Radeka_New_Directions_..._091506
... channel and the channel stops. The potentials among the channel, the channel stops and the window must be arranged so that the conduction path between the window and the channel stops is pinched-off , i.e., that the field lines from the window reach the buried channel and not the channel stops ...
... channel and the channel stops. The potentials among the channel, the channel stops and the window must be arranged so that the conduction path between the window and the channel stops is pinched-off , i.e., that the field lines from the window reach the buried channel and not the channel stops ...
AMUSE-Virgo Super-massive black holes vs. nuclear star clusters: the X-ray view
... Virgo Cluster Survey (ACSVCS, Cote’ et al mass range: 1E+8.5-1E+12 black hole mass range: 1E+5-1E+9 ...
... Virgo Cluster Survey (ACSVCS, Cote’ et al mass range: 1E+8.5-1E+12 black hole mass range: 1E+5-1E+9 ...
Multi-wavelength Astronomy Multi
... Gyro radiation is produced by electrons whose velocities are much smaller than the speed of light: v << c. Mildly relativistic electrons(kinetic energies comparable with rest mass c2) emit cyclotron radiation, and ultrarelativistic electrons (kinetic energies >> rest mass c2) produce synchrotron ...
... Gyro radiation is produced by electrons whose velocities are much smaller than the speed of light: v << c. Mildly relativistic electrons(kinetic energies comparable with rest mass c2) emit cyclotron radiation, and ultrarelativistic electrons (kinetic energies >> rest mass c2) produce synchrotron ...
7telescopes3s
... sensitive and easier to use than a plate, allows you to store and reduce data electronically Today, light is moved around with fiber optic cables and data is moved electronically ...
... sensitive and easier to use than a plate, allows you to store and reduce data electronically Today, light is moved around with fiber optic cables and data is moved electronically ...
X-ray output should be time variable
... Bright stars in the spectral range earlier than about B3 are soft X-ray sources, with LX ~ 10-7 LBol THEORY •O star X-ray emission comes from shock-heated gas present in their stellar winds; for B stars, the situation is more uncertain, and their Xrays may be related to magnetic fields, at least in ...
... Bright stars in the spectral range earlier than about B3 are soft X-ray sources, with LX ~ 10-7 LBol THEORY •O star X-ray emission comes from shock-heated gas present in their stellar winds; for B stars, the situation is more uncertain, and their Xrays may be related to magnetic fields, at least in ...
1 Kepler`s Third Law
... most energy. Low frequency (long wavelength) photons are the least energetic. The constant, h, is called Plank’s constant and once again its purpose is to scale the equation so that it agrees with our system of measurement. Example: Q: Which type of photon carries the most energy, ultraviolet photon ...
... most energy. Low frequency (long wavelength) photons are the least energetic. The constant, h, is called Plank’s constant and once again its purpose is to scale the equation so that it agrees with our system of measurement. Example: Q: Which type of photon carries the most energy, ultraviolet photon ...
X-rays - Astronomy at Swarthmore College
... Chandra observations of massive stars, indicating that a surprising variety of high-energy physical processes are occurring in this class of stars. •Normal massive stars with strong radiation-driven winds have x-ray emitting plasma distributed throughout their winds: Standard wind-shock models expla ...
... Chandra observations of massive stars, indicating that a surprising variety of high-energy physical processes are occurring in this class of stars. •Normal massive stars with strong radiation-driven winds have x-ray emitting plasma distributed throughout their winds: Standard wind-shock models expla ...
Highlights of the Poster Session - Indico
... the universe since the Big Bang. They are flashes of gamma rays coming from seemingly random places in deep space at random times. GRBs last from milliseconds to minutes, often followed by an afterglow emission at longer wavelengths (X-ray, UV, optical, IR, and radio). Gamma-ray bursts are detected ...
... the universe since the Big Bang. They are flashes of gamma rays coming from seemingly random places in deep space at random times. GRBs last from milliseconds to minutes, often followed by an afterglow emission at longer wavelengths (X-ray, UV, optical, IR, and radio). Gamma-ray bursts are detected ...
Astro 10-Lecture 5: Heat, Light and the Structure of Atoms
... – ROY G. BIV (red orange yellow green blue indigo violet in order low energy to high) – Wavelengths from 0.0004 millimeters to 0.0007 millimeters. Usually use nm (10-9 m or Å 10-10 m) ...
... – ROY G. BIV (red orange yellow green blue indigo violet in order low energy to high) – Wavelengths from 0.0004 millimeters to 0.0007 millimeters. Usually use nm (10-9 m or Å 10-10 m) ...
Instruments and Methods of Astrophysical X-ray
... From Bragg/Thomson to Photoelectric The turning point of X-Ray Astronomy was the launch of Einstein satellite that first introduced the X-ray Optics. The dramatic increase in sensitivity for the detection of faint sources and the capability to resolve extended source with imaging detectors in the f ...
... From Bragg/Thomson to Photoelectric The turning point of X-Ray Astronomy was the launch of Einstein satellite that first introduced the X-ray Optics. The dramatic increase in sensitivity for the detection of faint sources and the capability to resolve extended source with imaging detectors in the f ...
NASA`s Chandra Sees Brightest Supernova Ever
... the SN and galaxy nucleus, respectively. Panel b is a Gaussian-smoothed version of this image, in which the sources are more clearly apparent. Panel c is a maximum likelihood reconstruction of the 0.5–2 keV image (see text for details). Panel d shows the Chandra PSF at the location of the galaxy on ...
... the SN and galaxy nucleus, respectively. Panel b is a Gaussian-smoothed version of this image, in which the sources are more clearly apparent. Panel c is a maximum likelihood reconstruction of the 0.5–2 keV image (see text for details). Panel d shows the Chandra PSF at the location of the galaxy on ...
Circumstellar interaction of supernovae and gamma-ray bursts
... Gamma-ray burst They were discovered serendipitously in the late 1960s by U.S. military satellites which were on the look out for Soviet nuclear testing in violation of the atmospheric nuclear test ban treaty. These satellites carried gamma ray detectors since a nuclear explosion produces gamma ray ...
... Gamma-ray burst They were discovered serendipitously in the late 1960s by U.S. military satellites which were on the look out for Soviet nuclear testing in violation of the atmospheric nuclear test ban treaty. These satellites carried gamma ray detectors since a nuclear explosion produces gamma ray ...
Is an RFQ a good candidate for a next
... In any accelerator design there will be tradeoffs and choices must be made. • How much physics remains to be studied by low-voltage(<1 MV), low-current DC accelerators by the time this facility will be built? Will higher current accelerators be needed? • Although DE/E=10-4 is most desirable, would ...
... In any accelerator design there will be tradeoffs and choices must be made. • How much physics remains to be studied by low-voltage(<1 MV), low-current DC accelerators by the time this facility will be built? Will higher current accelerators be needed? • Although DE/E=10-4 is most desirable, would ...
LXO-Hardware
... Research joint funded by UK industry (E2V) and PPARC Application in this case was X-ray macromolecular crystallography 5.5 cm x 4.1 cm active area, 3.2M pixel, 27 µm, 2 MHz pixel readout, Device is 3-sides buttable ...
... Research joint funded by UK industry (E2V) and PPARC Application in this case was X-ray macromolecular crystallography 5.5 cm x 4.1 cm active area, 3.2M pixel, 27 µm, 2 MHz pixel readout, Device is 3-sides buttable ...
Photons
... HST/NICMOS, (2) HST/WFPC2, (3) Washington, (4) ESO/EMMI, (5) ESO/WFI U BVRIZ + ESO/SOFI JHK, and (6) Johnson-CousinsGlass. All references are given in Sect. 4. To allow a good visualisation of the filter curves, they have been re-normalized to their maximum value of S λ . For the sake of comparison, ...
... HST/NICMOS, (2) HST/WFPC2, (3) Washington, (4) ESO/EMMI, (5) ESO/WFI U BVRIZ + ESO/SOFI JHK, and (6) Johnson-CousinsGlass. All references are given in Sect. 4. To allow a good visualisation of the filter curves, they have been re-normalized to their maximum value of S λ . For the sake of comparison, ...
Supernovae
... • Thus a stalled shock wave is revived by neutrino heating. • Boundary at ~150 km: – inside → matter falls into core – outside → matter is expelled. ...
... • Thus a stalled shock wave is revived by neutrino heating. • Boundary at ~150 km: – inside → matter falls into core – outside → matter is expelled. ...
the effect of an soft X-ray source near the compact object in LS 5039
... In Y&T 2010, e± scattered off stellar photons → each flux modulates by the anisotropy of IC scattering In this study, they scatter off isotropic photons → emerging photons with GeV & keV have isotropic distribution → No modulation in GeV & X-ray band ...
... In Y&T 2010, e± scattered off stellar photons → each flux modulates by the anisotropy of IC scattering In this study, they scatter off isotropic photons → emerging photons with GeV & keV have isotropic distribution → No modulation in GeV & X-ray band ...
Review for Exam 2
... 4. You should be able to explain and/or describe the following: a. Ptolemy’s model of the solar system b. Copernicus’ model of the solar system c. Kepler’s model of the solar system d. Retrograde motion using Ptolemy’s model, and using the Copernican model 5. Be able to describe the contributions of ...
... 4. You should be able to explain and/or describe the following: a. Ptolemy’s model of the solar system b. Copernicus’ model of the solar system c. Kepler’s model of the solar system d. Retrograde motion using Ptolemy’s model, and using the Copernican model 5. Be able to describe the contributions of ...
Gamma-Ray Telescopes
... particles. In addition, all of the detectors are surrounded by thin plastic anti-coincidence scintillators which respond to charged particles. If the energy deposited in the upper and lower modules is measured, then the direction of the incident γ -ray can be determined to be within a narrow ring on ...
... particles. In addition, all of the detectors are surrounded by thin plastic anti-coincidence scintillators which respond to charged particles. If the energy deposited in the upper and lower modules is measured, then the direction of the incident γ -ray can be determined to be within a narrow ring on ...
1 1.1. The Facility and Experimental Setup
... the AXAF science community. Of these, 982 tests were done without transmission gratings, mostly for the calibration of the High Resolution Mirror Assembly (HRMA), or of the facility (such as background, beam uniformity, alignment to facility axis, etc.). The HRMA X-ray Detection System (HXDS) obtain ...
... the AXAF science community. Of these, 982 tests were done without transmission gratings, mostly for the calibration of the High Resolution Mirror Assembly (HRMA), or of the facility (such as background, beam uniformity, alignment to facility axis, etc.). The HRMA X-ray Detection System (HXDS) obtain ...
1 Introduction Chapter
... the AXAF science community. Of these, 982 tests were done without transmission gratings, mostly for the calibration of the High Resolution Mirror Assembly (HRMA), or of the facility (such as background, beam uniformity, alignment to facility axis, etc.). The HRMA X-ray Detection System (HXDS) obtain ...
... the AXAF science community. Of these, 982 tests were done without transmission gratings, mostly for the calibration of the High Resolution Mirror Assembly (HRMA), or of the facility (such as background, beam uniformity, alignment to facility axis, etc.). The HRMA X-ray Detection System (HXDS) obtain ...
regan-gas-10jul2010
... Nucleons (protons and neutrons ~10-15m) have a substructure, three quarks in each nucleon (‘ups’ and ‘downs’)…but they don’t exists on their ...
... Nucleons (protons and neutrons ~10-15m) have a substructure, three quarks in each nucleon (‘ups’ and ‘downs’)…but they don’t exists on their ...
1e 1048.1−5937, xte j1810−197 and 4u 0142+61
... The most critical aspect of this analysis is the identification of the transition responsible for the emission feature. We will assume that the same transition is responsible for the 13 keV feature in each source. Koning et al. (2013) were able to constrain the energy of the transition in both the K ...
... The most critical aspect of this analysis is the identification of the transition responsible for the emission feature. We will assume that the same transition is responsible for the 13 keV feature in each source. Koning et al. (2013) were able to constrain the energy of the transition in both the K ...
The Chandra Orion Ultradeep Project Eric Feigelson
... • COUP shows X-rays can efficiently irradiate protoplanetary disks (Fe fluorescent line & proplyd absorption). • X-rays dominate disk ionization and may alter disk structure, dynamics & chemistry. If MHD turbulence is induced, planet formation processes may be substantially affected. The X-ray data ...
... • COUP shows X-rays can efficiently irradiate protoplanetary disks (Fe fluorescent line & proplyd absorption). • X-rays dominate disk ionization and may alter disk structure, dynamics & chemistry. If MHD turbulence is induced, planet formation processes may be substantially affected. The X-ray data ...
A Proposed Collaboration Between LIGO
... detecting the corresponding gravitational wave (GW) emissions by the laser interferometer gravitational wave observatory, LIGO. GWs are extremely hard to detect because they are weak signals in a floor of instrument noise. Optical observations of CCSNe are already used in coincidence with LIGO data, ...
... detecting the corresponding gravitational wave (GW) emissions by the laser interferometer gravitational wave observatory, LIGO. GWs are extremely hard to detect because they are weak signals in a floor of instrument noise. Optical observations of CCSNe are already used in coincidence with LIGO data, ...
X-ray astronomy detector
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.