Kinematic differences between NLS1 and BLAGN sources
It is well-known that the higher policyclic aromatic hydrocarbon (PAH) abundance, lower black hole mass, higher accretion rate and lower luminosities are among the major characteristics of Narrow-Line Seyfert galaxies (NLS1), when they are compared to Broad line Seyfert galaxies (BLS1). NLS1s may be...
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| creator | Lakićević, M Popović, L. Č Kovačević-Dojčinović, J |
| description | It is well-known that the higher policyclic aromatic hydrocarbon (PAH)
abundance, lower black hole mass, higher accretion rate and lower luminosities
are among the major characteristics of Narrow-Line Seyfert galaxies (NLS1),
when they are compared to Broad line Seyfert galaxies (BLS1). NLS1s may be
normal Seyfert galaxies at an early stage of evolution, their black holes may
still be growing and/or they could be special for some other reason. In this
work we discuss the findings that NLS1s have most of line and continuum
luminosities correlated with FWHM(H$\beta$), which may be the trace of their
rapid black hole mass grow. BLS1 do not show such trends. Also, PAHs may be
destroyed as the black hole grows and the starbursts are removed, for NLS1
objects. |
| doi_str_mv | 10.48550/arxiv.1808.02314 |
| format | Article |
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abundance, lower black hole mass, higher accretion rate and lower luminosities
are among the major characteristics of Narrow-Line Seyfert galaxies (NLS1),
when they are compared to Broad line Seyfert galaxies (BLS1). NLS1s may be
normal Seyfert galaxies at an early stage of evolution, their black holes may
still be growing and/or they could be special for some other reason. In this
work we discuss the findings that NLS1s have most of line and continuum
luminosities correlated with FWHM(H$\beta$), which may be the trace of their
rapid black hole mass grow. BLS1 do not show such trends. Also, PAHs may be
destroyed as the black hole grows and the starbursts are removed, for NLS1
objects.</description><identifier>DOI: 10.48550/arxiv.1808.02314</identifier><language>eng</language><subject>Physics - Astrophysics of Galaxies</subject><creationdate>2018-08</creationdate><rights>http://arxiv.org/licenses/nonexclusive-distrib/1.0</rights><oa>free_for_read</oa><woscitedreferencessubscribed>false</woscitedreferencessubscribed></display><links><openurl>$$Topenurl_article</openurl><openurlfulltext>$$Topenurlfull_article</openurlfulltext><thumbnail>$$Tsyndetics_thumb_exl</thumbnail><link.rule.ids>228,230,776,881</link.rule.ids><linktorsrc>$$Uhttps://arxiv.org/abs/1808.02314$$EView_record_in_Cornell_University$$FView_record_in_$$GCornell_University$$Hfree_for_read</linktorsrc><backlink>$$Uhttps://doi.org/10.48550/arXiv.1808.02314$$DView paper in arXiv$$Hfree_for_read</backlink></links><search><creatorcontrib>Lakićević, M</creatorcontrib><creatorcontrib>Popović, L. Č</creatorcontrib><creatorcontrib>Kovačević-Dojčinović, J</creatorcontrib><title>Kinematic differences between NLS1 and BLAGN sources</title><description>It is well-known that the higher policyclic aromatic hydrocarbon (PAH)
abundance, lower black hole mass, higher accretion rate and lower luminosities
are among the major characteristics of Narrow-Line Seyfert galaxies (NLS1),
when they are compared to Broad line Seyfert galaxies (BLS1). NLS1s may be
normal Seyfert galaxies at an early stage of evolution, their black holes may
still be growing and/or they could be special for some other reason. In this
work we discuss the findings that NLS1s have most of line and continuum
luminosities correlated with FWHM(H$\beta$), which may be the trace of their
rapid black hole mass grow. BLS1 do not show such trends. Also, PAHs may be
destroyed as the black hole grows and the starbursts are removed, for NLS1
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abundance, lower black hole mass, higher accretion rate and lower luminosities
are among the major characteristics of Narrow-Line Seyfert galaxies (NLS1),
when they are compared to Broad line Seyfert galaxies (BLS1). NLS1s may be
normal Seyfert galaxies at an early stage of evolution, their black holes may
still be growing and/or they could be special for some other reason. In this
work we discuss the findings that NLS1s have most of line and continuum
luminosities correlated with FWHM(H$\beta$), which may be the trace of their
rapid black hole mass grow. BLS1 do not show such trends. Also, PAHs may be
destroyed as the black hole grows and the starbursts are removed, for NLS1
objects.</abstract><doi>10.48550/arxiv.1808.02314</doi><oa>free_for_read</oa></addata></record> |
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| subjects | Physics - Astrophysics of Galaxies |
| title | Kinematic differences between NLS1 and BLAGN sources |
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