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DEGREE-SCALE ANISOTROPY IN THE COSMIC MICROWAVE BACKGROUND: SP94 RESULTS

机译:宇宙微波中的度数各向异性背景:SP94结果

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We present results from two observations of the cosmic microwave background (CMB) performed from the South Pole during the 1993-1994 austral summer. Each observation employed a 3° peak-to-peak sinusoidal, single-difference chop and consisted of a 20° x 1° strip on the sky. The first observation used a receiver which operates in three channels between 38 and 45 GHz (Q-band) with a FWHM beam which varies from 1° to 1.15°. The second observation overlapped the first observation and used a receiver which operates in four channels between 26 and 36 GHz (Ka-band) with a FWHM beam which varies from 1.5° to 1.7°. Significant correlated structure is observed in all channels for each observation. The spectrum of the structure is consistent with a CMB spectrum and is formally inconsistent with diffuse synchrotron and free-free emission at the 5 σ level. The amplitude of the structure is inconsistent with 20 K interstellar dust; however, the data do not discriminate against flat or inverted spectrum point sources. The root mean square amplitude (±1 σ) of the combined (Ka + Q) data is ΔT_(rms) = 41.2_(-6.7)~(+15.5) μK for an average window function which has a peak value of 0.97 at l = 68 and drops to e~(-0.5) of the peak value at l = 36 and l = 106. A band power estimate of the CMB power spectrum, C_l, gives < C_ll(l + 1)/(2π) >_B = 1.77_(-0.54)~(+1.58) x 10~(-10).
机译:我们提出了从1993年至1994年南极夏季从南极进行的两次宇宙微波背景(CMB)观测的结果。每次观察都使用3°峰-峰正弦单差斩波,并由20°x 1°的天空条组成。第一次观察使用的接收机工作在38到45 GHz(Q波段)之间的三个信道中,FWHM波束的变化范围是1°至1.15°。第二个观测值与第一个观测值重叠,并使用了一个接收机,该接收机在26至36 GHz(Ka频带)之间的四个信道中工作,其FWHM波束在1.5°至1.7°之间变化。对于每个观察,在所有通道中观察到重要的相关结构。该结构的光谱与CMB光谱一致,并且在形式上与5σ水平的扩散同步加速器和自由自由发射不一致。该结构的振幅与20 K星际尘埃不一致。但是,数据不能区分平坦或反向频谱点源。对于一个平均窗函数,其峰值为0.97时的平均值(Ka + Q)数据的均方根振幅(±1σ)为ΔT_(rms)= 41.2 _(-6.7)〜(+15.5)μK l = 68,并降至l = 36和l = 106时的峰值的e〜(-0.5)。CMB功率谱的频带功率估计C_1给出 _B = 1.77 _(-0.54)〜(+1.58)x 10〜(-10)。

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