Timing of the accreting millisecond pulsar IGR J17511-3057
... time and energy resolutions of 122 μs and 64 energy channels, respectively. We selected data in the energy range 2–25 keV to maximise the signal-to-noise ratio, since above ∼20 keV the background is the dominant signal. The X-ray flux follows a piecewise linear decay as showed in Fig. 1, with a peak ...
... time and energy resolutions of 122 μs and 64 energy channels, respectively. We selected data in the energy range 2–25 keV to maximise the signal-to-noise ratio, since above ∼20 keV the background is the dominant signal. The X-ray flux follows a piecewise linear decay as showed in Fig. 1, with a peak ...
ASTRONOMY AND ASTROPHYSICS The 10–200µm spectral
... Genzel et al. (1998) report the detection of both high-ionization (e.g. [O IV] λ25.9 µm, [N V] λ14.3 µm) and low–ionization (e.g. [Ne II] λ12.8 µm, [S III] λ18 µm) emission lines with the ISO short-wavelength grating spectrometer (SWS). The lowionization lines may be produced either by a starburst o ...
... Genzel et al. (1998) report the detection of both high-ionization (e.g. [O IV] λ25.9 µm, [N V] λ14.3 µm) and low–ionization (e.g. [Ne II] λ12.8 µm, [S III] λ18 µm) emission lines with the ISO short-wavelength grating spectrometer (SWS). The lowionization lines may be produced either by a starburst o ...
lhaaso-km2a
... them potentially very useful for calibration purposes. • Calibration of ED timing through the use of EAS events has been shown to be a robust, automatic approach enabling an independent calibration of many hardware ...
... them potentially very useful for calibration purposes. • Calibration of ED timing through the use of EAS events has been shown to be a robust, automatic approach enabling an independent calibration of many hardware ...
Folie 1 - Astroteilchenschule
... geometry: 24 x 24 pixels = 576 pixels within 1mm2 available up to 1024 pixels / mm² Operating voltage: 50 V to 58 V Gain: 105 up to ~ 5•106 single pixel time resolution: 570 ps FWHM single pixel recovery time: 1μs dark count rate: 106 counts per second at room temperature ...
... geometry: 24 x 24 pixels = 576 pixels within 1mm2 available up to 1024 pixels / mm² Operating voltage: 50 V to 58 V Gain: 105 up to ~ 5•106 single pixel time resolution: 570 ps FWHM single pixel recovery time: 1μs dark count rate: 106 counts per second at room temperature ...
Radio observations of the 13hXMM–Newton/ROSAT Deep X
... NRAO AIPS software. After removing the sidelobes of bright sources outside the X-ray survey area from the data, the noise level of the B-configuration map was close to the theoretical thermal noise level. Of the 24 h on-source during the A-configuration observations, 10 h were lost, or unusable, mai ...
... NRAO AIPS software. After removing the sidelobes of bright sources outside the X-ray survey area from the data, the noise level of the B-configuration map was close to the theoretical thermal noise level. Of the 24 h on-source during the A-configuration observations, 10 h were lost, or unusable, mai ...
INDIGO-KR_plancomm_pI_v3
... • Surface accuracy of mirrors 100 times better than telescope mirrors..Ultra-high reflective coatings : New technology for other fields • Vibration Isolation and suspension..Applications for mineral prospecting • Squeezing and challenging “quantum limits” in measurements. • Largest Ultra-high vacuum ...
... • Surface accuracy of mirrors 100 times better than telescope mirrors..Ultra-high reflective coatings : New technology for other fields • Vibration Isolation and suspension..Applications for mineral prospecting • Squeezing and challenging “quantum limits” in measurements. • Largest Ultra-high vacuum ...
Telescopes
... Interferometry can also be done with visible light but is much more difficult due to shorter wavelengths ...
... Interferometry can also be done with visible light but is much more difficult due to shorter wavelengths ...
The Swift satellite lives up to its name, revealing cosmic
... process additional energy is injected into the blast wave. Further indications of the continuation of the central engine arise in particularly long-lasting GRB prompt emission continuing for hundreds of seconds (e.g. GRB 070616, Starling et al. 2008) and lengthy afterglows, such as GRB 060729 which ...
... process additional energy is injected into the blast wave. Further indications of the continuation of the central engine arise in particularly long-lasting GRB prompt emission continuing for hundreds of seconds (e.g. GRB 070616, Starling et al. 2008) and lengthy afterglows, such as GRB 060729 which ...
Full-Text PDF
... down in less than a hundred seconds. It is usually argued that the balance of magnetic pressure with ram pressure from the disk can give an estimate of the possible magnetic flux accumulated around the central object. This argument is reasonable for accreting black hole systems such as AGNs and X-ra ...
... down in less than a hundred seconds. It is usually argued that the balance of magnetic pressure with ram pressure from the disk can give an estimate of the possible magnetic flux accumulated around the central object. This argument is reasonable for accreting black hole systems such as AGNs and X-ra ...
3011800000631
... dim isolated thermally emitting neutron stars (DINs) have rotation periods all in the same narrow range P = 3−12 s, giving rotation rates Ω ~ O(1)? As Psaltis and Miller (2002) have shown, dipole spindown (braking index n = 3) or spindown with any other power law index in the range n = 2−4, can prod ...
... dim isolated thermally emitting neutron stars (DINs) have rotation periods all in the same narrow range P = 3−12 s, giving rotation rates Ω ~ O(1)? As Psaltis and Miller (2002) have shown, dipole spindown (braking index n = 3) or spindown with any other power law index in the range n = 2−4, can prod ...
Polarimetric accuracy
... Achievable sensitivity depends on: • Seeing (and drifts); • Modulation speed; • Spatial intensity gradients of target; • Differential aberrations/beam wobble. ...
... Achievable sensitivity depends on: • Seeing (and drifts); • Modulation speed; • Spatial intensity gradients of target; • Differential aberrations/beam wobble. ...
Optical Variability of Hercules X-1/HZ Herculis
... from the other filters also show variability with the same period. To exclude any external fluctuations that could produce ’artificial’ variabilities, e.g. by the optics of the telescope itself or by other objects in the field of vision, the optical background was also analyzed with Fourier methods. ...
... from the other filters also show variability with the same period. To exclude any external fluctuations that could produce ’artificial’ variabilities, e.g. by the optics of the telescope itself or by other objects in the field of vision, the optical background was also analyzed with Fourier methods. ...
VIRUS Instrument Collimator Assembly
... volume-phase holographic (VPH) grating. These optics proved to be relatively straightforward to manufacture by many vendors (albeit at a wide range of costs and delivery times). 3.1.2 Selection of vendors Vendor selection was an important part of the instrument assembly process, particularly for opt ...
... volume-phase holographic (VPH) grating. These optics proved to be relatively straightforward to manufacture by many vendors (albeit at a wide range of costs and delivery times). 3.1.2 Selection of vendors Vendor selection was an important part of the instrument assembly process, particularly for opt ...
Sardinia_SA - Mullard Space Science Laboratory
... polars tend to emit at an approximately constant level, with occasional drops to fainter levels • There is a continuum of levels, but the states tend to be called “high”, “intermediate” and “low” • In low states the accretion rate drops, no reservoir in a disk, so the underlying stars can become vis ...
... polars tend to emit at an approximately constant level, with occasional drops to fainter levels • There is a continuum of levels, but the states tend to be called “high”, “intermediate” and “low” • In low states the accretion rate drops, no reservoir in a disk, so the underlying stars can become vis ...
Dark bursts - indico in2p3
... In some cases dark GRBs may have a bright radio afterglow, which is related to a dense circumburst medium (GRB 110709B, AVhost > 5.3m; GRB 111215A, AVhost > 8.5m, Zauderer+ 2013). The combination of radio and X-ray data allows to robustly determine the required extinction, instead of simply assuming ...
... In some cases dark GRBs may have a bright radio afterglow, which is related to a dense circumburst medium (GRB 110709B, AVhost > 5.3m; GRB 111215A, AVhost > 8.5m, Zauderer+ 2013). The combination of radio and X-ray data allows to robustly determine the required extinction, instead of simply assuming ...
The Milky Way-Pulsars and Isolated Neutron Stars
... on old V-2 (captured in Germany after the World War II) and Aerobee rockets, they were the first who detected X-rays from the very hot gas in the solar corona. However, the intensity of this radiation was found to be a factor 106 lower than that measured at optical wavelengths. In the late 1 X-rays ...
... on old V-2 (captured in Germany after the World War II) and Aerobee rockets, they were the first who detected X-rays from the very hot gas in the solar corona. However, the intensity of this radiation was found to be a factor 106 lower than that measured at optical wavelengths. In the late 1 X-rays ...
L. Zampieri - Astrophysics Group of the University of Crete
... L >> Ledd for 1 Msun (L>1.0e39 erg/s) Most compelling evidence of binary nature provided by detection of a modulation in the X-ray light curve of two ULXs, interpreted as the orbital period: M82 X-1 P~62 days (Kaaret et al. 2006a,b) NGC5408X-1 P~115 days (Strohmayer 2010; but see poster by Foste ...
... L >> Ledd for 1 Msun (L>1.0e39 erg/s) Most compelling evidence of binary nature provided by detection of a modulation in the X-ray light curve of two ULXs, interpreted as the orbital period: M82 X-1 P~62 days (Kaaret et al. 2006a,b) NGC5408X-1 P~115 days (Strohmayer 2010; but see poster by Foste ...
Summary of Talks at Growing Black Holes 2004 in Garching
... They use D4000/Hdelta to estimate a SFR from relations for normal galaxies. SigmaM_BH from Tremaine et al. Finding : lower mass black holes are the ones that are more active at the present time. Characteristic BH mass overall in their sample is 1e8 solar masses. Furthermore, the low mass BHs are g ...
... They use D4000/Hdelta to estimate a SFR from relations for normal galaxies. SigmaM_BH from Tremaine et al. Finding : lower mass black holes are the ones that are more active at the present time. Characteristic BH mass overall in their sample is 1e8 solar masses. Furthermore, the low mass BHs are g ...
Article - Agenda INFN
... K-B configuration consists of two perpendicular concave spherical mirrors in tandem. Rays from object point are reflected by the first mirror (tangential mirror here) and form a tangential line while not a point. Similarly, rays via the second mirror (sagittal mirror here) form a sagittal line. Thus ...
... K-B configuration consists of two perpendicular concave spherical mirrors in tandem. Rays from object point are reflected by the first mirror (tangential mirror here) and form a tangential line while not a point. Similarly, rays via the second mirror (sagittal mirror here) form a sagittal line. Thus ...
PowerPoint
... Electrons orbit the nucleus of each atom (a little like planets around the Sun) The nucleus consists of protons and neutrons Number of protons = number of electrons (so total charge is ...
... Electrons orbit the nucleus of each atom (a little like planets around the Sun) The nucleus consists of protons and neutrons Number of protons = number of electrons (so total charge is ...
Soudan Underground Laboratory
... When a muon neutrino hits an iron nucleus the collision results in the formation of a muon, this muon then passes through the iron plane and into the adjacent scintillator plane. As the muon passes through the scintillator it imparts some of its energy to electrons within the scintillator, exciting ...
... When a muon neutrino hits an iron nucleus the collision results in the formation of a muon, this muon then passes through the iron plane and into the adjacent scintillator plane. As the muon passes through the scintillator it imparts some of its energy to electrons within the scintillator, exciting ...
Soudan Underground Laboratory
... When a muon neutrino hits an iron nucleus the collision results in the formation of a muon, this muon then passes through the iron plane and into the adjacent scintillator plane. As the muon passes through the scintillator it imparts some of its energy to electrons within the scintillator, exciting ...
... When a muon neutrino hits an iron nucleus the collision results in the formation of a muon, this muon then passes through the iron plane and into the adjacent scintillator plane. As the muon passes through the scintillator it imparts some of its energy to electrons within the scintillator, exciting ...
Diapositiva 1
... First AGILE multi-λ campaign: 3C 279 Giuliani, D’Ammando, Vercellone, et al. 2009, A&A, 494, 509 First extragalactic source detected in gamma-ray by AGILE-GRID, monitored simultaneously in optical band by REM telescope and in X-rays by Swift = (210 38) 10-8 ph cm-2 s-1 E > 100 MeV
...
... First AGILE multi-λ campaign: 3C 279 Giuliani, D’Ammando, Vercellone, et al. 2009, A&A, 494, 509 First extragalactic source detected in gamma-ray by AGILE-GRID, monitored simultaneously in optical band by REM telescope and in X-rays by Swift
SAGE_prop
... Sun in most observed stellar coronae even in quiescence. The plasma parameters appear to depend on convection zone conditions and stellar rotation rates. Unfortunately, the high resolution instruments onboard XMM-Newton and Chandra are rather insensitive to emission from cool(er) plasma, and further ...
... Sun in most observed stellar coronae even in quiescence. The plasma parameters appear to depend on convection zone conditions and stellar rotation rates. Unfortunately, the high resolution instruments onboard XMM-Newton and Chandra are rather insensitive to emission from cool(er) plasma, and further ...
GAMMA BACKGROUND STUDIES FOR THE XENON
... The XENON Dark Matter Experiment, deployed at the Gran Sasso National Laboratory in Italy on March 2006, is a liquid noble gas detector designed to directly detect dark matter. The detector uses a dual-phase (gas/liquid) Xenon target to search for nuclear recoils associated with nucleus-WIMP interac ...
... The XENON Dark Matter Experiment, deployed at the Gran Sasso National Laboratory in Italy on March 2006, is a liquid noble gas detector designed to directly detect dark matter. The detector uses a dual-phase (gas/liquid) Xenon target to search for nuclear recoils associated with nucleus-WIMP interac ...
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.