TY - JOUR
T1 - The EDGE-CALIFA survey
T2 - The influence of galactic rotation on the molecular depletion time across the Hubble sequence
AU - Colombo, D.
AU - Kalinova, V.
AU - Utomo, D.
AU - Rosolowsky, E.
AU - Bolatto, A. D.
AU - Levy, R. C.
AU - Wong, T.
AU - Sanchez, S. F.
AU - Leroy, A. K.
AU - Ostriker, E.
AU - Blitz, L.
AU - Vogel, S.
AU - Mast, D.
AU - García-Benito, R.
AU - Husemann, B.
AU - Dannerbauer, H.
AU - Ellmeier, L.
AU - Cao, Y.
PY - 2018/4/1
Y1 - 2018/4/1
N2 - We present a kpc-scale analysis of the relationship between the molecular depletion time (τdepmol ) and the orbital time (τorb) across the field of 39 face-on local galaxies, selected from the EDGE-CALIFA sample. We find that, on average, 5 per cent of the available molecular gas is converted into stars per orbital time, or τ depmol ~ 20 τorb. The resolved relation shows a scatter of ~0.5 dex. The scatter is ascribable to galaxies of different morphologies that follow different τ depmol -τorb relations which decrease in steepness from early- to late types. The morphologies appear to be linked with the star formation rate surface density, the molecular depletion time, and the orbital time, but they do not correlate with the molecular gas content of the galaxies in our sample.We speculate that in our molecular gas rich, early-type galaxies, the morphological quenching (in particular the disc stabilization via shear), rather than the absence of molecular gas, is the main factor responsible for their current inefficient star formation.
AB - We present a kpc-scale analysis of the relationship between the molecular depletion time (τdepmol ) and the orbital time (τorb) across the field of 39 face-on local galaxies, selected from the EDGE-CALIFA sample. We find that, on average, 5 per cent of the available molecular gas is converted into stars per orbital time, or τ depmol ~ 20 τorb. The resolved relation shows a scatter of ~0.5 dex. The scatter is ascribable to galaxies of different morphologies that follow different τ depmol -τorb relations which decrease in steepness from early- to late types. The morphologies appear to be linked with the star formation rate surface density, the molecular depletion time, and the orbital time, but they do not correlate with the molecular gas content of the galaxies in our sample.We speculate that in our molecular gas rich, early-type galaxies, the morphological quenching (in particular the disc stabilization via shear), rather than the absence of molecular gas, is the main factor responsible for their current inefficient star formation.
KW - Galaxies: evolution
KW - Galaxies: kinematics and dynamics
KW - Galaxies: star formation
KW - Galaxies: structure
KW - ISM: molecules
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U2 - 10.1093/MNRAS/STX3233
DO - 10.1093/MNRAS/STX3233
M3 - Article
AN - SCOPUS:85043510277
VL - 475
SP - 1791
EP - 1808
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
SN - 0035-8711
IS - 2
ER -