标题： 低红移3CR源宿主星系中的凸起和盘：其径向亮度分布的近红外视图 显示英文标题

标题： Bulges and disks in the Host Galaxies of low redshift 3CR Sources: a near-IR view of their radial brightness profile

摘要： 我们分析了红外观测的3CR射电源宿主星系在z<0.3时的近红外光度分布和光度参数，以研究它们的物理性质。 我们的样本包括82个星系，其中22个（27%）是FR I型，60个（73%）是FR II型。 使用来自哈勃空间望远镜上的NICMOS和地面Telescopio Nazionale Galileo获取的近红外数据，我们发现52%的情况下光度分布可以用单一的Sersic定律很好地描述，而对于其余的对象（48%），需要包括一个指数分布，这可能表明存在盘结构。 这些星系的平均核心与盘光度比为(b/d) ~ 1.1。 对子样本的光度参数分析表明，FR I型和FR II型在有效表面亮度、有效半径和Sersic指数方面表现出相当相似的核心。 另一方面，FR I型和FR II型宿主中的盘平均显示出不同的特性。 与FR II型相比，FR I型的中心表面亮度较暗，尺度长度大两倍。 我们还利用两种不同的方法估计每个星系相关的黑洞质量，这两种方法声称黑洞质量（M_BH）与红外核心光度（L_bulge）和Sersic指数（n）之间有紧密的相关性。 我们的数据表明，通过这两种方法得到的质量具有较高的离散性，通过L_bulge得到的M_BH系统地高于通过n得到的值（约高3倍）。这一结果可能反映了我们样本中的星系没有找到L_bulge和n之间的相关性。 显示英文摘要

摘要： We analyze the near-infrared luminosity profiles and photometric parameters of the host galaxies of 3CR radio sources with z<0.3, to investigate their physical nature. Our sample includes 82 galaxies, of which 22 (27%) are FR Is and 60 (73%) are FR IIs. Using near-infrared data taken both with NICMOS onboard the Hubble Space Telescope and from the ground with the Telescopio Nazionale Galileo, we find that luminosity profiles are very well described by a single Sersic law in 52% of the cases and for the remaining objects (48%) it is necessary to include an exponential profile, which could indicate the presence of a disk. The average bulge to disk luminosity ratio for the galaxies is (b/d) ~ 1.1. The analysis of the photometric parameters of the sub samples indicates that FR Is and FR IIs show rather similar bulges in terms of effective surface magnitude, effective radius, and Sersic index. On the other hand, disks in FR Is and FR IIs hosts show, on average, different properties. Central surface magnitudes are dimmer and scale lengths are greater by a factor of 2 in FR Is when compared to FR IIs. We also estimate the black hole mass associated with each galaxy using two different methods that claim tight correlations between the black hole mass (M_BH) with the infrared bulge luminosity (L_bulge) and with the Sersic index (n). Our data indicate that masses obtained through these two methods show a high dispersion and M_BH obtained through L_bulge are systematically higher (by a factor of ~3) than those obtained using n. This result may reflect the fact that for our sample galaxies we do not find any correlation between L_bulge and n.