Elliptical Galaxies
... where Re , the effective radius, is the radius that contains half the total light of the galaxy and Ie is the surface brightness (the amount of light from a square arc second of the galaxy) at Re . This law can be integrated to give a finite total light of Itot = 7.22πRe 2 Ie . de Vaucouleurs’ law, ...
... where Re , the effective radius, is the radius that contains half the total light of the galaxy and Ie is the surface brightness (the amount of light from a square arc second of the galaxy) at Re . This law can be integrated to give a finite total light of Itot = 7.22πRe 2 Ie . de Vaucouleurs’ law, ...
AST 346, Galaxies, Part 6
... SBb NGC 3351, M95 The bar lacks young hot stars which are concentrated in knots in the spiral arms. Care must be taken in interpreting images of high-redshift galaxies. ...
... SBb NGC 3351, M95 The bar lacks young hot stars which are concentrated in knots in the spiral arms. Care must be taken in interpreting images of high-redshift galaxies. ...
Studies of molecular clouds at the Galactic centre Roland Karlsson DECLINATION (B1950)
... In spiral galaxies, radial transport of material is considered essential for the build-up of the energy budget and the evolution of the various phenomena that are observed at different galactocentric radii. In barred spiral galaxies like the Galaxy, large scale transversal bars are suggested to pump ...
... In spiral galaxies, radial transport of material is considered essential for the build-up of the energy budget and the evolution of the various phenomena that are observed at different galactocentric radii. In barred spiral galaxies like the Galaxy, large scale transversal bars are suggested to pump ...
The environment of high-redshift AGN OLIMPIA JUDIT FOGASY
... appearance, one has to look at the various ways a galaxy can grow. According to the currently accepted cosmological model, the Λ Cold Dark Matter model (ΛCDM), structure formation started from primordial density fluctuations followed by gravitational collapse of dark matter, leading to the formation ...
... appearance, one has to look at the various ways a galaxy can grow. According to the currently accepted cosmological model, the Λ Cold Dark Matter model (ΛCDM), structure formation started from primordial density fluctuations followed by gravitational collapse of dark matter, leading to the formation ...
FLARE SWG theme 3: high
... Quasars: in this talk we mean any AGN that can be detected by FLARE (including obscured) ...
... Quasars: in this talk we mean any AGN that can be detected by FLARE (including obscured) ...
– 1 – 1. Galaxy Observations 1.1.
... the nearby Coma cluster and the Shapley Supercluster of galaxies, studying galaxies of a wide luminosity (i.e. mass) range with moderate resolution but high accuracy spectra. A fixed aperture size is used for each galaxy, corresponding to a fixed physical size for each of the two galaxy clusters. Th ...
... the nearby Coma cluster and the Shapley Supercluster of galaxies, studying galaxies of a wide luminosity (i.e. mass) range with moderate resolution but high accuracy spectra. A fixed aperture size is used for each galaxy, corresponding to a fixed physical size for each of the two galaxy clusters. Th ...
lecture course
... undergoing nuclear fusion and releasing energy in the form of (mostly visible) electromagnetic waves. They have masses typically 0.1 to 100 times the mass of the sun, and have a blackbody spectrum that peaks at longer wavelengths for lower mass stars (it peaks at about 500 nm for the Sun). The evolu ...
... undergoing nuclear fusion and releasing energy in the form of (mostly visible) electromagnetic waves. They have masses typically 0.1 to 100 times the mass of the sun, and have a blackbody spectrum that peaks at longer wavelengths for lower mass stars (it peaks at about 500 nm for the Sun). The evolu ...
Introduction
... volume and mass limited, and includes galaxies of all morphological types inhabiting a range of different environments, from galaxies in the dense core of the Virgo cluster to relatively isolated systems. As such, the sample is ideal for disentangling the internal and environmental processes driving ...
... volume and mass limited, and includes galaxies of all morphological types inhabiting a range of different environments, from galaxies in the dense core of the Virgo cluster to relatively isolated systems. As such, the sample is ideal for disentangling the internal and environmental processes driving ...
The Host Galaxies of the Brightest Quasars: Gas
... as the quasars. These pioneering observations unambiguously established the connection between quasars and galaxies. The huge quantities of luminous energy escaping from quasars immediately leads to questions about the properties of their host galaxies. Are quasar host galaxies normal galaxies? Are ...
... as the quasars. These pioneering observations unambiguously established the connection between quasars and galaxies. The huge quantities of luminous energy escaping from quasars immediately leads to questions about the properties of their host galaxies. Are quasar host galaxies normal galaxies? Are ...
Full-text PDF
... them from forming stars at late times when their mass and morphology can still change through mergers. The result is a galaxy luminosity function with a sharper high-mass cutoff in which the most massive systems are red, dead and elliptical. To make quantitative predictions for the galaxy population ...
... them from forming stars at late times when their mass and morphology can still change through mergers. The result is a galaxy luminosity function with a sharper high-mass cutoff in which the most massive systems are red, dead and elliptical. To make quantitative predictions for the galaxy population ...
the stebbins galaxy: the origins of interstellar medium studies
... is far from that center, which must lie roughly in the direction of the constellation Sagittarius. This was a most important result and a transformative insight, which challenged the then current statistical models constructed, for example, by Jacobus C. Kapteyn (1851–1922) and Hugo von Seeliger (18 ...
... is far from that center, which must lie roughly in the direction of the constellation Sagittarius. This was a most important result and a transformative insight, which challenged the then current statistical models constructed, for example, by Jacobus C. Kapteyn (1851–1922) and Hugo von Seeliger (18 ...
Lifetime of merger features of equal
... a single stellar population using population synthesis models. This method is effective because of its simplicity and applicability. Several studies have examined the observable properties of merger remnants by assuming the total amount of dust extinction from empirical data (Kaviraj et al. 2009; Ga ...
... a single stellar population using population synthesis models. This method is effective because of its simplicity and applicability. Several studies have examined the observable properties of merger remnants by assuming the total amount of dust extinction from empirical data (Kaviraj et al. 2009; Ga ...
Galaxy Evolution
... ELLIPTICAL GALAXIES consist only of the bulge component and have no disk. LENTICULAR GALAXIES are essentially ellipticals with a very thin, often almost invisible disk, which gives them the shape of a lentil. SPIRAL GALAXIES have both a bulge and a disk with spiral arms. If a bar is present, this co ...
... ELLIPTICAL GALAXIES consist only of the bulge component and have no disk. LENTICULAR GALAXIES are essentially ellipticals with a very thin, often almost invisible disk, which gives them the shape of a lentil. SPIRAL GALAXIES have both a bulge and a disk with spiral arms. If a bar is present, this co ...
Galaxy Evolution Encyclopedia of Astronomy & Astrophysics eaa.iop.org Mauro Giavalisco
... ELLIPTICAL GALAXIES consist only of the bulge component and have no disk. LENTICULAR GALAXIES are essentially ellipticals with a very thin, often almost invisible disk, which gives them the shape of a lentil. SPIRAL GALAXIES have both a bulge and a disk with spiral arms. If a bar is present, this co ...
... ELLIPTICAL GALAXIES consist only of the bulge component and have no disk. LENTICULAR GALAXIES are essentially ellipticals with a very thin, often almost invisible disk, which gives them the shape of a lentil. SPIRAL GALAXIES have both a bulge and a disk with spiral arms. If a bar is present, this co ...
Galaxies
... Edwin Hubble noticed that there were Cepheid variable stars in the Andromeda “nebula” Using the luminosity, period relation for Cepheids and the measured luminosity, he showed that the Andromeda system was far outside of the Milky Way Hubble did similar studies with respect to many of the other “neb ...
... Edwin Hubble noticed that there were Cepheid variable stars in the Andromeda “nebula” Using the luminosity, period relation for Cepheids and the measured luminosity, he showed that the Andromeda system was far outside of the Milky Way Hubble did similar studies with respect to many of the other “neb ...
Article PDF - IOPscience
... Table 1, appear to show (1) a steady rise of the metallicity index [Fe/H] with time and (2) that the rate of star formation between 2.5 and 7 Gyr ago was an order of magnitude lower than it has been during the most recent 2È3 Gyr period. Since the two Ðelds studied by Dolphin are separated by 3.0 (2 ...
... Table 1, appear to show (1) a steady rise of the metallicity index [Fe/H] with time and (2) that the rate of star formation between 2.5 and 7 Gyr ago was an order of magnitude lower than it has been during the most recent 2È3 Gyr period. Since the two Ðelds studied by Dolphin are separated by 3.0 (2 ...
X. Nuclear star clusters in low-mass early-type galaxies
... 2005). Evidently, there is no consensus on the dominant formation channel of NSCs in dEs. And if such a dominant formation channel exists, it may well be dependent on the morphological type or mass of the host galaxy or indirectly on the environment. For the spiral galaxy NGC 4244, Hartmann et al. ( ...
... 2005). Evidently, there is no consensus on the dominant formation channel of NSCs in dEs. And if such a dominant formation channel exists, it may well be dependent on the morphological type or mass of the host galaxy or indirectly on the environment. For the spiral galaxy NGC 4244, Hartmann et al. ( ...
Andromeda Galaxy
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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.