论文标题
系外星髋关节65426 B的中分辨率光谱
A medium-resolution spectrum of the exoplanet HIP 65426 b
论文作者
论文摘要
中分辨率的积分场光谱仪（IFS），以及凯克/奥西里斯（Keck/Osiris），VLT/Muse或Sinfoni等自适应访问仪，作为增强大型地室中年轻的，气体巨型巨型外科体的检测和表征能力的新途径（> 5 au）。我们分析了年轻的巨型系外行星hip 65426 b的K频段VLT/SINFONI中分辨率（R_LAMBDA〜5577）观察结果。我们专用的IFS数据分析工具包（Textris）优化了立方体建筑物，恒星注册，并允许提取行星光谱。 A Bayesian inference with the nested sampling algorithm coupled with the self-consistent forward atmospheric models BT-SETTL15 and Exo-REM using the ForMoSA tool yields Teff=1560 +/- 100K, log(g)<4.40dex, [M/H]=0.05 +/- 0.22dex, and an upper limit on the C/O ratio (<0.55).该物体还通过所谓的“分子映射”技术重新发现对象。该技术产生一致的大气参数，但是在过程中，行星伪骨的丢失降低或修改了这些参数的约束。太阳能与微极c/o比表明，如果通过核心 - 核酸到水雪线（> 20 au）形成行星，则固体在形成时富集。但是，重力不稳定的形成不能排除。金属性与伯尔尼星球人口模型的大量jovian行星的大量丰富兼容。最后，我们测量的径向速度为26 +/- 15km/s，与我们对恒星的修订测量兼容。这是可以评估径向速度的第四个成像系外行星，说明了这种观察结果评估属于恒星形成区域的成像系统的共同进化的潜力，例如HIP 65426。
Medium-resolution integral-field spectrographs (IFS) coupled with adaptive-optics such as Keck/OSIRIS, VLT/MUSE, or SINFONI are appearing as a new avenue for enhancing the detection and characterization capabilities of young, gas giant exoplanets at large heliocentric distances (>5 au). We analyzed K-band VLT/SINFONI medium-resolution (R_lambda~5577) observations of the young giant exoplanet HIP 65426 b. Our dedicated IFS data analysis toolkit (TExTRIS) optimized the cube building, star registration, and allowed for the extraction of the planet spectrum. A Bayesian inference with the nested sampling algorithm coupled with the self-consistent forward atmospheric models BT-SETTL15 and Exo-REM using the ForMoSA tool yields Teff=1560 +/- 100K, log(g)<4.40dex, [M/H]=0.05 +/- 0.22dex, and an upper limit on the C/O ratio (<0.55). The object is also re-detected with the so-called "molecular mapping" technique. The technique yields consistent atmospheric parameters, but the loss of the planet pseudo-continuum in the process degrades or modifies the constraints on these parameters. The solar to sub-solar C/O ratio suggests an enrichment by solids at formation if the planet was formed beyond the water snowline (>20 au) by core-accretion. However, a formation by gravitational instability can not be ruled out. The metallicity is compatible with the bulk enrichment of massive Jovian planets from the Bern planet population models. Finally, we measure a radial velocity of 26 +/- 15km/s compatible with our revised measurement on the star. This is the fourth imaged exoplanet for which a radial velocity can be evaluated, illustrating the potential of such observations for assessing the coevolution of imaged systems belonging to star forming regions, such as HIP 65426.
