NGC 5957

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NGC 5957
NGC5957 - SDSS DR14.jpg
NGC 5957 imaged by the Sloan Digital Sky Survey
Observation data (J2000 epoch)
Constellation Serpens
Right ascension 15h 35m 23.2342s [1]
Declination +12° 02′ 51.203″ [1]
Redshift 0.006051 ± 0.000009 [1]
Heliocentric radial velocity 1,814 ± 3 km/s [1]
Distance 104 ± 7.2 Mly (31.8 ± 2.2 Mpc) [1]
Apparent magnitude  (V)12.1 [2]
Characteristics
Type (R')SAB(r)b [1]
Size~75,000  ly (23.1  kpc) (estimated) [1]
Apparent size  (V)2.8′ × 2.6′ [1]
Other designations
IRAS 15330+1212, UGC 9915, MCG +02-40-004, PGC 55520, CGCG 078-018 [1]

NGC 5957 is a spiral galaxy located in the constellation Serpens. It lies at a distance of about 100 million light years from Earth based on redshift-independent methods, which, given its apparent dimensions, means that NGC 5957 is about 75,000 light years across. [1] It was discovered by Heinrich d'Arrest on April 29, 1865. [3]

NGC 5957 has a bar which is 0.96 arcminutes across. At the end of the bar lies an inner ring with a diameter of 0.94 arcminutes. [4] From the ring emerge multiple spiral arms [5] which form an outer ring with a diameter of 2.38 arcminutes. [4] The nucleus of the galaxy has been found to be active and has been identified as a LINER. The nucleus emits H-alpha that can't be resolved. [6]

One supernova has been discovered in NGC 5957, SN 2025fvw. It was discovered by Kōichi Itagaki on 26 March 2025 at an apparent magnitude of 17.4. It was identified as a type Ia supernova. [7]

NGC 5957 forms a pair with NGC 5956. A. M. Garcia considers NGC 5970 a member of the group, naming it LGG 401. [8] Other nearby galaxies include NGC 5953, NGC 5954, and NGC 5962. [9]

References

  1. 1 2 3 4 5 6 7 8 9 10 "NASA/IPAC Extragalactic Database". Results for NGC 5957. Retrieved 2025-03-18.
  2. ↑ "Revised NGC Data for NGC 5957". spider.seds.org. Retrieved 30 March 2024.
  3. ↑ Seligman, Courtney. "NGC 5957". Celestial Atlas. Retrieved 19 November 2018.
  4. 1 2 Comerón, S.; Salo, H.; Laurikainen, E.; Knapen, J. H.; Buta, R. J.; Herrera-Endoqui, M.; Laine, J.; Holwerda, B. W.; Sheth, K.; Regan, M. W.; Hinz, J. L.; Muñoz-Mateos, J. C.; Gil de Paz, A.; Menéndez-Delmestre, K.; Seibert, M.; Mizusawa, T.; Kim, T.; Erroz-Ferrer, S.; Gadotti, D. A.; Athanassoula, E.; Bosma, A.; Ho, L. C. (February 2014). "ARRAKIS: atlas of resonance rings as known in the S 4 G". Astronomy & Astrophysics. 562: A121. arXiv: 1312.0866 . Bibcode:2014A&A...562A.121C. doi:10.1051/0004-6361/201321633.
  5. ↑ Laurikainen, E.; Salo, H. (February 2017). "Barlenses and X-shaped features compared: two manifestations of boxy/peanut bulges". Astronomy & Astrophysics. 598: A10. arXiv: 1609.01936 . Bibcode:2017A&A...598A..10L. doi:10.1051/0004-6361/201628936.
  6. ↑ Hermosa Muñoz, L.; Márquez, I.; Cazzoli, S.; Masegosa, J.; Agís-González, B. (April 2022). "A search for ionised gas outflows in an H α imaging atlas of nearby LINERs". Astronomy & Astrophysics. 660: A133. arXiv: 2201.05080 . Bibcode:2022A&A...660A.133H. doi:10.1051/0004-6361/202142629.
  7. ↑ "2025fvw | Transient Name Server". www.wis-tns.org. Retrieved 31 March 2025.
  8. ↑ Garcia, A. M. (1 July 1993). "General study of group membership. II. Determination of nearby groups". Astronomy and Astrophysics Supplement Series. 100: 47–90. Bibcode:1993A&AS..100...47G. ISSN   0365-0138.
  9. ↑ Makarov, Dmitry; Karachentsev, Igor (21 April 2011). "Galaxy groups and clouds in the local (z~ 0.01) Universe". Monthly Notices of the Royal Astronomical Society. 412 (4): 2498–2520. arXiv: 1011.6277 . Bibcode:2011MNRAS.412.2498M. doi: 10.1111/j.1365-2966.2010.18071.x . S2CID   119194025 . Retrieved 1 February 2025.
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