2006MNRAS.367..860B

Three sets of two-component profiles are used to simultaneously model the [OIII]λλ4959, 5007 and Hβ lines for the FeII-subtracted spectra of 149 narrow-line Seyfert 1 galaxies (NLS1s) from the Sloan Digital Sky Survey (SDSS). Using the linewidth of the narrow/core component of [OIII]λ5007 to trace the stellar velocity dispersion instead of using the total linewidth of [OIII]λ5007, we found that the SDSS NLS1s are still deviated from the M_bh-σ relation found in the nearby inactive galaxies. This suggests that the linewidth of the [OIII] narrow/core component is likely not a good tracer of bulge velocity dispersion in NLS1s, since some other studies indicate that NLS1s, like other active galactic nuclei (AGN), should follow the M_bh-σ relation. If we assume that the [OIII]5007/Hβ_n_line ratio emitted in the narrow-line region (NLR) ranges from one to 10, 63 objects are found to be satisfied with this criterion, and their Hβ broad components should be used to calculate their virial black hole masses. These 63 objects are statically consistent with the M_bh-σ_[OIII] relation. With the Chandra observation of some SDSS NLS1s, we find that one of these 63 objects (J143030.22-001115.1) cannot be classified as a genuine NLS1. Its narrow component of Hβ is coming from NLRs. This is consistent with its very flat hard X-ray spectrum found by researchers.