TY - JOUR
T1 - Simulations of jet heating in galaxy clusters
T2 - Successes and challenges
AU - Martizzi, Davide
AU - Quataert, Eliot
AU - Faucher-Giguère, Claude André
AU - Fielding, Drummond
N1 - Funding Information:
We thank the reviewer Geoffrey V. Bicknell for his feedback that allowed us to greatly increase the quality of our paper. We thank Greg Bryan, Yuan Li, Greg Meece, Brian O’Shea, Chris Reynolds, Karen Yang, and Mark Voit for their valuable comments on our paper. We also thank Jim Stone for useful conversations. DM was supported in part by the Swiss National Science Foundation postdoctoral fellowship grant P300P2 161062, in part by NASA ATP grant 12-APT12-0183, and in part by the CTA and DARK-Carlsberg Foundation Fellowship. EQ was supported in part by NASA ATP grant 12-APT12-0183, a Simons Investigator Award from the Simons Foundation and by NSF grant AST-1715070. CAFG was supported by NSF through grants AST-1412836, AST-1517491, AST-1715216, and CAREER award AST-1652522, NASA through grant NNX15AB22G, CXO through grant TM7-18007, and a Cottrell Scholar Award from the Research Corporation for Science Advancement. DF was supported by an NSF Graduate Research Fellowship. The simulations reported in this paper were run and processed on the Savio computer cluster at UC Berkeley and with resources provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center (allocations SMD-14-5492, SMD-14-5189, and SMD-15-6530).
Funding Information:
We thank the reviewer Geoffrey V. Bicknell for his feedback that allowed us to greatly increase the quality of our paper. We thank Greg Bryan, Yuan Li, Greg Meece, Brian O'Shea, Chris Reynolds, Karen Yang, and Mark Voit for their valuable comments on our paper. We also thank Jim Stone for useful conversations. DM was supported in part by the Swiss National Science Foundation postdoctoral fellowship grant P300P2 161062, in part by NASA ATP grant 12-APT12-0183, and in part by the CTA and DARK-Carlsberg Foundation Fellowship. EQ was supported in part by NASA ATP grant 12-APT12-0183, a Simons Investigator Award from the Simons Foundation and by NSF grant AST-1715070. CAFG was supported by NSF through grants AST-1412836, AST-1517491, AST-1715216, and CAREER award AST-1652522, NASA through grant NNX15AB22G, CXO through grant TM7-18007, and a Cottrell Scholar Award from the Research Corporation for Science Advancement. DF was supported by an NSF Graduate Research Fellowship. The simulations reported in this paperwere run and processed on the Savio computer cluster at UC Berkeley and with resources provided by the NASA High-End Computing (HEC) Program through the NASA Advanced Supercomputing (NAS) Division at Ames Research Center (allocations SMD-14-5492, SMD-14-5189, and SMD-15-6530).
Publisher Copyright:
© 2018 The Author(s).
PY - 2019/2/21
Y1 - 2019/2/21
N2 - We study how jets driven by active galactic nuclei influence the cooling flow in Perseus-like galaxy cluster cores with idealized, non-relativistic, hydrodynamical simulations performed with the Eulerian code ATHENA using high-resolution Godunov methods with low numerical diffusion. We use novel analysis methods to measure the cooling rate, the heating rate associated with multiple mechanisms, and the power associated with adiabatic compression/expansion. A significant reduction of the cooling rate and cooling flow within 20 kpc from the centre can be achieved with kinetic jets. However, at larger scales and away from the jet axis, the system relaxes to a cooling flow configuration. Jet feedback is anisotropic and is mostly distributed along the jet axis, where the cooling rate is reduced and a significant fraction of the jet power is converted into kinetic power of heated outflowing gas. Away from the jet axis weak shock heating represents the dominant heating source. Turbulent heating is significant only near the cluster centre, but it becomes inefficient at ∼50 kpc scales where it only represents a few per cent of the total heating rate. Several details of the simulations depend on the choice made for the hydro solver, a consequence of the difficulty of achieving proper numerical convergence for this problem: current physics implementations and resolutions do not properly capture multiphase gas that develops as a consequence of thermal instability. These processes happen at the grid scale and leave numerical solutions sensitive to the properties of the chosen hydro solver.
AB - We study how jets driven by active galactic nuclei influence the cooling flow in Perseus-like galaxy cluster cores with idealized, non-relativistic, hydrodynamical simulations performed with the Eulerian code ATHENA using high-resolution Godunov methods with low numerical diffusion. We use novel analysis methods to measure the cooling rate, the heating rate associated with multiple mechanisms, and the power associated with adiabatic compression/expansion. A significant reduction of the cooling rate and cooling flow within 20 kpc from the centre can be achieved with kinetic jets. However, at larger scales and away from the jet axis, the system relaxes to a cooling flow configuration. Jet feedback is anisotropic and is mostly distributed along the jet axis, where the cooling rate is reduced and a significant fraction of the jet power is converted into kinetic power of heated outflowing gas. Away from the jet axis weak shock heating represents the dominant heating source. Turbulent heating is significant only near the cluster centre, but it becomes inefficient at ∼50 kpc scales where it only represents a few per cent of the total heating rate. Several details of the simulations depend on the choice made for the hydro solver, a consequence of the difficulty of achieving proper numerical convergence for this problem: current physics implementations and resolutions do not properly capture multiphase gas that develops as a consequence of thermal instability. These processes happen at the grid scale and leave numerical solutions sensitive to the properties of the chosen hydro solver.
KW - Galaxies: active
KW - Galaxies: clusters: general
KW - Galaxies: jets
KW - Methods: numerical
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U2 - 10.1093/mnras/sty3273
DO - 10.1093/mnras/sty3273
M3 - Article
AN - SCOPUS:85060552345
SN - 0035-8711
VL - 483
SP - 2465
EP - 2486
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 2
ER -