Speaker
Description
Active galactic nuclei (AGN) are some of the brightest sources in the Universe, emitting light at all wavelengths due to their complex structure. Deep multi-wavelength extragalactic surveys are therefore important for understanding the full physics of AGN and their role in the formation and evolution of galaxies. The Lockman-SpReSO survey is one of the deepest multi-wavelength spectroscopic surveys in the far-infrared (FIR). It is a unique sample of AGN with deep FIR and optical spectroscopic data obtained using Herschel and the GTC 10m telescopes, respectively. Using Lockman-SpReSO, it is possible to study the relationship between the fundamental FIR and optical properties of galaxies. In this work we want to better understand the optical spectroscopic properties of type-2 FIR AGN by characterizing the emission line properties and comparing them with the FIR properties. Therefore We first obtain the emission spectra of AGN by running the Starlight code and by subtracting the continuum plus absorption spectra. Using the strong emission lines, we measure the line intensity, full width at half maximum (FWHM) and the equivalent width (EW) of all identified lines. Our analysis revealed that FIR-detected type-2 AGN exhibit similar strong emission lines to optically-selected AGN. We constructed a comprehensive catalogue of emission line measurements for 71 sources, which will be made publicly available. We found correlations between emission line luminosities and AGN luminosity, SFR, and IR luminosity, suggesting connections between the AGN, surrounding gas, star formation, and dust properties. We confirmed our source position in the NII-BPT diagram. We show that for FIR-detected AGN, there is relation between type-2 AGN luminosity and SFR. In addition we test the SFR that has been measured through SED fitting, by comparing the SED-derived SFR with the total (IR) luminosity itself and comparing the SED-derived SFR with the SFR calculated, which showed a good agreement.
| Stream | Science or Engineering |
|---|