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首页> 外文期刊>Astronomy and astrophysics >Interpreting the photometry and spectroscopy of directly imaged planets: a new atmospheric model applied to β Pictoris b and SPHERE observations
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Interpreting the photometry and spectroscopy of directly imaged planets: a new atmospheric model applied to β Pictoris b and SPHERE observations

机译：解释直接成像行星的光度学和光谱学：将新的大气模型应用于βPictoris b和SPHERE观测

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Context. Since the end of 2013 a new generation of instruments optimized to image young giant planets around nearby stars directly is becoming available on 8-m class telescopes, both at Very Large Telescope and Gemini in the southern hemisphere. Beyond the achievement of high contrast and the discovery capability, these instruments are designed to obtain photometric and spectral information to characterize the atmospheres of these planets. Aims. We aim to interpret future photometric and spectral measurements from these instruments, in terms of physical parameters of the planets, with an atmospheric model using a minimal number of assumptions and parameters. Methods. We developed the Exoplanet Radiative-convective Equilibrium Model (Exo-REM) to analyze the photometric and spectroscopic data of directly imaged planets. The input parameters are a planet’s surface gravity (g), effective temperature (Teff), and elemental composition. The model predicts the equilibrium temperature profile and mixing ratio profiles of the most important gases. Opacity sources include the H2-He collision-induced absorption and molecular lines from eight compounds (including CH4 updated with the Exomol line list). Absorption by iron and silicate cloud particles is added above the expected condensation levels with a fixed scale height and a given optical depth at some reference wavelength. Scattering was not included at this stage. Results. We applied Exo-REM to photometric and spectral observations of the planet β Pictoris b obtained in a series of near-infrared filters. We derived Teff = 1550 ± 150 K, log?(g) = 3.5 ± 1, and radius R = 1.76 ± 0.24 RJup (2σ error bars from photometric measurements). These values are comparable to those found in the literature, although with more conservative error bars, consistent with the model accuracy. We were able to reproduce, within error bars, the J- and H-band spectra of β Pictoris b. We finally investigated the precision to which the above parameters can be constrained from SPHERE measurements using different sets of near-infrared filters as well as low-resolution spectroscopy.
机译：上下文。自2013年底以来，优化用于直接对附近恒星周围的年轻巨型行星成像的新一代仪器已在8米级望远镜上使用，这两个望远镜都在甚大望远镜和南半球的双子座上使用。除了获得高对比度和发现能力之外，这些仪器还旨在获得光度和光谱信息，以表征这些行星的大气。目的我们的目标是使用最小数量的假设和参数，通过大气模型，根据行星的物理参数解释这些仪器的未来光度和光谱测量结果。方法。我们开发了系外行星辐射对流平衡模型（Exo-REM），以分析直接成像的行星的光度和光谱数据。输入参数是行星的表面重力（g），有效温度（Teff）和元素组成。该模型预测最重要气体的平衡温度曲线和混合比曲线。不透明度源包括H2-He碰撞诱导的吸收和来自八种化合物的分子线（包括用Exomol线列表更新的CH4）。铁和硅酸盐云颗粒的吸收在固定的标尺高度和某个参考波长处给定的光学深度的预期冷凝水平之上添加。在此阶段不包括散射。结果。我们将Exo-REM应用于通过一系列近红外滤光片获得的βPictoris b行星的光度和光谱观测。我们得出Teff = 1550±150 K，log？（g）= 3.5±1，半径R = 1.76±0.24 RJup（来自光度测量的2σ误差线）。这些值可与文献中的值相比较，尽管具有更保守的误差线，与模型精度一致。我们能够在误差条内复制βPictoris b的J和H谱带。我们最终研究了使用不同组的近红外滤光片以及低分辨率光谱从SPHERE测量中可以将上述参数限制到的精度。

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