Over the past decade, increasingly robust estimates of the dense molecular gas content in
galaxy populations between redshift z= 0 and the peak of cosmic galaxy/star formation (z∼ …

Context. Molecular gas is a necessary fuel for star formation. The CO (1− 0) transition is
often used to deduce the total molecular hydrogen but is challenging to detect in low …

We combine the recent determination of the evolution of the cosmic density of molecular gas
(H 2) using deep, volumetric surveys, with previous estimates of the cosmic density of stellar …

We present a self-consistent cross-calibration of the three main molecular gas mass tracers
in galaxies, namely the 12CO (1–0),[C i](3 P 1–3 P 0) lines, and the submm dust continuum …

We present a CO and atomic fine-structure line-luminosity function analysis using the ALMA
Spectroscopic Survey (ASPECS) in the Hubble Ultra Deep Field. ASPECS consists of two …

We report the first detailed measurement of the shape of the CO luminosity function at high
redshift, based on> 320 hr of the NSF's Karl G. Jansky Very Large Array (VLA) observations …

We use the results from the ALMA large program ASPECS, the spectroscopic survey in the
Hubble Ultra Deep Field (HUDF), to constrain CO luminosity functions of galaxies and the …

Distortions of the observed cosmic microwave background provide a direct measurement of
the microwave background temperature at redshifts from 0 to 1 (refs.,). Some additional …

Dusty star-forming galaxies at high redshift (1< z< 3) represent the most intense star-forming
regions in the universe. Key aspects to these processes are the gas heating and cooling …

Structural Evolution in Massive Galaxies at z ∼ 2 - IOPscience This site uses cookies. By
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