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NGC 4424

Today, NGC 4424 is a topic that generates great interest and impact in society. Whether due to its historical relevance, its impact on public health, its influence on popular culture or its relevance in the business field, NGC 4424 has captured the attention of millions of people around the world. From its origins to its evolution today, NGC 4424 has been the subject of debates, analyzes and studies that seek to understand its scope and meaning. In this article, we will explore the different facets of NGC 4424 and its influence on various aspects of our lives.

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NGC 4424
NGC 4424 imaged by the Vera C. Rubin Observatory
Observation data (J2000 epoch)
ConstellationVirgo
Right ascension12h 27m 11.575s[1]
Declination+09° 25′ 14.32″[1]
Redshift0.00146[2]
Heliocentric radial velocity442[3]
Distance13.5 Mly (4.1 Mpc)[4]
Group or clusterVirgo Cluster[5]
Characteristics
TypeSB(s)a peculiar[2]
Mass3.8+2.3
−1.4×108[4] M☉
Other designations
IRAS 12246+0941, 2MASX J12271158+0925138, UGC 7561, MCG +02-32-058, PGC 40809[6][7]

NGC 4424 is a spiral galaxy located in the equatorial constellation of Virgo. It was discovered February 27, 1865 by German astronomer Heinrich Louis d'Arrest.[8] This galaxy is located at a distance of 13.5[4] million light years and is receding with a heliocentric radial velocity of 442 km/s.[3] It has a morphological class of SB(s)a,[2] which normally indicates a spiral galaxy with a barred structure (SB), no inner ring feature (s), and tightly-wound spiral arms (a). The galactic plane is inclined at an angle of 62° to the line of sight from the Earth. It is a likely member of the Virgo Cluster of galaxies.[5]

NGC 4424 imaged by the Hubble Space Telescope; the smaller galaxy IC 3366 is below center

The galaxy NGC 4424 has a peculiar morphology with shells that give the appearance of a galaxy merger within the last half billion years. It has a long tail of hydrogen stretching 110 kpc to the south that is likely due to stripping from ram pressure. Because of the lack of gas, star formation has completely ceased in the outer parts of the galaxy, while there is still a mild amount occurring in the inner region. NGC 4424 will most likely end up as a lenticular galaxy by three billion years from now.[5]

There is no indication of a compact source of X-ray emission in the nucleus, but there is an ionized tail stretching ~10 kpc from the core.[5] The velocity dispersion at the core suggests there is a supermassive black hole (SMBH) with a mass of (0.8±0.2)×105 M☉.[9] Hubble images of this galaxy show a tidally-stretched cluster located at a projected distance of ~400 pc from the nucleus. This is probably the core of a captured galaxy. It contains a compact source that is emitting X-rays and may be an active massive black hole. In time this may merge with the core SMBH of NGC 4424.[9]

Supernovae

Two supernovae have been observed in NGC 4424:

  • SN 1895A (type unknown, mag. 12.5) was discovered by Max Wolf on March 16, 1895.[10][11]
  • SN 2012cg (Type Ia, mag. 16.9) was discovered by the LOSS program from images taken on May 17, 2012.[12][13] It reached maximum light (mag. 11.9) nine days later[14] and became the brightest supernova of the year 2012.[15] The supernova reached a peak absolute magnitude of −19.50±0.31 in the B (blue) band and synthesized 0.72±0.31 M☉ of the radioactive isotope nickel-56.[2] The available observations favor a merger of double degenerate progenitors as the source for the event.[16] The proximity of the galaxy made this one of the best studied supernova explosions to date.[16]

References

  1. ^ a b Brown, A. G. A.; et al. (Gaia collaboration) (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics. 616. A1. arXiv:1804.09365. Bibcode:2018A&A...616A...1G. doi:10.1051/0004-6361/201833051. Gaia DR2 record for this source at VizieR.
  2. ^ a b c d Chakradhari, N. K.; et al. (August 2019). "Optical and UV studies of type Ia supernovae SN 2009ig and SN 2012cg". Monthly Notices of the Royal Astronomical Society. 487 (2): 1886–1904. Bibcode:2019MNRAS.487.1886C. doi:10.1093/mnras/stz1358.
  3. ^ a b Tully, R. Brent (May 2015). "Galaxy Groups: A 2MASS Catalog". The Astronomical Journal. 149 (5): 14. arXiv:1503.03134. Bibcode:2015AJ....149..171T. doi:10.1088/0004-6256/149/5/171. S2CID 119285986. 171.
  4. ^ a b c Lianou, S.; et al. (November 2019). "Dust properties and star formation of approximately a thousand local galaxies". Astronomy & Astrophysics. 631: 19. arXiv:1906.02712. Bibcode:2019A&A...631A..38L. doi:10.1051/0004-6361/201834553. S2CID 174801441. A38.
  5. ^ a b c d Boselli, A.; et al. (December 2018). "A Virgo Environmental Survey Tracing Ionised Gas Emission (VESTIGE). IV. A tail of ionised gas in the merger remnant NGC4424". Astronomy & Astrophysics. 620: 16. arXiv:1810.09234. Bibcode:2018A&A...620A.164B. doi:10.1051/0004-6361/201833914. S2CID 229156290. A164.
  6. ^ "HyperLeda -object description". leda.univ-lyon1.fr. Retrieved 27 March 2017.
  7. ^ "NGC 4424". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 27 March 2017.
  8. ^ Anderson, Natali (Mar 27, 2017). "Hubble Observes Barred Spiral Galaxy NGC 4424". Science News. Retrieved 2021-12-25.
  9. ^ a b Graham, Alister W.; et al. (December 2021). "Potential Black Hole Seeding of the Spiral Galaxy NGC 4424 via an Infalling Star Cluster". The Astrophysical Journal. 923 (2): 14. arXiv:2112.05318. Bibcode:2021ApJ...923..146G. doi:10.3847/1538-4357/ac235b. S2CID 245117870. 146.
  10. ^ Wolf, M. (1925). "Variabilis (? Nova) 94.1925 Virginis". Astronomische Nachrichten. 226 (5): 75. Bibcode:1925AN....226...75W. doi:10.1002/asna.19252260504.
  11. ^ "SN 1895A". Transient Name Server. IAU. Retrieved 3 June 2025.
  12. ^ Kandrashoff, M.; et al. (May 2012). Green, D. W. E. (ed.). "Supernova 2012cg in NGC 4424 = Psn J12271283+0925132". Central Bureau Electronic Telegrams. 3111 (1): 1. Bibcode:2012CBET.3111....1K.
  13. ^ "SN 2012cg". Transient Name Server. IAU. Retrieved 3 June 2025.
  14. ^ Munari, U.; et al. (April 2013). "BVRI lightcurves of supernovae SN 2011fe in M101, SN 2012aw in M95, and SN 2012cg in NGC 4424". New Astronomy. 20: 30–37. arXiv:1209.4692. Bibcode:2013NewA...20...30M. doi:10.1016/j.newast.2012.09.003. S2CID 53975401.
  15. ^ Bishop, David. "Bright Supernovae - 2012". Rochester Astronomy. Retrieved 8 December 2024.
  16. ^ a b Shappee, B. J.; et al. (March 2018). "Strong Evidence against a Non-degenerate Companion in SN 2012cg". The Astrophysical Journal. 855 (1): 10. arXiv:1610.07601. Bibcode:2018ApJ...855....6S. doi:10.3847/1538-4357/aaa1e9. S2CID 73720425. 6.
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