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Determining star-formation rates in Active Galactic Nuclei hosts via stellar population synthesis
Monthly Notices of the Royal Astronomical Society ( IF 4.8 ) Pub Date : 2020-12-21 , DOI: 10.1093/mnras/staa3907 Rogério Riffel 1, 2 , Nicolas D Mallmann 1, 2 , Gabriele S Ilha 2, 3 , Thaisa Storchi-Bergmann 1, 2 , Rogemar A Riffel 2, 3 , Sandro B Rembold 2, 3 , Dmitry Bizyaev 4, 5 , Janaina C do Nascimento 1, 2 , Jaderson S Schimoia 2, 3 , Luiz N da Costa 2, 6 , Nicholas Fraser Boardman 7 , Médéric Boquien 8 , Guilherme S Couto 8
Monthly Notices of the Royal Astronomical Society ( IF 4.8 ) Pub Date : 2020-12-21 , DOI: 10.1093/mnras/staa3907 Rogério Riffel 1, 2 , Nicolas D Mallmann 1, 2 , Gabriele S Ilha 2, 3 , Thaisa Storchi-Bergmann 1, 2 , Rogemar A Riffel 2, 3 , Sandro B Rembold 2, 3 , Dmitry Bizyaev 4, 5 , Janaina C do Nascimento 1, 2 , Jaderson S Schimoia 2, 3 , Luiz N da Costa 2, 6 , Nicholas Fraser Boardman 7 , Médéric Boquien 8 , Guilherme S Couto 8
Affiliation
The effect of active galactic nuclei (AGN) feedback on the host galaxy, and its role in quenching or enhancing star-formation, is still uncertain due to the fact that usual star-formation rate (SFR) indicators -- emission-line luminosities based on the assumption of photoionisation by young stars -- cannot be used for active galaxies as the ionising source is the AGN. We thus investigate the use of SFR derived from the stellar population and its relation with that derived from the gas for a sample of 170 AGN hosts and a matched control sample of 291 galaxies. We compare the values of SFR densities obtained via the Ha emission line (SFRg) for regions ionised by hot stars according to diagnostic diagrams with those obtained from stellar population synthesis (SFRstars) over the last 1 to 100~Myr. We find that the SFRstars over the last 20~Myrs closely reproduces the SFRg, although a better match is obtained via the transformation: log(SFRstars) = (0.872+/-0.004) log(SFRg) -(0.075+/-0.006), which is valid for both AGN hosts and non-active galaxies. We also compare the reddening obtained via the gas Ha/Hb ratio with that derived via the full spectral fitting in the stellar population synthesis. We find that the ratio between the gas and stellar extinction is in the range 2.64 < A_Vgas/A_Vstar} < 2.85, in approximate agreement with previous results from the literature, obtained for smaller samples. We interpret the difference as being due to the fact that the reddening of the stars is dominated by that affecting the less obscured underlying older population, while the reddening of the gas is larger as it is associated to a younger stellar population buried deeper in the dust.
中文翻译：
通过恒星群合成确定活动星系核宿主的恒星形成率
由于通常的恒星形成率 (SFR) 指标——基于发射线光度的事实，活动星系核 (AGN) 反馈对宿主星系的影响及其在淬灭或增强恒星形成中的作用仍不确定假设年轻恒星会发生光电离——不能用于活动星系，因为电离源是 AGN。因此，我们针对 170 个 AGN 宿主的样本和 291 个星系的匹配对照样本，研究了源自恒星群的 SFR 的使用及其与源自气体的 SFR 的关系。我们将根据诊断图通过 Ha 发射线 (SFRg) 获得的热恒星电离区域的 SFR 密度值与从过去 1 到 100~Myr 的恒星群合成 (SFRstars) 获得的值进行比较。我们发现过去 20~Myrs 的 SFRstars 与 SFRg 非常接近，尽管通过转换获得了更好的匹配：log(SFRstars) = (0.872+/-0.004) log(SFRg) -(0.075+/-0.006) ，这对 AGN 主机和非活动星系都有效。我们还将通过气体 Ha/Hb 比率获得的变红与通过恒星群合成中的全光谱拟合得出的变红进行比较。我们发现气体和恒星消光之间的比率在 2.64 < A_Vgas/A_Vstar} < 2.85 的范围内，这与之前文献中获得的较小样本的结果大致一致。我们将这种差异解释为由于恒星变红主要受影响较少的潜在老年人群的影响，
更新日期：2020-12-21
中文翻译：
通过恒星群合成确定活动星系核宿主的恒星形成率
由于通常的恒星形成率 (SFR) 指标——基于发射线光度的事实，活动星系核 (AGN) 反馈对宿主星系的影响及其在淬灭或增强恒星形成中的作用仍不确定假设年轻恒星会发生光电离——不能用于活动星系，因为电离源是 AGN。因此，我们针对 170 个 AGN 宿主的样本和 291 个星系的匹配对照样本，研究了源自恒星群的 SFR 的使用及其与源自气体的 SFR 的关系。我们将根据诊断图通过 Ha 发射线 (SFRg) 获得的热恒星电离区域的 SFR 密度值与从过去 1 到 100~Myr 的恒星群合成 (SFRstars) 获得的值进行比较。我们发现过去 20~Myrs 的 SFRstars 与 SFRg 非常接近，尽管通过转换获得了更好的匹配：log(SFRstars) = (0.872+/-0.004) log(SFRg) -(0.075+/-0.006) ，这对 AGN 主机和非活动星系都有效。我们还将通过气体 Ha/Hb 比率获得的变红与通过恒星群合成中的全光谱拟合得出的变红进行比较。我们发现气体和恒星消光之间的比率在 2.64 < A_Vgas/A_Vstar} < 2.85 的范围内，这与之前文献中获得的较小样本的结果大致一致。我们将这种差异解释为由于恒星变红主要受影响较少的潜在老年人群的影响，
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