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The Compton-thick AGN Population and the $N_{\rm H}$ Distribution of Low-mass AGN in our Cosmic Backyard

T0 review · 3 major / 6 minor · reviewed 2026-08-07 · deepseek-v4-flash

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Pith's one-line read The paper directly measures a 32% Compton-thick fraction among AGN within 15 Mpc and finds the column density distribution matches the intrinsic Swift-BAT distribution, indicating hard X-ray surveys miss most of the most obscured AGN.

desk verdict A careful, genuinely new direct measurement of the local Compton-thick fraction, though the sample selection means the result applies to IR-bright [Ne V]-selected AGN rather than the full local AGN population. read the letter →

arxiv 2506.08527 v1 pith:GVGN4DSG submitted 2025-06-10 astro-ph.GA astro-ph.HE

A. Annuar , D. M. Alexander , P. Gandhi , G. B. Lansbury , M. N. Rosli , D. Stern , D. Asmus , D. R. Ballantyne
show 16 more authors
M. Baloković F. E. Bauer P. G. Boorman W.N. Brandt M. Brightman C.T.J. Chen A. Del Moro D. Farrah F. A. Harrison M. J. Koss L. Lanz S. Marchesi P. Mohanadas E. Nardini C. Ricci L. Zappacosta
This is my paper · ORCID
classification astro-ph.GAastro-ph.HE
keywords Compton-thickAGNcensuscolumndensitydistributionmid-infraredselectionlocaluniverselow-luminositySwift-BATX-rayspectroscopy
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

The paper sets out to count how many active galactic nuclei (AGN) in the local universe are Compton-thick, meaning hidden behind gas so dense that even hard X-rays are absorbed. Using a volume-limited, mid-infrared-selected sample of 19 AGN within 15 Mpc, the authors measure line-of-sight column densities from broadband X-ray spectra and find that 32% of the sample is Compton-thick. This fraction is far higher than the roughly 8% directly detected by the Swift-BAT hard X-ray survey, but it agrees with the intrinsic fraction that survey infers after correcting for its sensitivity limits. The result matters because it suggests that the most heavily obscured AGN, key contributors to the cosmic X-ray background, are not absent locally but are simply missed by flux-limited hard X-ray surveys.

What carries the argument

The central object is the volume-limited sample itself: 19 AGN within 15 Mpc selected by [Ne V] detection in Spitzer IRS spectra, chosen because the line's high ionization potential (97.1 eV) makes it a near-unambiguous AGN signature that is not extinguished by the torus or by host-galaxy dust. The column densities are then measured directly by fitting broadband Chandra and NuSTAR X-ray spectra with physically motivated torus models (MYtorus and Borus). The 15 Mpc volume limit makes the sample a near-complete census of AGN in the local volume, allowing direct counts of the Compton-thick population without relying on flux-based corrections.

What would settle it

A targeted mid-infrared spectroscopic survey of every IRAS RBGS galaxy within 15 Mpc that currently lacks a [Ne V] detection, focusing on warm-color silicate-absorption sources like NGC 4418; if such a survey uncovers previously missed AGN in numbers comparable to the current sample, the measured 32% Compton-thick fraction would be an underestimate rather than a true census.

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Extended reading notes

Core claim

Within 15 Mpc, the authors identify 19 AGN through the high-ionization [Ne V] \(\$\lambda$ 14.3\,\mu\text{m}\) line, a selection that is largely insensitive to both host-galaxy dust and torus obscuration. From Chandra and NuSTAR broadband spectra fitted with torus models, they establish that 14/19 (74%) of the AGN are obscured and 6/19 (32%) are Compton-thick with \(N_{\rm H} \gtrsim 1.5\$times10^{{24}}$\,\text{cm}^{-2}\). The measured \(N_{\rm H}\) distribution is consistent with the intrinsic distribution that the Swift-BAT survey infers after de-biasing, and it is inconsistent with the observed Swift-BAT distribution. In the low-luminosity regime \(L_{\rm 2-10,int}\$le10^{{42}}$\,\text{erg}\,\text{s}^{-1}\), the Compton-thick fraction is 19% (3/16), consistent with higher-luminosity samples, while all sources with \(L_{\rm 2-10,int}<$10^{{40}}$\,\text{erg}\,\text{s}^{-1}\) are unobscured or mildly obscured, suggesting the torus may be underdeveloped at very low accretion power.

Load-bearing premise

The sample is assumed to be a near-complete census of AGN within 15 Mpc, which requires that the [Ne V] line selects every active nucleus; an extremely buried nucleus, such as the compact obscured nucleus NGC 4418, could hide an AGN even from this mid-infrared line.

Editorial extensions

If this is right

  • The intrinsic Compton-thick fraction in the local universe is about one-third, so hard X-ray surveys such as Swift-BAT directly detect only a small part of the true obscured AGN population.
  • The \(N_{\rm H}\) distribution of local AGN matches the intrinsic Swift-BAT distribution, implying that the observed deficit of Compton-thick AGN is a sensitivity bias rather than a real absence.
  • Low-luminosity AGN with \(L_{\rm 2-10,int}\le10^{42}\,\text{erg}\,\text{s}^{-1}\) host a Compton-thick fraction consistent with brighter AGN, so obscuration does not drop abruptly at low luminosity.
  • AGN with \(L_{\rm 2-10,int}<10^{40}\,\text{erg}\,\text{s}^{-1}\) are all unobscured or mildly obscured, suggesting the torus is underdeveloped or absent at very low accretion rates.
  • The sample reaches black hole masses of roughly \(10^6\,M_\odot\), about 1.5 dex lower than Swift-BAT, opening the local census to low-mass black holes.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • The paper leaves implicit that the near-completeness claim, if accepted, implies the local universe hosts roughly four times more heavily obscured accretion than Swift-BAT directly traces; an independent check would be a blind high-resolution mid-IR survey of the same 15 Mpc volume rather than an IRAS-selected parent sample.
  • The sharp luminosity threshold at \(10^{40}\,\text{erg}\,\text{s}^{-1}\), below which no Compton-thick AGN appears, predicts that a larger volume-limited sample should show the Compton-thick fraction rising with luminosity, a trend that would support the receding-torus or disk-wind picture of AGN unification.
  • Because [Ne V] selection can miss compact obscured nuclei such as NGC 4418, the true local Compton-thick fraction could be even higher than 32%; deep silicate-absorption-selected follow-up of the parent galaxies would quantify this.
  • The method of mid-IR line selection plus NuSTAR broadband follow-up could be pushed to 30–50 Mpc with a next-generation high-energy X-ray mission, turning the local census into a three-dimensional map of obscuration as a function of luminosity and black hole mass.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

3 major / 6 minor

Summary. The paper presents a census of the Compton-thick (CT) AGN population and the column-density (NH) distribution for 19 mid-infrared-selected AGN within 15 Mpc, drawn from the GA09 parent sample of IRAS RBGS galaxies with f60 > 5.24 Jy and LIR > 3×10^9 Lsun that show [Ne V] emission. NH values and intrinsic 2–10 keV luminosities are measured from broadband X-ray spectroscopy with Chandra, XMM-Newton, NuSTAR, and Swift-BAT, using physically motivated torus models (MYtorus, Borus); six sources are analyzed or re-analyzed here. The authors report 6/19 (32+30/−18%) CT AGN, an NH distribution that agrees with the Swift-BAT inferred intrinsic NH distribution, a CT fraction of 3/16 (19+30/−14%) for low-luminosity AGN (L2−10,int ≤ 10^42 erg/s), and comparisons of black hole mass, stellar mass, star formation rate, and optical classification with the Swift-BAT AGN sample.

Significance. If the sample is representative of the local AGN population, this is the first direct CT census extending to intrinsic luminosities of ~10^37–10^43 erg/s, a regime inaccessible to hard X-ray surveys. The measured 32% CT fraction, compared with the ~8% directly observed by Swift-BAT and the ~27% intrinsic fraction inferred by Ricci et al. (2015), provides direct observational support for the view that hard X-ray surveys miss a substantial CT population due to sensitivity bias. The low-luminosity CT fraction and the host-galaxy comparisons probe new parameter space for low-mass AGN. Strengths of the paper include the newly obtained coordinated NuSTAR/Chandra/XMM-Newton observations (Table 2), the complete X-ray coverage (100% Chandra, 89% NuSTAR), the uniform re-analysis with torus models, and the transparent tabulation of NH values, their uncertainties, and literature sources. The principal risks are the small sample size and the dependence of the results on the IR-bright, [Ne V]-selected parent sample.

major comments (3)
  1. [§2.1 (Sample Completeness); abstract; §8 conclusions] The completeness argument in §2.1 establishes that GA09 did not demonstrably miss AGN within their IRAS/RBGS parent galaxy sample (f60 > 5.24 Jy, LIR > 3×10^9 Lsun, |b| > 5°), but it does not establish that the 19-object sample is a complete census of AGN within 15 Mpc. The paper itself names three known Swift-BAT AGN inside 15 Mpc that are excluded by these criteria (M81, NGC 4395, and M106), and the NGC 4418 case—used as the template for buried, [Ne V]-undetected nuclei—lies outside the volume at 31.9 Mpc. Because the headline claims (a 32% CT fraction and an NH distribution matching the Swift-BAT intrinsic distribution) are phrased for the local AGN population, the paper should quantify the sensitivity of these claims to the known exclusions and to a possible population of heavily buried non-[Ne V] nuclei. Merely adding the three known excluded AGN to the census would change the denominator from 19 to 22 and shift the central CT fraction from 32% to 27% if none of them is CT, a shift comparable to the quoted statistical uncertainty; the paper should state the direction and magnitude of this systematic effect, or explicitly condition the results on the IR-bright, mid-IR-selected parent population.
  2. [§6 and Table 3 (NGC 660 and NGC 1792)] The central 32% value is set against a single borderline object. NGC 660 is excluded from the CT count even though its NH is a lower limit (log NH = 23.78 in Table 3, from Annuar et al. 2020) with, per the table note, 'strong evidence for CT obscuration'; the same data support 7/19 (37%). Conversely, NGC 1792 is placed in the mildly obscured bin from an upper limit (log NH ≤ 22.39) although its AGN is undetected in both Chandra and NuSTAR, and the text acknowledges the nucleus could be extremely CT. The abstract should either quote the alternative count (7/19, 37%) or explicitly justify the adopted threshold (i.e., requiring NH ≥ 1.5×10^24 cm−2 while treating lower limits as non-CT detections); as written, the single headline number conceals a sensitivity that the body of the paper handles much more transparently.
  3. [§6 and Figure 13] The agreement between the sample NH distribution and the Swift-BAT intrinsic NH distribution is asserted from a visual comparison in Figure 13 without a quantitative measure. Given that this agreement is one of the two headline results in the abstract, the paper should either provide a statistical statement (for example, the 90% binomial interval on the 6/19 CT fraction against the BAT intrinsic fraction, which the text gives only in passing) or explicitly label the NH-distribution comparison as qualitative; the current wording 'agrees very well' is stronger than the evidence presented for a sample of 19 objects with several upper limits.
minor comments (6)
  1. [Abstract] The sentence 'the majority of our galaxy have lower stellar masses' should read 'the majority of our galaxies have lower stellar masses'.
  2. [Throughout] There are numerous missing spaces in citations (e.g., 'Gillietal.2007' in §1) and grammar slips such as 'NGC 3627 is a a spiral galaxy' in §4.4; these should be corrected in the final version.
  3. [§4.2 and Table 2] The text quotes the NuSTAR exposure for NGC 1792 as 22.9 ks, while Table 2 lists 45.7 ks as the total; please state in the text that the quoted figure is the combined two-FPM value or clarify the convention.
  4. [§4.2 and Figure 13] The treatment of NGC 1792's NH upper limit as a definite placement in the NH distribution histogram (mildly obscured bin) should be stated explicitly in the text or figure caption, since the source is undetected in both Chandra and NuSTAR.
  5. [§6] The phrase 'at a smaller distance of 20 Mpc' would be clearer as 'within 20 Mpc' when referring to the Ricci et al. (2015) distance-limited CT fraction.
  6. [Figure 13 caption] The yellow/blue color key for the two samples is described only in the caption; adding explicit labels directly on the histogram bars would improve readability.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the CT fraction is a direct count from X-ray spectral fits and the NH-distribution comparison is against an independent external survey.

full rationale

The paper's central claim (32+30/-18% CT fraction) is a direct observational count: 6/19 sources are classified as Compton-thick from NH values in Table 3, obtained from broadband X-ray spectral fitting, not from a model fitted to the aggregate fraction. The NH-distribution comparison is made against the Swift-BAT sample of Ricci et al. (2015), an independent external survey with its own sensitivity corrections, so the agreement is not imposed by construction. The sample-completeness argument in Section 2.1 is based on external checks (Swift-BAT detections, IRAS f60/f25 ratios, silicate absorption) and explicitly identifies excluded AGN (M81, NGC 4395, M106), so the 'near complete' claim is a stated assumption or limitation rather than a circular redefinition. Self-citations to Annuar et al. (2015, 2017, 2020) provide five NH measurements from earlier published work; these are independent measurements of individual sources and are not fitted parameters of the present census, and six other sources are re-analysed in this work. No fitted input is renamed as a prediction, and no load-bearing step reduces to its own input by construction.

Assumptions & free parameters 0 free parameters · 4 assumptions · 0 invented entities

The central claim rests on the N_H measurements from X-ray spectral fits, which are standard and published for most sources. No ad hoc fitted constants are introduced; the main assumptions are the completeness of the [Ne V] selection, the parent IRAS sample with an IR luminosity cut, and the fidelity of the spectral models and fixed parameters used for low-quality data. These are reasonable but not fully demonstrated.

assumptions (4)
  • domain assumption The [Ne V] 14.3 micron line is an unambiguous AGN indicator in this sample; alternative origins (Wolf-Rayet stars, fast shocks) are not responsible.
    This is the foundation of the GA09 AGN selection; Section 2 argues against alternatives but does not fully exclude them for each source.
  • domain assumption The parent sample (IRAS RBGS with L_IR > 3e9 L_sun) and the [Ne V] detection yield a near-complete AGN census within 15 Mpc, with no missed AGN due to extreme obscuration or the IR luminosity cut.
    Section 2.1 argues completeness using IR colors and the NGC 4418 case, but this is not a rigorous completeness test; low-IR-luminosity galaxies with AGN (e.g., NGC 4395) are excluded.
  • domain assumption The X-ray spectral models (MYtorus, Borus, absorbed power-law) and fixed parameters (photon index 1.8, solar abundances, cross-calibration constants) produce unbiased N_H measurements.
    Used throughout Section 4; for several sources with weak data, parameters are fixed to typical values, and the true photon index may differ, which can affect N_H.
  • domain assumption Literature black hole masses and bolometric corrections are reliable for the Eddington ratio analysis.
    Section 7.1 adopts M_BH from various methods (maser, velocity dispersion, bulge luminosity) and bolometric corrections from Elvis et al. (1994), Vasudevan et al. (2010), and Nemmen et al. (2014); systematic differences between methods could bias the comparison.

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Pith. "Pith review of The Compton-thick AGN Population and the $N_{\rm H}$ Distribution of Low-mass AGN in our Cosmic Backyard." pith.science (2026). https://pith.science/paper/GVGN4DSG

@misc{pith2026250608527,
  author       = {Pith},
  title        = {Pith review of: The Compton-thick AGN Population and the $N_\rm H$ Distribution of Low-mass AGN in our Cosmic Backyard},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/GVGN4DSG}},
  note         = {Machine review of arXiv:2506.08527}
}
abstract

We present a census of the Compton-thick (CT) active galactic nucleus (AGN) population and the column density ($N_{\rm{H}}$) distribution of AGN in our cosmic backyard using a mid-infrared selected AGN sample within 15 Mpc. The column densities are measured from broadband X-ray spectral analysis, mainly using data from $\textit{Chandra}$ and $\textit{NuSTAR}$. Our sample probes AGN with intrinsic 2-10 keV luminosities of $L_{\rm 2-10, int} = 10^{37}$-$10^{43}$ erg s$^{-1}$, reaching a parameter space inaccessible to more distant samples. We directly measure a 32$^{+30}_{-18}\%$ CT AGN fraction and obtain an $N_{\rm{H}}$ distribution that agrees with that inferred by the $\textit{Swift}$-BAT survey. Restricting the sample to the largely unexplored domain of low-luminosity AGN with $L_{\rm 2-10, int}$ $\leq$ $10^{42}$ erg s$^{-1}$, we found a CT fraction of 19$^{+30}_{-14}\%$, consistent with those observed at higher luminosities. Comparing the host-galaxy properties between the two samples, we find consistent star formation rates, though the majority of our galaxy have lower stellar masses (by $\approx 0.3$ dex). In contrast, the two samples have very different black hole mass ($M_{\rm BH}$) distributions, with our sample having $\approx$1.5 dex lower mean mass ($M_{\rm BH}$ $\sim$ 10$^{6}$ $M_\odot$). Additionally, our sample contains a significantly higher number of LINERs and H$_{\rm{II}}$-type nuclei. The Eddington ratio range probed by our sample, however, is the same as $\textit{Swift}$-BAT, although the latter dominates at higher accretion rates, and our sample is more evenly distributed. The majority of our sample with $\lambda_{\rm Edd} \ge$ 10$^{-3}$ tend to be CT, while those with $\lambda_{\rm Edd} <$ 10$^{-3}$ are mostly unobscured or mildly obscured.

Figures

Figures reproduced from arXiv: 2506.08527 by the authors.

Figure 1
Figure 1. Top: Distribution of IRAS 𝑓60𝜇m/ 𝑓25𝜇m ratio for the galaxies in GA09 (grey), our AGN sample (black solid line), and NGC 4418 (red). The pink shaded region marks a flux ratio of ≤ 5, indicating an AGN-dominated SED. Bottom: IRAS 𝑓60𝜇m/ 𝑓25𝜇m versus 9.8𝜇𝑚 silicate strength for GA09 galaxies (circles), our AGN sample (triangles), and NGC 4418 (star); silicate and 6.2𝜇𝑚 PAH equivalent-width measurements are taken from … view at source ↗
Figure 2
Figure 2. [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Top: Chandra RGB images of NGC 613 (Red: 0.5–1 keV, Green: 1–2 keV, Blue: 2–8 keV). The image is smoothed with a Gaussian function of radius 3 pixels, corresponding to 1.5′′ . Bottom: Best-fitting absorbed power-law model (top left), MYtorus (top right) and Borus (bottom) models to the spectra. The top panels show the data and unfolded model in 𝐸 2𝐹𝐸 units, whilst the bottom panels show the ratio between the data an… view at source ↗
Figures from the paper (13 more)
Figure 4
Figure 4. Figure 4: Top: Chandra and NuSTAR RGB images of NGC 1792 (Chandra - Red: 0.5–1 keV, Green: 1–2 keV, Blue: 2–8 keV; NuSTAR - Red: 3–8 keV, Green: 8–24 keV, Blue: 24–79 keV). The off-nuclear sources detected within the 20′′-radius extraction region in Chandra are labelled ON 1, ON…
Figure 5
Figure 5. Figure 5: Top: Chandra, XMM-Newton and NuSTAR RGB images of NGC 3621 (Chandra - Red: 0.5–1 keV, Green: 1–2 keV, Blue: 2–8 keV; XMM-Newton - Red: 0.5–1 keV, Green: 1–2 keV, Blue: 2–10 keV; NuSTAR - Red: 3–8 keV, Green: 8–24 keV, Blue: 24–79 keV). The off-nuclear sources which are…
Figure 6
Figure 6. Figure 6: Top: Chandra and NuSTAR RGB images of NGC 3627. Bottom: Best-fitting absorbed power-law (top left), MYtorus (top right) and Borus (bottom) models to the combined NuSTAR (red) and Chandra (black) data. Figure description is the same as [PITH_FULL_IMAGE:figures/full_fig…
Figure 7
Figure 7. Figure 7: Top: Chandra and NuSTAR RGB images of NGC 3628. The off-nuclear sources which were detected significantly detected within the 20′′-radius extraction region in Chandra are labelled as ON 1 and ON 2. Bottom: Best-fitting absorbed power-law model to the Chandra spectrum e…
Figure 8
Figure 8. Figure 8: Top: Chandra RGB image of NGC 4565. Bottom: Best-fitting absorbed power-law model to the data. Figure description is the same as [PITH_FULL_IMAGE:figures/full_fig_p012_8.png]
Figure 9
Figure 9. Figure 9: Intrinsic 2–10 keV luminosity vs. 𝑁H for our sample and the Swift￾BAT AGN at 𝐷 ≤ 100 Mpc.6 The dashed lines divide the low/high luminosity and obscured/unobscured AGN [PITH_FULL_IMAGE:figures/full_fig_p014_9.png]
Figure 10
Figure 10. Figure 10: Observed 2–10 keV flux vs. [O iii]λ5007Å flux corrected for the Balmer decrement plot for our sample. Red and blue circles marks Compton-thick and Compton-thin AGN on the basis of 𝑁H measurements from X-ray spectroscopy, respectively. The grey area indicates a region …
Figure 11
Figure 11. Figure 11: Observed 2–10 keV luminosities vs. 12𝜇m (left) and [Ne v] luminosities (right) for our sample. The solid lines for each plot correspond to the intrinsic relationships derived by Asmus et al. (2015) (scatter, 𝜎 ≈ 0.3 dex) and Weaver et al. (2010) (scatter, 𝜎 ≈ 0.5 dex)…
Figure 12
Figure 12. Figure 12: Top: CT AGN fraction as a function of distance for our sample (red) and the Swift-BAT AGN located within 100 Mpc (black). The grey region shows the range of the intrinsic CT AGN fraction inferred using the whole Swift-BAT AGN sample (i.e., over the entire range of X-r…
Figure 13
Figure 13. Figure 13: The 𝑁H distribution for our sample compared to the observed (left) and intrinsic (right) 𝑁H distributions of the Swift-BAT AGN sample with log 𝐿14−195 = 40.0–43.7 erg s−1 (Ricci et al. 2015). Yellow indicates those with 𝑁H measurements from other studies, whilst blue …
Figure 15
Figure 15. Figure 15: 𝑀∗ distributions for our sample (red) and the Swift-BAT sample (grey). 7.2 Host-Galaxy Properties In this section we compare the host-galaxy and optical AGN prop￾erties of our sample with those of the Swift-BAT AGN sample to investigate any potential differences betwe…
Figure 16
Figure 16. Figure 16: The distribution of Hubble type for our sample (red) and the Swift-BAT sample (grey; Kim et al. 2021) as compared to 𝑀∗. A reason for this could be due to the Swift-BAT sample having more bulge-dominated systems as compared to our sample (see [PITH_FULL_IMAGE:figures…
Figure 18
Figure 18. Figure 18: The distribution of optical nuclear classifications for our sample (red) and the Swift-BAT sample (grey). 7.2.3 Optical Type Finally, we compare the distribution of the optical classifications of the AGN in our sample with that of the Swift-BAT AGN sample (Oh et al. 2…

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Pith tools

Reviewed August 7, 2026 · model on record in the stance chip above.