Destruction of the central black hole gas reservoir through head-on galaxy collisions

Miki, Yuko; Mori, Masao; Kawaguchi, Toshihiro

doi:10.1038/s41550-020-01286-9

Cited by 3 publications

(2 citation statements)

References 88 publications

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“…In reality, even if the circumnuclear disk is destroyed by a galaxy collision (Miki et al 2021), it will soon be rebuilt if there is interstellar cold gas. For example, the disk mass M g,d grows rapidly from M g,d = 0 at t ∼ 0 as is shown in Figure 4(b).…”

Section: Roles Of the Interstellar Gas And The Circumnuclear Diskmentioning

confidence: 99%

Massive Molecular Gas as a Fuel Tank for Active Galactic Nuclei Feedback in Central Cluster Galaxies

Fujita,

Kawakatu,

Nagai

2021

Preprint

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Massive molecular gas has been discovered in giant elliptical galaxies at the centers of galaxy clusters. To reveal its role in AGN feedback in those galaxies, we construct a semi-analytic model of gas circulation. This model especially focuses on the massive molecular gas (interstellar cold gas on a scale of ∼ 10 kpc) and the circumnuclear disk ( 0.5 kpc). We consider the destruction of the interstellar cold gas by star formation and the gravitational instability for the circumnuclear disk. Our model can reproduce the basic properties of the interstellar cold gas and the circumnuclear disk such as their masses. We also find that the circumnuclear disk tends to stay at the boundary between stable and unstable states. This works as an 'adjusting valve' that regulates mass accretion toward the supermassive black hole. On the other hand, the interstellar cold gas serves as a 'fuel tank' in the AGN feedback. Even if the cooling of the galactic hot gas is prevented, the interstellar cold gas can sustain the AGN activities for 0.5 Gyr. We also confirm that the small entropy of the hot gas ( 30 keV cm 2 ) or the short cooling time ( 1 Gyr) is a critical condition for the existence of the massive molecular gas in the galaxy. The dissipation time of the interstellar cold gas may be related to the critical cooling time.

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Section: Roles Of the Interstellar Gas And The Circumnuclear Diskmentioning

confidence: 99%

Massive Molecular Gas as a Fuel Tank for Active Galactic Nuclei Feedback in Central Cluster Galaxies

Fujita,

Kawakatu,

Nagai

2021

Preprint

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“…When matter is accreted onto the disc surrounding the SMBH, enormous amounts of energy can be released through radiation (or relativistic jets), triggering the so-called galactic nuclear activity. Major mergers have been proposed as an efficient mechanism that causes the matter to lose most of its angular momentum and fall down to the inner regions of the galaxy on a relatively short timescale (e.g., Silk & Rees 1998;Volonteri et al 2003;Springel et al 2005, but see Miki et al 2021). At the same time, merging systems are known to induce intense star-formation activity through compression of the gas.…”

Section: Introductionmentioning

confidence: 99%

Remarkably high mass and velocity dispersion of molecular gas associated with a regular, absorption-selected type I quasar

Noterdaeme

Balashev

Combes

et al. 2021

A&A

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We present 3 mm observations of the quasar J0015+1842 at z = 2.63 with the NOrthern Extended Millimeter Array (NOEMA). Our data reveal molecular gas, traced with a Gaussian CO(3–2) line, with a remarkably high velocity dispersion (FWHM = 1010 ± 120 km s−1) that corresponds to a total molecular mass MH2 ≈ (3.4 − 17) × 1010 M⊙, depending on the adopted CO-to-H2 conversion factor αCO = (0.8 − 4.0) M⊙ (km s−1 pc2)−1. Assuming the 3 mm continuum emission is thermal, we derive a dust mass of about Mdust ∼ 5 × 108 M⊙. J0015+1842 is located in the molecular gas-rich region in the IR versus CO line luminosity diagram, in between the main locus of main-sequence and sub-millimetre galaxies and that of most other active galactic nuclei targeted so far for CO measurements. While the high velocity dispersion of the CO line suggests a merging system, J0015+1842 is observed to be a regular, only very moderately dust-reddened (AV ∼ 0.3 − 0.4) type I quasar from its UV-optical spectrum, from which we infer a mass of the super-massive black hole of about MBH ≈ 6 × 108 M⊙. We suggest that J0015+1842 is observed at a galaxy evolutionary stage where a massive merger has brought significant amounts of gas towards an actively accreting super-massive black hole (quasar). While the host still contains a large amount of dust and molecular gas with a high velocity dispersion, the quasar has already cleared the way towards the observer, likely through powerful outflows, as has recently been revealed by optical observations of the same object. High angular resolution observations of this and similar systems are expected to help us better determine the respective importance of evolution and orientation in the appearance of quasars and their host galaxies. These observations have the potential to investigate early feedback and star-formation processes in galaxies in their quasar phases.

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Massive Molecular Gas as a Fuel Tank for Active Galactic Nuclei Feedback In Central Cluster Galaxies

Fujita

Kawakatu

Nagai

2022

ApJ

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Massive molecular gas has been discovered in giant elliptical galaxies at the centers of galaxy clusters. To reveal its role in active galactic nucleus (AGN) feedback in those galaxies, we construct a semianalytical model of gas circulation. This model especially focuses on the massive molecular gas (interstellar cold gas on a scale of ∼10 kpc) and the circumnuclear disk (≲0.5 kpc). We consider the destruction of the interstellar cold gas by star formation and the gravitational instability for the circumnuclear disk. Our model can reproduce the basic properties of the interstellar cold gas and the circumnuclear disk, such as their masses. We also find that the circumnuclear disk tends to stay at the boundary between stable and unstable states. This works as an “adjusting valve” that regulates mass accretion toward the supermassive black hole. On the other hand, the interstellar cold gas serves as a “fuel tank” in the AGN feedback. Even if the cooling of the galactic hot gas is prevented, the interstellar cold gas can sustain the AGN activity for ≳0.5 Gyr. We also confirm that the small entropy of hot gas (≲30 keV cm2) or the short cooling time (≲1 Gyr) is a critical condition for the existence of massive amounts of molecular gas in the galaxy. The dissipation time of the interstellar cold gas may be related to the critical cooling time. The galaxy behavior is described by a simple relation among the disk stability, the cloud dissipation time, and the gas cooling rate.

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Destruction of the central black hole gas reservoir through head-on galaxy collisions

Cited by 3 publications

References 88 publications

Massive Molecular Gas as a Fuel Tank for Active Galactic Nuclei Feedback in Central Cluster Galaxies

Massive Molecular Gas as a Fuel Tank for Active Galactic Nuclei Feedback in Central Cluster Galaxies

Remarkably high mass and velocity dispersion of molecular gas associated with a regular, absorption-selected type I quasar

Massive Molecular Gas as a Fuel Tank for Active Galactic Nuclei Feedback In Central Cluster Galaxies

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