IRAS 05189-2524: Difference between revisions
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Revision as of 07:31, 8 May 2024
| 2MASX J05210136-2521450 | |
|---|---|
 Hubble image of 2MASX J05210136-2521450 | |
| Observation data | |
| Constellation | Lepus |
| Right ascension | 05h 21m 01.392s |
| Declination | -25d 21m 45.36s |
| Redshift | 0.042750 |
| Heliocentric radial velocity | 12,816 Km/s |
| Distance | 603 Mly (185 Mpc) |
| Apparent magnitude (V) | 15.4 |
| Characteristics | |
| Type | Pec; ULIRG, Sy2 |
| Size | 75,000 ly |
| Apparent size (V) | 0.46 x 0.44 arcmin |
| Notable features | Galaxy merger, luminous infrared galaxy |
| Other designations | |
| PGC 17155, 2MASS J05210139-2521452, IRAS 05189-2524, AKARI J0521013-252146, MRSS 486-006230, NVSS J052101-252145, 1WGA J0521.0-2521, SWIFT J0521.0-2522, LEDA 17155 | |
2MASX J05210136-2521450 is a type E[1] elliptical galaxy 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 thousand light-years.[2]
A luminous galaxy
2MASX J05210136-2521450 is classified as an ultraluminous infrared galaxy.[3] which is caused by the end product of two interacting gas-rich spiral galaxies that merged together.[4] It has a power output above 10 times that of our sun,[5] in which emits a tremendous amount of light at infrared wavelengths.[6] Not to mention, it is characterized by large dust masses and vigorous star formation activity[4] which was caused by the collision between the galaxies[6] and also the accretion activity around its supermassive black hole, which radiation is produced that heats up dust.[7]
It is proposed that 2MASX J05210136-2521450 represents the dust-enshrouded stages of a quasar.[8] Once the nuclei shed the obscuring dust, it allows the active galactic nucleus to dominate the decaying starburst, to become an optically selected quasar.[8]
Moreover, the merging process left its signs; 2MASX J05210136-2521450 presents a single bright nucleus and an outer structure consisting one-sided extension of the inner arms, with its tidal tail heading towards the opposite direction which was formed through material ripped from the galaxies by gravitational forces.[6] Possibly, the merger could strip the galaxies of both star-forming gas which could hint the signs of no new stars forming anytime.[9]
References
- ^ "HyperLeda -object description". atlas.obs-hp.fr. Retrieved 2024-05-08.
- ^ "Your NED Search Results". ned.ipac.caltech.edu. Retrieved 2024-05-08.
- ^ Sanders, D. B.; Surace, J. A.; Ishida, C. M. (1999). Barnes, J. E.; Sanders, D. B. (eds.). "Ultraluminous Infrared Galaxies". Galaxy Interactions at Low and High Redshift. Dordrecht: Springer Netherlands: 289–294. doi:10.1007/978-94-011-4665-4_73. ISBN 978-94-011-4665-4.
- ^ a b Nandi, S; Das, M; Dwarakanath, K S. "Tracing the evolution of ultraluminous infrared galaxies into radio galaxies with low frequency radio observations". academic.oup.com. Retrieved 2024-05-08.
- ^ Murphy, Thomas Williams (2000). Ultraluminous Infrared Galaxies: Power Sources and Ages Along the Merger Sequence (phd thesis). California Institute of Technology.
- ^ a b c information@eso.org. "A tale of galactic collisions". www.spacetelescope.org. Retrieved 2024-05-08.
- ^ "Are Ultra-Luminous Galaxies Colliding? | Center for Astrophysics | Harvard & Smithsonian". www.cfa.harvard.edu. Retrieved 2024-05-08.
- ^ a b Sanders, D. B.; Soifer, B. T.; Elias, J. H.; Madore, B. F.; Matthews, K.; Neugebauer, G.; Scoville, N. Z. (1988-02-01). "Ultraluminous Infrared Galaxies and the Origin of Quasars". The Astrophysical Journal. 325: 74. doi:10.1086/165983. ISSN 0004-637X.
- ^ published, Robert Lea (2022-09-06). "Violent mergers might be robbing galaxies of their star-birthing material". Space.com. Retrieved 2024-05-08.