Optics - MyCourses
... lens, for example, the rays of light propagating far away from the optical distance will refract closer to the lens than paraxial rays. With modern manufacturing systems aspherical lenses can already be manufactured at a reasonable cost by pressing lenses out of melt glass or plastic using a mold. A ...
... lens, for example, the rays of light propagating far away from the optical distance will refract closer to the lens than paraxial rays. With modern manufacturing systems aspherical lenses can already be manufactured at a reasonable cost by pressing lenses out of melt glass or plastic using a mold. A ...
the first simultaneous microlensing observations by two space
... companion, and the parallax measurement from Spitzer allows us to determine that it is a BD. This additional BD detection provides supporting evidence for a conclusion previously drawn from microlensing studies: that BDs around main sequence stars are relatively common at separations of a few au (Sh ...
... companion, and the parallax measurement from Spitzer allows us to determine that it is a BD. This additional BD detection provides supporting evidence for a conclusion previously drawn from microlensing studies: that BDs around main sequence stars are relatively common at separations of a few au (Sh ...
Where is the rest of the universe?
... Where is the rest of the Universe? If we can only “see” 4.9% of the universe, where is the other 95%? Dark matter Dark matter does not give off observable energy in any EM wavelength, but can be detected by watching the behavior of space objects. A few examples are: • The stars in the outer reaches ...
... Where is the rest of the Universe? If we can only “see” 4.9% of the universe, where is the other 95%? Dark matter Dark matter does not give off observable energy in any EM wavelength, but can be detected by watching the behavior of space objects. A few examples are: • The stars in the outer reaches ...
Powerpoint file - Physics @ CSU Stanislaus
... Camera lenses are categorized according to their focal lengths and maximum apertures. The longer the focal length, the larger the image inside the camera will be. The greater the size of the aperture, the more light the lens will admit. Focal length is the distance from the optical center of the len ...
... Camera lenses are categorized according to their focal lengths and maximum apertures. The longer the focal length, the larger the image inside the camera will be. The greater the size of the aperture, the more light the lens will admit. Focal length is the distance from the optical center of the len ...
Open access
... general lensing events, the Einstein time scale is the only measurable quantity related to the physical parameters of the lens. However, the time scale results from the combination of 3 physical parameters of the mass of the lens, M, the distance to the lens, DL , and the lens-source transverse spee ...
... general lensing events, the Einstein time scale is the only measurable quantity related to the physical parameters of the lens. However, the time scale results from the combination of 3 physical parameters of the mass of the lens, M, the distance to the lens, DL , and the lens-source transverse spee ...
Autumn semester 2013-14 - The University of Sheffield
... is not equidistant between the Earth and background luminous object. Hence, state how the angular diameter of lensing events is changed if the position of the lens is shifted along the line of sight, assuming the distance between the background object and observer is kept constant. ...
... is not equidistant between the Earth and background luminous object. Hence, state how the angular diameter of lensing events is changed if the position of the lens is shifted along the line of sight, assuming the distance between the background object and observer is kept constant. ...
슬라이드 1
... dn/dσ of early-type galaxies based on the SDSS DR5 data (Choi, Park, & Vogeley 2007). • For the lensing potential, we use the singular isothermal ellipsoid mass model. • Use CLASS + other radio-selected lens sample of 26 lenses. ...
... dn/dσ of early-type galaxies based on the SDSS DR5 data (Choi, Park, & Vogeley 2007). • For the lensing potential, we use the singular isothermal ellipsoid mass model. • Use CLASS + other radio-selected lens sample of 26 lenses. ...
Astronomy Scavenger Hunt Distances 1. What is the
... 11. What is the distance between the Milky Way and a group of galaxies known as the Virgo Cluster? 12. What is the distance between the Milky Way and the furthest object that can be seen by the Hubble Space Telescope? Sizes ...
... 11. What is the distance between the Milky Way and a group of galaxies known as the Virgo Cluster? 12. What is the distance between the Milky Way and the furthest object that can be seen by the Hubble Space Telescope? Sizes ...
Refraction_and_Lenses
... • The incident angle of light n=1 that causes refraction along r=900 the boundary between surfaces c n=1.5 • The angle of refraction will always be 90o • Only possible when going from more optically dense (high index of refraction) to less optically dense medium (low index of refraction • Only pos ...
... • The incident angle of light n=1 that causes refraction along r=900 the boundary between surfaces c n=1.5 • The angle of refraction will always be 90o • Only possible when going from more optically dense (high index of refraction) to less optically dense medium (low index of refraction • Only pos ...
It is sometimes difficult to find the polarity of an induced emf. The net
... refraction of light. Violet light is bent more than red light and the other colors fall in between. This is why a prism splits light into its component ...
... refraction of light. Violet light is bent more than red light and the other colors fall in between. This is why a prism splits light into its component ...
One or more bound planets per Milky Way star
... To derive the actual abundance of exoplanets from our survey, we proceeded as follows. Let the planetary mass function, f (log a, log M) ≡ dN/(d log a d log M), where N is the average number of planets per star. We then integrate the product f (log a, log M) S (log a, log M) over log a and log M. Th ...
... To derive the actual abundance of exoplanets from our survey, we proceeded as follows. Let the planetary mass function, f (log a, log M) ≡ dN/(d log a d log M), where N is the average number of planets per star. We then integrate the product f (log a, log M) S (log a, log M) over log a and log M. Th ...
concave lens - Broadneck High School
... raindrops (a). Because of dispersion, only one color from each raindrop reaches an observer (b). (Illustration not to scale) ...
... raindrops (a). Because of dispersion, only one color from each raindrop reaches an observer (b). (Illustration not to scale) ...
Week 7: Gravitational Lensing
... where M (< b) is the mass seen in projection within a distance b of the source. The simplest example is, of course, a point mass, which has a deflection angle α = 4GM/c2 b. Another example is the singular isothermal sphere (SIS) which has a density profile ρ(r) = σ 2 /(2πGr 2 ) as a function of radi ...
... where M (< b) is the mass seen in projection within a distance b of the source. The simplest example is, of course, a point mass, which has a deflection angle α = 4GM/c2 b. Another example is the singular isothermal sphere (SIS) which has a density profile ρ(r) = σ 2 /(2πGr 2 ) as a function of radi ...
Midterm
... The image is (a) on the same side of the lens as the stamp, (b) on the side of the lens opposite to the stamp, (c) inside the lens, (d) on both sides of the lens. (a) -----------------------------------8. A glass brick is submerged in water with refractive index 1.33. Light is incident on the glass ...
... The image is (a) on the same side of the lens as the stamp, (b) on the side of the lens opposite to the stamp, (c) inside the lens, (d) on both sides of the lens. (a) -----------------------------------8. A glass brick is submerged in water with refractive index 1.33. Light is incident on the glass ...
Chapter 14 Refraction ppt
... • The separation of light into colors arranged according to their frequency, by interaction with a prism or diffraction grating. ...
... • The separation of light into colors arranged according to their frequency, by interaction with a prism or diffraction grating. ...
Mr. Hartman/Ms. Slack Date:______ Chapter 19
... Light passing through a medium such as air, water, or glass, however, travels ________ _____________ than this. This is because the atoms that make up the material interact with the light waves and _________________________. The Refraction of Light Waves If a light wave travels from one medium to an ...
... Light passing through a medium such as air, water, or glass, however, travels ________ _____________ than this. This is because the atoms that make up the material interact with the light waves and _________________________. The Refraction of Light Waves If a light wave travels from one medium to an ...
ph607-14-a3uni - University of Kent
... from the nucleus in three years. Assuming the motion is in the plane of the sky and using a proper distance to 3C273 of 640 megaparsecs, show that the motion is superluminal. ...
... from the nucleus in three years. Assuming the motion is in the plane of the sky and using a proper distance to 3C273 of 640 megaparsecs, show that the motion is superluminal. ...
Hubblecast 70: Peering around cosmic corners Visual notes 00:00
... actually see fainter, and therefore more distant objects, than would otherwise be possible. Also, the images are magnified, so that we can see more detail – just like when using an ordinary magnifying glass. ...
... actually see fainter, and therefore more distant objects, than would otherwise be possible. Also, the images are magnified, so that we can see more detail – just like when using an ordinary magnifying glass. ...
MIRRORS & LENSES
... Chapter 18: Refraction and Lenses Pre-Class for Tuesday 4-10-12 In terms of light transmission, what is the difference between mirrors and lenses? ...
... Chapter 18: Refraction and Lenses Pre-Class for Tuesday 4-10-12 In terms of light transmission, what is the difference between mirrors and lenses? ...
Chap5-uLensing-c - Groupe d`Astronomie et Astrophysique
... Separation between light from source and lens is possible once angular separation has increased by a few mas, several years after the lens event. Difference in color between the source and the lens will result in a small displacement of the centroid with ...
... Separation between light from source and lens is possible once angular separation has increased by a few mas, several years after the lens event. Difference in color between the source and the lens will result in a small displacement of the centroid with ...
Notes and Hints for AP Physics Summer Assignment
... Notes and Hints for AP Physics Summer Assignment (Note: This is not a complete guide… you will need to use other online resources to find more information on some of these topics) In Honors, we discussed REFLECTION and the mirror equations (including ray diagrams). We also discussed REFRACTION and S ...
... Notes and Hints for AP Physics Summer Assignment (Note: This is not a complete guide… you will need to use other online resources to find more information on some of these topics) In Honors, we discussed REFLECTION and the mirror equations (including ray diagrams). We also discussed REFRACTION and S ...
talk at lensing and dark matter conference Ohio state 2004
... The number of non-Macho events is predicted to be much smaller than the 13-17 events observed (using standard LMC and Milky Way stellar populations.) ...
... The number of non-Macho events is predicted to be much smaller than the 13-17 events observed (using standard LMC and Milky Way stellar populations.) ...
Gravitational microlensing
Gravitational microlensing is an astronomical phenomenon due to the gravitational lens effect. It can be used to detect objects that range from the mass of a planet to the mass of a star, regardless of the light they emit. Typically, astronomers can only detect bright objects that emit much light (stars) or large objects that block background light (clouds of gas and dust). These objects make up only a tiny portion of the mass of a galaxy. Microlensing allows the study of objects that emit little or no light.When a distant star or quasar gets sufficiently aligned with a massive compact foreground object, the bending of light due to its gravitational field, as discussed by Einstein in 1915, leads to two distorted unresolved images resulting in an observable magnification. The time-scale of the transient brightening depends on the mass of the foreground object as well as on the relative proper motion between the background 'source' and the foreground 'lens' object.Since microlensing observations do not rely on radiation received from the lens object, this effect therefore allows astronomers to study massive objects no matter how faint. It is thus an ideal technique to study the galactic population of such faint or dark objects as brown dwarfs, red dwarfs, planets, white dwarfs, neutron stars, black holes, andMassive Compact Halo Objects. Moreover, the microlensing effect is wavelength-independent, allowing study of source objects that emit any kind of electromagnetic radiation.Microlensing by an isolated object was first detected in 1989. Since then, microlensing has been used to constrain the nature of the dark matter, detect extrasolar planets, study limb darkening in distant stars, constrain the binary star population, and constrain the structure of the Milky Way's disk. Microlensing has also been proposed as a means to find dark objects like brown dwarfs and black holes, study starspots, measure stellar rotation, and probe quasars including their accretion disks.