2020A&A...641A..12P


C.D.S. - SIMBAD4 rel 1.7 - 2020.11.28CET21:01:43

2020A&A...641A..12P - Astronomy and Astrophysics, volume 641A, 12-12 (2020/9-1)

Planck 2018 results. XII. Galactic astrophysics using polarized dust emission.

PLANCK COLLABORATION, AGHANIM N., AKRAMI Y., ALVES M.I.R., ASHDOWN M., AUMONT J., BACCIGALUPI C., BALLARDINI M., BANDAY A.J., BARREIRO R.B., BARTOLO N., BASAK S., BENABED K., BERNARD J.-P., BERSANELLI M., BIELEWICZ P., BOCK J.J., BOND J.R., BORRILL J., BOUCHET F.R., BOULANGER F., BRACCO A., BUCHER M., BURIGANA C., CALABRESE E., CARDOSO J.-F., CARRON J., CHARY R.-R., CHIANG H.C., COLOMBO L.P.L., COMBET C., CRILL B.P., CUTTAIA F., DE BERNARDIS P., DE ZOTTI G., DELABROUILLE J., DELOUIS J.-M., DI VALENTINO E., DICKINSON C., DIEGO J.M., DORE O., DOUSPIS M., DUCOUT A., DUPAC X., EFSTATHIOU G., ELSNER F., ENSSLIN T.A., ERIKSEN H.K., FALGARONE E., FANTAYE Y., FERNANDEZ-COBOS R., FERRIERE K., FINELLI F., FORASTIERI F., FRAILIS M., FRAISSE A.A., FRANCESCHI E., FROLOV A., GALEOTTA S., GALLI S., GANGA K., GENOVA-SANTOS R.T., GERBINO M., GHOSH T., GONZALEZ-NUEVO J., GORSKI K.M., GRATTON S., GREEN G., GRUPPUSO A., GUDMUNDSSON J.E., GUILLET V., HANDLEY W., HANSEN F.K., HELOU G., HERRANZ D., HIVON E., HUANG Z., JAFFE A.H., JONES W.C., KEIHANEN E., KESKITALO R., KIIVERI K., KIM J., KRACHMALNICOFF N., KUNZ M., KURKI-SUONIO H., LAGACHE G., LAMARRE J.-M., LASENBY A., LATTANZI M., LAWRENCE C.R., LE JEUNE M., LEVRIER F., LIGUORI M., LILJE P.B., LINDHOLM V., LOPEZ-CANIEGO M., LUBIN P.M., MA Y.-Z., MACIAS-PEREZ J.F., MAGGIO G., MAINO D., MANDOLESI N., MANGILLI A., MARCOS-CABALLERO A., MARIS M., MARTIN P.G., MARTINEZ-GONZALEZ E., MATARRESE S., MAURI N., McEWEN J.D., MELCHIORRI A., MENNELLA A., MIGLIACCIO M., MIVILLE-DESCHENES M.-A., MOLINARI D., MONETI A., MONTIER L., MORGANTE G., MOSS A., NATOLI P., PAGANO L., PAOLETTI D., PATANCHON G., PERROTTA F., PETTORINO V., PIACENTINI F., POLASTRI L., POLENTA G., PUGET J.-L., RACHEN J.P., REINECKE M., REMAZEILLES M., RENZI A., RISTORCELLI I., ROCHA G., ROSSET C., ROUDIER G., RUBINO-MARTIN J.A., RUIZ-GRANADOS B., SALVATI L., SANDRI M., SAVELAINEN M., SCOTT D., SIRIGNANO C., SUNYAEV R., SUUR-USKI A.-S., TAUBER J.A., TAVAGNACCO D., TENTI M., TOFFOLATTI L., TOMASI M., TROMBETTI T., VALIVIITA J., VANSYNGEL F., VAN TENT B., VIELVA P., VILLA F., VITTORIO N., WANDELT B.D., WEHUS I.K., ZACCHEI A. and ZONCA A.

Abstract (from CDS):

Observations of the submillimetre emission from Galactic dust, in both total intensity I and polarization, have received tremendous interest thanks to the Planck full-sky maps. In this paper we make use of such full-sky maps of dust polarized emission produced from the third public release of Planck data. As the basis for expanding on astrophysical studies of the polarized thermal emission from Galactic dust, we present full-sky maps of the dust polarization fraction p, polarization angle ψ, and dispersion function of polarization angles S. The joint distribution (one-point statistics) of p and NH confirms that the mean and maximum polarization fractions decrease with increasing NH. The uncertainty on the maximum observed polarization fraction, pmax=22.0–1.4+3.5% at 353GHz and 80' resolution, is dominated by the uncertainty on the Galactic emission zero level in total intensity, in particular towards diffuse lines of sight at high Galactic latitudes. Furthermore, the inverse behaviour between p and S found earlier is seen to be present at high latitudes. This follows the S ∝ p–1 relationship expected from models of the polarized sky (including numerical simulations of magnetohydrodynamical turbulence) that include effects from only the topology of the turbulent magnetic field, but otherwise have uniform alignment and dust properties. Thus, the statistical properties of p, ψ, and S for the most part reflect the structure of the Galactic magnetic field. Nevertheless, we search for potential signatures of varying grain alignment and dust properties. First, we analyse the product map Sxp, looking for residual trends. While the polarization fraction p decreases by a factor of 3-4 between NH=1020cm–2 and NH=2x1022cm–2, out of the Galactic plane, this product Sxp only decreases by about 25%. Because S is independent of the grain alignment efficiency, this demonstrates that the systematic decrease in p with NH is determined mostly by the magnetic-field structure and not by a drop in grain alignment. This systematic trend is observed both in the diffuse interstellar medium (ISM) and in molecular clouds of the Gould Belt. Second, we look for a dependence of polarization properties on the dust temperature, as we would expect from the radiative alignment torque (RAT) theory. We find no systematic trend of Sxp with the dust temperature Td, whether in the diffuse ISM or in the molecular clouds of the Gould Belt. In the diffuse ISM, lines of sight with high polarization fraction p and low polarization angle dispersion S tend, on the contrary, to have colder dust than lines of sight with low p and high S. We also compare the Planck thermal dust polarization with starlight polarization data in the visible at high Galactic latitudes. The agreement in polarization angles is remarkable, and is consistent with what we expect from the noise and the observed dispersion of polarization angles in the visible on the scale of the Planck beam. The two polarization emission-to-extinction ratios, RP/p and RS/V, which primarily characterize dust optical properties, have only a weak dependence on the column density, and converge towards the values previously determined for translucent lines of sight. We also determine an upper limit for the polarization fraction in extinction, pV/E(B-V), of 13% at high Galactic latitude, compatible with the polarization fraction p≃20% observed at 353GHz. Taken together, these results provide strong constraints for models of Galactic dust in diffuse gas.

Abstract Copyright: © Planck Collaboration 2020

Journal keyword(s): polarization - magnetic fields - turbulence - dust - extinction - local insterstellar matter - submillimeter: ISM

Simbad objects: 14

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Number of rows : 14

N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2021
#notes
1 * alf UMi cC* 02 31 49.09456 +89 15 50.7923 3.00 2.62 2.02 1.53 1.22 F8Ib 617 2
2 NAME Eri Bubble HI 03 52 -02.0           ~ 91 0
3 NAME Taurus Complex SFR 04 41.0 +25 52           ~ 3575 0
4 M 1 SNR 05 34 31.94 +22 00 52.2           ~ 5671 4
5 NAME ORI MOL CLOUD MoC 05 56 -01.8           ~ 868 1
6 NAME Rosette Nebula HII 06 31 40 +04 57.8           ~ 451 1
7 NAME Vela C Cld 08 57 -43.2           ~ 127 0
8 NAME Chamaeleon Region SFR 11 55 -78.0           ~ 699 0
9 NAME Musca Cld 12 23 -71.3           ~ 162 0
10 NAME Ophiuchus Molecular Cloud SFR 16 28 06 -24 32.5           ~ 3086 0
11 NAME Gal Center reg 17 45 40.04 -29 00 28.1           ~ 11831 0
12 NAME Aql Rift DNe 18 32 -01.0           ~ 240 1
13 NAME Gould Belt PoG ~ ~           ~ 730 1
14 NAME Local Bubble ISM ~ ~           ~ 709 0

    Equat.    Gal    SGal    Ecl

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2020.11.28-21:01:43

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