We assess broadband color filters for the two fast cameras on the PLAnetary Transits and Oscillations (PLATO) of stars space mission with respect to exoplanetary atmospheric characterization. We focus on Ultra Hot Jupiters and Hot Jupiters placed 25pc and 100pc away from the Earth and low mass low density planets placed 10pc and 25pc away. Our analysis takes as input literature values for the difference in transit depth between the broadband lower (500 to 675nm) wavelength interval (hereafter referred to as blue) and the upper (675-1125nm) broadband wavelength interval (hereafter referred to as red) for transmission, occultation and phase curve analyses. Planets orbiting main sequence central stars with stellar classes F, G, K and M are investigated. We calculate the signal-to-noise ratio with respect to photon and instrument noise for detecting the difference in transit depth between the two spectral intervals. Results suggest that bulk atmospheric composition and planetary geometric albedos could be detected for (Ultra) Hot Jupiters up to about 100pc (about 25pc) with strong (moderate) Rayleigh extinction. Phase curve information could be extracted for Ultra Hot Jupiters orbiting K and G dwarf stars up to 25pc away. For low mass low density planets, basic atmospheric types (primary and water-dominated) and the presence of sub-micron hazes in the upper atmosphere could be distinguished for up to a handful of cases up to about 10pc.

中文翻译：

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在行星凌日和恒星振荡 (PLATO) 任务中通过宽带滤色器进行大气表征

我们针对系外行星大气特征评估了星际凌日和振荡 (PLATO) 太空任务中两个快速相机的宽带滤色器。我们专注于距离地球 25 pc 和 100 pc 的超热木星和热木星，以及距离地球 10 pc 和 25 pc 的低质量低密度行星。我们的分析将宽带较低（500 至 675nm）波长间隔（以下称为蓝色）和较高（675-1125nm）宽带波长间隔（以下称为红色）之间的传输深度差异作为输入文献值传输、掩星和相位曲线分析。研究了围绕主序带中心恒星运行的行星，其恒星等级为 F、G、K 和 M。我们计算关于光子和仪器噪声的信噪比，以检测两个光谱区间之间的传输深度差异。结果表明，可以检测到（超）热木星的大量大气成分和行星几何反照率，高达约 100pc（约 25pc），具有强（中度）瑞利消光。可以提取围绕 K 和 G 矮星运行的超热木星的相位曲线信息，距离最远可达 25 pc。对于低质量低密度行星，基本的大气类型（主要和水占主导地位）和高层大气中亚微米雾霾的存在可以区分多达约 10% 的少数情况。结果表明，可以检测到（超）热木星的大量大气成分和行星几何反照率，高达约 100pc（约 25pc），具有强（中度）瑞利消光。可以提取围绕 K 和 G 矮星运行的超热木星的相位曲线信息，距离最远可达 25 pc。对于低质量低密度行星，基本的大气类型（主要和水占主导地位）和高层大气中亚微米雾霾的存在可以区分多达约 10% 的少数情况。结果表明，可以检测到（超）热木星的大量大气成分和行星几何反照率，高达约 100pc（约 25pc），具有强（中度）瑞利消光。可以提取围绕 K 和 G 矮星运行的超热木星的相位曲线信息，距离最远可达 25 pc。对于低质量低密度行星，基本的大气类型（主要和水占主导地位）和高层大气中亚微米雾霾的存在可以区分多达约 10% 的少数情况。