Stellar Continua
... I. The Paschen Continuum • The Paschen continuum slope (B-V) is a good temperature indicator • Varies smoothly with changing temperature • Slope is negative (blue is brighter) for hot stars and positive (visual is brighter) for cooler stars • B-V works as a temperature indicator from 3500K to 9000K ...
... I. The Paschen Continuum • The Paschen continuum slope (B-V) is a good temperature indicator • Varies smoothly with changing temperature • Slope is negative (blue is brighter) for hot stars and positive (visual is brighter) for cooler stars • B-V works as a temperature indicator from 3500K to 9000K ...
document
... • Years ago in ancient Egypt, archaeologists unearthed the tomb of the Apis-bulls and couldn’t believe what they had found. Leading to the tomb was a paved avenue lined by lions that were carved out of stone. To enter the tomb they had to walk through a long and high arched narrow passageway cut int ...
... • Years ago in ancient Egypt, archaeologists unearthed the tomb of the Apis-bulls and couldn’t believe what they had found. Leading to the tomb was a paved avenue lined by lions that were carved out of stone. To enter the tomb they had to walk through a long and high arched narrow passageway cut int ...
Draft paper (Published in ApJL)
... Although gas removal through interaction with the cosmic web is a robust feature of the simulation, the fate of the gas that remains in the galaxy or is accreted later is less clear, since it is subject to the complex (and poorlymodeled) process of star formation and associated feedback. Indeed, the ...
... Although gas removal through interaction with the cosmic web is a robust feature of the simulation, the fate of the gas that remains in the galaxy or is accreted later is less clear, since it is subject to the complex (and poorlymodeled) process of star formation and associated feedback. Indeed, the ...
The Photometric Properties of the HST Astrometer Fine Guidance
... nature of the wave front received by the FGSs for they are located in radial bays at the perimeter of the focal plane. Hence, the photometric behavior of the FGSs is not expected to change in the foreseeable future. One major change from the original scientific calibration plan for the FGSs is that ...
... nature of the wave front received by the FGSs for they are located in radial bays at the perimeter of the focal plane. Hence, the photometric behavior of the FGSs is not expected to change in the foreseeable future. One major change from the original scientific calibration plan for the FGSs is that ...
Sample
... consumes material, it becomes more massive so that the event horizon, the boundary where the escape velocity equals the speed of light, grows and the black hole occupies more space (Kormendy, 2000). Apparently, because of the crowded environment of the galactic center, an immense number of gas cloud ...
... consumes material, it becomes more massive so that the event horizon, the boundary where the escape velocity equals the speed of light, grows and the black hole occupies more space (Kormendy, 2000). Apparently, because of the crowded environment of the galactic center, an immense number of gas cloud ...
Document
... the past 8Gyr. This is consistent with starforming galaxies being transformed into4L* galaxies since z=1. “ While red galaxy mergers have been
observed, such mergers do not produce rapid growth of 4L* red gala ...
... the past 8Gyr. This is consistent with starforming galaxies being transformed into
Calculating Radial Velocities of Low Mass Eclipsing Binaries
... the same metallicity by assuming they were formed from the same material, so we get the metallicity for the M star from studying the primary star. Eclipsing binaries are classical two-body systems where two stars orbit each other around a ...
... the same metallicity by assuming they were formed from the same material, so we get the metallicity for the M star from studying the primary star. Eclipsing binaries are classical two-body systems where two stars orbit each other around a ...
Autumn Night sky Guide
... responds well to high power in a telescope. M15 has the distinction of containing the first planetary nebula to be discovered in a globular cluster, Pease 1. Don’t expect to be able to see it though. M31 – the Andromeda Galaxy M31 is a spiral galaxy very similar but rather larger than our Milky Way. ...
... responds well to high power in a telescope. M15 has the distinction of containing the first planetary nebula to be discovered in a globular cluster, Pease 1. Don’t expect to be able to see it though. M31 – the Andromeda Galaxy M31 is a spiral galaxy very similar but rather larger than our Milky Way. ...
to view poster PDF - Max-Planck
... . Observational studies have found evidence of a Galactic bar that has a radius of 4.4 kpc and is oriented about 44o relative to the Sun-Galactic center line of sight(Benjamin et al. 2005). The Galactic bar is the place where the circular orbit transits to elliptical orbit. Due to its potentials, cl ...
... . Observational studies have found evidence of a Galactic bar that has a radius of 4.4 kpc and is oriented about 44o relative to the Sun-Galactic center line of sight(Benjamin et al. 2005). The Galactic bar is the place where the circular orbit transits to elliptical orbit. Due to its potentials, cl ...
Extragalactic Globular Cluster Systems
... The globular clusters that were once within the merging protogalaxies are so dense that they survive intact and will orbit freely within the Galaxy. The surviving protogalaxies may be the precursors of the old satellite galaxies, some of which host old globular clusters such as Fornax, whose morphol ...
... The globular clusters that were once within the merging protogalaxies are so dense that they survive intact and will orbit freely within the Galaxy. The surviving protogalaxies may be the precursors of the old satellite galaxies, some of which host old globular clusters such as Fornax, whose morphol ...
An interesting nebular object in LDN 288
... a. HH 100 (see Fig.5a). It is situated near the well-known cone-like cometary nebula NGC 6729. There are two jets: one is a straight jet while the second one is spiral. b. SNO 35 [3] (see Fig.5b). This object (a in Fig.5b) has a spiral jet, at the end of which there is a condensation (b in Fig.5b). ...
... a. HH 100 (see Fig.5a). It is situated near the well-known cone-like cometary nebula NGC 6729. There are two jets: one is a straight jet while the second one is spiral. b. SNO 35 [3] (see Fig.5b). This object (a in Fig.5b) has a spiral jet, at the end of which there is a condensation (b in Fig.5b). ...
Clusters at low redshift
... – projected distance to 5th nearest neighbour – 3D density based on convolution with Gaussian kernel – cluster velocity dispersion ...
... – projected distance to 5th nearest neighbour – 3D density based on convolution with Gaussian kernel – cluster velocity dispersion ...
The Science case for the UV and optical cameras
... OF GLOBULAR CLUSTERS Globular cluster age measurement error is dominated by uncertainty on distance, which is, in general, ~10% => 0.2 mag distance modulus, which translates in a >25% error in age!!! ...
... OF GLOBULAR CLUSTERS Globular cluster age measurement error is dominated by uncertainty on distance, which is, in general, ~10% => 0.2 mag distance modulus, which translates in a >25% error in age!!! ...
MSci Astrophysics 210PHY412 - Queen's University Belfast
... Whatever the star-formation rate, the IMF seems constant Starburst regions, “normal” young clusters, low mass clusters in Milky Way, LMC, SMC all similar IMF not measured well beyond the Magellanic Clouds ...
... Whatever the star-formation rate, the IMF seems constant Starburst regions, “normal” young clusters, low mass clusters in Milky Way, LMC, SMC all similar IMF not measured well beyond the Magellanic Clouds ...
13.5 The HR Diagram By the early 1900s, astronomers had learned
... relation. Massive stars lie near the top of the main sequence; they are hotter and more luminous than low mass stars. Thus, from top to bottom along the main sequence, the star masses decrease but nevertheless lie in a relatively narrow range, from about 30 to 0.1 M⊙.We will see in the next chapter ...
... relation. Massive stars lie near the top of the main sequence; they are hotter and more luminous than low mass stars. Thus, from top to bottom along the main sequence, the star masses decrease but nevertheless lie in a relatively narrow range, from about 30 to 0.1 M⊙.We will see in the next chapter ...
Transparencies
... What is the 2MASS Redshift Survey? What is the acceleration on our Local Group of galaxies? Why do I think I am right? ...
... What is the 2MASS Redshift Survey? What is the acceleration on our Local Group of galaxies? Why do I think I am right? ...
Lab 15 How Many Galaxies Are There in the
... spend 10 entire days training this telescope on one small region of the sky to observe the faintest galaxies and learn about them. The image that was obtained is shown in Figure 15.2. First, let’s figure out how long it would take for the Space Telescope to take pictures like this over the entire sk ...
... spend 10 entire days training this telescope on one small region of the sky to observe the faintest galaxies and learn about them. The image that was obtained is shown in Figure 15.2. First, let’s figure out how long it would take for the Space Telescope to take pictures like this over the entire sk ...
Astronomy C - Scioly.org
... 58. Why are exoplanets (of any type) unlikely to be found in old stellar populations? 59. What is the term for a gas giant that has had its atmosphere stripped away? 60. How are ocean planets thought to form? 61. What is one possibility for why a planet may be orbiting in the opposite direction to t ...
... 58. Why are exoplanets (of any type) unlikely to be found in old stellar populations? 59. What is the term for a gas giant that has had its atmosphere stripped away? 60. How are ocean planets thought to form? 61. What is one possibility for why a planet may be orbiting in the opposite direction to t ...
RED DWARFS AND THE END OF THE MAIN SEQUENCE
... in only a Hubble time or two. Fortunately, this time scale can be extended by several conservation practices, including recycling of gas due to mass loss from evolved stars, infall onto the galactic disk, and the reduction of the star formation rate as the gas supply dwindles. With these effects inc ...
... in only a Hubble time or two. Fortunately, this time scale can be extended by several conservation practices, including recycling of gas due to mass loss from evolved stars, infall onto the galactic disk, and the reduction of the star formation rate as the gas supply dwindles. With these effects inc ...
in search of antimatter in the universe
... instead consider a much larger object, such as the gas shell of a supernova, then we obtain Figure 12. In this case, the emission line is just visible up to 600 parsecs, after which the brightness drops below 0.1 photons s-1m-2, and the emission line will be hard to distinguish from background noise ...
... instead consider a much larger object, such as the gas shell of a supernova, then we obtain Figure 12. In this case, the emission line is just visible up to 600 parsecs, after which the brightness drops below 0.1 photons s-1m-2, and the emission line will be hard to distinguish from background noise ...
Starbirth - Lincoln-Sudbury Regional High School
... and rotational effects playing a secondary role. Shockwaves are often involved, and are necessary if high mass star formation is to occur. We then looked at some observations of starbirth regions in our Galaxy, identifying characteristic features such as proplyds and jets. In the next Activity, we s ...
... and rotational effects playing a secondary role. Shockwaves are often involved, and are necessary if high mass star formation is to occur. We then looked at some observations of starbirth regions in our Galaxy, identifying characteristic features such as proplyds and jets. In the next Activity, we s ...
Black-Body SNR Formulation of Astronomical Camera
... where m is the brightness magnitude assigned to a star observed from Earth, f (·) is the mean spectral flux density at top of Earth’s atmosphere averaged over a defined band and Q(·) is the normalizing constant for that band [8]. We will not go into more details about astronomical magnitude systems ...
... where m is the brightness magnitude assigned to a star observed from Earth, f (·) is the mean spectral flux density at top of Earth’s atmosphere averaged over a defined band and Q(·) is the normalizing constant for that band [8]. We will not go into more details about astronomical magnitude systems ...
Active Galaxies
... •Galaxies that emit most of their light in IR - LIR > 1012 Lsun •Few in local universe; most beyond z > 1 •Nearly all are undergoing mergers - forming E’s •IR light is likely a combination of dust reprocessed AGN emission and starbursts. •Some AGN may manifest as ULIRGs during different stages of ...
... •Galaxies that emit most of their light in IR - LIR > 1012 Lsun •Few in local universe; most beyond z > 1 •Nearly all are undergoing mergers - forming E’s •IR light is likely a combination of dust reprocessed AGN emission and starbursts. •Some AGN may manifest as ULIRGs during different stages of ...
The Big Bang
... If the dust weren’t there, this would probably be classified as an elliptical galaxy. Instead it’s usually called “peculiar”. ...
... If the dust weren’t there, this would probably be classified as an elliptical galaxy. Instead it’s usually called “peculiar”. ...
D ASTROPHYSICS
... Sun and the Earth. It is really only useful when dealing with the distances of planets from the Sun. 1 AU = 1.50 × 10 11 m ≈ 8 light minutes The parsec (pc): This is the most commonly used unit of distance in astrophysics. 1 pc = 3.26 ly = 3.09 × 10 16 m Distances between nearby stars are measured i ...
... Sun and the Earth. It is really only useful when dealing with the distances of planets from the Sun. 1 AU = 1.50 × 10 11 m ≈ 8 light minutes The parsec (pc): This is the most commonly used unit of distance in astrophysics. 1 pc = 3.26 ly = 3.09 × 10 16 m Distances between nearby stars are measured i ...
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.