. We examine the morphology of this long-wavelength dust emission as seen by Planck, including a study of its outermost spiral arms, and investigate the dust heating mechanism across M 31. We find that dust dominating the longer wavelength emission (‚â≥0.3 mm) is heated by the diffuse stellar population (as traced by 3.6 Œºm emission), with the dust dominating the shorter wavelength emission heated by a mix of the old stellar population and star-forming regions (as traced by 24 Œºm emission). We also fit spectral energy distributions for individual 5' pixels and quantify the dust properties across the galaxy, taking into account these different heating mechanisms, finding that there is a linear decrease in temperature with galactocentric distance for dust heated by the old stellar population, as would be expected, with temperatures ranging from around 22 K in the nucleus to 14 K outside of the 10 kpc ring. Finally, we measure the integrated spectrum of the whole galaxy, which we find to be well-fitted with a global dust temperature of (18.2 ¬± 1.0) K with a spectral index of 1.62 ¬± 0.11 (assuming a single modified blackbody), and a significant amount of free-free emission at intermediate frequencies of 20-60 GHz, which corresponds to a star formation rate of around 0.12 M‚äô yr-1. We find a 2.3œÉ detection of the presence of spinning dust emission, with a 30 GHz amplitude of 0.7 ¬± 0.3 Jy, which is in line with expectations from our Galaxy.

AB - The Andromeda galaxy (M 31) is one of a few galaxies that has sufficient angular size on the sky to be resolved by the Planck satellite. Planck has detected M 31 in all of its frequency bands, and has mapped out the dust emission with the High Frequency Instrument, clearly resolving multiple spiralarms and sub-features. We examine the morphology of this long-wavelength dust emission as seen by Planck, including a study of its outermost spiral arms, and investigate the dust heating mechanism across M 31. We find that dust dominating the longer wavelength emission (‚â≥0.3 mm) is heated by the diffuse stellar population (as traced by 3.6 Œºm emission), with the dust dominating the shorter wavelength emission heated by a mix of the old stellar population and star-forming regions (as traced by 24 Œºm emission). We also fit spectral energy distributions for individual 5' pixels and quantify the dust properties across the galaxy, taking into account these different heating mechanisms, finding that there is a linear decrease in temperature with galactocentric distance for dust heated by the old stellar population, as would be expected, with temperatures ranging from around 22 K in the nucleus to 14 K outside of the 10 kpc ring. Finally, we measure the integrated spectrum of the whole galaxy, which we find to be well-fitted with a global dust temperature of (18.2 ¬± 1.0) K with a spectral index of 1.62 ¬± 0.11 (assuming a single modified blackbody), and a significant amount of free-free emission at intermediate frequencies of 20-60 GHz, which corresponds to a star formation rate of around 0.12 M‚äô yr-1. We find a 2.3œÉ detection of the presence of spinning dust emission, with a 30 GHz amplitude of 0.7 ¬± 0.3 Jy, which is in line with expectations from our Galaxy.

KW - galaxies: individual: Messier 31

KW - galaxies: ISM

KW - galaxies: structure

KW - radio continuum: galaxies

KW - submillimeter: galaxies

U2 - 10.1051/0004-6361/201424643

DO - 10.1051/0004-6361/201424643

M3 - Article

SN - 1432-0746

SN - 2329-1265

VL - 582

JO - Astronomy and Astrophysics

JF - Astronomy and Astrophysics

M1 - A28

ER -

Planck intermediate results. XXV. The Andromeda galaxy as seen by Planck

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