AN ULTRA-DEEP NEAR-INFRARED SPECTRUM OF
... emission. A possible post-starburst population may affect size measurements more strongly; although a 0.5 Gyr old stellar population can make up 10% of the total stellar mass, it could account for up to ∼ 40% of the optical light. Nevertheless, this spectrum shows that this compact galaxy is domin ...
... emission. A possible post-starburst population may affect size measurements more strongly; although a 0.5 Gyr old stellar population can make up 10% of the total stellar mass, it could account for up to ∼ 40% of the optical light. Nevertheless, this spectrum shows that this compact galaxy is domin ...
wing galaxies: a formation mechanism of the clumpy irregular galaxy
... that the observed velocity field of Mrk 297 is well reproduced on the basis of our model. As noted above, in our scheme, Mrk 297 is not a merger but an only interacting galaxy. Very recently, Sofue et al. (1990) detected 12 CO (J = 1 — 0) emission in Mrk 297 using the 45-m radio telescope of the Nob ...
... that the observed velocity field of Mrk 297 is well reproduced on the basis of our model. As noted above, in our scheme, Mrk 297 is not a merger but an only interacting galaxy. Very recently, Sofue et al. (1990) detected 12 CO (J = 1 — 0) emission in Mrk 297 using the 45-m radio telescope of the Nob ...
elt science case
... New observational facilities in the coming decade will try to address these questions. Furthermore, new fundamental question may arise: the evidence for dark energy was found only recently, and it added a new component to the Universe, the biggest component in terms of energy density at low redshift ...
... New observational facilities in the coming decade will try to address these questions. Furthermore, new fundamental question may arise: the evidence for dark energy was found only recently, and it added a new component to the Universe, the biggest component in terms of energy density at low redshift ...
Star clusters in M 33 - IV. A new survey from deep HST images
... with optical magnitudes was used to further constrain reddening and age for young M 33 clusters (Bianchi et al. 1999; Chandar et al. 1999c; hereafter Paper III). King profiles were fit to the brightest cluster radial profiles, and core radii are estimated in the range from <0.2 parsecs to ∼2 parsecs ...
... with optical magnitudes was used to further constrain reddening and age for young M 33 clusters (Bianchi et al. 1999; Chandar et al. 1999c; hereafter Paper III). King profiles were fit to the brightest cluster radial profiles, and core radii are estimated in the range from <0.2 parsecs to ∼2 parsecs ...
The GalMer database: galaxy mergers in the virtual observatory*
... curves of local spirals and dwarf galaxies, than the cuspy profiles predicted by Cold Dark Matter simulations (see Di Matteo et al. 2008a, Sect. 2.4.3 for a discussion). The stellar and gaseous discs follow the Miyamoto & Nagai (1975) density profile, with masses M∗ and Mg and vertical and radial sc ...
... curves of local spirals and dwarf galaxies, than the cuspy profiles predicted by Cold Dark Matter simulations (see Di Matteo et al. 2008a, Sect. 2.4.3 for a discussion). The stellar and gaseous discs follow the Miyamoto & Nagai (1975) density profile, with masses M∗ and Mg and vertical and radial sc ...
AN INITIAL MASS FUNCTION STUDY OF THE DWARF Please share
... the synthesis of composite populations using individual stellar clusters which are stochastically populated with stars, using the IMF as a probability distribution function. Other stochastic models are presented in Popescu & Hanson (2010), but are not used in this study. According to Cerviño & Luri ...
... the synthesis of composite populations using individual stellar clusters which are stochastically populated with stars, using the IMF as a probability distribution function. Other stochastic models are presented in Popescu & Hanson (2010), but are not used in this study. According to Cerviño & Luri ...
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.