J094700.09+254045.8

J094700.09+254045.8
SDSS image of J094700.09+254045.8
Observation data (J2000.0 epoch)
ConstellationLeo
Right ascension09h 47m 00.08s[1]
Declination+25° 40′ 45.82″[1]
Redshift0.109043[1]
Heliocentric radial velocity32,690 ± 6 km/s[1]
Distance1,569.6 ± 109.9 Mly (481.24 ± 33.69 Mpc)[1]
magnitude (J)13.49[1]
Characteristics
TypeSy1
Size~622,000 ly (190.7 kpc) (estimated)[1]
Other designations
2MASX J09470010+2540462, LEDA 2793671, OGC 0543, SDSS J094700.08+254045.7, ASK 593429.0, SDSS J094700.09+254045.8, [TTL2012] 443413[1]

J094700.09+254045.8 also known as OGC 543 and SDSS J094700.08+254045.7 is a massive barred spiral galaxy[2] located in the constellation of Leo. The redshift of the galaxy is (z) 0.109[1] and it is found to belong to a class of super spirals; i.e. a rare type of spiral galaxies that are more larger and distant as compared to the Milky Way.[3]

Description

J094700.09+254045.8 is classified as a grand-design spiral galaxy with defined spiral arms based on a deep convolutional neural network model that is used by astronomers in October 2022.[4] It has a bulge fraction ratio calculated as B/T = 0.21. The galactic disk is found to have a disk inclination of 43° at a position angle of 150° and a measured disk exponential scale of 17.31.[5]

Evidence found J094700.09+254045.8 is a Seyfert type 1 galaxy, hosting an active galactic nucleus (AGN). The inner regions of the nucleus are described to have bluer u – r colors compared to its inner disk, with further evidence of the u – r colors progressively being more bluer as the disk radius increases.[2] The stellar population of the galaxy is found mainly dominated by both old population of stars and also a young star population based on ultraviolet and near-infrared data points. Most of the near-infrared emission appears mainly dominated by both polycyclic aromatic hydrocarbons (PAHs) and warm interstellar dust produced through star formation. The total stellar mass is estimated to be 1.8+0.3−0.2 × 1011 M☉ while the total star formation is estimated to be 13.5 ± 0.2 M☉ per year based on the luminosity calculated by Wide-field Infrared Survey Explorer (WISE). A spectral energy distribution (SED) fit calculated the dust mass as 108 M☉.[5] A study published in 2025, has found the galaxy has presence of molecular gas.[6]

References

  1. 1 2 3 4 5 6 7 8 9 "NED Search results for J094700.09+254045.8". NASA/IPAC Extragalactic Database. Retrieved 2026-05-22.
  2. 1 2 Ogle, Patrick M.; Lanz, Lauranne; Appleton, Philip N.; Helou, George; Mazzarella, Joseph (2019-07-15). "A Catalog of the Most Optically Luminous Galaxies at z < 0.3: Super Spirals, Super Lenticulars, Super Post-mergers, and Giant Ellipticals". The Astrophysical Journal Supplement Series. 243 (1): 14. arXiv:1904.02806. Bibcode:2019ApJS..243...14O. doi:10.3847/1538-4365/ab21c3. ISSN 1538-4365.
  3. ↑ Day, Brian (2016-03-19). "Caltech astronomers discover giant 'super spiral' galaxies". Pasadena Star News. Retrieved 2026-05-22.
  4. ↑ Sarkar, Suman; Narayanan, Ganesh; Banerjee, Arunima; Prakash, Prem (2022-10-27). "Identification of Grand-design and Flocculent spirals from SDSS using deep convolutional neural network". Monthly Notices of the Royal Astronomical Society. 518 (1): 1022–1040. doi:10.1093/mnras/stac3096. ISSN 0035-8711.
  5. 1 2 Ogle, Patrick M.; Lanz, Lauranne; Nader, Cyril; Helou, George (2016-01-26). "Superluminous Spiral Galaxies". The Astrophysical Journal. 817 (2): 109. arXiv:1511.00659. Bibcode:2016ApJ...817..109O. doi:10.3847/0004-637x/817/2/109. ISSN 0004-637X.
  6. ↑ Cologni, R.; Salomé, P.; Le Borgne, D.; Guillard, P.; Boquien, M. (December 2025). "Failed quenching in massive spiral galaxies" (PDF). SF2A-2025: Proceedings of the Annual meeting of the French Society of Astronomy and Astrophysics. Eds.: A. Siebert, K. Baillié, M. Béthermin, F. Cantalloube, E. Josselin, N. Lagarde, J. Malzac, J. Richard, L. Selliez, O. Venot, held 1-4 July, 2025 at INP-ENSEEIHT, Toulouse: 429–432. Bibcode:2025sf2a.conf..429C.
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