Examples of AGN’ in a sentence
We highlight RG J0332 2732 and SMM J0332 2732 as ‘candidate AGN’ (open red squares) since there is some evidence that the velocity fields may be partially affected by AGN given their high values of [N II]/Hα (Section 3.3).
We note that the [O III] luminosities of our VLBI detections are in the range 106–2 107 L , consistent with the ‘weak AGN’ classification of Kauffmann et al.
Next, we calculate the error-weighted mean and standard deviation of the relevant q pa- rameter, noting points that deviate from the mean by more than 3σ (these being ‘radio-excess AGN’ candidates, as described by Donley et al.
The ‘No AGN’ model, which has the same cold, purely kinetic winds as the Fiducial model, has 60–85 per cent of all metals in the CGM in the cool-dense phase.The role of wind-heating in the CGM mass and metal budgets is complex.
The ‘No AGN’ simulation retains the same galactic wind scheme but does not include AGN feedback.
The full definitions of ’MIR-dominated’ and ’X-ray AGN’ are given in §9.
Downloaded from https://academic.oup.com/mnras/article/502/4/5593/6133466 by guest on 16 August 2022 For the power spectrum, the suppression at scales 1000 4 5000 seen in нTNG is comparable to that from Horizon-AGN, BAHAMAS ‘low AGN’, and HMcode REF.
A more meaningful measure is to select ‘radio AGN’ by assessing if the observed radio emission is dominated by star formation or by the AGN (e.g. Moric´ et al.
As part of the Spitzer snapshot program ‘Clusters Around Radio-loud AGN’ (CARLA), we observed the fields of 209 high-redshift radio galaxies (HzRGs) and 211 RLQs at 1.3 < z < 3.2. A description of the sample selection, observation strategy, data reduction, source ex- traction, determination of completeness limits and initial scientific results are given in Wylezalek et al.
We finally note that for sources with SSil < 2, both the AGN fraction and AGN luminosity should be considered as upper limits, because the ‘obscured AGN’ templates could be composite sources.Finally, we also performed the spectral decomposition of the Spitzer/IRS spectra of the IR-bright galaxy and quasar samples.