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REVIEW 1 major objections 6 minor 199 references

Discovery and characterization of 25 new quasars at 4.6 < z < 6.9 from wide-field multi-band surveys

T0 review · 1 major / 6 minor · reviewed 2026-08-07 · deepseek-v4-flash

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Pith's one-line read This paper reports the spectroscopic discovery of 25 new quasars at redshifts 4.6 to 6.9, six at $z\geq 6.5$, and characterizes their black hole masses, radio emission, and outflow properties.

desk verdict Solid new sample of 25 quasars; the dramatic CIV-MgII shift and 48,000 km/s outflow are honestly flagged as uncertain and should not block publication. read the letter →

arxiv 2505.15923 v1 pith:IVPYDEEN submitted 2025-05-21 astro-ph.GA

Silvia Belladitta , Eduardo Bañados , Zhang-Liang Xie , Roberto Decarli , Silvia Onorato , Jinyi Yang , Manuela Bischetti , Masafusa Onoue
show 13 more authors
Federica Loiacono Laura N. Martínez-Ramírez Chiara Mazzucchelli Frederick B. Davies Julien Wolf Jan-Torge Schindler Xiaohui Fan Feige Wang Fabian Walter Tatevik Mkrtchyan Daniel Stern Emanuele P. Farina Bram P. Venemans
This is my paper · ORCID
classification astro-ph.GA
keywords high-redshiftquasarssupermassiveblackholesbroadabsorptionlinesradio-loudquasaroutflowsLyman-breakselectionholemassesearlyUniverse
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 aims to expand the sparse census of luminous quasars shining when the universe was less than roughly a billion years old. It reports the spectroscopic confirmation of 25 new quasars at $4.6

What carries the argument

The load-bearing machinery is a set of dropout color selections that separate high-redshift quasar candidates from the main contaminants (ultracool dwarfs and low-redshift galaxies), followed by optical and near-infrared spectroscopy and template fitting to assign redshifts. The central frame for the physical measurements is the MgII broad emission line, which anchors the systemic redshift; CIV is then compared with MgII to measure outflow shifts, and single-epoch virial scaling relations convert the line widths and continuum luminosities into black hole masses. The CIV full-width-at-half-maximum is blueshift-corrected before the mass estimate, and velocity shifts follow from $(z_{\rm CIV}-z_{\rm MgII})/(1+z_{\rm MgII})$ times $c$.

What would settle it

A high-signal-to-noise, high-resolution spectrum of PSO J041+06 that cleanly resolves both CIV and MgII, combined with a submillimeter detection of [CII] to pin the systemic velocity independently, would settle whether the roughly $9000$ km/s CIV-MgII shift is real or an artifact of the weak CIV line.

Watch

Extended reading notes

Core claim

The paper's central claim is that 25 objects previously listed only as candidate quasars are genuine quasars, established through optical and near-infrared spectroscopy that detects the Lyman-$\alpha$ break and broad emission lines. The newly confirmed sources span $M_{1450}$ from $-25.4$ to $-27.0$, with six at $z\geq 6.5$; three are strong radio emitters with 1.4 GHz luminosities of $0.09$--$1.0\times 10^{34}\,\mathrm{erg\,s^{-1}\,Hz^{-1}}$ and radio-loudness between roughly 30 and 850. For seven quasars at $6.3<z<6.9$, the paper presents near-infrared spectra of CIV and MgII, uses single-epoch virial scaling relations to estimate black hole masses of $\log(M_{\rm BH}/M_\odot)=8.58$--$9.14$ and Eddington ratios of 0.74--2.2, and identifies PSO J041+06 as a weak-line quasar with an extreme $\sim 9000\,\mathrm{km\,s^{-1}}$ CIV-MgII blueshift. It also classifies three sources as high-ionization broad absorption line quasars, one with a possible absorbing outflow reaching $48000\,\mathrm{km\,s^{-1}}$, and reports a blazar-like radio spectrum, variability, and X-ray detection for PSO J200-13.

Load-bearing premise

The analysis assumes that the gas producing the magnesium emission line, not the carbon line, sits at the quasar's true rest velocity; if that gas is itself streaming away, or if the faint carbon line in one quasar is measured incorrectly, the headline outflow speed and the black hole masses would change.

Editorial extensions

If this is right

  • The six new $z\geq 6.5$ quasars enlarge the small set of luminous sources available for studying black hole accretion and reionization within the first billion years.
  • PSO J200-13, if confirmed as a blazar at $z=4.71$, provides a rare Earth-aligned jet in the early Universe with an X-ray counterpart and multi-frequency radio variability.
  • PSO J041+06 joins the rare class of weak-line quasars with a wind-dominated broad-line region at $z>6$, with the largest CIV-MgII shift currently known at those redshifts.
  • The three new high-ionization BAL quasars, including a possible $48000\,\mathrm{km\,s^{-1}}$ outflow in PSO J067-14, add direct constraints on powerful quasar winds and feedback in the early Universe.

Reading between the lines

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

  • If the color selections presented here prove as efficient as they appear, combining surveys with different filter responses could systematically recover quasars that sit just below the traditional Lyman-break color cuts.
  • If the MgII-based Eddington ratios near or above unity hold for the whole sample, super-Eddington accretion may be common among the most luminous $z>6$ quasars, which would ease theoretical timelines for assembling billion-solar-mass black holes within 0.7 Gyr.
  • A confirmed $48000\,\mathrm{km\,s^{-1}}$ absorbing outflow would be one of the fastest known and a strong test for radiation-driven wind models, which struggle to accelerate gas to such speeds.
  • Because most of the new quasars lie in the southern sky, they are immediate targets for submillimeter and future radio facilities to measure host-galaxy properties and surrounding gas.
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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

1 major / 6 minor

Summary. The paper reports the discovery and spectroscopic confirmation of 25 new quasars at 4.6<z<6.9, selected from multi-band optical, near-infrared, and radio surveys. It presents photometry and redshifts for all objects (Tables 2, A.1, A.2), including six quasars at z>=6.5, three radio-loud sources, and one candidate blazar (PSO J200-13). For a subsample of seven z>6.3 quasars it provides NIR spectroscopy, CIV and MgII line measurements, single-epoch black hole masses, and Eddington ratios. The paper also reports BAL features, a potential extreme CIV outflow in PSO J041+06, and a candidate 48000 km/s BAL in PSO J067-14.

Significance. The catalog itself is a valuable contribution to the high-redshift quasar sample: 25 new spectroscopically confirmed quasars with complete photometry, a documented list of 73 rejected contaminants, and a clear description of the selection methods. The MgII-based redshifts for two sources are checked against [CII] redshifts (PSO J037-08 and PSO J067-14), which lends credibility to the redshift scale. The radio-loud classification and blazar candidacy of PSO J200-13 are supported by multi-frequency radio data, variability, and an eROSITA detection. The paper's main intrinsic weakness is the emphasis on the ~9000 km/s CIV-MgII shift in PSO J041+06, which relies on a weak, low-S/N CIV line; this does not affect the discovery claim but does affect the physical interpretation presented as a headline result.

major comments (1)
  1. [Abstract; Sect. 5.1, Eq. (1)] The abstract states that PSO J041+06 shows a CIV-MgII velocity difference of approximately 9000 km/s and is 'one of the most extreme CIV outflows currently known,' yet the measurement rests on the peak redshift of a weak (REW about 6 A), low-S/N CIV line and on the assumption that MgII defines the systemic frame. The paper itself acknowledges in Sect. 5.1 that the CIV properties are uncertain and require higher S/N and resolution, but the abstract and Sect. 6 present the shift as an established result. This internal inconsistency should be fixed by qualifying the claim as tentative in the abstract and summary, and ideally by adding a brief statement of how the shift depends on continuum placement and possible MgII offsets.
minor comments (6)
  1. [Abstract] The abstract states 'Their masses (log[M_BH,MgII]=8.58-9.14) and Eddington ratios (lambda_Edd,MgII=0.74-2.2)', but Table 6 for the seven NIR-spectroscopy quasars gives log M_BH,MgII = 8.58-9.31 and lambda_Edd,MgII = 0.25-2.18. Please correct the ranges or specify the subset used.
  2. [Sect. 3.1] There is a typo 'ouwith' that should read 'with'.
  3. [Table C.3] The entry 'PSO254+25' is missing the 'J' and should be 'PSO J254+25' for consistency with the naming convention used throughout.
  4. [Sect. 2.4] The acronym appears as 'ALLWISE' here but as 'AllWISE' elsewhere in the paper; please standardize the spelling.
  5. [Sect. 2.5] The text cites 'Wolf J. et al. (2024)' while the reference list contains Wolf, J., Salvato, M., Belladitta, S., et al. 2024b; please disambiguate with the year-letter suffix.
  6. [Sect. 4.1.2] The subsection heading 'PSO J037-08, z = 6.725' omits the uncertainty that is given in Table 2 (6.725 +/- 0.002); adding it would improve consistency.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the 25-quasar catalog, redshifts, black-hole masses, and CIV-MgII shift rest on external templates, published scaling relations, and direct line measurements rather than on fitted inputs or self-citation chains.

full rationale

The paper's central claim is the spectroscopic discovery and characterization of 25 quasars, and this claim is self-contained observational work. Redshifts are obtained by chi-square template matching against four published composite quasar spectra (Bañados et al. 2016; D'Odorico et al. 2023; Onorato et al. 2025), and for seven sources from MgII line fits that are independently checked against [CII] redshifts for two objects (PSO J037−08: consistent to 4 ± 78 km/s; PSO J067−14: 359 ± 85 km/s), which is an external validation rather than a circular reference. The MgII black-hole masses use the Vestergaard & Osmer (2009) scaling relation and the CIV masses use Vestergaard & Peterson (2006) with the Coatman et al. (2017) blueshift correction; these are literature calibrations with external scatter estimates, not parameters fitted in this paper, so the masses are not predictions of fitted inputs. The ~9000 km/s CIV-MgII shift is the direct difference of two measured line redshifts computed with Eq. (1), and the paper explicitly labels the low-S/N CIV measurement as uncertain and requiring higher-quality data, which is a disclosed data-quality caveat rather than a circular step. The MgII-as-systemic assumption is a standard physical interpretation and a correctness risk, not a definitional equivalence. Selection procedures are cited from the authors' prior papers (Belladitta et al. 2023; Bañados et al. 2023; Wolf J. et al. 2024), but those are published, externally usable methods with stated photometric cuts, and no uniqueness theorem or unverified ansatz is imported to force the conclusions. No equation in the paper reduces to its own input, and no fitted parameter is renamed as a prediction.

Assumptions & free parameters 1 free parameters · 6 assumptions · 0 invented entities

The central claim does not rest on newly invented parameters. It uses standard single-epoch scaling relations, a fixed bolometric correction, and assumed spectral slopes from the literature; one radio spectral index is assumed for PSO J164+29 rather than measured. These are transparent inputs, not hidden fits.

free parameters (1)
  • Assumed radio spectral index for PSO J164+29 = 0.29 (assumed, not measured)
    Used to convert 144 MHz flux to rest-frame 5 GHz for the radio-loudness estimate R=21+/-10; the paper states R depends strongly on this assumption (Sect. 4.1.9).
assumptions (6)
  • domain assumption MgII single-epoch virial scaling relation (Vestergaard & Osmer 2009)
    Used in Eq. (2) to compute black hole mass from FWHM(MgII) and lambda L_lambda(3000 A); calibrated on lower-redshift quasars and carries 0.55 dex scatter.
  • domain assumption CIV scaling relation (Vestergaard & Peterson 2006) with Coatman et al. (2017) correction
    Used in Eqs. (3) and (4) for CIV-based masses; the correction for CIV blueshift is empirical and calibrated on lower-z samples.
  • domain assumption Bolometric luminosity correction Lbol = 5.15 x lambda L_lambda(3000 A)
    From Shen et al. (2008); used to compute Eddington ratios in Sect. 5.2.
  • domain assumption Rest-frame UV continuum slope alpha_nu = 0.44
    From Vanden Berk et al. (2001); used to extrapolate m1450 from z-band magnitudes and to compute rest-frame 4400 A flux densities for radio-loudness.
  • domain assumption MgII traces systemic redshift for the seven quasars with NIR spectra
    Underpins the CIV-MgII velocity shifts and the MgII black hole masses; the paper discusses this assumption in Sect. 5.1 and Sect. 5.2.
  • domain assumption Quasar composite templates used for Ly-alpha based redshifts are representative
    Templates from Banados et al. (2016), D'Odorico et al. (2023), and Onorato et al. (2025); adopted redshift uncertainty of 0.03 from template fitting.

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Pith. "Pith review of Discovery and characterization of 25 new quasars at 4.6 < z < 6.9 from wide-field multi-band surveys." pith.science (2026). https://pith.science/paper/IVPYDEEN

@misc{pith2026250515923,
  author       = {Pith},
  title        = {Pith review of: Discovery and characterization of 25 new quasars at 4.6 < z < 6.9 from wide-field multi-band surveys},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/IVPYDEEN}},
  note         = {Machine review of arXiv:2505.15923}
}
abstract

Luminous quasars at $z>4$ provide key insights into the early Universe. Their rarity necessitates wide-field multi-band surveys to efficiently separate them from the main astrophysical contaminants (i.e., ultracool dwarfs). To expand the sample of high-$z$ quasars, we conducted targeted selections using optical, infrared, and radio surveys, complemented by literature-based quasar candidate catalogs. In this paper, we report the discovery of \nqsos\ new quasars at $4.6<z<6.9$ (six at $z\geq6.5$), with $M_{1450}$ between $-$25.4 and $-$27.0. We also present new spectra of six $z>6.5$ quasars we selected, but whose independent discovery has already been published in the literature. Three of the newly discovered quasars are strong radio emitters (L$_{1.4~\rm GHz}$$=0.09-1.0\times$10$^{34}$erg s$^{-1}$ Hz$^{-1}$). Among them, one source at $z=4.71$ exhibits typical blazar-like properties, including a flat radio spectrum, radio-loudness $\sim$1000, and multi-frequency variability. It is also detected by SRG/eROSITA X-ray telescope (f$_{\rm 0.2-2.3keV} \sim 1.3\times10^{-13}$erg s$^{-1}$ cm$^{-2}$). In addition, for seven $6.3<z<6.9$ quasars we present near-infrared spectroscopy and estimate the central black hole mass from their C$\rm IV$ and Mg$\rm II$ broad emission lines.Their masses (log[M$_{\rm BH,MgII}$]$=8.58-9.14~\rm M_{\odot}$) and Eddington ratios ($\lambda_{\rm Edd,MgII}=0.74-2.2$) are consistent with other $z>6$ quasars reported in the literature. A $z = 6.3$ quasar exhibits a velocity difference of approximately $9000$ km s$^{-1}$ between the C$\rm IV$ and Mg$\rm II$ emission lines, making it one of the most extreme C$\rm IV$ outflows currently known. Additionally, the sample includes three high-ionization broad absorption line quasars. One of these quasars shows potential evidence of an extremely fast outflow feature, reaching $48000$ km s$^{-1}$.

Figures

Figures reproduced from arXiv: 2505.15923 by the authors.

Figure 1
Figure 1. Redshift vs. zP1 − zDE (bottom) and zDE − yP1 (top) colors. The blue, black, and red solid lines represent the color tracks of composite quasar spectra from Bañados et al. (2016), illustrating weak, average, and strong Lyα emission lines, respectively. The dotted lines indicate the color cuts for the [DELS+PS1] selection, as described in Section 2.2. The red circles represent quasars that meet the selection criteria… view at source ↗
Figure 2
Figure 2. Newly discovered spectra (25 sources, ∗ marked radio-loud objects) and new spectra publication (6 objects, marked with a ⋆) for the quasars reported in this paper. Only the part of the spectrum that covers the Lyman-α break is shown here. The noise spectrum is reported in gray. Sorted by increasing redshift. [CII]-based redshift and the one computed in this work from the MgII line (6.705±0.002, see [PITH_FULL_IMAGE… view at source ↗
Figure 3
Figure 3. NIR follow-up spectra of a sub-sample of quasars reported in this paper (sorted by increasing redshift). We show the NIR spectra of the newly discovered quasars PSO J041+06, PSO J335−15, PSO J067−14, PSO J217+04, PSO J037−08 and PSO J289+50 and the newly published NIR spectrum for the already known quasar PSO J162−01. The noise spectra are reported in gray. Shaded light gray areas highlight regions strongly affected… view at source ↗
Figures from the paper (4 more)
Figure 4
Figure 4. Figure 4: Radio flux densities as a function of the observed (bottom x-axis) and rest-frame (top x-axis) frequency of MQC J021+19 (left), MQC J133−02 (central), and PSO J200−13 (right). The corresponding radio surveys are shown in the legend. Due to the potential flux density va…
Figure 5
Figure 5. Figure 5: Normalised spectrum of PSO J067−14, smoothed to 500 km s−1 . The velocity axis in each panel is relative to the rest-frame wavelength of the ionic species indicated by the label. Vertical solid, dashed, dotted and dashed-dotted lines indicate the velocity associated wi…
Figure 6
Figure 6. Figure 6: Close-up views of the spectral fit of the CIV and MgII BELs. The orange curves depict the fitted models, comprising Gaussian components for the emission lines and a continuum model (see text for details). The transparent blue vertical line indicates the position of the…
Figure 7
Figure 7. Figure 7: CIV EW as a function of the CIV–MgII velocity shift for the quasars analyzed in this work. Dark blue triangles represent z > 5.7 quasars from Shen et al. (2019), Schindler et al. (2020) and Yang et al. (2021), while light blue stars shows the WLQs samples of Wu et al. …

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Pith tools

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