The Sagittarius dwarf irregular galaxy: Metallicity and stellar
... content in dwarf irregular galaxies (see Mateo 1998). Because of its high gas content, low luminosity, and especially its claimed very low metallicity, SagDIG may be a clue to the origin and evolution of dwarf galaxies. Although located at the border of the Local Group it is still close enough to al ...
... content in dwarf irregular galaxies (see Mateo 1998). Because of its high gas content, low luminosity, and especially its claimed very low metallicity, SagDIG may be a clue to the origin and evolution of dwarf galaxies. Although located at the border of the Local Group it is still close enough to al ...
The Sagittarius dwarf irregular galaxy
... content in dwarf irregular galaxies (see Mateo 1998). Because of its high gas content, low luminosity, and especially its claimed very low metallicity, SagDIG may be a clue to the origin and evolution of dwarf galaxies. Although located at the border of the Local Group it is still close enough to al ...
... content in dwarf irregular galaxies (see Mateo 1998). Because of its high gas content, low luminosity, and especially its claimed very low metallicity, SagDIG may be a clue to the origin and evolution of dwarf galaxies. Although located at the border of the Local Group it is still close enough to al ...
ppt 2.6 - NRAO: Socorro, New Mexico
... • the surroundings are “messy” and the outflow collides with nearby “stuff” • by observing the results of this collision, we can learn about the engine, its environment, and the relation between the engine and the environment • Concentrate on: Massive outflows from massive (non-exploding) stars • ne ...
... • the surroundings are “messy” and the outflow collides with nearby “stuff” • by observing the results of this collision, we can learn about the engine, its environment, and the relation between the engine and the environment • Concentrate on: Massive outflows from massive (non-exploding) stars • ne ...
The life-cycle of stars - Young Scientists Journal
... just 20 kilometers, yet masses three times that of the Sun [Figure 6].[3] Some neutron stars emit radio waves. These neutron stars are called pulsars. The waves seem to flash on and off, but this is only the case due to the beam of radio waves rotating around the poles of the stars, while the Earth ...
... just 20 kilometers, yet masses three times that of the Sun [Figure 6].[3] Some neutron stars emit radio waves. These neutron stars are called pulsars. The waves seem to flash on and off, but this is only the case due to the beam of radio waves rotating around the poles of the stars, while the Earth ...
measuring wavelength discrimination threshold along the entire
... (ergo wavelengths) is better in the middle range of the visible spectrum than at its boundaries. Wavelength discrimination ability is a kind of sensation threshold, which shows when we can discriminate between two different wavelength lights based on the different hue [1]. The smallest sensible diff ...
... (ergo wavelengths) is better in the middle range of the visible spectrum than at its boundaries. Wavelength discrimination ability is a kind of sensation threshold, which shows when we can discriminate between two different wavelength lights based on the different hue [1]. The smallest sensible diff ...
Light
... more energy. Photons are light particles that contain certain amounts of energy based on their frequency and wavelength. ...
... more energy. Photons are light particles that contain certain amounts of energy based on their frequency and wavelength. ...
Stars in the Sky Stars in the Sky
... This is called the Doppler effect. It works with both sound and light. As a light source moves away quickly, its light looks redder. This particular Doppler effect is called red shift. The farther apart two galaxies are moving, the faster the galaxies are moving apart. From the perspective of each g ...
... This is called the Doppler effect. It works with both sound and light. As a light source moves away quickly, its light looks redder. This particular Doppler effect is called red shift. The farther apart two galaxies are moving, the faster the galaxies are moving apart. From the perspective of each g ...
II. The Universe Around Us
... which parallax angle is 1”; 1 pc = 3.086×1016 m (≈3.26 light years; 1 kpc = 3.086×1019 m, 1 Mpc = 3.086×1022 m) • 1 M = 1.989×1030 kg, 1L = 3.839×1026 W • 1 Å = 10-10 m (0.1 nm) • 1 eV = 1.602×10-19 J ASTR378 ...
... which parallax angle is 1”; 1 pc = 3.086×1016 m (≈3.26 light years; 1 kpc = 3.086×1019 m, 1 Mpc = 3.086×1022 m) • 1 M = 1.989×1030 kg, 1L = 3.839×1026 W • 1 Å = 10-10 m (0.1 nm) • 1 eV = 1.602×10-19 J ASTR378 ...
The Nobel Prize in Physics 2005
... light phenomena. But what is light and how do various kinds of light differ from each other? How does light emitted by a candle differ from the beam produced by a laser in a CD player? According to Albert Einstein, the speed of light in empty space is constant. Is it possible to use light to measure ...
... light phenomena. But what is light and how do various kinds of light differ from each other? How does light emitted by a candle differ from the beam produced by a laser in a CD player? According to Albert Einstein, the speed of light in empty space is constant. Is it possible to use light to measure ...
page proofs
... Shapley argued that the Milky Way was the entire universe and all the nebulae were therefore to be found within it. Curtis argued that some nebulae were actually separate galaxies of stars, well outside the Milky Way. For Curtis to be right, these galaxies must lie at enormous distances from the Ear ...
... Shapley argued that the Milky Way was the entire universe and all the nebulae were therefore to be found within it. Curtis argued that some nebulae were actually separate galaxies of stars, well outside the Milky Way. For Curtis to be right, these galaxies must lie at enormous distances from the Ear ...
Formation and Evolution of Infalling Disks Around Protostars
... Summary part2: Star Formation Triggered by First Supernovae Supernovae of first stars ...
... Summary part2: Star Formation Triggered by First Supernovae Supernovae of first stars ...
Background Presentation
... Sonoma State University A group of people working collaboratively to educate the public about current and future NASA high energy astrophysics/astronomy missions. Swift Led by Prof. Lynn Cominsky ...
... Sonoma State University A group of people working collaboratively to educate the public about current and future NASA high energy astrophysics/astronomy missions. Swift Led by Prof. Lynn Cominsky ...
Optical Sources
... This laser is called a Fabry-Perot laser diode (FP-LD) Semiconductor-air interface produces a reflection coefficient at normal incidence of ...
... This laser is called a Fabry-Perot laser diode (FP-LD) Semiconductor-air interface produces a reflection coefficient at normal incidence of ...
Pulsations in White Dwarfs
... Extremely rare (14 / 25,000) carbonatmosphere white dwarfs discovered in 2007 only. They bunch around Teff~20,000 K and have very high surface gravities. They are likely all highly magnetic (>1 MGauss) and half them pulsate. Low-degree (1,2), low- to mid-order g-mode ...
... Extremely rare (14 / 25,000) carbonatmosphere white dwarfs discovered in 2007 only. They bunch around Teff~20,000 K and have very high surface gravities. They are likely all highly magnetic (>1 MGauss) and half them pulsate. Low-degree (1,2), low- to mid-order g-mode ...
Oort Cloud Evolu on in a Long
... Thomas Nordlander, Hans Rickman, Bengt Gustafsson Uppsala Astron. Observatory ...
... Thomas Nordlander, Hans Rickman, Bengt Gustafsson Uppsala Astron. Observatory ...
mass loss of massive stars - of /proceedings
... Garcia, M., Herrero, A., Najarro, F., Lennon, D. J., & Alejandro Urbaneja, M. 2014, ApJ, 788, 64 Haubois, X., Perrin, G., Lacour, S., et al. 2009, A&A, 508, 923 Humphreys, R. M. & Davidson, K. 1979, ApJ, 232, 409 Kervella, P., Perrin, G., Chiavassa, A., et al. 2011, A&A, 531, A117 Leitherer, C., Rob ...
... Garcia, M., Herrero, A., Najarro, F., Lennon, D. J., & Alejandro Urbaneja, M. 2014, ApJ, 788, 64 Haubois, X., Perrin, G., Lacour, S., et al. 2009, A&A, 508, 923 Humphreys, R. M. & Davidson, K. 1979, ApJ, 232, 409 Kervella, P., Perrin, G., Chiavassa, A., et al. 2011, A&A, 531, A117 Leitherer, C., Rob ...
Hydrogen Greenhouse Planets Beyond the Habitable Zone
... nebula. Should the Kepler mission be extended (∼6 yr), planets at 1.5-2 AU, the inner boundary where a hydrogen atmosphere is retained (Figure 3), could be confirmed with 3 transits. Measuring mass would be at the limit of current Doppler ...
... nebula. Should the Kepler mission be extended (∼6 yr), planets at 1.5-2 AU, the inner boundary where a hydrogen atmosphere is retained (Figure 3), could be confirmed with 3 transits. Measuring mass would be at the limit of current Doppler ...
Atmospheric Monitoring for High Energy Gamma Ray Cherenkov
... phase function. In this work we present its design details and the first laboratory tests of the receiver by means of optical alignment and collection efficiency. In this frame, we also present and propose a complete, novel and non-invasive characterization technique of the etalons to be used for th ...
... phase function. In this work we present its design details and the first laboratory tests of the receiver by means of optical alignment and collection efficiency. In this frame, we also present and propose a complete, novel and non-invasive characterization technique of the etalons to be used for th ...
Putting a Spin on the Solar System
... Who's "In" and Who's "Out?" Scientists studying the solar system saw the same patterns that you saw in your model. They discovered that planets were made from either of two basic types of matter. Some planets are composed of mostly rock and metal and have solid rocky surfaces. These are called terre ...
... Who's "In" and Who's "Out?" Scientists studying the solar system saw the same patterns that you saw in your model. They discovered that planets were made from either of two basic types of matter. Some planets are composed of mostly rock and metal and have solid rocky surfaces. These are called terre ...
Astronomical spectroscopy
Astronomical spectroscopy is the study of astronomy using the techniques of spectroscopy to measure the spectrum of electromagnetic radiation, including visible light, which radiates from stars and other hot celestial objects. Spectroscopy can be used to derive many properties of distant stars and galaxies, such as their chemical composition, temperature, density, mass, distance, luminosity, and relative motion using Doppler shift measurements.