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 must be reexamined if we predict that NLS1s harbor fast rising small SMBH with excessive accretion charge. Contemplating the effects of the random velocity and the inclination in SMBH mass estimation of NLS1s, Decarli et al. 2008) find that these effects would enhance the mass for NLS1s by 0.84 dex, which can account for the mass distinction between NLS1s and BLS1s.
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2005; Barth et al. POSTSUBSCRIPT is essential. The central SMBH mass in AGNs is a key parameter to know the nuclear power mechanism as properly as 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 also a query for other sorts 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 equivalent width (EW) of BC for our 209 NLS1s in pattern B is 19.4±8.6plus (Learn Even more Here)-or-minus19.48.619.4pm 8.619.Four ± 8.6Å and 16.1±8.0plus (www.pipihosa.com/2018/06/29/4184665-little-known-oil-stock-outperformed-dividend-aristocrats/)-or-minus16.18.016.1pm 8.016.1 ± 8.0Å for IC EW. 1994; Rodriguez-Ardila et al. There is no such thing as a correlation between them. For 12 NLS1s, Dietrich et al. 2005), and it’s urged that BC and IC are emitted from two distinct emission area.
We select objects by the next criteria: (1) the sign-to-noise ratio (S/N) is larger than 15. The S/N is measured within the wavelength 4800-5040Å, overlaying the range for line-fitting. POSTSUBSCRIPT. Then we visually check these spectra one by one. In the long run, we’ve got a pattern of 329 NLS1s. Then we use the strategy of Peterson et al. 30%. The primary criterion results in about 900 NLS1s. BLR at the same time. POSTSUBSCRIPT is calculated from the error of FWHM for BC and IC in the line fit.
2004). POSTSUBSCRIPT relation. Make the mass deviation smaller by 0.19 dex.19 dex. 2005). If these 23 NLS1s follow the Tremaine et al. 2006) have some objects that can’t be labeled by NLS1s. POSTSUBSCRIPT relation present in inactive galaxies. 11.1. It is possible that the sample of Zhou et al. It is possible that there exists true NLS1s with fast growing small SMBH. 2005, their figure 3), though it’s not the case for the sample of Greene & Ho (2006) (also see Barth et al.