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Дата изменения: Mon Dec 23 18:23:59 2013 Дата индексирования: Fri Feb 28 17:29:38 2014 Кодировка: Поисковые слова: dark nebula |
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Catalogue of agn classification |
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In April 2009, the table contained 88707 objects with activity classification.
In the work we have made some differences regarding to VCV-12 catalogue:
(i) For the moment, some objects from VCV-12 are still not cross-identified in HyperLeda;
(ii) For all "types" of BL which exist in VCV-12 (BL, BL?, blank and ? ) we have use the flag BL;
(iii) We denoted as Q all objects brighter than absolute magnitude Mabs=23;
AGNCLASS | DESCRIPTION |
Q | Quasi-stellar objects. Have very high luminosities (Mabs<-23) and broad emission lines (FWHM=5,000- 30,000km/s) with a large red-shift ( VCV-12 ). |
BL | BL Lacertae type object. No emission or absorption lines deeper than ~ 2% are seen in any part of the optical spectrum, or only extremely week absorption and/or emission lines are observed, as a rule at minimum of their very highly variable phase. So that their redshifts can only be determined from features in the spectral of their host galaxies. They show polarization and are strong radio sources ( Lawrence 1987 , ,Miller et al. 1978). |
HP | Hight polarized objects ( VCV-12 ). |
S1 | Broad-line Seyfert 1. Have broad permitted Balmer HI lines (FWHM=1000-10000km/s, typical is 2000-6000km/s) and narrow forbidden lines (FWHM=300-1000km/s). Physically are the same objects as QSOs, but having smaller luminosities (Mabs>-23). According to Winkler (1992),Hb/[OIII]5007>5.0. |
S1n | Narrow-line Seyfert 1. Defined by Osterbrock & Pogge (1985) as soft X-ray sources, having narrow permitted lines only slightly broader than the forbidden ones; many FeI, FeII, FeIII, and often strong [FeVII] and [FeX] emission lines present, unlike what is seen in Seyfert 2s. FWHM(Hb)<2000km/s ( Goodrich 1989). |
S1i | S1 with a broad Paschen Hbeta line, indicating the presence of a highly reddened BLR ( Goodrich et al. 1994 ). |
S1h | S2 which show S1 like spectra in polarized light ( Antonucci & Miller 1985 ; Miller & Goodrich 1990 ; Tran et al. 1992 ). |
S2 | Show relatively narrow (compared to S1) emission in both permitted Balmer and forbidden lines, with almost the same FWHM, typically in the range of 300-1000 km/s. No broad component is visible. A secondary classification criterion is [OIII]5007/Hb>=3 , to distinguish against S1n ( Khachikian & Weedman 1974 , Veilleux and Osterbrock 1987 , Lawrence 1987 ). |
S2? | Probable S2 galaxy ( VCV-12 ). |
S1.2 | AGN which share parameters that are intermediate between those of classical Sy1 and Sy2 galaxies. According to Winkler (1992) , 2.0<Hb/[OIII]5007<5.0. Often related to S1n. |
S1.5 | AGN which share parameters that are intermediate between those of classical Sy1 and Sy2 galaxies; have easily discernible narrow HI profile superposed on broad wings. According to Winkler (1992), 0.333<Hb/[OIII]5007<2.0. |
S1.8 | AGN which share parameters that are intermediate between those of classical Sy1 and Sy2 galaxies; have relatively weak broad Ha and Hb components superposed on strong narrow lines. According to Winkler (1992), Hb/[OIII]5007<0.333. |
S1.9 | AGN which share parameters that are intermediate between those of classical Sy1 and Sy2 galaxies; have relatively weak broad Ha component superposed on a strong narrow line. The broad component of Hb is not seen. According to Winkler (1992), Hb/[OIII]5007<0.333. |
S | AGN objects without classification ( VCV-12). |
S? | Possibly Seyfert galaxies ( VCV-12 ). |
S3 | LINERS or Low-Ionization Nuclear Emission-line Region. Introduced by Heckman (1980) , they are low activity AGN. Have S2-like spectra with relatively strong low-ionization lines (OI,OII). I([OII]3727)/I([OIII]5007)>=1,I([OI]6300)/I([OIII]5007)>=1/3. [NII]6584/Ha>0.6 . |
S3b | S3 with broad Balmer lines ( Ho, Filippenko & Sargent 1997 ). |
S3h | S3 with broad Balmer lines seen only in polarized light ( VCV-12 ). |
H2 | Extragalactic HII regions. Have spectra with strong narrow (FWHM<=300km/s) emission line spectrum, but with a ratio [OIII]/Hb>=3 and ([NII]6584/)Ha<0.5, coupled with a blue continuum ( Veilleux and Osterbrock 1987). |
SB | Starburst nuclei or Starburst. The major observable feature that distinguishes SB form Sy is their strong narrow emission lines (FWHM<=300km/s). According to Balzano (1983), SB is a spiral galaxy with a bright, blue nucleus that emits a strong narrow emission line spectrum similar to low-ionization HII region spectra. They have strong, narrow (FWHM<=250km/s) low-ionization ([OIII]/Hb<3) emission lines. Absolute luminosities are -17.5>M>-22.5. Characterized them conspicuous stellar or semistellar nuclei. |
em | Object with emission line spectrum. No further precision. |
HyperLeda | Questions: leda@univ-lyon1.fr |