Planck early results. XVII. Origin of the submillimetre excess dust emission in the Magellanic Clouds

被引:126
作者
Ade, P. A. R. [73 ]
Aghanim, N. [48 ]
Arnaud, M. [59 ]
Ashdown, M. [5 ,57 ]
Aumont, J. [48 ]
Baccigalupi, C. [71 ]
Balbi, A. [30 ]
Banday, A. J. [1 ,8 ,65 ]
Barreiro, R. B. [54 ]
Bartlett, J. G. [4 ,55 ]
Battaner, E. [78 ]
Benabed, K. [49 ]
Benoit, A. [47 ]
Bernard, J. -P. [1 ,8 ]
Bersanelli, M. [27 ,42 ]
Bhatia, R. [6 ]
Bock, J. J. [55 ]
Bonaldi, A. [38 ]
Bond, J. R. [7 ]
Borrill, J. [64 ,74 ]
Bot, C. [69 ]
Bouchet, F. R. [49 ]
Boulanger, F. [48 ]
Bucher, M. [4 ]
Burigana, C. [41 ]
Cabella, P. [30 ]
Cardoso, J. -F. [4 ,49 ,60 ,61 ]
Catalano, A. [4 ,58 ]
Cayon, L. [20 ]
Challinor, A. [9 ,51 ,57 ]
Chamballu, A. [45 ]
Chiang, L. -Y [50 ]
Chiang, C. [19 ]
Christensen, P. R. [31 ,68 ]
Clements, D. L. [45 ]
Colombi, S. [49 ]
Couchot, F. [63 ]
Coulais, A. [58 ]
Crill, B. P. [55 ]
Cuttaia, F. [41 ]
Danese, L. [71 ]
Davies, R. D. [56 ]
Davis, R. J. [56 ]
de Bernardis, P. [26 ]
de Gasperis, G. [30 ]
de Rosa, A. [41 ]
de Zotti, G. [38 ,71 ]
Delabrouille, J. [4 ]
Delouis, J. -M. [49 ]
Desert, F. -X. [44 ]
机构
[1] Univ Toulouse, UPS OMP, IRAP, F-31028 Toulouse 4, France
[2] Aalto Univ Metsahovi Radio Observ, Kylmala 02540, Finland
[3] ESRIN, Agenzia Spaziale Italiana Sci Data Ctr, Frascati, Italy
[4] Univ Paris 07, CNRS UMR7164, Paris, France
[5] Univ Cambridge, Cavendish Lab, Astrophys Grp, 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 Cambridge, DAMTP, Ctr Math Sci, Cambridge CB3 0WA, England
[10] CEA Saclay, DSM Irfu SPP, F-91191 Gif Sur Yvette, France
[11] Natl Space Inst, DTU Space, Copenhagen, Denmark
[12] Univ Oviedo, Dept Fis, E-33007 Oviedo, Spain
[13] Univ Toronto, Dept Astron & Astrophys, Toronto, ON M5S 3H8, Canada
[14] Tokyo Gakugei Univ, Dept Astron & Earth Sci, Tokyo 1848501, Japan
[15] Osaka Prefecture Univ, Grad Sch Sci, Dept Phys Sci, Naka Ku, Sakai, Osaka 5998531, Japan
[16] Univ British Columbia, Dept Phys & Astron, Vancouver, BC V5Z 1M9, Canada
[17] Univ Helsinki, Dept Phys, Helsinki, Finland
[18] Nagoya Univ, Dept Phys, Chikusa Ku, Nagoya, Aichi 4648602, Japan
[19] Princeton Univ, Dept Phys, Princeton, NJ 08544 USA
[20] Purdue Univ, Dept Phys, W Lafayette, IN 47907 USA
[21] Univ Calif Berkeley, Dept Phys, Berkeley, CA 94720 USA
[22] Univ Calif Davis, Dept Phys, Davis, CA 95616 USA
[23] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA
[24] Univ Illinois, Dept Phys, Urbana, IL 61801 USA
[25] Univ Padua, Dipartimento Fis G Galilei, I-35131 Padua, Italy
[26] Univ Roma La Sapienza, Dipartimento Fis, Rome, Italy
[27] Univ Milan, Dipartimento Fis, Milan, Italy
[28] Univ Trieste, Dipartimento Fis, Trieste, Italy
[29] Univ Ferrara, Dipartimento Fis, I-44122 Ferrara, Italy
[30] Univ Roma Tor Vergata, Dipartimento Fis, I-00173 Rome, Italy
[31] Niels Bohr Inst, Discovery Ctr, DK-2100 Copenhagen, Denmark
[32] Univ La Laguna, Dpto Astrofis, E-38206 Tenerife, Spain
[33] European So Observ, ESO Vitacura, Santiago 19, Chile
[34] European Space Agcy, ESAC, Planck Sci Off, Madrid, Spain
[35] European Space Agcy, Estec, NL-2201 AZ Noordwijk, Netherlands
[36] Aalto Univ, Univ Helsinki, Helsinki Inst Phys, Helsinki, Finland
[37] Osserv Astrofis Catania, INAF, I-95125 Catania, Italy
[38] Osserv Astron Padova, INAF, Padua, Italy
[39] Osserv Astron Roma, INAF, I-00040 Monte Porzio Catone, Italy
[40] Osserv Astron Trieste, INAF, I-34131 Trieste, Italy
[41] INAF IASF Bologna, Bologna, Italy
[42] INAF IASF Milano, Milan, Italy
[43] Univ Paris 11, INRIA, Rech Informat Lab, F-91405 Orsay, France
[44] Univ Grenoble 1, IPAG, CNRS INSU, UMR 5274, F-38041 Grenoble, France
[45] Univ London Imperial Coll Sci Technol & Med, Blackett Lab, Astrophys Grp, London SW7 2AZ, England
[46] CALTECH, Infrared Proc & Anal Ctr, Pasadena, CA 91125 USA
[47] Univ Grenoble 1, CNRS, Inst Neel, Grenoble, France
[48] Univ Paris 11, Inst Astrophys Spatiale, CNRS UMR8617, Orsay, France
[49] Univ Paris 06, Inst Astrophys Paris, CNRS UMR7095, Paris, France
[50] Acad Sinica, Inst Astron & Astrophys, Taipei 115, Taiwan
关键词
Magellanic Clouds; dust; extinction; ISM: structure; galaxies: ISM; infrared: galaxies; submillimeter: galaxies; HERSCHEL PHOTOMETRIC-OBSERVATIONS; SPECTRAL ENERGY-DISTRIBUTION; PROBE WMAP OBSERVATIONS; GIANT MOLECULAR CLOUDS; FORMING DWARF GALAXIES; SPITZER SURVEY; APERTURE SYNTHESIS; INFRARED-EMISSION; CENTIMETER EXCESS; INTERSTELLAR DUST;
D O I
10.1051/0004-6361/201116473
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
The integrated spectral energy distributions (SED) of the Large Magellanic Cloud (LMC) and Small Magellanic Cloud (SMC) appear significantly flatter than expected from dust models based on their far-infrared and radio emission. The still unexplained origin of this millimetre excess is investigated here using the Planck data. The integrated SED of the two galaxies before subtraction of the foreground (Milky Way) and background (CMB fluctuations) emission are in good agreement with previous determinations, confirming the presence of the millimetre excess. In the context of this preliminary analysis we do not propose a full multi-component fitting of the data, but instead subtract contributions unrelated to the galaxies and to dust emission. The background CMB contribution is subtracted using an internal linear combination (ILC) method performed locally around the galaxies. The foreground emission from the Milky Way is subtracted as a Galactic Hi template, and the dust emissivity is derived in a region surrounding the two galaxies and dominated by Milky Way emission. After subtraction, the remaining emission of both galaxies correlates closely with the atomic and molecular gas emission of the LMC and SMC. The millimetre excess in the LMC can be explained by CMB fluctuations, but a significant excess is still present in the SMC SED. The Planck and IRAS-IRIS data at 100 mu m are combined to produce thermal dust temperature and optical depth maps of the two galaxies. The LMC temperature map shows the presence of a warm inner arm already found with the Spitzer data, but which also shows the existence of a previously unidentified cold outer arm. Several cold regions are found along this arm, some of which are associated with known molecular clouds. The dust optical depth maps are used to constrain the thermal dust emissivity power-law index (beta). The average spectral index is found to be consistent with beta = 1.5 and beta = 1.2 below 500 mu m for the LMC and SMC respectively, significantly flatter than the values observed in the Milky Way. Also, there is evidence in the SMC of a further flattening of the SED in the sub-mm, unlike for the LMC where the SED remains consistent with beta = 1.5. The spatial distribution of the millimetre dust excess in the SMC follows the gas and thermal dust distribution. Different models are explored in order to fit the dust emission in the SMC. It is concluded that the millimetre excess is unlikely to be caused by very cold dust emission and that it could be due to a combination of spinning dust emission and thermal dust emission by more amorphous dust grains than those present in our Galaxy.
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页数:17
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