Understanding large-scale structure in the SSA22 protocluster region using cosmological simulations

Abstract

We investigate the nature and evolution of large-scale structure within the SSA22 protocluster region at $z=3.09$ using cosmological simulations. A redshift histogram constructed from current spectroscopic observations of the SSA22 protocluster reveals two separate peaks at $z=3.065$ (blue) and $z=3.095$ (red). Based on these data, we report updated overdensity and mass calculations for the SSA22 protocluster. We find ${\delta }_{b,gal}=4.8\pm 1.8$, ${\delta }_{r,gal}=9.5\pm 2.0$ for the blue and red peaks, respectively, and ${\delta }_{t,gal}=7.6\pm 1.4$ for the entire region. These overdensities correspond to masses of $M_b=(0.76\pm 0.17)\times 10^{15}{h}^{-1}{M}_{\odot }$, $M_r=(2.15\pm 0.32)\times 10^{15}{h}^{-1}{M}_{\odot }$, and $M_t=(3.19\pm 0.40)\times 10^{15}{h}^{-1}{M}_{\odot }$ for the red, blue, and total peaks, respectively. We use the Small MultiDark Planck (SMDPL) simulation to identify comparably massive $z\sim 3$ protoclusters, and uncover the underlying structure and ultimate fate of the SSA22 protocluster. For this analysis, we construct mock redshift histograms for each simulated $z\sim 3$ protocluster, quantitatively comparing them with the observed SSA22 data. We find that the observed double-peaked structure in the SSA22 redshift histogram corresponds not to a single coalescing cluster, but rather the proximity of a $\sim 10^{15}{h}^{-1}{M}_{\odot }$ protocluster and at least one $>10^{14}{h}^{-1}{M}_{\odot }$ cluster progenitor. Such associations in the SMDPL simulation are easily understood within the framework of hierarchical clustering of dark matter halos. We finally find that the opportunity to observe such a phenomenon is incredibly rare, with an occurrence rate of $7.4h^3 \mbox{ Gpc}^{-3}$.

13 pages, 8 figures, Accepted to ApJ

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