The differences in the narrow-line region of nearby QSOs 1 and QSOs 2 – II. Signatures of kinetic feedback
- 1Departamento de Astronomia, Universidade Federal do Rio Grande do Sul , Av. Bento Gonçalves 9500, 91501-970 Porto Alegre, RS ,
- 2European Southern Observatory , Karl-Schwarzschild-Straße 2, D-85748 Garching bei Munchen ,
- 3Astronomisches Rechen-Institut, Zentrum für Astronomie der Universität Heidelberg , Mönchhofstr 12-14, D-69120 Heidelberg ,
Abstract
We compare the integrated kinematic properties of the narrow-line region (NLR) of ∼1500 type 1 and ∼700 type 2 quasi-stellar objects (QSOs) at 0.4 ≤ z ≤ 0.5 using emission-line profiles from Sloan Digital Sky Survey-IV spectra. The NLR [O iii]λ5007 and H β emission lines are fitted using a two-component model comprising a narrow (vn, σ n) and a broad component (vb, σ b), while fainter lines are fitted with a single Gaussian component. Both QSO types exhibit similar median narrow-component velocities (vn≈ 0) and velocity dispersions (σ n lt 200 km s−1), consistent with motion driven by the host galaxy’s gravitational potential. However, parameters associated with the broad, high-velocity gas component (vb, v05, v10, v[ Ne small V], σ b, W80, and W90) differ: QSOs 1 display larger blueshifts and broader emission lines than QSOs 2. This suggests that these components trace active galactic nuclei (AGNs) outflows, that appear stronger in QSOs 1, leading to higher estimated mass-outflow rates (Ṁout) and kinetic powers (Ėout). Rather than offering absolute determinations of Ṁout and Ėout – which remain subject to physical uncertainties – this statistical study supports the higher NLR excitation found for QSOs 1 in Paper I, as an orientation effect: In QSOs 1, we observe gas closer to the AGN core, where velocities and velocity dispersions are intrinsically higher. Nevertheless, the trend of QSOs 2 exhibiting higher average [O iii] luminosities than QSOs 1 suggests an evolutionary contribution, where QSOs 2 represent an early obscured AGN phase followed by a blowout phase that reveals the central core as a QSO 1.
Related
- The kinetic Sunyaev Zeldovich effect as a benchmark for AGN feedback models in hydrodynamical simulations: insights from DESI + ACT
- Interpreting the stacked kinetic SZ signal II: the degeneracy between satellite galaxies and baryonic feedback
- Jet--ISM Interactions in Gaseous Disks: Simulating Kinetic Feedback in the Radio Galaxy 3C 326 N
- Jet–ISM interactions in gaseous discs: simulating kinetic feedback in the radio galaxy 3C 326 N
- Topological Signatures of AGN Feedback in the Simba Simulations
BibTeX
@article{hauschildroier2026differences,
title = {{The differences in the narrow-line region of nearby QSOs 1 and QSOs 2 – II. Signatures of kinetic feedback}},
author = {Gabriel R Hauschild-Roier and Thaisa Storchi-Bergmann and Rogério Riffel and Vincenzo Mainieri and Lara Gatto},
journal = {Monthly Notices of the Royal Astronomical Society},
year = {2026},
month = oct,
doi = {10.1093/mnras/stag1898},
url = {https://academic.oup.com/mnras/article/doi/10.1093/mnras/stag1898/8898886},
note = {CC BY 4.0},
}
RIS
TY - JOUR
TI - The differences in the narrow-line region of nearby QSOs 1 and QSOs 2 – II. Signatures of kinetic feedback
AU - Gabriel R Hauschild-Roier
AU - Thaisa Storchi-Bergmann
AU - Rogério Riffel
AU - Vincenzo Mainieri
AU - Lara Gatto
PY - 2026
DA - 2026/10/09
JO - Monthly Notices of the Royal Astronomical Society
DO - 10.1093/mnras/stag1898
UR - https://academic.oup.com/mnras/article/doi/10.1093/mnras/stag1898/8898886
AB - We compare the integrated kinematic properties of the narrow-line region (NLR) of ∼1500 type 1 and ∼700 type 2 quasi-stellar objects (QSOs) at 0.4 ≤ z ≤ 0.5 using emission-line profiles from Sloan Digital Sky Survey-IV spectra. The NLR [O iii]λ5007 and H β emission lines are fitted using a two-component model comprising a narrow (v_n, σ _n) and a broad component (v_b, σ _b), while fainter lines are fitted with a single Gaussian component. Both QSO types exhibit similar median narrow-component velocities (v_n≈ 0) and velocity dispersions (σ _ n lt 200 km s^−1), consistent with motion driven by the host galaxy’s gravitational potential. However, parameters associated with the broad, high-velocity gas component (v_b, v_05, v_10, v_[ Ne small V], σ _ b, W80, and W90) differ: QSOs 1 display larger blueshifts and broader emission lines than QSOs 2. This suggests that these components trace active galactic nuclei (AGNs) outflows, that appear stronger in QSOs 1, leading to higher estimated mass-outflow rates (Ṁ_out) and kinetic powers (Ė_out). Rather than offering absolute determinations of Ṁ_out and Ė_out – which remain subject to physical uncertainties – this statistical study supports the higher NLR excitation found for QSOs 1 in Paper I, as an orientation effect: In QSOs 1, we observe gas closer to the AGN core, where velocities and velocity dispersions are intrinsically higher. Nevertheless, the trend of QSOs 2 exhibiting higher average [O iii] luminosities than QSOs 1 suggests an evolutionary contribution, where QSOs 2 represent an early obscured AGN phase followed by a blowout phase that reveals the central core as a QSO 1.
SN - 0035-8711
SN - 1365-2966
ER -