PAPER / ARXIV:2609.08962
P. Mas-Buitrago (1), S. Kruk (2), D. O'Ryan (2), M. T. Nardone (2), A. La Marca (3 and 4), P. Awad (4), M. Baes (5), M. Fossati (6 and 7), T. Géron (8), Z. Ghaffari (9 and 10), M. Girardi (11 and 9), C. J. Lintott (12), J. G. Sorce (13 and 14), B. Altieri (2), F. Durret (15), V. Pettorino (3), B. Y. Irureta-Goyena (16), B. Simmons (17), J. Reerink (2), H. Domínguez Sánchez (18), J. H. Knapen (19 and 20), F. Shankar (21), E. Duran-Camacho (19 and 20), J. M. Pérez-Martínez (19 and 20), M. Walmsley (22 and 23), N. Auricchio (24), C. Baccigalupi (10 and 9 and 25 and 26), M. Baldi (27 and 24 and 28), S. Bardelli (24), P. Battaglia (24), A. Biviano (9 and 10), M. Bolzonella (24), A. Bonchi (29), E. Branchini (30 and 31 and 7), M. Brescia (32 and 33), J. Brinchmann (34 and 35 and 36), S. Camera (37 and 38 and 39), G. Cañas-Herrera (4), V. Capobianco (39), C. Carbone (40), J. Carretero (41 and 42), M. Castellano (43), G. Castignani (24), S. Cavuoti (33 and 44), A. Cimatti (45), C. Colodro-Conde (19), G. Congedo (46), C. J. Conselice (23), L. Conversi (47 and 2), Y. Copin (48), A. Costille (49), F. Courbin (50 and 51 and 52), H. M. Courtois (53), M. Cropper (54), H. Degaudenzi (55), G. De Lucia (9), H. Dole (14), F. Dubath (55), X. Dupac (2), S. Dusini (56), A. Ealet (48), M. Fabricius (57 and 58), M. Farina (59), R. Farinelli (24), S. Ferriol (48), P. Fosalba (60 and 61), S. Fotopoulou (62), M. Frailis (9), E. Franceschi (24), M. Fumana (40), S. Galeotta (9), K. George (63), B. Gillis (46), C. Giocoli (24 and 28), P. Gómez-Alvarez (64 and 2), J. Gracia-Carpio (57), A. Grazian (65), F. Grupp (57 and 58), S. Gwyn (66), W. Holmes (67), I. M. Hook (17), F. Hormuth (68), A. Hornstrup (69 and 70), M. Huertas-Company (19 and 71 and 72), K. Jahnke (73), M. Jhabvala (74), B. Joachimi (75), S. Kermiche (76), A. Kiessling (67), B. Kubik (48), M. Kümmel (58), M. Kunz (77), H. Kurki-Suonio (78 and 79), A. M. C. Le Brun (80), S. Ligori (39), P. B. Lilje (81), V. Lindholm (78 and 79), I. Lloro (82), G. Mainetti (83), O. Mansutti
RESUMO
Galaxy clusters provide unique laboratories for studying environmental effects on galaxy evolution. The morphology--density ($T$--$\Sigma$) and morphology--cluster-centric radius ($T$--$R$) relations trace how galaxy morphology is influenced by the environment, but previous studies at intermediate redshifts have been limited in both sample size and radial coverage. We use the Euclid Quick Data Release 1 (Q1) visual morphology catalogue to measure the $T$--$\Sigma$ and $T$--$R$ relations for smooth, featured-or-disc, and barred galaxies in known clusters at $0.2\leq z\leq 0.5$, extending this analysis to large cluster-centric distances ($3 R_{500c}$) and studying their dependence on stellar mass. Using photometric redshifts and stellar masses provided by Euclid, we identify 1754 cluster members within $1.5 R_{500c}$, distributed across 71 clusters. We classify the identified galaxies as smooth, featured-or-disc, or barred using the predicted vote fractions provided by the Zoobot deep learning foundation model in the Q1 visual morphology catalogue. We confirm the $T$--$\Sigma$ relation in all the stellar mass ranges studied, with a stronger influence of the cluster environment on galaxy morphology in the densest parts of the cluster and closer to the cluster centre. Beyond $1.5 R_{500c}$, the morphological segregation weakens, with featured-or-disc galaxies overtaking smooth galaxies at the lowest densities, consistent with the growing contribution of field interlopers in the cluster outskirts. For barred galaxies, we find a tentative decline of the bar fraction toward lower densities that is most pronounced for the most massive galaxies. In conclusion, our results show that the cluster environment drives a progressive transformation of galaxy morphology, with the loss of disc structure becoming more pronounced towards the cluster core, where environmental processes act most efficiently.
NO MESMO MAPA