OGC 1304

OGC 1304
SDSS image of OGC 1304
Observation data (J2000.0 epoch)
ConstellationCorona Borealis
Right ascension16h 01m 40.62s[1]
Declination+27° 18′ 15.83″[1]
Redshift0.164398[1]
Heliocentric radial velocity49,285 ± 6 km/s[1]
Distance2,376.6 ± 166.4 Mly (728.67 ± 51.01 Mpc)[1]
Group or clusterGMBCG J240.41924+27.30444
magnitude (J)14.29[1]
Characteristics
TypeBrCIG[1]
Size~432,300 ly (132.55 kpc) (estimated)[1]
Other designations
2MASX J16014061+2718161, KUG 1559+274, SDSS J160140.61+271815.9, PGC 56730, GMBCG J240.41924+27.30444 BCG, ASK 328711.0

OGC 1304 also known as 2MASX J16014061+2718161, is a massive spiral galaxy located in the constellation of Corona Borealis. The redshift of the galaxy is (z) 0.164[1] and it is categorized as a super spiral galaxy; a class of spirals considered to be larger and more distant compared to the Milky Way.[2]

Description

OGC 1304 is the brightest cluster galaxy (BCG) of the galaxy cluster, GMBCG J240.41924+27.30444. The appearance of the galaxy is disturbed, with distorted spiral structure components and further evidence of two bulges being present, indicating an ongoing galaxy merger.[3][4] The galaxy is also confirmed to be located inside a dense galaxy environment, with several satellite galaxies detected within its position.[4] There are also detections of hydrogen-alpha emission in its optical spectrum.[5]

The total isophotal diameter of the galaxy is measured to be 82.3 kiloparsecs. The bulge fraction ratio has been estimated as B/T = 0.04, with the galactic disk displaying an inclination of 59° and orientated at the position angle of 180°. The disk exponential scale length is estimated to be Rd = 11.43.[3] The inclination angle of the galaxy is 60°, while the position angle of the galaxy's major axis is 116°.[6]

A star formation rate of 1.37 Mʘ per year has been estimated for the galaxy based a 12 micrometer band system by the Wide-field Infrared Survey Explorer, with a gas mass of 10.6 Mʘ. The total stellar mass of the stars is 11.63 Mʘ via an estimation of the W-1 band luminosity. The maximum deprojected speed of the galaxy has been found to be vmax = 453 kilometers per seconds.[7]

References

  1. ^ a b c d e f g h i "NED Search results for OGC 1304". NASA/IPAC Extragalactic Database. Retrieved 2026-05-24.
  2. ^ Day, Brian (2016-03-19). "Caltech astronomers discover giant 'super spiral' galaxies". Pasadena Star News. Retrieved 2026-05-24.
  3. ^ a b 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.
  4. ^ a b Bogdán, Ákos; Lovisari, Lorenzo; Kovács, Orsolya E.; Andrade-Santos, Felipe; Jones, Christine; Forman, William R.; Kraft, Ralph P. (2018-12-17). "Detection of a Star-forming Galaxy in the Center of a Low-mass Galaxy Cluster". The Astrophysical Journal. 869 (2): 105. arXiv:1811.04958. Bibcode:2018ApJ...869..105B. doi:10.3847/1538-4357/aaee71. ISSN 0004-637X.
  5. ^ 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.
  6. ^ Di Teodoro, Enrico M; Posti, Lorenzo; Ogle, Patrick M; Fall, S Michael; Jarrett, Thomas (2021-09-11). "Rotation curves and scaling relations of extremely massive spiral galaxies". Monthly Notices of the Royal Astronomical Society. 507 (4): 5820–5831. doi:10.1093/mnras/stab2549. ISSN 0035-8711.
  7. ^ Ogle, Patrick M.; Jarrett, Thomas; Lanz, Lauranne; Cluver, Michelle; Alatalo, Katherine; Appleton, Philip N.; Mazzarella, Joseph M. (2019-10-07). "A Break in Spiral Galaxy Scaling Relations at the Upper Limit of Galaxy Mass". The Astrophysical Journal Letters. 884 (1): L11. arXiv:1909.09080. Bibcode:2019ApJ...884L..11O. doi:10.3847/2041-8213/ab459e. ISSN 2041-8205.

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