一个突出的尘埃带星系NGC 4370的多波段成像观测
Multiband imaging observations of a prominent dust lane galaxy NGC 4370
摘要：
本文利用Hanle的Himalaya Chandra望远镜（HCT）的光学宽带（BVRI）成像观测和2MASS的近红外（J，H，K $_s$）图像，研究了一个著名的尘埃带星系NGC 4370中星际尘埃的消光特性。NGC 4370属于室女座星系团（VCC 0758），与NGC 4365在10 $\arcmin$处形成非交互作用的一对。NGC 4370拥有一条平行于其光学主轴的突出尘埃带，几乎延伸到1 \arcmin。NGC 4370的消光曲线与银河系的消光曲线平行，这意味着NGC 4370中尘埃的性质与银河系中典型粒子的性质相同。发现$R_V$值等于2.85 $\pm$ 0.05，与尘埃带星系的观测值一致。用消光系数和IRAS通量密度估算的NGC 4370尘埃总量分别等于$4.4\times 10^4$ \msol和$2.0\times 10^5$ \msol。至于这个星系中尘埃和ISM的起源，这个星系在其生命周期中积累的尘埃不足以解释光学方法检测到的质量，这反过来意味着ISM可能是由NGC 4370通过合并事件获得的。还试图研究ISM的多个阶段之间的明显空间对应关系，即，热气体，温暖的气体和尘埃在这个星系通过获得光学发射地图从窄带成像和扩散X射线发射地图从分析\emph{Chandra}档案数据。这种分析意味着尘埃和温暖的气体之间的物理联系，就它们的物理共存和共同起源而言。
英文摘要：
In this paper we present extinction properties of interstellar dust in a prominent dust lane galaxy NGC 4370 based on the optical broad band (BVRI) imaging observations taken from the Himalaya Chandra Telescope (HCT), Hanle and the near-IR (J,H,K$_s$) images taken from the 2MASS archive. NGC 4370 belongs to the Virgo cluster (VCC 0758) and form a non-interactive pair with NGC 4365 at 10$\arcmin$. NGC 4370 hosts a prominent dust lane running parallel to its optical major axis and is extended almost up to 1\arcmin. The extinction curve derived for NGC 4370 is found to run parallel to Galactic extinction curve, implying that the properties of dust in NGC 4370 are identical to those of the canonical grains in the Milky Way. The $R_V$ value is found to be equal to 2.85$\pm$0.05 and is consitent with the values reported for the dust lane galaxies. The total dust content of NGC 4370 estimated using optical extinction and IRAS flux densities are found to be equal to $4.4\times 10^4$ \msol and $2.0\times 10^5$ \msol, respectively. As regard to the origin of dust and ISM in this galaxy, the accumulated dust by this galaxy over its life-time is insufficient to account for the detected mass by optical means, which in turn imply that the ISM might have been acquired by the NGC 4370 through a merger like event. An attempt is also made to study the apparent spatial correspondence between the multiple phases of ISM, i.e., hot gas, warm gas and dust in this galaxy by obtaining optical emission maps from narrow band imaging and diffuse X-ray emission map obtained from the analysis of \emph{Chandra} archival data. This analysis implies a physical connection between the dust and warm gas in terms of their physical co-existence and common origin too.
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