标题： 一个SINFONI积分场光谱探测星系与富线氢吸收系统的对应关系 - I. 新的探测和对穿越与关联吸收体的限制 显示英文标题

标题： A SINFONI Integral Field Spectroscopy Survey for Galaxy Counterparts to Damped Lyman-alpha Systems - I. New Detections and Limits for Intervening and Associated Absorbers

摘要： 对被背景类星体光谱吸收所探测到的富线族（DLA）和次富线族（sub-DLA）星系的研究依赖于用更传统的方法识别导致吸收现象的星系。积分场光谱提供了一种高效检测亮类星体附近暗弱星系的方法，并且可以立即确认红移。在这里，我们报告了从6个目标类星体吸收体样本中检测到的一个DLA和一个sub-DLA星系发出的Hα发射线。我们推导出对于z_abs=1.009的DLA，在类星体Q0302-223方向上b=25 kpc处F(Hα)=7.7±2.7×10^-17 erg/s/cm² (SFR=1.8±0.6 M_sun/yr)，而对于z_abs=0.887的sub-DLA，在类星体Q1009-0026方向上b=39 kpc处F(Hα)=17.1±6.0×10^-17 erg/s/cm² (SFR=2.9±1.0 M_sun/yr)。这些结果与文献中之前报道的类星体吸收体低恒星形成率一致。我们利用NII 6585/Hα比值来推导HII发射金属丰度，并将其与从高分辨率光谱中得出的中性气体HI吸收金属丰度进行比较。在一种情况下，发现吸收金属丰度实际上高于发射线金属丰度。对于其余对象，我们达到了约F(Hα)~10^-17 erg/s/cm²的3σ限制流量（对应于z~1时SFR~0.1 M_sun/yr和z~2时SFR~1 M_sun/yr），即地面观测所能达到的最低值之一。我们还介绍了两个与C IV系统相关的、偶然在我们的数据中发现的其他星系。 显示英文摘要

摘要： Detailed studies of Damped and sub-Damped Lyman-alpha systems (DLA), the galaxies probed by the absorption they produce in the spectra of background quasars, rely on identifying the galaxy responsible for the absorber with more traditional methods. Integral field spectroscopy provides an efficient way of detecting faint galaxies near bright quasars, further providing immediate redshift confirmation. Here, we report the detection of H-alpha emission from a DLA and a sub-DLA galaxy among a sample of 6 intervening quasar absorbers targeted. We derive F(H-alpha)=7.7+/-2.7*10^-17 erg/s/cm^2 (SFR=1.8+/-0.6 M_sun/yr) at impact parameter b=25 kpc towards quasar Q0302-223 for the DLA at z_abs=1.009 and F(H-alpha)=17.1+/-6.0*10^-17 erg/s/cm^2 (SFR=2.9+/-1.0 M_sun/yr) at b=39 kpc towards Q1009-0026 for the sub-DLA at z_abs=0.887. These results are in line with low star formation rates previously reported in the literature for quasar absorbers. We use the NII 6585/H-alpha ratio to derive the HII emission metallicities and compare them with the neutral gas H I absorption metallicities derived from high-resolution spectra. In one case, the absorption metallicity is actually found to be higher than the emission line metallicity. For the remaining objects, we achieve 3-sigma limiting fluxes of the order F(H-alpha)~10^-17 erg/s/cm^2 (corresponding to SFR~ 0.1 M_sun/yr at z~1 and ~1 M_sun/yr at z~2), i.e. among the lowest that have been possible with ground-based observations. We also present two other galaxies associated with C IV systems and serendipitously discovered in our data.