Feedback and galaxy dynamics: A study of turbulence and star formation in 34 galaxies using the PHANGS survey (2403.12927v1)

Abstract: The correlation between interstellar turbulent speed and local star formation rate surface density, Sigma_SFR, is studied using CO observations in the PHANGS survey. The local velocity dispersion of molecular gas, sigma, increases with Sigma_SFR, but the virial parameter, alpha_vir, is about constant, suggesting the molecular gas remains self-gravitating. The correlation arises because sigma depends on the molecular surface density, Sigma_mol, and object cloud mass, M_mol, with the usual molecular cloud correlations, while Sigma_SFR increases with both of these quantities because of a nearly constant star formation efficiency for CO. Pressure fluctuations with Delta Sigma_SFR are also examined. Azimuthal variations of molecular pressure, Delta P_mol, have a weaker correlation with Delta Sigma_SFR than expected from the power-law correlation between the total quantities, suggesting slightly enhanced SFR efficiency per molecule in spiral arms. Dynamical equilibrium pressure and star formation rate correlate well for the whole sample, as P_DE~Sigma_SFR^1.3, which is steeper than in other studies. The azimuthal fluctuations, Delta P_DE(Delta Sigma_SFR), follow the total correlation P_DE(Sigma_SFR) closely, hinting that some of this correlation may be a precursor to star formation, rather than a reaction. Galactic dynamical processes correlate linearly such that Sigma_SFR~(Sigma_gas R)^1.0\m0.3) for total gas surface density Sigma_gas and galactic dynamical rates, R, equal to kappa, A, or Omega, representing epicyclic frequency, shear rate A, and orbit rate Omega. These results suggest important roles for both feedback and galactic dynamics.