普朗克中间结果。LII。行星通量密度
Planck intermediate results. LII. Planet flux densities
摘要：
通量密度的测量描述了五个行星，火星，木星，土星，天王星和海王星，在六个普朗克高频仪器频带（100-857 GHz），然后这些模型和现有的数据进行比较。在我们的分析中，我们还包括在普朗克低频仪器的三个频率（30，44和70 GHz）下对木星和土星亮度的估计。这些结果提供了对这些行星的内在亮度和亮度随时间变化的限制。大多数行星通量密度的估计受到系统误差的限制，但在许多情况下仍然产生优于1%的测量结果。将普朗克HFI、威尔金森微波各向异性探测器（WMAP）和阿塔卡马宇宙学望远镜（ACT）的数据应用到一个模型中，该模型将土星环对行星总通量密度的贡献结合起来，表明土星环系统的光谱指数$β_\mathrm{ring} = 2.30\pm0.03$在30-1000 GHz频率范围内的最佳拟合值。对于所有五颗行星（不包括木星在353 GHz的观测），普朗克-HFI测量值和采用的模型预测值之间的平均比值分别为0.997、0.997、1.018和1.032（100、143、217和353 GHz）。因此，模型对行星热力学温度的预测与普朗克HFI探测器在大约3%水平上的绝对校准是一致的。我们将我们的测量结果与最近发表的宇宙微波背景实验结果进行了比较。特别是，我们观察到，普朗克HFI和WMAP测量的通量密度同意在2%以内。这些结果允许在毫米波长范围内进行实验，以与普朗克交叉校准，并改进行星科学中使用的辐射传输模型。
英文摘要：
Measurements of flux density are described for five planets, Mars, Jupiter, Saturn, Uranus, and Neptune, across the six Planck High Frequency Instrument frequency bands (100-857 GHz) and these are then compared with models and existing data. In our analysis, we have also included estimates of the brightness of Jupiter and Saturn at the three frequencies of the Planck Low Frequency Instrument (30, 44, and 70 GHz). The results provide constraints on the intrinsic brightness and the brightness time-variability of these planets. The majority of the planet flux density estimates are limited by systematic errors, but still yield better than 1% measurements in many cases. Applying data from Planck HFI, the Wilkinson Microwave Anisotropy Probe (WMAP), and the Atacama Cosmology Telescope (ACT) to a model that incorporates contributions from Saturn's rings to the planet's total flux density suggests a best fit value for the spectral index of Saturn's ring system of $β_\mathrm{ring} = 2.30\pm0.03$ over the 30-1000 GHz frequency range. The average ratio between the Planck-HFI measurements and the adopted model predictions for all five planets (excluding Jupiter observations for 353 GHz) is 0.997, 0.997, 1.018, and 1.032 for 100, 143, 217, and 353 GHz, respectively. Model predictions for planet thermodynamic temperatures are therefore consistent with the absolute calibration of Planck-HFI detectors at about the three-percent-level. We compare our measurements with published results from recent cosmic microwave background experiments. In particular, we observe that the flux densities measured by Planck HFI and WMAP agree to within 2%. These results allow experiments operating in the mm-wavelength range to cross-calibrate against Planck and improve models of radiative transport used in planetary science.
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