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IRAS 10565+2448 has a disturbed morphology. The large galaxy in the system shows dust lanes running through its main body while the smaller galaxy (the westernmost object), has a curved tidal tail pulled downwards from the object. A third galaxy is possibly shown as secondary smaller nucleus located northwest from the primary nucleus in the large galaxy. It is also a late-stage merger as both east and west nuclei components in the system have a projected separation of 6.7 kiloparsecs. It has an obscured X-ray emission with a luminosity of both LSX = 1.21 x 10 erg s and LHX = 1.6 x 10 erg s. The source appears as Compton-thin obscurer with an absorption column density of 0.05-0.04 x 10 cm.
The large galaxy in the IRAS 10565+2448 is found to be active. It is categorized as a H II galaxy and a starburst galaxy. It is more luminous when compared to its smaller companion galaxy. It contains a superficial and broad blueshifted HI absorption interpreted as molecular outflows with a mass rate of 140 MΘ yr suggesting it is driven by a radio jet. The large galaxy also shows detections of dust continuum, J = 4-3 ground rotational transition of carbon monoxide (CO) and atomic carbon. It has a compact radio source appearing structured at 8.44 GHz with a rotating CO ring found nearly-face on but lesser inside an outer disk beyond the galaxy's nuclear ring.
The smaller galaxy contains a source of CO(1–0) emission. It has blue and redshifted CO(1–0) wings with an approximate size of 2.15 ± 0.32 kiloparsecs and 2.22 ± 0.30 kiloparsecs based on a circular Gaussian fit. However, the emission from the CO(1–0) narrow core is more condensed than its wings. There is also proof of a plume of CO(1–0) stretching southwest at blueshifted velocities of -150 km and systematic velocity.
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HST image of IRAS 10565+2448
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