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Spiral arms, bar shape and bulge microlensing in the Milky Way

Bissantz, Nicolai ; Gerhard, Ortwin

In: Monthly Notices of the Royal Astronomical Society, 2002, vol. 330, no. 3, p. 591-608

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    Title
    • Spiral arms, bar shape and bulge microlensing in the Milky Way
    Author
    • Bissantz, Nicolai. Astronomisches Institut der Universität Basel, Venusstrasse 7, CH-4102 Binningen, Switzerland
    • Gerhard, Ortwin. Astronomisches Institut der Universität Basel, Venusstrasse 7, CH-4102 Binningen, Switzerland
    Document Type
    • Postprint
    OAI-PMH Identifier
    • oai:doc.rero.ch:296985
    Summary
    A new model for the luminosity distribution in the inner Milky Way is found, using a non-parametric penalized maximum-likelihood algorithm to deproject a dereddened COBE/ DIRBE L-band map of the inner Galaxy. The model is also constrained by the apparent magnitude (line-of-sight) distributions of clump giant stars in certain bulge fields. An important new feature is the inclusion of a spiral arm model in the disc. Spiral arms make the model appear broader on the sky; thus our bar is more elongated than in previous eight-fold symmetric models. They also lead to a smoother disc model interior to the Sun. The bar length is ≈3.5 kpc, and its axis ratios are 1:(0.3-0.4):0.3, independent of whether the spiral arm model is four-armed or two-armed. The larger elongation in the plane makes it possible to reproduce the observed clump giant distributions as well. With only the surface brightness data, a small model degeneracy is found even for fixed orientation of the bar, amounting to about ±0.1 uncertainty in the in-plane axial ratio. Including the clump giant data removes most of this degeneracy and also places additional constraints on the orientation angle of the bar. We estimate 15°≲ϕbar≲30°, with the best models obtained for 20°≲ϕbar≲25°. We use our reference model to predict a microlensing optical depth map towards the bulge, normalizing its mass by the observed terminal velocity curve. For clump giant sources at (l,b)=(3°.9, −3°.8) we find τ−6≡τ/10−6=1.27, within 1.8σ of the new MACHO measurement given by Popowski et al. The value for all sources at (l,b)=(2°.68, −3°.35) is τ−6=1.1, still >3σ away from the published MACHO DIA value. The dispersion of these τ−6 values within our models is ≃10 per cent. Because the distribution of sources is well fitted by the near-infrared model, increasing the predicted optical depths by >20 per cent will be difficult. Thus the high value of the measured clump giant optical depth argues for a near-maximal disc in the Milky Way