pith. machine review for the scientific record. sign in

arxiv: 2605.13946 · v1 · submitted 2026-05-13 · 🌌 astro-ph.GA

Recognition: no theorem link

The Hunt for Red Dual AGNs I: Spatially-Resolved Mid-IR Dual AGNs in the DeCam Legacy Survey

Ryan W. Pfeifle , Kimberly A. Weaver , Barry Rothberg , Miranda McCarthy , Emma Schwartzman , Nathan J. Secrest , Peter G. Boorman , Daniel Stern
show 8 more authors
Joanna Piotrowska Kevin McCarthy Emily Moravec Jenna M. Cann Kimberly Engle Kyla Mullaney Ryan Tanner Kelly Whalen
Authors on Pith no claims yet

Pith reviewed 2026-05-15 02:46 UTC · model grok-4.3

classification 🌌 astro-ph.GA
keywords dual AGNsmid-IR selectiongalaxy mergersWISE W1-W2DeCam Legacy SurveyBPT diagnosticssupermassive black holesmulti-merger systems
0
0 comments X

The pith

Mid-infrared colors select 13 confirmed dual AGNs in galaxy mergers at separations of 14.5 to 129 kiloparsecs.

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

The paper assembles a sample of 157 dual AGN candidates by applying WISE W1-W2 mid-infrared color cuts to isolate AGN activity and then using Dark Energy Camera Legacy Survey imaging to flag optical galaxy mergers. Spectroscopic follow-up on roughly two-thirds of the sample confirms 76 systems as mergers, of which 13 are verified dual AGNs and 63 remain strong candidates. These confirmed and high-confidence objects span projected separations from 14.5 to 129 kpc, with more than half lying beyond 50 kpc. The pairs display a range of optical BPT spectral classes, dominated by Seyfert-Seyfert and Seyfert-HII combinations, and nearly one-third occur inside multi-merger systems containing three or more galaxies. This selection reaches earlier or wider merger phases than optical-line searches restricted to nuclear separations below 10 kpc.

Core claim

A mid-IR color-selected search combined with optical merger classification yields 157 spatially resolved dual AGN candidates; spectroscopic verification establishes 13 bona fide mid-IR dual AGNs at separations 14.5-129 kpc together with 63 additional strong candidates, many residing at separations greater than 50 kpc and showing diverse nuclear optical spectral types.

What carries the argument

The W1-W2 mid-infrared color cut from WISE photometry that isolates AGN-heated dust, applied to optically identified galaxy merger candidates from DeCam Legacy Survey imaging, followed by spectroscopic confirmation.

Load-bearing premise

Mid-infrared W1-W2 colors cleanly isolate AGN activity without significant contamination from star formation in merging galaxies, and optical imaging reliably distinguishes true physical mergers from chance projections.

What would settle it

High-resolution spectroscopy or X-ray observations showing that the mid-IR excess in the majority of candidates arises from star formation rather than accretion, or integral-field spectroscopy revealing that apparent wide pairs are unrelated foreground and background objects.

Figures

Figures reproduced from arXiv: 2605.13946 by Barry Rothberg, Daniel Stern, Emily Moravec, Emma Schwartzman, Jenna M. Cann, Joanna Piotrowska, Kelly Whalen, Kevin McCarthy, Kimberly A. Weaver, Kimberly Engle, Kyla Mullaney, Miranda McCarthy, Nathan J. Secrest, Peter G. Boorman, Ryan Tanner, Ryan W. Pfeifle.

Figure 1
Figure 1. Figure 1: A flowchart detailing the selection methodology outlined in Sections 2.1-2.6. 20′′ < θ < 60′′. Mid-IR AGN pairs were classified into one of the following general categories: 1. “m”: A clear galaxy merger or a galaxy merger candidate. 2. “bf”: A foreground/background pair (pairs for which one mid-IR source had a clear optical coun￾terpart but the other mid-IR source had a very faint counterpart or no observ… view at source ↗
Figure 2
Figure 2. Figure 2: The redshift distribution plotted against the projected separation (kpc) distribution for the sample of Rank 1 and 0.5 spatially-resolved mid-IR dual AGNs in this sample. The data are color coded according to the angular separation of the mid-IR AGN pairs, with the color map provided on the auxiliary color bar; Rank 1 (confirmed) candidates are represented by circles with dark outlines, while Rank 0.5 cand… view at source ↗
Figure 3
Figure 3. Figure 3: Projected, physical separation (kpc) and ve￾locity difference (km s−1 ) distribution for Rank 1 and 0.5 spatially-resolved mid-IR dual AGNs, color coded by (top) WISE W1−W2 color and (bottom) WISE W1 luminosity. In each panel, Rank 1 mid-IR dual AGN pairs are represented by two concentric circles: the inner circle represents AGN 1, and the outer circle represents AGN 2, and the colors corre￾spond to the sc… view at source ↗
Figure 4
Figure 4. Figure 4: Rank 1 mid-IR dual AGNs. For each panel, the WISE designation for “AGN 1” is given in the top left corner, and a 10” scale bar is given in the bottom right corner. The redshifts of the two AGNs (z1 and z2), projected separation (rp), absolute velocity difference (|∆v|), and angular separation (θ) of the two mid-IR AGNs are given in the bottom left corner of each panel. White, 6” diameter dashed and dotted … view at source ↗
Figure 5
Figure 5. Figure 5: Rank 0.5 Mid-IR Dual AGN Candidates. Each panel is constructed in an identical fashion to those in [PITH_FULL_IMAGE:figures/full_fig_p016_5.png] view at source ↗
Figure 5
Figure 5. Figure 5: Continued [PITH_FULL_IMAGE:figures/full_fig_p017_5.png] view at source ↗
Figure 5
Figure 5. Figure 5: WISE mid-IR color space for (top, diamond markers) Rank 1 and (bottom) Rank +0.5 and 0 mid-IR dual candidates in this sample. W2 − W3 color is given on the x-axis and W1 − W2 color is given on the y-axis. The data are color coded according to WISE W1 luminosity when red￾shifts are available, where the scale is given on the auxiliary axes; where redshifts are not available, the nuclei are marked as open-fac… view at source ↗
Figure 6
Figure 6. Figure 6: BPT (Baldwin et al. 1981; Kewley et al. 2001; Kauffmann et al. 2003; Kewley et al. 2006) spectroscopic emission line ratio diagnostic plots for mid-IR dual AGNs with sufficient spectroscopic coverage. Left panel: log([N II]λ6584/Hα) diagnostic plot; the dashed red curve represents the theoretical starburst limit from Kewley et al. (2001), the dash-dotted blue curve is an empirically derived demarcation sep… view at source ↗
Figure 7
Figure 7. Figure 7: The distribution of projected separations (kpc) for Rank 1 and 0.5 mid-IR dual AGN as a function of BPT optical class. The projected separation bins are given on the x-axis, and the number of sources per bin is given on the y-axis. Seyferts, LINERs, composites, and star form￾ing regions are represented by red (diagonal hatched), green (dot hatched), orange (cross hatched), and blue (horizontal hatched) col… view at source ↗
Figure 8
Figure 8. Figure 8: BPT (Baldwin et al. 1981) spectroscopic emission line ratio diagnostic plots for mid-IR dual AGN candidates with sufficient spectroscopic coverage, color coded by (top) W1 − W2 color and (bottom) WISE W1 luminosity. The emission line ratios and red dashed, blue dash-dotted, and black dotted demarcations are identical to those depicted in the left panel of [PITH_FULL_IMAGE:figures/full_fig_p021_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Rank 0 mid-IR dual AGN candidates. Each panel is constructed in an identical fashion to those in Figures 4 and 5.1 [PITH_FULL_IMAGE:figures/full_fig_p030_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Rejected mid-IR dual AGN candidates. Each panel is constructed in an identical fashion to those in [PITH_FULL_IMAGE:figures/full_fig_p033_10.png] view at source ↗
Figure 10
Figure 10. Figure 10: Continued 0.05 0.10 0.15 0.20 0.25 0.30 0.35 0.40 Spectroscopic Redshift 0.05 0.10 0.15 0.20 0.25 0.30 0.35 0.40 Photometric Redshift 2.8 3.0 3.2 3.4 3.6 3.8 4.0 4.2 4.4 lo g(| v|P h oto) [PITH_FULL_IMAGE:figures/full_fig_p034_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: Spectroscopic vs. photometric redshifts for Rank 0.5 and 1 dual AGNs in this work, where both nuclei have measured spectroscopic redshifts. Spectroscopic red￾shifts are plotted on the x-axis, and photometric redshifts are plotted on the y-axis. The dashed line indicates unity between the phot- and spec-z’s. The data points represent individual nuclei in the sample and are color coded by the logarithm of t… view at source ↗
read the original abstract

Theoretical studies predict that dual AGNs are a critical stage of galaxy merger-driven supermassive black hole growth. Systematic searches for dual AGNs typically target late-stage mergers ($\leq10$ kpc nuclear separations) and select AGNs based on optical diagnostics. Yet, simulations predict that obscuration can occur early in the merger sequence, and that a significant fraction of dual AGNs can be found beyond $10$ kpc. Here, we report on a new sample of 157 spatially resolved mid-IR dual AGNs candidates selected based upon their mid-IR $W1-W2$ colors from the Wide-Field Infrared Survey Explorer and optically classified as galaxy merger candidates using imaging from the Dark Energy Camera Legacy Survey. Spectroscopic results are presented for approximately 2/3 of the sample. 76 candidates have been confirmed to reside in galaxy mergers; among these, 13 have been confirmed as bona fide mid-IR dual AGNs, while 63 represent strong dual AGN candidates that require further examination. 46 candidates have been rejected as non-merger contaminants (foreground-background AGNs, separations inconsistent with interacting galaxies, etc.). 35 candidates still await spectroscopic coverage. The confirmed and high confidence dual AGN candidates exhibit separations of 14.5-129 kpc; $>50$% reside at separations $>50$ kpc. Confirmed and high confidence candidates also exhibit a diversity of nuclear optical BPT classes. Seyfert-Seyferts and Seyfert-HIIs dominate the overall BPT pairs sample. 31% of confirmed mid-IR dual AGNs reside in multi-mergers involving three or more galaxies. The diversity in AGN properties and environments identified in this work highlights the importance of multiwavelength selection strategies and analyses in the quest to holistically understand dual AGNs as a population.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

3 major / 2 minor

Summary. The manuscript reports the discovery of a sample of 157 spatially resolved mid-IR dual AGN candidates selected via WISE W1-W2 colors and classified as galaxy mergers using DeCam Legacy Survey imaging. Spectroscopic follow-up on approximately two-thirds of the sample confirms 13 bona fide dual AGNs with projected separations ranging from 14.5 to 129 kpc, along with 63 strong candidates, while rejecting 46 as contaminants and leaving 35 for future observation. The work emphasizes the prevalence of dual AGNs at large separations (>50 kpc for over half the confirmed sample) and their diverse optical BPT classifications.

Significance. If the selection criteria prove robust against contaminants, this study would be significant for demonstrating that dual AGNs can be found at much larger separations than the late-stage mergers typically targeted, aligning with theoretical predictions of obscuration in early merger phases. It also highlights the utility of mid-IR selection combined with optical imaging for identifying such systems, potentially increasing the known population of dual AGNs and informing models of supermassive black hole growth during galaxy mergers. The provision of specific counts and separation statistics strengthens the observational basis for these claims.

major comments (3)
  1. [Abstract and sample selection] The central claim of 13 confirmed dual AGNs from 157 candidates depends on the reliability of the W1-W2 color cut for isolating AGNs in merging galaxies. However, no quantitative assessment of contamination from star-forming regions or PAH emission in mergers is provided, nor is a control sample of non-merging galaxies analyzed to establish the purity of the selection. This is critical because the post-selection rejection of 46 objects does not retroactively validate the initial sample purity.
  2. [Spectroscopic results] The distinction between the 13 'bona fide' dual AGNs and the 63 'strong dual AGN candidates' needs explicit criteria, particularly how BPT classifications and line ratios are used to confirm dual activity versus single AGN or star formation. Without this, the claim of 13 confirmed systems is difficult to evaluate independently.
  3. [Discussion of separations] The statement that >50% of confirmed and high-confidence candidates reside at >50 kpc separations is central to the paper's novelty, but the potential for line-of-sight projections in DeCam visual classifications is not quantitatively addressed, which could inflate the number of wide pairs.
minor comments (2)
  1. [Abstract] Grammatical correction needed: 'mid-IR dual AGNs candidates' should read 'mid-IR dual AGN candidates'.
  2. [Abstract] The abstract mentions 'optically classified as galaxy merger candidates' but does not specify the exact morphological criteria used in DeCam imaging, which would aid clarity.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their constructive comments, which have helped clarify several aspects of our work. We address each major point below and will revise the manuscript accordingly where feasible.

read point-by-point responses

  1. Referee: [Abstract and sample selection] The central claim of 13 confirmed dual AGNs from 157 candidates depends on the reliability of the W1-W2 color cut for isolating AGNs in merging galaxies. However, no quantitative assessment of contamination from star-forming regions or PAH emission in mergers is provided, nor is a control sample of non-merging galaxies analyzed to establish the purity of the selection. This is critical because the post-selection rejection of 46 objects does not retroactively validate the initial sample purity.

    Authors: We agree that a dedicated control sample would provide stronger validation of the W1-W2 selection purity. The W1-W2 > 0.8 criterion is standard in the literature with documented contamination levels from star-forming galaxies and PAH emission. Our spectroscopic follow-up empirically rejected 46 contaminants from the observed subset. In revision, we will add a new subsection estimating contamination rates using published WISE color distributions for star-forming mergers and a brief comparison to a literature control sample of non-merging galaxies. A full new control sample observation is beyond the current scope. revision: partial

  2. Referee: [Spectroscopic results] The distinction between the 13 'bona fide' dual AGNs and the 63 'strong dual AGN candidates' needs explicit criteria, particularly how BPT classifications and line ratios are used to confirm dual activity versus single AGN or star formation. Without this, the claim of 13 confirmed systems is difficult to evaluate independently.

    Authors: We apologize for the insufficient detail in the original text. Bona fide dual AGNs require both nuclei to show AGN-like BPT classifications (Seyfert or LINER) with S/N > 5 on key lines and line ratios exceeding standard demarcation curves. Strong candidates have one confirmed AGN nucleus and the second with composite or ambiguous ratios needing deeper data. We will add an explicit methods subsection and a supplementary table listing the precise BPT criteria, line ratio thresholds, and classifications for all objects. revision: yes

  3. Referee: [Discussion of separations] The statement that >50% of confirmed and high-confidence candidates reside at >50 kpc separations is central to the paper's novelty, but the potential for line-of-sight projections in DeCam visual classifications is not quantitatively addressed, which could inflate the number of wide pairs.

    Authors: We acknowledge this concern. Our visual classifications require clear tidal features and morphological disturbances in DeCam imaging, which strongly favor physical interactions. In the revised manuscript, we will add a quantitative estimate of random alignment probability in the discussion, calculated from the galaxy surface density in the DeCam Legacy Survey and the observed separation range, demonstrating that the chance superposition rate is low (<5%) for systems with interaction signatures. revision: yes

Circularity Check

0 steps flagged

No circularity: purely observational catalog from external surveys with independent spectroscopic confirmation

full rationale

The paper reports a sample of dual AGN candidates selected via established W1-W2 color cuts from public WISE data and visual merger classification from public DeCam Legacy Survey imaging, followed by external spectroscopic follow-up on ~2/3 of the objects. No equations, derivations, fitted parameters, or self-referential definitions appear in the provided text. Selection criteria are applied directly to survey catalogs without reduction to prior results by the same authors. The 13 confirmed dual AGNs and 63 high-confidence candidates are outcomes of this pipeline, not inputs renamed as predictions. Self-citations, if present, are not load-bearing for any central claim. This is a standard observational catalog paper whose results are externally falsifiable via the cited surveys and spectra.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The central claim rests on standard domain assumptions for AGN identification via mid-IR colors and merger detection via optical imaging; no free parameters or invented entities are introduced.

axioms (2)
  • domain assumption Mid-IR W1-W2 colors reliably select AGNs with limited contamination from star-forming galaxies
    Invoked in candidate selection from WISE photometry; standard but known to have some overlap with other sources.
  • domain assumption DeCam Legacy Survey imaging can be used to classify galaxy mergers via morphology
    Used to select merger candidates; relies on visual or automated morphological criteria.

pith-pipeline@v0.9.0 · 5702 in / 1545 out tokens · 36479 ms · 2026-05-15T02:46:04.230410+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

114 extracted references · 114 canonical work pages · 5 internal anchors

  1. [1]

    N., Adelman-McCarthy, J

    Abazajian, K. N., Adelman-McCarthy, J. K., Ag¨ ueros, M. A., et al. 2009, ApJS, 182, 543, doi: 10.1088/0067-0049/182/2/543

    work page doi:10.1088/0067-0049/182/2/543 2009

  2. [2]

    M., et al

    Agazie, G., Anumarlapudi, A., Archibald, A. M., et al. 2023a, ApJL, 951, L8, doi: 10.3847/2041-8213/acdac6 —. 2023b, ApJL, 952, L37, doi: 10.3847/2041-8213/ace18b

    work page doi:10.3847/2041-8213/acdac6 2041

  3. [3]

    2020, ApJS, 249, 3, doi: 10.3847/1538-4365/ab929e

    Ahumada, R., Allende Prieto, C., Almeida, A., et al. 2020, ApJS, 249, 3, doi: 10.3847/1538-4365/ab929e

    work page doi:10.3847/1538-4365/ab929e 2020

  4. [4]

    L., Wu, X.-B., Yang, J., et al

    Ai, Y. L., Wu, X.-B., Yang, J., et al. 2016, AJ, 151, 24, doi: 10.3847/0004-6256/151/2/24

    work page doi:10.3847/0004-6256/151/2/24 2016

  5. [5]

    2011, ApJS, 193, 29, doi: 10.1088/0067-0049/193/2/29

    Aihara, H., Allende Prieto, C., An, D., et al. 2011, ApJS, 193, 29, doi: 10.1088/0067-0049/193/2/29

    work page doi:10.1088/0067-0049/193/2/29 2011

  6. [6]

    G., Groves, B

    Allen, M. G., Groves, B. A., Dopita, M. A., Sutherland, R. S., & Kewley, L. J. 2008, ApJS, 178, 20, doi: 10.1086/589652

    work page doi:10.1086/589652 2008

  7. [7]

    F., Argudo-Fern´ andez, M., et al

    Almeida, A., Anderson, S. F., Argudo-Fern´ andez, M., et al. 2023, ApJS, 267, 44, doi: 10.3847/1538-4365/acda98

    work page doi:10.3847/1538-4365/acda98 2023

  8. [8]

    2023, Living Reviews in Relativity, 26, 2, doi: 10.1007/s41114-022-00041-y

    Amaro-Seoane, P., Andrews, J., Arca Sedda, M., et al. 2023, Living Reviews in Relativity, 26, 2, doi: 10.1007/s41114-022-00041-y

    work page doi:10.1007/s41114-022-00041-y 2023

  9. [9]

    L., Gandhi, P., et al

    Asmus, D., Greenwell, C. L., Gandhi, P., et al. 2020, MNRAS, 494, 1784, doi: 10.1093/mnras/staa766

    work page doi:10.1093/mnras/staa766 2020

  10. [10]

    J., Stern, D., Noirot, G., et al

    Assef, R. J., Stern, D., Noirot, G., et al. 2018, ApJS, 234, 23, doi: 10.3847/1538-4365/aaa00a

    work page doi:10.3847/1538-4365/aaa00a 2018

  11. [11]

    1981 , month = feb, journal =

    Baldwin, J. A., Phillips, M. M., & Terlevich, R. 1981, PASP, 93, 5, doi: 10.1086/130766

    work page doi:10.1086/130766 1981

  12. [12]

    Barnes, J. E. 2016, MNRAS, 455, 1957, doi: 10.1093/mnras/stv2381

    work page doi:10.1093/mnras/stv2381 2016

  13. [13]

    E., & Hernquist, L

    Barnes, J. E., & Hernquist, L. 1996, ApJ, 471, 115, doi: 10.1086/177957

    work page doi:10.1086/177957 1996

  14. [14]

    S., Comerford, J

    Barrows, R. S., Comerford, J. M., Stern, D., & Assef, R. J. 2021, ApJ, 922, 179, doi: 10.3847/1538-4357/ac1352 —. 2023, ApJ, 951, 92, doi: 10.3847/1538-4357/acd2d3

    work page doi:10.3847/1538-4357/ac1352 2021

  15. [15]

    C., Blandford, R

    Begelman, M. C., Blandford, R. D., & Rees, M. J. 1980, Nature, 287, 307, doi: 10.1038/287307a0

    work page doi:10.1038/287307a0 1980

  16. [16]

    and Wilkinson, M

    Matt, G. 2008, MNRAS, 386, 105, doi: 10.1111/j.1365-2966.2008.13078.x

    work page doi:10.1111/j.1365-2966.2008.13078.x 2008

  17. [17]

    F., Satyapal, S., & Ellison, S

    Blecha, L., Snyder, G. F., Satyapal, S., & Ellison, S. L. 2018, MNRAS, 478, 3056, doi: 10.1093/mnras/sty1274

    work page doi:10.1093/mnras/sty1274 2018

  18. [18]

    A., & Barnes, J

    Blumenthal, K. A., & Barnes, J. E. 2018, MNRAS, 479, 3952, doi: 10.1093/mnras/sty1605

    work page doi:10.1093/mnras/sty1605 2018

  19. [19]

    2011, ApJ, 729, 85, doi: 10.1088/0004-637X/729/2/85

    Callegari, S., Kazantzidis, S., Mayer, L., et al. 2011, ApJ, 729, 85, doi: 10.1088/0004-637X/729/2/85

    work page doi:10.1088/0004-637x/729/2/85 2011

  20. [20]

    R., Dotti, M., Volonteri, M., et al

    Capelo, P. R., Dotti, M., Volonteri, M., et al. 2017, MNRAS, 469, 4437, doi: 10.1093/mnras/stx1067

    work page doi:10.1093/mnras/stx1067 2017

  21. [21]

    R., Volonteri, M., Dotti, M., et al

    Capelo, P. R., Volonteri, M., Dotti, M., et al. 2015, MNRAS, 447, 2123, doi: 10.1093/mnras/stu2500

    work page doi:10.1093/mnras/stu2500 2015

  22. [22]

    The Pan-STARRS1 Surveys

    Chambers, K. C., Magnier, E. A., Metcalfe, N., et al. 2016, arXiv e-prints, arXiv:1612.05560, doi: 10.48550/arXiv.1612.05560

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.1612.05560 2016

  23. [23]

    2024, The Open Journal of Astrophysics, 7, 28, doi: 10.33232/001c.116179

    Chen, N., Mukherjee, D., Di Matteo, T., et al. 2024, The Open Journal of Astrophysics, 7, 28, doi: 10.33232/001c.116179

    work page doi:10.33232/001c.116179 2024

  24. [24]

    2023, MNRAS, 522, 1895, doi: 10.1093/mnras/stad834

    Chen, N., Di Matteo, T., Ni, Y., et al. 2023, MNRAS, 522, 1895, doi: 10.1093/mnras/stad834

    work page doi:10.1093/mnras/stad834 2023

  25. [25]

    2022, ApJ, 925, 162, doi: 10.3847/1538-4357/ac401b Cid Fernandes, R., Stasi´ nska, G., Mateus, A., & Vale Asari, N

    Chen, Y.-C., Hwang, H.-C., Shen, Y., et al. 2022, ApJ, 925, 162, doi: 10.3847/1538-4357/ac401b Cid Fernandes, R., Stasi´ nska, G., Mateus, A., & Vale Asari, N. 2011, MNRAS, 413, 1687, doi: 10.1111/j.1365-2966.2011.18244.x Cid Fernandes, R., Stasi´ nska, G., Schlickmann, M. S., et al. 2010, MNRAS, 403, 1036, doi: 10.1111/j.1365-2966.2009.16185.x

    work page doi:10.3847/1538-4357/ac401b 2022

  26. [26]

    M., Pooley, D., Barrows, R

    Comerford, J. M., Pooley, D., Barrows, R. S., et al. 2015, ApJ, 806, 219, doi: 10.1088/0004-637X/806/2/219

    work page doi:10.1088/0004-637x/806/2/219 2015

  27. [27]

    R., Knigge, C., Drew, J

    Dekel, A. 2008, MNRAS, 384, 386, doi: 10.1111/j.1365-2966.2007.12730.x 36Pfeifle et al

    work page doi:10.1111/j.1365-2966.2007.12730.x 2008

  28. [28]

    2012, Research in Astronomy and Astrophysics, 12, 1197, doi: 10.1088/1674-4527/12/9/003

    Cui, X.-Q., Zhao, Y.-H., Chu, Y.-Q., et al. 2012, Research in Astronomy and Astrophysics, 12, 1197, doi: 10.1088/1674-4527/12/9/003

    work page doi:10.1088/1674-4527/12/9/003 2012

  29. [29]

    M., Wright, E

    Cutri, R. M., Wright, E. L., Conrow, T., et al. 2021 De Rosa, A., Vignali, C., Husemann, B., et al. 2018, MNRAS, 480, 1639, doi: 10.1093/mnras/sty1867 De Rosa, A., Vignali, C., Bogdanovi´ c, T., et al. 2019, NewAR, 86, 101525, doi: 10.1016/j.newar.2020.101525 De Rosa, A., Vignali, C., Severgnini, P., et al. 2023, MNRAS, 519, 5149, doi: 10.1093/mnras/stac3...

    work page doi:10.1093/mnras/sty1867 2021

  30. [30]

    J., Lang, D., et al

    Dey, A., Schlegel, D. J., Lang, D., et al. 2019, AJ, 157, 168, doi: 10.3847/1538-3881/ab089d Di Matteo, P., Combes, F., Melchior, A.-L., & Semelin, B. 2007, A&A, 468, 61, doi: 10.1051/0004-6361:20066959

    work page doi:10.3847/1538-3881/ab089d 2019

  31. [31]

    C., & Hernquist, L

    Dubinski, J., Mihos, J. C., & Hernquist, L. 1996, ApJ, 462, 576, doi: 10.1086/177174

    work page doi:10.1086/177174 1996

  32. [32]

    2017, MNRAS, 470, L49, doi: 10.1093/mnrasl/slx076

    Simard, L. 2017, MNRAS, 470, L49, doi: 10.1093/mnrasl/slx076

    work page doi:10.1093/mnrasl/slx076 2017

  33. [33]

    L., Viswanathan, A., Patton, D

    Ellison, S. L., Viswanathan, A., Patton, D. R., et al. 2019, MNRAS, 487, 2491, doi: 10.1093/mnras/stz1431

    work page doi:10.1093/mnras/stz1431 2019

  34. [34]

    M., Phillips, A

    Faber, S. M., Phillips, A. C., Kibrick, R. I., et al. 2003, in Society of Photo-Optical Instrumentation Engineers (SPIE) Conference Series, Vol. 4841, Instrument Design and Performance for Optical/Infrared Ground-based Telescopes, ed. M. Iye & A. F. M. Moorwood, 1657–1669, doi: 10.1117/12.460346

    work page doi:10.1117/12.460346 2003

  35. [35]

    2000, ApJL, 539, L9, doi: 10.1086/312838

    Ferrarese, L., & Merritt, D. 2000, ApJL, 539, L9, doi: 10.1086/312838

    work page doi:10.1086/312838 2000

  36. [36]

    2024, Universe, 10, 237, doi: 10.3390/universe10060237

    Foord, A., Cappelluti, N., Liu, T., et al. 2024, Universe, 10, 237, doi: 10.3390/universe10060237

    work page doi:10.3390/universe10060237 2024

  37. [37]

    D., Djorgovski, S

    Fu, H., Myers, A. D., Djorgovski, S. G., et al. 2015a, ApJ, 799, 72, doi: 10.1088/0004-637X/799/1/72

    work page doi:10.1088/0004-637x/799/1/72

  38. [38]

    2015b, ApJL, 815, L6, doi: 10.1088/2041-8205/815/1/L6

    Yan, L. 2015b, ApJL, 815, L6, doi: 10.1088/2041-8205/815/1/L6

    work page doi:10.1088/2041-8205/815/1/l6 2041

  39. [39]

    D., et al

    Fu, H., Yan, L., Myers, A. D., et al. 2012, ApJ, 745, 67, doi: 10.1088/0004-637X/745/1/67

    work page doi:10.1088/0004-637x/745/1/67 2012

  40. [40]

    J., et al

    Fu, H., Zhang, Z.-Y., Assef, R. J., et al. 2011, ApJL, 740, L44, doi: 10.1088/2041-8205/740/2/L44

    work page doi:10.1088/2041-8205/740/2/l44 2011

  41. [41]

    L., Gross, A

    Fu, H., Steffen, J. L., Gross, A. C., et al. 2018, ApJ, 856, 93, doi: 10.3847/1538-4357/aab364

    work page doi:10.3847/1538-4357/aab364 2018

  42. [42]

    2012, ApJS, 201, 31, doi: 10.1088/0067-0049/201/2/31

    Ge, J.-Q., Hu, C., Wang, J.-M., Bai, J.-M., & Zhang, S. 2012, ApJS, 201, 31, doi: 10.1088/0067-0049/201/2/31

    work page doi:10.1088/0067-0049/201/2/31 2012

  43. [43]

    2000, ApJL, 539, L13, doi: 10.1086/312840

    Gebhardt, K., Bender, R., Bower, G., et al. 2000, ApJL, 539, L13, doi: 10.1086/312840

    work page doi:10.1086/312840 2000

  44. [44]

    2021, MNRAS, 504, 393, doi: 10.1093/mnras/stab808 G¨ ultekin, K., Richstone, D

    Guainazzi, M., De Rosa, A., Bianchi, S., et al. 2021, MNRAS, 504, 393, doi: 10.1093/mnras/stab808 G¨ ultekin, K., Richstone, D. O., Gebhardt, K., et al. 2009, ApJ, 698, 198, doi: 10.1088/0004-637X/698/1/198

    work page doi:10.1093/mnras/stab808 2021

  45. [45]

    2023, ApJ, 949, 49, doi: 10.3847/1538-4357/acc5e1

    He, L., Hou, M., Li, Z., Feng, S., & Liu, X. 2023, ApJ, 949, 49, doi: 10.3847/1538-4357/acc5e1

    work page doi:10.3847/1538-4357/acc5e1 2023

  46. [46]

    F., Schmitz, M., et al

    Helou, G., Madore, B. F., Schmitz, M., et al. 1991, in Astrophysics and Space Science Library, Vol. 171, Databases and On-line Data in Astronomy, ed. M. A. Albrecht & D. Egret, 89–106, doi: 10.1007/978-94-011-3250-3 10

    work page doi:10.1007/978-94-011-3250-3 1991

  47. [47]

    2020, ApJ, 900, 79, doi: 10.3847/1538-4357/aba4a7

    Hou, M., Li, Z., & Liu, X. 2020, ApJ, 900, 79, doi: 10.3847/1538-4357/aba4a7

    work page doi:10.3847/1538-4357/aba4a7 2020

  48. [48]

    2023, ApJ, 943, 50, doi: 10.3847/1538-4357/acaaf9

    Hou, M., Li, Z., Liu, X., et al. 2023, ApJ, 943, 50, doi: 10.3847/1538-4357/acaaf9

    work page doi:10.3847/1538-4357/acaaf9 2023

  49. [49]

    2019, ApJ, 882, 41, doi: 10.3847/1538-4357/ab3225

    Hou, M., Liu, X., Guo, H., et al. 2019, ApJ, 882, 41, doi: 10.3847/1538-4357/ab3225

    work page doi:10.3847/1538-4357/ab3225 2019

  50. [50]

    2020, ApJ, 891, 140, doi: 10.3847/1538-4357/ab733e

    Saito, Y. 2020, ApJ, 891, 140, doi: 10.3847/1538-4357/ab733e

    work page doi:10.3847/1538-4357/ab733e 2020

  51. [51]

    2014, ApJ, 780, 106, doi: 10.1088/0004-637X/780/1/106

    Imanishi, M., & Saito, Y. 2014, ApJ, 780, 106, doi: 10.1088/0004-637X/780/1/106

    work page doi:10.1088/0004-637x/780/1/106 2014

  52. [52]

    2010, AJ, 140, 403, doi: 10.1088/0004-6256/140/2/403

    Inada, N., Oguri, M., Shin, M.-S., et al. 2010, AJ, 140, 403, doi: 10.1088/0004-6256/140/2/403

    work page doi:10.1088/0004-6256/140/2/403 2010

  53. [53]

    H., Cohen, M., Masci, F., et al

    Jarrett, T. H., Cohen, M., Masci, F., et al. 2011, ApJ, 735, 112, doi: 10.1088/0004-637X/735/2/112

    work page doi:10.1088/0004-637x/735/2/112 2011

  54. [54]

    2023, ApJS, 265, 25, doi: 10.3847/1538-4365/acaf89

    Jin, J.-J., Wu, X.-B., Fu, Y., et al. 2023, ApJS, 265, 25, doi: 10.3847/1538-4365/acaf89

    work page doi:10.3847/1538-4365/acaf89 2023

  55. [55]

    Merloni, S

    Kauffmann, G., Heckman, T. M., Tremonti, C., et al. 2003, MNRAS, 346, 1055, doi: 10.1111/j.1365-2966.2003.07154.x

    work page doi:10.1111/j.1365-2966.2003.07154.x 2003

  56. [56]

    J., Dopita, M

    Kewley, L. J., Dopita, M. A., Sutherland, R. S., Heisler, C. A., & Trevena, J. 2001, ApJ, 556, 121, doi: 10.1086/321545

    work page internal anchor Pith review doi:10.1086/321545 2001

  57. [57]

    Ram Pressure Stripping of Disc Galaxies: The Role of the Inclination Angle , shorttitle =

    Kewley, L. J., Groves, B., Kauffmann, G., & Heckman, T. 2006, MNRAS, 372, 961, doi: 10.1111/j.1365-2966.2006.10859.x

    work page doi:10.1111/j.1365-2966.2006.10859.x 2006

  58. [58]

    2003, ApJL, 582, L15, doi: 10.1086/346145

    Komossa, S., Burwitz, V., Hasinger, G., et al. 2003, ApJL, 582, L15, doi: 10.1086/346145

    work page doi:10.1086/346145 2003

  59. [59]

    Kormendy, J., & Ho, L. C. 2013, ARA&A, 51, 511, doi: 10.1146/annurev-astro-082708-101811

    work page internal anchor Pith review doi:10.1146/annurev-astro-082708-101811 2013

  60. [60]

    1995, ARA&A, 33, 581, doi: 10.1146/annurev.aa.33.090195.003053

    Kormendy, J., & Richstone, D. 1995, ARA&A, 33, 581, doi: 10.1146/annurev.aa.33.090195.003053

    work page doi:10.1146/annurev.aa.33.090195.003053 1995

  61. [61]

    2012, ApJL, 746, L22, doi: 10.1088/2041-8205/746/2/L22

    Koss, M., Mushotzky, R., Treister, E., et al. 2012, ApJL, 746, L22, doi: 10.1088/2041-8205/746/2/L22

    work page doi:10.1088/2041-8205/746/2/l22 2012

  62. [62]

    J., Blecha, L., Bernhard, P., et al

    Koss, M. J., Blecha, L., Bernhard, P., et al. 2018, Nature, 563, 214, doi: 10.1038/s41586-018-0652-7

    work page doi:10.1038/s41586-018-0652-7 2018

  63. [63]

    2023, Research Notes of the American Astronomical Society, 7, 214, doi: 10.3847/2515-5172/ad0044 Spatially-Resolved Mid-IR Dual AGNs in DeCaLs37

    Labrie, K., Simpson, C., Cardenes, R., et al. 2023, Research Notes of the American Astronomical Society, 7, 214, doi: 10.3847/2515-5172/ad0044 Spatially-Resolved Mid-IR Dual AGNs in DeCaLs37

    work page doi:10.3847/2515-5172/ad0044 2023

  64. [64]

    W., & Schlegel, D

    Lang, D., Hogg, D. W., & Schlegel, D. J. 2016, AJ, 151, 36, doi: 10.3847/0004-6256/151/2/36

    work page doi:10.3847/0004-6256/151/2/36 2016

  65. [65]

    2010, Monthly Notices of the Royal Astronomical Society, 408, 1181, doi: 10.1111/j.1365-2966.2010.17197.x

    Lintott, C., Schawinski, K., Bamford, S., et al. 2011, MNRAS, 410, 166, doi: 10.1111/j.1365-2966.2010.17432.x

    work page doi:10.1111/j.1365-2966.2010.17432.x 2011

  66. [66]

    and Wilkinson, M

    Lintott, C. J., Schawinski, K., Slosar, A., et al. 2008, MNRAS, 389, 1179, doi: 10.1111/j.1365-2966.2008.13689.x

    work page doi:10.1111/j.1365-2966.2008.13689.x 2008

  67. [67]

    2013, ApJ, 762, 110, doi: 10.1088/0004-637X/762/2/110

    Liu, X., Civano, F., Shen, Y., et al. 2013, ApJ, 762, 110, doi: 10.1088/0004-637X/762/2/110

    work page doi:10.1088/0004-637x/762/2/110 2013

  68. [68]

    E., Shen, Y., & Strauss, M

    Liu, X., Greene, J. E., Shen, Y., & Strauss, M. A. 2010a, ApJL, 715, L30, doi: 10.1088/2041-8205/715/1/L30

    work page doi:10.1088/2041-8205/715/1/l30 2041

  69. [69]

    Liu, X., Lazio, T. J. W., Shen, Y., & Strauss, M. A. 2018, ApJ, 854, 169, doi: 10.3847/1538-4357/aaab47

    work page doi:10.3847/1538-4357/aaab47 2018

  70. [70]

    Liu, X., Shen, Y., & Strauss, M. A. 2012, ApJ, 745, 94, doi: 10.1088/0004-637X/745/1/94

    work page doi:10.1088/0004-637x/745/1/94 2012

  71. [71]

    A., & Greene, J

    Liu, X., Shen, Y., Strauss, M. A., & Greene, J. E. 2010b, ApJ, 708, 427, doi: 10.1088/0004-637X/708/1/427

    work page doi:10.1088/0004-637x/708/1/427

  72. [72]

    A., & Hao, L

    Liu, X., Shen, Y., Strauss, M. A., & Hao, L. 2011, ApJ, 737, 101, doi: 10.1088/0004-637X/737/2/101

    work page doi:10.1088/0004-637x/737/2/101 2011

  73. [73]

    2019, ApJ, 887, 90, doi: 10.3847/1538-4357/ab54c3

    Liu, X., Hou, M., Li, Z., et al. 2019, ApJ, 887, 90, doi: 10.3847/1538-4357/ab54c3

    work page doi:10.3847/1538-4357/ab54c3 2019

  74. [74]

    2012 , month = apr, journal =

    Wisotzki, L. 2012, MNRAS, 424, 2876, doi: 10.1111/j.1365-2966.2012.21427.x

    work page doi:10.1111/j.1365-2966.2012.21427.x 2012

  75. [75]

    2012 , month = apr, journal =

    Mateos, S., Alonso-Herrero, A., Carrera, F. J., et al. 2012, MNRAS, 426, 3271, doi: 10.1111/j.1365-2966.2012.21843.x

    work page doi:10.1111/j.1365-2966.2012.21843.x 2012

  76. [76]

    C., Max, C

    McGurk, R. C., Max, C. E., Medling, A. M., Shields, G. A., & Comerford, J. M. 2015, ApJ, 811, 14, doi: 10.1088/0004-637X/811/1/14

    work page doi:10.1088/0004-637x/811/1/14 2015

  77. [77]

    C., Max, C

    McGurk, R. C., Max, C. E., Rosario, D. J., et al. 2011, ApJL, 738, L2, doi: 10.1088/2041-8205/738/1/L2

    work page doi:10.1088/2041-8205/738/1/l2 2011

  78. [78]

    C., Dubinski, J., & Hernquist, L

    Mihos, J. C., Dubinski, J., & Hernquist, L. 1998, ApJ, 494, 183, doi: 10.1086/305179 Milosavljevi´ c, M., & Merritt, D. 2001, ApJ, 563, 34, doi: 10.1086/323830 M¨ uller-S´ anchez, F., Comerford, J. M., Nevin, R., et al. 2015, ApJ, 813, 103, doi: 10.1088/0004-637X/813/2/103

    work page doi:10.1086/305179 1998

  79. [79]

    B., & Gunn, J

    Oke, J. B., & Gunn, J. E. 1982, PASP, 94, 586, doi: 10.1086/131027

    work page doi:10.1086/131027 1982

  80. [80]

    R., Faria, L., Hani, M

    Patton, D. R., Faria, L., Hani, M. H., et al. 2024, MNRAS, 529, 1493, doi: 10.1093/mnras/stae608

    work page doi:10.1093/mnras/stae608 2024

Showing first 80 references.