Galactic wind X-ray heating of the intergalactic medium during the Epoch of Reionization
Galactic wind X-ray heating of the intergalactic medium during the Epoch of Reionization
复制标题
再电离时期星系间介质的银河风X射线加热
DOI：
10.1093/mnras/stx1857
复制
发表时间：
2017
影响因子：
4.8
通讯作者：
S. Kohn
中科院分区：
文献类型：
--
作者：
A. Meiksin;S. Khochfar;J. Paardekooper;C. D. Vecchia;S. Kohn
计算了再电离(EOR)时期星系风的漫射软X射线发射率。我们考虑了两个分析模型，压力驱动的风和超泡模型，以及包括第一个十亿年(FiBY)计划的气体动力学的3D宇宙模拟。分析模型被归一化，以匹配附近宇宙中恒星形成星系的漫射X射线发射率。宇宙学模拟使用物理激励的恒星形成和风的处方，并包括辐射传递修正。这些模型和模拟都发现，在EoR期间，通过21厘米的测量，现有和计划中的无线电设施可以检测到星系间介质的足够加热。虽然解析模型预测相对于宇宙微波背景的21厘米发射信号被设置为8-10美元，但FiBY模拟中的预测信号保持吸收，直到再电离完成。根据型号的不同，21厘米吸收差值亮度温度最低可达$\Delta T\simeq-130$至$-200$MK。考虑到来自高质量X射线双星的额外热量，将向发射的转变推进到$z_{\rm TRANS}\simeq 10-12$，较浅的吸收特征具有最小的$\Delta T\simeq-110$到$-140$mK。21厘米的信号可能是区分风模型的一种手段，而超级气泡模型更倾向于更早地重新加热。虽然早期向发射的转变可能表明X射线双星在再加热过程中占主导地位，但最早发生的向发射的转变将表明存在额外的热源。
The diffuse soft X-ray emissivity from galactic winds is computed during the Epoch of Reionization (EoR). We consider two analytic models, a pressure-driven wind and a superbubble model, and a 3D cosmological simulation including gas dynamics from the First Billion Years (FiBY) project. The analytic models are normalized to match the diffuse X-ray emissivity of star-forming galaxies in the nearby Universe. The cosmological simulation uses physically motivated star formation and wind prescriptions, and includes radiative transfer corrections. The models and the simulation all are found to produce sufficient heating of the Intergalactic Medium to be detectable by current and planned radio facilities through 21 cm measurements during the EoR. While the analytic models predict a 21 cm emission signal relative to the Cosmic Microwave Background sets in by $z_{\rm trans} \simeq 8 - 10$, the predicted signal in the FiBY simulation remains in absorption until reionization completes. The 21 cm absorption differential brightness temperature reaches a minimum of $\Delta T \simeq -130$ to $-200$ mK, depending on model. Allowing for additional heat from high mass X-ray binaries pushes the transition to emission to $z_{\rm trans} \simeq 10 - 12$, with shallower absorption signatures having a minimum of $\Delta T \simeq -110$ to $-140$ mK. The 21 cm signal may be a means of distinguishing between the wind models, with the superbubble model favouring earlier reheating. While an early transition to emission may indicate X-ray binaries dominate the reheating, a transition to emission as early as $z_{\rm trans} > 12$ would suggest the presence of additional heat sources.
DOI：
10.1088/1538-3873/129/974/045001
发表时间：
2017-04-01
影响因子：
3.5
作者：
DeBoer, David R.;Parsons, Aaron R.;Zheng, Haoxuan
通讯作者：
Zheng, Haoxuan
影响因子：
6.5
作者：
van Haarlem, M. P.;Wise, M. W.;van Zwieten, J.
通讯作者：
van Zwieten, J.