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IC 5325

In today's world, IC 5325 is a topic that sparks great interest and debate. This issue has captured the attention of a wide spectrum of society, from academics and experts in the field to ordinary people who want to better understand this phenomenon. Its impact extends to multiple areas, such as economy, politics, culture and daily life. In this article we will explore different perspectives and approaches related to IC 5325, with the aim of shedding light on its relevance today and its potential influence in the future.

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IC 5325
IC 5325 imaged by Legacy Surveys
Observation data (J2000 epoch)
ConstellationPhoenix
Right ascension23h 28m 43.4728s[1]
Declination−41° 20′ 00.038″[1]
Redshift0.005013 ± 0.000023 [1]
Heliocentric radial velocity1,503 ± 7 km/s[1]
Distance68.2 ± 4.9 Mly (20.9 ± 1.5 Mpc)[1]
Apparent magnitude (V)11.0[2]
Characteristics
TypeSAB(rs)bc [1]
Size~74,000 ly (22.6 kpc) (estimated)[1]
Apparent size (V)2.8′ × 2.5′[1]
Other designations
ESO 347- G 018, AM 2325-413, MCG -07-48-004, IRAS 23260-4136, PGC 71548

IC 5325 is a spiral galaxy in the constellation Phoenix. The galaxy lies about 70 million light years away from Earth, which means, given its apparent dimensions, that IC 5325 is approximately 75,000 light years across.[1] It was discovered by Lewis Swift in 1897.[3]

Characteristics

IC 5325 is characterised as an intermediate spiral galaxy, with a weak bar. Its bulge is circular in its brightest region but it becomes oval at its fainter parts. At each end of the oval emerges a spiral arm. These two spiral arms are the most prominent. The galaxy has in total four significant arms and its spiral pattern is flocculent. The western arm has the higher surface brightness.[4] The arms appear fragmented and with many blue knots.[5] The galaxy is seen nearly face-on, at an inclination of about 25°.[6]

As observed in ultraviolet by GALEX the inner region of the disk is brighter. IC 5325 is brighter in far ultraviolet than near ultraviolet, indicating intense star formation within the last 100 million years. The current star formation rate is estimated to be 0.31–0.41 M☉ per year. The galaxy doesn't appear to have significant amounts of cold dust.[7] In the centre of the galaxy lies a supermassive black hole, whose mass is estimated to be 106.97 ± 0.48 (3.1 - 28 millions) M☉, based on the pitch angle of the spiral arms.[8]

Nearby galaxies

IC 5325 is a member of the NGC 7582 galaxy group.[9] Other members of the group include NGC 7552, NGC 7582, NGC 7590, and NGC 7599, which are also known as the Grus Quartet,[10] NGC 7531, NGC 7632, and NGC 7496.[9] This group, along with the group centred around IC 1459 form the Grus cloud, a region of elevated galaxy density. The Grus cloud, along with the nearby Pavo-Indus cloud, lies between the Local Supercluster and Pavo–Indus Supercluster.[11]

Supernova

One supernova has been observed in IC 5325: SN 2013F (type Ib/c, mag. 17.1) was discovered on 5 January 2013 by the Catalina Real-time Transient Survey and Stan Howerton.[12][13]

References

  1. ^ a b c d e f g h i "NASA/IPAC Extragalactic Database". Results for IC 5325. Retrieved 2 February 2025.
  2. ^ "Revised NGC Data for IC 5325". spider.seds.org. Retrieved 30 March 2024.
  3. ^ Seligman, Courtney. "IC 5325 (= PGC 71548)". Celestial Atlas. Retrieved 19 November 2018.
  4. ^ Eskridge, Paul B.; Frogel, Jay A.; Pogge, Richard W.; Quillen, Alice C.; Berlind, Andreas A.; Davies, Roger L.; DePoy, D. L.; Gilbert, Karoline M.; Houdashelt, Mark L.; Kuchinski, Leslie E.; Ramirez, Solange V.; Sellgren, K.; Stutz, Amelia; Terndrup, Donald M.; Tiede, Glenn P. (November 2002). "Near-Infrared and Optical Morphology of Spiral Galaxies". The Astrophysical Journal Supplement Series. 143 (1): 73–111. arXiv:astro-ph/0206320. Bibcode:2002ApJS..143...73E. doi:10.1086/342340.
  5. ^ Donzelli, C. J.; Ferreiro, D. L. (February 1998). "Imaging and spectroscopy of ten southern galaxies selected from a catalogue of peculiar galaxies". Astronomy and Astrophysics Supplement Series. 127 (3): 527–542. Bibcode:1998A&AS..127..527D. doi:10.1051/aas:1998117.
  6. ^ French, David M.; Wakker, Bart P. (1 July 2020). "Evidence for a Rotational Component in the Circumgalactic Medium of Nearby Galaxies*". The Astrophysical Journal. 897 (2): 151. arXiv:2006.09323. Bibcode:2020ApJ...897..151F. doi:10.3847/1538-4357/ab9905.
  7. ^ Singh, Swapnil; Ashby, M L N; Vig, Sarita; Ghosh, S K; Jarrett, T; Crawford, T M; Malkan, Matthew A; Archipley, M; Vieira, J D (12 May 2021). "The cold dust content of the nearby galaxies IC 5325, NGC 7496, NGC 7590, and NGC 7599". Monthly Notices of the Royal Astronomical Society. 504 (3): 4143–4159. arXiv:2104.06236. doi:10.1093/mnras/stab1048.
  8. ^ Davis, Benjamin L.; Berrier, Joel C.; Johns, Lucas; Shields, Douglas W.; Hartley, Matthew T.; Kennefick, Daniel; Kennefick, Julia; Seigar, Marc S.; Lacy, Claud H. S. (20 June 2014). "The Black Hole Mass Function Derived from Local Spiral Galaxies". The Astrophysical Journal. 789 (2): 124. arXiv:1405.5876. Bibcode:2014ApJ...789..124D. doi:10.1088/0004-637X/789/2/124. S2CID 119302157.
  9. ^ a b Makarov, Dmitry; Karachentsev, Igor (21 April 2011). "Galaxy groups and clouds in the local (z~ 0.01) Universe". Monthly Notices of the Royal Astronomical Society. 412 (4): 2498–2520. arXiv:1011.6277. Bibcode:2011MNRAS.412.2498M. doi:10.1111/j.1365-2966.2010.18071.x. S2CID 119194025.
  10. ^ Bakich, Michael E. (2010). 1,001 Celestial Wonders to See Before You Die. New York, New York: Springer Science+Business Media, LLC. p. 334. Bibcode:2010ocws.book.....B. ISBN 978-1-4419-1777-5.
  11. ^ Fouque, P.; Proust, D.; Quintana, H.; Ramirez, A.; Proust, D.; Quintana, H.; Ramirez, A. (1993). "Dynamics of the Pavo-Indus and Grus Clouds of Galaxies" (PDF). Astronomy and Astrophysics Supplement Series. 100 (3): 493–500. Bibcode:1993A&AS..100..493F.{{cite journal}}: CS1 maint: multiple names: authors list (link)
  12. ^ Howerton, S.; Drake, A. J.; Djorgovski, S. G.; Mahabal, A.; Graham, M. J.; Williams, R.; Prieto, J. L.; Catelan, M.; McNaught, R. H.; Christensen, E.; Larson, S. M.; Elias-Rosa, N.; Pastorello, A.; Benetti, S.; Stritzinger, M.; Morrell, N.; Contreras, C.; Hsiao, E. Y. (2013). "Supernova 2013F in IC 5325 = PSN J23284503-4119562". Central Bureau Electronic Telegrams (3380): 1. Bibcode:2013CBET.3380....1H.
  13. ^ "SN 2013F". Transient Name Server. IAU. Retrieved 21 March 2025.
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