IRAS 10565+2448
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| IRAS 10565+2448 | |
|---|---|
.jpg) HST image of IRAS 10565+2448 | |
| Observation data (J2000 epoch) | |
| Constellation | Leo |
| Right ascension | 10h 59m 18.13s |
| Declination | +24° 32′ 34.54″ |
| Redshift | 0.043100 |
| Heliocentric radial velocity | 12,921 km/s |
| Distance | 625 Mly (191.62 Mpc) |
| Apparent magnitude (B) | 15.7 |
| Characteristics | |
| Type | LINER; ULIRG, HII |
| Apparent size (V) | 0.4' x 0.3' |
| Notable features | luminous infrared galaxy |
| Other designations | |
| IRAS F10565+2448, 2XMM J105918.1+243234, PGC 33083, NVSS J105918+243235, LEDA 1709876 | |
IRAS 10565+2448 known as IRAS F10565+2448, is a galaxy merger located in the constellation of Leo. It is located at a distance of 625 million light years from Earth. It is classified as an ultraluminous infrared galaxy[1] with an infrared luminosity of 1.2×1012 LΘ. It has a star formation rate of 131.8 MΘ yr−1.[2]
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.[3] A third galaxy is possibly shown as secondary smaller nucleus located northwest from the primary nucleus in the large galaxy.[4] 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.[5] It has an obscured X-ray emission with a luminosity of both LSX = 1.21×1041 erg s−1 and LHX = 1.6×1041 erg s−1. The source appears as Compton-thin obscurer with an absorption column density of 0.05+0.07
−0.04×1022 cm−2.[6]
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.[4] It is more luminous when compared to its smaller companion galaxy.[7] It contains a superficial and broad blueshifted HI absorption interpreted as molecular outflows with a mass rate of 140 MΘ yr−1 suggesting it is driven by a radio jet.[2] The large galaxy also shows detections of dust continuum, J = 4-3 ground rotational transition of carbon monoxide (CO) and atomic carbon.[8] It has a compact radio source appearing structured at 8.44 GHz[9] with a rotating CO ring found nearly-face on but lesser inside an outer disk beyond the galaxy's nuclear ring.[10]
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−1 and systematic velocity.[11]
