PoS(ICRC2015)707 - Proceeding of science
... which uses Geiger-mode Avalanche Photo Diodes (G-APDs) as photo sensors. It is located at the Observatorio del Roque de los Muchachos on the Canary Island of La Palma (Spain) and since October 2011 it observes very high energy gamma-ray sources in the Northern hemisphere by detecting air showers pro ...
... which uses Geiger-mode Avalanche Photo Diodes (G-APDs) as photo sensors. It is located at the Observatorio del Roque de los Muchachos on the Canary Island of La Palma (Spain) and since October 2011 it observes very high energy gamma-ray sources in the Northern hemisphere by detecting air showers pro ...
X-ray telescopes
... In 1948 Burnight discovered that the Sun emitted x-rays, and his results from exposing casettes of photographic film at the top of the Earth’s atmosphere on a V2 rocket flight ushered in the era of solar x-ray research. The first x-ray picture of the Sun was obtained in 1960 with a pinhole camera ex ...
... In 1948 Burnight discovered that the Sun emitted x-rays, and his results from exposing casettes of photographic film at the top of the Earth’s atmosphere on a V2 rocket flight ushered in the era of solar x-ray research. The first x-ray picture of the Sun was obtained in 1960 with a pinhole camera ex ...
English Summary
... However, since the central regions of an AGN are axisymmetric, orientation relative to the observer is also an important factor when classifying an AGN. The subpopulation of quasars that form radio jets are called radio-loud quasars. They contain a compact dust ring or torus around their black hole ...
... However, since the central regions of an AGN are axisymmetric, orientation relative to the observer is also an important factor when classifying an AGN. The subpopulation of quasars that form radio jets are called radio-loud quasars. They contain a compact dust ring or torus around their black hole ...
Absorption of high-energy gamma rays in Cygnus X-3
... in the optical depth for very-high energy (>100 GeV) gamma rays (Ford 1984; Protheroe & Stanev 1987; Moskalenko et al. 1993; Bednarek 2010). Some Wolf-Rayet stars present an excess in soft X-rays with luminosities up to ∼1033 erg s−1 , particularly in nitrogen-rich stars (e.g. Skinner et al. 2010). ...
... in the optical depth for very-high energy (>100 GeV) gamma rays (Ford 1984; Protheroe & Stanev 1987; Moskalenko et al. 1993; Bednarek 2010). Some Wolf-Rayet stars present an excess in soft X-rays with luminosities up to ∼1033 erg s−1 , particularly in nitrogen-rich stars (e.g. Skinner et al. 2010). ...
Poster
... wide wavelength range (0.6 - 5 mm) --> chromatic slit losses off-axis telescope and wide field of view --> significant distortion reflective optics (including dispersive elements) --> large, variable slit curvature multi-object spectrograph --> every detector pixel sees every wavelength ...
... wide wavelength range (0.6 - 5 mm) --> chromatic slit losses off-axis telescope and wide field of view --> significant distortion reflective optics (including dispersive elements) --> large, variable slit curvature multi-object spectrograph --> every detector pixel sees every wavelength ...
n,n - Osaka University
... interactions between the n’s and the nuclei in the collapsing region of the star. SN1987A confirmed that the collapse is low-entropy; the n’s took seconds to get out rather than the tens of 10 ms in which they’re produced.= 11 MeV, =16 MeV, and =
=25 MeV?? But the ne ...
... interactions between the n’s and the nuclei in the collapsing region of the star. SN1987A confirmed that the collapse is low-entropy; the n’s took seconds to get out rather than the tens of 10 ms in which they’re produced.
The Quadrupole Cusp: A Universal Accelerator, or From Radiation
... • Now that we know there are trapping regions of the cusp, e.g. periodic orbits, we can display those orbits with a Poincaré section. Then we can potentially demonstrate the invariant tori and chaotic orbits. • Unfortunately, I only realized the advantage of this approach after plotting 4000 traject ...
... • Now that we know there are trapping regions of the cusp, e.g. periodic orbits, we can display those orbits with a Poincaré section. Then we can potentially demonstrate the invariant tori and chaotic orbits. • Unfortunately, I only realized the advantage of this approach after plotting 4000 traject ...
THE SOLAR WIND INTERACTION WITH VENUS AND MARS
... on a line that makes an angle of 120◦ to the Mars-Sun line. The maximum flux is 4.6 · 107 . The image is in a polar format, with azimuth on the x-axis and elevation on the y-axis. The look direction is toward the center of Mars. The location of the brightest spot corresponds to the solar direction a ...
... on a line that makes an angle of 120◦ to the Mars-Sun line. The maximum flux is 4.6 · 107 . The image is in a polar format, with azimuth on the x-axis and elevation on the y-axis. The look direction is toward the center of Mars. The location of the brightest spot corresponds to the solar direction a ...
Beyond the Rainbow
... various parts of the electromagnetic spectrum, the variety of colors comprising visible light are made of waves that have different lengths between successive crests or troughs. Red waves are the longest, violet the shortest. William Herschel, the discoverer of Uranus, was the first to explore the r ...
... various parts of the electromagnetic spectrum, the variety of colors comprising visible light are made of waves that have different lengths between successive crests or troughs. Red waves are the longest, violet the shortest. William Herschel, the discoverer of Uranus, was the first to explore the r ...
Document
... Future space-based observatories in the 10 - 40 micron spectral regime will be passively cooled to about 30 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 so ...
... Future space-based observatories in the 10 - 40 micron spectral regime will be passively cooled to about 30 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 so ...
Fake Source Experiment for Chandra ACIS Observations
... Fig. 5 Source number count (cumulative log (N)-log(S)) plot of a sample run of XFAKE. Events of fake sources are added on a scaled blank sky event image. Input source list is generated by assuming power-law log(N)-log(S) (power index=1, green line) and fake sources are randomly distributed. Input fa ...
... Fig. 5 Source number count (cumulative log (N)-log(S)) plot of a sample run of XFAKE. Events of fake sources are added on a scaled blank sky event image. Input source list is generated by assuming power-law log(N)-log(S) (power index=1, green line) and fake sources are randomly distributed. Input fa ...
Ionizing particle fluxes in the near
... shows that the results at various sites of measurements coincide with each other within the error bars and do not contradict the value obtained at the ground with account of barometric effect [7]. Ratio of count rates of an omnidirectional counter and a telescope k depends on particle composition an ...
... shows that the results at various sites of measurements coincide with each other within the error bars and do not contradict the value obtained at the ground with account of barometric effect [7]. Ratio of count rates of an omnidirectional counter and a telescope k depends on particle composition an ...
First Results Using the Medipix2 Photon Counting ASIC as Readout
... 256 x 256 pixels sensitive to positive or negative input charge (free choice of different detector materials) pixel-by-pixel detector leakage current compensation window in energy discriminators designed to be linear over a large range 13-bit counter per pixel count rate: ~1 MHz/pixel (0.33 G ...
... 256 x 256 pixels sensitive to positive or negative input charge (free choice of different detector materials) pixel-by-pixel detector leakage current compensation window in energy discriminators designed to be linear over a large range 13-bit counter per pixel count rate: ~1 MHz/pixel (0.33 G ...
Chapter 2 Observing the Electromagnetic Spectrum
... exposure, 30 ′′ across. Credit: A. Mattingly, Grove Creek Observatory. the entire electromagnetic region, they too are sources of increasing ’pollution’ for ground-based observations, when recorded as streaks of light across long exposure wide-field images near to, or through (Figure 2.3) objects of ...
... exposure, 30 ′′ across. Credit: A. Mattingly, Grove Creek Observatory. the entire electromagnetic region, they too are sources of increasing ’pollution’ for ground-based observations, when recorded as streaks of light across long exposure wide-field images near to, or through (Figure 2.3) objects of ...
X-Ray and Extreme Ultraviolet Emission from Comets
... black holes. As electromagnetic radiation with wavelength λ between about 0.01 nm and 100 nm (1 nm = 10 –9 m), extreme ultraviolet (EUV) and X-ray radiation are important for solar system and astrophysical applications because the photons are sufficiently energetic and penetrating to ionize neutral ...
... black holes. As electromagnetic radiation with wavelength λ between about 0.01 nm and 100 nm (1 nm = 10 –9 m), extreme ultraviolet (EUV) and X-ray radiation are important for solar system and astrophysical applications because the photons are sufficiently energetic and penetrating to ionize neutral ...
as Word doc - Virtual Observatory
... WorldWide Telescope has the concept of a study and a survey: Study – is usually a single or composite image of one object in space. Survey – is usually a comprehensive collection of data from a large area of the sky. A study is loaded from a “Collection” by clicking a thumbnail in the top panel. ...
... WorldWide Telescope has the concept of a study and a survey: Study – is usually a single or composite image of one object in space. Survey – is usually a comprehensive collection of data from a large area of the sky. A study is loaded from a “Collection” by clicking a thumbnail in the top panel. ...
WorldWide Telescope: Sky Mode
... WorldWide Telescope has the concept of a study and a survey: • Study – is usually a single or composite image of one object in space. • Survey – is usually a comprehensive collection of data from a large area of the sky. A study is loaded from a “Collection” by clicking a thumbnail in the top panel. ...
... WorldWide Telescope has the concept of a study and a survey: • Study – is usually a single or composite image of one object in space. • Survey – is usually a comprehensive collection of data from a large area of the sky. A study is loaded from a “Collection” by clicking a thumbnail in the top panel. ...
MAGIC-II - (CTA) Japan
... Atmospheric monitoring, associated science & instrument calib. Observatory operation and access Data handling, data processing, data management and access Risk assessment and quality assurance, production planning ...
... Atmospheric monitoring, associated science & instrument calib. Observatory operation and access Data handling, data processing, data management and access Risk assessment and quality assurance, production planning ...
LENA
... • SuperKamiokande has 170 background events in 1489 days (efficiency 33% ) •In LENA, this would scale down to a background of ~ 5 / y and after PSD-analysis this could be suppressed in LENA to ~ 0.25 / y ! (efficiency ~ 70% ) •A 30 kt detector (~ 1034 protons as target) would have a sensitivity of ...
... • SuperKamiokande has 170 background events in 1489 days (efficiency 33% ) •In LENA, this would scale down to a background of ~ 5 / y and after PSD-analysis this could be suppressed in LENA to ~ 0.25 / y ! (efficiency ~ 70% ) •A 30 kt detector (~ 1034 protons as target) would have a sensitivity of ...
Hard X-Ray Polarization – a Diagnostic of Electron
... Three pairs of detectors with similar background : detectors 8/9, detectors 3/5 and detectors 4/6. The data from detectors 3-6 can be used as background estimate for the polarimeter mode detectors 8/9. ...
... Three pairs of detectors with similar background : detectors 8/9, detectors 3/5 and detectors 4/6. The data from detectors 3-6 can be used as background estimate for the polarimeter mode detectors 8/9. ...
MICROQUASARS - Osservatorio Astronomico di Roma-INAF
... Sgr A*, LINERs, FR I & BL Lac are analogous to ...
... Sgr A*, LINERs, FR I & BL Lac are analogous to ...
Chapter 20: Radiant Energy from the Sun
... The Electromagnetic Spectrum While all electromagnetic waves travel at the same speed in a vacuum, they may differ in wavelength and frequency. The electromagnetic spectrum can be divided into regions according to wavelength or frequency. These regions are named radio waves, microwaves, infrared rad ...
... The Electromagnetic Spectrum While all electromagnetic waves travel at the same speed in a vacuum, they may differ in wavelength and frequency. The electromagnetic spectrum can be divided into regions according to wavelength or frequency. These regions are named radio waves, microwaves, infrared rad ...
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.