The Bursty Star Formation Histories of Low-mass Galaxies at 0.4 < z < 1 Revealed by Star Formation Rates Measured From Hβ and FUV - Archive ouverte HAL Access content directly
Journal Articles The Astrophysical Journal Year : 2016

The Bursty Star Formation Histories of Low-mass Galaxies at 0.4 < z < 1 Revealed by Star Formation Rates Measured From Hβ and FUV

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Yicheng Guo
  • Function : Author
Marc Rafelski
  • Function : Author
S. M. Faber
  • Function : Author
David C. Koo
  • Function : Author
Mark R. Krumholz
  • Function : Author
Jonathan R. Trump
  • Function : Author
S. P. Willner
  • Function : Author
Ricardo Amorín
  • Function : Author
Guillermo Barro
  • Function : Author
Eric F. Bell
  • Function : Author
Jonathan P. Gardner
  • Function : Author
Eric Gawiser
  • Function : Author
Anton M. Koekemoer
  • Function : Author
Camilla Pacifici
  • Function : Author
Pablo G. Pérez-González
  • Function : Author
Swara Ravindranath
  • Function : Author
Naveen Reddy
  • Function : Author
Harry I. Teplitz
  • Function : Author
Hassen Yesuf
  • Function : Author

Abstract

We investigate the burstiness of star formation histories (SFHs) of galaxies at 0.4 < z < 1 by using the ratio of star formation rates (SFRs) measured from Hβ and FUV (1500 Å) (Hβ-to-FUV ratio). Our sample contains 164 galaxies down to stellar mass (M *) of 108.5 M in the CANDELS GOODS-N region, where Team Keck Redshift Survey Keck/DEIMOS spectroscopy and Hubble Space Telescope/WFC3 F275W images from CANDELS and Hubble Deep UV Legacy Survey are available. When the ratio of Hβ- and FUV-derived SFRs is measured, dust extinction correction is negligible (except for very dusty galaxies) with the Calzetti attenuation curve. The Hβ-to-FUV ratio of our sample increases with M * and SFR. The median ratio is ∼0.7 at M * ∼ 108.5 M (or SFR ∼ 0.5 M yr-1) and increases to ∼1 at M * ∼ 1010 M (or SFR ∼ 10 M yr-1). At M * < 109.5 M , our median Hβ-to-FUV ratio is lower than that of local galaxies at the same M *, implying a redshift evolution. Bursty SFH on a timescale of a few tens of megayears on galactic scales provides a plausible explanation for our results, and the importance of the burstiness increases as M * decreases. Due to sample selection effects, our Hβ-to-FUV ratio may be an upper limit of the true value of a complete sample, which strengthens our conclusions. Other models, e.g., non-universal initial mass function or stochastic star formation on star cluster scales, are unable to plausibly explain our results.

Dates and versions

insu-03667692 , version 1 (13-05-2022)

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Yicheng Guo, Marc Rafelski, S. M. Faber, David C. Koo, Mark R. Krumholz, et al.. The Bursty Star Formation Histories of Low-mass Galaxies at 0.4 < z < 1 Revealed by Star Formation Rates Measured From Hβ and FUV. The Astrophysical Journal, 2016, 833, ⟨10.3847/1538-4357/833/1/37⟩. ⟨insu-03667692⟩
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