IRAS 05189-2524

IRAS 05189-2524 is a galaxy merger located in the constellation Lepus. It is located 603 million light-years away from the Solar System and has an approximate diameter of 75,000 light-years.

A luminous galaxy
IRAS 05189-2524 is classified as an ultraluminous infrared galaxy (ULIRG), which is formed by two interacting gas-rich spiral galaxies that merged together. Signs left by merging process, included a single bright nucleus and an outer structure consisting one-sided extension of the inner arms, with its tidal tail formed by material ripped from the galaxies by gravitational forces.

IRAS 05189-2524 is one of the brightest local ULIRG in X-ray with a E = 2–10 keV continuum luminosity of ~1043 erg/s This tend to vary overtime in which the E = 0.5–2 keV was relatively constant during the 2001-2002 observation done by XMM Newton and Chandra. But in 2006 study done by Suzaku shows it was a factor of ~30 lower. The galaxy has a power output above 10 times that of our sun, emitting a tremendous amount of light at infrared wavelengths.

Moreover, IRAS 05189-2524 is classified an optical Seyfert 2 galaxy, presenting a hidden broadline region. A study noticed there is ~70% percent of the bolometric luminosity attributed to its active galactic nucleus, thus making it a quasar. It is represented by its dust enshrouded stage which is shed overtime by the nuclei. There is a sign of high-velocity large-scale outflows detached in neutral, ionized and molecular gas phrases.

An observation by XMM Newton and NuSTAR, shows evidence for a blueshifted Fe K absorption feature at E = 7.8 KeV which indicates there is an ultrafast outflow (UFO) with vout = 0.11 ± 0.01c. A relative disk reflection in the broadband X-ray spectrum, shows a highly asymmetric board Fe Kα emission line that extends down to 3 KeV with a Compton scattering component above 10 KeV.

Further studies shows there is a new, quasi-luminous hard X-ray and near-IR spectra in IRAS 05189-2524. The Seyfert nucleus is Compton-thin and the near-IR board lines are seen in transmission, similar to X-rays and the medium has an Aṿ/ɴH ratio that is lower than Galactic. Also, the increase in obscuration at latter approach shows less △Aṿ/△Nн compared to Galactic, thus supporting a correlation between the proximity to the center and properties of obscuring matter. Most of the observed polarization is due to dichroism given the fact, the measured AV is compatible with the broad component of Нα seen in transmission.

There are Na i D emission in the system traces dusty filaments on the near side of an extended active galactic nucleus in IRAS 05189-2524 which has projected velocities up to 2000 km/s. These filaments simultaneously obscure the stellar continuum, serving as complementary probe of the wind, in which they are the strongest in regions of low foreground obscuration.