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arXiv 1601.04660astro-ph.COastro-ph.GA
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与1.7 <z <3.3的低密度中性氢气相关的三重电离碳：积分N（HI）-N（CIV）关系

Triple-ionised carbon associated with the low-density neutral hydrogen gas at 1.7 < z < 3.3: the integrated N(HI)-N(CIV) relation

Tae-Sun Kim, R. F. Carswell, C. Mongardi, A. M. Partl, J. P. Muecket, P. Barai, S. Criatiani

备注：
Accepted for publication on MNRAS, 26 pages, 20 figures, 4 tables. On-line materials are found in the submitted civ.tar.gz file: complete Table 2, complete Table 3, complete Table 4, velocity plots civ1.pdf, civ2.pdf, civ3.pdf, civ4.pdf and civ5.pdf
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摘要：

通过对23个高质量UVES/VLT和HIRES/Keck类星体光谱中183个1.7 <z <3.3的CIV系统的Voigt轮廓拟合分析，我们发现大多数CIV系统（约75%）在HI和CIV的积分柱密度之间表现出良好的标度关系，红移演化可以忽略不计，当所有HI和CIV分量的柱密度在以CIV通量最小值为中心的给定（-150，+150）km/sec范围内积分时。综合CIV柱密度N在logN（HI，sys）= 14.0 - 15.5和logN（HI，sys）= 15.0时，CIV（sys）随N（HI，sys）的增加而增加（CIV，sys）= 11.8--14.0，然后在log N（HI，sys）> 16时变得几乎与N（HI，sys）无关，具有大的分散性：在logN（HI，sys）= 14--22时，logN（CIV，sys）= C1/（log（NHI，sys）+C2）+C3，C1 =-1.90 +0.55，C2 =-14.11 +0.19，C3 = 14.76 +0.17。陡峭（平坦）的部分主要是无SiIV（SiIV富集）的CIV系统。外推N（HI，sys）-N（CIV，sys）关系意味着log N（HI）<14的大多数吸收器实际上没有CIV。N（HI，sys）-N（CIV，sys）关系对于单个组分、团簇或小于+-100 km/sec的积分速度范围不成立。无论HI + CIV气体在IGM暗条中的位置如何，还是在中间的星系晕中，如果CIV的视线范围小于HI，并且在较大的碰撞参量下，N（CIV，sys）比N（HI，sys）下降得更快，则这是可以预期的。

英文摘要：

From the Voigt profile fitting analysis of 183 intervening CIV systems at 1.7 < z < 3.3 in 23 high-quality UVES/VLT and HIRES/Keck QSO spectra, we find that a majority of CIV systems (~75%) display a well-characterised scaling relation between integrated column densities of HI and CIV with a negligible redshift evolution, when column densities of all the HI and CIV components are integrated within a given (-150, +150) km/sec range centred at the CIV flux minimum. The integrated CIV column density N(CIV, sys) increases with N(HI, sys) at log N(HI, sys) = 14.0--15.5 and log N(CIV, sys) = 11.8--14.0, then becomes almost independent of N(HI, sys) at log N(HI, sys) > 16, with a large scatter: at log N(HI, sys) = 14--22, log N(CIV, sys) = C1 / (log(NHI, sys) + C2) + C3, with C1 = -1.90+0.55, C2 = -14.11+0.19 and C3 = 14.76+0.17, respectively. The steep (flat) part is dominated by SiIV-free (SiIV-enriched) CIV systems. Extrapolating the N(HI, sys)-N(CIV, sys) relation implies that most absorbers with log N(HI) < 14 are virtually CIV-free. The N(HI, sys)-N(CIV, sys) relation does not hold for individual components, clumps or the integration velocity range less than +-100 km/sec. It is expected if the line-of-sight extent of CIV is smaller than HI and N(CIV, sys) decreases more rapidly than N(HI, sys) at the larger impact parameter, regardless of the location of the HI+CIV gas in the IGM filaments or in the intervening galactic halos.

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