In addition to the X-rays observed with Chandra, other data critical for this result came from NASA's Spitzer Space Telescope and the ground-based, infrared Two Micron All Sky Survey.

This is the Hidden Universe of the Spitzer Space Telescope, exploring the mysteries of infrared astronomy with your host Dr. Robert Hurt.

这是神秘宇宙斯皮策空间望远镜的发现，这个望远镜是罗伯特·赫尔特用来探索红外天文学奥秘的利器。

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So say three teams of scientists who used the Spitzer space telescope to capture the light spectrum of two known extrasolar planets.

三支科学家小组用斯必择空间望远镜捕获了两个已知的太阳系外行星的光谱。

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The James Webb Space Telescope, named after NASA's second director, will have a mirror seven times the size of the Hubble Space Telescope.

詹姆斯韦伯太空望远镜后，美国宇航局的另一名董事命名，将会有一个镜子七倍大的哈勃太空望远镜。

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With this week's NASA reauthorization, we continue progress on Hubble's successor, the James Webb Space Telescope.

有了本周的NASA重新授权法案，我们可以在哈勃继任者，詹姆斯.韦伯太空望远镜上取得更多进展。

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NASA's James Webb Space Telescope, due to launch in 2018, should be powerful enough to detect chlorofluorocarbons, CFCs.

将于2018年发射的美国宇航局的詹姆斯韦伯太空望远镜应该强大到足以检测氯氟化碳，氯氟烃。

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Its successor is the James Webb Space Telescope, an infrared optimized space observatory scheduled to be deployed in2014.

哈勃望远镜的”接班人“将是一架詹姆斯•韦伯太空望远镜。这架望远镜计划于2014年发射，是一套红外线优化太空观测系统。

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The James Webb Space Telescope is a complex engineering project.

詹姆士·韦伯太空望远镜是一项复杂的工程项目。

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The JWST, if it does eventually fly, would surely do some spectacular science.

JWST若能最终得以升空，它必将完成一些科学壮举。

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It's called an Einstein ring, because he predicted that, too.

还是爱因斯坦预测到了这种光环，因此这个环也被叫做爱因斯坦光环。

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Preparation of Metallic Ultra-fine Powders Using Wire Electrical Explosion Method and Development of the Apparatus; The Equation of State and Explosive Energy of Type II Supernova

超细粉的电爆法制备及其设备的开发II型超新星的物态方程与爆发能量

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, we consider SN 1979c should be classified to type II supernova with some special characteristics.

根据这颗超新星的光变曲线、在星系中的位置及爆发期间辐射的总能量等主要特征，我们认为SN1979c是某些性质比较特殊的II型超新星。

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The Equation of State and Explosive Energy of Type II Supernova

II型超新星的物态方程与爆发能量

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The data of high-redshift SNe Ia could make constraints on the cosmic density parameters Ω M, Ω A as well as the deceleration factor qo, and hence determining the ultimate fate of our universe.

基于对邻近星系Ia超新星的理解，高红移Ia超新星的数据可对宇宙密度参数ΩM、ΩA及减速因子q0作出限制，并对膨胀宇宙的最终命运作出判定。

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Blue supernovae of type Ia ( SNe Ia) are the best calibrated standard candles, the dispersion of the intrinsic peak luminosity approaches to 0 11 mag.

蓝Ia超新星是迄今天文学家已知的校准得最好的标准烛光，峰值光度弥散仅为0.11mag。

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First, statistical analysis on type Ia supernovae ( hereafter SNe Ia) has been done by using Asiago Supernova Catalogue ( ASC).

首先利用Asiago超新星星表对Ia超新星作了统计分析。

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Once the absolute luminosity of SNe Ia is determined, we can get the value of the Hubble parameter.

一旦它们的绝对光度得到标定，就可以定出哈勃常数H0。

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The former are relatively homogeneous SNe Ia subsample, which can serve as good extragalactic distance indicator;

蓝Ia超新星构成了相对均匀的Ia超新星样本，是较好的距离指示器；

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Spirals are more efficient SNe Ia producers, comparing with elliptical galaxies.

旋涡星系中Ia超新星的产生率比椭圆星系的要高。

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However, the existence of the latter indicates the diverse properties of SNe Ia as a whole.

而红Ia超新星的存在则表明了Ia超新星整体多样性的特点。

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AM the selected OH/ IR sources have optical or infrared identification. Most of them are associated with late-type (> M5) Mira variables.

所选127个OH/IR脉泽源全部是有光学或红外证认的，其中大部分是光谱型>M5的长周期变星（主要是Mira变星）。

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