@Article{RosaRodKraMilCar:2021:PhPrEv,
author = "Rosa, D. A. and Rodrigues, I. and Krabbe, A. C. and Milone,
Andr{\'e} de Castro and Carvalho, S.",
affiliation = "{Universidade do Vale do Para{\'{\i}}ba (UNIVAP)} and
{Universidade do Vale do Para{\'{\i}}ba (UNIVAP)} and
{Universidade do Vale do Para{\'{\i}}ba (UNIVAP)} and {Instituto
Nacional de Pesquisas Espaciais (INPE)} and {Universidade do Vale
do Para{\'{\i}}ba (UNIVAP)}",
title = "The physical properties and evolution of the interacting system AM
1204-292",
journal = "Monthly Notices of the Royal Astronomical Society",
year = "2021",
volume = "501",
number = "3",
pages = "3750--3766",
month = "Mar.",
abstract = "We investigate interaction effects in the stellar and gas
kinematics, stellar population, and ionized gas properties of the
interacting galaxy pair AM 1204-292,composed of NGC 4105 and NGC
4106. The data consist of long-slit spectra in the range 3000-7050
Å. The massive E3 galaxy NGC 4105 presents a flat stellar velocity
profile, while the ionized gas is in strong rotation, suggesting
an external origin. Its companion, NGC 4106, shows asymmetries in
the radial velocity field, likely due to the interaction. The
dynamics of the interacting pair were modelled using the P-Gadget3
treepm/sph code, from which we show that the system has just
passed the first perigalacticum, which triggered an outbreak of
star formation, currently at full maximum. We characterized the
stellar population properties using the stellar population
synthesis code starlight and, on average, both galaxies are
predominantly composed of old stellar populations. NGC 4105 has a
slightly negative age gradient, comparable with that of the most
massive elliptical galaxies, but a steeper metallicity gradient.
The SB0 galaxy NGC 4106 presents smaller radial variations in both
age and metallicity in comparison with intermediate-mass
early-type galaxies. These gradients have not been disturbed by
interaction, since the star formation happened very recently and
was not extensive in mass. Electron density estimates for the pair
are systematically higher than those obtained in isolated
galaxies. The central O/H abundances were obtained from
photoionization models in combination with emission-line ratios,
which resulted in 12 + log(O/H) = 9.03 ± 0.02 and 12 + log(O/H) =
8.69 ± 0.05 for NGC 4105 and NGC 4106, respectively.",
doi = "10.1093/mnras/staa3850",
url = "http://dx.doi.org/10.1093/mnras/staa3850",
issn = "0035-8711 and 1365-2966",
language = "en",
targetfile = "rosa_physical.pdf",
urlaccessdate = "20 maio 2024"
}