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Autores principales: Ortiz, Ashley, Ramakrishnan, Vandana, Lee, Kyoung-Soo, Dey, Arjun, Guo, Yucheng, Pinarski, Ethan, Raichoor, Anand, Valdes, Francisco, Aguilar, J., Ahlen, Steven, Artale, Maria Celeste, Bianchi, Davide, Bliese, August, Brooks, David, Canning, Rebecca, Cerdosino, Maria, Claybaugh, Todd, Cuceu, Andrei, de la Macorra, Axel, Doel, Peter, Forero, Jaime, Gawiser, Eric, Gaztanaga, Enrique, Gontcho, Satya, Gronwall, Caryl, Guaita, Lucia, Gutierrez, Gaston, Herrera-Alcantar, Hiram K., Hwang, Ho Seong, Jeong, Woong-Seob, Joyce, Dick, Kehoe, Robert, Kisner, Theodore, Kremin, Anthony, Kumar, Ankit, Lahav, Ofer, Landriau, Martin, Lee, Jaehyun, Lee, Seong-Kook, Guillou, Laurent Le, Manera, Marc, Meisner, Aaron, Miquel, Ramon, Moon, Byeongha, Moustakas, John, Myers, Adam, Nadathur, Seshadri, Palanque-Delabrouille, Nathalie, Park, Changbom, Percival, Will, Perez-Rafols, Ignasi, Prada, Francisco, Puvvada, Eshwar, Rossi, Graziano, Sanchez, Eusebio, Schlegel, David, Schubnell, Michael, Silber, Joseph Harry, Song, Hyunmi, Sprayberry, David, Tarle, Gregory, Troncoso, Paulina, Uzsoy, Ana Sofia, Weaver, Benjamin, Yang, Yujin, Zhou, Rongpu, Zou, Hu
Formato: Preprint
Publicado: 2026
Materias:
Astrophysics of Galaxies
Acceso en línea:https://arxiv.org/abs/2603.09739
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  • Protoclusters represent sites of accelerated galaxy formation and extreme astrophysical activity characteristic of dense environments. Identifying massive protoclusters and mapping their spatial structures are therefore crucial first steps in understanding how the large-scale environment influences galaxy evolution. We combine wide-field Ly$α$ imaging from the ODIN survey with extensive DESI and ancillary spectroscopy across the extended COSMOS and XMM-LSS fields ($\approx$14 deg$^2$) to search for massive protoclusters. We confirm six systems at $z\approx 2.4$ and $z\approx 3.1$, reconstruct their three-dimensional structures, estimate descendant halo masses, and, for one structure at $z\approx 3.12$, demonstrate that overlapping narrowband filters ($NB497$ and $N501$) provide accurate redshift tomography for emission-line galaxies. One protocluster at $z\approx 2.45$ overlaps with one of the LATIS tomographic fields, enabling direct comparison between galaxy and H {\sc i} overdensities traced by Ly$α$ forest absorption. Another at $z\approx 3.12$ hosts a massive quiescent galaxy ($M_{\ast} \approx 1.2 \times 10^{11}M_\odot$), indicating early quenching in a dense environment. By comparing Ly$α$ emission properties across environments, we find that protocluster galaxies exhibit higher median line fluxes and a deficit of faint emitters relative to the field. The effect is strongest when both 2D and 3D density information are combined, indicating that galaxies in the densest protocluster cores are most affected by environmental processes. This effect is stronger at $z\approx3.1$ than at $z\approx2.4$, suggesting possible redshift evolution.

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