Planck early results. XXI. Properties of the interstellar medium in the Galactic plane

被引：58

作者：

Abergel, A. ^{[47
]}

Ade, P. A. R. ^{[71
]}

Aghanim, N. ^{[47
]}

Arnaud, M. ^{[58
]}

Ashdown, M. ^{[5
,56
]}

Aumont, J. ^{[47
]}

Baccigalupi, C. ^{[69
]}

Balbi, A. ^{[28
]}

Banday, A. J. ^{[1
,8
,64
]}

Barreiro, R. B. ^{[53
]}

Bartlett, J. G. ^{[4
,54
]}

Battaner, E. ^{[76
]}

Benabed, K. ^{[48
]}

Benoit, A. ^{[46
]}

Bernard, J-P ^{[1
,8
]}

Bersanelli, M. ^{[25
,41
]}

Bhatia, R. ^{[6
]}

Bock, J. J. ^{[54
]}

Bonaldi, A. ^{[37
]}

Bond, J. R. ^{[7
]}

Borrill, J. ^{[63
,72
]}

Bouchet, F. R. ^{[48
]}

Boulanger, F. ^{[47
]}

Bucher, M. ^{[4
]}

Burigana, C. ^{[40
]}

Cabella, P. ^{[28
]}

Cardoso, J-F ^{[4
,48
,59
,60
]}

Catalano, A. ^{[4
,57
]}

Cayon, L. ^{[18
]}

Challinor, A. ^{[10
,50
,56
]}

Chamballu, A. ^{[44
]}

Chiang, L-Y ^{[49
]}

Chiang, C. ^{[17
]}

Christensen, P. R. ^{[29
]}

Colombi, S. ^{[48
]}

Couchot, F. ^{[62
]}

Coulais, A. ^{[57
]}

Crill, B. P. ^{[54
]}

Cuttaia, F. ^{[40
]}

Dame, T. M. ^{[34
]}

Danese, L. ^{[69
]}

Davies, R. D. ^{[55
]}

Davis, R. J. ^{[55
]}

de Bernardis, P. ^{[24
]}

de Gasperis, G. ^{[28
]}

de Rosa, A. ^{[40
]}

de Zotti, G. ^{[37
,69
]}

Delabrouille, J. ^{[4
]}

Delouis, J-M ^{[48
]}

Desert, F-X ^{[43
]}

机构：

[1] Univ Toulouse, UPS OMP IRAP, F-31028 Toulouse 4, France

[2] Aalto Univ, Metsahovi Radio Observ, Kylmala 02540, Finland

[3] Agenzia Spaziale Italiana Sci Data Ctr, ESRIN, Frascati, Italy

[4] Univ Paris 07, CNRS, UMR7164, Paris, France

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

[6] ALMA Santiago Cent Off, Santiago, Chile

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

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

[9] Univ Oslo, Ctr Math Applicat, Oslo, Norway

[10] Univ Cambridge, Ctr Math Sci, DAMTP, Cambridge CB3 0WA, England

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

[12] Natl Space Inst, DTU Space, Copenhagen, Denmark

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

[14] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H8, Canada

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

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

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

[18] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA

[19] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA

[20] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA

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

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

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

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

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

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

[27] Univ Ferrara, Dipartimento Fis, I-44122 Ferrara, Italy

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

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

[30] Univ La Laguna, Dpto Astrofis, E-38206 Tenerife, Spain

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

[32] European Space Agcy, ESAC, Sci Off, Madrid, Spain

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

[34] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA

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

[36] Osserv Astrofis Catania, INAF, I-95125 Catania, Italy

[37] Osserv Astron Padova, INAF, Padua, Italy

[38] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy

[39] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy

[40] INAF IASF Bologna, Bologna, Italy

[41] INAF IASF Milano, Milan, Italy

[42] Univ Paris 11, INRIA, Rech Informat Lab, F-91405 Orsay, France

[43] Univ Grenoble 1, IPAG, CNRS INSU, UMR 5274, F-38041 Grenoble, France

[44] Univ London Imperial Coll Sci Technol & Med, Astrophys Grp, Blackett Lab, London SW7 2AZ, England

[45] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA

[46] Univ Grenoble 1, Inst Neel, CNRS, F-38041 Grenoble, France

[47] Univ Paris 11, Inst Astrophys Spatiale, CNRS, UMR8617, F-91405 Orsay, France

[48] Univ Paris 06, Inst Astrophys Paris, CNRS UMR7095, Paris, France

[49] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan

[50] Univ Cambridge, Inst Astron, Cambridge CB3 0HA, England

来源：

ASTRONOMY & ASTROPHYSICS | 2011年 / 536卷

关键词：

ISM: general; Galaxy: general; radio continuum: ISM; submillimeter: ISM; infrared: ISM; radiation mechanisms: general; PROBE WMAP OBSERVATIONS; SPINNING DUST EMISSION; GAMMA-RAY EMISSION; MILKY-WAY; INFRARED-EMISSION; EXCESS EMISSION; EXTINCTION; ORIGIN; LIMITS; CLOUD;

D O I：

10.1051/0004-6361/201116455

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Planck has observed the entire sky from 30 GHz to 857 GHz. The observed foreground emission contains contributions from different phases of the interstellar medium (ISM). We have separated the observed Galactic emission into the different gaseous components (atomic, molecular and ionised) in each of a number of Galactocentric rings. This technique provides the necessary information to study dust properties (emissivity, temperature, etc.), as well as other emission mechanisms as a function of Galactic radius. Templates are created for various Galactocentric radii using velocity information from atomic (neutral hydrogen) and molecular ((CO)-C-12) observations. The ionised template is assumed to be traced by free-free emission as observed by WMAP, while 408 MHz emission is used to trace the synchrotron component. Gas emission not traced by the above templates, namely "dark gas", as evidenced using Planck data, is included as an additional template, the first time such a component has been used in this way. These templates are then correlated with each of the Planck frequency bands, as well as with higher frequency data from IRAS and DIRBE along with radio data at 1.4 GHz. The emission per column density of the gas templates allows us to create distinct spectral energy distributions (SEDs) per Galactocentric ring and in each of the gaseous tracers from 1.4 GHz to 25 THz (12 mu m). The resulting SEDs allow us to explore the contribution of various emission mechanisms to the Planck signal. Apart from the thermal dust and free-free emission, we have probed the Galaxy for anomalous (e.g., spinning) dust as well as synchrotron emission. We find the dust opacity in the solar neighbourhood, tau/N-H = 0.92 +/- 0.05x10(-25) cm(2) at 250 mu m, with no significant variation with Galactic radius, even though the dust temperature is seen to vary from over 25 K to under 14 K. Furthermore, we show that anomalous dust emission is present in the atomic, molecular and dark gas phases throughout the Galactic disk. Anomalous emission is not clearly detected in the ionised phase, as free-free emission is seen to dominate. The derived dust propeties associated with the dark gas phase are derived but do not allow us to reveal the nature of this phase. For all environments, the anomalous emission is consistent with rotation from polycyclic aromatic hydrocarbons (PAHs) and, according to our simple model, accounts for (25 +/- 5)% (statistical) of the total emission at 30 GHz.

引用

页数：18

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