Slide 1
... The ability to detect spectral line emission from CO or C+ in a normal galaxy like the Milky Way at a redshift of z = 3, in less than 24 hours of observation. The ability to image the gas kinematics in a solar-mass protostellar/ protoplanetary disk at a distance of 150 pc (roughly, the distance ...
... The ability to detect spectral line emission from CO or C+ in a normal galaxy like the Milky Way at a redshift of z = 3, in less than 24 hours of observation. The ability to image the gas kinematics in a solar-mass protostellar/ protoplanetary disk at a distance of 150 pc (roughly, the distance ...
Spring 2015 Mercury - Astronomical Society of the Pacific
... A quarter-century and five servicing missions later, Hubble is performing better than ever. But perhaps the most fascinating aspect of Hubble’s history is that it’s making observations that were never envisioned when it was being designed and built. Here’s one example. In the July 1982 Scientific Am ...
... A quarter-century and five servicing missions later, Hubble is performing better than ever. But perhaps the most fascinating aspect of Hubble’s history is that it’s making observations that were never envisioned when it was being designed and built. Here’s one example. In the July 1982 Scientific Am ...
- StealthSkater
... planets. Apparently the formation of a planetary system robs the star of much of its rotational momentum. For two reasons, then, we eliminate stars of class 'F4' and above: (1) most of them rotate rapidly and thus seem to be planet-less; and (2) their stable lifespans are too brief for advanced life ...
... planets. Apparently the formation of a planetary system robs the star of much of its rotational momentum. For two reasons, then, we eliminate stars of class 'F4' and above: (1) most of them rotate rapidly and thus seem to be planet-less; and (2) their stable lifespans are too brief for advanced life ...
The Physical Origins of The Morphology
... monly invoked. In any case, gas-deficient spiral galaxies in clusters do exist (e.g., Giovanelli & Haynes 1985), which indicates that gas stripping occurs. Eventually, in all these scenarios, gas stripping removes the fuel for star formation, presumably producing a quiescent galaxy which is similar ...
... monly invoked. In any case, gas-deficient spiral galaxies in clusters do exist (e.g., Giovanelli & Haynes 1985), which indicates that gas stripping occurs. Eventually, in all these scenarios, gas stripping removes the fuel for star formation, presumably producing a quiescent galaxy which is similar ...
A numerical study of recent tidal interactions between dwarf galaxies
... These simulations demonstrated that the presence of a Milky Way-like dark matter halo has an influence on the evolution of the dwarf galaxies. In all studies tidal stripping and tidal tails were observed. These interactions also led to star formation bursts in the dwarf galaxies. And there was stat ...
... These simulations demonstrated that the presence of a Milky Way-like dark matter halo has an influence on the evolution of the dwarf galaxies. In all studies tidal stripping and tidal tails were observed. These interactions also led to star formation bursts in the dwarf galaxies. And there was stat ...
PDF - ASSA
... la Ponte, Graham Low, Albie Lombard, and Jacques Mare, are engaged with their own programmes as they work through the Top-100. Find out more at [ http://assa.saao.ac.za/sections/ deep-sky/nebulae-clusters/assa-top-100/ ]. ...
... la Ponte, Graham Low, Albie Lombard, and Jacques Mare, are engaged with their own programmes as they work through the Top-100. Find out more at [ http://assa.saao.ac.za/sections/ deep-sky/nebulae-clusters/assa-top-100/ ]. ...
X. Nuclear star clusters in low-mass early-type galaxies
... limiting magnitude on the bright side of the magnitude range since for this paper we focus exclusively on NSCs in dE galaxies: it has been found that low-mass (non-dwarf) ellipticals often have a central light excess, but lack the distinct surface brightness bump and often distinct colours seen in l ...
... limiting magnitude on the bright side of the magnitude range since for this paper we focus exclusively on NSCs in dE galaxies: it has been found that low-mass (non-dwarf) ellipticals often have a central light excess, but lack the distinct surface brightness bump and often distinct colours seen in l ...
- Spiral - Imperial College London
... For this, we employ disc area coverages from the SATIRES model (with “S” standing for the satellite era, see Krivova et al. 2011). SATIRE-S distinguishes three active components (together often referred to as active regions) representing spot umbra, spot penumbra, and faculae. The part of the solar ...
... For this, we employ disc area coverages from the SATIRES model (with “S” standing for the satellite era, see Krivova et al. 2011). SATIRE-S distinguishes three active components (together often referred to as active regions) representing spot umbra, spot penumbra, and faculae. The part of the solar ...
Cassiopeia Kelly Pearce
... within the boundary of the constellation. These observable objects include both New General Catalogue objects and Messier objects. New General Catalogue is a catalogue of recorded deep sky objects and is referred to as NGC (SEDS, The Messier Catalog, 2010). The first of these objects, NGC 457, is al ...
... within the boundary of the constellation. These observable objects include both New General Catalogue objects and Messier objects. New General Catalogue is a catalogue of recorded deep sky objects and is referred to as NGC (SEDS, The Messier Catalog, 2010). The first of these objects, NGC 457, is al ...
Here
... of the currently known sample are presented and discussed. The star formation rates derived from the FIR luminosity range from about 300 to 5000 M⊙ year−1 and the molecular mass from 4 × 109 to 1 × 1011 M⊙ . At the lower end, these star formation rates, gas masses, and diameters are similar to those ...
... of the currently known sample are presented and discussed. The star formation rates derived from the FIR luminosity range from about 300 to 5000 M⊙ year−1 and the molecular mass from 4 × 109 to 1 × 1011 M⊙ . At the lower end, these star formation rates, gas masses, and diameters are similar to those ...
Spectroscopic Studies of Evolved Stars and Planetary Nebulae
... Evolved stars and planetary nebulae are rich and varied sites of molecule and dust formation. These objects undergo dramatic mass loss which ultimately enriches the interstellar medium. In this thesis, a number of studies, outlined below, have been undertaken to better understand the chemical and ph ...
... Evolved stars and planetary nebulae are rich and varied sites of molecule and dust formation. These objects undergo dramatic mass loss which ultimately enriches the interstellar medium. In this thesis, a number of studies, outlined below, have been undertaken to better understand the chemical and ph ...
an introduction to astrophysics
... In order to successfully study one or both of the Open University’s Level 3 courses, S382 Astrophysics or S383 The Relativistic Universe, you should already be familiar with various topics in cosmology, astronomy, planetary science, physics and mathematics. The level of skills, knowledge and underst ...
... In order to successfully study one or both of the Open University’s Level 3 courses, S382 Astrophysics or S383 The Relativistic Universe, you should already be familiar with various topics in cosmology, astronomy, planetary science, physics and mathematics. The level of skills, knowledge and underst ...
A Spitzer mid-infrared spectral survey of mass
... mass-loss: the so-called superwind phase. After this final burst of activity, the star remains as a hot, compact white dwarf of mass 0.6– 1.4 M . The expanding ejecta surrounding the star become ionized and form a planetary nebula, before dispersing into the interstellar medium (ISM). The superwind ...
... mass-loss: the so-called superwind phase. After this final burst of activity, the star remains as a hot, compact white dwarf of mass 0.6– 1.4 M . The expanding ejecta surrounding the star become ionized and form a planetary nebula, before dispersing into the interstellar medium (ISM). The superwind ...
12-1 - Piscataway High School
... arc. A parsec is 206,265 AU, which equals roughly 3.26 ly (light-years).* The blurring caused by Earth’s atmosphere makes star images about 1 second of arc in diameter, and that makes it difficult to measure parallax from Earth’s surface. Even when astronomers average together many observations, they ...
... arc. A parsec is 206,265 AU, which equals roughly 3.26 ly (light-years).* The blurring caused by Earth’s atmosphere makes star images about 1 second of arc in diameter, and that makes it difficult to measure parallax from Earth’s surface. Even when astronomers average together many observations, they ...
Stellar Evolution Nucleosynthesis
... Helium fusion tough—larger charge leads to greater repulsion. Worse, the fusion of two helium nuclei doesn’t work; 4He more stable than Beryllium (8Be). Need three 4He nuclei to make carbon (12C). Only works because of resonant state of carbon predicted by ...
... Helium fusion tough—larger charge leads to greater repulsion. Worse, the fusion of two helium nuclei doesn’t work; 4He more stable than Beryllium (8Be). Need three 4He nuclei to make carbon (12C). Only works because of resonant state of carbon predicted by ...
Mapping the Pathways of Galaxy Transformation Across Time and
... Is “quenching” the termination of star formation or the compression of star formation histories (SFHs)? I discuss the deep implications this reframing has for what we see as and how we study core processes shaping galaxy life-cycles. As a lens, I use two outcomes from the IMACS Cluster-Building Surv ...
... Is “quenching” the termination of star formation or the compression of star formation histories (SFHs)? I discuss the deep implications this reframing has for what we see as and how we study core processes shaping galaxy life-cycles. As a lens, I use two outcomes from the IMACS Cluster-Building Surv ...
2 Justification and benefits in joining TMT
... The TMT partnership will form in the next two years, which offers a once in a lifetime opportunity that China simply cannot miss. China has a rich and proud history in astronomy; Chinese civilisation kept the best record for comets, Sun spots, and supernovae in the world. For example, the supernovae ...
... The TMT partnership will form in the next two years, which offers a once in a lifetime opportunity that China simply cannot miss. China has a rich and proud history in astronomy; Chinese civilisation kept the best record for comets, Sun spots, and supernovae in the world. For example, the supernovae ...
The MORGANA model for the rise of galaxies and active nuclei
... We present the Model for the Rise of Galaxies and Active Nuclei (MORGANA), a new code for the formation and evolution of galaxies and active galactic nuclei (AGNs). Starting from the merger trees of dark matter (DM) haloes and a model for the evolution of substructure within the haloes, the complex ...
... We present the Model for the Rise of Galaxies and Active Nuclei (MORGANA), a new code for the formation and evolution of galaxies and active galactic nuclei (AGNs). Starting from the merger trees of dark matter (DM) haloes and a model for the evolution of substructure within the haloes, the complex ...
Physical Processes in the Interstellar Medium
... which trace so-called “dark molecular gas”, i.e. clouds with high H2 fractions but little CO (see e.g. Pineda et al. 2013). The molecular gas surface density shows a pronounced peak within the central 500 pc of the Galaxy, a region known as the Central Molecular Zone (CMZ). It then falls off sharply ...
... which trace so-called “dark molecular gas”, i.e. clouds with high H2 fractions but little CO (see e.g. Pineda et al. 2013). The molecular gas surface density shows a pronounced peak within the central 500 pc of the Galaxy, a region known as the Central Molecular Zone (CMZ). It then falls off sharply ...
Radiative winds, accretion disks and massive stars physics using
... from the ground state, the line is a resonance line and the scattering is called resonance scattering. Most P Cygni profiles are formed from resonance scattering. • Line emission by recombination – If an ion in a stellar wind collides with an electron it can recombine. The most likely recombination ...
... from the ground state, the line is a resonance line and the scattering is called resonance scattering. Most P Cygni profiles are formed from resonance scattering. • Line emission by recombination – If an ion in a stellar wind collides with an electron it can recombine. The most likely recombination ...
exploring anticorrelations and light element variations
... for 10 northern GCs. Some of these clusters are well studied, such as M3, M13, M92, and M15, while others have been poorly studied (NGC 5466), or have been only recently discussed in the literature, such as M2 (Yong et al. 2014). ...
... for 10 northern GCs. Some of these clusters are well studied, such as M3, M13, M92, and M15, while others have been poorly studied (NGC 5466), or have been only recently discussed in the literature, such as M2 (Yong et al. 2014). ...
Evolution of Circumstellar Disks Around Normal Stars
... Spitzer Space Telescope and high contrast images of spectacular individual systems. Detection statistics that were very uncertain with IRAS and ISO sensitivity now can be compared with models of planetary system evolution, placing our solar system in context. Advances in planetary system dynamical t ...
... Spitzer Space Telescope and high contrast images of spectacular individual systems. Detection statistics that were very uncertain with IRAS and ISO sensitivity now can be compared with models of planetary system evolution, placing our solar system in context. Advances in planetary system dynamical t ...
Science Case for the Chinese Participation of TMT
... The TMT partnership will form in the next two years, which offers a once in a lifetime opportunity that China simply cannot miss. China has a rich and proud history in astronomy; Chinese civilisation kept the best record for comets, Sun spots, and supernovae in the world. For example, the supernovae ...
... The TMT partnership will form in the next two years, which offers a once in a lifetime opportunity that China simply cannot miss. China has a rich and proud history in astronomy; Chinese civilisation kept the best record for comets, Sun spots, and supernovae in the world. For example, the supernovae ...
Element Segregation in Low Metallicity Stars and the Primordial
... Stellar models including element segregation predict a surface lithium depletion which depends on the effective temperature, the age and the metallicity of the stars. This prediction is in contradiction with the observations of the lithium plateau in Pop II stars. However, as discussed above, the li ...
... Stellar models including element segregation predict a surface lithium depletion which depends on the effective temperature, the age and the metallicity of the stars. This prediction is in contradiction with the observations of the lithium plateau in Pop II stars. However, as discussed above, the li ...
Grand Design and Flocculent Spirals in the Spitzer Survey of Stellar
... stars dominate. The sample includes flocculent, multiple arm, and grand design types with a wide range of Hubble and bar types. We find that most optically flocculent galaxies are also flocculent in the mid-IR because of star formation uncorrelated with stellar density waves, whereas multiple arm an ...
... stars dominate. The sample includes flocculent, multiple arm, and grand design types with a wide range of Hubble and bar types. We find that most optically flocculent galaxies are also flocculent in the mid-IR because of star formation uncorrelated with stellar density waves, whereas multiple arm an ...
H II region
An H II region is a large, low-density cloud of partially ionized gas in which star formation has recently taken place. The short-lived blue stars forged in these regions emit copious amounts of ultraviolet light that ionize the surrounding gas. H II regions—sometimes several hundred light-years across—are often associated with giant molecular clouds. The first known H II region was the Orion Nebula, which was discovered in 1610 by Nicolas-Claude Fabri de Peiresc.H II regions are named for the large amount of ionised atomic hydrogen they contain, referred to as H II, pronounced H-two by astronomers (an H I region being neutral atomic hydrogen, and H2 being molecular hydrogen). Such regions have extremely diverse shapes, because the distribution of the stars and gas inside them is irregular. They often appear clumpy and filamentary, sometimes showing bizarre shapes such as the Horsehead Nebula. H II regions may give birth to thousands of stars over a period of several million years. In the end, supernova explosions and strong stellar winds from the most massive stars in the resulting star cluster will disperse the gases of the H II region, leaving behind a cluster of birthed stars such as the Pleiades.H II regions can be seen to considerable distances in the universe, and the study of extragalactic H II regions is important in determining the distance and chemical composition of other galaxies. Spiral and irregular galaxies contain many H II regions, while elliptical galaxies are almost devoid of them. In the spiral galaxies, including the Milky Way, H II regions are concentrated in the spiral arms, while in the irregular galaxies they are distributed chaotically. Some galaxies contain huge H II regions, which may contain tens of thousands of stars. Examples include the 30 Doradus region in the Large Magellanic Cloud and NGC 604 in the Triangulum Galaxy.