A Chandra observation of the X-ray environment and jet of 3C 31

We have used a deep Chandra observation of the central regions of the twin-jet Fanaroff–Riley class I (FRI) radio galaxy 3C 31 to resolve the thermal X-ray emission in the central few kpc of the host galaxy, NGC 383, where the jets are thought to be decelerating rapidly. This allows us to make high-precision measurements of the density, temperature and pressure distributions in this region, and to show that the X-ray emitting gas in the centre of the galaxy has a cooling time of only  5×10⁷ yr  . In a companion paper, these measurements are used to place constraints on models of the jet dynamics.
A previously unknown one-sided X-ray jet in 3C 31, extending up to 8 arcsec from the nucleus, is detected and resolved. Its structure and steep X-ray spectrum are similar to those of X-ray jets known in other FRI sources, and we attribute the radiation to synchrotron emission from a high-energy population of electrons. In situ particle acceleration is required in the region of the jet where bulk deceleration is taking place.
We also present X-ray spectra and luminosities of the galaxies in the Arp 331 chain of which NGC 383 is a member. The spectrum and spatial properties of the nearby bright X-ray source 1E 0104+3153 are used to argue that the soft X-ray emission is mostly due to a foreground group of galaxies rather than to the background broad absorption-line quasar.     

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.     

Holocene environmental reconstruction from deltaic deposits in northeast Greenland

Terraces of different age in the Zackenberg delta, located at 74°N in northeast Greenland, have provided the opportunity for an interdisciplinary approach to the investigation of Holocene glacial, periglacial, pedological, biological and archaeological conditions that existed during and after delta deposition. The raised Zackenberg delta accumulated mainly during the Holocene Climatic Optimum, starting slightly prior to 9500 cal. yr BP (30 m a.s.l.) and continued until at least 6300 cal. yr BP (0.5 m a.s.l.). Evidence of sea‐level change is based on conventional ¹⁴C dates of shells from the marine delta bottomsets, ¹⁴C AMS dating of macroscopic plant material from the foresets and of fluvial deposits. Arthropod and plant remains from 7960 cal. yr BP in the delta foresets include the oldest evidence of the arctic hare in Greenland and evidence of a rich herb flora slightly different from the modern flora. Empetrum nigrum and Salix herbacea remains indicate a summer temperature at least as high as today during delta deposition. Post‐depositional nivation activity, dated by luminescence, lichenometry and Schmidt Hammer measurements indicate mainly late Holocene activity, at least since 2900 yr BP, including Little Ice Age (LIA) avalanche activity. Pedological analyses of fossil podsols in the Zackenberg delta, including ¹⁴C AMS dating of selected organic rich B‐horizons, show continued podsol development during the Holocene Climatic Optimum and into the subsequent colder period of the late Holocene, until 3000–2400 yr BP. A Neo‐Eskimo house ruin found on the lower part of the delta, presently being eroded by the sea, is dated to AD 1800. It presumably was abandoned prior to AD 1869, and suggests that some of the last Eskimos that lived in northeast Greenland might have occupied the Zackenberg delta. Copyright © 2002 John Wiley & Sons, Ltd.     

Chandra measurements of the X-ray core and cluster of 3C 220.1

We report results of an 18-ks exposure with the ACIS instrument on Chandra of the powerful z =0.62 radio galaxy 3C 220.1. The X-ray emission separates into cluster gas of emission-weighted kT ∼5 keV , 0.7–12 keV luminosity (to a radius of 45 arcsec) of 5.6×10⁴⁴ erg s⁻¹ and unresolved emission (coincident with the radio core). While the extended X-ray emission is clearly thermal in nature, a straightforward cooling-flow model, even in conjunction with a point-source component, is a poor fit to the radial profile of the X-ray emission. This is despite the fact that the measured properties of the gas suggest a massive cooling flow of ∼130 M_⊙ yr⁻¹, and the data show weak evidence for a temperature gradient. The central unresolved X-ray emission has a power-law spectral energy index α ∼0.7 and 0.7–12 keV luminosity of 10⁴⁵ erg s⁻¹, and any intrinsic absorption is relatively small. The two-point spectrum of the core emission between radio and X-ray energies has α _rx=0.75 . Since this is a flatter spectrum than seen in other sources where the X-ray emission is presumed to be radio-related, regions close to the active galactic nucleus (AGN) in this source may dominate the central X-ray output, as is believed to be the case for lobe-dominated quasars. Simple unification models would be challenged if this were found to be the case for a large fraction of high-power radio galaxies.     

Evidence for Chemical Heterogeneity in the Nucleus of C/1995 O1 (Hale–Bopp)

We present an analysis of OH, CN, and C₂ jets observed in thecoma of Comet Hale–Bopp on UT April 22, 23, and 25, 1997. Monte Carlomodels designed to simulate the gas jets were employed to analyze thenuclear active areas responsible for the observed coma gas jets. Ourresults indicate that four active areas are necessary to reproduce theCN and C₂ jets while five active areas are required to simulatethe OH jets. The additional OH active area must produce significantlevels of OH, but cannot emit measurable quantities of either carbonradical. This difference suggests that the nucleus of Comet Hale–Boppis chemically heterogeneous.     

Comet Hale–Bopp: Velocity Field Of Ions From Fabry-Pérot Imaging

Fabry-Pérot interferograms of comet Hale-Bopp were obtained on several nights in March and April 1997. For this purpose we utilized the 2-channel focal reducer of the Max-Planck-Institute for Aeronomy at the 2-m telescope of the Pik Terskol Observatory. Solid Fabry-Pérot etalons of resolving power 30000 were used in both channels of the focal reducer. The main aim of this study is to measure the velocities and abundances of OH⁺ and H₂O⁺, both ions closely related to the same parent molecule, H₂O. In the blue channel interferograms we identified several individual OH⁺ rotational lines of the A³Π_i - X³Σ⁻ (0-0) transition and measured their Doppler shifts. The target emissions in the red channel were the H₂O⁺ lines of the A²A₁ − X²B₁ (10-0) band. We found that the line of sight velocities, obtained from the Doppler shifted wavelengths of emissions in the comet are higher in sunward direction than in the plasma tail and do not exceed 20 km s^–1. The corresponding values, deprojected in antisolar direction, are consistent with predictions by magnetohydrodynamical models of the solar-wind-comet interaction, when one accounts for the extremely high gas production rate of comet Hale-Bopp. This revised version was published online in July 2006 with corrections to the Cover Date.     

内蒙古林西县北三段银铅多金属矿床碳、氧、硫、铅同位素特征及成矿物质来源

本文对内蒙古林西县北三段银铅多金属矿床矿体的碳、氧、硫、铅同位素进行了测定,并对其成矿物质来源及演化进行了探讨。矿区样品的δ34S‰变化范围为-0.24‰~2.37‰,平均值为1.29‰,初步认为矿石中的硫主要来源于深部岩浆,并有少量生物还原硫的加入。样品的δ13CPDB变化范围为-4.57‰~-7.33‰,平均值为-5.96‰,δ18O为-3.4‰~-4.8‰,平均值为-4.06‰;δ13CPDB-δ18OSMOW关系表明,矿体中的碳可能主要由基性-超基性岩浆提供,并有部分来源于地层,且受大气水影响明显。铅同位素表明北三段矿床的成矿物质可能由造山带物质和地幔物质两部分提供。     

晚中新世-上新世黄土高原佳县红粘土剖面碳同位素记录与C4植被演化

新生代C4植被开始扩张的年代、过程和驱动机制是全球古气候变化研究的焦点问题.中国黄土高原的黄土-红粘土剖面保存了连续的古生态演化记录,是研究这一关键科学问题的理想载体.本文选择黄土高原北部佳县厚达64m的红粘土剖面(8.2～2.7Ma),对190个层位的次生方解石矿物进行了无机碳同位素测试,由此分析了晚中新世-上新世末的C4植被扩张和演化过程.C4植被持续增长与全球冰盖的扩张基本一致,表明气候变冷很可能导致了黄土高原区域气候的干旱化与降雨季节性的增强.C4植被的扩张存在明显的3个阶段,分别以6.6Ma和3.6Ma为界限,每一次扩张增加10％左右,暗示了全球性的构造事件对黄土高原植被演化的控制.此外,佳县红粘土剖面呈现10次持续时间为10 ～ 20万年的碳同位素正漂移事件,平均每40万年发生一次,说明40万年轨道周期也控制着C4植被的演化.     

黄土高原西部地区黄土地层有机质主要来源分析*

黄土有机质的主要来源是决定其稳定碳同位素(δ13Corg.)能否应用于重建过去C3/C4相对丰度变化及相应的古气候变化的关键基础科学问题.如若黄土地层当中的有机质主要由粉尘携带而来,而非当地植被,显然其δ13Corg.不是一个局地植被过去C3/C4相对丰度变化及古气候变化的良好指示器.本文对黄土高原西部地区(六盘山以西)新获得和已发表的相关数据进行综合分析,尝试对该地区黄土有机质的主要来源进行定量的分析.结果表明,总体而言,该地区黄土地层有机质主要来源于当地植被,由粉尘携带而来的有机质贡献量不超过8％,所造成的有机碳同位素变化幅度不超过1.7‰.这些结果说明该地区的黄土地层有机质δ13Corg.是可以用来重建过去C3/C4植物相对丰度及相应的古气候变化的.为了更精确的重建,后续的工作应当更多考虑粉尘搬运过程当中的有机质输入以及粉尘沉积之后的微生物活动的可能潜在影响.     

基于IDL的资源一号02C星HR影像RFM几何校正

资源一号(ZY-1)02C卫星作为我国高分辨率遥感数据卫星之一,正广泛应用于各个领域.该卫星数据采用国际上广泛使用的有理函数模型(Rational Function Model,RFM),并提供有理函数多项式系数(Rational PolynomialCoefficients,RPC).针对ZY-1 02C星1级辐射校正数据格式特点,在充分了解数据文件结构基础上,使用IDL语言进行开发,通过RFM反演其RPC,实现HR影像的几何校正等预处理.实验结果表明,程序执行快速稳定,精度可靠,影像镶嵌效果好,可以有效使用RFM实现大数据量影像的系统几何校正,避免重复操作中间数据的繁琐步骤,提高工作效率,具有实用价值.