  We review a large body of literature for concentrations of halogens in
chondrites and stellar halogen data used for solar system abundances (i.e.,
representative abundances of the solar system at the time of its formation) and
associated analytical problems. Claims of lower solar system chlorine, bromine
and iodine abundances from recent analyses of CI-chondrites are untenable
because of incompatibility of such low values with nuclear abundance
systematics and measurements of halogens in the sun and other stars. We suspect
analytical problems associated with these peculiar rock types caused lower
analytical results in several studies. Mass concentrations in CI-chondrites are
F=92+-20 ppm, Cl=717+-110 ppm, Br=3.77+-0.90 ppm, and I=0.77+-0.31 ppm, and
abundances normalized to N(Si) =10^6 atoms are N(F)=1270+-270, N(Cl)=5290+-810,
N(Br)=12.3+-2.9, and N(I)=1.59+-0.64. Meteoritic values scaled to present-day
photospheric abundances with log N(H)=12 are A(F)=4.61+-0.09, A(Cl)=5.23+-0.06,
A(Br)=2.60+-0.09, and A(I)=1.71+-0.15. These recommended present-day solar
system abundances compare to the sunspot values of N(F)=776+-260,
A(F)=4.40+-0.25, and N(Cl)=5500+-810, A(Cl)=5.25+-0.12 and are consistent with
F and Cl abundance ratios in other stars and other astronomical environments.
The chlorine abundance of 776+-21 ppm by Yokoyama et al. (2022) for the
CI-chondrite-like asteroid Ryugu is consistent with the chlorine abundance
evaluated for CI-chondrites here. Updated equilibrium 50% condensation
temperatures from our previous work (Lodders 2003, Fegley & Schaefer 2010,
Fegley & Lodders 2018) considering solid-solution and kinetic inhibition
effects are 713K (F), 427K (Cl), 392K (Br) and 312K (I) at 10^-4 bar total
pressure. Condensation temperatures computed with lower halogen abundances do
not represent the correct condensation temperatures from a solar composition
gas. (abridged)
