
Gravitational Wave Astronomy - Center for Gravitational Wave Physics
... Verify Source Identity Can we identify optical counterparts to LISA sources? ...
... Verify Source Identity Can we identify optical counterparts to LISA sources? ...
Red shift in spectra of galaxies
... in the ultraviolet area of the spectrum is determined by the radiation of hot stars of our Galaxy. Apparently, the higher temperature T of the star surface, the more photons in ultraviolet radiation it emits. However, the number of stars having this temperature sharply decreases with the growth of T ...
... in the ultraviolet area of the spectrum is determined by the radiation of hot stars of our Galaxy. Apparently, the higher temperature T of the star surface, the more photons in ultraviolet radiation it emits. However, the number of stars having this temperature sharply decreases with the growth of T ...
(and 4m) NGST - National Optical Astronomy Observatory
... mass dynamics within individual Galaxies • Local variations in starformation rate Multiple IFU spectroscopy R ~ 5,000 – 10,000 GSMT 3 hour, 3s limit at R=5,000 0.1”x0.1” IFU pixel (sub-kpc scale structures) ...
... mass dynamics within individual Galaxies • Local variations in starformation rate Multiple IFU spectroscopy R ~ 5,000 – 10,000 GSMT 3 hour, 3s limit at R=5,000 0.1”x0.1” IFU pixel (sub-kpc scale structures) ...
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... At the energies concerned, pair production is the dominant process for γ-ray absorption in matter. In satellite instruments the pair is directly observed (Fig. 8). In addition, a satellite detector can be furnished with an anti-coincidence shield to effectively discriminate against the dominant back ...
... At the energies concerned, pair production is the dominant process for γ-ray absorption in matter. In satellite instruments the pair is directly observed (Fig. 8). In addition, a satellite detector can be furnished with an anti-coincidence shield to effectively discriminate against the dominant back ...
XMM-Newton observatory-I. The spacecraft and operations
... 5. Science analysis software The software used to generate the products has been produced by the SSC and the XMM-Newton SOC, with the extensive support by the instrument hardware teams. It is run in a fixed configuration for the pipeline generation. However the complete set of tasks is bundled toget ...
... 5. Science analysis software The software used to generate the products has been produced by the SSC and the XMM-Newton SOC, with the extensive support by the instrument hardware teams. It is run in a fixed configuration for the pipeline generation. However the complete set of tasks is bundled toget ...
Nature template - PC Word 97
... from 2005.819 to 2005.831 during the first X-ray flare implies that acceleration of subTeV-energy electrons was particularly efficient at this time. These same electrons both produce X-rays from synchrotron radiation and scatter the X-ray photons to GeV -ray energies that are boosted to the TeV ran ...
... from 2005.819 to 2005.831 during the first X-ray flare implies that acceleration of subTeV-energy electrons was particularly efficient at this time. These same electrons both produce X-rays from synchrotron radiation and scatter the X-ray photons to GeV -ray energies that are boosted to the TeV ran ...
X-ray Binaries in Nearby Galaxies
... long-standing problem with distance estimates: very hard to study the X-ray luminosity function and spatial distribution other properties, e.g., orbital period, donor masses known only for a few systems ...
... long-standing problem with distance estimates: very hard to study the X-ray luminosity function and spatial distribution other properties, e.g., orbital period, donor masses known only for a few systems ...
ppt - chris.engelbrecht.nithep.ac.za
... 1E 0102.2-7219 (Figure 1) is an oxygen-rich supernova remnant in the Small Magellanic Cloud. X-ray observations reveal the blast wave andyield a shock radius of 22 arcseconds at the 60 kpc distance of the SMC. The spectrum of the blast wave yields a temperature of kTx 0.8 keV and an ionization tim ...
... 1E 0102.2-7219 (Figure 1) is an oxygen-rich supernova remnant in the Small Magellanic Cloud. X-ray observations reveal the blast wave andyield a shock radius of 22 arcseconds at the 60 kpc distance of the SMC. The spectrum of the blast wave yields a temperature of kTx 0.8 keV and an ionization tim ...
Probing the Earth`s interior with a large
... KamLAND has reported 152 events in the energy region relevant for geoneutrinos within a measuring time of 749 days and 3.5 × 1031 target protons. From these events 127 ± 13 are due to background [17]. The most relevant background for the KamLAND site are reactor antineutrinos (80.4 ± 7.2 events). Fo ...
... KamLAND has reported 152 events in the energy region relevant for geoneutrinos within a measuring time of 749 days and 3.5 × 1031 target protons. From these events 127 ± 13 are due to background [17]. The most relevant background for the KamLAND site are reactor antineutrinos (80.4 ± 7.2 events). Fo ...
Tod E. Strohmayer - UCLA Physics & Astronomy
... • Continuum spectroscopy; Lobs = 4pR2 s Teff4 = 4p d2 fobs • Eddington limited bursts; LEdd = 4pR2 s TEddeff4 = g(M, R) • For most likely rotation rates, line widths are rotationally dominated, measure line widths and can constrain R (if W known). • If detect several absorption lines in a series (Ha ...
... • Continuum spectroscopy; Lobs = 4pR2 s Teff4 = 4p d2 fobs • Eddington limited bursts; LEdd = 4pR2 s TEddeff4 = g(M, R) • For most likely rotation rates, line widths are rotationally dominated, measure line widths and can constrain R (if W known). • If detect several absorption lines in a series (Ha ...
Clusters of Galaxies
... Even More History" • X-ray emission from clusters of galaxies was not predicted and its discovery " was essentially serendipitous. " • The first detections of what we now know as cluster x-ray emission was from rocket flights in the 1960s (Friedman and Byram 1967, Bradt et al 1967) which discover ...
... Even More History" • X-ray emission from clusters of galaxies was not predicted and its discovery " was essentially serendipitous. " • The first detections of what we now know as cluster x-ray emission was from rocket flights in the 1960s (Friedman and Byram 1967, Bradt et al 1967) which discover ...
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... Au-edges (Nowak et al. 2011). For the back illuminated XIS1, the energy range in between the edges (1.88 keV–2.19 keV) was ignored as well because of significant discrepancies to the front-illuminated XIS0 and XIS3. The spectral channels of XIS were added such that a combined signal-to-noise ratio o ...
... Au-edges (Nowak et al. 2011). For the back illuminated XIS1, the energy range in between the edges (1.88 keV–2.19 keV) was ignored as well because of significant discrepancies to the front-illuminated XIS0 and XIS3. The spectral channels of XIS were added such that a combined signal-to-noise ratio o ...
3P29.pdf
... Almeria (Spain), with the Fibre Optics Cassegrain Echelle Spectrometer (FOCES) (Pfeiffer et al. 1998). During this observing run, a 2048x2048 pixel 150µ Site#1d15 CCD detector was used. The spectrograph set up was chosen to cover the Hα (6563 Å) and Ca II IRT (8498, 8542, 8662 Å) lines. The waveleng ...
... Almeria (Spain), with the Fibre Optics Cassegrain Echelle Spectrometer (FOCES) (Pfeiffer et al. 1998). During this observing run, a 2048x2048 pixel 150µ Site#1d15 CCD detector was used. The spectrograph set up was chosen to cover the Hα (6563 Å) and Ca II IRT (8498, 8542, 8662 Å) lines. The waveleng ...
DSSD and SSD Simulation with Silvaco
... • Very high instrumental background induced by Cosmic rays • Best sensitivity made by the COMPTEL instrument CGRO mission (1991 – 2000) COMPTEL instrument: two separate detectors • Scatterer • Calorimeter ...
... • Very high instrumental background induced by Cosmic rays • Best sensitivity made by the COMPTEL instrument CGRO mission (1991 – 2000) COMPTEL instrument: two separate detectors • Scatterer • Calorimeter ...
“Other ideas for gamma ray instruments” 1) Preserving the highest energies
... * More electron synchrotron cooling -> Compact object variability recovered at high energy -> Morphology%Energy relation as in HESS J1825-137 * Increased Hadron Larmor radius ->Morphology%Energy inverted compared to electron * More Klein Nishina suppression -> Hadron/Electron discrimination from spe ...
... * More electron synchrotron cooling -> Compact object variability recovered at high energy -> Morphology%Energy relation as in HESS J1825-137 * Increased Hadron Larmor radius ->Morphology%Energy inverted compared to electron * More Klein Nishina suppression -> Hadron/Electron discrimination from spe ...
05_LectureOutline
... • Refracting telescopes make images with a lens • Reflecting telescopes with a mirror • Modern research telescopes are all reflectors • CCDs are used for data collection ...
... • Refracting telescopes make images with a lens • Reflecting telescopes with a mirror • Modern research telescopes are all reflectors • CCDs are used for data collection ...
Bolometers evolution - Chalmers University of Technology
... wave region with polarization and variability data • Catalog of all-sky submm point sources at tens mJy level (high sensitivity limited by confusion and extraterrestrial background in its spectral minimum) • Photometric spectra (SED), and their variability, high redshift evaluations • Syunyaev-Zeldo ...
... wave region with polarization and variability data • Catalog of all-sky submm point sources at tens mJy level (high sensitivity limited by confusion and extraterrestrial background in its spectral minimum) • Photometric spectra (SED), and their variability, high redshift evaluations • Syunyaev-Zeldo ...
Searching for Quantum Gravity using Gamma Ray Bursts Frederick Kuehn
... ๏ It is possible that for one burst the high energy emission is systematically delayed which would cause a fake signal for that burst ๏ Most analyses use single (very bright) bursts, to make the measurements (e.g. astro-ph/0610571) ❖ Looking ...
... ๏ It is possible that for one burst the high energy emission is systematically delayed which would cause a fake signal for that burst ๏ Most analyses use single (very bright) bursts, to make the measurements (e.g. astro-ph/0610571) ❖ Looking ...
- Wiley Online Library
... The 511 keV positron annihilation line and the lower maximum energy are visible in the raw data (Figure S4 of the auxiliary material). [11] Table 1 lists the improvements in the fitting statistic, D (C‐Stat), from adding positrons to electrons‐only fits. We conducted simulations to demonstrate that ...
... The 511 keV positron annihilation line and the lower maximum energy are visible in the raw data (Figure S4 of the auxiliary material). [11] Table 1 lists the improvements in the fitting statistic, D (C‐Stat), from adding positrons to electrons‐only fits. We conducted simulations to demonstrate that ...
Earth`s Atmosphere & Telescopes
... light differently. (Mirrors can focus all colors equally well) • Generally reflectors are less expensive than refractors of similar size for these reasons. The World’s Largest Refractor. The 40 inch diameter telescope at Yerkes Observatory built in 1897. ...
... light differently. (Mirrors can focus all colors equally well) • Generally reflectors are less expensive than refractors of similar size for these reasons. The World’s Largest Refractor. The 40 inch diameter telescope at Yerkes Observatory built in 1897. ...
The Quest for Gamma Rays: Exploring the Most Violent Places in the
... • pion decay - Highly energetic protons that interact with matter produce particles called pions. Pions then decay to gamma rays. Cosmic rays, which are dominated by protons, permeate our galaxy, but we don’t know exactly where they originate. We expect the sources of cosmic rays to also produce gam ...
... • pion decay - Highly energetic protons that interact with matter produce particles called pions. Pions then decay to gamma rays. Cosmic rays, which are dominated by protons, permeate our galaxy, but we don’t know exactly where they originate. We expect the sources of cosmic rays to also produce gam ...
L95 IRON-RICH EJECTA IN THE SUPERNOVA
... original Raymond & Smith (1977) code (and subsequent revisions) that accurately models the overall flux of the Fe Lshell emission but is less accurate at modeling its detailed spectral variation with photon energy because of limitations in the availability of atomic data. This is the case to a great ...
... original Raymond & Smith (1977) code (and subsequent revisions) that accurately models the overall flux of the Fe Lshell emission but is less accurate at modeling its detailed spectral variation with photon energy because of limitations in the availability of atomic data. This is the case to a great ...
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.