Spectral Properties of AGN with Very Weak [O III] Lines

The spectral properties of a sample of 58 Active GalacticNuclei (AGN) spectra, in which emission [O~III] $lambdalambda$4959, 5007 AA lines are weak or totally absent, are analyzed. In order to investigate thephysical reason for the [O~III] emission suppression, the spectral propertiesof the weak [O~...
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Autor*in:	Kovacevic, J. [verfasserIn]

Format:	E-Artikel
Sprache:	Englisch

Erschienen:	2011

Schlagwörter:	Galaxies: active Galaxies: emission lines

Übergeordnetes Werk:	In: Serbian Astronomical Journal - Astronomical Observatory, Department of Astronomy, Belgrade, 2008, 182(2011), Seite 17-24
Übergeordnetes Werk:	volume:182 ; year:2011 ; pages:17-24

Links:	Link aufrufen Link aufrufen Journal toc

Katalog-ID:	DOAJ041893468

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520			\|a The spectral properties of a sample of 58 Active GalacticNuclei (AGN) spectra, in which emission [O~III] $lambdalambda$4959, 5007 AA lines are weak or totally absent, are analyzed. In order to investigate thephysical reason for the [O~III] emission suppression, the spectral propertiesof the weak [O~III] spectra sample are compared with the same properties of asample of 269 spectra with the strong [O~III] lines. The spectra are obtainedfrom Sloan Digital Sky Survey (SDSS) Database. It is found that the objectswith the weak or absent [O~III] $lambdalambda$4959, 5007 AA linesgenerally have the high continuum luminosities (log($lambda$L$_{5100}$) $<$45), that they are very rare at smaller redshifts ($z <$ 0.3) and that theyusually have strong starburst influence. From the sample with weak or absent[O~III] lines, two boundary subgroups may be distinguished: the subgroup witha strong H$beta$ narrow component and subgroup with a very weak or negligibleH$beta$ narrow component. The physical causes for the [O~III] linessuppressing are probably different in these two subgroups: the [O~III] linesare absent in objects with strong narrow H$beta$ probably because of strongstarburst (SB) activity, which produces high density of the gas, while in theobjects with the negligible narrow H$beta$, the reason for [O~III] and narrowH$beta$ suppression may be a low covering factor.
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allfields	(DE-627)DOAJ041893468 (DE-599)DOAJ23730661014b4c8595cff391d9351f77 DE-627 ger DE-627 rakwb eng QB1-991 Kovacevic, J. verfasserin aut Spectral Properties of AGN with Very Weak [O III] Lines 2011 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier The spectral properties of a sample of 58 Active GalacticNuclei (AGN) spectra, in which emission [O~III] $lambdalambda$4959, 5007 AA lines are weak or totally absent, are analyzed. In order to investigate thephysical reason for the [O~III] emission suppression, the spectral propertiesof the weak [O~III] spectra sample are compared with the same properties of asample of 269 spectra with the strong [O~III] lines. The spectra are obtainedfrom Sloan Digital Sky Survey (SDSS) Database. It is found that the objectswith the weak or absent [O~III] $lambdalambda$4959, 5007 AA linesgenerally have the high continuum luminosities (log($lambda$L$_{5100}$) $<$45), that they are very rare at smaller redshifts ($z <$ 0.3) and that theyusually have strong starburst influence. From the sample with weak or absent[O~III] lines, two boundary subgroups may be distinguished: the subgroup witha strong H$beta$ narrow component and subgroup with a very weak or negligibleH$beta$ narrow component. The physical causes for the [O~III] linessuppressing are probably different in these two subgroups: the [O~III] linesare absent in objects with strong narrow H$beta$ probably because of strongstarburst (SB) activity, which produces high density of the gas, while in theobjects with the negligible narrow H$beta$, the reason for [O~III] and narrowH$beta$ suppression may be a low covering factor. Galaxies: active Galaxies: emission lines Astronomy In Serbian Astronomical Journal Astronomical Observatory, Department of Astronomy, Belgrade, 2008 182(2011), Seite 17-24 (DE-627)538218460 (DE-600)2378699-1 18209289 nnns volume:182 year:2011 pages:17-24 https://doaj.org/article/23730661014b4c8595cff391d9351f77 kostenfrei http://saj.matf.bg.ac.rs/182/pdf/017-024.pdf kostenfrei https://doaj.org/toc/1450-698X Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ SSG-OLC-PHA GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_206 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2003 GBV_ILN_2005 GBV_ILN_2009 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2055 GBV_ILN_2111 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 182 2011 17-24
spelling	(DE-627)DOAJ041893468 (DE-599)DOAJ23730661014b4c8595cff391d9351f77 DE-627 ger DE-627 rakwb eng QB1-991 Kovacevic, J. verfasserin aut Spectral Properties of AGN with Very Weak [O III] Lines 2011 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier The spectral properties of a sample of 58 Active GalacticNuclei (AGN) spectra, in which emission [O~III] $lambdalambda$4959, 5007 AA lines are weak or totally absent, are analyzed. In order to investigate thephysical reason for the [O~III] emission suppression, the spectral propertiesof the weak [O~III] spectra sample are compared with the same properties of asample of 269 spectra with the strong [O~III] lines. The spectra are obtainedfrom Sloan Digital Sky Survey (SDSS) Database. It is found that the objectswith the weak or absent [O~III] $lambdalambda$4959, 5007 AA linesgenerally have the high continuum luminosities (log($lambda$L$_{5100}$) $<$45), that they are very rare at smaller redshifts ($z <$ 0.3) and that theyusually have strong starburst influence. From the sample with weak or absent[O~III] lines, two boundary subgroups may be distinguished: the subgroup witha strong H$beta$ narrow component and subgroup with a very weak or negligibleH$beta$ narrow component. The physical causes for the [O~III] linessuppressing are probably different in these two subgroups: the [O~III] linesare absent in objects with strong narrow H$beta$ probably because of strongstarburst (SB) activity, which produces high density of the gas, while in theobjects with the negligible narrow H$beta$, the reason for [O~III] and narrowH$beta$ suppression may be a low covering factor. Galaxies: active Galaxies: emission lines Astronomy In Serbian Astronomical Journal Astronomical Observatory, Department of Astronomy, Belgrade, 2008 182(2011), Seite 17-24 (DE-627)538218460 (DE-600)2378699-1 18209289 nnns volume:182 year:2011 pages:17-24 https://doaj.org/article/23730661014b4c8595cff391d9351f77 kostenfrei http://saj.matf.bg.ac.rs/182/pdf/017-024.pdf kostenfrei https://doaj.org/toc/1450-698X Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ SSG-OLC-PHA GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_206 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2003 GBV_ILN_2005 GBV_ILN_2009 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2055 GBV_ILN_2111 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 182 2011 17-24
allfields_unstemmed	(DE-627)DOAJ041893468 (DE-599)DOAJ23730661014b4c8595cff391d9351f77 DE-627 ger DE-627 rakwb eng QB1-991 Kovacevic, J. verfasserin aut Spectral Properties of AGN with Very Weak [O III] Lines 2011 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier The spectral properties of a sample of 58 Active GalacticNuclei (AGN) spectra, in which emission [O~III] $lambdalambda$4959, 5007 AA lines are weak or totally absent, are analyzed. In order to investigate thephysical reason for the [O~III] emission suppression, the spectral propertiesof the weak [O~III] spectra sample are compared with the same properties of asample of 269 spectra with the strong [O~III] lines. The spectra are obtainedfrom Sloan Digital Sky Survey (SDSS) Database. It is found that the objectswith the weak or absent [O~III] $lambdalambda$4959, 5007 AA linesgenerally have the high continuum luminosities (log($lambda$L$_{5100}$) $<$45), that they are very rare at smaller redshifts ($z <$ 0.3) and that theyusually have strong starburst influence. From the sample with weak or absent[O~III] lines, two boundary subgroups may be distinguished: the subgroup witha strong H$beta$ narrow component and subgroup with a very weak or negligibleH$beta$ narrow component. The physical causes for the [O~III] linessuppressing are probably different in these two subgroups: the [O~III] linesare absent in objects with strong narrow H$beta$ probably because of strongstarburst (SB) activity, which produces high density of the gas, while in theobjects with the negligible narrow H$beta$, the reason for [O~III] and narrowH$beta$ suppression may be a low covering factor. Galaxies: active Galaxies: emission lines Astronomy In Serbian Astronomical Journal Astronomical Observatory, Department of Astronomy, Belgrade, 2008 182(2011), Seite 17-24 (DE-627)538218460 (DE-600)2378699-1 18209289 nnns volume:182 year:2011 pages:17-24 https://doaj.org/article/23730661014b4c8595cff391d9351f77 kostenfrei http://saj.matf.bg.ac.rs/182/pdf/017-024.pdf kostenfrei https://doaj.org/toc/1450-698X Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ SSG-OLC-PHA GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_206 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2003 GBV_ILN_2005 GBV_ILN_2009 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2055 GBV_ILN_2111 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 182 2011 17-24
allfieldsGer	(DE-627)DOAJ041893468 (DE-599)DOAJ23730661014b4c8595cff391d9351f77 DE-627 ger DE-627 rakwb eng QB1-991 Kovacevic, J. verfasserin aut Spectral Properties of AGN with Very Weak [O III] Lines 2011 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier The spectral properties of a sample of 58 Active GalacticNuclei (AGN) spectra, in which emission [O~III] $lambdalambda$4959, 5007 AA lines are weak or totally absent, are analyzed. In order to investigate thephysical reason for the [O~III] emission suppression, the spectral propertiesof the weak [O~III] spectra sample are compared with the same properties of asample of 269 spectra with the strong [O~III] lines. The spectra are obtainedfrom Sloan Digital Sky Survey (SDSS) Database. It is found that the objectswith the weak or absent [O~III] $lambdalambda$4959, 5007 AA linesgenerally have the high continuum luminosities (log($lambda$L$_{5100}$) $<$45), that they are very rare at smaller redshifts ($z <$ 0.3) and that theyusually have strong starburst influence. From the sample with weak or absent[O~III] lines, two boundary subgroups may be distinguished: the subgroup witha strong H$beta$ narrow component and subgroup with a very weak or negligibleH$beta$ narrow component. The physical causes for the [O~III] linessuppressing are probably different in these two subgroups: the [O~III] linesare absent in objects with strong narrow H$beta$ probably because of strongstarburst (SB) activity, which produces high density of the gas, while in theobjects with the negligible narrow H$beta$, the reason for [O~III] and narrowH$beta$ suppression may be a low covering factor. Galaxies: active Galaxies: emission lines Astronomy In Serbian Astronomical Journal Astronomical Observatory, Department of Astronomy, Belgrade, 2008 182(2011), Seite 17-24 (DE-627)538218460 (DE-600)2378699-1 18209289 nnns volume:182 year:2011 pages:17-24 https://doaj.org/article/23730661014b4c8595cff391d9351f77 kostenfrei http://saj.matf.bg.ac.rs/182/pdf/017-024.pdf kostenfrei https://doaj.org/toc/1450-698X Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ SSG-OLC-PHA GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_206 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2003 GBV_ILN_2005 GBV_ILN_2009 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2055 GBV_ILN_2111 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 182 2011 17-24
allfieldsSound	(DE-627)DOAJ041893468 (DE-599)DOAJ23730661014b4c8595cff391d9351f77 DE-627 ger DE-627 rakwb eng QB1-991 Kovacevic, J. verfasserin aut Spectral Properties of AGN with Very Weak [O III] Lines 2011 Text txt rdacontent Computermedien c rdamedia Online-Ressource cr rdacarrier The spectral properties of a sample of 58 Active GalacticNuclei (AGN) spectra, in which emission [O~III] $lambdalambda$4959, 5007 AA lines are weak or totally absent, are analyzed. In order to investigate thephysical reason for the [O~III] emission suppression, the spectral propertiesof the weak [O~III] spectra sample are compared with the same properties of asample of 269 spectra with the strong [O~III] lines. The spectra are obtainedfrom Sloan Digital Sky Survey (SDSS) Database. It is found that the objectswith the weak or absent [O~III] $lambdalambda$4959, 5007 AA linesgenerally have the high continuum luminosities (log($lambda$L$_{5100}$) $<$45), that they are very rare at smaller redshifts ($z <$ 0.3) and that theyusually have strong starburst influence. From the sample with weak or absent[O~III] lines, two boundary subgroups may be distinguished: the subgroup witha strong H$beta$ narrow component and subgroup with a very weak or negligibleH$beta$ narrow component. The physical causes for the [O~III] linessuppressing are probably different in these two subgroups: the [O~III] linesare absent in objects with strong narrow H$beta$ probably because of strongstarburst (SB) activity, which produces high density of the gas, while in theobjects with the negligible narrow H$beta$, the reason for [O~III] and narrowH$beta$ suppression may be a low covering factor. Galaxies: active Galaxies: emission lines Astronomy In Serbian Astronomical Journal Astronomical Observatory, Department of Astronomy, Belgrade, 2008 182(2011), Seite 17-24 (DE-627)538218460 (DE-600)2378699-1 18209289 nnns volume:182 year:2011 pages:17-24 https://doaj.org/article/23730661014b4c8595cff391d9351f77 kostenfrei http://saj.matf.bg.ac.rs/182/pdf/017-024.pdf kostenfrei https://doaj.org/toc/1450-698X Journal toc kostenfrei GBV_USEFLAG_A SYSFLAG_A GBV_DOAJ SSG-OLC-PHA GBV_ILN_11 GBV_ILN_20 GBV_ILN_22 GBV_ILN_23 GBV_ILN_24 GBV_ILN_31 GBV_ILN_39 GBV_ILN_40 GBV_ILN_60 GBV_ILN_62 GBV_ILN_63 GBV_ILN_65 GBV_ILN_69 GBV_ILN_70 GBV_ILN_73 GBV_ILN_95 GBV_ILN_105 GBV_ILN_110 GBV_ILN_151 GBV_ILN_161 GBV_ILN_170 GBV_ILN_206 GBV_ILN_213 GBV_ILN_230 GBV_ILN_285 GBV_ILN_293 GBV_ILN_370 GBV_ILN_602 GBV_ILN_2003 GBV_ILN_2005 GBV_ILN_2009 GBV_ILN_2011 GBV_ILN_2014 GBV_ILN_2055 GBV_ILN_2111 GBV_ILN_4012 GBV_ILN_4037 GBV_ILN_4112 GBV_ILN_4125 GBV_ILN_4126 GBV_ILN_4249 GBV_ILN_4305 GBV_ILN_4306 GBV_ILN_4307 GBV_ILN_4313 GBV_ILN_4322 GBV_ILN_4323 GBV_ILN_4324 GBV_ILN_4325 GBV_ILN_4335 GBV_ILN_4338 GBV_ILN_4367 GBV_ILN_4700 AR 182 2011 17-24
language	English
source	In Serbian Astronomical Journal 182(2011), Seite 17-24 volume:182 year:2011 pages:17-24
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callnumber-first	Q - Science
author	Kovacevic, J.
spellingShingle	Kovacevic, J. misc QB1-991 misc Galaxies: active misc Galaxies: emission lines misc Astronomy Spectral Properties of AGN with Very Weak [O III] Lines
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topic_title	QB1-991 Spectral Properties of AGN with Very Weak [O III] Lines Galaxies: active Galaxies: emission lines
topic	misc QB1-991 misc Galaxies: active misc Galaxies: emission lines misc Astronomy
topic_unstemmed	misc QB1-991 misc Galaxies: active misc Galaxies: emission lines misc Astronomy
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title	Spectral Properties of AGN with Very Weak [O III] Lines
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title_full	Spectral Properties of AGN with Very Weak [O III] Lines
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title_sort	spectral properties of agn with very weak [o iii] lines
callnumber	QB1-991
title_auth	Spectral Properties of AGN with Very Weak [O III] Lines
abstract	The spectral properties of a sample of 58 Active GalacticNuclei (AGN) spectra, in which emission [O~III] $lambdalambda$4959, 5007 AA lines are weak or totally absent, are analyzed. In order to investigate thephysical reason for the [O~III] emission suppression, the spectral propertiesof the weak [O~III] spectra sample are compared with the same properties of asample of 269 spectra with the strong [O~III] lines. The spectra are obtainedfrom Sloan Digital Sky Survey (SDSS) Database. It is found that the objectswith the weak or absent [O~III] $lambdalambda$4959, 5007 AA linesgenerally have the high continuum luminosities (log($lambda$L$_{5100}$) $<$45), that they are very rare at smaller redshifts ($z <$ 0.3) and that theyusually have strong starburst influence. From the sample with weak or absent[O~III] lines, two boundary subgroups may be distinguished: the subgroup witha strong H$beta$ narrow component and subgroup with a very weak or negligibleH$beta$ narrow component. The physical causes for the [O~III] linessuppressing are probably different in these two subgroups: the [O~III] linesare absent in objects with strong narrow H$beta$ probably because of strongstarburst (SB) activity, which produces high density of the gas, while in theobjects with the negligible narrow H$beta$, the reason for [O~III] and narrowH$beta$ suppression may be a low covering factor.
abstractGer	The spectral properties of a sample of 58 Active GalacticNuclei (AGN) spectra, in which emission [O~III] $lambdalambda$4959, 5007 AA lines are weak or totally absent, are analyzed. In order to investigate thephysical reason for the [O~III] emission suppression, the spectral propertiesof the weak [O~III] spectra sample are compared with the same properties of asample of 269 spectra with the strong [O~III] lines. The spectra are obtainedfrom Sloan Digital Sky Survey (SDSS) Database. It is found that the objectswith the weak or absent [O~III] $lambdalambda$4959, 5007 AA linesgenerally have the high continuum luminosities (log($lambda$L$_{5100}$) $<$45), that they are very rare at smaller redshifts ($z <$ 0.3) and that theyusually have strong starburst influence. From the sample with weak or absent[O~III] lines, two boundary subgroups may be distinguished: the subgroup witha strong H$beta$ narrow component and subgroup with a very weak or negligibleH$beta$ narrow component. The physical causes for the [O~III] linessuppressing are probably different in these two subgroups: the [O~III] linesare absent in objects with strong narrow H$beta$ probably because of strongstarburst (SB) activity, which produces high density of the gas, while in theobjects with the negligible narrow H$beta$, the reason for [O~III] and narrowH$beta$ suppression may be a low covering factor.
abstract_unstemmed	The spectral properties of a sample of 58 Active GalacticNuclei (AGN) spectra, in which emission [O~III] $lambdalambda$4959, 5007 AA lines are weak or totally absent, are analyzed. In order to investigate thephysical reason for the [O~III] emission suppression, the spectral propertiesof the weak [O~III] spectra sample are compared with the same properties of asample of 269 spectra with the strong [O~III] lines. The spectra are obtainedfrom Sloan Digital Sky Survey (SDSS) Database. It is found that the objectswith the weak or absent [O~III] $lambdalambda$4959, 5007 AA linesgenerally have the high continuum luminosities (log($lambda$L$_{5100}$) $<$45), that they are very rare at smaller redshifts ($z <$ 0.3) and that theyusually have strong starburst influence. From the sample with weak or absent[O~III] lines, two boundary subgroups may be distinguished: the subgroup witha strong H$beta$ narrow component and subgroup with a very weak or negligibleH$beta$ narrow component. The physical causes for the [O~III] linessuppressing are probably different in these two subgroups: the [O~III] linesare absent in objects with strong narrow H$beta$ probably because of strongstarburst (SB) activity, which produces high density of the gas, while in theobjects with the negligible narrow H$beta$, the reason for [O~III] and narrowH$beta$ suppression may be a low covering factor.
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title_short	Spectral Properties of AGN with Very Weak [O III] Lines
url	https://doaj.org/article/23730661014b4c8595cff391d9351f77 http://saj.matf.bg.ac.rs/182/pdf/017-024.pdf https://doaj.org/toc/1450-698X
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Spectral Properties of AGN with Very Weak [O III] Lines

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