Context. The 4-Dimensional Eigenvector 1 empirical formalism (4DE1) and its Main Sequence (MS) for quasars emerged as a powerful tool to organise the quasar diversity since several key observational measures and physical parameters are systematically changing along it. Aims. The trends of the 4DE1 are very well established to explain all the diversity seen in low-redshift quasar samples. Nevertheless, the situation is by far less clear when dealing with high-luminosity and high-redshift sources. We aim to evaluate the behaviour of our 22 high-redshift (2.2 ≤ z ≤ 3.7) and high-luminosity (47.39 ≤ L bol ≤ 48.36) quasars in the context of the 4DE1. Methods. Our approach involves studying quasar physics through spectroscopic exploration of UV and optical emission line diagnostics. We are using new observations from the ISAAC instrument at ESO-VLT and mainly from the SDSS to cover the optical and the UV rest-frames, respectively. Emission lines are characterised both through a quantitative parametrisation of the line profiles, and by decomposing the emission line profiles using multicomponent fitting routines. Results. We provide spectrophotometric properties and line profile measurements for Hβ+[O iii]λλ4959,5007, as well as for Si ivλ1397+O iv]λ1402, C ivλ1549+He iiλ1640, 1900 Å blend (including Al iiiλ1860, Si iii]λ1892, and C iii]λ1909). Six out of the 22 objects present a significant blueshifted component on the Hβ profile, and in 14/22 cases an Hβ outflowing component associated to [O iii] is detected. The majority of [O iii]λλ4959,5007 emission line profiles show blueshifted velocities larger than 250 km s −1 . We reveal extremely broad [O iii]λλ4959,5007 emission that is comparable to the width of Hβ broad profile in some highly accreting quasars. [O iii]λλ4959,5007 and C ivλ1549 blueshifts show very high amplitudes and a high degree of correlation. Line width and shift are correlated for both [O iii]λλ4959,5007 and C ivλ1549, suggesting that emission from outflowing gas is providing a substantial broadening to both lines. Otherwise, the links between C ivλ1549 centroid velocity at half intensity (c(1/2)), Eddington ratio (L/L Edd ), and bolometric luminosity are found to be in agreement with previous studies of high-luminosity quasars. Conclusions. Our analysis suggests that the behaviour of quasars of very high luminosity all along the main sequence is strongly affected by powerful outflows involving a broad range of spatial scales. The main sequence correlations remain valid at high redshift and high luminosity even if a systematic increase in line width is observed. Scaling laws based on UV Al iiiλ1860 and Hβ emission lines are equally reliable estimators of M BH .

Much effort has been done in order to better understand the active galactic nuclei mechanisms behind the relativistic jets observed in radio-loud sources. These phenomena are commonly seen in luminous objects with intermediate/high redshift such as quasars, so that the analysis of the spectroscopic properties of these sources may be a way to clarify this issue. Measurements are presented and contextualized taking advantage of the set of correlations associated with the quasar Main Sequence (MS), a parameter space that allows to connect observed properties to the relative relevance of radiative and gravitational forces. In the redshift range we consider, the low-ionization HI Balmer line Hβ is shifted into the near infrared. Here we present first results of a sample of 22 high-luminosity quasars with redshift between 1.4 and 3.8. Observations covering the Hβ spectral region were collected with the IR spectrometer ISAAC at ESO-VLT. Additional data were collected from SDSS in order to cover the UV region of our sources. The comparison between the strong C IV λ1549 high-ionization line and Hβ in terms of line widths and shifts with respect to the rest-frame leads to an evaluation of the role of radiative forces in driving an accretion disk wind. While for non-jetted quasars the wind properties have been extensively characterized as a function of luminosity and other physical parameters, the situation is by far less clear for jetted sources. The overarching issue is the effect of the relativistic jets on the wind, and on the structure of the emitting region in general. We present results from our analysis of the optical and UV line profiles aimed to identifying the wind contribution to the line emission.Resumo. Muito esforço vem sendo realizado para entender os mecanismos que envolvem os núcleos ativos de galáxias que estão por trás dos jatos relativisticos observados em objetos radio-loud. Esses fenômenos são normalmente detectados em galáxias luminosas de intermediário/alto redshift como os quasares, por exemplo. Uma maneira de clarificar esse comportamento é através da análise das propriedades espectroscópicas desses objetos. As medidas aqui apresentadas são contextualizadas com as correlações associadas à Main Sequence (MS) de quasares, um espaço de parâmetros que nos permite conectar propriedades observacionais com a relativa relevância das forças radiativas e gravitacionais. No intervalo de redshift que consideramos, a linha de Balmer de baixa ionização Hβ apresenta um shift para o infravermelho próximo. Neste trabalho, apresentamos os resultados iniciais de uma amostra de 22 quasares de alta luminosidade com redshift entre 1.4 e 3.8. As observações que compreendem o intervalo ótico foram coletadas a partir do espectrógrafo em infravermelho ISAAC do ESO-VLT. Dados adicionais para cubrir o intervalo em UV da amostra foram obtidos através do SDSS. A comparação entre a linha de alta ionização C IV λ1549 e Hβ em termos de largura e shifts das linhas com respeito ao rest-frame leva a uma avaliação do papel das forças...