Markarian 590

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Markarian 590
NGC863 - SDSS DR14.jpg
NGC 863 by SDSS
Observation data (J2000 epoch)
Constellation Cetus
Right ascension 02h 14m 33.6s [1]
Declination −00° 46′ 00″ [1]
Redshift 0.026385 ± 0.000040 [1]
Heliocentric radial velocity 7,910 ± 10 km/s [1]
Distance 297 ± 19 Mly (91.1 ± 5.7 Mpc) [1]
Apparent magnitude  (V)13.2
Characteristics
Type SA(s)a [1]
Apparent size  (V)1.1′ × 1.0′ [1]
Notable featuresSeyfert galaxy
Other designations
NGC 863, NGC 866, NGC 885, UGC 1727, MCG +00-06-056, PGC 8586 [1]

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. [1] It is a change looking Seyfert galaxy.

Contents

Observational history

Markarian 590 was discovered by William Herschel on January 6, 1785. The galaxy was also discovered independently by Lewis Swift on 3 October 1886, while he also catalogued it again as a different galaxy on 31 October 1886, and thus the galaxy is listed three times in the New General Catalogue. John Louis Emil Dreyer described it as very faint, round, brighter middle, stellar. [2]

One supernova has been observed in Markarian 590, SN 2018djd. SN 2018djd is a type Ia supernova [3] discovered by All Sky Automated Survey for SuperNovae (ASAS-SN) on 12 July 2018. The supernova was detected in images obtained on 10.61 July 2018, when it had a magnitude of 16.5. [4] It reached a maximum apparent magnitude of 15.4. [5]

Characteristics

The central region of Markarian 590 by the Hubble Space Telescope. NGC 863 -HST-606.png
The central region of Markarian 590 by the Hubble Space Telescope.

The nucleus of Markarian 590 has been found to be active. 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 4593 is estimated to be (47.5±7.4)×106  M☉ based on reverberation mapping. [6]

The active galactic nucleus (AGN) of Markarian 590 has been categorised as change looking. [7] This category of Seyfert galaxies is characterised by a change in the spectrum, with the broad emission lines disappearing or appearing, and thus changing the galaxy from to type I to type II and vice versa. [8] Markarian 590 was originally characterised as a type I Seyfert galaxy, but later observations categorised the galaxy as type 1.5 [9] and type 1.9-2. [8]

The broad line emission of Markarian 590 strengthened by a factor of tens from the 1970s to the 1990s and then decreased about 100 times in the 2000s in optical, UV, and X-ray wavelengths, and the broad component of the Hβ emission line disappeared completely. [8] Observations by Suzaku X-ray satellite in 2011 revealed that the soft X-ray excess emission could no longer be detected, while the X-ray continuum flux had minimal change. [10] The X-ray spectrum doesn't show evidence of obstruction; [8] instead the variation is caused by a change in accretion rate. [11] Observations of the galaxy in the infrared wavelengths revealed a sharp decrease in luminosity between 2000 and 2001. Also, during the low activity period, the radius of the circumnuclear dust torus decreased to 32 light days. [12] In 2014, the soft excess emission had reappeared in observations by Chandra X-ray Observatory, as well as the broad MgII emission line. [7]

The radio emission of the galaxy is concentrated to a single core source, and extends to two components at a radius of about 2 arcsec (~1 kpc) and 6 arcsec (~3 kpc) from the core, that probably are related to the ring-like molecular gas structures observed in CO(3-2) imaging. [11] The outer gas ring is probably related to the spiral arms of the galaxy while the inner ring is related to faint dust lanes. The central molecular gas mass is estimated to be less than 1.6×105  M☉ , not significantly less than other AGNs. [13] A faint parsec-scale radio jet extending 2.8 mas to the north has been detected using very-long-baseline interferometry. [14] The radio emission exhibits long term variation that follows that of the other wavelengths. [11]

X-ray observations of the galaxy has shown the presence of ultra fast outflows, in the form of blueshifted absorption lines of O viii, Ne ix, Si xiv, and Mg xii. [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 this luminosity is not produced by the 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 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">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">NGC 4151</span> Galaxy in the constellation Canes Venatici

NGC 4151 is an intermediate spiral Seyfert galaxy with weak inner ring structure located 15.8 megaparsecs from Earth in the constellation Canes Venatici. The galaxy was first mentioned by William Herschel on March 17, 1787; it was one of the six Seyfert galaxies described in the paper which defined the term. It is one of the nearest galaxies to Earth to contain an actively growing supermassive black hole. The black hole would have a mass on the order of 2.5 million to 30 million solar masses. It was speculated that the nucleus may host a binary black hole, with about 40 million and about 10 million solar masses respectively, orbiting with a 15.8-year period. This is, however, still a matter of active debate.

<span class="mw-page-title-main">NGC 4051</span> Galaxy in the constellation Ursa Major

NGC 4051 is an intermediate spiral galaxy in the constellation of Ursa Major. It was discovered on 6 February 1788 by John Herschel.

<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 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 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 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 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 931</span> Galaxy in the constellation Triangulum

NGC 931 is a spiral galaxy located in the constellation Triangulum. It is located at a distance of circa 200 million light-years from Earth, which, given its apparent dimensions, means that NGC 931 is about 200,000 light years across. It was discovered by Heinrich d'Arrest on September 26, 1865. It is classified as a Seyfert galaxy.

<span class="mw-page-title-main">NGC 3393</span> Galaxy in the constellation Hydra

NGC 3393 is a barred spiral galaxy located in the constellation Hydra. It is located at a distance of circa 180 million light-years from Earth, which, given its apparent dimensions, means that NGC 3393 is about 140,000 light-years across. It was discovered by John Herschel on March 24, 1835. It is a Type II Seyfert galaxy, known to host two supermassive black holes, which are the nearest known pair of supermassive black holes to Earth.

<span class="mw-page-title-main">Markarian 273</span> Galaxy in the constellation of Ursa Major

Markarian 273 is a galaxy merger located in the constellation Ursa Major. It is located at a distance of about 500 million light years from Earth, which, given its apparent dimensions, means that Markarian 273 is about 130,000 light years across. It is an ultraluminous infrared galaxy and a Seyfert galaxy.

<span class="mw-page-title-main">NGC 4253</span> Galaxy in the constellation of Coma Berenices

NGC 4253 is a barred spiral galaxy located in the constellation Coma Berenices. It is located at a distance of about 185 million light years from Earth, which, given its apparent dimensions, means that NGC 4253 is about 65,000 light years across. It was discovered by William Herschel on February 3, 1788. It is a Seyfert galaxy.

<span class="mw-page-title-main">NGC 5135</span> Galaxy in the constellation Hydra

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.

<span class="mw-page-title-main">NGC 5683</span> Galaxy in the constellation Boötes

NGC 5683 is a type S0-a lenticular galaxy with a bar located in the Boötes constellation. It is 513 million light-years away from the Solar System and has an approximate diameter of 256,000 light-years meaning it is larger compared to the Milky Way. NGC 5683 was discovered by George Johnstone Stoney on April 13, 1850.

<span class="mw-page-title-main">Markarian 817</span> Barred spiral galaxy in the constellation Draco

Markarian 817 is a barred spiral galaxy located in the constellation Draco. It is located 456 million light-years from Earth, which, given its apparent dimensions, means that Markarian 817 is about 80,000 light-years across. It is a Seyfert galaxy.

References

  1. 1 2 3 4 5 6 7 8 9 "NASA/IPAC Extragalactic Database". Results for NGC 863. Retrieved 2023-05-06.
  2. ↑ Seligman, Courtney. "NGC 863". Celestial Atlas. Retrieved 19 November 2018.
  3. ↑ "ATel #11864: Spectroscopic classification of 12 transients with du Pont". The Astronomer's Telegram. 17 July 2018. Retrieved 17 June 2023.
  4. ↑ "ATel #11848: ASASSN-18pb: Discovery of A Probable Supernova in Seyfert 1 AGN host Mrk 590". The Astronomer's Telegram. 13 July 2018. Retrieved 17 June 2023.
  5. ↑ "Bright Supernovae - 2018". www.rochesterastronomy.org. Retrieved 17 June 2023.
  6. ↑ Peterson, B. M.; Ferrarese, L.; Gilbert, K. M.; Kaspi, S.; Malkan, M. A.; Maoz, D.; Merritt, D.; Netzer, H.; Onken, C. A.; Pogge, R. W.; Vestergaard, M.; Wandel, A. (October 2004). "Central Masses and Broad-Line Region Sizes of Active Galactic Nuclei. II. A Homogeneous Analysis of a Large Reverberation-Mapping Database". The Astrophysical Journal. 613 (2): 682–699. arXiv: astro-ph/0407299 . Bibcode:2004ApJ...613..682P. doi:10.1086/423269. hdl: 1885/33814 . S2CID   16308360.
  7. 1 2 Mathur, S.; Denney, K. D.; Gupta, A.; Vestergaard, M.; De Rosa, G.; Krongold, Yair; Nicastro, F.; Collinson, J.; Goad, M.; Korista, K.; Pogge, R. W.; Peterson, B. M. (18 October 2018). "The Changing-look Quasar Mrk 590 Is Awakening". The Astrophysical Journal. 866 (2): 123. arXiv: 1810.06616 . Bibcode:2018ApJ...866..123M. doi: 10.3847/1538-4357/aadd91 . hdl: 2381/45545 .
  8. 1 2 3 4 Denney, K. D.; De Rosa, G.; Croxall, K.; Gupta, A.; Bentz, M. C.; Fausnaugh, M. M.; Grier, C. J.; Martini, P.; Mathur, S.; Peterson, B. M.; Pogge, R. W.; Shappee, B. J. (17 November 2014). "THE TYPECASTING OF ACTIVE GALACTIC NUCLEI: Mrk 590 NO LONGER FITS THE ROLE". The Astrophysical Journal. 796 (2): 134. arXiv: 1404.4879 . Bibcode:2014ApJ...796..134D. doi:10.1088/0004-637X/796/2/134. S2CID   119742660.
  9. ↑ Osterbrock, D. E. (August 1977). "Spectrophotometry of Seyfert 1 galaxies". The Astrophysical Journal. 215: 733. Bibcode:1977ApJ...215..733O. doi:10.1086/155407.
  10. ↑ Rivers, Elizabeth; Markowitz, Alex; Duro, Refiz; Rothschild, Richard (1 November 2012). "A SUZAKU OBSERVATION OF Mkn 590 REVEALS A VANISHING SOFT EXCESS". The Astrophysical Journal. 759 (1): 63. arXiv: 1210.3330 . Bibcode:2012ApJ...759...63R. doi:10.1088/0004-637X/759/1/63. S2CID   118423911.
  11. 1 2 3 Koay, J. Y.; Vestergaard, M.; Bignall, H. E.; Reynolds, C.; Peterson, B. M. (21 July 2016). "Parsec-scale radio morphology and variability of a changing-look AGN: the case of Mrk 590". Monthly Notices of the Royal Astronomical Society. 460 (1): 304–316. doi: 10.1093/mnras/stw975 . hdl: 10150/621462 .
  12. ↑ Kokubo, Mitsuru; Minezaki, Takeo (1 February 2020). "Rapid luminosity decline and subsequent reformation of the innermost dust distribution in the changing-look AGN Mrk 590". Monthly Notices of the Royal Astronomical Society. 491 (4): 4615–4633. arXiv: 1904.08946 . doi: 10.1093/mnras/stz3397 .
  13. ↑ Koay, J. Y.; Vestergaard, M.; Casasola, V.; Lawther, D.; Peterson, B. M. (21 January 2016). "ALMA probes the molecular gas reservoirs in the changing-look Seyfert galaxy Mrk 590". Monthly Notices of the Royal Astronomical Society. 455 (3): 2745–2764. arXiv: 1509.09203 . doi: 10.1093/mnras/stv2495 .
  14. ↑ Yang, Jun; van Bemmel, Ilse; Paragi, Zsolt; Komossa, S; Yuan, Feng; Yang, Xiaolong; An, Tao; Koay, J Y; Reynolds, C; Oonk, J B R; Liu, Xiang; Wu, Qingwen (28 January 2021). "A parsec-scale faint jet in the nearby changing-look Seyfert galaxy Mrk 590". Monthly Notices of the Royal Astronomical Society: Letters. 502 (1): L61–L65. arXiv: 2101.04629 . doi: 10.1093/mnrasl/slab005 .
  15. ↑ Gupta, A.; Mathur, S.; Krongold, Y. (9 December 2014). "DETECTION OF HIGH VELOCITY OUTFLOWS IN THE SEYFERT 1 GALAXY Mrk 590". The Astrophysical Journal. 798 (1): 4. arXiv: 1406.5968 . doi:10.1088/0004-637X/798/1/4. S2CID   119028585.
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