Ch_25
... Dissemination or sale of any part of this work (including on the World Wide Web) will destroy the integrity of the work and is not permitted. The work and materials from it should never be made available to students except by instructors using the accompanying text in their classes. All recipients o ...
... Dissemination or sale of any part of this work (including on the World Wide Web) will destroy the integrity of the work and is not permitted. The work and materials from it should never be made available to students except by instructors using the accompanying text in their classes. All recipients o ...
Quiz # 3
... 9. One technique that astronomers are now using to increase the amount of detail that can be recorded with telescopes is A) spinning huge tubs of mercury, thus producing very large parabolic surfaces at relatively low cost. B) antireflective coatings, where the mirror is coated with a substance such ...
... 9. One technique that astronomers are now using to increase the amount of detail that can be recorded with telescopes is A) spinning huge tubs of mercury, thus producing very large parabolic surfaces at relatively low cost. B) antireflective coatings, where the mirror is coated with a substance such ...
Slide 1
... The camera is general purpose detector with a universal face-plate for attachment to various ...
... The camera is general purpose detector with a universal face-plate for attachment to various ...
Slides
... limiting the capability of observations Studies have revealed a direct relationship between the detection capability of a telescope and the cleanliness and efficiency of the coatings (Dierickx, 1992). To ensure maximum reflectivity, mirror surfaces have to cleaned and re-aluminized from time to time ...
... limiting the capability of observations Studies have revealed a direct relationship between the detection capability of a telescope and the cleanliness and efficiency of the coatings (Dierickx, 1992). To ensure maximum reflectivity, mirror surfaces have to cleaned and re-aluminized from time to time ...
SOLAR ORBITER All the space you need
... Solar Orbiter will, through a novel orbital design and an advanced suite of scientific instruments, provide the observations required to take Solar Science to the next level. Launch date is 2017 ...
... Solar Orbiter will, through a novel orbital design and an advanced suite of scientific instruments, provide the observations required to take Solar Science to the next level. Launch date is 2017 ...
Optics requirements for the Generation-X x
... There are approaches to controlling those errors. ...
... There are approaches to controlling those errors. ...
Main Sequence Star
... telescope Collects radio waves from space Can be used at anytime or weather ...
... telescope Collects radio waves from space Can be used at anytime or weather ...
Chapter 18 - Firelands Local Schools
... answer many questions, but new technologies have presented new questions that were unthinkable even 10 years ago. Telescopes ...
... answer many questions, but new technologies have presented new questions that were unthinkable even 10 years ago. Telescopes ...
Point Spread Function
... reasons. First, aberrations in the optical system will spread the image over a finite area. Second, diffraction effects will also spread the image, even in a system that has no aberrations. optical transfer function The optical transfer function (OTF) of an imaging system ( camera, video, system, mi ...
... reasons. First, aberrations in the optical system will spread the image over a finite area. Second, diffraction effects will also spread the image, even in a system that has no aberrations. optical transfer function The optical transfer function (OTF) of an imaging system ( camera, video, system, mi ...
PS#3
... 3. A white dwarf star has a radius of 7x10 cm and a temperature of 10,000K. What is its luminosity? Compare to the Sun. ...
... 3. A white dwarf star has a radius of 7x10 cm and a temperature of 10,000K. What is its luminosity? Compare to the Sun. ...
A Chandra Observation of the Massive Star-Forming
... V. X-ray Emission from Massive Stars X-ray emission detected from all OB stars earlier than B1. The brightest source is WR 93 Lx/Lbol~10-7 for the O stars Candidate O stars were found using X-ray luminosity, constant lightcurves, and near IR colors ...
... V. X-ray Emission from Massive Stars X-ray emission detected from all OB stars earlier than B1. The brightest source is WR 93 Lx/Lbol~10-7 for the O stars Candidate O stars were found using X-ray luminosity, constant lightcurves, and near IR colors ...
astro20 telescopes - Las Positas College
... almost all data is recorded on CCD’s (charge coupled devices) – silicon wafer with a two dimensional array of elements called pixels ...
... almost all data is recorded on CCD’s (charge coupled devices) – silicon wafer with a two dimensional array of elements called pixels ...
CHANDRA AUTOMATED POINT SOURCE PROCESSING FOR CALIBRATION MONITORING Chandra X-ray Center (CXC)
... (bright) sources are apparent with EE radii less than 2.3 arcsec. The curve fits a polynomial of the form, EE = 8e-5θ2-0.01θ+3.0. By filtering on time or energy we can detect shifts in this fit which indicate any mirror alignment problems. The Orion Nebula Cluster was observed for 1 million seconds ...
... (bright) sources are apparent with EE radii less than 2.3 arcsec. The curve fits a polynomial of the form, EE = 8e-5θ2-0.01θ+3.0. By filtering on time or energy we can detect shifts in this fit which indicate any mirror alignment problems. The Orion Nebula Cluster was observed for 1 million seconds ...
Review Game
... 16. List 4 advantages of the Hubble Space Telescope over ground-based telescopes. 17. Telescopes operating at this wavelength must be cooled to observe faint astronomical objects. 18. At which wavelength range is there no current or planned space observatory? 19. In what part of the electromagnetic ...
... 16. List 4 advantages of the Hubble Space Telescope over ground-based telescopes. 17. Telescopes operating at this wavelength must be cooled to observe faint astronomical objects. 18. At which wavelength range is there no current or planned space observatory? 19. In what part of the electromagnetic ...
Projet d`observation
... • X-ray: Space telescopes (due to atmospheric absorption) • Currently 5 operational missions: Rossi-XTE (‘95), Chandra (‘99), XMM• ...
... • X-ray: Space telescopes (due to atmospheric absorption) • Currently 5 operational missions: Rossi-XTE (‘95), Chandra (‘99), XMM• ...
Document
... 1. Why is it important that telescopes be large? 2. Why do most modern telescopes use a large mirror rather than a large lens? 3. Why are observatories in such remote locations? 4. Do astronomers use ordinary photographic film to take pictures of the sky? Do they actually look through large telescop ...
... 1. Why is it important that telescopes be large? 2. Why do most modern telescopes use a large mirror rather than a large lens? 3. Why are observatories in such remote locations? 4. Do astronomers use ordinary photographic film to take pictures of the sky? Do they actually look through large telescop ...
Light and Optical Systems - Topic 5 Practice Quiz
... Microscopes have limits in terms of their magnification because of the types of lenses that are used. To magnify objects by different amounts, scientists would use this part of the compound ...
... Microscopes have limits in terms of their magnification because of the types of lenses that are used. To magnify objects by different amounts, scientists would use this part of the compound ...
Lecture 3, Optical and UV Astronomy
... Wide-field CCD imager with near-UV to near-IR capabilities. High QE gave jump in sensitivity. Wide field channel has 3.4’ FOV and plate scale of 0.05” Wide Field Camera 3 (WFC3): WFC3 has two CCD arrays, one for UV/optical imaging (200-1000nm) with 2.7’ FOV and 0.04” pixels, and one for IR (800-1700 ...
... Wide-field CCD imager with near-UV to near-IR capabilities. High QE gave jump in sensitivity. Wide field channel has 3.4’ FOV and plate scale of 0.05” Wide Field Camera 3 (WFC3): WFC3 has two CCD arrays, one for UV/optical imaging (200-1000nm) with 2.7’ FOV and 0.04” pixels, and one for IR (800-1700 ...
The Orion 190-mm Maksutov-Newtonian
... but I found this to be simple and straightforward. The entire collimation process took about five minutes. The telescope is designed for use as an astrograph. This means the optical path from the primary mirror to the focuser is shorter than that of a normal telescope of the same focal length to all ...
... but I found this to be simple and straightforward. The entire collimation process took about five minutes. The telescope is designed for use as an astrograph. This means the optical path from the primary mirror to the focuser is shorter than that of a normal telescope of the same focal length to all ...
Document
... • Reasonably compact and portable up to focal lengths of 1000mm. • Excellent for faint deep sky objects such as remote galaxies, nebulae and star clusters. • Reasonably good for lunar and planetary work. • Low in optical aberrations. ...
... • Reasonably compact and portable up to focal lengths of 1000mm. • Excellent for faint deep sky objects such as remote galaxies, nebulae and star clusters. • Reasonably good for lunar and planetary work. • Low in optical aberrations. ...
Document
... The Faulkes Telescopes are large telescopes that can see far into space. There are two of them – one in Hawaii and one in Australia. These telescopes are named after a man called Bill Faulkes, who paid for these telescopes to be built. The telescopes are like robots, which can be controlled by peop ...
... The Faulkes Telescopes are large telescopes that can see far into space. There are two of them – one in Hawaii and one in Australia. These telescopes are named after a man called Bill Faulkes, who paid for these telescopes to be built. The telescopes are like robots, which can be controlled by peop ...
XMM-Newton
The XMM-Newton, also known as the X-ray Multi-Mirror Mission and the High Throughput X-ray Spectroscopy Mission, is an orbiting X-ray observatory launched by ESA in December 1999 on an Ariane 5 rocket. It is named in honor of Sir Isaac Newton. The telescope was placed in a very eccentric 48 hour elliptical orbit at 40°; at its apogee it is nearly 114,000 kilometres (71,000 mi) from Earth, while the perigee is only 7,000 kilometres (4,300 mi).