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6.1 Introduction
... previous generation of stars which themselves presumably formed out of pristine gas. Thus, the chemical composition of the most metal-poor stars known is one of the means at our disposal to shed light on the nature of the ‘First Stars’, sometimes referred to as Population III stars. A further exampl ...
... previous generation of stars which themselves presumably formed out of pristine gas. Thus, the chemical composition of the most metal-poor stars known is one of the means at our disposal to shed light on the nature of the ‘First Stars’, sometimes referred to as Population III stars. A further exampl ...
Apollo 8 Technical Debriefing, Part 1
... covers. I had to use Program 23 by turning the shaft by trunnion to Sirius and then use Sirius for the first sextant calibration. There was a lot more light scatter in the scanning telescope than I had believed there would be prior to flight. At first this appeared to be the case at almost any attit ...
... covers. I had to use Program 23 by turning the shaft by trunnion to Sirius and then use Sirius for the first sextant calibration. There was a lot more light scatter in the scanning telescope than I had believed there would be prior to flight. At first this appeared to be the case at almost any attit ...
Transparencies - Rencontres de Moriond
... Broad-band (ugrizy; 350nm-1050nm) internal photometric accuracy of 0.010 mag (zero-point across the sky). Relative astrometric accuracy of 10 mas. ...
... Broad-band (ugrizy; 350nm-1050nm) internal photometric accuracy of 0.010 mag (zero-point across the sky). Relative astrometric accuracy of 10 mas. ...
Document
... Origin of the anomalous abundances The Ap phenomenon must be a surface phenomenon since the overabundance of rare earth elements (e.g. Eu is overabundant by a factor of up to 104 ) is so great that a signficant fraction of the supply of such elements in the Universe would be contained in Ap stars i ...
... Origin of the anomalous abundances The Ap phenomenon must be a surface phenomenon since the overabundance of rare earth elements (e.g. Eu is overabundant by a factor of up to 104 ) is so great that a signficant fraction of the supply of such elements in the Universe would be contained in Ap stars i ...
PHYS3380_110215_bw - The University of Texas at Dallas
... Convection and Size •In stars more than 1.3 times the mass of the Sun, the nuclear fusion of hydrogen into helium occurs via CNO cycle instead of the proton-proton chain. The CNO process is very temperature sensitive, so the core is very hot but the temperature falls off rapidly. Therefore, the cor ...
... Convection and Size •In stars more than 1.3 times the mass of the Sun, the nuclear fusion of hydrogen into helium occurs via CNO cycle instead of the proton-proton chain. The CNO process is very temperature sensitive, so the core is very hot but the temperature falls off rapidly. Therefore, the cor ...
THE DENSEST GALAXY
... Using the Keck/DEIMOS spectrum, the integrated velocity dispersion of M60-UCD1 was measured by crosscorrelating the region around the Ca triplet with a library of templates of the same resolution and wavelength coverage, as described by Strader et al. (2011). This value is σp = 68 ± 5 km s−1 . The r ...
... Using the Keck/DEIMOS spectrum, the integrated velocity dispersion of M60-UCD1 was measured by crosscorrelating the region around the Ca triplet with a library of templates of the same resolution and wavelength coverage, as described by Strader et al. (2011). This value is σp = 68 ± 5 km s−1 . The r ...
Article PDF - IOPscience
... The redshift measurements suggest a relative radial distance of Δz = 0.38 between the two QSOs. Only about a dozen other systems of projected QSO pairs with Δθ < 4.50 arcsec have been reported in the systematic search by Hennawi et al. (2006a, see Tables 8 and 9), Inada et al. (2012), and More et al ...
... The redshift measurements suggest a relative radial distance of Δz = 0.38 between the two QSOs. Only about a dozen other systems of projected QSO pairs with Δθ < 4.50 arcsec have been reported in the systematic search by Hennawi et al. (2006a, see Tables 8 and 9), Inada et al. (2012), and More et al ...
Stars and Stellar Evolution The Hertzsprung
... construct a plot of absolute magnitude versus colour - called a colourmagnitude diagram. The relative ease and convenience with which colour indices (such as B - V) may be determined for vast numbers of stars dictates the popularity of colour-magnitude plots. The resulting diagrams are very similar ...
... construct a plot of absolute magnitude versus colour - called a colourmagnitude diagram. The relative ease and convenience with which colour indices (such as B - V) may be determined for vast numbers of stars dictates the popularity of colour-magnitude plots. The resulting diagrams are very similar ...
Chapter 12 Star Stuff How do stars form?
... • Two quantum particles—electrons, nuclei, etc—cannot be in the same place at the same time • So they can only get so close • When a protostar has contracted to the point where it can’t contract anymore without particles being in the same place… • That’s one way of conceptualizing degeneracy pressur ...
... • Two quantum particles—electrons, nuclei, etc—cannot be in the same place at the same time • So they can only get so close • When a protostar has contracted to the point where it can’t contract anymore without particles being in the same place… • That’s one way of conceptualizing degeneracy pressur ...
Document
... • The uncertainties in the f value is what limits you in practice. These depend on laboratory measurements, and for many lines poor values are known. • A differential analysis is usually employed. That is the ratio of abundances between stars (best if they have the same effective temperature). In th ...
... • The uncertainties in the f value is what limits you in practice. These depend on laboratory measurements, and for many lines poor values are known. • A differential analysis is usually employed. That is the ratio of abundances between stars (best if they have the same effective temperature). In th ...
ISNS3371_041007_bw
... of thermal radiation. Second Law. If thermal radiation passes through a thin gas that is cooler than the thermal emitter, dark absorption lines are superimposed on the continuous spectrum. The gas absorbs certain wavelengths. This is called an absorption spectrum or dark line spectrum. Third Law. Vi ...
... of thermal radiation. Second Law. If thermal radiation passes through a thin gas that is cooler than the thermal emitter, dark absorption lines are superimposed on the continuous spectrum. The gas absorbs certain wavelengths. This is called an absorption spectrum or dark line spectrum. Third Law. Vi ...
Chapter 8 Pre-galactic enrichment of the IGM 8.1 Summary
... The simulation was initialized at z=99 and was allowed to evolve to z=15 using the Eulerian adaptive mesh refinement code Enzo (as described in Chapter 2). The simulation was stopped at z = 15 and all halos with dark matter mass MDM ≥ 5 × 105 M! were found using the HOP halo-finding algorithm [196] ...
... The simulation was initialized at z=99 and was allowed to evolve to z=15 using the Eulerian adaptive mesh refinement code Enzo (as described in Chapter 2). The simulation was stopped at z = 15 and all halos with dark matter mass MDM ≥ 5 × 105 M! were found using the HOP halo-finding algorithm [196] ...
The densest galaxy - SelectedWorks
... We report the discovery of a remarkable ultra-compact dwarf galaxy around the massive Virgo elliptical galaxy NGC 4649 (M60), which we call M60-UCD1. With a dynamical mass of 2.0 × 108 M0 but a half-light radius of only ∼24 pc, M60-UCD1 is more massive than any ultra-compact dwarfs of comparable siz ...
... We report the discovery of a remarkable ultra-compact dwarf galaxy around the massive Virgo elliptical galaxy NGC 4649 (M60), which we call M60-UCD1. With a dynamical mass of 2.0 × 108 M0 but a half-light radius of only ∼24 pc, M60-UCD1 is more massive than any ultra-compact dwarfs of comparable siz ...
Post-Main Sequence Evolution – Low and Intermediate Mass Stars
... AGB stars are known to lose mass at a prodigious rate during their final stages, around 10-5 - 10-4 solar masses per year. This obviously cannot persist for much over 100,000 years. The mass loss is driven in part by the pulsational instability of the thin helium shell. These pulses grow more violen ...
... AGB stars are known to lose mass at a prodigious rate during their final stages, around 10-5 - 10-4 solar masses per year. This obviously cannot persist for much over 100,000 years. The mass loss is driven in part by the pulsational instability of the thin helium shell. These pulses grow more violen ...
Survey of Astronomy A110 The Nature of Stars
... If only one set of spectral lines is seen, it is a single-line spectroscopic binary. If two sets of spectral lines are seen, it is a double-line spectroscopic binary. In this case the mass ratio of the two components can be determined. Only when we know the orbit inclination, can we determine the in ...
... If only one set of spectral lines is seen, it is a single-line spectroscopic binary. If two sets of spectral lines are seen, it is a double-line spectroscopic binary. In this case the mass ratio of the two components can be determined. Only when we know the orbit inclination, can we determine the in ...
Observing Stellar Evolution
... might provide some interesting insight into how stars are categorized and how they work. When they did this, they found that most stars fell along a line that went from blue and hot (at the upper left) to red and cool (at the lower right). This line is called the 'main sequence'. The 'main sequence' ...
... might provide some interesting insight into how stars are categorized and how they work. When they did this, they found that most stars fell along a line that went from blue and hot (at the upper left) to red and cool (at the lower right). This line is called the 'main sequence'. The 'main sequence' ...
Gamma-Ray Bursts: The Brightest Explosions in the Universe Arne
... (Introduction to the The ultra-luminous Universe: Gamma-Ray Bursts and Active Galactic Nuclei Session) ...
... (Introduction to the The ultra-luminous Universe: Gamma-Ray Bursts and Active Galactic Nuclei Session) ...
Notes 6 - University of Northern Iowa
... can be used to directly test computer models of not only the evolutionary paths of stars but also stellar pulsation models. But not all stars in this phase are pulsating stars like Cepheids or RR Lyre, so that also needs to be explained. The region of instability is relatively narrow, and star will ...
... can be used to directly test computer models of not only the evolutionary paths of stars but also stellar pulsation models. But not all stars in this phase are pulsating stars like Cepheids or RR Lyre, so that also needs to be explained. The region of instability is relatively narrow, and star will ...
100 Binocular Deep Sky Objects
... in a group, but usually 2 objects in a group. Seeing DSOs in groups makes observing that much more enjoyable. Many of these objects are challenging and may not be seen unless observing with large binoculars or in very dark skies. In some cases I discuss what can be seen in various sizes of binocular ...
... in a group, but usually 2 objects in a group. Seeing DSOs in groups makes observing that much more enjoyable. Many of these objects are challenging and may not be seen unless observing with large binoculars or in very dark skies. In some cases I discuss what can be seen in various sizes of binocular ...
PDF
... reproduce both the degree of fluctuations observed in the microwave background and correlations found in the local galaxy distribution. It predicts that dark-matter halos assemble hierarchically from smaller examples according to their mutual gravitational attraction. However, in describing how gala ...
... reproduce both the degree of fluctuations observed in the microwave background and correlations found in the local galaxy distribution. It predicts that dark-matter halos assemble hierarchically from smaller examples according to their mutual gravitational attraction. However, in describing how gala ...
ppt - NRAO
... E.g.: Taurus (of course), Orion is much larger than the Orion Nebula, It is not clear if all of Perseus is at the same distance (NGC1333 vs. IC 348), Ophiuchus streamers, etc.. (Note that these regions tend to be heavily obscured, so optical experiments are unlikely to improve significantly the situ ...
... E.g.: Taurus (of course), Orion is much larger than the Orion Nebula, It is not clear if all of Perseus is at the same distance (NGC1333 vs. IC 348), Ophiuchus streamers, etc.. (Note that these regions tend to be heavily obscured, so optical experiments are unlikely to improve significantly the situ ...
Constraining the formation of the Milky Way: Ages
... Overall, we do not anticipate the simplifications of our approach to affect significantly any of our results. On the other hand, what we gain with the above simplifications is a new tool to study the chemodynamics of our Galaxy, which is complementary to fully self-consistent models, and where the o ...
... Overall, we do not anticipate the simplifications of our approach to affect significantly any of our results. On the other hand, what we gain with the above simplifications is a new tool to study the chemodynamics of our Galaxy, which is complementary to fully self-consistent models, and where the o ...
Presentation - Relativity Group
... • temperature dictates the types of ions or molecules which exist • this, in turn, determines the number and relative strengths of absorption lines in the star’s spectrum • this fact was discovered by Cecilia Payne-Gaposchkin in 1925 ...
... • temperature dictates the types of ions or molecules which exist • this, in turn, determines the number and relative strengths of absorption lines in the star’s spectrum • this fact was discovered by Cecilia Payne-Gaposchkin in 1925 ...
NASA FUSE Satellite Solves the Case of the Missing Deuterium
... levels in such regions. Primordial deuterium concentrations are about 27 parts per million. FUSE finds concentrations as high as 23 parts per million in our galaxy. Scientists had assumed, based on theory that at least a third of the deuterium would have been destroyed over time, leaving less than t ...
... levels in such regions. Primordial deuterium concentrations are about 27 parts per million. FUSE finds concentrations as high as 23 parts per million in our galaxy. Scientists had assumed, based on theory that at least a third of the deuterium would have been destroyed over time, leaving less than t ...
International Ultraviolet Explorer
![](https://en.wikipedia.org/wiki/Special:FilePath/International_Ultraviolet_Explorer.gif?width=300)
The International Ultraviolet Explorer (IUE) was an astronomical observatory satellite primarily designed to take ultraviolet spectra. The satellite was a collaborative project between NASA, the UK Science Research Council and the European Space Agency (ESA). The mission was first proposed in early 1964, by a group of scientists in the United Kingdom, and was launched on January 26, 1978 aboard a NASA Delta rocket. The mission lifetime was initially set for 3 years, but in the end it lasted almost 18 years, with the satellite being shut down in 1996. The switch-off occurred for financial reasons, while the telescope was still functioning at near original efficiency.It was the first space observatory to be operated in real time by astronomers who visited the groundstations in the United States and Europe. Astronomers made over 104,000 observations using the IUE, of objects ranging from solar system bodies to distant quasars. Among the significant scientific results from IUE data were the first large scale studies of stellar winds, accurate measurements of the way interstellar dust absorbs light, and measurements of the supernova SN1987A which showed that it defied stellar evolution theories as they then stood. When the mission ended, it was considered the most successful astronomical satellite ever.