The HI mass function of star-forming galaxies at $\mathbf{z}\sim 0.35$

Abstract

The neutral atomic hydrogen (HI) mass function (HIMF) describes the distribution of the HI content of galaxies at any epoch; its evolution provides an important probe of models of galaxy formation and evolution. Here, we report Giant Metrewave Radio Telescope HI 21cm spectroscopy of blue star-forming galaxies at $z\approx 0.20-0.42$ in the Extended Groth Strip, which has allowed us to determine the scaling relation between the average HI mass (${\mathrm{M}}_{\mathrm{HI}}$) and the absolute B-band magnitude (${\mathrm{M}}_{\mathrm{B}}$) of such galaxies at $z\approx 0.35$, by stacking the HI 21cm emission signals of galaxy subsamples in different ${\mathrm{M}}_{\mathrm{B}}$ ranges. We combine this ${\mathrm{M}}_{\mathrm{HI}}-{\mathrm{M}}_{\mathrm{B}}$ scaling relation (with a scatter assumed to be equal to that in the local Universe) with the known B-band luminosity function of star-forming galaxies at these redshifts to determine the HIMF at $z\approx 0.35$. We show that the use of the correct scatter in the ${\mathrm{M}}_{\mathrm{HI}}-{\mathrm{M}}_{\mathrm{B}}$ scaling relation is critical for an accurate estimate of the HIMF. We find that the HIMF has evolved significantly from $z\approx 0.35$ to $z\approx 0$, i.e. over the last four Gyr, especially at the high-mass end. High-mass galaxies, with ${\mathrm{M}}_{\mathrm{HI}}\gtrsim 10^{10}{\mathrm{M}}_{\odot }$, are a factor of $\approx 3.4$ less prevalent at $z\approx 0.35$ than at $z\approx 0$. Conversely, there are more low-mass galaxies, with ${\mathrm{M}}_{\mathrm{HI}}\approx 10^9{\mathrm{M}}_{\odot }$, at $z\approx 0.35$ than in the local Universe. While our results may be affected by cosmic variance, we find that massive star-forming galaxies have acquired a significant amount of HI through merger events or accretion from the circumgalactic medium over the past four Gyr.

arXiv commentAccepted for publication in The Astrophysical Journal Letters

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