Identification of High-Redshift Galaxy Overdensities in GOODS-N and GOODS-S

Abstract

We conduct a systematic search for high-redshift galaxy overdensities at $4.9<z_{\mathrm{spec}}<8.9$ in both the GOODS-N and GOODS-S fields using JWST/NIRCam imaging from JADES and JEMS in addition to JWST/NIRCam wide field slitless spectroscopy from FRESCO. High-redshift galaxy candidates are identified using HST+JWST photometry spanning $\lambda =0.4-5.0\mu \mathrm{m}$. We confirmed the redshifts for roughly a third of these galaxies using JWST/FRESCO spectroscopy over $\lambda =3.9-5.0\mu \mathrm{m}$ through identification of either $\mathrm{H}\alpha$ or $\left[\mathrm{OIII}\right]\lambda 5008$ around the best-fit photometric redshift. The rest-UV magnitudes and continuum slopes of these galaxies were inferred from the photometry: the brightest and reddest objects appear in more dense environments and thus are surrounded by more galaxy neighbors than their fainter and bluer counterparts, suggesting accelerated galaxy evolution within overdense environments. We find $17$ significant (${\delta }_{\mathrm{gal}}\ge 3.04$, $N_{\mathrm{galaxies}}\ge 4$) galaxy overdensities across both fields ($7$ in GOODS-N and $10$ in GOODS-S), including the two highest redshift spectroscopically confirmed galaxy overdensities to date at $⟨z_{\mathrm{spec}}⟩=7.954$ and $⟨z_{\mathrm{spec}}⟩=8.222$ (representing densities around $\sim 6$ and $\sim 12$ times that of a random volume). We estimate the total halo mass of these large-scale structures to be $11.5\le {\log }_{10}\left(M_{\mathrm{halo}}/M_{\odot }\right)\le 13.4$ using an empirical stellar mass to halo mass relation, which are likely underestimates as a result of incompleteness. These protocluster candidates are expected to evolve into massive galaxy clusters with ${\log }_{10}\left(M_{\mathrm{halo}}/M_{\odot }\right)\gtrsim 14$ by $z=0$.

Resubmitted to ApJ based on reviewer report; main text has 19 pages, 7 figures (including one figure set), and 2 tables. arXiv admin note: text overlap with arXiv:2302.10217

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