活动星系中黑洞质量标度关系的局域基线。I.试点研究的方法和结果
A Local Baseline of the Black Hole Mass Scaling Relations for Active Galaxies. I. Methodology and Results of Pilot Study
摘要：
我们利用高质量的Keck/LRIS长缝光谱仪对从SDSS中选取的25个局部活动星系（0.02<z<0.1; MBH>10^7 M_sun）的实验样品进行了研究，以研究黑洞质量（MBH）与宿主星系性质之间的关系.我们确定恒星运动学的宿主星系，推导恒星速度色散配置文件和旋转曲线从三个光谱区域（包括CaH&K，MgIb三重态，和CaII三重态）。此外，我们进行表面光度SDSS图像，使用新开发的代码联合多波段分析。BH的质量是由Hbeta发射线的宽度和5100 A活动星系核的亮度来估算的。结合光谱和成像的结果，我们可以研究四种MBH标度关系：MBH-sigma，MBH-L（sph），MBH-M（sph，*），MBH-M（sph，dyn）。我们发现以下结果。首先，恒星速度分散从孔径光谱（例如SDSS光纤光谱或未解决的数据从遥远的星系）可以偏置，这取决于孔径大小，AGN污染，和宿主星系形态。然而，这样的偏差不能解释在更高的红移MBH-sigma关系中看到的偏移。第二，虽然CaT区域是最干净的确定恒星速度色散，无论是MgIb区域，修正FeII发射，和CaHK区域，虽然经常淹没的活动星系核幂律连续谱和发射线，可以给出准确的结果在百分之几。第三，我们的试点样品的MBH标度关系的斜率和散射与其他本地活动和非活动星系。在本系列的下一篇文章中，我们将量化尺度关系，利用约100个对象的完整样本。
英文摘要：
We present high-quality Keck/LRIS longslit spectroscopy of a pilot sample of 25 local active galaxies selected from the SDSS (0.02<z<0.1; MBH>10^7 M_sun) to study the relations between black hole mass (MBH) and host-galaxy properties. We determine stellar kinematics of the host galaxy, deriving stellar-velocity dispersion profiles and rotation curves from three spectral regions (including CaH&K, MgIb triplet, and CaII triplet). In addition, we perform surface photometry on SDSS images, using a newly developed code for joint multi-band analysis. BH masses are estimated from the width of the Hbeta emission line and the host-galaxy free 5100A AGN luminosity. Combining results from spectroscopy and imaging allows us to study four MBH scaling relations: MBH-sigma, MBH-L(sph), MBH-M(sph,*), MBH-M(sph,dyn). We find the following results. First, stellar-velocity dispersions determined from aperture spectra (e.g. SDSS fiber spectra or unresolved data from distant galaxies) can be biased, depending on aperture size, AGN contamination, and host-galaxy morphology. However, such a bias cannot explain the offset seen in the MBH-sigma relation at higher redshifts. Second, while the CaT region is the cleanest to determine stellar-velocity dispersions, both the MgIb region, corrected for FeII emission, and the CaHK region, although often swamped by the AGN powerlaw continuum and emission lines, can give results accurate to within a few percent. Third, the MBH scaling relations of our pilot sample agree in slope and scatter with those of other local active and inactive galaxies. In the next papers of the series we will quantify the scaling relations, exploiting the full sample of ~100 objects.
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