2004/09/22 by Kentaro Aoki, Toshihiro Kawaguchi, Kouji Ohta · 2 citations
Physics and Astronomy · #Accretion (finance) #Active galactic nucleus #Astronomy #Astrophysical Phenomena and Observations #Astrophysics #Blueshift #Doubly ionized oxygen #Emission spectrum #Galaxies: Formation, Evolution, Phenomena #Galaxy #Gamma-ray bursts and supernovae #Line (geometry) #Luminosity #Optics #Photoluminescence #Physics #Quasar #Redshift #Spectral line #astro-ph
paper · pdf · doi:10.1086/426075
published as Astrophys.J. 618 (2005) 601-608 · Accepted for publication in The Astrophysical Journal
arxiv created 2004/09/22 · openalex publication_date 2005/01/10 · arxiv updated 2009/12/01 · openalex created_date 2016/06/24 · openalex updated_date 2026/08/05
We have obtained optical intermediate-resolution spectra ( R = 3000) of the narrow-line quasars DMS 0059-0055 and PG 1543+489. The [O III] emission line in DMS 0059-0055 is blueshifted by 880 km s -1 relative to Hβ. We also confirm that the [O III] emission line in PG 1543+489 has a relative blueshift of 1150 km s -1 . These two narrow-line quasars show the largest [O III] blueshifts known to date among type 1 active galactic nuclei (AGNs). The [O III] emission lines in both objects are broad (1000-2000 km s -1 ), and those in DMS 0059-0055 show strong blue asymmetry. We interpret the large blueshift and the profile of the [O III] lines as the result of an outflow interacting with circumnuclear gas. Among type 1 AGNs with large blueshifted [O III], there is no correlation between the Eddington ratios and the amount of [O III] blueshift. Combining our new data with published results, we confirm that the Eddington ratios of such AGNs are the highest among AGNs with the same black hole mass. These facts suggest that the Eddington ratio is a necessary condition for [O III] blueshifts or that the [O III] blueshifts weakly depend on the Eddington ratio. Our new sample suggests that there are possibly other necessary conditions to produce an outflow than a high Eddington ratio: a large black hole mass (>10 7 M ☉ ), a high mass accretion rate (>2 M ☉ yr -1 ), or a large luminosity [λ L λ (5100 Å) > 10 44.6 ergs s -1 ].