A Local Baseline of the Black Hole Mass Scaling Relations for Active
  Galaxies. I. Methodology and Results of Pilot Study
  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.
