The Astrophysical Journal (Jan 2025)

CEERS: Increasing Scatter along the Star-forming Main Sequence Indicates Early Galaxies Form in Bursts

  • Justin W. Cole,
  • Casey Papovich,
  • Steven L. Finkelstein,
  • Micaela B. Bagley,
  • Mark Dickinson,
  • Kartheik G. Iyer,
  • L. Y. Aaron Yung,
  • Laure Ciesla,
  • Ricardo O. Amorín,
  • Pablo Arrabal Haro,
  • Rachana Bhatawdekar,
  • Antonello Calabrò,
  • Nikko J. Cleri,
  • Alexander de la Vega,
  • Avishai Dekel,
  • Ryan Endsley,
  • Eric Gawiser,
  • Mauro Giavalisco,
  • Nimish P. Hathi,
  • Michaela Hirschmann,
  • Benne W. Holwerda,
  • Jeyhan S. Kartaltepe,
  • Anton M. Koekemoer,
  • Ray A. Lucas,
  • Sara Mascia,
  • Bahram Mobasher,
  • Pablo G. Pérez-González,
  • Giulia Rodighiero,
  • Kaila Ronayne,
  • Sandro Tacchella,
  • Benjamin J. Weiner,
  • Stephen M. Wilkins

DOI
https://doi.org/10.3847/1538-4357/ad9a6a
Journal volume & issue
Vol. 979, no. 2
p. 193

Abstract

Read online

We present the star formation rate–stellar mass (SFR– M _* ) relation for galaxies in the Cosmic Evolution Early Release Science survey at 4.5 ≤ z ≤ 12. We model the JWST and Hubble Space Telescope rest-UV and rest-optical photometry of galaxies with flexible star formation histories (SFHs) using BAGPIPES. We consider SFRs averaged from the SFHs over 10 Myr (SFR _10 ) and 100 Myr (SFR _100 ), where the photometry probes SFRs on these timescales, effectively tracing nebular emission lines in the rest-optical (on ~10 Myr timescales) and the UV/optical continuum (on ~100 Myr timescales). We measure the slope, normalization and intrinsic scatter of the SFR– M _* relation, taking into account the uncertainty and the covariance of galaxy SFRs and M _* . From z ~ 5 to 9 there is larger scatter in the SFR _10 – M _* relation, with $\sigma (\mathrm{log}{\rm{S}}{\rm{F}}{{\rm{R}}}_{100})=0.4$ dex, compared to the SFR _100 – M _* relation, with $\sigma (\mathrm{log}SF{R}_{10})=0.1$ dex. This scatter increases with redshift and increasing stellar mass, at least out to z ~ 7. These results can be explained if galaxies at higher redshift experience an increase in star formation variability and form primarily in short, active periods, followed by a lull in star formation (i.e., “napping” phases). We see a significant trend in the ratio R _SFR = SFR _10 /SFR _100 in which, on average, R _SFR decreases with increasing stellar mass and increasing redshift. This yields a star formation “duty cycle” of ~40% for galaxies with $\mathrm{log}{M}_{* }/{M}_{\odot }\geqslant 9.3$ at z ~ 5, declining to ~20% at z ~ 9. Galaxies also experience longer lulls in star formation at higher redshift and at higher stellar mass, such that galaxies transition from periods of higher SFR variability at z ≳ 6 to smoother SFR evolution at z ≲ 4.5.

Keywords