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Mapping the molecular gas content of the universe is key to our understandingof the build-up of galaxies over cosmic time. Spectral line scans in deepfields, such as the Hubble Ultra Deep Field (HUDF), provide a unique view onthe cold gas content out to high redshift. By conducting`spectroscopy-of-everything', these flux-limited observations are sensitive tothe molecular gas in galaxies without preselection, revealing the cold gascontent of galaxies that would not be selected in traditional studies. In orderto capitalize on the molecular gas observations, knowledge about the physicalconditions of the galaxies detected in molecular gas, such as theirinterstellar medium conditions, is key. Fortunately, deep surveys withintegral-field spectrographs are providing an unprecedented view of the galaxypopulation, providing redshifts and measurements of restframe UV/optical linesfor thousands of galaxies. We present the results from the synergy between theALMA Spectroscopic Survey of the HUDF (ASPECS), with deep integral fieldspectroscopy from the MUSE HUDF survey and multi-wavelength data. We discussthe nature of the galaxies detected in molecular gas without preselection andtheir physical properties, such as star formation rate and metallicity. We showhow the combination of ALMA and MUSE integral field spectroscopy can constrainthe physical properties in galaxies located around the main sequence during thepeak of galaxy formation.

Nature and physical properties of ALMA selected galaxies using MUSE spectroscopy