R - Institut d`Astrophysique de Paris
... SVOM = Space-based multiband astronomical Variable Objects Monitor ...
... SVOM = Space-based multiband astronomical Variable Objects Monitor ...
electronic imaging in
... structure, a slab of such material behaves the same at all points. Semiconductor crystals can be "grown" in a controlled way from a melt, and moreover, the electrical properties can be tailored by introducing so-called impurity atoms into the crystal structure at the atomic level, so that by microsc ...
... structure, a slab of such material behaves the same at all points. Semiconductor crystals can be "grown" in a controlled way from a melt, and moreover, the electrical properties can be tailored by introducing so-called impurity atoms into the crystal structure at the atomic level, so that by microsc ...
Title The Correlation between Dispersion Measure and X
... offer high-quality spectra with minimal background contamination. Any joint fits with other X-ray telescopes are not considered, in order to avoid cross-calibration uncertainties. 2. We adopted only NH values from actual X-ray spectral fits in which the NH is allowed to vary freely, and ignored any ...
... offer high-quality spectra with minimal background contamination. Any joint fits with other X-ray telescopes are not considered, in order to avoid cross-calibration uncertainties. 2. We adopted only NH values from actual X-ray spectral fits in which the NH is allowed to vary freely, and ignored any ...
Gamma Ray Bursts
... Gamma Ray Bursts - GRB (0.01-100s) g–ray pulses From pointlike sources in the sky Brighter than the rest of the sky (in g-rays) Energy 1051 erg (=1010 years of Sun emission) Distance up to z=4.5 (13·109 light years) Frequency 2-3 per day So far >3000 observed including ~100 in visible l ...
... Gamma Ray Bursts - GRB (0.01-100s) g–ray pulses From pointlike sources in the sky Brighter than the rest of the sky (in g-rays) Energy 1051 erg (=1010 years of Sun emission) Distance up to z=4.5 (13·109 light years) Frequency 2-3 per day So far >3000 observed including ~100 in visible l ...
CORONAL EVOLUTION OF THE SUN IN TIME: HIGH
... the X-ray emission of a solar analog during its main-sequence evolution, based on low-resolution X-ray spectroscopic data from the ROSAT and ASCA satellites. Among the principal findings of that work was a clear trend of decreasing coronal electron temperatures as a solar analog ages, following the ...
... the X-ray emission of a solar analog during its main-sequence evolution, based on low-resolution X-ray spectroscopic data from the ROSAT and ASCA satellites. Among the principal findings of that work was a clear trend of decreasing coronal electron temperatures as a solar analog ages, following the ...
Modeling the Spectral Energy Distributions and Variability
... Observed brightness combined with large distance implies huge energy output of GRBs, if they are emitting isotropically: E ~ 1054 erg L ~ 1051 erg/s ...
... Observed brightness combined with large distance implies huge energy output of GRBs, if they are emitting isotropically: E ~ 1054 erg L ~ 1051 erg/s ...
AVS03ML - Brigham Young University
... – Octagonal Chamber Light enters the chamber and is reflected from the surface being studied. The reflected light is measured as a function of angle. ...
... – Octagonal Chamber Light enters the chamber and is reflected from the surface being studied. The reflected light is measured as a function of angle. ...
INDIGO-KR_plancomm_pI
... • Thirty Meter Telescope: Resolving multiple AGNs, optical follow-up, … – Understanding most energetic cosmic events .. Supernovae, Gamma-ray • INO: cross correlate neutrino signals from SN event bursts, LMXB’s, Magnetars • LSST: Astro-transients with GW triggers, Cosmic distribution of dark – New c ...
... • Thirty Meter Telescope: Resolving multiple AGNs, optical follow-up, … – Understanding most energetic cosmic events .. Supernovae, Gamma-ray • INO: cross correlate neutrino signals from SN event bursts, LMXB’s, Magnetars • LSST: Astro-transients with GW triggers, Cosmic distribution of dark – New c ...
The Historical Evolution of the Telescope
... single photons to charge individual CCD pixels. X-ray photons are capable of producing very large charges in a CCD sensor. Microcalorimters, however, are only capable of detecting photons one at a time. Despite this limitation, the lack of x-ray photons directed towards earth allows microcalorimeter ...
... single photons to charge individual CCD pixels. X-ray photons are capable of producing very large charges in a CCD sensor. Microcalorimters, however, are only capable of detecting photons one at a time. Despite this limitation, the lack of x-ray photons directed towards earth allows microcalorimeter ...
0004-637X 778 2 119
... the period derivative, Ṗ , of the neutron star is independent of both Ṁ and P if the source is not close to rotational equilibrium, that is, when ω∗2 is not close to unity. The neutron star reaches maximum Ṗ in the accretion phase. The maximum value of Ṗ is proportional to B02 , where B0 is the ...
... the period derivative, Ṗ , of the neutron star is independent of both Ṁ and P if the source is not close to rotational equilibrium, that is, when ω∗2 is not close to unity. The neutron star reaches maximum Ṗ in the accretion phase. The maximum value of Ṗ is proportional to B02 , where B0 is the ...
Search for solar axions with the CAST experiment
... CAST: Tracking precision Solar filming Twice per year (March and September) we can film the Sun through the window A camera is placed on top of the magnet and is aligned with the bore axis Corrections for visible light refractions are taken into account ...
... CAST: Tracking precision Solar filming Twice per year (March and September) we can film the Sun through the window A camera is placed on top of the magnet and is aligned with the bore axis Corrections for visible light refractions are taken into account ...
2. Bright AGN phase
... becomes transparent and the nucleus can be seen. 3. Death of bright AGNs radiation of AGNs expels gases to quench both accretion and star formation. 4. Faint AGN phases accreting at very low rates 0.01M / M Edd . ...
... becomes transparent and the nucleus can be seen. 3. Death of bright AGNs radiation of AGNs expels gases to quench both accretion and star formation. 4. Faint AGN phases accreting at very low rates 0.01M / M Edd . ...
Transparencies - Rencontres de Moriond
... observational results (X, Gamma, IR) The supermassive BLACK HOLE PARADIGM at center of galaxies is now HARDLY ESCAPABLE All results point to an EXTRAORDINARY LOW LUMINOSITY of the GC BH environment. WHY ? The FLARE phenomenon is likely THE KEY TO REACH THE HORIZON of the BH ...
... observational results (X, Gamma, IR) The supermassive BLACK HOLE PARADIGM at center of galaxies is now HARDLY ESCAPABLE All results point to an EXTRAORDINARY LOW LUMINOSITY of the GC BH environment. WHY ? The FLARE phenomenon is likely THE KEY TO REACH THE HORIZON of the BH ...
Laboratory Astrophysics: Spectral Analysis of Photoionized Neon J ames MacArthur
... ions. The density squared dependence of the collisional ionization rate makes it the dominant process in high density plasmas, while the linear dependence of the photoionization rate makes it the dominant process in a low density plasma in a radiation field. The last piece of information Equation (1 ...
... ions. The density squared dependence of the collisional ionization rate makes it the dominant process in high density plasmas, while the linear dependence of the photoionization rate makes it the dominant process in a low density plasma in a radiation field. The last piece of information Equation (1 ...
Minutes SSWG_2 - Space Astronomy Laboratory
... of the SALT instrumentation was yet to be defined. It was felt that as far as possible, SALT instruments should be built by members of the SALT consortium, but that did not preclude an instrument PI involving outside parties, if necessary. For the time being, however, it was felt that all avenues sh ...
... of the SALT instrumentation was yet to be defined. It was felt that as far as possible, SALT instruments should be built by members of the SALT consortium, but that did not preclude an instrument PI involving outside parties, if necessary. For the time being, however, it was felt that all avenues sh ...
slides ppt
... • Precise GW/ timing can be achieved at better than 1 ms. • Absolute neutrino masses can be investigated below the present lower limit of 2 eV down to 0.6 – 0.8 eV in a direct way. • When masses are known from other methods or found to be smaller than 0.5 eV, relative GW/ timing provides a new t ...
... • Precise GW/ timing can be achieved at better than 1 ms. • Absolute neutrino masses can be investigated below the present lower limit of 2 eV down to 0.6 – 0.8 eV in a direct way. • When masses are known from other methods or found to be smaller than 0.5 eV, relative GW/ timing provides a new t ...
Laboratory Astrophysics: Spectral Analysis of Photoionized Neon
... 1.2, hotter plasmas would have a larger standard deviation in energy). When only photoexcitation is included (no ionizing photons are present in the model) in the middle pane on the left, the higher n transitions like β and γ are more pronounced, since their upper levels (the 1snp He-like levels wit ...
... 1.2, hotter plasmas would have a larger standard deviation in energy). When only photoexcitation is included (no ionizing photons are present in the model) in the middle pane on the left, the higher n transitions like β and γ are more pronounced, since their upper levels (the 1snp He-like levels wit ...
The X-ray emission from shock cooling zones in O star winds
... the order of a few cooling times. Since the density and temperature stratification of the post-shock region change during the course of this contraction and expansion, and since these quantities enter non-linearly into the shock emission coefficient, the thermal instability will certainly affect the ...
... the order of a few cooling times. Since the density and temperature stratification of the post-shock region change during the course of this contraction and expansion, and since these quantities enter non-linearly into the shock emission coefficient, the thermal instability will certainly affect the ...
Gamma Ray Bursts (GRB)
... Gamma Ray Bursts are separated into two classes: long-duration bursts and shortduration bursts. Long duration bursts – Gamma Ray Bursts that last more than 2 seconds. Short-duration bursts – Gamma Ray Bursts that last less than 2 seconds. Short duration bursts range from a few milliseconds to 2 seco ...
... Gamma Ray Bursts are separated into two classes: long-duration bursts and shortduration bursts. Long duration bursts – Gamma Ray Bursts that last more than 2 seconds. Short-duration bursts – Gamma Ray Bursts that last less than 2 seconds. Short duration bursts range from a few milliseconds to 2 seco ...
GRB – The Afterglow
... consisting of a central BH and a surrounding torus is much more promising BH-torus system geometry: relatively baryon-poor regions along the rotational axis thermal energy release preferentially above the BH poles via e.g. anti- annihilation can lead to collimated, highly relativistic jets ...
... consisting of a central BH and a surrounding torus is much more promising BH-torus system geometry: relatively baryon-poor regions along the rotational axis thermal energy release preferentially above the BH poles via e.g. anti- annihilation can lead to collimated, highly relativistic jets ...
The Telescope - Salt Lake Astronomical Society
... History of the Telescope For as long as man has been capable of wondering, the night sky has provided subject material to wonder about. Trying to see more clearly and to find greater detail of the objects in the sky had been a desire of all the ancient astronomers. The true beginning of telescopes i ...
... History of the Telescope For as long as man has been capable of wondering, the night sky has provided subject material to wonder about. Trying to see more clearly and to find greater detail of the objects in the sky had been a desire of all the ancient astronomers. The true beginning of telescopes i ...
THE SOFT STATE OF CYGNUS X-1 OBSERVED WITH
... considerations. For the reflected emission, we use the XILLVER reflection model because it incorporates the effects of viewing angle (i.e., the disk inclination, i) on the observed reflection spectrum. We use the combination of XILLVER and RELCONV to remain consistent with the approach of Tomsick et al ...
... considerations. For the reflected emission, we use the XILLVER reflection model because it incorporates the effects of viewing angle (i.e., the disk inclination, i) on the observed reflection spectrum. We use the combination of XILLVER and RELCONV to remain consistent with the approach of Tomsick et al ...
Chandra HETGS Multiphase Spectroscopy Of The Young
... torus is visible ( X-ray maximum). At low viewing angles, some of the torus is occulted ( X-ray minimum). ...
... torus is visible ( X-ray maximum). At low viewing angles, some of the torus is occulted ( X-ray minimum). ...
Hidden57_rf
... spectacular images that have become the icons of modern astronomy. By expanding your vision beyond the visible into an array of “colours” that span the full spectrum of light, you will be able to gain a more complete picture of the Universe than has ever been possible before in human history. These ...
... spectacular images that have become the icons of modern astronomy. By expanding your vision beyond the visible into an array of “colours” that span the full spectrum of light, you will be able to gain a more complete picture of the Universe than has ever been possible before in human history. These ...
Review of High Energy Astrophysics Research in Mainland China
... • Hard X-ray Modulation Telescope (future satellite mission) • Gamma-ray burst monitor aboard the Shen-Zhou-II space lab. • Balloon-borne hard X-ray telescope ...
... • Hard X-ray Modulation Telescope (future satellite mission) • Gamma-ray burst monitor aboard the Shen-Zhou-II space lab. • Balloon-borne hard X-ray telescope ...
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.