Papers › z~2 dual AGN host galaxies are disky: stellar kinematics in the ASTRID Simulation
z~2 dual AGN host galaxies are disky: stellar kinematics in the ASTRID Simulation
Ekaterine Dadiani, Tiziana Di Matteo, Nianyi Chen, Patrick Lachance, Yue Shen, Yu-Ching Chen, Rupert Croft, Yueying Ni, Simeon Bird
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We study dual AGN host galaxy morphologies at z=2 using the ASTRID simulation, selecting black hole (BH) pairs with small separation (Δr<30kpc), high mass (M_(BH,12)>10⁷M_⊙), and luminosity (L_(bol,12)>10⁴³erg/s). We kinematically decompose (using MORDOR) ∼1000 dual AGN hosts into standard components - a `disk' (thin and thick disk, pseudo-bulge) and 'bulge' (bulge and halo) and define disk-dominated galaxies by the disk-to-total D/T≥0.5. In ASTRID, 60.9±2.1% of dual AGN hosts (independent of separation) are disk-dominated, with the D/T distribution peaking at ∼0.7. Notably, hosts of BH pairs have similar morphologies (most either both disk or bulge-dominated). In dual-AGN hosts, the D/T increases from ∼17% at M_*∼10⁹ M_⊙ to 64% for M_* ∼10^(11.5) M_⊙, and the pseudo-bulge is the dominant component of the disk fraction at the high mass end. Moreover, dual AGN hosts exhibit a higher fraction of disk/large pseudo-bulge than single-AGN hosts. The Disk-to-Total ratio is approximately constant with BH mass or AGN luminosity. We also create mock images of dual AGN host galaxies, employing morphological fitting software Statmorph to calculate morphological parameters and compare them with our kinematic decomposition results. Around 83.3±2.4% of galaxies display disk-like profiles, of which ∼60.7±2.2% are kinematically confirmed as disks. Se\'rsic indices and half-mass radii of dual AGN host galaxies align with observational measurements from HST at z∼2. Around 34% are identified as mergers from the Gini-M₂₀ relation. We find two dual AGN hosted by galaxies that exhibit disk-like se\'rsic index n₁₂<1 and (D/T)₁₂>0.5, which are in remarkable agreement with properties of recently discovered dual quasars in disk galaxies at z∼2.
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