AGN surveys to study galaxy evolution along cosmic times
... “The observed line intensities [....] in NGC1068 and 4151 closely resemble the line intensities of the planetary nebula NGC7027” and “The hydrogen lines in NGC4151 and 7469 are of unusual interest, being composed of relatively narrow cores (1100 km/sec wide) superposed on very wide wings (7500 km/se ...
... “The observed line intensities [....] in NGC1068 and 4151 closely resemble the line intensities of the planetary nebula NGC7027” and “The hydrogen lines in NGC4151 and 7469 are of unusual interest, being composed of relatively narrow cores (1100 km/sec wide) superposed on very wide wings (7500 km/se ...
Far-infrared line emission from high
... reaches ∼2.5 mJy and it is displaced from the centre of the galaxy by about 100 km s−1 . This is due to the fact that the gas within the central kpc of our galaxy is highly ionized by the massive stars that form there. We find that 95 per cent of the total [C II] flux originates from the CNM, and on ...
... reaches ∼2.5 mJy and it is displaced from the centre of the galaxy by about 100 km s−1 . This is due to the fact that the gas within the central kpc of our galaxy is highly ionized by the massive stars that form there. We find that 95 per cent of the total [C II] flux originates from the CNM, and on ...
The new X-ray universe
... of sources) and at the known distance of M82 this implied that it was “ultraluminous” (Lx >1039 erg s–1; the source in M82 varies up 1041 erg s–1). While the existence of such objects was hinted at by earlier missions, a substantial number have now been found in Chandra and XMM observations of nearb ...
... of sources) and at the known distance of M82 this implied that it was “ultraluminous” (Lx >1039 erg s–1; the source in M82 varies up 1041 erg s–1). While the existence of such objects was hinted at by earlier missions, a substantial number have now been found in Chandra and XMM observations of nearb ...
What Drives the Stellar Mass Growth of Early-Type
... We will build upon our expertise and existing toolkit to examine galaxies at an earlier epoch, providing rigorous, consistent, and minimally biased comparison samples for evaluating physical scenarios of galaxy formation and assembly. One fundamental aspect of this proposal is the major investment i ...
... We will build upon our expertise and existing toolkit to examine galaxies at an earlier epoch, providing rigorous, consistent, and minimally biased comparison samples for evaluating physical scenarios of galaxy formation and assembly. One fundamental aspect of this proposal is the major investment i ...
129 DYNAMICAL STREAMS IN THE SOLAR NEIGHBOURHOOD B
... alone is not sufficient to create the observed streams. Nevertheless, De Simone et al. (2004) have shown that the structure of the local distribution function could well be due to a lumpy potential related to the presence of strong transient spiral waves. Besides those simulations, a recent model of ...
... alone is not sufficient to create the observed streams. Nevertheless, De Simone et al. (2004) have shown that the structure of the local distribution function could well be due to a lumpy potential related to the presence of strong transient spiral waves. Besides those simulations, a recent model of ...
Chapter 15.3 Galaxy Evolution
... - Protogalactic clouds then collapse to form disk galaxies. - The difference of galaxies come from two sources: 1. The initial conditions of the protogalactic clouds are different, either the spin or the density, which results in different type of galaxies. 2. Later interactions or collisions of g ...
... - Protogalactic clouds then collapse to form disk galaxies. - The difference of galaxies come from two sources: 1. The initial conditions of the protogalactic clouds are different, either the spin or the density, which results in different type of galaxies. 2. Later interactions or collisions of g ...
Cosmology Physics 466E Olbers Paradox Cosmological principle
... the galactic center of clouds of ionized hydrogen (in astrophysical terminology, HII regions). This was done by measurement of the Doppler shift of their H-alpha emission lines. The hydrogen clouds move with the stars and other visible matter in the galaxies. Their velocities are more easily and dir ...
... the galactic center of clouds of ionized hydrogen (in astrophysical terminology, HII regions). This was done by measurement of the Doppler shift of their H-alpha emission lines. The hydrogen clouds move with the stars and other visible matter in the galaxies. Their velocities are more easily and dir ...
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... star-forming galaxies seen in deep images. Since the late 1970s it has been known that there are many more such systems than expected from our knowledge of the locally observed population. One of the first results from the Cambridge HST surveys was the identification of a strong increase with redshi ...
... star-forming galaxies seen in deep images. Since the late 1970s it has been known that there are many more such systems than expected from our knowledge of the locally observed population. One of the first results from the Cambridge HST surveys was the identification of a strong increase with redshi ...
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.