HE0450-2958

HE0450-2958 is an unusual quasar. It has been called the "naked quasar" and the "quasar without a home" because it appears to lack a host galaxy. It is estimated to lie approximately one billion parsecs away.

HE0450-2958

Quasar HE0450-2958 as imaged by the HST. The quasar is near the center of the image; no obvious host galaxy is seen. Near the top of the image is a strongly disturbed and star-forming galaxy. Near the quasar is a blob of gas that is apparently being ionized by the quasar radiation. The pointlike object on the lower right is a foreground star seen by chance in the field of view.
Observation data (Epoch J2000)
ConstellationCaelum
Right ascension04h 52m 30.0s[1]
Declination−29° 53′ 35″[1]
Redshift0.286041 ± 0.000093
(73867 ± 28 km/s[1])
Distance3 billion light-years (1 Gpc)[2]
TypeSy1[1]
Apparent magnitude (V)16.0[1]
Other designations
LEDA 75249,[1] QSO B0450-2958, 2MASSI J0452300-295335, 6dFGS gJ045230.1-295335, 2MASX J04523006-2953353, NVSS J045230-295336, IRAS F04505-2958, QSO B0450-299, IRAS 04505-2958, RBS 597, 1RXS J045230.4-295329
See also: Quasar, List of quasars

History

A team of researchers led by Pierre Magain of the University of Liège, Belgium announced their findings in the September 14, 2005 issue of the journal Nature.[2] The quasar lies close in the sky to a disturbed, starburst galaxy (see figure, upper left). However, no galaxy was seen around the quasar itself (figure, middle), leading the authors to speculate

One might suggest that the host galaxy has disappeared from our view as a result of the collision [which formed the disturbed galaxy], but it is hard to imagine how the complete disruption of a galaxy could happen.

In order for the quasar's host galaxy to have escaped detection, Magain et al. estimated that it would need to be approximately five magnitudes (100 times) dimmer than expected for such a quasar, or to have a radius of 300 light-years or less (typical quasars are embedded in galaxies 5000 to 50,000 light-years across).

Shortly after Magain et al.'s paper was published, three theoretical papers appeared, all in the week of November 6, 2005, which claimed to explain the peculiar properties of this object. Two of the papers—from groups in Cambridge, Massachusetts[3] and Cambridge, England[4]—suggested that the quasar was a supermassive black hole that had been ejected from the center of the nearby, disturbed galaxy, either by gravitational radiation recoil or by an interaction involving three black holes. The ejection velocity would have to be approximately 1000 km/s in order to place the quasar so far from its original host galaxy.

The third paper,[5] from a team led by David Merritt, critically examined the ejection hypothesis and concluded that it could not be correct. The two main arguments were: (1) The quasar spectrum reveals it to be a narrow-line Seyfert 1 galaxy. NLS1's are believed to have abnormally small black holes; since black hole size is strongly correlated with galaxy size, the host galaxy of the quasar should also be abnormally small, explaining why it had not been detected by Magain et al. (2) The quasar spectrum also reveals the presence of a classic, narrow emission line region (NLR). The gas producing the narrow lines lies roughly a thousand light-years from the black hole, and such gas could not remain bound to the black hole following a kick large enough to remove it from its host galaxy. These authors concluded that the "naked" quasar was in fact a perfectly normal, narrow-line Seyfert galaxy that happened to lie close on the sky to a disturbed galaxy.

The "quasar without a home".

A number of scientific studies since 2005 have supported this conclusion. (1) Kim et al. (2006) [6] made a more careful attempt to find the quasar's host galaxy. They concluded that it was impossible to rule out the presence of a galaxy given the confusing light from the quasar. (2) Zhou et al. (2007) [7] observed the X-ray emission from the quasar and used it to estimate the mass of the black hole. They confirmed a small mass for the black hole, implying an even fainter host galaxy than predicted by Merritt et al. (3) Feain et al. (2007) [8] detected radio emission from the quasar, which they interpreted as indicating ongoing star formation, which "contradicts any suggestion that this is a 'naked' quasar'".

The current scientific consensus is that HE0450-2958 probably does have a host galaxy but that it is difficult to see behind the bright quasar light.

Recently, the consensus has been questioned after a European Southern Observatory study.[9]

A study in 2010 discovered a "blob" of emission near the quasar. This blob is thought to be the disturbed and compact host galaxy for the quasar.[10]

See also

References
  1. "Nasa/Ipac Extragalactic Database". Results for HB89 0450-299. Retrieved 2006-11-27.
  2. Magain, P. et al. (2005), Discovery of a bright quasar without a massive host galaxy, Nature, 437, 381
  3. Hoffman, L. and Loeb, A. (2005), Three-Body Kick to a Bright Quasar out of Its Galaxy During a Merger, arXiv:astro-ph/0511242
  4. Haehnelt, M. et al. (2005), Possible evidence for the ejection of a supermassive black hole from an ongoing merger of galaxies, arXiv:astro-ph/0511245
  5. Merritt, David; et al. (April 2006). "The nature of the HE0450-2958 system". Monthly Notices of the Royal Astronomical Society. 367 (4): 1746–1750. arXiv:astro-ph/0511315. Bibcode:2006MNRAS.367.1746M. doi:10.1111/j.1365-2966.2006.10093.x. S2CID 55834970.
  6. Kim, M. et al. (2006), The Host Galaxy of the Quasar HE 0450-2958, The Astrophysical Journal, 658, 107
  7. Zhou, X.-L. et al. (2007), X-Ray Properties of the Quasar HE 0450-2958, The Astronomical Journal, 133, 432
  8. Feain, I. et al. (2007), Dressing a Naked Quasar: Star Formation and Active Galactic Nucleus Feedback in HE 0450-2958, The Astrophysical Journal, 662, 872
  9. Elbaz.D. et al. (2009) Quasar induced galaxy formation: a new paradigm? Astronomy & Astrophysics 507, 1359–1374
  10. Letawe, G.; Magain, P. (2010). "Deep near-infrared imaging of the HE0450-2958 system". Astronomy and Astrophysics. 515: A84. arXiv:1003.3746. Bibcode:2010A&A...515A..84L. doi:10.1051/0004-6361/201014175. S2CID 53142733.
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