Group Scaling Relations From a Cosmological Hydrodynamic Simulation: No Pre-heating Required?

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dc.creatorDavé, Romeel
dc.creatorKatz, Neal
dc.creatorHernquist, Lars
dc.creatorWeinberg, David
dc.date2001-09-21
dc.date.accessioned2026-07-07T02:00:12Z
dc.date.available2026-07-07T02:00:12Z
dc.descriptionWe investigate the X-ray vs. optical scaling relations of poor groups to small clusters (sigma~100-700 km/s) identified in a cosmological hydrodynamic simulation of a Lambda-CDM universe, with cooling and star formation but no pre-heating. We find that the scaling relations between X-ray luminosity, X-ray temperature, and velocity dispersion show significant departures from the relations predicted by simple hydrostatic equilibrium models or simulations without cooling, having steeper L_X-sigma and L_X-T_X slopes and a "break" at \~200 km/s (~0.3 keV). These departures arise because the hot (X-ray emitting) gas fraction varies substantially with halo mass in this regime. Our predictions roughly agree with observations. Thus radiative cooling is a critical physical process in modeling galaxy groups, and may present an alternative to ad hoc models such as pre-heating or entropy floors for explaining X-ray group scaling relations.
dc.description4 pages, to be puplished in the proceedings of the ''Sesto 2001-Tracing Cosmic Evolution with Galaxy Clusters''
dc.identifierhttps://arxiv.org/abs/astro-ph/0109394
dc.identifierhttp://arxiv.org/abs/astro-ph/0109394
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/3373
dc.subjectAstrophysics
dc.titleGroup Scaling Relations From a Cosmological Hydrodynamic Simulation: No Pre-heating Required?
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