NGC 5474

NGC 5474
Hubble image of NGC 5474.
Observation data (J2000 epoch)
ConstellationUrsa Major
Right ascension14h 05m 01.6s
Declination+53° 39′ 44″
Redshift273 ± 9 km/s
Distance21.2 ± 2.2 Mly (6.5 ± 0.7 Mpc)
Apparent magnitude (V)11.3
Characteristics
TypeSA(s)cd pec
Size27,500 ly (8.43 kpc) (estimated)
Apparent size (V)4.8′ × 4.3′
Other designations
UGC 9013, PGC 50216

NGC 5474 is a peculiar dwarf spiral galaxy in the M101 group. Located in the Ursa Major constellation approximately 6.98 Mpc away from Earth, it is a satellite companion to the larger Pinwheel Galaxy (M101), a grand-design spiral. NGC 5474 is in a weakly bound orbit, with a projected distance of 90kpc from M101's photometric center, and of the four satellite galaxies in the M101 group, it is M101's closest companion.

A previous interaction with the Pinwheel Galaxy left NGC 5474 strongly distorted, with the disk is offset relative to the nucleus. The star formation in this galaxy (as traced by hydrogen spectral line emission) is also offset from the nucleus. NGC 5474 shows some signs of a spiral structure. As a result, this galaxy is often classified as a dwarf spiral galaxy, a relatively rare group of dwarf galaxies.

M101 Interaction

Approximately 200 Myr ago, NGC 5474 and M101 collided, with NGC 5474 passing through the west side of M101's outer disk and leaving the morphology of both galaxies distorted. The mass ratio between M101 and NGC 5474 is large — M101 being roughly an order of magnitude more massive — meaning the interaction was strongly asymmetric, with NGC 5474 subject to significant tidal forces while M101 itself shows comparatively modest perturbations. NGC 5474 was left significantly distorted; The photometric center of NGC 5474 has been dramatically offset from the kinematic center of the disk, although it still displays a weak, lopsided spiral arm structure. No significant tidal tails are present around either NGC 5474 or M101, which can be explained by a dual retrograde geometry of the interaction.

This configuration is analogous to other well-studied dwarf-dominant pairs in the local universe, such as the Large Magellanic Cloud and Milky Way system, where the lower-mass companion experiences dramatic morphological and star formation consequences.

While the strongest phase of interaction between the galaxies has passed, and the two galaxies are not projected to have another close encounter within the next billion years, the two galaxies remain connected gravitationally as well as through a shared gas bridge. Hydrogen line observations reveal an extended neutral hydrogen bridge and asymmetric envelope connecting NGC 5474 to M101. This is consistent with tidal stripping, as the gas stream is oriented in the expected direction of M101's tidal force. Additionally, a lack of high-to-intermediate velocity clouds around the dwarf galaxy suggests that the gas bridge is created by M101 siphoning off gas from NGC 5474.

NGC 5474's morphological change is ongoing. The revolution of its stellar disk is opposite to its orbital revolution, so the distortion may diminish after several galactic rotations. The galaxy is unlikely to completely return to its original form as the spiral arm structure in disk galaxies is dependent on its rotational velocity, a parameter that would have been affected by the retrograde collision.

Star Formation

Star formation rates are generally low for dwarf galaxies, but NGC 5474 is brighter than the conventional dwarf galaxy limit by 1.5 mag. Its irregular spiral structure is also not necessarily a limiter on star formation. Both grand design and flocculent spirals are shown to have similar rates of star formation. Their differences lie in the concentration of star formation: within smaller regions for well-defined arms, or more spread out throughout the stellar disk for discontinuous arms. However, the relative lack of a neutral hydrogen reservoir could have a limiting effect on NGC 5474's star formation rate.

Morphological Questions

There is a possibility that the compact bulge of NGC 5474 is itself a dwarf elliptical companion in a polar orbit around the stellar disk. The gravitational interaction of this type of system could produce the same observed asymmetric spiral arm structure as well as the observed distorted HI distribution. Other supporting arguments for this hypothesis include mismatched star formation rate peaks between the bulge and the disk, as well as a relative velocity difference.

See also

References

  1. ↑ "A dwarf galaxy ravaged by grand design". Picture of the Week. ESA/Hubble. Retrieved 17 June 2014.
  2. ↑ R. W. Sinnott, ed. (1988). The Complete New General Catalogue and Index Catalogue of Nebulae and Star Clusters by J. L. E. Dreyer. Sky Publishing Corporation and Cambridge University Press. ISBN 978-0-933346-51-2.
  3. 1 2 3 4 5 6 7 8 9 10 "NASA/IPAC Extragalactic Database". Results for NGC 5474. Retrieved 2006-09-20.
  4. ↑ A. Sandage; J. Bedke (1994). Carnegie Atlas of Galaxies. Washington, D.C.: Carnegie Institution of Washington. ISBN 978-0-87279-667-6.
  5. ↑ Kenney, Jeffrey D. P.; Scoville, Nick Z.; Wilson, Christine D. (1991-01-10). "The star-forming disk and CO bar in M101". The Astrophysical Journal. 366: 432. doi:10.1086/169577. ISSN 0004-637X.
  6. 1 2 Drozdovsky, I. O.; Karachentsev, I. D. (2000). "Photometric distances to six bright resolved galaxies". Astronomy and Astrophysics Supplement. 142 (3): 425–432. Bibcode:2000A&AS..142..425D. doi:10.1051/aas:2000155.
  7. 1 2 3 Bellazzini, M.; Annibali, F.; Tosi, M.; Mucciarelli, A.; Cignoni, M.; Beccari, G.; Nipoti, C.; Pascale, R. (2020-02-20). "The strange case of the peculiar spiral galaxy NGC 5474: New pieces of a galactic puzzle". Astronomy & Astrophysics. 634: A124. arXiv:2001.02413. doi:10.1051/0004-6361/201937284. ISSN 0004-6361.
  8. 1 2 R. M. Gonzalez Delgado; E. Perez; C. Tadhunter; J. M. Vilchez; J. M. Rodriguez-Espinosa (2000). "H II Region Population in a Sample of Nearby Galaxies with Nuclear Activity. I. Data and General Results". Astrophysical Journal Supplement. 108 (1): 155. Bibcode:1997ApJS..108..155G. doi:10.1086/312951.
  9. 1 2 3 Mihos, J. Christopher; Harding, Paul; Spengler, Chelsea E.; Rudick, Craig S.; Feldmeier, John J. (2013-01-10). "THE EXTENDED OPTICAL DISK OF M101". The Astrophysical Journal. 762 (2): 82. arXiv:1211.3095. doi:10.1088/0004-637X/762/2/82. ISSN 0004-637X.
  10. ↑ Besla, Gurtina; Kallivayalil, Nitya; Hernquist, Lars; van der Marel, Roeland P.; Cox, T. J.; Kereš, Dušan (2012-04-11). "The role of dwarf galaxy interactions in shaping the Magellanic System and implications for Magellanic Irregulars: The Magellanic System". Monthly Notices of the Royal Astronomical Society. 421 (3): 2109–2138. arXiv:1201.1299. doi:10.1111/j.1365-2966.2012.20466.x.
  11. 1 2 Gallagher, John S.; Hunter, Deidre A. (1984-09-01). "Structure and Evolution of Irregular Galaxies". Annual Review of Astronomy and Astrophysics. 22 (1): 37–74. doi:10.1146/annurev.aa.22.090184.000345. ISSN 0066-4146.
  12. ↑ info@noirlab.edu. "NGC 5474". www.noirlab.edu. Retrieved 2026-08-28.
  13. ↑ Elmegreen, Bruce G.; Elmegreen, Debra Meloy (1986-12-15). "Do density waves trigger star formation?". The Astrophysical Journal. 311: 554. doi:10.1086/164795. ISSN 0004-637X.
  14. ↑ Cepa, Jordi; Beckman, John E. "Star Formation Triggering by Density Waves in the Grand Design Spirals NGC 3992 and NGC 628". The Astrophysical Journal. 349: 497. doi:10.1086/168335. ISSN 0004-637X.
  15. ↑ Kennicutt, Robert C. (1998-09-01). "STAR FORMATION IN GALAXIES ALONG THE HUBBLE SEQUENCE". Annual Review of Astronomy and Astrophysics. 36 (1): 189–231. arXiv:astro-ph/9807187. doi:10.1146/annurev.astro.36.1.189. ISSN 0066-4146.
  16. ↑ Bortolini, G; Cignoni, M; Sacchi, E; Tosi, M; Annibali, F; Pascale, R; Bellazzini, M; Calzetti, D; Adamo, A; Dale, Daniel A; Fumagalli, M; Gallagher, John S; Grasha, K; Johnson, Kelsey E; Linden, Sean T (2023-11-27). "The spatially resolved star formation history of the dwarf spiral galaxy NGC 5474". Monthly Notices of the Royal Astronomical Society. 527 (3): 5339–5355. arXiv:2311.08160. doi:10.1093/mnras/stad3524. ISSN 0035-8711.
  17. ↑ Rownd, B. K.; Dickey, J. M.; Helou, G. (1994-11-04). "H I distribution and kinematics in the peculiar spiral galaxy NGC 5474". The Astronomical Journal. 108: 1638. doi:10.1086/117185.