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]
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.
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