Clues to the Physical Origin of Weak MgII Absorption Systems

Details Clues to the Physical Origin of Weak MgII Absorption Systems Clues to the Physical Origin of Weak MgII Absorption Systems

Dec 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999aas...195.5703r&link_type=abstract

American Astronomical Society, 195th AAS Meeting, #57.03; Bulletin of the American Astronomical Society, Vol. 31, p.1459

Astronomy and Astrophysics

Astronomy

Scientific paper

Much has been learned about the chemical and ionization conditions of the weak MgII (EWr <0.3 { Angstroms}) intervening absorption systems found in quasar spectra. At z 1, weak MgII systems are twice as common as the strong MgII systems known to be associated with normal galaxies, but seem not to be directly associated with bright (L*) galaxies (Churchill et al., 1999, ApJS, 120, 51.) Most do not show Lyman limit breaks, which requires N(HI)<16.8 cm-2 (Churchill et al., 1999, ApJ, submitted.) Their metallicities are greater than 3 to 10% of Solar. Single-cloud weak MgII systems outnumber double-cloud systems by at least 4:1. This requires a covering factor less than 0.2, so that lines of sight, on average, encounter only one absorber. Most weak systems contain at least two phases of gas: a high-ionization component with Doppler parameter b 50 km/s, and a low-ionization component with 2

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