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NGC 3277

Coordinates: Sky map 10h 32m 55.4506s, +28° 30′ 42.409″
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NGC 3277
NGC 3277 imaged by SDSS
Observation data (J2000 epoch)
ConstellationLeo Minor[1]
Right ascension10h 32m 55.4506s[2]
Declination+28° 30′ 42.409″[2]
Redshift0.004720±0.00000900[2]
Heliocentric radial velocity1,415±3 km/s[2]
Distance148.34 ± 17.58 Mly (45.480 ± 5.389 Mpc)[2]
Group or clusterNGC 3254 group (LGG 197)
Apparent magnitude (V)12.50[2]
Characteristics
TypeSA(r)ab[2]
Size~103,600 ly (31.75 kpc) (estimated)[2]
Apparent size (V)1.9′ × 1.7′[2]
Other designations
IRAS 10301+2846, 2MASX J10325545+2830422, UGC 5731, MCG +05-25-022, PGC 31166, CGCG 154-026[2]

NGC 3277 is a spiral galaxy in the constellation of Leo Minor. Its velocity with respect to the cosmic microwave background is 1,712±21 km/s, which corresponds to a Hubble distance of 82.4 ± 5.9 Mly (25.26 ± 1.80 Mpc).[2] However, five non-redshift measurements give a much farther mean distance of 148.34 ± 17.58 Mly (45.480 ± 5.389 Mpc).[3] It was discovered by German-British astronomer William Herschel on 11 April 1785.[4][1]

NGC 3277 is a Seyfert II galaxy, i.e. it has a quasar-like nucleus with very high surface brightnesses whose spectra reveal strong, high-ionisation emission lines, but unlike quasars, the host galaxy is clearly detectable.[5]

NGC 3254 group

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NGC 3277 is a member of the NGC 3254 group (also known as LGG 197), which contains five galaxies, including NGC 3245A [d], NGC 3245, NGC 3254, and NGC 3265 [fr].[6][7]

Supernova

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One Supernova has been observed in NGC 3277:

  • SN 2025coe (Type Ib-Ca-rich, mag. 17.4) was discovered by Kōichi Itagaki on 24 February 2025.[8] Its light curves displayed multiple distinct peaks which is very rare among known calcium-rich supernovae, with only SN 2019ehk showing similar features.[9] It had an exceptionally large projected physical offset of ~39.3 kpc (~317.7″) from the galactic center, making it the most distant multi-peaked calcium-rich supernova ever discovered relative to its host galaxy.[9] The progenitor system might have been ejected through dynamical interactions.[9]

See also

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References

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  1. 1 2 Seligman, Courtney. "New General Catalogue Objects: NGC 3277". Celestial Atlas. Retrieved 31 December 2025.
  2. 1 2 3 4 5 6 7 8 9 10 11 "Results for object NGC 3277". NASA/IPAC Extragalactic Database. NASA and Caltech. Retrieved 31 December 2025.
  3. ↑ "Distance Results for NGC 3277". NASA/IPAC Extragalactic Database. NASA. Retrieved 31 December 2025.
  4. ↑ Herschel, William (1786). "Catalogue of One Thousand New Nebulae and Clusters of Stars" (PDF). Philosophical Transactions of the Royal Society of London. 76: 457–499. Bibcode:1786RSPT...76..457H. doi:10.1098/rstl.1786.0027.
  5. ↑ "NGC 3277". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 31 December 2025.
  6. ↑ "LGG 197". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 31 December 2025.
  7. ↑ Garcia, A. M. (1993). "General study of group membership. II. Determination of nearby groups". Astronomy and Astrophysics Supplement Series. 100: 47. Bibcode:1993A&AS..100...47G.
  8. ↑ "SN 2025coe". Transient Name Server. IAU. Retrieved 31 December 2025.
  9. 1 2 3 Chen, Chun; Sun, Ning-Chen; Xi, Qiang; et al. (2025). "SN 2025coe: A Multiple-Peaked Calcium-Strong Transient from a White-Dwarf Progenitor". The Astrophysical Journal. arXiv:2510.00135. Bibcode:2025arXiv251000135C.
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  • Wikimedia Commons logo Media related to NGC 3277 at Wikimedia Commons
  • NGC 3277 on WikiSky: DSS2, SDSS, GALEX, IRAS, Hydrogen α, X-Ray, Astrophoto, Sky Map, Articles and images
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