{"arxiv_id":"astro-ph/0602088","incoming":{"papers":4,"sentences":6,"groups":[{"kind":"background","label":"Cites it as background","papers":1,"sentences":1,"quotes":[{"arxiv_id":"1112.3764","title":"Galaxy pairs as a probe for mergers at z ~ 2","url":"/paper/1112.3764","section":"Introduction","sentence":"Typically merger candidates are identified from photometric catalogues through either pair selection [ref] or morphology [ref] .","intent_p":0.82,"contests_p":null}]}],"unlabelled_sentences":5},"outgoing":{"papers":0,"sentences":0,"groups":[],"unlabelled_sentences":0},"claims":[{"relation":"contradicts","label":"States a conflicting result","papers":[{"arxiv_id":"1001.2772","url":"/paper/1001.2772","title":"The CFHTLS Deep Catalog of Interacting Galaxies I. Merger Rate Evolution to z=1.2","main_claim":"We conclude that (1) the optical galaxy merger fraction does evolve with redshift, (2) the merger fraction depends mildly on stellar mass, with lower mass galaxies having higher merger fractions at z<1, and (3) star formation is triggered at all phases of a merger, with larger enhancements at later stages, consistent with N-body simulations.","p":0.96}]}],"thresholds":{"intent_p":0.8,"supports_p":0.95,"contests_p":0.7},"method":"Citing sentences come from each paper's LaTeX source; every \\cite marks the sentence and the works it cites. Pith's classifier typed each sentence. A label is shown at intent probability 0.8 or more (0.95 for support), a contest at 0.7 or more. Measured accuracy against two blind model families is at https://pith.science/accuracy. The quoted sentences are the citing authors' own.","held_up":{"arxiv_id":"astro-ph/0602088","kind":"model","paper_version":2,"prompt_version":"held-up-v3.5","generated_at":"2026-10-27T17:09:41+00:00","loaded_at":"2026-10-28T01:02:56.144793+00:00","evidence":"substantial","account":[],"groups":[{"kind":"method_or_tool","label":"Uses its method or tool","papers":8,"entries":[{"p":0.95,"quote":null,"citing":[{"self":false,"year":2021,"title":"On the Nature of AGN and Star Formation Enhancement in the $z = 3.1$ SSA22 Protocluster: The HST WFC3 IR View","arxiv_id":"2106.13846"}],"verified":true,"paraphrase":"Adopted this paper's G-M20 classifications, which place galaxies with G > -0.14 M20 + 0.33 as merger-like and those below that line with G > 0.14 M20 + 0.80 as bulge-dominated."},{"p":0.81,"quote":{"text":"Here, we include dividing lines between the regions of mergers, Sb/Sc/Irr and E/S0/Sa galaxy types taken from [ref] , according to the following definitions, Mergers: G $>$ $-$0.14$×$M20 + 0.33; Early(E/S0/Sa): G $≤$ $-$0.14$×$M20 + 0.33, and G $>$ 0.14$×$M20 + 0.80; Late(Sb/Ir): G $≤$ $-$0.14$×$M20 + 0.33, and G $≤$ 0.14$×$M20 + 0.80.","citing":"2312.15957","section":"Non-parametric morphology"},"citing":[{"self":false,"year":2023,"title":"Host galaxy and nuclear properties of IR-selected AGNs with and without outflow signatures","arxiv_id":"2312.15957"}],"verified":true,"paraphrase":"Included dividing lines between mergers, Sb/Sc/Irr and E/S0/Sa galaxy types taken from this paper."},{"p":0.98,"quote":{"text":"The bulge statistic $F(G, M_20)$: defined as [ref] [equation] which means the line intersects at $(G_0, M_20,0)=(0.533, -1.75)$ and is also perpendicular to the line separating merging and non-merging galaxies. here selects $G>0.14M_20+0.80$ as the function of $F(G, M_20)$ and $G>-0.14M_20+0.33$ [ref] as the function of $S(G, M_20)$, and if $F(G, M_20)>0$ means the galaxy is ETG, otherwise, the galaxy is LTG and also is closely related to Concentration index (C) and Sérsic index.","citing":"2504.18194","section":"Non-parametric Measurements"},"citing":[{"self":false,"year":2025,"title":"A Morphological Study on AGN-host Dwarf Galaxies","arxiv_id":"2504.18194"}],"verified":true,"paraphrase":"Selected G > -0.14 M20 + 0.33 as a function of S(G, M20) following this paper."},{"p":0.88,"quote":{"text":"The lines denote the boundary between mergers, disk galaxies, and ellipticals/S0s following [ref] .","citing":"2312.14263","section":"Morphology measures of mock observations"},"citing":[{"self":false,"year":2023,"title":"z~2 dual AGN host galaxies are disky: stellar kinematics in the ASTRID Simulation","arxiv_id":"2312.14263"}],"verified":true,"paraphrase":"Drew lines marking the boundary between mergers, disk galaxies, and ellipticals/S0s following this paper."},{"p":0.94,"quote":{"text":"The division lines are obtained from [ref] with the following definitions for Extended Groth Strip (EGS) galaxies at $0.2<z<1.2$: $Mergers: G > -0.14 M_20+0.33$, $E/S0/Sa: G≤-0.14 M_20+0.33 & G > 0.14M_20+0.80$, and $Sb/Sc/Irr: G ≤-0.14M_20+0.33 & G ≤0.14M_20+0.80$.","citing":"2111.15289","section":"Non-parametric Parameter Diagnostics"},"citing":[{"self":false,"year":2021,"title":"A Morphological Study on Galaxies Hosting Optical Variability-Selected AGNs in the COSMOS Field","arxiv_id":"2111.15289"}],"verified":true,"paraphrase":"Obtained its division lines between E/S0/Sa, Sb/Sc/Irr and mergers from this paper's definitions for Extended Groth Strip galaxies at 0.2<z<1.2."},{"p":0.99,"quote":{"text":"The Gini-M20 statistics [ref] classify z19863 as a merger based on the stellar emission (F182M) but a non-merger based on the gas emission (F210M-F182M).","citing":"2403.13285","section":"Merger activity"},"citing":[{"self":false,"year":2024,"title":"MOSEL survey: Spatially offset Lyman-continuum emission in a new emitter at z=3.088","arxiv_id":"2403.13285"}],"verified":true,"paraphrase":"Used the Gini-M20 statistics of this paper, which classify z19863 as a merger based on stellar emission but a non-merger based on gas emission."},{"p":1.0,"quote":{"text":"We refer to [ref] for demarcating the galaxy population into spirals/ irregular, elliptical/ lenticular, and merger candidates on $G$ vs. $M20$ plane.","citing":"2401.13073","section":"Morphological classification using non-parametric methods"},"citing":[{"self":false,"year":2024,"title":"Exploring filament galaxies using {\\em AstroSat}/ UVIT","arxiv_id":"2401.13073"}],"verified":true,"paraphrase":"Referred to this paper for demarcating the galaxy population into spirals/irregular, elliptical/lenticular, and merger candidates on the G vs. M20 plane."}],"papers_all":23,"self_papers":1,"self_entries":[{"p":1.0,"quote":null,"citing":[{"self":true,"year":2024,"title":"A Complete 16 $\\mu$m selected Galaxy Sample at $z \\sim 1$. II: Morphological Analysis","arxiv_id":"2405.06984"}],"verified":true,"paraphrase":"Visually identified galaxy pairs and galaxies with distorted morphologies using the criteria in this paper."}]},{"kind":"comparison","label":"Compares with it","papers":2,"entries":[{"p":0.96,"quote":null,"citing":[{"self":false,"year":2021,"title":"The Connection between Mergers and AGN Activity in Simulated and Observed Massive Galaxies","arxiv_id":"2101.01729"}],"verified":true,"paraphrase":"Found its synthetic morphologies tend to lie along this paper's dividing line between mergers and non-mergers and exhibit a shallower slope than the corresponding locus of CANDELS galaxies."},{"p":1.0,"quote":null,"citing":[{"self":false,"year":2021,"title":"Morphological Evolution of the Hosts of Far-Infrared/Submillimeter Galaxies","arxiv_id":"2109.02875"}],"verified":true,"paraphrase":"Found its Gini-M20 results consistent with its visual classification, with nearly all its E galaxies in the region of this paper's E/S0/Sa galaxies and most of its D galaxies where their disk galaxies would populate."}],"papers_all":9,"self_papers":0,"self_entries":[]}],"counts":{"by_kind":{"data_used":1,"comparison":9,"method_or_tool":23,"supports_this_paper":1},"dropped":{"relied_on":0,"unknown_ids":0,"account_lines":0,"contest_vetoed":0,"below_threshold":0,"contest_drawback":0,"contest_without_basis":0,"contest_not_one_sentence":0,"contest_on_group_citation":0},"papers_read":20,"self_papers":27,"citing_papers":99,"sentences_read":29,"citing_sentences":177,"unambiguous_read":29,"typed_independent":22,"independent_papers":72,"by_kind_independent":{"data_used":1,"comparison":5,"method_or_tool":17}},"input_sha256":"5007f49e640c91f865622e22022fad5bbdc5fa0478f400698725910e878b94dd","method":"For a paper with five or more citing arXiv papers, Pith selected up to 40 citing sentences its citation classifier typed, read those whose citation markers point at this paper alone, and wrote one paraphrase for each later paper in each group, each resting on one sentence. A later paper is listed under a label only when the classifier gives one of its sentences that label at intent probability 0.8 or more (0.95 for support), Pith's reading of the sentence finds that the citing paper itself did it, and a second check of the paraphrase against the sentence passes. The section lists uses only: building on the paper, using its method, tool, data or values, comparing with it and citing it as support. It does not list criticism or disagreement, so their absence says nothing about how the paper has been received. Code counted the papers, wrote the summary from the listed entries, set the evidence level and linked each entry to its citing paper. Quotes are copied from the citing sentence and shown only when the citing paper's licence is CC BY, CC BY-SA or CC0; otherwise the paraphrase is shown. Papers that share an author with this one are listed apart. A paper with fewer citing papers gets a line counted by code, which names uses only: a later paper whose only label is a contest is counted as not described.","line":null,"summary":"9 later papers by other authors are listed below: 7 used its method or tool and 2 compared their own results with it. 1 more paper by the same authors is listed: 1 used its method or tool."},"_links":{"html":"https://pith.science/paper/astro-ph/0602088"}}