Astronomy:NGC 5383

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NGC 5383
DESI Legacy DR10 image of NGC 5383
Observation data (J2000 epoch)
ConstellationCanes Venatici
Right ascension13h 57m 04.97s
Declination+41° 50' 46.42"
Redshift0.007572
Helio radial velocity2431
Distance110.71 Mly (33.94 Mpc)
Group or clusterLGG 363
Apparent magnitude (V)11.4
Characteristics
TypeSB(rs)b pec
Mass311.87 billion (halo and stellar mass) M☉
Size151,800 ly (46,540 pc)
Other designations
UGC 8875, Markarian 281, LEDA 49618, Z 219-33, MaNGA 1-575771, KUG 1355+420

NGC 5383 also known as Markarian 281, is a grand design spiral galaxy, barred spiral galaxy, starburst galaxy, and radio galaxy in the constellation of Canes Venatici.[1][2][3] The galaxy has an visual magnitude of 11.4, which is visible with a small telescope.[4] The galaxy is considered a prototype barred spiral galaxy along with NGC 1300.[5] The galaxy is very near, at redshift z = 0.007572, equivalent to a distance of roughly 111 million light years (34 megaparsecs).[2] The galaxy is located in the galaxy cluster designated LGG 363, which includes this galaxy, NGC 5362, NGC 5353, and NGC 5337.[6] NGC 5383 was discovered on April 9th, 1787 by William Herschel, and was described as "considerably bright, considerably large, round, and a gradually brighter middle".[4]

Characteristics

NGC 5383 is a typical sized spiral galaxy in the galaxy cluster, LGG 363.[1] The galaxy has a physical diameter of 152,000 light years (46,540 parsecs), or about one and half times the size of the Milky Way.[2] This diameter is based on an angular diameter of 4.71 arcmin (282 arcsecs) from the 2MASS K-band total mag and a mean redshift-independent distance of ~111 million light years (~34 megaparsecs) away.[2]

NGC 5383 has a large, massive, diffuse halo composed of neutral atomic hydrogen.[7] The halo of NGC 5383 has a size of 1.63 million light years (500,000 parsecs), and the halo has a stellar population of mainly metal-poor white dwarfs.[7] The large halo of NGC 5383 has an estimated mass of 263 billion M☉, or roughly four or five times less massive than the halo of the Milky Way.[8]

NGC 5383 has a predicted stellar mass of 48.6 billion M☉, or approximately 4 times less massive than the stellar mass of the Milky Way.[8] The galaxy has a young stellar population of O-type stars and B-type stars in the galactic bulge of NGC 5383.[9] The galaxy is also considered as a mild starburst galaxy with a star-formation rate of 0.126 M☉, similar to the star-formation rate of IC 10.[2][10]

NGC 5383 has a corrected absolute B magnitude of -21.3 based on an apparent B magnitude of 12.5, which is equal to a total galactic luminosity of 48 billion L☉.[11]

NGC 5383 has ten to twenty bright H II regions, similar to the giant H II regions in the Pinwheel Galaxy (Messier 101).[12] Five of these H II regions near the galactic center of NGC 5383 have been classified as emission nebulae.[13] The largest of the H II regions are up to 13,000 light years (4,000 parsecs) across, and the total mass of the H II regions is 2 billion M☉.[10]

NGC 5383 is interacting with three known galaxies, UGC 8877, LAMOST J135707.72+415027.2, and LAMOST J135700.66+415114.9.[14][15][16] One of these galaxies, UGC 8877 is warping the dust lane of NGC 5383, causing these two galaxies to be connected by a gas flow extending 147,000 light years (45,000 parsecs) across.[16]

The galactic center of NGC 5383 contains a active galactic nucleus (also known as an AGN)[1] The active galactic nucleus is powered by a 63.1 million M☉ central supermassive black hole (also referred as an SMBH), which accretes matter and ejects it forming the galaxy's radio lobes.[17]

It was first found in 1978 that NGC 5383 was a radio galaxy, and hosted galaxy-scale relativistic jets that are 46,000 light years (14,000 parsecs) across.[12] In 2023, it was discovered in the second data-release of the LOFAR Two-Metre Sky Survey (LoTSS) that NGC 5383 generated radio lobes with an extent of 214,000 light years (65,550 parsecs) across.[18] The double radio lobed structure of NGC 5383 have a class II Fanaroff-Riley morphology, which are edge-brightened and far more luminous than their counterpart.[18] NGC 5383 is the second spiral DRAGN discovered that it is hosted by a grand-design spiral galaxy.

Supernova

One supernova has been identified in NGC 5383: SN 2005cc, which had a peak magnitude of 17.7 and it was classified a peculiar Type Ia supernova (SNIa pec).[19] SN 2005cc was discovered in May 2005 by Tim Puckett and Alex Langoussis.[20] Type Ia supernovae happen when two stars merge together, with one of the stars being a white dwarf.

See also

References

  1. ↑ 1.0 1.1 1.2 "SIMBAD Results for NGC 5383". https://simbad.u-strasbg.fr/simbad/sim-id?Ident=NGC+5383. 
  2. ↑ 2.0 2.1 2.2 2.3 2.4 "NED Results for NGC 5383". https://ned.ipac.caltech.edu/byname?objname=NGC+5383. 
  3. ↑ Elmegreen, Debra (1990). "Evidence for Small Halos in Grand Design Spiral Galaxies". The Astrophysical Journal 364: 412. doi:10.1086/169423. Bibcode: 1990ApJ...364..412E. https://ui.adsabs.harvard.edu/abs/1990ApJ...364..412E/abstract. Retrieved 2025-12-16. 
  4. ↑ 4.0 4.1 "New General Catalog Objects: NGC 5350-5399". https://cseligman.com/text/atlas/ngc53a.htm#5383. 
  5. ↑ Maeda, Fumiya (2018). "Large velocity dispersion of molecular gas in bars of strongly barred galaxies NGC 1300 and NGC 5383". Publications of the Astronomical Society of Japan 70 (3). doi:10.1093/pasj/psy028. Bibcode: 2018PASJ...70...37M. https://ui.adsabs.harvard.edu/abs/2018PASJ...70...37M/abstract. Retrieved 2025-12-16. 
  6. ↑ "SIMBAD Results for LGG 363". https://simbad.u-strasbg.fr/simbad/sim-id?Ident=LGG+363. 
  7. ↑ 7.0 7.1 Barton, Ian (1997). "Deep Surface Photometry of Spiral Galaxy NGC 5383: Observational Techniques and Halo Constraints". The Astronomical Journal 114: 655. doi:10.1086/118500. Bibcode: 1997AJ....114..655B. https://ui.adsabs.harvard.edu/abs/1997AJ....114..655B/abstract. Retrieved 2025-12-16. 
  8. ↑ 8.0 8.1 Angeloudi, Eirini (2024). "Constraints on the in situ and ex situ stellar masses in nearby galaxies obtained with artificial intelligence". Nature Astronomy 8 (10): 1310. doi:10.1038/s41550-024-02327-3. Bibcode: 2024NatAs...8.1310A. https://ui.adsabs.harvard.edu/abs/2024NatAs...8.1310A/abstract. Retrieved 2025-12-16. 
  9. ↑ Ann, H. B. (2001). "Young Populations in the Nuclei of Barred Galaxies". Astrophysics and Space Science 276 (2–4): 683. doi:10.1023/A:1017589212527. Bibcode: 2001Ap&SS.276..683A. https://ui.adsabs.harvard.edu/abs/2001Ap%26SS.276..683A/abstract. Retrieved 2025-12-16. 
  10. ↑ 10.0 10.1 Sheth, Kartik (2000). "Molecular Gas, Dust, and Star Formation in the Barred Spiral NGC 5383". The Astrophysical Journal 532 (1): 221. doi:10.1086/308530. Bibcode: 2000ApJ...532..221S. https://ui.adsabs.harvard.edu/abs/2000ApJ...532..221S/abstract. Retrieved 2025-12-16. 
  11. ↑ Peterson, C. J. (1978). "The velocity field of the barred spiral galaxy NGC 5383". The Astrophysical Journal 219: 31. doi:10.1086/155752. Bibcode: 1978ApJ...219...31P. https://ui.adsabs.harvard.edu/abs/1978ApJ...219...31P/abstract. Retrieved 2025-12-16. 
  12. ↑ 12.0 12.1 Sancisi, R. (1978). "Radio continuum emission from the barred spiral galaxy NGC 5383". Astronomy and Astrophysics 67 (2). Bibcode: 1978A&A....67L..21S. https://ui.adsabs.harvard.edu/abs/1978A%26A....67L..21S/abstract. Retrieved 2025-12-16. 
  13. ↑ Lynds, B. T. (1974). "An atlas of dust and H II regions in galaxies". The Astrophysical Journal Supplement Series 28: 391. doi:10.1086/190324. Bibcode: 1974ApJS...28..391L. https://ui.adsabs.harvard.edu/abs/1974ApJS...28..391L/abstract. Retrieved 2025-12-16. 
  14. ↑ "SIMBAD Results for LAMOST J135700.66+415114.9". https://simbad.u-strasbg.fr/simbad/sim-id?Ident=LAMOST%20J135700.66%2B415114.9%20. 
  15. ↑ "SIMBAD Results for LAMOST J135707.72+415027.2". https://simbad.u-strasbg.fr/simbad/sim-id?Ident=+LAMOST+J135707.72%2B415027.2&NbIdent=1&Radius=2&Radius.unit=arcmin&submit=submit+id. 
  16. ↑ 16.0 16.1 Huntley, J. M. (1978). "Gas flow in the barred spiral galaxy NGC 5383". The Astrophysical Journal 225: L101. doi:10.1086/182803. Bibcode: 1978ApJ...225L.101H. https://ui.adsabs.harvard.edu/abs/1978ApJ...225L.101H/abstract. Retrieved 2025-12-16. 
  17. ↑ Arzoumanian, Zaven (2021). "The NANOGrav 11 yr Data Set: Limits on Supermassive Black Hole Binaries in Galaxies within 500 Mpc". The Astrophysical Journal 914 (2): 121. doi:10.3847/1538-4357/abfcd3. Bibcode: 2021ApJ...914..121A. 
  18. ↑ 18.0 18.1 Hardcastle, M. J. (2023). "The LOFAR Two-Metre Sky Survey. VI. Optical identifications for the second data release". Astronomy & Astrophysics 678: A151. doi:10.1051/0004-6361/202347333. Bibcode: 2023A&A...678A.151H. https://ui.adsabs.harvard.edu/abs/2023A%26A...678A.151H/abstract. Retrieved 2025-12-16. 
  19. ↑ Barbon, R. (2008). "VizieR Online Data Catalog: Asiago Supernova Catalogue (Version 2008-Mar)". Vizier Online Data Catalog. Bibcode: 2008yCat.2283....0B. https://ui.adsabs.harvard.edu/abs/2008yCat.2283....0B/abstract. Retrieved 2025-12-16. 
  20. ↑ Puckett, T.; Langoussis, A.; Harris, B. (2005). "Supernova 2005cc in NGC 5383". Central Bureau Electronic Telegrams (154): 1. Bibcode: 2005CBET..154....1P. http://www.cbat.eps.harvard.edu/iau/cbet/000100/CBET000154.txt. 



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