Editing Canis Major Overdensity (section)

==Dispute==

Several studies cast doubts on the true nature of this overdensity.<ref name="Lopez-Corredoira20012">{{Cite arXiv |eprint=1207.2749 |class=astro-ph.GA |first1=M. |last1=Lopez-Corredoira |first2=A. |last2=Moitinho |title=Comments on the "Monoceros" affair |date=Jul 2012 |last3=Zaggia |first3=S. |last4=Momany |first4=Y. |last5=Carraro |first5=G. |last6=Hammersley |first6=P. L. |last7=Cabrera-Lavers |first7=A. |last8=Vazquez |first8=R. A.}}</ref> Some research suggests that the trail of stars is actually part of the warped galactic [[thin disk]] and [[thick disk]] population and not a result of the collision of the [[Milky Way]] with a dwarf spheroidal galaxy.<ref name="Momany2004">{{Cite journal |last1=Momany |first1=Y. |last2=Zaggia |first2=S. R. |last3=Bonifacio |first3=P. |last4=Piotto |first4=G. |last5=De Angeli |first5=F. |last6=Bedin |first6=L. R. |last7=Carraro |first7=G. |date=July 2004 |title=Probing the Canis Major stellar over-density as due to the Galactic warp |journal=Astronomy and Astrophysics |volume=421 |issue=2 |pages=L29 |arxiv=astro-ph/0405526 |bibcode=2004A&A...421L..29M |doi=10.1051/0004-6361:20040183|s2cid=6371010 }}</ref> Investigation of the area in 2009 yielded only ten [[RR Lyrae variable]] stars, which is consistent with the Milky Way's [[Galactic halo|halo]] and thick disk populations rather than a separate dwarf spheroidal galaxy.<ref>{{Cite journal |last1=Mateu, Cecilia |last2=Vivas, A. Katherina |last3=Zinn, Robert |last4=Miller, Lissa R. |last5=Abad, Carlos |year=2009 |title=No Excess of RR Lyrae Stars in the Canis Major Overdensity |journal=The Astronomical Journal |volume=37 |issue=5 |pages=4412–23 |arxiv=0903.0376 |bibcode=2009AJ....137.4412M |doi=10.1088/0004-6256/137/5/4412|s2cid=18967866 }}</ref>