Planck intermediate results. XIV. Dust emission at millimetre wavelengths in the Galactic plane

被引：38

作者：

Ade, P. A. R. ^{[80
]}

Aghanim, N. ^{[55
]}

Alves, M. I. R. ^{[55
]}

Arnaud, M. ^{[68
]}

Ashdown, M. ^{[7
,65
]}

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

Aumont, J. ^{[55
]}

Baccigalupi, C. ^{[79
]}

Banday, A. J. ^{[11
,84
]}

Barreiro, R. B. ^{[62
]}

Bartlett, J. G. ^{[1
,63
]}

Battaner, E. ^{[86
]}

Benabed, K. ^{[56
,83
]}

Benoit-Levy, A. ^{[25
,56
,83
]}

Bernard, J. -P. ^{[11
,84
]}

Bersanelli, M. ^{[33
,46
]}

Bielewicz, P. ^{[11
,79
,84
]}

Bobin, J. ^{[68
]}

Bonaldi, A. ^{[64
]}

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

Borrill, J. ^{[14
,81
]}

Bouchet, F. R. ^{[56
,83
]}

Boulanger, F. ^{[55
]}

Bucher, M. ^{[1
]}

Burigana, C. ^{[31
,45
]}

Butler, R. C. ^{[45
]}

Cardoso, J. -F. ^{[1
,56
,69
,70
]}

Catalano, A. ^{[67
,71
]}

Chamballu, A. ^{[16
,55
,68
]}

Chiang, H. C. ^{[8
,27
]}

Chiang, L. -Y. ^{[58
]}

Christensen, P. R. ^{[36
,77
]}

Clements, D. L. ^{[52
]}

Colombi, S. ^{[56
,83
]}

Colombo, L. P. L. ^{[24
,63
]}

Couchot, F. ^{[66
]}

Crill, B. P. ^{[12
,63
]}

Curto, A. ^{[7
,62
]}

Cuttaia, F. ^{[45
]}

Danese, L. ^{[79
]}

Davies, R. D. ^{[64
]}

Davis, R. J. ^{[64
]}

de Bernardis, P. ^{[32
]}

de Rosa, A. ^{[45
]}

de Zotti, G. ^{[42
,79
]}

Delabrouille, J. ^{[1
]}

Dickinson, C. ^{[64
]}

Diego, J. M. ^{[62
]}

Dole, H. ^{[54
,55
]}

Donzelli, S. ^{[46
]}

机构：

[1] Univ Paris Diderot, CNRS IN2P3, CEA Irfu, Observ Paris,Sorbonne Paris Cite,APC, F-75205 Paris 13, 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, ZA-7701 Rondebosch, South Africa

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

[6] Agenzia Spaziale Italiana, I-00198 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 0355, Chile

[10] Univ Toronto, CITA, Toronto, ON M5S 3H8, Canada

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

[12] CALTECH, Pasadena, CA 91125 USA

[13] Ctr Estudios Fis Cosmos Aragon, Teruel 44001, Spain

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

[15] CSIC, Madrid 28037, 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] Radboud Univ Nijmegen, Dept Astrophys, IMAPP, NL-6500 GL Nijmegen, Netherlands

[22] Univ Calif Berkeley, Dept Elect Engn & Comp Sci, Berkeley, CA 94720 USA

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

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

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

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

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

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

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

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

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

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

[33] Univ Milan, Dipartimento Fis, I-20133 Milan, Italy

[34] Univ Trieste, Dipartmento Fis, I-34127 Trieste, Italy

[35] Univ Roma Tor Vergata, Dipartimento Fis, I-00133 Rome, Italy

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

[37] Univ La Laguna, Dept Astrofis, E-38206 Tenerife, Spain

[38] ESO Vitacura, European So Observ, Santiago 19001, Chile

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

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

[41] Aalto Univ, Univ Helsinki, Helsinki Inst Phys, FIN-00014 Helsinki, Finland

[42] INAF Osservatorio Astron Padova, I-35122 Padua, Italy

[43] INAF Osservatorio Astron Roma, I-00040 Monte Porzio Catone, Italy

[44] INAF Osservatorio Astron Trieste, I-34143 Trieste, Italy

[45] INAF IASE Bologna, I-40129 Bologna, Italy

[46] INAF IASF Milano, I-20133 Milan, Italy

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

[48] Univ Roma La Sapienza, Ist Nazl Fis Nucl, Sez Roma 1, I-00185 Rome, Italy

[49] Natl Inst Nucl Phys, I-34127 Trieste, Italy

[50] Univ Grenoble 1, CNRS INSU, UMR 5274, Inst Planetol & Astrophys Grenoble, F-38041 Grenoble, France

来源：

ASTRONOMY & ASTROPHYSICS | 2014年 / 564卷

基金：

欧洲研究理事会;

关键词：

ISM: general; Galaxy: general; radiation mechanisms: general; radio continuum: ISM; submillimeter: ISM; PRE-LAUNCH STATUS; SPECTRAL ENERGY-DISTRIBUTIONS; MU-M; TEMPERATURE-DEPENDENCE; SUBMILLIMETER EXCESS; MICROWAVE EMISSION; INTERSTELLAR DUST; MODEL; HERSCHEL; INDEX;

D O I：

10.1051/0004-6361/201322367

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We use Planck HFI data combined with ancillary radio data to study the emissivity index of the interstellar dust emission in the frequency range 100-353 GHz, or 3-0.8 mm, in the Galactic plane. We analyse the region l = 20 degrees-44 degrees and vertical bar b vertical bar <= 4 degrees where the free-free emission can be estimated from radio recombination line data. We fit the spectra at each sky pixel with a modified blackbody model and two opacity spectral indices, beta(mm) and beta(FIR), below and above 353 GHz, respectively. We find that beta(mm) is smaller than beta(FIR), and we detect a correlation between this low frequency power-law index and the dust optical depth at 353 GHz, tau(353). The opacity spectral index beta(mm) increases from about 1.54 in the more diffuse regions of the Galactic disk, vertical bar b vertical bar = 3 degrees-4 degrees and tau(353) similar to 5 x 10(-5), to about 1.66 in the densest regions with an optical depth of more than one order of magnitude higher. We associate this correlation with an evolution of the dust emissivity related to the fraction of molecular gas along the line of sight. This translates into beta(mm) similar to 1.54 for a medium that is mostly atomic and beta(mm) similar to 1.66 when the medium is dominated by molecular gas. We find that both the two-level system model and magnetic dipole emission by ferromagnetic particles can explain the results. These results improve our understanding of the physics of interstellar dust and lead towards a complete model of the dust spectrum of the Milky Way from far-infrared to millimetre wavelengths.

引用

页数：13

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