We present a characterization of the physical properties of a sample of 35 securely-detected, dusty galaxies in the deep ALMA 1.2-mm image obtained as part of the ALMA Spectroscopic Survey in the {\it Hubble} Ultra Deep Field (ASPECS) Large Program. This sample is complemented by 26 additional sources identified via an optical/infrared source positional prior. Using their well-characterized spectral energy distributions, we derive median stellar masses and star formation rates (SFR) of $4.8\times10^{10}~M_\odot$ and 30 $M_\odot$ yr$^{-1}$, and interquartile ranges of $(2.4-11.7)\times10^{10}~M_\odot$ and $20-50~M_\odot$ yr$^{-1}$, respectively. We derive a median spectroscopic redshift of 1.8 with an interquartile range $1.1-2.6$, significantly lower than sub-millimeter galaxies detected in shallower, wide-field surveys. We find that 59\%$\pm$13\%, 6\%$\pm$4\%, and 34\%$\pm$9\% of our sources are within, above and below $\pm0.4$ dex from the SFR- stellar mass relation or main-sequence (MS), respectively. The ASPECS galaxies closely follow the SFR-molecular gas mass relation and other previously established scaling relations, confirming a factor of five increase of the gas-to-stellar mass ratio from $z=0.5$ to $z=2.5$, and a mild evolution of the gas depletion timescales with a typical value of 0.7 Gyr at $z=1-3$. ASPECS galaxies located significantly below the MS, a poorly exploited parameter space, have low gas-to-stellar mass ratios of $\sim0.1-0.2$ and long depletion timescales $>1$ Gyr. Galaxies along the MS dominate the cosmic density of molecular gas at all redshifts. Systems above the main sequence have an increasing contribution to the total gas reservoirs from $z<1$ to $z=2.5$, while the opposite is found for galaxies below the MS.

中文翻译：

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哈勃超深场中的 ALMA 光谱巡天：最暗的尘土星形成星系的性质

我们在 ALMA 1.2 毫米深图像中展示了 35 个安全检测到的尘埃星系样本的物理特性表征，该图像是 {\it Hubble} 超深场 (ASPECS) 大型计划中 ALMA 光谱调查的一部分. 该样本由通过光学/红外源位置先验识别的 26 个附加源进行补充。使用它们充分表征的光谱能量分布，我们推导出中值恒星质量和恒星形成率 (SFR) 为 $4.8\times10^{10}~M_\odot$ 和 30 $M_\odot$yr$^{-1}$，和四分位距分别为 $(2.4-11.7)\times10^{10}~M_\odot$ 和 $20-50~M_\odot$ yr$^{-1}$。我们得出的光谱红移中值为 1.8，四分位数范围为 1.1-2.6 美元，明显低于在较浅的宽视场调查中检测到的亚毫米星系。我们发现 59\%$\pm$13\%，6\%$\pm$4\% 和 34\%$\pm$9\% 我们的来源在 SFR-恒星质量关系或主序 (MS) 的 $\pm0.4$ dex 之内、之上和之下， 分别。ASPECS 星系密切遵循 SFR-分子气体质量关系和其他先前建立的比例关系，确认气体与恒星的质量比从 $z=0.5$ 增加到 $z=2.5$ 增加了五倍，并且一个温和的气体消耗时间尺度的演变，在 $z=1-3$ 时典型值为 0.7 Gyr。ASPECS 星系明显位于 MS 下方，这是一个未充分利用的参数空间，具有 $\sim0.1-0.2$ 的低气体与恒星质量比和长耗尽时间尺度 $>1$ Gyr。沿着 MS 的星系在所有红移处主导着分子气体的宇宙密度。主层序之上的系统对总气藏的贡献从$z<1$到$z=2。