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Electromagnetic Spectrum - Introduction
... We may think that radio waves are completely different physical objects or events than gamma-rays. They are produced in very different ways, and we detect them in different ways. But are they really different things? The answer is 'no'. Radio waves, visible light, X-rays, and all the other parts of ...
... We may think that radio waves are completely different physical objects or events than gamma-rays. They are produced in very different ways, and we detect them in different ways. But are they really different things? The answer is 'no'. Radio waves, visible light, X-rays, and all the other parts of ...
detectors in missions for Aull
... Gamma Ray Detection Airshowers • It is possible to detect gamma rays by the presence of their byproducts produced in Earth’s atmosphere. • Ground-based gamma ray telescopes actually detect Cherenkov radiation emitted by high energy particles produced through the interaction of the gamma rays and at ...
... Gamma Ray Detection Airshowers • It is possible to detect gamma rays by the presence of their byproducts produced in Earth’s atmosphere. • Ground-based gamma ray telescopes actually detect Cherenkov radiation emitted by high energy particles produced through the interaction of the gamma rays and at ...
Diffuse TeV Emission from the Galactic Center
... Intensity assuming Sagittarius A* as source of relativistic protons matched to intensity range of HESS (Wommer et al. 2008) ...
... Intensity assuming Sagittarius A* as source of relativistic protons matched to intensity range of HESS (Wommer et al. 2008) ...
X-ray and UV Transients
... • If we scale the GALEX area by ~103, we can expect >10 events y-1 even if the sensitivity is 102 less. • The observed signals have UV flux~host, so confusion with (even mildly) variable sources is an issue unless additional information is available • A combined UV survey+optical SN survey like PTF ...
... • If we scale the GALEX area by ~103, we can expect >10 events y-1 even if the sensitivity is 102 less. • The observed signals have UV flux~host, so confusion with (even mildly) variable sources is an issue unless additional information is available • A combined UV survey+optical SN survey like PTF ...
Gamma Rays - Ohio University Physics and Astronomy
... D) Coded Masks Coded mask casts a shadow pattern on the detector, which can be unfolded to calculate the distribution of sources in the field of view. ...
... D) Coded Masks Coded mask casts a shadow pattern on the detector, which can be unfolded to calculate the distribution of sources in the field of view. ...
Science 8: Unit C: Light and Optical Systems
... • Stars and galaxies which produce light radiation also produce a wide spectrum of waves which are invisible to our eyes. Everything from radio waves with 1-2 km in wavelength to high energy gamma rays. ...
... • Stars and galaxies which produce light radiation also produce a wide spectrum of waves which are invisible to our eyes. Everything from radio waves with 1-2 km in wavelength to high energy gamma rays. ...
Dublin - University of Warwick
... Signatures of merging BHs (disruption rates 1 per decade) Possible accelerators of ultra-high energy cosmic rays ...
... Signatures of merging BHs (disruption rates 1 per decade) Possible accelerators of ultra-high energy cosmic rays ...
Homework #3 Chapter 2: Light and Motion Due
... Normally, the number of electrons in an atom equals the number of protons in the nucleus, and the electrons are in their lowest energy level, the "ground state." When an atom is excited, an electron absorbs energy from an outside source and moves to a higher energy orbital. The precisely defined ene ...
... Normally, the number of electrons in an atom equals the number of protons in the nucleus, and the electrons are in their lowest energy level, the "ground state." When an atom is excited, an electron absorbs energy from an outside source and moves to a higher energy orbital. The precisely defined ene ...
The X-ray/hard X-ray/gamma-ray connection of gamma
... hard X-ray emission expected if it is non-accreting. ...
... hard X-ray emission expected if it is non-accreting. ...
Copyright 2004 Society of Photo-Optical Instrumentation Engineers. This
... • SSD Icing Effect: Because SSD was cooled to the liquid nitrogen temperature, even in its vacuum container, there was still a small amount of trapped water which condensed on the surface of the SSD to form a very thin layer of ice. This thin ice layer decreases the transmission of low energy X-rays ...
... • SSD Icing Effect: Because SSD was cooled to the liquid nitrogen temperature, even in its vacuum container, there was still a small amount of trapped water which condensed on the surface of the SSD to form a very thin layer of ice. This thin ice layer decreases the transmission of low energy X-rays ...
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... due to a very wide X-ray eclipse In the hard X-ray range (18-60 keV) the eclipse form and width are very variable. ...
... due to a very wide X-ray eclipse In the hard X-ray range (18-60 keV) the eclipse form and width are very variable. ...
Document
... – Monitor FOV of 8 sr (shall overlap that of the LAT) – Notify observers world-wide: • Recognize bursts in realtime • Determine burst positions to few degree accuracy • Transmit (within seconds) GRB coordinates to the ground • Re-point the main instrument to GRB positions within 10 minutes ...
... – Monitor FOV of 8 sr (shall overlap that of the LAT) – Notify observers world-wide: • Recognize bursts in realtime • Determine burst positions to few degree accuracy • Transmit (within seconds) GRB coordinates to the ground • Re-point the main instrument to GRB positions within 10 minutes ...
ppt
... Roberto Soria & Kinwah Wu (MSSL/UCL) M83 is a barred spiral galaxy with a starburst nucleus, located in the Centaurus A group, at a distance of 3.7 Mpc. It was observed by Chandra in 2000 April. About 55% of the total emission in the nuclear region is unresolved. About 80% of the unresolved nuclear ...
... Roberto Soria & Kinwah Wu (MSSL/UCL) M83 is a barred spiral galaxy with a starburst nucleus, located in the Centaurus A group, at a distance of 3.7 Mpc. It was observed by Chandra in 2000 April. About 55% of the total emission in the nuclear region is unresolved. About 80% of the unresolved nuclear ...
High Energy Processes in Young Stellar Objects
... Magnetic loop with both feet in the disk Binary YSOs but less important Reconnection and displacement of footprint are more likely to occur in YSOs due to more possible magnetic configuration offered by star-star, star-disk, disk-disk interaction ...
... Magnetic loop with both feet in the disk Binary YSOs but less important Reconnection and displacement of footprint are more likely to occur in YSOs due to more possible magnetic configuration offered by star-star, star-disk, disk-disk interaction ...
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... • CMOS = Complementary Metal Oxide Semiconductor; it’s a process, not a particular device ...
... • CMOS = Complementary Metal Oxide Semiconductor; it’s a process, not a particular device ...
The Ultraluminous X-ray Source in Holmberg IX and its Environment
... The two main hypotheses to explain the high luminosity of ULXs are intermediate mass black holes (IMBHs) having 102 to 105 solar masses (Colbert & Mushotzky 1999) or non-isotropic emission beamed into our line-of-sight (King et al. 2001). Here, we are interested in one of these objects, Holmberg IX ...
... The two main hypotheses to explain the high luminosity of ULXs are intermediate mass black holes (IMBHs) having 102 to 105 solar masses (Colbert & Mushotzky 1999) or non-isotropic emission beamed into our line-of-sight (King et al. 2001). Here, we are interested in one of these objects, Holmberg IX ...
Gamma-Ray Astroparticle Physics
... A second array, the Michigan Anti Mu (MIA), is made of 2500 square meters of buried counters in 16 patches. MIA measures the muon content of the showers, which allows to reject > 90% of the events as hadronic background ...
... A second array, the Michigan Anti Mu (MIA), is made of 2500 square meters of buried counters in 16 patches. MIA measures the muon content of the showers, which allows to reject > 90% of the events as hadronic background ...
Lecture 16, AGN Evolution
... Accretion History of the Universe We can now infer the present-day supermassive black hole mass density accreted by AGN and compare it with the ...
... Accretion History of the Universe We can now infer the present-day supermassive black hole mass density accreted by AGN and compare it with the ...
High Energy Astrophysics and Transient Science (or, a tale of radio
... LOFAR observation cycle zero starts in January, over one quarter of all observing time is transient searches – whatever the LOFAR transient is, we should find 10s – 100s of them.. ...
... LOFAR observation cycle zero starts in January, over one quarter of all observing time is transient searches – whatever the LOFAR transient is, we should find 10s – 100s of them.. ...
Who’s Afraid of a Stellar Superflare? Rachel Osten GSFC
... in globular clusters, super-bolometric X-ray luminosities superflaring in normal stars -- Schaefer et al. (2000) normal solar-like stars undergoing flaring events with energy releases 1033-1038 ergs, occurring roughly once every 100 years or so ...
... in globular clusters, super-bolometric X-ray luminosities superflaring in normal stars -- Schaefer et al. (2000) normal solar-like stars undergoing flaring events with energy releases 1033-1038 ergs, occurring roughly once every 100 years or so ...
PowerPoint - Chandra X
... Reference: H. Marshall et al “A High Resolution X-ray Image of the Jet in M87”, http://xxx.lanl.gov/abs/astro-ph/0109160 Scale: 25 arcsec along the jet ...
... Reference: H. Marshall et al “A High Resolution X-ray Image of the Jet in M87”, http://xxx.lanl.gov/abs/astro-ph/0109160 Scale: 25 arcsec along the jet ...
Discovering X-ray Bright Neutron Stars for Current and Next-Generation
... platform for many-target surveys (Fox 04) • Rapid slewing give high duty cycle for short observations (c.f. Chandra, XMM) • Multiple targets per orbit • X-ray telescope – Better PSF than ROSAT PSPC – Similar sensitivity – Detect BSC sources in < 1 ksec ...
... platform for many-target surveys (Fox 04) • Rapid slewing give high duty cycle for short observations (c.f. Chandra, XMM) • Multiple targets per orbit • X-ray telescope – Better PSF than ROSAT PSPC – Similar sensitivity – Detect BSC sources in < 1 ksec ...
X-ray astronomy detector
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X-ray astronomy detectors are instruments that detect X-rays for use in the study of X-ray astronomy.X-ray astronomy is an observational branch of astronomy which deals with the study of X-ray emission from celestial objects. X-radiation is absorbed by the Earth's atmosphere, so instruments to detect X-rays must be taken to high altitude by balloons, sounding rockets, and satellites. X-ray astronomy is part of space science.X-ray astronomy detectors have been designed and configured primarily for energy and occasionally for wavelength detection using a variety of techniques usually limited to the technology of the time.