A Canis Major over-density imaging survey. I. Stellar content and star-count maps : A distinctly elongated body of main sequence stars

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dc.creatorButler, D. J.
dc.creatorMartinez-Delgado, D.
dc.creatorRix, H-W.
dc.creatorPenarrubia, J.
dc.creatorde Jong, J. T. A.
dc.date2006-09-12
dc.date.accessioned2026-07-07T11:26:01Z
dc.date.available2026-07-07T11:26:01Z
dc.description[Abridged] We present first results from a large-area (~80degx20deg), sparsely sampled two-filter (B,R) imaging survey towards the Canis Major stellar over-density, claimed to be a disrupting Milky Way satellite galaxy. Utilizing stellar colour-magnitude diagrams reaching to B ~ 22 mag, we provide a first delineation of its surface density distribution using main sequence stars. Its projected shape is highly elongated, nearly parallel to the Galactic plane, with an axis ratio of >~ 5:1, substantially more so than what Martin et al. originally found. We also provide a first map of a prominent over-density of blue, presumably younger main sequence stars, which appears to have a maximum near [l,b = 240,-7 deg]. The young population is markedly more localized. We estimate an upper limit on the line-of-sight (l.o.s.) depth of the old population based on the main sequence width, obtaining sigma_los < 1.8 +/- 0.3 kpc, at an adopted D_helio = 7.5 +/- 1 kpc. For the young stellar population, we find sigma_los < 1.5 kpc. There are different explanations for the CMa over-density: (a) a partially disrupting dwarf galaxy on a low-latitude orbit, (b) a projection of the warped outer Galactic disk, and (c) a projection of an out-of-plane spiral arm. While the data provide no firm arguments against the less well-defined third scenario, they have clear implications for each of the others: (a) We infer from the strong elongation in longitude, and simulations in the literature, that the over-density is unlikely to be a gravitationally bound system at the present epoch, but may well be just a recently disrupted satellite remnant. (b) Based on modeling, the line-of-sight depth of the over-density in old stars is clearly inconsistent with published locally axi-symmetric descriptions of the warped Galactic disk.
dc.description27 pages, 15 figures, Submitted to AJ. Several figures are given as JPEGs. High res. version: www.mpia-hd.mpg.de/homes/butler/cma.pdf.gz
dc.identifierhttps://arxiv.org/abs/astro-ph/0609316
dc.identifierhttp://arxiv.org/abs/astro-ph/0609316
dc.identifierAstron.J.133:2274-2290,2007
dc.identifierdoi:10.1086/512726
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/195694
dc.subjectAstrophysics
dc.titleA Canis Major over-density imaging survey. I. Stellar content and star-count maps : A distinctly elongated body of main sequence stars
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