Critical-Angle Transmission Gratings for High Resolution, Large Area Soft X-Ray Spectroscopy
... ΔE) and resolving power (large R = λ/Δλ). The x-ray band of interest for these science objectives extends over more than two orders of magnitude in energy. High quality spectroscopy over such a large band cannot be obtained with a single instrument. For example, imaging spectroscopy with a spectral ...
... ΔE) and resolving power (large R = λ/Δλ). The x-ray band of interest for these science objectives extends over more than two orders of magnitude in energy. High quality spectroscopy over such a large band cannot be obtained with a single instrument. For example, imaging spectroscopy with a spectral ...
GRB prompt emission
... – compare with equipartition Most energy estimates require knowledge of the geometry of the outflow – radius and cross check with ISS-derived radius ...
... – compare with equipartition Most energy estimates require knowledge of the geometry of the outflow – radius and cross check with ISS-derived radius ...
GRB prompt emission
... – compare with equipartition Most energy estimates require knowledge of the geometry of the outflow – radius and cross check with ISS-derived radius ...
... – compare with equipartition Most energy estimates require knowledge of the geometry of the outflow – radius and cross check with ISS-derived radius ...
Five Years of Swift Science: GRBs and More!
... – A very large field of view for finding GRBs & quasars • BREADTH versus Depth for rare objects (Critical) ...
... – A very large field of view for finding GRBs & quasars • BREADTH versus Depth for rare objects (Critical) ...
PDF only - at www.arxiv.org.
... equipartition. If the filaments are falling, then g should be replaced by the tidal acceleration, which is smaller by l/R, reducing Br by a factor of 2, comparable with the equipartition value. Note that the required magnetic field is inversely proportional to the radius of the filamentary threads w ...
... equipartition. If the filaments are falling, then g should be replaced by the tidal acceleration, which is smaller by l/R, reducing Br by a factor of 2, comparable with the equipartition value. Note that the required magnetic field is inversely proportional to the radius of the filamentary threads w ...
Wavelength calibration from 1 − 5µ m for the CRIRES+ high
... and modelling of the atmospheric conditions, based on simultaneously measured sounding data, is required, as eg. high-altitude winds induce significant uncertainties (≤ 25m/s) on the line positions.8 Telluric molecules such as CO2 can be used with CRIRES and have demonstrated radial velocity precisi ...
... and modelling of the atmospheric conditions, based on simultaneously measured sounding data, is required, as eg. high-altitude winds induce significant uncertainties (≤ 25m/s) on the line positions.8 Telluric molecules such as CO2 can be used with CRIRES and have demonstrated radial velocity precisi ...
Gamma-Ray Line Emission from Radioactive Isotopes in Stars and
... and difficulties. We discuss their nature briefly, addressing a few of the physical aspects involved. The treatment of convection, and its implications, constitute one problem area common to several source types. The convective coupling between mass zones in both the oxygen-neon and hydrogen shell-b ...
... and difficulties. We discuss their nature briefly, addressing a few of the physical aspects involved. The treatment of convection, and its implications, constitute one problem area common to several source types. The convective coupling between mass zones in both the oxygen-neon and hydrogen shell-b ...
The fuelling of local supermassive black holes
... Thanks to Chandra (=highest angular resolution ever), a few of these questions can be addressed [ both the hot ISM and the nuclear emission show up in the X-ray band ]. ...
... Thanks to Chandra (=highest angular resolution ever), a few of these questions can be addressed [ both the hot ISM and the nuclear emission show up in the X-ray band ]. ...
The Historical X-ray Transient KY TrA in quiescence
... 0.09, R = 22.3 ± 0.1 and V = 23.6 ± 0.1. Similar brightness in the I-band was measured in 2004 May and 2010 June. Variability was analysed from series of images taken in 2004, spanning 0.6 h, and in two blocks of 6 h during 2007. We find that the target is not variable in any data set above the erro ...
... 0.09, R = 22.3 ± 0.1 and V = 23.6 ± 0.1. Similar brightness in the I-band was measured in 2004 May and 2010 June. Variability was analysed from series of images taken in 2004, spanning 0.6 h, and in two blocks of 6 h during 2007. We find that the target is not variable in any data set above the erro ...
ROSAT Ian R. Stevens* and David K. Strickland*
... NGC 1365, finding evidence for a soft thermal component, which dominates at low energies, a hard power-law component and strong Fe K emission at around 6.6 keV. Iyomoto et al. (1997) interpreted the power-law emission as being due to a lowluminosity AGN. We have reanalysed both ROSAT PSPC observatio ...
... NGC 1365, finding evidence for a soft thermal component, which dominates at low energies, a hard power-law component and strong Fe K emission at around 6.6 keV. Iyomoto et al. (1997) interpreted the power-law emission as being due to a lowluminosity AGN. We have reanalysed both ROSAT PSPC observatio ...
Vicky Kaspi Chandra Anomalous X-ray Pulsars Fotis Gavriil
... • SGRs (5): giant flares, short bursts, spectral changes, pulse profile changes, timing anomalies… • AXPs (9): short bursts, outbursts, slow flux changes, long-lived flares, glitches… – Most recognized only since 2002 ...
... • SGRs (5): giant flares, short bursts, spectral changes, pulse profile changes, timing anomalies… • AXPs (9): short bursts, outbursts, slow flux changes, long-lived flares, glitches… – Most recognized only since 2002 ...
Results from the ANTARES Neutrino Telescope Giorgio Giacomelli
... that of neutrino induced muons by many orders of magnitude. They are produced by high energy cosmic rays interacting with atomic nuclei of the upper atmosphere producing charged pions and kaons, which then decay into muons and neutrinos. Atmospheric muons are used to check the detector response and ...
... that of neutrino induced muons by many orders of magnitude. They are produced by high energy cosmic rays interacting with atomic nuclei of the upper atmosphere producing charged pions and kaons, which then decay into muons and neutrinos. Atmospheric muons are used to check the detector response and ...
... level, either as a shower of secondary particles from the resulting electromagnetic cascade or as a flash of Cherenkov light from the passage of these particles through the earth’s atmosphere. As in the CGRO range, γ-ray observations are severely limited by the charged cosmic particle flux which giv ...
Hunting for Orphaned Central Compact Objects among Radio Pulsars
... are listed in Table 1. While the pulsars have large characteristic ages of ∼ 108 years, we note that their true age could be much younger, particularly if they were born spinning slowly (see Ng et al. 2007; Bogdanov et al. 2014). There is an archival Chandra on-axis ACIS-S observation of PSR J1355−6 ...
... are listed in Table 1. While the pulsars have large characteristic ages of ∼ 108 years, we note that their true age could be much younger, particularly if they were born spinning slowly (see Ng et al. 2007; Bogdanov et al. 2014). There is an archival Chandra on-axis ACIS-S observation of PSR J1355−6 ...
Direct Dark Matter Search with the XENON100 Experiment
... (3.7 km water equivalent) reduces the cosmic muon background by a factor of 106 . The event-byevent 3D positioning capability of TPC allows volume fiducialization. With the self-shielding power of liquid xenon, as well as a 99 kg liquid xenon active veto, the electromagnetic radiation background is ...
... (3.7 km water equivalent) reduces the cosmic muon background by a factor of 106 . The event-byevent 3D positioning capability of TPC allows volume fiducialization. With the self-shielding power of liquid xenon, as well as a 99 kg liquid xenon active veto, the electromagnetic radiation background is ...
The Sun as an X-Ray Star. III. Flares
... 2. From each EM(T ) proÐle we synthesize the corresponding spectrum Ðltered through the spectral response and e†ective area of two instruments, namely ASCA/SIS and ROSAT /PSPC. 3. We bin the Ñare into three (or more) long time segments, (at least) one including the rise phase, one the Ñare maximum, ...
... 2. From each EM(T ) proÐle we synthesize the corresponding spectrum Ðltered through the spectral response and e†ective area of two instruments, namely ASCA/SIS and ROSAT /PSPC. 3. We bin the Ñare into three (or more) long time segments, (at least) one including the rise phase, one the Ñare maximum, ...
THE STAR FORMATION AND NUCLEAR ACCRETION HISTORIES OF NORMAL GALAXIES
... ability to detect X-ray emission from the AGES galaxies through the stacking approach. In Section 3 we provide further details of our stacking analysis and use Monte Carlo simulations to test it and to refine our choices of signal and background apertures. In Section 4 we present measurements of the ...
... ability to detect X-ray emission from the AGES galaxies through the stacking approach. In Section 3 we provide further details of our stacking analysis and use Monte Carlo simulations to test it and to refine our choices of signal and background apertures. In Section 4 we present measurements of the ...
The AzTEC mm-wavelength camera
... 1996; Mauskopf et al. 1997; Turner et al. 2001). The wafer is organized into six pie-shaped regions (hextants) that together contain the 144 optically active bolometers and their wiring. The detectors are arranged in a close-packed hexagonal configuration with a spacing set by the detector feedhorn ...
... 1996; Mauskopf et al. 1997; Turner et al. 2001). The wafer is organized into six pie-shaped regions (hextants) that together contain the 144 optically active bolometers and their wiring. The detectors are arranged in a close-packed hexagonal configuration with a spacing set by the detector feedhorn ...
full text pdf
... Npxl locus in Figure 1 is the domain of replicated instruments. The 4 m instruments HERMES, WEAVE and 4MOST are able to use the CCD pixels more efficiently, than assumed for the detector size loci in the figure, due to the coarser plate-scale of these smaller telescopes, and hence are able to rise ...
... Npxl locus in Figure 1 is the domain of replicated instruments. The 4 m instruments HERMES, WEAVE and 4MOST are able to use the CCD pixels more efficiently, than assumed for the detector size loci in the figure, due to the coarser plate-scale of these smaller telescopes, and hence are able to rise ...
ROSAT Isolated Neutron Stars
... Formation of molecular chains by covalent bonding along the field direction RX J0720.4-3125 Interactions between molecular chains can RX lead to the formation J1856.5-3754 of a 3D condensate Fe condensation H temperature Critical depends on B and chemical composition (Lai & Salpeter 1997; Lai ...
... Formation of molecular chains by covalent bonding along the field direction RX J0720.4-3125 Interactions between molecular chains can RX lead to the formation J1856.5-3754 of a 3D condensate Fe condensation H temperature Critical depends on B and chemical composition (Lai & Salpeter 1997; Lai ...
D2.2 - aspera
... The sensitivity of nowadays laser interferometers to gravitational waves with frequencies larger than a few hundred Hz, is limited by photon shot noise. To bypass this limitation it is necessary to increase the amount of photons stored inside the interferometer. One way to achieve this aim is to use ...
... The sensitivity of nowadays laser interferometers to gravitational waves with frequencies larger than a few hundred Hz, is limited by photon shot noise. To bypass this limitation it is necessary to increase the amount of photons stored inside the interferometer. One way to achieve this aim is to use ...
PDF of scale model - MESSENGER Education
... track variations in surface spectra and gather topographic information. A pivot platform will help point it in whatever direction the scientists choose. The two instruments will enable MESSENGER to “see” much like our two eyes do. Gamma-Ray and Neutr on Spectr ometer (GRNS): This instrument will det ...
... track variations in surface spectra and gather topographic information. A pivot platform will help point it in whatever direction the scientists choose. The two instruments will enable MESSENGER to “see” much like our two eyes do. Gamma-Ray and Neutr on Spectr ometer (GRNS): This instrument will det ...
Neutron Stars - Lick Observatory
... to be below ~2.5M" depending on the stiffness of the nuclear EoS, but it could be lower if phase transitions take place. Observations of large neutron star masses of order ~2.3M" would therefore restrict the equation of state (EoS) severely for dense matter. Glitches are sudden speed-ups in the rota ...
... to be below ~2.5M" depending on the stiffness of the nuclear EoS, but it could be lower if phase transitions take place. Observations of large neutron star masses of order ~2.3M" would therefore restrict the equation of state (EoS) severely for dense matter. Glitches are sudden speed-ups in the rota ...
Interplay of Direct, Pre-Equilibrium, and Compound Processes in
... • Cross section calculations for compound reactions: Require reliable structure input (which is often not available) • Indirect cross section approaches: Require a solid understanding of the reaction processes involved • Pickup reactions: A good description of the fragmentation of hole states ...
... • Cross section calculations for compound reactions: Require reliable structure input (which is often not available) • Indirect cross section approaches: Require a solid understanding of the reaction processes involved • Pickup reactions: A good description of the fragmentation of hole states ...
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.