Star Formation Laws and Efficiencies across 80 Nearby Galaxies
Creators: name: Sun, Jiayi
name: Leroy, Adam K.
name: Ostriker, Eve C.
name: Meidt, Sharon
name: Rosolowsky, Erik
name: Schinnerer, Eva
name: Wilson, Christine D.
name: Utomo, Dyas
name: Belfiore, Francesco
name: Blanc, Guillermo A.
name: Emsellem, Eric
name: Faesi, Christopher
name: Groves, Brent
name: Hughes, Annie
name: Koch, Eric W.
name: Kreckel, Kathryn
name: Liu, Daizhong
name: Pan, Hsi-An
name: Pety, Jerome
name: Querejeta, Miguel
name: Razza, Alessandro
name: Saito, Toshiki
name: Sardone, Amy
name: Usero, Antonio
name: Williams, Thomas G.
name: Bigiel, Frank
name: Bolatto, Alberto D.
name: Chevance, Melanie
name: Dale, Daniel A.
name: Gensior, Jindra
name: Glover, Simon C. O.
name: Grasha, Kathryn
name: Henshaw, Jonathan D.
name: Jimenez-Donaire, Maria J.
name: Klessen, Ralf S.
name: Kruijssen, J. M. Diederik
name: Murphy, Eric J.
name: Neumann, Lukas
name: Teng, Yu-Hsuan
name: Thilker, David A.
Publisher: name: arXiv
Year: 2023
Subjects: subject: Astrophysics of Galaxies (astro-ph.GA)
subject: FOS: Physical sciences
subject: FOS: Physical sciences

description: We measure empirical relationships between the local star formation rate (SFR) and properties of the star-forming molecular gas on 1.5 kpc scales across 80 nearby galaxies. These relationships, commonly referred to as "star formation laws," aim at predicting the local SFR surface density from various combinations of molecular gas surface density, galactic orbital time, molecular cloud free-fall time, and the interstellar medium dynamical equilibrium pressure. Leveraging a multiwavelength database built for the PHANGS survey, we measure these quantities consistently across all galaxies and quantify systematic uncertainties stemming from choices of SFR calibrations and the CO-to-H$_2$ conversion factors. The star formation laws we examine show 0.3-0.4 dex of intrinsic scatter, among which the molecular Kennicutt-Schmidt relation shows a $\sim$10% larger scatter than the other three. The slope of this relation ranges $β\approx0.9{-}1.2$, implying that the molecular gas depletion time remains roughly constant across the environments probed in our sample. The other relations have shallower slopes ($β\approx0.6{-}1.0$), suggesting that the star formation efficiency (SFE) per orbital time, the SFE per free-fall time, and the pressure-to-SFR surface density ratio (i.e., the feedback yield) may vary systematically with local molecular gas and SFR surface densities. Last but not least, the shapes of the star formation laws depend sensitively on methodological choices. Different choices of SFR calibrations can introduce systematic uncertainties of at least 10-15% in the star formation law slopes and 0.15-0.25 dex in their normalization, while the CO-to-H$_2$ conversion factors can additionally produce uncertainties of 20-25% for the slope and 0.10-0.20 dex for the normalization.
description: 10 pages main text + 2 appendices. ApJL in press. Data products available at https://www.canfar.net/storage/list/phangs/RELEASES/Sun_etal_2023 . Slides summarizing key results can be found at https://www.dropbox.com/s/5gsegexeo9n0t05/Sun_et_PHANGS_2023.pptx?dl=0