Vasiliki Pavlidou - Center for Particle and Gravitational Astrophysics
... nearby transient (merger between compact objects ?) GLAST detects it as a very bright transient gamma-ray source. Follow up with Cherenkov detectors - high angular resolution. LIGO detects gravitational wave emission; nature of progenitor known at high confidence A success story Low-energy m ...
... nearby transient (merger between compact objects ?) GLAST detects it as a very bright transient gamma-ray source. Follow up with Cherenkov detectors - high angular resolution. LIGO detects gravitational wave emission; nature of progenitor known at high confidence A success story Low-energy m ...
3. Neutron Star X-ray Binaries
... The intersection between the function, RA/R*, and the basic condition plane, RA/R*=1, indicates the combination of the magnetic field and the mass accretion rate values for which plasma pressure and magnetic field pressure balance each other at the surface of the star. This ensures that the initial ...
... The intersection between the function, RA/R*, and the basic condition plane, RA/R*=1, indicates the combination of the magnetic field and the mass accretion rate values for which plasma pressure and magnetic field pressure balance each other at the surface of the star. This ensures that the initial ...
Topics in optical photon detection
... observed by Hertz (1887), and described through the absorption of quantised energy (photons) by Einstein (1905) ...
... observed by Hertz (1887), and described through the absorption of quantised energy (photons) by Einstein (1905) ...
LIM Transient Explorer
... transmissive filter. This would increase SNR by a factor of 1.8 Reflectance of S-pol is ~ 14%. Two in series would be ~2% for half of polarized light which would give very high “red leak” (~1%) in visible. Diffuse background would increase by 150%, meaning 40% reduction in SNR. Overall gain factor ...
... transmissive filter. This would increase SNR by a factor of 1.8 Reflectance of S-pol is ~ 14%. Two in series would be ~2% for half of polarized light which would give very high “red leak” (~1%) in visible. Diffuse background would increase by 150%, meaning 40% reduction in SNR. Overall gain factor ...
ly Searching the Sky: The Swift Mission and High Energy Physics Connections
... Dark bursts may be 10 times more numerous than GRBs, while many GRBs are missed because they are not in the FOV of a telescope. ...
... Dark bursts may be 10 times more numerous than GRBs, while many GRBs are missed because they are not in the FOV of a telescope. ...
Lecture 2. Isolated Neutron Stars – I.
... UHURU The satellite was launched on December 12, 1970. The program was ended in March 1973. The other name SAS-1 2-20 keV The first full sky survey. 339 sources. ...
... UHURU The satellite was launched on December 12, 1970. The program was ended in March 1973. The other name SAS-1 2-20 keV The first full sky survey. 339 sources. ...
Identification of the optical counterparts of high-mass X
... BeX tend to contain fast rotating neutron star, while persistent BeX show pulse periods above ∼ 200 s (Negueruela 2005). A search in the SIMBAD database yields that only about one third of HMXBs in the Milky Way have well-established optical counterparts. One of the largest hindrances to the identif ...
... BeX tend to contain fast rotating neutron star, while persistent BeX show pulse periods above ∼ 200 s (Negueruela 2005). A search in the SIMBAD database yields that only about one third of HMXBs in the Milky Way have well-established optical counterparts. One of the largest hindrances to the identif ...
Tsinghua Center for Astrophysics and the Dark - CPPM
... • Diffraction limited galaxy shape measurements in one broad visible R/I/Z band. • Redshift determination by Photo-z measurements in 3 YJH NIR bands to H(AB)=24 mag, 5σ point source ...
... • Diffraction limited galaxy shape measurements in one broad visible R/I/Z band. • Redshift determination by Photo-z measurements in 3 YJH NIR bands to H(AB)=24 mag, 5σ point source ...
Next Lecture
... EM DETECTORS (continued) Photon Detectors • Respond to individual photon interaction with electron(s) • Phase not preserved • Broad-band above threshold frequency • Instantaneous response proportional to collected photon rate (not energy deposition) • Many devices are integrating (store photoelectro ...
... EM DETECTORS (continued) Photon Detectors • Respond to individual photon interaction with electron(s) • Phase not preserved • Broad-band above threshold frequency • Instantaneous response proportional to collected photon rate (not energy deposition) • Many devices are integrating (store photoelectro ...
Slide 1
... and finally neutrinos. Protons with E>1020eV interact several times before degrading under the GKZ cut-off producing many ne and n neutrinos. The energy of produced neutrinos is more than 1018eV ...
... and finally neutrinos. Protons with E>1020eV interact several times before degrading under the GKZ cut-off producing many ne and n neutrinos. The energy of produced neutrinos is more than 1018eV ...
PPT
... Investigate evolution of X-ray output, energy, flaring rate in first few Myr. Investigate dependence of X-ray output, temperature of X-ray emitting gas on mass, age, accretion-rate, rotation ...
... Investigate evolution of X-ray output, energy, flaring rate in first few Myr. Investigate dependence of X-ray output, temperature of X-ray emitting gas on mass, age, accretion-rate, rotation ...
X-ray Emission Line Profile Diagnostics of Hot Star Winds
... We calculate line profiles using a 4-parameter model 3 parameters describe the spatial and velocity distribution of the emission: Ro is the minimum radius of X-ray emission, while b describes the acceleration of the wind and q parameterizes the radial dependence of the filling factor. 1 parameter, ...
... We calculate line profiles using a 4-parameter model 3 parameters describe the spatial and velocity distribution of the emission: Ro is the minimum radius of X-ray emission, while b describes the acceleration of the wind and q parameterizes the radial dependence of the filling factor. 1 parameter, ...
Compton scattering in strong gravity
... We have presented a new numerical code, COMPGR along with some technical details behind its treatment of general relativistic radiation transport. Its capabilities include namely Compton scattering with proper treatment of geodesic photon propagation between collision events and as such it finds its ...
... We have presented a new numerical code, COMPGR along with some technical details behind its treatment of general relativistic radiation transport. Its capabilities include namely Compton scattering with proper treatment of geodesic photon propagation between collision events and as such it finds its ...
ppt - MIT Haystack Observatory
... 260 ppm in TSI, it was energetically dominant over the X-ray counterpart, with Ltot ~100 Lx Emslie et al. (2005) note “. . .the total flare energy could be significantly higher than any of the ...
... 260 ppm in TSI, it was energetically dominant over the X-ray counterpart, with Ltot ~100 Lx Emslie et al. (2005) note “. . .the total flare energy could be significantly higher than any of the ...
Mass Estimate of Black Hole Candidates GRS 1758
... III. If the point where the gravitational attraction between the two stars is equal (Inner Lagrange Point) occurs near the surface of the Companion Star, matter will be stripped from the Companion Star into an Accretion Disc that forms around the Compact ...
... III. If the point where the gravitational attraction between the two stars is equal (Inner Lagrange Point) occurs near the surface of the Companion Star, matter will be stripped from the Companion Star into an Accretion Disc that forms around the Compact ...
Chapter 38
... a) The circumference of an electron’s orbit in an atom is an integer multiple of the electron’s wavelength. b) The positive charge within an atom is concentrated within a very small volume within an atom. c) A low pressure monatomic gas can be made to emit electromagnetic waves viewed as a series of ...
... a) The circumference of an electron’s orbit in an atom is an integer multiple of the electron’s wavelength. b) The positive charge within an atom is concentrated within a very small volume within an atom. c) A low pressure monatomic gas can be made to emit electromagnetic waves viewed as a series of ...
UNIT TWO Astronomical Instruments and Light
... 43. A ____________ is used to measure the brightness and color of stars. 44. A wave on a lake is found to have a wavelength of 2 m and a frequency of 0.3 Hz. What is the speed of this wave? 45. A telescope that is 1.0 meters in diameter has a focal length of 10 meters. If an eyepiece with a focal le ...
... 43. A ____________ is used to measure the brightness and color of stars. 44. A wave on a lake is found to have a wavelength of 2 m and a frequency of 0.3 Hz. What is the speed of this wave? 45. A telescope that is 1.0 meters in diameter has a focal length of 10 meters. If an eyepiece with a focal le ...
ISOLATED, MASSIVE SUPERGIANTS NEAR THE GALACTIC
... rameters and derived luminosities for the two detected sources are listed in Table 3, and the spectra are displayed in Figure 4. Finally, massive stars, particularly those in binaries, are often variable X-ray sources. Therefore, we examined whether X-ray light curves for H2 and X174516.1 were consi ...
... rameters and derived luminosities for the two detected sources are listed in Table 3, and the spectra are displayed in Figure 4. Finally, massive stars, particularly those in binaries, are often variable X-ray sources. Therefore, we examined whether X-ray light curves for H2 and X174516.1 were consi ...
Slide 1
... the ROIC (to translate the detector’s signals into image information). • When a photon is incident on the detector, it excites an electron-hole pair, which are then freed from the silicon crystal lattice and carried to opposite sides of the device (where the current is collected in localized areas c ...
... the ROIC (to translate the detector’s signals into image information). • When a photon is incident on the detector, it excites an electron-hole pair, which are then freed from the silicon crystal lattice and carried to opposite sides of the device (where the current is collected in localized areas c ...
Activity: Multiwavelength Bingo - Chandra X
... Activity: Multiwavelength Bingo background: Almost everything that we know about distant objects in the Universe comes from studying the light that is emitted or reflected by them. The entire range of energies of light is called the electromagnetic spectrum. Our eyes are sensitive only to a narrow b ...
... Activity: Multiwavelength Bingo background: Almost everything that we know about distant objects in the Universe comes from studying the light that is emitted or reflected by them. The entire range of energies of light is called the electromagnetic spectrum. Our eyes are sensitive only to a narrow b ...
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.