直接发现HD206893系统中的内部系外行星。在行星质量同伴中燃烧氘的证据

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直接发现HD206893系统中的内部系外行星。在行星质量同伴中燃烧氘的证据

Direct discovery of the inner exoplanet in the HD206893 system. Evidence for deuterium burning in a planetary-mass companion

论文作者

Hinkley, S., Lacour, S., Marleau, G. -D., Lagrange, A. M., Wang, J. J., Kammerer, J., Cumming, A., Nowak, M., Rodet, L., Stolker, T., Balmer, W. -O., Ray, S., Bonnefoy, M., Mollière, P., Lazzoni, C., Kennedy, G., Mordasini, C., Abuter, R., Aigrain, S., Amorim, A., Asensio-Torres, R., Babusiaux, C., Benisty, M., Berger, J. -P., Beust, H., Blunt, S., Boccaletti, A., Bohn, A., Bonnet, H., Bourdarot, G., Brandner, W., Cantalloube, F., Caselli, P., Charnay, B., Chauvin, G., Chomez, A., Choquet, E., Christiaens, V., Clénet, Y., Foresto, V. Coudé du, Cridland, A., Delorme, P., Dembet, R., de Zeeuw, P. T., Drescher, A., Duvert, G., Eckart, A., Eisenhauer, F., Feuchtgruber, H., Galland, F., Garcia, P., Lopez, R. Garcia, Gardner, T., Gendron, E., Genzel, R., Gillessen, S., Girard, J. H., Grandjean, A., Haubois, X., Heißel, G., Henning, Th., Hippler, S., Horrobin, M., Houllé, M., Hubert, Z., Jocou, L., Keppler, M., Kervella, P., Kreidberg, L., Lapeyrère, V., Bouquin, J. -B. Le, Léna, P., Lutz, D., Maire, A. -L., Mang, F., Mérand, A., Meunier, N., Monnier, J. D., Mordasini, C., Mouillet, D., Nasedkin, E., Ott, T., Otten, G. P. P. L., Paladini, C., Paumard, T., Perraut, K., Perrin, G., Philipot, F., Pfuhl, O., Pourré, N., Pueyo, L., Rameau, J., Rickman, E., Rubini, P., Rustamkulov, Z., Samland, M., Shangguan, J., Shimizu, T., Sing, D., Straubmeier, C., Sturm, E., Tacconi, L. J., van Dishoeck, E. F., Vigan, A., Vincent, F., Ward-Duong, K., Widmann, F., Wieprecht, E., Wiezorrek, E., Woillez, J., Yazici, S., Young, A., Zicher, N., Collaboration, the GRAVITY

论文摘要

长期精确的径向速度（RV）对附近的STAR HD206893的监测以及系统中的异常情况表明系统中存在附加的内部伴侣。在这里，我们描述了使用VLTI/Gravity仪器进行这种RV漂移和适当运动异常的伴侣的多上ch搜索结果。利用HARPS光谱仪的持续精确RV测量以及Gaia宿主星体的信息，我们在三个时期内报告了伴随HD206893C的高显着性检测，并清楚地证明了开普勒轨道运动的证据。我们使用$ \ sim $ 50-100 $μ$ arcsec精确的天文统计使我们得出动态质量为12.7 $^{+1.2} _ { - 1.0} $ m $ _ {\ rm jup} $，y骨分离和3.53 $^$ 0.08} $} HD206893C。我们适合系统中两个同伴的轨道，都利用Gaia天文统计和RVS来提供对B成分先前不确定质量的精确动力学估计，因此得出了$ 155 \ PM15 $ MYR的年龄。我们发现，通过云层大气进行了参数化的理论大气/进化模型，这些模型融合了HD206893C的氘燃烧，可同时拟合HD206893B和C的亮度。除了利用长期的RV信息外，这项工作是直接成像发现真正以Gaia Astrestrestremitry指导的真实成像的早期示例。有望利用GAIA天文标准是识别和表征其他直接成像行星的主要技术之一。最后，这一发现是光学干涉仪直接检测和表征外极行星的另一个例子，在冰线轨道分离2-4 \，AU。

Long term precise radial velocity (RV) monitoring of the nearby star HD206893, as well as anomalies in the system proper motion, have suggested the presence of an additional, inner companion in the system. Here we describe the results of a multi-epoch search for the companion responsible for this RV drift and proper motion anomaly using the VLTI/GRAVITY instrument. Utilizing information from ongoing precision RV measurements with the HARPS spectrograph, as well as Gaia host star astrometry, we report a high significance detection of the companion HD206893c over three epochs, with clear evidence for Keplerian orbital motion. Our astrometry with $\sim$50-100 $μ$arcsec precision afforded by GRAVITY allows us to derive a dynamical mass of 12.7$^{+1.2}_{-1.0}$ M$_{\rm Jup}$ and an orbital separation of 3.53$^{+0.08}_{-0.06}$ au for HD206893c. Our fits to the orbits of both companions in the system utilize both Gaia astrometry and RVs to also provide a precise dynamical estimate of the previously uncertain mass of the B component, and therefore derive an age of $155\pm15$ Myr. We find that theoretical atmospheric/evolutionary models incorporating deuterium burning for HD206893c, parameterized by cloudy atmospheres provide a good simultaneous fit to the luminosity of both HD206893B and c. In addition to utilizing long-term RV information, this effort is an early example of a direct imaging discovery of a bona fide exoplanet that was guided in part with Gaia astrometry. Utilizing Gaia astrometry is expected to be one of the primary techniques going forward to identify and characterize additional directly imaged planets. Lastly, this discovery is another example of the power of optical interferometry to directly detect and characterize extrasolar planets where they form at ice-line orbital separations of 2-4\,au.

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