X-ray Emission of Baryonic Gas in the Universe: Luminosity-Temperature Relationship and Soft-Band Background

Abstract

We study the X-ray emission of baryon fluid in the universe using the WIGEON cosmological hydrodynamic simulations. It has been revealed that cosmic baryon fluid in the nonlinear regime behaves like Burgers turbulence, i.e. the fluid field consists of shocks. Like turbulence in incompressible fluid, the Burgers turbulence plays an important role in converting the kinetic energy of the fluid to thermal energy and heats the gas. We show that the simulation sample of the $\Lambda$CDM model without adding extra heating sources can fit well the observed distributions of X-ray luminosity versus temperature ($L_{\mathrm{x}}$ vs. $T$) of galaxy groups and is also consistent with the distributions of X-ray luminosity versus velocity dispersion ($L_{\mathrm{x}}$ vs. $\sigma$). Because the baryonic gas is multiphase, the $L_{\mathrm{x}}-T$ and $L_{\mathrm{x}}-\sigma$ distributions are significantly scattered. If we describe the relationships by power laws $L_{\mathrm{x}}\propto T^{{\alpha }_{LT}}$ and $L_{\mathrm{x}}\propto {\sigma }^{{\alpha }_{LV}}$, we find ${\alpha }_{LT}>2.5$ and ${\alpha }_{LV}>2.1$. The X-ray background in the soft $0.5-2$ keV band emitted by the baryonic gas in the temperature range $10^5<T<10^7$ K has also been calculated. We show that of the total background, (1) no more than 2% comes from the region with temperature less than $10^{6.5}$ K, and (2) no more than 7% is from the region of dark matter with mass density ${\rho }_{\mathrm{dm}}<50{\bar{\rho }}_{\mathrm{dm}}$. The region of ${\rho }_{\mathrm{dm}}>50{\bar{\rho }}_{\mathrm{dm}}$ is generally clustered and discretely distributed. Therefore, almost all of the soft X-ray background comes from clustered sources, and the contribution from truly diffuse gas is probably negligible. This point agrees with current X-ray observations.

arXiv comment32 pages including 14 figures and 2 tables. Final version for publication in ApJ

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• Dynamical Effect of the Turbulence of IGM on the Baryon Fraction Distribution
• Estimating Power Spectrum of Sunyaev-Zeldovich Effect from the Cross-Correlation between WMAP and 2MASS
• Log-Poisson Hierarchical Clustering of Cosmic Neutral Hydrogen and Ly-alpha Transmitted Flux of QSO Absorption Spectrum
• Scaling Relation between Sunyaev-Zel'dovich Effect and X-ray Luminosity and Scale-Free Evolution of Cosmic Baryon Field
• Statistical and dynamical decoupling of the IGM from Dark Matter