Active Galactic Nuclei and Star Formation in nearby Galaxies (AGNSTRONG). I. Sample and Strategy

• Published in: The Astronomical journal 2024-07, Vol.168 (1), p.36
• Main Authors: Le, Huynh Anh N., Qin, Chen, Xue, Yongquan, Zhu, Shifu, N. Nguyen, Kim Ngan, Xia, Ruisong, Lin, Xiaozhi
• Format: Article
• Language: English
• Subjects: Active galactic nuclei; Active galaxies; Astrophysics; Galaxies; Interstellar medium; Kinematics; Molecular gases; Outflow; Relativistic effects; Research methods; Spectral energy distribution; Star & galaxy formation; Star formation; Stars
• ISSN: 0004-6256; 1538-3881
• DOI: 10.3847/1538-3881/ad4ce9

We introduce our project, AGNSTRONG (Active Galactic Nuclei and STaR fOrmation in Nearby Galaxies). Our research goals encompass investigating the kinematic properties of ionized and molecular gas outflows, understanding the impact of AGN feedback, and exploring the coevolution dynamics between AGN strength activity and star formation activity. We aim to conduct a thorough analysis to determine whether there is an increase or suppression in star formation rates (SFRs) among targets with and without powerful relativistic jets. Our sample consists of 35 nearby AGNs with and without powerful relativistic jet detections. Utilizing submillimeter continuum observations at 450 and 850 μ m from SCUBA-2 at the James Clerk Maxwell Telescope, we determine SFRs for our sources using spectral energy distribution (SED) fitting models. Additionally, we employ high-quality, spatially resolved spectra from UV-optical to near-infrared bands obtained with the Double Spectrograph and Triple Spectrograph mounted on the 200 inch Hale Telescope at Palomar Observatory to study their multiphase gas outflow properties. This paper presents an overview of our sample selection methodology, research strategy, and initial results of our project. We find that the SFRs determined without including the submillimeter data in the SED fitting are overestimated by ∼0.08 dex compared to those estimated with the inclusion of submillimeter data. Additionally, we compare the estimated SFRs in our work with those traced by the 4000 Å break, as provided by the Max Planck Institute for Astrophysics and Johns Hopkins University catalog. We find that our determined SFRs are systematically higher than those traced by the 4000 Å break. Finally, we outline our future research plans.