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arXiv 2602.20397astro-ph.GA
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约束NGC 4254中恒星形成与热星际介质子银河系关系

Constraining the Sub-Galactic Relationship Between Star Formation and the Hot Interstellar Medium in NGC 4254

Middle Tennessee State University（中田纳西州立大学）；Pennsylvania State University（宾夕法尼亚州立大学）；University of Arkansas（阿肯色大学）；The Ohio State University（俄亥俄州立大学）；European Southern Observatory（欧洲南方天文台）
Erik B. Monson, Bret D. Lehmer, Amirnezam Amiri, Karina Barboza, Ashley Barnes, Antara R. Basu-Zych, Daniel A. Dale, Sanskriti Das, Simthembile Dlamini, Simon C… 展开作者

Erik B. Monson, Bret D. Lehmer, Amirnezam Amiri, Karina Barboza, Ashley Barnes, Antara R. Basu-Zych, Daniel A. Dale, Sanskriti Das, Simthembile Dlamini, Simon C. O. Glover, Kathryn Kreckel, Laura A. Lopez, Sebastian Lopez, Smita Mathur, Hsi-An Pan, Jennifer A. Rodriguez, Karin M. Sandstrom, Sumit K. Sarbadhicary, Jiayi Sun, Thomas G. Williams

备注：
28 pages, 2 page appendix, 18 figures, 8 tables. Submitted to AAS journals
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AI总结：

本研究通过分析NGC 4254中恒星形成与热星际介质的关系，揭示了超新星反馈对热气体的影响，并确定了温度和X射线产率的缩放关系。

摘要：

我们通过结合空间分辨的恒星形成历史（SFHs）和贝叶斯X射线光谱拟合，研究NGC 4254（M99）中恒星形成与X射线发射在约kpc尺度上的关系。我们通过灵活的SFHs模型测量子银河系恒星形成率（SFR），并利用Chandra数据生成去点源的弥散X射线发射图。我们提取并拟合5个由其SFR密度Σ_SFR选择的区域的光谱，推导出热气体的亮度和等离子体温度。我们检查NGC 4254中的子银河系kT-Σ_SFR和L^gas_X-Σ_SFR缩放关系，并与来自核心坍缩超新星（CCSNe）反馈到ISM的简单模型的预测进行比较。NGC 4254的热气体发射与CCSNe能量在ISM中热化约40-50%一致，并且CCSNe喷射物的质量加载率随Σ_SFR^{-1/3}减少。我们的优化模型表明温度和X射线产生效率分别随Σ_SFR缩放为kT = (0.72^{+0.26}_{-0.18} keV) Σ_SFR^{0.34±0.10}和η= (0.03^{+0.omeg-0.01}) Σ_SFR^{0.34±0.18}，对于Σ_SFR = 0.01-0.13 M_⊙ yr^{-1} kpc^{-2}。我们还利用PHANGS计划的数据比较热ISM与其他ISM相的性质。某一区域的弥散X射线发射平均比Hα发射弱200倍，我们发现热ISM的压力高于银河系大尺度动态平衡压力，这与热ISM向周围介质膨胀一致。

英文摘要：

We investigate the relationship between star formation and X-ray emission from the hot interstellar medium (ISM) on $\sim$kpc scales in NGC 4254 (M99) by combining spatially resolved star formation histories (SFHs) and Bayesian X-ray spectral fitting. We measure sub-galactic star formation rates (SFR) by modeling spectrophotometric UV-IR data with flexible SFHs, and we produce point-source-subtracted maps of the diffuse X-ray emission using Chandra data. We extract and fit the spectra of 5 regions selected by their SFR density $Σ_{\rm SFR}$, deriving hot gas luminosities and plasma temperatures. We examine the sub-galactic $kT-Σ_{\rm SFR}$ and $L^{\rm gas}_X-Σ_{\rm SFR}$ scaling relations in NGC 4254, and compare to predictions from simple models of the feedback into the ISM from core collapse supernovae (CCSNe). The hot gas emission from NGC 4254 is consistent with thermalization of $\approx 40-50\%$ of the energy from CCSNe in the ISM, and mass-loading of the CCSNe ejecta which decreases as $Σ_{\rm SFR}^{-1/3}$. Our optimized model implies a temperature and X-ray production efficiency that scale as $kT = (0.72^{+0.26}_{-0.18}~{\rm keV}) Σ_{\rm SFR}^{0.34\pm0.10}$ and $η= (0.03^{+0.02}_{-0.01}) Σ_{\rm SFR}^{0.34\pm0.18}$, respectively, for $Σ_{\rm SFR} = 0.01-0.13~{\rm M_{\odot}~yr^{-1}~kpc^{-2}}$. We also compare the properties of the hot ISM to other ISM phases using data from the PHANGS program. The diffuse X-ray emission of a given region is on average 200 times fainter than the H$α$ emission, and we see evidence that the hot ISM is over-pressurized compared to the large-scale dynamical equilibrium pressure of the galaxy, consistent with expansion of the hot ISM into the ambient medium.

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