大量富气合并的深HST H波段成像调查。II。QUEST PG类星体
A Deep HST H-Band Imaging Survey of Massive Gas-Rich Mergers. II. The QUEST PG QSOs
摘要：
我们报告的结果，从深HST NICMOS H波段成像调查的28 z < 0.3类星体从帕洛玛绿色（PG）的样本。该程序是QUEST（类星体/ ULIRG演化研究）的一部分，并补充了论文I中提出的26个高核ULIRG的类似数据集。我们的分析表明，类星体的比例与椭圆主机是较高的类星体与未检测到的远红外（FIR）发射，小红外过剩，和发光的主机。主机的FIR-微弱类星体显示出一种趋势，有不太明显的合并引起的形态异常和较大的类星体到主机的光度比平均比主机的FIR-明亮的类星体，符合后期合并的演变从FIR-明亮的FIR-微弱的类星体。在我们的样本中，射电安静的PG类星体的球体大小和总的主机亮度在统计上与论文I中提出的ULIRG主机没有区别，而射电大声的PG类星体系统更大，更明亮。ULIRG和PG类星体的椭圆主机落在附近，但不完全是，不活跃的椭球体的基本面。我们证实了在论文I中指出的系统趋势，即具有小（<2kpc）球状体的天体比不活跃的球状体亮约1等。主色和波长对它们大小的依赖支持了这样一种观点，即这些偏差至少部分是由于非核恒星的形成。然而，这些偏差的幅度并不取决于主机R-H颜色。按面值计算（即，没有对灭绝或年轻恒星星族的存在进行修正），H波段球状体-宿主光度表明BH质量约为5 - 200 x 10^7太阳质量，类星体和超红外类星体的亚爱丁顿质量吸积率。这些结果进行了比较与出版的BH质量估计来自其他方法。（节略）
英文摘要：
We report the results from a deep HST NICMOS H-band imaging survey of 28 z < 0.3 QSOs from the Palomar-Green (PG) sample. This program is part of QUEST (Quasar / ULIRG Evolution STudy) and complements a similar set of data on 26 highly-nucleated ULIRGs presented in Paper I. Our analysis indicates that the fraction of QSOs with elliptical hosts is higher among QSOs with undetected far-infrared (FIR) emission, small infrared excess, and luminous hosts. The hosts of FIR-faint QSOs show a tendency to have less pronounced merger-induced morphological anomalies and larger QSO-to-host luminosity ratios on average than the hosts of FIR-bright QSOs, consistent with late-merger evolution from FIR-bright to FIR-faint QSOs. The spheroid sizes and total host luminosities of the radio-quiet PG QSOs in our sample are statistically indistinguishable from the ULIRG hosts presented in Paper I, while those of radio-loud PG QSOs are systematically larger and more luminous. ULIRGs and PG QSOs with elliptical hosts fall near, but not exactly on, the fundamental plane of inactive spheroids. We confirm the systematic trend noted in Paper I for objects with small (< 2 kpc) spheroids to be up to ~1 mag. brighter than inactive spheroids. The host colors and wavelength dependence of their sizes support the idea that these deviations are due at least in part to non-nuclear star formation. However, the amplitudes of these deviations does not depend on host R-H colors. Taken at face value (i.e., no correction for extinction or the presence of a young stellar population), the H-band spheroid-host luminosities imply BH masses ~5 -- 200 x 10^7 M_sun and sub-Eddington mass accretion rates for both QSOs and ULIRGs. These results are compared with published BH mass estimates derived from other methods. (abridged)
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