Monoceros Ring

From Wikipedia, the free encyclopedia
Jump to navigation Jump to search

The Monoceros Ring is a long, complex, ringlike filament of stars that wraps around the Milky Way three times. This is proposed to consist of a stellar stream torn from the Canis Major Dwarf Galaxy by tidal forces as part of the process of merging with the Milky Way over a period of billions of years, although this view has long been disputed.[1] The ring contains 100 million solar masses and is 200,000 light years long.[2]


The stream of stars was first reported in 2002 by astronomers conducting the Sloan Digital Sky Survey. It was in the course of investigating this ring of stars, and a closely spaced group of globular clusters similar to those associated with the Sagittarius Dwarf Elliptical Galaxy, that the Canis Major Dwarf Galaxy was discovered.[3]


In 2006, a study using 2MASS data cast doubts on the nature of the "Ring", arguing that the data suggests that the ring is actually part of the warped galactic disc of the Milky Way.[1] However, observations using the Anglo-Australian Telescope published in 2007 suggest that a warped disc cannot create the observed structure, which must therefore be formed either by a flare of the Galactic Disc or have an extra-Galactic origin.[4]

Several members of the scientific community recently restated their position affirming the Monoceros structure is nothing more than an over-density produced by the flared and warped thick disk of the Milky Way.[5]

In 2015, a study by an international team of scientists suggested, after sorting and sifting through galactic data from the Sloan Digital Sky Survey, that the Milky Way is actually 50 percent larger than previously thought.[6] It turned out that the disk of the Milky Way is not just a disk of stars in a flat plane, but is instead corrugated. As it radiates outward from the Sun, there appears to be at least four ripples in the disk of the Milky Way. Scientists assume that this pattern is going to be found throughout the disk.[7]

One way of thinking about this is to imagine being on the ocean when the waves are very high, or standing in hilly terrain. The next rise in the waves or the hills blocks the view of what lies beyond. In the same way, the next rise in the galactic structure is blocking view of what lies beyond, which apparently is a significant portion of the galactic disk. Based on the distance of the Monoceros Ring, the diameter of the Milky Way increases from 100,000-120,000 light years to somewhere around 150,000-180,000 light years across. In this revised paradigm, rather than lying at two-thirds of the galaxy's radius, the solar system lies about halfway between the core and the edge.[8]

N-body simulations have been used to investigate the possible location of the progenitor of this structure and these calculations show that, if the Ring has a dwarf galaxy progenitor, it might be found in the background of one out of eight specific areas in the sky.[9] A subsequent analysis, that used Gaia DR2 data, found a bimodal Gaussian distribution towards Galactic coordinates (271, +2) degrees in Vela, which is one of the locations of the progenitor proposed in the previous study.[10] This finding may signal the presence of the progenitor of the Monoceros Ring, but the authors indicate that it might also be compatible with the existence of an unrelated kinematically coherent structure.


  1. ^ a b Y. Momany; et al. (2006). "Outer structure of the Galactic warp and flare: explaining the Canis Major over-density" (PDF). Astronomy and Astrophysics. 451 (2): 515–38. arXiv:astro-ph/0603385Freely accessible. Bibcode:2006A&A...451..515M. doi:10.1051/0004-6361:20054081. 
  2. ^ Ibata, Rodrigo; Gibson, Brad (April 2007). "The Ghosts of Galaxies Past". Scientific American. 296 (4): 40–45. Bibcode:2007SciAm.296d..40I. doi:10.1038/scientificamerican0407-40. PMID 17479629. 
  3. ^ Newberg; et al. (1 April 2002). "The Ghost of Sagittarius and Lumps in the Halo of the Milky Way". The Astrophysical Journal. 569 (1): 245–274. arXiv:astro-ph/0111095Freely accessible. Bibcode:2002ApJ...569..245N. doi:10.1086/338983. 
  4. ^ Conn, Blair C.; Lane, Richard R.; Lewis, Geraint F.; Gil-Merino, Rodrigo; Irwin, Mike J.; Ibata, Rodrigo A.; Martin, Nicolas F.; Bellazzini, Michele; Sharp, Robert; Tuntsov, Artem V.; Ferguson, Annette M. N. (April 1, 2007). "The AAT/WFI survey of the Monoceros Ring and Canis Major dwarf galaxy". Monthly Notices of the Royal Astronomical Society. 376 (3): 939–959. arXiv:astro-ph/0701664Freely accessible. Bibcode:2007MNRAS.376..939C. doi:10.1111/j.1365-2966.2007.11503.x. 
  5. ^ M. Lopez-Corredoira, A; et al. (July 2012). "Comments on the "Monoceros" affair". arXiv:1207.2749Freely accessible. Bibcode:2012arXiv1207.2749L. 
  6. ^ Mary L. Martialay (March 11, 2015). "The Corrugated Galaxy—Milky Way May Be Much Larger Than Previously Estimated" (Press release). Rensselaer Polytechnic Institute. Archived from the original on March 13, 2015. 
  7. ^ Scott Sutherland (March 16, 2015). "This 'corrugated' view of the Milky Way just made our home galaxy a LOT bigger". The Weather Network. Archived from the original on March 19, 2015. 
  8. ^ Yan Xu; et al. (March 1, 2015). "Rings and Radial Waves in the Disk of the Milky Way". The Astrophysical Journal. 801 (2). arXiv:1503.00257Freely accessible. Bibcode:2015ApJ...801..105X. doi:10.1088/0004-637X/801/2/105. 
  9. ^ Magda Guglielmo; et al. (March 11, 2018). "On the origin of the Monoceros Ring - I. Kinematics, proper motions, and the nature of the progenitor". Monthly Notices of the Royal Astronomical Society. 474 (4): 4584–4593. arXiv:1711.06682Freely accessible. Bibcode:2018MNRAS.474.4584G. doi:10.1093/mnras/stx3048. 
  10. ^ de la Fuente Marcos, Raúl; de la Fuente Marcos, Carlos (21 November 2018). "Searching for the lost Unicorn: a prominent feature in the radial velocity distribution of stars in Vela from Gaia DR2 data". Monthly Notices of the Royal Astronomical Society Letters. 481 (1): L64–L68. arXiv:1808.09921Freely accessible. Bibcode:2018MNRAS.481L..64D. doi:10.1093/mnrasl/sly163.