the effect of an soft X-ray source near the compact object in LS 5039
... U100eV U Ostar ~ L100eV LOstar ( ROstar R100eV ) 2 ~ 103 No variation in GeV & X-ray band In Y&T 2010, e± scattered off stellar photons → each flux modulates by the anisotropy of IC scattering In this study, they scatter off isotropic photons → emerging photons with GeV & keV have isotropic dist ...
... U100eV U Ostar ~ L100eV LOstar ( ROstar R100eV ) 2 ~ 103 No variation in GeV & X-ray band In Y&T 2010, e± scattered off stellar photons → each flux modulates by the anisotropy of IC scattering In this study, they scatter off isotropic photons → emerging photons with GeV & keV have isotropic dist ...
Supermassive black hole activity in local field early
... Virgo vs Field: Down-sizing Slopes consistent between the field and Virgo samples; also holds for detections only, as well as for the weighted subsamples Intercept slightly higher for the field sample ...
... Virgo vs Field: Down-sizing Slopes consistent between the field and Virgo samples; also holds for detections only, as well as for the weighted subsamples Intercept slightly higher for the field sample ...
PHYSICAL PROPERTIES OF THE AXP 4U 0142+61 FROM X
... fits. The obtained values of the parameters are consistent with each other within 1 , as well as with the results of the simultaneous fit. For comparison, we have also used the empirical blackbody plus power-law model to fit all XMM-Newton data simultaneously (still allowing for a contribution from ...
... fits. The obtained values of the parameters are consistent with each other within 1 , as well as with the results of the simultaneous fit. For comparison, we have also used the empirical blackbody plus power-law model to fit all XMM-Newton data simultaneously (still allowing for a contribution from ...
Lecture 1, Overview and Basic Concepts (April 2)
... - GALEX (2003-2011), UV surveys, imaging and spectroscopic observations in two bands: Far UV 1350-1780Å and Near UV 1770-2730Å ...
... - GALEX (2003-2011), UV surveys, imaging and spectroscopic observations in two bands: Far UV 1350-1780Å and Near UV 1770-2730Å ...
Identification of the optical counterparts of high-mass X
... used to identify optical counterparts in the Magellanic Clouds (Grebel 1997; Stevens et al. 1999). Good candidates are then those that occupy the upper left parts of the colour-colour diagram and lie inside or very close to the X-ray uncertainty region. Under these conditions the colour-colour diagr ...
... used to identify optical counterparts in the Magellanic Clouds (Grebel 1997; Stevens et al. 1999). Good candidates are then those that occupy the upper left parts of the colour-colour diagram and lie inside or very close to the X-ray uncertainty region. Under these conditions the colour-colour diagr ...
X-Ray Scattering from Warm Dense Matter at Vulcan
... This makes the TAW area a versatile laboratory for experiments on WDM. Counter propagating long pulse beams simultaneously irradiate a plastic coated aluminium target (targets are produced on site, allowing user flexibility on their design). As the plastic ablates, the rocket like expansion drives s ...
... This makes the TAW area a versatile laboratory for experiments on WDM. Counter propagating long pulse beams simultaneously irradiate a plastic coated aluminium target (targets are produced on site, allowing user flexibility on their design). As the plastic ablates, the rocket like expansion drives s ...
ppt
... Use the joint data sets to get insights into the evolution of the ICM physics • S-Z integrated pressure along the line of sight • X L-T (z) relation ...
... Use the joint data sets to get insights into the evolution of the ICM physics • S-Z integrated pressure along the line of sight • X L-T (z) relation ...
An X-ray and Radio Study of the Varying Expansion Velocities in
... “projection” boxes in ds97 , and range in width from 20-60′′ , chosen to lie along the shock front. We made our boxes large enough to provide good statistics within the region of interest, but small enough so that the curved shock front remains mostly straight. There are two gaps in our coverage: on ...
... “projection” boxes in ds97 , and range in width from 20-60′′ , chosen to lie along the shock front. We made our boxes large enough to provide good statistics within the region of interest, but small enough so that the curved shock front remains mostly straight. There are two gaps in our coverage: on ...
Black holes in binary systems and galatic nuclei
... the mass distribution of BHs has been considered by Postnov and Cherepashchuk (2003). Deficit of low-mass BH and the gap in the range (2 – 4) M may be due to enhanced quantum evaporation of BH which have been suggested in some multidimensional models of gravity (e.g. Randall and Sundrom, 1999). In ...
... the mass distribution of BHs has been considered by Postnov and Cherepashchuk (2003). Deficit of low-mass BH and the gap in the range (2 – 4) M may be due to enhanced quantum evaporation of BH which have been suggested in some multidimensional models of gravity (e.g. Randall and Sundrom, 1999). In ...
Lecture 2. Isolated Neutron Stars – I.
... The old zoo of neutron stars In 60s the first X-ray sources have been discovered. They were neutron stars in close binary systems, BUT ... .... they were «not recognized».... Now we know hundreds of X-ray binaries with neutron stars in the Milky Way and in other galaxies. ...
... The old zoo of neutron stars In 60s the first X-ray sources have been discovered. They were neutron stars in close binary systems, BUT ... .... they were «not recognized».... Now we know hundreds of X-ray binaries with neutron stars in the Milky Way and in other galaxies. ...
A Compact Central Object in the Supernova Remnant Kes 79
... al 2002) and Galactic (Grindlay et al. 2002). The hardness ratio, HR = H-S/H+S where S is the number of counts from 0.3 to 2.5 keV and H is the number of counts from 2.5 to 8 keV. There is no counterpart brighter than R magnitude 19 for the central source (1) or for sources 2 and 5. Because the spec ...
... al 2002) and Galactic (Grindlay et al. 2002). The hardness ratio, HR = H-S/H+S where S is the number of counts from 0.3 to 2.5 keV and H is the number of counts from 2.5 to 8 keV. There is no counterpart brighter than R magnitude 19 for the central source (1) or for sources 2 and 5. Because the spec ...
AMNH_colloquium_2May07_v7b
... O star X-ray emission line profiles are broadened, shifted, and asymmetric as the wind-shock scenario predicts But the degree of asymmetry requires significantly lower wind optical depths than are expected in these stars Clumping and the associated porosity can, in principle, alleviate this problem, ...
... O star X-ray emission line profiles are broadened, shifted, and asymmetric as the wind-shock scenario predicts But the degree of asymmetry requires significantly lower wind optical depths than are expected in these stars Clumping and the associated porosity can, in principle, alleviate this problem, ...
Gamma - Ray Observations of Olaf Reimer
... Many known X-ray PWN now identified as TeV emitters and almost all of the highest spin-down power radio pulsars have associated TeV emission – Efficient particle accelerators May be easier to detect in TeV than keV ? – Integration over pulsar lifetime for TeV electrons (less cooling) – TeV instrumen ...
... Many known X-ray PWN now identified as TeV emitters and almost all of the highest spin-down power radio pulsars have associated TeV emission – Efficient particle accelerators May be easier to detect in TeV than keV ? – Integration over pulsar lifetime for TeV electrons (less cooling) – TeV instrumen ...
X-ray Emission from Massive Stars
... X-rays from shock-heating in linedriven winds The Doppler desaturation that’s so helpful in driving a flow via momentum transfer in spectral lines is inherently unstable The line-driven instability (LDI) arises when a parcel of wind material is accelerated above the local flow speed, which moves it ...
... X-rays from shock-heating in linedriven winds The Doppler desaturation that’s so helpful in driving a flow via momentum transfer in spectral lines is inherently unstable The line-driven instability (LDI) arises when a parcel of wind material is accelerated above the local flow speed, which moves it ...
X-ray Polarimetry - XMM-Newton Science Operations Centre
... state’ are likely associated with Compton up-scattering of thermal photons by a hot (~109K) corona • This corona likely encloses some or all of the thermal disk • Details of the corona conditions (extent, temperature, location) have not been well constrained by spectra or temporal signatures • Polar ...
... state’ are likely associated with Compton up-scattering of thermal photons by a hot (~109K) corona • This corona likely encloses some or all of the thermal disk • Details of the corona conditions (extent, temperature, location) have not been well constrained by spectra or temporal signatures • Polar ...
Cosmic Feedback from Supermassive Black Holes
... Feedback and galaxy formation Every massive galaxy appears to have a massive black hole at its center whose mass is about 0.2% of the mass of the galaxy's bulge (Tremaine et al. 2002). It is now widely considered that the black hole may have brought about this correlation by regulating the amount of ...
... Feedback and galaxy formation Every massive galaxy appears to have a massive black hole at its center whose mass is about 0.2% of the mass of the galaxy's bulge (Tremaine et al. 2002). It is now widely considered that the black hole may have brought about this correlation by regulating the amount of ...
Letter to the Editor - Max-Planck
... efficiency, cannot produce more than ∼1039 erg s−1 for a ∼10 M black hole. This is in agreement with our picture for the beamed hard state, where, in a manner similar to that of blazars, the thermal and/or coronal X-ray flux is swamped by the jet emission and no reflection features should be observ ...
... efficiency, cannot produce more than ∼1039 erg s−1 for a ∼10 M black hole. This is in agreement with our picture for the beamed hard state, where, in a manner similar to that of blazars, the thermal and/or coronal X-ray flux is swamped by the jet emission and no reflection features should be observ ...
Most-likely Black Holes
... • X-ray emission region is very small • No stable star exists with given mass & size ...
... • X-ray emission region is very small • No stable star exists with given mass & size ...
Millisecond Pulsar Binaries at Transition
... From RXTE/ASM flux upper limits, it is likely that no accretion to the pulsar occurred during the time Since the relaxation time for the companion is much longer than 10 yrs since the interacting activity of the binary, the mass transfer and disk formation may occur again, providing a good source fo ...
... From RXTE/ASM flux upper limits, it is likely that no accretion to the pulsar occurred during the time Since the relaxation time for the companion is much longer than 10 yrs since the interacting activity of the binary, the mass transfer and disk formation may occur again, providing a good source fo ...
PPT - Chandra X
... 3. Fit the grouped spectrum (Chi-squared data-variance statistics, Levenberg-Marquardt optimization, kT1 [0.01-2] and kT2 [1-10] keV 4. If E(B-V) is unknown, fit again with kT, NH floating 5. Freeze kT and NH; fit for abundances 6. If two temperatures have not been found or the chi-squared statistic ...
... 3. Fit the grouped spectrum (Chi-squared data-variance statistics, Levenberg-Marquardt optimization, kT1 [0.01-2] and kT2 [1-10] keV 4. If E(B-V) is unknown, fit again with kT, NH floating 5. Freeze kT and NH; fit for abundances 6. If two temperatures have not been found or the chi-squared statistic ...
Ten Years Of XMM-Newton: Scientific Achievements And Future Prospects Norbert Schartel
... W. Shakespeare, 1623, The Tempest, Act 2, Scene 1 ...
... W. Shakespeare, 1623, The Tempest, Act 2, Scene 1 ...
Copyright 2004 Society of Photo-Optical Instrumentation Engineers. This
... The C-continuum measurements have the advantage of providing the effective area for nearly the entire Chandra energy band. But extreme care has to be taken for the data analysis and results evaluation details. Following issues has to be resolved and calculated correctly: • Pileup: Pileups occur whe ...
... The C-continuum measurements have the advantage of providing the effective area for nearly the entire Chandra energy band. But extreme care has to be taken for the data analysis and results evaluation details. Following issues has to be resolved and calculated correctly: • Pileup: Pileups occur whe ...
Deep Chandra Observations of the Arches and Quintuplet Clusters at... Hui Dong Q. Daniel Wang ( &
... The diffuse emission has a spectrum that is substantially harder than that of the point-like sources. In the core region (e.g. ≤ 15”, for Arches). The potential contamination of faint undetected point-like sources could be upto ∼ 65%, but mostly at energies ≤ 4 keV. The remaining diffuse emission ca ...
... The diffuse emission has a spectrum that is substantially harder than that of the point-like sources. In the core region (e.g. ≤ 15”, for Arches). The potential contamination of faint undetected point-like sources could be upto ∼ 65%, but mostly at energies ≤ 4 keV. The remaining diffuse emission ca ...
samba2002v2
... reconstruction of the photoemission angle is possible by evaluating the absorption point (or impact point) identified, in the first pass algorithm, with the barycentre. In asymmetric charge distributions, the third momentum (M3) lies along the major axis on the side, with respect to the barycentre, ...
... reconstruction of the photoemission angle is possible by evaluating the absorption point (or impact point) identified, in the first pass algorithm, with the barycentre. In asymmetric charge distributions, the third momentum (M3) lies along the major axis on the side, with respect to the barycentre, ...
History of X-ray astronomy
The history of X-ray astronomy begins in the 1920s, with interest in short wave communications for the U.S. Navy. This was soon followed by extensive study of the earth's ionosphere. By 1927, interest in the detection of X-ray and ultraviolet (UV) radiation at high altitudes inspired researchers to launch Goddard's rockets into the upper atmosphere to support theoretical studies and data gathering. The first successful rocket flight equipped with instrumentation able to detect solar ultraviolet radiation occurred in 1946. X-ray solar studies began in 1949. By 1973 a solar instrument package orbited on Skylab providing significant solar data.In 1965 the Goddard Space Flight Center program in X-ray astronomy was initiated with a series of balloon-borne experiments. In the 1970s this was followed by high altitude sounding rocket experiments, and that was followed by orbiting (satellite) observatories.The first rocket flight to successfully detect a cosmic source of X-ray emission was launched in 1962 by a group at American Science and Engineering (AS&E).X-ray wavelengths reveal information about the bodies (sources) that emit them.