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arxiv: 2606.01603 · v1 · pith:PK64B4HYnew · submitted 2026-06-01 · 🌌 astro-ph.GA

Signatures of Accreting Black Holes in Line Intensity Mapping

Erika Ogata , Kana Moriwaki , Adam Lidz , Rui Lan Jun , Naoki Yoshida This is my paper

Pith reviewed 2026-06-28 14:14 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords line intensity mappingaccreting black holesH alphaHe IIshot noisevoxel intensity distributioncosmic noonpower spectrum
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The pith

Accreting black holes supply 40-60% of Hα and 60-80% of He II line intensity around cosmic noon.

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

Line intensity mapping measures the collective glow from many galaxies in specific spectral lines to trace large-scale structure and star formation history. Earlier models attributed most of this glow in lines such as Hα to star-forming regions alone. The work adds the contribution from accreting black holes by post-processing a cosmological simulation that tracks both processes. The black-hole term proves comparable to or larger than the star-formation term in the average brightness and overwhelmingly controls the small-scale fluctuations. Because upcoming surveys will measure these quantities, the models used to interpret the data must include black-hole emission to avoid systematic error.

Core claim

Mock Hα and He II intensity maps built from the IllustrisTNG simulation that include both star-formation and black-hole accretion show that accreting black holes contribute 40-60 per cent of the mean Hα intensity and 60-80 per cent of the mean He II intensity near cosmic noon. Because black-hole-powered sources are rare yet luminous, they dominate the shot-noise term of the power spectrum and raise the small-scale clustering amplitude, most strongly for He II. The same maps indicate that a SPHEREx-like survey can reach the black-hole-influenced bright end of the Hα voxel intensity distribution at z ≲ 4 while a CDIM-like experiment can access the black-hole-dominated regime of He II.

What carries the argument

The sub-grid black-hole accretion model and the associated Hα and He II line-emission prescriptions applied to the IllustrisTNG simulation, which assign luminosities to both star-forming galaxies and accreting black holes.

If this is right

  • Black-hole emission supplies 40-60 per cent of the mean Hα intensity and 60-80 per cent of the mean He II intensity around cosmic noon.
  • Black-hole sources dominate the shot-noise component of the power spectrum for both lines.
  • Black-hole emission raises the small-scale clustering amplitude, especially for He II.
  • SPHEREx can measure the black-hole-influenced bright tail of the Hα voxel intensity distribution at redshifts below 4.
  • A CDIM-like experiment can reach the black-hole-dominated portion of the He II maps.

Where Pith is reading between the lines

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

  • Omitting black holes from LIM models would lead to overestimates of the cosmic star-formation rate density inferred from the same lines.
  • Other rest-frame optical or UV lines that are bright in active galactic nuclei may show analogous black-hole dominance once modeled.
  • Joint analysis of multiple lines could separate the black-hole and star-formation contributions without relying solely on the simulation.

Load-bearing premise

The simulation's sub-grid rules for how black holes accrete and how much Hα and He II light they produce at the bright end match what happens in real galaxies.

What would settle it

A measured Hα or He II voxel intensity distribution or power spectrum from SPHEREx or a comparable survey that lies outside the range predicted when black-hole accretion is included but inside the range predicted when it is omitted.

Figures

Figures reproduced from arXiv: 2606.01603 by Adam Lidz, Erika Ogata, Kana Moriwaki, Naoki Yoshida, Rui Lan Jun.

Figure 1
Figure 1. Figure 1: Intensity maps of H𝛼 (top) and He ii (bottom) emission at 𝑧 = 4 for a representative spectral bin in the SPHEREx-like mock survey. The color scale shows the total intensity, including both SF- and BH-powered components. Blue points indicate regions where the BH-powered contribution dominates over the SF contribution within individual voxels. include an auxiliary short-wavelength band spanning 0.25–0.93 𝜇m … view at source ↗
Figure 2
Figure 2. Figure 2: Redshift evolution of the mean line intensity and the role of BH￾powered emission for H𝛼 and He ii. Top panel: mean intensity 𝐼𝑖 for H𝛼 (blue) and He ii (pink). Colored curves show the total intensity (BH+SF), while grey curves indicate the SF-powered component; solid and dashed lines distinguish the Chabrier (H𝛼_C and HeII_C) and Salpeter (H𝛼_S and HeII_S) models, respectively. Middle panel: fractional co… view at source ↗
Figure 3
Figure 3. Figure 3: Voxel intensity distributions (VIDs) of the H𝛼 (top two rows) and He ii (bottom two rows) at 𝑧 = 1 − 6, shown for a representative spectral bin in each redshift slice. The distributions are rescaled to an effective survey area of 200 deg2 , corresponding to the SPHEREx deep field. Colored histograms show the total emission (BH+SF), while grey histograms indicate the contribution from SF alone. Solid and da… view at source ↗
Figure 4
Figure 4. Figure 4: Redshift evolution of the effective bias, 𝑏𝑖 , for H𝛼 and He ii emission in the Chabrier-IMF model. The grey dashed curve shows the bias associated with the SF-powered component, while the blue and pink solid curves show the total biases for H𝛼 and He ii, respectively, including both SF- and BH-powered emission. contributes more than 50 per cent both to the total intensity and to the voxel population. In c… view at source ↗
Figure 5
Figure 5. Figure 5: Auto- and cross-power spectra of the H𝛼 and He ii intensity fields at redshifts 𝑧 = 4 (top row) and 𝑧 = 6 (bottom row). Each row shows, from left to right, the auto-power spectra of H𝛼, He ii, and their cross-power spectrum. In all panels, the colored curves indicate the total emission including both BH-powered and SF-powered components, while grey curves show the contribution from SF alone. to avoid an ex… view at source ↗
Figure 6
Figure 6. Figure 6: Scale dependence of the fractional contribution of BH-powered emission to the three-dimensional power spectra of the H𝛼 and He ii line-intensity fields. From left to right, the panels show the auto-power spectra of H𝛼, the auto-power spectra of He ii, and their cross-power spectra. The top row corresponds to the redshift shells centred at 𝑧 ≃ 1 − 3, while the bottom row shows the results for 𝑧 ≃ 4 − 6. In … view at source ↗
Figure 7
Figure 7. Figure 7: Integrated signal-to-noise ratio of the power spectra as a function of redshift for H𝛼 (top), He ii (middle), and the H𝛼–He ii cross-power spectrum (bottom), computed over the range 𝑘min = 0.1 to 𝑘max = 10.0 ℎ cMpc−1 . In each panel, the darker curves show the predictions for a SPHEREx-like survey, while the lighter curves show those for a CDIM-like survey. Solid and dashed curves correspond to the total (… view at source ↗
Figure 8
Figure 8. Figure 8: Impact of masking voxels associated with bright accreting BHs on the shot-noise component of the H𝛼 power spectrum. The horizontal axis shows the number of masked voxels per spectral slice, 𝑁mask, scaled to a SPHEREx-like survey area of 200, deg2 . Voxels are removed sequentially in order of decreasing BH bolometric luminosity. Top panel shows the quantity 1 − 𝑃 SF AGNmask/𝑃 BH+SF AGNmask, which measures t… view at source ↗
Figure 9
Figure 9. Figure 9: The bottom panel shows the corresponding evolution of the summed squared fluxes, Σgal𝐹 2 𝑖,gal, normalized by the no-attenuation model, which serves as a simple proxy for the shot-noise contri￾bution. Unlike the mean intensity, the shot-noise proxy is strongly suppressed by attenuation and ionizing-photon escape, because it is dominated by bright compact sources within galaxies rather than diffuse IGM emis… view at source ↗
read the original abstract

Line-intensity mapping (LIM) has attracted growing attention as a powerful technique for probing the large-scale distribution of galaxies and the cosmic history of star formation through unresolved line emission. Existing LIM models for galaxy-associated lines, such as H$\alpha$, often assume that the dominant contribution to observed emission arises from star-forming activity, while the role of accreting black holes (BHs) remains largely unexplored. In this study, we use the IllustrisTNG cosmological hydrodynamical simulation to construct mock intensity maps of H$\alpha$ and He II, including contributions from both star formation and BH accretion. We show that the BH contribution to the mean intensity is significant, reaching $\sim$40--60 per cent for H$\alpha$ and $\sim$60--80 per cent for He II around cosmic noon. Owing to the large luminosity weight of rare, bright sources, BH-powered emission dominates the shot-noise component of the power spectrum and significantly boosts the small-scale clustering amplitude, particularly for He II. We assess the implications for forthcoming LIM surveys and show that SPHEREx can probe the BH-influenced bright end of the H$\alpha$ voxel intensity distribution (VID) at $z\lesssim4$, and a CDIM-like experiment can further access the BH-dominated regime of He II. Our results demonstrate that accreting BHs represent an essential component of LIM signals, which was previously underappreciated. We thus conclude that accurately modeling the BH contribution is crucial for a physically complete interpretation of future LIM observations.

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 / 2 minor

Summary. The paper uses the IllustrisTNG hydrodynamical simulation to generate mock Hα and He II intensity maps that include both star-formation and black-hole accretion contributions. It reports that accreting BHs supply 40–60% of the mean Hα intensity and 60–80% of the mean He II intensity near cosmic noon, dominate the shot-noise term of the power spectrum, and boost small-scale clustering; the work then discusses detectability of these effects with SPHEREx and a CDIM-like experiment.

Significance. If the simulation results are robust, the finding that BH accretion is a major, previously under-appreciated contributor to LIM signals would require revisions to existing star-formation-only models and would affect the design and interpretation of forthcoming intensity-mapping surveys. The simulation-based approach supplies concrete, falsifiable predictions for the voxel intensity distribution and power-spectrum shape that can be tested by future data.

major comments (2)
  1. [Section 3] Section 3 (line-emission modeling): the quoted 40–60% and 60–80% mean-intensity fractions are obtained by post-processing IllustrisTNG halos with a specific sub-grid BH accretion prescription and line-luminosity scaling; no error bars, parameter-variation tests, or direct comparison to observed Hα/He II luminosity functions at the bright end (where the VID and shot-noise term are dominated) are provided, rendering the central quantitative claims sensitive to an unvalidated modeling choice.
  2. [Section 4.2] Section 4.2 (power-spectrum results): the claim that BH emission dominates the shot-noise component and boosts small-scale clustering rests on the same unvalidated bright-end luminosity function; if the simulated AGN number density at high L is systematically high, both the reported fractions and the clustering boost are overstated by construction.
minor comments (2)
  1. [Figure 3] Figure 3 caption: the color scale for the VID panels is not labeled with units, making quantitative comparison to the text fractions difficult.
  2. [Section 2.3] Section 2.3: the precise definition of the BH versus star-formation luminosity cut (e.g., Eddington ratio threshold) is stated only qualitatively; an explicit equation would improve reproducibility.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the detailed and constructive report. The comments highlight important aspects of model validation that we will strengthen in the revised manuscript. Below we respond point by point to the major comments.

read point-by-point responses

  1. Referee: [Section 3] Section 3 (line-emission modeling): the quoted 40–60% and 60–80% mean-intensity fractions are obtained by post-processing IllustrisTNG halos with a specific sub-grid BH accretion prescription and line-luminosity scaling; no error bars, parameter-variation tests, or direct comparison to observed Hα/He II luminosity functions at the bright end (where the VID and shot-noise term are dominated) are provided, rendering the central quantitative claims sensitive to an unvalidated modeling choice.

    Authors: We agree that the quantitative fractions depend on the specific sub-grid accretion model and line-luminosity relations adopted from IllustrisTNG. While the simulation itself has been calibrated to a broad set of observational constraints, we did not include direct comparisons to observed Hα or He II luminosity functions at the bright end in the original submission. In the revised manuscript we will add such comparisons using available observational data, include a brief discussion of modeling uncertainties, and note the absence of a full parameter-variation study as a limitation of the current work. revision: yes

  2. Referee: [Section 4.2] Section 4.2 (power-spectrum results): the claim that BH emission dominates the shot-noise component and boosts small-scale clustering rests on the same unvalidated bright-end luminosity function; if the simulated AGN number density at high L is systematically high, both the reported fractions and the clustering boost are overstated by construction.

    Authors: We concur that the shot-noise dominance and small-scale power boost are sensitive to the bright-end AGN number density. The revisions described in response to the first comment—specifically the addition of luminosity-function comparisons—will directly test whether the simulated bright-end densities are consistent with observations. If discrepancies are found, we will qualify the power-spectrum claims accordingly in the revised text. revision: yes

Circularity Check

0 steps flagged

No significant circularity; simulation outputs are independent computed quantities

full rationale

The paper's central results (BH fractions of mean intensity and shot-noise dominance) are obtained by direct post-processing of IllustrisTNG halo catalogs with fixed sub-grid accretion rates and line-luminosity prescriptions. No derivation chain, equation, or self-citation reduces the reported percentages to a fit or tautology; the outputs are model-evaluated quantities rather than re-expressions of the inputs. Self-citations, if present, are not load-bearing for the headline claims. This is a standard simulation study whose conclusions stand or fall on the fidelity of the underlying sub-grid model, not on any internal circular reduction.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

The central claim rests on the accuracy of IllustrisTNG's black-hole accretion and line-emission sub-grid models; no free parameters, axioms, or invented entities are explicitly introduced in the abstract.

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