Our SBs and MSs are located in a dense environment. To better understand the environmental effect on gas turbulence, we compare the four cluster members with field galaxies from the literature. The data included in Figs. 5 and 6 contain molecular and ionized gas observations. The ionized gas observations of the star-forming galaxies, sorted by redshifts from the lowest to the highest, are from surveys GHASP (log M*[M⊙]=9.4–11.0; log



M



∗


avg


$ M_{\mathrm{*}}^{\mathrm{avg}} $


[M⊙]=10.6; Epinat et al. 2010), DYNAMO (log M*[M⊙]=9.0–11.8; log



M



∗


avg


$ M_{\mathrm{*}}^{\mathrm{avg}} $


[M⊙]=10.3; Green et al. 2014), MUSE and KMOS (log M*[M⊙]=8.0-11.1; log



M



∗


avg


$ M_{\mathrm{*}}^{\mathrm{avg}} $


[M⊙]=9.4, 9.8 at z ∼ 0.7, 1.3; Swinbank et al. 2017), KROSS (log M*[M⊙] = 8.7–11.0; log



M



∗


avg


$ M_{\mathrm{*}}^{\mathrm{avg}} $


[M⊙]=9.9; Johnson et al. 2018), KMOS3D (log M*[M⊙]=9.0–11.7; log



M



∗


avg


$ M_{\mathrm{*}}^{\mathrm{avg}} $


[M⊙]=10.5, 10.6, 10.7 at z ∼ 0.9, 1.5, 2.3; Wisnioski et al. 2015; Übler et al. 2019), MASSIV (log M*[M⊙]=9.4–11.0; log



M



∗


avg


$ M_{\mathrm{*}}^{\mathrm{avg}} $


[M⊙]=10.2; Epinat et al. 2012), SIGMA (log M*[M⊙]=9.2–11.8; log



M



∗


avg


$ M_{\mathrm{*}}^{\mathrm{avg}} $


[M⊙]=10.0; Simons et al. 2016), SINS (log M*[M⊙]=9.8–11.5; log



M



∗


avg


$ M_{\mathrm{*}}^{\mathrm{avg}} $


[M⊙]=10.8; Förster Schreiber et al. 2009; Cresci et al. 2009), LAW09 (log M*[M⊙]=9.0–10.9; log



M



∗


avg


$ M_{\mathrm{*}}^{\mathrm{avg}} $


[M⊙]=10.3; Law et al. 2009), AMAZE (log M*[M⊙]=9.2–10.6; log



M



∗


avg


$ M_{\mathrm{*}}^{\mathrm{avg}} $


[M⊙]=10.0; Gnerucci et al. 2011), and KDS (log M*[M⊙]=9.0–10.5; log



M



∗


avg


$ M_{\mathrm{*}}^{\mathrm{avg}} $


[M⊙]=9.8; Turner et al. 2017). The molecular gas observations of the star-forming galaxies, sorted by redshifts, are from the HERACLES survey (log M*[M⊙]=7.1–10.9; log



M



∗


avg


$ M_{\mathrm{*}}^{\mathrm{avg}} $


[M⊙]=10.5; Leroy et al. 2008, 2009) and the PHIBSS survey (log M*[M⊙]=10.6-11.2; log



M



∗


avg


$ M_{\mathrm{*}}^{\mathrm{avg}} $


[M⊙]=11.0; Tacconi et al. 2013). We note that although the velocity dispersion measured from the molecular gas is ∼10−15 km s−1 lower than from the ionized gas (with extra contributions from thermal broadening and expansion of the HII regions) in the local Universe, this difference becomes smaller with increasing redshift (Übler et al. 2019). Some field SBs with individual CO observations (Calistro Rivera et al. 2018; Barro et al. 2017; Swinbank et al. 2011; Tadaki et al. 2017, 2019) are indicated with blue triangles in Figs. 5 and 6. When possible, we also identified the field starbursts (orange symbols in Figs. 5 and 6) within the above star-forming samples, requiring their SFR to be at least 0.5 dex higher than the MS. In general, the gas in these field starbursts is slightly more turbulent than in main-sequence galaxies, showing a higher σ0, especially at 2   z   4. A similar trend of increasing σ0 as galaxies move above the MS at a fixed stellar mass is shown for star-forming galaxies at z = 0−3 (e.g., Perna et al. 2022; Wisnioski et al. 2015), suggesting that mergers or interactions would increase gas σ0 as they enhance star formation.
Citation: Cresci et al. 2009
Citation function: Uses