The nature of H{\sc i}-absorption-selected galaxies at $z\approx 4$

Abstract

We report a Karl G. Jansky Very Large Array (JVLA) search for redshifted CO(1-0) or CO(2-1) emission, and a Hubble Space Telescope Wide Field Camera~3 (HST-WFC3) search for rest-frame near-ultraviolet (NUV) stellar emission, from seven HI-selected galaxies associated with high-metallicity ([M/H]~$\ge -1.3$) damped Ly$\hat{I}\pm$ absorbers (DLAs) at $z\approx 4$. The galaxies were earlier identified by ALMA imaging of their [CII]~158$\hat{I}¼$m emission. We also used the JVLA to search for CO(2-1) emission from the field of a low-metallicity ([M/H]~$=-2.47$) DLA at $z\approx 4.8$. No statistically significant CO emission is detected from any of the galaxies, yielding upper limits of $M_{mol}<(7.4-17.9)\times 10^{10}\times (\hat{I}{\pm }_{CO}/4.36)M_{\odot }$ on their molecular gas mass. We detect rest-frame NUV emission from four of the seven [CII]~158$\hat{I}¼$m-emitting galaxies, the first detections of the stellar continuum from HI-selected galaxies at $z\gtrsim 4$. The HST-WFC3 images yield typical sizes of the stellar continua of $\approx 2-4$~kpc and inferred dust-unobscured star-formation rates (SFRs) of $\approx 5.0-17.5M_{\odot }$/yr, consistent with, or slightly lower than, the total SFRs estimated from the far-infrared (FIR) luminosity. We further stacked the CO(2-1) emission signals of six [CII]~158$\hat{I}¼$m-emitting galaxies in the image plane. Our non-detection of CO(2-1) emission in the stacked image yields the limit $M_{mol}<4.1\times 10^{10}\times (\hat{I}{\pm }_{CO}/4.36)M_{\odot }$ on the average molecular gas mass of the six galaxies. Our molecular gas mass estimates and NUV SFR estimates in HI-selected galaxies at $z\approx 4$ are consistent with those of main-sequence galaxies with similar [CII]~158$\hat{I}¼$m and FIR luminosities at similar redshifts. However, the NUV emission in the HI-selected galaxies appears more extended than that in main-sequence galaxies at similar redshifts.

16 pages, 6 figures, accepted for publication in ApJ