$doc.title
... main drawback of stacking analysis is that we can’t easily measure the scatter -> need to assume one ...
... main drawback of stacking analysis is that we can’t easily measure the scatter -> need to assume one ...
Chapter 24: Studying the Stars
... • Refracting telescope – use lenses to refract or bend light • First used by Galileo • Mostly smaller telescopes • The objective lens produces an image by bending light from distant objects so that light converges on a focus (central point) ...
... • Refracting telescope – use lenses to refract or bend light • First used by Galileo • Mostly smaller telescopes • The objective lens produces an image by bending light from distant objects so that light converges on a focus (central point) ...
Document
... K. They will make use of large, sensitive detector arrays with low-power dissipation array readout electronics. Improvements in sensitivity, stability, array size, and power consumption are sought. In particular, novel doping approaches to extend wavelength response, lower dark current and readout n ...
... K. They will make use of large, sensitive detector arrays with low-power dissipation array readout electronics. Improvements in sensitivity, stability, array size, and power consumption are sought. In particular, novel doping approaches to extend wavelength response, lower dark current and readout n ...
File
... – Radio Telescopes study radio waves from earth. – Space Telescopes travel out of Earth’s atmosphere to study the other types of radiation not visible to the naked eye, and the radiation that cannot make it through earth’s protective atmosphere. ...
... – Radio Telescopes study radio waves from earth. – Space Telescopes travel out of Earth’s atmosphere to study the other types of radiation not visible to the naked eye, and the radiation that cannot make it through earth’s protective atmosphere. ...
Document
... The Objective is the main light-gathering apparatus of the telescope. Our telescope has an 8” diameter mirror for its objective. ...
... The Objective is the main light-gathering apparatus of the telescope. Our telescope has an 8” diameter mirror for its objective. ...
radio telescope
... Detecting Invisible Radiation Advantages of Radio Telescopes • Radio telescopes are much less affected by turbulence in the atmosphere, clouds, and the weather. • No protective dome is required, which reduces the cost of construction. • Radio telescopes can “see” through interstellar dust clouds t ...
... Detecting Invisible Radiation Advantages of Radio Telescopes • Radio telescopes are much less affected by turbulence in the atmosphere, clouds, and the weather. • No protective dome is required, which reduces the cost of construction. • Radio telescopes can “see” through interstellar dust clouds t ...
radio telescope
... Detecting Invisible Radiation Advantages of Radio Telescopes • Radio telescopes are much less affected by turbulence in the atmosphere, clouds, and the weather. • No protective dome is required, which reduces the cost of construction. • Radio telescopes can “see” through interstellar dust clouds t ...
... Detecting Invisible Radiation Advantages of Radio Telescopes • Radio telescopes are much less affected by turbulence in the atmosphere, clouds, and the weather. • No protective dome is required, which reduces the cost of construction. • Radio telescopes can “see” through interstellar dust clouds t ...
Topic 4 Assignment - Science 9 Portfolio
... ground-based astronomical telescope by counteracting the effects of the atmosphere on the image. A deforming mirror in the light path of the telescope maintains a pointlike image of the celestial body using either a real star or a laser beam as a reference. Triangulation- the process of determining ...
... ground-based astronomical telescope by counteracting the effects of the atmosphere on the image. A deforming mirror in the light path of the telescope maintains a pointlike image of the celestial body using either a real star or a laser beam as a reference. Triangulation- the process of determining ...
Chapter 19
... Light and other forms of radiation carry information about space Electromagnetic radiation travels in all directions in certain types of waves Scientists interpret these waves to learn ...
... Light and other forms of radiation carry information about space Electromagnetic radiation travels in all directions in certain types of waves Scientists interpret these waves to learn ...
Hubble Space Telescope - University of Southern California
... • Instruments: The Wide Field Planetary Camera (JPL) consists of four cameras that are used for general astronomical observations from far-UV to near-IR. The Faint Object Camera (ESA) uses cumulative exposures to study faint objects. The Faint Object Spectrograph (FOS) is used to analyze the propert ...
... • Instruments: The Wide Field Planetary Camera (JPL) consists of four cameras that are used for general astronomical observations from far-UV to near-IR. The Faint Object Camera (ESA) uses cumulative exposures to study faint objects. The Faint Object Spectrograph (FOS) is used to analyze the propert ...
Slide 1
... to noise (SNR) ratio of 105:1 by combining a series of images of a target star over an extended integration time. – This is the SNR required to definitively observe an exo-planet transit in front of its parent star. – The target star will be between 0 and 4th magnitude ...
... to noise (SNR) ratio of 105:1 by combining a series of images of a target star over an extended integration time. – This is the SNR required to definitively observe an exo-planet transit in front of its parent star. – The target star will be between 0 and 4th magnitude ...
pptx
... dishes with a total collecting area of 1 km2 and a baseline of 3000 km. It will be built in Australia and Africa and will be 100 times more sensitive than the VLA. ...
... dishes with a total collecting area of 1 km2 and a baseline of 3000 km. It will be built in Australia and Africa and will be 100 times more sensitive than the VLA. ...
Foundation 1 - Discovering Astronomy
... Advanced technology is spawning a new generation of equipment to view the universe • CCDs (charge-coupled devices) • Large telescopes on remote mountain tops – Mauna Kea in Hawaii – Cerro Pachon in Chile ...
... Advanced technology is spawning a new generation of equipment to view the universe • CCDs (charge-coupled devices) • Large telescopes on remote mountain tops – Mauna Kea in Hawaii – Cerro Pachon in Chile ...
Part F
... ROSAT (1990-1999) the ROentgen SATellite, was an X-ray observatory designed to make an all-sky survey in soft x-rays (0.1 keV-2 keV). Its sensitivity to X-rays was over 1000 times greater than Uhuru. The X-ray mirror assembly was a grazing incidence four-fold nested Wolter I telescope with an 84 cm ...
... ROSAT (1990-1999) the ROentgen SATellite, was an X-ray observatory designed to make an all-sky survey in soft x-rays (0.1 keV-2 keV). Its sensitivity to X-rays was over 1000 times greater than Uhuru. The X-ray mirror assembly was a grazing incidence four-fold nested Wolter I telescope with an 84 cm ...
Science 9 Unit 5: Space Name:
... The technique of using a number of telescopes in combination is called interferometry. When working together, these telescopes can detect objects in space with better clarity and at greater distances than any current Earth-based observatory. The Hubble Space Telescope ( HST ) The HST makes one com ...
... The technique of using a number of telescopes in combination is called interferometry. When working together, these telescopes can detect objects in space with better clarity and at greater distances than any current Earth-based observatory. The Hubble Space Telescope ( HST ) The HST makes one com ...
Document
... UV and EUV Imaging mirrors with simultaneously large aperture (1-4 m diameter), low mass (520 kg/m2), accurate figure (~0.01 wave rms or better at 632 nm), and low micro-roughness (<1 nm @ <1 mm period). Figure accuracy must be maintained through launch and on-orbit (including, for mirrors subjected ...
... UV and EUV Imaging mirrors with simultaneously large aperture (1-4 m diameter), low mass (520 kg/m2), accurate figure (~0.01 wave rms or better at 632 nm), and low micro-roughness (<1 nm @ <1 mm period). Figure accuracy must be maintained through launch and on-orbit (including, for mirrors subjected ...
“Other ideas for gamma ray instruments” 1) Preserving the highest energies
... * More Klein Nishina suppression -> Hadron/Electron discrimination from spectral profiles * 100TeV gamma from knee energy CR -> Chance to address the origin of the knee (CR acceleration and propagat.) * >10TeV gamma ray astronomy = higher angular resolution ...
... * More Klein Nishina suppression -> Hadron/Electron discrimination from spectral profiles * 100TeV gamma from knee energy CR -> Chance to address the origin of the knee (CR acceleration and propagat.) * >10TeV gamma ray astronomy = higher angular resolution ...
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).