ARCADE 2 OBSERVATIONS OF GALACTIC RADIO EMISSION

被引:59
作者
Kogut, A. [1 ]
Fixsen, D. J. [2 ]
Levin, S. M. [3 ]
Limon, M. [4 ]
Lubin, P. M. [5 ]
Mirel, P. [1 ]
Seiffert, M. [4 ]
Singal, J. [6 ]
Villela, T. [7 ]
Wollack, E.
Wuensche, C. A. [7 ]
机构
[1] NASA, Goddard Space Flight Ctr, Wyle Informat Syst, Greenbelt, MD 20771 USA
[2] Univ Maryland, Dept Phys & Astron, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA
[3] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA
[4] Columbia Univ, Columbia Astrophys Lab, New York, NY 10027 USA
[5] Univ Calif Santa Barbara, Dept Phys, Santa Barbara, CA 93106 USA
[6] Kavli Inst Particle Astrophys & Cosmol, SLAC Natl Accelerator Lab, Menlo Pk, CA 94025 USA
[7] Inst Nacl Pesquisas Espaciais, Div Astrophys, BR-12245970 Sao Jose Dos Campos, SP, Brazil
基金
美国国家航空航天局; 美国国家科学基金会;
关键词
cosmic background radiation; radiation mechanisms: non-thermal; radio continuum: ISM; MICROWAVE BACKGROUND-RADIATION; ABSOLUTE SKY BRIGHTNESS; 45-MHZ CONTINUUM SURVEY; FOREGROUND EMISSION; SYNCHROTRON EMISSION; SPECTRAL INDEX; GHZ; MAPS; MHZ; TEMPERATURE;
D O I
10.1088/0004-637X/734/1/4
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
We use absolutely calibrated data from the ARCADE 2 flight in 2006 July to model Galactic emission at frequencies 3, 8, and 10 GHz. The spatial structure in the data is consistent with a superposition of free-free and synchrotron emission. Emission with spatial morphology traced by the Haslam 408 MHz survey has spectral index beta(synch) = -2.5 +/- 0.1, with free-free emission contributing 0.10 +/- 0.01 of the total Galactic plane emission in the lowest ARCADE 2 band at 3.15 GHz. We estimate the total Galactic emission toward the polar caps using either a simple plane-parallel model with csc vertical bar b vertical bar dependence or a model of high-latitude radio emission traced by the COBE/FIRAS map of C II emission. Both methods are consistent with a single power law over the frequency range 22 MHz to 10 GHz, with total Galactic emission toward the north polar cap T-Gal = 10.12 +/- 0.90 K and spectral index beta = -2.55 +/- 0.03 at reference frequency 0.31 GHz. Emission associated with the plane-parallel structure accounts for only 30% of the observed high-latitude sky temperature, with the residual in either a Galactic halo or an isotropic extragalactic background. The well-calibrated ARCADE 2 maps provide a new test for spinning dust emission, based on the integrated intensity of emission from the Galactic plane instead of cross-correlations with the thermal dust spatial morphology. The Galactic plane intensity measured by ARCADE 2 is fainter than predicted by models without spinning dust and is consistent with spinning dust contributing 0.4 +/- 0.1 of the Galactic plane emission at 23 GHz.
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页数:9
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