MIRACLE II：通过多云模型揭示NGC 1365环核区多相气体的相互作用
MIRACLE II: Unveiling the multi-phase gas interplay in the circumnuclear region of NGC 1365 via multi-cloud modeling
AI总结：
研究通过多云模型分析NGC 1365环核区的多相气体，揭示星核活动与分子气体的相互作用，首次应用自洽方法确定出流特性。
摘要：
我们通过多云模型研究了附近 Seyfert 1.8 银河 NGC 1365 环核区的多相气体，观测背景为中红外活动环状发射（MIRACLE）计划。我们结合了 JWST/MIRI、VLT/MUSE 和 ALMA 的空间解析光谱观测数据，研究了电离原子气体和温暖及冷分子相。MIRI 数据揭示了超过 40 条中红外发射线，来自电离和温暖分子气体。动量图显示，冷和温暖分子气体都遵循恒星盘的旋转，沿着环核区。电离气体的流量和运动学模式取决于电离势（IP）：低 IP 物种（<25 eV）追踪盘，而高 IP 线（高达 ~120 eV）追踪出流物质。[O III]5700 和 [Ne V]14 线都追踪东南核出流锥。此外，[Ne V]14 检测到西北反锥，光学观测中被遮挡，因此在 [O III]5700 中不可见。中红外诊断不同于光学诊断，清楚地揭示了AGN是核区的主要电离源。高 IP 物种的发射在空间上与电离锥重合，而不是与恒星形成区域重合。利用 [Ne V]24/[Ne V]14 比率，我们推导出电子密度为 (750±440) cm^(-3)，与 [S II] 光学双线的值一致。首次应用了结合先进光电离和运动学模型（HOMERUN+MOKA3D）的自洽方法，以约束内在出流性质，克服了简化经典方法的限制。利用 JWST/MIRI 和 VLT/MUSE 的协同作用，HOMERUN 复制了从光学到中红外超过 60 条发射线的流量，区分了 AGN 和恒星形成贡献，得到了出流质量、几何形状和能量的稳健估计。
英文摘要：
We present a multi-phase study of the gas in the circumnuclear region (~1.1x1.0 kpc^2) of the nearby Seyfert 1.8 galaxy NGC 1365, observed in the context of the Mid-IR Activity of Circumnuclear Line Emission (MIRACLE) program. We combined spatially resolved spectroscopic observations from JWST/MIRI, VLT/MUSE, and ALMA to investigate the ionized atomic gas and the warm and cold molecular phases. MIRI data revealed over 40 mid-IR emission lines from ionized and warm molecular gas. Moment maps show that both cold and warm molecular gas follow the rotation of the stellar disk along the circumnuclear ring. The ionized gas displays flux and kinematic patterns that depend on ionization potential (IP): low-IP species (<25 eV) trace the disk, while higher-IP lines (up to ~120 eV) trace outflowing material. The [O III]5700 and [Ne V]14 lines both trace the southeast nuclear outflow cone. Additionally, [Ne V]14 detects the northwest counter-cone, obscured in the optical and thus invisible in [O III]5700. Mid-IR diagnostics, unlike optical ones, clearly reveal the AGN as the primary ionization source in the nucleus. Emission from high-IP species is spatially coincident with the ionization cones and not with star-forming regions. Using the [Ne V]24/[Ne V]14 ratio, we derive an electron density of (750+-440) cm^(-3), in agreement with values from the [S II] optical doublet. For the first time, we apply a fully self-consistent approach combining advanced photoionization and kinematic models (HOMERUN+MOKA3D) to constrain intrinsic outflow properties, overcoming the limitations of simplified classical methods. Exploiting the synergy of JWST/MIRI and VLT/MUSE, HOMERUN reproduces fluxes of over 60 emission lines from optical to mid-IR, disentangling AGN and star formation contributions and yielding robust estimates of outflow mass, geometry, and energetics.
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
