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NGC 4442
DESI Legacy DR10 image of NGC 4442
Observation data (J2000 epoch)
ConstellationVirgo
Right ascension12h 28m 03.88s
Declination+09° 48' 13.43"
Redshift0.00117
Heliocentric radial velocity351
Distance48.01 Mly (14.72 Mpc)
Group or clusterVirgo Cluster
Apparent magnitude (V)10.6
Characteristics
TypeSB0
Mass162.2 billion M☉
Size83,100 ly (25,490 pc)
Other designations
UGC 7583, LEDA 40950, Z 70-100, VCC 1062

NGC 4442 also known as UGC 7583, is a barred lenticular galaxy, luminous infrared galaxy and active galaxy in the constellation of Virgo.[1][2] The galaxy is 48 million light years (or 14,720,000 parsecs) away at a spectroscopic redshift z = 0.00117.[2][3] The galaxy has a visual magnitude of 10.6[3], which is visible using a telescope with an aperture of 6 inches or more, and it can be observed in both hemispheres during certain times of the year.[4] The galaxy is located in the Virgo Cluster, along with other notable galaxies such as Messier 87 and the Eyes Galaxies.[1] The galaxy was discovered on April 15, 1784 by German-British astronomer, William Herschel.[5]

Physical properties

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NGC 4442 is medium-sized barred lenticular galaxy located in the Virgo Cluster, and it was listed as the 1,062nd object in the Virgo Cluster Catalog (VCC).[1][2] The galaxy has an estimated width of 83,000 light years (or 25,490 parsecs) across, or about 3/4 the size of the Milky Way.[2] This size is based on an 2MASS K-band total angular diameter of 5.95 arcmin (or 357 arcsecs) and a mean redshift-independent distance of 48 million light years (or 14,720,000 parsecs).[2]

NGC 4442 has a stellar mass of 162 billion M☉, or 10^11.21.[6] The galaxy is roughly 3/4th the stellar mass of the Milky Way.[6] The galaxy has a large stellar population of red-giant branch stars (also known as RGB stars), with an average age of 3.92 billion years old, and an mean mass of 1.09 M☉.[7] The neutral atomic hydrogen in the galaxy has an mass of 54.9 million M☉, and this gas is usually found in the outer regions of the galaxy such as the galactic halo.[6]

NGC 4442 has a K-band luminosity of 550 billion L☉, or 10^11.74 and therefore it is classified as a luminous infrared galaxy (also referred as LIRGs).[6] The galaxy is one of the closest luminous infrared galaxies known[2], with a similar distance to other nearby luminous infrared galaxies such as Messier 77.

NGC 4442 has a star-formation rate of 10.7 M☉ per year, extremely high for gas-poor lenticular galaxies.[8] Despite its high-star formation rate it is not classified as a starburst galaxy, and the galaxy's star-formation rate is comparable to other lenticular galaxies such as Messier 85.[9] The total mass of the ionized atomic hydrogen in the galaxy, which mostly includes the star-forming regions is 109.6 million M☉, or 10^8.04.[6]

The galactic center of NGC 4442 shows a clear active galactic nucleus (also called AGNs), which is a region at the center of a galaxy that is extremely luminous and bright.[1][9] The active galactic nucleus is powered by a massive supermassive black hole (also known as SMBHs) with a mass of 5.25 billion M☉[10] or roughly 1,200 times more massive than Sagittarius A*, which is the central black hole of the Milky Way.

NGC 4442 has a population of 219 globular clusters, however some of them are potentially not globular clusters and are candidates.[11][12] The globular clusters have angular radii between 0.0103 and 0.1042 arcsecs, corresponding to a half-light radius ranging from 2.41 to 24.3 light years (or 0.74 to 7.44 parsecs).[11]

Supernova

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One supernova has been identified in NGC 4442: SN 2021qvv, which had a peak magnitude of 13.8 in July 2021, and it was classified as a Type Ia supernova (abbreviated as SNIa).[13] SN 2021qvv was discovered on June 24, 2021, by the Las Cumbres Observatory.[13] The supernova had a maximum absolute luminosity of -16.42, equivalent to 316 million L☉ and was considered a underluminous supernova similar to other supernovae such as SN 2006mr.[13] The supernova was formed by the collision of two white dwarfs with predicted masses of 0.85 M☉ and 1.1 M☉, creating a super-Chandrasekhar white dwarf which collapsed and exploded.[13]

See also

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  • Messier 85, a lenticular galaxy that has a similar star-formation rate.
  • Messier 77, another nearby luminous infrared galaxy.
  • NGC 1277, another lenticular galaxy hosting a similar mass central black hole.
  • NGC 1316, host of the underluminous supernova, SN 2006mr.

References

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  1. ^ a b c d "SIMBAD Results for NGC 4442". SIMBAD. Retrieved 2025-12-22.
  2. ^ a b c d e f "NED Results for NGC 4442". NASA/IPAC Extragalactic Database. Retrieved 2025-12-22.
  3. ^ a b "In The Sky- NGC 4442". In The Sky. Retrieved 2025-12-22.
  4. ^ "The Sky Live- NGC 4442". The Sky Live. Retrieved 2025-12-22.
  5. ^ "New General Catalog Objects: NGC 4400-4449". New General Catalog Objects. Retrieved 2025-12-22.
  6. ^ a b c d e Tempel, Elmo (2018). "Bayesian group finder based on marked point processes. Method and feasibility study using the 2MRS data set". NASA Ads. 618. arXiv:1806.04469. Bibcode:2018A&A...618A..81T. doi:10.1051/0004-6361/201833217. Retrieved 2025-12-23.
  7. ^ Damsted, S. (2024). "AXES-SDSS: Comparison of SDSS galaxy groups with all-sky X-ray extended sources". NASA Ads. 690: A52. arXiv:2403.17055. Bibcode:2024A&A...690A..52D. doi:10.1051/0004-6361/202449591. Retrieved 2025-12-22.
  8. ^ Hoyer, Nils (2021). "The nucleation fraction of local volume galaxies". NASA Ads. 507 (3): 3246. arXiv:2107.05313. Bibcode:2021MNRAS.507.3246H. doi:10.1093/mnras/stab2277. Retrieved 2025-12-23.
  9. ^ a b Asmus, D. (2020). "Local AGN survey (LASr): I. Galaxy sample, infrared colour selection, and predictions for AGN within 100 Mpc". NASA Ads. 494 (2): 1784. arXiv:2003.05959. Bibcode:2020MNRAS.494.1784A. doi:10.1093/mnras/staa766. Retrieved 2025-12-22.
  10. ^ Dullo, Bililign (2020). "The Black Hole Mass-Color Relations for Early- and Late-type Galaxies: Red and Blue Sequences". NASA Ads. 898 (1): 83. arXiv:2006.10128. Bibcode:2020ApJ...898...83D. doi:10.3847/1538-4357/ab9dff. Retrieved 2025-12-23.
  11. ^ a b Andrés, Jordán (2009). "The ACS Virgo Cluster Survey XVI. Selection Procedure and Catalogs of Globular Cluster Candidates". NASA Ads. 180 (1): 54. Bibcode:2009ApJS..180...54J. doi:10.1088/0067-0049/180/1/54. Retrieved 2025-12-22.
  12. ^ Biao, Li (2015). "A Gemini/GMOS Study of Intermediate Luminosity Early-type Virgo Cluster Galaxies. I. Globular Cluster and Stellar Kinematics". NASA Ads. 806 (1): 133. arXiv:1505.05421. Bibcode:2015ApJ...806..133L. doi:10.1088/0004-637X/806/1/133. Retrieved 2025-12-22.
  13. ^ a b c d Graur, O. (2023). "No plateau observed in late-time near-infrared observations of the underluminous Type Ia supernova 2021qvv". NASA Ads. 526 (2): 2977. arXiv:2306.12858. Bibcode:2023MNRAS.526.2977G. doi:10.1093/mnras/stad2960. Retrieved 2025-12-23.
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