The best detection conditions for pulsars in the Galactic disk  

作　　者：XU XiangYang WANG Chen HAN JinLin HU Lin 

机构地区：[1]College of Science, Guizhou University, Guiyang 550025, China [2]National Astronomical Observatories, Chinese Academy of Sciences, Beijing 100012, China

出　　处：《Science China(Physics,Mechanics & Astronomy)》2011年第3期552-557,共6页中国科学：物理学、力学、天文学（英文版）

基　　金：supported by the National Natural Science Foundation of China (Grant Nos. 10773016, 10821001 and 10833003);the Initialization Fund for President Award Winner of Chinese Academy of Sciences

摘　　要：Radio detection of pulsars in the Galactic disk is strongly affected by the dispersion and scattering effect of the interstellar medium and the Galactic background radio emission. In order to know the best conditions for discovery of pulsars, we select and simulate pulsar samples in the Galactic disk, and calculate the detection probability with various observation conditions (such as observational frequency, telescope aperture, receiver bandwidth and integration time). We have found that the detection fraction increases with the telescope aperture, receiver bandwidth and integration time. To detect pulsars in the nearer half of the Galactic disk, the observation frequency should be in the range of 1-2 GHz, while for pulsars in the farther half of the disk, the frequency should be in the range of 3.5-4.5 GHz. Due to the strong influence of scattering, the short period pulsars are hard to be detected, especially for pulsars in the farther half of the Galactic disk.Radio detection of pulsars in the Galactic disk is strongly affected by the dispersion and scattering effect of the interstellar medium and the Galactic background radio emission. In order to know the best conditions for discovery of pulsars, we select and simulate pulsar samples in the Galactic disk, and calculate the detection probability with various observation conditions （such as observational frequency, telescope aperture, receiver bandwidth and integration time）. We have found that the detection fraction increases with the telescope aperture, receiver bandwidth and integration time. To detect pulsars in the nearer half of the Galactic disk, the observation frequency should be in the range of 1–2 GHz, while for pulsars in the farther half of the disk, the frequency should be in the range of 3.5–4.5 GHz. Due to the strong influence of scattering, the short period pulsars are hard to be detected, especially for pulsars in the farther half of the Galactic disk.

关 键 词：pulsars neutron stars radio telescopes scattering of electromagnetic radiation in plasmas 

分 类 号：P145.6[天文地球—天体物理] TN957.51[天文地球—天文学]