COSMIC TEMPERATURE-FLUCTUATIONS FROM 2 YEARS OF COBE DIFFERENTIAL MICROWAVE RADIOMETERS OBSERVATIONS

The first two years of COBE Differential Microwave Radiometers (DMR) o bservations of the cosmic microwave background (CMB) anisotropy are an alyzed and compared with our previously published first year results. The results are consistent, but the addition of the second year of dat a increases the precision and accuracy of the detected CMB temperature fluctuations. The 2 yr 53 GHz data are characterized by rms temperatu re fluctuations of (Delta T)(rms)(7 degrees) = 44 +/- 7 mu K and (Delt a T)(rms)(10 degrees) = 30.5 +/- 2.7 mu K at 7 degrees and 10 degrees angular resolution, respectively. The 53 x 90 GHz cross-correlation am plitude at zero lag is C(0)(1/2) = 36 +/- 5 mu K (68% CL) for the unsm oothed (7 degrees resolution) DMR data. We perform a likelihood analys is of the cross-correlation function, with Monte Carlo simulations to infer biases of the method, for a power-law model of initial density f luctuations, P(k) proportional to k(n). The Monte Carlo simulations in dicate that derived estimates of n are biased by +0.11 +/- 0.0l, while the subset of simulations with a low quadrupole (as observed) indicat e a bias of +0.31 +/- 0.04. Derived values for 68% confidence interval s are given corrected (and not corrected) for our estimated biases. In cluding the quadrupole anisotropy, the most likely quadrupole-normaliz ed amplitude is Q(rms-PS) = 14.3(-3.3)(+5.2) mu K (12.8(-3.3)(+5.2) mu K) with a spectral index n = 1.42(0.55)(+0.49) (n = 1.53(-0.55)(+0.49 )). With n fixed to 1.0 the most likely amplitude is 18.2 +/- 1.5 mu K (17.4 +/- 1.5 mu K). The marginal likelihood of n is 1.42 +/- 0.37 (1 .53 +/- 0.37). Excluding the quadrupole anisotropy, the most likely qu adrupole-normalized amplitude is Q(rms-PS) = 17.4(-5.2)(+7.5) mu K (15 .8(-5.2)(+7.5) mu K) with a spectral index n = 1.11(-0.55)(+0.60) (n = 1.22(-0.55)(+0.60)) With n fixed to 1.0 the most likely amplitude is 18.6 +/- 1.6 mu K (18.2 +/- 1.6 mu K). The marginal likelihood of n is 1.11 +/- 0.40 (1.22 +/- 0.40). Our best estimate of the dipole from t he 2 yr DMR data is 3.363 +/- 0.024 mK toward Galactic coordinates (l, b) = (264 degrees.4 +/- 0 degrees.2, +48 degrees.1 +/- 0 degrees.4), and our best estimate of the rms quadrupole amplitude in our sky is 6 +/- 3 mu K (68% CL).