NGDEEP Epoch 1: The Faint-End of the Luminosity Function at $z \sim$ 9-12 from Ultra-Deep JWST Imaging

Author:

Gene C. K. Leung, Micaela B. Bagley, Steven L. Finkelstein, Henry C. Ferguson, Anton M. Koekemoer, Pablo G. Perez-Gonzalez, Alexa Morales, Dale D. Kocevski, Guang Yang, Rachel S. Somerville, Stephen M. Wilkins, L. Y. Aaron Yung, Seiji Fujimoto, Rebecca L. Larson, Casey Papovich, Nor Pirzkal, Danielle A. Berg, Jennifer M. Lotz, Marco Castellano, Oscar A. Chavez Ortiz, Yingjie Cheng, Mark Dickinson, Mauro Giavalisco, Nimish P. Hathi, Taylor A. Hutchison, Intae Jung, Jeyhan S. Kartaltepe, Priyamvada Natarajan, Barry Rothberg

Keyword:

Astrophysics, Astrophysics of Galaxies, Astrophysics of Galaxies (astro-ph.GA)

journal:

date:

2023-06-08 16:00:00

Abstract

We present a robust sample of very high-redshift galaxy candidates from the first epoch of {\it JWST}/NIRCam imaging from the Next Generation Extragalactic Exploratory Deep (NGDEEP) Survey. The NGDEEP NIRCam imaging in the Hubble Ultra Deep Field Parallel Field 2 (HUDF-Par2) reaches $m=30.4$ (5$\sigma$, point-source) in F277W, making it the deepest public {\it JWST} GO imaging dataset to date. We describe our detailed data reduction process of the six-filter broad-band {\it JWST}/NIRCam imaging, incorporating custom corrections for systematic effects to produce high-quality calibrated images. Using robust photometric redshift selection criteria, we identify a sample of 38 $z \gtrsim 9$ galaxy candidates. These objects span a redshift range of $z=8.5-15.8$, and apparent magnitudes of $m_\mathrm{F277W} = 27-30.5$ AB mag, reaching $\sim 1.5$ mag deeper than previous public {\it JWST} imaging surveys. We calculate the rest-frame ultraviolet (UV) luminosity function at $z \sim$ 9 and 11, and present a new measurement of the luminosity function faint-end slope at $z \sim 11$. There is no significant evolution in the faint-end slope and number density from $z=9$ to 11. Comparing our results with theoretical predictions, we find that some models produce better agreement at the faint end than the bright end. These results will help to constrain how stellar feedback impacts star formation at these early epochs.

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