Hubble Space Telescope imaging of the progenitor sites of six nearby core-collapse supernovae

The search for the progenitors of six core-collapse supernovae (CCSNe) in archival Hubble Space Telescope ( HST ) WFPC2 pre-explosion imaging is presented. These SNe are 1999an, 1999br, 1999ev, 2000ds, 2000ew and 2001B. Post-explosion imaging of the SNe, with the HST ACS/WFC, has been utilized with the technique of differential astrometry to identify the progenitor locations on the pre-explosion imaging. SNe 1999br, 1999ev, 2000ew and 2001B are recovered in late-time imaging, and estimates of the progenitor locations on the pre-explosion imaging, with subpixel accuracy, have been made. Only the progenitor of the Type II-P SN 1999ev has been recovered, on pre-explosion F555W imaging, at a 4.8σ significance level. Assuming a red supergiant progenitor, the pre-explosion observation is consistent with   M _ZAMS= 15–18 M_⊙  . The progenitors of the other five SNe were below the 3σ detection threshold of the pre-explosion observations. The detection thresholds were translated to mass limits for the progenitors by comparison with stellar evolution models. Pre-explosion observations of the peculiarly faint SN 1999br limit the mass of a red supergiant progenitor to   M _ZAMS < 12 M_⊙  . Analysis has been extended, from previous studies, to include possible detections of high- T _eff, high-mass stars by conducting synthetic photometry of model Wolf–Rayet star spectra. The mass limits for the Type II-P SNe 1999an and 1999br are consistent with previously determined mass limits for this type of SN. The detection limits for the progenitors of the Type Ibc SNe (2000ds, 2000ew and 2001B) do not permit differentiation between high-mass Wolf–Rayet progenitors or low-mass progenitors in binaries.     

Chandra observations of the X-ray jet in 3C 66B

Our Chandra observation of the FR I radio galaxy 3C 66B has resulted in the first detection of an X-ray counterpart to the previously known radio, infrared and optical jet. The X-ray jet is detected up to 7 arcsec from the core and has a steep X-ray spectrum, α ≈1.3±0.1 . The overall X-ray flux density and spectrum of the jet are consistent with a synchrotron origin for the X-ray emission. However, the inner knot in the jet has a higher ratio of X-ray to radio emission than the others. This suggests that either two distinct emission processes are present or differences in the acceleration mechanism are required; there may be a contribution to the emission from the inner knot from an inverse Compton process or it may be the site of an early strong shock in the jet. The peak of the brightest radio and X-ray knot is significantly closer to the nucleus in the X-ray than in the radio, which may suggest that the knots are privileged sites for high-energy particle acceleration. 3C 66B's jet is similar both in overall spectral shape and in structural detail to those in more nearby sources such as M87 and Centaurus A.     

A search for giant pulses in Vela-like pulsars

We have carried out a survey for 'giant pulses' in six young, Vela-like pulsars. In no cases did we find single pulses with flux densities more than 10 times the mean flux density. However, in PSR  B1706–44  we have detected giant micro-pulses very similar to those seen in the Vela pulsar. In PSR  B1706–44  these giant micro-pulses appear on the trailing edge of the profile and have an intrinsic width of ∼1 ms. The cumulative probability distribution of their intensities is best described by a power law. If the power law continues to higher intensities, then  3.7×10⁶  rotations are required to obtain a pulse with 20× the mean pulse flux. This number is similar to the giant pulse rate in PSR B1937+21 and PSR  B1821–24  but significantly higher than that for the Crab.     

The Forming Conditions of and Ore-searching Direction for B, Mg,Pb, Zn and Au Deposits in the Liaoji Proterozoic Rift

The Proterozoic was the first of severa1 impor-tant transitional periods in the earth's evolutionaryhistory. Linear .rifts over1apped on the b4se ofArchean granite -- greenstone and high -- grade gneissregimes. Along with the formation and evolution ofthe…     

BiOBr/铁改性蒙脱石对罗丹明B的光催化降解性能研究

在低温条件下通过铁改性蒙脱石与BiOBr复合成功合成了一种新型的光催化材料,称为BiOBr/Fe-Mt。运用X射线粉末衍射(XRD)、透射电镜(TEM)、傅立叶转换红外光谱(FTIR)、紫外可见漫反射光谱(UV-Vis DRS)对BiOBr/Fe-Mt材料进行表征。同时以λ400 nm的可见光为光源,开展该催化剂对罗丹明B(Rh B)的光催化降解实验以评估其光催化活性。结果表明,支撑材料投加量被固定在2.5 g的条件下,采用铁改性蒙脱石制备的BiOBr/Fe-Mt材料对Rh B的光催化降解活性高于采用钠基蒙脱石制备的BiOBr/Na-Mt。光催化活性的显著提高,主要归因于:1 BiOBr/Fe-Mt的禁带宽度降低至2.46 e V,或可能形成了BiOBr/铁氧化物异质结结构;2 BiOBr/Fe-Mt上仅发生较少的十六烷基三甲基溴化铵有机分子残留。这些结构因素均可以有效促进BiOBr/Fe-Mt上Rh B的光催化降解。     

地理信息系统在城市规划管理中的应用

以往的城市规划业务流程更多的是在C/S结构的软件系统下实现,近几年随着网络技术的发展,大部分已转向在B/S结构下实现,但由于地理信息系统技术在B/S结构下的空间数据管理及更新等操作上的技术瓶颈,要求它要以新的方式为规划管理业务提供图形支持。本文从将这种图形支持分成几个大的功能模块的基础上,阐述如何将地理信息系统的新技术应用到规划行业,并开发应用系统。     

多目标珊瑚岛礁地貌遥感信息提取方法——以西沙永乐环礁为例

南海珊瑚岛礁资源极为丰富,实时、快速、高效、准确地获取大范围珊瑚岛礁地貌遥感信息具有现实意义.研究提出了一种双尺度转化下的模型与数据混合驱动的岛礁地貌信息提取框架,并设计了珊瑚岛礁地貌分类体系及相应技术流程:首先采用自上而下模型驱动的GVF Snake模型进行宏观地理分带的粗分割,然后采用自下而上数据驱动的云影极值抑制下多阈值OTSU分类算法进行微观地貌类型的精细分类,最终利用区域生长算法提取离散分布的暗沙、暗滩等浅水地貌单元.针对西沙永乐环礁利用CBERS-02B数据进行实验,精度验证表明:珊瑚岛礁地貌遥感信息提取方法总体精度优于经典数据驱动的监督分类算法,且具有抗噪能力强、顾及空间拓扑关系、自动灵活等特点.     

‘Bubbling’ and the Kyoto mechanisms

Abstract

The Kyoto Protocol allows a group of Annex B countries to fulfill their emissions limitation commitments jointly by forming a “bubble” equal to their collective commitment. Annex B countries, whether members of a bubble or not, can use the Kyoto mechanisms to help meet their emissions limitation commitments. I argue that Kyoto mechanism rules should be applied to Parties individually regardless of their membership in a bubble. This means there are virtually no advantages to joining a bubble, but it is not clear that the option to form a bubble should confer benefits on the members relative to other Annex B Parties that do not join a bubble.