SSM hardware
... • Most other experiments on ASTROSAT are pointed to a specific object for relatively long periods of time (~hours to days). • Scanning mechanism necessary for monitors to scan the sky multiple times per day. • FOV of two monitors forms an ‘X’ in the sky. Third detector views the perpendicular direct ...
... • Most other experiments on ASTROSAT are pointed to a specific object for relatively long periods of time (~hours to days). • Scanning mechanism necessary for monitors to scan the sky multiple times per day. • FOV of two monitors forms an ‘X’ in the sky. Third detector views the perpendicular direct ...
PowerPoint - Chandra X
... detected by Chandra are shown in gold, while optical data from ESO’s Very Large Telescope are shown in yellowwhite and blue, and infrared data from Spitzer are red. ...
... detected by Chandra are shown in gold, while optical data from ESO’s Very Large Telescope are shown in yellowwhite and blue, and infrared data from Spitzer are red. ...
No Slide Title
... • Cen X-2 brighter and softer than Sco X-1. Tau X-1 also detected. (Cen X-3 not seen) • SL 723 (July 1968) and 724 (April 1969) with largest PCS to date, 2 x 1380 cm2 • spectra of brightest sources ...
... • Cen X-2 brighter and softer than Sco X-1. Tau X-1 also detected. (Cen X-3 not seen) • SL 723 (July 1968) and 724 (April 1969) with largest PCS to date, 2 x 1380 cm2 • spectra of brightest sources ...
1 kg -1 - Daya Bay Reactor Neutrino Experiment in Hong Kong
... HPGe (mass 1 kg) enclosed by active NaI/CsI anti-Compton, further by passive shieldings & cosmic veto selection: single-event after cosmic-veto, anti-Comp., PSD TEXONO data (571/128 days) ON/OFF) [PRL 90, 2003 ; PRD ...
... HPGe (mass 1 kg) enclosed by active NaI/CsI anti-Compton, further by passive shieldings & cosmic veto selection: single-event after cosmic-veto, anti-Comp., PSD TEXONO data (571/128 days) ON/OFF) [PRL 90, 2003 ; PRD ...
Study Systematics on the ICM metallicity measurements
... weak emission compared to the continuum IS NOT A SOLID AND ROBUST ESTIMATE Iron estimate for systems of 2-3 keV can likely be biased towards higher values since this is a critical temperature range where we mix together plasma presenting either strong Fe-L or strong Fe-K lines. ...
... weak emission compared to the continuum IS NOT A SOLID AND ROBUST ESTIMATE Iron estimate for systems of 2-3 keV can likely be biased towards higher values since this is a critical temperature range where we mix together plasma presenting either strong Fe-L or strong Fe-K lines. ...
The Making of the Chandra X - ray Observatory
... ACIS – proposed 49 CCDs! HRC LETG HETG FPCS – Focal Plane Crystal Spectrometer z ...
... ACIS – proposed 49 CCDs! HRC LETG HETG FPCS – Focal Plane Crystal Spectrometer z ...
PowerPoint Presentation - Isolated Neutron Stars, solid crust
... we can measure the surface temperature and reconstruct the cooling history of the source. we can detect/undetect spectral features, constraining chemical composition and/or magnetic field strength in the atmosphere. ...
... we can measure the surface temperature and reconstruct the cooling history of the source. we can detect/undetect spectral features, constraining chemical composition and/or magnetic field strength in the atmosphere. ...
Physics 127 Descriptive Astronomy Homework #3 Key (Chapter 2
... 2-1. For each of the following wavelengths, state whether it is in the radio, microwave, infrared, visible, ultraviolet, X-ray, or gamma-ray portion of the electromagnetic spectrum and explain your reasoning: (a) 2.6 μm, (b) 34 m, (c) 0.54 nm, (d) .0032 nm, (e) 0.620 μm, (f) 310 nm, (g) 0.012 m. In ...
... 2-1. For each of the following wavelengths, state whether it is in the radio, microwave, infrared, visible, ultraviolet, X-ray, or gamma-ray portion of the electromagnetic spectrum and explain your reasoning: (a) 2.6 μm, (b) 34 m, (c) 0.54 nm, (d) .0032 nm, (e) 0.620 μm, (f) 310 nm, (g) 0.012 m. In ...
Full paper - The Institute of Mathematical Sciences
... medium energy resolution spectral studies and localization of Transients in soft and hard X-ray bands. • A Scanning Sky X-ray Monitor to detect and monitor Transients and known objects. • High time resolution (10 µs ) and high count rate capability ( 40 k Counts with PHA and 60 k Counts without PHA ...
... medium energy resolution spectral studies and localization of Transients in soft and hard X-ray bands. • A Scanning Sky X-ray Monitor to detect and monitor Transients and known objects. • High time resolution (10 µs ) and high count rate capability ( 40 k Counts with PHA and 60 k Counts without PHA ...
Homework 2: Due 2/02/2010
... 4. Extra Credit (4pts). You want to detect the following objects, all of which emit (approximately) black body spectrum. At what wavelength should you look to maximize the flux you receive from the object? a. A star like the Sun with a temperature of 6000 K b. A planet like the Earth with a tempera ...
... 4. Extra Credit (4pts). You want to detect the following objects, all of which emit (approximately) black body spectrum. At what wavelength should you look to maximize the flux you receive from the object? a. A star like the Sun with a temperature of 6000 K b. A planet like the Earth with a tempera ...
An Analysis of the Behavior of Vela X-1
... compact object is ~283 seconds and it is not changing. – The compact object is a neutron star based on its luminosity (from the energy spectrum flux) of ~1036 ergs sec-1 – It is a pulsar because it is in a MXRB and has a Power law Model fit. Literature support: Kretschmar, 2004, Charles and Seward, ...
... compact object is ~283 seconds and it is not changing. – The compact object is a neutron star based on its luminosity (from the energy spectrum flux) of ~1036 ergs sec-1 – It is a pulsar because it is in a MXRB and has a Power law Model fit. Literature support: Kretschmar, 2004, Charles and Seward, ...
stars - Chandra X
... too slow: T too low, no X-rays; (Curran+ 2011): optical-depth effects mixture of structured flows increasing with accretion rate? ...
... too slow: T too low, no X-rays; (Curran+ 2011): optical-depth effects mixture of structured flows increasing with accretion rate? ...
Document
... Detectors located nearby the circulating beam in the first two planes (arrays 1 and 2) should be thin enough in order to avoid any noticeable distortion caused by multiple scattering in the measured particle trajectories (100-300 mm @ UHV). High granularity strip detectors providing at least a 0.1 m ...
... Detectors located nearby the circulating beam in the first two planes (arrays 1 and 2) should be thin enough in order to avoid any noticeable distortion caused by multiple scattering in the measured particle trajectories (100-300 mm @ UHV). High granularity strip detectors providing at least a 0.1 m ...
L129 DISCOVERY OF A NEW 89 SECOND X
... Spectral analysis of relatively faint X-ray sources at low Galactic latitudes is complicated by the presence of diffuse emission from the Galactic ridge. Recent work by Valinia & Marshall (1998) indicates that the pointing direction of XTE J1906109 is outside the bright, thin component of the ridge ...
... Spectral analysis of relatively faint X-ray sources at low Galactic latitudes is complicated by the presence of diffuse emission from the Galactic ridge. Recent work by Valinia & Marshall (1998) indicates that the pointing direction of XTE J1906109 is outside the bright, thin component of the ridge ...
PowerPoint - Chandra X
... Most of the oxygen in the universe is thought to be dispersed into space by core-collapse supernovas. The oxygen ejecta from such supernovas is most readily detected through its X-radiation. Chandra observations have revealed the presence of substantial amounts of oxygen in N132D, particularly in th ...
... Most of the oxygen in the universe is thought to be dispersed into space by core-collapse supernovas. The oxygen ejecta from such supernovas is most readily detected through its X-radiation. Chandra observations have revealed the presence of substantial amounts of oxygen in N132D, particularly in th ...
Nobel Prize in Physics 2002: Riccardo Giaconni
... Earth, as the atmosphere acts like an absorbing layer. It may sound strange since X-rays easily pass through our body (except the bones). Although the atmosphere is very tenuous compared to our body, the total thickness offered by it is much larger and X-rays suffer considerable absorption in it. Th ...
... Earth, as the atmosphere acts like an absorbing layer. It may sound strange since X-rays easily pass through our body (except the bones). Although the atmosphere is very tenuous compared to our body, the total thickness offered by it is much larger and X-rays suffer considerable absorption in it. Th ...
Galactic Neighborhood and (Chandra-enabled) X-ray Astrophysics Q. Daniel Wang
... Approach 2: Deep large-scale X-ray mapping: • Individual observations have to be deep to remove enough background sources, which causes the cosmic variance. • To check physical properties of hot plasma near outer boundaries if they are present. Mkn 231, 0.5 Ms ACIS 0.5-8 keV Veilleux et al. 201 ...
... Approach 2: Deep large-scale X-ray mapping: • Individual observations have to be deep to remove enough background sources, which causes the cosmic variance. • To check physical properties of hot plasma near outer boundaries if they are present. Mkn 231, 0.5 Ms ACIS 0.5-8 keV Veilleux et al. 201 ...
X-ray effects on protoplanetary disks
... Schisano et al. 2010; Shang et al. 2010; Owen et al. 2010 ...
... Schisano et al. 2010; Shang et al. 2010; Owen et al. 2010 ...
X-ray Astronomy
... • Soft X-rays are emitted by hot gas (T ~ 2-3 MK) in the interior of the superbubble. This bright object forms the background for the "shadow" of a filament of gas and dust. The filament is shown by the overlaid contours, which represent 100 micron emission from dust at a temperature of about 30 K a ...
... • Soft X-rays are emitted by hot gas (T ~ 2-3 MK) in the interior of the superbubble. This bright object forms the background for the "shadow" of a filament of gas and dust. The filament is shown by the overlaid contours, which represent 100 micron emission from dust at a temperature of about 30 K a ...
スライド タイトルなし - X-ray Astronomy Group at ISAS
... shielding. The HXD sensor is consisting of 16 main detectors and the surrounding 20 crystal scintillators for active shielding. Each detector unit consists of two types of detectors: Gadolinium silicate (GSO) crystal buried deep in the bottom of the Wellshape Bismuth germanate (BGO) crystal, and PIN ...
... shielding. The HXD sensor is consisting of 16 main detectors and the surrounding 20 crystal scintillators for active shielding. Each detector unit consists of two types of detectors: Gadolinium silicate (GSO) crystal buried deep in the bottom of the Wellshape Bismuth germanate (BGO) crystal, and PIN ...
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.