Altmetric

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

File Description SizeFormat 
1407.5452v3.pdfAccepted version5.21 MBAdobe PDFView/Open
Title: Planck intermediate results XXV. The Andromeda galaxy as seen by Planck
Authors: Ade, PAR
Aghanim, N
Arnaud, M
Ashdown, M
Aumont, J
Baccigalupi, C
Banday, AJ
Barreiro, RB
Bartolo, N
Battaner, E
Battye, R
Benabed, K
Bendo, GJ
Benoit-Levy, 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
Dore, O
Douspis, M
Ducout, A
Dupac, X
Efstathiou, G
Elsner, F
Ensslin, TA
Eriksen, HK
Finelli, F
Forni, O
Frailis, M
Fraisse, AA
Franceschi, E
Frejsel, A
Galeotta, S
Ganga, K
Giard, M
Giraud-Heraud, Y
Gjerlow, E
Gonzalez-Nuevo, J
Gorski, KM
Gregorio, A
Gruppuso, A
Hansen, FK
Hanson, D
Harrison, DL
Henrot-Versille, S
Hernandez-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
Keihanen, E
Keskitalo, R
Kisner, TS
Kneissl, R
Knoche, J
Kunz, M
Kurki-Suonio, H
Lagache, G
Lahteenmaki, A
Lamarre, J-M
Lasenby, A
Lattanzi, M
Lawrence, CR
Leonardi, R
Levrier, F
Liguori, M
Lilje, PB
Linden-Vornle, M
Lopez-Caniego, M
Lubin, PM
Macias-Perez, JF
Madden, S
Maffei, B
Maino, D
Mandolesi, N
Maris, M
Martin, PG
Martinez-Gonzalez, E
Masi, S
Matarrese, S
Mazzotta, P
Mendes, L
Mennella, A
Migliaccio, M
Miville-Deschenes, M-A
Moneti, A
Montier, L
Morgante, G
Mortlock, D
Munshi, D
Murphy, JA
Naselsky, P
Nati, F
Natoli, P
Norgaard-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
Rubino-Martin, 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
Item Type: Journal Article
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 (≳0.3 mm) is heated by the diffuse stellar population (as traced by 3.6 μm 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 μm 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⊙ yr-1. We find a 2.3σ 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.
Issue Date: 30-Sep-2015
Date of Acceptance: 5-Sep-2015
URI: http://hdl.handle.net/10044/1/44002
DOI: http://dx.doi.org/10.1051/0004-6361/201424643
ISSN: 1432-0746
Publisher: EDP Sciences
Volume: 582
Copyright Statement: © 2015 ESO
Sponsor/Funder: Science and Technology Facilities Council (STFC)
Science and Technology Facilities Council (STFC)
Science and Technology Facilities Council (STFC)
Science and Technology Facilities Council (STFC)
Science and Technology Facilities Council (STFC)
Funder's Grant Number: ST/H001239/1
ST/J001368/1
ST/K001051/1
ST/K004131/1
ST/N001206/1
Keywords: Science & Technology
Physical Sciences
Astronomy & Astrophysics
galaxies: individual: Messier 31
galaxies: structure
galaxies: ISM
submillimeter: galaxies
radio continuum: galaxies
MULTIBAND IMAGING PHOTOMETER
RADIO-CONTINUUM SURVEY
PRE-LAUNCH STATUS
SPITZER-SPACE-TELESCOPE
FAR-INFRARED LUMINOSITY
SPINNING DUST EMISSION
RESOLUTION IRAS MAPS
STAR-FORMATION RATES
LOCAL GROUP GALAXIES
COMPLETE CO SURVEY
astro-ph.GA
0201 Astronomical And Space Sciences
Publication Status: Published
Article Number: ARTN A28
Appears in Collections:Physics
Astrophysics
Faculty of Natural Sciences



Items in DSpace are protected by copyright, with all rights reserved, unless otherwise indicated.

Creative Commons