NGC 3516

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NGC 3516
NGC 3516.png
NGC 3516 by Hubble Space Telescope
Observation data (J2000 epoch)
Constellation Ursa Major
Right ascension 11h 06m 47.5s [1]
Declination +72° 34′ 07″ [1]
Redshift 0.008836 ± 0.000023 [1]
Heliocentric radial velocity 2649 ± 7 km/s [1]
Distance 165 ± 50 Mly (51.5 ± 15.1 Mpc) [1]
Apparent magnitude  (V)11.5 [2]
Characteristics
Type (R)SB(s)0^0^ [1]
Apparent size  (V)1.7′ × 1.3′ [1]
Notable featuresSeyfert galaxy
Other designations
UGC 6153, MCG +12-11-009, PGC 33623 [1]

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. [3]

Contents

Characteristics

In 1943, this galaxy was one of six nebulae listed by American astronomer Carl Keenan Seyfert that showed broad emission lines in their nuclei. [4] Members of this class of objects became known as Seyfert galaxies, and they were noted to have a higher than normal surface brightness in their nuclei. NGC 3516 is believed to host a supermassive black hole whose mass is estimated to be (4.27±1.46)×107 M☉ based on broad emission-line reverberation mapping [5] or 23000000M☉ as measured based on velocity dispersion. [6]

Due to its high brightness in both UV and X-rays, and its prominent and clear active galactic nucleus absorption features, it has been an ideal laboratory for studying the AGN warm-absorber outflows with high-resolution spectroscopy. Over the past few decades, there have been many UV and X-ray case studies of the ionized outflows in NGC 3516. [7] NGC 3516 has been a remarkably variable AGN, showing changes in both the intrinsic continuum [8] and the intrinsic absorption by the ionized outflows. [9] In 2014, the broad lines almost disappeared, probably becoming obstructed, and thus the galaxy has been identified as a changing-look AGN, meaning it changed spectra between type 1 and type 2 AGN. [10]

The galaxy has been found to emit radiowaves, with the source extending towards the north for about 0.65 arcseconds. [11] That structure is a bit curved and probably is related to the gaseous outflow. [12] A spiral dust feature measuring 3 arcseconds in diameter is visible north of the nucleus. A blue filamentary feature is visible northeast of the nucleus and another blue feature is visible 1.5 arcseconds southwest of the nucleus. [13]

Nearby galaxies

NGC 3516 is a relatively isolated galaxy. Near galaxies include NGC 3147 with its group that NGC 3155, UGC 5570, UGC 5686, and UGC 5689, NGC 3183, NGC 3348, and NGC 3364. [14] Garcia identified NGC 3516 as a member of group that also includes the galaxies NGC 3348, and NGC 3364. [15]

Related Research Articles

An active galactic nucleus (AGN) is a compact region at the center of a galaxy that emits a significant amount of energy across the electromagnetic spectrum, with characteristics indicating that the luminosity is not produced by stars. Such excess, non-stellar emissions have been observed in the radio, microwave, infrared, optical, ultra-violet, X-ray and gamma ray wavebands. A galaxy hosting an AGN is called an active galaxy. The non-stellar radiation from an AGN is theorized to result from the accretion of matter by a supermassive black hole at the center of its host galaxy.

<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 quasars. 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">NGC 3227</span> Galaxy in the constellation Leo

NGC 3227 is an intermediate spiral galaxy that is interacting with the dwarf elliptical galaxy NGC 3226. 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 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">Low-ionization nuclear emission-line region</span> Type of galactic nucleus

A low-ionization nuclear emission-line region (LINER) is a type of galactic nucleus that is defined by its spectral line emission. The spectra typically include line emission from weakly ionized or neutral atoms, such as O, O+, N+, and S+. Conversely, the spectral line emission from strongly ionized atoms, such as O++, Ne++, and He+, is relatively weak. The class of galactic nuclei was first identified by Timothy Heckman in the third of a series of papers on the spectra of galactic nuclei that were published in 1980.

<span class="mw-page-title-main">NGC 7319</span> Galaxy in the constellation Pegasus

NGC 7319 is a highly distorted barred spiral galaxy that is a member of the compact Stephan's Quintet group located in the constellation Pegasus, some 311 megalight-years distant from the Milky Way. The galaxy's arms, dust and gas have been highly disturbed as a result of the interaction with the other members of the Quintet. Nearly all of the neutral hydrogen has been stripped from this galaxy, most likely as a result of a collision with NGC 7320c some 100 million years ago. A pair of long, parallel tidal tails extend southward from NGC 7319 in the direction of NGC 7320c, and is undergoing star formation.

<span class="mw-page-title-main">Ionization cone</span> Astronomical phenomenon

Ionization cones are cones of ionized material extending from active galactic nuclei, predominantly observed in type II Seyfert galaxies. They are detected through their emission of electromagnetic radiation in the visible and infrared parts of the spectrum. The main method of observation is through spectroscopy, using spectral line analysis to measure the shape of the ionized region and the condition of the material such as temperature, density, composition, and degree of ionization.

<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 3367</span> Spiral galaxy in the constellation Leo

NGC 3367 is a barred spiral galaxy located in the constellation Leo. It is located at a distance of about 120 million light years from Earth, which, given its apparent dimensions, means that NGC 3367 is about 85,000 light years across. It was discovered by William Herschel on March 19, 1784.

<span class="mw-page-title-main">NGC 7213</span> Galaxy in the constellation Grus

NGC 7213 is a lenticular galaxy located in the constellation Grus. It is located at a distance of circa 70 million light-years from Earth, which, given its apparent dimensions, means that NGC 7213 is about 75,000 light-years across. It was discovered by John Herschel on September 30, 1834. It is an active galaxy with characteristics between a type I Seyfert galaxy and LINER.

<span class="mw-page-title-main">NGC 7130</span> Galaxy in the constellation Piscis Austrinus

NGC 7130 is a spiral galaxy located in the constellation Piscis Austrinus. It is located at a distance of about 220 million light years from Earth, which, given its apparent dimensions, means that NGC 7130 is about 100,000 light years across. It was discovered by John Herschel on September 25, 1834, and discovered independently by Lewis Swift on September 17, 1897. The location of the galaxy given in the New General Catalogue was off by 30 arcminutes in declination from the location of the galaxy.

<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 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 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 5728</span> Spiral galaxy in the constellation Libra

NGC 5728 is an active barred spiral galaxy located 146 million light years away in the southern constellation of Libra. It was discovered on May 7, 1787 by William Herschel. The designation comes from the New General Catalogue of J. L. E. Dreyer, published in 1888. It has an apparent visual magnitude of 13.40 and spans an angle of 3.4 arcminutes. The galaxy shows a red shift of 0.00935 and has a heliocentric radial velocity of 2,803 km/s. It has an estimated mass of 72 billion times the mass of the Sun and stretches around 30 kpc across.

<span class="mw-page-title-main">NGC 7592</span> Interacting galaxy system in the constellation Aquarius

NGC 7592 is an interacting galaxy system located 300 million light years away in the constellation Aquarius. It was discovered by William Herschel on September 20, 1784. The total infrared luminosity is 1011.33 L☉, and thus it is categorised as a luminous infrared galaxy. One of the galaxies hosts a type 2 Seyfert nucleus.

<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">Markarian 590</span> Galaxy in the constellation of Cetus

Markarian 590, also known as NGC 863, NGC 866, and NGC 885, is a spiral galaxy located in the constellation Cetus. It is located at a distance of about 300 million light years from Earth, which, given its apparent dimensions, means that NGC 863 is about 110,000 light years across. It is a change looking Seyfert galaxy.

<span class="mw-page-title-main">NGC 2110</span>

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">NGC 5135</span>

NGC 5135 is a barred spiral galaxy located in the constellation Hydra. It is located at a distance of about 200 million light years from Earth. It was discovered by John Herschel on May 8, 1834. It is a Seyfert galaxy.

References

  1. 1 2 3 4 5 6 7 8 "NASA/IPAC Extragalactic Database". Results for NGC 3516. Retrieved 2016-01-18.
  2. ↑ "Revised NGC Data for NGC 3516". spider.seds.org. Retrieved 25 November 2018.
  3. ↑ Seligman, Courtney. "NGC 3516". Celestial Atlas. Retrieved 19 November 2018.
  4. ↑ Seyfert, Carl K. (January 1943), "Nuclear Emission in Spiral Nebulae", Astrophysical Journal, 97: 28, Bibcode:1943ApJ....97...28S, doi:10.1086/144488.
  5. ↑ Peterson, Bradley M. (2013). "Measuring the Masses of Supermassive Black Holes" (PDF). Space Science Reviews. 183 (1–4): 253. Bibcode:2014SSRv..183..253P. doi:10.1007/s11214-013-9987-4. S2CID   255067404. Archived from the original (PDF) on 2019-07-26. Retrieved 2023-05-27.
  6. ↑ Nelson, Charles H. (2000). "Black Hole Mass, Velocity Dispersion, and the Radio Source in Active Galactic Nuclei". The Astrophysical Journal. 544 (2): L91–L94. arXiv: astro-ph/0009188 . Bibcode:2000ApJ...544L..91N. doi:10.1086/317314. S2CID   117449813.
  7. ↑ Mehdipour, Missagh; Kriss, Gerard A.; Brenneman, Laura W.; Costantini, Elisa; Kaastra, Jelle S.; Branduardi-Raymont, Graziella; Di Gesu, Laura; Ebrero, Jacobo; Mao, Junjie (1 January 2022). "Changing-look Event in NGC 3516: Continuum or Obscuration Variability?". The Astrophysical Journal. 925 (1): 84. arXiv: 2112.06297 . Bibcode:2022ApJ...925...84M. doi: 10.3847/1538-4357/ac42ca . hdl: 1887/3515508 . CC-BY icon.svg This article contains quotations from this source, which is available under the Creative Commons Attribution 4.0 Unported (CC BY 4.0) license.
  8. ↑ Ilić, D.; Oknyansky, V.; Popović, L. č.; Tsygankov, S. S.; Belinski, A. A.; Tatarnikov, A. M.; Dodin, A. V.; Shatsky, N. I.; Ikonnikova, N. P.; Rakić, N.; Kovačević, A.; Marčeta-Mandić, S.; Burlak, M. A.; Mishin, E. O.; Metlova, N. V.; Potanin, S. A.; Zheltoukhov, S. G. (June 2020). "A flare in the optical spotted in the changing-look Seyfert NGC 3516". Astronomy & Astrophysics. 638: A13. arXiv: 2004.01308 . Bibcode:2020A&A...638A..13I. doi:10.1051/0004-6361/202037532. S2CID   214795047.
  9. ↑ Dunn, Jay P.; Parvaresh, Rozhin; Kraemer, S. B.; Crenshaw, D. Michael (23 February 2018). "Evolution of the Outflows in NGC 3516". The Astrophysical Journal. 854 (2): 166. arXiv: 1805.04406 . Bibcode:2018ApJ...854..166D. doi: 10.3847/1538-4357/aaa95d .
  10. ↑ Shapovalova, A I; Popović, L č; Afanasiev, V L; Ilić, D; Kovačević, A; Burenkov, A N; Chavushyan, V H; Marčeta-Mandić, S; Spiridonova, O; Valdes, J R; Bochkarev, N G; Patiño-Álvarez, V; Carrasco, L; Zhdanova, V E (1 June 2019). "Long-term optical spectral monitoring of a changing-look active galactic nucleus NGC 3516 – I. Continuum and broad-line flux variability". Monthly Notices of the Royal Astronomical Society. 485 (4): 4790–4803. arXiv: 1902.10845 . doi:10.1093/mnras/stz692.
  11. ↑ Nagar, Neil M.; Wilson, Andrew S.; Mulchaey, John S.; Gallimore, Jack F. (February 1999). "Radio Structures of Seyfert Galaxies. VIII. A Distance- and Magnitude-Limited Sample of Early-Type Galaxies". The Astrophysical Journal Supplement Series. 120 (2): 209–245. arXiv: astro-ph/9901236 . Bibcode:1999ApJS..120..209N. doi: 10.1086/313183 .
  12. ↑ Miyaji, Takamitsu; Wilson, Andrew S.; Perez-Fournon, Ismael (January 1992). "The radio source and bipolar nebulosity in the Seyfert galaxy NGC 3516". The Astrophysical Journal. 385: 137. Bibcode:1992ApJ...385..137M. doi:10.1086/170922.
  13. ↑ Regan, Michael W.; Mulchaey, John S. (June 1999). "Using HUBBLE SPACE TELESCOPE Imaging of Nuclear Dust Morphology to Rule Out Bars Fueling Seyfert Nuclei". The Astronomical Journal. 117 (6): 2676–2694. arXiv: astro-ph/9903053 . Bibcode:1999AJ....117.2676R. doi: 10.1086/300888 .
  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.
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