标题： 金星近红外光谱仪$-$深空类星体调查：钱德拉视角 显示英文标题

标题： Gemini Near Infrared Spectrograph$-$Distant Quasar Survey: the Chandra View

摘要： 我们展示了钱德拉对63个来自金星近红外光谱仪$-$遥远类星体调查（GNIRS-DQS）源的观测，其中54个在第24轮观测中被进行了快照观测。总共55个源在至少一个X射线波段被明确检测到，我们对剩余的八个源设定了严格的X射线通量上限。结合这些源的静止框架紫外-光学光谱数据，我们评估X射线是否可以作为类星体吸积率的可靠指示器，特别是在最高可访问红移处。我们利用最近修改的基于H$\beta$的爱丁顿光度比估计器，以及C IV$\lambda$1549发射线参数空间来研究与光学-X射线光谱斜率（$\alpha_{\mathrm{ox}}$）和有效硬X射线幂律光子指数（$\Gamma$）的趋势和相关性。我们发现$\alpha_{\mathrm{ox}}$并不能改进基于H$\beta$或C IV 的当前吸积率估计。 相反，在我们的样本限制内，我们确认了以前的发现，即C IV参数空间可能是吸积率的一个更好的指示器，直到$z\sim3.5$。 我们还发现，我们一些源的小子集的平均$\Gamma$值，以及我们源在不同分组中的平均$\Gamma$值，与其各自相对较高的爱丁顿光度比一致。 需要对我们的X射线探测源进行更深入的X射线观测，以准确测量$\Gamma$并测试该参数是否可以作为稳健、无偏的吸积率诊断工具。 显示英文摘要

摘要： We present Chandra observations of 63 sources from the Gemini Near Infrared Spectrograph$-$Distant Quasar Survey (GNIRS-DQS) of which 54 were targeted by snapshot observations in Cycle 24. A total of 55 sources are clearly detected in at least one X-ray band, and we set stringent upper limits on the X-ray fluxes of the remaining eight sources. In combination with rest-frame ultraviolet-optical spectroscopic data for these sources, we assess whether X-rays can provide a robust accretion-rate indicator for quasars, particularly at the highest accessible redshifts. We utilize a recently modified H$\beta$-based Eddington luminosity ratio estimator, as well as the C IV $\lambda$1549 emission-line parameter space to investigate trends and correlations with the optical-X-ray spectral slope ($\alpha_{\mathrm{ox}}$) and the effective hard-X-ray power-law photon index ($\Gamma$). We find that $\alpha_{\mathrm{ox}}$ does not improve current accretion-rate estimates based on H$\beta$ or C IV. Instead, within the limitations of our sample, we confirm previous findings that the C IV parameter space may be a better indicator of the accretion rate up to $z\sim3.5$. We also find that the average $\Gamma$ values for a small subset of our sources, as well as the average $\Gamma$ value in different groupings of our sources, are consistent with their respective relatively high Eddington luminosity ratios. Deeper X-ray observations of our X-ray-detected sources are needed for measuring $\Gamma$ accurately and testing whether this parameter can serve as a robust, un-biased accretion-rate diagnostic.