NGC 5506

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NGC 5506
Ngc5506-hst-606.png
NGC 5506 by the Hubble Space Telescope
Observation data (J2000 epoch)
Constellation Virgo
Right ascension 14h 13m 14.9s [1]
Declination −03° 12′ 27″ [1]
Redshift 0.006084 ± 0.000009 [1]
Heliocentric radial velocity 1,824 ± 3 km/s [1]
Distance 77 ± 15 Mly (23.6 ± 4.6 Mpc) [1]
Apparent magnitude  (V)11.9
Characteristics
Type Sa pec sp [1]
Apparent size  (V)3.16′ × 0.75′ [1]
Notable featuresSeyfert galaxy
Other designations
UGCΑ 387, MRK 1376, MCG +00-36-028, PGC 50782 [1]

NGC 5506 is a spiral galaxy located in the constellation Virgo. It is located at a distance of about 75 million light years from Earth, which, given its apparent dimensions, means that NGC 5506 is about 80,000 light years across. [1] It was discovered by William Herschel on April 15, 1787. [2] It is a Seyfert galaxy. [1]

Contents

Characteristics

NGC 5506 is a spiral galaxy seen edge-on, with dust lanes visible south of the nucleus. [3]

Active nucleus

The nucleus of NGC 5506 has been found to be active and it has been categorised as a narrow line type I Seyfert galaxy, and is the brightest such nucleus. [4] The classification of the active nucleus had been an issue of debate, as it lacked broad emission lines in the visual wavelength. However, broader lines were observed in the infrared, [5] indicating that the broad line region is obscured in visual light. [4]

The most accepted theory for the energy source of active galactic nuclei is the presence of an accretion disk around a supermassive black hole. The mass of the black hole in the centre of NGC 5506 is estimated to be 8.8×107  M☉ based on stellar velocity dispersion and 5.1×106 M☉ based on the MBH–σ⋆ relation and X-ray variability. [6]

NGC 5506 is a bright X-ray source, detected by all X-ray space observatories, starting with Uhuru. [7] The X-ray spectrum indicates that there is both a compton-thick and a compton-thin absorber. The compton-thick absorber is a dust torus around the supermassive black hole at a distance of around one parsec, while the compton thin absorbs the softer X-rays emitted by the nucleus. [7] The soft emission by the nucleus extends to a distance of about 350 pc and is attributed to reflection of the nuclear emission by photoionized gas. [7] The inclination of the accretion disk is estimated to be between 40° and 50°. [8] The iron line is complex, indicating emission by neutral and ionised iron. [9] A broad component of the Fe Kα fluorescent emission line was observed by XMM-Newton. [10]

The galaxy also emits radiowaves. The galaxy exhibits a central source that accounts for 75% of the total emission and diffuse wing-like emission towards the north-west and east of the nucleus and a low-surface-brightness halo measuring 2.75 arcseconds in diameter that surrounds these features. [11] The features have no clear axis of symmetry. [12] The galaxy has been found to host an H2O megamaser. [13]

Nearby galaxies

NGC 5506 is the foremost galaxy in a galaxy group known as the NGC 5506 Group. Other members of the group include NGC 5507, while IC 978 lies a bit farther away. [14] Garcia identified as members of group also the galaxies NGC 5496, and UGC 9057. [15] NGC 5506 forms a pair with NGC 5507, which lies 4 arcminutes from it. [16] The group is part of the Virgo III Groups, a very obvious chain of galaxy groups on the left side of the Virgo cluster, stretching across 40 million light years of space. [17]

Related Research Articles

<span class="mw-page-title-main">Seyfert galaxy</span> Class of active galaxies with very bright nuclei

Seyfert galaxies are one of the two largest groups of active galaxies, along with quasar host galaxies. They have quasar-like nuclei with very high surface brightnesses whose spectra reveal strong, high-ionisation emission lines, but unlike quasars, their host galaxies are clearly detectable.

<span class="mw-page-title-main">Messier 88</span> Galaxy in the constellation Coma Berenices

Messier 88 is a spiral galaxy about 50 to 60 million light-years away from Earth in the constellation Coma Berenices. It was discovered by Charles Messier in 1781.

<span class="mw-page-title-main">NGC 5548</span> Type I Seyfert galaxy in the constellation Boötes

NGC 5548 is a Type I Seyfert galaxy with a bright, active nucleus. This activity is caused by matter flowing onto a 65 million solar mass (M☉) supermassive black hole at the core. Morphologically, this is an unbarred lenticular galaxy with tightly-wound spiral arms, while shell and tidal tail features suggest that it has undergone a cosmologically-recent merger or interaction event. NGC 5548 is approximately 245 million light years away and appears in the constellation Boötes. The apparent visual magnitude of NGC 5548 is approximately 13.3 in the V band.

<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 2992</span> Seyfert galaxy in the constellation Hydra

NGC 2992 is a Seyfert galaxy located 103 million light years distant in the equatorial constellation of Hydra. It was discovered in 1785 by Anglo-German astronomer William Herschel.

<span class="mw-page-title-main">NGC 3147</span> Galaxy in the constellation Draco

NGC 3147 is a spiral galaxy located in the constellation Draco. It is located at a distance of about 130 million light years from Earth, which, given its apparent dimensions, means that NGC 3147 is about 140,000 light years across. It was discovered by William Herschel on April 3, 1785.

<span class="mw-page-title-main">NGC 4939</span> Spiral galaxy in the constellation Virgo

NGC 4939 is a large spiral galaxy located in the constellation Virgo. It is located at a distance of about 120 million light years from Earth, which, given its apparent dimensions, means that NGC 4939 is about 190,000 light years across. It was discovered by William Herschel on March 25, 1786.

<span class="mw-page-title-main">NGC 985</span> Ring galaxy in the constellation Cetus

NGC 985 is a ring galaxy in the constellation of Cetus. It is located about 550 million light years away from Earth, which means, given its apparent dimensions, that NGC 985 is approximately 160,000 light years across. It was discovered by Francis Leavenworth in 1886. It is a type 1 Seyfert galaxy.

<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 1386</span> Galaxy in the constellation Eridanus

NGC 1386 is a spiral galaxy located in the constellation Eridanus. It is located at a distance of circa 53 million light years from Earth, which, given its apparent dimensions, means that NGC 1386 is about 50,000 light years across. It is a Seyfert galaxy, the only one in Fornax Cluster.

<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 5363</span> Galaxy in the constellation Virgo

NGC 5363 is a lenticular galaxy located in the constellation Virgo. It is located at a distance of circa 65 million light years from Earth, which, given its apparent dimensions, means that NGC 5363 is about 100,000 light years across. It was discovered by William Herschel on January 19, 1784. It is a member of the NGC 5364 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 2273</span> Galaxy in the constellation Lynx

NGC 2273 is a barred spiral galaxy located in the constellation Lynx. It is located at a distance of circa 95 million light years from Earth, which, given its apparent dimensions, means that NGC 2273 is about 100,000 light years across. It was discovered by Nils Dunér on September 15, 1867.

<span class="mw-page-title-main">NGC 7679</span> Galaxy in the constellation Pisces

NGC 7679 is a lenticular galaxy with a peculiar morphology in the constellation Pisces. It is located at a distance of about 200 million light years from Earth, which, given its apparent dimensions, means that NGC 7679 is about 60,000 light years across. It was discovered by Heinrich d'Arrest on September 23, 1864. The total infrared luminosity is 1011.05 L☉, and thus it is categorised as a luminous infrared galaxy. NGC 7679 is both a starburst galaxy and a Seyfert galaxy.

<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">NGC 7172</span> Galaxy in the constellation of Piscis Austrinus

NGC 7172 is a spiral galaxy located in the constellation Piscis Austrinus. It is located at a distance of about 110 million light years from Earth, which, given its apparent dimensions, means that NGC 7172 is about 100,000 light years across. It was discovered by John Herschel on September 23, 1834.

<span class="mw-page-title-main">NGC 3516</span> Galaxy in the constellation of Ursa Major

NGC 3516 is a barred lenticular galaxy in the constellation of Ursa Major. NGC 3516 is located about 150 million light years away from Earth, which means, given its apparent dimensions, that NGC 3516 is approximately 100,000 light years across. It was discovered by William Herschel on April 3, 1785.

<span class="mw-page-title-main">NGC 5252</span> Galaxy in the constellation of Virgo

NGC 5252 is a lenticular galaxy located in the constellation Virgo. It is located at a distance of about 220 to 320 million light years from Earth, which, given its apparent dimensions, means that NGC 5252 is about 100,000 light years across. It was discovered by William Herschel on February 2, 1786.

<span class="mw-page-title-main">NGC 2110</span> Galaxy in the constellation Orion

NGC 2110 is a lenticular galaxy located in the constellation Orion. It is located at a distance of about 120 million light years from Earth, which, given its apparent dimensions, means that NGC 2110 is about 90,000 light years across. It was discovered by William Herschel on October 5, 1785. It is a Seyfert galaxy.

<span class="mw-page-title-main">IRAS 19254-7245</span> Galaxy in the constellation Pavo

IRAS 19254-7245, more commonly referred as the "Superantennae", are a pair of interacting galaxies located in the constellation of Pavo. It is located 820 million light years from Earth. It is an ultraluminous infrared galaxy and a Seyfert galaxy.

References

  1. 1 2 3 4 5 6 7 8 9 10 "NASA/IPAC Extragalactic Database". Results for NGC 5506. Retrieved 2023-05-06.
  2. ↑ Seligman, Courtney. "NGC 5506". Celestial Atlas. Retrieved 19 November 2018.
  3. ↑ Martini, Paul; Regan, Michael W.; Mulchaey, John S.; Pogge, Richard W. (June 2003). "Circumnuclear Dust in Nearby Active and Inactive Galaxies. I. Data". The Astrophysical Journal Supplement Series. 146 (2): 353–406. Bibcode:2003ApJS..146..353M. doi: 10.1086/367817 .
  4. 1 2 Nagar, N. M.; Oliva, E.; Marconi, A.; Maiolino, R. (August 2002). "NGC 5506 unmasked as a Narrow Line Seyfert 1:: A direct view of the broad line region using near-IR spectroscopy". Astronomy & Astrophysics. 391 (2): L21 –L24. arXiv: astro-ph/0207432 . Bibcode:2002A&A...391L..21N. doi: 10.1051/0004-6361:20021039 .
  5. ↑ Goodrich, Robert W.; Veilleux, Sylvain; Hill, Gary J. (February 1994). "Infrared spectroscopy of Seyfert 2 galaxies: A look through the obscuring Torus?". The Astrophysical Journal. 422: 521. Bibcode:1994ApJ...422..521G. doi: 10.1086/173746 .
  6. ↑ Nikołajuk, M.; Czerny, B.; Gurynowicz, P. (21 April 2009). "NLS1 galaxies and estimation of their central black hole masses from the X-ray excess variance method". Monthly Notices of the Royal Astronomical Society. 394 (4): 2141–2152. arXiv: 0901.1442 . Bibcode:2009MNRAS.394.2141N. doi: 10.1111/j.1365-2966.2009.14478.x .
  7. 1 2 3 Bianchi, S.; Balestra, I.; Matt, G.; Guainazzi, M.; Perola, G. C. (April 2003). "The recent X–ray history of NGC 5506". Astronomy & Astrophysics. 402 (1): 141–149. arXiv: astro-ph/0302349 . Bibcode:2003A&A...402..141B. doi: 10.1051/0004-6361:20030210 .
  8. ↑ Sun, Shangyu; Guainazzi, Matteo; Ni, Qingling; Wang, Jingchun; Qian, Chenyang; Shi, Fangzheng; Wang, Yu; Bambi, Cosimo (1 August 2018). "Multi-epoch analysis of the X-ray spectrum of the active galactic nucleus in NGC 5506". Monthly Notices of the Royal Astronomical Society. 478 (2): 1900–1910. arXiv: 1704.03716 . doi: 10.1093/mnras/sty1233 .
  9. ↑ Matt, G.; Guainazzi, M.; Perola, G. C.; Fiore, F.; Nicastro, F.; Cappi, M.; Piro, L. (October 2001). "The complex iron line of NGC 5506". Astronomy & Astrophysics. 377 (3): L31 –L34. arXiv: astro-ph/0108508 . Bibcode:2001A&A...377L..31M. doi: 10.1051/0004-6361:20011209 .
  10. ↑ Guainazzi, M.; Bianchi, S.; Matt, G.; Dadina, M.; Kaastra, J.; Malzac, J.; Risaliti, G. (June 2010). "Final verdict from XMM-Newton: the X-ray obscured Seyfert galaxy NGC 5506 has a broad Fe Kα line: Broad Kα Fe line in NGC 5506". Monthly Notices of the Royal Astronomical Society: no. arXiv: 1004.1442 . doi: 10.1111/j.1365-2966.2010.16805.x .
  11. ↑ Orienti, M.; Prieto, M. A. (1 February 2010). "Radio structures of the nuclei of nearby Seyfert galaxies and the nature of the missing diffuse emission". Monthly Notices of the Royal Astronomical Society. 401 (4): 2599–2610. arXiv: 0911.0852 . Bibcode:2010MNRAS.401.2599O. doi: 10.1111/j.1365-2966.2009.15837.x .
  12. ↑ Middelberg, E.; Roy, A. L.; Nagar, N. M.; Krichbaum, T. P.; Norris, R. P.; Wilson, A. S.; Falcke, H.; Colbert, E. J. M.; Witzel, A.; Fricke, K. J. (April 2004). "Motion and properties of nuclear radio components in Seyfert galaxies seen with VLBI". Astronomy & Astrophysics. 417 (3): 925–944. arXiv: astro-ph/0402142 . Bibcode:2004A&A...417..925M. doi: 10.1051/0004-6361:20040019 .
  13. ↑ Braatz, J. A.; Wilson, A. S.; Henkel, C. (December 1994). "The discovery of five new H2O megamasers in active galaxies". The Astrophysical Journal. 437: L99. Bibcode:1994ApJ...437L..99B. doi:10.1086/187692.
  14. ↑ Makarov, Dmitry; Karachentsev, Igor (21 April 2011). "Galaxy groups and clouds in the local (z~ 0.01) Universe". Monthly Notices of the Royal Astronomical Society. 412 (4): 2498–2520. arXiv: 1011.6277 . Bibcode:2011MNRAS.412.2498M. doi: 10.1111/j.1365-2966.2010.18071.x . S2CID   119194025.
  15. ↑ Garcia, A. M. (1 July 1993). "General study of group membership. II. Determination of nearby groups". Astronomy and Astrophysics Supplement Series. 100: 47–90. Bibcode:1993A&AS..100...47G. ISSN   0365-0138.
  16. ↑ de Vaucouleurs, G.; de Vaucouleurs, A.; Corwin, J. R. (1 January 1976). "Second reference catalogue of bright galaxies". Second Reference Catalogue of Bright Galaxies. 1976. Bibcode:1976RC2...C......0D.
  17. ↑ "The Virgo III Groups". www.atlasoftheuniverse.com. Retrieved 9 January 2019.
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