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We have obtained low resolution (~20 Angstrom FWHM) slit spectra of 10 quasar candidates located within one degree of the z = 2.181 quasar Q0122-380 with the objective of searching for signs of large scale structure matching the intervening rich absorption complexes seen over the redshift range 1.81<z<1.97 toward this object. Of the 8 confirmed quasars, 4 turn out to have redshifts z < 1.8, placing them well in front of the redshift range of interest. Two of the three confirmed quasars at redshift z > 1.8 show no obvious absorption matching that of Q0122-380 at our spectral resolution and signal-to-noise ratio. The third object at a redshift of z = 1.868 displays strong z_{abs} sim z_{em} absorption systems at z = 1.84 and z = 1.86 and a possibly BAL-like trough at z = 1.76. If not intrinsic in nature, the former two systems could potentially be related to the absorption seen in Q0122-380, albeit over a distance of 50.2 arcmin (D_perp simeq 15 h^{-1} Mpc at z = 1.9).
In this paper we present near infrared (NIR) imaging data of the host galaxy of the broad absorption line quasar (BALQ) at z=2.169, serendipitously found close to 3C48. The data were obtained with the ESO-VLT camera ISAAC during period 67. We find ex
I report the discovery of blueshifted broad absorption line (BAL) troughs in at least six transitions of the Balmer series of hydrogen (Hbeta to H9) and in CaII, MgII and excited FeII in the quasar SDSS J125942.80+121312.6. This is only the fourth ac
Broad absorption lines (BALs) in quasar spectra identify high velocity outflows that likely exist in all quasars and could play a major role in feedback to galaxy evolution. Studying the variability in these BALs can help us understand the structure,
We present observations of 11 quasars, selected in the range z = 2.2-4.1, obtained with ESAs Superconducting Tunnel Junction (STJ) camera on the WHT. Using a single template quasar spectrum, we show that we can determine the redshifts of these object
CRTS J084133.15+200525.8 is an optically bright quasar at z=2.345 that has shown extreme spectral variability over the past decade. Photometrically, the source had a visual magnitude of V~17.3 between 2002 and 2008. Then, over the following five year