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infrared galaxies
相关语句
  红外星系
     AN HST SURFACE PHOTOMETRIC STUDY OF ULTRALUMINOUS INFRARED GALAXIES
     极亮红外星系的HST面源测光研究
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  相似匹配句对
     Infrared Radiations of Active Galaxies
     活动星系的红外辐射
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     Observational Research On Galaxies In the Infrared
     星系的红外观测研究
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     Infrared Dryer
     红外烘干装置
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     The Infrared Handhook
     “红外手册”简介
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     Interacting Galaxies
     星系相互作用
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  infrared galaxies
Some properties of the IR-radio relationship of luminous infrared galaxies
      
This was particularly useful, since it resulted in the understanding of the power production, excitation and fuelling mechanisms in the nuclei of active galaxies including the intriguing but so far elusive ultraluminous infrared galaxies.
      
Current instruments are limited to studying truly pathologic objects at these redshifts, meaning hyper-luminous infrared galaxies (LFIR~1013L⊙).
      
Luminous and Ultraluminous infrared galaxies (ULIRGs) contain the most intense regions of star formation in the local universe.
      
Luminous infrared galaxies with the submillimeter array: probing the extremes of star formation
      
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The IRAS survey at 12, 25, 60 and 100 m gives us a possibility to study the infrared properties of the different kinds of galaxies systematically. A catalog was prepared by C. J. Lons-dale et al. (1985) in which the IRAS point sources identified as galaxies and quasars are listed. Generally speaking, the main processes of IR radiation in galaxies are the re-radiation of dust in the star forming regions and non-thermal power law radiation of activity in the nuclei. The dust content in the early types of the galaxies...

The IRAS survey at 12, 25, 60 and 100 m gives us a possibility to study the infrared properties of the different kinds of galaxies systematically. A catalog was prepared by C. J. Lons-dale et al. (1985) in which the IRAS point sources identified as galaxies and quasars are listed. Generally speaking, the main processes of IR radiation in galaxies are the re-radiation of dust in the star forming regions and non-thermal power law radiation of activity in the nuclei. The dust content in the early types of the galaxies is low, but attention has recently been drawn to a class of apparently elliptical galaxic-s which contain various quantities of dust, usually in a lane along an optical axis of the galaxies. Jura (1977) considered that the dust lanes are excellent potential sites for star formation. In this paper the infrared luminosities and F1R/FB are intercompared between the two samples of E and EO galaxies with and without dust lanes.E. Sadler (1984) published a complete sample of E and EO galaxies with B 14 mag. and DEC. -32. It contains 248 galaxies of which 38 are listed in the Lonsdale's Catalog with confirmed flux quantities in the 60 and 100 m bands.38 infrared galaxies are divided into two samples. The first consists of 6 galaxies with dust lanes, which are listed in The Catalog of Dusty Elliptical Galaxies compiled by K. Ebne-ter and B. Balick (1985). It is the latest list of dusty elliptical galaxies. The second sample consists of another 32 galaxies without dust lanes.The far infrared luminosities, LIR, of 38 galaxies have been calculated using the integrated far infrared (40-120) fluxes, FIR, given in Lonsdale's Catalog and radial velocities listed in Sadler's Catalogs (H = 75 km/s/Mpc). The quantity FB is determined by the formulalog FB=- 8.19-0.4Band the correction for interstellar extinction is performed with the method given in RC2 de Vaucouleur et al., (1976). The values of LIR and FIR/FB for the two samples are listed in the tables 1 and 2. The average log LIR for the two samples are 9.37 and 9.31 respectively. The average values of log FIR/FB are -0.15 and 0.05.The Mann-Whitney U-Test is used to check the distributions of log LIF and log FIR/FB for the two samples. The adopted null hypothesis is: the distributions of log LIF and log FIR/FB for the two samples are indistinguishable at the significant level =0.05. We found the associated probabilities for distributions of log LIR to be 0.32 and for log FIR/FB, 0.10. They are all larger than = 0.05. We can conclude from these tests that we can not refuse the null hypothesis, namely, the distributions of log LIR and FIR/FB for the two samples i.e., E and SO galaxies with and without dust lanes, could be considered as identical at the given sig- nificant level.An IRAS color-color diagram is given in the figure, in which the galaxies listed in the Sadler's and Ebneter's catalogs and identified as IRAS sources with confirmed fluxes 25, 60, and 100 m are plotted. All of E and EO galaxies without dust lanes are located in the region of normal galaxies, as pointed out by Rowan-Robinson et al. (1984). 3 out of 7 galaxies with dust lanes are located far from this region. They are NGC 1052, 7213, and IC 5063. NGC 1052 is a LINER and its IRAS properties have been discussed by Neugebauer et al. (1984). NGC 7213 is Seyfert 1 and IC 5063 is Seyfert 2 as listed in the Veron's catalog (1985).Finally it can be concluded: 1. There is no evidence that" the dust lanes in E and EO galaxies are strong infrared sources arising from star forming regions. 2. A few E and EO galaxies with dust lanes are shown to be sites where peculiar infrared radiation processes are going on: these are all active galaxies.

IRAS在12,25,60和100μm的巡天,给我们提供了研究各类星系红外辐射特性的可能。为了研究具有尘带的E和SO星系的红外辐射特性,我们利用了E.Sadler给出的完备的E和SO星系表。在该星系表中共列出248个夭体,其中38个被证记为IRAS点源,且又有确切的60和100μm的流量值。在这38个天体中有6个被列在K.Ebneter和B.Balik最新发表的具有全带的椭圆星系表中。我们以这6个星系作为具有尘带的E和SO星系的样本,其它32个没有尘带的E和SO星系即作为对照样本。为了讨论具有尘带的椭圆星系的红外辐射特性,我们利用非参数Mann-Whitney检验,对这两个样本的LIR和FIR/FB的分布作了讨论,结果是在对于置信度α=0.05的水平上,我们不能拒绝另一假设:这两个样本的LIR和FIR/FB的分布是相同的。对于同时具有25,60和100μm确切流量的E和SO星系我们讨论了它们的双色图,结果发现,不具尘带的E和SO星系都处于Rowan-Robinson.et al所指出的正常星系区,而一些具有尘和带的ESO星系,则远离这一区域,它们是LINER和SEYFERT星系。

The luminosity-metallicity (L-Z) relation ( stellar mass-metallicity, mass-Z, relation) is one of the fundamental parameters of galaxies, and can trace the assembly history of metals and stellar masses in the galaxies.We review the study progress about the L-Z and mass-Z relations of galaxies.including the local, the intermediate-z (0.4 < z< 1) and the high-z (z > 2) galaxies. Since the observations extend to a wide cosmic time scale,this can help to undertand and the evolutionary process of the L-Z relations...

The luminosity-metallicity (L-Z) relation ( stellar mass-metallicity, mass-Z, relation) is one of the fundamental parameters of galaxies, and can trace the assembly history of metals and stellar masses in the galaxies.We review the study progress about the L-Z and mass-Z relations of galaxies.including the local, the intermediate-z (0.4 < z< 1) and the high-z (z > 2) galaxies. Since the observations extend to a wide cosmic time scale,this can help to undertand and the evolutionary process of the L-Z relations of galaxies, hence to understand the whole evolutionary scenario of galaxies. In Sect.2. we introduce the relations between B band absolute magnitudes and metallicities (MB-Z) of nearby galaxies, including the irregular, the spiral galaxies, the UV-selected and nearby HII galaxies, the KISS sample, the 2dFGRS sample, and the SDSS galaxies. We present some of the important formulas of such relations.In Sect. 3. we present the study about the relationship between near-infrared J, H, K band absolute magnitudes and metallicities of nearby galaxies. The majority is the result of 400 KISS galaxies obtained from 2MASS. We also mention the MK-Z relations of a small sample of distant luminous infrared galaxies. In Sect.4, we specially introduce the relations between stellar mass and metallicities of nearby star-forming galaxies derived from the SDSS database. All these results show that the more luminous (massive) galaxies are more metal-rich generally. The luminosity correlates with metallicity over 10 magnitudes in luminosity and 2 dex in metallicity, with indication that the relationship may be environmental and morphology free. In Sect.5, we introduce the L-Z (mass-Z) relations of the intermediate-z and high-z galaxies. With the increasing ability of observations, more and more distant galaxies have been obtained their L-Z (mass-Z) relations, such as the intermediate-z(0.4 < z < 1) luminous infrared galaxies, the galaxies selected from GOODS, CFRS, DGSS fields, and the high-z(z≈3)LBGs. These results show that there exists one L-Z (mass-Z) relation in the distant universe, where the less luminous galaxies may have lower metallicities generally. Especially, comparing the L-Z (mass-Z) relations of these distant galaxies with those of the local ones, it shows that the distant ones are more metal-deficient than the local ones at a given luminosity or stellar mass, i.e. the galaxies with 0.4 < z < 1 are about 0.14-0.4 dex more metal-deficient, and the galaxies with z > 2 are about 0.56-0.7 dex more metal-deficient relatively. They should produce these important parts of their metals in the consequent evolutionary process. The conclusions and prospects are given in Sect.6.

金属丰度与星系光度是星系的重要特征参量,研究它们之间的关系有助于理解星系中恒星质量与金属成分的累积过程。评述了星系的光度-金属丰度关系的最新研究进展,包括对近邻星系、中等红移星系(0.42)的研究结果.由于观测样本跨越较宽的宇宙学时标,可以由此来探讨这一关系的演化过程,从而帮助理解星系演化的整体图景。

 
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