The differences in the Narrow Line Region of nearby QSOs 1 and QSOs 2: II - Signatures of kinetic feedback

Clicks: 12
ID: 331903
2026
Free PDF
Article Quality & Performance Metrics
Overall Quality
Not rated
Combines reader engagement with the AI quality analysis. This article has not been analysed, so there is no overall score — reader engagement is measured and shown alongside.
AI Quality Assessment
Not analyzed
Readership in this journal
Emerging

Ranked #1,179 of 1,339 articles by views in monthly notices of the royal astronomical society

Most read Least read

Bar heights use a square-root scale. Only the 120 most-read articles are drawn; the journal has 1,339 in total.

Mint this article as an NFT
Not yet minted

Create a permanent, verifiable on-chain record of this article on the Scimatic Network. The NFT is held in your Journament account, and you can withdraw it to your own wallet at any time.

5 SUSD one-off · no wallet required
Sign in to mint
Abstract
Abstract We compare the integrated kinematic properties of the Narrow-Line Region (NLR) of ~1500 type 1 and ~700 type 2 QSOs at 0.4 ≤ z ≤ 0.5 using emission-line profiles from SDSS-IV spectra. The NLR [O iii]λ5007 and Hβ emission lines are fitted using a two-component model comprising a narrow (vn, σn) and a broad component (vb, σb), while fainter lines are fitted with a single Gaussian component. Both QSO types exhibit similar median narrow-component velocities (vn ≈ 0) and velocity dispersions (σn < 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$_{[Ne\, {\sc v}]}$, σb, 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 (AGN) outflows, that appear stronger in QSOs 1, leading to higher estimated mass-outflow rates ($\dot{\mathrm{M}}_\mathrm{out}$) and kinetic powers ($\dot{\mathrm{E}}_\mathrm{out}$). Rather than offering absolute determinations of $\dot{\mathrm{M}}_\mathrm{out}$ and $\dot{\mathrm{E}}_\mathrm{out}$ – 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.
Reference Key
openalex_W7220698037 Use this key to autocite in the manuscript while using SciMatic Manuscript Manager or Thesis Manager
Authors Gabriel R Hauschild Roier, Thaisa Storchi-Bergmann, Rogério Riffel, Vincenzo Mainieri, Lara Gatto
Are you one of these authors? Claim your profile
Journal monthly notices of the royal astronomical society
Year 2026
DOI
10.1093/mnras/stag1898
URL
https://doi.org/10.1093/mnras/stag1898
Keywords Keywords not found

Citations

No citations found. To add a citation, contact the admin at info@scimatic.org

Comments

No comments yet. Be the first to comment on this article.