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In the host galaxies of radio active galactic nuclei (AGN), kinematically disturbed gas due to jet-driven feedback is a widely observed phenomenon. Simulations predict that the impact of jets on the surrounding gas changes as they grow. Useful insights into this phenomenon can be obtained by characterising radio AGN into different evolutionary stages and studying their impact on gas kinematics. We present a systematic study of the gas kinematics for a sample of 5\,720 radio AGN up to $z$\,sim \,0.8 with a large 1.4\,GHz luminosity range of $ and 1\,693 detections. Our careful separation of radio emission from AGN and star formation allows us to isolate the impact of radio jets. Taking advantage of the wide frequency coverage of LOFAR and VLA surveys from $144-3000$\,MHz, we determine the radio spectral shapes, using them to characterise sources into different stages of the radio AGN life cycle. We determine the kinematics from SDSS spectra and link it to the life cycle. Our main conclusion is that the gas is sim \,3 times more likely to be disturbed in the peaked spectrum (PS) sources (that represent a young phase of activity) than non-peaked spectrum (NPS) sources (that represent more evolved sources) at $z<0.4$. This changes to a factor of sim \,2 at $z>0.4$. This shows that on average, the strong impact of jets is limited to the initial stages of the radio AGN life cycle. At later stages, the impact on gas is more gentle. We also determine the dependence of this trend on 1.4\,GHz and luminosities, and find that the difference between the two groups increases with 1.4\,GHz luminosity. Young radio AGN with $L_ 1.4GHz have the most extreme impact on Using a stacking analysis, we are further able to trace the changing impact on in the high frequency peaked spectrum (i.e. youngest), low frequency peaked spectrum ( less young ), and non-peaked spectrum (evolved) radio AGN.
In the host galaxies of radio active galactic nuclei (AGN), kinematically disturbed gas due to jet-driven feedback is a widely observed phenomenon. Simulations predict that the impact of jets on the surrounding gas changes as they grow. Useful insights into this phenomenon can be obtained by characterising radio AGN into different evolutionary stages and studying their impact on gas kinematics. We present a systematic study of the gas kinematics for a sample of 5\,720 radio AGN up to $z$\,sim \,0.8 with a large 1.4\,GHz luminosity range of $ and 1\,693 detections. Our careful separation of radio emission from AGN and star formation allows us to isolate the impact of radio jets. Taking advantage of the wide frequency coverage of LOFAR and VLA surveys from $144-3000$\,MHz, we determine the radio spectral shapes, using them to characterise sources into different stages of the radio AGN life cycle. We determine the kinematics from SDSS spectra and link it to the life cycle. Our main conclusion is that the gas is sim \,3 times more likely to be disturbed in the peaked spectrum (PS) sources (that represent a young phase of activity) than non-peaked spectrum (NPS) sources (that represent more evolved sources) at $z<0.4$. This changes to a factor of sim \,2 at $z>0.4$. This shows that on average, the strong impact of jets is limited to the initial stages of the radio AGN life cycle. At later stages, the impact on gas is more gentle. We also determine the dependence of this trend on 1.4\,GHz and luminosities, and find that the difference between the two groups increases with 1.4\,GHz luminosity. Young radio AGN with $L_ 1.4GHz have the most extreme impact on Using a stacking analysis, we are further able to trace the changing impact on in the high frequency peaked spectrum (i.e. youngest), low frequency peaked spectrum ( less young ), and non-peaked spectrum (evolved) radio AGN.
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 μm 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.
Radio spectral shape of quasars can provide insight into the ages of quasars. We have compiled data for 1804 quasars with z ≲ 1 from the Sloan Digital Sky Survey (SDSS). Additionally, these quasars were also mapped by the Low-Frequency Array at 144 MHz and the Very Large Array Sky Survey at 3000 MHz. The radio spectral index, designated as α 3000 144 (with S(ν) ∝ ν α ), is analyzed between 144 and 3000 MHz as a proxy for the ages of quasars. We measure the [O III] λ5007 emission line in the SDSS spectra. A strong correlation was found between the equivalent width of the core component of the [O III] λ5007 emission line and α 3000 144 . This relationship suggests that the core component of the [O III] λ5007 emission line could potentially serve as a surrogate for the evolutionary stage of a quasar. The quasars at an early stage of evolutions tend to show weaker [O III] λ5007 emission, while older quasars exhibit stronger [O III] λ5007 emission.
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