Open AccessWhat controls the [O iii ]λ5007 line strength in active galactic nuclei?
Author(s) -
Baskin Alexei,
Laor Ari
Publication year - 2005
Publication title -
monthly notices of the royal astronomical society
Language(s) - English
Resource type - Journals
SCImago Journal Rank - 2.058
H-Index - 383
eISSN - 1365-2966
pISSN - 0035-8711
DOI - 10.1111/j.1365-2966.2005.08841.x
Subject(s) - doubly ionized oxygen , physics , quasar , astrophysics , line (geometry) , active galactic nucleus , emission spectrum , photoionization , luminosity , galaxy , ionization , black hole (networking) , astronomy , spectral line , ion , geometry , computer network , routing protocol , mathematics , routing (electronic design automation) , quantum mechanics , link state routing protocol , computer science
Active galactic nuclei (AGN) display an extreme range in the narrow emission‐line equivalent widths. Specifically, in the Palomar–Green (PG) quasar sample, the equivalent width of the narrow [O iii ]λ5007 line has a range of >300 (<0.5 to 157 Å), while the broad Hβ line, for example, has a range of 10 only (23 to 230 Å). The strength of [O iii ]λ5007 is modulated by the covering factor (CF) of the narrow‐line region (NLR) gas, its density ( n e ) and ionization parameter ( U ). To explore which of these factors produces the observed large range in [O iii ]λ5007 strength, we measure the strength of the matching narrow Hβ and [O iii ]λ4363 lines, detected in 40 out of the 87 PG quasars with z < 0.5 in the Boroson & Green sample. The photoionization code cloudy is then used to infer CF, n e and U in each object, assuming a single uniform emitting zone. We find that the range of CF (∼0.02–0.2) contributes about twice as much as the range in both n e and U towards modulating the strength of the [O iii ]λ5007 line. The CF is inversely correlated with luminosity, but it is not correlated with L / L Edd as previously speculated. The single‐zone [O iii ]λ5007 emitting region is rather compact, having R NLR = 40 L 0.45 44 pc . These emission lines can also be fitted with an extreme two‐zone model, where [O iii ]λ4363 is mostly emitted by a dense ( n e = 10 7 cm −3 ) inner zone at R in NLR = L 0.5 44 pc , and [O iii ]λ5007 by a low‐density ( n e = 10 3 cm −3 ) extended outer zone at R out NLR = 750 L 0.34 44 pc . Such an extended [O iii ]λ5007 emission should be well resolved by Hubble Space Telescope imaging of luminous AGN. Further constraints on the radial gas distribution in the NLR can be obtained from the spectral shape of the infrared continuum emitted by the associated dust.