标题： 形成恒星的矮星系的红外特性：室女座星团中的蓝 compact 矮星系 显示英文标题

标题： Infrared Properties of Star Forming Dwarf Galaxies: Blue Compact Dwarfs in the Virgo Cluster

摘要： 一个包含16个蓝致密矮星系（BCDs）的样本已在墨西哥OAN-SPM的2.1米望远镜上使用近红外（NIR）在$J$和$K_s$进行成像。 大多数目标达到了高达$\mu_J$= 24 mag arcsec$^{-2}$和$\mu_{K_s}$= 23 mag arcsec$^{-2}$的等高线。 表面亮度分布可以通过两个分量的总和来拟合整个半径范围：一个双曲正割（sech）函数，已知它适合dIs的光度分布，以及一个高斯分量，用于量化中心附近的恒星爆发。 计算了等光度和总的近红外星等，并得出了在$\mu_J$= 23 mag arcsec$^{-2}$和$\mu_{K_s}$= 22 mag arcsec$^{-2}$处的半长轴。 通过轮廓拟合量化了弥散基底成分和年轻恒星爆发。 大多数颜色剖面显示出一个恒定的颜色值，在$J-K_s$=0.7 到 0.9 mag 之间。 对于大多数蓝压缩星系 (BCDs)，弥散成分代表了近红外光的主要部分，恒星爆发增强了不到约 0.3 mag 的流量。 发现盘状尺度长度与盘状星等之间以及盘状半长轴与盘状星等之间存在线性相关关系。 总体而言，具有更亮弥散成分的星系在中心更大且更亮。 中心爆发与弥散成分相关联，亮度更高的 BCD 具有更强的恒星爆发，表明质量更大的天体正在更有效地形成恒星。 BCDs 落在由矮不规则星系 (dIs) 在论文 I 中定义的基本平面（“fundamental plane”）上，遵循同样的盘状绝对星等、盘状中心面亮度和氢线宽（$W_{20}$）之间的关系，尽管散布范围比 dIs 的大。 [一句话省略] 显示英文摘要

摘要： A sample of 16 blue compact dwarf galaxies (BCDs) in the Virgo Cluster has been imaged in the near-infrared (NIR) in $J$ and $K_s$ on the 2.1m telescope at OAN-SPM in Mexico. Isophotes as faint as $\mu_J$ = 24 mag arcsec$^{-2}$ and $\mu_{K_s}$ = 23 mag arcsec$^{-2}$ have been reached in most of the targets. Surface brightness profiles can be fitted across the whole range of radii by the sum of two components: a hyperbolic secant (sech) function, which is known to fit the light profiles of dIs, and a Gaussian component, which quantifies the starburst near the centre. Isophotal and total fitted NIR magnitudes have been calculated, along with semimajor axes at $\mu_J$ = 23 mag arcsec$^{-2}$ and $\mu_{K_s}$ = 22 mag arcsec$^{-2}$. The diffuse underlying component and the young starburst have been quantified using the profile fitting. Most color profiles show a constant color, between $J-K_s$=0.7 to 0.9 mag. The diffuse component represents the overwhelming majority of the NIR light for most BCDs, the starburst enhancing the flux by less than about 0.3 mag. Linear correlations were found between the sech scale length and the sech magnitude, and between the sech semimajor axis and the sech magnitude. Overall, galaxies with more luminous diffuse components are larger and brighter in the centre. The central burst correlates with the diffuse component, with brighter BCDs having stronger star-bursts, suggesting that more massive objects are forming stars more efficiently. BCDs lie on the ``fundamental plane'' defined by dwarf irregulars (dISs) in Paper I, following the same relation between sech absolute magnitude, sech central surface brightness, and the hydrogen line-width $W_{20}$, although the scatter is larger than for the dIs. [one sentence cut]