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首页> 外文期刊>The Astrophysical journal >THE STAR FORMATION RATE INTENSITY DISTRIBUTION FUNCTION: IMPLICATIONS FOR THE COSMIC STAR FORMATION RATE HISTORY OF THE UNIVERSE
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THE STAR FORMATION RATE INTENSITY DISTRIBUTION FUNCTION: IMPLICATIONS FOR THE COSMIC STAR FORMATION RATE HISTORY OF THE UNIVERSE

机译：恒星形成率强度分布函数：对宇宙宇宙恒星形成率历史的启示

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摘要

We address the effects of cosmological surface brightness dimming on observations of faint galaxies by examining the distribution of "unobscured" star formation rate intensities versus redshift. We use the star formation rate intensity distribution function to assess the ultraviolet luminosity density versus redshift, based on our photometry and photometric redshift measurements of faint galaxies in the Hubble Deep Field (HDF) and the Hubble Deep Field-South (HDF-S) Wide Field Planetary Camera 2 and Near-Infrared Camera and Multi-Object Spectrometer fields. We find that (1) previous measurements have missed a dominant fraction of the ultraviolet luminosity density of the universe at high redshifts by neglecting cosmological surface brightness dimming effects, which are important at redshifts larger than z ≈ 2; (2) the incidence of the highest intensity star-forming regions increases monotonically with redshift; and (3) the ultraviolet luminosity density plausibly increases monotonically with redshift through the highest redshifts observed. By measuring the spectrum of the luminosity density versus redshift, we also find that (4) previous measurements of the ultraviolet luminosity density at redshifts z < 2 must be reduced by a factor of ≈ 2 to allow for the spectrum of the luminosity density between rest-frame wavelengths 1500 and 2800 A. And, by comparing with observations of high-redshift damped Lyα absorption systems detected toward background quasi-stellar objects, we further find that (5) the distribution of star formation rate intensities matches the distribution of neutral hydrogen column densities at redshifts z ≈ 2-5, which establishes a quantitative connection between high-redshift galaxies and high column density gas and suggests that high-redshift damped Lyα absorption systems trace lower star formation rate intensity regions of the same galaxies detected in starlight in the HDF and HDF-S. Because our measurements neglect the effects of obscuration by dust, they represent lower limits to the total star formation rate density.
机译：我们通过检查“无遮盖的”恒星形成速率强度与红移的分布，来解决宇宙表面亮度降低对微弱星系观测的影响。我们使用哈勃深场（HDF）和南哈勃深场（HDF-S）的微弱星系的光度法和光度法红移测量，使用恒星形成率强度分布函数来评估紫外线发光密度与红移的关系行星摄像机2和近红外摄像机以及多对象光谱仪字段。我们发现（1）先前的测量通过忽略宇宙学的表面亮度调光效果而错过了在高红移下宇宙的紫外线发光密度的主要部分，这在大于z≈2的红移上很重要; （2）最高强度恒星形成区的发生率随红移单调增加; （3）随着观察到的最高红移，红移的紫外光度密度似乎单调增加。通过测量光度密度与红移的光谱，我们还发现（4）必须将先前在红移z <2时的紫外线光度密度测量值降低≈2，以允许静止之间的光度密度光谱框架波长1500和2800A。并且，通过与对背景准星体探测到的高红移阻尼Lyα吸收系统的观察结果进行比较，我们进一步发现（5）恒星形成速度强度的分布与中性氢的分布相匹配红移z≈2-5时的柱密度，建立了高红移星系与高柱密度气体之间的定量联系，并表明高红移阻尼Lya吸收系统追踪了在星光下检测到的同一星系的较低恒星形成率强度区域。 HDF和HDF-S。由于我们的测量结果忽略了尘埃遮盖的影响，因此它们代表了总恒星形成速率密度的下限。

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