advertised article:

The Color-Magnitude Diagram in Baade's Window Revisited
M. Kiraga, B. Paczynski, Z.K. Stanek, 1997
ApJ 485, 611

An Upper Limit to the Age of the Galactic Bar
A.A. Cole, M.D. Weinberg, 2002
ApJ 574, L43-L46

Stellar populations in the Galactic bulge
E. Vanhollebeke, M. A. T. Groenewegen, L. Girardi, 2009
A&A 498, 95

comment on articles:

In my papers I, II and III it is noted that the stellar disc density is too high when modeled with an exponential function. It is likely better to replace the 'exp(-x)' distribution function with '0.5*sech(x)'. It is not necessary to adopt a sech^2(x) distribution function.

Mapping the stellar age of the Milky Way bulge with the VVV I. The method
F. Surot et al., 2019
A&A 623, A168
Interesting to see that after 25 years the age of 8-9 Gyr that was determined in paper III is still in good agreement with the new results.

advertised article:
The red tail of carbon stars in the LMC: Models meet 2MASS and DENIS observations [PDF]
P. Marigo, L. Girardi, C. Chiosi, 2003,
A&A 403, 225-237

advertised article:
Age determinations of main-sequence stars: combining different methods [PDF]
R. Lachaume, C. Dominik, T. Lanz, H.J. Habing, 1999
A&A 348, 897-909

advertised article:
The Sgr dSph hosts a metal-rich population [PDF]
P. Bonifacio, L. Sbordone, G. Marconi, L. Pasquini, and V. Hill, 2004,
A&A 414, 503-514 (astro-ph/0310872)

Carbon Stars in the Bulge - or Beyond It?
R. Wahlin, K. Eriksson, B. Gustafsson, N. Ryde, B. Westerlund, D.L. Lambert
in 'Why Galaxies Care About AGB Stars: Their Importance as Actors and Probes' F. Kerschbaum; C. Charbonnel, R.F. Wing (eds.), 2007
ASP Conference Series Vol 378, 410

Occam's razor states that one should proceed to simpler theories until simplicity can be traded for greater explanatory power. A simpler model can capture the underlying structure better and has a better predictive performance without the need for complicated stellar evolutionary models.

comment on article:
Carbon Stars in the Sagittarius Dwarf Galaxy
in 'The stellar content of Local Group galaxies' Patricia Whitelock and Russell Cannon (eds.)
Proceedings IAU Symposium 192, 136

"After the discovery of the SDG, Ng suggested that the C stars might be members of this galaxy rather than of the Bulge and he has since written several papers on the subject. In the most recent of the series Ng (1998) acknowledges that the Bulge C stars are indeed possibly in the Bulge, but suggests they were formed during the SDG's last passage through the Bulge."

This is a wrong interpretation of what I wrote in the Ng (1998) paper. I did not acknowledge that the Bulge C Stars are located in the Bulge! I wrote that the crossing of the SDG occurred 14.8 kpc behind the bulge.

"For this he requires the SDG be moving in the opposite direction to that suggested ...., i.e. away from, rather than towards, the Bulge"

I oversimplified the case to avoid a discussion about how the C-stars will be plunging back and forth to and through the disc after they have been formed. Actually the requirement of the SDG moving in an opposite direction is not necessary. I used it to demonstrate the star formation power of a recent disc crossing from the numerical simulations from Ibata & Razoumov (1998).
So I do need a recent crossing, it is not relevant in which direction the SDG is moving. It is important that the 'Bulge C-stars'are formed in a recent crossing. So the age of the C-stars is up to about 1 Gyr in agreement with Paper I and my suggestion still holds that the 'Bulge C-stars' are related, but not a member, of SDG.