Work on Catalogue Paper:

 

The figure 3 was suggested to be changed by referee so I have changed the fig3.a (top) color from cyan to black and the middle one to blue and cut the reference line zero from fig3.c (down)

(I use program in line  434 of "ref_fit_calibration.m"  located at  C:\Users\alireza\Work\Work In Progress\Research\P18 Re_fit_calibration. I used "AftbefPCA_sp52355_0574_016.eps" as fig 3)

I have answered one of the referees point as:

referee: >Similarly, since another component of this work is the advocacy of
>using the line dispersion over the FWHM, it would also be interesting
>to see if sigma_line(MgII) tracks sigma_line(Hbeta) better than
>FWHM(MgII) tracks FWHM(Hb) for the RM sample.

(Pat) TODO: make figure for inclusion and/or description in paper (these plots didn't help our argument)

(Ali): I should add this to answer to referee:
We have submitted another paper to MNRAS to address this point (the advocacy of using the line dispersion over the FWHM) and to distinguish potential biases caused due using FWHM(MgII). Since the subject is broader than just one paragraph or a section, we prefer not to adress it here.

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these are remin for tomorrow:

TODO:
Figure out how many of 126 partial-duplication quasars should be
added back to the catalog and add them back with correct DR3c flags.
No need to mention the issue to the referee.

 

 

TODO:
[As for demonstrating, you could plot a few objects where a noise spike
was fit in the bb case but the full line was recovered in the ab case.]

(Ali) I can add this in addition to what I have in the top of this page.

 

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