Markarian 1018

Last updated
Markarian 1018
The active galaxy Markarian 1018.jpg
The Seyfert galaxy Markarian 1018.
Observation data (J2000 epoch)
Constellation Cetus
Right ascension 02h 06m 15.98s
Declination −00° 17′ 29.23″
Redshift 0.042957
Heliocentric radial velocity 12,878 km/s
Distance 607 Mly (186.1 Mpc)
Apparent magnitude  (V)15.5
Apparent magnitude  (B)15.9
Characteristics
Type S0; merger?, Sy 1.5
Apparent size  (V)0.99' x 0.52'
Notable features Seyfert galaxy
Other designations
UGC 1597, UM 393, PGC 8029, MCG +00-06-030, CGCG 387-034

Markarian 1018 (Mrk 1018), also known as UGC 1597, is a lenticular galaxy with a peculiar structure located in the constellation Cetus. It is located at an approximate distance of 607 million light years from Earth and has an apparent dimensions of 0.99 by 0.52 arcmin. [1] It is classified as a change looking[ clarification needed ] Seyfert galaxy and galaxy merger.

Contents

Characteristics

Markarian 1018 is a post merger product of two colliding galaxies indicated by the presence of its disturbed galactic envelope, tidal tails and a faint loop of light surrounding it. [2] [3] [4] It has a stellar mass measured as log M*/Mʘ = 10.92 and a total star formation of 0.6 Mʘ yr−1. [5] It has an active galactic nucleus (AGN) like most types of active galaxies with the energy source originating from an accretion disk around its supermassive black hole. The mass of the black hole in Markarian 1018 varies however. In a 2011 study, its mass is around log (MBH/Mʘ) = 8.15 . [6] But later studies showed the mass is (MBH/Mʘ) = 7.4. [7] and subsequently (MBH/Mʘ) = 7.84. [8]

The black hole in the center of Markarian 1018 as observed by Chandra X-ray Observatory. Markarian 1018.jpg
The black hole in the center of Markarian 1018 as observed by Chandra X-ray Observatory.

The appearance of Markarian 1018 is known to shift from a bright to a dim state when observed in X-rays as well as both optical and ultraviolet models detected by Hubble Space Telescope, Sloan Digital Sky Survey and GALEX. This is likely caused by the disruption of the fueling of its black hole by an interaction of a likely secondary black hole in the galaxy. [9] [10]

The AGN of Markarian 1018 is described change looking[ clarification needed ]. It was originally a type 1.9 Seyfert galaxy. Between the years 1979 and 1984, it underwent a transition to become a type I. During the change, its ultraviolet and optical line emission strengthened. [11] However, Markarian 1018 has since changed back into type 1.9 after a period of 30 years. Its broad line flux declined with a Hα factor of 4.75 ± 0.5 while its broad emission lines vanished. [7] This makes the galaxy the first known change looking[ clarification needed ] AGN to undergo two transitions in a full cycle. [12] It also shows a very weak continuum with the presence of indistinctive Hα and Hβ emission lines best fitted by a line component with a measurement of FWHM ≈ 7200 km s−1. [13]

The X-ray source of Markarian 1018 has gone through a spectral variation. Between 2005 and 2019, its hardness ratio significantly increased from 0.2 ± 0.1 to 0.4 ± 0.1, between both the 0.5-2 and 2-10 keV bands. In additional, the broadband in the galaxy became dim, as the X-ray, ultraviolet and optical luminosities went down by factors of > 7, > 24 and ~ 9. This sharp decrease is suggested by lower ultraviolet emission. Further evidence also points out the hot medium properties of Markarian 1018 clearly remains the same while a warm component is found to cool down to a temperature of ~ 0.2 keV, suggesting the cooling process plays a major role in weakening the accretion disk's magnetic fields and the cause of ultraviolet dimming. [14]

In late 2016, Markarian 1018 suddenly stopped dimming. It underwent a flaring period in which the galaxy showed an outburst; its magnitude level rising by ~ 0.25 U-band per month until early 2017 according to confirmation from Hubble and Chandra X-ray Observatory. Following resumption of monitoring in July 2017, it has since been only found ~ 0.4 magnitude higher than its flaring period. [5] It has since gone through another outburst this time in 2020. While much of its optical spectrum and primary X-ray flux remained constant, its 6.4 keV iron line strengthened through increased emission. This suggests the accretion rate in Markarian 1018 has changed drastically in short-term. [15]

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">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">Markarian 231</span> Seyfert galaxy in the constellation Ursa Major

Markarian 231 is a Type-1 Seyfert galaxy that was discovered in 1969 as part of a search of galaxies with strong ultraviolet radiation. It contains the nearest known quasar. Markarian 231 is located about 581 million light years away from Earth, in the constellation of Ursa Major.

<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">Markarian 1034</span> Interacting galaxies in the constellation of Triangulum

Markarian 1034 is a pair of spiral galaxies comprising PGC 9074 and PGC 9071, located in the constellation Triangulum. They are located at a distance of 465 million light-years from Earth and are classified as luminous infrared galaxies.

<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 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 3599</span> Lenticular galaxy in the Leo constellation

NGC 3599 is a lenticular galaxy located in the constellation Leo. It was discovered by William Herschel on March 14, 1784. The galaxy is located at a distance of 67 million light-years (20.4 Mpc) from the Sun. NGC 3599 is a member of the Leo II group of galaxies in the Virgocentric flow.

<span class="mw-page-title-main">NGC 2617</span> Galaxy in the constellation Hydra

NGC 2617 is a Seyfert galaxy in the equatorial constellation of Hydra. It was discovered on February 12, 1885, by French astronomer Édouard Stephan. In 1888, Danish astronomer J. L. E. Dreyer described it as "extremely faint, very small, 2 very faint stars involved". It is located at an estimated distance of 202 million light years. In the infrared, the galaxy has an angular size of 0.693 by 0.652 arcminutes.

<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 an unbarred 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">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">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.

<span class="mw-page-title-main">I Zwicky 1</span> Galaxy in the constellation Pisces

I Zwicky 1, also known as UGC 545, is a galaxy located in the constellation Pisces. It is located 847 million light-years from Earth and is said to be the nearest quasar (QSO) due to its high optical nuclear luminosity of MV = -23.8 mag.

<span class="mw-page-title-main">PG 0844+349</span> Galaxy in the constellation Lynx

PG 0844+349, also known as TON 951, is a galaxy in the southern constellation Lynx, near the border of Cancer. Its redshift is 0.064000, putting the galaxy at 849 million light-years away from Earth.

<span class="mw-page-title-main">Markarian 463</span> Galaxy in the constellation of Boötes

Markarian 463 known as UGC 8850, is a galaxy merger located in the constellation Boötes. It is located 706 million light years from Earth. It is classified a double nucleus Seyfert galaxy.

<span class="mw-page-title-main">IC 485</span> Spiral galaxy in the constellation Gemini

IC 485 is a spiral galaxy located in the constellation of Gemini, located 375 million light years from Earth. It was discovered by the Austrian astronomer, Rudolf Spitaler on March 6, 1891. It has an estimated diameter of 1.35' x 0.32' arcmin, meaning the galaxy is about 135,000 light years across.

<span class="mw-page-title-main">MCG +08-11-011</span> Galaxy in the constellation Auriga

MCG +08-11-011 known as UGC 3374, is a galaxy located in the constellation of Auriga. It is located 401 million light years from Earth and is classified as a Seyfert galaxy.

<span class="mw-page-title-main">Markarian 876</span> Galaxy in the constellation Draco

Markarian 876 known as PG 1613+658, is an elliptical galaxy located in the constellation of Draco. With a velocity relative to the cosmic microwave background of 36,302 ± 60 kilometers per seconds, the galaxy is located 1.75 billion light years from Earth. It is a Seyfert galaxy.

<span class="mw-page-title-main">RX J1633.3+4718</span> Narrow-line Seyfert galaxy located in the constellation Hercules

RX J1633.3+4718 known as RXS J16333+4718 according to VLBI Network observations, is a narrow-line Seyfert 1 galaxy, located in the constellation of Hercules. It has a redshift of (z) 0.116 and is located 1.75 billion light years from Earth. The first known reference to this galaxy comes from a radio source which was identified in 1995 in the IRAS catalogue as F16319+4725.

References

  1. ↑ "Your NED Search Results". ned.ipac.caltech.edu. Retrieved 2024-10-02.
  2. ↑ Kim, D.-C.; Yoon, Ilsang; Evans, A. S. (2018-07-01). "Recoiling Supermassive Black Hole in Changing-look AGN Mrk 1018". The Astrophysical Journal. 861 (1): 51. arXiv: 1805.05251 . Bibcode:2018ApJ...861...51K. doi: 10.3847/1538-4357/aac77d . ISSN   0004-637X.
  3. ↑ information@eso.org. "The active galaxy Markarian 1018". www.esahubble.org. Retrieved 2024-10-02.
  4. ↑ Nowakowski, Tomasz; Phys.org. "Study investigates recent outburst in the active galaxy Markarian 1018". phys.org. Retrieved 2024-10-02.
  5. 1 2 Krumpe, M.; Husemann, B.; Tremblay, G. R.; Urrutia, T.; Powell, M.; Davis, T. A.; Scharwächter, J.; Dexter, J.; Busch, G.; Combes, F.; Croom, S. M.; Eckart, A.; McElroy, R. E.; Perez-Torres, M.; Leung, G. (November 2017). "The Close AGN Reference Survey (CARS) - Mrk 1018 halts dimming and experiences strong short-term variability⋆". Astronomy & Astrophysics. 607: L9. arXiv: 1710.09382 . Bibcode:2017A&A...607L...9K. doi:10.1051/0004-6361/201731967. ISSN   0004-6361.
  6. ↑ Bennert, Vardha N.; Auger, Matthew W.; Treu, Tommaso; Woo, Jong-Hak; Malkan, Matthew A. (2011-11-14). "THE RELATION BETWEEN BLACK HOLE MASS AND HOST SPHEROID STELLAR MASS OUT TOz∼ 2". The Astrophysical Journal. 742 (2): 107. arXiv: 1102.1975 . Bibcode:2011ApJ...742..107B. doi:10.1088/0004-637x/742/2/107. ISSN   0004-637X.
  7. 1 2 McElroy, R. E.; Husemann, B.; Croom, S. M.; Davis, T. A.; Bennert, V. N.; Busch, G.; Combes, F.; Eckart, A.; Perez-Torres, M.; Powell, M.; Scharwächter, J.; Tremblay, G. R.; Urrutia, T. (September 2016). "The Close AGN Reference Survey (CARS) - Mrk 1018 returns to the shadows after 30 years as a Seyfert 1". Astronomy & Astrophysics. 593: L8. arXiv: 1609.04423 . Bibcode:2016A&A...593L...8M. doi:10.1051/0004-6361/201629102. ISSN   0004-6361.
  8. ↑ Noda, Hirofumi; Done, Chris (2018-08-01). "Explaining changing-look AGN with state transition triggered by rapid mass accretion rate drop". Monthly Notices of the Royal Astronomical Society. 480 (3): 3898–3906. arXiv: 1805.07873 . doi: 10.1093/mnras/sty2032 . ISSN   0035-8711.
  9. ↑ "Markarian 1018: Starvation Diet for Black Hole Dims Brilliant Galaxy". chandra.harvard.edu. Retrieved 2024-10-02.
  10. ↑ "A Galaxy Is Fading Because a Black Hole Is Starving to Death". Inverse. 2016-11-09. Retrieved 2024-10-02.
  11. ↑ Cohen, Ross D.; Rudy, Richard J.; Puetter, R. C.; Ake, T. B.; Foltz, Craig B. (1986-12-01). "Variability of Markarian 1018: Seyfert 1.9 to Seyfert 1". The Astrophysical Journal. 311: 135. Bibcode:1986ApJ...311..135C. doi:10.1086/164758. ISSN   0004-637X.
  12. ↑ Lyu, Bing; Yan, Zhen; Yu, Wenfei; Wu, Qingwen (2021-06-01). "Long-term and multiwavelength evolution of a changing-look AGN Mrk 1018". Monthly Notices of the Royal Astronomical Society. 506 (3): 4188–4198. arXiv: 2106.03059 . doi: 10.1093/mnras/stab1581 . ISSN   0035-8711.
  13. ↑ Hutsemékers, D.; Agís González, B.; Marin, F.; Sluse, D. (December 2020). "Spectropolarimetry of the changing-look active galactic nucleus Mrk 1018". Astronomy & Astrophysics. 644: L5. arXiv: 2011.12634 . Bibcode:2020A&A...644L...5H. doi:10.1051/0004-6361/202039760. ISSN   0004-6361.
  14. ↑ Veronese, S.; Vignali, C.; Severgnini, P.; Matzeu, G. A.; Cignoni, M. (March 2024). "Interpreting the long-term variability of the changing-look AGN Mrk 1018". Astronomy & Astrophysics. 683: A131. arXiv: 2312.07663 . Bibcode:2024A&A...683A.131V. doi:10.1051/0004-6361/202348098. ISSN   0004-6361.
  15. ↑ Brogan, R.; Krumpe, M.; Homan, D.; Urrutia, T.; Granzer, T.; Husemann, B.; Neumann, J.; Gaspari, M.; Vaughan, S. P.; Croom, S. M.; Combes, F.; Pérez Torres, M.; Coil, A.; McElroy, R.; Winkel, N. (September 2023). "Still alive and kicking: A significant outburst in changing-look AGN Mrk 1018". Astronomy & Astrophysics. 677: A116. arXiv: 2307.14139 . Bibcode:2023A&A...677A.116B. doi:10.1051/0004-6361/202346475. ISSN   0004-6361.
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.