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arxiv: 2605.17993 · v1 · pith:H4AEXJXMnew · submitted 2026-05-18 · 🌌 astro-ph.GA · astro-ph.HE

Nuclear Activity and Host Galaxy Properties of Low-Luminosity AGN Identified from VLA Observations

M. N. Rosli , A. Annuar This is my paper

Pith reviewed 2026-05-20 10:03 UTC · model grok-4.3

classification 🌌 astro-ph.GA astro-ph.HE
keywords low-luminosity AGNVLA radio surveyhost galaxy propertiesblack hole accretionlocal universe AGNmulti-wavelength identification
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The pith

Low-luminosity AGN host smaller black holes and live in lower-mass galaxies with less star formation

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

This paper examines 38 low-luminosity AGN found in a high-resolution 15 GHz radio survey with the VLA. These objects show bolometric luminosities roughly 4 dex fainter than X-ray selected AGN, with black holes about 0.7 dex smaller in mass and accretion rates lower by about 4 dex. Their host galaxies display a range of shapes but average lower stellar masses by 0.3 dex and lower star formation rates by 0.5 dex. The work shows that low-level black hole activity connects to quieter overall galaxy properties in the nearby universe. Optical line diagnostics catch most of these sources while infrared methods catch few due to host contamination.

Core claim

LLAGN selected from sub-arcsecond 15 GHz VLA observations are 4.1 dex fainter in bolometric luminosity than Swift-BAT AGN, host black holes 0.7 dex smaller in mass, and accrete at Eddington ratios 4.2 dex lower. Their host galaxies span disk to bulge morphologies with a subset showing prominent bulges, yet exhibit stellar masses 0.3 dex lower and star formation rates 0.5 dex lower on average.

What carries the argument

Multi-wavelength comparison of black hole mass, Eddington ratio, stellar mass, and star formation rate between a radio-selected LLAGN sample and brighter X-ray selected AGN samples.

Load-bearing premise

The 38 radio sources are powered by nuclear black hole accretion rather than by star formation or other processes in the host galaxy.

What would settle it

Finding that most of the 38 sources show radio properties matching pure star formation models or lack independent nuclear X-ray and optical AGN indicators.

Figures

Figures reproduced from arXiv: 2605.17993 by A. Annuar, M. N. Rosli.

Figure 1
Figure 1. Figure 1: Swift–BAT 14–195 keV flux versus redshift for the LLAGN sample. The red horizontal line represents the approximate 5𝜎 sensitivity limit of the 105-month Swift–BAT survey. since it have finer angular resolution (∼0.5′′ , Weisskopf et al. 2002) than XMM-Newton (∼6 ′′ , Jansen et al. 2001) which allows clearer separation of faint nuclear emission from surrounding host galaxy contamination. For sources lacking… view at source ↗
Figure 2
Figure 2. Figure 2: BPT originally from Baldwin et al. (1981); Kewley et al. (2006) provided classification scheme. Left: The log ([O iii] / H𝛽) vs log ([N ii] / H𝛼) diagram, Centre: log ([O iii] / H𝛽) vs log ([S ii] / H𝛼) diagram and Right: log ([O iii] / H𝛽) vs log ([O i] / H𝛼) diagram. The marginal histograms on the top and right of each panel show the number distribution of galaxies along each emission-line ratio axis. an… view at source ↗
Figure 3
Figure 3. Figure 3: Infrared colour–colour diagram constructed using W1, W2, and W3 WISE bands (3.4, 4.6, and 12 𝜇m, respectively). The AGN selection wedge defined by Mateos et al. (2012) is shown by the black solid line where sources within this region are classified as AGN, while sources outside the wedge are expected to not host an AGN, suggesting mid-IR emission that is dominated by star-formation activity. The top and ri… view at source ↗
Figure 4
Figure 4. Figure 4: Venn diagram showing the distribution of our LLAGN detected across X-ray, optical and IR wavelengths. The numbers indicate the amount of source detected in individual wavebands and their overlaps, with five sources detected in all bands and three sources remain undetected at any of those wavelengths. Each subset is annotated with its average AGN and host galaxy properties (e.g., bolometric luminosity, Eddi… view at source ↗
Figure 5
Figure 5. Figure 5: Distributions of AGN properties for our LLAGN sample (grey) compared with the Swift–BAT AGN (blue; Koss et al. 2017) and an additional LLAGN sample from Ho 2009 (red). Panels show bolometric luminosity (a), black hole mass (b), and Eddington ratio (c). and a p-value of 7.8×10−59, confirming that the two samples occupy different luminosity regimes. We further compared our LLAGN sample with the local LLAGN p… view at source ↗
Figure 6
Figure 6. Figure 6: Distributions of host galaxy properties for our LLAGN sample (grey) compared with the Swift–BAT AGN sample (blue; Shimizu et al. 2017; Koss et al. 2011; Kim et al. 2021) and an additional LLAGN sample from Ho 2009 (red). Panels show stellar rate (a), star formation rate (b), and host galaxy Hubble type (c). (𝐷 = 0.343, 𝑝 = 0.01). While the two samples partially overlap, our LLAGN extend toward lower host m… view at source ↗
Figure 7
Figure 7. Figure 7: BPT diagram of log( [O iii]/H𝛽) vs. log( [S ii]/H𝛼). The solid curve (Kewley et al.(2006)) marks the AGN–star formation division (assumed 50% AGN), while dashed curves trace mixing from pure star formation (0%) to pure AGN (100%). The AGN fraction is estimated from a galaxy’s position along this sequence. compare our results with LLAGN population from Ho (2009), which exhibits a mean of ⟨log(SFR/𝑀⊙ yr−1 )⟩… view at source ↗
read the original abstract

Low-luminosity active galactic nuclei (LLAGN; $L_{\rm bol} < 10^{42}$~erg~s$^{-1}$) may comprise a significant fraction of the local AGN population, yet their weak emission makes them difficult to detect. In this paper, we analyse 38 LLAGN identified from a 15~GHz sub-arcsecond Very Large Array survey and assess the effectiveness of X-ray, optical, and infrared wavelengths in identifying LLAGN. We found that optical emission-line diagnostics recovered $84.2^{+15.8}_{-22.9}$\% (32/38) of the sample, X-rays detected $63.2^{+25.7}_{-19.6}$\% (24/38), and infrared methods only identified $13.2^{+14.5}_{-8.0}$\% (5/38), reflecting limited X-ray sensitivity, weak or absent optical lines, and strong host galaxy contamination in the infrared. Compared to \textit{Swift}--BAT AGN, our LLAGN are $\sim$ 4.1~dex fainter in bolometric luminosity (log $L_{\mathrm{bol}} \approx$ 39.3 - 41.9 erg s$^{-1}$), host smaller black holes ($\sim$0.7~dex lower), and accrete at much lower rates (log $\lambda_{\text{Edd}} \approx$ -6.5 to -1.3, i.e., $\sim$ 4.2~dex lower). Host galaxies span a broad range of morphologies, from disk- to bulge-dominated, with a subset exhibiting prominent bulges, potentially representing systems where nuclear activity has faded while the bulge remains dominant. LLAGN also reside in galaxies with lower stellar masses ($\sim$0.3~dex) and suppressed star formation rates ($\sim$0.5~dex) relative to \textit{Swift}--BAT AGN. Overall, LLAGN in our sample systematically host smaller and weakly accreting black holes, residing in galaxies with diverse morphologies, but lower stellar masses and reduced star formation activity, demonstrating the connection between low-level black hole accretion and host galaxy properties in the local Universe.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

1 major / 0 minor

Summary. The manuscript analyzes 38 low-luminosity AGN (LLAGN) selected from a 15 GHz sub-arcsecond VLA survey. It reports multi-wavelength recovery rates using optical emission-line diagnostics (84.2^{+15.8}_{-22.9}% or 32/38), X-rays (63.2^{+25.7}_{-19.6}% or 24/38), and infrared methods (13.2^{+14.5}_{-8.0}% or 5/38). The LLAGN sample is compared to Swift-BAT AGN, showing ~4.1 dex fainter bolometric luminosities (log L_bol ≈ 39.3–41.9 erg s^{-1}), ~0.7 dex smaller black holes, ~4.2 dex lower Eddington ratios (log λ_Edd ≈ -6.5 to -1.3), ~0.3 dex lower stellar masses, and ~0.5 dex suppressed star formation rates, with host galaxies spanning diverse morphologies from disk- to bulge-dominated.

Significance. If the radio-selected sources are confirmed as genuine nuclear accretors, the work supplies concrete empirical evidence for systematic differences between LLAGN and higher-luminosity AGN, including quantified dex offsets in black-hole mass, accretion rate, stellar mass, and SFR. The asymmetric uncertainties on detection fractions and the parameter-free nature of the direct observational comparisons strengthen the assessment of multi-wavelength identification effectiveness and the link between low-level accretion and host-galaxy properties in the local Universe.

major comments (1)
  1. Abstract: The reported 0.7 dex offset in black-hole mass, 4.2 dex offset in Eddington ratio, and 0.3–0.5 dex offsets in stellar mass and SFR relative to Swift-BAT AGN rest on the assumption that the 15 GHz radio emission in all 38 sources traces nuclear accretion. The abstract notes strong host-galaxy contamination in the infrared and only 13% recovery there, yet provides no quantitative test (radio spectral index, compactness, radio-to-FIR ratio, or variability) to place an upper limit on star-formation contributions to the 15 GHz flux. If even 20–30% of the sample is dominated by host processes, the claimed systematic connection between low-level accretion and host properties becomes unreliable.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their constructive and detailed review of our manuscript. We have addressed the major comment concerning the assumption that the 15 GHz radio emission traces nuclear accretion by clarifying the role of sub-arcsecond resolution in the selection and by adding supporting discussion. We believe these changes strengthen the presentation without altering the core conclusions.

read point-by-point responses

  1. Referee: Abstract: The reported 0.7 dex offset in black-hole mass, 4.2 dex offset in Eddington ratio, and 0.3–0.5 dex offsets in stellar mass and SFR relative to Swift-BAT AGN rest on the assumption that the 15 GHz radio emission in all 38 sources traces nuclear accretion. The abstract notes strong host-galaxy contamination in the infrared and only 13% recovery there, yet provides no quantitative test (radio spectral index, compactness, radio-to-FIR ratio, or variability) to place an upper limit on star-formation contributions to the 15 GHz flux. If even 20–30% of the sample is dominated by host processes, the claimed systematic connection between low-level accretion and host properties becomes unreliable.

    Authors: We appreciate this important caveat. The sample is drawn from a 15 GHz VLA survey that explicitly uses sub-arcsecond resolution to isolate compact radio cores, which are a hallmark of nuclear AGN activity rather than the extended emission typical of star formation; this selection strategy is described in Section 2 of the manuscript. The low infrared recovery rate (13%) is consistent with the weak mid-IR emission expected from low-accretion-rate LLAGN and does not imply SF dominance in the radio. To directly address the request for quantitative tests, we have added a new paragraph in the revised discussion that applies the radio-to-FIR correlation for star-forming galaxies to place an upper limit on possible SF contributions, finding that SF is unlikely to account for the observed 15 GHz flux in the large majority of sources. We have also updated the abstract to state that the radio sources are selected on the basis of compact emission indicative of nuclear accretion. While we lack multi-frequency or multi-epoch data for spectral-index or variability analysis across the full sample, the combination of high-resolution selection, optical (84%) and X-ray (63%) confirmation rates, and the new radio-to-FIR estimate supports the nuclear interpretation for the bulk of the sample. Even allowing for modest (20–30%) contamination, the reported dex offsets remain robust as they are driven by the confirmed AGN subset. revision: partial

Circularity Check

0 steps flagged

No circularity in empirical LLAGN sample comparison

full rationale

The paper is an observational analysis of 38 radio-selected LLAGN sources, reporting recovery rates across wavelengths and direct statistical offsets in measured quantities (bolometric luminosity, black-hole mass, Eddington ratio, stellar mass, SFR) relative to an independent Swift-BAT comparison sample. No equations, fitted parameters, or derivations are present that reduce any reported result to its own inputs by construction. All claims rest on independently measured observables from separate surveys; the analysis is therefore self-contained with no self-definitional, fitted-input, or self-citation load-bearing steps.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

Claims rest on standard AGN classification diagnostics and bolometric luminosity conversions from radio, X-ray, optical, and IR data; no new free parameters or invented entities are introduced.

axioms (2)
  • domain assumption Radio emission at 15 GHz with sub-arcsecond resolution reliably traces low-level nuclear accretion in these galaxies.
    This underpins the initial sample selection and all subsequent multiwavelength comparisons.
  • domain assumption Black hole masses and Eddington ratios derived from available multiwavelength data are accurate enough for statistical comparison across samples.
    Used to report the ~0.7 dex and ~4.2 dex differences.

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