共查询到20条相似文献，搜索用时 31 毫秒
1.
Knight CA Robertson DS Rogers AE Shapiro II Whitney AR Clark TA Goldstein RM Marandino GE Vandenberg NR 《Science (New York, N.Y.)》1971,172(3978):52-54
Observations with the Goldstone-Haystack radio interferometer of the quasars 3C 279 and 3C 273 have disclosed the presence of fine structure in their radio emissions. Although the interpretation is not unique, the fringe-amplitude data for quasar 3C 279 are quite consistent with emissions from two points, each contributing equally to the correlated flux. The separation of the two points is estimated to be (1.55 +/- 0.05) x 10(-3) arc second, or about 20 light years at the distance of 3 x 10(9) light years inferred from optical red-shift data. The formal uncertainty in the right-ascension component of the separation is about 6 x 10(-6) arc second; differential proper motion in this direction at half the speed of light could be discerned within a year. The fringe-amplitude data of quasar 3C 273 allow similar, but less definitive, interpretations. 相似文献
2.
Overview and initial results of the very long baseline interferometry space observatory programme 总被引：2，自引：0，他引：2
H Hirabayashi H Hirosawa H Kobayashi Y Murata PG Edwards EB Fomalont K Fujisawa T Ichikawa T Kii JEJ Lovell GA Moellenbrock R Okayasu M Inoue N Kawaguchi S Kameno KM Shibata Y Asaki T Bushimata S Enome S Horiuchi T Miyaji T Umemoto V Migenes K Wajima J Nakajima al et 《Science (New York, N.Y.)》1998,281(5384):1825-1829
High angular resolution images of extragalactic radio sources are being made with the Highly Advanced Laboratory for Communications and Astronomy (HALCA) satellite and ground-based radio telescopes as part of the Very Long Baseline Interferometry (VLBI) Space Observatory Programme (VSOP). VSOP observations at 1.6 and 5 gigahertz of the milli-arc-second-scale structure of radio quasars enable the quasar core size and the corresponding brightness temperature to be determined, and they enable the motions of jet components that are close to the core to be studied. Here, VSOP images of the gamma-ray source 1156+295, the quasar 1548+056, the ultraluminous quasar 0014+813, and the superluminal quasar 0212+735 are presented and discussed. 相似文献
3.
The optical double quasar 0957+561 has been interpreted as the gravitational double image of a single object. A radio map made with the Very Large Array of the National Radio Astronomy Observatory shows unresolved sources coincident With the optical images as well as a complex of related extended emission. Although the results cannot rule out the gravitational lens hypothesis, the complex radio structure is more easily interpreted as two separate quasars. The optical and radio properties of the two quasars are so similar that the two must have been formed at the same time with similar initial conditions. 相似文献
4.
A full 12-hour synthesis at 6-centimeter wavelength with the Very Large Array confirms the major features previously reported for the double quasar 0957+561. In addition, the existence of radio jets apparently associated with both quasars is demonstrated. Gravitational lens models are now favored on the basis of recent optical observations, and the radio jets place severe constraints on such models. Further radio observations of the double quasar are needed to establish the expected relative time delay in variations between the images. 相似文献
5.
Terrell J 《Science (New York, N.Y.)》1966,154(3754):1281-1288
Many difficulties face the conventional interpretation of the red shift of quasars as a Hubble shift, with associated immense distances. These objects are not of galactic size or nature, and are not associated with galaxies or clusters of galaxies. The continuing energy source for such enormous powers for a period of 10(6) to 10(7) years has not been clearly revealed. The absence of the expected absorption for the Lyman-alpha spectral line of hydrogen is a new difficulty. Because of the relativistic limit on the diameter which can produce rapid fluctuations of light output, there may not be enough surface to radiate the required light.A similar and perhaps more serious difficulty exists for the fluctuating radio output. Calculations given here for synchrotron radiation self-absorption lead to a reasonably accurate formula for the angular diameter of a radio source. For the quasar 3C 273B these relations indicate a conflict with the usually assumed distance. However, the discrepancy may be explained in terms of strong variation of radio diameter with frequency. For CTA 102 the conflict is more serious, and could be explained -for cosmological distance-only by rejecting the data of Sholomitskii. These difficulties are removed by the hypothesis that the observed quasars were ejected from a gravitational collapse at the center of our own galaxy, which may have occurred roughly 5 million years ago. The resultant distances, of the order of a million lightyears, reduce the energy problem by a factor of 10(6) or 10(7). On this basis the optical diameter would be less than a light-hour, about the size of the earth's orbit. A rotating mass of a few thousand solar masses with this diameter would account for the unusual line width, could easily produce the required radiated energy, and could readily account for observed short fluctuation periods and variations in spectrum. It is suggested that the radio output may be produced by high-speed passage of the quasar through intergalactic gas. This would probably correspond to a radio size of a few light-years or less, in agreement with the fluctuations. Since the radio power would be considerably less than that of radio galaxies, it is suggested that radio galaxies may have ejected groups of quasars. This would explain the peculiarly distant locations of the radio sources for many such galaxies. The objections to this model that have been raised are apparently not fatal. In particular, the receding hydrogen cloud discovered by Koehler to be in the line of sight to 3C 273 is more plausibly interpreted as having been ejected from our own galaxy, in the manner observed for other galaxies, than as being associated with the Virgo cluster of galaxies. The latter interpretation, which would place 3C 273 further away, is in conflict with Lyman-alpha absorption data for 3C 9 and other quasars. Thus the local model seems to give a reasonable explanation not only of quasars but also of radio galaxies, bothv of which seem largely to defy explanation on other grounds. Whether or not this model is valid, it is clear that an understanding of quasars will radically change our understanding of the universe. 相似文献
6.
Before the launch of the Compton Gamma Ray Observatory (CGRO), the only source of >100-megaelectron volt (MeV) gamma radiation known outside our galaxy was the quasar 3C 273. After less than a year of observing, 13 other extragalactic sources have been discovered with the Energetic Gamma Ray Experiment Telescope (EGRET) on CGRO, and it is expected that many more will be found before the full sky survey is complete. All 14 sources show evidence of blazar properties at other wavelengths; these properties include high optical polarization, extreme optical variability, flat-spectrum radio emission associated with a compact core, and apparent superluminal motion. Such properties are thought to be produced by those few, rare extragalactic radio galaxies and quasars that are favorably aligned to permit us to look almost directly down a relativistically outflowing jet of matter expelled from a supermassive black hole. Although the origin of the gamma rays from radio jets is a subject of much controversy, the gamma-ray window probed by CGRO is providing a wealth of knowledge about the central engines of active galactic nuclei and the most energetic processes occurring in nature. 相似文献
7.
Molecular gas in the host galaxy of the lensed quasar 0957+561 (QSO 0957+561) at the redshift of 1.41 has been detected in the carbon monoxide (CO) line. This detection shows the extended nature of the molecular gas distribution in the host galaxy and the pronounced lensing effects due to the differentially magnified CO luminosity at different velocities. The estimated mass of molecular gas is about 4 x 10(9) solar masses, a molecular gas mass typical of a spiral galaxy like the Milky Way. A second, weaker component of CO is interpreted as arising from a close companion galaxy that is rich in molecular gas and has remained undetected so far. Its estimated molecular gas mass is 1.4 x 10(9) solar masses, and its velocity relative to the main galaxy is 660 kilometers per second. The ability to probe the molecular gas distribution and kinematics of galaxies associated with high-redshift lensed quasars can be used to improve the determination of the Hubble constant H(0). 相似文献
8.
Ground-based observations of the object IRAS 14348-1447, which was discovered with the Infrared Astronomical Satellite, show that it is an extremely luminous colliding galaxy system that emits more than 95 percent of its energy at far-infrared wavelengths. IRAS 14348-1447, which is receeding from the sun at 8 percent of the speed of light, has a bolometric luminosity more than 100 times larger than that of our galaxy, and is therefore as luminous as optical quasars. New optical, infrared, and spectroscopic measurements suggest that the dominant luminosity source is a dustenshrouded quasar. The fuel for the intense activity is an enormous supply of molecular gas. Carbon monoxide emission has been detected at a wavelength of 2.6 millimeters by means of a new, more sensitive receiver recently installed on the 12-meter telescope of the National Radio Astronomy Observatory. IRAS 14348-1447 is the most distant and luminous source of carbon monoxide line emission yet detected. The derived mass of interstellar molecular hydrogen is 6 x 10(10) solar masses. This value is approximately 20 times that of the molecular gas content of the Milky Way and is similar to the largest masses of atomic hydrogen found in galaxies. A large mass of molecular gas may be a prerequisite for the formation of quasars during strong galactic collisions. 相似文献
9.
Sadeh D 《Science (New York, N.Y.)》1967,158(3805):1176-1178
The probability that a galaxy gathers light from another remote galaxy, and deflects and focuses it toward an observer on Earth, is calculated according to various cosmologic models. I pose the question of whether an object called a quasar is a single, intrinsically luminous entity or the result of accidental alignment, along the line of sight, of two normal galaxies, the more distant of which has its light amplified by the gravitational-lens effect of the nearer galaxy. If galaxies are distributed at random in the universe, the former alternative is true. But, if we assume that most galaxies exist in pairs, we can find about 30 galaxies occurring exactly one behind the other in such a way as to enable amplification of the order of 50. This model explains also the variations in intensity in quasars, but fails to explain others of their observed properties. 相似文献
10.
Pasquarello A Petri I Salmon PS Parisel O Car R Toth E Powell DH Fischer HE Helm L Merbach A 《Science (New York, N.Y.)》2001,291(5505):856-859
We determined the structure of the hydrated Cu(II) complex by both neutron diffraction and first-principles molecular dynamics. In contrast with the generally accepted picture, which assumes an octahedrally solvated Cu(II) ion, our experimental and theoretical results favor fivefold coordination. The simulation reveals that the solvated complex undergoes frequent transformations between square pyramidal and trigonal bipyramidal configurations. We argue that this picture is also consistent with experimental data obtained previously by visible near-infrared absorption, x-ray absorption near-edge structure, and nuclear magnetic resonance methods. The preference of the Cu(II) ion for fivefold instead of sixfold coordination, which occurs for other cations of comparable charge and size, results from a Jahn-Teller destabilization of the octahedral complex. 相似文献
11.
Levy GS Linfield RP Ulvestad JS Edwards CD Jordan JF DI Nardo SJ Christensen CS Preston RA Skjerve LJ Stavert LR Burke BF Whitney AR Cappallo RJ Rogers AE Blaney KB Maher MJ Ottenhoff CH Jauncey DL Peters WL Nishimura T Hayashi T Takano T Yamada T Hirabayashi H Morimoto M Inoue M Shiomi T Kawaguchi N Kunimori H 《Science (New York, N.Y.)》1986,234(4773):187-189
An orbiting spacecraft and ground observatories have been used to obtain interferometric observations of cosmic radio sources. The Tracking and Data Relay Satellite System (TDRSS) was used as the orbiting observatory in conjunction with two 64- meter radio telescopes at ground observatories, one in Australia and one in Japan. The quasars 1730-130 (NRAO 530), 1510-089, and 1741-038 were observed at a frequency of 2.3 gigahertz, and a maximum projected baseline of 1.4 earth diameters was achieved. All quasar observations for which valid data were acquired resulted in detected fringes. Many of the techniques proposed for a dedicated very long baseline interferometry observatory in space were used successfully in this experiment. 相似文献
12.
Finding direct evidence for plasma instability in extragalactic jets is crucial for understanding the nature of relativistic outflows from active galactic nuclei. Our radio interferometric observations of the quasar 3C273 made with the orbiting radio telescope, HALCA, and an array of ground telescopes have yielded an image in which the emission across the jet is resolved, revealing two threadlike patterns that form a double helix inside the jet. This double helical structure is consistent with a Kelvin-Helmholtz instability, and at least five different instability modes can be identified and modeled by a light jet with a Lorentz factor of 2 and Mach number of 3.5. The model reproduces in detail the internal structure of the jet on scales of up to 30 milli-arc seconds ( approximately 300 parsecs) and is consistent with the general morphology of the jet on scales of up to 1 kiloparsec. 相似文献
13.
Reflectance spectra (0.3 to 2.6 micrometers) of 14 C, G, B, and F asteroids and 21 carbonaceous chondrite powders are compared in detail. Only three thermally metamorphosed CM-Cl chondrites that have a weak ultraviolet absorption are shown to have close counterparts among those asteroids. Reflectance spectra of heated Murchison CM2 chondrite are compared with the average C and G type asteroid spectra. Murchison heated at 600 degrees to 1000 degrees C exhibits a similar weak ultraviolet absorption and provides the best analog for those spectra. Comparison of ultraviolet absorption strengths between 160 C, G, B, and F asteroids and carbonaceous chondrites suggests that surface minerals of most of those asteroids are thermally metamorphosed at temperatures around 600 degrees to 1000 degrees C. 相似文献
14.
MAGIC Collaboration Albert J Aliu E Anderhub H Antonelli LA Antoranz P Backes M Baixeras C Barrio JA Bartko H Bastieri D Becker JK Bednarek W Berger K Bernardini E Bigongiari C Biland A Bock RK Bonnoli G Bordas P Bosch-Ramon V Bretz T Britvitch I Camara M Carmona E Chilingarian A Commichau S Contreras JL Cortina J Costado MT Covino S Curtef V Dazzi F De Angelis A De Cea Del Pozo E de Los Reyes R De Lotto B De Maria M De Sabata F Mendez CD Dominguez A Dorner D Doro M Errando M Fagiolini M 《Science (New York, N.Y.)》2008,320(5884):1752-1754
The atmospheric Cherenkov gamma-ray telescope MAGIC, designed for a low-energy threshold, has detected very-high-energy gamma rays from a giant flare of the distant Quasi-Stellar Radio Source (in short: radio quasar) 3C 279, at a distance of more than 5 billion light-years (a redshift of 0.536). No quasar has been observed previously in very-high-energy gamma radiation, and this is also the most distant object detected emitting gamma rays above 50 gigaelectron volts. Because high-energy gamma rays may be stopped by interacting with the diffuse background light in the universe, the observations by MAGIC imply a low amount for such light, consistent with that known from galaxy counts. 相似文献
15.
16.
以猪血为原材料,通过硫酸铵盐析和柱层析等方法,分离纯化出2种半胱氨酸蛋白抑制剂激肽原（kininogen）．激肽原Ⅰ的得率为0．7％,纯化倍数为613．7;激肽原Ⅱ的得率为24．1％,纯化倍数为295．7．SDS—PAGE结果表明,激肽原Ⅰ和激肽原Ⅱ的分子质量分别为58ku和116ku．激肽原Ⅰ和激肽原Ⅱ对白鲢鱼（Hypophthalmichthys molitrix ）鱼浆中肌原纤维蛋白降解都有一定的抑制作用,当激肽原Ⅱ添加量为鱼浆质量的0．03％时,可以使鱼糜凝胶强度提高24％．因此,激肽原可作为添加剂有效提高鱼糜制品的凝胶强度． 相似文献
17.
Arp H 《Science (New York, N.Y.)》1966,151(3715):1214-1216
Pairs of radio sources which are separated by from 2 degrees to 6 degrees on the sky have been investigated. In a number of cases peculiar galaxies have been found approximately midway along a line joining the two radio sources. The central peculiar galaxies belong mainly to a certain class in the recently compiled Atlas of Peculiar Galaxies. Among the radio sources so far associated with the peculiar galaxies are at least five known quasars. These quasars are indicated to be not at cosmological distances (that is, red shifts not caused by expansion of the universe) because the central peculiar galaxies are only at distances of 10 to 100 megaparsecs. The absolute magnitudes of these quasars are indicated to be in the range of brightness of normal galaxies and downward. Some of the radio sources which have been found to be associated with peculiar galaxies are galaxies themselves. It is therefore implied that ejection of material took place within or near the parent peculiar galaxies with speeds between 10(2) and 10(4) kilometers per second. After traveling for times of the order of 10(7) to 10(9) years, the luminous matter (galaxies) and radio sources (plasma) have reached their observed separations from the central peculiar galaxy. The large red shifts measured for the quasars would seem to be either (i) gravitational, (ii) collapse velocities of clouds of material falling toward the center of these compact galaxies, or (iii) some as yet unknown cause. 相似文献
18.
于2013—2021年1、4、7、10月，在澳门路氹城生态保护区设置2个采样区，各3个采样点，调查分析浮游动物群落结构的时空变化，并初步评估水体受扰动状况。结果表明：在澳门路氹城生态保护区共鉴定出171种浮游动物(含9类浮游幼虫)，其中一区鉴定出156种，二区鉴定出116种；浮游动物分属于8个类群，主要优势类群为轮虫(57种)、桡足类(48种)和纤毛虫(33种)；一区浮游动物丰度为6.00~240.33 ind/L，平均为(59.27±58.39) ind/L，二区浮游动物丰度为3.00~62.58 ind/L，平均为(19.20±16.82) ind/L；一区和二区浮游动物群落结构区域差异显著，一区物种数和丰度显著大于二区的，一区的Shannon–Winner多样性指数、Margalef丰富度指数和Pielou均匀度指数均值显著小于二区的，一区浮游动物丰度年际变化波动大于二区的，可见一区环境较二区更加敏感，一区受人类活动影响较大；2013—2016年浮游动物优势种主要为轮虫(污染指示种)，2017—2021年浮游动物优势种主要为桡足类(非污染指示种)，更替率为100%，除一区2017—2021年的Shannon–Winner多样性指数小于2013—2016年的外，两区域其余生物多样性指数均大于2013—2016年的，说明保护区水质有所改善。 相似文献
19.
为研究石墨烯（Graphene,GN）对喹诺酮类抗生素在地下水中运移的影响,以环丙沙星（Ciprofloxacin,CIP）和诺氟沙星（Norfloxacin,NOR）作为两种典型的喹诺酮类抗生素污染物,通过批量吸附实验和砂柱实验研究GN对CIP和NOR在饱和多孔介质中运移的影响。吸附实验结果表明,GN对两种抗生素污染物均具有较好的吸附性能,GN对CIP和NOR的Langmuir最大吸附容量分别为270.68 mg·g-1和178.36 mg·g-1。砂柱实验结果表明：随着多孔介质中GN含量从10 mg增加到80 mg,CIP和NOR在一维砂柱中的迁移能力降低;随着流速和电解质浓度（Na+和Ca2+）的增大,回收率逐步升高,CIP和NOR的运移能力也逐步增强。根据BDST模型对不同条件下的CIP和NOR在一维砂柱中的运移过程进行了模拟和预测,模型对穿透时间的预测值与实验值接近,表明BDST模型能较好地预测多孔介质中GN对CIP和NOR迁移能力的影响。 相似文献
20.
天然气水合物生成条件预测模型的比较 总被引：12，自引：0，他引：12
天然气水合物理论预测模型是在Van der Waals-Platteeuw模型的基础上发展起来的。目前,预测天然气水合物形成条件的模型有8种,即两种经验或半经验模型(KK和回归公式)和6种热力学相态平衡理论模型,采用这8种模型对给定压力下水合物的形成温度进行了计算,与实测值相比,计算值都偏小。在低压下(压力小于5MPa)时计算值相差不大,误差较小;但当压力大于5 MPa后,计算值相差较大。其中采用两种经验或半经验模型(KK和回归公式)计算给定压力下水合物的形成温度时,计算值偏低。而6种热力学相态平衡理论模型计算误差较小,误差大小顺序为VDW>PP>HJ>NR>Du＆Guo88>Chen＆Guo96。其中Du＆Guo88和Chen＆Guo96两种模型计算最精确。 相似文献