NGC 7424

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NGC 7424
Phot-33c-04-fullres.jpg
NGC 7424 seen by VLT's wide-field imager VIMOS
Observation data (J2000 epoch)
Constellation Grus
Right ascension 22h 57m 18s [1]
Declination −41° 04′ 14″ [1]
Redshift 0.003132 (939 ± 2 km/s) [1]
Distance 37.5 Mly (11.5 Mpc) [2]
Apparent magnitude  (V)11.0 [1]
Characteristics
Type SAB(rs)cd [1]
Apparent size  (V)9.5 x 8.1 arcmin [1]
Notable featuressimilar to the Milky Way
Other designations
PGC 070096

NGC 7424 is a barred spiral galaxy located 37.5 million light-years away in the southern constellation Grus (the Crane). Its size (about 100,000 light-years) makes it similar to our own galaxy, the Milky Way. [3] It is called a "grand design" galaxy because of its well defined spiral arms. Two supernovae and two ultraluminous X-ray sources have been discovered in NGC 7424.

Contents

Characteristics

NGC 7424 is intermediate between normal spirals (SA) and strongly barred galaxies (SB). Other features include the presence of a central ring-like structure and a relatively low core brightness relative to the arms. The redder color of the prominent bar indicates an older population of stars while the bright blue color of the loose arms indicates the presence of ionised hydrogen and clusters of massive young stars. NGC 7424 is listed as a member of the IC 1459 Grus Group of galaxies, but is suspected of being a "field galaxy"; that is, not gravitationally bound to any group. [4]

Supernovae

Two supernovae have been observed in NGC 7424:

Hubble Space Telescope image of surviving companion to supernova SN 2001ig HST image of surviving companion to supernova SN 2001ig.png
Hubble Space Telescope image of surviving companion to supernova SN 2001ig

In 2006, Anglo-Australian Observatory astronomer Stuart Ryder et al. found what they argued could be the binary companion to SN 2001ig using the Gemini Observatory. It is a massive A or F class star that had an eccentric orbit around the progenitor, a Wolf-Rayet star. They believe that the companion periodically stripped the outer hydrogen-rich envelope of the progenitor, accounting for the observed spectral changes. [7] [8] Princeton University fellow Alicia Soderberg et al. also believe that the progenitor was a Wolf-Rayet star, but suggest that the periodic mass loss was a result of the intense stellar wind these stars produce. [9]

In a paper published in March 2018, Ryder et al. announced that the surviving companion had been observed with the Hubble Space Telescope in the ultraviolet. [10] This is the first time a companion to a Type IIb supernova has been imaged. [11]

Ultraluminous X-ray sources

In May and June 2002, Roberto Soria and his colleagues at the Harvard-Smithsonian Center for Astrophysics discovered two Ultraluminous X-ray sources (ULXs) with the Chandra X-ray Observatory. ULXs are objects that emit tremendous amounts of X-rays (> 1032 watts or 1039 erg/s), assuming they radiate isotropically (the same in all directions). This amount is larger than currently understood stellar processes (including supernovae) but smaller than the amount of X-rays emitted by active galactic nuclei, which accounts for their alternate name, Intermediate-luminosity X-ray Objects (IXOs). The source designated ULX1 was found in a relatively empty interarm region, far from any bright clusters or star-forming complexes, and showed a 75% increase in X-ray luminosity over the course of 20 days. ULX2 was found in an exceptionally bright young stellar complex, and showed an order of magnitude increase over the same time period. [2]

References

  1. 1 2 3 4 5 6 "NASA/IPAC Extragalactic Database". Results for NGC 7424. Retrieved 26 November 2008.
  2. 1 2 Soria, R.; et al. (August 2006), "Multiband Study of NGC 7424 and its Two Newly-discovered ULXs", Monthly Notices of the Royal Astronomical Society , 370 (4): 1666–1676, arXiv: astro-ph/0606080 , Bibcode:2006MNRAS.370.1666S, doi: 10.1111/j.1365-2966.2006.10629.x , S2CID   17098189
  3. ↑ "Explosions in majestic spiral galaxy beauties". Spaceflight Now. 5 December 2004. Retrieved 27 November 2008.
  4. ↑ Yahil, A.; Vidal, N. V. (June 1977), "The Velocity Distribution of Galaxies in Clusters", Astrophysical Journal, 214: 347, Bibcode:1977ApJ...214..347Y, doi: 10.1086/155257
  5. ↑ Evans, R. O.; White, B.; Bembrick, C. (2001). "Supernova 2001ig in NGC 7424". International Astronomical Union Circular (7772): 1. Bibcode:2001IAUC.7772....1E . Retrieved 21 February 2014.
  6. ↑ "SN 2017bzb". Transient Name Server. IAU . Retrieved 29 August 2025.
  7. ↑ Ryder, S.; et al. (April 2004), "Modulations in the radio light curve of the Type IIb supernova 2001ig: evidence for a Wolf-Rayet binary progenitor?", Monthly Notices of the Royal Astronomical Society, 349 (3): 1093–1100, arXiv: astro-ph/0401135 , Bibcode:2004MNRAS.349.1093R, doi: 10.1111/j.1365-2966.2004.07589.x , S2CID   18132819
  8. ↑ Ryder, S.; et al. (June 2006), "A post-mortem investigation of the Type IIb supernova 2001ig", Monthly Notices of the Royal Astronomical Society, 369 (1): L32 –L36, arXiv: astro-ph/0603336 , Bibcode:2006MNRAS.369L..32R, doi: 10.1111/j.1745-3933.2006.00168.x , S2CID   15543433
  9. ↑ Soderberg, A.; et al. (October 2006), "The Radio and X-Ray Luminous SN 2003bg and the Circumstellar Density Variations around Radio Supernovae", Astrophysical Journal, 651 (2): 1005–1018, arXiv: astro-ph/0512413 , Bibcode:2006ApJ...651.1005S, doi:10.1086/507571, S2CID   954954
  10. ↑ Ryder, S.; et al. (March 2018), "Ultraviolet Detection of the Binary Companion to the Type IIb SN 2001ig", The Astrophysical Journal, 856 (1): 83, arXiv: 1801.05125 , Bibcode:2018ApJ...856...83R, doi: 10.3847/1538-4357/aaaf1e , S2CID   119383171
  11. ↑ Hille, Karl (2018-04-26). "Stellar Thief Is the Surviving Companion to a Supernova". NASA. Retrieved 27 April 2018.
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