重新审视GJ 504系统。结合干涉测量、径向速度和高对比度成像数据
The GJ 504 system revisited. Combining interferometric, radial velocity, and high contrast imaging data
摘要：
已知G型恒星GJ 504 A拥有一颗3至35 MJup的伴星，其温度、质量和投影分离都有助于使其成为行星形成理论和巨行星和轻棕矮星大气模型的测试案例。我们收集了CHARA干涉仪，SOPHIE摄谱仪和VLT/SPHERE高对比度成像仪的数据，以重新审视系统的特性。我们测得GJ 504 A的半径为1.35+/-0.04 Rsun，得到该系统的等时年龄为21+/-2Myr或4.0+/-1.8 Gyr，视线恒星自转轴倾角为$162.4_{-4.3}^{+3.8}$度或$18.6_{-3.8}^{+4.3}$度。我们在Y2，Y3，J3，H2和K1双波段SPHERE图像中重新检测到伴星。GJ 504 b完整的1-4 $μ$ m SED形状最好由具有中间年龄的T8-T9.5天体（$\leq1.5$ Gyr）和/或不寻常的尘埃大气和/或超太阳金属丰度复制。所有六个大气模型都使用GJ 504 b的$\mathrm{T_{eff}=550 \pm 50}$ K，并指向低表面重力（3.5-4.0 dex）。金属丰度值的准确性受到模型到模型系统学的限制。它不随C/O比而退化。我们推导出$\mathrm{log\:L/L_{\odot}=-6.15\pm0.15}$ dex的同伴兼容质量的$\mathrm{M=1.3^{+0.6}_{-0.3}M_{Jup}}$和$\mathrm{M=23^{+10}_{-9} M_{Jup}}$的年轻和老年的年龄范围，分别。半长轴大于27.8au，偏心率小于0.55。GJ~ 504 b的后倾角与GJ~ 504 A的旋转轴不重合。我们结合径向速度和多历元成像数据，以排除额外的对象（90%概率）。年轻和老系统年龄的sma分别大于2.5和30 $\mathrm{M_{Jup}}$，范围为0.01-80 au。这颗伴星是在我们的核心吸积模型合成的行星群的包络中。
英文摘要：
The G-type star GJ504A is known to host a 3 to 35 MJup companion whose temperature, mass, and projected separation all contribute to make it a test case for the planet formation theories and for atmospheric models of giant planets and light brown dwarfs. We collected data from the CHARA interferometer, SOPHIE spectrograph, and VLT/SPHERE high contrast imager to revisit the properties of the system. We measure a radius of 1.35+/- 0.04Rsun for GJ504A which yields isochronal ages of 21+/-2Myr or 4.0+/-1.8Gyr for the system and line-of-sight stellar rotation axis inclination of $162.4_{-4.3}^{+3.8}$ degrees or $18.6_{-3.8}^{+4.3}$ degrees. We re-detect the companion in the Y2, Y3, J3, H2, and K1 dual band SPHERE images. The complete 1-4 $μ$m SED shape of GJ504b is best reproduced by T8-T9.5 objects with intermediate ages ($\leq1.5$Gyr), and/or unusual dusty atmospheres and/or super-solar metallicities. All six atmospheric models used yield $\mathrm{T_{eff}=550 \pm 50}$K for GJ504b and point toward a low surface gravity (3.5-4.0 dex). The accuracy on the metallicity value is limited by model-to-model systematics. It is not degenerate with the C/O ratio. We derive $\mathrm{log\:L/L_{\odot}=-6.15\pm0.15}$ dex for the companion compatible with masses of $\mathrm{M=1.3^{+0.6}_{-0.3}M_{Jup}}$ and $\mathrm{M=23^{+10}_{-9} M_{Jup}}$ for the young and old age ranges, respectively. The semi-major axis (sma) is above 27.8 au and the eccentricity lower than 0.55. The posterior on GJ~504b's orbital inclination suggests a misalignment with GJ~504A rotation axis. We combine the radial velocity and multi-epoch imaging data to exclude additional objects (90\% prob.) more massive than 2.5 and 30 $\mathrm{M_{Jup}}$ with sma in the range 0.01-80 au for the young and old system ages, respectively. The companion is in the envelope of the population of planets synthetized with our core-accretion model.
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