Pith. sign in

REVIEW 3 major objections 6 minor 58 references

Search for spatial coincidences between galaxy mergers and Fermi-LAT 4FGL-DR4 sources

T0 review · 3 major / 6 minor · reviewed 2026-08-06 · deepseek-v4-flash

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

Pith's one-line read Twenty-one of 3,166 galaxy mergers coincide with Fermi-LAT gamma-ray sources at less than 5 percent chance of random alignment.

desk verdict A useful first cross-match and candidate list, but the per-object p-values don't establish a global excess, and the 'secure' label is stronger than the statistics support. read the letter →

arxiv 2507.03970 v2 pith:GYR5WJTB submitted 2025-07-05 astro-ph.HE astro-ph.COastro-ph.GA

Siddhant Manna , Shantanu Desai This is my paper
classification astro-ph.HEastro-ph.COastro-ph.GA
keywords galaxymergersFermi-LAT4FGL-DR4gamma-raysourcesspatialcross-matchingactivegalacticnucleiPoissonstatisticsunassociatedFermi
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

This paper reports the first systematic spatial cross-match between a large morphologically selected sample of galaxy mergers and the Fermi-LAT gamma-ray source catalog. From 3,166 high-confidence CNN-selected mergers with SDSS r-band magnitudes, the authors find 38 mergers inside the 4σ positional uncertainty ellipses of 4FGL-DR4 sources, and 21 of those associations have Poisson match probabilities below 0.05, which they classify as statistically secure. Five of the secure counterparts are unassociated gamma-ray sources, three of which show no obvious AGN signatures in optical, X-ray, or radio data. The authors read the result as support for the scenario in which mergers trigger accretion onto supermassive black holes and produce gamma-ray-emitting AGN, and they propose merger catalogs as physically motivated priors for identifying Fermi sources without known counterparts.

What carries the argument

The load-bearing statistical object is the Poisson chance-coincidence probability p = 1 − $e^{{−μ}}$ with μ = πab n_s(>S). Here a and b are the semi-major and semi-minor axes of each 4FGL-DR4 source's positional uncertainty ellipse, matched at a conservative 4σ threshold, and n_s(>S) is the surface density of merger candidates with SDSS r-band flux greater than the candidate's flux, computed by counting brighter mergers in the full catalog and dividing by the estimated 6190 deg² sky footprint. This converts each spatial overlap into a probability that it arose by chance, and the p < 0.05 threshold defines the secure list. The machinery also includes the merger selection pipeline: a strict probability threshold on the CNN merger scores and a 0.1-arcsecond cross-match to SDSS DR16.

What would settle it

Recompute the 21 p-values using a local merger surface density measured in an annulus around each Fermi source rather than the global 6190 deg² footprint; if fewer than 21 associations survive at p < 0.05, the claimed secure matches are artifacts of the uniform-background assumption.

Watch

Extended reading notes

Core claim

Cross-matching 3,166 high-confidence galaxy mergers (selected from 328,151 CNN candidates by requiring merger probability > 0.95 in every fold, then matched to SDSS DR16) against 4FGL-DR4 yields 38 spatial coincidences within the 4σ positional uncertainty ellipses of Fermi sources. Using the Poisson chance-coincidence probability p = 1 − $e^{{−πab n_s(>S)}}$, where a and b are the ellipse semi-axes and n_s(>S) is the flux-dependent surface density of mergers brighter than the SDSS counterpart, 21 of these matches have p < 0.05 and are classified as statistically secure. Their 4FGL-DR4 classifications are four FSRQs, six BL Lacs, three BCUs, three radio galaxies, and five unassociated sources; none is a pulsar. A control sample with the merger coordinates randomly shifted by up to 2 degrees yields zero matches, while the 70 galaxy pairs from the CNOC2 catalog also produce no associations. The paper concludes that mergers can host gamma-ray-emitting AGN activity and that the five unassociated counterparts may point to a previously unrecognized population of gamma-ray sources.

Load-bearing premise

The chance-coincidence background is one global number—the count of mergers brighter than the candidate divided by a single uniform sky area of about 6190 square degrees—so if that footprint or the merger catalog's clustering is wrong, every p-value scales and the 21-match list could shrink or grow.

Editorial extensions

If this is right

  • 21 of 38 positional coincidences are secure at p < 0.05; 62% are blazar-type (FSRQ, BLL, BCU), three are radio galaxies, and none is a pulsar.
  • Five secure counterparts are unassociated Fermi sources; three show no AGN signatures in SDSS, RASS, or FIRST and are plausible merger-driven emitters.
  • A control sample with merger positions randomly shifted by up to 2 degrees produces zero matches, supporting the interpretation that the 21 associations are not chance coincidences.
  • The 70 CNOC2 close galaxy pairs show no Fermi associations within the same threshold, so the positive result is specific to the large morphologically selected merger sample.
  • Merger catalogs can serve as physically motivated priors for identifying unassociated Fermi-LAT sources, a use the paper explicitly proposes.

Reading between the lines

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

  • If the association is real, a stacking analysis of all 3,166 mergers, not only those inside error ellipses, should reveal a collective gamma-ray excess; that test would be independent of the 4σ threshold and is not performed in the paper.
  • The three unassociated counterparts without AGN signatures are the cleanest targets for follow-up: deep X-ray and radio observations would decide whether merger-driven emission is actually present, a step the paper itself calls for.
  • Replacing the uniform 6190 deg² footprint with a locally measured merger surface density, or with a full angular cross-correlation between the merger catalog and 4FGL-DR4, would convert the 21 matches into a population-level excess measurement.
  • The same Poisson machinery could be applied to future merger catalogs from deeper surveys, turning a sparse list of 21 matches into a measurement of the merger-triggered gamma-ray source fraction and its evolution with redshift.
Share X Bluesky LinkedIn Reddit HN

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 6 minor

Summary. The paper cross-matches a high-confidence sample of 3,166 CNN-selected galaxy mergers (derived from Ackermann et al. 2018) with the Fermi-LAT 4FGL-DR4 catalog. Using a 4σ positional matching radius and a Poisson chance-coincidence framework (Eqs. 1–2), the authors report 38 spatial coincidences, of which 21 have p<0.05 and are classified as “statistically secure” matches; five of these are unassociated Fermi sources. The paper also searches 70 galaxy pairs from the CNOC2/Patton et al. (2005) catalog and finds no p<0.05 counterparts. The central claim is that the 21 matches are unlikely to be random associations.

Significance. If correct, this would be the first systematic indication that a morphologically selected galaxy-merger population contains gamma-ray-emitting members, and it would motivate using merger catalogs as priors for classifying unassociated Fermi sources. The paper has genuine strengths: it uses a standard Poisson cross-match formalism, public catalogs, a transparent data-provenance statement in Section 2.1, a full table of matches, and an explicit control-sample attempt. However, the statistical support for the headline result is incomplete: the paper does not provide a global chance-coincidence budget, and the single shifted control is not a calibrated null. The result is currently suggestive rather than secure.

major comments (3)
  1. [Section 3, Eq. (2)] The claim that 21 of 38 coincidences are “statistically secure” is based on per-object p-values, but the paper never computes the global expected number of chance coincidences, Λ = Σ_i μ_i, summed over all 4FGL-DR4 sources. Under the null, the expected number of spatial coincidences is Λ, and for the small μ_i typical in this analysis the expected number of coincidences with p<0.05 is also approximately Λ; it is not 0.05×38. Without Λ, the observed 38 coincidences and 21 “secure” matches cannot be interpreted as an excess. Please report Λ, its Poisson uncertainty, and a Monte Carlo distribution of the number of matches and of the p-values under the null, and adjust the significance claims accordingly.
  2. [Section 3, control-sample paragraph] The shifted control sample is a single realization and is not a calibrated null. A shift of ±2° should approximately preserve the local merger surface density, so under the Poisson model the shifted sample should produce an expected number of chance coincidences close to the unshifted expectation; zero matches in one realization is therefore either an unlikely fluctuation or a sign that the shift does not preserve the survey mask/selection function. Please replace this with a Monte Carlo control using many independent shifts that preserve the 4FGL and SDSS footprints and the merger clustering, and report the distribution of the number of coincidences and of the p-values. A non-merger baseline (e.g., random SDSS galaxies with similar magnitude and redshift distributions) should also be included to test whether the excess is specific to mergers.
  3. [Section 2, Eq. (1)] The surface density n_s(>S) is estimated by dividing counts from the merger catalog by a single footprint area of 6190 deg^2, obtained from an RA/Dec binning whose bin size is not specified. Because every p-value in Eq. (2) scales linearly with n_s, uncertainty in the footprint and in the binning choice propagates directly into the list of 21 “secure” matches. Moreover, the merger catalog is strongly clustered (Figure 3), so a uniform global density may not represent the local chance-coincidence rate. Please specify the binning, quote an uncertainty on the footprint, and compare with a local-density estimate of n_s (e.g., from shuffled or nearest-neighbor catalogs).
minor comments (6)
  1. [Abstract] The phrase “galaxy mergers (Ackermann et al., 2018) catalog” is ungrammatical and should be rephrased.
  2. [Section 3 and Table 1] The text uses “4σ positional uncertainty ellipse” and “95% positional uncertainty (σ)” interchangeably; please define σ precisely and state whether the quoted separations are in units of the 1σ, 95%, or 4σ ellipse.
  3. [Author line] The surname appears as “Mannaa” in the author line and as “Manna” in the email address; please make this consistent.
  4. [Section 1] The statement that a 1 arcminute search around UGC 12914/5, UGC 813/6, VV 114, NGC 660, and NGC 3256 found no 4FGL-DR4 matches is made without listing the exact search parameters or the resulting upper limits; adding a short table or explicit thresholds would make the statement reproducible.
  5. [Section 3] The observation that none of the 21 secure matches is a pulsar would be more informative if compared with the expected pulsar fraction among randomly selected 4FGL-DR4 sources of similar flux.
  6. [References] Several reference entries contain LaTeX artifacts (e.g., “V orontsov-Velyaminov”, “V oges”, “C.E., Czarapata, P.C.”); these should be cleaned up before final submission.

Circularity Check

0 steps flagged · score 1.0 of 10

No significant circularity: the merger-Fermi association probabilities use standard external thresholds and an independent chance-coincidence background; no load-bearing fitted input or self-citation.

full rationale

The derivation chain is self-contained against external benchmarks. The merger sample is from Ackermann et al. (2018), and the gamma-ray positions and error ellipses are from the external 4FGL-DR4 catalog. Equations 1 and 2 use the standard Poisson chance-coincidence framework (Browne and Cohen 1978; Downes et al. 1986; Biggs et al. 2011; Zhang et al. 2022), with 4-sigma and p<0.05 thresholds imported from Zhang et al. (2022) rather than tuned to this dataset. Estimating n_s(>S) from the public merger catalog itself is the conventional way to define a null density for positional matching; it is not fitted to reproduce the 21 claimed associations and each candidate is treated individually. The shifted control is an additional null check, not an input to the p-values. The only self-citation (Ramakrishnan and Desai 2025) appears in a list of prior Fermi cross-matching studies and does not support any central premise. Statistical concerns about not reporting the total expected number of chance coincidences across the full 4FGL search and about the uncalibrated single shifted control affect the evidential strength of the claim, but they are not circularity because the claimed associations are not obtained by fitting a parameter to the gamma-ray data or by equating a prediction to its defining input.

Assumptions & free parameters 3 free parameters · 4 assumptions · 0 invented entities

The analysis uses no fitted theoretical parameters and introduces no new physical entities. The inputs are public catalogs, standard Poisson statistics, and hand-chosen analysis thresholds (pm>0.95, 4 sigma, p<0.05). The key uncontrolled inputs are the effective sky area (6,190 deg^2), from which all surface densities are derived, and the single-realization position-shifted control.

free parameters (3)
  • merger probability threshold (pm) = >0.95
    Hand-chosen threshold applied to all four CNN folds to define the high-confidence merger sample; affects sample size, surface density, and hence all p-values.
  • positional uncertainty threshold = 4 sigma
    Adopted from Zhang et al. (2022), not fitted; defines the matching ellipse and thus the chance-coincidence area.
  • sky area estimation binning = not specified
    The effective footprint of 6,190 deg^2 is computed by binning RA/Dec; the bin size is a choice that affects the surface density estimate and therefore every p-value.
assumptions (4)
  • standard math Poisson chance coincidence model: mu = pi*a*b*n_s(>S), p = 1 - exp(-mu)
    Standard approach from Browne and Cohen (1978), Downes et al. (1986), and Zhang et al. (2022); assumes independent Poisson fluctuations in the number of background mergers per ellipse.
  • domain assumption Uniform surface density of mergers over the estimated footprint
    The Poisson formula approximates the merger background as locally uniform; the real SDSS footprint geometry and merger clustering could bias mu. Invoked in Eq. 1.
  • domain assumption 4FGL-DR4 positional error ellipses correctly represent the localization uncertainty
    The match uses the catalog's 4 sigma error ellipses; if the ellipses are underestimated, particularly for faint sources, the chance-coincidence probability would be underestimated. Invoked in the matching procedure in Section 2.
  • domain assumption Position-shifted control sample is a valid null
    Shifting all mergers by random offsets within +/-2 degrees in RA and Dec is assumed to preserve the sample sky distribution while breaking physical associations; only a single realization is used. Section 3.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Search for spatial coincidences between galaxy mergers and Fermi-LAT 4FGL-DR4 sources." pith.science (2026). https://pith.science/paper/GYR5WJTB

@misc{pith2026250703970,
  author       = {Pith},
  title        = {Pith review of: Search for spatial coincidences between galaxy mergers and Fermi-LAT 4FGL-DR4 sources},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/GYR5WJTB}},
  note         = {Machine review of arXiv:2507.03970}
}
abstract

We present a systematic search for spatial association between a high confidence sample of 3,166 morphologically selected galaxy mergers drawn from the initial convolutional neural network (CNN) catalog of 328,151 candidate mergers and refined through SDSS cross-matching and the Fermi Large Area Telescope Fourth Source Catalog Data Release 4 (4FGL-DR4) catalog of gamma-ray sources detected by the Fermi Large Area Telescope (LAT). Using a conservative 4$\sigma$ positional uncertainty threshold and a Poisson based statistical framework, we identify 21 statistically significant associations with match probabilities $p < 0.05$. Among these are known classes of gamma-ray emitters such as Flat-Spectrum Radio Quasars (FSRQs), BL Lacertae objects (BLL), and radio galaxies bolstering the hypothesis that merger driven processes can fuel high energy activity. Intriguingly, five of the associated sources remain unclassified in 4FGL-DR4, hinting at a possible link between galaxy mergers and a hitherto unrecognized population of gamma-ray sources. The dominance of AGN like matches supports the scenario in which mergers trigger accretion onto central supermassive black holes, initiating AGN activity observable at gamma-ray energies. Moreover, the recurrent presence of unassociated sources among secure matches underscores the potential of merger catalogs as physically motivated priors in gamma-ray source identification efforts. This work constitutes the first dedicated effort to explore associations between gamma-ray sources and a large, morphologically selected sample of galaxy mergers catalog, opening new avenues for understanding the role of galaxy interactions in high-energy astrophysics.

Figures

Figures reproduced from arXiv: 2507.03970 by the authors.

Figure 1
Figure 1. Methodological workflow used in Ackermann et al. (2018), illustrating the training and evaluation pipeline for galaxy merger classification using CNNs and transfer learning from ImageNet. This figure has been adapted from Ackermann et al. (2018). To isolate high-confidence systems, we applied a strict threshold of pm > 0.95 across all four classifier outputs, retaining only those galaxies that satisfied this criteri… view at source ↗
Figure 2
Figure 2. Filtering workflow for galaxy merger catalog refinement. The process reduces 328,151 initial candidates [PITH_FULL_IMAGE:figures/full_fig_p006_2.png] view at source ↗
Figure 3
Figure 3. Aitoff projection showing the sky distribution of 3,166 galaxy mergers (Ackermann et al., 2018) with SDSS r-band magnitudes. Positions are plotted in equatorial coordinates (RA, Dec). The probability of random coincidence (i.e., the p-value) is then given by: p = 1 − e −µ . (2) A small value p indicates a low probability of random association, which implies a more reliable counterpart match. We adopt a primary thres… view at source ↗
Figures from the paper (4 more)
Figure 4
Figure 4. Figure 4: Redshift distribution comparison between the full merger catalog (gray) and the 21 matched mergers (red). The [PITH_FULL_IMAGE:figures/full_fig_p011_4.png]
Figure 5
Figure 5. Figure 5: r-band magnitude distribution comparison between the full merger catalog (gray) and the 21 matched mergers (blue). The matched sample spans a range of magnitudes from ∼14 to ∼17.5 mag, representative of the brighter portion of the full sample. 11 [PITH_FULL_IMAGE:figu…
Figure 6
Figure 6. Figure 6: Angular separation (in units of positional uncertainty [PITH_FULL_IMAGE:figures/full_fig_p012_6.png]
Figure 7
Figure 7. Figure 7: Merger positions located within the 4σ positional uncertainty ellipses of their associated Fermi sources. Each panel corresponds to a different matched Fermi source. The blue dot indicates the Fermi source position, while the red cross marks the galaxy merger with the …

Discussion (0). Sign in to comment.

Reference graph

Works this paper leans on

58 extracted references · 24 canonical work pages

  1. [1]

    The table is sorted in decreasing order of p-value

    13 Table 1: Complete list of 21 secure matches between Fermi 4FGL-DR4 sources and galaxy mergers, defined by p-value < 0.05. The table is sorted in decreasing order of p-value. Uncertainties in r-band magnitudes are from SDSS DR16 photometry; redshift uncertainties are from SIMBAD; flux errors are calculated from r-band magnitudes. Fermi Source Merger RA ...

    work page 1937

  2. [3]

    doi: 10.3847/1538-4365/ab929e, arXiv:1912.02905. Atwood, W.B., Abdo, A.A., Ackermann, M., Althouse, W., Anderson, B., Axelsson, M., Baldini, L., Ballet, J., Band, D.L., Barbiellini, G., Bartelt, J., Bastieri, D., Baughman, B.M., Bechtol, K., Bédérède, D., Bellardi, F., Bellazzini, R., Berenji, B., Bignami, G.F., Bisello, D., Bissaldi, E., Blandford, R.D.,...

    arXiv 1912

  3. [4]

    doi: 10.3847/1538-4365/ab16f4, arXiv:1903.11124. Darg, D.W., Kaviraj, S., Lintott, C.J., Schawinski, K., Sarzi, M., Bamford, S., Silk, J., Proctor, R., Andreescu, D., Murray, P., Nichol, R.C., Raddick, M.J., Slosar, A., Szalay, A.S., Thomas, D., Vandenberg, J.,

    arXiv 1903

  4. [7]

    Astrophys

    The Large Area Telescope on the Fermi Gamma-Ray Space Telescope Mission. Astrophys. J. 697, 1071–1102. doi: 10.1088/0004-637X/697/2/1071, arXiv:0902.1089. Ballet, J., Bruel, P., Burnett, T.H., Lott, B., The Fermi-LAT collaboration,

    arXiv

  5. [10]

    Paliya, V .S., Pérez, E., García-Benito, R., Ajello, M., Prada, F., Alberdi, A., Suh, H., Chandra, C.H.I., Domínguez, A., Marchesi, S., Di Matteo, T., Hartmann, D., Chiaberge, M.,

    3847/1538-4357/acd172, arXiv:2304.10934. Paliya, V .S., Pérez, E., García-Benito, R., Ajello, M., Prada, F., Alberdi, A., Suh, H., Chandra, C.H.I., Domínguez, A., Marchesi, S., Di Matteo, T., Hartmann, D., Chiaberge, M.,

    arXiv

  6. [12]

    Compact Groups of Galaxies in Sloan Digital Sky Survey and LAMOST Spectral Survey: I. The Catalogs

    doi: 10.3847/1538-4365/ab5c26, arXiv:1911.11478. Appendix A. SDSS Flux Conversion Methodology SDSS magnitudes are reported in the asinh magnitude system (Lupton et al., 1999), which handle low S /N and negative fluxes more robustly than traditional Pogson magnitudes. The inverse asinh formula for converting r-band apparent magnitudes (mr) to fluxes is: fr...

    work page Pith review arXiv 1911

  7. [18]

    Imagenet: A large-scale hierarchical image database, in: 2009 IEEE Conference on Computer Vision and Pattern Recognition, pp. 248–255. doi: 10.1109/CVPR.2009. 5206848. Downes, A.J.B., Peacock, J.A., Savage, A., Carrie, D.R.,

    doi:10.1109/cvpr.2009 2009

  8. [23]

    Comparison of black hole growth in galaxy mergers with GASOLINE and RAMSES. Astron. & Astrophys. 592, A62. doi:10.1051/ 0004-6361/201527143, arXiv:1508.02224. Gaia Collaboration,

    work page Pith review arXiv

Show all 58 references
  1. [26]

    doi:10.1093/pasj/psx135, arXiv:1706.07436

    Galaxy interactions trigger rapid black hole growth: An unprecedented view from the Hyper Suprime-Cam survey 70, S37. doi:10.1093/pasj/psx135, arXiv:1706.07436. Himes, M., Jagannathan, P., Frail, D.A., Schinzel, F., Gupta, N., Balashev, S.A., Combes, F., Deka, P.P., Klöckner, ...

    arXiv

  2. [30]

    Astrophys

    A Catalog of Morphologically Identified Merging Galaxies. Astrophys. J. Suppl. Ser. 181, 233–237. doi: 10.1088/0067-0049/181/1/233. Kashiyama, K., Mészáros, P.,

    doi

  3. [32]

    arXiv e-prints , arXiv:2506.09136 arXiv:2506.09136

    Mergers of galaxies. arXiv e-prints , arXiv:2506.09136 arXiv:2506.09136. Kozieł-Wierzbowska, D., Goyal, A., ˙Zywucka, N.,

    arXiv

  4. [33]

    Krizhevsky, A., Sutskever, I., Hinton, G.E.,

    doi:10.3847/1538-4365/ab63d3, arXiv:1912.09959. Krizhevsky, A., Sutskever, I., Hinton, G.E.,

    1912 arXiv

  5. [34]

    Imagenet classification with deep convolutional neural networks. Commun. ACM 60, 84–90. doi:10.1145/3065386. Lintott, C., Schawinski, K., Bamford, S., Slosar, A., Land, K., Thomas, D., Edmondson, E., Masters, K., Nichol, R.C., Raddick, M.J., Szalay, A., Andreescu, D., Murray, ...

    doi

  6. [35]

    MNRAS 410, 166–178

    Galaxy Zoo 1: data release of morphological classifications for nearly 900 000 galaxies. MNRAS 410, 166–178. doi: 10.1111/j.1365-2966. 2010.17432.x, arXiv:1007.3265. Lintott, C.J., Schawinski, K., Slosar, A., Land, K., Bamford, S., Thomas, D., Raddick, M.J., Nichol, R.C., Szal...

    2010

  7. [36]

    MNRAS 389, 1179–1189

    Galaxy Zoo: morphologies derived from visual inspection of galaxies from the Sloan Digital Sky Survey. MNRAS 389, 1179–1189. doi:10.1111/j.1365-2966.2008.13689. x, arXiv:0804.4483. Lisenfeld, U., Völk, H.J.,

    2008

  8. [37]

    Shock acceleration of relativistic particles in galaxy-galaxy collisions. Astron. & Astrophys. 524, A27. doi: 10.1051/0004-6361/201015083, arXiv:1009.1659. Liu, X., Shen, Y ., Strauss, M.A., Hao, L.,

    arXiv

  9. [40]

    Roma- BZCAT: a multifrequency catalogue of blazars. Astron. & Astrophys. 495, 691–696. doi: 10.1051/0004-6361: 200810161, arXiv:0810.2206. Mayer, M.G.F., Becker, W.,

    arXiv

  10. [45]

    JCAP 2025,

    Search for transient gamma-ray emission from magnetar flares using Fermi-LAT. JCAP 2025,

    2025

  11. [47]

    MNRAS 436, 997–1016

    The environments of luminous radio galaxies and type-2 quasars. MNRAS 436, 997–1016. doi: 10.1093/ mnras/stt1595, arXiv:1308.4725. Satyapal, S., Ellison, S.L., McAlpine, W., Hickox, R.C., Patton, D.R., Mendel, J.T.,

    arXiv

  12. [48]

    Merger-induced AGN activity as traced by the Wide-field Infrared Survey Explorer

    Galaxy pairs in the Sloan Digital Sky Survey - IX. Merger-induced AGN activity as traced by the Wide-field Infrared Survey Explorer. MNRAS 441, 1297–1304. doi: 10.1093/mnras/stu650, arXiv:1403.7531. Scudder, J.M., Ellison, S.L., Torrey, P., Patton, D.R., Mendel, J.T.,

    arXiv

  13. [49]

    Tracing changes in star formation rate and metallicity out to separations of 80 kpc

    Galaxy pairs in the Sloan Digital Sky Survey - V . Tracing changes in star formation rate and metallicity out to separations of 80 kpc. MNRAS 426, 549–565. doi:10.1111/j.1365-2966.2012.21749.x, arXiv:1207.4791. Stoughton, C., Lupton, R.H., Bernardi, M., Blanton, M.R., Burles, ...

    2012

  14. [50]

    Ramos Almeida, C., Bessiere, P.S., Tadhunter, C.N., Inskip, K.J., Morganti, R., Dicken, D., González-Serrano, J.I., Holt, J.,

    doi: 10.1088/1475-7516/2025/07/050, arXiv:2412.03900. Ramos Almeida, C., Bessiere, P.S., Tadhunter, C.N., Inskip, K.J., Morganti, R., Dicken, D., González-Serrano, J.I., Holt, J.,

    2025 arXiv

  15. [51]

    Chiaberge, M., Gilli, R., Lotz, J.M., Norman, C.,

    doi: 10.3847/1538-4357/acaa33, arXiv:2212.05115. Chiaberge, M., Gilli, R., Lotz, J.M., Norman, C.,

    arXiv

  16. [52]

    Torres, D.F.,

    doi:10.1088/0004-637X/ 788/1/45, arXiv:1404.4937. Torres, D.F.,

    arXiv

  17. [53]

    doi:10.3847/1538-4365/ac6751, arXiv:2201.11184. Ackermann, M., Ajello, M., Allafort, A., Baldini, L., Ballet, J., Bastieri, D., Bechtol, K., Bellazzini, R., Berenji, B., Bloom, E.D., Bonamente, E., Borgland, A.W., Bouvier, A., Bregeon, J., Brigida, M., Bruel, P., Buehler, R., ...

    arXiv

  18. [54]

    Search for the multi-wavelength counterparts to extragalactic unassociated Fermi γ-ray sources. Astron. & Astrophys. 694, A176. doi: 10.1051/0004-6361/202452366, arXiv:2412.19314. V oges, W., Aschenbach, B., Boller, T., Bräuninger, H., Briel, U., Burkert, W., Dennerl, K., Engl...

    arXiv

  19. [55]

    The ROSAT all-sky survey bright source catalogue. Astron. & Astrophys. 349, 389–405. doi: 10.48550/arXiv.astro-ph/9909315, arXiv:astro-ph/9909315. V orontsov-Velyaminov, B.A., Noskova, R.I., Arkhipova, V .P.,

    doi arXiv

  20. [57]

    Zhang, L., Vieira, J.D., Ajello, M., Malkan, M.A., Archipley, M.A., Capota, J., Foster, A., Madejski, G.,

    doi: 10.3847/1538-4357/aab774, arXiv:1712.09754. Zhang, L., Vieira, J.D., Ajello, M., Malkan, M.A., Archipley, M.A., Capota, J., Foster, A., Madejski, G.,

    arXiv

  21. [81]

    Hopkins, P.F., Hernquist, L., Cox, T.J., Di Matteo, T., Robertson, B., Springel, V .,

    doi: 10.3847/1538-4357/ada1cf, arXiv:2412.12470. Hopkins, P.F., Hernquist, L., Cox, T.J., Di Matteo, T., Robertson, B., Springel, V .,

    arXiv

  22. [101]

    Lupton, R.H., Gunn, J.E., Szalay, A.S.,

    doi: 10.1088/0004-637X/737/2/101, arXiv:1104.0950. Lupton, R.H., Gunn, J.E., Szalay, A.S.,

    arXiv

  23. [117]

    Zheng, Y .L., Shen, S.Y .,

    doi: 10.3847/1538-4357/ac966f, arXiv:2206.06228. Zheng, Y .L., Shen, S.Y .,

    arXiv

  24. [133]

    Patton, D.R., Grant, J.K., Simard, L., Pritchet, C.J., Carlberg, R.G., Borne, K.D.,

    doi: 10.3847/1538-4357/ab754f, arXiv:2004.02703. Patton, D.R., Grant, J.K., Simard, L., Pritchet, C.J., Carlberg, R.G., Borne, K.D.,

    2004 arXiv

  25. [147]

    Chollet, F.,

    doi:10.1088/0004-637X/806/2/147, arXiv:1505.07419. Chollet, F.,

    arXiv

  26. [164]

    Ackermann, S., Schawinski, K., Zhang, C., Weigel, A.K., Turp, M.D.,

    doi: 10.1088/0004-637X/755/2/164, arXiv:1206.1346. Ackermann, S., Schawinski, K., Zhang, C., Weigel, A.K., Turp, M.D.,

    arXiv

  27. [220]

    Astrophys. J. 617, 966–986. doi:10.1086/425415, arXiv:astro-ph/0407240. Ulgiati, A., Paiano, S., Pintore, F., Russell, T.D., Sbarufatti, B., Pinto, C., Ambrosi, E., D’Aì, A., Cusumano, G., Del Santo, M.,

    arXiv

  28. [717]

    Wenger, M., Ochsenbein, F., Egret, D., Dubois, P., Bonnarel, F., Borde, S., Genova, F., Jasniewicz, G., Laloë, S., Lesteven, S., Monier, R.,

    doi:10.1080/10556790108208213. Wenger, M., Ochsenbein, F., Egret, D., Dubois, P., Bonnarel, F., Borde, S., Genova, F., Jasniewicz, G., Laloë, S., Lesteven, S., Monier, R.,

    doi

  29. [1978]

    MNRAS 182, 181–187

    Quasars near bright galaxies - results from the Jodrell Bank 966-MHz survey. MNRAS 182, 181–187. doi: 10.1093/mnras/182.2.181. Bruzewski, S., Schinzel, F.K., Taylor, G.B.,

    doi

  30. [1986]

    MNRAS 218, 31–62

    The Parkes selected regions : powerful radio galaxies and quasars at high redshifts. MNRAS 218, 31–62. doi: 10.1093/mnras/218.1.31. Duarte Puertas, S., Vilchez, J.M., Iglesias-Páramo, J., Kehrig, C., Pérez-Montero, E., Rosales-Ortega, F.F.,

    doi

  31. [1999]

    A Modified Magnitude System that Produces Well-Behaved Magnitudes, Colors, and Errors Even for Low Signal-to-Noise Ratio Measurements. Astron. J. 118, 1406–1410. doi: 10.1086/ 301004, arXiv:astro-ph/9903081. Massaro, E., Giommi, P., Leto, C., Marchegiani, P., Maselli, A., Perr...

    arXiv

  32. [2000]

    The CDS reference database for as- tronomical objects

    The SIMBAD astronomical database. The CDS reference database for as- tronomical objects. Astronomy and Astrophysics Supplement Series 143, 9–22. doi: 10.1051/aas:2000332, arXiv:astro-ph/0002110. Yuan, C., Mészáros, P., Murase, K., Jeong, D.,

    arXiv

  33. [2002]

    Sloan Digital Sky Survey: Early Data Release. Astron. J. 123, 485–548. doi: 10.1086/324741. Taylor, M.B.,

    doi

  34. [2004]

    Catalog of Double Nucleus Disk Galaxies. Astron. J. 128, 62–67. doi:10.1086/421371. Goulding, A.D., Greene, J.E., Bezanson, R., Greco, J., Johnson, S., Leauthaud, A., Matsuoka, Y ., Medezinski, E., Price- Whelan, A.M.,

    doi

  35. [2005]

    A Hubble Space Telescope 17 Snapshot Survey of Dynamically Close Galaxy Pairs in the CNOC2 Redshift Survey. Astron. J. 130, 2043–2057. doi:10.1086/491672, arXiv:astro-ph/0507417. Ramakrishnan, V ., Desai, S.,

    arXiv

  36. [2006]

    Astrophys

    A Unified, Merger-driven Model of the Origin of Starbursts, Quasars, the Cosmic X-Ray Background, Supermassive Black Holes, and Galaxy Spheroids. Astrophys. J. Suppl. Ser. 163, 1–49. doi: 10.1086/499298, arXiv:astro-ph/0506398. Hoyos, C., Aragón-Salamanca, A., Gray, M.E., Malt...

    arXiv

  37. [2008]

    Galaxy Pairs in the Sloan Digital Sky Survey. I. Star Formation, Active Galactic Nucleus Fraction, and the Mass-Metallicity Relation. Astron. J. 135, 1877–1899. doi:10.1088/0004-6256/135/5/1877, arXiv:0803.0161. 16 Gabor, J.M., Capelo, P.R., V olonteri, M., Bournaud, F., Bello...

    arXiv

  38. [2009]

    Astrophys

    The Seventh Data Release of the Sloan Digital Sky Survey. Astrophys. J. Suppl. Ser. 182, 543–558. doi: 10.1088/0067-0049/182/2/543, arXiv:0812.0649. Abdollahi, S., Acero, F., Baldini, L., Ballet, J., Bastieri, D., Bellazzini, R., Berenji, B., Berretta, A., Bissaldi, E., Bland-...

    arXiv

  39. [2010]

    MNRAS 401, 1043–1056

    Galaxy Zoo: the fraction of merging galaxies in the SDSS and their morphologies. MNRAS 401, 1043–1056. doi: 10.1111/j. 1365-2966.2009.15686.x, arXiv:0903.4937. Deng, J., Dong, W., Socher, R., Li, L.J., Li, K., Fei-Fei, L.,

    2009

  40. [2011]

    MNRAS 413, 2314–2338

    The LABOCA survey of the Extended Chandra Deep Field-South - radio and mid-infrared counterparts to submillimetre galaxies. MNRAS 413, 2314–2338. doi: 10.1111/j.1365-2966.2010.18132.x, arXiv:1012.0305. Bouri, S., Parashari, P., Das, M., Laha, R.,

    2010

  41. [2012]

    Description and application to the Space Telescope A901 /902 Galaxy Evolution Survey

    A new automatic method to identify galaxy mergers - I. Description and application to the Space Telescope A901 /902 Galaxy Evolution Survey. MNRAS 419, 2703–2724. doi:10.1111/j.1365-2966.2011.19918.x, arXiv:1109.6828. Hwang, C.Y ., Chang, M.Y .,

    2011

  42. [2013]

    MNRAS 431, 2661–2672

    The merger fraction of active and inactive galaxies in the local Universe through an improved non-parametric classifica- tion. MNRAS 431, 2661–2672. doi: 10.1093/mnras/stt358, arXiv:1303.0036. D’Abrusco, R., Álvarez Crespo, N., Massaro, F., Campana, R., Chavushyan, V ., Landon...

    arXiv

  43. [2014]

    Astro- phys

    Galaxy Mergers as a Source of Cosmic Rays, Neutrinos, and Gamma Rays. Astro- phys. J. Lett. 790, L14. doi: 10.1088/2041-8205/790/1/L14, arXiv:1405.3262. Kaviraj, S.,

    arXiv

  44. [2016]

    arXiv e-prints , arXiv:1610.02357doi:10.48550/arXiv.1610.02357, arXiv:1610.02357

    Xception: Deep Learning with Depthwise Separable Convolutions. arXiv e-prints , arXiv:1610.02357doi:10.48550/arXiv.1610.02357, arXiv:1610.02357. Cotini, S., Ripamonti, E., Caccianiga, A., Colpi, M., Della Ceca, R., Mapelli, M., Severgnini, P., Segreto, A.,

    doi arXiv

  45. [2017]

    Aperture-free star formation rate of SDSS star-forming galaxies. Astron. & Astrophys. 599, A71. doi: 10.1051/ 0004-6361/201629044, arXiv:1611.07935. Ellison, S.L., Patton, D.R., Mendel, J.T., Scudder, J.M.,

    arXiv

  46. [2018]

    MNRAS 479, 415–425

    Using transfer learning to detect galaxy mergers. MNRAS 479, 415–425. doi: 10.1093/mnras/sty1398, arXiv:1805.10289. Ahumada, R., Allende Prieto, C., Almeida, A., Anders, F., Anderson, S.F., Andrews, B.H., Anguiano, B., Arcodia, R., Armengaud, E., Aubert, M., Avila, S., Avila-R...

    arXiv

  47. [2020]

    VizieR On-line Data Catalog: I/350

    VizieR Online Data Catalog: Gaia EDR3 (Gaia Collaboration, 2020). VizieR On-line Data Catalog: I/350. Originally published in: 2021A&A...649A...1G. doi: 10.26093/cds/vizier.1350. Gimeno, G.N., Díaz, R.J., Carranza, G.J.,

    2020 doi

  48. [2023]

    arXiv e-prints , arXiv:2307.12546doi:10.48550/arXiv.2307.12546, arXiv:2307.12546

    Fermi Large Area Telescope Fourth Source Catalog Data Release 4 (4FGL-DR4). arXiv e-prints , arXiv:2307.12546doi:10.48550/arXiv.2307.12546, arXiv:2307.12546. Becker, R.H., White, R.L., Helfand, D.J.,

    doi arXiv

  49. [2024]

    Searching for X-ray counterparts of unassociated Fermi-LAT sources and rotation- powered pulsars with SRG /eROSITA. Astron. & Astrophys. 684, A208. doi: 10.1051/0004-6361/202348620, arXiv:2401.17295. Negro, M., Crnogor ˇcevi´c, M., Burns, E., Charles, E., Marcotulli, L., Caputo, R.,

    arXiv

  50. [2025]

    Physical Review D 111, 063059

    First search for high-energy neutrino emission from galaxy mergers. Physical Review D 111, 063059. doi:10.1103/PhysRevD.111.063059, arXiv:2404.06539. Browne, I.W.A., Cohen, A.M.,

    arXiv

Pith tools

Reviewed August 6, 2026 · model on record in the stance chip above.