The colour–magnitude relation of globular clusters in Centaurus and
... GC mass can also occur as a result of dynamical evolution, via preferential loss of low-mass stars (Kruijssen & Lamers 2008; Anders et al. 2009; Kruijssen 2009). This makes lower-mass GCs bluer than their colour for an unaltered stellar mass function, thus qualitatively creating a trend in the direc ...
... GC mass can also occur as a result of dynamical evolution, via preferential loss of low-mass stars (Kruijssen & Lamers 2008; Anders et al. 2009; Kruijssen 2009). This makes lower-mass GCs bluer than their colour for an unaltered stellar mass function, thus qualitatively creating a trend in the direc ...
STRUCTURAL CHARACTERISTICS AND STELLAR
... 1991). The area weighted colors are less a ected and should be more representative of the underlying stellar population. Indeed, this is a much greater concern for broad band colors of HSB disks, where the star formation rate and H II region covering factor are higher. Due to bad weather, some galax ...
... 1991). The area weighted colors are less a ected and should be more representative of the underlying stellar population. Indeed, this is a much greater concern for broad band colors of HSB disks, where the star formation rate and H II region covering factor are higher. Due to bad weather, some galax ...
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... alone. Only upon combining them does the strong relation in Figure 1 become apparent. Data over this large dynamic range (a factor of 100) in surface brightness have not previously been available. 2.1. Selection E†ects The data have been selected to be as inclusive as possible given the demands plac ...
... alone. Only upon combining them does the strong relation in Figure 1 become apparent. Data over this large dynamic range (a factor of 100) in surface brightness have not previously been available. 2.1. Selection E†ects The data have been selected to be as inclusive as possible given the demands plac ...
Beasts of the Southern Wild: Discovery of nine Ultra Faint satellites
... detectable with surveys like SDSS out to a small fraction of the MW virial radius. As a result, their total number in the Galaxy must be reconstructed under the assumption of the shape of their galactocentric radial distribution. Given that only a handful of such objects are known today, their radia ...
... detectable with surveys like SDSS out to a small fraction of the MW virial radius. As a result, their total number in the Galaxy must be reconstructed under the assumption of the shape of their galactocentric radial distribution. Given that only a handful of such objects are known today, their radia ...
Weak gravitational lensing
While the presence of any mass bends the path of light passing near it, this effect rarely produces the giant arcs and multiple images associated with strong gravitational lensing. Most lines of sight in the universe are thoroughly in the weak lensing regime, in which the deflection is impossible to detect in a single background source. However, even in these cases, the presence of the foreground mass can be detected, by way of a systematic alignment of background sources around the lensing mass. Weak gravitational lensing is thus an intrinsically statistical measurement, but it provides a way to measure the masses of astronomical objects without requiring assumptions about their composition or dynamical state.