SIMBAD references

We present a combined optical and X-ray analysis of the rich cluster ABELL 1882 (A1882) with the aim of identifying merging substructure and understanding the recent assembly history of this system. Our optical data consist of spectra drawn from the Galaxy and Mass Assembly survey, which lends itself to this kind of detailed study thanks to its depth and high spectroscopic completeness. We use 283 spectroscopically confirmed cluster members to detect and characterize substructure. We complement the optical data with X-ray data taken with both Chandra and XMM. Our analysis reveals that A1882 harbors two main components, A1882A and A1882B, which have a projected separation of ∼2 Mpc and a line of sight velocity difference of υ_los ∼ -428_–139⁺¹⁸⁷ km/s. The primary system, A1882A, has velocity dispersion σ_v = 500_–26⁺²³ km/s and Chandra (XMM) temperature kT = 3.57±0.17 keV (3.31_–0.27^+0.28 keV) while the secondary, A1882B, has σ_v = 457_–101⁺¹⁰⁸ km/s and Chandra (XMM) temperature kT = 2.39±0.28 keV (2.12±0.20 keV). The optical and X-ray estimates for the masses of the two systems are consistent within the uncertainties and indicate that there is twice as much mass in A1882A (M₅₀₀= 1.5-1.9x10¹⁴ M_☉) when compared with A1882B (M₅₀₀ = 0.8-1.0x10¹⁴ M_☉). We interpret the A1882A/A1882B system as being observed prior to a core passage. Supporting this interpretation is the large projected separation of A1882A and A1882B and the dearth of evidence for a recent (<2 Gyr) major interaction in the X-ray data. Two-body analyses indicate that A1882A and A1882B form a bound system with bound incoming solutions strongly favored. We compute blue fractions of f_b= 0.28±0.09 and 0.18 ±0.07 for the spectroscopically confirmed member galaxies within r₅₀₀ of the centers of A1882A and A1882B, respectively. These blue fractions do not differ significantly from the blue fraction measured from an ensemble of 20 clusters with similar mass and redshift.