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首页> 外文期刊>The Astrophysical journal >A NEW H I 21 CENTIMETER ABSORBER ASSOCIATED WITH THE H I DEFICIENT INTERACTING GALAXIES G0248+430
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A NEW H I 21 CENTIMETER ABSORBER ASSOCIATED WITH THE H I DEFICIENT INTERACTING GALAXIES G0248+430

机译：与H I交互相互作用星系G0248 + 430关联的H I 21计时器

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摘要

We present high-resolution (～2") H I 21 cm and CO(1-0) observations of the quasar (QSO) galaxy pair 0248+430. The QSO Q0248+430 (z_(em) = 1.313) has been found to show two metal absorption-line systems at redshifts z_a ～ 0.052, which are consistent with the redshift of a foreground luminous infrared galaxy 15" (～11 h~(-1) kpc) away. In our observations, the CO emission of this foreground galaxy, G0248+430, shows broad velocity distribution (～173 km s~(-1)) but is spatially confined to a small unresolved region less than 1.5 x 1.5 h~(-1) kpc; the H_2 mass based on the traditional conversion factor is ≈ 10~(10) solar mass, which is approximately 30 times the H_2 mass within a similar region of the Milky Way. On the other hand, no significant H I 21 cm emission is found in the foreground galaxy; the mass of the neutral atomic hydrogen is less than 6 x 10~8 solar mass. Toward the QSO we discover a new H I 21 cm absorber with ∫ τ dv ～0.26 km s~(-1) at the redshift of one of the metal absorption components; however, we did not detect significant CO(1 -0) absorption toward the QSO. The H I column density is large enough for the absorber to be classified as a damped Lyα system. We also derive the H I mass and spin temperature for this metal-line absorption system. We discuss the relation of this H I absorber and the depletion of the H I in the foreground galaxy. We find that this H I absorber has very high metal abundance and is intrinsically different from the normal damped Lyα absorption systems, although both have similar spin temperatures and hydrogen column densities.
机译：我们提出了类星体（QSO）对0248 + 430的高分辨率（〜2“）HI 21 cm和CO（1-0）观测结果。发现QSO Q0248 + 430（z_（em）= 1.313）显示了两个金属吸收线系统，其红移z_a〜0.052，与前景发光红外星系15“（〜11 h〜（-1）kpc）以外的红移一致。在我们的观测中，该前景星系G0248 + 430的CO发射显示出较宽的速度分布（〜173 km s〜（-1）），但在空间上被限制在一个小于1.5 x 1.5 h〜（-1）的小未解析区域）kpc;基于传统转换因子的H_2质量约为≈10〜（10）太阳质量，约为银河系类似区域内H_2质量的30倍。另一方面，在前景星系中没有发现显着的H I 21 cm发射。中性原子氢的质量小于6 x 10〜8太阳质量。朝向QSO，我们发现了一种新的H I 21 cm吸收器，其中一种金属吸收组分的红移处∫τdv〜0.26 km s〜（-1）。但是，我们没有检测到明显的CO（1 -0）对QSO的吸收。 H I柱密度足够大，可以将吸收器归类为阻尼Lyα系统。我们还导出了该金属线吸收系统的H I质量和自旋温度。我们讨论了这个H I吸收体与前景星系中H I耗竭之间的关系。我们发现这种H I吸收剂具有很高的金属丰度，并且与正常的阻尼Lyα吸收体系本质上不同，尽管两者的旋转温度和氢柱密度都相似。

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