Supermassive Black Hole Fueling in IllustrisTNG: Impact of Environment

Abstract

Abstract We study the association between active galactic nuclei (AGNs) and environment at scales of 0.01–1 <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msup> <mml:mrow> <mml:mi>h</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>1</mml:mn> </mml:mrow> </mml:msup> </mml:math> Mpc in the IllustrisTNG simulated universe ( TNG100 ). We identify supermassive black hole (BH) pairs and multiples within scales of 0.01, 0.1, and 1 <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msup> <mml:mrow> <mml:mi>h</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>1</mml:mn> </mml:mrow> </mml:msup> </mml:math> Mpc and examine their AGN activity in relation to randomly selected pairs and multiples. The number density of BHs in TNG100 is n = 0.06 h 3 Mpc −3 at z ≲ 1.5 ( n = 0.02 h 3 Mpc −3 at z = 3). About ∼10% and ∼1% of these BHs live in pairs and multiples, respectively, within 0.1 <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msup> <mml:mrow> <mml:mi>h</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>1</mml:mn> </mml:mrow> </mml:msup> </mml:math> Mpc scales. These systems have enhanced likelihood (up to factors of 3–6) of containing high Eddington ratio ( η ≳ 0.7) AGNs compared to random pairs and multiples. Conversely, the likelihood of an AGN to live in 0.1 <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msup> <mml:mrow> <mml:mi>h</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>1</mml:mn> </mml:mrow> </mml:msup> </mml:math> Mpc scale BH systems is also higher (by factors ∼4 for η ≳ 0.7) compared to random pairs and multiples. ∼10% of ultra-hard X-ray selected AGNs in TNG100 have detectable 2–10 keV AGN companions on 0.1 <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msup> <mml:mrow> <mml:mi>h</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>1</mml:mn> </mml:mrow> </mml:msup> </mml:math> Mpc scales, consistent with observations. On larger spatial scales (∼1 <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msup> <mml:mrow> <mml:mi>h</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>1</mml:mn> </mml:mrow> </mml:msup> </mml:math> Mpc), however, no significant enhancements in AGN activity exist, even at high Eddington ratios. This implies that small-scale (≲0.1 <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msup> <mml:mrow> <mml:mi>h</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>1</mml:mn> </mml:mrow> </mml:msup> </mml:math> Mpc) AGN enhancement is likely driven by galaxy interactions and mergers. Nonetheless, the overall percentage of AGNs living in ≲0.1 <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:msup> <mml:mrow> <mml:mi>h</mml:mi> </mml:mrow> <mml:mrow> <mml:mo>−</mml:mo> <mml:mn>1</mml:mn> </mml:mrow> </mml:msup> </mml:math> Mpc scale multiples is still subdominant (≲40%). Furthermore, the associated Eddington ratio enhancements of BH systems (as well as merging BHs) is only up to factors of ∼2–3. Our results support the existence of merger-AGN connection in TNG100 . However, it plays a relatively minor role in fueling the AGN population.

Topics & Concepts