  Tidal interactions between galaxies often give rise to tidal tails, which can
harbor concentrations of stars and interstellar gas resembling dwarf galaxies.
Some of these tidal dwarf galaxies (TDGs) have the potential to detach from
their parent galaxies and become independent entities, but their long-term
survival is uncertain. In this study, we conducted a search for detached TDGs
associated with a sample of 39 interacting galaxy pairs in the local Universe
using infrared, ultraviolet, and optical images. We employed IR colors and
UV/optical/IR spectral energy distributions to identify potential interlopers,
such as foreground stars or background quasars. Through spectroscopic
observations using the Boller and Chivens spectrograph at San Pedro M\'artir
Observatory, we confirmed that six candidate TDGs are at the same redshift as
their putative parent galaxy pairs. We identified and measured emission lines
in the optical spectra and calculated nebular oxygen abundances, which range
from log(O/H) = 8.10 $\pm$ 0.01 to 8.51 $\pm$ 0.02. We have serendipitously
discovered an additional detached TDG candidate in Arp72 using available
spectra from SDSS. Utilizing the photometric data and the CIGALE code for
stellar population and dust emission fitting, we derived the stellar masses,
stellar population ages, and stellar metallicities for these detached TDGs.
Compared to standard mass-metallicity relations for dwarf galaxies, five of the
seven candidates have higher than expected metallicities, confirming their
tidal origins. One of the seven candidates remains unclear due to large
uncertainties in metallicity, and another has stellar and nebular metallicities
compatible with those of a preexisting dwarf galaxy. The latter object is
relatively compact in the optical relative to its stellar mass, in contrast to
the other candidate TDGs [abridged].
