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arxiv: 2606.05312 · v1 · pith:QSJW2P7Lnew · submitted 2026-06-03 · 🌌 astro-ph.HE · astro-ph.GA

The WISSHFUL program: the highest redshift UFO discovered in a non-lensed QSO

G. Lanzuisi , L. Borrelli , E. Piconcelli , G. Chartas , A. Luminari , J. Reeves , V. Braito , E. Bertola
show 23 more authors
S. Bianchi A. Comastri M. Brusa C. Vignali F. Vito S. Marchesi M. Cappi M. Dadina L. Zappacosta A. Tortosa M. Bischetti G. Vietri F. Salvestrini G. Bruni M. Fanelli E. Kammoun X. Zhao G. Matzeu F. Tombesi A. Marinucci M. Gaspari T. Misawa D. Stern
This is my paper

Pith reviewed 2026-06-28 04:46 UTC · model grok-4.3

classification 🌌 astro-ph.HE astro-ph.GA
keywords quasarsultra-fast outflowsX-ray spectroscopyhigh-redshift AGNblack-hole feedbackcosmic noonactive galactic nuclei
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The pith

X-ray observations detect ultra-fast outflows in the highest-redshift non-lensed quasar

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

The WISSHFUL program uses XMM-Newton to observe luminous quasars at cosmic noon. For WISSH13 at redshift 3.294, joint XMM-Newton and NuSTAR data yield the highest-quality broadband X-ray spectrum yet obtained for a non-lensed quasar at this distance. Continuum modeling gives a soft photon index near 2, reflection fraction 1.4-1.8, and cutoff energy 60-80 keV. Two absorption features at 7.5 and 10 keV rest-frame are identified as blueshifted highly ionized iron lines, revealing a stratified ultra-fast outflow with components at 0.1c and 0.3c. Each component shows a mass outflow rate of 20 solar masses per year and kinetic power that is 1% or 10% of the quasar's bolometric luminosity, fractions comparable to those measured in lower-redshift active galaxies.

Core claim

The central claim is the detection of two significant absorption features at ∼7.5 and ∼10 keV rest-frame, interpreted as a blueshifted blend of Fe XXV Heα and Fe XXVI Lyα, indicating two kinematic components of a highly ionized, high-column ultra-fast outflow with velocities ∼0.1c and ∼0.3c. The slower component is seen in both 2017 and 2024 data while the faster one appears only in 2024; each carries a mass outflow rate ∼20 M⊙ yr⁻¹ (15% of the accretion rate) and kinetic power of order 1% or 10% of bolometric luminosity.

What carries the argument

Blueshifted absorption lines of highly ionized iron (Fe XXV and Fe XXVI) that trace the velocity, ionization, and column of the two ultra-fast outflow components.

If this is right

  • The slower wind component persists across multiple years while the faster component varies on year timescales.
  • Each outflow component expels mass at a rate corresponding to 15% of the black-hole accretion rate.
  • The kinetic power injected by the winds is 1% and 10% of the quasar's bolometric luminosity.
  • These relative kinetic-power fractions are similar to those measured in lower-redshift AGN.
  • The detection extends the study of ultra-fast outflows to the peak epoch of quasar activity at cosmic noon.

Where Pith is reading between the lines

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

  • If outflows with these properties are common at z∼3, they could supply the mechanical feedback needed to regulate star formation in massive galaxies during the era when most black-hole growth occurred.
  • The observed variability between epochs suggests the wind structure changes on timescales of years, which could be mapped with repeated observations.
  • The low coronal temperature implied by the cutoff energy may be a signature of super-Eddington accretion disks and could be tested against disk-corona models.

Load-bearing premise

The absorption features at ∼7.5 and ∼10 keV are correctly identified as blueshifted highly ionized iron lines from an outflow rather than other spectral components, instrumental effects, or modeling artifacts.

What would settle it

A new broadband X-ray observation with comparable or better signal-to-noise that shows no significant absorption features at the reported rest-frame energies would falsify the ultra-fast outflow detection.

Figures

Figures reproduced from arXiv: 2606.05312 by A. Comastri, A. Luminari, A. Marinucci, A. Tortosa, C. Vignali, D. Stern, E. Bertola, E. Kammoun, E. Piconcelli, F. Salvestrini, F. Tombesi, F. Vito, G. Bruni, G. Chartas, G. Lanzuisi, G. Matzeu, G. Vietri, J. Reeves, L. Borrelli, L. Zappacosta, M. Bischetti, M. Brusa, M. Cappi, M. Dadina, M. Fanelli, M. Gaspari, S. Bianchi, S. Marchesi, T. Misawa, V. Braito, X. Zhao.

Figure 1
Figure 1. Figure 1: Panel a shows the best-fit PEX model with the full XMM￾Newton and NuSTAR data set. pn and MOS1+2 data are shown with different colors for each observation, identified by its name. The reflection-only component is shown in black. Panels b, c, and d, show residuals for the PL, CPL and PEX models, respectively. Residuals for the REFL and CREFL models are not shown for clarity, as they are indistinguishable fr… view at source ↗
Figure 2
Figure 2. Figure 2: Top row: Confidence contours for the PEX model, [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 4
Figure 4. Figure 4: Rest-frame equivalent widths for WISSH13 (orange and [PITH_FULL_IMAGE:figures/full_fig_p006_4.png] view at source ↗
Figure 3
Figure 3. Figure 3: Blind line scans over the 5–12 keV rest frame band. The [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figure 5
Figure 5. Figure 5: Confidence contours (at 68, 90, 99% confidence levels) for [PITH_FULL_IMAGE:figures/full_fig_p007_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Redshift contours from the fit with xstar tables with vturb = 5000, km,s −1 , for UFO1 (left) and UFO2 (right). The horizontal green lines mark the 68, 90, and 99% confidence levels. The 90% constraints on z are converted to vout values quoted in the red labels (see text for details). importance and power of long, dedicated spectroscopic campaigns in high-z QSOs to go beyond the detection of the most extre… view at source ↗
Figure 7
Figure 7. Figure 7: UFO energetics for WISSH13 and literature samples: local Seyferts (T10, blue diamonds), low-z QSOs from SUBWAYS [PITH_FULL_IMAGE:figures/full_fig_p008_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Momentum rate vs. velocity of different outflow phases [PITH_FULL_IMAGE:figures/full_fig_p009_8.png] view at source ↗
read the original abstract

We present the first results from the WISSHFUL program, an XMM-Newton heritage program targeting luminous QSOs at Cosmic Noon. We report on recent simultaneous XMM-Newton and NuSTAR observations of the Super-Eddington accreting quasar WISSH13 at z=3.294, which provide the highest quality broadband X-ray spectrum to date for a non-lensed QSO at this redshift. Physical modeling of the continuum reveals a soft photon index ($\Gamma\sim2$) and strong reflection ($R\sim1.4-1.8$), despite the weak narrow Fe emission, and a low high-energy cut-off ($E_{cut}\sim60-80$ keV, $kTe = 15-20$ keV, depending on the model adopted). Most notably, we detect two significant (at $96.7\%$ and $98.9\%$ confidence level, respectively) absorption features at $\sim7.5$ and $\sim10$ keV rest-frame, interpreted as a blueshifted blend of Fe XXV He$\alpha$ and Fe XXVI Ly$\alpha$. These features indicate the presence of two kinematic components of a highly ionized, high column Ultra-Fast Outflow (UFO) with a velocity of $v_{out}\sim0.1c$ and $v_{out}\sim0.3c$, respectively. The slower wind is consistently detected in an archival 2017 XMM-Newton observation, whereas the faster wind is detected only in 2024. This stratified and variable wind exhibits extreme energetics, with a mass outflow rate of $\dot{M}_{out}\sim20M_{\odot}/yr$ (corresponding to $15\% \dot{M}_{acc}$) for each component, and a kinetic power of the order of $\sim1$ and $\sim10\%$ of the bolometric luminosity, respectively. While this represents one of the most powerful UFOs ever detected, its kinetic power is a similar fraction of the QSO's bolometric luminosity compared to lower-redshift AGN. We present several theoretical frameworks to explain the peculiar accretion and ejection properties of this remarkable QSO at 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 reports simultaneous XMM-Newton and NuSTAR observations of the z=3.294 quasar WISSH13 from the WISSHFUL program. It claims detection of two absorption features at ~7.5 keV and ~10 keV (rest-frame) at 96.7% and 98.9% confidence, interpreted as blueshifted Fe XXV Heα and Fe XXVI Lyα from a stratified UFO with v_out ~0.1c and ~0.3c. Continuum modeling yields Γ~2, R~1.4-1.8, E_cut~60-80 keV; derived outflow properties include Ṁ_out~20 M_⊙ yr⁻¹ per component (~15% of Ṁ_acc) and kinetic powers ~1% and ~10% of L_bol. The faster component appears only in the 2024 epoch.

Significance. If the line identifications hold after rigorous statistical tests, the result would establish the highest-redshift non-lensed UFO detection and demonstrate that extreme outflow energetics are already in place at Cosmic Noon with fractions of L_bol comparable to lower-redshift AGN. The XMM+NuSTAR broadband coverage for an unlensed z>3 source is a technical strength, as is the reported epoch-to-epoch variability.

major comments (3)
  1. [Abstract and spectral fitting section] Abstract and spectral fitting section: the reported 96.7% and 98.9% confidence levels correspond to marginal (~2σ) detections. The manuscript must supply Monte-Carlo-derived false-alarm probabilities that incorporate the look-elsewhere effect across the full 5–15 keV search window and the discrete choices of reflection model and cutoff energy.
  2. [Physical modeling section] Physical modeling section: the continuum is parameterized by Γ≈2, R≈1.4–1.8 and E_cut≈60–80 keV. No contour plots or alternative-model tests are described to quantify possible degeneracies between these parameters and the narrow absorption residuals; such tests are required to confirm that the features are not artifacts of continuum mismatch.
  3. [Outflow energetics paragraph] Outflow energetics paragraph: Ṁ_out~20 M_⊙ yr⁻¹ and the quoted kinetic powers assume specific values for ionization parameter, covering fraction and launch radius. The paper should state how these quantities are constrained by the X-ray data alone and propagate the resulting uncertainties into the reported percentages of L_bol.
minor comments (2)
  1. [Abstract] Abstract: the exact statistical method used to obtain the 96.7% and 98.9% confidence levels (Δχ², F-test, etc.) is not stated and should be specified.
  2. [Figures and text] Figure captions and text: ensure all energies are consistently quoted in the rest frame and that residual plots are shown with the same energy scale as the data/model panels.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for the constructive comments on our manuscript. We address each major point below and will incorporate revisions to strengthen the statistical and modeling sections as outlined.

read point-by-point responses

  1. Referee: [Abstract and spectral fitting section] Abstract and spectral fitting section: the reported 96.7% and 98.9% confidence levels correspond to marginal (~2σ) detections. The manuscript must supply Monte-Carlo-derived false-alarm probabilities that incorporate the look-elsewhere effect across the full 5–15 keV search window and the discrete choices of reflection model and cutoff energy.

    Authors: We agree that the detections are marginal and that a rigorous assessment of the false-alarm probability is required. In the revised manuscript we will add Monte Carlo simulations that scan the full 5–15 keV band and vary the reflection model and cutoff energy to properly account for the look-elsewhere effect. revision: yes

  2. Referee: [Physical modeling section] Physical modeling section: the continuum is parameterized by Γ≈2, R≈1.4–1.8 and E_cut≈60–80 keV. No contour plots or alternative-model tests are described to quantify possible degeneracies between these parameters and the narrow absorption residuals; such tests are required to confirm that the features are not artifacts of continuum mismatch.

    Authors: We recognize the need to demonstrate that the absorption lines are robust against continuum degeneracies. The revised version will include contour plots of Γ, R and E_cut together with fits using alternative reflection models to show that the residuals at ~7.5 and ~10 keV persist. revision: yes

  3. Referee: [Outflow energetics paragraph] Outflow energetics paragraph: Ṁ_out~20 M_⊙ yr⁻¹ and the quoted kinetic powers assume specific values for ionization parameter, covering fraction and launch radius. The paper should state how these quantities are constrained by the X-ray data alone and propagate the resulting uncertainties into the reported percentages of L_bol.

    Authors: The ionization parameter is constrained by the observed line centroid energies and the lack of lower-ionization absorption in the spectrum. Covering fraction and launch radius, however, rely on standard UFO assumptions. We will explicitly state these constraints and assumptions in the revised text and propagate the associated uncertainties into the reported Ṁ_out and kinetic-power fractions. revision: partial

Circularity Check

0 steps flagged

No circularity: purely observational line detection from new X-ray data

full rationale

The paper reports XMM-Newton + NuSTAR spectral fitting on fresh observations of WISSH13, identifying two absorption features at ~7.5 and ~10 keV rest-frame and converting their energies to outflow velocities via the standard relativistic Doppler formula. No parameter is fitted to a subset of the data and then re-labeled as a prediction; no self-citation supplies a uniqueness theorem or ansatz that the present analysis depends upon; the continuum model (power-law + reflection + cutoff) is chosen from standard XSPEC components and the line identifications are presented as an interpretation of the residuals rather than a quantity forced by the fit itself. The claimed velocities and energetics are therefore independent outputs of the data reduction, not reductions of the inputs by construction.

Axiom & Free-Parameter Ledger

5 free parameters · 2 axioms · 0 invented entities

The claim rests on standard X-ray spectral modeling assumptions and line identifications for UFOs; several continuum and wind parameters are fitted to the data.

free parameters (5)
  • outflow velocities = 0.1c and 0.3c
    Fitted from the observed energies of the absorption features
  • photon index Gamma = ~2
    Fitted from continuum modeling
  • reflection fraction R = 1.4-1.8
    Fitted from physical modeling
  • high-energy cutoff E_cut = 60-80 keV
    Fitted from modeling
  • mass outflow rate = ~20 M_sun/yr per component
    Derived from fitted column, velocity, and ionization
axioms (2)
  • domain assumption Standard AGN X-ray continuum and reflection models apply at z=3.294
    Used to interpret the broadband spectrum and derive physical parameters
  • domain assumption Absorption features originate from blueshifted highly ionized Fe in an outflow
    Central interpretation linking the 7.5 and 10 keV features to UFO components

pith-pipeline@v0.9.1-grok · 6099 in / 1737 out tokens · 21399 ms · 2026-06-28T04:46:16.935678+00:00 · methodology

discussion (0)

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