Planck intermediate results IX. Detection of the Galactic haze with Planck

被引：103

作者：

Ade, P. A. R. ^{[83
]}

Aghanim, N. ^{[57
]}

Arnaud, M. ^{[71
]}

Ashdown, M. ^{[6
,67
]}

Atrio-Barandela, F. ^{[17
]}

Aumont, J. ^{[57
]}

Baccigalupi, C. ^{[82
]}

Balbi, A. ^{[34
]}

Banday, A. J. ^{[8
,88
]}

Barreiro, R. B. ^{[64
]}

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

Battaner, E. ^{[89
]}

Benabed, K. ^{[58
,86
]}

Benoit, A. ^{[55
]}

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

Bersanelli, M. ^{[32
,47
]}

Bonaldi, A. ^{[66
]}

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

Borrill, J. ^{[12
,84
]}

Bouchet, F. R. ^{[58
,86
]}

Burigana, C. ^{[30
,46
]}

Cabella, P. ^{[35
]}

Cardoso, J. -F. ^{[1
,58
,72
,73
]}

Catalano, A. ^{[70
,74
]}

Cayon, L. ^{[28
]}

Chary, R. -R. ^{[54
]}

Chiang, L. -Y. ^{[60
]}

Christensen, P. R. ^{[36
,79
]}

Clements, D. L. ^{[53
]}

Colombo, L. P. L. ^{[21
]}

Coulais, A. ^{[70
]}

Crill, B. P. ^{[80
]}

Cuttaia, F. ^{[46
]}

Danese, L. ^{[82
]}

D'Arcangelo, O. ^{[65
]}

Davis, R. J. ^{[66
]}

de Bernardis, P. ^{[31
]}

de Gasperis, G. ^{[34
]}

de Rosa, A. ^{[46
]}

de Zotti, G. ^{[44
,82
]}

Delabrouille, J. ^{[1
]}

Dickinson, C. ^{[66
]}

Diego, J. M. ^{[64
]}

Dobler, G. ^{[68
]}

Dole, H. ^{[56
,57
]}

Donzelli, S. ^{[47
]}

Dore, O. ^{[9
]}

Doerl, U. ^{[77
]}

Douspis, M. ^{[57
]}

Dupac, X. ^{[38
]}

机构：

[1] Univ Paris Diderot, Sorbonne Paris Cite, APC, CNRS IN2P3,CEA Irfu,Observ Paris, F-75205 Paris 13, France

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

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

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

[5] Agenzia Spaziale Italiana, Rome, Italy

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

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

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

[9] CALTECH, Pasadena, CA 91125 USA

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

[11] CEFCA, Teruel 44001, Spain

[12] Lawrence Berkeley Natl Lab, Computat Cosmol Ctr, Berkeley, CA USA

[13] CSIC, Madrid, Spain

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

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

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

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

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

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

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

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

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

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

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

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

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

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

[28] Purdue Univ, Dept Stat, W Lafayette, IN 47907 USA

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

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

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

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

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

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

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

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

[37] ULL, Dpto Astrofis, Tenerife 38206, Spain

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

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

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

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

[42] INAF Osserv Astrofis Catania, Catania, Italy

[43] INAF Osserv Astron Roma, Monte Porzio Catone, Italy

[44] INAF Osserv Astron Trieste, Trieste, Italy

[45] INAF Ist Radioastron, I-40129 Bologna, Italy

[46] INAF IASF Bologna, Bologna, Italy

[47] INAF IASF Milano, Milan, Italy

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

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

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

来源：

ASTRONOMY & ASTROPHYSICS | 2013年 / 554卷

基金：

美国国家航空航天局;

关键词：

Galaxy: nucleus; ISM: structure; ISM: bubbles; radio continuum: ISM; PROBE WMAP OBSERVATIONS; PRE-LAUNCH STATUS; BAYESIAN COMPONENT SEPARATION; INTERSTELLAR-MEDIUM EMISSION; SPINNING DUST; POWER SPECTRUM; MICROWAVE; RADIATION; TEMPLATE; MAPS;

D O I：

10.1051/0004-6361/201220271

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Using precise full-sky observations from Planck, and applying several methods of component separation, we identify and characterise the emission from the Galactic "haze" at microwave wavelengths. The haze is a distinct component of diffuse Galactic emission, roughly centered on the Galactic centre, and extends to vertical bar b vertical bar similar to 35-50 degrees in Galactic latitude and vertical bar l vertical bar similar to 15-20 degrees in longitude. By combining the Planck data with observations from the Wilkinson Microwave Anisotropy Probe, we were able to determine the spectrum of this emission to high accuracy, unhindered by the strong systematic biases present in previous analyses. The derived spectrum is consistent with power-law emission with a spectral index of -2.56 +/- 0.05, thus excluding free-free emission as the source and instead favouring hard-spectrum synchrotron radiation from an electron population with a spectrum (number density per energy) dN/dE proportional to E-2.1. At Galactic latitudes vertical bar b vertical bar < 30 degrees, the microwave haze morphology is consistent with that of the Fermi gamma-ray "haze" or "bubbles", while at b similar to -50 degrees we have identified an edge in the microwave haze that is spatially coincident with the edge in the gamma-ray bubbles. Taken together, this indicates that we have a multi-wavelength view of a distinct component of our Galaxy. Given both the very hard spectrum and the extended nature of the emission, it is highly unlikely that the haze electrons result from supernova shocks in the Galactic disk. Instead, a new astrophysical mechanism for cosmic-ray acceleration in the inner Galaxy is implied.

引用

页数：15

共 69 条

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