Molecular Gas Mass Measurements of an Active, Starburst Galaxy at z ≈ 2.6 Using ALMA Observations of the [C i], CO, and Dust Emission

We present new Atacama Large Millimeter/submillimeter Array (ALMA) observations of a starburst galaxy at cosmic noon hosting a radio-loud active galactic nucleus: PKS 0529-549 at z = 2.57. To investigate the conditions of its cold interstellar medium, we use ALMA observations that spatially resolve the [C i] fine-structure lines, [C i] (2–1) and [C i] (1–0), CO rotational lines, CO (7–6) and CO (4–3), and the rest-frame continuum emission at 461 and 809 GHz. The four emission lines display different morphologies, suggesting spatial variation in the gas excitation conditions. The radio jets have just broken out of the molecular gas but not through the more extended ionized gas halo. The [C i] (2–1) emission is more extended (≈8 kpc × 5 kpc) than detected in previous shallower ALMA observations. The [C i] luminosity ratio implies an excitation temperature of 44 ± 16 K, similar to the dust temperature. Using the [C i] lines, CO (4–3), and 227 GHz dust continuum, we infer the mass of molecular gas Mmol using three independent approaches and typical assumptions in the literature. All approaches point to a massive molecular gas reservoir of about 1011M☉, but the exact values differ by up to a factor of 4. Deep observations are critical in correctly characterizing the distribution of cold gas in high-redshift galaxies, and highlight the need to improve systematic uncertainties in inferring accurate molecular gas masses.