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      波段

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  band

    THE OBSERVATION AND RESULTS OF TOTAL FLUX AT 2cm BAND DURING THE TOTAL SOLAR ECLIPSE OF Feb. 16,1980.

    1980年2月16日日全食2厘米波段总强度射电望远镜观测结果

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    THE POINTING CALIBRATION OF PMO 13.7M TELESCOPE AT 22 GHz BAND

    紫台13.7米望远镜在22GHz波段的指向校准

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    In the study,the quasars PKS 1510-089 were observed with the 1m telescope at Yunnan Observatory. A detected significant optical change of near 1mag within the time scale of 1 h indicates that the target is very active in the R band during the observation period.

    用中科院云南天文台1 m望远镜对类星体PKS 1510-089进行观测,监测到其在不足1 h的时标里变幅约1 mag的剧烈光变,说明在观测期间,目标在R波段是极其活跃的.

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    and NVSS, FIRST in radio wave band.

    射电波段主要介绍了NVSS和FIRST巡天。

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    The Measure Method and Data Analysis of Centimeter Wave Band Background-Noise's Level

    厘米波段背景噪声电平的测量方法及数据分析

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  wave band

    and NVSS, FIRST in radio wave band.

    射电波段主要介绍了NVSS和FIRST巡天。

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    The Measure Method and Data Analysis of Centimeter Wave Band Background-Noise's Level

    厘米波段背景噪声电平的测量方法及数据分析

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    The energy band of hard X-ray, with strong penetrability, is an important astrophysical wave band.

    硬X射线能段是天体物理的重要波段，由于具有较强的穿透能力，因而它可以携带辐射区的很多信息。

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    In this paper we use the 9400MHz (Toyokawa), 3750MHz (Toyokawa) and 2800MHz (Ottawa), the three standard wave band of solar Radio Observation acknowledged by the world, to make the accuracies by folding-regression analysis of 8800MHz, 4995MHz and 2695MHz at Manila Observatory of the USAF. In the period of Jan. 1980-Dec. 1982, results show that the r.

    本文以国际公认的太阳射电三个定标标准波段9400MHz(Toyoka-wa),3750MHz(Toyokawa)和2800MHz(Ottawa)的观测资料为依据,对美国空军(USAF)太阳射电全球巡视网在马尼拉观测站的三个波段8800MHz,4995MHz和2695MHz的强度观测资料进行折叠回归分析。

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    VO will hold all sky and all wave band data from radio, infrared ray to gamma ray and it will get the most elaborate observation result.

    拥有每个波段的观测数据,从射电、红外、……到γ射线:拥有最精细的观测结果:观测条件永远最佳,没有月光的干扰、没有阴天、没有沙尘暴,全天候的可用性;

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  bands

    Most of the sources were observed at three bands: 4.8GHz, 8GHz and 14.5GHz.

    大多数源都包含了3个波段的观测数据:4 .8GHz ,8GHz和14 .5GHz。

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    (3) The mean spectral index derived for the samples is 1.50 ± 0.34 between J to K bands and 1.14 ± 0.42 between K to A bands, respectively.

    (3)我们的Be星样本的平均谱指数在J到K波段和K到A波段间分别是1.50±0.34和1.14±0.42。

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    We get reasonable light curves in B and V bands and find a positive correlation between variability and spectral slope.

    我们得到了活动星系核在B、V波段合理的光变曲线以及光谱斜率和光度之间的正相关性。

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    We constructed the mid-to-far infrared SEDs of each sample source after measuring the five bands mid-infrared flux (3.6,4.5,5.8,8.0,24μm) and matching the two far-infrared flux (70 and 160μm) from Frayer et al.

    对SPITZER中红外五个波段(3.6，4.5，5.8，8.0，24μm)进行处理，结合Frayer给出的70，160μm测光值，得到了样本的中远红外光谱能量分布。

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    The characteristics of the solar microwave bursts with the proton events are investigated from the data which have been obtained in the three bands of 9375 MHz, 3653 MHz and 2902 MHz since 1978 at Yunnan Observatory.

    本工作用云南天文台1978年以来在9375MHz、3653MHz和2902MHz三个波段的微波爆发资料研究了伴随质子事件的微波爆发特征。

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  range

    The wavelengths for the Hartmann-Shack wavefront sensor and the imaging observation range from 400-700 nm and 700-1000 nm respectively.

    系统中哈特曼波前传感器的工作波段为400-700 nm,系统成像波段为700-900 nm。

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    With the developing of science and technology, the corresponding optical components are required exigently, which work at hard X-ray radiation, for extend the applying range of X-ray optical component.

    随着科学技术发展的需要，人们迫切需要在硬X射线波段建立相应的光学元件，拓展X射线光学元件的应用范围。

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    Because the photospheric temperature of carbon stars are less than 3000K and the temperature of rich-dust envelope formed by the mass loss is lower, and therefore most of the energy from carbon stars are radiated between 1 to 60um range, in which the vibrational and ro-vibrational bands of many molecules also lies, the study of infrared spectra in this wavelength range is very important to reveal chemical compositions, dust formation process, the atmospheric structure and evolutionary status of stars.

    碳星光球的有效温度不超过3000K，同时较大的质量损失率形成了富碳的尘埃壳层，以致于它的辐射能量主要集中在1—60μm的红外波段上，并且许多分子的转动振动能谱也集中在红外，因此在红外波段的研究对揭示碳星化学成份及其分布、尘埃形成过程、恒星大气结构和演化状态都有十分重要的意义。

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    Variability is a common phenomenon in AGN and is observed over wide range from radio to X-ray.

    光变是活动星系核的普遍现象,从射电到X射线的所有波段都观测到了活动星系核的光变。

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    The spectral range covered by photography is 5700—6300A,the effective wave length is 6000A. The camera was carefully adjusted,scattered light was negli- gible(<1%).

    观测是用三物镜照相仪进行的,有效波段为5700—6300埃,有效波长为6000埃,仪器散射光很小(<1％)。

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  band
       Frequency-Domain Bounds for Nonnegative, Unsharply Band-Limited Functions
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       Aliasing error bounds are derived for one- and two-channel sampling series analogous to the Whittaker-Kotel'nikov-Shannon series, and for the multi-band sampling series, and a "derivative" extension of it, due to Dodson, Beaty, et al.
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       In this paper we give a further investigation of the method introduced by the author in [1, Frequency-domain bounds for nonnegative unsharply band-limited functions] for proving bounds for functions with nonnegative Fourier transforms.
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       Finite energy band-limited functions are reconstructed iteratively
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       Unique reconstruction of band-limited signals by a Mallat-Zhong wavelet transform algorithm
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  wave band
       The mutant chlorotica 2004 proved to have an increased intensity of a long-wave band of the light-harvesting complex I at both 23°C (745 nm) and -196°C (728 nm).
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       A prototype of the plasma density sensor operating in the 3-cm wave band has a sensitivity to the electron density of ～108cm-3; the resolved volume is ～1 cm in diameter and 4 cm in length.
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       Methods for Measuring the Characteristics of Electrodynamic Systems in the Millimetric Wave Band
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       Experimental methods and an automated computer-based setup for studying electrodynamic resonance systems in the millimetric wave band are described.
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       A bench for precision measurement of rejection-filter frequency characteristics in the 2-mm wave band
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  bands
       In this paper for the two-dimensional diffusion equation, the net region is divided into bands, a special kind of block.
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       Meanwhile, the average of mean square error of spectra within 46 spectrum bands is reduced to 9.69.
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       The simulated results show that FSS may operate in different bands and especially generate a large reduction in the resonant frequency for a fixed unit cell size through different loadings.
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       Random amplification of polymorphic DNA analysis showed that the variant DNA bands were consistent in M1 and M2 generations treated with both γ-radiation and ion implantation.
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       Also, Lys residue and disulfide bands are necessary to protect the catalysis of the AKP.
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  range
       Among all image transforms, the classical (Euclidean) Fourier transform has had the widest range of applications in image processing.
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       The Hausdorff and packing dimensions of the range BH ([0, 1]N), the
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       As the main application it is shown that, in general, a localization operator possesses the Fredholm property, and thus its range is closed in the target space.
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       We then use interpolation method to identify these spaces with the classical ones for a certain range of p, q >amp;gt; 1.
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       However, the Mattila integral, associated with the Falconer distance problem for these measures is unbounded in the range $0 >amp;lt; s >amp;lt; \frac{d^2}{2d-1}$.
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         According to the international convention,we have carried out the photographic photometry on the U,B,V system,with the recommended plate-filter combinations:U— Kodak 103a-O+UG2;B—103a-o+GG13 and V—103a-D+GG11.Our telescope is a 15 cm Zeiss astrograph (UV objective).With the data in hand,we cal- culated the effective wave length of the blue combination.(103a-o+GG13)to be 4440A and the yellow combination (103a-D+GG11) 5610A.Both are longer than that of the respective B,V system. When we determine the magnitud...
            本文叙述根据较差测量法,试用柯达103a—D+GG11、103a—O+GG13及103a—O+UG2组合,对本台口径15厘米折光镜进行 U、B、V 系统照相测光.结果表明,前两种组合的有效波长约为5610及4440,比 B、V 系统的长.焦点照相结果,星等与标准值有系统差.这具望远镜消色差在蓝紫波段,当在其他波段测光时,焦距调节对星等测定极为敏感.但存在一个焦距调节范围,在此范围内照相,可以消去系统差.这个范围对三种组合都不同.103a—D+GG11,约在该组合的焦点以外2毫米处,可变范围约±0.2毫米;对103a—O+GG13,从该组合焦外1.5厘米到星象显著变大的焦外;对103a—O+UG2,从该组合焦外约1毫米到星象显著变大的焦外.为校验上述结果,拍摄了疏散星团M45, M45,NGC752和IC4665.用103a—D+GG11还观测了红化 O 星协 CygⅥ.在我们使用这架望远镜进行照相测光工作所要求的精度下,这个方法是可以应用的.我们使用萨尔托累光瞳光度计(Sartorius Iris Photometer)测量底片,讨论了测量方法及误差.此外,还考察了导星不好的初步后果,...
文摘来源
         Photometric observations of Nova Her 1963 were started in Peking on Feb.18, 1963,with a photoelectric photometer mounted on a 15 cm aluminized Cassegrain reflec- tor.The Nova was observed in the ultraviolet,blue,yellow,and red as well as through four relatively narrow-band filters whose commercial type designations being S43,S47, S50 and S53,with maximum transmissions of the cell-field lens-filter combination at about 4300,4550,4850 and 5230(?) respectively. Table 1 lists the types and parameters of the fil...
            北京天文台筹备处自制了一架光电光度计,在1963年2月到6月间进行了对1963年武仙座新星的光电观测.所用的波段,宽波段滤光片是 UG1、GG13、BG12、GG11和 RG1,窄波段是 S43、S47、S50和 S53.
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         At the total solar eclipse on 1968 September 22,observable in Western China, photographic observation of the polarization of solar corona was made separately on ground and in an airplane,Good photographs of the corona were obtained with a three-objective camera(ground:D=8cm,F=120cm;airplane;D=10cm,F= 100cm).The spectral range covered by photography is 5700—6300A,the effective wave length is 6000A.The camera was carefully adjusted,scattered light was negli- gible(<1%). Through photometric measurement,the abs...
            本文叙述1968年9月22日日全食所作的日冕偏振照相观测及资料分析结果。观测是用三物镜照相仪进行的,有效波段为5700—6300埃,有效波长为6000埃,仪器散射光很小(<1％)。光度测量得到1.1—3.5R_⊙的日冕绝对亮度和偏振;日冕接近极大型,东西南北都不十分对称;偏振的径向程度较好,赤道区平均偏振度在1.5—1.6R_⊙达到极大,P_(max)=0.45;全食时天空背景较亮(I_天=3.27×10~9H_⊙,P_天=20.7％,电矢量指向天顶),处理中作了相应改正,最后,采用平均日冕模型,计算了赤道区的电子密度和温度,并分离了K冕和F冕。
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