  Sirius-like systems are wide binaries composed of a white dwarf (WD) and a
companion of a spectral type earlier than M0. The WD progenitor evolves in
isolation, but its wind during the AGB phase pollutes the companion surface and
transfers some angular momentum. Within SHINE survey that uses SPHERE at the
VLT, we acquired images of HD2133, HD114174, and CD-567708 and combined this
data with high resolution spectra of the primaries, TESS, and literature data.
We performed accurate abundance analyses for the MS. We found brighter J and K
magnitudes for HD114174B than obtained previously and extended the photometry
down to 0.95 micron. Our new data indicate a higher temperature and then
shorter cooling age (5.57+/-0.02 Gyr) and larger mass (0.75+/-0.03 Mo) for this
WD than previously assumed. This solved the discrepancy previously found with
the age of the MS star. The two other WDs are less massive, indicating
progenitors of ~1.3 Mo and 1.5-1.8 Mo for HD2133B and CD-56 7708B,
respectively. We were able to derive constraints on the orbit for HD114174 and
CD-56 7708. The composition of the MS stars agrees fairly well with
expectations from pollution by the AGB progenitors of the WDs: HD2133A has a
small enrichment of n-capture elements, which is as expected for pollution by
an AGB star with a mass <1.5 Mo; CD-56 7708A is a previously unrecognized mild
Ba-star, which is expected due to pollution by an AGB star with a mass in the
range of 1.5-3.0 Mo; and HD114174 has a very moderate excess of n-capture
elements, which is in agreement with the expectation for a massive AGB star to
have a mass >3.0 Mo. On the other hand, none of these stars show the excesses
of C that are expected to go along with those of n-capture elements. This might
be related to the fact that these stars are at the edges of the mass range
where we expect nucleosynthesis related to thermal pulses.
