Bibcode
Planck Collaboration; Ade, P. A. R.; Aghanim, N.; Alina, D.; Aniano, G.; Armitage-Caplan, C.; Arnaud, M.; Ashdown, M.; Atrio-Barandela, F.; Aumont, J.; Baccigalupi, C.; Banday, A. J.; Barreiro, R. B.; Battaner, E.; Beichman, C.; Benabed, K.; Benoit-Lévy, A.; Bernard, J.-P.; Bersanelli, M.; Bielewicz, P.; Bock, J. J.; Bond, J. R.; Borrill, J.; Bouchet, F. R.; Boulanger, F.; Burigana, C.; Cardoso, J.-F.; Catalano, A.; Chamballu, A.; Chary, R.-R.; Chiang, H. C.; Christensen, P. R.; Colombi, S.; Colombo, L. P. L.; Combet, C.; Couchot, F.; Coulais, A.; Crill, B. P.; Curto, A.; Cuttaia, F.; Danese, L.; Davies, R. D.; Davis, R. J.; de Bernardis, P.; de Rosa, A.; de Zotti, G.; Delabrouille, J.; Désert, F.-X.; Dickinson, C.; Diego, J. M.; Donzelli, S.; Doré, O.; Douspis, M.; Dunkley, J.; Dupac, X.; Efstathiou, G.; Enßlin, T. A.; Eriksen, H. K.; Falgarone, E.; Fanciullo, L.; Finelli, F.; Forni, O.; Frailis, M.; Fraisse, A. A.; Franceschi, E.; Galeotta, S.; Ganga, K.; Ghosh, T.; Giard, M.; Giraud-Héraud, Y.; González-Nuevo, J.; Górski, K. M.; Gregorio, A.; Gruppuso, A.; Guillet, V.; Hansen, F. K.; Harrison, D. L.; Helou, G.; Hernández-Monteagudo, C.; Hildebrandt, S. R.; Hivon, E.; Hobson, M.; Holmes, W. A.; Hornstrup, A.; Huffenberger, K. M.; Jaffe, A. H.; Jaffe, T. R.; Jones, W. C.; Juvela, M.; Keihänen, E.; Keskitalo, R.; Kisner, T. S.; Kneissl, R.; Knoche, J.; Kunz, M.; Kurki-Suonio, H.; Lagache, G.; Lähteenmäki, A.; Lamarre, J.-M.; Lasenby, A. et al.
Referencia bibliográfica
Astronomy and Astrophysics, Volume 576, id.A106, 17 pp.
Advertised on:
4
2015
Revista
Número de citas
87
Número de citas referidas
75
Descripción
The Planck survey provides unprecedented full-sky coverage of the
submillimetre polarized emission from Galactic dust. In addition to the
information on the direction of the Galactic magnetic field, this also
brings 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, and therefore of the important
dust model parameters, composition, size, and shape. Using ancillary
catalogues of interstellar polarization and extinction of starlight, we
obtain the degree of polarization, pV, and the optical depth
in the V band to the star, τV. Toward these stars we
measure the submillimetre polarized intensity, PS, and total
intensity, IS, in the Planck 353 GHz channel. We compare the
column density measure in the visible, E(B - V), with that inferred from
the Planck product map of the submillimetre dust optical depth and
compare the polarization direction (position angle) in the visible with
that in the submillimetre. 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, RS
/V = (PS/IS) /
(pV/τV) and RP/p =
PS/pV, the latter focusing directly on the
polarization properties of the aligned grain population alone.We find
RS /V = 4.2, with statistical and systematic uncertainties
0.2 and 0.3, respectively, and RP/p = 5.4 MJy
sr-1, with uncertainties 0.2 and 0.3 MJy sr-1,
respectively. Our estimate of RS /V is compatible with
predictions based on a range of polarizing dust models that have been
developed for the diffuse interstellar medium. This estimate provides
new empirical validation of many of the common underlying assumptions of
the models, but is not yet very discriminating among them. However, our
estimate of RP/p is not compatible with predictions, which
are too low by a factor of about 2.5. This more discriminating
diagnostic, RP/p, indicates that changes to the optical
properties in the models of the aligned grain population are required.
These new diagnostics, together with the spectral dependence in the
submillimetre from Planck,will be important for constraining and
understanding the full complexity of the grain models, and for
interpreting the Planck thermal dust polarization and refinement of the
separation of this contamination of the cosmic microwave background.
Appendices are available in electronic form at http://www.aanda.org
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Rafael
Rebolo López