The most extreme high-z radio quasars in the eRASS:1 X-ray survey

A. Caccianiga; A. Moretti; A. Rossi; B. Arsioli; E. Marini; L. Ighina; L. N. Mart\'inez-Ram\'irez; L. Palmieri; T. Connor; Y. Beletsky

REVIEW 2 major objections 5 minor 295 references

The most extreme high-z radio quasars in the eRASS:1 X-ray survey

T0 review · 2 major / 5 minor · reviewed 2026-08-15 · deepseek-v4-flash

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Pith's one-line read A new eRASS-based census finds five times more X-ray-bright blazars at z>4 than a non-evolving jet model predicts, supporting the IC/CMB mechanism.

desk verdict The spectroscopic sample is a real contribution; the claimed rule-out of a non-evolving X-ray-to-radio ratio is plausible but under-supported because the prediction rests on an extrapolated radio luminosity function with unpropagated uncertainty. read the letter →

arxiv 2608.04078 v1 pith:Q2N6GCOR submitted 2026-08-04 astro-ph.GA astro-ph.HE

L. Ighina , L. Palmieri , L. N. Martínez-Ramírez , A. Caccianiga , T. Connor , A. Moretti , B. Arsioli , Y. Beletsky

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E. Marini A. Rossi

This is my paper · ORCID

classification astro-ph.GAastro-ph.HE

keywords high-redshiftquasarsblazarseROSITAX-raysurveysradio-loudAGNIC/CMBrelativisticjetsLymandropout

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

Combining X-ray detections from the first eROSITA all-sky survey with radio and optical/NIR photometry, the paper builds a sample of 68 high-redshift quasar candidates, spectroscopically confirms 39 at z>3.5, and adds 14 new radio quasars at z>4, a 65% increase in the known population in the surveyed area. The central claim is that the completeness-corrected number counts of the 26 X-ray-bright blazars in this sample rule out a scenario in which the X-ray-to-radio luminosity ratio of blazars does not evolve with redshift: counts at z=4-4.3 are about five times larger than the constant-ratio model predicts. The counts are broadly consistent with the fractional IC/CMB model, in which cosmic microwave background photons are inverse-Compton scattered by jet electrons, with an energy density scaling as (1+z)^4. If correct, this confirms that the apparent X-ray brightening of high-redshift blazars is a real population-level effect rather than a selection artifact, and it strengthens the idea that jets at z>4 efficiently upscatter CMB photons.

What carries the argument

The load-bearing machinery is the comparison between the observed cumulative number of X-ray-selected blazars, N_{\rm blazar}(>z), and the prediction of a fractional IC/CMB model. In the model, the X-ray-to-radio luminosity ratio evolves as L_X/L_R(z) = (L_X/L_R(0)) [(1-A_0) + A_0(1+z)^4], where A_0 is the fraction of X-ray emission produced by inverse-Compton scattering of CMB photons at z=0; the mock blazar population is generated by integrating the radio luminosity function of blazars and then detecting it with the eRASS:1 sky-dependent sensitivity. The observed counts come from the roughly 30% blazar fraction among spectroscopically confirmed targets, applied to the candidates not yet observed.

What would settle it

A complete spectroscopic census of the 22 unobserved candidates: if fewer than about 4-5 of them turn out to be z>4 blazars, or if they concentrate at z<4, the fivefold excess at z=4-4.3 shrinks and the claimed rejection of the constant X-ray-to-radio model weakens.

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Extended reading notes

Core claim

Using the eRASS:1 X-ray catalogue matched to RACS-mid radio and DELVE optical/NIR data, the authors select 68 z>4 quasar candidates via Lyman-dropout colour criteria and obtain spectra for 46 of them. Of these, 39 are confirmed at z>3.5, 14 at z>4. Using the X-ray-to-UV intensity ratio \tilde{\$\alpha$}_{\rm ox}<1.355 to identify blazars, they find 26 blazars at z>4. Comparing the redshift distribution of these blazars, corrected for selection completeness (90%, 76%, and 58% dropout recovery for the g-, r-, and i-dropouts), with the predictions of a fractional IC/CMB model built on the radio luminosity function of blazars, they conclude that a constant X-ray-to-radio ratio is ruled out (by a factor of about five at z=4-4.3) and that the data are broadly consistent with the IC/CMB model, although with a residual about 2.6 $\sigma$ excess of z>4 blazars and an overprediction at z>4.7.

Load-bearing premise

The completeness corrections and the roughly 30% blazar fraction measured on the spectroscopically confirmed targets are assumed to transfer to the 22 candidates that were not observed and to the dropout-incomplete redshift bins; if those unobserved candidates have different redshifts or a different blazar fraction, the completeness-corrected number counts change.

Editorial extensions

If this is right

The 14 new z>4 radio quasars raise the known population in the eRASS:1/DELVE/RACS area by about 65%, showing that the high-redshift radio-quasar census is far from complete.
A constant X-ray-to-radio ratio for blazars is ruled out: completeness-corrected counts at z=4-4.3 are about five times higher than that model predicts.
The observed counts are broadly consistent with the fractional IC/CMB model, supporting inverse-Compton scattering of CMB photons as the dominant source of the extra X-ray emission at high redshift.
The model overpredicts the number of blazars at z>4.7, suggesting that the redshift evolution of the X-ray enhancement may not follow the simple (1+z)^4 scaling at the highest redshifts.
The 26 blazars at z>4 form a sample for future VLBI and X-ray follow-up to constrain jet orientation and accretion properties in the early Universe.

Reading between the lines

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

If the IC/CMB enhancement is real, deeper eRASS scans and wider-area surveys should find even more X-ray-bright blazars at z>5.5, where the (1+z)^4 boost becomes extreme; the current upper limits at z>5.7 are still based on only two sources.
The residual excess of z>4 blazars over the IC/CMB best fit, if it survives completeness corrections, could point to additional X-ray production from super-Eddington accretion or from a redshift-dependent jet composition, alternatives the paper explicitly leaves open.
The ~65% increase in known z>4 radio quasars implies that simple extrapolations from the current census underestimate the true space density; a full-spectroscopic census of the remaining 22 candidates would test whether the corrected counts at z~4 are indeed as high as reported.
The blazar classification relies entirely on the \tilde{\alpha}_{\rm ox} threshold; adding VLBI brightness-temperature measurements to a subsample would test whether the X-ray-selected excess really corresponds to relativistic boosting rather than to a softer spectral component.

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Editorial analysis

A structured set of objections, weighed in public.

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

Desk Editor's Note

read the letter

Short version: this paper delivers something real — 39 newly confirmed z>3.5 radio-emitting quasars, 14 at z>4, from the eRASS/RACS/DELVE combination, with discovery spectra in the appendix. That is a substantial observational addition and a 65% increase in the known z>4 radio quasar population in the surveyed area. The statistical comparison to IC/CMB models is the weakest part, and the decisive problem is not the one the reader flagged.

The selection and spectroscopy are careful. Cross-match radii are derived from simulations, dropout completeness is measured against known z>4 quasars (90/76/58% for g/r/i drops), the four missed known sources are accounted for with specific explanations, and the SED screening against low-z ellipticals is sensible. The 85% confirmation rate is credible. The catalog with radio, optical, and X-ray luminosities and alpha_ox will be useful. Blazar classification via alpha_ox < 1.355 is a single threshold from earlier work, but the cross-check with radio loudness and with Sbarrato et al. for 10 overlapping sources makes it acceptable for a statistical sample.

The model comparison in Sec. 5.2 is where I would push back. The claim to rule out a constant X/R ratio rests on the ~5x excess at z=4–4.3. The reader's concern about transferring the ~30% blazar fraction to unobserved candidates is real but not fatal for that claim: unobserved candidates can only add blazars, so the observed counts would go up, not down. The load-bearing issue is the absolute normalization of the prediction. In Fig. 6, the prediction integrates the Mao et al. radio luminosity function and assumes it holds at z>4, where it is an extrapolation. The shaded band varies photon index and A0, but not the RLF normalization or faint-end slope. If those carry a factor-of-two or three uncertainty — not an unlikely amount for an extrapolated LF — the discrepancy drops to below 2–3 sigma. That uncertainty needs to be propagated before the word "rule out" is warranted.

A related caveat: the model parameters come from the same group's prior papers. That is not circularity in the strong sense, because the eRASS sample is new data used for comparison rather than fitting. Still, the sentence that the discrepancy reduces when model uncertainties are included is doing a lot of work, and those model uncertainties are not fully mapped.

Bottom line: this deserves serious refereeing. The observational core is strong, the catalog is a contribution, and the model section is fixable by a more honest treatment of the prediction band. The paper is for the high-redshift blazar/AGN population crowd, and the referee should focus on Sec. 5.2 and the RLF error budget. If that is addressed, I would be happy to see it in MNRAS.

Referee Report

2 major / 5 minor

Summary. The paper constructs a sample of high-redshift radio quasars by cross-matching eRASS:1 X-ray sources with RACS-mid radio and DELVE optical/NIR data. Applying Ly-alpha dropout criteria to the X-ray/radio-selected catalog yields 68 quasar candidates; spectroscopic follow-up of 46 targets confirms 39 quasars at z>3.5, of which 14 are at z>4. Using the alpha_ox<1.355 criterion, the authors identify 26 z>4 blazars in the combined new and literature sample. They then compare the cumulative number of z>4 blazars with predictions from a constant X-ray-to-radio ratio model and a fractional IC/CMB evolution model, concluding that the constant scenario is ruled out while the IC/CMB model is broadly consistent with the data.

Significance. If the central model comparison holds, this is the largest X-ray-selected statistical sample of z>4 blazars to date and provides one of the cleanest tests of IC/CMB-driven X-ray evolution at high redshift. The paper's strengths are its careful sample construction, the extensive spectroscopic campaign with discovery spectra in Appendix A, the explicit discussion of incompleteness, and the new sample itself: the 14 new z>4 radio quasars represent an approximately 65% increase in the known population in the survey area. The main weakness is that the headline rule-out of the constant X/R scenario rests on an absolute model prediction whose dominant systematic uncertainties are not propagated into the comparison.

major comments (2)

[Section 5.2, Eq. (1), Fig. 6] The constant X/R prediction shown as the dashed blue curve in Fig. 6 is an absolute count obtained by integrating the Mao et al. (2017) radio luminosity function at z>4 and combining it with the local X/R distribution. The shaded band around the curve varies only the photon index (Gamma_X=1.3-1.7) and the A0 parameter; it does not include uncertainties in the Mao et al. RLF normalization, its faint-end slope, or the local X/R distribution parameters (log(X/R)=1.95, sigma=0.35). Because the claimed exclusion is based on comparing the observed 26 counts with a prediction of roughly 5 at z=4-4.3, an unpropagated factor-of-two-to-three systematic uncertainty in the z>4 RLF could reduce the significance of the rule-out substantially. Please propagate these uncertainties, for example by varying the Mao et al. parameters within their quoted errors or by adopting an empirical envelope from the local X/R distribution, and report the resulting significance for excluding the constant model.
[Section 5.2, Sec. 6] The only quantitative significance quoted in the model comparison, approximately 2.6 sigma, refers to the discrepancy between the data and the IC/CMB best-fit model, not to the exclusion of the constant X/R model. The statement 'we can rule out a scenario where the X/R ratios in blazars does not evolve as a function of redshift' is therefore not backed by a stated test statistic for the constant model. Please provide the formal significance of the exclusion, including both Poisson and propagated systematic uncertainties, and adjust the abstract and conclusions if that significance falls below the threshold implied by the word 'rule out'.

minor comments (5)

[Section 3] The text reads 'we confirmed the high-z nature of 397, 14 of which are at z>4'; the number should be 39, not 397.
[Section 3] 'The high faction of confirmed candidates' should be 'the high fraction of confirmed candidates'.
[Section 5.1] The phrase 'aoresecure classification' appears to be a typo for 'a more secure classification'.
[Fig. 6 caption] The caption states that the upper limit at z~5.5 is based on the two blazars in the Russian half of the sky, while the text identifies the z=5.7 upper limit with the non-confirmation of any i-dropout candidates and the Russian-half sources as a lower limit. Please make the caption consistent with the text.
[Sections 2.2 and 5.2] The completeness correction in Fig. 6 uses dropout completeness fractions (90%, 76%, 58%) derived from all known z>4 quasars in DELVE, not specifically from the X-ray/radio-selected subset, and the approximately 30% identification efficiency is based on the 46 brighter observed targets. Please state explicitly how these corrections are applied to the literature-known sources, and discuss the systematic uncertainty this choice introduces into the corrected counts. Since unobserved candidates can only add counts, this does not threaten the exclusion of the constant model, but it does affect the claimed shape of N(>z) and the comparison at z>4.7.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the model comparison uses new eRASS data against fixed parameters from prior work, with no parameter fitted to the claimed result.

full rationale

The paper's central test—comparing the number of z>4 eRASS blazars with the constant X/R and IC/CMB predictions—is not circular. The expected counts are generated by integrating the Mao et al. (2017) radio luminosity function and applying the X/R distribution and A0 parameters from Ighina et al. (2021). Those parameters were fitted to radio-selected blazar samples at z~1 and z~4.5 (Sec. 5.2), not to the eRASS:1 data presented here, and the observed counts are new measurements. The blazar classification threshold (tilde_alpha_ox = 1.355) is likewise taken from Ighina et al. (2019) and is cross-checked against the radio-loudness criterion R=80, which gives the same z>4 blazar count. No parameter in this paper is fitted to the quantity being predicted; the completeness corrections are standard selection-function estimates. The self-citations are therefore independent support rather than a derivation loop. The skeptic's concern about the Mao et al. RLF normalization at z>4 is a statistical and robustness issue, not circularity.

Assumptions & free parameters 6 free parameters · 5 assumptions · 0 invented entities

The central model comparison rests on distributions and completeness factors carried in from prior work rather than fitted here. No new physical entities are introduced. The main free parameters are the IC/CMB model inputs from Ighina et al. 2021 and the assumed blazar photon index.

free parameters (6)

log(X/R)_0 = 1.95
Mean of the logarithmic Gaussian distribution for the X-ray-to-radio luminosity ratio of blazars at z=0, adopted from Ighina et al. 2021 and used in Eq. 1 to predict eRASS counts.
sigma_X/R = 0.35
Width of the same distribution from Ighina et al. 2021, used to compute the mock blazar population.
log(A0) = -2.74
Mean fractional IC/CMB contribution to X-ray emission at z=0, from Ighina et al. 2021, governing the redshift evolution in Eq. 1.
sigma_A0 = 0.66
Width of the A0 distribution from Ighina et al. 2021, used to propagate model uncertainty in the predicted counts.
Gamma_X = 1.5
Assumed photon index for blazars used to convert X-ray luminosity to flux in the model simulations (Sec 5.2). It is a fixed modeling choice, not fitted here.
Dropout completeness factors = 0.90, 0.76, 0.58
Measured from known z>4 quasars in the DELVE area for g-, r-, and i-dropouts; used to correct the observed blazar counts, so they directly affect the comparison.

assumptions (5)

standard math A flat LCDM cosmology with H0=70 km/s/Mpc, Omega_m=0.3, and Omega_Lambda=0.7 is adopted.
Stated in Sec 1; standard in the field and used for luminosity distances.
domain assumption The radio luminosity function of blazars from Mao et al. (2017) correctly describes the parent population when building mock samples.
Used in Sec 5.2 to construct the mock blazar population; if the RLF is inaccurate, the expected counts shift.
domain assumption The X-ray-to-radio luminosity ratio and the fractional IC/CMB contribution A0 at z=0 follow log-Gaussian distributions with the parameters from Ighina et al. 2021.
Assumed to apply to the eRASS-selected blazar population even though calibrated on radio-selected samples.
domain assumption Blazar classification based solely on the alpha_ox < 1.355 criterion is statistically reliable for the sample.
Stated in Sec 5.1; the number counts of blazars at z>4 depend on this classification being unbiased in aggregate.
domain assumption The dropout selection completeness measured from known quasars transfers to the newly selected candidates.
Used in Sec 5.2 to correct observed counts; if the new candidates have a different magnitude or color distribution, the completeness correction is biased.

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Cite this review

Pith. "Pith review of The most extreme high-z radio quasars in the eRASS:1 X-ray survey." pith.science (2026). https://pith.science/paper/Q2N6GCOR

@misc{pith2026260804078,
  author       = {Pith},
  title        = {Pith review of: The most extreme high-z radio quasars in the eRASS:1 X-ray survey},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/Q2N6GCOR}},
  note         = {Machine review of arXiv:2608.04078}
}

abstract

We present the selection and identification of high-z radio quasars from a combination of X-ray (eROSITA All-Sky Survey), optical/NIR (DECam Local Volume Exploration), and radio (Rapid ASKAP Continuum Survey) surveys. After building a sample of 68 new high-z quasar candidates, we performed follow-up spectroscopic observations on 46 sources, confirming 39 to have redshifts z>3.5. For the subset of radio quasars at z>4, the 14 new sources identified here represent an increase of $\sim$65% in the known population of objects above the same flux limits in the same area. Using X-ray-to-optical relative intensity, we identified blazars in our sample, which we then used to compare the total number of z>4, X-ray selected blazars to the predictions of a fractional IC/CMB model previously proposed in the literature. Overall we find a relatively good agreement, even considering the potential biases in the redshift distribution from the incompleteness of the spectroscopic follow-up and the blazar classification criteria. The sources presented in this work represent a sample well suited for investigating the evolution of the most extreme systems in the early Universe, including their relativistic jets and accretion properties

Figures

Figures reproduced from arXiv: 2608.04078 by the authors.

**Figure 1.** Example of the optical/NIR SED of an 𝑟-dropout candidate selected with the criteria described in the text. As shown with the templates overlaid, the observed optical emission can be explained by both an elliptical galaxy at 𝑧 ∼ 0.9 (black line; from Polletta et al. 2007) and a 𝑧 ∼ 4.7 quasar (gray line; from Polletta et al. 2007). Based on the additional IR coverage provided by the VHS and CatWISE surveys, we exclud… view at source ↗

**Figure 2.** [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗

**Figure 3.** Sky distribution of the high-𝑧 quasars selected from the eRASS:1 survey. Objects already reported in the literature are marked by blue squares, while quasars newly discovered in this work are shown with orange (𝑧 < 4) and red (𝑧 > 4) circles. The shaded blue area corresponds to the area covered by eRASS:1 below Dec.=+30◦ , where most of the sky is covered by DELVE. monochromatic luminosity at 2500 Å we assumed a pow… view at source ↗

Figures from the paper (3 more)

**Figure 4.** Figure 4: Distribution of the 𝛼ox parameter as a function of the UV luminosity at 2500 Å for the high-𝑧 quasars selected in this work. As a reference we also report the 0 < 𝑧 < 7 quasars discussed in Lusso et al. 2020 (𝑧 > 3.5 sources are highlighted with black circles) as well…

**Figure 5.** Figure 5: Distribution of the 𝛼˜ox (top panel) and the radio-loudness (in logarithm scale; bottom panel) parameters as a function of redshift. Red circles indicate the new sources discovered in this work, while blue squares show sources already reported in the literature in the …

**Figure 6.** Figure 6 [PITH_FULL_IMAGE:figures/full_fig_p008_6.png]

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