Determination of silver ion based on the redshift of emission wavelength of quantum dots functionalized with rhodanine

A simple and selective method for the determination of silver ions was developed by utilizing the red- shift in emission wavelength of the core-shell CdSe/Cd5 quantum dots （QDs） functionalized with rhodanine upon the addition of Ag＋. A linear relationship was observed between the shift and the increase in concentration of Ag＋ in the range of 0.0125-12.5 μmol/L. The mechanism of the red-shift was investigated and suggested that the coordination between Ag＋ and rhodanine on the QDs surface caused an increase of particle size, which resulted in the red-shift of the QDs＇ emission wavelength. A detection limit of 2 nmol/L was achieved. The developed method showed superior selectivity and was successfully applied to the determination of silver in environmental samples.     

一种快速求红移和证认谱线的新方法--伪三角法

对于河外天体，谱线证认和红移确定是光谱分析的第一步。本文在仔细分析天体光谱特点的基础上，提出了一种全新的求红移和证认谱线的新方法--伪三角法。该方法利用最强的三根谱线的波长信息构造“三角形”，通过将最大角的“余弦”与已知模板的“余弦”表相匹配，反推得到相应的标准谱线波长，并进而得到红移值。通过这个红移值，可以得到所有的谱线的标准位置，这就相当于谱线证认。结果表明：这种方法在大大减少运算量的同时，保持了较高的正确识别率和极低的误识率。这对海量光谱数据的处理具有重要的意义。同时，该方法立意新颖，简单明了，容易实现。缺点是对于谱线少于3根的光谱以及噪声很大的光谱不能有效地处理。     

Structural,optical and magnetic properties of chromium and manganese co-doped SnO2 nanoparticles

The rutile phase Sn_0.99-xMn_xCr_0.01O₂ (x = 0.00, 0.01, 0.03, 0.05 and 0.07) nanoparticles were synthesized by facile chemical co-precipitation method using poly ethylene glycol (PEG) as a capping agent. The samples were characterized by EDAX to confirm the expected stoichiometry. The X-ray diffraction (XRD), transmission electron microscopy (TEM) and Fourier transform infrared (FTIR) spectroscopy analyses of these samples showed the formation of impurity free crystals with a single phase rutile type tetragonal crystal structure as that of (P4₂/mnm) of SnO₂. Optical absorption spectra and corresponding Tauc's plots showed a redshift of the absorption edge in SnO₂ after being co-doped with Cr and Mn. The samples were examined for its magnetic property using vibrating sample magnetometer which indicated that transition of magnetic signals from ferromagnetic to the paramagnetic nature with inclusion of Mn content in SnO₂: Cr host matrix. The observed magnetic behavior is well supported with the bound magnetic polarons (BMPs) model.     

Constant gravitational fields and redshift of light

The solutions of Einsteins's equations in a constant energy-momentum tensor field are Ricci curvature homogeneous. Convenient perturbations of a Lorentz solvmanifold yield such curvature homogeneous metrics, prescribing redshift of light and singularities.     

一种新的活动星系光谱红移自动测量方法

星系红移的自动测量对进行大样本天文学研究如宇宙学大尺度结构研究具有重要意义。星系一般分为正常星系和活动星系两种,活动星系光谱一般具有较明显的发射线特征。文章提出了一种不用精确提取谱线而快速测量活动星系光谱红移的方法。该方法包括步骤：(1)对待测光谱进行去噪;(2)利用小波变换提取低频成分光谱,并用去噪后光谱减去低频谱得到残差谱;(3)计算残差谱的均方差,并保留大于阈值的波长集合(4)根据标准谱线表计算所有候选红移;(5)利用Parzen窗估计方法计算红移密度最大点,并在邻域内求均值确定最终红移。对模拟数据和SDSS DR7部分实测数据的测试表明,该方法是鲁棒的并且具有较高的红移测量正确率。     

基于多分辨率融合距离的低质量星系光谱红移测量方法

星系光谱红移测量是大规模天体光谱巡天项目中的一个重要研究内容,其目的是从在光谱中测量出对应星系由于多普勒效应引起的红移。随着银河系外巡天项目的开展,观测目标距离(红移)越来越远,其星等越来越暗,光谱的质量也随之越来越差,如何能够有效准确地从这些低质量的光谱测量出红移是河外巡天面临的一个重要问题。基于此问题,充分考虑到低质量星系光谱的特点及数据特征,新定义了一种针对低质量巡天光谱数据的多分辨率融合距离,以此为基础提出一种针对低质量星系光谱的红移测量方法。该方法充分结合不同分辨率下光谱的特征,计算距离时首先将模板光谱和待测光谱同时降到多个相同分辨率下,该分辨率下所有波长采样点都计算一个偏差进而得到一个距离,然后将多个分辨率下得到的距离通过加权得到一个融合距离。基于多分辨率融合距离提出的星系红移测量方法,能够有效的解决低质量星系光谱的红移无法准确测量的问题。研究了不同信噪比下红移测量的精度,在信噪比大于5之后,该方法测量准确率可以达到90%以上。大量实验表明,提出的方法在星系光谱质量较低的情况可以非常准确地从中测量出红移,测量误差和红移大小无关,可以很好地应用于大规模巡天数据的星系光谱红移测量中。     

星系哈勃红移的非多普勒效应解释

分析了多普勒效应在解释星系哈勃红移现象时,星系际光传播过程存在的能量不守恒和宇宙膨胀时空不平权两大问题;提出了＂时空物质属性＂的3个基本假设;最后阐述了星系哈勃红移的非多普勒效应解释。     

Constraints on dark energy and modified gravity models by the Cosmological Redshift Drift test

We study cosmological constraints on the various accelerating models of the universe using the time evolution of the cosmological redshift of distant sources. The important characteristic of this test is that it directly probes the expansion history of the universe. In this work we analyze the various models of the universe which can explain the late time acceleration, within the framework of General Theory of Relativity (GR) (XCDM, scalar field potentials) and beyond GR (f(R)$f(R)$ gravity model).     

一种基于交叉相关的类星体的红移测量方法

给出了一种新的类星体光谱的红移测量方法。首先,利用提取出的发射谱线信息确定一组红移候选;然后,按这些红移候选将静止模板光谱红移,计算所得光谱与目标光谱的相关值;最后,确定最大相关值对应的红移候选为目标光谱的红移。相对于已有的基于谱线匹配的方法,此方法的性能受谱线提取效果的影响较小。实验结果表明： 此方法的鲁棒性较好,性能优于基于谱线匹配的方法。     

Redshift modification of pulsars and magnetars by relativistic plasmas and vacuum polarization

The redshifts of emissions from pulsars and magnetars consist of two components: gravitational and non-gravitational redshifts. The latter results from the electromagnetic and kinetic effects of relativistic plasmas, characterized by refractive indices and streaming velocities of the media, respectively. The vacuum polarization effect induced by strong magnetic fields can modify the refractive indices of the media, and thus leads to a modification to the redshifts. The Gordon effective metric is introduced to study the redshifts of emissions. The modification of the gravitational redshift, caused by the effects of relativistic plasmas and vacuum polarization, is obtained.