Photoionization Modeling of a z=2 Multiple Cloud Weak MgII Absorber

Details Photoionization Modeling of a z=2 Multiple Cloud Weak MgII Absorber Photoionization Modeling of a z=2 Multiple Cloud Weak MgII Absorber

Dec 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aas...211.5402g&link_type=abstract

American Astronomical Society, AAS Meeting #211, #54.02; Bulletin of the American Astronomical Society, Vol. 39, p.823

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Scientific paper

Strong MgII absorbers are generally thought to be associated with luminous galaxies and their disks and halos. Weak MgII absorbers (Wr(2796)<0.3Ang)are more loosely associated with luminous galaxies, and may be produced in dwarf galaxy winds, tidal debris, spiral disk outskirts, high velocity clouds, and/or the cosmic web. Previous studies of multiple cloud weak MgII absorbers at z=1 find a range of metallicities ranging from 3 percent of the solar value up to substantially supersolar values. This suggests different mechanisms of origin.
Here we present constraints on the z=1.97 absorber seen in an archival VLT/UVES high resolution spectrum of the quasar Q0122-380. This system is unique in that it has very high quality coverage of many transitions, including Lyman-alpha, MgII, FeII, SiII, AlII, CII, AlIII, SiIII, SiIV, CIV, and NV. A two phase solution is needed to fit both the low ionization and high ionization transitions, and the lower density, high ionization phase includes clouds at velocities at which low ionization absorption is not detected. The entire system extends over more than 600km/s in velocity. The AlII absorption is overproduced by most photoionization models. This discrepancy may be reconciled either by using a supersolar metallicity or by reducing the abundance of aluminum relative to other elements. We present two families of models that reproduce the data, and discuss implications for the origin
of high redshift multiple cloud weak MgII absorbers.

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