Variability selected low luminosity active galactic nuclei in the 4 Ms chandra deep field south

∆t p seconds where s = [0, ∞), and the index p denotes the time placement of the window measured in seconds from the beginning of the trial. For instance, in Fig. To determine whether

First, the sound horizon scale can be recov- ered from the non-linear angular correlation functions to a precision of ≤0.75 per cent applying the parametric fit described in the

Relationship between the total cluster stellar mass and the photometric blue fraction for the ALHAMBRA cluster and group sample stacked into different redshift bins. The galaxy

As a means to probe the possible fractal structure of the galaxy distribution we have studied the scaling of the num- ber density and angular correlation function of galaxies

The tentative spin and parity assignment to the observed levels in 44 S is based on the comparison between the calcu- lated and experimental (i) excitation energies, (ii)

The proposed strategy combines the active method to improve the vector control strategy in order to limit fault in current at low voltage dips and the passive method

The spectra of this galaxy was modelled with a narrow (second panel) and a secondary (third panel) kinematical components per emission line plus a broad component under Hα..

 The expansionary monetary policy measures have had a negative impact on net interest margins both via the reduction in interest rates and –less powerfully- the flattening of the