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arXiv · 1001.2311

MgII absorption systems with W_0 > 0.1 Åfor a radio selected sample of 77 QSOs and their associated magnetic fields at high redshifts

M. L. Bernet·F. Miniati·S. J. Lilly
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Abstract

We present a catalogue of MgII absorption systems obtained from high resolution UVES/VLT data of 77 QSOs in the redshift range 0.6 < z < 2.0, and down to an equivalent width W_0 > 0.1 Å. The statistical properties of our sample are found to be in agreement with those from previous work in the literature. However, we point out that the previously observed increase with redshift of dN/dz for weak absorbers, pertains exclusively to very weak absorbers with W_0 < 0.1 Å. Instead, dN/dz for absorbers with W_0 in the range 0.1-0.3 Åactually decreases with redshift, similarly to the case of strong absorbers. We then use this catalogue to extend our earlier analysis of the links between the Faraday Rotation Measure of the quasars and the presence of intervening MgII absorbing systems in their spectra. In contrast to the case with strong MgII absorption systems W_0 > 0.3 Å, the weaker systems do not contribute significantly to the observed Rotation Measure of the background quasars. This is possibly due to the higher impact parameters of the weak systems compared to strong ones, suggesting that the high column density magnetized material that is responsible for the Faraday Rotation is located within about 50 kpc of the galaxies. Finally, we show that this result also rules out the possibility that some unexpected secondary correlation between the quasar redshift and its intrinsic Rotation Measure is responsible for the association of high Rotation Measure and strong intervening MgII absorption that we have presented elsewhere, since this would have produced an equal effect for the weak absorption line systems, which exhibit a very similar distribution of quasar redshifts.

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M. L. Bernet, F. Miniati, S. J. Lilly. 2010-01-13. MgII absorption systems with W_0 > 0.1 Åfor a radio selected sample of 77 QSOs and their associated magnetic fields at high redshifts. https://doi.org/10.1088/0004-637x%2F711%2F1%2F380

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