The AGN contribution to the UV–FIR luminosities of interacting galaxies and its role in identifying the main sequence
The AGN contribution to the UV–FIR luminosities of interacting galaxies and its role in identifying the main sequence
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DOI：
10.1093/mnras/staa2813
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发表时间：
2020-09
影响因子：
4.8
通讯作者：
A. F. R. Padilla;A. F. R. Padilla;A. F. R. Padilla;M. Ashby;H. Smith;J. R. Mart'inez-Galarza;Aliza G. Beverage;Aliza G. Beverage;J. Dietrich;J. Dietrich;M. Higuera-G.;A. Weiner
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文献类型：
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作者：
A. F. R. Padilla;A. F. R. Padilla;A. F. R. Padilla;M. Ashby;H. Smith;J. R. Mart'inez-Galarza;Aliza G. Beverage;Aliza G. Beverage;J. Dietrich;J. Dietrich;M. Higuera-G.;A. Weiner
活动星系核(AGN)的辐射在许多星系的演化中扮演着重要的角色，包括发光和超发光系统(U/LIRG)以及合并系统。然而，它的影响的程度、持续时间和确切的影响仍然不完全清楚。为了评估活动星系核对相互作用系统的影响，我们给出了189个邻近星系的光谱能量分布(SED)分析。我们使用来自GALEX、SDSS、2MASS、IRAS、WISE、Spitzer和Herschel的数据，收集并系统地将档案宽带成像马赛克从紫外线重新缩减到远红外。我们使用来自Spitzer/IRS的光谱从跟踪恒星形成和活动星系核活动的精细结构线中获得通量。利用SED模拟和拟合工具Cigale，我们得到了这些星系中恒星形成区和活动星系核占主导地位的核区ISM的物理条件。我们研究了恒星形成率(SFRS)和活动星系核分数贡献($f{Rm{AGN}}$)是如何依赖于恒星质量、星系类型和合并阶段的。我们发现，质量大于10^{10}\rm{M}的发光星系很可能明显偏离了传统的星系主序关系。有趣的是，这组天体中的红外活动星系核光度和恒星质量比SFR和恒星质量要紧密得多。我们发现埋藏的活动星系核可能在$f{\rm{AGN}}$-[Ne V]/[Ne II]平面上占据明亮的恒星爆发和纯活动星系核之间的轨迹。我们发现$f_{\rm{agn}}$与后期的合并之间存在适度的相关性。
Emission from active galactic nuclei (AGNs) is known to play an important role in the evolution of many galaxies including luminous and ultraluminous systems (U/LIRGs), as well as merging systems. However, the extent, duration, and exact effects of its influence are still imperfectly understood. To assess the impact of AGNs on interacting systems, we present a Spectral Energy Distribution (SED) analysis of a sample of 189 nearby galaxies. We gather and systematically re-reduce archival broad-band imaging mosaics from the ultraviolet to the far-infrared using data from GALEX, SDSS, 2MASS, IRAS, WISE, Spitzer and Herschel. We use spectroscopy from Spitzer/IRS to obtain fluxes from fine-structure lines that trace star formation and AGN activity. Utilizing the SED modelling and fitting tool CIGALE, we derive the physical conditions of the ISM, both in star-forming regions and in nuclear regions dominated by the AGN in these galaxies. We investigate how the star formation rates (SFRs) and the fractional AGN contributions ($f_{\rm{AGN}}$) depend on stellar mass, galaxy type, and merger stage. We find that luminous galaxies more massive than about $10^{10} \rm{M}_{*}$ are likely to deviate significantly from the conventional galaxy main-sequence relation. Interestingly, infrared AGN luminosity and stellar mass in this set of objects are much tighter than SFR and stellar mass. We find that buried AGNs may occupy a locus between bright starbursts and pure AGNs in the $f_{\rm{AGN}}$-[Ne V]/[Ne II] plane. We identify a modest correlation between $f_{\rm{AGN}}$ and mergers in their later stages.