FEEDBACK IN THE LOCAL UNIVERSE: The
... cavities (in blue). Such correspondence is typical of cool core clusters with cavities and extended radio sources, presenting strong circumstantial evidence in support of the AGN feedback model. See Bîrzan et al. (2004) for a comprehensive census of the currently known X-ray cavity systems in groups ...
... cavities (in blue). Such correspondence is typical of cool core clusters with cavities and extended radio sources, presenting strong circumstantial evidence in support of the AGN feedback model. See Bîrzan et al. (2004) for a comprehensive census of the currently known X-ray cavity systems in groups ...
ppt - ciera
... Chandra and XMM fields reveals no new 530 s pulsars, so there is a <0.5% chance of finding a magnetar in any field (Nechita, Gaensler, Muno, et al. in prep). • The pulsar is well within the cluster, with a <10% chance of being an unrelated X-ray source. ...
... Chandra and XMM fields reveals no new 530 s pulsars, so there is a <0.5% chance of finding a magnetar in any field (Nechita, Gaensler, Muno, et al. in prep). • The pulsar is well within the cluster, with a <10% chance of being an unrelated X-ray source. ...
Science with the Constellation
... features (specifically, the broad iron Ka line) are strongly distorted by gravitational effects and so provide a powerful probe of the physics of the accretion flow as well as the space-time geometry close to the black hole. The high throughput and broad-band response of Constellation-X will allow u ...
... features (specifically, the broad iron Ka line) are strongly distorted by gravitational effects and so provide a powerful probe of the physics of the accretion flow as well as the space-time geometry close to the black hole. The high throughput and broad-band response of Constellation-X will allow u ...
Fake Source Experiment for Chandra ACIS Observations
... Fake Source Experiment for Chandra ACIS Observations Eunhyeuk Kim(CfA), Paul Martini(OSU,CfA), Minsun Kim(CfA), & Dong-Woo Kim(CfA) High spatial resolution Chandra X-ray observations have resolved many point sources in both galaxies and clusters of galaxies. The observed spatial distribution of thes ...
... Fake Source Experiment for Chandra ACIS Observations Eunhyeuk Kim(CfA), Paul Martini(OSU,CfA), Minsun Kim(CfA), & Dong-Woo Kim(CfA) High spatial resolution Chandra X-ray observations have resolved many point sources in both galaxies and clusters of galaxies. The observed spatial distribution of thes ...
white dwarf
... just the multi-temperature thermal bremsstrahlung component from the hot radial accretion flow – no soft reprocessed component from the white dwarf • Main explanation is likely to be the larger area over which accretion takes place, but also photoelectric absorption is important ...
... just the multi-temperature thermal bremsstrahlung component from the hot radial accretion flow – no soft reprocessed component from the white dwarf • Main explanation is likely to be the larger area over which accretion takes place, but also photoelectric absorption is important ...
N Brickhouse
... • ATOMDB (Smith et al. 2001; Foster et al. 2012) • Collisionally ionized X-ray sources include: - Hot gas in galaxies - Hot gas in clusters of galaxies - Hot gas in the interstellar medium - Ejecta and shocks in supernova remnants - Shocks in hot star winds and binary colliding winds - Shocks from m ...
... • ATOMDB (Smith et al. 2001; Foster et al. 2012) • Collisionally ionized X-ray sources include: - Hot gas in galaxies - Hot gas in clusters of galaxies - Hot gas in the interstellar medium - Ejecta and shocks in supernova remnants - Shocks in hot star winds and binary colliding winds - Shocks from m ...
this PDF file - University of Leicester
... conform to each individual scenario discussed, it is very difficult to do so, especially for the “X-ray only” case. Metroid Prime would have to change its body temperature of the order of 107 K in order to accomplish the ability to switch between all 3 of these scenarios. Therefore it is deemed impo ...
... conform to each individual scenario discussed, it is very difficult to do so, especially for the “X-ray only” case. Metroid Prime would have to change its body temperature of the order of 107 K in order to accomplish the ability to switch between all 3 of these scenarios. Therefore it is deemed impo ...
PDF
... with ultra-high magnetic fields, so-called “magnetars” (Duncan & Thompson 1992). In this model, the X-ray emission is powered either by decay of the large magnetic field (Thompson & Duncan 1996) or neutron star cooling enhanced by the presence of the strong field (Heyl & Hernquist 1997a). Assuming m ...
... with ultra-high magnetic fields, so-called “magnetars” (Duncan & Thompson 1992). In this model, the X-ray emission is powered either by decay of the large magnetic field (Thompson & Duncan 1996) or neutron star cooling enhanced by the presence of the strong field (Heyl & Hernquist 1997a). Assuming m ...
Nature template - PC Word 97
... linear distance of ~2 light-years ~ 21018 cm between the end of the ACZ and the core at 7 mm wavelength. The flatness of the radio spectrum down to ~0.7 mm wavelength20 implies that the jet is a self-similar cone with constant Lorentz factor downstream of the point where the jet cross-section becom ...
... linear distance of ~2 light-years ~ 21018 cm between the end of the ACZ and the core at 7 mm wavelength. The flatness of the radio spectrum down to ~0.7 mm wavelength20 implies that the jet is a self-similar cone with constant Lorentz factor downstream of the point where the jet cross-section becom ...
The ROSAT galactic plane survey: ASTRONOMY AND
... signature of chromospheric and associated coronal activity (e.g. Schrijver 1983, Maggio et al. 1987). When the chromospheric activity was not found at the level expected from the intensity of the X-ray source (see below) or when no bright GSC star was conspicuous in the error circle, we obtained B a ...
... signature of chromospheric and associated coronal activity (e.g. Schrijver 1983, Maggio et al. 1987). When the chromospheric activity was not found at the level expected from the intensity of the X-ray source (see below) or when no bright GSC star was conspicuous in the error circle, we obtained B a ...
X-ray sources in the starburst spiral galaxy M 83
... point sources are detected (above 3.5-σ) in the ACIS S3 image, and 15 of them are within the inner 1600 region of the galaxy. A point source with Lx ≈ 3 × 1038 erg s−1 in the 0.3–8.0 keV band is found to coincide with the infra-red nuclear photometric peak, one of the two dynamical nuclei of the gal ...
... point sources are detected (above 3.5-σ) in the ACIS S3 image, and 15 of them are within the inner 1600 region of the galaxy. A point source with Lx ≈ 3 × 1038 erg s−1 in the 0.3–8.0 keV band is found to coincide with the infra-red nuclear photometric peak, one of the two dynamical nuclei of the gal ...
A neutron star with a carbon atmosphere in the Cassiopeia A
... (4 km and 5 km, respectively) are much smaller than the theoretical size of a neutron star RNS (∼ 10 km; ref. 14). This would suggest the emission region is a hot spot on the neutron star surface, which would probably result in X-ray pulsations as the hot spot rotated with the star. However, these p ...
... (4 km and 5 km, respectively) are much smaller than the theoretical size of a neutron star RNS (∼ 10 km; ref. 14). This would suggest the emission region is a hot spot on the neutron star surface, which would probably result in X-ray pulsations as the hot spot rotated with the star. However, these p ...
L. Moustakas
... HDFN and the CDFS regions (~ 300 square arcmin in total) with the most powerful telescopes over the widest wavelength range 30 times larger solid angle than HDFN + HDFS Based on large programs with Spitzer, HST, Chandra, Newton, VLT, and more. All datasets and derived products are open to the ...
... HDFN and the CDFS regions (~ 300 square arcmin in total) with the most powerful telescopes over the widest wavelength range 30 times larger solid angle than HDFN + HDFS Based on large programs with Spitzer, HST, Chandra, Newton, VLT, and more. All datasets and derived products are open to the ...
end-of-summer report
... of magnetic activity pattern on this time scale. Consequently, some groups, or epochs, have a 7 month range while others are 2 months long. The epochs that individual observations were grouped to are shown in Tables 3 and 4. This grouping procedure provides more counts for the distinct spectra, whic ...
... of magnetic activity pattern on this time scale. Consequently, some groups, or epochs, have a 7 month range while others are 2 months long. The epochs that individual observations were grouped to are shown in Tables 3 and 4. This grouping procedure provides more counts for the distinct spectra, whic ...
A relativistic iron emission line from the neutron star low-mass X
... Key words. line: identification – line: profiles – X-rays: individuals: GX 3+1 – X-rays: binaries – stars: neutron ...
... Key words. line: identification – line: profiles – X-rays: individuals: GX 3+1 – X-rays: binaries – stars: neutron ...
Mass Estimate of Black Hole Candidates GRS 1758
... 3. From the Chandra Handbook, a “ghost” artifact, a secondary image, appears on one side of every source, due to the Saturation of the High Gain Amplifiers. The brightness of the ghost image is reported to be 0.1% of the source. 4. The fake jet is about 0.01% of the brightness of the center of the s ...
... 3. From the Chandra Handbook, a “ghost” artifact, a secondary image, appears on one side of every source, due to the Saturation of the High Gain Amplifiers. The brightness of the ghost image is reported to be 0.1% of the source. 4. The fake jet is about 0.01% of the brightness of the center of the s ...
High Resolution Chandra Spectroscopy of Gamma Cassiopeia (B0
... thermal spectrum of the X-rays. However, while the star is now established as part of a binary system (see Harmanec et al. 2000; Miroshnichenko, Bjorkman, & Krugov 2002), the wide separation (P ≈ 204 days, with low to moderate eccentricity) makes it difficult to understand the high Lx if the compani ...
... thermal spectrum of the X-rays. However, while the star is now established as part of a binary system (see Harmanec et al. 2000; Miroshnichenko, Bjorkman, & Krugov 2002), the wide separation (P ≈ 204 days, with low to moderate eccentricity) makes it difficult to understand the high Lx if the compani ...
X-ray activity cycle on the active ultra
... gratings. These two reflection-grating spectrometers (RGS) provide high spectral resolution (E/ΔE ≈ 200–800) in the energy range 0.35–2.5 keV. Useful data were obtained from the EPIC and the RGS detectors (see Table 1 for a detailed account). AB Dor A, which is a very bright target with many emissio ...
... gratings. These two reflection-grating spectrometers (RGS) provide high spectral resolution (E/ΔE ≈ 200–800) in the energy range 0.35–2.5 keV. Useful data were obtained from the EPIC and the RGS detectors (see Table 1 for a detailed account). AB Dor A, which is a very bright target with many emissio ...
Hoffmann_Photon_Science_Novosibirsk_1__2015
... proportional to (BL)^2 •Therefore a strong magnet ic field needs to be pointed to the sun ...
... proportional to (BL)^2 •Therefore a strong magnet ic field needs to be pointed to the sun ...
PPT
... Large field of view (30 arcmin diameter) 3 telescopes, each with EPIC CCD detector Measures position, arrival time and energy of each detected X-ray photon Energy range 0.15 – 15 keV Survey profits from archive observations of individual interesting objects (O stars, outburst T Tauri stars) and cali ...
... Large field of view (30 arcmin diameter) 3 telescopes, each with EPIC CCD detector Measures position, arrival time and energy of each detected X-ray photon Energy range 0.15 – 15 keV Survey profits from archive observations of individual interesting objects (O stars, outburst T Tauri stars) and cali ...
PHY418 Particle Astrophysics
... following several years of observations by Vela defence satellites • these were designed to ...
... following several years of observations by Vela defence satellites • these were designed to ...
Discovery of Kilohertz Quasi-periodic Oscillations from 4U 1820
... 4U 18202303 implies that the secondary is an almost completely degenerate helium white dwarf with mass 10.058 – 0.078 MJ. Models for the formation of such an ultra–shortperiod binary include the collision of a neutron star with a giant, with subsequent “spiral-in” and ejection of the envelope (Verbu ...
... 4U 18202303 implies that the secondary is an almost completely degenerate helium white dwarf with mass 10.058 – 0.078 MJ. Models for the formation of such an ultra–shortperiod binary include the collision of a neutron star with a giant, with subsequent “spiral-in” and ejection of the envelope (Verbu ...
The Radio and X-ray Jet
... Fidelis and Semper This group requested BST spectra of the objects found in the Bubble Deep Field, in particular the blue galaxy-like objects, the small red objects, and the objects that look like fuzzy balls. The time allocation committee rejected this proposal: given that it took 120 orbits to ev ...
... Fidelis and Semper This group requested BST spectra of the objects found in the Bubble Deep Field, in particular the blue galaxy-like objects, the small red objects, and the objects that look like fuzzy balls. The time allocation committee rejected this proposal: given that it took 120 orbits to ev ...
A CHANDRA X-RAY STUDY OF THE DENSE GLOBULAR CLUSTER TERZAN... C. O. Heinke, P. D. Edmonds, J. E. Grindlay, and...
... color information did not uncover any promising candidates because of the crowding and overlapping Airy profiles, although it did identify two truly variable stars, one of which was shown to be an RR Lyrae variable. This paper is organized as follows. Section 2.1 describes the observations we used. S ...
... color information did not uncover any promising candidates because of the crowding and overlapping Airy profiles, although it did identify two truly variable stars, one of which was shown to be an RR Lyrae variable. This paper is organized as follows. Section 2.1 describes the observations we used. S ...
Document
... soft X-ray flare from 3 galaxies which were classified as non-active from ground based spectra. ...
... soft X-ray flare from 3 galaxies which were classified as non-active from ground based spectra. ...
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.