原子储存泡技术是氢微波激射器(氢脉泽)的关键技术。传统的石英薄壁储存泡位于TE011模的空心圆柱谐振腔的中心。为了缩小氢脉泽谐振腔和原子储存泡的体积采用了蓝宝石加载谐振腔取代传统的腔泡结构,并将蓝宝石晶体的内壁作为原子储存泡...原子储存泡技术是氢微波激射器(氢脉泽)的关键技术。传统的石英薄壁储存泡位于TE011模的空心圆柱谐振腔的中心。为了缩小氢脉泽谐振腔和原子储存泡的体积采用了蓝宝石加载谐振腔取代传统的腔泡结构,并将蓝宝石晶体的内壁作为原子储存泡,分析了脉泽工作状态的变化。为了消除蓝宝石加载腔的腔频率随温度的敏感变化(-60 k Hz/K)对脉泽自激振荡频率相对大的牵引效应,在蓝宝石加载谐振腔中再加载具有负介电常数温度系数的钛酸锶晶体,将腔频率温度系数近似地补偿到零。实现了采用介质加载谐振腔的氢脉泽的自激振荡,并通过锁相环实现氢脉泽对晶体振荡器的控制而形成稳定的频率源,短期稳定度指标在量级上达到了主动型氢原子钟(氢钟)的指标(1 000 s稳定度达1.5×10-14)。展开更多
A new radio spectral receiving system has been installed on the 25 m radio telescope of the Urumqi Astronomical Observatory. The back end is a surface acoustic wave chirp transform spectrometer (SAW CZT), used for the...A new radio spectral receiving system has been installed on the 25 m radio telescope of the Urumqi Astronomical Observatory. The back end is a surface acoustic wave chirp transform spectrometer (SAW CZT), used for the first time in radio astronomy. The calibration of the line observations has carefully been investigated for the new-type spectrometer. In order to test the feasibility of the prototype spectrometer, we observed water maser emission from a number of known Galactic sources. We describe the observed spectra of W49N, W3(OH), 2248+600 and 1909+090. We found that W49N spectrum showed high-velocity features ranging from -330 to 146 km s-1. In comparison with the spectra observed by Medicina, the feature at the LSR velocity -52 km s-1 in the W3(OH) presented the rapid variation in flux density.展开更多
文摘原子储存泡技术是氢微波激射器(氢脉泽)的关键技术。传统的石英薄壁储存泡位于TE011模的空心圆柱谐振腔的中心。为了缩小氢脉泽谐振腔和原子储存泡的体积采用了蓝宝石加载谐振腔取代传统的腔泡结构,并将蓝宝石晶体的内壁作为原子储存泡,分析了脉泽工作状态的变化。为了消除蓝宝石加载腔的腔频率随温度的敏感变化(-60 k Hz/K)对脉泽自激振荡频率相对大的牵引效应,在蓝宝石加载谐振腔中再加载具有负介电常数温度系数的钛酸锶晶体,将腔频率温度系数近似地补偿到零。实现了采用介质加载谐振腔的氢脉泽的自激振荡,并通过锁相环实现氢脉泽对晶体振荡器的控制而形成稳定的频率源,短期稳定度指标在量级上达到了主动型氢原子钟(氢钟)的指标(1 000 s稳定度达1.5×10-14)。
基金the National Natural Science Foundation of China (Grant No. 10073004) the Joint Laboratory of Radio Astronomy, the Chinese Academy of Sciences.
文摘A new radio spectral receiving system has been installed on the 25 m radio telescope of the Urumqi Astronomical Observatory. The back end is a surface acoustic wave chirp transform spectrometer (SAW CZT), used for the first time in radio astronomy. The calibration of the line observations has carefully been investigated for the new-type spectrometer. In order to test the feasibility of the prototype spectrometer, we observed water maser emission from a number of known Galactic sources. We describe the observed spectra of W49N, W3(OH), 2248+600 and 1909+090. We found that W49N spectrum showed high-velocity features ranging from -330 to 146 km s-1. In comparison with the spectra observed by Medicina, the feature at the LSR velocity -52 km s-1 in the W3(OH) presented the rapid variation in flux density.
