Simulations of high-z galaxy observations with an ELT-MOS
Simulations of high-z galaxy observations with an ELT-MOS
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使用 ELT-MOS 模拟高 z 星系观测
DOI：
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发表时间：
2014
期刊：
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通讯作者：
L. Pentericci
中科院分区：
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作者：
K. Disseau;M. Puech;H. Flores;F. Hammer;Yanbin Yang;L. Pentericci
我们提出了模拟观测的一个主要的科学案例为39米E-ELT，即检测非常高的z星系。我们模拟了在z = 7处检测UV星际谱线以及在z = 9处检测莱曼α谱线和莱曼断裂，两者均使用MOAO辅助IFU和GLAO馈电光纤。这些模拟是用我们在E-ELT A阶段研究框架内开发的科学模拟器进行的。首先，我们给出了这个模拟器，这是耦合到一个公共的Web接口WEBSIM的功能描述，然后我们给出了一个例子，它的实际使用约束的高层次规格的MOSAIC，一个新的多对象光谱仪的概念，E-ELT。我们的模拟表明，最具约束力的情况是紫外星际线的检测。发现最佳像素尺寸为~80 mas，这允许在40小时的积分时间内检测高达JAB ~27的紫外线。使用80 mas/像素IFU和仅10小时积分时间内，分别检测到高达JAB ~30和JAB ~28的莱曼α发射器和莱曼断裂电子束。使用MOAO馈入IFU的检测限通常比使用GLAO馈入光纤的检测限弱约0.5-1 mag，但在使用GLAO馈入光纤的模式下，多路复用要大一个数量级。我们探索最佳的观测策略，考虑这些观测限制，以及预期的目标密度的每一个观测模式。
We present simulated observations of one of the major science cases for the 39m E-ELT, namely the detection of very high-z galaxies. We simulated the detection of UV interstellar lines at z = 7 and the detection of the Lyman alpha line and the Lyman break at z = 9, both with MOAO-assisted IFUs and GLAO-fed fibers. These simulations are performed with the scientific simulator we developped in the frame of the E-ELT phase A studies. First, we give a functional description of this simulator, which is coupled to a public web interface WEBSIM, and we then give an example of its practical use to constrain the high level specifications of MOSAIC, a new multi-object spectrograph concept for the E-ELT. Our simulations show that the most constraining case is the detection of UV interstellar lines. The optimal pixel size is found to be ~80 mas, which allows detecting UV lines up to JAB ~27 in 40 hours of integration time. Lyman Alpha Emitters and Lyman Break Galaxies are detected respectively up to JAB ~30 and JAB ~28 with a 80 mas/pixel IFU and within only 10 hours of integration time. Detection limits are typically ~0.5-1 mag fainter using MOAO-fed IFUs than using GLAO-fed fibers, but the multiplex is one magnitude larger in the mode using GLAO-fed fibers. We explore the optimal observational strategy for each observing mode considering these observing limits as well as the expected target densities.