论文标题
鹰和插图tng预测正常星系周围的卷乳介质的分辨osita X射线观察
EAGLE and Illustris-TNG predictions for resolved eROSITA X-ray observations of the circumgalactic medium around normal galaxies
论文作者
论文摘要
我们模拟了附近热X射线冠的堆叠观察结果，与鹰和Illustris-TNG流体动力模拟相关。开发了一条正向建模管道，以预测4年的色素观测和堆叠图像分析，包括工具性和天体物理背景的影响。我们提出了一个实验，以堆叠Z〜0.01星系，这些星系被特定的星形形成速率（SSFR）隔开，以检查高和低SSFR星系的热（t> = 10^6 K）圆形循环介质（CGM）如何有所不同。模拟表明，低质量的热CGM（M_*〜10^{10.5} MSOL），高SSFR（定义为SSFR排名最高的最高三分之一）中央星系，可用于半乳酸半径r〜30-50 kpc。两项模拟都预测，低SSFR星系（SSFR的下三分之一）在固定恒星质量处的亮度较低，而Illustris-TNG则可以预测高SSFR星系周围比Eagle更明亮的冠状动脉。这两个模拟都预测可检测到的排放量为r〜150-200 kpc的堆栈中，以高质量（M_*〜10^{11.0} MSOL）星系为中心，Eagle预测了更明亮的X射线卤素。扩展的软X射线光度与病毒半径内的圆形气体质量密切相关（F_ {CGM}）。对这两个模拟的事先分析已经确定，F_ {CGM}的驱逐反馈主要由黑洞生长驱动，这通过抑制ISM的补充来消除星系生长。两种模拟都预测，阿罗西塔堆栈不仅应首次最终检测和解决l^*星系周围的热CGM，而且还提供了对巴里昂循环运作方式的有力探索，为此，在最新的模拟之间仍未达成共识。
We simulate stacked observations of nearby hot X-ray coronae associated with galaxies in the EAGLE and Illustris-TNG hydrodynamic simulations. A forward modeling pipeline is developed to predict 4-year eROSITA observations and stacked image analysis, including the effects of instrumental and astrophysical backgrounds. We propose an experiment to stack z~0.01 galaxies separated by specific star-formation rate (sSFR) to examine how the hot (T>=10^6 K) circumgalactic medium (CGM) differs for high- and low-sSFR galaxies. The simulations indicate that the hot CGM of low-mass (M_*~10^{10.5} Msol), high-sSFR (defined as the top one-third ranked by sSFR) central galaxies will be detectable to a galactocentric radius r~30-50 kpc. Both simulations predict lower luminosities at fixed stellar mass for the low-sSFR galaxies (the lower third of sSFR) with Illustris-TNG predicting 3x brighter coronae around high-sSFR galaxies than EAGLE. Both simulations predict detectable emission out to r~150-200 kpc for stacks centered on high-mass (M_*~10^{11.0} Msol) galaxies, with EAGLE predicting brighter X-ray halos. The extended soft X-ray luminosity correlates strongly and positively with the mass of circumgalactic gas within the virial radius (f_{CGM}). Prior analyses of both simulations have established that f_{CGM} is reduced by expulsive feedback driven mainly by black hole growth, which quenches galaxy growth by inhibiting replenishment of the ISM. Both simulations predict that eROSITA stacks should not only conclusively detect and resolve the hot CGM around L^* galaxies for the first time, but provide a powerful probe of how the baryon cycle operates, for which there remains an absence of consensus between state-of-the-art simulations.
