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// Workers AI · dad joke modeWhat did NGC 3377A say to NGC 3377? You're a galaxy ahead.

Coordinates: Sky map 10h 47m 22.4s, 14° 04′ 17″
From Wikipedia, the free encyclopedia
NGC 3377A
HST image of UGC 5889
Observation data (J2000 epoch)
ConstellationLeo[1]
Right ascension10h 47m 22.401s[2]
Declination+14° 04′ 16.697″[2]
Heliocentric radial velocity573 km/s[3]
Distance25.2 Mly (7.73 Mpc)[4]
Group or clusterM96 Group
Apparent magnitude (V)13.7[1]
Apparent magnitude (B)14.3[1]
Characteristics
TypeSAB(s)m[5]
Mass2.3×108[4] M☉
Apparent size (V)2.2′ × 2.1′[1]
Notable featuresSpiral morphology
Other designations
NGC 3377A, UGC 5889, LEDA 32226, PGC 32226, DDO 88,[6] ZWG 66.14[1]

NGC 3377A is a dwarf irregular galaxy[7] in the equatorial constellation of Leo.[1] Alternatively, it is identified as DDO 88 or UGC 5889. The distance to this galaxy is 25.2 million light-years (7.73 Mpc).[4] The earliest known reference to this galaxy is from the 1959 publication A Catalogue of Dwarf Galaxies by Canadian astronomer Sidney van den Bergh, where it is listed as DDO 88.[8] Therefore, this galaxy, despite its common name, was not a part of the original New General Catalogue.

Observations

[edit]

This very low surface brightness galaxy is being viewed nearly face-on.[9] It is a typical dwarf irregular galaxy[7] with a morphological class of SAB(s)m.[5] The galaxy is small and faint, with a somewhat boxy shape that is probably hosting a stellar bar. It is gas rich with an extended envelope of neutral hydrogen. Several holes have been identified in this gas, with the largest spanning 2 kpc.[7] The latter radius is half that of the optical galaxy,[10] and it is surrounded by a large ring of enhanced neutral hydrogen emission.[7] The outer morphology of NGC 3377A is similar to a dwarf spiral galaxy with loosely wound arms.[11][12]

Star formation in NGC 3377A is low, occurring at an averate rate of 0.0033 M☉ per year.[9][11] Over the last 200 million years, star formation appears to have occurred in spurts.[13] NGC 3377A is currently in the midst of one such outburst, with new stars being formed in small, bright, evenly distributed regions in the outer parts of the galaxy.[14] A total of 83 young stellar groups have been identified. Many of these occur in "knots" of hydrogen-alpha emission.[9] The central region primarily consists of older stellar populations.[14]

NGC 3377 and NGC 3377A imaged by Legacy Surveys

NGC 3377A is a member of the M96 Group (Leo I) of galaxies[14] and is located at an angular separation of 7′ to the northwest of the giant elliptical galaxy NGC 3377.[9]

NGC 3377A may be a companion of NGC 3377. The pair have a velocity difference of 120 km s−1[9] and a projected separation of around 72 kly (22 kpc).[11] NGC 3377A has a low rotation rate for its luminosity, suggesting this a tidal dwarf with a lower level of dark matter than is typical.[7]

References

[edit]
  1. 1 2 3 4 5 6 Frommert, Hartmut, Revised NGC Data for NGC 3377, Students for the Exploration and Development of Space, retrieved 2026-09-13.
  2. 1 2 Vallenari, A.; et al. (Gaia collaboration) (2023), "Gaia Data Release 3. Summary of the content and survey properties", Astronomy and Astrophysics, 674: A1, arXiv:2208.00211, Bibcode:2023A&A...674A...1G, doi:10.1051/0004-6361/202243940, S2CID 244398875. Gaia DR3 record for this source at VizieR.
  3. ↑ Buta, Ronald J. (September 2019), "The systematics of galaxy morphology in the comprehensive de Vaucouleurs revised Hubble-Sandage classification system: application to the EFIGI sample", Monthly Notices of the Royal Astronomical Society, 488 (1) stz1693: 590–608, arXiv:1906.08124, Bibcode:2019MNRAS.488..590B, doi:10.1093/mnras/stz1693.
  4. 1 2 3 Karachentsev, Igor D.; et al. (January 2017), "The Local Tully-Fisher Relation for Dwarf Galaxies", The Astronomical Journal, 153 (1): 17, arXiv:1611.02574, Bibcode:2017AJ....153....6K, doi:10.3847/1538-3881/153/1/6, S2CID 119388974, 6.
  5. 1 2 de Vaucouleurs, G.; et al. (1991), Third reference catalogue of bright galaxies, 9, New York: Springer-Verlag.
  6. ↑ "NGC 3377A", SIMBAD, Centre de données astronomiques de Strasbourg, retrieved 2026-09-14.
  7. 1 2 3 4 5 Simpson, Caroline E.; et al. (January 2005), "DDO 88: A Galaxy-sized Hole in the Interstellar Medium", The Astronomical Journal, 129 (1): 160–177, arXiv:astro-ph/0409739, Bibcode:2005AJ....129..160S, doi:10.1086/426364.
  8. ↑ Van Den Bergh, Sidney (1959). "A Catalogue of Dwarf Galaxies". Publications of the David Dunlap Observatory. 2 (5): 147. Bibcode:1959PDDO....2..147V.
  9. 1 2 3 4 5 Vicari, A.; et al. (March 2002), "Large-scale star formation in galaxies. II. The spirals NGC 3377A, NGC 3507 and NGC 4394. Young star groupings in spirals", Astronomy and Astrophysics, 384: 24–32, Bibcode:2002A&A...384...24V, doi:10.1051/0004-6361:20011803.
  10. ↑ Hunter, Deidre A.; et al. (September 2024), "The Interstellar Medium in Dwarf Irregular Galaxies", Annual Review of Astronomy and Astrophysics, 62 (1): 113–155, arXiv:2402.17004, Bibcode:2024ARA&A..62..113H, doi:10.1146/annurev-astro-052722-104109.
  11. 1 2 3 Knezek, Patricia M.; et al. (March 1999), "Evolutionary Status of Dwarf 'Transition' Galaxies", The Astrophysical Journal, 514 (1): 119–132, arXiv:astro-ph/9810119, Bibcode:1999ApJ...514..119K, doi:10.1086/306921.
  12. ↑ Sandage, Allan; Hoffman, G. Lyle (October 1991), "NGC 4286 and NGC 3377A: Galaxies with Mixed Morphologies between the Dwarf Im and dE/dSO Types", Astrophysical Journal Letters, 379: L45, Bibcode:1991ApJ...379L..45S, doi:10.1086/186150.
  13. ↑ Vallenari, A.; et al. (June 2005), "The star formation history of the LSB galaxy UGC 5889", Astronomy and Astrophysics, 435 (3): 821–829, arXiv:astro-ph/0502357, Bibcode:2005A&A...435..821V, doi:10.1051/0004-6361:20041138.
  14. 1 2 3 Schmidtobreick, L.; et al. (December 2007), Vallenari, Antonella; et al. (eds.), "Surface Photometry of UGC 5889", From Stars to Galaxies: Building the Pieces to Build Up the Universe, proceedings of the conference held 16–20 October 2006 at Istituto Veneto di Scienze, Lettere ed Arti, Venice, Italy, ASP Conference Series, vol. 374, p. 285, Bibcode:2007ASPC..374..285S.
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