GA-NIFS: AGN activity in a Ly{\alpha} emitter within a triple-AGN system anchored by a passive galaxy at z=3

Bruno Rodr\'iguez Del Pino; Elena Bertola; Francesco D'Eugenio; Giacomo Venturi; Giovanni Cresci; Hannah \"Ubler; Isabella Lamperti; J. Andrew Bunker; Mahmoud Hamed; Michele Ginolfi

REVIEW 2 major objections 4 minor 3 references

LAE2, a faint Lyα emitter 30 kpc from the quenched galaxy GS10578 at z≈3, is an active galactic nucleus, making the system a compact triple-AGN environment.

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

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2026-08-03 12:54 UTC pith:UWAOFF33

load-bearing objection The paper adds real rest-frame optical evidence for an AGN in LAE2 and a plausible scattering interpretation for LAE1, but the headline HeII/Hβ lower limit is weakened by an unquantified aperture mismatch; other evidence supports the AGN claim. the 2 major comments →

arxiv 2601.00960 v1 pith:UWAOFF33 submitted 2026-01-02 astro-ph.GA

GA-NIFS: AGN activity in a Ly{α} emitter within a triple-AGN system anchored by a passive galaxy at z=3

Michele Perna , Santiago Arribas , Mahmoud Hamed , Francesco D'Eugenio , J. Andrew Bunker , Stefano Carniani , St\'ephane Charlot , Roberto Maiolino

show 10 more authors

Bruno Rodr\'iguez Del Pino Hannah \"Ubler Torsten B\"oker Elena Bertola Giovanni Cresci Isabella Lamperti Giacomo Venturi Michele Ginolfi Montserrat Villar Mart\'in Sandra Zamora

This is my paper

classification astro-ph.GA

keywords active galactic nucleiLyα emittershigh-redshift galaxiesquiescent galaxiesmultiple AGNJWST NIRSpec IFUHeII emission linesblack hole growth

verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

The paper is trying to establish that LAE2, a low-mass Lyα emitter in the vicinity of the massive quiescent galaxy GS10578, is powered by an AGN rather than by star formation. The key evidence combines a MUSE detection of UV HeIIλ1640 with new JWST/NIRSpec optical Hβ: using the recombination ratio HeIIλ1640/λ4687 = 6.47, the authors derive a lower limit HeIIλ4687/Hβ > 0.16, which falls in the AGN-only region of the HeII/Hβ versus [NII]/Hα diagnostic plane. With the previously known AGN in GS10578 (AGN-A) and the AGN in a close satellite (AGN-B), the system then hosts three AGN within roughly 30 kpc. The paper further argues that the companion LAE1, detected only in Lyα, is not an independent galaxy but likely traces resonantly scattered Lyα light from LAE2. If correct, this shows that black-hole growth and gas accretion can continue around a massive galaxy long after its own star formation has ceased.

Core claim

LAE2's ionized gas is powered by an AGN. Although HeIIλ4687 and [NII] are not directly detected in the new NIRSpec data, the detected MUSE HeIIλ1640 flux, converted through the recombination ratio HeIIλ1640/λ4687 = 6.47, implies HeIIλ4687/Hβ ≥ 0.16. This lower limit places LAE2 in the AGN-only region of the HeII/Hβ versus [NII]/Hα diagnostic diagram, beyond what pure stellar photoionization can produce. Since GS10578 already hosts one AGN and a close satellite hosts a second, LAE2 completes a triple-AGN system within ~30 kpc. In addition, LAE1 shows only broad asymmetric Lyα, no continuum, and no optical nebular lines; its Lyα profile closely matches that of LAE2, suggesting that LAE1 is res

What carries the argument

The central tool is the recombination ratio of the HeII lines, HeIIλ1640/λ4687 = 6.47 at Te ≈ 10^4 K and ne ≈ 100 cm^-3. Multiplying the MUSE-measured UV HeIIλ1640 flux by 1/6.47 and dividing by the NIRSpec Hβ flux converts the UV detection into an optical HeII/Hβ lower limit. On the HeII/Hβ versus [NII]/Hα plane this lower limit sits above an empirical AGN/star-forming demarcation, in a region that stellar photoionization cannot populate. The same recombination assumption also anchors the Lyα escape-fraction estimates, while a comparison of the Lyα spectral profiles of LAE1 and LAE2 provides the kinematic argument that LAE1 is scattered emission.

Load-bearing premise

The AGN classification rests on combining the MUSE HeIIλ1640 flux measured at 0.7″ resolution with the NIRSpec Hβ flux from a 0.15″ aperture with no relative aperture bias, and on the assumption that the local empirical AGN/star-forming boundary on the HeII diagram still holds for low-metallicity gas at z≈3.

What would settle it

A deep NIRSpec spectrum that resolves HeIIλ4687 at the same aperture as Hβ: if it yields log(HeIIλ4687/Hβ) < −0.80 after accounting for dust, or if spatially resolved MUSE data show that HeIIλ1640 is extended well beyond the region traced by Hβ, then the AGN-only placement would fail. A direct detection of an X-ray or radio counterpart to LAE2 would instead confirm the claim.

Watch this falsifier. Get emailed when new claim-graph text bears on it.

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If this is right

The GS10578 system contains three active nuclei within ~30 kpc, one of the most compact multi-AGN environments known at z>3.
LAE1 is most plausibly resonantly scattered Lyα emission from LAE2, not an independent galaxy, implying that Lyα-only sources around quenched galaxies may trace circumgalactic gas rather than in-situ star formation.
Black-hole growth and gas accretion can continue in low-mass satellites and nearby gas-rich structures even while the massive central galaxy has been quenched for ~0.5 Gyr.
A low-mass galaxy at z≈3, with stellar mass near 10^7.8 M☉, can host an AGN whose hard ionizing spectrum is revealed by HeII lines.
The quenched host GS10578 sits in a gas-rich, dynamically active environment, suggesting that quenching of the central galaxy does not require a quiescent large-scale environment.

Where Pith is reading between the lines

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

Editorial extension: if the HeII-based AGN identification holds, it implies that low-mass galaxies at z≈3 can grow black holes efficiently in dense environments, an important constraint for early SMBH seeding and hierarchical assembly models.
Editorial extension: the aperture matching between MUSE HeIIλ1640 (0.7″ PSF) and NIRSpec Hβ (0.15″ aperture) is the main systematic uncertainty; future PSF-matched or spatially resolved measurements of HeIIλ4687 with NIRSpec would directly test the AGN classification.
Editorial extension: a deep X-ray or radio observation of LAE2 could independently confirm the AGN and measure its accretion luminosity, since the source is radio-quiet and currently lacks direct continuum AGN detection.
Editorial extension: the Ciii] upper limit for LAE1 leaves room for an extremely low-mass stellar component; deeper rest-UV spectroscopy could distinguish between a purely scattered Lyα halo and a faint galaxy.

Editorial analysis

A structured set of objections, weighed in public.

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

Desk Editor's Note

The paper adds real rest-frame optical evidence for an AGN in LAE2 and a plausible scattering interpretation for LAE1, but the headline HeII/Hβ lower limit is weakened by an unquantified aperture mismatch; other evidence supports the AGN claim.

read the letter

Quick take: this is a solid observational paper that credibly confirms AGN activity in LAE2 and offers a plausible scattering origin for LAE1. The new NIRSpec IFU data are real, the analysis is generally careful, and the paper deserves a serious referee. But the sharpest claim — that the HeII/Hβ lower limit places LAE2 in a definite AGN-only region — is not as robust as written.

What is genuinely new: the first rest-frame optical detection of LAE2, with Hβ, [OIII], and Hα, the spatially resolved clumpy morphology and irregular kinematics, and the argument that LAE1 is dominated by resonantly scattered Lyα from LAE2 rather than in-situ star formation. The SED analysis with an explicit AGN component (fAGN ≈ 0.4) adds independent support. The paper is honest about the limits of the BPT at low metallicity and about the alternative interpretations for LAE1.

The soft spot is the construction of the HeII4687/Hβ lower limit in Sect. 4.1. The authors divide the MUSE HeII1640 flux (measured at 0.7″ PSF) by the NIRSpec Hβ flux from a 0.15″ aperture and call the result a lower limit because dust suppresses the UV line. But the aperture mismatch has the opposite potential bias: Table 1 shows Hα grows by roughly a factor of three between the 0.15″ and 0.5″ apertures. If Hβ grows similarly, the derived HeII4687/Hβ could drop from 0.16 to about 0.05, moving below the local AGN demarcation. The cited compactness of HeII1640 relative to Lyα does not settle this, since the comparison is not with Hβ in the same aperture. Calling the ratio a conservative lower limit is therefore not justified without quantifying the relative aperture correction.

That said, the AGN interpretation does not rest solely on this diagram. The high [OIII]/Hβ, the broad velocity dispersion, the UV line ratios from earlier MUSE work, and the SED AGN fraction all point the same direction. The HeII lower limit is supporting evidence, not the whole case. The paper should soften the word "definite" and add a matched-aperture estimate or an explicit treatment of the aperture uncertainty. The LAE1 scattering scenario is well argued, and the paper appropriately leaves a low-mass stellar population as an unexcluded alternative.

For a reader working on high-z AGN or quenched galaxies, this is a useful data point and a good example of how JWST and MUSE complement each other. I would send it to peer review with a request to address the aperture issue; the central conclusion will probably survive, but the paper will be stronger if the strongest diagnostic is put on firmer ground.

Referee Report

2 major / 4 minor

Summary. This paper reports new JWST/NIRSpec IFU observations (G235H/F170LP, 3.9 h) of two Lyα emitters, LAE1 and LAE2, near the quiescent galaxy GS10578 at z=3.064. LAE2 shows strong [OIII], Hβ, and Hα but no [NII], [SII], or HeII4687. By combining MUSE HeII1640 with NIRSpec Hβ from the r=0.15″ aperture, the authors derive HeII4687/Hβ > 0.16 and place LAE2 in the AGN-only region of the Shirazi & Brinchmann diagram, concluding that LAE2 hosts an AGN and that the system contains three AGN within ~30 kpc. LAE1 is detected only in Lyα; the authors argue its broad asymmetric Lyα profile and the similarity to LAE2’s Lyα profile favour a resonant-scattering interpretation powered by LAE2, while explicitly noting that a low-mass stellar population cannot be fully excluded. An SED fit with an AGN component gives log(M*/M⊙)=7.78, SFR≈0.13 M⊙/yr, and fAGN=0.40±0.17.

Significance. If the AGN classification of LAE2 is robust, the system represents a rare, compact triple-AGN environment around a massive quiescent galaxy at z>3, with implications for SMBH growth in dense environments and for feedback around quenched galaxies. The paper has clear strengths: new deep NIRSpec IFU data, integrated and spaxel-by-spaxel analyses, explicit flux and upper-limit tables, a quantitative SED analysis, and a careful attempt to distinguish scattering from in-situ star formation for LAE1. The scientific case is interesting and the data are appropriate. However, the central AGN claim currently rests on a single cross-aperture line-ratio construction whose systematic uncertainty is not bounded; this must be addressed before the classification can be considered established.

major comments (2)

[§4.1 and Table 1] The AGN-only classification is derived by combining the MUSE HeII1640 flux (PSF ~0.7″) with the NIRSpec Hβ flux from the r=0.15″ aperture. Table 1 shows that Hα grows by a factor ~3 between r=0.15″ (log L=41.24) and r=0.5″ (log L=41.72). If Hβ follows the same radial growth, the inferred HeII4687/Hβ drops from 0.16 to ~0.05 (log ≈ −1.3), which can fall below the Shirazi & Brinchmann AGN demarcation at the measured [NII]/Hα upper limit. The statement that HeII1640 is more compact than Lyα does not justify dividing a MUSE-integrated flux by a 0.15″ NIRSpec flux, nor is the result a conservative lower limit in the presence of this aperture mismatch. Please either use an aperture-matched Hβ measurement, or quantify the maximum allowable aperture correction and propagate it into the diagnostic placement, and state explicitly whether the conclusion changes.
[§4.1 / §5.1] The only diagnostic that places LAE2 in an unambiguous 'AGN-only' region is the local Shirazi & Brinchmann (2012) HeII4687/Hβ–[NII]/Hα diagram, applied to a low-metallicity (Z≈0.16 Z⊙) system at z≈3. The text notes that high-redshift systems differ from the local population, but does not quantify how the AGN/star-forming boundary shifts for low-metallicity, young stellar populations that can produce strong HeII. Since the central claim depends on this boundary, a quantitative check with photoionization or stellar-population models appropriate to the LAE2 SED would materially strengthen the paper. Without this, even after fixing the aperture issue, the classification retains an unquantified systematic uncertainty.

minor comments (4)

[Title page] The header dates 'Received September 15, 1996; accepted March 16, 1997' appear to be a template artifact and should be corrected or removed.
[Fig. 2] The axis labels show 'H' for the Balmer lines; please write Hβ and Hα explicitly, as is done in the text.
[Appendix A / §5.1] The SED-derived fAGN=0.40±0.17 is described as confirming the AGN contribution, but the SED fit explicitly includes an AGN component because the AGN is already assumed from §4. This is not an independent check and should be reframed as a consistency test, not additional evidence.
[§5.3] The equations in this section are not numbered. Also, Eq. (1) uses β for the UV spectral slope while the SED appendix uses different notation; please clarify and number the equations for easier reference.

Circularity Check

0 steps flagged

No significant circularity: LAE2 AGN classification rests on independent MUSE+NIRSpec line measurements and external calibrations.

full rationale

The paper's central claim (LAE2 hosts an AGN) is derived from a direct combination of an observed MUSE HeII1640 line and an observed NIRSpec Hβ line, converted with the external pyneb recombination ratio (HeII1640/4687=6.47) and compared with the external Shirazi & Brinchmann (2012) AGN/star-forming boundary. No parameter is fitted to the target classification and then re-predicted: the HeII4687/Hβ lower limit is a measurement under stated assumptions (dust preferentially suppresses UV). The aperture mismatch concern (MUSE 0.7 arcsec HeII vs NIRSpec 0.15 arcsec Hβ) is a systematic-uncertainty issue and a correctness risk, but it does not constitute circularity: the ratio is not defined to equal the classification boundary by construction. The SED-derived fAGN in Appendix A is explicitly conditioned on the line-ratio classification ('Given the confirmed AGN nature of LAE2 (Sect. 4), we included ... AGN models') and is presented as consistency, not as primary evidence; it is not used to establish the AGN. References to Perna et al. (2025c) supply previously published AGN-A/AGN-B context and are not the load-bearing derivation for LAE2 itself. The escape-fraction estimates use external calibrations (Sobral & Matthee 2019) and recombination theory; they are not inputs to the AGN conclusion. No equation in the paper reduces to its own input, and no self-citation chain uniquely forces the central result.

Axiom & Free-Parameter Ledger

12 free parameters · 6 axioms · 0 invented entities

The AGN classification rests on standard recombination physics and empirical diagnostic diagrams whose applicability to z≈3 low-metallicity systems is assumed; SED parameters are fit outputs, not inputs. The paper introduces no new physical entities, and the 'scattering screen' is a model interpretation rather than an invented conserved quantity or force.

free parameters (12)

fAGN (LAE2) = 0.40 ± 0.17
AGN fractional contribution from CIGALE SED fit to LAE2 photometry (Table A.1); supports the AGN interpretation but is not the primary diagnostic.
log(M*/M⊙) LAE2 = 7.78 +0.18 −0.32
Stellar mass from SED fit; reported in Table A.1.
SFR LAE2 = 0.13 ± 0.07 M⊙/yr
Star-formation rate from SED fit; consistent with Balmer-line estimate.
starburst age LAE2 = 416 ± 162 Myr
Age of the dominant stellar population from SED fit.
metallicity LAE2 = 0.16 ± 0.13 Z⊙
Sub-solar metallicity from SED fit.
log U LAE2 = -1.39 ± 0.49
Ionization parameter from SED nebular modeling.
AV LAE2 = 0.07 ± 0.05 mag
Visual extinction from SED fit.
log(M*/M⊙) LAE1 = 6.19 +0.18 −0.32 (upper limit)
Derived from anchor-point SED fit using F444W as a 2σ 'detection'; upper limit used to argue against in-situ star formation.
SFR LAE1 = 0.02 ± 0.03 M⊙/yr (upper limit)
SED-based upper limit for LAE1.
fesc(Lyα) LAE2 = 0.15–0.27
From Lyα/Hα and Sobral & Matthee (2019) EW calibration; assumes Case B and dust-free.
fesc(Lyα) LAE1 = ≳0.64
Lower limit from Lyα/Hα and EW-based calibration; used to argue for scattering rather than star formation.
EW(Lyα) LAE1 = ≳140 Å
Lower limit derived from non-detection of continuum; used in the Sobral & Matthee calibration.

axioms (6)

domain assumption Case B recombination with Te=10^4 K, ne=100 cm^-3 gives Lyα/Hα=8.22 and HeII1640/λ4687=6.47
Used in Sect. 4.1–4.2 to convert HeII1640 to HeII4687 and derive Lyα escape fractions; AGN-photoionized low-metallicity gas may deviate from these values.
domain assumption The Shirazi & Brinchmann (2012) HeII/Hβ versus [NII]/Hα demarcation, calibrated on local galaxies, separates AGN from star-forming systems at z≈3 for low-metallicity gas
Section 4.1, Fig. 4 right: the 'AGN-only' region is assumed to remain valid at high redshift.
domain assumption 3σ upper limits on [NII] and HeII4687 are treated as the actual line ratios for placement on diagnostic diagrams
Table 1; a non-detection at 3σ does not exclude a weaker line that could shift the classification.
domain assumption The empirical fesc(Lyα)–EW(Lyα) calibration of Sobral & Matthee (2019) is applicable to LAE2 and LAE1
Section 4.2; the calibration was built from star-forming galaxies, not AGN, and may not hold for LAE2.
domain assumption LAE1 continuum upper limit, UV slope β=−2.62, and the Llerena et al. (2022) EW(Lyα)-EW(Ciii]) correlation are valid for the Ciii] prediction
Section 5.3; used to predict expected Ciii] luminosity and compare to MUSE upper limit.
ad hoc to paper Resemblance of LAE1 and LAE2 Lyα profiles indicates a common scattering medium
Section 5.2; an interpretive assumption: similar profiles could also arise from two independent systems with similar kinematics and outflows.

pith-pipeline@v1.3.0-alltime-deepseek · 19529 in / 13260 out tokens · 109195 ms · 2026-08-03T12:54:58.066009+00:00 · methodology

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Cite this review

Pith. "Pith review of GA-NIFS: AGN activity in a Ly{\alpha} emitter within a triple-AGN system anchored by a passive galaxy at z=3." pith.science (2026). https://pith.science/paper/UWAOFF33

@misc{pith2026260100960,
  author       = {Pith},
  title        = {Pith review of: GA-NIFS: AGN activity in a Ly\alpha emitter within a triple-AGN system anchored by a passive galaxy at z=3},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/UWAOFF33}},
  note         = {Machine review of arXiv:2601.00960}
}

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read the original abstract

Massive quenched galaxies at z>3 challenge models of early galaxy evolution, as their rapid formation and abrupt quenching require efficient feedback, often linked to active galactic nuclei (AGN). The quiescent galaxy GS10578 at z=3.1 is a key example of this population. Previous JWST/NIRSpec IFU data revealed an AGN outflow and uncovered a compact pair of AGN separated by ~5 kpc. In addition, VLT/MUSE spectroscopy has identified a third AGN candidate at a projected distance of ~30 kpc, associated with a luminous Lya emitter (LAE2) characterised by high-ionisation UV lines, although rest-frame optical diagnostics were not previously available. We aim to confirm the nature of LAE2 using rest-frame optical diagnostics enabled by new JWST data, and to characterise the physical and ionisation properties of both LAE2 and a distinct nearby Lya emitter (LAE1) that lacks any detectable continuum counterpart. We analyse new NIRSpec IFU observations targeting the optical nebular lines of LAE1 and LAE2, complemented with MUSE data, as part of the GA-NIFS project. We extract integrated and spatially resolved spectra, construct emission-line maps, and use standard diagnostic diagrams to determine ionisation sources and kinematics. LAE2 exhibits line ratios fully consistent with an embedded AGN. Its optical lines display a clumpy morphology and irregular kinematics on sub-kpc scales. Except for Lya, LAE1 remains undetected in all nebular lines and in JWST imaging. The similarity of the LAE1 and LAE2 Lya profiles in both velocity and flux suggests that LAE1 traces resonantly scattered emission rather than in-situ star formation. Our analysis reveals that the environment of GS10578 contains both multi-black-hole activity and gas structures on tens-of-kpc scales, offering new insights into how feedback and satellite interactions influence the late evolutionary stages of quenched massive galaxies.

Figures

Figures reproduced from arXiv: 2601.00960 by Bruno Rodr\'iguez Del Pino, Elena Bertola, Francesco D'Eugenio, Giacomo Venturi, Giovanni Cresci, Hannah \"Ubler, Isabella Lamperti, J. Andrew Bunker, Mahmoud Hamed, Michele Ginolfi, Michele Perna, Montserrat Villar Mart\'in, Roberto Maiolino, Sandra Zamora, Santiago Arribas, Stefano Carniani, St\'ephane Charlot, Torsten B\"oker.

**Figure 2.** Figure 2: Integrated NIRSpec spectrum of LAE2 extracted within a circular aperture of r = 0.15′′. The main emission features are labeled, showing strong detections of Hβ, [O iii]λλ4960,5008, and Hα. The He iiλ4687, [N ii], and [S ii] lines are not detected above the 3σ noise level of the data. 4.1. Optical line ratio diagnostics We investigated the dominant ionisation source for the emitting gas in LAE2 using the cl… view at source ↗

**Figure 3.** Figure 3: Hα and [O iii] flux distributions, along with the [O iii] moment-1 (velocity) and moment-2 (velocity dispersion) maps of LAE2. The flux maps reveal the clumpy morphology of LAE2. The velocity map displays a velocity gradient along the south-east north-west direction in addition to a redshifted component in the northern part of the LAE2, possibly due to an additional component overlapping on the LOS. The co… view at source ↗

**Figure 4.** Figure 4: BPT and He ii diagnostic diagrams. Left: [N ii]/Hα versus [O iii]/Hβ for LAE2 (red symbol), compared with local SDSS galaxies (grey points; Abazajian et al. 2009). The solid (Kewley et al. 2001) and dashed (Kauffmann et al. 2003) curves mark the classical boundaries between star-forming galaxies (below the curves) and AGN (above). Right: [N ii]/Hα versus He ii λ4687/Hβ for LAE2 (large red symbols), and loc… view at source ↗

**Figure 5.** Figure 5: Emission line profiles of LAE2 (grey) and LAE1 (green) in velocity space. Lyα and He ii lines from MUSE spectrum, and [O iii] and Hα from NIRSpec IFS, both integrated over an aperture r = 0.5 ′′. The vertical line indicates the systemic velocity (v = 0) of LAE2. 2022), well above the star-formation rates inferred for LAE2 from its hydrogen recombination lines (Sect. 5.3). This elevated velocity dispersion… view at source ↗

**Figure 6.** Figure 6: Lyα narrow–band image obtained by integrating the MUSE cube over the velocity range [–900, +600] km s−1 around the Lyα line at the systemic redshift of the GS10578 galaxy. The background image shows the spatial distribution of the Lyα flux, with a compass in the top–left corner indicating the North and East directions and a 1.2′′ scale bar in the bottom–left. Superimposed are the spectra extracted from 3 ×… view at source ↗

discussion (0)

Reference graph

Works this paper leans on

3 extracted references · 1 linked inside Pith

[1]

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[2]

4), we included Fritz et al

Given the confirmed AGN nature of LAE2 (Sect. 4), we included Fritz et al. (2006) clumpy torus models in our SED fitting analysis. We sampled optical depths at 9.7 microns ranging from 0.3 to 10, torus opening angles between 60 and 140 degrees, and three viewing angles corresponding to face-on, intermediate, and edge-on configurations (Type 1, intermediat...

2006
[2024]

For LAE2, we extracted aperture photometry using an elliptical aperture optimized to capture the source’s morphology while maximizing S/N

do not provide meaningful additional constraints on the fits. For LAE2, we extracted aperture photometry using an elliptical aperture optimized to capture the source’s morphology while maximizing S/N. LAE2 is detected in 13 filters (average S/N∼7.5), including 7 strong detections (S/N∼11) and 6 tentative detections (S/N∼3). For LAE1, located 0.9 ′′ (∼7 kp...

2019

[1] [1]

N., Adelman-McCarthy, J

Abazajian, K. N., Adelman-McCarthy, J. K., Agüeros, M. A., et al. 2009, ApJS, 182, 543 Alberts, S., Lyu, J., Shivaei, I., et al. 2024, ApJ, 976, 224 Bacon, R., Conseil, S., Mary, D., et al. 2017, A&A, 608, A1 Baker, W. M., Lim, S., D’Eugenio, F., et al. 2025, MNRAS, 539, 557 Baldwin, J. A., Phillips, M. M., & Terlevich, R. 1981, PASP, 93, 5 Bertola, E., C...

Pith/arXiv arXiv 2009

[2] [2]

4), we included Fritz et al

Given the confirmed AGN nature of LAE2 (Sect. 4), we included Fritz et al. (2006) clumpy torus models in our SED fitting analysis. We sampled optical depths at 9.7 microns ranging from 0.3 to 10, torus opening angles between 60 and 140 degrees, and three viewing angles corresponding to face-on, intermediate, and edge-on configurations (Type 1, intermediat...

2006

[3] [2024]

For LAE2, we extracted aperture photometry using an elliptical aperture optimized to capture the source’s morphology while maximizing S/N

do not provide meaningful additional constraints on the fits. For LAE2, we extracted aperture photometry using an elliptical aperture optimized to capture the source’s morphology while maximizing S/N. LAE2 is detected in 13 filters (average S/N∼7.5), including 7 strong detections (S/N∼11) and 6 tentative detections (S/N∼3). For LAE1, located 0.9 ′′ (∼7 kp...

2019