Photometric and spectroscopic detection of the primary transit of the 111-day-period planet HD 80 606 b
Photometric and spectroscopic detection of the primary transit of the 111-day-period planet HD 80 606 b
复制标题
对 111 天周期行星 HD 80 606 b 的主凌日进行光度和光谱探测
DOI：
10.1051/0004-6361/200911954
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发表时间：
2009
影响因子：
6.5
通讯作者：
A. Vidal
中科院分区：
文献类型：
--
作者：
C. Moutou;G. Hébrard;F. Bouchy;A. Eggenberger;I. Boisse;X. Bonfils;D. Gravallon;D. Ehrenreich;T. Forveille;X. Delfosse;M. Desort;A. Lagrange;C. Lovis;M. Mayor;F. Pepe;C. Perrier;F. Pont;D. Queloz;N. Santos;D. Ségransan;S. Udry;A. Vidal
我们报告了太阳系外行星 HD 80 606 b 的主要凌日现象，这要归功于上普罗旺斯天文台进行的光度和光谱观测，同时使用 120 厘米望远镜上的 CCD 相机和 193 厘米望远镜上的 SOPHIE 摄谱仪进行观测。我们在两个数据集中以相同的时间观察了交通的整个出口及其部分中心部分。入侵发生在日落之前，因此没有被观察到。整个过境时间为 9.5 至 17.2 小时。这些数据允许测量行星半径（$R_{\mathrm{p}} = 0.9 \pm 0.10\,{R}_{\rm Jup}$）并完善系统的其他参数。径向速度测量显示检测到了前向罗西特-麦克劳林效应，并提供了自旋轨道未对准的提示。如果得到证实，这种错位将证实 HD 80 606 b 的不寻常轨道结构归因于 Kozai 迁移的假设。 HD 80 606 b是迄今为止检测到的周期最长的凌日行星。它异常小的半径强化了行星半径与从恒星接收到的入射通量之间的观察到的关系，并为理论提出了新的问题。它绕着一颗明亮的恒星 ($V=9$) 运行，为大量后续研究提供了机会。
We report the detection of the primary transit of the extra-solar planet HD 80 606 b, thanks to photometric and spectroscopic observations performed at the Observatoire de Haute-Provence, simultaneously with the CCD camera at the 120-cm telescope and the SOPHIE spectrograph on the 193-cm telescope. We observed the whole egress of the transit and partially its central part, in both datasets with the same timings. The ingress occurred before sunset so was not observed. The full duration of the transit was between 9.5 and 17.2 h. The data allows the planetary radius to be measured ($R_{\mathrm{p}} = 0.9 \pm 0.10\,{R}_{\rm Jup}$) and other parameters of the system to be refined. Radial velocity measurements show the detection of a prograde Rossiter-McLaughlin effect, and provide a hint of a spin-orbit misalignment. If confirmed, this misalignment would corroborate the hypothesis that HD 80 606 b owes its unusual orbital configuration to Kozai migration. HD 80 606 b is by far the transiting planet on the longest period detected today. Its unusually small radius reinforces the observed relationship between the planet radius and the incident flux received from the star and opens new questions for theory. Orbiting a bright star ($V=9$), it opens opportunities for numerous follow-up studies.