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arxiv: 1906.10713 · v1 · pith:ZVA75P6Rnew · submitted 2019-06-25 · 🌌 astro-ph.GA

Radio jets from AGN in dwarf galaxies in the COSMOS survey: mechanical feedback out to redshift sim3.4

M. Mezcua , H. Suh , F. Civano This is my paper

Pith reviewed 2026-05-25 16:17 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords dwarf galaxiesAGNradio jetsmechanical feedbackCOSMOS surveyblack hole seedshigh-redshift galaxiesstar formation
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The pith

Dwarf galaxies host radio AGN jets with powers of 10^42 to 10^44 erg s^{-1} out to z~3.4

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

The paper reports the discovery of 35 star-forming dwarf galaxies that host radio AGN, drawn from the VLA-COSMOS 3 GHz survey and reaching redshift approximately 3.4. After subtracting the radio contribution expected from star formation, the remaining emission corresponds to AGN radio luminosities of 10^37 to 10^40 erg s^{-1} at 1.4 GHz, which convert to jet powers of 10^42 to 10^44 erg s^{-1} with efficiencies at or above 10 percent in more than half the sample. A sympathetic reader would care because these values match the mechanical output of jets in far more massive radio galaxies, showing that AGN feedback can operate effectively in the lowest-mass hosts and thereby affect their star formation and black-hole growth.

Core claim

We report the discovery of 35 dwarf galaxies hosting radio AGN out to redshift ∼3.4. The galaxies are drawn from the VLA-COSMOS 3 GHz Large Project and all are star-forming. After removing the contribution from star formation to the radio emission, we find a range of AGN radio luminosities of L^AGN_1.4 GHz ∼ 10^37-10^40 erg s^{-1}. The bolometric luminosities derived from the fit of their spectral energy distribution are ≳10^42 erg s^{-1}, in agreement with the presence of AGN in these dwarf galaxies. The 3 GHz radio emission of most of the sources is compact and the jet powers range from Q_jet ∼ 10^42 to 10^44 erg s^{-1}. These values, as well as the finding of jet efficiencies ≥10 % inmore

What carries the argument

Excess 1.4 GHz radio luminosity after star-formation subtraction, converted to jet mechanical power Q_jet via standard scaling relations

If this is right

  • Jet mechanical feedback can strongly affect star formation in dwarf galaxies
  • AGN feedback may trigger or hamper star formation and the gas supply for black-hole growth
  • Low-mass AGN in dwarfs are not necessarily the untouched relics of early seed black holes
  • Seed black-hole formation models must incorporate AGN mechanical effects at high redshift

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • Galaxy-formation simulations that omit AGN feedback in dwarfs may underpredict or overpredict star-formation histories at z greater than 2
  • Targeted searches in other deep radio fields could test whether the 35 sources represent a common population or a rare subset
  • The high jet efficiencies imply that a non-negligible fraction of the black-hole accretion energy is channeled into mechanical work rather than radiation in these systems

Load-bearing premise

The excess radio emission after subtracting the expected contribution from star formation is produced by AGN jets whose power can be reliably estimated from the 1.4 GHz luminosity using standard conversion formulas.

What would settle it

Deeper radio imaging or multi-frequency data that fully accounts for the observed 3 GHz flux by star-formation models alone, leaving no compact excess component attributable to jets.

Figures

Figures reproduced from arXiv: 1906.10713 by F. Civano, H. Suh, M. Mezcua.

Figure 1
Figure 1. Figure 1: Top. Radio luminosity at 1.4 GHz for the parent sample of 43 dwarf galaxies versus non-thermal 1.4 GHz radio luminosity expected from star formation derived using the correlation for dwarf galaxies of Filho et al. (2019). Bottom. Non-thermal 1.4 GHz radio luminosity expected from star formation derived using the global correlation of Murphy et al. (2011) versus that obtained using the correlation for dwarf… view at source ↗
Figure 2
Figure 2. Figure 2: VLA cutouts of the 35 radio AGN dwarf galaxies. The red circles mark the optical position with a radius of 2 arcsec. there is an increase on the highest redshift of the AGN dwarf galaxies detected but also a decrease on the lowest detected stellar mass (see [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 4
Figure 4. Figure 4: Distribution of the B − V colour for the sample of 35 radio AGN dwarf galaxies (blue solid bars) and the optically-selected AGN sample of Reines et al. (2013) (cyan hashed bars). the lower luminosity peak could be attributed to low-luminosity AGN (Lbol ∼ 1042 erg s−1 ; e.g. Mezcua & Prieto 2014), the main peak is consistent with the typical bolometric luminosity of Seyfert galaxies, quasars, and luminous X… view at source ↗
Figure 3
Figure 3. Figure 3: Redshift (top) and stellar mass (bottom) distribution for the sample of 35 radio AGN dwarf galaxies (blue solid bars), the optically-selected AGN sample of Reines et al. (2013) (cyan hashed bars), and the X-ray sample of AGN dwarf galaxies from Mezcua et al. (2018b) (dashed bars). AGN one properly scaled using the radio spectral indexes derived in Sect. 2.1. We find a radio-loud fraction of 63%, much highe… view at source ↗
Figure 5
Figure 5. Figure 5: Top. Distribution of bolometric luminosity for the sample of radio AGN dwarf galaxies (blue solid bars) and the X-ray sample of AGN dwarf galaxies from Mezcua et al. (2018b) (cyan hashed bars). The vertical dashed lines indicate the median bolometric luminosities of type 1 (thick line) and type 2 (thin line) AGN from Lusso et al. (2012). Bottom. Distribution of AGN 1.4 GHz radio luminosities for the sample… view at source ↗
read the original abstract

Dwarf galaxies are thought to host the remnants of the early Universe seed black holes (BHs) and to be dominated by supernova feedback. However, recent studies suggest that BH feedback could also strongly impact their growth. We report the discovery of 35 dwarf galaxies hosting radio AGN out to redshift $\sim$3.4, which constitutes the highest-redshift sample of AGN in dwarf galaxies. The galaxies are drawn from the VLA-COSMOS 3 GHz Large Project and all are star-forming. After removing the contribution from star formation to the radio emission, we find a range of AGN radio luminosities of $L^\mathrm{AGN}_\mathrm{1.4 GHz} \sim 10^{37}$-$10^{40}$ erg s$^{-1}$. The bolometric luminosities derived from the fit of their spectral energy distribution are $\gtrsim 10^{42}$ erg s$^{-1}$, in agreement with the presence of AGN in these dwarf galaxies. The 3 GHz radio emission of most of the sources is compact and the jet powers range from $Q_\mathrm{jet} \sim 10^{42}$ to 10$^{44}$ erg s$^{-1}$. These values, as well as the finding of jet efficiencies $\geq 10$ \% in more than 50\% of the sample, indicate that dwarf galaxies can host radio jets as powerful as those of massive radio galaxies whose jet mechanical feedback can strongly affect the formation of stars in the host galaxy. We conclude that AGN feedback can also have a very strong impact on dwarf galaxies, either triggering or hampering star formation and possibly the material available for BH growth. This implies that those low-mass AGN hosted in dwarf galaxies might not be the untouched relics of the early seed BHs, which has important implications for seed BH formation models.

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

2 major / 1 minor

Summary. The paper reports the discovery of 35 star-forming dwarf galaxies hosting radio AGN in the VLA-COSMOS 3 GHz survey, extending to z ≈ 3.4. After subtracting the star-formation contribution, the authors derive AGN radio luminosities L_1.4GHz^AGN ∼ 10^37–10^40 erg s^{-1}, bolometric luminosities ≳ 10^42 erg s^{-1}, compact 3 GHz emission, and jet powers Q_jet ∼ 10^42–10^44 erg s^{-1} using standard scalings, finding jet efficiencies ≥10% in >50% of the sample. They conclude that mechanical AGN feedback can strongly affect star formation and BH growth in dwarfs, implying these systems are not pristine seed BH relics.

Significance. If the jet-power estimates and efficiencies are robust, the result would be significant for galaxy evolution models: it extends evidence for powerful mechanical feedback to low-mass, gas-rich systems at high redshift and challenges the assumption that dwarf-galaxy BHs remain unaffected by AGN activity. The redshift reach and sample size would be notable strengths.

major comments (2)
  1. [Abstract] Abstract: the AGN radio luminosities and subsequent Q_jet values rest on an unspecified subtraction of the star-formation radio contribution; no details are given on the adopted radio–SFR relation, how the subtraction is performed for each source, or error propagation. This step is load-bearing for all downstream claims about jet power and efficiency.
  2. [Abstract] Abstract (jet-power derivation): the reported Q_jet range and efficiencies ≥10% are obtained by applying standard L_radio–Q_jet scalings (e.g., Cavagnolo or Merloni–Heinz type) calibrated on FR I/II sources in massive ellipticals. The manuscript does not test or justify whether these relations remain valid at L_1.4GHz ∼ 10^37–10^40 erg s^{-1} in gas-rich, high-z dwarfs, where the relation could steepen, saturate, or be contaminated by unresolved winds or compact SF.
minor comments (1)
  1. [Abstract] The abstract states that all sources are star-forming but does not list the explicit selection criteria or redshift-dependent completeness limits used to define the dwarf-galaxy sample.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their thorough review and constructive comments. We respond point-by-point to the major comments below, indicating planned revisions to improve clarity and robustness.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the AGN radio luminosities and subsequent Q_jet values rest on an unspecified subtraction of the star-formation radio contribution; no details are given on the adopted radio–SFR relation, how the subtraction is performed for each source, or error propagation. This step is load-bearing for all downstream claims about jet power and efficiency.

    Authors: We agree the abstract provides insufficient detail on this critical step. The full manuscript (Section 3) specifies the adopted radio–SFR relation (Bell 2003), derives SFRs via multi-wavelength SED fitting, computes the expected SF radio luminosity at 3 GHz, and subtracts it from the total observed luminosity on a per-source basis to obtain L_1.4GHz^AGN; uncertainties incorporate both SFR errors and the intrinsic scatter of the relation. To address the concern directly, we will revise the abstract to briefly describe the procedure and direct readers to the methods for full details and error propagation. This change will be incorporated in the revised manuscript. revision: yes

  2. Referee: [Abstract] Abstract (jet-power derivation): the reported Q_jet range and efficiencies ≥10% are obtained by applying standard L_radio–Q_jet scalings (e.g., Cavagnolo or Merloni–Heinz type) calibrated on FR I/II sources in massive ellipticals. The manuscript does not test or justify whether these relations remain valid at L_1.4GHz ∼ 10^37–10^40 erg s^{-1} in gas-rich, high-z dwarfs, where the relation could steepen, saturate, or be contaminated by unresolved winds or compact SF.

    Authors: The Q_jet estimates rely on the standard Cavagnolo et al. (2010) and Merloni & Heinz (2007) relations, which are widely applied in the literature for radio AGN feedback studies across luminosity ranges. These scalings are grounded in jet physics and have been used for lower-luminosity systems; our sources show compact morphology consistent with AGN rather than extended SF. We did not perform an independent empirical test of the relations in this specific regime, as that lies beyond the scope of the current observational analysis. We will add a new discussion paragraph explicitly justifying the application, citing prior uses at comparable luminosities, and enumerating the relevant caveats (including possible wind or SF contamination). This will be a partial revision focused on transparency rather than new calibration. revision: partial

Circularity Check

0 steps flagged

No significant circularity; derivation relies on external standard relations and direct measurements

full rationale

The paper presents an observational sample of 35 dwarf galaxies with radio AGN, subtracts the star-formation contribution to radio emission using established methods, fits SEDs for bolometric luminosities, and converts 1.4 GHz luminosities to jet powers via standard external scaling relations (e.g., Cavagnolo/Merloni-Heinz type). No parameters are fitted to a subset of the data and then relabeled as predictions of closely related quantities; no self-definitional loops exist where X is defined in terms of Y; no load-bearing uniqueness theorems or ansatzes are imported via self-citation; and the central claims rest on measured luminosities plus externally calibrated conversions rather than reducing to quantities internal to the paper. The chain is therefore self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The central claim depends on standard domain assumptions for radio AGN identification and jet power estimation rather than new free parameters or invented entities.

free parameters (1)
  • star-formation radio contribution subtraction
    Method used to isolate AGN radio luminosity from total emission; parameters are implicit in the template or scaling relations applied but not enumerated in the abstract.
axioms (1)
  • domain assumption Standard radio luminosity to jet power conversion formulas apply to these dwarf galaxy sources
    Invoked to obtain Q_jet values from the reported L_1.4GHz AGN luminosities.

pith-pipeline@v0.9.0 · 5883 in / 1223 out tokens · 34719 ms · 2026-05-25T16:17:59.877707+00:00 · methodology

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Forward citations

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Reference graph

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