What is Optics? Photonics?
... • Think of optics as the science of light. It’s a branch of physics that describes the behavior and properties of light and the interaction of light with matter. It’s about what light is made of and how it behaves. • Light allows us to see, but it also transmits sound, cuts things, and controls elec ...
... • Think of optics as the science of light. It’s a branch of physics that describes the behavior and properties of light and the interaction of light with matter. It’s about what light is made of and how it behaves. • Light allows us to see, but it also transmits sound, cuts things, and controls elec ...
January
... Except for the probes that have been sent to the planets, astronomers cannot reach out and touch their experiment, which is the universe itself. One of the key measurements in Astronomy is distance. To measure distances, the astronomer must rely on the light from any object. Distances are then deter ...
... Except for the probes that have been sent to the planets, astronomers cannot reach out and touch their experiment, which is the universe itself. One of the key measurements in Astronomy is distance. To measure distances, the astronomer must rely on the light from any object. Distances are then deter ...
lecture CH8 A chem161pikul
... 1. Which electromagnetic radiation has a higher energy? Radio waves or microwaves? UV light or X rays? 2. How does thermal imaging work? (Use what you have learned about the electromagnetic spectrum to briefly explain). 3. Blue, red, and green lasers have wavelengths of 445 nm, 635 nm, and 532 nm re ...
... 1. Which electromagnetic radiation has a higher energy? Radio waves or microwaves? UV light or X rays? 2. How does thermal imaging work? (Use what you have learned about the electromagnetic spectrum to briefly explain). 3. Blue, red, and green lasers have wavelengths of 445 nm, 635 nm, and 532 nm re ...
PowerPoint Presentation - Mullard Space Science Laboratory
... SGRB in the first hundred seconds is ~ 1050 erg. LGRB are a few hundreds to a few thousand times more energetic. Now there are evidences that LGRB are associated with violent explosions of massive stars [13,14], while SGRB are believed to be caused by compact-star merging. Here, we consider various ...
... SGRB in the first hundred seconds is ~ 1050 erg. LGRB are a few hundreds to a few thousand times more energetic. Now there are evidences that LGRB are associated with violent explosions of massive stars [13,14], while SGRB are believed to be caused by compact-star merging. Here, we consider various ...
Nemcova abstract- ICPIG.rtf - Queen`s University Belfast
... quickly heats reaching boiling point within around 2 minutes depending on the solution. The hydrogen peroxide production and pH change were measured using Quantofix and Sigma test strips respectively. The current is determined via the various impedance influencing factors dependent on the environmen ...
... quickly heats reaching boiling point within around 2 minutes depending on the solution. The hydrogen peroxide production and pH change were measured using Quantofix and Sigma test strips respectively. The current is determined via the various impedance influencing factors dependent on the environmen ...
The Universe - UMass Astronomy
... What is the farthest thing/object we have identified from Earth? It really depends on what you mean by `object’. The farthest we think we will ever be able to `see’ is the Cosmic Microwave Background. The farthest galaxy, so far, is at redshift z=7, equivalent to an age of the Universe of less than ...
... What is the farthest thing/object we have identified from Earth? It really depends on what you mean by `object’. The farthest we think we will ever be able to `see’ is the Cosmic Microwave Background. The farthest galaxy, so far, is at redshift z=7, equivalent to an age of the Universe of less than ...
Spectroscopic Study of Argon DC Glow Discharge
... where I, λ, g, and f are the total intensity, wavelength, statistical weight, and absorption oscillator strength, respectively, of one line and E is its excitation energy. The corresponding quantities for the other line are I % , λ% , g % , f % , and E % . The values of the above parameters have bee ...
... where I, λ, g, and f are the total intensity, wavelength, statistical weight, and absorption oscillator strength, respectively, of one line and E is its excitation energy. The corresponding quantities for the other line are I % , λ% , g % , f % , and E % . The values of the above parameters have bee ...
Objective Classification of Galaxy Spectra using the Information Bottleneck Method
... photon counts in each spectrum to unity, we can consider it as a conditional probability, the probability of observing a photon at a speci c wavelength from a given galaxy. This view of the ensemble of spectra as a conditional probability distribution function enables us to undertake the information ...
... photon counts in each spectrum to unity, we can consider it as a conditional probability, the probability of observing a photon at a speci c wavelength from a given galaxy. This view of the ensemble of spectra as a conditional probability distribution function enables us to undertake the information ...
Early Star-Forming Galaxies and the Reionisation of the Universe
... forming galaxies is the Lyman α emission line at rest wavelength of 121.6nm, produced internally by gas heated by young stars. The observability of Lyman α emission is sensitive to the ionisation state of the IGM, as the observed line strength can be attenuated by intervening neutral hydrogen. The ...
... forming galaxies is the Lyman α emission line at rest wavelength of 121.6nm, produced internally by gas heated by young stars. The observability of Lyman α emission is sensitive to the ionisation state of the IGM, as the observed line strength can be attenuated by intervening neutral hydrogen. The ...
Teacher`s Guide - Discovery Education
... Develop custom worksheets, educational puzzles, online quizzes, and more with the free teaching tools offered on the Discoveryschool.com Web site. Create and print support materials, or save them to a Custom Classroom account for future use. To learn more, visit ...
... Develop custom worksheets, educational puzzles, online quizzes, and more with the free teaching tools offered on the Discoveryschool.com Web site. Create and print support materials, or save them to a Custom Classroom account for future use. To learn more, visit ...
Light 1 Mathematical representation of light (EM waves)
... In comparison to the sun, artificial light sources can be made to emit in specific frequencies. These light sources are known as spectral lamps and typically make use of the well defined energy levels in atoms to emit light of well defined frequencies, as indicated by the relation between the energy ...
... In comparison to the sun, artificial light sources can be made to emit in specific frequencies. These light sources are known as spectral lamps and typically make use of the well defined energy levels in atoms to emit light of well defined frequencies, as indicated by the relation between the energy ...
Neutron Stars and Black Holes
... Since the Schwarzschild radius of a black hole is rSch = 2 GM / c2, the radius of a black hole is proportional to its mass. A one billion solar mass black hole will have a radius of 3 X 109 km. Since one Astronomical Unit ~ 1.5 X 108 km, it follows that a one billion solar mass black hole has a rad ...
... Since the Schwarzschild radius of a black hole is rSch = 2 GM / c2, the radius of a black hole is proportional to its mass. A one billion solar mass black hole will have a radius of 3 X 109 km. Since one Astronomical Unit ~ 1.5 X 108 km, it follows that a one billion solar mass black hole has a rad ...
4. Star Formation
... of well under a second!. The potential energy of the cloud (E pot = − GM2 / R) has to be released. For the Sun this amounts to 3.8·1041 J, equivalent of 31.6·106 yrs of solar luminosity. But star formation timescales are much shorter than this. Hence the energy has to be radiated/transported away, d ...
... of well under a second!. The potential energy of the cloud (E pot = − GM2 / R) has to be released. For the Sun this amounts to 3.8·1041 J, equivalent of 31.6·106 yrs of solar luminosity. But star formation timescales are much shorter than this. Hence the energy has to be radiated/transported away, d ...
Optics: Against the spread of the light
... like a cannonball, and to follow a parabolic trajectory. Features within the beams were seen to ‘accelerate’ by starting to move transverse to their direction of propagation. This behaviour may mimic that of a quantummechanical particle placed in a constant gravitational field3. It would be interest ...
... like a cannonball, and to follow a parabolic trajectory. Features within the beams were seen to ‘accelerate’ by starting to move transverse to their direction of propagation. This behaviour may mimic that of a quantummechanical particle placed in a constant gravitational field3. It would be interest ...
File - GENERAL DEPARTMENT
... present. It comes to this state after absorbing a photon of energy hf or by some other inelastic collision. The atom has now become an excited atom. A short time later, the atom will move itself to its ground state, emitting a photon of energy hf. We call this process spontaneous emission – spontane ...
... present. It comes to this state after absorbing a photon of energy hf or by some other inelastic collision. The atom has now become an excited atom. A short time later, the atom will move itself to its ground state, emitting a photon of energy hf. We call this process spontaneous emission – spontane ...
Lect16-3-28-and-30-1..
... opposite rings Burrows found a common center. However, it is offset from the heart of the supernova ejecta. When Burrows did a detailed inspection of the HST image, he found a dim object which may be the source of the beam at the predicted location. The object is about 1/3 light-year from the center ...
... opposite rings Burrows found a common center. However, it is offset from the heart of the supernova ejecta. When Burrows did a detailed inspection of the HST image, he found a dim object which may be the source of the beam at the predicted location. The object is about 1/3 light-year from the center ...
Final report - Columbia University
... in mirror movements as necessary. I wrote a C++ code (snapshotv3.cpp) that can accept either a specific image (.png or .jpg, for example) and output the peak intensity in pixel coordinates (dimensions of 640x480 pixels). If no image is specified, the code engages a USB–connected webcam and processe ...
... in mirror movements as necessary. I wrote a C++ code (snapshotv3.cpp) that can accept either a specific image (.png or .jpg, for example) and output the peak intensity in pixel coordinates (dimensions of 640x480 pixels). If no image is specified, the code engages a USB–connected webcam and processe ...
Color-Magnitude Diagram Lab Manual
... 1. One technique that is useful for locating objects is called star hopping. This involves using the locations of known bright objects to find fainter ones. Although this virtual telescope can perfectly slew to an object by its right ascension and declination, real telescopes are not so precise. In ...
... 1. One technique that is useful for locating objects is called star hopping. This involves using the locations of known bright objects to find fainter ones. Although this virtual telescope can perfectly slew to an object by its right ascension and declination, real telescopes are not so precise. In ...
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.