论文标题
SRG/EROSITA数据中宇宙网络细丝的X射线排放
X-ray emission from cosmic web filaments in SRG/eROSITA data
论文作者
论文摘要
使用公开可用的Erosita最终赤道深度调查（EFEDS）数据，我们根据所有能量频段的组合，检测到463个细丝的堆叠X射线排放位置为3.8 Sigma。同时，我们发现零假设下的测量概率为〜0.0017。在Sloan数字天空调查中，将细丝鉴定出星系，范围从30 MPC到100 MPC的长度为0.2 <Z <0.6。在掩盖已解决的星系组和群集后，用EFEDS X射线计数速率图在能量范围内的EFEDS X射线计数速率映射以及从Rosat，Chandra，Chandra，XMM-Newton和Erosita观测值中确定的X射线点源进行堆叠。另外，通过从细丝刺中减去10-20 MPC的区域中的信号，可以消除漫射X射线前景和背景排放或任何残余贡献。对于堆叠的信号，我们进行了X射线光谱分析，这表明该信号与热发射有关。根据具有血浆排放的天体血浆排放代码的模型，具有β= 2/3的β模型气体分布，检测到的X射线信号可以解释为在平均气体温度的热气中，平均气体温度为1.0（+0.3 -3 -3 -0.2）KEV kev和21 +-5的气体过度的气体温度为1.0（+0.3 -0.3 -2）。
Using the publicly available eROSITA Final Equatorial Depth Survey (eFEDS) data, we detected the stacked X-ray emissions at the position of 463 filaments at a significance of 3.8 sigma based on the combination of all energy bands. In parallel, we found that the probability of the measurement under the null hypothesis is ~0.0017. The filaments were identified with galaxies in the Sloan Digital Sky Survey survey, ranging from 30 Mpc to 100 Mpc in length at 0.2 < z < 0.6. The stacking of the filaments was performed with the eFEDS X-ray count-rate maps in the energy range between 0.4 - 2.3 keV after masking the resolved galaxy groups and clusters and the identified X-ray point sources from the ROSAT, Chandra, XMM-Newton, and eROSITA observations. In addition, diffuse X-ray foreground and background emissions or any residual contribution were removed by subtracting the signal in the region between 10 - 20 Mpc from the filament spines. For the stacked signal, we performed an X-ray spectral analysis, which indicated that the signal is associated with a thermal emission. According to a model with the astrophysical plasma emission code for the plasma emission and with a beta-model gas distribution with beta=2/3, the detected X-ray signal can be interpreted as emission from hot gas in the filaments with an average gas temperature of 1.0 (+0.3 -0.2) keV and a gas overdensity of 21 +- 5 at the center of the filaments.
