Cold versus Warm Dark Matter Simulations of a Galaxy Group
... immediately apparent from this figure: (1) there are far fewer small substructures and (2) the two groups differ substantially, cosmographically speaking. In Figures 3(a and c), we show the co-moving and physical distance between the three pairs of group members as a function of look-back time, norm ...
... immediately apparent from this figure: (1) there are far fewer small substructures and (2) the two groups differ substantially, cosmographically speaking. In Figures 3(a and c), we show the co-moving and physical distance between the three pairs of group members as a function of look-back time, norm ...
Environmental dependence of bulge
... Stellar masses have been obtained from the MPA-JHU DR7, derived through spectral energy distribution fitting using the Bruzual & Charlot (2003) synthesis population models, and converted to a Chabrier (2003) initial mass function (IMF), in line with the theoretical models described below. Our team h ...
... Stellar masses have been obtained from the MPA-JHU DR7, derived through spectral energy distribution fitting using the Bruzual & Charlot (2003) synthesis population models, and converted to a Chabrier (2003) initial mass function (IMF), in line with the theoretical models described below. Our team h ...
A large Hα survey at z = 2.23, 1.47, 0.84 and 0.40
... problems/limitations result from the difficulty of obtaining both large-area, large-sample, clean and deep observations (to overcome both cosmic variance and avoid large extrapolations down to faint luminosities). One way to make significant progress in our understanding of star formation at high re ...
... problems/limitations result from the difficulty of obtaining both large-area, large-sample, clean and deep observations (to overcome both cosmic variance and avoid large extrapolations down to faint luminosities). One way to make significant progress in our understanding of star formation at high re ...
![arXiv:1601.01542v1 [astro-ph.GA] 7 Jan 2016](http://s1.studyres.com/store/data/017487687_1-243c4cbda96da53325dd347b0c588a3e-300x300.png)
$^{13} $ CO/C $^{18} $ O Gradients Across the Disks of Nearby
... whole EMPIRE or ALMA area for each target. We observe widespread 13 CO(1-0) from each galaxy while C18 O(1-0) is fainter, requiring substantial averaging to achieve good signal to noise. After averaging, we detect C18 O at good significance for six targets in EMPIRE. The other two, NGC 2903 and NGC ...
... whole EMPIRE or ALMA area for each target. We observe widespread 13 CO(1-0) from each galaxy while C18 O(1-0) is fainter, requiring substantial averaging to achieve good signal to noise. After averaging, we detect C18 O at good significance for six targets in EMPIRE. The other two, NGC 2903 and NGC ...
Astronomy Astrophysics Spectral energy distributions of an AKARI-SDSS-GALEX sample of galaxies
... derives physical information about galaxies by fitting their UVto-far-IR SED (Noll et al. 2009b; Giovannoli et al. 2010). A Bayesian analysis is used to derive galaxy properties similar to that developed by Kauffmann et al. (2003a). CIGALE combines a UV-optical stellar SED and a dust, IR-emitting com ...
... derives physical information about galaxies by fitting their UVto-far-IR SED (Noll et al. 2009b; Giovannoli et al. 2010). A Bayesian analysis is used to derive galaxy properties similar to that developed by Kauffmann et al. (2003a). CIGALE combines a UV-optical stellar SED and a dust, IR-emitting com ...
The Properties of Super Star Clusters in A Sample of
... “Super star clusters” are the most massive extreme in the continuum of young star clusters. In this thesis, I examine the properties of such super star clusters in a sample of starburst galaxies with space and ground-based observations and in the optical, mid-infrared, and radio regimes. Using optic ...
... “Super star clusters” are the most massive extreme in the continuum of young star clusters. In this thesis, I examine the properties of such super star clusters in a sample of starburst galaxies with space and ground-based observations and in the optical, mid-infrared, and radio regimes. Using optic ...
Galaxy morphology, luminosity, and environment in the SDSS DR7
... For the SDSS survey, visual classification has become possible thanks to the Galaxy Zoo project (Lintott et al. 2008) that will help us to study the morphology and the LF in detail in the future. Recently Huertas-Company et al. (2011) have published an automated morphological classification based on ...
... For the SDSS survey, visual classification has become possible thanks to the Galaxy Zoo project (Lintott et al. 2008) that will help us to study the morphology and the LF in detail in the future. Recently Huertas-Company et al. (2011) have published an automated morphological classification based on ...
Acta Polytechnica
... The properties of hard X-rays and the cluster magnetic fields have been studied for about ten clusters so far. There is no significant detection of IC emission by Suzaku, giving the upper limits on the level of ∼ 10−11 erg s−1 cm−2 . Thus no clear relationship between the non-thermal X-ray and radio ...
... The properties of hard X-rays and the cluster magnetic fields have been studied for about ten clusters so far. There is no significant detection of IC emission by Suzaku, giving the upper limits on the level of ∼ 10−11 erg s−1 cm−2 . Thus no clear relationship between the non-thermal X-ray and radio ...
The Physical Origins of The Morphology
... and Padilla & Strauss (2008). Such an approach is complementary to studies of morphology, defined either visually or otherwise, because it makes no assumptions about the connection with galaxy structure. Because, in addition, we select our sample spectroscopically, our analysis is completely indepen ...
... and Padilla & Strauss (2008). Such an approach is complementary to studies of morphology, defined either visually or otherwise, because it makes no assumptions about the connection with galaxy structure. Because, in addition, we select our sample spectroscopically, our analysis is completely indepen ...
CONNECTING ANGULAR MOMENTUM AND GALACTIC DYNAMICS
... The evolution and distribution of the angular momentum of dark matter halos have been discussed in several studies over the last decades. In particular, the idea arose that angular momentum conservation should allow to infer the total angular momentum of the entire dark matter halo from measuring th ...
... The evolution and distribution of the angular momentum of dark matter halos have been discussed in several studies over the last decades. In particular, the idea arose that angular momentum conservation should allow to infer the total angular momentum of the entire dark matter halo from measuring th ...
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.