Large-scale structure formation and the segregation of dark and baryonic matter

Details Large-scale structure formation and the segregation of dark and baryonic matter Large-scale structure formation and the segregation of dark and baryonic matter

Jul 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995aipc..336..441m&link_type=abstract

Dark matter. AIP Conference Proceedings, Volume 336, pp. 441-445 (1995).

Mathematics

Logic

4

Atomic Processes And Interactions, Dark Matter, Origin, Formation, Evolution, Age, And Star Formation

Scientific paper

We have developed an improved version of SPH-Adaptive SPH (ASPH)-for cosmological gas dynamical simulations. We have applied our ASPH method to three models-Hot, Cold, and Mixed Hot-and-Cold Dark Matter (HDM, CDM, and CHDM)-to simulate large-scale structure formation in 2D. We have analyzed these simulations to determine how the ratio of gas to total density in each differs from that of their universal mean values-the density bias-as a function of the degree of overdensity of the matter. All three models show a tendency for the gas density to be anti-biased (i.e., gas mass fraction less than its mean value) in regions of highest overdensity, while positively biased in regions of moderate overdensity. This anti-bias trend may cause models like these with Ω=1 and with Ωb limited by standard Big-Bang nucleosynthesis to be inconsistent with previous X-ray and optical determinations of the baryonic mass fraction in rich clusters. To test this, we focus on CDM, study the bias inside simulation clusters and pick one to simulate the standard procedure for X-ray mass determinations. Fitting X-ray brightness profiles of clusters to measure total cluster mass, assuming isothermal sphere and hydrostatic equilibrium, can give approximately correct results, while underestimating the gas fraction somewhat.

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