排序方式： 共有34条查询结果，搜索用时 31 毫秒
11.
D. A. Varshalovich A. V. Ivanchik P. Petitjean R. Srianand C. Ledoux 《Astronomy Letters》2001,27(11):683-685
Having analyzed the spectrum of the quasar PKS 1232+0.82 taken by Petitjean et al. (2000), we identified HD molecular lines in an absorption system at redshift z=2.3377. We estimated the column density of HD molecules in this system, N(HD) = (1?4) × 1014cm?2. The excitation temperature of the first rotational level J=1 relative to the ground state J=0 is T ex=70 ± 7 K. As far as we know, this is the first detection of HD molecules at high redshift. 相似文献
12.
塞佛特星系ＮＧＣ1 0 6 8是一个非常令人注目的特殊天体 ,它是Ｓｅｙｆｅｒｔ[1]发现的第一批此类星系中离我们最近 (1 9Ｍｐｃ,取Ｈ0 =6 0ｋｍｓ- 1Ｍｐｃ- 1)和最亮的一个塞佛特星系 ,因此天文学家从射电到Ｘ 射线整个电磁波段对它进行了详尽的观测和研究。ＮＧＣ1 0 6 8最初被归类为塞佛特ＩＩ型天体 ,但是通过对其偏振光的光谱观测 ,发现了认为被遮挡住的塞佛特Ｉ型核发出的± 432 0ｋｍ/ｓ的宽Ｈβ发射线 ,因此被认为是活动星系核统一模型的一个范例 (见文 [2 ] )。射电与光学的观测资料都表明ＮＧＣ1 0 6 8的中心部分有激烈的喷射活动… 相似文献
13.
Pei-sheng Chen Hong-guang Shan Pin Zhang Yi-fei Gao 《Astrophysics and Space Science》2006,302(1-4):17-25
The 2MASS observation of the infrared quasars (IR QSOs) known so far is presented in this paper. Compared with the optical
selected quasars, infrared quasars are more dust-enshrouded and have redder colors and steeper spectral indices in the near
infrared. In consequence, they are much younger than the optical selected quasars. The result may be helpful to the suggestion
that the evolution links could be the ULIRGs - > the IR QSOs - > the optical selected quasars.
This publication makes use of data products from the Two Micron All Sky Survey (2MASS), which is a joint project of the University
of Massachusetts and the Infrared Processing and Analysis Center, funded by the National Aeronautics and Space Administration
and the National Science Foundation of the United States. 相似文献
14.
J. Nakajima Y. Koyama M. Sekido N. Kurihara T. Kondo M. Kimura N. Kawaguchi 《Experimental Astronomy》2001,11(1):57-69
We report on the detection of VLBI fringes from quasars by a new VLBI system operating at 1 Gbps (1024 Mbits-per-second). Newly developed 1024 Msps (mega sample-per-second) AD samplers and 1024 Mbps recorders were used for the observations. A correlator with external buffers was used for the 1024 Mbps correlation processing of the tapes data.Our new VLBI system enabled 1024 Mbps VLBI, and this allowed the sampling of a 512 MHz bandwidth from a radio telescope receiver. This is the highest sampling speed ever used for VLBI, and the widest bandwidth used for VLBI observation. Initial sensitivity as evaluated by SNR comparison with earlier VLBI systems produced results to matched the expanded bandwidth. In our first observations, simultaneous optical fibre linked real-time VLBI observations were made to check the validity of data and precisely detemine the clock offsets among the radio telescopes. 相似文献
15.
The possible cosmological variation of the proton-to-electron mass ratio μ = m p/m e was estimated by measuring the H2 wavelengths in the spectra of distant quasars. We analyze high-resolution (FWHM≈7 km s?1) spectra of the two damped Lyman-α systems at redshifts z abs=2.3377 and 3.0249 observed in the spectra of the quasars Q 1232+082 and Q 0347?382, respectively. Our analysis yielded the most conservative estimate for the possible variation of μ in the past ～ 10 Gyr, Δμ/μ = (5.7 ± 3.8) × 10?5. Since the significance of this result does not exceed 1.5σ, further observations are needed to increase the statistical significance. This is the most stringent limit on the possible cosmological variation of μ to date. 相似文献
16.
光学选射电噪类星体的射电性质 总被引：1，自引：0，他引：1
对类星体进行多波段的观测和研究,是了解类星体本质的一个重要途径．LBQS类星体是目前公认较为完备的一个光学选类星体样本,利用此样本与最新的485GHz全天射电源表进行了交叉证认,共找到了34个类星体的对应射电源．计算证明,这34个类星体都是射电噪的类星体．所得研究结果表明,射电噪类星体的射电光度与光学光度之间存在线性相关性． 相似文献
17.
本文对Hewitt＆Burbidge1993年的表中列出的6761颗类星体作进一步的统计分析．全部类星体发射线范围是从0到4．9．统计分析结果表明,平均而言,吸收物质和类星体本身有联系的占46％,各间隔中差异很大,最多的在间隔zem＝0．2－0．3和3．6－3．7中占100％,最少的在0．7－0．8间隔中为零．纵看各图的分布,zem＝2．0的间隔,有明显的突出性,如类星体发射线红移值和吸收线类星体数都在zem＝2为峰值,各间隔中有吸收线≥3条和≥6条的峰值也在zem＝2等． 相似文献
18.
Tao An Xiao-Yu Hong Wen-Xia Feng Jun-Hui Zhao Shanghai Astronomical Observatory Chinese Academy of Sciences Shanghai National Astronomical Observatories Chinese Academy of Sciences Beijing Harvard-Smithsonian Center for Astrophysics Garden Street MS Cambridge MA 《中国天文和天体物理学报》2004,4(6):527-532
We observed 1938-155, a broad line radio galaxy (BLRG), with the Very Large Array (VLA) at 90cm with an angular resolution of 6.8" × 4.0". The source consists of two components separated by 4 arcsec (- 20kpc, for H0 = 65km s-1 Mpc-1, q0 = 0.5) along the SE-NW direction. Both components show steep-spectra with a similar spectral index α - 0.83 ± 0.07 (Sv ∝ v-α). The bright double components are surrounded by a low-brightness cocoon. The radio properties of the two bright components are consistent with the hot spots produced by twin jets. An upper limit of - 0.0008 for the core dominance parameter (R) is inferred, suggesting there is no prominent radio core in the source. Assuming a modest viewing angle 30f77, a jet velocity is estimated - 0.07 c, based on the jet to counter-jet brightness ratio (J). The lower limit in jet speed inferred is consistent with no Doppler beaming effect on the jet. The radio galaxy 1938-155 could be an exceptional BLRG with no prominent radio core or jet. 相似文献
19.
Samuel Boissier 《Astrophysics and Space Science》2002,281(1-2):457-460
We model the chemical and spectrophotometric evolution of the Milky Way, spiral galaxies and Low Surface Brightness Galaxies
in a consistent way. Some consequences with respect to the nature of Damped Lyman-α systems (DLAs) are investigated.
This revised version was published online in September 2006 with corrections to the Cover Date. 相似文献
20.
Tao An Xiao-Yu Hong Wei-Hua WangShanghai Astronomical Observatory Chinese Academy of Sciences Shanghai National Astronomical Observatories Chinese Academy of Sciences Beijing 《中国天文和天体物理学报》2004,4(1):28-36
We present radio images of the compact steep spectrum (CSS) quasar 3C 286 acquired with the Very Large Array (VLA) at 8.4 and 22.5 GHz. The source exhibits a two-sided core-jet structure with a bright central component and two extended components one to the east (P.A. 100°) and another to the southwest (P.A. - 116°). From the compact core, an extension runs towards the southwest component up to - 0.7 arcsecond. The emission between the primary central component and the southwest component exhibits a knotty structure. A gradual change of the jet position angles from -135° to -120° in the inner southwest jet suggests a local bend. The position angle changes of the major eastern components E2 and El suggest that the eastern jet likely follows a curved trace. The bends in the jet trace may be associated with a relativistic precession or some interaction between the jet and the ambient matter. A mean spectral index of a22.58.4 - -0.76 (Sv ∝ va) is estimated for the core component. Steep spectra are also 相似文献