The correlation between galaxy morphology and star
... et al. 2010; Cassata et al. 2010). The number density of these galaxies rapidly increases, by a factor of five, from z ∼ 2 to z ∼ 1, and they are up to 5 times more compact in size than local ones with similar mass (Cassata et al. 2011, 2013). Recent works have suggested, however, that a large fract ...
... et al. 2010; Cassata et al. 2010). The number density of these galaxies rapidly increases, by a factor of five, from z ∼ 2 to z ∼ 1, and they are up to 5 times more compact in size than local ones with similar mass (Cassata et al. 2011, 2013). Recent works have suggested, however, that a large fract ...
Isolated elliptical galaxies in the local Universe
... fraction of ellipticals with younger stellar populations is predicted than in clusters (Kauffmann 1996; Niemi et al. 2010). This may indicate different formation histories. Theoretical models suggest that ellipticals in clusters form through dissipative infall of gas and numerous mergers that took pla ...
... fraction of ellipticals with younger stellar populations is predicted than in clusters (Kauffmann 1996; Niemi et al. 2010). This may indicate different formation histories. Theoretical models suggest that ellipticals in clusters form through dissipative infall of gas and numerous mergers that took pla ...
... Theory and observations point to a variety of processes that redistribute energy in disks. In Section 2, we review evidence that bars and ovals rearrange disk gas into outer rings, inner rings, and central mass concentrations. The resulting star formation produces a central stellar subsystem that ha ...
Galaxy pairs in the Sloan Digital Sky Survey III. Evidence of induced
... roles of gas-rich versus gas-poor galaxies in interactions and mergers has yielded some conflicting results, due in part to the methods used to identify these systems and detect their star formation. Interacting galaxies which are identified based on morphological signs of interactions are strongly ...
... roles of gas-rich versus gas-poor galaxies in interactions and mergers has yielded some conflicting results, due in part to the methods used to identify these systems and detect their star formation. Interacting galaxies which are identified based on morphological signs of interactions are strongly ...
environmental effects on galaxy evolution in nearby clusters
... X-ray luminosity, evolutionary stage) they represent the most suitable ”laboratory” for comparative studies. By combining for the first time GALEX UV observations with optical, near and far infrared data, the evolutionary history of cluster galaxies is studied. The main goals of this thesis are: (a) ...
... X-ray luminosity, evolutionary stage) they represent the most suitable ”laboratory” for comparative studies. By combining for the first time GALEX UV observations with optical, near and far infrared data, the evolutionary history of cluster galaxies is studied. The main goals of this thesis are: (a) ...
Abstract The Star Formation History of Low Surface Brightness Galaxies
... The star formation histories of low surface brightness galaxies are interesting but poorly constrained. These objects tend to be rather blue, contradicting the initial impression that they may simply be faded remnants of higher surface brightness galaxies whose star formation has finished. Other sce ...
... The star formation histories of low surface brightness galaxies are interesting but poorly constrained. These objects tend to be rather blue, contradicting the initial impression that they may simply be faded remnants of higher surface brightness galaxies whose star formation has finished. Other sce ...
THE UV-OPTICAL COLOR MAGNITUDE DIAGRAM. II. PHYSICAL
... different morphological types. We find, among other trends, that our measure of the star formation rate surface density, SFR , is nearly constant along this sequence. We discuss this result and implications for galaxies at higher redshift. For the first time, we report on measurements of the local ...
... different morphological types. We find, among other trends, that our measure of the star formation rate surface density, SFR , is nearly constant along this sequence. We discuss this result and implications for galaxies at higher redshift. For the first time, we report on measurements of the local ...
Observational Studies of Interacting Galaxies and the Development
... photometric studies better constrain the number density evolution of wet and dry mergers through five CFHTLS broad band photometry up to z ∼ 1. Meanwhile, by comparing the merger and elliptical galaxy mass density function, I discovered that the most massive mergers are not all formed via merging pr ...
... photometric studies better constrain the number density evolution of wet and dry mergers through five CFHTLS broad band photometry up to z ∼ 1. Meanwhile, by comparing the merger and elliptical galaxy mass density function, I discovered that the most massive mergers are not all formed via merging pr ...
Observational evidence for AGN feedback in early
... strength of the Balmer lines that is at least what expected by recombination theory. From the fit to the stellar continuum and absorption features, we measure the line-of-sight velocity dispersions. From subtraction of the emission-line spectrum from the observed one, we get the clean absorption lin ...
... strength of the Balmer lines that is at least what expected by recombination theory. From the fit to the stellar continuum and absorption features, we measure the line-of-sight velocity dispersions. From subtraction of the emission-line spectrum from the observed one, we get the clean absorption lin ...
Identifying the progenitor set of present-day early
... We present a comprehensive theoretical study, using a semi-analytical model within the standard LCDM framework, of the photometric properties of the progenitors of present-day early-type galaxies in the redshift range 0 < z < 1. We explore progenitors of all morphologies and study their characterist ...
... We present a comprehensive theoretical study, using a semi-analytical model within the standard LCDM framework, of the photometric properties of the progenitors of present-day early-type galaxies in the redshift range 0 < z < 1. We explore progenitors of all morphologies and study their characterist ...
Galaxy And Mass Assembly (GAMA): Gas Fueling of Spiral Galaxies
... et al. 2011). For cosmological DMH detailed thermodynamic considerations of this process find a transition mass between these two modes, i.e., where the free-fall timescale equals the cooling timescale at the virial radius of ∼1011–1012 Me (Kereš et al. 2005; Dekel & Birnboim 2006).20 As such, the ac ...
... et al. 2011). For cosmological DMH detailed thermodynamic considerations of this process find a transition mass between these two modes, i.e., where the free-fall timescale equals the cooling timescale at the virial radius of ∼1011–1012 Me (Kereš et al. 2005; Dekel & Birnboim 2006).20 As such, the ac ...
Galaxies - hwchemistry
... of galaxies, however, they find that the measured masses are much larger than expected from the luminosities of the galaxies. • This seems to be true of most galaxies. – Measured masses of galaxies amount to 10 to 100 times more mass than you would expect from the appearance of galaxies. ...
... of galaxies, however, they find that the measured masses are much larger than expected from the luminosities of the galaxies. • This seems to be true of most galaxies. – Measured masses of galaxies amount to 10 to 100 times more mass than you would expect from the appearance of galaxies. ...
Preliminary Talk Abstract Book - MoCA
... Clusters of galaxies are the most massive virialised cosmic structures. The diversity of their environmental conditions, from the dense cores to the sparse outskirts, allows them to be used as observational laboratories for the study of the environmental drivers of galaxy evolution. Furthermore, the ...
... Clusters of galaxies are the most massive virialised cosmic structures. The diversity of their environmental conditions, from the dense cores to the sparse outskirts, allows them to be used as observational laboratories for the study of the environmental drivers of galaxy evolution. Furthermore, the ...
The SAMI Galaxy Survey: extraplanar gas, galactic winds, and their
... [S ii] to Balmer line ratios. This extraplanar gas in nearby prototype wind systems represents a very violent form of interactions between discs and haloes. In galaxies lacking spectacular large-scale winds, narrowband Hα imaging in nearby late-type edge-on galaxies reveals that eDIG is very common, ...
... [S ii] to Balmer line ratios. This extraplanar gas in nearby prototype wind systems represents a very violent form of interactions between discs and haloes. In galaxies lacking spectacular large-scale winds, narrowband Hα imaging in nearby late-type edge-on galaxies reveals that eDIG is very common, ...
Mapping the Pathways of Galaxy Transformation Across Time and
... University of Arizona, Steward Observatory ...
... University of Arizona, Steward Observatory ...
Andromeda Galaxy
The Andromeda Galaxy (/ænˈdrɒmɨdə/), also known as Messier 31, M31, or NGC 224, is a spiral galaxy approximately 780 kiloparsecs (2.5 million light-years) from Earth. It is the nearest major galaxy to the Milky Way and was often referred to as the Great Andromeda Nebula in older texts. It received its name from the area of the sky in which it appears, the constellation of Andromeda, which was named after the mythological princess Andromeda. Being approximately 220,000 light years across, it is the largest galaxy of the Local Group, which also contains the Milky Way, the Triangulum Galaxy, and about 44 other smaller galaxies.The Andromeda Galaxy is the most massive galaxy in the Local Group as well. Despite earlier findings that suggested that the Milky Way contains more dark matter and could be the most massive in the grouping, the 2006 observations by the Spitzer Space Telescope revealed that Andromeda contains one trillion (1012) stars: at least twice the number of stars in the Milky Way, which is estimated to be 200–400 billion.The Andromeda Galaxy is estimated to be 1.5×1012 solar masses, while the mass of the Milky Way is estimated to be 8.5×1011 solar masses. In comparison, a 2009 study estimated that the Milky Way and M31 are about equal in mass, while a 2006 study put the mass of the Milky Way at ~80% of the mass of the Andromeda Galaxy. The Milky Way and Andromeda are expected to collide in 3.75 billion years, eventually merging to form a giant elliptical galaxy or perhaps a large disk galaxy.At 3.4, the apparent magnitude of the Andromeda Galaxy is one of the brightest of any of the Messier objects, making it visible to the naked eye on moonless nights even when viewed from areas with moderate light pollution. Although it appears more than six times as wide as the full Moon when photographed through a larger telescope, only the brighter central region is visible to the naked eye or when viewed using binoculars or a small telescope and would it hence appear to be but another star.