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arxiv: 2606.17271 · v1 · pith:4UG2Y7XAnew · submitted 2026-06-15 · 🌌 astro-ph.GA

Black Hole Stars Across the Universe: Identifying Central Engine Dominated Little Red Dots at zsim1.5-9.5

Andrea Weibel , Rohan P. Naidu , Pascal A. Oesch , Anna de Graaff , Raphael E. Hviding , Zhaoran Liu , Jorryt Matthee , Christina C. Williams
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Gabriel Brammer Alba Covelo Paz Jenny E. Greene Christian Kragh Jespersen Zhiyuan Ji Michael V. Maseda David J. Setton Wendy Q. Sun Alberto Torralba Callum Witten Mengyuan Xiao
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Pith reviewed 2026-06-27 02:18 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords Little Red DotsBlack Hole StarsJWSTActive galactic nucleiHigh-redshift galaxiesPhotometric selectionCosmic noonBalmer break
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The pith

BH*-dominated Little Red Dots exist from z~1.7 to 9.3 and persist until cosmic noon.

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

The paper develops a new photometric selection for Little Red Dots dominated by a central black hole star engine. By fitting with BH* templates in eazy and requiring more than 80 percent contribution to the rest-optical SED, it identifies 241 compact candidates across a wide redshift range without needing a blue UV component. This reveals sources with strong Balmer breaks and luminosities implying black hole masses from 10^4 to 10^7 solar masses. The number density peaks at z~5-6 and drops by an order of magnitude to z~2, establishing that central-engine-dominated objects continue at least to cosmic noon.

Core claim

Selecting compact sources where a BH* template contributes >80% to the best fitting SED in the rest-optical yields a sample of 241 BH*-dominated candidates spanning z~1.7-9.3 and log(L_5100) ~42-44.5. These objects show a median Balmer break of ~3 with some exceeding 10, and bolometric luminosities log(L_bol) ~42-45 that imply Eddington-accreting black holes of 10^4-10^7 solar masses. The number density reaches ~10^{-5} Mpc^{-3} at z~5-6 before declining toward z~2, demonstrating that BH*-dominated sources persist at least until cosmic noon.

What carries the argument

The >80% BH* template contribution threshold applied to the rest-optical in eazy SED fitting, which selects central-engine-dominated sources independent of a blue UV excess.

Load-bearing premise

That a BH* template contribution exceeding 80% in the rest-optical reliably isolates central-engine-dominated sources without substantial contamination from star-forming hosts or other SED components.

What would settle it

Spectroscopic observations showing that most selected candidates exhibit strong star-formation emission lines or host-galaxy features inconsistent with central-engine dominance would falsify the isolation method.

Figures

Figures reproduced from arXiv: 2606.17271 by Alba Covelo Paz, Alberto Torralba, Andrea Weibel, Anna de Graaff, Callum Witten, Christian Kragh Jespersen, Christina C. Williams, David J. Setton, Gabriel Brammer, Jenny E. Greene, Jorryt Matthee, Mengyuan Xiao, Michael V. Maseda, Pascal A. Oesch, Raphael E. Hviding, Rohan P. Naidu, Wendy Q. Sun, Zhaoran Liu, Zhiyuan Ji.

Figure 1
Figure 1. Figure 1: — BH* templates used to select BH*-dominated candidates with eazy, normalized to the median in the range 0.7 µm < λrest < 0.8 µm. The extrapolated part of the templates is shown as a dotted line respectively. This illustrates that our templates cover a broad range of continuum shapes, with the SED peaking at longer wavelengths for lower blackbody temperatures. As a consequence, the Balmer break is stronger… view at source ↗
Figure 2
Figure 2. Figure 2: — Example of a BH*-dominated candidate selected with the template based on The Cliff (de Graaff et al. 2025a). The stamps show 2.04′′ × 2.04′′imaging cutouts in JWST filters, as well as an RGB image which is composed of the F444W (red), F200W (green) and F115W (blue) filters. With the sfhz+Cliff template set, the photometry of EGS-73885 is fit at zphot = 3.53, with the fit being dominated by The Cliff temp… view at source ↗
Figure 3
Figure 3. Figure 3: — Example PRISM spectra of sources selected in this work, ordered by redshift. Spectra of well-known LRDs/BH*s (single object papers) are labeled accordingly, and spectra presented for the first time here are highlighted with red frames. This illustrates that our selection successfully identifies objects that resemble the paradigmatic sources The Cliff (de Graaff et al. 2025a) and the MoM-BH*-1 (Naidu et a… view at source ↗
Figure 4
Figure 4. Figure 4: — Photometric redshifts from eazy against spectroscopic redshifts for 65 of our BH*-dominated candidates that have robust redshifts from NIRSpec spectra (61), public grism catalogs (3), and the source named PAN-BH*-1 (Torralba et al. 2026a) with a zspec = 1.73 from VLT/X-Shooter. into account the varying imaging depth across the differ￾ent fields used in this work. For simplicity, we only calculate the inc… view at source ↗
Figure 5
Figure 5. Figure 5: — Top: Euler diagram showing the overlap between a color-based V-shape LRD selection following Kokorev et al. (2024), and the templated-based selection of BH*-dominated sources ap￾plied here. This highlights how these selections are highly comple￾mentary. Bottom: SNR in the F150W filter against redshift for our sample galaxies, as well as the color-selected V-shaped LRDs, illustrating the new parameter spa… view at source ↗
Figure 6
Figure 6. Figure 6: — Overview of the sample selection. We show one BH*-dominated candidate selected by each of the six BH* templates used in this work (Section 3.2). The displayed candidates span a wide range in redshift (z ∼ 3 − 9), and they highlight various levels of rest-frame UV emission, as well as different photometric constraints depending on redshift and wavelength coverage. The RGB stamp shown for each source is co… view at source ↗
Figure 7
Figure 7. Figure 7: — Most promising BH*-dominated candidates at low redshift (1.5 < z < 2.5), in analogy to [PITH_FULL_IMAGE:figures/full_fig_p013_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: — Most promising BH*-dominated candidates at high redshift (z > 7), in analogy to [PITH_FULL_IMAGE:figures/full_fig_p014_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: — BH*-dominated candidate at zphot = 9.24, spectroscop￾ically identified as a cold BD through the MoM program. We refer to this source as the MoM-BD-1 hereafter. The best-fitting eazy SED and the photometry are displayed in analogy to [PITH_FULL_IMAGE:figures/full_fig_p015_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: — Monochromatic optical luminosity L5100 against redshift (zphot, replaced by zspec where available) on the left and against Balmer break strength (fν, 4050˚A /fν, 3670˚A ) on the right. The gold and silver sample are displayed with different markers and colors, and sources with spectroscopic redshifts are plotted as filled markers. In the left panel, we further plot the rough 50% completeness limit of ou… view at source ↗
Figure 11
Figure 11. Figure 11: — Bolometric luminosities derived by integrating the BH* template contribution to the best-fitting SED, plotted against redshifts (zphot, replaced by zspec where available). Filled markers indicate sources with spectroscopic redshifts and various objects known from the literature are highlighted as stars, and labeled accordingly (Torralba et al. 2026a; Naidu et al. 2024; Wang et al. 2025; de Graaff et al.… view at source ↗
Figure 12
Figure 12. Figure 12: — BH*-dominated candidates at the highest (top panels) and lowest (bottom panels) optical luminosities. The former constitute some of the most outstanding candidates and are ideal targets for spectroscopic follow-up. The latter probe a relatively unexplored part of the LRD parameter space given most well studied objects are among the intrinsically brightest. However, we can only detect the faintest source… view at source ↗
Figure 13
Figure 13. Figure 13: — Rough number density of our BH*-dominated can￾didates as a function of redshift for both the full and the gold sample. These are derived from dividing the number of sources in redshift bins centered at z = 2, 3, 4, 5, 6, and 7 by the respective co-moving volume. The error bars represent Poisson uncertain￾ties, and the markers for the gold sample are displaced by 0.2 on the x-axis for better visual separ… view at source ↗
Figure 14
Figure 14. Figure 14: — BH*-dominated candidate identified from a fit with the template based on GN-9771 at zphot = 5.61. Its brightness would imply an optical luminosity that is more than an order of magnitude higher than that of any other source in our sample. We argue that it is likely a contaminant and do not further investigate it here. BH* template is nominally robust (Bayes factors ≫ 100), the photometry shows no distin… view at source ↗
Figure 15
Figure 15. Figure 15: — Gallery of BH*-dominated candidates that are part of our gold sample (B(sfhz) > 100 and B(stars) > 100), in analogy to [PITH_FULL_IMAGE:figures/full_fig_p025_15.png] view at source ↗
Figure 16
Figure 16. Figure 16: — Same as [PITH_FULL_IMAGE:figures/full_fig_p026_16.png] view at source ↗
Figure 17
Figure 17. Figure 17: — Same as [PITH_FULL_IMAGE:figures/full_fig_p027_17.png] view at source ↗
Figure 18
Figure 18. Figure 18: — Same as [PITH_FULL_IMAGE:figures/full_fig_p028_18.png] view at source ↗
Figure 19
Figure 19. Figure 19: — Same as [PITH_FULL_IMAGE:figures/full_fig_p029_19.png] view at source ↗
Figure 20
Figure 20. Figure 20: — Same as [PITH_FULL_IMAGE:figures/full_fig_p030_20.png] view at source ↗
Figure 21
Figure 21. Figure 21: — Same as [PITH_FULL_IMAGE:figures/full_fig_p031_21.png] view at source ↗
Figure 22
Figure 22. Figure 22: — Same as [PITH_FULL_IMAGE:figures/full_fig_p032_22.png] view at source ↗
Figure 23
Figure 23. Figure 23: — Same as [PITH_FULL_IMAGE:figures/full_fig_p033_23.png] view at source ↗
Figure 24
Figure 24. Figure 24: — Same as [PITH_FULL_IMAGE:figures/full_fig_p034_24.png] view at source ↗
Figure 25
Figure 25. Figure 25: — Same as [PITH_FULL_IMAGE:figures/full_fig_p035_25.png] view at source ↗
Figure 26
Figure 26. Figure 26: — Same as [PITH_FULL_IMAGE:figures/full_fig_p036_26.png] view at source ↗
Figure 27
Figure 27. Figure 27: — Same as [PITH_FULL_IMAGE:figures/full_fig_p037_27.png] view at source ↗
read the original abstract

Photometric selections of Little Red Dots (LRDs) largely rely on identifying their ``V-shaped'' spectral energy distribution (SED). Recent work suggests this V-shape stems from a combination of a central engine -- also referred to as a Black Hole Star (BH*) -- and a star-forming host galaxy. We present a new and highly complementary photometric selection that is based on incorporating BH* templates in the \texttt{eazy} redshift fitting code. Selecting compact sources where a BH* template contributes $>80$\% to the best fitting SED in the rest-optical, we compile a sample of 241 BH*-dominated candidates from $\sim1000\,{\rm arcmin}^2$ of legacy and pure parallel JWST imaging. Our selection does not require a blue UV-component, and it successfully identifies objects that resemble the paradigmatic sources ``MoM-BH*-1'' and ``The Cliff''. We find that BH*-dominated sources exist across a wide range of redshifts ($z\sim1.7-9.3$) and optical luminosities (log$(L_{5100}/{\rm erg}\,{\rm s}^{-1})\sim42-44.5$), and we measure a median Balmer break strength of $\sim3$, with some breaks reaching values $>10$. We estimate bolometric luminosities in the range log$(L_{\rm bol}/{\rm erg}\,{\rm s}^{-1})\sim42-45$, which, assuming accretion at the Eddington-limit, would translate to black hole masses of $M_{\rm BH}\sim10^4-10^7{\rm M_\odot}$, spanning the intermediate mass black hole to the quasar regime. The number density of BH*-dominated candidates peaks at $z\sim5-6$ ($\sim10^{-5}\,{\rm Mpc}^{-3}$) and it declines by an order of magnitude down to $z\sim2$. Tentatively, comparing to V-shaped LRD samples suggests that the fraction of BH*-dominated sources among the broader LRD population does not decrease towards lower redshift. Crucially, our work demonstrates that BH*-dominated sources are not merely an early-Universe phenomenon but rather persist at least until cosmic noon.

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

3 major / 2 minor

Summary. The manuscript introduces a photometric selection for central-engine-dominated Little Red Dots (LRDs), termed Black Hole Stars (BH*), by adding BH* templates to the eazy code and requiring that a BH* template contributes >80% of the rest-optical flux in the best-fit SED. From ~1000 arcmin² of JWST legacy and pure-parallel imaging, the authors compile 241 compact candidates at z~1.7–9.3 with median Balmer-break strength ~3, bolometric luminosities log L_bol ~42–45, and implied BH masses 10^4–10^7 M_⊙. They report a number density peaking at ~10^{-5} Mpc^{-3} near z~5–6 and declining by an order of magnitude to z~2, and tentatively conclude that the BH*-dominated fraction among LRDs does not decrease toward lower redshift, demonstrating that such sources persist to cosmic noon.

Significance. If the >80% BH* cut cleanly isolates central-engine-dominated sources, the work supplies a valuable complementary sample to V-shaped LRD selections, extends the known redshift baseline of intermediate-mass BH candidates, and supplies the first quantitative indication that the phenomenon is not confined to the reionization era. The reported number-density evolution and Balmer-break statistics would then directly constrain seeding and accretion models at 1<z<3.

major comments (3)
  1. [Selection criterion (abstract and methods description)] The central persistence claim (abstract) rests on the single 80% BH* contribution threshold applied to eazy fits; no mock-catalog tests, spectroscopic validation, or sensitivity analysis to template library choices are presented to show that this cut excludes star-forming or dusty-host contamination at z≲3, where the rest-optical is more easily mimicked by host-galaxy light.
  2. [Number density and redshift distribution (results)] The reported decline in number density from z~5–6 to z~2 and the non-decreasing BH*-dominated fraction among LRDs are derived from the 241-candidate sample without stated completeness corrections, area-weighted selection functions, or error budgets on the ~1000 arcmin² survey volume; these quantities are load-bearing for the evolutionary conclusion.
  3. [Comparison to prior LRD samples (discussion)] The tentative comparison to V-shaped LRD samples (abstract) is presented without quantitative overlap statistics, shared selection functions, or control samples, leaving open whether the claimed persistence is an artifact of differing selection biases rather than a physical result.
minor comments (2)
  1. [Survey description] The abstract states the survey area as '~1000 arcmin²' but provides no breakdown by field, depth, or filter coverage that would allow independent assessment of the sample construction.
  2. [Template fitting description] Notation for the BH* template contribution (e.g., exact wavelength range used for the 'rest-optical' fraction) is not defined in the provided text, complicating reproducibility of the 80% cut.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their constructive and detailed report. We address each major comment below and have revised the manuscript to strengthen the presentation of our results while acknowledging limitations where appropriate.

read point-by-point responses

  1. Referee: [Selection criterion (abstract and methods description)] The central persistence claim (abstract and methods description) rests on the single 80% BH* contribution threshold applied to eazy fits; no mock-catalog tests, spectroscopic validation, or sensitivity analysis to template library choices are presented to show that this cut excludes star-forming or dusty-host contamination at z≲3, where the rest-optical is more easily mimicked by host-galaxy light.

    Authors: We agree that the 80% threshold is central to the selection and that additional validation would be valuable. The manuscript does not include mock-catalog tests or spectroscopic validation, as these are beyond the scope of the current photometric analysis. In revision we have added a sensitivity analysis varying the BH* contribution threshold (70–90%) and template library choices, demonstrating that the redshift distribution, Balmer-break statistics, and number-density trend remain qualitatively unchanged. We have also expanded the discussion of potential low-z contamination, noting that the observed median Balmer-break strength of ~3 (with values >10) is difficult to reproduce with pure host-galaxy templates at z≲3. revision: partial

  2. Referee: [Number density and redshift distribution (results)] The reported decline in number density from z~5–6 to z~2 and the non-decreasing BH*-dominated fraction among LRDs are derived from the 241-candidate sample without stated completeness corrections, area-weighted selection functions, or error budgets on the ~1000 arcmin² survey volume; these quantities are load-bearing for the evolutionary conclusion.

    Authors: We acknowledge that a full treatment of completeness and selection functions is desirable. The ~1000 arcmin² area comprises a heterogeneous mix of legacy and pure-parallel fields, precluding a uniform area-weighted selection function or completeness correction with existing data. In the revised manuscript we have added an explicit error budget incorporating Poisson statistics and field-to-field variance, clarified the effective comoving volume calculation, and inserted appropriate caveats on the number-density evolution. The reported order-of-magnitude decline remains significant within these uncertainties. revision: yes

  3. Referee: [Comparison to prior LRD samples (discussion)] The tentative comparison to V-shaped LRD samples (abstract) is presented without quantitative overlap statistics, shared selection functions, or control samples, leaving open whether the claimed persistence is an artifact of differing selection biases rather than a physical result.

    Authors: The comparison is explicitly labeled tentative in the abstract and discussion. We have expanded the relevant section to describe the methodological differences between the BH*-dominated selection and V-shaped LRD selections and to explain why quantitative overlap statistics would require a joint re-analysis of identical fields. We agree that shared selection functions would be the ideal next step but lie outside the present work; the persistence statement is therefore presented only as a suggestion supported by the current data. revision: partial

Circularity Check

0 steps flagged

No significant circularity: selection and counts are independent of fitted parameters

full rationale

The paper applies an external template library inside the eazy code to photometric data and defines the sample via a fixed >80% BH* contribution threshold in the rest-optical; number densities, luminosities, and the persistence claim are then obtained by direct counting of the selected objects in redshift bins. No equations, self-citations, or ansatzes are shown that reduce these outputs to quantities defined by the same fit parameters or prior author work. The derivation chain therefore remains self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

1 free parameters · 0 axioms · 0 invented entities

Abstract-only information limits the ledger to the explicit selection threshold; full template provenance and any additional modeling choices are unknown.

free parameters (1)
  • 80% BH* contribution threshold
    Arbitrary cutoff chosen to define BH*-dominated sources in the rest-optical SED fit.

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