Mass and Metallicity Distribution Function of halos of simulated Disk
... also failed to create galaxies in which most baryonic matter resides in the thin disk, as observed in the Milky Way. Abadi et al (2003) create a stellar halo which contains over 60 % of the total stellar mass of the system , and a thin disk which constitues only 17%, more akin to an s0 than a late t ...
... also failed to create galaxies in which most baryonic matter resides in the thin disk, as observed in the Milky Way. Abadi et al (2003) create a stellar halo which contains over 60 % of the total stellar mass of the system , and a thin disk which constitues only 17%, more akin to an s0 than a late t ...
Galaxies and their properties
... 4. Irregular galaxies. These appear as patchy objects, dominated by few HII regions (= regions dominated by interstellar atomic, fully ionized hydrogen, i.e., H + ). Elliptical and lenticulars together are often referred to as early type galaxies, while spirals and irregulars are late type galaxies. ...
... 4. Irregular galaxies. These appear as patchy objects, dominated by few HII regions (= regions dominated by interstellar atomic, fully ionized hydrogen, i.e., H + ). Elliptical and lenticulars together are often referred to as early type galaxies, while spirals and irregulars are late type galaxies. ...
chapter 24 instructor notes
... known Shapley-Curtis debate on the extent of the Galactic system. The merits of the arguments presented on both sides of this debate have been the subject of considerable study over the years, but it was years later before the true extragalactic nature of the spiral nebulae was recognized. Although ...
... known Shapley-Curtis debate on the extent of the Galactic system. The merits of the arguments presented on both sides of this debate have been the subject of considerable study over the years, but it was years later before the true extragalactic nature of the spiral nebulae was recognized. Although ...
2013. CCAT. All Rights Reserved.
... X-Spec: a Multi-Object Wideband Spectrograph for CCAT: Concept and Technology Development C.M. Bradford for the X-Spec study team We are developing X-Spec, a multi-object wide-band direct-detection spectrometer for CCAT. X-Spec is designed for rapid full-band (195-510 GHz), moderate resolution (R~70 ...
... X-Spec: a Multi-Object Wideband Spectrograph for CCAT: Concept and Technology Development C.M. Bradford for the X-Spec study team We are developing X-Spec, a multi-object wide-band direct-detection spectrometer for CCAT. X-Spec is designed for rapid full-band (195-510 GHz), moderate resolution (R~70 ...
SWIRE
... The case for SWIRE • SIRTF will offer a unique chance to sample a largely unexplored waveband at 3 <λ<10 μm • This will allow photometric measurements of the baryonic mass in stars for an enormous number of distant and high-z galaxies • This is one of the main targets of our Legacy Program, SWIRE • ...
... The case for SWIRE • SIRTF will offer a unique chance to sample a largely unexplored waveband at 3 <λ<10 μm • This will allow photometric measurements of the baryonic mass in stars for an enormous number of distant and high-z galaxies • This is one of the main targets of our Legacy Program, SWIRE • ...
The Formation and Evolution of Massive Black Holes - Ira-Inaf
... alternative view, the galaxy-regulated hypothesis, the galaxy sets the MBH mass by regulating the amount of gas that trickles to the MBH. One of the most interesting results that has recently emerged on black hole and galaxy growth is the strong link between the global black hole growth rate and the ...
... alternative view, the galaxy-regulated hypothesis, the galaxy sets the MBH mass by regulating the amount of gas that trickles to the MBH. One of the most interesting results that has recently emerged on black hole and galaxy growth is the strong link between the global black hole growth rate and the ...
Course Outline - Tony Bacigalupo
... populated with stars at the center of the Galaxy The interstellar medium blocks our view of the center The center of the Galaxy is in the direction of Sagittarius ...
... populated with stars at the center of the Galaxy The interstellar medium blocks our view of the center The center of the Galaxy is in the direction of Sagittarius ...
The Formation and Evolution of the Milky Way
... (that is, the most massive ones) and more slowly in those elements produced essentially by type Ia supernovae and the low- and intermediate-mass stars. So the ratio of two elements—such as oxygen (O) and iron—that are returned to the interstellar medium on different timescales can be used as a “cloc ...
... (that is, the most massive ones) and more slowly in those elements produced essentially by type Ia supernovae and the low- and intermediate-mass stars. So the ratio of two elements—such as oxygen (O) and iron—that are returned to the interstellar medium on different timescales can be used as a “cloc ...
Cepheid Stars as standard candles for distance measurements
... first variable star which was analyzed in detail, stars of a similar brightness variation are called Cepheids. Later on, Belopolsky could explain the variation in brightness by radius variation of such stars by dint of Doppler effect. He detected a periodic shift of spectral lines of δ Cephei. Cephe ...
... first variable star which was analyzed in detail, stars of a similar brightness variation are called Cepheids. Later on, Belopolsky could explain the variation in brightness by radius variation of such stars by dint of Doppler effect. He detected a periodic shift of spectral lines of δ Cephei. Cephe ...
ASPEN WORKSHOP 2003
... determine the upper fine structure level population using its 1335.7Ang absorption line, seen in half of DLAs, (which has same profile as SiII 1808) (Upper level generally has much larger population than CMWB would produce) Use Fe depletion to estimate dust/gas ratio Cooling/heating rate per atom (c ...
... determine the upper fine structure level population using its 1335.7Ang absorption line, seen in half of DLAs, (which has same profile as SiII 1808) (Upper level generally has much larger population than CMWB would produce) Use Fe depletion to estimate dust/gas ratio Cooling/heating rate per atom (c ...
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.