Titlebook: Lessons from the Local Group; A Conference in hono Kenneth Freeman,Bruce Elmegreen,Matthew Woolway Conference proceedings 2015 Springer Int

AMITY

The Galactic Bulge, boxy/peanut-shaped bulge which we believe formed via instabilities of the disk rather than through mergers. The bulge of the Milky Way therefore appears to be a dynamical product of the early Galactic disk, without significant contamination from mergers with other galaxies. The instabilities are be

變色龍

The Galactic Bar,amical studies in the Gaia era. Here we discuss the pronounced peanut shape of the Galactic bulge that has resulted from recent star count analysis, in particular from the VVV survey. We also discuss the question whether the Milky Way has an inner disky pseudo-bulge, and show preliminary evidence fo

弄皺

The Challenge of Galactic Cartography: Lessons from the Milky Way, how or whether to include “historical” knowledge, based on traveler accounts, in their maps. I describe how we are now facing a similar problem in Galactic cartography as we try to reconcile older views of the Galactic disk based on the photometric distances to stars and kinematic distance to neutr

HIKE

Subjugate

enflame

Dust in the Local Group,ects of dust extinction in inferring the true luminosity and colors of reddened astrophysical objects. Together with the extinction spectral features, the extinction curve contains important information about the dust size distribution and composition. This review summarizes our current knowledge of

Mosaic

Milky Way Metallicities and Fossil Cosmology,of our Galaxy. In particular it is suggested that the solar vicinity provides an unrepresentative sampling of the disk MDF and that no G-dwarf problem generalizable to the whole disk can be inferred from the solar vicinity, nor constrains on the infall time scale. I suggest that the best place to lo

身體萌芽

Cirrhosis

Coterminous

Cloud and Star Formation in Spiral Arms,onal instabilities, arguing that the former is prevalent at lower galactic surface densities and the latter at higher. Cloud masses are also limited by stellar feedback, which can be effective before clouds reach their maximum mass. We show other properties of clouds in simulations with different le