Studying the warm hot intergalactic medium in emission: a reprise
Studying the warm hot intergalactic medium in emission: a reprise
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研究发射中的暖热星际介质：重演
DOI：
10.1093/mnras/stad1495
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发表时间：
2023
影响因子：
4.8
通讯作者：
ZuHone, J.
中科院分区：
文献类型：
--
作者：
Parimbelli, G.;Branchini, E.;Viel, M.;Villaescusa-Navarro, F.;ZuHone, J.
温热的星际介质(WHIM)包含了很大一部分“缺失的重子”。它在排放中的检测仍然是一个挑战。像雅典娜卫星上的X-IFU这样的集成场分光仪将确保在吸收和发射中进行奇想探测，并首次允许我们调查其物理性质。在我们的研究中，我们使用CAMELS模拟来模拟OVII和OVIII离子线的表面亮度图，并计算光子计数和两点关联函数等汇总统计数据来推断突发事件的性质。我们的发现证实了可探测到的奇想发射主要与星系晕有关，奇想的性质显示出从∼0.5时到现在的最小演化。通过探索CAMELS套件中的一系列参数，我们研究了WHIM属性对宇宙学的敏感性，以及受活动星系核和恒星活动影响的能量反馈机制。这种方法允许我们将宇宙学方面与重子过程分开，并对后者施加限制。此外，我们还使用类似于X-IFU的光谱仪提供了对突发事件观测的预报。我们预计每个像素探测1-3条奇想发射线，并绘制出围绕光环的奇想发射轮廓，最长可达几十角分钟，超过了奇想发射器的典型大小。总体而言，我们的工作证明了发射研究的潜力，以探索心血来潮的最密集阶段，揭示其物理性质，并提供对宇宙和重子过程的洞察。
The warm-hot intergalactic medium (WHIM) contains a significant portion of the ‘missing baryons’. Its detection in emission remains a challenge. Integral field spectrometers like X-IFU on board of the Athena satellite will secure WHIM detection in absorption and emission and, for the first time, allow us to investigate its physical properties. In our research, we use the CAMELS simulations to model the surface brightness maps of the OVII and OVIII ion lines and compute summary statistics like photon counts and 2-point correlation functions to infer the properties of the WHIM. Our findings confirm that detectable WHIM emission is primarily associated with galaxy haloes, and the properties of the WHIM show minimal evolution fromz∼ 0.5 to the present time. By exploring a wide range of parameters within the CAMELS suite, we investigate the sensitivity of WHIM properties to cosmology and energy feedback mechanisms influenced by active galactic nuclei and stellar activity. This approach allows us to separate the cosmological aspects from the baryonic processes and place constraints on the latter. Additionally, we provide forecasts for WHIM observations using a spectrometer similar to X-IFU. We anticipate detecting 1–3 WHIM emission lines per pixel and mapping the WHIM emission profile around haloes up to a few tens of arcminutes, surpassing the typical size of a WHIM emitter. Overall, our work demonstrates the potential of emission studies to probe the densest phase of the WHIM, shedding light on its physical properties and offering insights into the cosmological and baryonic processes at play.