B3-VLA CSS样品。VIII：斯隆数字巡天的新光学识别。年轻射电源的紫外光谱能量分布
The B3-VLA CSS sample. VIII: New optical identifications from the Sloan Digital Sky Survey. The ultraviolet-optical spectral energy distribution of the young radio sources
摘要：
致密陡谱射电源和千兆赫峰谱射电源（CSS/GPS）通常被认为是年轻射电源。近年来，我们在许多波长上研究了从B3-VLA星表中选出的这些天体的一个样本：B3-VLA CSS样本。只有约60%的光源被光学识别。我们的目标是增加光学识别的数量，并研究年轻射电源的宿主星系的性质。我们将CSS B3-VLA样本与斯隆数字巡天（SDSS）DR 7进行了交叉相关，并使用来自UKIRT和2 MASS的可用GALEX（DR 4/5和6）和近红外数据补充了SDSS测光。我们获得了八个暗星系和一个类星体和两个类星体候选者的新的身份和光度红移。总的来说，我们有27个星系的SDSS测光在五个波段，我们推导出紫外光光谱能量分布（UV-O-SED）。我们将我们的调查扩展到从文献中选择的其他CSS/GPS。大多数的星系显示出过量的紫外线（UV）辐射相比，UV-O-SED的本地无线电安静的椭圆。我们发现了一个强烈的依赖于红移的紫外线过剩，并分析它假设它是从核心（隐藏类星体）或从一个年轻的恒星星族（YSP）产生。我们还比较了我们的CSS/GPS源的UV-O-SED与文献中的大尺寸（LSO）强大的射电源的选择。如果紫外线过剩的主要过程是由一个YSP引起的，我们的结论是，它是合并过程的结果，也引发了一些时间延迟的射电源的发病。我们没有看到由射电源本身触发的YSP的主要贡献的证据。
英文摘要：
Compact steep-spectrum radio sources and giga-hertz peaked spectrum radio sources (CSS/GPS) are generally considered to be mostly young radio sources. In recent years we studied at many wavelengths a sample of these objects selected from the B3-VLA catalog: the B3-VLA CSS sample. Only ~ 60 % of the sources were optically identified. We aim to increase the number of optical identifications and study the properties of the host galaxies of young radio sources. We cross-correlated the CSS B3-VLA sample with the Sloan Digital Sky Survey (SDSS), DR7, and complemented the SDSS photometry with available GALEX (DR 4/5 and 6) and near-IR data from UKIRT and 2MASS. We obtained new identifications and photometric redshifts for eight faint galaxies and for one quasar and two quasar candidates. Overall we have 27 galaxies with SDSS photometry in five bands, for which we derived the ultraviolet-optical spectral energy distribution (UV-O-SED). We extended our investigation to additional CSS/GPS selected from the literature. Most of the galaxies show an excess of ultra-violet (UV) radiation compared with the UV-O-SED of local radio-quiet ellipticals. We found a strong dependence of the UV excess on redshift and analyzed it assuming that it is generated either from the nucleus (hidden quasar) or from a young stellar population (YSP). We also compare the UV-O-SEDs of our CSS/GPS sources with those of a selection of large size (LSO) powerful radio sources from the literature. If the major process of the UV excess is caused by a YSP, our conclusion is that it is the result of the merger process that also triggered the onset of the radio source with some time delay. We do not see evidence for a major contribution from a YSP triggered by the radio sources itself.
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