TY - JOUR
T1 - ODIN
T2 - Identifying Protoclusters and Cosmic Filaments Traced by Lyα-emitting Galaxies
AU - Ramakrishnan, Vandana
AU - Lee, Kyoung Soo
AU - Artale, Maria Celeste
AU - Gawiser, Eric
AU - Yang, Yujin
AU - Park, Changbom
AU - Chiang, Yi Kuan
AU - Ciardullo, Robin
AU - Dey, Arjun
AU - Gronwall, Caryl
AU - Guaita, Lucia
AU - Hwang, Ho Seong
AU - Im, Sang Hyeok
AU - Jeong, Woong Seob
AU - Kim, Seongjae
AU - Kumar, Ankit
AU - Lee, Jaehyun
AU - Lee, Seong Kook
AU - Moon, Byeongha
AU - Padilla, Nelson
AU - Pope, Alexandra
AU - Popescu, Roxana
AU - Singh, Akriti
AU - Song, Hyunmi
AU - Troncoso, Paulina
AU - Valdes, Francisco
AU - Zabludoff, Ann
N1 - Publisher Copyright:
© 2024. The Author(s). Published by the American Astronomical Society.
PY - 2024/12/1
Y1 - 2024/12/1
N2 - To understand the formation and evolution of massive cosmic structures, studying them at high redshift, in the epoch when they formed the majority of their mass, is essential. The One-hundred-deg2 DECam Imaging in Narrowbands (ODIN) survey is undertaking the widest-area narrowband program to date, to use Lyα-emitting galaxies (LAEs) to trace the large-scale structure (LSS) of the Universe on the scale of 10-100 cMpc at three cosmic epochs. In this work, we present results at z = 3.1 based on early ODIN data in the COSMOS field. We identify protoclusters and cosmic filaments using multiple methods and discuss their strengths and weaknesses. We then compare our observations against the IllustrisTNG suite of cosmological hydrodynamical simulations. The two are in excellent agreement, identifying a similar number and angular size of structures above a specified density threshold. We successfully recover the simulated protoclusters with log(M z=0/M ⊙) ≳ 14.4 in ∼60% of the cases. With these objects, we show that the descendant masses of our observed protoclusters can be estimated purely based on our 2D measurements, finding a median z = 0 mass of ∼1014.5 M ⊙. The lack of information on the radial extent of each protocluster introduces a ∼0.4 dex uncertainty in its descendant mass. Finally, we show that the recovery of the cosmic web in the vicinity of protoclusters is both efficient and accurate. The similarity of our observations and the simulations implies that our structure selection is likewise robust and efficient, demonstrating that LAEs are reliable tracers of the LSS.
AB - To understand the formation and evolution of massive cosmic structures, studying them at high redshift, in the epoch when they formed the majority of their mass, is essential. The One-hundred-deg2 DECam Imaging in Narrowbands (ODIN) survey is undertaking the widest-area narrowband program to date, to use Lyα-emitting galaxies (LAEs) to trace the large-scale structure (LSS) of the Universe on the scale of 10-100 cMpc at three cosmic epochs. In this work, we present results at z = 3.1 based on early ODIN data in the COSMOS field. We identify protoclusters and cosmic filaments using multiple methods and discuss their strengths and weaknesses. We then compare our observations against the IllustrisTNG suite of cosmological hydrodynamical simulations. The two are in excellent agreement, identifying a similar number and angular size of structures above a specified density threshold. We successfully recover the simulated protoclusters with log(M z=0/M ⊙) ≳ 14.4 in ∼60% of the cases. With these objects, we show that the descendant masses of our observed protoclusters can be estimated purely based on our 2D measurements, finding a median z = 0 mass of ∼1014.5 M ⊙. The lack of information on the radial extent of each protocluster introduces a ∼0.4 dex uncertainty in its descendant mass. Finally, we show that the recovery of the cosmic web in the vicinity of protoclusters is both efficient and accurate. The similarity of our observations and the simulations implies that our structure selection is likewise robust and efficient, demonstrating that LAEs are reliable tracers of the LSS.
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U2 - 10.3847/1538-4357/ad83cb
DO - 10.3847/1538-4357/ad83cb
M3 - Article
AN - SCOPUS:85211380599
SN - 0004-637X
VL - 977
JO - Astrophysical Journal
JF - Astrophysical Journal
IS - 1
M1 - 119
ER -