![Open clusters and associations in the Gaia era](http://s1.studyres.com/store/data/016146695_1-b3be50e2423441f534fcc2c3b1e756f8-300x300.png)
Open clusters and associations in the Gaia era
... an issue if the survey does not extend beyond the cluster tidal radius, especially if there is mass segregation as the incompleteness level will then depend on mass. Moreover, objects might be missed around bright stars due to contrast issue, in crowded regions or in area with high extinction. As fo ...
... an issue if the survey does not extend beyond the cluster tidal radius, especially if there is mass segregation as the incompleteness level will then depend on mass. Moreover, objects might be missed around bright stars due to contrast issue, in crowded regions or in area with high extinction. As fo ...
Astrometry of Asteroids
... astronomers for a particular The Equatorial Coordinates purpose. One of the most important catalogs is called the FK5 Catalog, because it is one of the fundamental catalogs used as a reference for measuring the positions to other stars in the sky (see the next section of this manual). The FK5 Catalo ...
... astronomers for a particular The Equatorial Coordinates purpose. One of the most important catalogs is called the FK5 Catalog, because it is one of the fundamental catalogs used as a reference for measuring the positions to other stars in the sky (see the next section of this manual). The FK5 Catalo ...
Astronomy Astrophysics NGC 7419 as a template for red supergiant clusters &
... Context. The open cluster NGC 7419 is known to contain five red supergiants and a very high number of Be stars. However, there are conflicting reports about its age and distance that prevent a useful comparison with other clusters. Aims. We intend to obtain more accurate parameters for NGC 7419, usi ...
... Context. The open cluster NGC 7419 is known to contain five red supergiants and a very high number of Be stars. However, there are conflicting reports about its age and distance that prevent a useful comparison with other clusters. Aims. We intend to obtain more accurate parameters for NGC 7419, usi ...
Can we account for the dust
... Mid- and far-IR emission of galaxies ◦ Thermal emission from dust grains ...
... Mid- and far-IR emission of galaxies ◦ Thermal emission from dust grains ...
Evidence for 1000 km/s Molecular Outflows in the Local ULIRG
... same outflow, then Eq. (1) suggests that the spatial extent of Na D and Hα should be larger (∼ 0.4 kpc) while the spatial scale for the OH winds measured by Herschel would be more compact (. 0.1 kpc) than the CO wind. The fact that wind velocities measured in molecular outflows are larger than in th ...
... same outflow, then Eq. (1) suggests that the spatial extent of Na D and Hα should be larger (∼ 0.4 kpc) while the spatial scale for the OH winds measured by Herschel would be more compact (. 0.1 kpc) than the CO wind. The fact that wind velocities measured in molecular outflows are larger than in th ...
original version
... that are temporarily increased, often by very large amounts. We know from observations that this can and does happen, in the most extreme form as Ultra-Luminous InfraRed Galaxies (ULIRGs), and numerical simulations can also produce much enhanced SFRs (e.g., [1,2]). A question that is vital is whethe ...
... that are temporarily increased, often by very large amounts. We know from observations that this can and does happen, in the most extreme form as Ultra-Luminous InfraRed Galaxies (ULIRGs), and numerical simulations can also produce much enhanced SFRs (e.g., [1,2]). A question that is vital is whethe ...
here
... – where Sν is the flux density, κν is the mass absorption coefficient [e.g. Hildebrand 1983] – Fits typically invoke a spectral index for the opacity, and one or two temperature components, – can have significant optical depths at λ < 60µm and may have to ...
... – where Sν is the flux density, κν is the mass absorption coefficient [e.g. Hildebrand 1983] – Fits typically invoke a spectral index for the opacity, and one or two temperature components, – can have significant optical depths at λ < 60µm and may have to ...
In Class Activity Manual - Department of Physics and Astronomy
... minutes to highlight the main point and uncover any large problems the groups encountered. This is your best chance to give immediate feedback. ❏ I aim for about one group activity per class, occasionally two. If you can arrange it, go for class periods longer than 50 minutes. I schedule my class f ...
... minutes to highlight the main point and uncover any large problems the groups encountered. This is your best chance to give immediate feedback. ❏ I aim for about one group activity per class, occasionally two. If you can arrange it, go for class periods longer than 50 minutes. I schedule my class f ...
A Spectroscopic Survey of a Sample of Active M Dwarfs.
... interested in seeing whether other indications of youth are present. It has long been known that single M dwarfs decline in activity with age. The discovery of the TW Hydrae Association (Kastner et al. 1997; Webb et al. 1999) shows that very young stars can be found in the immediate solar neighbourh ...
... interested in seeing whether other indications of youth are present. It has long been known that single M dwarfs decline in activity with age. The discovery of the TW Hydrae Association (Kastner et al. 1997; Webb et al. 1999) shows that very young stars can be found in the immediate solar neighbourh ...
Empirical properties of Very Massive Stars
... observed while according to Figer (2005), there should be 18 of them. Therefore, very massive stars are important not only for stellar physics, but also for star formation and the interplay between stars and the interstellar medium, both locally and on galactic scales. The reminder of this chapter f ...
... observed while according to Figer (2005), there should be 18 of them. Therefore, very massive stars are important not only for stellar physics, but also for star formation and the interplay between stars and the interstellar medium, both locally and on galactic scales. The reminder of this chapter f ...
variable star type designations in vsx
... A pipe character ( | ) between two different types signifies a logical OR; the classification is uncertain and all possible types are indicated. An example of this is ELL|DSCT, where the star may be an ellipsoidal binary system or a DSCT-type pulsating variable with half the given period. A plus cha ...
... A pipe character ( | ) between two different types signifies a logical OR; the classification is uncertain and all possible types are indicated. An example of this is ELL|DSCT, where the star may be an ellipsoidal binary system or a DSCT-type pulsating variable with half the given period. A plus cha ...
The Life Cycle of Stars: Supernovae in Starbursts by Jason Kezwer
... peak magnitude we use Hubble Space Telescope archival data to subtract off the nuclear background and find an absolute magnitude of MK = −22.19 ± 0.16 (nonabsorbed). This exceeds the luminosity of a typical core collapse supernova by roughly 3.5 magnitudes; rather, the observed variations in nuclear ...
... peak magnitude we use Hubble Space Telescope archival data to subtract off the nuclear background and find an absolute magnitude of MK = −22.19 ± 0.16 (nonabsorbed). This exceeds the luminosity of a typical core collapse supernova by roughly 3.5 magnitudes; rather, the observed variations in nuclear ...
Kidd_Thesis_2015April15_Final.
... oscillation is when the entire star’s surface is either completely moving outwards or completely moving inwards at the same time [5]. The first-overtone Cepheids have much more symmetric light curves, and they tend to have smaller amplitudes in their light curves than the fundamental-mode Cepheids [ ...
... oscillation is when the entire star’s surface is either completely moving outwards or completely moving inwards at the same time [5]. The first-overtone Cepheids have much more symmetric light curves, and they tend to have smaller amplitudes in their light curves than the fundamental-mode Cepheids [ ...
HST observations of the field star population in the Large Magellanic
... suggests an age for the younger population of slightly less than 1 Gyr, or of ~ 2 Gyr, depending on the adopted metallicity. The redder peak corresponds to a population with age ~2-4 Gyr, again depending on metallicity. Given the proximity of our field to the bar, we tentatively identify the younger ...
... suggests an age for the younger population of slightly less than 1 Gyr, or of ~ 2 Gyr, depending on the adopted metallicity. The redder peak corresponds to a population with age ~2-4 Gyr, again depending on metallicity. Given the proximity of our field to the bar, we tentatively identify the younger ...
Kidd_Thesis_2015April14_Final.
... oscillation is when the entire star’s surface is either completely moving outwards or completely moving inwards at the same time [5]. The first-overtone Cepheids have much more symmetric light curves, and they tend to have smaller amplitudes in their light curves than the fundamental-mode Cepheids [ ...
... oscillation is when the entire star’s surface is either completely moving outwards or completely moving inwards at the same time [5]. The first-overtone Cepheids have much more symmetric light curves, and they tend to have smaller amplitudes in their light curves than the fundamental-mode Cepheids [ ...
What keeps stars shining? What holds them up? Lecture 14. The
... converted to energy by famous equation E = Mc2. More later) Stability: Why doesn't all the Hydrogen in the Universe spontaneously fuse in a humongous Hydrogen Bomb? The hydrogen nuclei (pure protons) in the first step have positive charge, so they push each other away. Must slam them together very h ...
... converted to energy by famous equation E = Mc2. More later) Stability: Why doesn't all the Hydrogen in the Universe spontaneously fuse in a humongous Hydrogen Bomb? The hydrogen nuclei (pure protons) in the first step have positive charge, so they push each other away. Must slam them together very h ...
Dark Matter
... is organized into planets (including the Earth) orbiting around a star: the Sun. We also know that stars collect themselves into galaxies, on a scale much larger than the solar system (about 100 million times larger!). Our Sun is an average star in an average galaxy called the Milky Way. The Milky W ...
... is organized into planets (including the Earth) orbiting around a star: the Sun. We also know that stars collect themselves into galaxies, on a scale much larger than the solar system (about 100 million times larger!). Our Sun is an average star in an average galaxy called the Milky Way. The Milky W ...
Lecture 16 - UWO Computer Science
... Algorithms for hierarchical clustering can be divided into two types: ...
... Algorithms for hierarchical clustering can be divided into two types: ...
A Zoo of Galaxies - Portsmouth Research Portal
... A galaxy is a massive collection of stars, gas and interstellar dust. To first order, the optical colour of a galaxy tells about the types of stars which live in the galaxy (ignoring the complications of dust which can redden some types of galaxies quite significantly e.g. Masters et al. 2003, 2010a ...
... A galaxy is a massive collection of stars, gas and interstellar dust. To first order, the optical colour of a galaxy tells about the types of stars which live in the galaxy (ignoring the complications of dust which can redden some types of galaxies quite significantly e.g. Masters et al. 2003, 2010a ...
A Project Underway to Build an Inexpensive 8-Meter Telescope
... Microlensing follow-up groups (PLANET, FUN, MOA) want to pick the ~100 best of these lightcurves in terms of early planet-like deviations in microlensing fit. ...
... Microlensing follow-up groups (PLANET, FUN, MOA) want to pick the ~100 best of these lightcurves in terms of early planet-like deviations in microlensing fit. ...
Probing the Dark Matter Content of Local Group Dwarf Spheroidal
... values typical of globular star clusters, this provided the first hint that the dSphs were a class of stellar system distinct from the globular clusters, despite the fact that in many cases their stellar mass ...
... values typical of globular star clusters, this provided the first hint that the dSphs were a class of stellar system distinct from the globular clusters, despite the fact that in many cases their stellar mass ...
Fluorine abundances in dwarf stars of the solar neighbourhood⋆
... nine cool main-sequence dwarfs of the solar neighbourhood. The resolving power of the spectra was R ∼ 50 000 and the exposure times were chosen to achieve a signal-to-noise ratio (S/N) larger than 200. The reduction and calibration of the spectra were carried out with the standard CRIRES pipeline pr ...
... nine cool main-sequence dwarfs of the solar neighbourhood. The resolving power of the spectra was R ∼ 50 000 and the exposure times were chosen to achieve a signal-to-noise ratio (S/N) larger than 200. The reduction and calibration of the spectra were carried out with the standard CRIRES pipeline pr ...
On the origin of lopsidedness in galaxies as determined
... Although such features are generically referred to as “lopsidedness,” m = 1 distortions are only truly a measurement of lopsidedness if the phase of the component is constant, or nearly so, with radius. This distinction has been noted in some discussions of the m = 1 decompositions (Li et al. 2011), ...
... Although such features are generically referred to as “lopsidedness,” m = 1 distortions are only truly a measurement of lopsidedness if the phase of the component is constant, or nearly so, with radius. This distinction has been noted in some discussions of the m = 1 decompositions (Li et al. 2011), ...
Chapter 12
... t is hard to believe that the stars we see in the night sky as tiny glints of light are in reality huge, dazzling balls of gas and that many are vastly larger and brighter than our Sun. They look dim to us only because they are so far away—several light-years (trillions of miles) to even the nearest ...
... t is hard to believe that the stars we see in the night sky as tiny glints of light are in reality huge, dazzling balls of gas and that many are vastly larger and brighter than our Sun. They look dim to us only because they are so far away—several light-years (trillions of miles) to even the nearest ...
Planetary Nebulae: Observational Properties, Mimics, and Diagnostics
... Subtraction or quotient imaging has been applied to digitized photographic survey plates and films; for example, Cappellaro et al. (1994) found three new PN and a Herbig-Haro object by comparing digitized POSS red and infrared (IR) plates. This procedure works because the I-band filter passes relati ...
... Subtraction or quotient imaging has been applied to digitized photographic survey plates and films; for example, Cappellaro et al. (1994) found three new PN and a Herbig-Haro object by comparing digitized POSS red and infrared (IR) plates. This procedure works because the I-band filter passes relati ...
Cosmic distance ladder
The cosmic distance ladder (also known as the extragalactic distance scale) is the succession of methods by which astronomers determine the distances to celestial objects. A real direct distance measurement of an astronomical object is possible only for those objects that are ""close enough"" (within about a thousand parsecs) to Earth. The techniques for determining distances to more distant objects are all based on various measured correlations between methods that work at close distances and methods that work at larger distances. Several methods rely on a standard candle, which is an astronomical object that has a known luminosity.The ladder analogy arises because no one technique can measure distances at all ranges encountered in astronomy. Instead, one method can be used to measure nearby distances, a second can be used to measure nearby to intermediate distances, and so on. Each rung of the ladder provides information that can be used to determine the distances at the next higher rung.