We aim to place new, strengthened constraints on the luminosity function (LF) of H-alpha emitting galaxies at redshift z=2.2, and to further constrain the instantaneous star-formation rate density of the universe (rho*). We have used the new HAWK-I instrument at ESO-VLT to obtain extremely deep narrow-band (line; NB2090) and broad-band (continuum; Ks) imaging observations. The target field is in the GOODS-South, providing us with a rich multi-wavelength auxiliary data set, which we utilise for redshift confirmation and to estimate dust content. We use this new data to measure the faint-end slope (alpha) of LF(H-alpha) with unprecedented precision. The data are well fit by a Schechter function and also a single power-law, yielding alpha=(-1.72 +/- 0.20) and (-1.77 +/- 0.21), respectively. Thus we are able to confirm the steepening of alpha from low- to high-z predicted by a number of authors and observed at other wavelengths. We combine our LF data-points with those from a much shallower but wider survey at z=2.2 (Geach et al. 2008), constructing a LF spanning a factor of 50 in luminosity. Re-fitting the Schechter parameters, we obtain log L*=(43.07+/-0.22)erg s^-1 ; log phi*=(-3.45+/-0.52)Mpc^-3 ; alpha=(-1.60+/-0.15). We integrate over LF(Halpha) and apply a correction for dust attenuation to determine the instantaneous cosmic star-formation rate density at z=2 without assuming alpha or extrapolating it from lower-z. Our measurement of rho* is (0.215+/-0.090) Msun yr^-1 Mpc^-3, integrated over a range of 37 <log(LHhalpha / erg s^-1) < 47.
Precise weak lensing constraints from deep high-resolution $K_\mathrm{s}$ images: VLT/HAWK-I analysis of the super-massive galaxy cluster RCS2$J$232727.7$-$020437 at $z=0.70$
High Precision Analyses of Lyman alpha Damping Wing of Gamma-Ray Bursts in the Reionization Era: On the Controversial Results from GRB 130606A at z = 5.91
Swift GRB 130606 A在z = 5.91处的空前明亮的余辉给我们提供了一个通过高精度分析Ly α吸收的红阻尼翼来探测再电离时代的独特机会，但不同望远镜观测到的光谱对星系际介质（IGM）中中性氢分数（fHI）的限制是矛盾的。在这里，我们研究的起源，这种差异进行分析的频谱VLT与我们自己的分析代码以前用于适应斯巴鲁频谱。虽然VLT团队没有报告使用VLT光谱的IGM HI的证据，但我们证实了我们之前的结果，即更喜欢非零IGM HI（当IGM HI扩展到GRB红移时，最佳拟合f_HI ~ 0.06）。不含IGM HI的模型的VLT光谱拟合残差显示出与斯巴鲁光谱相同的系统趋势。我们认为，两个小组之间的差异可能是由于配件所采用的波长范围不同;我们的波长范围比VLT团队的更宽，而且我们避免了深Ly α吸收的最短波长范围（lambda_obs < 8426 A），因为这一区域主要由宿主星系中的HI控制，并且宿主星系HI速度分布的系统不确定性很大。我们还研究了这些结果的灵敏度，通过Ly α截面公式，从经典的洛伦兹函数到最近的一个考虑到完全量子力学散射。研究发现，对非零IGM HI的偏好对截面公式的选择是稳健的，但它在定量上是不可忽略的，因此在未来的分析中应该小心。
VLT/UVES observations of extremely strong intervening damped Lyman-alpha systems: Molecular hydrogen and excited carbon, oxygen and silicon at log N(HI)=22.4
VLT-SINFONI sub-kpc study of the star formation in local LIRGs and ULIRGs: Analysis of the global $Σ_{\rm SFR}$ structure and characterisation of individual star-forming clumps
A SINFONI Integral Field Spectroscopy Survey for Galaxy Counterparts to Damped Lyman-alpha Systems - II. Dynamical Properties of the Galaxies towards Q0302-223 and Q1009-0026
Spectroscopic confirmation of z~7 LBGs: probing the earliest galaxies and the epoch of reionization
我们在ESO/VLT上展示了FORS 2超深光谱活动的最终结果，以确认从我们的VLT/Hawk-I成像调查中选择的三个独立领域的z~7“z-波段脱落”候选者。我们特别报道了在NTT深场中新发现的两个红移约为6.7的星系：这两个星系都显示出Ly-alpha发射线，其静止坐标系EW为15-20 A量级，光度为2-4 X 10^{42} erg/s。我们还提出了一个样本的i-dropout星系的超深观测的结果，从中我们设置了一个坚实的上限的分数的闯入者。在观察到的20个z-dropout中，我们确认了5个星系在6.7 < z < 7.1。这系统地低于根据较低红移观测得出的预期：特别是有一个显着缺乏对象与中间Ly-alpha EW（20和55 A之间）。我们的结论是LBG中Ly-alpha发射的分数从z~3到z~6不断增加的趋势很可能从z~6到z~7反转。解释观测到的LAE分数在辍学人口与再电离之间的快速变化需要一个快速演变的中性部分的氢在宇宙中。假设宇宙在z=6时完全电离，并采用Dijkstra et al.（2011）的半解析模型，我们发现我们的数据要求中性氢分数在时间Δ z ~ 1内发生Δ chi_{HI} ~ 0.6量级的变化，前提是逃逸分数在相同的红移间隔内没有显著增加。
