V <i>z</i> -GAL: Probing Cold Molecular Gas in Dusty Star-forming Galaxies at <i>z</i> = 1–6

Abstract We present the first results of V z -GAL, a high-redshift CO( J = 1–0) large survey with the Karl G. Jansky Very Large Array, targeting 92 Herschel-selected, infrared-luminous, dusty star-forming galaxies at redshifts 1–6. These sources are selected based on having redshifts and mid-/high- J CO transitions from the NOrthern Extended Millimeter Array z –GAL survey. We successfully detect CO( J = 1–0) emission in 90/92 galaxies at the expected positions and redshifts, including nine tentative detections at 2 σ –3 σ significance, and CO( J = 2–1) emission in 10 of these galaxies. The CO( J = 1–0) luminosities suggest apparent gas masses in the range <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mi>μ</mml:mi> <mml:msub> <mml:mrow> <mml:mi>M</mml:mi> </mml:mrow> <mml:mrow> <mml:msub> <mml:mrow> <mml:mi mathvariant="normal">H</mml:mi> </mml:mrow> <mml:mrow> <mml:mn>2</mml:mn> </mml:mrow> </mml:msub> </mml:mrow> </mml:msub> </mml:math> = (2–20) × 10 11 ( α CO /4.0) M ⊙ , which implies gas depletion times of 50–600 Myr. These timescales show similar spread as local ULIRGs, suggesting a self-regulatory mechanism that maintains a consistent star formation rate per unit gas mass in starbursts across redshifts. To quantify the contribution of “excitation correction” factors to gas mass estimates, we calculate median CO line brightness temperature ratios of r 21 = 0.88 ± 0.25, r 31 = 0.61 ± 0.22, r 41 = 0.49 ± 0.15, r 51 = 0.47 ± 0.13, and r 61 = 0.28 ± 0.13. Accounting for these corrections results in a reduced scatter in “gas mass–star formation rate” relations. We also find a median log( <mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" overflow="scroll"> <mml:mi>L</mml:mi> <mml:msub> <mml:mrow> <mml:mo accent="true">′</mml:mo> </mml:mrow> <mml:mrow> <mml:mo stretchy="false">[</mml:mo> <mml:mi mathvariant="normal">CI</mml:mi> <mml:mo stretchy="false">]</mml:mo> <mml:msup> <mml:mrow> <mml:mo stretchy="false">(</mml:mo> </mml:mrow> <mml:mrow> <mml:mn>3</mml:mn> </mml:mrow> </mml:msup> <mml:msub> <mml:mrow> <mml:mi>P</mml:mi> </mml:mrow> <mml:mrow> <mml:mn>1</mml:mn> </mml:mrow> </mml:msub> <mml:msup> <mml:mrow> <mml:mo>−</mml:mo> </mml:mrow> <mml:mrow> <mml:mn>3</mml:mn> </mml:mrow> </mml:msup> <mml:msub> <mml:mrow> <mml:mi>P</mml:mi> </mml:mrow> <mml:mrow> <mml:mn>0</mml:mn> </mml:mrow> </mml:msub> <mml:mo stretchy="false">)</mml:mo> </mml:mrow> </mml:msub> <mml:mo>/</mml:mo> <mml:mi>L</mml:mi> <mml:msub> <mml:mrow> <mml:mo accent="true">′</mml:mo> </mml:mrow> <mml:mrow> <mml:mi mathvariant="normal">CO</mml:mi> <mml:mo stretchy="false">(</mml:mo> <mml:mi>J</mml:mi> <mml:mo>=</mml:mo> <mml:mn>1</mml:mn> <mml:mo>−</mml:mo> <mml:mn>0</mml:mn> <mml:mo stretchy="false">)</mml:mo> </mml:mrow> </mml:msub> <mml:mo stretchy="false">)</mml:mo> <mml:mo>=</mml:mo> <mml:mo>−</mml:mo> <mml:mn>0.71</mml:mn> <mml:mo>±</mml:mo> <mml:mn>0.12</mml:mn> </mml:math> for a subsample of 23 sources, consistent with the ratios derived for local star-forming galaxies. Together, our findings are in agreement with common conditions in the cold gas reservoirs among star-forming galaxies over a broad range in star formation modes, efficiencies, and scales.