2MASX J22550681+0058396
| 2MASX J22550681+0058396 | |
|---|---|
.jpg) Hubble Space Telescope image of 2MASX J22550681+0058396 (located right) | |
| Observation data (J2000 epoch) | |
| Constellation | Pisces |
| Right ascension | 22h 55m 06.80s |
| Declination | +00° 58′ 40.10″ |
| Redshift | 0.053301 |
| Helio radial velocity | 15,979 km/s |
| Distance | 733 Mly (224.7 Mpc) |
| Apparent magnitude (V) | 15.7 |
| Characteristics | |
| Type | E-S0, S0, LINER |
| Size | 95,000 ly |
| Apparent size (V) | 0.50 x 0.39 arcmin |
| Other designations | |
| SDSS J225506.72+005839.9, PGC 1180817, ASK 024736.0, 2MASS J22550679+0058401, NSA 005287, MaNGA 01-028337, 2CXO J225506.8+005839, NPM1G +00.0615, SSTSL J225506.80+005840.4, LEDA 1180817 | |
2MASX J22550681+0058396 or known as PGC 1180817, is a type E-S0[1] lenticular galaxy located in constellation Pisces. It is located 733 million light-years from the Solar System and has an approximate diameter of 95,000 light-years.[2]
Characteristics[edit]
2MASX J22550681+0058396 has an active galactic nucleus (AGN). It is a LINER galaxy[2][3] whose nucleus presents an emission spectrum characterized by broad lines of weak ion atoms.[2] This is an interesting object since not only it represents the most numerous active galactic nuclei population but the link between normal and active galaxies suggested by low-X-ray luminosity.[4]
Moreover, 2MASX J22550681+0058396 is a post-starburst galaxy[5] which is caused by end product of galaxies that have merged within the past billion years.[6][7] The merger event had caused the gas to drive up to the center and created an abundance of new stars, of which the brightest are visible in the remanent galaxy's core.[6] This might be due to burst duration increasing with stellar mass, from 120 to 250 Myr, indicating there is enough molecular gas available in close pairs to fuel the burst.[8]
Visible shells and tails surrounding 2MASX J22550681+0058396, are also caused[6] in which the shells are formed through radial merger events while tails are remnants of circular merger infall, suggesting that the orbital angular momentum plays a more crucial role in transforming the host galaxy as expected.[9]
References[edit]
- ↑ "HyperLeda -object description". atlas.obs-hp.fr. Retrieved 2024-05-08.
- ↑ 2.0 2.1 2.2 "Your NED Search Results". ned.ipac.caltech.edu. Retrieved 2024-05-08.
- ↑ Coldwell, Georgina V.; Alonso, Sol; Duplancic, Fernanda; Mesa, Valeria (2018-05-11). "LINER galaxy properties and the local environment". Monthly Notices of the Royal Astronomical Society. 476 (2): 2457–2464. arXiv:1803.00946. doi:10.1093/mnras/sty395. ISSN 0035-8711.
- ↑ Márquez, Isabel; Masegosa, Josefa; González-Martin, Omaira; Hernández-Garcia, Lorena; Pović, Mirjana; Netzer, Hagai; Cazzoli, Sara; del Olmo, Ascensión (2017). "The AGN Nature of LINER Nuclear Sources". Frontiers in Astronomy and Space Sciences. 4: 34. Bibcode:2017FrASS...4...34M. doi:10.3389/fspas.2017.00034. ISSN 2296-987X.
- ↑ Pawlik, M. M.; McAlpine, S.; Trayford, J. W.; Wild, V.; Bower, R.; Crain, R. A.; Schaller, M.; Schaye, J. (May 2019). "The diverse evolutionary pathways of post-starburst galaxies". Nature Astronomy. 3 (5): 440–446. arXiv:1903.11050. Bibcode:2019NatAs...3..440P. doi:10.1038/s41550-019-0725-z. ISSN 2397-3366.
- ↑ 6.0 6.1 6.2 information@eso.org. "Cosmic Wonderland". www.spacetelescope.org. Retrieved 2024-05-08.
- ↑ "Astronomers discover how galaxies form through mergers". Astronomers discover how galaxies form through mergers. Retrieved 2024-05-08.
- ↑ MM Reeves, Andrew; J Hudson, Michael. "How many stars form in galaxy mergers?". academic.oup.com. Retrieved 2024-05-08.
- ↑ Valenzuela, Lucas M.; Remus, Rhea-Silvia (2023-05-15), "A stream come true: Connecting tidal tails, shells, streams, and planes with galaxy kinematics and formation history", Astronomy & Astrophysics, 686, arXiv:2208.08443, doi:10.1051/0004-6361/202244758
Template:Pisces (constellation)
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