[PDF] Top 20 Galaxy modelling through stellar population synthesis

... this population, and investigated its ...neighbour population – thin disc and halo populations resp. This population dominates the counts only at medium latitudes and at distance between 1 to 4 kpc ... See full document

... than modelling the physical processes that we think go into galaxy formation, use statistical methods to match galaxies to their corresponding dark matter haloes ...each galaxy is not tracked, ... See full document

... starburst stellar models, overplotted on this SDSS galaxy data, as a function of stellar population age and ...the galaxy population during their ...single-age stellar ... See full document

... elliptical galaxy into gaseous form over its lifetime (Sandage and Visvanathan 1978b and references therein), but 21 cm observations show upper limits to galactic H I which are an order of magnitude less than this ... See full document

... the galaxy stellar mass function that we obtain from our data for the whole COSMOS field, irrespective of the environment, is consistent with the result by ...the galaxy stellar mass function ... See full document

... of stellar mass assembly and the discovery of the “downsizing” effect (Cowie et ...The galaxy observations are usually interpreted by comparing them to the stellar pop- ulation synthesis ... See full document

... the stellar population information from the IFS data cubes is based on the full spectral synthesis ...spectral synthesis methods, substantial changes in the results are more likely to come ... See full document

... The dust content of the model galaxy is treated in a two- component manner as described by Wood et al. (2008) in order to take account of both large grains and small transiently heated grains. Large grains with ... See full document

... The excess star formation and the other three problems are all symptoms of the overcooling catastrophe. Fully cosmological numerical galaxy simulations consistently contain an excess of low angular momentum ... See full document

... when galaxy mergers take ...more galaxy mergers, the galaxies governed by the algorithm have an increased chance of fuelling their central galaxies, which would increase bulge stellar mass at the ... See full document

... the galaxy disc (a relatively small effect), and consider where they would reside in a size–luminosity plane (Brodie et ...peculiar population of large and bright objects like ω ... See full document

... versus stellar mass and in- dicates that scatter decreases slightly at the lowest and highest stellar ...and stellar kinematics would correlate more strongly with stellar structures, however ... See full document

... different galaxy types because we use the same sampling volume for galaxies with different size, the rms magnetic fields of cold particles saturates to roughly 10 µG in all cases except CosmoDwarf, in good ... See full document

... Our study only focuses on the tracers of the M31 stellar halo. Therefore, to select only objects dwelling in the halo, we restrict the above sample of 2637 PNe to those with a projected distance of |Y| ≥ 5 kpc, ... See full document

... of stellar evolution models, particularly at the low metallicities and in the binary environments required to create the most massive transients? Barrett et ...our stellar models that are ... See full document

... inner Galaxy as described in Prantzos ...the Galaxy (the inner disk and Galactic bulge), and that these positrons tend to annihilate in the dense, warm outer shells of molecular clouds that occupy the inner ... See full document

... Recently, there have been several photometry-based surveys searching for metal- poor stars, such as SkyMapper (Schmidt et al. 2005; Keller et al. 2012) and PRISTINE (Starkenburg et al. 2017). Both of these surveys rely ... See full document

... propagating through the entire disc, whereas many-armed or flocculent galaxies are asso- ciated with more fragmented spiral ...spiral galaxy must be ... See full document

... (2008)). This star shows evidence for surface differential rotation, with the equatorial regions rotating faster than the poles. The mag- netic field is dominantly toroidal with a mostly non-axisymmetric poloidal ... See full document

... We can also compare our catalog with other published lists of young massive stars. A complete catalog for UCHII regions exists from the recently completed CORNISH blind radio survey (Purcell et al. 2013). A ... See full document