Abstract:
Observations have found that for star-forming galaxies (SFGs) there is a relative#2;ly tight relation between star formation rate (ψSFR) and stellar mass (M∗) (i.e. lg ψSFR-lg M∗,
known as main sequence), with a typical scatter of 0.2 ∼ 0.4 dex. The main sequence plays
an important role in constraining theoretical models of galaxy evolution and is one of the
basic relations describing the evolution of galaxies. Recent years we have witnessed great
progress in both observational and theoretical work on the main sequence and its evolution.
Firstly, the key steps involved in the process of obtaining the main sequence are introduced,
focusing on the method of measuring ψSFR of galaxy and the method of selecting the SFGs
from the complete sample of galaxies. Using different methods causes systematic deviations
between the obtained main sequence. Then the main issues and progress on the studies of
the main sequence are presented. The main sequence shows a bending at massive end with
respect to the slope obtained in the low-mass end. There are mainly two explanations for
bending, including the formation of a bulge component in SFGs and the lessening of cold#2;accretion. The relation between the scatter of main sequence and the stellar mass (σSFR-M∗)
shows the characteristic of U-shape. This may indicate that supernovae feedback increases
the scatter at low-mass end and active galactic nuclei feedback is important for increasing
the scatter at massive end. In addition, in the mid- and high-redshift, the normalization
of the main sequence obtained by theory is always lower than the observational result by
0.2 ∼ 0.5 dex. So far, this problem has not been effectively solved. The high-redshift SFGs
data from JWST can help us understand main sequence more comprehensively
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