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首页> 外文期刊>The Astrophysical journal >THE FIRST DETECTIONS OF THE EXTRAGALACTIC BACKGROUND LIGHT AT 3000, 5500, AND 8000 A. Ⅲ. COSMOLOGICAL IMPLICATIONS
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THE FIRST DETECTIONS OF THE EXTRAGALACTIC BACKGROUND LIGHT AT 3000, 5500, AND 8000 A. Ⅲ. COSMOLOGICAL IMPLICATIONS

机译：探测3000、5500和8000 A的星系外背景光的第一步。Ⅲ。宇宙学意义

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We have used the Hubble Space Telescope Wide Field, and Planetary Camera 2 in combination with ground-based spectroscopy to measure the integrated flux of galaxies at optical wavelengths―the extragalac-tic background light (EBL). We have also computed the integrated light from individual galaxy counts in the images used to measure the EBL and in the Hubble Deep Field. We find that flux in galaxies as measured by standard galaxy photometry methods has generally been underestimated by about 50%, resulting from missed flux in the outer, lower surface brightness parts of galaxies and from associated errors in the estimated sky level. Comparing the corrected, integrated flux from individual galaxies with our total EBL measurement, We find that there is yet further light that contributes to the background that is not represented by galaxy counts and that the total flux in individually detected sources is a factor of 2-3 less than the EBL from 8000 to 3000 A. We show that a significant fraction of the EBL may come from normal galaxies at z < 4, which are simply undetectable as a result of K-corrections and cosmological surface brightness dimming. This result is consistent with results from recent redshift surveys at z < 4. In the context of some simple models, we discuss the constraints placed by the EBL on evolution in the luminosity density at z > 1; while significant flux comes from galaxies beyond the current detection limits, this evolution cannot be tightly constrained by our data. Based on our measurements of the optical EBL, combined with previously published measurements of the UV and IR EBL, we estimate that the total EBL from 0.1 to 1000 μm is 100 +- 20 nW m~(-2) sr~(-1). If the total EBL were produced entirely by stellar nucleosynthesis, then we estimate that the total baryonic mass processed through stars is Ω_* = 0.0062(+-0.0022) h~(-2) in units of the critical density. For currently favored values of the baryon density Ω_B this corresponds to 0.33 +- 0.12Ω_B. This estimate is smaller by roughly 7% if we allow for a contribution of 7 h_(0.7) nW m~(-2) sr~(-1) to the total EBL from accretion onto central black holes. This estimate of Ω_* suggests that the universe has been enriched to a total metal mass of 0.21 (+-0.13) Z_☉Ω_B, which is consistent with other observational estimates of the cumulative metal mass fraction of stars, stellar remnants, and the intracluster medium of galaxy clusters in the local universe.
机译：我们已经使用了哈勃太空望远镜宽视场和行星相机2结合地面光谱学来测量在光学波长（星系外背景光（EBL））下星系的积分通量。我们还从用于测量EBL的图像和哈勃深场中的各个星系计数中计算了积分光。我们发现，通过标准星系光度法测量的星系通量通常被低估了约50％，这是由于星系的外，下表面亮度部分的通量缺失以及估计的天空水平相关的误差所致。将来自各个星系的校正后的积分通量与我们的总EBL测量值进行比较，我们发现还有更多的光对背景有贡献，这不是由星系计数所代表的，并且单独检测到的源中的总通量是2的倍数比8000至3000 A的EBL小3倍。我们证明，EBL的很大一部分可能来自z <4的正常星系，这是由于K校正和宇宙学表面亮度变暗而根本无法检测到的。此结果与z <4处最近的红移调查的结果一致。在一些简单模型的背景下，我们讨论了EBL对z> 1时光密度变化的约束。尽管来自银河系的大量通量超出了当前的检测极限，但是我们的数据不能严格限制这种演化。根据我们对光学EBL的测量结果，再结合先前发布的对UV和IR EBL的测量结果，我们估计从0.1到1000μm的总EBL为100 +-20 nW m〜（-2）sr〜（-1） 。如果总的EBL完全由恒星核合成产生，那么我们估计通过恒星加工的总重子质量为Ω_* = 0.0062（+-0.0022）h〜（-2），以临界密度为单位。对于重子密度Ω_B的当前优选值，这对应于0.33±0.12Ω_B。如果我们允许将7 h_（0.7）nW m〜（-2）sr〜（-1）的贡献从中央黑洞积聚到总EBL中，则该估计值将减小约7％。 Ω_*的这一估计值表明宇宙已经富集到总金属质量为0.21（+ -0.13）Z_☉Ω_B，这与恒星，恒星残留物和团簇内的累积金属质量分数的其他观测估计值一致当地宇宙中银河星团的媒介。

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