NGC 1275

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NGC 1275
NGC 1275 Hubble.jpg
Hubble Space Telescope image of NGC 1275
Observation data (J2000 epoch)
Constellation Perseus
Right ascension 03h 19m 48.1s [1]
Declination +41° 30′ 42″ [1]
Redshift 5264 ± 11 km/s [1]
z=0.017559 [1]
Distance 222 million light-years
68.2 Mpc [2]
Group or cluster Perseus Cluster
Apparent magnitude  (V)12.6 [1]
Characteristics
Type cD;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.

Contents

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). Dazzling Galaxy.jpg
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]

Supernovae

Three supernovae have been observed in NGC 1275:

Related Research Articles

<span class="mw-page-title-main">Perseus Cluster</span> Galaxy cluster in the constellation Perseus

The Perseus cluster is a cluster of galaxies in the constellation Perseus. It has a recession speed of 5,366 km/s and a diameter of 863′. It is one of the most massive objects in the known universe, containing thousands of galaxies immersed in a vast cloud of multimillion-degree gas.

<span class="mw-page-title-main">NGC 3226</span> Dwarf elliptical galaxy in the constellation Leo

NGC 3226 is a dwarf elliptical galaxy that is interacting with the spiral galaxy NGC 3227. The two galaxies are one of several examples of a spiral with a dwarf elliptical companion that are listed in the Atlas of Peculiar Galaxies. Both galaxies may be found in the constellation Leo. It is a member of the NGC 3227 Group of galaxies, which is a member of the Leo II Groups, a series of galaxies and galaxy clusters strung out from the right edge of the Virgo Supercluster.

<span class="mw-page-title-main">NGC 1566</span> Galaxy in the constellation Dorado

NGC 1566, sometimes known as the Spanish Dancer, is an intermediate spiral galaxy in the constellation Dorado, positioned about 3.5° to the south of the star Gamma Doradus. It was discovered on May 28, 1826 by Scottish astronomer James Dunlop. At 10th magnitude, it requires a telescope to view. The distance to this galaxy remains elusive, with measurements ranging from 6 Mpc up to 21 Mpc.

<span class="mw-page-title-main">NGC 4921</span> Galaxy in the constellation Coma Berenices

NGC 4921 is a large barred spiral galaxy in the Coma Cluster, located in the constellation Coma Berenices. It was discovered by German-British astronomer William Herschel on 11 April 1785. It is about 320 million light-years from Earth. The galaxy has a nucleus with a bar structure that is surrounded by a distinct ring of dust that contains recently formed, hot blue stars. The outer part consists of unusually smooth, poorly distinguished spiral arms.

<span class="mw-page-title-main">Abell 2390</span> Galaxy cluster in the constellation Pegasus

Abell 2390 is a massive galaxy cluster located in the constellation Pegasus. It is classified as an X-ray and rich galaxy clusters measured cooling rate of 200-300 Mʘyr-1. The galaxy cluster contains a cD galaxy called Abell 2390 BCG, associated with a complex radio source, B2151+141.

<span class="mw-page-title-main">NGC 4550</span> Galaxy in the constellation Virgo

NGC 4550 is a barred lenticular galaxy located in the constellation of Virgo that can be seen with amateur telescopes. It lies at a distance of 50 million light-years from the Milky Way and is a member of the Virgo Cluster.

<span class="mw-page-title-main">NGC 5643</span> Galaxy in the constellation Lupus

NGC 5643 is an intermediate spiral galaxy in the constellation Lupus. Based on the tip of the red-giant branch distance indicator, it is located at a distance of about 40 million light-years. NGC 5643 has an active galactic nucleus and is a type II Seyfert galaxy.

<span class="mw-page-title-main">NGC 4111</span> Galaxy in constellation Canes Venatici

NGC 4111 is a lenticular galaxy in the constellation Canes Venatici. It is located at a distance of circa 50 million light-years from Earth, which, given its apparent dimensions, means that NGC 4111 is about 55,000 light-years across. It was discovered by William Herschel in 1788. NGC 4111 possesses both thin and thick discs.

<span class="mw-page-title-main">NGC 3941</span> Galaxy in the constellation Ursa Major

NGC 3941 is a barred lenticular galaxy located in the constellation Ursa Major. It is located at a distance of circa 40 million light years from Earth, which, given its apparent dimensions, means that NGC 3941 is about 40,000 light years across. It was discovered by William Herschel in 1787.

<span class="mw-page-title-main">NGC 7469</span> Galaxy located in the constellation Pegasus

NGC 7469 is an intermediate spiral galaxy in the constellation of Pegasus. NGC 7469 is located about 200 million light-years away from Earth, which means, given its apparent dimensions, that NGC 7469 is approximately 90,000 light-years across. It was discovered by William Herschel on November 12, 1784.

<span class="mw-page-title-main">NGC 5965</span> Spiral galaxy in the constellation Draco

NGC 5965 is a spiral galaxy located in the constellation Draco. It is located at a distance of circa 150 million light years from Earth, which, given its apparent dimensions, means that NGC 5965 is about 260,000 light years across. It was discovered by William Herschel on May 5, 1788.

<span class="mw-page-title-main">NGC 4665</span> Galaxy in the constellation of Virgo

NGC 4665, also catalogued as NGC 4624 and NGC 4664, is a barred lenticular or spiral galaxy located in the constellation Virgo. It is a member of the Virgo II Groups, a series of galaxies and galaxy clusters strung out from the southern edge of the Virgo Supercluster. It is located at a distance of circa 60 million light years from Earth, which, given its apparent dimensions, means that NGC 4665 is about 75,000 light years across. NGC 4665 lies 2 and 3/4 degrees east-south east of Delta Virginis and 50 arcminutes southwest of 35 Virginis. It can be viewed through a moderately sized telescope with 23x magnification, forming a pair with an 11th magnitude star 1.5 arcminutes southwest. It is part of the Herschel 400 Catalogue.

<span class="mw-page-title-main">NGC 4636</span> Galaxy in the constellation Virgo

NGC 4636 is an elliptical galaxy located in the constellation Virgo. It is a member of the NGC 4753 Group of galaxies, which is a member of the Virgo II Groups, a series of galaxies and galaxy clusters strung out from the southern edge of the Virgo Supercluster. It is located at a distance of about 55 million light years from Earth, which, given its apparent dimensions, means that NGC 4636 is about 105,000 light years across.

<span class="mw-page-title-main">NGC 5846</span> Galaxy in the constellation Virgo

NGC 5846 is an elliptical galaxy located in the constellation Virgo. It is located at a distance of circa 90 million light years from Earth, which, given its apparent dimensions, means that NGC 5846 is about 110,000 light years across. It was discovered by William Herschel on February 24, 1786. It lies near 110 Virginis and is part of the Herschel 400 Catalogue. It is a member of the NGC 5846 Group of galaxies, itself one of the Virgo III Groups strung out to the east of the Virgo Supercluster of galaxies.

<span class="mw-page-title-main">NGC 4278</span> Galaxy in the constellation Coma Berenices

NGC 4278 is an elliptical galaxy located in the constellation Coma Berenices. It is located at a distance of circa 55 million light years from Earth, which, given its apparent dimensions, means that NGC 4278 is about 65,000 light years across. It was discovered by William Herschel on March 13, 1785. NGC 4278 is part of the Herschel 400 Catalogue and can be found about one and 3/4 of a degree northwest of Gamma Comae Berenices even with a small telescope.

<span class="mw-page-title-main">NGC 4076</span> Galaxy in the constellation Coma Berenices

NGC 4076 is a spiral galaxy located 290 million light-years away in the constellation Coma Berenices. The galaxy was discovered by astronomer William Herschel on April 27, 1785 and is a member of the NGC 4065 Group.

<span class="mw-page-title-main">NGC 4298</span> Galaxy in the constellation Coma Berenices

NGC 4298 is a flocculent spiral galaxy located about 53 million light-years away in the constellation Coma Berenices. The galaxy was discovered by astronomer William Herschel on April 8, 1784 and is a member of the Virgo Cluster.

<span class="mw-page-title-main">NGC 4302</span> Galaxy in the constellation Coma Berenices

NGC 4302 is an edge-on spiral galaxy located about 55 million light-years away in the constellation Coma Berenices. It was discovered by astronomer William Herschel on April 8, 1784 and is a member of the Virgo Cluster.

<span class="mw-page-title-main">NGC 4325</span> Galaxy

NGC 4325 is an elliptical galaxy located about 330 million light-years away in the constellation Virgo. It was discovered by astronomer Heinrich d'Arrest on April 15, 1865, who described it as "vF, vS, iR, nf of 2". Despite being listed in the Virgo Cluster catalog as VCC 616, it is not a member of the Virgo Cluster but instead a background galaxy.

References

The location of NGC 1275 (circled in red) NGC1275Location.png
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 19 November 2006.
  2. 1 2 "Distance Results for NGC 1275". NASA/IPAC Extragalactic Database. Retrieved 31 March 2010.
  3. ↑ Ho LC, Filippenko AV, Sargent WL (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). "Optical investigations of radio sources (Introductory Lecture)". Radio Astronomy. 4: 107. Bibcode:1957IAUS....4..107M.
  5. ↑ Gillmon K, Sanders JS, Fabian AC (2003). "An X-ray absorption analysis of the high-velocity system in NGC 1275". Monthly Notices of the Royal Astronomical Society. 348: 159–164. arXiv: astro-ph/0310784 . doi: 10.1111/j.1365-2966.2004.07336.x .
  6. ↑ Gallagher JS, Lee M, Canning R, Fabian A, O'Connell RW, Sanders J, et al. (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 (March 1970). "Improved Photographs of the NGC 1275 Phenomenon". The Astrophysical Journal. 159: L151. Bibcode:1970ApJ...159L.151L. doi:10.1086/180500. ISSN   0004-637X.
  8. ↑ Hatch NA, Crawford CS, Fabian AC, Johnstone RM (2005). "On the origin and excitation of the extended nebula surrounding NGC 1275". Monthly Notices of the Royal Astronomical Society. 367 (2): 433–448. arXiv: astro-ph/0512331 . doi: 10.1111/j.1365-2966.2006.09970.x . ISSN   0035-8711.
  9. ↑ "Hubble Sees Magnetic Monster in Erupting Galaxy". Newswise. 20 August 2008. Retrieved 21 August 2008.
  10. 1 2 Fabian AC, Johnstone RM, Sanders JS, Conselice CJ, Crawford CS, Gallagher JS, et al. (21 August 2008). "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 K (21 August 2008). "Hubble Images Solve Galactic Filament Mystery". The New York Times .
  12. ↑ Lim J, Ao YP, Dinh-v-Trung DV (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 R (2007). "Star Formation in the Perseus Cluster Cooling Flow". HST Proposal ID #11207. Cycle 16: 11207. Bibcode:2007hst..prop11207O.
  14. ↑ Wilman RJ, Edge AC, Johnstone RM (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 PJ, Dopita MA, Beck TL (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. ↑ Marsden BG (29 January 1968). "Circular No. 2051". Central Bureau for Astronomical Telegrams. Smithsonian Astrophysical Observatory. Retrieved 2 December 2024.
  17. ↑ "SN 1968A". Transient Name Server. IAU . Retrieved 29 March 2023.
  18. ↑ Luckas P, Trondal O, Schwartz M, Newton J, Puckett T, Peoples M, et al. (2006). "Supernovae 2005my, 2005mz, 2005na". International Astronomical Union Circular (8655): 1. Bibcode:2006IAUC.8655....1L.
  19. ↑ "SN 2005mz". Transient Name Server. IAU . Retrieved 29 March 2023.
  20. ↑ "SN 2024xav". Transient Name Server. IAU . Retrieved 28 August 2024.
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