SED的高峰和加尔默罗郊区的涟漪
Spikes in the SED and Ripples in the Outskirts of Galaxies
摘要：
我们描述了一种新的方法，使我们能够定量地描述银河系卫星从外部气体盘的扰动分析，而不需要他们的光学知识。我们已经证明了这种方法的有效性，我们称之为潮汐分析，通过将其应用于本地螺旋与已知的光学同伴，包括M51和NGC 1512。这些星系的范围从有一个低质量的伴星（大约是主星系质量的百分之一）到有一个相当大质量的伴星（大约是主星系质量的三分之一）。这种方法对天体物理学的许多领域都有广泛的影响--间接探测暗物质（或暗物质主导的矮星系），以及利用它来破译卫星对星系盘的动力学影响。在这里，我们提出了一些初步的结果上的紧急SED和图像，计算沿这些动态模拟的时间序列，使用3-D自洽蒙特卡罗辐射转移代码RADISHE。我们探讨恒星形成的处方，以及它们如何影响紧急的SED和图像。我们的目标是确定SED的颜色，主要是受星系的相互作用的历史，而不是显着影响的恒星形成处方的选择。如果成功的话，我们也许能够利用主星系的紫外-红外辐射来了解它最近的相互作用历史。
英文摘要：
We describe a new method that allows us to quantitatively characterize galactic satellites from analysis of disturbances in outer gas disks, without requiring knowledge of their optical light. We have demonstrated the validity of this method, which we call Tidal Analysis, by applying it to local spirals with known optical companions, including M51 and NGC 1512. These galaxies span the range from having a low mass companion (~ one-hundredth the mass of the primary galaxy) to a fairly massive companion (~ one-third the mass of the primary galaxy). This approach has broad implications for many areas of astrophysics - for the indirect detection of dark matter (or dark-matter dominated dwarf galaxies), and for galaxy evolution in its use as a decipher of the dynamical impact of satellites on galactic disks. Here, we present some preliminary results on the emergent SEDs and images, calculated along the time sequence of these dynamical simulations using the 3-D self-consistent Monte Carlo radiative transfer code RADISHE. We explore star formation prescriptions and how they affect the emergent SEDs and images. Our goal is to identify SED colors that are primarily affected by the galaxy's interaction history, and not significantly affected by the choice of star formation prescription. If successful, we may be able to utilize the emergent UV-IR SED of the primary galaxy to understand its recent interaction history.
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