标题： 低红移3CR源寄主星系中的 bulge 和 disk：它们径向亮度分布的近红外观测视角 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： 我们分析了红移 z < 0.3 的 3CR 射电源宿主星系的近红外亮度分布和测光参数，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。 利用来自哈勃太空望远镜上的 NICMOS 和地面的特纳伽利略望远镜的近红外数据，我们发现有 52% 的情况下亮度分布可以用单一的 Sersic 律很好地描述，而剩余的星系（48%）则需要加入指数分布，这可能表明盘状结构的存在。 这些星系的平均核球与盘状结构亮度比为 (b/d) ≈ 1.1。 子样本的测光参数分析显示，FR I 型和 FR II 型在有效面亮度、有效半径和 Sersic 指数方面显示出相当相似的核球。 另一方面，FR I 型和 FR II 型宿主星系中的盘状结构表现出不同的特性。 中央表面亮度较暗且尺度长度更大，FR I 型是 FR II 型的两倍。 我们还使用两种不同的方法估计了每个星系相关的黑洞质量，这两种方法声称黑洞质量 (M_BH) 与红外核球亮度 (L_bulge) 和 Sersic 指数 (n) 之间存在紧密的相关性。 我们的数据显示，通过这两种方法得到的质量具有较高的离散性，并且通过 L_bulge 得到的 M_BH 系统性地更高（约高 3 倍），这可能反映了我们样本中的星系没有发现 L_bulge 和 n 之间的任何相关性。 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.