Planck intermediate results. XXI. Comparison of polarized thermal emission from Galactic dust at 353 GHz with interstellar polarization in the visible

被引：23

作者：

Ade, P. A. R. ^{[82
]}

Aghanim, N. ^{[56
]}

Alina, D. ^{[11
,87
]}

Aniano, G. ^{[56
]}

Armitage-Caplan, C. ^{[85
]}

Arnaud, M. ^{[69
]}

Ashdown, M. ^{[7
,66
]}

Atrio-Barandela, F. ^{[19
]}

Aumont, J. ^{[56
]}

Baccigalupi, C. ^{[81
]}

Banday, A. J. ^{[11
,87
]}

Barreiro, R. B. ^{[63
]}

Battaner, E. ^{[89
,90
]}

Beichman, C. ^{[12
]}

Benabed, K. ^{[57
,86
]}

Benoit-Levy, A. ^{[25
,57
,89
]}

Bernard, J. -P. ^{[11
,87
]}

Bersanelli, M. ^{[34
,48
]}

Bielewicz, P. ^{[11
,81
,87
]}

Bock, J. J. ^{[12
,64
]}

Bond, J. R. ^{[10
]}

Borrill, J. ^{[14
,83
]}

Bouchet, F. R. ^{[57
,86
]}

Boulanger, F. ^{[56
]}

Burigana, C. ^{[32
,47
]}

Cardoso, J. -F. ^{[1
,57
,70
,71
]}

Catalano, A. ^{[68
,72
]}

Chamballu, A. ^{[16
,56
,69
]}

Chary, R. -R. ^{[55
]}

Chiang, H. C. ^{[8
,28
]}

Christensen, P. R. ^{[78
]}

Colombi, S. ^{[57
,86
]}

Colombo, L. P. L. ^{[24
,64
]}

Combet, C. ^{[72
]}

Couchot, F. ^{[67
]}

Coulais, A. ^{[68
]}

Crill, B. P. ^{[64
,79
]}

Curto, A. ^{[7
,63
]}

Cuttaia, F. ^{[47
]}

Danese, L. ^{[81
]}

Davies, R. D. ^{[65
]}

Davis, R. J. ^{[65
]}

de Bernardis, P. ^{[33
]}

de Rosa, A. ^{[47
]}

de Zotti, G. ^{[44
,81
]}

Delabrouille, J. ^{[1
]}

Desert, F. -X. ^{[52
,53
]}

Dickinson, C. ^{[65
]}

Diego, J. M. ^{[63
]}

Donzelli, S. ^{[48
]}

机构：

[1] Univ Paris Diderot, Observ Paris, CEA,Irfu,Sorbonne Paris Cite, APC,AstroParticule & Cosmol,CNRS,IN2P3, F-75205 Paris, France

[2] Aalto Univ, Metsahovi Radio Observ, Aalto 00076, Finland

[3] Aalto Univ, Dept Radio Sci & Engn, Aalto 00076, Finland

[4] African Inst Math Sci, Cape Town, South Africa

[5] Agenzia Spaziale Italiana, Sci Data Ctr, I-00133 Rome, Italy

[6] Agenzia Spaziale Italiana, I-00133 Rome, Italy

[7] Univ Cambridge, Cavendish Lab, Astrophys Grp, Cambridge CB3 0HE, England

[8] Univ KwaZulu Natal, Sch Math Stat & Comp Sci, Astrophys & Cosmol Res Unit, ZA-4000 Durban, South Africa

[9] ALMA Santiago Cent Off, Atacama Large Millimeter Submillimeter Array, Santiago, Chile

[10] Univ Toronto, CITA, Toronto, ON M55 3H8, Canada

[11] CNRS, IRAP, F-31028 Toulouse 4, France

[12] CALTECH, Pasadena, CA 91125 USA

[13] CEFCA, Teruel 44001, Spain

[14] Univ Calif Berkeley, Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA 94720 USA

[15] CSIC, Madrid, Spain

[16] CEA Saclay, DSM, Irfu, SPP, F-91191 Gif Sur Yvette, France

[17] Tech Univ Denmark, Natl Space Inst, DTU Space, DK-2800 Lyngby, Denmark

[18] Univ Geneva, Dept Phys Theor, CH-1211 Geneva 4, Switzerland

[19] Univ Salamanca, Fac Ciencias, Dept Fis Fundamental, E-37008 Salamanca, Spain

[20] Univ Oviedo, Dept Fis, E-33007 Oviedo, Spain

[21] Univ Toronto, Dept Astron & Astrophys, Toronto, ON, Canada

[22] Radboud Univ Nijmegen, IMAPP, Dept Astrophys, NL-6500 GL Nijmegen, Netherlands

[23] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada

[24] Univ So Calif, Dept Phys & Astron, Dana & David Dornsife Coll Letter Arts & Sci, Los Angeles, CA 90089 USA

[25] UCL, Dept Phys & Astron, London WC1E 6BT, England

[26] Florida State Univ, Dept Phys, Tallahassee, FL 32306 USA

[27] Univ Helsinki, Dept Phys, Helsinki, Finland

[28] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA

[29] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA

[30] Univ Illinois, Dept Phys, Urbana, IL USA

[31] Univ Padua, Dipartimento Fis Astron G Galilei, I-35131 Padua, Italy

[32] Univ Ferrara, Dipartimento Fis & Sci Terra, I-44122 Ferrara, Italy

[33] Univ Roma La Sapienza, Dipartimento Fis, I-00185 Rome, Italy

[34] Univ Milan, Dipartimento Fis, Milan, Italy

[35] Univ Trieste, Dipartimento Fis, Trieste, Italy

[36] Univ Roma Tor Vergata, Dipartimento Fis, I-00173 Rome, Italy

[37] Niels Bohr Inst, Discovery Ctr, DK-2100 Copenhagen, Denmark

[38] Univ La Laguna, Dept Astrofis, Tenerife, Spain

[39] European So Observ, ESO Vitacura, Santiago 19, Chile

[40] European Space Agcy, Planck Sci Off, ESAC, Madrid, Spain

[41] European Space Agcy, Estec, NL-2201 AZ Noordwijk, Netherlands

[42] Aalto Univ, Univ Helsinki, Helsinki Inst Phys, Helsinki, Finland

[43] INAF Osservatorio Astrofis Catania, Catania, Italy

[44] INAF Osservatorio Astron Padova, Padua, Italy

[45] INAF Osservatorio Astron Roma, Monte Porzio Catone, Italy

[46] INAF Osservatorio Astron Trieste, Trieste, Italy

[47] INAF IASF Bologna, Bologna, Italy

[48] INAF IASF Milano, Milan, Italy

[49] Ist Nazl Fis Nucl, Sez Bologna, I-40126 Bologna, Italy

[50] Univ Roma La Sapienza, INFN, Sez Roma 1, I-00185 Rome, Italy

来源：

ASTRONOMY & ASTROPHYSICS | 2015年 / 576卷

基金：

欧洲研究理事会;

关键词：

polarization; dust; extinction; ISM: clouds; ISM: magnetic fields; submillimeter: ISM; PROBE WMAP OBSERVATIONS; LINEAR-POLARIZATION; SUBMILLIMETER POLARIZATION; WAVELENGTH DEPENDENCE; INFRARED POLARIZATION; MU-M; EXTINCTION; SPECTRUM; STARS; ORION;

D O I：

10.1051/0004-6361/201424087

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

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, 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,I- 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 di ff use 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 di ff use 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 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. 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.

引用

页数：17

共 68 条

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Bock, J. J. ;

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Aumont, J. ;

Baccigalupi, C. ;

Banday, A. J. ;

Barreiro, R. B. ;

Bartlett, J. G. ;

Battaner, E. ;

Benabed, K. ;

Benoit, A. ;

Benoit-Levy, A. ;

Bernard, J. -P. ;

Bersanelli, M. ;

Bielewicz, P. ;

Bobin, J. ;

Bock, J. J. ;

Bonaldi, A. ;

Bond, J. R. ;

Borrill, J. ;

Bouchet, F. R. ;

Bridges, M. ;

Bucher, M. ;

Burigana, C. ;

Butler, R. C. ;

Calabrese, E. ;

Cappellini, B. ;

Cardoso, J. -F. ;

Catalano, A. ;

Challinor, A. ;

Chamballu, A. ;

Chary, R. -R. ;

Chen, X. ;

Chiang, H. C. ;

Chiang, L. -Y ;

Christensen, P. R. ;

Church, S. ;

Clements, D. L. ;

Colombi, S. ;

Colombo, L. P. L. ;

Couchot, F. ;

Coulais, A. ;

Crill, B. P. ;

Curto, A. ;

Cuttaia, F. ;

Danese, L. ;

Davies, R. D. .

ASTRONOMY & ASTROPHYSICS, 2014, 571

← 1 2 3 4 5 6 7 →

共 68 条

[1] Planck 2013 results. XI. All-sky model of thermal dust emission [J].

Abergel, A. ;

Ade, P. A. R. ;

Aghanim, N. ;

Alves, M. I. R. ;

Aniano, G. ;

Armitage-Caplan, C. ;

Arnaud, M. ;

Ashdown, M. ;

Atrio-Barandela, F. ;

Aumont, J. ;

Baccigalupi, C. ;

Banday, A. J. ;

Barreiro, R. B. ;

Bartlett, J. G. ;

Battaner, E. ;

Benabed, K. ;

Benoit, A. ;

Benoit-Levy, A. ;

Bernard, J. -P. ;

Bersanelli, M. ;

Bielewicz, P. ;

Bobin, J. ;

Bock, J. J. ;

Bonaldi, A. ;

Bond, J. R. ;

Borrill, J. ;

Bouchet, F. R. ;

Boulanger, F. ;

Bridges, M. ;

Bucher, M. ;

Burigana, C. ;

Butler, R. C. ;

Cardoso, J. -F. ;

Catalano, A. ;

Chamballu, A. ;

Chary, R. -R. ;

Chiang, H. C. ;

Chiang, L. -Y ;

Christensen, P. R. ;

Church, S. ;

Clemens, M. ;

Clements, D. L. ;

Colombi, S. ;

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