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We summarize the recent results on the observed COBE‐DMR two year sky rms temperature fluctuations. A ‘‘cross‐RMS’’ statistic is used to infer the Qrms‐PS normalization for a scale‐invariant (n=1) spectral model. The method is extended to the normalization of other cosmological power spectra.

We summarize the results of the Cosmic Microwave Background (CMB) anisotropy measurements of the COBE‐DMR using the first two years of data. The inference of angular power spectrum parameters from the DMR data is complicated by the need to omit Galaxy contaminated regions of the sky, preventing the spherical harmonics from forming an orthogonal basis set over the remaining sky. The COBE‐DMR team has implemented three methods for deducing the power spectrum parameters. These include: a two‐point correlation function analysis (Bennett et al. 1994); an analysis in terms of orthogonal modes constructed on the cut sphere (Gorski et al. 1994); and an analysis of a modified Hauser‐Peebles power spectrum (Wright et al. 1994). These methods for deducing the power spectrum are discussed and the results are summarized and compared.