E+A星系的UV性质：对反馈驱动恒星形成猝灭的限制
The UV properties of E+A galaxies: constraints on feedback-driven quenching of star formation
摘要：
我们提出了第一个大规模的研究E+A（后星爆）星系，采用测光在紫外线（UV）波长。我们发现产生E+A星系的星暴通常发生在最后一个Gyrs内，并在短时间尺度（< 0.1 Gyrs）内在残余物中产生很高比例（20- 60%）的恒星质量。我们发现，我们的E+A星系的光度和隐含的恒星形成率（SFR）在星爆之间的紧密相关性。虽然低光度的E+As（M（z）> -20）显示出每年小于50个太阳质量的SFR，但它们的发光对应物（M（z）< -22）显示出每年大于300和高达2000个太阳质量的SFR，这表明低红移宇宙中的发光和超发光红外星系可能是附近大质量E+A星系的祖先。我们对E+A系统中截断星暴的猝灭特性进行了全面的研究，发现对于质量小于10^10 MSun的星系，猝灭效率随着星系质量的增加而降低。然而，对于质量大于10^10 MSun的星系，这种趋势是相反的，淬火效率随着星系质量的增加而增加。注意到发生这种反转的质量阈值与活动星系核在附近星系中变得更加丰富的质量非常一致，我们使用简单的能量论证来证明猝灭效率的双峰行为与活动星系核和超新星（SN）是一致的，它们分别是M ~ 10^10 MSun以上和M ~ 10^10 MSun以下负反馈的主要来源。（节略）
英文摘要：
We present the first large-scale study of E+A (post-starburst) galaxies that incorporates photometry in the ultraviolet (UV) wavelengths. We find that the starburst that creates the E+A galaxy typically takes place within the last Gyr and creates a high fraction (20-60 percent) of the stellar mass in the remnant over a short timescale (< 0.1 Gyrs). We find a tight correlation between the luminosity of our E+A galaxies and the implied star formation rate (SFR) during the starburst. While low-luminosity E+As (M(z) > -20) exhibit implied SFRs of less than 50 solar masses per year, their luminous counterparts (M(z) < -22) shows SFRs greater than 300 and as high as 2000 solar masses per year, suggesting that luminous and ultra-luminous infrared galaxies in the low-redshift Universe could be the progenitors of massive nearby E+A galaxies. We perform a comprehensive study of the characteristics of the quenching that truncates the starburst in E+A systems.We find that, for galaxies less massive than 10^10 MSun, the quenching efficiency decreases as the galaxy mass increases. However, for galaxies more massive than 10^10 MSun, this trend is reversed and the quenching efficiency increases with galaxy mass. Noting that the mass threshold at which this reversal occurs is in excellent agreement with the mass above which AGN become significantly more abundant in nearby galaxies, we use simple energetic arguments to show that the bimodal behaviour of the quenching efficiency is consistent with AGN and supernovae (SN) being the principal sources of negative feedback above and below M ~ 10^10 MSun respectively. (abridged)
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