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国家自然科学基金(11233005)

作品数:7 被引量:0H指数:0
相关作者:林伟鹏王如彬杜莹徐爱蕾更多>>
相关机构:中国科学院大学中山大学中国科学院上海天文台更多>>
发文基金:国家自然科学基金国家重点基础研究发展计划更多>>
相关领域:天文地球生物学自动化与计算机技术更多>>

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7 条 记 录,以下是 1-7
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How to co-add images? I. A new iterative method for image reconstruction of dithered observations
2017年
By employing the previous Voronoi approach and replacing its nearest neighbor approx- imation with Drizzle in iterative signal extraction, we develop a fast iterative Drizzle algorithm, namedfiDrizzle, to reconstruct the underlying band-limited image from undersampled dithered frames. Compared with the existing iDrizzle, the new algorithm improves rate of convergence and accelerates the computational speed. Moreover, under the same conditions (e.g. the same number of dithers and iterations), fiDrizzle can make a better quality reconstruction than iDrizzle, due to the newly discov- ered High Sampling caused Decelerating Convergence (HSDC) effect in the iterative signal extraction process.fiDrizzle demonstrates its powerful ability to perform image deconvolution from undersampled dithers.
Lei WangGuo-Liang Li
Color gradients of the galaxies at 0.5<z<1Ⅰ.Dependence on galaxy global properties
2018年
We investigate the color gradients of galaxies at 0.5 < z < 1.0, using a sample of ~35 000 galaxies with both spectroscopy from the final data release of the VIMOS Public Extragalactic Redshift Survey(VIPERS), and photometry in ultraviolet/optical/near-infrared bands from the VIPERS-MultiLambda Survey(VIPERS-MLS) and the Canada-France-Hawaii Telescope Legacy Survey(CFHTLS).We estimate rest-frame colors, stellar mass, star formation rate from fitting the Spectral Energy Distribution(SED) for each galaxy, as well as a two-zone color ?(u-r), defined as the difference in rest-frame(u-r) color between the outer and inner region of the galaxy. We find that the two-zone color shows weak or no correlations with all galaxy properties considered except stellar mass. On average, ?(u-r) decreases with increasing stellar mass, indicating relatively red colors in galactic centers of more massive galaxies. We then compare the properties of "red-cored" and "blue-cored" galaxies,defined to have either a negative or a positive ?(u-r) respectively. Although the two types of galaxies show similar distributions in most properties, we find massive red-cored galaxies with M*> 1010.5M⊙to have larger sizes at given stellar mass(thus lower surface mass densities), and less massive red-cored galaxies with M*< 1010.5M⊙to have lower central galaxy fraction. These findings can be understood if one assumes that the star formation process happens from inside out, in the same way as recently emphasized in studies of low-z galaxies. The similarity between the galaxies at intermediate redshifts and those at low redshifts supports the idea that galaxy evolution since z~1 has been mainly driven by secular processes internal to galaxies rather than galaxy mergers or external environment.
Zhi-Xiong LiangCheng Li
Color gradients of the galaxies at 0.5<z<1Ⅱ.Clustering properties
2018年
We investigate the dependence of clustering on luminosity, stellar mass and color gradient for galaxies at 0.5 < z < 1, using a sample of;300 galaxies from the final data release of the VIMOS Public Extragalactic Redshift Survey(VIPERS-PDR2). We estimate both the auto-correlation function for galaxy samples selected by B-band absolute magnitude and stellar mass, and the cross-correlation function of galaxy samples selected by color gradient with respect to the full galaxy sample. The autocorrelation function amplitudes at fixed scale are found to positively correlate with both galaxy luminosity and stellar mass, and the effect holds for all the scales probed(0.2 h;Mpc < rp< 20 h;Mpc),in good agreement with previous measurements based on an earlier data release of VIPERS. When the stellar mass is limited to a narrow range, we find the clustering power to be essentially independent of galaxy color gradient, and this conclusion is true for all the masses and all the scales considered here. In a parallel paper, we find that the half-light radius is the only galaxy property other than stellar mass that is related to color gradient. Considering the previous finding that clustering depends weakly on galaxy structure at given mass, the non-dependence of clustering on color gradient found here reinforces our conclusion that the color gradient and structural parameters of a galaxy are intrinsically related to each other.
Zhi-Xiong LiangCheng Li
宇宙大尺度结构数值模拟的研究进展
2018年
宇宙的结构是由初始密度扰动发展而成的。在引力和宇宙膨胀的作用下,初始密度扰动不断增长,经过线性和非线性阶段,逐渐演化为现今的宇宙结构。在一个给定的宇宙学模型下,可以用一系列动力学方程来描述宇宙中暗物质和重子物质的运动及演化历史。在过去的几十年间,随着算法的完善和计算机技术的发展,从最初几十个粒子的纯引力模拟到1010个粒子在秒差距量级的多体加流体动力学模拟,大量不同的数值模拟技术被用来研究宇宙结构的形成和演化。在这个过程中,数值模拟的分辨率和精度不断提高,模型中对重子物质物理过程的描述也越来越完善。这些模拟技术与观测结果相结合,使人们对宇宙的大尺度结构以及星系团的形成和演化有了更深刻的理解,也在一定程度上影响了观测的发展方向和设备研发。不同数值模拟结果在纯引力研究方面得到了较好的统一,但不同的星系模型使得流体模拟的结果存在较大的差异。
唐林林伟鹏
关键词:宇宙大尺度结构数值模拟多体动力学流体动力学
嗅球中神经元间的相互作用及同步运动分析
2013年
嗅球对嗅觉信息的处理是嗅觉系统信号编码的一个重要环节,其中兴奋性的僧帽细胞(Mitral Cell,MC)与抑制性的颗粒细胞(Granular Cell,GC)的相互作用尤为关键。本文首先介绍了嗅觉系统网络中关于同步振荡的研究现状,然后建立嗅球中僧帽细胞及颗粒细胞的动力学模型,仿真得到了单个僧帽细胞、颗粒细胞以及僧帽细胞与颗粒细胞在耦合条件下神经元的发放模式。结果表明,僧帽细胞对颗粒细胞有兴奋性作用,而颗粒细胞对僧帽细胞有抑制性作用,细胞放电序列随着突触连接强度的改变而改变。此外,建立简单的嗅觉网络模型,分析了当颗粒细胞分别构成环形和网格状两种拓扑结构时,不同网络对两个僧帽细胞同步性的影响,用同步性指标ISI-distance刻画同步程度。数值分析表明颗粒细胞网格状的拓扑结构对僧帽细胞的同步性作用更为明显一些。
徐爱蕾杜莹王如彬
关键词:嗅球颗粒细胞网络建模
An empirical model to form and evolve galaxies in dark matter halos
2016年
Based on the star formation histories of galaxies in halos with different masses, we develop an empirical model to grow galaxies in dark matter halos. This model has very few ingredients, any of which can be associated with observational data and thus be efficiently assessed. By applying this model to a very high resolution cosmological N-body simulation, we predict a number of galaxy properties that are a very good match to relevant observational data. Namely, for both centrals and satellites, the galaxy stellar mass functions up to redshift z=4 and the conditional stellar mass functions in the local universe are in good agreement with observations. In addition, the two point correlation function is well predicted in the different stellar mass ranges explored by our model. Furthermore, after applying stellar population synthesis models to our stellar composition as a function of redshift, we find that the luminosity functions in the 0.1 u,0.19, 0.1r, 0.1i and 0.1z bands agree quite well with the SDSS observational results down to an absolute magnitude at about -17.0. The SDSS conditional luminosity function itself is predicted well. Finally, the cold gas is derived from the star formation rate to predict the HI gas mass within each mock galaxy. We find a remarkably good match to observed HI-to-stellar mass ratios. These features ensure that such galaxy/gas catalogs can be used to generate reliable mock redshift surveys.
Shi-Jie LiYou-Cai ZhangXiao-Hu YangHui-Yuan WangDylan TweedCheng-Ze LiuLei YangFeng ShiYi LuWen-Tao LuoJian-Wen Wei
关键词:COSMOLOGYHALOS
Probing the Missing Baryons via kSZ Stacking
2016年
Kinetic Sunyaev-Zel'dovich (kSZ) stacking has great potential to become a powerful probe of missing baryons, due to advances in CMB experiments and galaxy surveys. In this paper, we study kSZ stacking in hydrodynamic simulations with different gastrophysics. We quantify the kSZ stacking signal as a function of halo mass, redshift and projection depth. We compare between different simulations to estimate the impact of gastrophysics such as cooling and supernova feedback. Furthermore, we measure the contribution from warm-hot intergalactic medium (WHIM), which is believed to be the reservoir for most, if not all, missing baryons. We find that the WHIM contribution is significant, at the level of ~ 10%-70%, depending on the angular separation from the stacked halos and other factors. However, contribution from the intracluster medium along the line of sight is in general non-negligible. This complexity requires more detailed and comprehensive analysis on probing the missing baryons with kSZ stacking.
Han MiaoWei-Peng LinPeng-Jie Zhang
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