NGC 5371

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NGC 5371
NGC 5371.jpg
NGC 5371 imaged by a 24 inch telescope
Observation data (J2000 epoch)
Constellation Canes Venatici
Right ascension 13h 55m 39.9s [1]
Declination +40° 27′ 42.4″ [1]
Redshift 0.00850±0.00019 [2]
Heliocentric radial velocity 2,552±1 km/s [3]
Distance 129.5 ± 32.4  Mly (39.70 ± 9.92  Mpc) [4]
Apparent magnitude  (V)11.3 [5]
Characteristics
Type SAB(rs)bc [5]
Mass 1.86×1011 [4] (baryonic)  M☉
Size146,000 ly (44.80 kpc) [6]
Apparent size  (V)4.4′ × 3.5′ [5]
Other designations
NGC 5371 and 5390, UGC 8846, PGC 49514 [7]

NGC 5371 is a face-on spiral galaxy in the northern constellation Canes Venatici. It was discovered on January 14, 1788 by German-British astronomer William Herschel. The nearby NGC 5390 appears to be a duplicate entry for NGC 5371, since there is nothing at the former's position. [8] NGC 5371 has an apparent magnitude of 11.3 and an angular size of 4.4′ × 3.5′. [5] It is located at a distance of 129.5 ± 32.4 million light-years (39.70 ± 9.92  Mpc ) from the Milky Way, [4] and is receding with a heliocentric radial velocity of 2,552 km/s. The galaxy appears to be weakly interacting with the nearby, equidistant Hickson 68 group of galaxies, and thus may be a member. [3] Collectively, they are sometimes dubbed the Big Lick galaxy group, after the city of Roanoke, Virginia. [9]

NGC 5371 (left) and Hickson 68 (right) Hickson 68 and NGC 5371 (50685694858).jpg
NGC 5371 (left) and Hickson 68 (right)

The morphological classification of NGC 5371 in the De Vaucouleurs system is SAB(rs)bc, [5] indicating a weakly barred spiral galaxy (SAB) with a transitional inner ring structure (rs), and moderately wound spiral arms (bc). The galactic plane is inclined at an angle of 45°±5° to the plane of the sky, with the major axis oriented along a position angle of 195°±3°. [10] This is classified as a LINER-type galaxy and may be in a post-starburst phase. There is an extended or double source of X-ray emission. [11]

Two supernovae have been observed in NGC 5371. Type II-L supernova SN 1994Y was spotted on August 19, 1994, reaching peak B magnitude of 14.2 on August 30. [12] Type IIb supernova SN 2020bio was discovered January 29, 2020. The progenitor may have undergone extensive mass loss, shedding nearly all of its hydrogen envelope. [13]

References

  1. 1 2 Brown, A. G. A.; et al. (Gaia collaboration) (2021). "Gaia Early Data Release 3: Summary of the contents and survey properties". Astronomy & Astrophysics . 649: A1. arXiv: 2012.01533 . Bibcode:2021A&A...649A...1G. doi: 10.1051/0004-6361/202039657 . S2CID   227254300. (Erratum:  doi:10.1051/0004-6361/202039657e). Gaia EDR3 record for this source at VizieR.
  2. ↑ Abazajian, Kevork N.; et al. (2009). "The Seventh Data Release of the Sloan Digital Sky Survey". The Astrophysical Journal Supplement Series. 182 (2): 543–558. arXiv: 0812.0649 . Bibcode:2009ApJS..182..543A. doi:10.1088/0067-0049/182/2/543. S2CID   14376651.
  3. 1 2 van Driel, W.; et al. (November 2016). "NIBLES: an H I census of stellar mass selected SDSS galaxies. I. The Nançay H I survey". Astronomy & Astrophysics. 595: 43. arXiv: 1607.02787 . Bibcode:2016A&A...595A.118V. doi:10.1051/0004-6361/201528048. S2CID   118623916. A118.
  4. 1 2 3 Lelli, Federico; et al. (January 2016). "The Small Scatter of the Baryonic Tully-Fisher Relation". The Astrophysical Journal Letters. 816 (1). id. L14. arXiv: 1512.04543 . Bibcode:2016ApJ...816L..14L. doi: 10.3847/2041-8205/816/1/L14 .
  5. 1 2 3 4 5 König, Michael; Binnewies, Stefan (2017). The Cambridge Photographic Atlas of Galaxies. Cambridge University Press. p. 113. ISBN   9781108103091.
  6. ↑ "NED Results For NGC 5371" . Retrieved 2025-05-03.
  7. ↑ "NGC 5371", SIMBAD , Centre de données astronomiques de Strasbourg , retrieved 2024-04-12.
  8. ↑ Seligman, Courney. "NGC Objects: NGC 5350 - 5399". Celestial Atlas. Retrieved 2024-04-12.
  9. ↑ Brazell, Owen. "April 2014 - Galaxy of the Month: Hickson 68 in Canes Venatici". Webb Deep SKy Society. Retrieved 2024-04-12.
  10. ↑ Fridman, A. M.; et al. (January 2005). "The orientation parameters and rotation curves of 15 spiral galaxies". Astronomy and Astrophysics. 430: 67–81. arXiv: astro-ph/0409622 . Bibcode:2005A&A...430...67F. doi:10.1051/0004-6361:200400087.
  11. ↑ Komossa, Stefanie; et al. (September 1999). "X-ray properties of LINERs". Astronomy and Astrophysics. 349: 88–96. arXiv: astro-ph/9907119 . Bibcode:1999A&A...349...88K.
  12. ↑ Tsvetkov, D. Yu.; Pavlyuk, N. N. (January 1997). "Observations of the supernovae SN 1994Y, 1994ae, and 1995J". Astronomy Letters. 23 (1): 26–29. Bibcode:1997AstL...23...26T.
  13. ↑ Pellegrino, C.; et al. (September 2023). "SN 2020bio: A Double-peaked, H-poor Type IIb Supernova with Evidence of Circumstellar Interaction". The Astrophysical Journal. 954 (1). id. 35. arXiv: 2301.04662 . Bibcode:2023ApJ...954...35P. doi: 10.3847/1538-4357/ace595 .
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