透视环：V582 Mon（KH 15 D）的近红外光度测定
Seeing Through the Ring: Near-Infrared Photometry of V582 Mon (KH 15D)
摘要：
我们研究的光和颜色的演化的金牛座T的二进制KH 15 D通过测光获得的波长在0.55和8.0 $μ$ m之间。这些数据是由Cerro-Tololo美洲天文台1.3米SMARTS望远镜上的ANDICAM和斯皮策空间望远镜上的IRAC收集的。我们表明，该系统的circumbinary环，它作为一个屏幕，覆盖和揭露不同部分的双轨道作为环进动，已达到一个方向，其中较亮的组件（星B）完全或几乎完全出现在每个轨道周期。较暗的部分（A星）在所有相位都被屏幕完全遮蔽。屏幕的前缘和后缘以每秒$\sim$ 15米的速度在天空中移动，这与半径和宽度为$\sim$ 4 AU，岁差周期为$\sim$ 6500年的环的预期一致。光和颜色的变化继续表明，屏幕是尖锐的边缘和不透明的\emph{VRIJH}波长。然而，我们发现在2.2，3.6，和4.5 $μ$ m的环边缘的透明度增加。在CSI 2264活动期间发生的日食开始时看到的变红特别表明大尘埃颗粒的选择性灭绝。与此同时，在恒星B下沉时观察到的逐渐变蓝表明了环边缘的前向散射效应。在明亮的阶段，系统的SED没有显示出红外过量发射的证据，这些红外过量发射可以归因于来自环或其他尘埃成分的8微米的辐射。
英文摘要：
We examine the light and color evolution of the T Tauri binary KH 15D through photometry obtained at wavelengths between 0.55 and 8.0 $μ$m. The data were collected with ANDICAM on the 1.3 m SMARTS telescope at Cerro-Tololo Inter-American Observatory and with IRAC on the Spitzer Space Telescope. We show that the system's circumbinary ring, which acts as a screen that covers and uncovers different portions of the binary orbit as the ring precesses, has reached an orientation where the brighter component (star B) fully or nearly fully emerges during each orbital cycle. The fainter component (star A) remains fully occulted by the screen at all phases. The leading and trailing edges of the screen move across the sky at the same rate of $\sim$15 meters per second, consistent with expectation for a ring with a radius and width of $\sim$4 AU and a precession period of $\sim$6500 years. Light and color variations continue to indicate that the screen is sharp edged and opaque at \emph{VRIJH} wavelengths. However, we find an increasing transparency of the ring edge at 2.2, 3.6, and 4.5 $μ$m. Reddening seen at the beginning of the eclipse that occurred during the CSI 2264 campaign particularly suggests selective extinction by a population of large dust grains. Meanwhile, the gradual bluing observed while star B is setting is indicative of forward scattering effects at the edge of the ring. The SED of the system at its bright phase shows no evidence of infrared excess emission that can be attributed to radiation from the ring or other dust component out to 8 microns.
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