{ "id": "1405.0873", "version": "v2", "published": "2014-05-05T12:31:06.000Z", "updated": "2015-03-12T06:36:26.000Z", "title": "Planck intermediate results. XXI. Comparison of polarized thermal emission from Galactic dust at 353 GHz with interstellar polarization in the visible", "authors": [ "Planck Collaboration", "P. A. R. Ade", "N. Aghanim", "D. Alina", "G. Aniano", "C. Armitage-Caplan", "M. Arnaud", "M. Ashdown", "F. Atrio-Barandela", "J. Aumont", "C. Baccigalupi", "A. J. Banday", "R. B. Barreiro", "E. Battaner", "C. Beichman", "K. Benabed", "A. Benoit-Lévy", "J. -P. Bernard", "M. Bersanelli", "P. Bielewicz", "J. J. Bock", "J. R. Bond", "J. Borrill", "F. R. Bouchet", "F. Boulanger", "C. Burigana", "J. -F. Cardoso", "A. Catalano", "A. Chamballu", "R. -R. Chary", "H. C. Chiang", "P. R. Christensen", "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", "F. -X. Désert", "C. Dickinson", "J. M. Diego", "S. Donzelli", "O. Doré", "M. Douspis", "J. Dunkley", "X. Dupac", "T. A. Enßlin", "H. K. Eriksen", "E. Falgarone", "L. Fanciullo", "F. Finelli", "O. Forni", "M. Frailis", "A. A. Fraisse", "E. Franceschi", "S. Galeotta", "K. Ganga", "T. Ghosh", "M. Giard", "Y. Giraud-Héraud", "J. González-Nuevo", "K. M. Górski", "A. Gregorio", "A. Gruppuso", "V. Guillet", "F. K. Hansen", "D. L. Harrison", "G. Helou", "C. Hernández-Monteagudo", "S. R. Hildebrandt", "E. Hivon", "M. Hobson", "W. A. Holmes", "A. Hornstrup", "K. M. Huffenberger", "A. H. Jaffe", "T. R. Jaffe", "W. C. Jones", "M. Juvela", "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", "F. Levrier", "M. Liguori", "P. B. Lilje", "M. Linden-Vørnle", "M. López-Caniego", "P. M. Lubin", "J. F. Macías-Pérez", "B. Maffei", "A. M. Magalhães", "D. Maino", "N. Mandolesi", "M. Maris", "D. J. Marshall", "P. G. Martin", "E. Martínez-González", "S. Masi", "S. Matarrese", "P. Mazzotta", "A. Melchiorri", "L. Mendes", "A. Mennella", "M. Migliaccio", "M. -A. Miville-Deschênes", "A. Moneti", "L. Montier", "G. Morgante", "D. Mortlock", "D. Munshi", "J. A. Murphy", "P. Naselsky", "F. Nati", "P. Natoli", "C. B. Netterfield", "F. Noviello", "D. Novikov", "I. Novikov", "C. A. Oxborrow", "L. Pagano", "F. Pajot", "R. Paladini", "D. Paoletti", "F. Pasian", "O. Perdereau", "L. Perotto", "F. Perrotta", "F. Piacentini", "M. Piat", "D. Pietrobon", "S. Plaszczynski", "F. Poidevin", "E. Pointecouteau", "G. Polenta", "L. Popa", "G. W. Pratt", "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", "B. Rusholme", "M. Sandri", "G. Savini", "D. Scott", "L. D. Spencer", "V. Stolyarov", "R. Stompor", "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", "A. Zonca" ], "categories": [ "astro-ph.GA" ], "abstract": "The Planck survey provides unprecedented full-sky coverage of the submillimetre polarized emission from Galactic dust, bringing new constraints on the properties of dust. The dust grains that emit the radiation seen by Planck in the submillimetre also extinguish and polarize starlight in the visible. Comparison of the polarization of the emission and of the interstellar polarization on selected lines of sight probed by stars provides unique new diagnostics of the emission and light scattering properties of dust. Using ancillary catalogues of interstellar polarization and extinction of starlight, we obtain the degree of polarization, $p_V$ , and the optical depth in the V band to the star, $\\tau_V$. Toward these stars we measure the submillimetre polarized intensity, $P_S$, and total intensity, $I_S$, in the Planck 353 GHz channel. For those lines of sight through the diffuse interstellar medium with comparable values of the estimated column density and polarization directions close to orthogonal, we correlate properties in the submillimetre and visible to find two ratios, $R_{S/V} = (P_S/I_S)/(p_V/\\tau_V)$ and $R_{P/p} = P_S/p_V$ , the latter focusing directly on the polarization properties of the aligned grain population alone. We find $R_{S/V}$ = 4.2, with statistical and systematic uncertainties 0.2 and 0.3, respectively, and $R_{P/p}$ = 5.4 MJy sr$^{-1}$, with uncertainties 0.2 and 0.3 MJy sr$^{-1}$, respectively. Our estimate of $R_{S/V}$ is compatible with predictions based on a range of polarizing dust models that have been developed for the diffuse interstellar medium. However, our estimate of $R_{P/p}$ is not compatible with predictions, which are too low by a factor of about 2.5. This more discriminating diagnostic, $R_{P/p}$, indicates that changes to the optical properties in the models of the aligned grain population are required.", "revisions": [ { "version": "v1", "updated": "2014-05-05T12:31:06.000Z", "title": "Planck intermediate results. XXI. Comparison of polarized thermal emission from Galactic dust at 353 GHz with optical interstellar polarization", "abstract": "The Planck survey provides unprecedented full-sky coverage of the submillimetre polarized emission from Galactic dust, bringing new constraints on the properties of dust. The dust grains that emit the radiation seen by Planck in the submillimetre also extinguish and polarize starlight in the optical. Using ancillary catalogues of interstellar polarization and extinction of starlight, we obtain the degree of polarization, $p_V$, and the optical depth in the $V$ band to the star, $\\tau_V$. We extract the submillimetre polarized intensity, $P_S$, and total intensity, $I_S$, measured toward these stars in the Planck 353 GHz channel. We compare the position angle measured in the optical with that measured at 353 GHz, and the column density measure $E(B - V)$ with that inferred from the Planck product map of the submillimetre dust optical depth. For those lines of sight suitable for this comparison, we measure the polarization ratios $R_{S/V} = (P_S/I_S)/(p_V/\\tau_V)$ and $R_{P/p} = P_S / p_V$ through a correlation analysis. We find $R_{S/V} = 4.3$ with statistical and systematic uncertainties 0.2 and 0.4, respectively, and $R_{P/p} = 5.6$ MJy sr$^{-1}$, with statistical and systematic uncertainties 0.2 and 0.4 MJy sr$^{-1}$, respectively. Our estimate of $R_{S/V}$ is reasonably compatible with current dust models, not yet very discriminating among them. However, the observed $R_{P/p}$ is a more discriminating diagnostic for the polarizing grain population and is not compatible with predictions of dust models, the observations being higher by a factor of about 2.5. These new diagnostics from Planck, including the spectral dependence in the submillimetre, will be important for constraining and understanding the full complexity of the grain models, and for further interpretation of the Planck thermal dust polarization.", "comment": null, "journal": null, "doi": null }, { "version": "v2", "updated": "2015-03-12T06:36:26.000Z" } ], "analyses": { "keywords": [ "interstellar polarization", "planck intermediate results", "polarized thermal emission", "galactic dust", "diffuse interstellar medium" ], "publication": { "doi": "10.1051/0004-6361/201424087", "journal": "Astronomy and Astrophysics", "year": 2015, "month": "Apr", "volume": 576 }, "note": { "typesetting": "TeX", "pages": 0, "language": "en", "license": "arXiv", "status": "editable", "inspire": 1294210, "adsabs": "2015A&A...576A.106P" } } }