ODIN: Probing the LAE Ly α Luminosity Function across Cosmic Time and Different Environments

作者：Gautam Nagaraj, Robin Ciardullo, C. Gronwall, Vandana Ramakrishnan, Kyoung-Soo Lee, Eric Gawiser, Nicole Firestone, Govind Ramgopal, J. Aguilar, S. P. Ahlen, D. Bianchi, D. Brooks, F. J. Castander, T. Claybaugh, Andrei Cuceu, Axel de la Macorra, Arjun Dey, Biprateep Dey, P. Doel, J. E. Forero-Romero, E. Gaztañaga, Satya Gontcho A Gontcho, G. Gutiérrez, H. K. Herrera-Alcantar, K. Honscheid, Mustapha Ishak, R. Kehoe, D. Kirkby, Theodore Kisner, Anthony Kremin, Martin Landriau, L. Le Guillou, M. E. Levi, C. Magneville, Marc Manera, P. Martini, Aaron Meisner, R. Miquel, John Moustakas, N. Palanque‐Delabrouille, Francisco Prada, Ignasi Pérez-Ràfols, Graziano Rossi, Lado Samushia, E. Sánchez, David J. Schlegel, M. Schubnell, Hee‐Jong Seo, J. Silber, David Sprayberry, G. Tarlé, F. Valdés, B. A. Weaver, Martin White, Rongpu Zhou, Hu Zou · 发表于：The Astrophysical Journal · 年份：2025 · DOI：10.3847/1538-4357/ae1969 · 被引用次数：2 · 研究领域：Galaxies: Formation, Evolution, Phenomena、Astronomy and Astrophysical Research、Gamma-ray bursts and supernovae

Abstract The ubiquity and relative ease of discovery make 2 ≲ z ≲ 5 Ly α emitting galaxies (LAEs) ideal tracers for large-scale structure of the distant Universe. In addition, because Ly α is a resonance line, but frequently observed at large equivalent width, it is potentially a probe of galaxy evolution. The LAE Ly α luminosity function (LF) is an essential measurement for making progress on both of these topics. Although several studies have computed the LAE LF, very few have delved into how the function varies with environment. The large area and depth of the One-hundred-deg 2 DECam Imaging in Narrowbands (ODIN) survey makes such measurements possible at the cosmic noon redshifts of z ∼ 2.4, 3.1, and 4.5. In this initial work, we present algorithms needed to rigorously compute the LAE LF, and test them on the ∼16,000 ODIN LAEs found in the extended COSMOS field. Using these limited samples, we find weak evidence that protocluster environments suppress the numbers of faint LAEs compared to the field. We also find that the LF decreases in number density and evolves towards a steeper faint-end slope over cosmic time from z ∼ 4.5 to z ∼ 2.4.