NGC 6051

Last updated
NGC 6051
NGC6051 - SDSS DR14.jpg
SDSS image of NGC 6051.
Observation data (J2000 epoch)
Constellation Serpens
Right ascension 16h 04m 56.6s
Declination +23° 55′ 57.7″
Redshift 0.031404
Heliocentric radial velocity 9,415 Km/s
Distance 453 Mly (138.8 Mpc)
Group or cluster AWM 4
Apparent magnitude  (V)0.19
Apparent magnitude  (B)0.26
Surface brightness 13.71
Characteristics
Type cD; E
Size250,000 ly (approximately 76.65 kpc)
Apparent size  (V)1.3' x 0.9'
Other designations
PGC 57006, UGC 10178, 4C +24.36, MCG +04-38-021, GIN 487

NGC 6051 is a giant elliptical galaxy located in the constellation of Serpens. The galaxy lies 453 million light-years from Earth, which means given its apparent dimensions, the galaxy is around 250,000 light-years across. [1] It is the brightest cluster galaxy inside a relaxed poor cluster called AWM 4, a fossil system, [2] making up of at least 30 galaxy members. [3]

Contents

Observational history

NGC 6051 was discovered by Edouard Stephan on June 20, 1881. According to John Louis Emil Dreyer, he described it as faint small round object with a bright middle nucleus and a 10th magnitude star to southeast. [4] SIMBAD and Hyperleda databases listed NGC 6051 as IC 4588, [5] [6] but according to Harold Corwin, these galaxies are two separate objects. [7] O'Sullivan and associates (2011) have them as separate entities, with NGC 6051 being the central dominant galaxy of a cluster. [8]

Characteristics

NGC 6051 is a Type cD galaxy. [9] It is much more luminous compared to other galaxies in AWM 4, [10] with a law surface brightness profile, [3] but does not have a stellar envelope. [11]

The nucleus in NGC 6051 is considered active and it is a radio galaxy. [12] It is classified as a Fanaroff-Riley class hybrid transition of Type I and Type II. Hosting a wide-angle tailed powerful radio source, [13] [14] NGC 6051 contains two reflection-symmetrical wiggled radio jets and large radio lobes emerging from its radio core by ~ 80 kiloparsecs (kpc). [15] The most accepted theory for this active galactic nuclei (AGN) activity, is the presence of a supermassive black hole. The mass of the black hole in NGC 6051 is estimated to be 9.57 ± 0.02 M⊙ based on the MBH - MK correlation. [16]

According to the jet to counterjet brightness ratio, the central ~ 10 kpc jet region of NGC 6051 is potentially orientated closer to the plane of the sky. From the analysis of gradually steepening spectral index, the jets and lobes have an estimated lifetime of 160 million years old. This indicates the source of NGC 6051 is old. [15] [13]

A study has found traces of iron inside the entrained gas produced from the central region of NGC 6051, with a mass of ~1.4 x 106 M⊙. With the energy amount of ~4.5 x 1057 erg, the gas might been transported out from the galaxy by its jets, to a certain extent of enriching the intracluster medium. [14]

See also

Related Research Articles

<span class="mw-page-title-main">NGC 1275</span> Seyfert galaxy in the constellation Perseus

NGC 1275 is a type 1.5 Seyfert galaxy located around 237 million light-years away in the direction of the constellation Perseus. NGC 1275 is a member of the large Perseus Cluster of galaxies.

<span class="mw-page-title-main">Somak Raychaudhury</span> Indian astrophysicist

Somak Raychaudhury is an Indian astrophysicist. He is the Vice-Chancellor at Ashoka University and was the Director of the Inter-University Centre for Astronomy and Astrophysics (IUCAA), Pune. He is on leave from Presidency University, Kolkata, India, where he is a Professor of Physics, and is also affiliated to the University of Birmingham, United Kingdom. He is known for his work on stellar mass black holes and supermassive black holes. His significant contributions include those in the fields of gravitational lensing, galaxy dynamics and large-scale motions in the Universe, including the Great Attractor.

<span class="mw-page-title-main">NGC 1407</span> Elliptical galaxy in the constellation Eridanus

NGC 1407 is an elliptical galaxy in Eridanus. It is at a distance of 76 million light-years from Earth. It is the brightest galaxy in the NGC 1407 Group, part of the Eridanus Group, with NGC 1407 being its brightest member. NGC 1400, the second-brightest of the group lies 11.8 arcmin away.

<span class="mw-page-title-main">NGC 4570</span> Galaxy in the constellation Virgo

NGC 4570 is an edge-on lenticular galaxy located about 57 million light-years away in the constellation Virgo. NGC 4570 was discovered by astronomer William Herschel on April 13, 1784 and is a member of the Virgo Cluster.

<span class="mw-page-title-main">NGC 708</span> Galaxy in the constellation Andromeda

NGC 708 is an elliptical galaxy located 240 million light-years away in the constellation Andromeda and was discovered by astronomer William Herschel on September 21, 1786. It is classified as a cD galaxy and is the brightest member of Abell 262. NGC 708 is a weak FR I radio galaxy and is also classified as a type 2 Seyfert galaxy.

<span class="mw-page-title-main">NGC 741</span> Formerly active radio galaxy in the constellation of Pisces

NGC 741, also known as PGC 7252, is a formerly active radio galaxy in the constellation of Pisces. Located 74.13 Mpc away, NGC 741 is part of a group of galaxies including NGC 742 and PGC 7250. NGC 741 and NGC 742 recently collided, although the disruption was minor. Radio filaments have been found connecting NGC 741 to NGC 742, and due to the bent structure of the radio filaments, NGC 741 is estimated to be moving at 1400 km/s with respect to its local group, suggesting that ram-pressure stripping was created as a product of the former merger.

<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 4061</span> Galaxy in the constellation Coma Berenices

NGC 4061 is an elliptical galaxy located 310 light-years away in the constellation Coma Berenices. It was discovered by astronomer William Herschel on April 27, 1785. It was rediscovered by John Herschel on April 29, 1832. It is listed both as NGC 4061 and NGC 4055. NGC 4061 is a member of the NGC 4065 Group and forms an interacting pair with its companion, NGC 4065 as evidenced by distortions in their optical isophotes.

<span class="mw-page-title-main">NGC 4065</span> Galaxy in the constellation Coma Berenices

NGC 4065 is an elliptical galaxy located 300 million light-years away in the constellation Coma Berenices. The galaxy was discovered by astronomer William Herschel on April 27, 1785. It was then rediscovered by John Herschel on April 29, 1832 and was listed as NGC 4057. NGC 4065 is the brightest member of the NGC 4065 Group.

<span class="mw-page-title-main">NGC 4070</span> Galaxy in the constellation Coma Berenices

NGC 4070 is an elliptical galaxy located 340 million light-years away in the constellation Coma Berenices. NGC 4070 was discovered by astronomer William Herschel on April 27, 1785. It was rediscovered by John Herschel on April 29, 1832 and was listed as NGC 4059. The galaxy is a member of the NGC 4065 Group.

<span class="mw-page-title-main">NGC 4074</span> Galaxy in the constellation Coma Berenices

NGC 4074 is a peculiar lenticular galaxy located 310 million light-years away in the constellation Coma Berenices. It 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 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 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">NeVe 1</span> Galaxy in the constellation Ophiuchus

NeVe 1 is a supergiant elliptical galaxy, which is the central, dominant member and brightest cluster galaxy (BCG) of the Ophiuchus Cluster. It lies at a distance of about 411 million light-years away from Earth and is located behind the Zone of Avoidance region in the sky. It is the host galaxy of the Ophiuchus Supercluster eruption, the most energetic astronomical event known.

<span class="mw-page-title-main">NGC 4324</span> Galaxy in the constellation of Virgo

NGC 4324 is a lenticular galaxy located about 85 million light-years away in the constellation Virgo. It was discovered by astronomer Heinrich d'Arrest on March 4, 1862. NGC 4324 has a stellar mass of 5.62 × 1010M☉, and a baryonic mass of 5.88 × 1010M☉. The galaxy's total mass is around 5.25 × 1011M☉. NGC 4324 is notable for having a ring of star formation surrounding its nucleus. It was considered a member of the Virgo II Groups until 1999, when its distance was recalculated and it was placed in the Virgo W Group.

<span class="mw-page-title-main">4C+55.16</span> Seyfert 2 galaxy in the constellation Ursa Major

4C+55.16 is an elliptical galaxy, classified type E, located in Ursa Major. The galaxy lies about 2.84 billion light-years from Earth, which means given its apparent dimensions, 4C+55.16 is approximately 445,000 light-years across making it a type-cD galaxy. It is the brightest cluster galaxy (BCG) in a cluster of the same name.

<span class="mw-page-title-main">IRAS 09104+4109</span> Galaxy in the constellation Lynx

IRAS 09104+4109 is a galaxy located in the constellation Lynx. With a redshift of 0.440797, the light travel time for this galaxy, corresponds to 4.8 billion light-years from Earth. It is the brightest cluster galaxy in MACS J0913.7+4056 galaxy cluster and classified as a hyperluminous infrared galaxy.

<span class="mw-page-title-main">MRC 2011-298</span> Brightest cluster galaxy in the constellation Sagittarius

MRC 2011-298 is an elliptical galaxy with an active galactic nucleus, located in the constellation of Sagittarius. It is located 2.1 billion light-years away from Earth. MRC 2011-298 is the brightest cluster galaxy in the galaxy cluster, Abell 3670 and classfied as a dumbbell galaxy, an optical system with two galactic nuclei separated by 7″, corresponding to ≃17 kpc according to the adopted cosmology, with similar magnitude and a common stellar halo. The galaxy is known to have an ellipticity of ε = 0.28 and a position angle of PA  =  24° that is measured from north to east.

<span class="mw-page-title-main">Abell 2219 BCG</span> Brightest cluster galaxy in the constellation Hercules

Abell 2219 BCG, also known as LEDA 2285869, is a massive type-cD elliptical galaxy residing as the brightest cluster galaxy (BCG) in the Abell 2219 galaxy cluster located in constellation Hercules. At the redshift of 0.224, the galaxy is around 2.7 billion light-years from Earth.

<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

  1. ↑ "NED Search Results for NGC 6051". ned.ipac.caltech.edu. Retrieved 2024-09-07.
  2. ↑ Zibetti, Stefano; Pierini, Daniele; Pratt, Gabriel W. (2009-01-11). "Are fossil groups a challenge of the cold dark matter paradigm?". Monthly Notices of the Royal Astronomical Society. 392 (2): 525–536. arXiv: 0809.2036 . Bibcode:2009MNRAS.392..525Z. doi: 10.1111/j.1365-2966.2008.14098.x . ISSN   0035-8711.
  3. 1 2 O'Sullivan, E.; Vrtilek, J. M.; Kempner, J. C.; David, L. P.; Houck, J. C. (2005-03-11). "AWM 4 - an isothermal cluster observed with XMM-Newton". Monthly Notices of the Royal Astronomical Society. 357 (4): 1134–1150. arXiv: astro-ph/0412430 . Bibcode:2005MNRAS.357.1134O. doi: 10.1111/j.1365-2966.2005.08749.x . ISSN   0035-8711.
  4. ↑ "New General Catalog Objects: NGC 6050 - 6099". cseligman.com. Retrieved 2024-09-07.
  5. ↑ "NGC 6051". simbad.u-strasbg.fr. Retrieved 2024-09-07.
  6. ↑ "Hyperleda results for NGC 6051". archive.wikiwix.com. Retrieved 2024-09-07.
  7. ↑ "Corwin's description on IC 4588". www.darkerview.com. Retrieved 2024-09-07.
  8. ↑ O'Sullivan, Ewan; et al. (March 2011). "A deep Chandra observation of the poor cluster AWM 4 - II. The role of the radio jets in enriching the intracluster medium". Monthly Notices of the Royal Astronomical Society. 411 (3): 1833–1842. arXiv: 1010.0610 . Bibcode:2011MNRAS.411.1833O. doi: 10.1111/j.1365-2966.2010.17812.x .
  9. ↑ Rebusco, P.; Churazov, E.; Bohringer, H.; Forman, W. (2006-11-11). "Effect of turbulent diffusion on iron abundance profiles". Monthly Notices of the Royal Astronomical Society. 372 (4): 1840–1850. arXiv: astro-ph/0608491 . Bibcode:2006MNRAS.372.1840R. doi: 10.1111/j.1365-2966.2006.10977.x . ISSN   0035-8711.
  10. ↑ Gastaldello, Fabio; Buote, David A.; Brighenti, Fabrizio; Mathews, William G.; Temi, Pasquale; Ettori, Stefano; Heinz, Sebastian; Wilcots, Eric (2009). "AGN Feedback in Galaxy Groups: The Two Interesting Cases of AWM 4 and NGC 5044". AIP Conference Proceedings. 1201. AIP: 237–240. arXiv: 0909.0600 . Bibcode:2009AIPC.1201..237G. doi:10.1063/1.3293045.
  11. ↑ Schombert, James M. (August 1987). "The structure of brightest cluster members. II - Mergers". The Astrophysical Journal Supplement Series. 64: 643. Bibcode:1987ApJS...64..643S. doi:10.1086/191212. ISSN   0067-0049.
  12. ↑ Velzen, Sjoert van; Falcke, Heino; Schellart, Pim; Nierstenhöfer, Nils; Kampert, Karl-Heinz (2012-08-01). "Radio galaxies of the local universe - All-sky catalog, luminosity functions, and clustering". Astronomy & Astrophysics. 544: A18. arXiv: 1206.0031 . Bibcode:2012A&A...544A..18V. doi:10.1051/0004-6361/201219389. ISSN   0004-6361.
  13. 1 2 Giacintucci, Simona; Vrtilek, Jan M.; Murgia, Matteo; Raychaudhury, Somak; O'Sullivan, Ewan J.; Venturi, Tiziana; David, Laurence P.; Mazzotta, Pasquale; Clarke, Tracy E.; Athreya, Ramana M. (2008-07-01). "A Giant Metrewave Radio Telescope Multifrequency Radio Study of the Isothermal Core of the Poor Galaxy Cluster AWM 4". The Astrophysical Journal. 682 (1): 186–198. arXiv: 0804.1906 . Bibcode:2008ApJ...682..186G. doi:10.1086/589280. ISSN   0004-637X.
  14. 1 2 O’Sullivan, Ewan; Giacintucci, Simona; David, Laurence P.; Vrtilek, Jan M.; Raychaudhury, Somak (2010-11-17). "A deep Chandra observation of the poor cluster AWM 4 - II. The role of the radio jets in enriching the intracluster medium". Monthly Notices of the Royal Astronomical Society. 411 (3): 1833–1842. doi: 10.1111/j.1365-2966.2010.17812.x . ISSN   0035-8711.
  15. 1 2 Giacintucci, Simona; O’Sullivan, Ewan; Vrtilek, Jan; David, Laurence P.; Raychaudhury, Somak; Venturi, Tiziana; Athreya, Ramana M.; Clarke, Tracy E.; Murgia, Matteo; Mazzotta, Pasquale; Gitti, Myriam; Ponman, Trevor; Ishwara-Chandra, C. H.; Jones, Christine; Forman, William R. (2011-04-21). "A COMBINED LOW-RADIO FREQUENCY/X-RAY STUDY OF GALAXY GROUPS. I. GIANT METREWAVE RADIO TELESCOPE OBSERVATIONS AT 235 MHz AND 610 MHz". The Astrophysical Journal. 732 (2): 95. arXiv: 1103.1364 . Bibcode:2011ApJ...732...95G. doi:10.1088/0004-637x/732/2/95. ISSN   0004-637X.
  16. ↑ Mezcua, M.; Hlavacek-Larrondo, J.; Lucey, J. R.; Hogan, M. T.; Edge, A. C.; McNamara, B. R. (2017-10-30). "The most massive black holes on the Fundamental Plane of black hole accretion". Monthly Notices of the Royal Astronomical Society. 474 (1): 1342–1360. doi: 10.1093/mnras/stx2812 . ISSN   0035-8711.
This page is based on this Wikipedia article
Text is available under the CC BY-SA 4.0 license; additional terms may apply.
Images, videos and audio are available under their respective licenses.