tokens: the motivation for the selection of the volume for LASr. Next, we require a galaxy parent sample highly complete in terms of galaxies sufficiently massive to host an AGN, which can then be used to select AGN from. We will see that current local galaxy samples do not fulfil this criterion so that we have to assemble our own galaxy parent sample. Finally, we describe the assembly of the galaxy properties relevant for this work, namely the coordinates, redshifts, and distances, allowing us to find the MIR counterparts of the galactic nuclei and compute their luminosities. 2.1 Selection of the volume We wish to construct a highly complete census of SMBH growth in the local Universe. The choice of volume to be used for this purpose is motivated by several factors. In order to obtain a census that is representative for the whole AGN population, the volume needs to be representative of the larger scale, low redshift Universe. It is estimated that cosmological isotropy is reached for length scales of ∼200 h −1 Mpc with h = H 0 /100 km s −1 Mpc −1 and H 0 the Hubble constant (Sarkar, Pandey Khatri 2019 ). The volume should also be large enough to sample rarer AGN sub-populations in sufficient numbers to yield statistically robust conclusions on their relevance. Here particular emphasis should be on the high luminosity AGN regime because these may dominate the integrated black hole growth and AGN feedback (e.g. Aird et al. 2010 ; Fabian 2012 ). However, high-luminosity AGN have a low space density. For example, current estimates of the AGN luminosity function in X-rays, e.g. Aird et al. ( 2015 ), let us expect a space density of Mpc −3 for AGN with an intrinsic X-ray luminosity of , e.g. ∼20 objects within a sphere of 200 Mpc radius. On the other hand, the volume should be small enough so that the depth of the all-sky surveys, used to identify and characterize the AGN, is sufficient to probe the lower parts of the AGN luminosity range. This is particularly important in the X-rays where extinction is large for obscured AGN. For example, the final all-sky maps of eROSITA and ART-XC are expected to have depths of and at 2–10 keV, respectively (Merloni et al. 2012 ; Pavlinsky et al. 2018 ), which corresponds to a distance of 150–250 Mpc for an observed X-ray luminosity of . However, CT AGN are suppressed by easily a factor of 10 to ∼100 at these wavelengths. The MIR is much less affected by extinction, but sensitivity is the key restricting factor, i.e. the WISE all-sky maps have an average depth capable of detecting an AGN with a 12 luminosity up to a distance of 220 Mpc with ≥3σ in band 3 (W3∼11.6 mag; WISE documentation 1 ). Another factor to take into account is that the completeness of our parent sample of galaxies directly restricts the completeness of our AGN search. According to a recent estimate, our all-sky redshift completeness is only for galaxies with a redshift z 0.03 (Kulkarni, Perley Miller 2018 ), and the completeness is quickly
ner_tags: O O O O O O O O O B-Survey O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObjectRegion I-CelestialObjectRegion O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-CelestialObjectRegion I-CelestialObjectRegion I-CelestialObjectRegion O O O O O O O O O O O O O O O O O B-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula I-Formula O B-Model I-Model O B-Model I-Model B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation O O O O O O O O O O O O O O O O O O O B-Wavelength O B-Citation I-Citation I-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O O O B-Wavelength O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Wavelength O O O O O O O O O O O O O O B-Instrument O B-Telescope O O O O O O O O B-Wavelength I-Wavelength O B-Citation I-Citation I-Citation I-Citation O B-Citation I-Citation I-Citation I-Citation O O O O O O O O O O O O B-Wavelength O O O O O O O O O O O O O O O O O O O O B-Wavelength O O O O O O O O O O O O O O O B-Telescope O O O O O O O O O O O O O O O O O O O O O O O O O B-Wavelength I-Wavelength B-Formula I-Formula B-Citation I-Citation I-Citation O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O O B-Formula I-Formula B-Citation I-Citation I-Citation I-Citation O O O O O O