Impact of Atmospheric Transmittance and NLTE Correction on Simulation of High Spectral Infrared Atmospheric Sounder onboard FY-3E

大气透射率和NLTE订正对FY-3E红外高光谱大气探测模拟的影响

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Supported by the Startup Project of Donghai Laboratory (DH-2023QD0002), National Key Research and Development Program of China (2021YFB3900400), and Hunan Provincial Natural Science Foundation of China (2021JC0009).
DOI: 10.1007/s13351-024-3121-2

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    Abstract

  • Abstract

    With the launch of the first civilian early-morning orbit satellite Fengyun-3E (FY-3E), higher demands are placed on the accuracy of radiative transfer simulations for hyperspectral infrared data. Therefore, several key issues are investigated in the paper. First, the accuracy of the fast atmospheric transmittance model implemented in the Advanced Research and Modeling System (ARMS) has been evaluated with both the line-by-line radiative transfer model (LBLRTM) and the actual satellite observations. The results indicate that the biases are generally less than 0.25 K when compared to the LBLRTM, while below 1.0 K for the majority of the channels when compared to the observations. However, during both comparisons, significant biases are observed in certain channels. The accuracy of Hyperspectral Infrared Atmospheric Sounder-II (HIRAS-II) onboard FY-3E is comparable to, and even superior to that of the Cross-track Infrared Sounder (CrIS) onboard NOAA-20. Furthermore, apodization is a crucial step in the processing of hyperspectral data in that the apodization function is utilized as the instrument channel spectral response function to produce the satellite channel-averaged transmittance. To further explore the difference between the apodized and unapodized simulations, Sinc function is adopted in the fast transmittance model. It is found that the use of Sinc function can make the simulations fit the original satellite observations better. When simulating with apodized observations, the use of Sinc function exhibits larger deviations compared to the Hamming function. Moreover, a correction module is applied to minimize the impact of Non-Local Thermodynamic Equilibrium (NLTE) in the shortwave infrared band. It is verified that the implementation of the NLTE correction model leads to a significant reduction in the bias between the simulation and observation for this band.

    摘要

    针对首颗民用晨昏轨道卫星FY-3E红外高光谱大气探测，研究了影响卫星观测模拟的几个关键问题。建立快速大气透过率模型，并与逐线辐射传输模式LBLRTM和实际卫星观测比较，评估模型的精度。通过hamming和Sinc函数进一步探讨了切趾和非切趾模拟之间的差异，构建减少非局部热力学平衡NLTE效应的订正模块。与LBLRTM相比，模型偏差一般小于0.25K；与观测结果相比，大多数通道的偏差都低于1.0K。FY-3E红外高光谱大气探测器HIRAS-II的精度相当甚至优于NOAA-20跨轨道红外探测器CrIS。使用Sinc函数可以使模拟更好地拟合原始卫星观测，和使用hamming函数模拟与切趾观测的拟合相比，前者的偏差更大一些。NLTE订正显著降低了短波红外波段卫星模拟和实际观测之间的偏差。本研究为FY-3E红外高光谱大气探测的应用提供了技术基础和支持。

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    Fig.  1.   Illustrations of the apodized and unapodized spectral response functions.

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    Fig.  2.   Scheme of HIRAS-II for the clear-sky filtering process at 0700 UTC 15 March 2022.

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    Fig.  3.   Bias and std of brightness temperature simulated between the fast transmittance model implemented in ARMS and LBLRTM.

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    Fig.  4.   Bias between simulation and satellite observation for both FY-3E HIRAS-II and NOAA-20 CrIS on 15 March 2022.

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    Fig.  5.   As in Fig. 4, but for the std.

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    Fig.  6.   Bias of the brightness temperature observation unapodized and simulated with and without apodization of HIRAS-II on 15 March 2022, respectively.

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    Fig.  7.   The difference between the simulated brightness temperature with and without apodization of HIRAS-II on 15 March 2022.

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    Fig.  8.   (a) Bias and (b) std between the brightness temperature simulation of ARMS with NLTE correction module and LBLRTM performed on six solar zenith angles in the 2200–2400-cm−1 SW band. The labels A1–A6 are corresponding to solar zenith angle with the values of 0.0, 40.0, 60.0, 80.0, 85.0, and 90.0.

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    Fig.  9.   (a) Bias and (b) std between observed and simulated brightness temperature in the SW band for 4 cases of HIRAS-II on 15 March 2022.

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    Fig.  10.   (a) Brightness temperature difference between 667.5 and 2336.25 cm−1, (b) OMB distribution of the LTE model, (c) OMB distribution of the fast NLTE model, and (d) solar zenith angle of HIRAS-II from 0000 to 1200 UTC 15 March 2022.

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