EVOLUTION OF INTRINSIC SCATTER IN THE SFR-STELLAR MASS CORRELATION AT 0.5 < z < 3
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EVOLUTION OF INTRINSIC SCATTER IN THE SFR-STELLAR MASS CORRELATION AT 0.5 < z < 3

  • Author(s): Kurczynski, Peter
  • Gawiser, Eric
  • Acquaviva, Viviana
  • Bell, Eric F
  • Dekel, Avishai
  • de Mello, Duilia F
  • Ferguson, Henry C
  • Gardner, Jonathan P
  • Grogin, Norman A
  • Guo, Yicheng
  • Hopkins, Philip F
  • Koekemoer, Anton M
  • Koo, David C
  • Lee, Seong-Kook
  • Mobasher, Bahram
  • Primack, Joel R
  • Rafelski, Marc
  • Soto, Emmaris
  • Teplitz, Harry I
  • et al.
Abstract

We present estimates of intrinsic scatter in the Star Formation Rate (SFR) - Stellar Mass (M*) correlation in the redshift range 0.5 < z < 3.0 and in the mass range 10^7 < M* < 10^11 Msun. We utilize photometry in the Hubble Ultradeep Field (HUDF12), Ultraviolet Ultra Deep Field (UVUDF) campaigns and CANDELS/GOODS-S. We estimate SFR, M* from broadband Spectral Energy Distributions (SEDs) and the best available redshifts. The maximum depth of the HUDF photometry (F160W 29.9 AB, 5 sigma depth) probes the SFR-M* correlation down to M* ~ 10 ^7 Msun, a factor of 10-100X lower in M* than previous studies, and comparable to dwarf galaxies in the local universe. We find the slope of the SFR-M* relationship to be near unity at all redshifts and the normalization to decrease with cosmic time. We find a moderate increase in intrinsic scatter with cosmic time from 0.2 to 0.4 dex across the epoch of peak cosmic star formation. None of our redshift bins show a statistically significant increase in intrinsic scatter at low mass. However, it remains possible that intrinsic scatter increases at low mass on timescales shorter than ~ 100 Myr. Our results are consistent with a picture of gradual and self-similar assembly of galaxies across more than three orders of magnitude in stellar mass from as low as 10^7 Msun.

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