Reference : The use of gravitational microlensing to scan the structure of BAL QSOs
Scientific journals : Article
Physical, chemical, mathematical & earth Sciences : Space science, astronomy & astrophysics
http://hdl.handle.net/2268/6560
The use of gravitational microlensing to scan the structure of BAL QSOs
English
Hutsemekers, Damien mailto [Université de Liège - ULg > Département d'astrophys., géophysique et océanographie (AGO) > Astroph. extragalactique et observations spatiales (AEOS) >]
Surdej, Jean mailto [Université de Liège - ULg > Département d'astrophys., géophysique et océanographie (AGO) > Astroph. extragalactique et observations spatiales (AEOS) >]
van Drom, E. [Univ. de Liege, Liege, Belgium]
1-Jun-1994
Astrophysics & Space Science
Springer Science & Business Media B.V.
216
361-365
Yes (verified by ORBi)
International
0004-640X
Dordrecht
The Netherlands
[en] ABSORPTION SPECTRA ; ASTRONOMICAL SPECTROSCOPY ; GAS FLOW ; GRAVITATIONAL LENSES ; INTERSTELLAR GAS ; LINE SPECTRA ; QUASARS ; STELLAR GRAVITATION ; STELLAR MODELS ; STELLAR SPECTRA ; CARBON ; MAGNETOHYDRODYNAMIC FLOW ; PLASMA JETS ; SILICON ; STELLAR WINDS
[en] Approximately 10% of the quasi-stellar objects (QSOs) show broad absorption lines (BAL) in their spectra which, if interpreted in terms of Doppler velocities, reveal the presence of high velocity gas outflows. One of these BAL QSOs is known to be gravitationally lensed. It therefore constitutes a good candidate to search for microlensing effects, i.e., the selective amplification of different line forming regions. Considering current models for the BAL region, we have investigated the effects of moving microlenses on the line profiles, and we conclude that these effects strongly depend on the adopted model. A regular spectroscopic monitoring of lensed BAL QSOs would therefore be highly valuable to distinguish between the various models proposed so far to interpret the origin of broad absorption lines.
http://hdl.handle.net/2268/6560
10.1007/BF00982519
http://adsabs.harvard.edu/abs/1994Ap%26SS.216..361H

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