S5 0014+81

S5 0014+81 is a distant, compact, hyperluminous, broad-absorption line quasar or blazar located near the high declination region of the constellation Cepheus, near the North Equatorial Pole.

Characteristics

The object is a blazar, in fact an OVV (optically violent variable) quasar, the most energetic subclass of objects known as active galactic nuclei, produced by the rapid accretion of matter by a central supermassive black hole, changing the gravitational energy to light energy that can be visible at cosmic distances. In the case of S5 0014+81 it is one of the most luminous quasars known, with a total luminosity of over 1041 watts,[2] equal to an absolute bolometric magnitude of -31.5. If the quasar were at a distance of 280 light-years from Earth, it would give as much energy per square meter as the Sun despite being 18 million times more distant. The quasar’s luminosity is therefore about 3 x 1014 (300 trillion) times the Sun,[3] or over 25,000 times as luminous as all the 100 to 400 billion stars of the Milky Way Galaxy combined,[4] making it one of the most powerful objects in the observable universe. However, because of its huge distance of 12.1 billion light-years it can only be studied by spectroscopy. The central black hole of the quasar devours an extremely huge amount of matter, equivalent to 4,000 solar masses of material every year.

The quasar is also a very strong source of radiation, from gamma-rays and X-rays down to radio waves. The quasar is located at a distance where the observed redshift of quasars and stars are extremely similar, making the two objects difficult to distinguish using the standard spectroscopic redshift and the photometric redshift determination, and hence must be treated by other special techniques to successfully determine the nature of the object.

The quasar’s designation, S5, is from the Fifth Survey of Strong Radio Sources, 0014+81 was its coordinates in epoch B1950.0. It also has the other designation 6C B0014+8120,[1] from the Sixth Cambridge Survey of radio sources by Cambridge University.

The host galaxy of S5 0014+81 is a giant elliptical starburst galaxy, with the apparent magnitude of 24.

Supermassive black hole

Artist’s conception of a supermassive black hole devouring matter in an accretion disc with a relativistic jet of material emanating from the black hole perpendicular to the disc

The Swift spacecraft, used by astronomers to determine the mass of the black hole of S5 0014+81

The host galaxy of S5 0014+81 is an FSRQ blazar, a giant elliptical galaxy that hosts a supermassive black hole in its center, which may be responsible for the intense activity of this blazar.

In 2009, a team of astronomers using the Swift Spacecraft used the luminosity output of S5 0014+81 to measure the mass of the central black hole. To their surprise, they found out that the central black hole of S5 0014+81 is actually 10,000 times more massive than the black hole at the center of our galaxy, or equivalent to 40 billion solar masses.[5] This makes it one of the most massive black holes ever discovered, more than six times the value of the black hole of Messier 87, which was thought to be the largest black hole for almost 60 years, and was coined to be an “ultramassive” black hole. The Schwarzschild radius of this black hole is 118.35 billion kilometers. So, this black hole has an external horizon showing a diameter of 236.7 billion kilometers, 1,600 astronomical units, or about 40 times the radius of Pluto’s orbit, and shows a mass equivalent to four Large Magellanic Clouds. What is even more astounding is that the monstrous black hole exists so early in the universe, at only 1.6 billion years after the Big Bang. This suggests that supermassive black holes grew up very quickly.

However, there are some cautions about the study. First, the method used was actually an indirect method of calculation, and not Keplerian orbital estimation; the latter being a more precise estimate. It is unlikely for a quasar as luminous as S5 0014+81, which will just outshine the stars within its vicinity, thereby making estimates very inaccurate. Second, the spectrum used is actually a long spectrum, not accounting for the observed parameters. Third, the quasar is surrounded by a large accretion disc, a few parsecs in size, and it shines at 40% of its Eddington luminosity, the maximum luminosity through which radiation pressure is strong enough to blow up the disc away from the gravitational influence of the central black hole, so the observed characteristics are unknown due to intervening dust and gases. However, the possibility of an ultramassive black hole has not been ruled out entirely, since only a black hole of that mass can account for the observed power output of the quasar.

Evolution models based on the mass of S5 0014+81’s supermassive black hole predict that it will live for roughly 1.342×1099 years (near the end of the Black Hole Era of the Universe, when it is more than 1088 times its current age), before it dissipates by the Hawking radiation.[6] However, it is undergoing accretion, so it may take longer than the stated time for it to dissipate.

References

  1. Jump up to:a b c d e f g h “NED results for object S5 0014+81”. NASA/IPAC EXTRAGALACTIC DATABASE.
  2. Jump up^ 1.2×1041 watts. Kühr, Helmut; Liebert, James W.; Strittmatter, Peter A.; Schmidt, Gary D.; et al. (15 December 1983). “The most luminous quasar – S5 0014+81”. Astrophysical Journal. Bibcode:1983ApJ…275L..33K. doi:10.1086/184166.
  3. Jump up^ Solar luminosity is 3.846×1026 watts. “Sun Facts”. nasa.gov. 14 January 2015.
  4. Jump up^ The Milky Way absolute visual magnitude is -20.6. Huchra, John P. (2009). “The Properties of Galaxies”. harvard.edu. Harvard-Smithsonian Center for Astrophysics. Retrieved 18 January 2015.
  5. Jump up^ Ghisellini, Gabriele; Foschini, Luigi; Volonteri, Marta; Ghirlanda, Giancarlo; et al. (14 Jul 2009). “The blazar S5 0014+813: a real or apparent monster?”. Monthly Notices of the Royal Astronomical Society399 (1): L24–L28. Bibcode:2009MNRAS.399L..24G. arXiv:0906.0575 Freely accessible. doi:10.1111/j.1745-3933.2009.00716.x. 17:53:24 GMT.
  6. Jump up^ Page, Don N. (1976). “Particle Emission Rates from a Black Hole: Massless Particles from an Uncharged, Nonrotating Hole”. Physical Review D13 (2): 198–206. Bibcode:1976PhRvD..13..198P. doi:10.1103/PhysRevD.13.198. See in particular equation (27).

By Trinh Manh Do

%d bloggers like this: