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A Universal Temperature Profile for Galaxy Clusters | | C. Loken
; M.L. Norman
; E. Nelson
; J. Burns
; G.L. Bryan
; P. Motl
; | | Date: |
3 Jul 2002 | | Journal: | Astrophys.J. 579 (2002) 571-576 | | Subject: | astro-ph | | Affiliation: | CITA), M.L. Norman (UCSD), E. Nelson (UCSD), J. Burns (Colorado), G.L. Bryan (Oxford), P. Motl (Colorado | | Abstract: | We investigate the predicted present-day temperature profiles of the hot, X-ray emitting gas in galaxy clusters for two cosmological models - a current best-guess LCDM model and standard cold dark matter (SCDM). Our numerically-simulated "catalogs" of clusters are derived from high-resolution (15/h kpc) simulations which make use of a sophisticated, Eulerian-based, Adaptive Mesh-Refinement (AMR) code that faithfully captures the shocks which are essential for correctly modelling cluster temperatures. We show that the temperature structure on Mpc-scales is highly complex and non-isothermal. However, the temperature profiles of the simulated LCDM and SCDM clusters are remarkably similar and drop-off as $T +AFw-propto (1+-r/a_x)^{-+AFw-delta}$ where $a_x +AFw-sim r_{vir}/1.5$ and $+AFw-delta +AFw-sim 1.6$. This decrease is in good agreement with the observational results of Markevitch et al.(1998) but diverges, primarily in the innermost regions, from their fit which assumes a polytropic equation of state. Our result is also in good agreement with a recent sample of clusters observed by BeppoSAX though there is some indication of missing physics at small radii ($r<0.2 r_{vir}$). We discuss the interpretation of our results and make predictions for new x-ray observations that will extend to larger radii than previously possible. Finally, we show that, for $r>0.2 r_{vir}$, our universal temperature profile is consistent with our most recent simulations which include both radiative cooling and supernovae feedback. | | Source: | arXiv, astro-ph/0207095 | | Services: | Forum | Review | PDF | Favorites | |
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