lecture course
... centres and absolute B magnitudes between about -25 and -15, and dwarf ellipticals, which have low brightnesses at their centres and absolute B magnitudes fainter than about -18. The faintest galaxies known are dwarf ellipticals. Elliptical galaxies are featureless, with brightness profiles that are ...
... centres and absolute B magnitudes between about -25 and -15, and dwarf ellipticals, which have low brightnesses at their centres and absolute B magnitudes fainter than about -18. The faintest galaxies known are dwarf ellipticals. Elliptical galaxies are featureless, with brightness profiles that are ...
- Isaac Newton Group of Telescopes
... radiating much more energy than in later stages of their evolution. More massive brown dwarfs in the Pleiades should be detectable in sufficiently deep surveys. After only 0.3% of the clusters area had been explored using IAC80 telescope at Teide Observatory, a faint object was detected, whose extr ...
... radiating much more energy than in later stages of their evolution. More massive brown dwarfs in the Pleiades should be detectable in sufficiently deep surveys. After only 0.3% of the clusters area had been explored using IAC80 telescope at Teide Observatory, a faint object was detected, whose extr ...
New Generation Ground-Based Optical/Infrared Telescopes
... are discussed elsewhere in this encyclopedia. Astronomers strive to build ever-larger telescopes in order to collect as much light as possible. While cosmologists need the large collecting area of telescopes to study the distant universe, solar system astronomers need the large collecting area to st ...
... are discussed elsewhere in this encyclopedia. Astronomers strive to build ever-larger telescopes in order to collect as much light as possible. While cosmologists need the large collecting area of telescopes to study the distant universe, solar system astronomers need the large collecting area to st ...
Galaxies - WordPress.com
... D does not suffice to keep the cluster together for more than one or two billion years ...
... D does not suffice to keep the cluster together for more than one or two billion years ...
Digital Universe Guide - American Museum of Natural History
... night sky as seen from Earth. With the left mouse button pressed, you can pan around the sky to your heart’s content. How do you move away from the Sun, though, and begin flying around the stars? Turn on the stars and turn off the open clusters and globular clusters (click on their group buttons). B ...
... night sky as seen from Earth. With the left mouse button pressed, you can pan around the sky to your heart’s content. How do you move away from the Sun, though, and begin flying around the stars? Turn on the stars and turn off the open clusters and globular clusters (click on their group buttons). B ...
X-Ray Spectroscopy of Stars
... X-rays have also been detected from brown dwarfs; again, the emission mechanism is supposedly coronal. Similarly, in low-mass pre-main sequence stars, i.e., T Tauri stars or (low-mass) protostars, intense steady and flaring X-ray radiation is also thought to originate predominantly in hot coronal pl ...
... X-rays have also been detected from brown dwarfs; again, the emission mechanism is supposedly coronal. Similarly, in low-mass pre-main sequence stars, i.e., T Tauri stars or (low-mass) protostars, intense steady and flaring X-ray radiation is also thought to originate predominantly in hot coronal pl ...
Here - NASA/IPAC Extragalactic Database
... H ii regions are ionized clouds of gas associated with zones of recent star formation. They are powered by one, a few, or a cluster of massive stars (depending on the resolution at which one is working). The effective temperatures T? of the ionizing stars lie in the range 35 000 – 50 000 K. The nebu ...
... H ii regions are ionized clouds of gas associated with zones of recent star formation. They are powered by one, a few, or a cluster of massive stars (depending on the resolution at which one is working). The effective temperatures T? of the ionizing stars lie in the range 35 000 – 50 000 K. The nebu ...
User`s Manual for DAOPHOT II This manual is intended as a guide
... reasonable degree of success, but it may be to your advantage to check the quality of the profile fits visually on an image display before accepting the final product. (3) The shape of the point-spread function is assumed to be spatially constant or to vary smoothly with position within the frame; i ...
... reasonable degree of success, but it may be to your advantage to check the quality of the profile fits visually on an image display before accepting the final product. (3) The shape of the point-spread function is assumed to be spatially constant or to vary smoothly with position within the frame; i ...
PH607lec08
... In barred S0 galaxies the bar is often the only structure visible in the disk. In types SBa and later the bar often connects to a spiral pattern extending to larger radii (e.g. NGC 1300). Viewed face-on, bars typically appear to have axial ratios of 2. The surface brightness within the bar is often ...
... In barred S0 galaxies the bar is often the only structure visible in the disk. In types SBa and later the bar often connects to a spiral pattern extending to larger radii (e.g. NGC 1300). Viewed face-on, bars typically appear to have axial ratios of 2. The surface brightness within the bar is often ...
An X-Ray, Optical and Infra-red study of High-Mass X
... First and foremost I would like to thank my supervisor, Malcolm Coe, for his continued guidance and support. His drive to obtain and exploit all manner of data has given me a wealth of information on which to base my thesis and sent me to some of the world’s most incredible places in the process. I ...
... First and foremost I would like to thank my supervisor, Malcolm Coe, for his continued guidance and support. His drive to obtain and exploit all manner of data has given me a wealth of information on which to base my thesis and sent me to some of the world’s most incredible places in the process. I ...
Stellar Intensity Interferometry: The Background John Davis Sydney Institute for Astronomy
... Calibrated with a standard source of wide band noise fed simultaneously into both channels in place of the photomultiplier outputs before and after each night of observations • The scale of the correlation depends on instrumental parameters and the scale changes if, for example, the detectors are c ...
... Calibrated with a standard source of wide band noise fed simultaneously into both channels in place of the photomultiplier outputs before and after each night of observations • The scale of the correlation depends on instrumental parameters and the scale changes if, for example, the detectors are c ...
Strongly suggested reading: The Milky Way`s stellar disk
... coupled with the stars’ photospheric element abundances and constraints on their ages. We know that in principle this enormous wealth of information about the stellar body of our Galaxy holds a key to recognizing and understanding some of the mechanisms that create and evolve disk galaxies. And it h ...
... coupled with the stars’ photospheric element abundances and constraints on their ages. We know that in principle this enormous wealth of information about the stellar body of our Galaxy holds a key to recognizing and understanding some of the mechanisms that create and evolve disk galaxies. And it h ...
Astronomy 113 Laboratory Manual - UW
... Polaris, the North Star, has long shown the way to travelers. At sea the only "landmarks" are celestial. It was Polaris that guided sailors around the globe, and not only by showing the way North. Using a sextant a European captain sailing to the New World could also accurately find the ship's latit ...
... Polaris, the North Star, has long shown the way to travelers. At sea the only "landmarks" are celestial. It was Polaris that guided sailors around the globe, and not only by showing the way North. Using a sextant a European captain sailing to the New World could also accurately find the ship's latit ...
New brown dwarfs and giant planets
... Stellar kinematics are usually modelled as Gaussian distributions (s(U), s(V), s(W) ) But disk kinematics are more complex: ...
... Stellar kinematics are usually modelled as Gaussian distributions (s(U), s(V), s(W) ) But disk kinematics are more complex: ...
MPA Anniversary Brochure - Max Planck Institute for Astrophysics
... tradition of independent individual theoretical research may be endangered. I do not believe this danger to be real. While the way in which we pursue our science has changed, the most important drivers of research are the same at MPA today as when it was founded. They are a fascination with the extr ...
... tradition of independent individual theoretical research may be endangered. I do not believe this danger to be real. While the way in which we pursue our science has changed, the most important drivers of research are the same at MPA today as when it was founded. They are a fascination with the extr ...
A Budget and Accounting of Metals at z~ 0: Results from the COS
... mic metals are in the CGM and IGM, it has been difficult to do a full accounting in the low redshift Universe. Restframe UV spectra—and thus space-based observations— are needed in order to probe the dominant ionic transitions and infer column densities, mass budgets, and kinematics. The COS-Halos s ...
... mic metals are in the CGM and IGM, it has been difficult to do a full accounting in the low redshift Universe. Restframe UV spectra—and thus space-based observations— are needed in order to probe the dominant ionic transitions and infer column densities, mass budgets, and kinematics. The COS-Halos s ...
The size of AB Doradus A from VLTI/AMBER interferometry⋆
... Our radius measurement of AB Dor A is in reasonable agreement with previous estimates based on other techniques, i.e. techniques based on the projected equatorial velocity (∼1 R ; Maggio et al. 2000), and techniques based on the empirical Barnes et al. (1978) relationship between radius and V − R c ...
... Our radius measurement of AB Dor A is in reasonable agreement with previous estimates based on other techniques, i.e. techniques based on the projected equatorial velocity (∼1 R ; Maggio et al. 2000), and techniques based on the empirical Barnes et al. (1978) relationship between radius and V − R c ...
The composition and nature of the dust shell surrounding the binary
... of the detached shell was also measured in the CO (J= 1 − 0) rotational line and was found to be about 40 km s−1 (Josselin et al. 1998). This is high for a low mass AGB star and suggests a massive progenitor. The difference with the [N II] line is remarkable and is probably related to the extended n ...
... of the detached shell was also measured in the CO (J= 1 − 0) rotational line and was found to be about 40 km s−1 (Josselin et al. 1998). This is high for a low mass AGB star and suggests a massive progenitor. The difference with the [N II] line is remarkable and is probably related to the extended n ...
Physical Properties of the Gas and Dust in the Orion B Molecular
... as indicated by the same distances and the presence of a low-level CO emission bridge without a discontinuity in velocity. However, in contrast to the Orion A cloud, the Orion B cloud has no overall velocity gradient. Maddalena et al. (1986) derive a total mass of 8 × 104 M⊙ for the Orion B GMC. The ...
... as indicated by the same distances and the presence of a low-level CO emission bridge without a discontinuity in velocity. However, in contrast to the Orion A cloud, the Orion B cloud has no overall velocity gradient. Maddalena et al. (1986) derive a total mass of 8 × 104 M⊙ for the Orion B GMC. The ...
PDF - STRW Local - Universiteit Leiden
... Leiden Observatory is part of the Faculty of Science and hosts both the Bachelor and Master studies in astronomy of Leiden University. The three-year bachelor in astronomy is currently followed by about 100 students, and provides a broad basis in astronomy, with important components in physics, math ...
... Leiden Observatory is part of the Faculty of Science and hosts both the Bachelor and Master studies in astronomy of Leiden University. The three-year bachelor in astronomy is currently followed by about 100 students, and provides a broad basis in astronomy, with important components in physics, math ...