Abstract
Abstract We present the analysis of a sample of Hα, Hβ, and [O ii] emission line galaxies from the OTELO survey, with masses typically below log ( M * / M ⊙ ) ∼ 9.4 and redshifts between z ∼ 0.4 and 1.43. We study the star formation rate, star formation rate density, and their number density and evolution with redshift. We obtain a robust estimate of the specific star formation rate—stellar mass relation based on the lowest-mass sample published so far. We also determine a flat trend of the star formation rate density (SFRD) and number density with redshift. Our results suggest a scenario of no evolution of the number density of galaxies, regardless of their masses, up to redshift z ∼ 1.4. This implies a gradual change of the relative importance of the star-forming processes, from high-mass galaxies to low-mass galaxies, with decreasing redshift. We also find little or no variation of the SFRD in the redshift range of 0.4 < z < 1.43.
Highlights
The study of star formation along the cosmic times provides an outstanding insight into the main physical processes driving the evolution of galaxies at cosmological scales
There is a tight relationship between star formation rate (SFR) and stellar mass for star-forming galaxies—the main sequence (MS)—in both the local and high-redshift universe
Previous works have shown that the star formation rate density (SFRD) declines along cosmic time, the samples used are composed by high-mass galaxies
Summary
The study of star formation along the cosmic times provides an outstanding insight into the main physical processes driving the evolution of galaxies at cosmological scales. Previous works have shown that the star formation rate density (SFRD) declines along cosmic time (see, for example, Harish et al 2020; Sobral et al 2013), the samples used are composed by high-mass galaxies. Some studies, such as Mobasher et al (2009) who used a sample of galaxies with masses larger than 109.5 Me, concluded that the massive systems have had their major star formation activity at earlier epochs (z > 2) than the lower-mass galaxies.
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