NGC 1275
Hubble Space Telescope image of NGC 1275
Observation data (J2000 epoch)
ConstellationPerseus
Right ascension03h 19m 48.1s[1]
Declination+41° 30′ 42″[1]
Redshift5264 ± 11 km/s[1]
z=0.017559[1]
Distance222 million light-years
68.2 Mpc[2]
Group or clusterPerseus Cluster
Apparent magnitude (V)12.6[1]
Characteristics
TypecD;pec;NLRG[1]
Apparent size (V)2.2′ × 1.7′[1]
Other designations
Perseus A,[1] PGC 12429,[1] UGC 2669,[1] QSO B0316+413, Caldwell 24, 3C 84[1]

NGC 1275 (also known as Perseus A or Caldwell 24) is a type 1.5 Seyfert galaxy[3] located around 237 million light-years away[2] in the direction of the constellation Perseus. NGC 1275 is a member of the large Perseus Cluster of galaxies.

Properties

NGC 1275 consists of two galaxies, a central type-cD galaxy in the Perseus Cluster, and a so-called high velocity system (HVS) which lies in front of it. The HVS is moving at 3000 km/s[4] towards the dominant system, and is believed to be merging with the Perseus Cluster. The HVS is not affecting the cD galaxy as it lies at least 200 thousand light years from it.[5] However tidal interactions are disrupting it and the ram pressure produced by its interaction with the intracluster medium of Perseus is stripping its gas as well as producing large amounts of star formation within it[6]

Wide multi-wavelength composite view of NGC 1275. An active supermassive black hole in the galaxy powers strong jets of particles into the Perseus Cluster, causing the gas present to reach 60 million degrees Celsius and emit X-ray light (in blue).

The central cluster galaxy contains a massive network of spectral line emitting filaments,[7] which apparently are being dragged out by rising bubbles of relativistic plasma generated by the central active galactic nucleus.[8] Long gaseous filaments made up of threads of gas stretch out beyond the galaxy, into the multimillion-degree, X-ray–emitting gas that fills the cluster. The amount of gas contained in a typical thread is approximately one million times the mass of the Sun. They are only 200 light-years wide, are often very straight, and extend for up to 20,000 light-years.[9]

The existence of the filaments poses a problem. As they are much cooler than the surrounding intergalactic cloud, it is unclear how they have existed for such a long time, or why they have not warmed, dissipated or collapsed to form stars.[10][11] One possibility is that weak magnetic fields (about one-ten-thousandth the strength of Earth's field) exert enough force on the ions within the threads to keep them together.[10][11]

NGC 1275 contains 13 billion solar masses of molecular hydrogen that seems to be infalling from Perseus' intracluster medium in a cooling flow, both feeding its active nucleus[12] and fueling significant amounts of star formation[13]

The presence of an active nucleus demonstrates that a supermassive black hole is present in NGC 1275's center. The black hole is surrounded by a rotating disk of molecular gas.[14] High-resolution observations of the rotation of this disk obtained using adaptive optics at the Gemini North telescope indicate a central mass of approximately 800 million Solar masses, including both the mass of the black hole and of the inner core of the gas disk.[15]

Two supernovae have been observed in NGC 1275: SN 1968A (type unknown, mag. 15.5),[16] and SN 2005mz (type Ia, mag. 18.2).[17]

References

The location of NGC 1275 (circled in red)
  1. 1 2 3 4 5 6 7 8 9 10 11 "NASA/IPAC Extragalactic Database". Results for NGC 1275. Retrieved 2006-11-19.
  2. 1 2 "Distance Results for NGC 1275". NASA/IPAC Extragalactic Database. Retrieved 2010-03-31.
  3. ↑ Ho, Luis C.; Filippenko, Alex V.; Sargent, Wallace L. W. (October 1997). "A Search for "Dwarf" Seyfert Nuclei. III. Spectroscopic Parameters and Properties of the Host Galaxies". Astrophysical Journal Supplement. 112 (2): 315–390. arXiv:astro-ph/9704107. Bibcode:1997ApJS..112..315H. doi:10.1086/313041. S2CID 17086638.
  4. ↑ Minkowski R., 1957, in IAU Symp 4, Radio astronomy, p107
  5. ↑ Gillmon K., Sanders J.S., Fabian A.C., An X-ray absorption analysis of the high-velocity system in NGC 1275, 2004, MNRAS, 348, 159
  6. ↑ Gallagher, John S. III; Lee, M.; Canning, R.; Fabian, A.; O'Connell, R. W.; Sanders, J.; Zweibel, E. (2010). "Dusty Gas and New Stars: Disruption of the High Velocity Intruder Galaxy Falling Towards NGC 1275". Bulletin of the American Astronomical Society. 42: 552. Bibcode:2010AAS...21536308G.
  7. ↑ Lynds R., Improved Photographs of the NGC1275 Phenomenon, 1970, ApJ, 159, L151
  8. ↑ Hatch N.A., Crawford C.S., Johnstone R.M., Fabian A.C.: On the origin and excitation of the extended nebula surrounding NGC1275, 2006, MNRAS, 367, 433
  9. ↑ Hubble Sees Magnetic Monster in Erupting Galaxy Newswise, Retrieved on August 21, 2008.
  10. 1 2 A. C. Fabian; et al. (2008-08-21). "Magnetic support of the optical emission line filaments in NGC 1275". Nature. 454 (7207): 968–970. arXiv:0808.2712. Bibcode:2008Natur.454..968F. doi:10.1038/nature07169. PMID 18719583. S2CID 4321500.
  11. 1 2 Chang, Kenneth (2008-08-21). "Hubble Images Solve Galactic Filament Mystery". The New York Times.
  12. ↑ Lim, Jeremy; Ao, Yi Ping; Dinh-v-Trung, Dinh-V-Trung (2008). "Radially Inflowing Molecular Gas in NGC 1275 Deposited by an X-Ray Cooling Flow in the Perseus Cluster". The Astrophysical Journal. 672 (1): 252–265. arXiv:0712.2979. Bibcode:2008ApJ...672..252L. doi:10.1086/523664. S2CID 119249662.
  13. ↑ O'Connell, Robert (2007). "Star Formation in the Perseus Cluster Cooling Flow". HST Proposal ID #11207. Cycle 16: 11207. Bibcode:2007hst..prop11207O.
  14. ↑ Wilman, R. J.; Edge, A. C.; Johnstone, R. M. (2005). "The nature of the molecular gas system in the core of NGC 1275". Monthly Notices of the Royal Astronomical Society. 359 (2): 755–764. arXiv:astro-ph/0502537. Bibcode:2005MNRAS.359..755W. doi:10.1111/j.1365-2966.2005.08956.x. S2CID 18190288.
  15. ↑ Scharwächter, J.; McGregor, P. J.; Dopita, M. A.; Beck, T. L. (2013). "Kinematics and excitation of the molecular hydrogen accretion disc in NGC 1275". Monthly Notices of the Royal Astronomical Society. 429 (3): 2315. arXiv:1211.6750. Bibcode:2013MNRAS.429.2315S. doi:10.1093/mnras/sts502. S2CID 119177559.
  16. ↑ Transient Name Server entry for SN 1968A. Retrieved 29 March 2023.
  17. ↑ Transient Name Server entry for SN 2005mz. Retrieved 29 March 2023.
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