Volume 406, Number 1, July IV 2003
|Page(s)||65 - 73|
|Published online||17 November 2003|
Outflowing material in the = 4.92 BAL QSO SDSS J160501.21-011220.0 *
NCRA, Post Bag 3, Ganeshkhind, Pune 411 007, India e-mail: firstname.lastname@example.org
2 IUCAA, Post Bag 4, Ganeshkhind, Pune 411 007, India e-mail: email@example.com
3 Institut d'Astrophysique de Paris – CNRS, 98bis Boulevard Arago, 75014 Paris, France
4 LERMA, Observatoire de Paris, 61 rue de l'Observatoire, 75014 Paris, France e-mail: firstname.lastname@example.org
5 European Southern Observatory, Alonso de Córdova 3107, Casilla 19001, Vitacura, Santiago, Chile e-mail: email@example.com
Accepted: 6 May 2003
We present the analysis of broad absorption lines (BALs) seen in the spectrum of the zem 4.92 QSO SDSS J160501.21-011220.0. Our high spectral resolution UVES spectrum shows two well-detached absorption line systems at zabs = 4.685 and 4.855. The system at zabs = 4.855 covers the background source completely, suggesting that the gas is located outside the broad emission line region. On the contrary, the system at zabs = 4.685, which occults only the continuum source, has a covering factor of the order of 0.9. Physical conditions are investigated in the BAL system at zabs = 4.855 using detailed photoionization models. The observed H i absorption line together with the limits on C ii and Si ii absorptions suggest that 16 < log N(H i) (cm-2) < 17 in this system. Comparison with models show that the observed column densities of N v , Si iv and C iv in this system require that nitrogen is underabundant by more than a factor of 3 compared to silicon if the ionizing radiation is similar to a typical QSO spectrum. This is contrary to what is usually derived for the emission line gas in QSOs. We show that the relative suppression in the N v column density can be explained for Solar abundance ratios or abundance ratios typical of Starburst abundances if an ionizing spectrum devoid of X-rays is used instead. Thus, if the composition of BAL is like that of the emission line regions it is most likely that the cloud sees a spectrum devoid of X-rays similar to what we observe from this QSO. This is consistent with the fact that none of our models have high Compton optical depths to remove X-rays from the QSO. Similar arguments lead to the conclusion that the system at zabs = 4.685 as well is not Compton thick. Using simple Eddington arguments we show that the mass of the central black hole is ∼. This suggests that the accretion onto a seed black hole must have started as early as 11.
Key words: quasars: absorption lines / quasars: individual: SDSS J160501.21-011220.0
© ESO, 2003
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