更新時間：2021-06-11 09:42:58作者：admin2
朋友，如果您每天收到十封這樣的郵件，您不會每一封都拿到這里來請人幫你翻譯才看得懂吧？
看來沒有人幫你翻譯，我就來試試吧：
If his team sees a companion object to a star in more than one NICMOS picture, and it appears to have moved along an orbit, follow-up observations will be made with ground-based telescopes. If they see something once but its brightness and separation from the star would be reasonable for a planet, they will also do follow-up observations with ground-based telescopes.
如果他的小組在不只上一張NICMOS照片中觀察到一顆恒星的伴星，而且它似乎在沿著特定的軌道發(fā)生了位移，將用地面的望遠(yuǎn)鏡進(jìn)行后續(xù)跟蹤觀察。如果他們觀察到某天體一次，而且其亮度和與該恒星的距離可以合理地解釋為一顆行星，他們也會利用地面望遠(yuǎn)鏡進(jìn)行后續(xù)跟蹤觀察。
Taking the image of an exoplanet is not an easy task. Planets can be billions of times fainter than the star around which they orbit and are typically located at separations smaller than 1/2000th the angular size of the full moon from their star. The planet recovered in the NICMOS data is about 100,000 times fainter than the star when viewed in the near-infrared.
給外行星拍照并不是一項輕而易舉的工作。行星的亮度可能只是它們所圍繞運行的恒星亮度的幾千萬分之一，而且這些行星與恒星的分離通常在與恒星滿月時的視角1/2000還小的角度。在NICMOS數(shù)據(jù)中發(fā)現(xiàn)的行星大約僅為通過近紅外線觀察的恒星的亮度的十萬分之一。
"Even when using the best telescopes available, with the best resolution, the light from the bright star spills out in the area where the much fainter planets are located, making them impossible to see. It is essential to subtract out this bright glare of stellar light from the image to see faint dots, i.e., planets that could be hidden underneath," says Rene Doyon of the University of Montreal.
“即使使用最先進(jìn)的望遠(yuǎn)鏡，最大的精度，恒星發(fā)出的光照射到行星所位于的區(qū)域內(nèi)更暗的行星所在區(qū)域，使其很難被觀測到。因此將在照片中將這種耀眼的星光濾掉便至關(guān)重要，這樣才能看到微弱的小點，即可能暗藏在后面的行星，”蒙特利爾大學(xué)的Rene Doyon說。
The stability of how light is scattered in the NICMOS camera, called the point spread function (PSF), is key for using Hubble images to recover planets. This technique works by taking images of different stars and combining them to create a PSF of a star that closely resembles the star that is being studied for planets. This requires a reasonably steady PSF because images of different stars are taken on different days. Atmospheric conditions would vary from day-to-day for ground-based telescopes, but not for a space telescope that enjoys unprecedented image stability over repeated visits to a target.
光分散在NICMOS照相機中的穩(wěn)定性能，亦稱為點分散功能(PSF)，對使用哈博望遠(yuǎn)鏡發(fā)現(xiàn)行星是一項關(guān)鍵技術(shù)。這一技術(shù)的工作原理是將拍到的不同恒星的照片組合在一起，形成一個恒星的PSF點分散照片，使其近似正在研究中的行星所圍繞的該恒星。這就要求在不同時間對不同的恒星拍照得到相對穩(wěn)定的PSF點分散照片。地面望遠(yuǎn)鏡會因大氣條件的變化而導(dǎo)致每次拍照的結(jié)果有差異，但太空望遠(yuǎn)鏡則可提供無可比擬的對同一目標(biāo)反復(fù)觀察從而使獲得的圖像穩(wěn)定性更高。
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