HD 114174 B的中红外高对比度成像：一个“类彗星”双星系统的视年龄离散
Mid-Infrared High-Contrast Imaging of HD 114174 B : An Apparent Age Discrepancy in a "Sirius-Like" Binary System
摘要：
我们对HD 114174轨道上发现的微弱的“类彗星”伴星进行了新的观测。之前在凯克使用NIRC 2在中红外波长下对HD 114174 B进行成像的尝试导致未检测到。我们用大双筒望远镜和LMIRCam进行的新的L '波段观测，以高信噪比（10 $σ$）恢复了伴星（$ΔL$ = 10.15 $\pm$ 0.15等，$ρ$ = 0.675“$\pm$ 0.016”）。这一测量代表了迄今为止在亚弧秒距离上最深的L'高对比度成像探测，包括太阳系外行星。我们确认HD 114174 B的近红外颜色与冷白矮星的解释一致（$J-L'$ = 0.76 $\pm$ 0.19等，$K-L'$ = 0.64 $\pm$ 0.20）。新的模型拟合对象的光谱能量分布表明温度$T_{\rm eff}$ = 4260 $\pm$ 360 K，表面重力log g = 7.94 $\pm$ 0.03，冷却年龄t $_{c} \approx$ 7.8 Gyr，和质量$M$ = 0.54 $\pm$ 0.01 $M_{\odot}$。我们发现，理论大气模型给出的冷却年龄不同意HD 114174 A的年龄来自两个等时线和陀螺年代学分析。我们推测可能的情况，以解释小学和中学之间的明显年龄差异。HD 114174 B是附近的一颗基准白矮星，最终将通过持续的多普勒和天体测量监测来估计动力学质量。详细描述其物理特性的努力将测试理论大气模型，并提高我们对白矮星演化，冷却和祖质量的理解。
英文摘要：
We present new observations of the faint "Sirius-like" companion discovered to orbit HD 114174. Previous attempts to image HD 114174 B at mid-infrared wavelengths using NIRC2 at Keck have resulted in a non-detection. Our new L'-band observations taken with the Large Binocular Telescope and LMIRCam recover the companion ($ΔL$ = 10.15 $\pm$ 0.15 mag, $ρ$ = 0.675'' $\pm$ 0.016'') with a high signal-to-noise ratio (10 $σ$). This measurement represents the deepest L' high-contrast imaging detection at sub-arcsecond separations to date, including extrasolar planets. We confirm that HD 114174 B has near-infrared colors consistent with the interpretation of a cool white dwarf ($J-L'$ = 0.76 $\pm$ 0.19 mag, $K-L'$ = 0.64 $\pm$ 0.20). New model fits to the object's spectral energy distribution indicate a temperature $T_{\rm eff}$ = 4260 $\pm$ 360 K, surface gravity log g = 7.94 $\pm$ 0.03, a cooling age t$_{c} \approx$ 7.8 Gyr, and mass $M$ = 0.54 $\pm$ 0.01 $M_{\odot}$. We find that the cooling age given by theoretical atmospheric models do not agree with the age of HD 114174 A derived from both isochronological and gyrochronological analyses. We speculate on possible scenarios to explain the apparent age discrepancy between the primary and secondary. HD 114174 B is a nearby benchmark white dwarf that will ultimately enable a dynamical mass estimate through continued Doppler and astrometric monitoring. Efforts to characterize its physical properties in detail will test theoretical atmospheric models and improve our understanding of white dwarf evolution, cooling, and progenitor masses.
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