发现的毫角秒分辨率不能分辨的近红外源目录
A catalog of near-IR sources found unresolved with milliarcsecond resolution
摘要：
校准是光学干涉测量长期存在的问题之一，特别是在长基线的情况下，这需要角尺寸在毫角秒尺度上的恒星，并且没有可探测的伴星。虽然校准器系统通常已经建立了近红外在明亮的源制度（K $\la 3$ \，mag），现代大型干涉仪是敏感的显着微弱的幅度。我们的目标是提供一个列表的来源发现未解决的直接观测具有高角分辨率和动态范围，可用于选择干涉校准。为此，我们使用了大量的月球掩星记录与ISAAC仪器在VLT选择源发现是无法解决的，没有密切的同伴。一种算法已被用来确定每个源实现的极限角分辨率，同时考虑到从光变曲线的遮蔽和未遮蔽部分建立的噪声模型。我们获得了556个源的角大小上限，其星等范围从K $_{\rm s} \approx$ 4到10不等，中值为7.2等。可能未被探测到的伴星（在$\approx 0\farcs5$内）的角大小上限范围从K $_{\rm s} \approx$ 8到13不等，中值为11.5等。三分之一的源的角大小为$\le 1$，三分之二的角大小为$\le 2$毫弧秒。这个未分辨源的列表与当前大型干涉测量设施的能力很好地匹配。我们还提供了可用的交叉识别，幅度，光谱类型和其他辅助信息。一小部分的来源被发现是潜在的变量。该列表涵盖了银河系隆起的部分，特别是银河系中心附近，那里的灭绝非常重要，传统的校准列表往往是不够的。
英文摘要：
Calibration is one of the long-standing problems in optical interferometric measurements, particularly with long baselines which demand stars with angular sizes on the milliarcsecond scale and no detectable companions. While systems of calibrators have been generally established for the near-infrared in the bright source regime (K$\la 3$\,mag), modern large interferometers are sensitive to significantly fainter magnitudes. We aim at providing a list of sources found unresolved from direct observations with high angular resolution and dynamic range, which can be used to choose interferometric calibrators. To this purpose, we have used a large number of lunar occultations recorded with the ISAAC instrument at the VLT to select sources found to be unresolved and without close companions. An algorithm has been used to determine the limiting angular resolution achieved for each source, taking into account a noise model built from occulted and unocculted portions of the light curves. We have obtained upper limits on the angular sizes of 556 sources, with magnitudes ranging from K$_{\rm s} \approx$4 to 10, with a median of 7.2\,mag. The upper limits on possible undetected companions (within $\approx 0\farcs5$) range from K$_{\rm s} \approx$8 to 13, with a median of 11.5\,mag. One-third of the sources have angular sizes $\le 1$, and two-thirds $\le 2$ milliarcseconds. This list of unresolved sources matches well the capabilities of current large interferometric facilities. We also provide available cross-identifications, magnitudes, spectral types, and other auxiliary information. A fraction of the sources are found to be potentially variable. The list covers parts of the Galactic Bulge and in particular the vicinity of the Galactic Center, where extinction is very significant and traditional lists of calibrators are often insufficient.
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