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We report molecular gas mass estimates obtained from a stacking analysis ofCO line emission in the ALMA Spectroscopic Survey (ASPECS) using thespectroscopic redshifts from the optical integral field spectroscopic survey bythe Multi Unit Spectroscopic Explorer (MUSE) of the {\it Hubble} Ultra DeepField (HUDF). Stacking was performed on subsets of the sample of galaxiesclassified by their stellar mass and position relative to the main-sequencerelation (on, above, below). Among all the CO emission lines, from \cotwoone toCO(6-5), with redshifts accessible via the ASPECS Band~3 and the MUSE data,\cotwoone provides the strongest constraints on the molecular gas content. Wedetect \cotwoone emission in galaxies down to stellar masses of$\log{(M_*/M_\odot)}=10.0$. Below this stellar mass, we present a newconstraint on the molecular gas content of $z\sim1.5$ main-sequence galaxies bystacking based on the MUSE detections. We find that the molecular gas mass ofmain-sequence galaxies continuously decreases with stellar mass down to$\log{(M_*/M_\odot)}\approx9.0$. Assuming a metallicity-based CO--to--$\rm H_2$conversion factor, the molecular gas-to-stellar mass ratio from$\log{(M_*/M_\odot)}\sim9.0$ to $\sim10.0$ does not seem to decrease as fast asfor $\log{(M_*/M_\odot)}>10.0$, which is in line with simulations and studiesat lower redshift. The inferred molecular gas density $\rho{\rm(H_2)}=(0.49\pm0.09)\times10^8\,{\rm M_\odot\,Mpc^{-3}}$ of MUSE-selectedgalaxies at $z\sim1.5$ is comparable with the one derived in the HUDF with adifferent CO selection. Using the MUSE data we recover most of the CO emissionin our deep ALMA observations through stacking, demonstrating the synergybetween volumetric surveys obtained at different wavebands.

astrophysical journal/the astrophysical journal

The ALMA Spectroscopic Survey in the HUDF: Constraining the Molecular  Content at $\log{(M_*/M_\odot)} \sim 9.5$ with CO stacking of MUSE detected  $z\sim1.5$ Galaxies