Microscopes
... Also known as ‘depth of field’, this is the distance (measured in the direction of the optical axis) between the two planes which define the limits of acceptable image sharpness when the microscope is focused on an object. As the numerical aperture (NA) increases, the depth of focus becomes shallowe ...
... Also known as ‘depth of field’, this is the distance (measured in the direction of the optical axis) between the two planes which define the limits of acceptable image sharpness when the microscope is focused on an object. As the numerical aperture (NA) increases, the depth of focus becomes shallowe ...
Lecture 26
... • There was a great deal of debate for many years about the nature of quasars • Some astronomers argued there was some strange process producing the high red shifts. • The question is now settled, as very deep imaging with the central source blocked out (like is done to image exoplanets around stars ...
... • There was a great deal of debate for many years about the nature of quasars • Some astronomers argued there was some strange process producing the high red shifts. • The question is now settled, as very deep imaging with the central source blocked out (like is done to image exoplanets around stars ...
Today`s Powerpoint
... All these effects are unnoticeable in our daily experience! They are tiny in Earth’s gravity, but large in a black hole’s. ...
... All these effects are unnoticeable in our daily experience! They are tiny in Earth’s gravity, but large in a black hole’s. ...
SHADES paper VII (b)
... (LOFAR, eMerlin, Hawaii, La Palma) 300 deg2 in KIDS-N (SKA pathfinders for HI and radio continuum; shallower LOFAR; visible from Atacama, ESO, La Palma) 400 deg2 in KIDS-S (SKA pathfinders for HI and radio continuum; SPT/SZ surveys; ALMA; GAMA; DES over part) ...
... (LOFAR, eMerlin, Hawaii, La Palma) 300 deg2 in KIDS-N (SKA pathfinders for HI and radio continuum; shallower LOFAR; visible from Atacama, ESO, La Palma) 400 deg2 in KIDS-S (SKA pathfinders for HI and radio continuum; SPT/SZ surveys; ALMA; GAMA; DES over part) ...
here - UMD Physics
... Any light coming from the right is polarized at 45 deg by the polarizer, and is then rotated to be horizontal by the Faraday crystal and is blocked by the vertical polarizer – giving one-way directionality. ...
... Any light coming from the right is polarized at 45 deg by the polarizer, and is then rotated to be horizontal by the Faraday crystal and is blocked by the vertical polarizer – giving one-way directionality. ...
Introduction Contact Weak Lensing: Method The NOAO Deep Wide
... —the Dark Energy. Experiments like the JDEM missions and LSST will use gravitational lensing as a tool to measure dark energy and its properties. There are two types of gravitational lensing: strong lensing occurs when the curvature is great enough to cause multiple imaging—the same background objec ...
... —the Dark Energy. Experiments like the JDEM missions and LSST will use gravitational lensing as a tool to measure dark energy and its properties. There are two types of gravitational lensing: strong lensing occurs when the curvature is great enough to cause multiple imaging—the same background objec ...
Refraction Rules for a Converging Lens
... optical fibers. The fibers are so small that once the light is introduced into the fiber with an angle within the confines of the numerical aperture of the fiber, it will continue to reflect off the walls of the fiber and thus can travel long distances in the fiber. Bundles of such fibers can accomp ...
... optical fibers. The fibers are so small that once the light is introduced into the fiber with an angle within the confines of the numerical aperture of the fiber, it will continue to reflect off the walls of the fiber and thus can travel long distances in the fiber. Bundles of such fibers can accomp ...
light – reflection and refraction
... to the principal axis meet or appear to meet after reflection from the mirror. The distance between the pole (P) and the focus (F) is called as the focal length. It is represented as ‘f’. The focal length is half the curvature. Uses of concave mirror 1) It is used as a shaving mirror since it fo ...
... to the principal axis meet or appear to meet after reflection from the mirror. The distance between the pole (P) and the focus (F) is called as the focal length. It is represented as ‘f’. The focal length is half the curvature. Uses of concave mirror 1) It is used as a shaving mirror since it fo ...
Grade 10 Optics Unit Outline - RosedaleGrade10Science
... 0.90. What is the speed of light in this material? Write down all givens, show your steps (algebra or formula triangle). Why would this material be so special? ...
... 0.90. What is the speed of light in this material? Write down all givens, show your steps (algebra or formula triangle). Why would this material be so special? ...
2 Marks Questions
... frequency and (iii) wavelength of light in glass. Assume that the frequency of light remains the same in both medium? 3) Draw a ray diagram showing the image formation by a concave mirror when an object is placed:- (a) between pole and focus of the mirror. (b) between focus and centre of curvature o ...
... frequency and (iii) wavelength of light in glass. Assume that the frequency of light remains the same in both medium? 3) Draw a ray diagram showing the image formation by a concave mirror when an object is placed:- (a) between pole and focus of the mirror. (b) between focus and centre of curvature o ...
1. INTRODUCTION 2. MASS AND LIGHT
... 2. The argument of ° 2 fails because the intervening structures happen to be contained within 5¡ of the LMC center (although they must extend over at least the inner D3¡ to account for the observed events). This possibility could only apply to a self-gravitating structure and not to an intrinsically ...
... 2. The argument of ° 2 fails because the intervening structures happen to be contained within 5¡ of the LMC center (although they must extend over at least the inner D3¡ to account for the observed events). This possibility could only apply to a self-gravitating structure and not to an intrinsically ...
Reflection of light by spherical Mirrors
... Light is a form of energy, which enable us to see the object. Reflection of Light When the light is allowed to fall on highly polished surface, such as mirror, most of the light gets reflected. Laws of Reflection 1. The angle of incidence is always equal toangle of reflection.i = r 2. The incident r ...
... Light is a form of energy, which enable us to see the object. Reflection of Light When the light is allowed to fall on highly polished surface, such as mirror, most of the light gets reflected. Laws of Reflection 1. The angle of incidence is always equal toangle of reflection.i = r 2. The incident r ...
Angular Momentum of Dark Matter Black Holes
... ROM [9] is correct for stellar-collapse black holes but is not applicable to the model of [3] which employs primordial black holes. This issue was discussed also in [10]. This ROM upper limit arises from the lack of any observed departure of the CMB spectrum from the predicted black-body curve or of ...
... ROM [9] is correct for stellar-collapse black holes but is not applicable to the model of [3] which employs primordial black holes. This issue was discussed also in [10]. This ROM upper limit arises from the lack of any observed departure of the CMB spectrum from the predicted black-body curve or of ...
Objective Test on Light – Reflection and Refraction
... 14. Three uses of concave mirrors are ________ and ________. 15. 1/u + 1/v = 1/f is called ________ 16. The value of magnification ‘m’ will be ________ for real images and ________ for virtual images in case of mirrors. 17. The unit of ‘m’ will be ________. 18. m = +3 indicates that image is _______ ...
... 14. Three uses of concave mirrors are ________ and ________. 15. 1/u + 1/v = 1/f is called ________ 16. The value of magnification ‘m’ will be ________ for real images and ________ for virtual images in case of mirrors. 17. The unit of ‘m’ will be ________. 18. m = +3 indicates that image is _______ ...
Contents - arXiv.org
... Gravitational Microlensing can be thought of as a version of strong gravitational lensing in which the image separation is too small to be resolved. Multiple images are formed, but their typical separation – ∆θ ≈ 2 θE – is far below the limiting resolution determined by observational constraints. Gi ...
... Gravitational Microlensing can be thought of as a version of strong gravitational lensing in which the image separation is too small to be resolved. Multiple images are formed, but their typical separation – ∆θ ≈ 2 θE – is far below the limiting resolution determined by observational constraints. Gi ...
ERRORS OF REFRACTION
... It is a condition in which a point of light cannot be made to produce a punctate image upon the retina by any spherical correcting lens ...
... It is a condition in which a point of light cannot be made to produce a punctate image upon the retina by any spherical correcting lens ...
lab - UCSC Physics
... respectively. In each case, where is the image plane; is the image virtual or real; and what is the magnification? 3. (Slightly challenging) You have at your disposal a lens with given focal length f. You may place the lens anywhere between an object plane and an image plane, which are separated by ...
... respectively. In each case, where is the image plane; is the image virtual or real; and what is the magnification? 3. (Slightly challenging) You have at your disposal a lens with given focal length f. You may place the lens anywhere between an object plane and an image plane, which are separated by ...
SSS in young stellar populations: progenitors of the
... breakup velocity (Townsend et al., 2004) • Emission lines believed to arise in decretion disk which forms due to massive rotation • Evidence that rapid rotation is due to CBE (e.g. existence of Be/NS binaries) ...
... breakup velocity (Townsend et al., 2004) • Emission lines believed to arise in decretion disk which forms due to massive rotation • Evidence that rapid rotation is due to CBE (e.g. existence of Be/NS binaries) ...
Solutions of Chapter 4 4.1. Compare light microscopy, transmission
... 4.4. How can you obtain SEM images with the best resolution by adjusting operation parameters? The best resolution will result from optimizing the probe size, probe current density, and eliminate astigmatism. High resolution of SEM requires reduce probe size. The probe current should maintain at cer ...
... 4.4. How can you obtain SEM images with the best resolution by adjusting operation parameters? The best resolution will result from optimizing the probe size, probe current density, and eliminate astigmatism. High resolution of SEM requires reduce probe size. The probe current should maintain at cer ...
Experiment 10 - WFU Physics Home
... The optical axis of a lens is a line through the center of the lens and perpendicular to the plane of the lens. The focal point of the converging lens is that point on the optical axis at which rays of light from an infinitely remote source on the optical axis (like the sun) converge. The focal poin ...
... The optical axis of a lens is a line through the center of the lens and perpendicular to the plane of the lens. The focal point of the converging lens is that point on the optical axis at which rays of light from an infinitely remote source on the optical axis (like the sun) converge. The focal poin ...
슬라이드 1
... However, the observed stellar mass in these galaxies is significantly less than ~ 1011M⊙ - 1012M⊙ in a typical local cD galaxy. → The majority of the stars have yet to form. ...
... However, the observed stellar mass in these galaxies is significantly less than ~ 1011M⊙ - 1012M⊙ in a typical local cD galaxy. → The majority of the stars have yet to form. ...
Black Holes
... weightless. Einstein says these are equivalent. So in freefall, the light and the ball also travel in straight lines. 3. Now imagine two people in freefall on Earth, passing a ball back and forth. From their perspective, they pass the ball in a straight line. From a stationary perspective, the ball ...
... weightless. Einstein says these are equivalent. So in freefall, the light and the ball also travel in straight lines. 3. Now imagine two people in freefall on Earth, passing a ball back and forth. From their perspective, they pass the ball in a straight line. From a stationary perspective, the ball ...
Bright Field Microscopy
... The smaller the distance between the two specific objects that can be distinguished apart, the greater the resolution power of the microscope. Minimal distance between two objects = (0.612 X ) / NA The larger NA, the smaller the resolvable distance and hence, the more efficient the resolution power ...
... The smaller the distance between the two specific objects that can be distinguished apart, the greater the resolution power of the microscope. Minimal distance between two objects = (0.612 X ) / NA The larger NA, the smaller the resolvable distance and hence, the more efficient the resolution power ...
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.