2006) have some objects that should not be labeled as NLS1s. 5007 from NLRs is commonly taken to be around 10% (e.g. Osterbrock & Pogge 1985; McGill et al. The definition of NLS1s should be reexamined if we think that NLS1s harbor fast growing small SMBH with high accretion fee. Contemplating the consequences of the random velocity and the inclination in SMBH mass estimation of NLS1s, Decarli et al. 2008) find that these effects would improve the mass for NLS1s by 0.Eighty four dex, which may account for the mass difference between NLS1s and BLS1s.
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2005; Barth et al. POSTSUBSCRIPT is very important. The central SMBH mass in AGNs is a key parameter to understand the nuclear energy mechanism as properly because the cosmic formation and evolution of SMBHs and their host galaxies (e.g. Rees 1984; Gebhardt et al. 2000; Greene & Ho 2006; Shen et al. 2005; Watson Mathur & Grupe 2007; Ryan et al. 2000; Ferrarese & Merrit 2000; Tremaine et al. POSTSUBSCRIPT (e.g., Kaspi et al. 2007; Komossa & Xu 2007). It remains additionally a question for other forms of AGNs (e.g., Nelson et al. 2008; Woo et al.
1998; Wills et al., 1993; Brotherton et al. 2000; Leighly 2004; Dietrich et al. FWHM in NLS1s. The equal width (EW) of BC for our 209 NLS1s in pattern B is 19.4±8.6plus-or-minus19.48.619.4pm 8.619.Four ± 8.6Å and 16.1±8.0plus-or-minus16.18.016.1pm 8.016.1 ± 8.0Å for IC EW. 1994; Rodriguez-Ardila et al. There isn’t a correlation between them. For 12 NLS1s, Dietrich et al. 2005), and it is steered that BC and IC are emitted from two distinct emission region.
We select objects by the next criteria: (1) the signal-to-noise ratio (S/N) is larger than 15. The S/N is measured in the wavelength 4800-5040Å, covering the range for line-fitting. POSTSUBSCRIPT. Then we visually test these spectra one after the other. In the long run, we have now a sample of 329 NLS1s. Then we use the strategy of Peterson et al. 30%. The first criterion leads to about 900 NLS1s. BLR at the same time. POSTSUBSCRIPT is calculated from the error of FWHM for BC and IC in the road match.
2004). POSTSUBSCRIPT relation. Make the mass deviation smaller by 0.19 dex.19 dex. 2005). If these 23 NLS1s comply with the Tremaine et al. 2006) have some objects that can’t be categorized by NLS1s. POSTSUBSCRIPT relation found in inactive galaxies. 11.1. It is feasible that the pattern of Zhou et al. It is feasible that there exists true NLS1s with fast growing small SMBH. 2005, their determine 3), although it’s not the case for the sample of Greene & Ho (2006) (also see Barth et al.
