AI 中文总结
本研究结合 JWST、HST 的多波段光谱数据，证实热木星 HAT-P-1 b 大气富含水、二氧化碳，可能含硫化氢，金属丰度约为太阳的 10 倍，是热木星大气研究的基准天体。
AI 中文摘要
作为詹姆斯·韦布空间望远镜（JWST）系外行星大巡天调查的一部分，我们利用全色透射光谱学将此前研究过的热木星 HAT-P-1 b 的光学和近红外大气，与 JWST 可探测的更长波长分子带关联起来。我们呈现了 JWST NIRSpec G395H 在 2.7–5.3 微米波段对热木星 HAT-P-1 b 的透射光谱，并将新光谱与存档的哈勃空间望远镜（HST）STIS 和 WFC3 观测数据结合，开展 0.3–5.3 微米的大气分析。我们使用 Eureka!、FIREFLy 和 Tswift 三个独立管道对 JWST 数据进行处理，发现在 G395H 波段通带内的透射光谱相互一致。大气反演得出了水（H₂O）和二氧化碳（CO₂）的强证据，其贝叶斯因子分别为 log₁₀B_H₂O=8.9 和 log₁₀B_CO₂=52.3，同时还得出了硫化氢（H₂S）的初步证据（log₁₀B_H₂S=1.4）。H₂O 和 CO₂ 的联合约束支持大气接近化学平衡，金属丰度 log₁₀ M/H=0.99⁺⁰·¹⁹₋₀·₁₄，约为太阳的 10 倍，或相对于近太阳金属丰度的宿主恒星约为 9 倍，碳氧比（C/O）的 3σ 上限小于 0.52。由于在该温度范围内，H₂O 和 CO₂ 提供的金属丰度对垂直混合相对不敏感，它们的联合探测表明大气成分主要由整体富集而非强非平衡输运决定。我们未发现云的显著证据；相反，光谱中分子结构的持续存在反对强云消光作用。初步的 H₂S 信号若得到证实，将进一步表明所探测压力下的光化学处理有限。总体而言，分子清单、富集金属丰度和低 C/O 比表明 HAT-P-1 b 是富氧大气，确立其为热木星大气成分比较研究的基准天体。
英文摘要
As part of JWST's Exoplanet Grand Tour Survey, we use panchromatic transmission spectroscopy to connect HAT-P-1 b's previously studied optical and near-infrared atmosphere to the longer-wavelength molecular bands accessible with JWST. We present JWST NIRSpec G395H transmission spectroscopy of the hot Jupiter HAT-P-1 b over 2.7--5.3~$μ$m, and combine the new spectrum with archival HST STIS and WFC3 observations for a 0.3--5.3~$μ$m atmospheric analysis. We independently reduce the JWST data with the Eureka!, FIREFLy, and Tswift pipelines, finding mutually consistent transmission spectra across the G395H bandpass. Atmospheric retrievals yield strong evidence for H$_2$O and CO$_2$ with Bayes factors of $\log_{10}B_{\mathrm{H_2O}}=8.9$ and $\log_{10}B_{\mathrm{CO_2}}=52.3$, while providing tentative evidence for H$_2$S ($\log_{10}B_{\mathrm{H_2S}}=1.4$). The joint H$_2$O and CO$_2$ constraints favor an atmosphere near chemical equilibrium, with $\log_{10} \text{M/H}=0.99^{+0.19}_{-0.14}$, corresponding to $\sim10\times$ Solar or $\sim9\times$ relative to the near-solar metallicity host star, and a 3$σ$ upper limit of C/O $<0.52$. Because H$_2$O and CO$_2$ provide a metallicity comparatively insensitive to vertical mixing in this temperature regime, their combined detection suggests the composition is dominated by bulk enrichment rather than strong disequilibrium transport. We find no significant evidence for clouds; instead, the persistence of molecular structure across the spectrum argues against strong cloud muting. The tentative H$_2$S signal, if confirmed, would further suggest limited photochemical processing at the pressures probed. Together, the molecular inventory, enriched metallicity, and low C/O ratio point to an oxygen-rich atmosphere and establish HAT-P-1 b as a benchmark for comparative studies of hot-Jupiter atmospheric composition.
Comments25 pages, 11 figures, 5 tables. Accepted to The Astronomical Journal; final revision pending
