中国丽江积分视场光纤光谱仪(China Lijiang Integral Field Unit,简称CHILI)是中国第一台用于夜天文观测的科学级积分视场光纤光谱仪,安装在丽江天文观测站2.4 m光学望远镜上。CHILI运输到中国前,在美国德克萨斯大学奥斯汀分校(Univers...中国丽江积分视场光纤光谱仪(China Lijiang Integral Field Unit,简称CHILI)是中国第一台用于夜天文观测的科学级积分视场光纤光谱仪,安装在丽江天文观测站2.4 m光学望远镜上。CHILI运输到中国前,在美国德克萨斯大学奥斯汀分校(University of Texas at Austin)进行了实验室测试。本次实验主要针对CHILI的蓝端,主要测试内容有本底、平场、暗场和波长定标。为了明确知道谱线在像素位置上的精准波长和CHILI探测器的分辨能力,对测试数据进行了波长定标和光谱分辨能力的计算。结果显示,CHILI蓝端的波长范围约为3 500～5 300,在此波长范围内,光谱分辨本领FW H M■5,其对应的光谱分辨率R=λ/?λ约为600～1 000,符合CHILI预期要求。展开更多
P141.5 95010688类量体光谱的Monte Carlo模拟及高红移类量体颜色法巡天中的选择效应=Discussions on selectioneffects of multcolor survey for high red-shiftQSQs by using Monte-Carlo simulations[刊,中]/樊晓辉,陈建生(中科院北...P141.5 95010688类量体光谱的Monte Carlo模拟及高红移类量体颜色法巡天中的选择效应=Discussions on selectioneffects of multcolor survey for high red-shiftQSQs by using Monte-Carlo simulations[刊,中]/樊晓辉,陈建生(中科院北京天文台)//天体物理学报.—1994,14(2).—124—136利用已知的统计结果对高红移类星体光谱进行Monte Carlo模拟,得到了VBVRI五色测光的色指数,并利用模拟的选择判据计算了选择效应函数。当2.4【z【3.0时,选择效应来自于与主序星的的混淆;当z】3.0时,则是由于较暗的类星体与晚型矮星同时从U.B等颜色的图象上消失,导致可利用色指数的减少。图8表3参16(严寒)展开更多
A recently released XMM-Newton note revealed a significant calibration issue between nuclear spectroscopic telescope array(NuSTAR)and XMM-Newton European Photon Imaging Camera(EPIC)and provided an empirical correction...A recently released XMM-Newton note revealed a significant calibration issue between nuclear spectroscopic telescope array(NuSTAR)and XMM-Newton European Photon Imaging Camera(EPIC)and provided an empirical correction to the EPIC effective area.To quantify the bias caused by the calibration issue in the joint analysis of XMM-NuSTAR spectra and verify the effectiveness of the correction,in this work,we perform joint-fitting of the NuSTAR and EPIC-pn spectra for a large sample of 104 observation pairs of 44 X-ray bright active galactic nuclei(AGN).The spectra were extracted after requiring perfect simultaneity between the XMM-Newton and NuSTAR exposures(merging good time intervals(GTIs)from two missions)to avoid bias due to the rapid spectral variability of the AGN.Before the correction,the EPIC-pn spectra are systematically harder than the corresponding NuSTAR spectra by■subsequently yielding significantly underestimated cutoff energy E_(cut)and the strength of reflection component R when performing joint-fitting.We confirm that the correction is highly effective and can commendably erase the discrepancy in best-fitΓ,E_(cut),and R.We thus urge the community to apply the correction when joint-fitting XMM-NuSTAR spectra,but note that the correction is limited to 3–12 keV and therefore not applicable when the soft X-ray band data are included.Besides,we show that as merging GTIs from two missions would cause severe loss of NuSTAR net exposure time,in many cases,joint-fitting yields no advantage compared with utilizing NuSTAR data alone.Finally,We present a technical note on filtering periods of high background flares for XMM-Newton EPIC-pn exposures in the small window(SW)mode.展开更多
文摘中国丽江积分视场光纤光谱仪(China Lijiang Integral Field Unit,简称CHILI)是中国第一台用于夜天文观测的科学级积分视场光纤光谱仪,安装在丽江天文观测站2.4 m光学望远镜上。CHILI运输到中国前,在美国德克萨斯大学奥斯汀分校(University of Texas at Austin)进行了实验室测试。本次实验主要针对CHILI的蓝端,主要测试内容有本底、平场、暗场和波长定标。为了明确知道谱线在像素位置上的精准波长和CHILI探测器的分辨能力,对测试数据进行了波长定标和光谱分辨能力的计算。结果显示,CHILI蓝端的波长范围约为3 500～5 300,在此波长范围内,光谱分辨本领FW H M■5,其对应的光谱分辨率R=λ/?λ约为600～1 000,符合CHILI预期要求。
文摘P141.5 95010688类量体光谱的Monte Carlo模拟及高红移类量体颜色法巡天中的选择效应=Discussions on selectioneffects of multcolor survey for high red-shiftQSQs by using Monte-Carlo simulations[刊,中]/樊晓辉,陈建生(中科院北京天文台)//天体物理学报.—1994,14(2).—124—136利用已知的统计结果对高红移类星体光谱进行Monte Carlo模拟,得到了VBVRI五色测光的色指数,并利用模拟的选择判据计算了选择效应函数。当2.4【z【3.0时,选择效应来自于与主序星的的混淆;当z】3.0时,则是由于较暗的类星体与晚型矮星同时从U.B等颜色的图象上消失,导致可利用色指数的减少。图8表3参16(严寒)
基金supported by the National Natural Science Foundation of China(12033006,12192221,123B2042).
文摘A recently released XMM-Newton note revealed a significant calibration issue between nuclear spectroscopic telescope array(NuSTAR)and XMM-Newton European Photon Imaging Camera(EPIC)and provided an empirical correction to the EPIC effective area.To quantify the bias caused by the calibration issue in the joint analysis of XMM-NuSTAR spectra and verify the effectiveness of the correction,in this work,we perform joint-fitting of the NuSTAR and EPIC-pn spectra for a large sample of 104 observation pairs of 44 X-ray bright active galactic nuclei(AGN).The spectra were extracted after requiring perfect simultaneity between the XMM-Newton and NuSTAR exposures(merging good time intervals(GTIs)from two missions)to avoid bias due to the rapid spectral variability of the AGN.Before the correction,the EPIC-pn spectra are systematically harder than the corresponding NuSTAR spectra by■subsequently yielding significantly underestimated cutoff energy E_(cut)and the strength of reflection component R when performing joint-fitting.We confirm that the correction is highly effective and can commendably erase the discrepancy in best-fitΓ,E_(cut),and R.We thus urge the community to apply the correction when joint-fitting XMM-NuSTAR spectra,but note that the correction is limited to 3–12 keV and therefore not applicable when the soft X-ray band data are included.Besides,we show that as merging GTIs from two missions would cause severe loss of NuSTAR net exposure time,in many cases,joint-fitting yields no advantage compared with utilizing NuSTAR data alone.Finally,We present a technical note on filtering periods of high background flares for XMM-Newton EPIC-pn exposures in the small window(SW)mode.
