دورية أكاديمية
Planck intermediate results : XXIII Galactic plane emission components derived from Planck with ancillary data
| العنوان: | Planck intermediate results : XXIII Galactic plane emission components derived from Planck with ancillary data |
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| المؤلفون: | P. A. R. Ade, N. Aghanim, M. I. R. Alves, M. Arnaud, M. Ashdown, F. Atrio Barandela, J. Aumont, C. Baccigalupi, A. J. Banday, R. B. Barreiro, E. Battaner, K. Benabed, A. Benoit Lévy, J. P. Bernard, P. Bielewicz, J. Bobin, A. Bonaldi, J. R. Bond, F. R. Bouchet, F. Boulanger, C. Burigana, J. F. Cardoso, A. Catalano, A. Chamballu, H. C. Chiang, P. R. Christensen, D. L. Clements, S. Colombi, L. P. L. Colombo, C. Combet, F. Couchot, B. P. Crill, 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, S. Donzelli, O. Doré, M. Douspis, X. Dupac, G. Efstathiou, T. A. Enßlin, H. K. Eriksen, F. Finelli, O. Forni, M. Frailis, E. Franceschi, S. Galeotta, K. Ganga, R. T. Génova Santos, T. Ghosh, M. Giard, G. Giardino, Y. Giraud Héraud, J. González Nuevo, K. M. Górski, A. Gregorio, A. Gruppuso, F. K. Hansen, D. L. Harrison, S. Henrot Versillé, D. Herranz, S. R. Hildebrandt, E. Hivon, M. Hobson, A. Hornstrup, W. Hovest, K. M. Huffenberger, A. H. Jaffe, T. R. Jaffe, W. C. Jones, E. Keihänen, R. Keskitalo, T. S. Kisner, R. Kneissl, J. Knoche, M. Kunz, H. Kurki Suonio, G. Lagache, A. Lähteenmäki, J. M. Lamarre, A. Lasenby, C. R. Lawrence, R. Leonardi, M. Liguori, P. B. Lilje, M. Linden Vørnle, M. López Caniego, P. M. Lubin, J. F. Macías Pérez, N. Mandolesi, P. G. Martin, E. Martínez González, S. Masi, M. Massardi, S. Matarrese, P. Mazzotta, P. R. Meinhold, A. Melchiorri, L. Mendes, M. Migliaccio, S. Mitra, M. A. Miville Deschênes, A. Moneti, L. Montier, G. Morgante, D. Mortlock, D. Munshi, J. A. Murphy, P. Naselsky, F. Nati, P. Natoli, H. U. Nørgaard Nielsen, F. Noviello, D. Novikov, I. Novikov, C. A. Oxborrow, L. Pagano, F. Pajot, R. Paladini, D. Paoletti, F. Pasian, T. J. Pearson, M. Peel, O. Perdereau, F. Perrotta, F. Piacentini, M. Piat, E. Pierpaoli, D. Pietrobon, S. Plaszczynski, E. Pointecouteau, G. Polenta, N. Ponthieu, L. Popa, G. W. Pratt, S. Prunet, J. L. Puget, J. P. Rachen, W. T. Reach, R. Rebolo, W. Reich, M. Reinecke, M. Remazeilles, C. Renault, S. Ricciardi, T. Riller, I. Ristorcelli, G. Rocha, C. Rosset, G. Roudier, J. A. Rubiño Martín, B. Rusholme, M. Sandri, G. Savini, D. Scott, L. D. Spencer, V. Stolyarov, A. W. Strong, D. Sutton, A. S. Suur Uski, J. F. Sygnet, J. A. Tauber, D. Tavagnacco, L. Terenzi, C. T. Tibbs, L. Toffolatti, M. Tristram, M. Tucci, L. Valenziano, J. Valiviita, B. Van Tent, J. Varis, P. Vielva, F. Villa, L. A. Wade, B. D. Wandelt, R. Watson, D. Yvon, A. Zacchei, A. Zonca, M. Bersanelli, D. Maino, A. Mennella, M. Tomasi |
| المساهمون: | P.A.R. Ade, N. Aghanim, M.I.R. Alve, M. Arnaud, M. Ashdown, F. Atrio-Barandela, J. Aumont, C. Baccigalupi, A.J. Banday, R.B.Barreiro, E. Battaner, K. Benabed, A. Benoit-Lévy, J.P. Bernard, M. Bersanelli, P. Bielewicz, J. Bobin, A. Bonaldi, J.R. Bond, F.R. Bouchet, F. Boulanger, C. Burigana, J.F. Cardoso, A. Catalano, A. Chamballu, H. C. Chiang, P. R. Christensen, D. L. Clement, S. Colombi, L. P. L. Colombo, C. Combet, F. Couchot, B.P. Crill, F. Cuttaia, L. Danese, R.D. Davie, R.J. Davi, P. de Bernardi, A. de Rosa, G. de Zotti, J. Delabrouille, C. Dickinson, J.M. Diego, S. Donzelli, O. Doré, M. Douspi, X. Dupac, G. Efstathiou, T.A. Enßlin, H.K. Eriksen, F. Finelli, O. Forni, M. Fraili, E. Franceschi, S. Galeotta, K. Ganga, R.T. Génova-Santo, T. Ghosh, M. Giard, G. Giardino, Y. Giraud-Héraud, J. González-Nuevo, K.M. Górski, A. Gregorio, A. Gruppuso, F.K. Hansen, D.L. Harrison, S. Henrot-Versillé, D. Herranz, S.R. Hildebrandt, E. Hivon, M. Hobson, A. Hornstrup, W. Hovest, K.M. Huffenberger, A.H. Jaffe, T.R. Jaffe, W.C. Jone, E. Keihänen, R. Keskitalo, T.S. Kisner, R. Kneissl, J. Knoche, M. Kunz, H. Kurki-Suonio, G. Lagache, A. Lähteenmäki, J.M. Lamarre, A. Lasenby, C. R. Lawrence, R.Leonardi, M. Liguori, P.B. Lilje, M. Linden-Vørnle, M. López-Caniego, P.M. Lubin, J.F. Macías-Pérez, D. Maino, N. Mandolesi, P.G. Martin |
| بيانات النشر: | EDP Sciences |
| سنة النشر: | 2015 |
| المجموعة: | The University of Milan: Archivio Istituzionale della Ricerca (AIR) |
| مصطلحات موضوعية: | Galaxy: disk, Galaxy: general, ISM: general, Radiation mechanisms: general, Radio continuum: ISM, Submillimeter: ISM, Astronomy and Astrophysic, Space and Planetary Science, Settore FIS/05 - Astronomia e Astrofisica |
| الوصف: | Planck data when combined with ancillary data provide a unique opportunity to separate the diffuse emission components of the inner Galaxy. The purpose of the paper is to elucidate the morphology of the various emission components in the strong star-formation region lying inside the solar radius and to clarify the relationship between the various components. The region of the Galactic plane covered is l = 300° → 0° → 60° wherestar-formation is highest and the emission is strong enough to make meaningful component separation. The latitude widths in this longitude range lie between 1 and 2, which correspond to FWHM z-widths of 100-200 pc at a typical distance of 6 kpc. The four emission components studied here are synchrotron, free-free, anomalous microwave emission (AME), and thermal (vibrational) dust emission. These components are identified by constructing spectral energy distributions (SEDs) at positions along the Galactic plane using the wide frequency coverage of Planck (28.4-857GHz) in combination with low-frequency radio data at 0.408-2.3 GHz plus WMAP data at 23-94 GHz, along with far-infrared (FIR) data from COBE-DIRBE and IRAS. The free-free component is determined from radio recombination line (RRL) data. AME is found to be comparable in brightness to the free-free emission on the Galactic plane in the frequency range 20-40 GHz with a width in latitude similar to that of the thermal dust; it comprises 45 ± 1% of the total 28.4 GHz emission in the longitude range l = 300° → 0° → 60°. The free-free component is the narrowest, reflecting the fact that it is produced by current star-formation as traced by the narrow distribution of OB stars. It is the dominant emission on the plane between 60 and 100 GHz. RRLs from this ionized gas are used to assess its distance, leading to a free-free z-width of FWHM ≈ 100 pc. The narrow synchrotron component has a low-frequency brightness spectral index β synch ≈ -2.7 that is similar to the broad synchrotron component indicating that they are both populated by the ... |
| نوع الوثيقة: | article in journal/newspaper |
| اللغة: | English |
| العلاقة: | info:eu-repo/semantics/altIdentifier/wos/WOS:000360020200013; volume:580; firstpage:A13; lastpage:1; numberofpages:27; journal:ASTRONOMY & ASTROPHYSICS; http://hdl.handle.net/2434/387727Test; info:eu-repo/semantics/altIdentifier/scopus/2-s2.0-84937874975 |
| DOI: | 10.1051/0004-6361/201424434 |
| الإتاحة: | https://doi.org/10.1051/0004-6361/201424434Test http://hdl.handle.net/2434/387727Test |
| حقوق: | info:eu-repo/semantics/openAccess |
| رقم الانضمام: | edsbas.979C450E |
| قاعدة البيانات: | BASE |
| DOI: | 10.1051/0004-6361/201424434 |
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