Development of Silicon Detectors
... Fast transfer of signals into the frame store Slow (low noise) read out from the frame store Out of time event probability: 0.2% (factor 30 lower than at XMM) ...
... Fast transfer of signals into the frame store Slow (low noise) read out from the frame store Out of time event probability: 0.2% (factor 30 lower than at XMM) ...
Cygnus X3 - IceCube Neutrino Observatory
... We have an interest in performing a general search which covers many orders of magnitude of flare duration to find occurrences undetected or undetectable with photon emission. We fit for the best mean and sigma of a Gaussian in time to find the strongest flare from a given source location. Here back ...
... We have an interest in performing a general search which covers many orders of magnitude of flare duration to find occurrences undetected or undetectable with photon emission. We fit for the best mean and sigma of a Gaussian in time to find the strongest flare from a given source location. Here back ...
Discovery of the optical counterpart to the X
... about 8 were bright enough in Hα to call our attention. The position of each one of these potential candidates with respect to the satellites error circle was then checked. Of these relatively strong Hα emitters only one lied inside the WFC BeppoSAX satellite position uncertainty circles (Fig.1). As ...
... about 8 were bright enough in Hα to call our attention. The position of each one of these potential candidates with respect to the satellites error circle was then checked. Of these relatively strong Hα emitters only one lied inside the WFC BeppoSAX satellite position uncertainty circles (Fig.1). As ...
Towards the pair spectroscopy of the Hoyle state in 12C
... spectrometer works and that the main source of the background is the high energy photons from the target itself. This is dominated by the 4.439 MeV E2 transition from the first excited state in 12 C. Using extensive simulations, a new absorber system has subsequently been designed. The shape of the ...
... spectrometer works and that the main source of the background is the high energy photons from the target itself. This is dominated by the 4.439 MeV E2 transition from the first excited state in 12 C. Using extensive simulations, a new absorber system has subsequently been designed. The shape of the ...
RIChilights
... Charged particles in turn emit Cherenkov light: – Blueish flash – ~2ns duration – ~1º aperture ...
... Charged particles in turn emit Cherenkov light: – Blueish flash – ~2ns duration – ~1º aperture ...
LOCALIZATION AND OBSERVATIONS OF GRB010921 BY THE …
... Early afterglows will be carefully studied the missing link between the prompt emission and the afterglow will be identified; The jet configuration will be identified universal structured jet model could be validated by future data; With accumulation of a large sample of spectral informati ...
... Early afterglows will be carefully studied the missing link between the prompt emission and the afterglow will be identified; The jet configuration will be identified universal structured jet model could be validated by future data; With accumulation of a large sample of spectral informati ...
The Electromagnetic Spectrum
... succeeded in combining the light from three small optical telescopes to produce a single, remarkably clear, image. Each telescope is only 0.4 m in diameter, but when the equipment is positioned 6 m apart, the resulting resolution is a stunning 0.01" ...
... succeeded in combining the light from three small optical telescopes to produce a single, remarkably clear, image. Each telescope is only 0.4 m in diameter, but when the equipment is positioned 6 m apart, the resulting resolution is a stunning 0.01" ...
Astronomy Astrophysics Astrophysical parameters and orbital solution of the peculiar X-ray
... covering a field of view (FOV) of 6◦ by 90◦ FWHM. Each SSC was sensitive in the energy range of approximately 1.5–12 keV, with on-axis effective areas of ∼10 cm2 , ∼30 cm2 , and ∼23 cm2 at 2, 5, and 10 keV, respectively. The ASM monitored the sky between January 1996 and December 2011. The ASM light ...
... covering a field of view (FOV) of 6◦ by 90◦ FWHM. Each SSC was sensitive in the energy range of approximately 1.5–12 keV, with on-axis effective areas of ∼10 cm2 , ∼30 cm2 , and ∼23 cm2 at 2, 5, and 10 keV, respectively. The ASM monitored the sky between January 1996 and December 2011. The ASM light ...
N Brickhouse
... Ne varies only slightly. • Variable Te means rt changes. • Assuming NH is from pre-shock gas, we can get path length
and thus the filling factor.
...
... Ne varies only slightly. • Variable Te means rt changes. • Assuming NH is from pre-shock gas, we can get path length
GLAST Proposal Review
... clear fiber light guides for long runs) – Two sets of fibers for each tile – Tiles overlap in one dimension – 8 scintillating fiber ribbons cover gaps in other dimension (not shown) – Supported on self-standing composite shell – Covered by thermal blanket + micrometeoroid shield (not shown) ...
... clear fiber light guides for long runs) – Two sets of fibers for each tile – Tiles overlap in one dimension – 8 scintillating fiber ribbons cover gaps in other dimension (not shown) – Supported on self-standing composite shell – Covered by thermal blanket + micrometeoroid shield (not shown) ...
CASA Concept for HROS - Thirty Meter Telescope
... This manuscript provides a broad overview of the CU-HROS concept. Additional details on elements of the design, in particular the fiber-fed IFUs and dichroics, are presented in a companion paper in this volume (Osterman et al. 2006) 1. HROS will be a multi-purpose high-resolution optical spectrograp ...
... This manuscript provides a broad overview of the CU-HROS concept. Additional details on elements of the design, in particular the fiber-fed IFUs and dichroics, are presented in a companion paper in this volume (Osterman et al. 2006) 1. HROS will be a multi-purpose high-resolution optical spectrograp ...
X-ray activity cycle on the active ultra
... gratings. These two reflection-grating spectrometers (RGS) provide high spectral resolution (E/ΔE ≈ 200–800) in the energy range 0.35–2.5 keV. Useful data were obtained from the EPIC and the RGS detectors (see Table 1 for a detailed account). AB Dor A, which is a very bright target with many emissio ...
... gratings. These two reflection-grating spectrometers (RGS) provide high spectral resolution (E/ΔE ≈ 200–800) in the energy range 0.35–2.5 keV. Useful data were obtained from the EPIC and the RGS detectors (see Table 1 for a detailed account). AB Dor A, which is a very bright target with many emissio ...
2 workshop on X-ray and XUV active optics
... ESRF Optical Metrology Applied to bent optical surfaces ...
... ESRF Optical Metrology Applied to bent optical surfaces ...
pasta Jos´e A. Pons , Daniele Vigan`o and Nanda Rea
... dissipation of the magnetic field, which in principle predicts that pulsars of longer periods (20100 s) should be visible. In models D and E, the slow release of magnetic energy through Joule heating keeps the neutron star bright and visible much longer than for models A, B and C. The luminosity of ...
... dissipation of the magnetic field, which in principle predicts that pulsars of longer periods (20100 s) should be visible. In models D and E, the slow release of magnetic energy through Joule heating keeps the neutron star bright and visible much longer than for models A, B and C. The luminosity of ...
Light: The Cosmic Messenger
... Radio Telescopes • A radio telescope is like a giant mirror that reflects radio waves to a focus ...
... Radio Telescopes • A radio telescope is like a giant mirror that reflects radio waves to a focus ...
NEW PARTICLES FROM NUCLEAR REACTIONS IN THE SUN Max
... for new particles. In particular reaction (3) gives monoenergetic particles (5.5 MeV) and being both M1 and E1 can couple to particles of various s p i n parity. Due to the frequent occurrence of (3) compared to any other reaction giving particles of comparable energy, the resulting simple " b o x " ...
... for new particles. In particular reaction (3) gives monoenergetic particles (5.5 MeV) and being both M1 and E1 can couple to particles of various s p i n parity. Due to the frequent occurrence of (3) compared to any other reaction giving particles of comparable energy, the resulting simple " b o x " ...
The PAMELA Space Experiment
... On the other side, when the two planets lie on different spiral lines the electron flux decreases. For PAMELA the minimum threshold energy for electron detection is 50 MeV. In this energy range, however, geomagnetic shielding will reduce the active observation time reducing total counts. Neverthele ...
... On the other side, when the two planets lie on different spiral lines the electron flux decreases. For PAMELA the minimum threshold energy for electron detection is 50 MeV. In this energy range, however, geomagnetic shielding will reduce the active observation time reducing total counts. Neverthele ...
Activity 6 The Electromagnetic Spectrum and Your Community
... In 1666, Isaac Newton found that he could split light into a spectrum of colors. As he passed a beam of sunlight through a glass prism, a spectrum of colors appeared from red to violet. Newton deduced that visible light was in fact a mixture of different kinds of light. About 10 years later, Christi ...
... In 1666, Isaac Newton found that he could split light into a spectrum of colors. As he passed a beam of sunlight through a glass prism, a spectrum of colors appeared from red to violet. Newton deduced that visible light was in fact a mixture of different kinds of light. About 10 years later, Christi ...
Bright Quasar 3C 273 Encyclopedia of Astronomy & Astrophysics eaa.iop.org Thierry J-L Courvoisier
... 3C 273 is clearly a very luminous object indeed. Its light output corresponds to 1014 times that of the Sun. Most quasars do not radiate substantially in the radio part of the electromagnetic spectrum, and are called radio quiet quasars. A small fraction, of which 3C 273 is a member, do, however. Th ...
... 3C 273 is clearly a very luminous object indeed. Its light output corresponds to 1014 times that of the Sun. Most quasars do not radiate substantially in the radio part of the electromagnetic spectrum, and are called radio quiet quasars. A small fraction, of which 3C 273 is a member, do, however. Th ...
the chandra deep field–north survey. xvii. evolution of
... stellar rotation from a magnetized stellar wind. Thirteen X-ray sources are associated with late-type stars; 11 of these constitute a well-defined sample for statistical analysis. This sample consists of two G, two K0–K4, and seven M2–M5 stars with median V-band magnitude around 19 and median distan ...
... stellar rotation from a magnetized stellar wind. Thirteen X-ray sources are associated with late-type stars; 11 of these constitute a well-defined sample for statistical analysis. This sample consists of two G, two K0–K4, and seven M2–M5 stars with median V-band magnitude around 19 and median distan ...
Cosmology: Black Holes, Dark Matter and Dark Energy
... of a beam of high-energy electrons with microwave photons. The high-energy beam is thought to have been produced by explosive activity related to gas swirling around a supermassive black hole. The length of the jet and the observed bright knots of X-ray emission suggest that the explosive activity i ...
... of a beam of high-energy electrons with microwave photons. The high-energy beam is thought to have been produced by explosive activity related to gas swirling around a supermassive black hole. The length of the jet and the observed bright knots of X-ray emission suggest that the explosive activity i ...
Space telescopes - International Space Science Institute
... between the three types is the ratio of focal length to total system length, i.e., the minimum physical length of the telescope. The focal length of a Type I system is practically given by the distance from the paraboloid/hyperboloid intersection plane to the system focus. Therefore the physical tel ...
... between the three types is the ratio of focal length to total system length, i.e., the minimum physical length of the telescope. The focal length of a Type I system is practically given by the distance from the paraboloid/hyperboloid intersection plane to the system focus. Therefore the physical tel ...
ms
... Gaussian probability distribution functions with the parameters discussed above. There are two other model parameters that are needed to convert the observables to a measurement of the neutron star mass and radius: the hydrogen mass fraction X in the atmosphere and the color correction factor fc . T ...
... Gaussian probability distribution functions with the parameters discussed above. There are two other model parameters that are needed to convert the observables to a measurement of the neutron star mass and radius: the hydrogen mass fraction X in the atmosphere and the color correction factor fc . T ...
The GMT Consortium Large Earth Finder Sagi Ben-Ami Smithsonian Astrophysical Observatory
... • The GMT is one of the three next generation optical telescope. • Segmented Gregorian design (six off axis and one on axis 8.4m mirrors) with an effective aperture of 25.4m diameter. • F/8.2 with a FoV of 24’. Plate Scale of 1’’ mm-1. • Site: Cerro Las Campanas in Chile’s Atacama desert. ...
... • The GMT is one of the three next generation optical telescope. • Segmented Gregorian design (six off axis and one on axis 8.4m mirrors) with an effective aperture of 25.4m diameter. • F/8.2 with a FoV of 24’. Plate Scale of 1’’ mm-1. • Site: Cerro Las Campanas in Chile’s Atacama desert. ...
Pulsars
... • In both cases, zero temperature energy – the Fermi energy, supports the star and prevents further collapse • From exclusion principle, each allowed energy state can be occupied by no more than two particles of opposite spin • Electrons in a White Dwarf occupy a small volume and have very well defi ...
... • In both cases, zero temperature energy – the Fermi energy, supports the star and prevents further collapse • From exclusion principle, each allowed energy state can be occupied by no more than two particles of opposite spin • Electrons in a White Dwarf occupy a small volume and have very well defi ...
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.