红色间歇泉的射电形态
Radio Morphology of Red Geysers
摘要：
我们提出了150 MHz，1.4 GHz和3 GHz的无线电成像（LoTSS，FIRST和VLASS）和空间分辨电离气体特性（SDSS IV-MANGA）的140个本地（$z<0.1$）早期型“红间歇泉”星系。这些星系的恒星形成活动较低（SFR $\sim \rm 0.01\ M_{\odot} yr^{-1}$），但在空间分辨的发射线图中显示出独特的扩展模式，这些模式被解释为活动星系核（AGN）驱动的大尺度电离风。在这项工作中，我们确认，红色间歇泉主机低光度射电源（$\rm L_{1.4GHz} \sim 10^{22} W Hz^{-1}$）。在42个无线电探测到的红色间歇泉中，有32个在LoTSS和FIRST中进行了空间分辨，其无线电大小在$\sim 5-25$ kpc之间变化。有三个源的无线电大小超过40千秒差距。大多数显示出紧凑的无线电形态，并与低功率紧凑无线电源（“FR 0”星系）或“无线电安静类星体”相一致。它们可能是由小规模活动星系核驱动的喷流提供动力的，这些喷流在目前无线电数据的$5"$分辨率下仍无法解决。扩展的射电源，不属于“紧凑”的形态类，表现出陡峭的频谱与中值频谱指数$-0.67$表示的主导地位，分瓣组件。拥有扩展射电源的红色间歇泉也具有最低的特定恒星形成率，这表明它们要么对周围的星际介质有更大的影响，要么平均在更大质量的晕中发现。电离风锥和扩展射电特征的排列度为0 $^{\circ}$或90 $^{\circ}$，表明星际介质和中心射电活动星系核之间可能存在相互作用。
英文摘要：
We present 150 MHz, 1.4 GHz, and 3 GHz radio imaging (LoTSS, FIRST and VLASS) and spatially resolved ionized gas characteristics (SDSS IV-MaNGA) for 140 local ($z<0.1$) early-type "red geyser" galaxies. These galaxies have low star formation activity (SFR $\sim \rm 0.01\ M_{\odot} yr^{-1}$), but show unique extended patterns in spatially-resolved emission line maps that have been interpreted as large-scale ionized winds driven by active galactic nuclei (AGN). In this work we confirm that red geysers host low-luminosity radio sources ($\rm L_{1.4GHz} \sim 10^{22} W Hz^{-1}$). Out of 42 radio-detected red geysers, 32 are spatially resolved in LoTSS and FIRST, with radio sizes varying between $\sim 5-25$ kpc. Three sources have radio sizes exceeding 40 kpc. A majority display a compact radio morphology and are consistent with either low-power compact radio sources ("FR0" galaxies) or "radio-quiet quasars". They may be powered by small-scale AGN-driven jets which remain unresolved at the current $5"$ resolution of radio data. The extended radio sources, not belonging to the "compact" morphological class, exhibit steeper spectra with a median spectral index of $-0.67$ indicating the dominance of lobed components. The red geysers hosting extended radio sources also have the lowest specific star formation rates, suggesting they either have a greater impact on the surrounding interstellar medium or are found in more massive halos on average. The degree of alignment of the ionized wind cone and the extended radio features are either 0$^{\circ}$ or 90$^{\circ}$, indicating possible interaction between the interstellar medium and the central radio AGN.
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