Characterizing Compact 15-33 GHz Radio Continuum Sources in Local U/LIRGs
Y. Song, S. T. Linden, A. S. Evans, L. Barcos-Munoz, E. J. Murphy, E. Momjian, T. Diaz-Santos, K. L. Larson, G. C. Privon, X. Huang, L. Armus, J. M. Mazzarella,… 展开作者
Y. Song, S. T. Linden, A. S. Evans, L. Barcos-Munoz, E. J. Murphy, E. Momjian, T. Diaz-Santos, K. L. Larson, G. C. Privon, X. Huang, L. Armus, J. M. Mazzarella, V. U, H. Inami, V. Charmandaris, C. Ricci, K. L. Emig, J. McKinney, I. Yoon, D. Kunneriath, T. S. -Y. Lai, E. E. Rodas-Quito, A. Saravia, T. Gao, W. Meynardie, D. B. Sanders
本文分析了在63个本地（超）发光红外星系（U/LIRGs; $L_{\rm IR} \ge 10^{11} L_\odot$）中探测到的$\lesssim 0''.1 - 0''.2$ pc尺度致密射电连续源，使用了卡尔G. Jansky甚大阵。根据辅助数据集和文献资料，我们共识别出133个有效半径为8 - 170 pc的致密射电源，并将它们分为4类：“活动星系核”（AGN）、“活动星系核/星暴复合核”（AGN/SBnuc）、“星暴核”（SBnuc）和“恒星形成团块”（SF）。我们发现，“AGN”和“AGN/SBnuc”更频繁地出现在合并的后期，其33 GHz光度和面密度比“SBnuc”和“SF”高出3倍，这可能是由于前者的极端核星暴和/或AGN活动所致。使用33 GHz连续辐射总量（SFR $\sim 0.14 - 13$ M $_\odot$ yr $^{-1}$，$Σ_{\rm SFR} \sim 13 - 1600$ M $_\odot$ yr $^{-1}$ kpc $^{-2}$）和来自HII区域的无热辐射（中值SFR $_{\rm th} \sim 0.4$ M $_\odot$ yr $^{-1}$，$Σ_{\rm SFR_{th}} \sim 44$ M $_\odot$ yr $^{-1}$ kpc $^{-2}$）测量“SF”和“SBnuc”的恒星形成率（SFR）和表面密度（$Σ_{\rm SFR}$）。这些值比在附近正常（非U/LIRG）中测量的类似大小的团块高1 - 2倍。与“SBnuc”和“SF”（$\sim -0.46$）相比，后者的15 - 33 GHz光谱指数中值（$\sim -0.08$）也更平坦，这可能反映了超新星和/或局部U/LIRGs中ISM密度的更高的非热贡献，这些贡献直接导致和/或导致了它们在100 pc尺度上的极端恒星形成活动。
英文摘要：
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.
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