TON 618

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TON 618
[[File: TON 618 SDSS9 version 2.jpg |1089px|alt= TON 618 SDSS9 version 2.jpg ]]
TON 618, imaged by the Sloan Digital Sky Survey Data Release 9 (DR9). The quasar appears as the bright, bluish-white dot at the center.
Observation data (Epoch J2000.0)
Constellation Canes Venatici
Right ascension 12h 28m 24.9s [1]
Declination +31° 28′ 38″ [1]
Redshift 2.219 [1]
Distance
  • 3.31  Gpc (10.8  Gly)
    (light travel distance)
  • 5.59  Gpc (18.2  Gly)
    (comoving distance, present proper distance)
    [1]
Type Quasar [1]
Apparent magnitude  (V)15.9 [1]
Notable featuresHyperluminous quasar in a Lyman-alpha blob
Other designations
FBQS J122824.9+312837, B2 1225+31, QSO 1228+3128, 7C 1225+3145, CSO 140, 2E 2728, Gaia DR1 4015522739308729728 [1]
See also: Quasar, List of quasars

TON 618 (abbreviation of Tonantzintla 618) is a hyperluminous, broad-absorption-line, radio-loud quasar, and Lyman-alpha blob [2] located near the border of the constellations Canes Venatici and Coma Berenices, with the projected comoving distance of approximately 18.2 billion light-years from Earth. [a] It possesses one of the most massive black holes ever found, at 40.7 billion M☉. [3]

Contents

Observational history

As quasars were not recognized until 1963, [4] the nature of this object was unknown when it was first noted in a 1957 survey of faint blue stars (mainly white dwarfs) that lie away from the plane of the Milky Way. On photographic plates taken with the 0.7 m Schmidt telescope at the Tonantzintla Observatory in Mexico, it appeared "decidedly violet" and was listed by the Mexican astronomers Braulio Iriarte and Enrique Chavira as entry number 618 in the Tonantzintla Catalogue. [5]

In 1970, a radio survey at Bologna in Italy discovered radio emissions from TON 618, indicating that it was a quasar. [6] Marie-Helene Ulrich then obtained optical spectra of TON 618 at the McDonald Observatory which showed emission lines typical of a quasar. From the high redshift of the lines Ulrich deduced that TON 618 was very distant, and hence was one of the most luminous quasars known. [7]

Components

Supermassive black hole

Size comparison of the event horizons of the black holes of TON 618 and Phoenix A. The orbit of Neptune (white oval) is included for comparison. Phoenix A compared to Ton 618 and the Orbit of Neptune.jpg
Size comparison of the event horizons of the black holes of TON 618 and Phoenix A. The orbit of Neptune (white oval) is included for comparison.

As a quasar, TON 618 is believed to be the active galactic nucleus at the center of a galaxy, the engine of which is a supermassive black hole feeding on intensely hot gas and matter in an accretion disc. Given its observed redshift of 2.219, the light travel time of TON 618 is estimated to be approximately 10.8 billion years. Due to the brilliance of the central quasar, the surrounding galaxy is outshone by it and hence is not visible from Earth. With an absolute magnitude of −30.7, it shines with a luminosity of 4×1040 watts, or as brilliantly as 140 trillion times that of the Sun, making it one of the brightest objects in the known Universe. [1]

Like other quasars, TON 618 has a spectrum containing emission lines from cooler gas much further out than the accretion disc, in the broad-line region. The size of the broad-line region can be calculated from the brightness of the quasar radiation that is lighting it up. [8] Shemmer and coauthors used both NV and CIV emission lines in order to calculate the widths of the Hβ spectral line of at least 29 quasars, including TON 618, as a direct measurement of their accretion rates and hence the mass of the central black hole. [9]

The emission lines in the spectrum of TON 618 have been found to be unusually wide, [7] indicating that the gas is travelling very fast; the full width half maxima of TON 618 has been the largest of the 29 quasars, with hints of 10,500 km/s speeds of infalling material by a direct measure of the Hβ spectral line, indication of a very strong gravitational force. [9] From this, the mass of the central black hole of TON 618 has been estimated to be at 66 billion solar masses. [9] This is considered one of the highest masses ever recorded for such an object; higher than the mass of all the stars in the Milky Way galaxy combined, which is 64 billion solar masses, [10] and 15,300 times more massive than Sagittarius A*, the Milky Way's central black hole. With such high mass, TON 618 may fall into a proposed new classification of ultramassive black holes. [11] [12] A black hole of this mass has a Schwarzschild radius of 1,300 AU (about 390 billion km or 0.04 ly in diameter) which is more than 40 times the distance from Neptune to the Sun, and its event horizon is large enough to fit over 30 solar systems inside of it.

A more recent measurement in 2019 by Ge and colleagues which utilizes the C IV emission line, an alternative spectral line to Hβ, using the same data reproduced by the earlier paper by Shemmer found a lower relative velocity of the surrounding gas of 2,761 ± 423 km/s, which indicate a lower mass for the central black hole at 40.7 billion solar masses, consequentially lower than the previous estimate. [3]

Lyman-alpha nebula

A computer simulated close-up view of a Lyman-alpha blob. A similar gas cloud is present at TON 618. Computer simulation of a Lyman-alpha Blob.jpg
A computer simulated close-up view of a Lyman-alpha blob. A similar gas cloud is present at TON 618.

The nature of TON 618 as a Lyman-alpha emitter has been well documented since at least the 1980s. [13] Lyman-alpha emitters are characterized by their significant emission of the Lyman-alpha line, an ultraviolet wavelength emitted by neutral hydrogen. Such objects, however, have been very difficult to study due to the Lyman-alpha line being strongly absorbed by air in the Earth's atmosphere, limiting study of Lyman-alpha emitters to those objects with high redshifts. TON 618, with its luminous emission of Lyman-alpha radiation along with its high redshift, has made it one of the most important objects in the study of the Lyman-alpha forest. [14]

Observations made by the Atacama Large Millimeter Array (ALMA) in 2021 revealed the apparent source of the Lyman-alpha radiation of TON 618: an enormous cloud of gas surrounding the quasar and its host galaxy. [2] This would make it a Lyman-alpha blob (LAB), one of the largest such objects yet known.

LABs are huge collections of gases, or nebulae, that are also classified as Lyman-alpha emitters. These enormous, galaxy-sized clouds are some of the largest nebulae known to exist, with some identified LABs in the 2000s reaching sizes of at least hundreds of thousands of light-years across. [15]

In the case of TON 618, the enormous Lyman-alpha nebula surrounding it has the diameter of at least 100 kiloparsecs (330,000 light-years), twice the size of the Milky Way. [2] The nebula consists of two parts: an inner molecular outflow and an extensive cold molecular gas in its circumgalactic medium, each having the mass of 50 billion M☉, [2] with both of them being aligned to the radio jet produced by the central quasar. The extreme radiation from TON 618 excites the hydrogen in the nebula so much that it causes to glow brightly in the Lyman-alpha line, consistent with the observations of other LABs driven by their inner galaxies. [16] Since both quasars and LABs are precursors of modern-day galaxies, the observation on TON 618 and its enormous LAB gave insight to the processes that drive the evolution of massive galaxies, [2] in particular probing their ionization and early development.

See also

Other notable objects in the Tonantzintla Catalogue

Notes

  1. ↑ This distance may seem to contradict the age of the Universe and is greater than the oldest light of the most distant objects. However, the time difference corresponds to another quantity, light-travel distance, which is only 10.8 billion light years. See Distance measures (cosmology) which explains the distance measures used in cosmology.

Related Research Articles

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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">3C 273</span> Brightest quasar from Earth located in the constellation Virgo

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

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<span class="mw-page-title-main">Supermassive black hole</span> Largest type of black hole

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<span class="mw-page-title-main">Lyman-alpha blob</span> Astronomical object type

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<span class="mw-page-title-main">Lyman-alpha emitter</span>

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<span class="mw-page-title-main">Lyman-alpha blob 1</span> Lyman-alpha blob in the constellation of Aquarius

Lyman-alpha blob 1 (LAB-1) is a giant cosmic cloud of gas located in the constellation of Aquarius, approximately 11.5 billion light-years from Earth with a redshift (z) of 3.09. It was discovered unexpectedly in 2000 by Charles Steidel and colleagues, who were surveying for high-redshift galaxies using the 200 inch Hale Telescope at the Palomar Observatory. The researchers had been investigating the abundance of galaxies in the young Universe when they came across two objects which would become known as Lyman-alpha blobs—huge concentrations of gases emitting the Lyman-alpha emission line of hydrogen.

<span class="mw-page-title-main">WISE J224607.57−052635.0</span> Most luminous galaxy in the Universe

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

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<span class="mw-page-title-main">UM 287</span> Quasar located in the constellation Cetus

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References

  1. 1 2 3 4 5 6 7 8 "NED results for object TON 618". NASA/IPAC EXTRAGALACTIC DATABASE. Archived from the original on 2021-08-15. Retrieved 2021-08-15.
  2. 1 2 3 4 5 Li, Jianrui; Emonts, B. H. C.; Cai, Z.; Prochaska, J. X.; Yoon, I.; Lehnert, M. D.; Zhang, S.; Wu, Y.; Li, Jianan; Li, Mingyu; Lacy, M.; Villar-Martín, M. (25 November 2021). "Massive Molecular Outflow and 100 kpc Extended Cold Halo Gas in the Enormous Lyα Nebula of QSO 1228+3128". The Astrophysical Journal Letters. 922 (2): L29. arXiv: 2111.06409 . Bibcode:2021ApJ...922L..29L. doi: 10.3847/2041-8213/ac390d . S2CID   244102865.
  3. 1 2 Ge, Xue; Bi-Xuan, Zhao; Wei-Hao, Bian; Green Richard, Frederick (21 March 2019). "The Blueshift of the C IV Broad Emission Line in QSOs". The Astronomical Journal. 157 (4): 14. arXiv: 1903.08830 . Bibcode:2019AJ....157..148G. doi: 10.3847/1538-3881/ab0956 . S2CID   84842636.
  4. ↑ "1963: Maarten Schmidt Discovers Quasars". Observatories of the Carnegie Institution for Science. Archived from the original on 1 February 2019. Retrieved 21 October 2017.
  5. ↑ Iriarte, Braulio; Chavira, Enrique (1957). "Estrellas Azules en el Casquete Galactico Norte (Blue stars in the North Galactic Cap)" (PDF). Boletín de los Observatorios de Tonantzintla y Tacubaya. 2 (16): 3–36. Archived (PDF) from the original on 22 October 2017. Retrieved 21 October 2017.
  6. ↑ Colla, G.; Fanti, C.; Ficarra, A.; Formiggini, L.; Gandolfi, E.; Grueff, G.; Lari, C.; Padrielli, L.; Roffi, G.; Tomasi, P; Vigotti, M. (1970). "A catalogue of 3235 radio sources at 408 MHz". Astronomy & Astrophysics Supplement Series. 1 (3): 281. Bibcode:1970A&AS....1..281C.
  7. 1 2 Ulrich, Marie-Helene (1976). "Optical spectrum and redshifts of a quasar of extremely high intrinsice luminosity: B2 1225+31". The Astrophysical Journal. 207: L73–L74. Bibcode:1976ApJ...207L..73U. doi: 10.1086/182182 .
  8. ↑ Kaspi, Shai; Smith, Paul S.; Netzer, Hagai; Maos, Dan; Jannuzi, Buell T.; Giveon, Uriel (2000). "Reverberation measurements for 17 quasars and the size-mass-luminosity relations in active galactic nuclei". The Astrophysical Journal. 533 (2): 631–649. arXiv: astro-ph/9911476 . Bibcode:2000ApJ...533..631K. doi:10.1086/308704. S2CID   119022275.
  9. 1 2 3 Shemmer, O.; Netzer, H.; Maiolino, R.; Oliva, E.; Croom, S.; Corbett, E.; di Fabrizio, L. (2004). "Near-infrared spectroscopy of high-redshift active galactic nuclei: I. A metallicity-accretion rate relationship". The Astrophysical Journal. 614 (2): 547–557. arXiv: astro-ph/0406559 . Bibcode:2004ApJ...614..547S. doi:10.1086/423607. S2CID   119010341.
  10. ↑ McMillan, P. J. (July 2011). "Mass models of the Milky Way". Monthly Notices of the Royal Astronomical Society. 414 (3): 2446–2457. arXiv: 1102.4340 . Bibcode:2011MNRAS.414.2446M. doi: 10.1111/j.1365-2966.2011.18564.x . S2CID   119100616.
  11. ↑ Irving, Michael (21 February 2018). ""Ultramassive" black holes may be the biggest ever found – and they're growing fast". New Atlas. Archived from the original on 31 March 2019. Retrieved 21 August 2018.
  12. ↑ "From Super to Ultra: Just How Big Can Black Holes Get?". NASA – Chandra X-Ray Observatory. 18 December 2012. Archived from the original on 17 June 2019. Retrieved 21 August 2018.
  13. ↑ Sargent, W. L. W.; Young, P. J.; Boksenberg, A.; Tytler, D. (1980). "The distribution of Lyman-alpha absorption lines in the spectra of six QSOs: evidence for an intergalactic origin". The Astrophysical Journal Supplement Series. 42: 41. Bibcode:1980ApJS...42...41S. doi: 10.1086/190644 .
  14. ↑ Khare, P.; Srianand, R.; York, D. G.; Green, R.; Welty, D.; Huang, K.-L.; Bechtold, J. (1997). "The Lyman alpha forest towards B2 1225 + 317". Monthly Notices of the Royal Astronomical Society. 285 (1): 167–180. arXiv: astro-ph/9612163 . doi: 10.1093/mnras/285.1.167 . Archived from the original on 2022-01-29. Retrieved 2022-01-29.
  15. ↑ Steidel, C. C.; Adelberger, K. L.; Shapley, A. E. (2000). "Lyα Imaging of a Proto–Cluster Region at ⟨ z ⟩ = 3.09". Astrophysical Journal . 532 (1): 170–82. arXiv: astro-ph/9910144 . Bibcode:2000ApJ...532..170S. doi:10.1086/308568. S2CID   10353723.
  16. ↑ "Giant Space Blob Glows from Within". ESO Press Release. 17 August 2011. Archived from the original on 28 September 2011. Retrieved 18 August 2011.
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