Planck early results. XX. New light on anomalous microwave emission from spinning dust grains

被引：151

作者：

Ade, P. A. R. ^{[70
]}

Aghanim, N. ^{[46
]}

Arnaud, M. ^{[57
]}

Ashdown, M. ^{[5
,55
]}

Aumont, J. ^{[46
]}

Baccigalupi, C. ^{[68
]}

Balbi, A. ^{[28
]}

Banday, A. J. ^{[8
,63
,75
]}

Barreiro, R. B. ^{[52
]}

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

Battaner, E. ^{[77
]}

Benabed, K. ^{[47
]}

Benoit, A. ^{[45
]}

Bernard, J-P ^{[8
,75
]}

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

Bhatia, R. ^{[6
]}

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

Bonaldi, A. ^{[37
]}

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

Borrill, J. ^{[62
,71
]}

Bouchet, F. R. ^{[47
]}

Boulanger, F. ^{[46
]}

Bucher, M. ^{[4
]}

Burigana, C. ^{[40
]}

Cabella, P. ^{[28
]}

Cappellini, B. ^{[41
]}

Cardoso, J-F ^{[4
,47
,58
,59
]}

Casassus, S. ^{[74
]}

Catalano, A. ^{[4
,56
]}

Cayon, L. ^{[18
]}

Challinor, A. ^{[10
,49
,55
]}

Chamballu, A. ^{[43
]}

Chary, R-R ^{[44
]}

Chen, X. ^{[44
]}

Chiang, L-Y ^{[48
]}

Chiang, C. ^{[17
]}

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

Clements, D. L. ^{[43
]}

Colombi, S. ^{[47
]}

Couchot, F. ^{[61
]}

Coulais, A. ^{[56
]}

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

Cuttaia, F. ^{[40
]}

Danese, L. ^{[68
]}

Davies, R. D. ^{[1
]}

Davis, R. J. ^{[1
]}

de Bernardis, P. ^{[24
]}

de Gasperis, G. ^{[28
]}

de Rosa, A. ^{[40
]}

de Zotti, G. ^{[37
,68
]}

机构：

[1] Univ Manchester, Jodrell Bank Ctr Astrophys, Sch Phys & Astron, Manchester M13 9PL, Lancs, England

[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, Planck Sci Off, Madrid, Spain

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

[34] Haverford Coll, Dept Astron, Haverford, PA 19041 USA

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

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

[45] Univ Grenoble 1, CNRS, Inst Neel, Grenoble, France

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

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

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

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

[50] Univ Oslo, Inst Theoret Astrophys, Oslo, Norway

来源：

ASTRONOMY & ASTROPHYSICS | 2011年 / 536卷

基金：

美国国家航空航天局;

关键词：

ISM: general; Galaxy: general; radiation mechanisms: general; radio continuum: ISM; submillimeter: ISM; PROBE WMAP OBSERVATIONS; PRE-LAUNCH STATUS; POLYCYCLIC AROMATIC-HYDROCARBON; INTERSTELLAR RADIATION-FIELD; PERSEUS MOLECULAR-COMPLEX; CENTIMETER-WAVE CONTINUUM; GALACTIC FOREGROUNDS; BRIGHT SIDE; DARK CLOUD; FULL-SKY;

D O I：

10.1051/0004-6361/201116470

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Anomalous microwave emission (AME) has been observed by numerous experiments in the frequency range similar to 10-60 GHz. Using Planck maps and multi-frequency ancillary data, we have constructed spectra for two known AME regions: the Perseus and rho Ophiuchi molecular clouds. The spectra are well fitted by a combination of free-free radiation, cosmic microwave background, thermal dust, and electric dipole radiation from small spinning dust grains. The spinning dust spectra are the most precisely measured to date, and show the high frequency side clearly for the first time. The spectra have a peak in the range 20-40 GHz and are detected at high significances of 17.1 sigma for Perseus and 8.4 sigma for rho Ophiuchi. In Perseus, spinning dust in the dense molecular gas can account for most of the AME; the low density atomic gas appears to play a minor role. In rho Ophiuchi, the similar to 30 GHz peak is dominated by dense molecular gas, but there is an indication of an extended tail at frequencies 50-100 GHz, which can be accounted for by irradiated low density atomic gas. The dust parameters are consistent with those derived from other measurements. We have also searched the Planck map at 28.5 GHz for candidate AME regions, by subtracting a simple model of the synchrotron, free-free, and thermal dust. We present spectra for two of the candidates; S140 and S235 are bright H II regions that show evidence for AME, and are well fitted by spinning dust models.

引用

页数：17

共 12 条

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