Lecture 4
... Measuring distances is a difficult issue in Astronomy. The sky is seen in 2-dimensions, the third one is not accessible directly. Only projected distances are measured. Distances of galaxies are essentially measured thanks to their general move due to the universe expansion. In the nearby universe o ...
... Measuring distances is a difficult issue in Astronomy. The sky is seen in 2-dimensions, the third one is not accessible directly. Only projected distances are measured. Distances of galaxies are essentially measured thanks to their general move due to the universe expansion. In the nearby universe o ...
pdf of talk
... • Early results have improved measurements of the distance to the Galactic Center and rotational velocity • R0 = 8.4 ± 0.6 kpc • 0 = 254 ± 16 km/s One of 10 top-cited astrophysics papers between 2009 and 2011 ...
... • Early results have improved measurements of the distance to the Galactic Center and rotational velocity • R0 = 8.4 ± 0.6 kpc • 0 = 254 ± 16 km/s One of 10 top-cited astrophysics papers between 2009 and 2011 ...
Finnish Centre for Astronomy with ESO
... cosmology, active galaxies, and galaxy formation and evolution, through properties of nearby galaxies, to supernovae and their progenitor stars, stellar magnetic activity, star formation and exoplanets in our own Galaxy. In our research, we use radio to gamma-rays multi-wavelength observational data ...
... cosmology, active galaxies, and galaxy formation and evolution, through properties of nearby galaxies, to supernovae and their progenitor stars, stellar magnetic activity, star formation and exoplanets in our own Galaxy. In our research, we use radio to gamma-rays multi-wavelength observational data ...
Galaxy Hunters Article, Cosmology Information, First Star Facts
... Cepheid variable. This type of star has a wonderful property: Its brightness waxes and wanes like clockwork, and the longer it takes to vary, the greater the star's intrinsic brightness. That means the star can be used to measure cosmic distances. By comparing the true brightness of the Cepheid in M ...
... Cepheid variable. This type of star has a wonderful property: Its brightness waxes and wanes like clockwork, and the longer it takes to vary, the greater the star's intrinsic brightness. That means the star can be used to measure cosmic distances. By comparing the true brightness of the Cepheid in M ...
CUSPS AND CORES IN GALAXIES:PROBLEMS AND - Cosmo-ufes
... Figures illustrating the basic observables and results typical for X-ray analyses of cluster mass distributions. Typically, the X-ray image is split up into a series of circular, concentric annuli, with the spectrum of each annulus compared to a plasma model to infer the gas density and temperature. ...
... Figures illustrating the basic observables and results typical for X-ray analyses of cluster mass distributions. Typically, the X-ray image is split up into a series of circular, concentric annuli, with the spectrum of each annulus compared to a plasma model to infer the gas density and temperature. ...
Co-Evolution of Galactic Nuclei and Globular Cluster Systems
... dynamical friction, globular star clusters have spiraled from larger radii to the inner few parsecs of a galaxy and there deposited a dense and massive concentration of stars. These stars would form a NSC which, via various dynamical processes, may produce the seed of a supermassive black hole. The ...
... dynamical friction, globular star clusters have spiraled from larger radii to the inner few parsecs of a galaxy and there deposited a dense and massive concentration of stars. These stars would form a NSC which, via various dynamical processes, may produce the seed of a supermassive black hole. The ...
Galaxies - WordPress.com
... some astronomers believe that giant elliptical galaxies are formed from A the collapse of a small cluster of galaxies into one giant galaxy B the collisional merging of galaxies in an irregular cluster of galaxies C stars pulled from nearby galaxies in a cluster by a larger-than-normal elliptical ga ...
... some astronomers believe that giant elliptical galaxies are formed from A the collapse of a small cluster of galaxies into one giant galaxy B the collisional merging of galaxies in an irregular cluster of galaxies C stars pulled from nearby galaxies in a cluster by a larger-than-normal elliptical ga ...
PEGASUS, THE FLYING HORSE Pegasus is a constellation in the
... with a redshift of 0.0027. It was discovered by musician-astronomer William Herschel in 1784 and was later one of the first nebulous objects to be described as "spiral" by William Parsons. Another of Pegasus's galaxies is NGC 7742, a Type 2 Seyfert galaxy. Located at a distance of 77 million light-y ...
... with a redshift of 0.0027. It was discovered by musician-astronomer William Herschel in 1784 and was later one of the first nebulous objects to be described as "spiral" by William Parsons. Another of Pegasus's galaxies is NGC 7742, a Type 2 Seyfert galaxy. Located at a distance of 77 million light-y ...
sections 23-25 powerpoint
... bluer in colour than isolated galaxies, presumably because of the presence of recently-created hot young stars. It is believed that a tidal interaction with another galaxy has induced star formation, although the resulting excess luminosity is hidden behind obscuring clouds of gas and dust. Such gal ...
... bluer in colour than isolated galaxies, presumably because of the presence of recently-created hot young stars. It is believed that a tidal interaction with another galaxy has induced star formation, although the resulting excess luminosity is hidden behind obscuring clouds of gas and dust. Such gal ...
spatially resolved properties of the stellar populations
... assembled their mass through dissipative processes and in-situ star formation. The star formation is induced by cold flow accretion or by gas-rich mergers. Then, ex-situ star formation formed by minor mergers of galaxies with the central more massive one. Because the central core of these ETG have e ...
... assembled their mass through dissipative processes and in-situ star formation. The star formation is induced by cold flow accretion or by gas-rich mergers. Then, ex-situ star formation formed by minor mergers of galaxies with the central more massive one. Because the central core of these ETG have e ...
Galaxy Spiral Arms
... mass such as the Sun. Our Milky Way Galaxy has distributed mass, where hundreds of billions of individual stars all contribute to the total mass of the Galaxy. On a gross scale, that mass is relatively symmetrical, so for our gravitational effect on any other galaxy, yes, our entire Galaxy acts as t ...
... mass such as the Sun. Our Milky Way Galaxy has distributed mass, where hundreds of billions of individual stars all contribute to the total mass of the Galaxy. On a gross scale, that mass is relatively symmetrical, so for our gravitational effect on any other galaxy, yes, our entire Galaxy acts as t ...
Feedback - Cambridge University Press
... halos with fb ≈ 1, combined with the relatively short gas cooling times in many massive clusters, suggests that something is preventing gas from turning into stars. One possible explanation is that the gas is heated by active galactic nuclei, which are seen in almost all clusters with cooling times ...
... halos with fb ≈ 1, combined with the relatively short gas cooling times in many massive clusters, suggests that something is preventing gas from turning into stars. One possible explanation is that the gas is heated by active galactic nuclei, which are seen in almost all clusters with cooling times ...
From Cosmic Birth to Living Earth - Association of Universities for
... towards constructing a general purpose, long-life, space-based observatory that is capable of finding planets showing signs of life. Such an observatory would be able to survey hundreds of planetary systems and detect dozens of Earth-like planets in the habitable zones around their stars. It would a ...
... towards constructing a general purpose, long-life, space-based observatory that is capable of finding planets showing signs of life. Such an observatory would be able to survey hundreds of planetary systems and detect dozens of Earth-like planets in the habitable zones around their stars. It would a ...
- Cosmotography
... dwarfs have been identified observationally (Stinson et al. 2009), but it is not clear if these stars were accreted, or formed in-situ. Star formation in dwarfs is thought to occur in stochastic episodes (Tolstoy et al. 2009; Weisz et al. 2011), which could be triggered by accretion events. An iconi ...
... dwarfs have been identified observationally (Stinson et al. 2009), but it is not clear if these stars were accreted, or formed in-situ. Star formation in dwarfs is thought to occur in stochastic episodes (Tolstoy et al. 2009; Weisz et al. 2011), which could be triggered by accretion events. An iconi ...
script
... into the universe of galaxies beyond. As we journey outward to distant galaxies we discover a surprising fact: the distant galaxies look much different than the galaxies closer to our Milky Way. Why is this? As it turns out, the light from these distant galaxies takes a much longer time to reach us ...
... into the universe of galaxies beyond. As we journey outward to distant galaxies we discover a surprising fact: the distant galaxies look much different than the galaxies closer to our Milky Way. Why is this? As it turns out, the light from these distant galaxies takes a much longer time to reach us ...
Messier 87
Messier 87 (also known as Virgo A or NGC 4486, and generally abbreviated to M87) is a supergiant elliptical galaxy in the constellation Virgo. One of the most massive galaxies in the local universe, it is notable for its large population of globular clusters—M87 contains about 12,000 compared to the 150-200 orbiting the Milky Way—and its jet of energetic plasma that originates at the core and extends outward at least 1,500 parsecs (4,900 light-years), travelling at relativistic speed. It is one of the brightest radio sources in the sky, and is a popular target for both amateur astronomy observations and professional astronomy study.French astronomer Charles Messier discovered M87 in 1781, cataloguing it as a nebulous feature while searching for objects that would confuse comet hunters. The second brightest galaxy within the northern Virgo Cluster, M87 is located about 16.4 million parsecs (53.5 million light-years) from Earth. Unlike a disk-shaped spiral galaxy, M87 has no distinctive dust lanes. Instead, it has an almost featureless, ellipsoidal shape typical of most giant elliptical galaxies, diminishing in luminosity with distance from the centre. Forming around one sixth of M87's mass, the stars in this galaxy have a nearly spherically symmetric distribution, their density decreasing with increasing distance from the core. At the core is a supermassive black hole, which forms the primary component of an active galactic nucleus. This object is a strong source of multiwavelength radiation, particularly radio waves. M87's galactic envelope extends out to a radius of about 150 kiloparsecs (490,000 light-years), where it has been truncated—possibly by an encounter with another galaxy. Between the stars is a diffuse interstellar medium of gas that has been chemically enriched by elements emitted from evolved stars.