Ade, P.A.R. and Aghanim, N. and Alves, M.I.R. and Arnaud, M. and Ashdown, M. and Atrio-Barandela, F. and Aumont, J. and Baccigalupi, C. and Balbi, A. and Banday, A.J. and Barreiro, R.B. and Bartlett, J.G. and Battaner, E. and Bedini, L. and Benabed, K. and Benoit, A. and Bernard, J.-P. and Bersanelli, M. and Bonaldi, A. and Bond, J.R. and Borrill, J. and Bouchet, F.R. and Boulanger, F. and Burigana, C. and Butler, R.C. and Cabella, P. and Cardoso, J.-F. and Chen, X. and Chiang, L.-Y. and Christensen, P.R. and Clements, D.L. and Colombi, S. and Colombo, L.P.L. and Coulais, A. and Cuttaia, F. and Davies, R.D. and Davis, R.J. and De Bernardis, P. and de Gasperis, G. and de Zotti, G. and Delabrouille, J. and Dickinson, C. and Diego, J.M. and Dobler, G. and Dole, H. and Donzelli, S. and Dore, O. and Douspis, M. and Dupac, X. and Enßlin, T.A. and Finelli, F. and Forni, O. and Frailis, M. and Franceschi, E. and Galeotta, S. and Ganga, K. and Genova-Santos, R.T. and Ghosh, T. and Giard, M. and Giardino, G. and Giraud-Héraud, Y. and Gonzalez-Nuevo, J. and Gorski, K.M. and Gregorio, A. and Gruppuso, A. and Hansen, F.K. and Harrison, D. and Hernandez-Monteagudo, C. and Hildebrandt, S.R. and Hivon, E. and Hobson, M. and Holmes, W.A. and Hornstrup, A. and Hovest, W. and Huffenberger, K.M. and Jaffe, A.H. and Jaffe, T.R. and Juvela, M. and Keihanen, E. and Keskitalo, R. and Kisner, T.S. and Knoche, J. and Kunz, M. and Kurki-Suonio, H. and Lagache, G. and Lahteenmaki, A. and Lamarre, J.-M. and Lasenby, A. and Lawrence, C.R. and Leach, S. and Leonardi, R. and Lilje, P.B. and Linden-Vornle, M. and Lubin, P.M. and Macias-Perez, J.F. and Maffei, B. and Maino, D. and Mandolesi, N. and Maris, M. and Marshall, D.J. and Martin, P.G. and Martinez-Gonzalez, E. and Masi, S. and Massardi, M. and Matarrese, S. and Mazzotta, P. and Melchiorri, A. and Mennella, A. and Mitra, S. and Miville-Deschenes, M.-A. and Moneti, A. and Montier, L. and Morgante, G. and Mortlock, D. and Munshi, D. and Murphy, J.Anthony and Naselsky, P. and Nati, F. and Natoli, P. and Norgaard-Nielsen, H.U. and Noviello, F. and Novikov, D. and Novikov, I. and Osborne, S. and Oxborrow, C.A. and Pajot, F. and Paladini, R. and Paoletti, D. and Peel, M. and Perotto, L. and Perrotta, F. and Piacentini, F. and Piat, M. and Pierpaoli, E. and Pietrobon, D. and Plaszczynski, S. and Pointecouteau, E. and Polenta, G. and Popa, L. and Poutanen, T. and Pratt, G.W. and Prunet, S. and Puget, J.-L. and Rachen, J.P. and Reach, W.T. and Rebolo, R. and Reinecke, M. and Renault, C. and Ricciardi, S. and Ristorcelli, I. and Rocha, G. and Rosset, C. and Rubino-Martin, J.A. and Rusholme, B. and Salerno, E. and Sandri, M. and Savini, G. and Scott, D. and Spencer, L. and Stolyarov, V. and Sudiwala, R. and Suur-Uski, A.-S. and Sygnet, J.-F. and Tauber, J.A. and Terenzi, L. and Tibbs, C.T. and Toffolatti, L. and Tomasi, M. and Tristram, M. and Valenziano, L. and Van Tent, B. and Varis, J. and Vielva, P. and Villa, F. and Vittorio, N. and Wade, L.A. and Wandelt, B.D. and Ysard, N. and Yvon, D. and Zacchei, A. and Zonca, A. (2013) Planck intermediate results. XII: Diffuse Galactic components in the Gould Belt system. Astronomy & Astrophysics, 557 (A53). ISSN 0004-6361

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Abstract

We perform an analysis of the diffuse low-frequency Galactic components in the southern part of the Gould Belt system (130° ≤ l ≤ 230° and −50° ≤ b ≤ −10°). Strong ultra-violet flux coming from the Gould Belt super-association is responsible for bright diffuse foregrounds that we observe from our position inside the system and that can help us improve our knowledge of the Galactic emission. Free-free emission and anomalous microwave emission (AME) are the dominant components at low frequencies (ν < 40 GHz), while synchrotron emission is very smooth and faint. We separated diffuse free-free emission and AME from synchrotron emission and thermal dust emission by using Planck data, complemented by ancillary data, using the correlated component analysis (CCA) component-separation method and we compared our results with the results of cross-correlation of foreground templates with the frequency maps. We estimated the electron temperature Te from Hα and free-free emission using two methods (temperature-temperature plot and cross-correlation) and obtained Te ranging from 3100 to 5200K for an effective fraction of absorbing dust along the line of sight of 30% (fd = 0.3). We estimated the frequency spectrum of the diffuse AME and recovered a peak frequency (in flux density units) of 25.5 ± 1.5 GHz. We verified the reliability of this result with realistic simulations that include biases in the spectral model for the AME and in the free-free template. By combining physical models for vibrational and rotational dust emission and adding the constraints from the thermal dust spectrum from Planck and IRAS, we are able to present a good description of the AME frequency spectrum for plausible values of the local density and radiation field.

Item Type:	Article
Additional Information:	Appendices are available in electronic form at http://www.aanda.org
Keywords:	Planck Collaboration; Galaxy: general; radio continuum: ISM; radiation mechanisms: general;
Academic Unit:	Faculty of Science and Engineering > Experimental Physics
Item ID:	14206
Identification Number:	https://doi.org/10.1051/0004-6361/201321160
Depositing User:	Dr. Anthony Murphy
Date Deposited:	18 Mar 2021 17:12
Journal or Publication Title:	Astronomy & Astrophysics
Publisher:	EDP Sciences
Refereed:	Yes
URI:	Publisher
Use Licence:	This item is available under a Creative Commons Attribution Non Commercial Share Alike Licence (CC BY-NC-SA). Details of this licence are available here

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