The PAU Survey: Active galactic nucleus galaxies in galaxy pairs

A. L. O'Mill; C. Padilla; D. G. Lambas; D. Navarro-Giron\'es; E. Gazta\~naga; E. J. Gonzalez; E. S\'anchez; F. Duplancic; F. J. Castander; F. Rodriguez

REVIEW

The PAU Survey: Active galactic nucleus galaxies in galaxy pairs

Astrophysics of Galaxies · Submitted 21 Oct 2026 · Published version · 210 references

Pith's verdict: PAUS photo-z allow a well-controlled study of AGN in pairs at z~0.5-1.0, showing a reddening trend and excess morphological disturbances; the results are suggestive but rest on a pair catalogue whose contamination estimate is acknowledged as non-representative.

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CitationA. L. O'Mill, C. Padilla, D. G. Lambas, D. Navarro-Giron\'es, E. Gazta\~naga, E. J. Gonzalez, E. S\'anchez, F. Duplancic, F. J. Castander, F. Rodriguez, H. Hildebrandt, I. Sevilla-Noarbe, I. V. Daza-Perilla, J. Carretero, J. Garc\'ia-Bellido, M. Eriksen, M. Mezcua, M. Siudek, P. Renard, P. Tallada-Cresp\'i, R. Casas, R. Miquel, S. Alonso, S. Serrano. "The PAU Survey: Active galactic nucleus galaxies in galaxy pairs." arXiv:2610.30309 (2026). https://pith.science/paper/PQSST3UX

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Editor's note

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I read through this paper. The central result is that AGN hosts in close pairs get progressively redder above z~0.5, while isolated AGNs and non-AGN pairs stay flat near Mg-Mr~0.6. They also find that AGN pairs are more often morphologically disturbed, and the effect holds across the redshift range. These are genuinely new observational constraints in an epoch where previous work often came up empty.

The analysis is carefully done. The multi-wavelength AGN catalogue (MIR, X-ray, optical line, quasar catalogue) gives broad coverage. The control samples are matched in redshift, absolute magnitude, and environment, plus a re-weighting for stellar mass. The authors test their photo-z quality separately for AGNs and find no systematic bias. They also explicitly flag the pair catalogue contamination as an upper limit of ~40% from a small spec-spec subsample, and say it is not representative. I think that is honest.

The soft spots are real but proportional. First, the contamination estimate: 385 spec-spec pairs out of 16,824 photo-z pairs is tiny, and the paper does not test whether contamination differs between AGN and non-AGN pairs. If it does, the colour and morphology contrasts could be biased. The authors acknowledge the limitation, but they do not quantify differential contamination. That is a real weakness. Second, the morphological classification (MD vs. non-MD) is done by a single author, with 85% internal consistency. It is plausible, but a second independent classifier or quantitative asymmetry metrics would strengthen it. Third, the causal language (“interactions play an increasingly important role”) is inferred; the paper is careful to say “suggest”, but it remains a correlation.

Who is this for? Anyone working on AGN triggering and galaxy interactions, especially at intermediate redshift. It will be a useful data point for models. I would support sending it to a serious referee. The referee should ask for a more robust contamination test (e.g., using the control samples to check if colour trends survive when restricting to spec-pairs, or a simple Monte Carlo that injects random projections at the estimated rate) and for some quantitative morphology metric, or at least a second look. The paper does not need to be perfect before review; it is worth engaging with.

Referee report

Significance

If the results stand, this work provides one of the first clean observational constraints on the interaction–AGN connection in the crucial transitional redshift range z~0.5–1.0, where local positive correlations disappear in higher-redshift studies. The use of PAUS narrow-band photometric redshifts (σ68≤0.02) is a genuine improvement over traditional broad-band surveys for identifying galaxy pairs beyond the local Universe. The construction of carefully matched control samples (redshift, luminosity, environment) with stellar-mass re-weighting is methodologically sound and raises the bar for such studies. The combined evidence from colour evolution, morphology, and pair kinematics is internally consistent and points to a physically plausible picture. The paper therefore addresses an open question in galaxy evolution with a novel dataset and a careful, multi-pronged analysis. Its conclusions, if verified, would motivate a revision of theoretical models of AGN triggering mechanisms across cosmic time.

Major objections (2)

[Appendix B and Section 3.1] Contamination of the photometric pair catalogue. The only empirical check of purity (Appendix B) uses 385 spec–spec pairs and finds a ~40% upper limit, but the authors correctly state that this subsample 'is not statistically representative of the full photometric pair catalogue' (sentence b434). This is a critical limitation for the paper's central claims because the colour trends and MD fractions are derived from the full photometric catalogue. If the true contamination is higher or, more worryingly, if it differs systematically between AGN and non-AGN pairs (e.g., because AGN hosts have different redshift distributions or are more often in chance alignments due to their brighter absolute magnitudes), then the observed differences could be diluted or artificially amplified. The paper does not test for differential contamination, and the spec–spec subsample is too small and selected in an unspecified way to rule it out. The PI consistency check (Fig. B.2) only validates the photo-z velocity proxy for physical spec–spec pairs, not the whole catalogue, and does not address differential effects. I request that the authors (a) clarify how the 385 spec–spec pairs were selected from the full pair catalogue (e.g., by field, redshift, magnitude); (b) test whether the AGN fraction among pairs with and without spectroscopic information differs; and (c) discuss how a plausible range of contamination levels (e.g., 20–40%) with conservative assumptions about differential bias would affect each of the main results (colour trends, MD fraction, PI evolution). Without this, the robustness of the conclusions cannot be fully assessed. The authors acknowledge this: “We note, however, that this estimate should be regarded as an upper limit, since the spec-spec subsample is not statistically represen- tative of the full photometric pair catalogue.”
[Section 4.2] Morphological classification performed by a single author with no independent validation. The visual classification into morphologically disturbed (MD) vs. non-MD pairs is described as performed by the first author and 'refined iteratively until a 85% agreement rate was achieved' (around sentence b243). It is unclear whether this 85% refers to intra-rater repeatability (same person re-classifying the same images) or inter-rater agreement with a second classifier. Because the MD fraction difference (24% vs 12%) is a key observational result supporting the interaction–AGN connection, the subjective element of the classification needs to be quantified more rigorously. I request that the authors (a) clarify the nature and measurement of the 85% agreement; (b) ideally have a second independent classifier evaluate a subset (e.g., 200 pairs) and report the inter-rater agreement (Cohen's κ or simple agreement fraction); and (c) show that the main MD-fraction difference between AGN and non-AGN pairs remains significant when considering only pairs classified as MD by both raters. If a second classifier is not feasible, a sensitivity test using automated morphological proxies (e.g., Gini, M20, or CAS parameters from the Legacy Survey images) would lend support to the visual classification.

Minor objections (8)

[Section 3.1 / Appendix B] The total number of galaxy pairs is stated as 11,635 in Section 3.1 (line after isolation criterion) but Appendix B begins with 'the pair sample comprising 16,824 systems'. Please clarify this discrepancy and ensure consistency throughout the manuscript.
[Section 3.1] The isolation criterion requires no neighbouring galaxy within 300 kpc and ΔV<3500 km/s with a magnitude difference <2.5. It is not explicitly stated that the neighbours are required to satisfy the same photo-z quality cuts. Please clarify.
[Section 4.1 / Fig. 5] The paper states that the colour difference between AGNs in pairs and controls exceeds 3σ for z_b>0.6. How is this significance computed from the bootstrap confidence intervals (16th and 84th percentiles)? If the 1σ intervals are used, a 3σ level requires that the median LOWESS curves are separated by more than ~3×(σ1+σ2)? Please provide the precise criterion used.
[Section 4.2] The R-quantile boundaries (Q1–Q4) are defined from the full pair sample? Or from the combined AGN+control sample? This should be stated explicitly, as the PI interpretation depends on it. Also, the R1 region (0<R≤0.54) contains only a small number of pairs; please provide the actual N for each R shell in the caption of Fig. 9 or in the text.
[Section 4.2 / Fig. 8] The horizontal offset applied to the MD markers to improve visibility is described but not shown clearly in the figure; the markers appear nearly superimposed. Consider using different symbol shapes or plotting the MD sub-samples in separate panels.
[Section 3.3] The matching algorithm allows up to three controls per AGN but 'the simultaneous matching in three parameters … prevented us from obtaining exactly three controls for every object.' It would be helpful to report the actual distribution of the number of controls per reference object (e.g., what fraction get 1, 2, or 3 controls?).
[Section 5] The first conclusion bullet states that AGNs in pairs become redder at higher redshifts 'while isolated AGNs remain comparatively bluer'. However, Fig. 5 shows that isolated AGNs (Control1) also show a mild reddening, though weaker. The phrasing could be more nuanced.
[General] Some references to 'Alonso et al. (in prep)' appear in the bibliography but are not cited in the text (e.g., Gonzalez et al. in prep). Please ensure all cited works are included and that 'in prep' works are described sufficiently if they are used to derive quantities used here.

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The paper

The paper claims

Using high-precision photometric redshifts from the PAU survey, this study finds that active galactic nuclei (AGNs) in galaxy pairs become progressively redder with redshift, especially beyond z=0.6, while isolated AGNs and non-AGN pairs…

The reading

This paper aims to establish a redshift-dependent link between galaxy interactions and AGN activity by exploiting the high-precision photometric redshifts of the PAU survey (σ68 ≤ 0.02). The authors identify 11,635 galaxy pairs out to z~1 and cross-match with multi-wavelength AGN catalogues to find 214 AGN hosts in pairs. They construct carefully matched control samples of isolated AGNs, non-AGN pairs, and isolated non-AGNs. The central finding is that AGNs in pairs show progressively redder rest-frame colours with increasing redshift (especially z > 0.6), whereas control samples show flat colour trends. Additionally, pairs hosting AGNs are preferentially morphologically disturbed and have smaller projected separations and velocity offsets. These results suggest that the efficiency of interactions in triggering nuclear activity increases at intermediate redshifts (z ~ 0.5–1.0), a regime where previous higher-redshift studies often failed to detect a connection. The work matters because it provides observational evidence that the interaction–AGN connection evolves with cosmic time, constraining models of black hole–galaxy co-evolution.

What carries the argument

The central enabler is the PAU survey's narrow-band photometric redshifts (40 filters, 4500–8500 Å, FWHM 130 Å) achieving σ68 ≤ 0.02 for iAB < 23 galaxies over 43 deg², which allows reliable pair identification to z~1. The pair-finding algorithm (Rodriguez et al. 2020) uses thresholds r_p < 100 kpc, ΔV < 3500 km/s, and an isolation criterion to exclude richer structures. AGN selection combines four complementary catalogues: mid-infrared (WISE R90), optical emission-line (BPT from SDSS), X-ray (2SXPS/4XMM with Bayesian classification), and a quasar catalogue (Milliquas). Control samples are matched in redshift, i-band absolute magnitude, and local overdensity (δ) to isolate the pair environment effect. Visual morphological classification from DESI Legacy Survey images identifies 'morphologically disturbed' (MD) pairs, providing a direct interaction signature.

Extended reading notes

Core claim

AGNs hosted by galaxy pairs show a clear redshift evolution in rest-frame colours: both (Mg−Mr) and (Mg−Mz) redden progressively towards higher redshifts, particularly beyond z ~ 0.5–0.6. In contrast, isolated AGNs and non-AGNs in pairs maintain flat colour trends around Mg−Mr ~ 0.65 across the same redshift range. The colour difference between AGNs in pairs and isolated AGNs exceeds 3σ at z > 0.6, and persists at 2σ after mass re-weighting. Furthermore, the fraction of morphologically disturbed galaxies is consistently ~12 percentage points higher among AGN in pairs than among non-AGN pairs (24% vs 12%). AGN-hosting pairs also exhibit smaller projected separations and velocity offsets, and a proximity index that evolves with redshift: AGN pairs become progressively tighter at lower redshifts, while non-AGN pairs show no evolution. The authors interpret these combined trends as evidence that galaxy interactions play an increasingly important role in triggering nuclear activity at intermediate redshifts (z ~ 0.5–1.0), with a link that weakens towards the local Universe.

Load-bearing premise

The pair catalogue's purity depends on the assumption that the photo-z precision and thresholds (ΔV < 3500 km/s, r_p < 100 kpc) distinguish physical pairs from chance projections, but the paper's own contamination analysis (based on a small, non-representative spec-spec subsample) finds an upper limit of ~40% spurious pairs, and if contamination differs systematically between AGN hosts and non-AGN hosts, the reported colour and morphological trends could be biased.

Editorial extensions

If this is right

If the redshift-dependent colour and morphological trends are physical, then models of AGN triggering must incorporate a declining efficiency of interaction-driven fuelling from z~1 to the present.
Future hydrodynamic simulations with AGN feedback (e.g., IllustrisTNG, EAGLE) should reproduce the observed colour–redshift relation for AGN in pairs, providing a test of feedback and gas circulation prescriptions.
The redder colours of pair-hosted AGNs at z>0.6 imply either enhanced dust obscuration or a distinct AGN population in interacting systems at these epochs, which will affect completeness of optical AGN surveys.
The work demonstrates that narrow-band photometric surveys can rival spectroscopic pair studies to z~1, opening a new window for interaction studies in wide fields without fibre-collision biases.
Extending the analysis to deeper fields or higher redshifts (z>1) will test whether the colour trend continues or reverses as one approaches the peak of cosmic star formation and AGN activity.

Reading between the lines

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

The colour reddening could be driven by increased dust obscuration in the central regions of interacting galaxies at higher redshift, implying that pairs at z>0.6 preferentially host obscured or mildly obscured AGN that are more efficiently revealed by MIR and X-ray selection.
If the observed colour trend is partially due to enhanced star formation in the pair hosts (rather than solely AGN-related dust), then the star formation–AGN connection in mergers must also be redshift-dependent — a prediction that could be tested with far-IR/submm data for the same sample.
The visual morphological classification, while iteratively refined, remains subjective and limited by surface-brightness sensitivity at higher redshift; automated merger statistics (e.g., Gini, M20, asymmetry) applied to deeper imaging could confirm the trend without human bias.
The reported upper limit of ~40% contamination in the pair catalogue, based on a small spec-spec subsample, leaves open the possibility that systematic projection effects differ for AGN hosts versus non-AGN hosts, which could affect the colour comparisons; a larger spectroscopic follow-up of PAUS pairs would settle this.

Original abstract

Aims. Leveraging the high-precision photometric redshifts of the Physics of the Accelerating Universe Survey (PAUS), we aim to investigate the connection between active galactic nuclei (AGNs) and galaxy pairs up to redshifts of $\sim1.0$. Methods. We identified 16,824 galaxy pairs with projected separations of $r_p < 100$ kpc and radial-velocity differences of $\Delta V < 3500$ km s$^{-1}$. AGNs were selected by cross-matching PAUS galaxies with multi-wavelength AGN catalogues, yielding 270 AGNs in pairs out of a parent sample of 8,880 AGNs in PAUS. We constructed control samples of isolated AGNs; non-AGNs in pairs; and isolated non-AGNs matched in redshift, absolute magnitude, and environment. Results. Active galactic nuclei in pairs show progressively redder rest-frame colours with increasing redshift, particularly at redshifts of $z\gtrsim 0.5$, whereas isolated AGNs and non-AGNs in pairs show no significant colour evolution and remain at $\mathrm{M_g-M_r}\sim0.65$. Pairs hosting AGNs are also preferentially morphologically disturbed interacting systems found at smaller projected separations and velocity offsets, consistent with more dynamically advanced interactions. Conclusions. These results provide evidence of a redshift-dependent link between galaxy interactions and AGN activity, suggesting that interactions play an increasingly important role in triggering nuclear activity at intermediate redshifts. This study highlights the unique capability of PAUS to probe AGN-galaxy interaction connections beyond the local Universe with unprecedented statistical power.

The compiled record

The paper's own sentences, arranged, kept beside the review and separate from it. Each label is drawn from a closed vocabulary; the number beside it is the probability the classifier gave that label. Numbers in the tables are the authors', checked by code. No sentence in this record was written by a model.

Compiled by classifier-1.13.0 via TypeSafe API, question bank abstract-p1-20260923, 2026-10-23: 1 request, 7,238 input tokens.

What the abstract itself states, as probabilities: claims first 0.06 · states limitation 0.07 · human participants 0.01 · controlled comparison 0.98 · randomized assignment 0.01 · states quantitative result 0.98 · compares with prior results 0.54 · mentions code or data availability 0.02.

The abstract, sentence by sentence

arXiv listing abstract v1. Results and the main claim are underlined; show every role.

Aims. Leveraging the high-precision photometric redshifts of the Physics of the Accelerating Universe Survey (PAUS), we aim to investigate the connection between active galactic nuclei (AGNs) and galaxy pairs up to redshifts of $\sim1.0$. Methods. We identified 16,824 galaxy pairs with projected separations of $r_p < 100$ kpc and radial-velocity differences of $\Delta V < 3500$ km s$^{-1}$. AGNs were selected by cross-matching PAUS galaxies with multi-wavelength AGN catalogues, yielding 270 AGNs in pairs out of a parent sample of 8,880 AGNs in PAUS. We constructed control samples of isolated AGNs; non-AGNs in pairs; and isolated non-AGNs matched in redshift, absolute magnitude, and environment. Results. Active galactic nuclei in pairs show progressively redder rest-frame colours with increasing redshift, particularly at redshifts of $z\gtrsim 0.5$, whereas isolated AGNs and non-AGNs in pairs show no significant colour evolution and remain at $\mathrm{M_g-M_r}\sim0.65$. Pairs hosting AGNs are also preferentially morphologically disturbed interacting systems found at smaller projected separations and velocity offsets, consistent with more dynamically advanced interactions. Conclusions. These results provide evidence of a redshift-dependent link between galaxy interactions and AGN activity, suggesting that interactions play an increasingly important role in triggering nuclear activity at intermediate redshifts. This study highlights the unique capability of PAUS to probe AGN-galaxy interaction connections beyond the local Universe with unprecedented statistical power.

background contribution method result interpretation main claim

What the classifier reports for each sentence. The number is the probability it gave the label.
#	sentence	role	the authors' own work	states the main conclusion	strength
s0	Aims.	background 0.55	0.03	0.01	unclear 1.00
s1	Leveraging the high-precision photometric redshifts of the Physics of the Accelerating Universe Survey (PAUS), we aim to investigate the connection between active galactic nuclei (AGNs) and galaxy pairs up to redshifts of $\sim1.0$. Methods.	contribution 0.63	0.34	0.01	unclear 0.62
s2	We identified 16,824 galaxy pairs with projected separations of $r_p < 100$ kpc and radial-velocity differences of $\Delta V < 3500$ km s$^{-1}$.	method 0.99	0.97	0.01	asserted 1.00
s3	AGNs were selected by cross-matching PAUS galaxies with multi-wavelength AGN catalogues, yielding 270 AGNs in pairs out of a parent sample of 8,880 AGNs in PAUS.	method 0.98	0.96	0.02	asserted 1.00
s4	We constructed control samples of isolated AGNs; non-AGNs in pairs; and isolated non-AGNs matched in redshift, absolute magnitude, and environment. Results.	method 0.99	0.95	0.01	asserted 0.79
s5	Active galactic nuclei in pairs show progressively redder rest-frame colours with increasing redshift, particularly at redshifts of $z\gtrsim 0.5$, whereas isolated AGNs and non-AGNs in pairs show no significant colour evolution and remain at $\mathrm{M_g-M_r}\sim0.65$.	result 1.00	0.94	0.15	asserted 1.00
s6	Pairs hosting AGNs are also preferentially morphologically disturbed interacting systems found at smaller projected separations and velocity offsets, consistent with more dynamically advanced interactions. Conclusions.	result 0.98	0.92	0.09	hedged possibility 0.52
s7	These results provide evidence of a redshift-dependent link between galaxy interactions and AGN activity, suggesting that interactions play an increasingly important role in triggering nuclear activity at intermediate redshifts.	interpretation 1.00	0.87	0.96	hedged possibility 0.89
s8	This study highlights the unique capability of PAUS to probe AGN-galaxy interaction connections beyond the local Universe with unprecedented statistical power.	contribution 0.55	0.51	0.07	asserted 0.99

What kind of paper the classifier reports this is: empirical study 1.00 · evidence from analysis of existing data 0.92.

What was examined, and what was not

sources read

arXiv listing abstract v1

not examined

full text
figures and tables
references and citing sentences
relations to other papers

levels run

P abstract

not run

S sections
T body sentences
C citations
R cross-paper relations

Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. Every number in the measurements table is the authors', checked by code. Record as JSON

Figures

**Figure 1.** Distribution of pair photo-z (zpairs; top), i-band absolute magnitude (Mi) of the brightest and the faintest galaxy in the system (bottom). The inset shows the relation between Mi and stellar mass (log(M∗/M⊙)) for galaxies in the pair sample. be genuine. This MIR-based approach is highly efficient at identifying dust-obscured AGNs, since ultraviolet (UV) and optical emission from the accretion disc absorbed by circumnuclear dust is reprocessed and re-emitted at MIR wavelengths. Regarding optical emission-line diagnostics (BPT-AGNs), we used the SDSS Portsmouth emission-line…

**Figure 2.** Distributions of photo-z (zb; top) and i-band absolute magnitude (Mi ; bottom) for the sample of 7342 AGNs and for each AGN subsample. We also included the distribution of 7342 non-AGN PAUS galaxies. At the top of the panels we show the number of galaxies, median value, and Q1 and Q3 percentiles of each sample. It is worth noting that PAUS fields are fully covered by the different AGN catalogues. Integrating samples across MIR, Xray, optical, and quasar catalogues provides a comprehensive perspective on the AGN population. This multi-wavelength analysis enhances the reliability of…

**Figure 3.** Normalised distributions of redshift (zb; top), absolute iband magnitude (Mi ; middle), and overdensity (δ; bottom). For each parameter, the upper panels show the distributions of the original samples: AGNs in pairs (black line with grey shading), isolated AGNs (dashed blue line), non-AGNs in pairs (dotdashed magenta line), and isolated non-AGNs (dotted red line). The lower panels display the corresponding distributions for the control samples matched to the AGNs in pairs: control 1 (isolated AGNs, dashed blue line), control 2 (non-AGNs in pairs, dot-dashed magenta line), and…

**Figure 4.** Confusion matrices showing the distribution of the three

**Figure 5.** shows the evolution of the (Mg − Mr) and (Mg − Mz) colour indices as a function of redshift. To characterize the underlying trends in these galaxy properties, we employed a nonparametric smoothing approach based on locally weighted scatterplot smoothing (LOWESS). This method allows us to model the median behaviour of the population without assuming a specific functional form. The degree of smoothing was controlled by a fractional bandwidth parameter f = 0.3, which determines the local bandwidth, h, as the distance to the f · N th nearest neighbour. This adaptive bandwidth…

**Figure 6.** Examples of non-MD (top) and MD (bottom) pairs at different redshifts. Images are 30′′ × 30′′ cut-outs from https:// www.legacysurvey.org/viewer/, using data from DR10 (Credit: Legacy Surveys / D. Lang (Perimeter Institute)). The markers indicate the pair barycentre (open red circle), the positions of both pair members (black crosses), and a scale bar. We also overlaid the coordinates and redshift of the pair in the bottom right corner. the different control samples (controls 1, 2, and 3). In the standard relations (main panels), AGNs in pairs exhibit the reddest colours for…

**Figure 7.** Top: Fraction of galaxies in MD pairs (FMD) for the AGN pair sample (solid black line) and the control 2 non-AGN pair sample (dot-dashed magenta line), shown in different redshift bins. The total number of galaxies in each sample per bin is listed in the figure. Bottom: Absolute difference between the two fractions, |d|, as a function of redshift. Errors were estimated using the beta distribution quantile technique (Cameron 2011). The visual classification was performed by the first author of this paper and refined iteratively until a 85% agreement rate was achieved. The final…

**Figure 8.** Normalised distributions of projected separation,

**Figure 9.** Normalised radial-velocity difference (∆V/∆Vmax) versus normalised projected distance (rp/rp,max) plane. The marked regions (R1–R4) correspond to the R quantile segmentation and are colour-coded according to the average photo-z (⟨zb⟩) of the individual paired galaxies within each shell. The number N indicates the total count of individual galaxies. Errors were calculated using bootstrap resampling. The upper panel shows the AGN pair sample, while the lower panel displays the corresponding control 2 sample of non-AGN pairs. Dots represent the subsamples of MD pairs. requirement…

**Figure 10.** Average value of PI as a function of mean photo-z ⟨zb⟩. The solid black line represents pairs hosting AGNs, while the dot-dashed magenta line corresponds to pairs hosting non-AGNs in the control 2 sample. The numbers of objects in each interval are listed. The errors were calculated using bootstrap resampling techniques. AGNs. These samples were carefully selected to match the redshift, absolute magnitude, and local overdensity distributions of AGNs in pair systems. Such control samples are crucial for reliably identifying similarities and differences in galaxy properties when…

Figures reproduced from arXiv:2610.30309 by the authors.

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The impact of void environment on AGN. , keywords =. doi:10.1093/mnras/stab2902 , adsurl =

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AGNs in massive galaxy clusters: Role of galaxy merging, infalling groups, cluster mass, and dynamical state. , keywords =. doi:10.1051/0004-6361/202348212 , archivePrefix =. 2401.05747 , primaryClass =

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SDSS-IV MaNGA: the role of the environment in AGN triggering. , keywords =. doi:10.1093/mnras/stad3584 , adsurl =

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The host galaxies of active galactic nuclei. , keywords =. doi:10.1111/j.1365-2966.2003.07154.x , archivePrefix =. astro-ph/0304239 , primaryClass =

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Galaxy pairs in the Sloan Digital Sky Survey - VIII. The observational properties of post-merger galaxies. , keywords =. doi:10.1093/mnras/stt1562 , archivePrefix =. 1308.3707 , primaryClass =

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A Multiwavelength Study of Active Galactic Nuclei in Post-merger Remnants. , keywords =. doi:10.3847/1538-4357/acb13d , archivePrefix =. 2301.06186 , primaryClass =

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Galaxy pairs in the Sloan Digital Sky Survey - IX. Merger-induced AGN activity as traced by the Wide-field Infrared Survey Explorer. , keywords =. doi:10.1093/mnras/stu650 , archivePrefix =. 1403.7531 , primaryClass =

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Incidence of WISE -selected obscured AGNs in major mergers and interactions from the SDSS. , keywords =. doi:10.1093/mnras/stw2620 , archivePrefix =. 1609.04832 , primaryClass =

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The X-ray view of merger-induced active galactic nuclei activity at low redshift. , keywords =. doi:10.1093/mnras/staa1692 , archivePrefix =. 2006.01850 , primaryClass =

View on Pith Pith review arXiv 2006
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Investigating the Effect of Galaxy Interactions on the Enhancement of Active Galactic Nuclei at 0.5 < z < 3.0. , keywords =. doi:10.3847/1538-4357/abbf59 , archivePrefix =. 2010.02710 , primaryClass =

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Galaxy Mergers up to z < 2.5. II. AGN Incidence in Merging Galaxies at Separations of 3-15 kpc. , keywords =. doi:10.3847/1538-4357/abdbb1 , archivePrefix =. 2101.05000 , primaryClass =

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Obscured AGN enhancement in galaxy pairs at cosmic noon: evidence from a probabilistic treatment of photometric redshifts. , keywords =. doi:10.1093/mnras/stad1300 , archivePrefix =. 2305.05692 , primaryClass =

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The environmental dependence of the relations between stellar mass, structure, star formation and nuclear activity in galaxies. , keywords =. doi:10.1111/j.1365-2966.2004.08117.x , archivePrefix =. astro-ph/0402030 , primaryClass =

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Environmental Dependence of Active Galactic Nucleus Activity. I. The Effects of Host Galaxy. , keywords =. doi:10.1088/0004-637X/699/2/1679 , archivePrefix =. 0904.2579 , primaryClass =

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Effect of the interactions and environment on nuclear activity. , keywords =. doi:10.1093/mnras/sts675 , archivePrefix =. 1212.4836 , primaryClass =

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On the relation between Seyfert 2 accretion rate and environment at z < 0.1. , keywords =. doi:10.1093/mnras/stt1920 , archivePrefix =. 1310.2618 , primaryClass =

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Occurrence of LINER galaxies within the galaxy group environment. , keywords =. doi:10.1093/mnras/stx294 , archivePrefix =. 1711.06291 , primaryClass =

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AGNs in small galaxy systems: comparing the main properties of active objects in pairs, triplets, and groups. , keywords =. doi:10.1093/mnras/stab1131 , archivePrefix =. 2107.01036 , primaryClass =

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Measuring Baryon Acoustic Oscillations Along the Line of Sight with Photometric Redshifts: The PAU Survey. , keywords =. doi:10.1088/0004-637X/691/1/241 , archivePrefix =. 0807.0535 , primaryClass =

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Precise photometric redshifts with a narrow-band filter set: the PAU survey at the William Herschel Telescope. , keywords =. doi:10.1093/mnras/stu801 , archivePrefix =. 1402.3220 , primaryClass =

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The Physics of the Accelerating Universe Survey: narrow-band image photometry. , keywords =. doi:10.1093/mnras/stad1399 , archivePrefix =. 2206.14022 , primaryClass =

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The Physics of the Accelerating Universe Camera. , keywords =. doi:10.3847/1538-3881/ab0412 , archivePrefix =. 1902.03623 , primaryClass =

View on Pith Pith review arXiv 1902
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The Cosmic Evolution Survey (COSMOS): Overview. , keywords =. doi:10.1086/516585 , archivePrefix =. astro-ph/0612305 , primaryClass =

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CFHTLenS: the Canada-France-Hawaii Telescope Lensing Survey. , keywords =. doi:10.1111/j.1365-2966.2012.21952.x , archivePrefix =. 1210.0032 , primaryClass =

View on Pith Pith review arXiv 2012
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CFHTLenS: the Canada-France-Hawaii Telescope Lensing Survey - imaging data and catalogue products. , keywords =. doi:10.1093/mnras/stt928 , archivePrefix =. 1210.8156 , primaryClass =

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The Kilo-Degree Survey. Experimental Astronomy , keywords =. doi:10.1007/s10686-012-9306-1 , archivePrefix =. 1206.1254 , primaryClass =

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The PAU survey: photometric calibration of narrow band images. , keywords =. doi:10.1093/mnras/stae1507 , archivePrefix =. 2406.06850 , primaryClass =

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The PAU Survey: Operation and orchestration of multi-band survey data. Astronomy and Computing , keywords =. doi:10.1016/j.ascom.2019.04.002 , archivePrefix =. 1811.02368 , primaryClass =

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The PAU Survey: an improved photo-z sample in the COSMOS field. , keywords =. doi:10.1093/mnras/staa3659 , archivePrefix =. 2007.11132 , primaryClass =

View on Pith Pith review arXiv 2007
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The PAU Survey: narrow-band photometric redshifts using Gaussian processes. , keywords =. doi:10.1093/mnras/stab711 , archivePrefix =. 2101.03723 , primaryClass =

View on Pith Pith review arXiv
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The PAU Survey and Euclid: Improving broadband photometric redshifts with multi-task learning. , keywords =. doi:10.1051/0004-6361/202245027 , archivePrefix =. 2209.10161 , primaryClass =

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The PAU Survey: Galaxy stellar population properties estimates with narrowband data. , keywords =. doi:10.1051/0004-6361/202449838 , archivePrefix =. 2405.20385 , primaryClass =

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Building a control sample for galaxy pairs. , keywords =. doi:10.1111/j.1365-2966.2009.15033.x , archivePrefix =. 0904.2845 , primaryClass =

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What drives the growth of black holes?. , keywords =. doi:10.1016/j.newar.2011.11.003 , archivePrefix =. 1112.1949 , primaryClass =

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Observational Tests of Active Galactic Nuclei Feedback: An Overview of Approaches and Interpretation. Galaxies , keywords =. doi:10.3390/galaxies12020017 , archivePrefix =. 2404.08050 , primaryClass =

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The Impact of Galaxy Interactions on Active Galactic Nucleus Activity in zCOSMOS. , keywords =. doi:10.1088/0004-637X/743/1/2 , archivePrefix =. 1109.1292 , primaryClass =

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The quest for dual and binary supermassive black holes: A multi-messenger view. , keywords =. doi:10.1016/j.newar.2020.101525 , archivePrefix =. 2001.06293 , primaryClass =

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Hydrodynamical evolution of black-hole binaries embedded in AGN discs - III. The effects of viscosity. , keywords =. doi:10.1093/mnras/stae504 , archivePrefix =. 2303.12207 , primaryClass =

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GA-NIFS: High number of dual active galactic nuclei at z 3. , keywords =. doi:10.1051/0004-6361/202453430 , archivePrefix =. 2310.03067 , primaryClass =

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UpSet: Visualization of Intersecting Sets , author=. IEEE Transactions on Visualization and Computer Graphics , volume=. 2014 , publisher=. doi:10.1109/TVCG.2014.2346248 , url=

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Cosmic Star-Formation History. , keywords =. doi:10.1146/annurev-astro-081811-125615 , archivePrefix =. 1403.0007 , primaryClass =

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The evolution of the X-ray luminosity functions of unabsorbed and absorbed AGNs out to z 5. , keywords =. doi:10.1093/mnras/stv1062 , archivePrefix =. 1503.01120 , primaryClass =

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CosmoHub and SciPIC: Massive cosmological data analysis, distribution and generation using a Big Data platform. Proceedings of the European Physical Society Conference on High Energy Physics. 5-12 July , year = 2017, month = jul, eid =. doi:10.22323/1.314.0488 , adsurl =

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2SXPS: An Improved and Expanded Swift X-Ray Telescope Point-source Catalog. , keywords =. doi:10.3847/1538-4365/ab7db9 , archivePrefix =. 1911.11710 , primaryClass =

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Galaxy pairs in the Sloan Digital Sky Survey - IV. Interactions trigger active galactic nuclei. , keywords =. doi:10.1111/j.1365-2966.2011.19624.x , archivePrefix =. 1108.2711 , primaryClass =

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Discussion

Disagree with the review, or know something it missed? Leave a comment, highlight any passage above to comment on it, or challenge this review formally.

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View on Pith 2025

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