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Old 13-April-2008, 04:43 AM
William William is online now
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Join Date: Jun 2007
Posts: 580
Default PHL 1811, Quasar Clustering, Binaries, Lack of Quasar Metallicity Evolution

In reply to parejkoj:

The papers I linked to above are recent quasar observations and recent confirmation of observational conclusions. I would assume that as these observations are presented and discussed at recent symposiums as puzzles, that you cannot explain the observations.

I am thinking of quasars as a puzzle that was not been solved, hence, I am interested in recent quasar observations and research. I am interested in the physics and observational data concerning the MECO hypothesis that asserts that BH can theoretically have hair and that there is observational data that supports that BH do have a strong intrinsic magnetic field.

As I said, I am also interested in Bell's observations and analysis. I believe by your comment that you are not interested in Bell's observations and analysis. I would assume, if Bell's and the MECO line of logic was correct, that additional observational data would either disprove or confirm that logic train.

Do you have any thoughts concerning the recent confirmation of quasar clustering or the discovery of quasar binaries?

Lack of quasar metallicity evolution with redshift? Super solar metallicity of high z quasars?

Quasar associated dust?

Lack of time dilation for high z quasars?

Quasar evolution of luminosity with redshift? Quasar space density evolution with redshift?

Explanation as to why there are no quasars at z=0?

PHL 1811 seems to have other unusual spectral features. This is another paper on PHL 1811.

"PHL 1811: The Local Prototype of the Lineless High-z SDSS QSOs" by Karen Leighly et al.

http://arxiv.org/abs/0705.0940v1

Quote:
HST STIS spectra of PHL 1811 reveal a very blue continuum with little evidence for absorption or scattering intrinsic to the quasar. High ionization lines are very weak; C IV has an equivalent width of only 5°A. Neither forbidden nor semiforbidden emission lines are detected. Fe II is the dominant line emission in the UV. High metallicity is implied by the large Fe II to Mg II ratio and relatively strong N V. Low-ionization emission lines of Al III, Na I D, and Ca II H & K are present, implying high optical depth.
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