本文選題：望遠(yuǎn)鏡 + 射頻干擾��； 參考：《天文學(xué)報(bào)》2017年05期

【摘要】：一直以來(lái),射電天文裝備不斷得到升級(jí)和發(fā)展,以使其具有更好的觀測(cè)性能,包括提高數(shù)據(jù)記錄的時(shí)間和頻率分辨率以及獲得更高的接收和記錄帶寬等.然而與之形成矛盾的是:國(guó)際電信聯(lián)盟(International Telecommunication Union,ITU)僅為射電天文分配了非常有限的頻譜資源,導(dǎo)致的后果是射電觀測(cè)設(shè)備不可避免地受到日益增強(qiáng)的非天文信號(hào)的影響,后者的來(lái)源主要是人類的通信活動(dòng)和日常生活,這就構(gòu)成了通常射電天文中所說(shuō)的射頻干擾(Radio Frequency Interference,RFI).射頻干擾會(huì)降低數(shù)據(jù)質(zhì)量甚至導(dǎo)致數(shù)據(jù)無(wú)效,對(duì)科學(xué)結(jié)果的影響越來(lái)越嚴(yán)重.對(duì)RFI消減的需求進(jìn)行分析,總結(jié)了RFI的特性、抑制和消減的技術(shù)和方案,并介紹了一些有代表性的射電望遠(yuǎn)鏡(或陣列)中采用的RFI消減方法;還分析比較了4種常用方案,即預(yù)防、預(yù)檢測(cè)、預(yù)相關(guān)和后相關(guān)的優(yōu)勢(shì)和不足.對(duì)RFI進(jìn)行準(zhǔn)確的識(shí)別和標(biāo)記是減少數(shù)據(jù)損失從而有效提高數(shù)據(jù)質(zhì)量的關(guān)鍵,也是發(fā)展RFI消減技術(shù)的最終目的.通過(guò)研究不難發(fā)現(xiàn),上述4種方案的組合運(yùn)用將具有更高的實(shí)用價(jià)值.近幾年來(lái),隨著高速數(shù)字信號(hào)處理和高性能計(jì)算的迅速發(fā)展,依賴大量計(jì)算的實(shí)時(shí)模式下的預(yù)檢測(cè)以及離線模式下從大型望遠(yuǎn)鏡陣列所產(chǎn)生的大規(guī)模干涉相關(guān)數(shù)據(jù)中檢測(cè)RFI已經(jīng)成為可能.
[Abstract]:Radio astronomical equipment has been continuously upgraded and developed to provide better observation performance, including improving the time and frequency resolution of data recording and obtaining higher receiving and recording bandwidth. Paradoxically, however, the International Telecommunication Union (ITU) has only allocated very limited spectrum resources for radio astronomy, with the consequence that radio observation equipment is inevitably affected by increasing non-astronomical signals. The source of the latter is mainly human communication activities and daily life, which constitutes the radio frequency interference called radio Frequency interference in radio astronomy. RF interference will reduce the quality of data and even lead to invalid data, which has more and more serious impact on scientific results. This paper analyzes the requirements of RFI subtraction, summarizes the characteristics, suppression and reduction techniques and schemes of RFI, introduces some RFI subtractive methods used in some representative radio telescopes (or arrays), and analyzes and compares four common schemes. The advantages and disadvantages of prevention, pre-detection, pre-correlation and post-correlation. Accurate identification and marking of RFI is the key to reduce data loss and improve data quality effectively. It is also the ultimate goal of developing RFI subtractive technology. It is not difficult to find that the combination of the above four schemes will have higher practical value. In recent years, with the rapid development of high-speed digital signal processing and high-performance computing, It is possible to detect RFI in real-time mode based on a large amount of computing and in off-line mode from large scale interference data generated by large telescope arrays.
【作者單位】： 中國(guó)科學(xué)院上海天文臺(tái);中國(guó)科學(xué)院射電天文重點(diǎn)實(shí)驗(yàn)室;
【基金】：中國(guó)科學(xué)技術(shù)部政府間國(guó)際合作專項(xiàng)(2016YFE0100300) 國(guó)家自然科學(xué)基金項(xiàng)目(11650110438) 中國(guó)科學(xué)院天文財(cái)政專項(xiàng);中國(guó)科學(xué)院戰(zhàn)略性先導(dǎo)科技專項(xiàng)(B類)(XDB23010300);中國(guó)科學(xué)院國(guó)際博士后項(xiàng)目(2016PM024);中國(guó)科學(xué)院青年創(chuàng)新促進(jìn)會(huì)資助
【分類號(hào)】：P161
，

本文編號(hào)：1973078