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.^[1]

IRAS 05189-2524 is classified as an ultraluminous infrared galaxy (ULIRG),^[2] which is formed by two interacting gas-rich spiral galaxies that merged together.^[3] 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.^[4]

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−1^[5] 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.^[6] The galaxy has a power output above 10 times that of our sun,^[7] emitting a tremendous amount of light at infrared wavelengths.^[4]

Moreover, IRAS 05189-2524 is classified an optical Seyfert 2 galaxy,^[6][8] presenting a hidden broadline region.^[9] A study noticed there is ∼70% percent of the bolometric luminosity attributed to its active galactic nucleus,^[10] thus making it a quasar. It is represented by its dust enshrouded stage^[11] which is shed overtime by the nuclei.^[11] There is a sign of high-velocity large-scale outflows detached in neutral, ionized and molecular gas phrases.^[12]

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.^[6] 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.^[13]

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 to Galactic.^[14] 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 A_V is compatible with the broad component of Нα seen in transmission.^[14]

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−1. 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.^[15]