论文标题
热型外球星的大气层通过过境光谱（心）IV解决。黄蜂-121 B的高分辨率传输光谱中原子和分子的光谱清单
Hot Exoplanet Atmospheres Resolved with Transit Spectroscopy (HEARTS) IV. A spectral inventory of atoms and molecules in the high-resolution transmission spectrum of WASP-121 b
论文作者
论文摘要
目的：我们调查WASP-121 B的传输光谱在高光谱分辨率下通过金属和分子吸收线路，并详细介绍了使用HST/STIS和WFC3观察到的光学传输光谱的现有解释。方法：我们使用互相关技术和直接差异光谱法来搜索使用HARPS光谱仪获得的高分辨率过境光谱中的钠和其他中性和电离原子，TIO，VO和SH。我们将化学和静水平衡的模型注入不同的温度和组成，以实现模型比较，并采用两种自举方法来测试我们检测的鲁棒性。结果：我们检测到中性MG，Na，Ca，Cr，Fe，Ni和V，我们预测它们的平衡状态与大量的VO相平衡，支持HST/WFC3的早期观察结果。 Ti和Tio的非检测支持以下假设：Ti通过冷陷阱机制耗尽了，如文献中所提出的那样。原子线深度被静水模型所预测的1.5至8倍，证实了最近的发现大气已经扩展。我们预测存在大量浓度的气相TIO $ _2 $，vo $ $ _2 $和TIS，这可能是热木星气氛中光学和NIR波长的重要吸收剂，但目前尚无准确的线列表数据。我们没有发现SH吸收的证据，发现膨胀的原子线可以可能解释使用HST/STIS在NUV中观察到的传输光谱的斜率。 Na d线显着扩大，并显示出其各自的15个标度高度的差异，这是等温静水压理论的预期。
Aims: We survey the transmission spectrum of WASP-121 b for line-absorption by metals and molecules at high spectral resolution, and elaborate on existing interpretations of the optical transmission spectrum observed with HST/STIS and WFC3. Methods: We use the cross-correlation technique and direct differential spectroscopy to search for sodium and other neutral and ionised atoms, TiO, VO and SH in high-resolution transit spectra obtained with the HARPS spectrograph. We inject models assuming chemical and hydrostatic equilibrium with varying temperature and composition to enable model comparison, and employ two bootstrap methods to test the robustness of our detections. Results: We detect neutral Mg, Na, Ca, Cr, Fe, Ni and V, which we predict exists in equilibrium with a significant quantity of VO, supporting earlier observations by HST/WFC3. Non-detections of Ti and TiO support the hypothesis that Ti is depleted via a cold-trap mechanism as has been proposed in the literature. Atomic line depths are under-predicted by hydrostatic models by a factor of 1.5 to 8, confirming recent findings that the atmosphere is extended. We predict the existence of significant concentrations of gas-phase TiO$_2$, VO$_2$ and TiS, which could be important absorbers at optical and NIR wavelengths in hot Jupiter atmospheres, but for which accurate line-list data is currently not available. We find no evidence for absorption by SH, and find that inflated atomic lines can plausibly explain the slope of the transmission spectrum observed in the NUV with HST/STIS. The Na D lines are significantly broadened and show a difference in their respective depths of 15 scale heights, which is not expected from isothermal hydrostatic theory.
