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arXiv 1901.04494astro-ph.GAastro-ph.CO
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发生GW150914-like事件的矮星系的演化

Evolution of dwarf galaxies hosting GW150914-like events

S. Marassi, L. Graziani, M. Ginolfi, R. Schneider, M. Mapelli, M. Spera, M. Alparone

备注：
MNRAS in press. Replaced with correct captions in figures A1 and A2 of the Appendix
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摘要：

在这里，我们提出了一个详细的分析不同的矮星系，候选主机合并的黑洞双星系统（BHB）产生GW 150914的事件的属性和演化。通过采用一种新的理论框架，将二进制粒子数合成程序\texttt{SeBa}与星系形成模型\texttt{GAMESH}耦合起来，我们可以在一个分辨率为4~cMpc的宇宙学体积中研究这些天体的详细演化，在其中心有一个类银河星系形成。我们确定了三类有趣的候选星系：MW祖星系，矮卫星星系和孤立演化的矮星系。我们发现：（ii）其中，$\sim44\%$由于预期信号的红移而并入MW晕祖星，而其余的矮星被发现是孤立的或作为MW的卫星，它们的演化强烈地受到特殊的动力学历史和环境反馈的影响;（iii）类GW150914双星形成环境的严格条件来自于它们DM晕的吸积历史和高红移宇宙中的辐射反馈;（iv）通过与DGS和ALLSMOG巡天观测到的星表比较，我们发现两个观测到的矮星符合我们模型预测的性质。最后，我们注意到如何目前的分析打开的可能性，建立未来的战略，宿主星系识别。

英文摘要：

Here we present a detailed analysis of the properties and evolution of different dwarf galaxies, candidate to host the coalescence of black hole binary systems (BHB) generating GW150914-like events. By adopting a novel theoretical framework coupling the binary population synthesis code \texttt{SeBa} with the Galaxy formation model \texttt{GAMESH}, we can investigate the detailed evolution of these objects in a well resolved cosmological volume of 4~cMpc, having a Milky Way-like (MW) galaxy forming at its center. We identify three classes of interesting candidate galaxies: MW progenitors, dwarf satellites and dwarf galaxies evolving in isolation. We find that: (i) despite differences in individual histories and specific environments the candidates reduce to only nine representative galaxies; (ii) among them, $\sim44\%$ merges into the MW halo progenitors by the redshift of the expected signal, while the remaining dwarfs are found as isolated or as satellites of the MW and their evolution is strongly shaped by both peculiar dynamical history and environmental feedback; (iii) a stringent condition for the environments where GW150914-like binaries can form comes from a combination of the accretion history of their DM halos and the radiative feedback in the high redshift universe; (iv) by comparing with the observed catalogues from DGS and ALLSMOG surveys we find two observed dwarfs respecting the properties predicted by our model. We finally note how the present analysis opens the possibility to build future strategies for host galaxy identification.

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