LeMMINGs。III。Palomar样本的e-MERLIN遗产调查。通过[O III ]探索活动星系和非活动星系核射电辐射的起源--射电联系
LeMMINGs. III. The e-MERLIN Legacy Survey of the Palomar sample. Exploring the origin of nuclear radio emission in active and inactive galaxies through the [O III] -- radio connection
摘要：
是什么决定了本星系的核射电辐射？我们结合光学[O III]线发射，强大的黑洞（BH）质量估计，和高分辨率e-MERLIN 1.5 GHz的数据，从LeMMINGS调查，一个完整的样本附近的280个，光学活性（LINER和Seyfert）和不活跃的HII和吸收线星系（ALG）。使用[O III]光度（$L_{\rm [O~III]}$）作为吸积功率的代理，本地星系遵循不同的序列在BH活动的光学无线电平面，这表明不同的起源的光学类的核无线电发射。发现它们的秒差距尺度核心（$L_{\rm core}$）的1.5-GHz射电光度与BH质量（$M_{\rm BH}$）和[O~III]光度成比例。在$M_{\rm BH} \sim$ 10 $^{6.5}$ M $_{\odot}$以下，来自非喷流HII星系的恒星过程以$L_{\rm core} \propto M_{\rm BH}^{0.61\pm0.33}$和$L_{\rm core} \propto L_{\rm [O~III]}^{0.79\pm0.30}$为主。在$M_{\rm BH} \sim$ 10 $^{6.5}$ M $_{\odot}$以上，吸积驱动的过程以$L_{\rm core} \propto M_{\rm BH}^{1.5-1.65}$和$L_{\rm core} \propto L_{\rm [O~III]}^{0.99-1.31}$占主导地位的活动星系：射电安静/响亮的LINER，塞弗特和喷流HII星系总是显示（尽管很低）的射电发射BH活动的签名，$L_{\rm 1.5\, GHz}\gtrsim$ 10 $^{19.8}$ W Hz $^{-1}$和$M_{\rm BH}\gtrsim10^{7}$ M $_{\odot}$，在一个广泛的爱丁顿标度吸积率（$\dot{m}$）。无线电静音和无线电大声班轮是由低$\dot{m}$光盘发射亚相对论和相对论射流，分别。低功率的慢喷流和盘/日冕风从中高$\dot{m}$盘占紧凑和边缘增亮的塞弗茨喷流，分别。喷流的HII星系可能拥有弱活动的BH。燃料匮乏的BH和经常性活动占ALG属性。[删节]
英文摘要：
What determines the nuclear radio emission in local galaxies? We combine optical [O III] line emission, robust black hole (BH) mass estimates, and high-resolution e-MERLIN 1.5-GHz data, from the LeMMINGs survey, of a statistically-complete sample of 280 nearby, optically active (LINER and Seyfert) and inactive HII and Absorption line galaxies [ALG]) galaxies. Using [O III] luminosity ($L_{\rm [O~III]}$) as a proxy for the accretion power, local galaxies follow distinct sequences in the optical-radio planes of BH activity, which suggest different origins of the nuclear radio emission for the optical classes. The 1.5-GHz radio luminosity of their parsec-scale cores ($L_{\rm core}$) is found to scale with BH mass ($M_{\rm BH}$) and [O~III] luminosity. Below $M_{\rm BH} \sim$10$^{6.5}$ M$_{\odot}$, stellar processes from non-jetted HII galaxies dominate with $L_{\rm core} \propto M_{\rm BH}^{0.61\pm0.33}$ and $L_{\rm core} \propto L_{\rm [O~III]}^{0.79\pm0.30}$. Above $M_{\rm BH} \sim$10$^{6.5}$ M$_{\odot}$, accretion-driven processes dominate with $L_{\rm core} \propto M_{\rm BH}^{1.5-1.65}$ and $L_{\rm core} \propto L_{\rm [O~III]}^{0.99-1.31}$ for active galaxies: radio-quiet/loud LINERs, Seyferts and jetted HII galaxies always display (although low) signatures of radio-emitting BH activity, with $L_{\rm 1.5\, GHz}\gtrsim$10$^{19.8}$ W Hz$^{-1}$ and $M_{\rm BH}\gtrsim10^{7}$ M$_{\odot}$, on a broad range of Eddington-scaled accretion rates ($\dot{m}$). Radio-quiet and radio-loud LINERs are powered by low-$\dot{m}$ discs launching sub-relativistic and relativistic jets, respectively. Low-power slow jets and disc/corona winds from moderately high to high-$\dot{m}$ discs account for the compact and edge-brightened jets of Seyferts, respectively. Jetted HII galaxies may host weakly active BHs. Fuel-starved BHs and recurrent activity account for ALG properties. [abridged]
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