论文标题
Ares IV：使用HST/WFC3摄像头探测两个温暖的小行星HD 106315 C和HD 3167 C的气氛
ARES IV: Probing the atmospheres of the two warm small planets HD 106315 c and HD 3167 c with the HST/WFC3 camera
论文作者
论文摘要
我们提出了两个中型行星的大气表征研究，将海王星的半径括起来：HD 106315 C（r $ _ {\ rm {p}} $ = 4.98 $ = 4.98 $ \ pm $ 0.23 r $ _ {\ oplus} $）和HD 3167 C）和HD 3167 C （r $ _ {\ rm {p}} $ = 2.740 $ _ { - 0.100}^{+0.106} $ r $ _ {\ oplus} $）。我们分析了用G141 Grism（1.125-1.650 $ $ m）获得的宽场摄像头3（WFC3）在哈勃太空望远镜上获得的空间扫描光谱观测。我们使用公开可用的iraclis管道和taurex3大气检索代码，并在两个行星的大气中检测水蒸气，大量$ \ log_ {10} [\ mathrm {h_2o}] = -2.1 = -2.1^{+0.7} {+0.7} $ \ log_ {10} [\ mathrm {h_2o}] = - 4.1^{+0.9} _ { - 0.9} $（$ \ sim $ 3.17 $σ$）分别用于HD 106315 C和HD 3167 C。 HD 106315 C的传输光谱还显示了吸收氨的可能证据（$ \ log_ {10} [\ MathRM {\ Mathrm {nh_3}] = - 4.3^{+0.7} _ { - 2.0} $，$ \ sim $ 1.97 $ 1.97 $ -even的特征，如果IT的特征，则Y MOUND MOINDERITY，而不是有意义的 - 与carement” $ \ sim $ 1.1-1.6〜 $ $ m m波长范围（$ \ log_ {10} [\ mathrm {co_ {2}}] = -2.4^{+0.7} _ { - 1.0} $ 3.28 $ 3.28 $）。但是，CO $ _2 $检测似乎很重要，必须仔细考虑并透视。实际上，1D均衡化学模型无法解释CO $ _2 $的存在，这可能是由于可能的系统学。讨论了云，CO和CH $ _4 $的其他贡献。 HD 106315 C和HD 3167 C将是即将到来的望远镜的有趣目标，例如James Webb太空望远镜（JWST）和大气遥感红外超球星大型苏联（Ariel）。
We present an atmospheric characterization study of two medium sized planets bracketing the radius of Neptune: HD 106315 c (R$_{\rm{P}}$=4.98 $\pm$ 0.23 R$_{\oplus}$) and HD 3167 c (R$_{\rm{P}}$=2.740$_{-0.100}^{+0.106}$ R$_{\oplus}$). We analyse spatially scanned spectroscopic observations obtained with the G141 grism (1.125 - 1.650 $μ$m) of the Wide Field Camera 3 (WFC3) onboard the Hubble Space Telescope. We use the publicly available Iraclis pipeline and TauREx3 atmospheric retrieval code and we detect water vapor in the atmosphere of both planets with an abundance of $\log_{10}[\mathrm{H_2O}]=-2.1^{+0.7}_{-1.3}$ ($\sim$5.68$σ$) and $\log_{10}[\mathrm{H_2O}]=-4.1^{+0.9}_{-0.9}$ ($\sim$3.17$σ$) for HD 106315 c and HD 3167 c, respectively. The transmission spectrum of HD 106315 c shows also a possible evidence of ammonia absorption ($\log_{10}[\mathrm {NH_3}]=-4.3^{+0.7}_{-2.0}$, $\sim$1.97$σ$ -even if it is not significant-), whilst carbon dioxide absorption features may be present in the atmosphere of HD 3167 c in the $\sim$1.1-1.6~$μ$m wavelength range ($\log_{10}[\mathrm{CO_{2}}]= -2.4^{+0.7}_{-1.0}$, $\sim$3.28$σ$). However the CO$_2$ detection appears significant, it must be considered carefully and put into perspective. Indeed, CO$_2$ presence is not explained by 1D equilibrium chemistry models, and it could be due to possible systematics. The additional contribution of clouds, CO and CH$_4$ are discussed. HD 106315 c and HD 3167 c will be interesting targets for upcoming telescopes such as the James Webb Space Telescope (JWST) and the Atmospheric Remote-Sensing Infrared Exoplanet Large-Survey (Ariel).
