Linking galaxy structural properties and star formation activity to black hole activity with IllustrisTNG

• Verfasst von: Habouzit, Mélanie [VerfasserIn]
• Verfasst von: Genel, Shy [VerfasserIn]
• Verfasst von: Somerville, Rachel S [VerfasserIn]
• Verfasst von: Kocevski, Dale [VerfasserIn]
• Verfasst von: Hirschmann, Michaela [VerfasserIn]
• Verfasst von: Dekel, Avishai [VerfasserIn]
• Verfasst von: Choi, Ena [VerfasserIn]
• Verfasst von: Nelson, Dylan [VerfasserIn]
• Verfasst von: Pillepich, Annalisa [VerfasserIn]
• Verfasst von: Torrey, Paul [VerfasserIn]
• Verfasst von: Hernquist, Lars [VerfasserIn]
• Verfasst von: Vogelsberger, Mark [VerfasserIn]
• Verfasst von: Weinberger, Rainer [VerfasserIn]
• Verfasst von: Springel, Volker [VerfasserIn]
• Titel: Linking galaxy structural properties and star formation activity to black hole activity with IllustrisTNG
• Verf.angabe: Mélanie Habouzit, Shy Genel, Rachel S. Somerville, Dale Kocevski, Michaela Hirschmann, Avishai Dekel, Ena Choi, Dylan Nelson, Annalisa Pillepich, Paul Torrey, Lars Hernquist, Mark Vogelsberger, Rainer Weinberger and Volker Springel
• E-Jahr: 2019
• Jahr: 2019 January 16
• Umfang: 31 S.
• Fussnoten: Gesehen am 27.07.2022
• Titel Quelle: Enthalten in: Royal Astronomical SocietyMonthly notices of the Royal Astronomical Society
• Ort Quelle: Oxford : Oxford Univ. Press, 1827
• Jahr Quelle: 2019
• Band/Heft Quelle: 484(2019), 4, Seite 4413-4443
• ISSN Quelle: 1365-2966
• DOI: doi:10.1093/mnras/stz102
• Datenträger: Online-Ressource
• Sprache: eng
• K10plus-PPN: 181101335X

Abstract

We study the connection between active galactic nuclei (AGN) and their host galaxies through cosmic time in the large-scale cosmological IllustrisTNG simulations. We first compare BH properties, i.e. the hard X-ray BH luminosity function, AGN galaxy occupation fraction, and distribution of Eddington ratios, to available observational constraints. The simulations produce a population of BHs in good agreement with observations, but we note an excess of faint AGN in hard X-ray ($L_{\rm x}\sim 10^{43-44}\, \rm erg/s$), and a lower number of bright AGN ($L_{\rm x}\gt 10^{44} \, \rm erg/s$), a conclusion that varies quantitatively but not qualitatively with BH luminosity estimation method. The lower Eddington ratios of the $10^{9}\, \rm M_{\odot }$ BHs compared to observations suggest that AGN feedback may be too efficient in this regime. We study galaxy star formation activity and structural properties, and design sample-dependent criteria to identify different galaxy types (star-forming/quiescent, extended/compact) that we apply both to the simulations and observations from the candels fields. We analyse how the simulated and observed galaxies populate the specific star formation rate - stellar mass surface density diagram. A large fraction of the $z$ = 0 $M_{\star }\geqslant 10^{11}\, \rm M_{\odot }$ quiescent galaxies first experienced a compaction phase (i.e. reduction of galaxy size) while still forming stars, and then a quenching event. We measure the dependence of AGN fraction on galaxies’ locations in this diagram. After correcting the simulations with a redshift and AGN luminosity-dependent model for AGN obscuration, we find good qualitative and quantitative agreement with observations. The AGN fraction is the highest among compact star-forming galaxies ($16-20{{\ \rm per\ cent}}$ at $z$ ∼ 1.5-2), and the lowest among compact quiescent galaxies ($6-10{{\ \rm per\ cent}}$ at $z$ ∼ 1.5-2).