Demystifying the Diverse IR SEDs of Type-1 AGNs from z~0 to z~6

Title: Demystifying the Diverse IR SEDs of Type-1 AGNs from z~0 to z~6 

Speaker: Jianwei Lyu (University of Arizona) 

Location:  the middle conference room , 3rd floor 

Time: 10:00 am, January 16th (Wednesday) 


To gain insights into the nature of AGN dust environment and explore its possible evolution, we have conducted a systematic research to reveal the connections behind the variations of AGN SEDs through a comparative study of local AGNs with high-z objects, covering broad ranges of luminosity (LAGN~108 1014 L) and redshift (z~06) (Lyu, Rieke & Alberts 2016, Lyu, Rieke & Shi 2017; Lyu & Rieke 2017; Lyu & Rieke 2018). We have shown a minimalist two-free-parameter semi-empirical model is good enough to reconcile the IR SED shapes of all major populations of type-1 AGNs, including local Seyfert-1 nuclei, normal blue quasars, extremely red quasars at z ?2–3 (Ross et al. 2015), AGNs with mid-IR excess emission at z ?0.7–2 (Xu et al. 2015), hot dust-obscured galaxies at z ?1.5–4 (Eisenhardt et al. 2012), and dust-free quasars at z ? 6 (Jiang et al. 2010). In fact, the commonly seen UV-optical extinction, the unexpected strong mid-IR polar dust emission, and the poorly-understood near- to mid-IR SED variations in type-1 AGNs can be physically connected in a similar fashion. It is highly likely that most type-1 AGNs, regardless of their luminosities and redshifts, share similar torus properties but differ mainly due to the extended (sub-kpc to kpc scales) polar dust component. By grouping similar SED behaviors together and summarizing observations in the literature, we have proposed that the AGN environment could be grouped into three general categories, in which feedbacks from the AGN and/or the host galaxy would influence the behavior of the polar dust component. The possibly frequent appearance of the AGN polar dust emission greatly complicates the interpretation of AGN IR properties and undermines the validity of estimating the torus dust covering factor from SEDs. The templates developed from this work can be generally applied in e.g., SED decompositions of galaxies with possible AGN contribution, IR AGN selections and the search for AGN candidates with strong polar dust emission. 

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