Long-term optical,X-ray and γ-ray data of blazar 3 C 279 have been compiled from Swift-XRT,RXTE-PCA,Fermi-LAT,SMARTS and literature.The source exhibits strong variability on long timescales.From the 1980 s until now,the optical R band light curve spans more than 32 yr,and a possible 5.6-yr-long quasi-periodic variation component has been found in it.The optical spectral behavior has been investigated.In the optical band,the mean spectral index is –1.71.The source exhibits an obvious special spectral behavior.In the low state,the source manifests a clear bluer-when-brighter behavior in the sense that the optical spectrum turns harder(flatter) when the brightness increases.While in the high state,the optical spectrum is stable,which means the source spectral index does not vary with brightness.The correlation analysis has been performed among optical,X-ray and γ-ray energy bands.The result indicates that the variations of γ-ray and X-ray bands are well correlated without time delay on the timescale of days,and their variations exhibit weak correlations with those of the optical band.The variations,especially outbursts,are simultaneous,but the magnitude of variations is disproportionate.The detailed analysis reveals that the main outbursts exhibit strong correlations in different γ-ray,X-ray and optical bands.
Bing-Kai ZhangMin JinXiao-Yun ZhaoLi ZhangBen-Zhong Dai
PKS 2155-304 is a well studied BL Lac object in the southern sky. The historical optical data during different periods have been collected and compiled. Light curves spanning 35 yr have been constructed. The R-band light curve has been analyzed by means of three methods: the epoch folding method,the Jurkevich method and the discrete correlation function method. It is derived that there is an evident periodic component of 317 d(i.e. 0.87 yr) superposed on a long-term trend with largeamplitude variation in the light curve. The variability of this source is accompanied by a slight color variation,and the brightness and color index are correlated with each other. On a long-term time scale,PKS 2155-304 exhibits a tendency of bluer-whenbrighter,which means the spectrum becomes flatter when the source brightens.
Bing-Kai ZhangXiao-Yun ZhaoChun-Xiao WangBen-Zhong Dai
目前,偏振遥感已被用于气溶胶卫星和地基遥感中,其仅对小粒子敏感。本研究以2007-2008年间的POLDER(Polarization and Directionality of the Earth’s Reflectances)和AERONET(Aerosol Robotic Network)合肥站的气溶胶数据为研究对象,探讨了偏振遥感对气溶胶粒子尺度的敏感性。利用AERONET合肥站的尺度分布数据和折射指数数据,计算了不同尺度范围内气溶胶粒子的光学厚度,并与对应的POLDER反演结果作拟合,通过寻找最佳拟合对应的尺度范围确定偏振遥感敏感的粒子尺度。结果表明,偏振遥感并非对所有尺度的小模式气溶胶粒子都敏感,在865 nm波段,其敏感的气溶胶粒子上限半径约为0.3μm左右。这一结果对指导气溶胶偏振遥感,以及理解和应用偏振遥感气溶胶产品等具有重要意义。
The long-term optical and infrared color variability of blazars has been investigated with monitoring data from the Small and Moderate Aperture Research Telescope System(SMARTS). The sample in this study consists of 49 flat spectrum radio quasars(FSRQs) and 22 BL Lacertae objects(BL Lacs). The fractional variability amplitudes of each source have been calculated in both optical R band and infrared J band. Overall, the variability amplitudes of FSRQs are larger than those of BL Lacs. The results also suggest that the variability amplitude of most FSRQs is larger at a lower energy band(J band) than at a higher one(R band), but the variability amplitude of BL Lacs is larger at the higher energy band. Both types of blazars display color variation along with variability in brightness. However, they show different variation behaviors in general. In the whole data set, 35 FSRQs exhibit redder-whenbrighter trends, and 11 FSRQs exhibit opposite trends; 11 BL Lacs follow bluer-whenbrighter trends, and seven BL Lacs follow opposite trends. A detailed examination indicates that there are 10 blazars showing redder-when-brighter trends in their low state, and bluer-when-brighter or stable-when-brighter trends in their high state. Some more complicated color behaviors have also been detected in several blazars. The nonthermal jet emission and the thermal emission from the accretion disk are employed to explain the observed color behaviors.
Bing-Kai ZhangXiao-Shan ZhouXiao-Yun ZhaoBen-Zhong Dai
