论文标题
表征紧凑型15-33 GHz无线电连续源
Characterizing Compact 15-33 GHz Radio Continuum Sources in Local U/LIRGs
论文作者
论文摘要
我们介绍了$ \ sim 100 $ PC规模的紧凑无线电连续源在63个本地（Ultra）（Ultra）发光红外星系中检测到的分析（U/LIRGS； $ l _ {\ rm Ir} \ rm ir} \ ge 10^{11}}}}}}} l _ \ odot $，使用fwhm $ \ \ $ \ ysim nose ossim commim 0 coss Karl G. Jansky非常大。我们总共确定了133个紧凑型无线电源，有效半径为8-170pc，它们分为四个主要类别：“ AGN”（AGN），“ AGN/SBNUC”（AGN/SBNUC”（Agn-Starburst复合核），“ SBNUC”（SBNUC），“ SBLERST核）和“ STARBURST核）和“ SF”（Star-Forming Classs） - 基于ANCILLARY DATASTAS和ANCILLARY DATASTAS。我们发现，与“ SBNUC”和“ SF”相比，在后期合并中更频繁地发生“ AGN”和“ AGN/SBNUC”，并且具有多达3个DEX较高的33 GHz亮度和表面密度，这可能归因于前者的极端核突象发生和/或AGN活性。恒星形成率（SFRS）和表面密度（$σ_ {\ rm sfr} $）使用总计33 GHz连续量发射（SFR $ \ sim 0.14-13 $ _ $ _ \ m $ _ \ odot $ yr $ yr $ yr $ yr $^{-1 16 00- $ sim $ yr $ sim， m $ _ \ odot $ yr $^{ - 1} $ kpc $^{ - 2} $）和来自HII区域的无热免费排放（中位sfr $ _ {\ rm th} \ sim th} \ sim 0.4 $ m $ m $ m $ _ \ odot $ _ \ odot $ yr $ yr $^yr $^{ - 1} $ sim sim sim sim，$ s s s c { m $ _ \ odot $ yr $^{ - 1} $ kpc $^{ - 2} $）。这些值比附近正常（非U/lirgs）中相似大小的团块测量的值高1-2个DEX。后者的中位数为15-33 GHz光谱指数（$ \ sim -0.08 $），而“ sbnuc”和“ sf”（$ \ sim -0.46 $），这可能反映出超级新星和/或ISM在u/lirg中的较高的非电压贡献，这些贡献直接导致u/或lirg scret cartic scret和/或scret scret corper corper和/或scret scret conty scret conter cont cart scret cont scret cont cont scret cont scret conts pc scret te他们的群体，以达到他们的标准。
We present the analysis of $\sim 100$pc-scale compact radio continuum sources detected in 63 local (Ultra) Luminous Infrared Galaxies (U/LIRGs; $L_{\rm IR} \ge 10^{11} L_\odot$), using FWHM $\lesssim 0''.1 - 0''.2$ resolution 15 and 33 GHz observations with the Karl G. Jansky Very Large Array. We identify a total of 133 compact radio sources with effective radii of 8 - 170pc, which are classified into four main categories -- "AGN" (AGN), "AGN/SBnuc" (AGN-starburst composite nucleus), "SBnuc" (starburst nucleus) and "SF" (star-forming clumps) -- based on ancillary datasets and the literature. We find that "AGN" and "AGN/SBnuc" more frequently occur in late-stage mergers and have up to 3 dex higher 33 GHz luminosities and surface densities compared with "SBnuc" and "SF", which may be attributed to extreme nuclear starburst and/or AGN activity in the former. Star formation rates (SFRs) and surface densities ($Σ_{\rm SFR}$) are measured for "SF" and "SBnuc" using both the total 33 GHz continuum emission (SFR $\sim 0.14 - 13$ M$_\odot$ yr$^{-1}$, $Σ_{\rm SFR} \sim 13 - 1600$ M$_\odot$ yr$^{-1}$ kpc$^{-2}$) and the thermal free-free emission from HII regions (median SFR$_{\rm th} \sim 0.4$ M$_\odot$ yr$^{-1}$, $Σ_{\rm SFR_{th}} \sim 44$ M$_\odot$ yr$^{-1}$ kpc$^{-2}$). These values are 1 - 2 dex higher than those measured for similar-sized clumps in nearby normal (non-U/LIRGs). The latter also have much flatter median 15 - 33 GHz spectral index ($\sim -0.08$) compared with "SBnuc" and "SF" ($\sim -0.46$), which may reflect higher non-thermal contribution from supernovae and/or ISM densities in local U/LIRGs that directly result from and/or lead to their extreme star-forming activities on 100\,pc scales.
