SIMBAD references

We use SDSS data to investigate the scaling relations of 127 No SOCS and 56 CIRS galaxy clusters at low redshift (z ≤ 0.10). We show that richness and both optical and X-ray luminosities are reliable mass proxies. The scatter in mass at a fixed observable is ∼40 per cent, depending on the aperture, sample and observable considered. For example, for the massive CIRS systems σ_lnM500|N500_= 0.33±0.05 and σ_lnM500|Lx_= 0.48±0.06. For the full sample σ_lnM500|N500_= 0.43±0.03 and σ_llnM500|Lx_= 0.56±0.06. The scaling relations based only on the richer systems (CIRS) are slightly flatter than those based on the full sample, but the discrepancies are within 1σ. We estimate substructure using 2D and 3D optical data, verifying that substructure has no significant effect on the cluster scaling relations (intercepts and slopes), independent of which substructure test we use. For a subset of 21 clusters, we estimate masses from the M-T_X relation using temperature measures from Base de Données Amas de Galaxies X. The scaling relations derived from the optical and X-ray masses are indeed very similar, indicating that our method consistently estimates the cluster mass and yields equivalent results regardless of the wavelength from which we measure mass. For massive systems, we represent the mass-richness relation by a function with the form ln(M₂₀₀) = A + Bxln(N₂₀₀/60), with M₂₀₀ being expressed in units of 10¹⁴M_☉. Using the virial mass, for CIRS clusters, we find A = (1.39±0.07) and B = (1.00±0.11). For the same sample, but using the masses obtained by the caustic method, we get A = (0.64±0.14) and B = (1.35±0.34). If we consider the mass as estimated from T_X(for the subset of 21 clusters with T_Xavailable) we derive A = (0.90±0.10) and B = (0.92 ± 0.10). The relations based on the virial mass have a scatter of σ_lnM200|N200_= 0.37±0.05, while σ_lnM200|N200_= 0.77±0.22 for the caustic mass and σ_lnM200|N200_= 0.34 ±0.08 for the temperature-based mass.