SUPERSHARP -通过光谱高角分辨率摄影进行系外行星研究的分段展开初级
SUPERSHARP - Segmented Unfolding Primary for Exoplanet Research via Spectroscopic High Angular Resolution Photography
摘要：
我们建议从大约100个地球大小的行星反射光的光谱中寻找生物特征，这些行星已经知道在它们的宜居带（HZ）中运行。对于G型和K型宿主的样本，这些行星中的大多数将与它们的宿主恒星相距25至50毫角秒（mas），并且暗10亿至100亿倍。为了在氧生物特征的波长（763纳米）处将行星的图像与其宿主恒星的图像分开，我们需要一个孔径为16米的望远镜。此外，在系外行星图像中的位置，来自主恒星的光的强度必须被抑制，否则系外行星将在眩光中消失。这带来了巨大的技术挑战。地球的大气层是湍流的，这使得它不可能在763 nm的地面上达到所需的对比度。因此，望远镜需要在太空中，为了将望远镜安装在火箭整流罩中，它必须在折叠时比工作时小4倍或更多倍。为了获得763 nm处的行星生物特征光谱，我们需要使用一个视场（FOV）为1000 x 1000毫角秒（mas）和光谱分辨率为100的积分场光谱仪（IFS）。这是一种设备，可以同时拍摄系外行星的许多照片，每张照片的波长略有不同，然后记录为具有两个空间维度和一个波长维度的数据立方体。在每一个数据立方体波长切片中，来自行星图像所在位置的主星的背景光必须最小化。这是通过阻挡来自主星的光的日冕仪和持续保持非常高精度的光学对准以使图像尽可能清晰的主动/自适应光学技术来实现的。这些都是设计研究中需要解决的技术挑战。
英文摘要：
We propose to search for biosignatures in the spectra of reflected light from about 100 Earth-sized planets that are already known to be orbiting in their habitable zones (HZ). For a sample of G and K type hosts, most of these planets will be between 25 and 50 milli-arcsec (mas) from their host star and 1 billion to 10 billion times fainter. To separate the planet's image from that of its host star at the wavelength (763nm) of the oxygen biosignature we need a telescope with an aperture of 16 metres. Furthermore, the intensity of the light from the host star at the position in the image of the exoplanet must be suppressed otherwise the exoplanet will be lost in the glare. This presents huge technical challenges. The Earth's atmosphere is turbulent which makes it impossible to achieve the required contrast from the ground at 763nm. The telescope therefore needs to be in space and to fit the telescope in the rocket fairing it must be a factor of 4 or more times smaller when folded than when operational. To obtain spectroscopy of the planet's biosignature at 763nm we need to use an integral field spectrometer (IFS) with a field of view (FOV) of 1000 x 1000 milli-arcsec (mas) and a spectral resolution of 100. This is a device that simultaneously takes many pictures of the exoplanet each at a slightly different wavelength which are then recorded as a data cube with two spatial dimensions and one wavelength dimension. In every data cube wavelength slice, the background light from the host star at the location of the planet image must be minimised. This is achieved via a coronagraph which blocks the light from the host star and active/adaptive optics techniques which continuously maintain very high accuracy optical alignment to make the images as sharp as possible. These are the technical challenges to be addressed in a design study.
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