New constraints on the evolution of the MHI-M* scaling relation combining CHILES and MIGHTEE-HI data

Abstract

The improved sensitivity of interferometric facilities to the 21-cm line of atomic hydrogen (HI) enables studies of its properties in galaxies beyond the local Universe. In this work, we perform a 21 cm line spectral stacking analysis combining the MIGHTEE and CHILES surveys in the COSMOS field to derive a robust HI-stellar mass relation at z=0.36. In particular, by stacking thousands of star-forming galaxies subdivided into stellar mass bins, we optimize the signal-to-noise ratio of targets and derive mean HI masses in the different stellar mass intervals for the investigated galaxy population. We combine spectra from the two surveys, estimate HI masses, and derive the scaling relation log10(MHI) = (0.32 +- 0.04)log10(M*) + (6.65 +- 0.36). Our findings indicate that galaxies at z=0.36 are HI richer than those at z=0, but HI poorer than those at z=1, with a slope consistent across redshift, suggesting that stellar mass does not significantly affect HI exchange mechanisms. We also observe a slower growth rate HI relative to the molecular gas, supporting the idea that the accretion of cold gas is slower than the rate of consumption of molecular gas to form stars. This study contributes to understanding the role of atomic gas in galaxy evolution and sets the stage for future development of the field in the upcoming SKA era.

23 pages, 16 figures, accepted for publication in ApJ

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• Emission-line Stacking of 21cm Intensity Maps with MeerKLASS: Inference Pipeline and Application to the L-band Deep-field Data
• MIGHTEE-HI: The direct detection of neutral hydrogen in galaxies at $z>0.25$
• The dark side of early galaxies: $\text{geko}$ uncovers dark-matter fractions at $z\sim 4-6$
• CHILES X: Molecular and atomic gas at intermediate redshift
• CHILES XII: The H I evolution of Luminous Compact Blue Galaxies between 0<z<0.48
• NeutralUniverseMachine: Predictions of HI gas in Different Theoretical Models
• The Baryon Budget of Galaxies across the First Billion Years
• Atomic hydrogen reservoirs in quiescent galaxies at z = 0.4
• Semi-empirical constraints on the HI mass function of star-forming galaxies and ${\Omega }_{\mathrm{HI}}$ at $z\sim 0.37$ from interferometric surveys