Figure 15 - available via license: Creative Commons Attribution 4.0 International
Content may be subject to copyright.
Circulation of entropy and gas mass in the fiducial MPG simulation at t = 700, 770, and 800 Myr during its low-power state. All figure elements are as in Figure 11. The AGN impulse propagating outward at 700 Myr fails to stop infall of lower-entropy gas along the jet axis. High-entropy bubbles can be seen rising outward at 770 Myr, but by that time an equatorial outflow has begun, as low-entropy gas falling inward along the poles squeezes out higher-entropy gas. At 800 Myr, another weak AGN outburst is propagating outward.
Source publication
Coupling between active galactic nuclei (AGNs) and the circumgalactic medium (CGM) is critical to the interplay between radiative cooling and feedback heating in the atmospheres of the universe’s most massive galaxies. This paper presents a detailed analysis of numerical simulations showing how kinetic AGN feedback with a strong momentum flux inter...
Similar publications
The physics behind the ionization structure of outflows from black holes is yet to be fully understood. Using archival observations with the Chandra/HETG gratings over the past two decades, we measured an absorption measure distribution for a sample of outflows in nine active galactic nuclei (AGNs), namely the dependence of outflow column density,...
![Figure 8. (left) [Ne V]/[Ne II] and (middle) [O IV]/[Ne II] as a...](publication/361274377/figure/fig4/AS:1166727958282243@1655181030123/left-Ne-V-Ne-II-and-middle-O-IV-Ne-II-as-a-function-of-AGN-fraction-The_Q320.jpg)
We present the results of a stacking analysis performed on Spitzer/Infrared Spectrograph high-resolution mid-infrared spectra of luminous infrared galaxies (LIRGs) in the Great Observatories All-Sky LIRG Survey (GOALS). By binning on mid-infrared active galactic nucleus (AGN) fraction and stacking spectra, we detect bright emission lines [Ne II] an...
A recent hydrodynamic model, the radiation-driven fountain model (Wada et al. 2016), presented a dynamical picture that active galactic nuclei (AGNs) tori sustain their geometrical thickness by gas circulation around AGNs, and previous papers have confirmed that this picture is consistent with multiwavelength observations of nearby Seyfert galaxies...
We present the discovery and analysis of J1316+2614 at z=3.6130, a UV-bright star-forming galaxy ($M_{\rm UV} \simeq -24.7$) with large escape of Lyman continuum (LyC) radiation. J1316+2614 is a young ($\simeq 10$ Myr) star-forming galaxy with $SFR \simeq 500 M_{\odot}$ yr$^{-1}$ and a starburst mass of log($M_{\star}/M_{\odot}) \simeq 9.7$. It sho...
Multiwavelength observations indicate that some starburst galaxies show a dominant nonthermal contribution from their central region. These active galactic nuclei (AGN)-starburst composites are of special interest, as both phenomena on their own are potential sources of highly energetic cosmic rays and associated γ -ray and neutrino emission. In th...
Citations
... This effect is caused by substantial (ICM) gas outflows driven by the jet and the subsequent rising of the lobe (not explicitly shown here, but see e.g. Chen et al. 2019;Prasad et al. 2022). ...
Feedback driven by jets from active galactic nuclei is believed to be responsible for reducing cooling flows in cool-core galaxy clusters. We use simulations to model feedback from hydrodynamic jets in isolated halos. While the jet propagation converges only after the diameter of the jet is well resolved, reliable predictions about the effects these jets have on the cooling time distribution function only require resolutions sufficient to keep the jet-inflated cavities stable. Comparing different model variations, as well as an independent jet model using a different hydrodynamics code, we show that the dominant uncertainties are the choices of jet properties within a given model. Independent of implementation, we find that light, thermal jets with low momentum flux tend to delay the onset of a cooling flow more efficiently on a $50$ Myr timescale than heavy, kinetic jets. The delay of the cooling flow originates from a displacement and boost in entropy of the central gas. If the jet luminosity depends on accretion rate, collimated, light, hydrodynamic jets are able to reduce cooling flows in halos, without a need for jet precession or wide opening angles. Comparing the jet feedback with a `kinetic wind' implementation shows that equal amounts of star formation rate reduction can be achieved by different interactions with the halo gas: the jet has a larger effect on the hot halo gas while leaving the denser, star forming phase in place, while the wind acts more locally on the star forming phase, which manifests itself in different time-variability properties.
... Ho we ver, once the bo w shock has cut a path through the ambient core, there would not be a significant continued supply of energy if the flow pattern becomes stationary. Prasad, Voit & O'Shea ( 2022 ) show that taking a narrow jet opening angle reduces the thrust per unit area and so increases the long-term coupling with the ambient gas. The simulations presented here allow us to quantify the amount of energy that may aid the support of the inner core. ...
Supersonic jets with excess gas pressure are associated with many phenomena including radio galaxies, protostars, volcanic plumes, rocket exhausts and champagne cork popping. Some common properties are derived here based on steady uniform hydrodynamic flow from a circular orifice. We present a systematic numerical study over a wide range of parameters for Mach 2 jets, concentrating on simulations of jets with pressures exceeding the ambient pressure. With cylindrical symmetry, we show how the location of the stand-off and following downstream shocks depend not only on the over-pressure but also on the density due to a feedback loop which results in an oscillatory flow pattern. We conclude that rapidly varying and gradually evolving shock patterns arise even from steady uniform jets. This can take the form of turbulent plumes at high over-pressures and regular oscillations at low over-pressures. We identify where this screeching contributes to noise and sound wave generation which may aid the regulation of star and galaxy formation. However, the main effect for such low Mach number jets is to drive a circulatory motion in which the ambient medium is driven out along the axial direction while mass and energy flow laterally inwards, setting up a large advection pattern. Once the initial bow shock has propagated out, the noise from the jet is insufficient to significantly alter the environment. High Mach number jets do not follow these conclusions and will be treated separately.
Radiative cooling and active galactic nucleus heating are thought to form a feedback loop that regulates the evolution of low-redshift cool-core galaxy clusters. Numerical simulations suggest that the formation of multiphase gas in the cluster core imposes a floor on the ratio of cooling time (tcool) to free-fall time (tff) at min(tcool/tff) ≈ 10. Observations of galaxy clusters show evidence for such a floor, and usually the cluster cores with min(tcool/tff) ≲ 30 contain abundant multiphase gas. However, there are important outliers. One of them is Abell 2029 (A2029), a massive galaxy cluster (M200 ≳ 1015 M⊙) with min(tcool/tff) ∼ 20, but little apparent multiphase gas. In this paper, we present high-resolution 3D hydrodynamic adaptive mesh refinement simulations of a cluster similar to A2029 and study how it evolves over a period of 1–2 Gyr. Those simulations suggest that A2029 self-regulates without producing multiphase gas because the mass of its central black hole (${\sim} 5 \times 10^{10} \, \mathrm{ M}_\odot$) is great enough for Bondi accretion of hot ambient gas to produce enough feedback energy to compensate for radiative cooling.
Feedback driven by jets from active galactic nuclei is believed to be responsible for reducing cooling flows in cool-core galaxy clusters. We use simulations to model feedback from hydrodynamic jets in isolated haloes. While the jet propagation converges only after the diameter of the jet is well resolved, reliable predictions about the effects these jets have on the cooling time distribution function only require resolutions sufficient to keep the jet-inflated cavities stable. Comparing different model variations, as well as an independent jet model using a different hydrodynamics code, we show that the dominant uncertainties are the choices of jet properties within a given model. Independent of implementation, we find that light, thermal jets with low momentum flux tend to delay the onset of a cooling flow more efficiently on a 50 Myr time-scale than heavy, kinetic jets. The delay of the cooling flow originates from a displacement and boost in entropy of the central gas. If the jet kinetic luminosity depends on accretion rate, collimated, light, hydrodynamic jets are able to reduce cooling flows in haloes, without a need for jet precession or wide opening angles. Comparing the jet feedback with a ‘kinetic wind’ implementation shows that equal amounts of star formation rate reduction can be achieved by different interactions with the halo gas: the jet has a larger effect on the hot halo gas while leaving the denser, star-forming phase in place, while the wind acts more locally on the star-forming phase, which manifests itself in different time-variability properties.
