Intermediate inclinations of type 2 Coronal-Line Forest AGN

Rose, M.; Elvis, M.; Crenshaw, M.; Glidden, Ana

doi:10.1093/mnrasl/slv056

Cited by 15 publications

(26 citation statements)

References 17 publications

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“…Among more face-on galaxies (b/a < 0.6), we do not always detect H i; when we detect H i the absorption lines can have lower column densities than in edgeon sources. When a source is 4.6 µm bright, the WISE colours (W2-W4) allow us to estimate the orientation of the circumnuclear dust with respect to the AGN (Crenshaw et al 2000;Fischer et al 2014;Rose et al 2015). Among the 42 4.6 µm bright sources of our sample, 28 have W2-W4< 6, which suggests an unobscured AGN, i.e.…”

Section: Dmentioning

confidence: 96%

Kinematics and physical conditions of H i in nearby radio sources

Maccagni

Morganti

Oosterloo

et al. 2017

A&A

222

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We present an analysis of the properties of neutral hydrogen (H i) in 248 nearby (0.02 < z < 0.25) radio galaxies with S 1.4 GHz > 30 mJy and for which optical spectroscopy is available. The observations were carried out with the Westerbork Synthesis Radio Telescope as the last large project before the upgrade of the telescope with phased array feed receivers (Apertif). The sample covers almost four orders of magnitude in radio power from log P 1.4 GHz = 22.5 W Hz −1 and 26.2 W Hz −1 . We detect H i in absorption in 27% ± 5.5% of the objects. The detections are found over the full range of radio power. However, the distribution and kinematics of the absorbing H i gas appear to depend on radio power, the properties of the radio continuum emission, and the dust content of the sources. Among the sources where H i is detected, gas with kinematics deviating from regular rotation is more likely found as the radio power increases. In the great majority of these cases, the H i profile is asymmetric with a significant blue-shifted component. This is particularly common for sources with log P 1.4 GHz > 24 W Hz −1 , where the radio emission is small, possibly because these radio sources are young. The same is found for sources that are bright in the mid-infrared, i.e. sources rich in heated dust. In these sources, the H i is outflowing likely under the effect of the interaction with the radio emission. Conversely, in dust-poor galaxies, and in sources with extended radio emission, at all radio powers we only detect H i distributed in a rotating disk. Stacking experiments show that in sources for which we do not detect H i in absorption directly, the H i has a column density that is lower than 3.5 × 10 17 (T spin /c f ) cm −2 . We use our results to predict the number and type of H i absorption lines that will be detected by the upcoming surveys of the Square Kilometre Array precursors and pathfinders (Apertif, MeerKAT, and ASKAP).

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Section: Dmentioning

confidence: 96%

Kinematics and physical conditions of H i in nearby radio sources

Maccagni

Morganti

Oosterloo

et al. 2017

A&A

222

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“…Rose et al (2015a) argue that even in the classical unification model with a toroidal obscuring region, a small fraction of viewing directions might result in both strong coronal lines and obscured broad-line region (another such example from the Reyes et al 2008 sample is analyzed by Villar-Martín et al 2011). This picture is consistent with the distribution of dust temperatures in these objects and in type 2 quasars, in that coronal-line AGNs are warmer as inferred from the infrared colors than are other type 2 quasars.…”

Section: [O Iii] Properties and Bolometric Luminositymentioning

confidence: 99%

Spectroscopic identification of type 2 quasars atz< 1 in SDSS-III/BOSS

Yuan

Strauss

Zakamska

2016

Mon. Not. R. Astron. Soc.

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The physics and demographics of type 2 quasars remain poorly understood, and new samples of such objects selected in a variety of ways can give insight into their physical properties, evolution, and relationship to their host galaxies. We present a sample of 2758 type 2 quasars at z 1 from the SDSS-III/BOSS spectroscopic database, selected on the basis of their emission-line properties. We probe the luminous end of the population by requiring the rest-frame equivalent width of [O III] to be > 100Å. We distinguish our objects from star-forming galaxies and type 1 quasars using line widths, standard emission line ratio diagnostic diagrams at z < 0.52 and detection of [Ne V]λ3426Å at z > 0.52.

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“…The computed inclinations of the type 1 AGNs studied in Fischer et al (2013) are clearly pole-on (á ñ = + -i 15 5 degrees) when compared to type 2 AGNs (á ñ = + -i 63 4 degrees). Interestingly, there is a lack of AGNs with inclinations that are intermediate between these distributions (Rose et al 2015b). Using WISE (W2-W4) colors as a proxy for the AGN inclination, Rose et al (2015b) showed that type 2 CLiF AGNs seem to have inclinations which are intermediate between typical type 1 and 2 AGNs.…”

Section: Clif Inclination Anglesmentioning

confidence: 99%

“…To support this, RET15 showed that the coronal line emitting region lies at a distance approximately equal to the dust sublimation radius, that is, the boundary of the inner torus wall (Suganuma et al 2006). Rose et al (2015b) employed the Fischer et al (2014) relation between inclination angle and mid-IR color to show that type 2 CLiF AGNs lie at angles intermediate between type 1 and type 2 AGNs.…”

Section: Introductionmentioning

confidence: 99%

A MODEL FOR TYPE 2 CORONAL LINE FOREST (CLiF) AGNs

Glidden

Rose

Elvis

et al. 2016

ApJ

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We present a model for the classification of Coronal Line Forest Active Galactic Nuclei (CLiF AGNs). CLiF AGNs are of special interest due to their remarkably large number of emission lines, especially forbidden highionization lines (FHILs). Rose et al. suggest that their emission is dominated by reflection from the inner wall of the obscuring region rather than direct emission from the accretion disk. This makes CLiF AGNs laboratories to test AGN-torus models. Modeling an AGN as an accreting supermassive black hole surrounded by a cylinder of dust and gas, we show a relationship between the viewing angle and the revealed area of the inner wall. From the revealed area, we can determine the amount of FHIL emission at various angles. We calculate the strength of [Fe VII]λ6087 emission for a number of intermediate angles (30°, 40°, and 50°) and compare the results with the luminosity of the observed emission line from six known CLiF AGNs. We find that there is good agreement between our model and the observational results. The model also enables us to determine the relationship between the type 2:type 1 AGN fraction vs the ratio of torus height to radius, h/r.

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Intermediate inclinations of type 2 Coronal-Line Forest AGN

Cited by 15 publications

References 17 publications

Kinematics and physical conditions of H i in nearby radio sources

Kinematics and physical conditions of H i in nearby radio sources

Spectroscopic identification of type 2 quasars atz< 1 in SDSS-III/BOSS

A MODEL FOR TYPE 2 CORONAL LINE FOREST (CLiF) AGNs

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