HLX-1

Last updated
Hyper-Luminous Xray source 1
ESO 243-49 (HST).jpg
ESO 243-49 (center) with HLX-1 (circled)
Observation data
Epoch J2000        Equinox J2000
Constellation Phoenix [1]
Right ascension 01h 10m 28.2s
Declination −46° 04′ 22.2″ [2]
Details
Mass 102-105  M☉

Hyper-Luminous X-ray source 1, commonly known as HLX-1, is an intermediate-mass black hole candidate located in the lenticular galaxy ESO 243-49 about 290 million light-years from Earth. The mass of its central black hole is estimated to be approximately 20,000 solar masses. [3] The source was discovered at the Institut de Recherche en Astrophysique et Planétologie (IRAP, formerly the CESR), Toulouse, France and gained interest from the scientific community because of strong evidence supporting it as an intermediate-mass black hole. [2] HLX-1 is possibly the remnant of a dwarf galaxy that may have been in a galactic collision with ESO 243-49. [4]

Discovery

The object was first observed in November 2004, in which it was seen as a source emitting X-rays in the outskirts of the spiral galaxy ESO 243-49 and was catalogued as 2XMM J011028.1-460421, but nicknamed "HLX-1". [5] In 2008, a team of astronomers led by Natalie Webb at the Institut de Recherche en Astrophysique et Planétologie in Toulouse, France, discovered HLX-1 and from the very high X-ray luminosity (~1 x 1042 erg s−1, 0.2-10.0 keV), as well as its X-ray characteristics, proposed that it was an intermediate mass black hole candidate. [2] Follow up analysis using further X-ray, [6] [7] [8] [9] [10] optical [11] [12] and radio [13] observations support the intermediate-mass black hole nature. In 2012, further work showed that there was a small cluster of stars amassed around HLX-1, leading Sean Farrell and collaborators [11] to conclude that the black hole was once the galactic center of a dwarf galaxy, which was consumed by ESO 243-49. [14] [15] Farrell remarked, "The fact that there's a very young cluster of stars indicates that the intermediate-mass black hole may have originated as the central black hole in a very low-mass dwarf galaxy. The dwarf galaxy was then swallowed by the more massive galaxy.". [16]

Related Research Articles

The study of galaxy formation and evolution is concerned with the processes that formed a heterogeneous universe from a homogeneous beginning, the formation of the first galaxies, the way galaxies change over time, and the processes that have generated the variety of structures observed in nearby galaxies. Galaxy formation is hypothesized to occur from structure formation theories, as a result of tiny quantum fluctuations in the aftermath of the Big Bang. The simplest model in general agreement with observed phenomena is the Lambda-CDM model—that is, that clustering and merging allows galaxies to accumulate mass, determining both their shape and structure. Hydrodynamics simulation, which simulates both baryons and dark matter, is widely used to study galaxy formation and evolution.

<span class="mw-page-title-main">Messier 87</span> Elliptical galaxy in the Virgo Galaxy Cluster

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<span class="mw-page-title-main">Intermediate-mass black hole</span> Class of black holes with a mass range of 100 to 100000 solar masses

An intermediate-mass black hole (IMBH) is a class of black hole with mass in the range 102–105 solar masses: significantly more than stellar black holes but less than the 105–109 solar mass supermassive black holes. Several IMBH candidate objects have been discovered in the Milky Way galaxy and others nearby, based on indirect gas cloud velocity and accretion disk spectra observations of various evidentiary strength.

<span class="mw-page-title-main">NGC 404</span> Galaxy in the constellation Andromeda

NGC 404 is a field galaxy located about 10 million light years away in the constellation Andromeda. It was discovered by William Herschel in 1784, and is visible through small telescopes. NGC 404 lies just beyond the Local Group and does not appear gravitationally bound to it. It is located within 7 arc-minutes of second magnitude star Mirach, making it a difficult target to observe or photograph and granting it the nickname "Mirach's Ghost".

<span class="mw-page-title-main">Messier 60</span> Elliptical galaxy in the constellation Virgo

Messier 60 or M60, also known as NGC 4649, is an elliptical galaxy approximately 57 million light-years away in the equatorial constellation of Virgo. Together with NGC 4647, it forms a pair known as Arp 116. Messier 60 and nearby elliptical galaxy Messier 59 were discovered by Johann Gottfried Koehler in April 1779, observing a comet in the same part of the sky. Charles Messier added both to his catalogue about three days after this.

<span class="mw-page-title-main">Dwarf galaxy</span> Small galaxy composed of up to several billion stars

A dwarf galaxy is a small galaxy composed of about 1000 up to several billion stars, as compared to the Milky Way's 200–400 billion stars. The Large Magellanic Cloud, which closely orbits the Milky Way and contains over 30 billion stars, is sometimes classified as a dwarf galaxy; others consider it a full-fledged galaxy. Dwarf galaxies' formation and activity are thought to be heavily influenced by interactions with larger galaxies. Astronomers identify numerous types of dwarf galaxies, based on their shape and composition.

<span class="mw-page-title-main">Messier 85</span> Elliptical galaxy in the constellation Coma Berenices

Messier 85 is a lenticular galaxy, or elliptical galaxy for other authors, in the Coma Berenices constellation. It is 60 million light-years away, and it is estimated to be 125,000 light-years across.

GCIRS 13E is an infrared and radio object near the Galactic Center. It is believed to be a cluster of hot massive stars, possibly containing an intermediate-mass black hole (IMBH) at its center.

<span class="mw-page-title-main">NGC 1313</span> Galaxy in the constellation Reticulum

NGC 1313 is a field galaxy and a irregular galaxy discovered by the Scottish astronomer James Dunlop on 27 September 1826. It has a diameter of about 50,000 light-years, or about half the size of the Milky Way.

<span class="mw-page-title-main">NGC 5286</span> Globular cluster in the constellation Centaurus

NGC 5286 is a globular cluster of stars located some 35,900 light years away in the constellation Centaurus. At this distance, the light from the cluster has undergone reddening from interstellar gas and dust equal to E(B – V) = 0.24 magnitude in the UBV photometric system. The cluster lies 4 arc-minutes north of the naked-eye star M Centauri. It was discovered by Scottish astronomer James Dunlop, active in Australia, and listed in his 1827 catalog.

<span class="mw-page-title-main">NGC 3783</span> Galaxy in the constellation Centaurus

NGC 3783 is a barred spiral galaxy located about 135 million light years away in the constellation Centaurus. It is inclined by an angle of 23° to the line of sight from the Earth along a position angle of about 163°. The morphological classification of SBa indicates a bar structure across the center (B) and tightly-wound spiral arms (a). Although not shown by this classification, observers note the galaxy has a luminous inner ring surrounding the bar structure. The bright compact nucleus is active and categorized as a Seyfert 1 type. This nucleus is a strong source of X-ray emission and undergoes variations in emission across the electromagnetic spectrum.

<span class="mw-page-title-main">NGC 6086</span> Galaxy in the constellation Corona Borealis

NGC 6086 is an elliptical galaxy in the constellation of Corona Borealis. It has an apparent magnitude of 12.7. A Type-cD galaxy, it is the brightest cluster galaxy in the cluster Abell 2162. In 2010, a supermassive black hole was discovered in NGC 6086.

<span class="mw-page-title-main">NGC 4203</span> Galaxy in the constellation Coma Berenices

NGC 4203 is the New General Catalogue identifier for a lenticular galaxy in the northern constellation of Coma Berenices. It was discovered on March 20, 1787 by English astronomer William Herschel, and is situated 5.5° to the northwest of the 4th magnitude star Gamma Comae Berenices and can be viewed with a small telescope. The morphological classification of NGC 4203 is SAB0−, indicating that it has a lenticular form with tightly wound spiral arms and a weak bar structure at the nucleus.

<span class="mw-page-title-main">NGC 1271</span> Galaxy in the constellation Perseus

NGC 1271 is a compact elliptical or lenticular galaxy located about 250 million light-years away in the constellation Perseus. The galaxy was discovered by astronomer Guillaume Bigourdan on November 14, 1884. NGC 1271 is a member of the Perseus Cluster and has a nuclear dust disk in its center. It also has an edge-on, intermediate-scale disk and has a central bulge. Like NGC 1277, NGC 1271 is a candidate "relic galaxy".

<span class="mw-page-title-main">NGC 1266</span> Galaxy in the constellation Eridanus

NGC 1266 is a lenticular galaxy in the constellation Eridanus. Although not currently starbursting, it has undergone a period of intense star formation in the recent past, ceasing only ≈500 Myr ago. The galaxy is host to an obscured active galactic nucleus.

<span class="mw-page-title-main">NGC 1395</span> Galaxy in the constellation Eridanus

NGC 1395 is an elliptical galaxy located in the constellation Eridanus. It is located at a distance of circa 75 million light years from Earth, which, given its apparent dimensions, means that NGC 1395 is about 130,000 light years across. It was discovered by William Herschel on November 17, 1784. It is a member of the Eridanus 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.

References

  1. ↑ Beatty, Kelly (2009-07-03). "New Candidates for Midsize Black Holes". Sky & Telescope. Archived from the original on 2012-05-03. Retrieved 2012-02-17.
  2. 1 2 3 Farrell, Sean (2009-07-02). "An intermediate-mass black hole of over 500 solar masses in the galaxy ESO 243-49". Nature . 460 (7251): 73–5. arXiv: 1001.0567 . Bibcode:2009Natur.460...73F. doi:10.1038/nature08083. PMID   19571880. S2CID   4344293.
  3. ↑ "ESO 243-49, a large spiral galaxy in Phoenix". 3 November 2012.
  4. ↑ Webb, Natalie (2010-02-19). "Chandra and Swift Follow-up Observations of the Intermediate Mass Black Hole in ESO 243-49". The Astrophysical Journal. 712 (1): L107–L110. arXiv: 1002.3625 . Bibcode:2010ApJ...712L.107W. doi:10.1088/2041-8205/712/1/L107. S2CID   118393250.
  5. ↑ Ford, Matt (2009-07-02). "Odd Black Hole Is Last Survivor of Its Galaxy". Ars Technica.
  6. ↑ Godet, Olivier (2009-09-24). "First evidence for spectral state transitions in the ESO243-49 hyper luminous X-ray source HLX-1". The Astrophysical Journal. 705 (2): L109–L112. arXiv: 0909.4458 . Bibcode:2009ApJ...705L.109G. doi:10.1088/0004-637X/705/2/L109. S2CID   272396.
  7. ↑ Godet, Olivier (2012-04-16). "Investigating slim disk solutions for HLX-1 in ESO 243-49". The Astrophysical Journal. 752 (1): 34. arXiv: 1204.3461 . Bibcode:2012ApJ...752...34G. doi:10.1088/0004-637X/752/1/34. S2CID   20418449.
  8. ↑ Servillat, Mathieu (2011-08-22). "X-ray Variability and Hardness of ESO 243-49 HLX-1: Clear Evidence for Spectral State Transitions". The Astrophysical Journal. 743 (1): 6. arXiv: 1108.4405 . Bibcode:2011ApJ...743....6S. doi:10.1088/0004-637X/743/1/6. S2CID   118687377.
  9. ↑ Davis, Shane (2011-04-13). "The Cool Accretion Disk in ESO 243-49 HLX-1: Further Evidence of an Intermediate Mass Black Hole". The Astrophysical Journal. 734 (2): 111. arXiv: 1104.2614 . Bibcode:2011ApJ...734..111D. doi:10.1088/0004-637X/734/2/111. S2CID   4730425.
  10. ↑ Lasota, Jean-Pierre (2011-02-21). "The origin of variability of the intermediate-mass black-hole ULX system HLX-1 in ESO 243-49". The Astrophysical Journal. 735 (2): 89. arXiv: 1102.4336 . Bibcode:2011ApJ...735...89L. doi:10.1088/0004-637X/735/2/89. S2CID   118611917.
  11. 1 2 Farrell, Sean (2012-01-10). "A Young Massive Stellar Population Around the Intermediate Mass Black Hole ESO 243-49 HLX-1". The Astrophysical Journal. 747 (1): L13. arXiv: 1110.6510 . Bibcode:2012ApJ...747L..13F. doi:10.1088/2041-8205/747/1/L13. S2CID   119291891.
  12. ↑ Wiersema, Klaas (2010-08-24). "A Redshift for the Intermediate Mass Black Hole Candidate HLX-1: Confirmation of its Association with the Galaxy ESO 243-49". The Astrophysical Journal. 721 (2): L102–L106. arXiv: 1008.4125 . Bibcode:2010ApJ...721L.102W. doi:10.1088/2041-8205/721/2/L102. S2CID   119194158.
  13. ↑ Webb, Natalie (2012-07-05). "Radio Detections During Two State Transitions of the Intermediate-Mass Black Hole HLX-1". Science . 337 (6094): 554–556. arXiv: 1311.6918 . Bibcode:2012Sci...337..554W. doi:10.1126/science.1222779. hdl:2060/20140010250. PMID   22767898. S2CID   1652904.
  14. ↑ Mann, Adam (2012-02-15). "Odd Black Hole Is Last Survivor of Its Galaxy". Wired News.
  15. ↑ Grossman, Lisa (2012-02-17). "Astrophile: 'Missing link' black hole is stress eater". New Scientist . Reed Business Information.
  16. ↑ Moskowitz, Chris (2012-02-16). "How a black hole survived the destruction of its galaxy". The Christian Science Monitor.
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