Using Multilayer Optics to Measure X-ray Polarization Herman L. Marshall (MIT CSR)
... to Measure X-ray Polarization Herman L. Marshall (MIT CSR) and E. Silver, H. Schnopper, S. Murray (SAO), M. Weisskopf (MSFC) ...
... to Measure X-ray Polarization Herman L. Marshall (MIT CSR) and E. Silver, H. Schnopper, S. Murray (SAO), M. Weisskopf (MSFC) ...
Theoretical Examination
... point source and ignore atmospheric refraction. (T5) GMRT beam transit Giant Metrewave Radio Telescope (GMRT), one of the world's largest radio telescopes at metre wavelengths, is located in western India (latitude: 19 ∘ 6′ N, longitude: 74∘ 3′ E). GMRT consists of 30 dish antennas, each with a diam ...
... point source and ignore atmospheric refraction. (T5) GMRT beam transit Giant Metrewave Radio Telescope (GMRT), one of the world's largest radio telescopes at metre wavelengths, is located in western India (latitude: 19 ∘ 6′ N, longitude: 74∘ 3′ E). GMRT consists of 30 dish antennas, each with a diam ...
What happens close to a black hole?
... heavier than a few solar masses A massive object at the center of our galaxy Active Galactic Nuclei Ultra-luminous X-ray (ULX) sources Gamma-ray bursts ...
... heavier than a few solar masses A massive object at the center of our galaxy Active Galactic Nuclei Ultra-luminous X-ray (ULX) sources Gamma-ray bursts ...
102 Applied Physics B.Tech. 1st Year (Term – II)
... prove that susceptibility of paramagnetic substance is inversely proportional to the absolute temperature. There are 2.54 x 1022 free electrons per cm3 in sodium. Calculate its Fermi energy and Fermi velocity (h = 6.63 x 10-34 J s, m=9.11 x 10-31 kg, kB= 1.38 x 10-23 J/K, 1eV,= 1.6 x 10-19 J) ...
... prove that susceptibility of paramagnetic substance is inversely proportional to the absolute temperature. There are 2.54 x 1022 free electrons per cm3 in sodium. Calculate its Fermi energy and Fermi velocity (h = 6.63 x 10-34 J s, m=9.11 x 10-31 kg, kB= 1.38 x 10-23 J/K, 1eV,= 1.6 x 10-19 J) ...
A Decade in the Life of the Massive Black-Hole Binary... Silas Laycock !
... • We folded the 12 X-ray light-curve segments on a series of trial periods spanning the 3σ uncertainty region for the orbital period reported by Silverman & Fillipenko (2008). • At each trial period we computed the mean count-rate in the phase range 0.4-0.6, which is mid-eclipse. • Chandra and XM ...
... • We folded the 12 X-ray light-curve segments on a series of trial periods spanning the 3σ uncertainty region for the orbital period reported by Silverman & Fillipenko (2008). • At each trial period we computed the mean count-rate in the phase range 0.4-0.6, which is mid-eclipse. • Chandra and XM ...
Deep Chandra Observations of the Arches and Quintuplet Clusters at... Hui Dong Q. Daniel Wang ( &
... contamination of faint undetected point-like sources could be upto ∼ 65%, but mostly at energies ≤ 4 keV. The remaining diffuse emission can be characterized by a plasma with a temperature of ∼ 5 × 107 K. The 0.3-8 keV luminosity of the emission is 1.6×1033 ergs s−1 for Quintuplet and 7.7×1033 ergs ...
... contamination of faint undetected point-like sources could be upto ∼ 65%, but mostly at energies ≤ 4 keV. The remaining diffuse emission can be characterized by a plasma with a temperature of ∼ 5 × 107 K. The 0.3-8 keV luminosity of the emission is 1.6×1033 ergs s−1 for Quintuplet and 7.7×1033 ergs ...
Poster
... successfully collecting data which already allowed a broad spectrum of physics analysis both concerning cosmic rays and the Earth radiation belts. Based on experience gathered during the first mission, a more ambitious detector, AMS-02, is being built to be installed on the ISS in 2007. The AMS-02 d ...
... successfully collecting data which already allowed a broad spectrum of physics analysis both concerning cosmic rays and the Earth radiation belts. Based on experience gathered during the first mission, a more ambitious detector, AMS-02, is being built to be installed on the ISS in 2007. The AMS-02 d ...
Click here to view Carolyn`s poster
... The first x-ray telescopes were launched in the 1970’s and the basic theory remains the same today, all x-ray telescopes are space borne, as x-rays from space do not penetrate the Earth’s atmosphere. An x-ray telescope works on the principle of external reflection, essentially an x-ray is ‘bounced’ ...
... The first x-ray telescopes were launched in the 1970’s and the basic theory remains the same today, all x-ray telescopes are space borne, as x-rays from space do not penetrate the Earth’s atmosphere. An x-ray telescope works on the principle of external reflection, essentially an x-ray is ‘bounced’ ...
Observing at Other Wavelengths
... X-Rays: The Origins Astronomical X-ray sources were first found unexpectedly in the 1960s, in rocket experiments. They come from highly energetic sources ...
... X-Rays: The Origins Astronomical X-ray sources were first found unexpectedly in the 1960s, in rocket experiments. They come from highly energetic sources ...
Theme 6 – Observing at Other Wavelengths
... Astronomical X-ray sources were first found unexpectedly in the 1960s, in rocket experiments. They come from highly energetic sources n ...
... Astronomical X-ray sources were first found unexpectedly in the 1960s, in rocket experiments. They come from highly energetic sources n ...
Homework 2 key: Radiation processes, Larmor formula
... Define useful constants, conversions (N.B. not all are needed for any given assignment) 23 J ...
... Define useful constants, conversions (N.B. not all are needed for any given assignment) 23 J ...
The activities of the Astronomical Institute of the Slovak Academy of
... the initiation and impulsive acceleration phase, and their associated flares. We found a close synchronization between the CME acceleration profile and the flare energy release as indicated by the RHESSI hard X-ray flux onsets, as well as peaks occur simultaneously within 5 minutes. These findings ...
... the initiation and impulsive acceleration phase, and their associated flares. We found a close synchronization between the CME acceleration profile and the flare energy release as indicated by the RHESSI hard X-ray flux onsets, as well as peaks occur simultaneously within 5 minutes. These findings ...
Black Holes in M83 - Astronomical Society of the Pacific
... temperatures while in the process of being swallowed up. • In this new case, there was no blue source present before the outburst, and so no hot, blue star. So what is the blue source and where did it come from? ...
... temperatures while in the process of being swallowed up. • In this new case, there was no blue source present before the outburst, and so no hot, blue star. So what is the blue source and where did it come from? ...
Paper 1 (pdf)
... Figure 1. Top: Schematic of a single detector receiving dispersed X-rays from gratings behind the telescope, as in Constellation-X. Two views are shown, where the z axis is along the telescope axis. The spectrometer dispersion axis is approximately parallel to the x axis, along the surface of the de ...
... Figure 1. Top: Schematic of a single detector receiving dispersed X-rays from gratings behind the telescope, as in Constellation-X. Two views are shown, where the z axis is along the telescope axis. The spectrometer dispersion axis is approximately parallel to the x axis, along the surface of the de ...
CHANDRA AUTOMATED POINT SOURCE PROCESSING FOR CALIBRATION MONITORING Chandra X-ray Center (CXC)
... shape of Chandra’s mirrors. The elongation and rotation as a function of chip position is an important quantity to measure and track over time, as any shifts must be explained. Our catalog will enable a “mega image” of all point source photons that have fallen on the focal plane. ACIS offers the cap ...
... shape of Chandra’s mirrors. The elongation and rotation as a function of chip position is an important quantity to measure and track over time, as any shifts must be explained. Our catalog will enable a “mega image” of all point source photons that have fallen on the focal plane. ACIS offers the cap ...
n - Indico
... – competes with 22Ne(a,n)25Mg neutron source for the s-process (formation of heavy elements) ...
... – competes with 22Ne(a,n)25Mg neutron source for the s-process (formation of heavy elements) ...
Barger - Chandra X-Ray Observatory (CXC)
... • Deep MIR and radio images are an obvious avenue for searching for highly-obscured AGNs, since extinction in the MIR & radio is small • People have tried to use combined MIR & radio selections, but to obtain a reliable upper limit on the possible population of X-ray undetected, obscured AGNs, a cle ...
... • Deep MIR and radio images are an obvious avenue for searching for highly-obscured AGNs, since extinction in the MIR & radio is small • People have tried to use combined MIR & radio selections, but to obtain a reliable upper limit on the possible population of X-ray undetected, obscured AGNs, a cle ...
NGC 1808 - Rencontres de Moriond
... • Although a massive SSC might be present within 30 pc of the NGC 1068 nucleus, contributing to most of the observed UV continuun, the energetics in the other ranges is dominated by the active source: + The contribution to soft X-rays might be non-negligible, but is is any case below 30%. + The con ...
... • Although a massive SSC might be present within 30 pc of the NGC 1068 nucleus, contributing to most of the observed UV continuun, the energetics in the other ranges is dominated by the active source: + The contribution to soft X-rays might be non-negligible, but is is any case below 30%. + The con ...
What does X-ray light show us?
... Gamma-rays are the most energetic form of light and are produced by the hottest regions of the universe. They are also produced by such violent events as supernova explosions or the destruction of atoms, and by less dramatic events, such as the decay of radioactive material in space. Things like su ...
... Gamma-rays are the most energetic form of light and are produced by the hottest regions of the universe. They are also produced by such violent events as supernova explosions or the destruction of atoms, and by less dramatic events, such as the decay of radioactive material in space. Things like su ...
Deep O/IR Survey Of Chandra Galactic Bulge Fields
... We are conducting near-IR and optical survey of archival Chandra fields in the Galactic Bulge, as part of the Chandra Multiwavelength Plane survey (ChaMPlane), which is an effort to measure the space density and luminosity function of all types of accreting binaries, particularly concentrating on th ...
... We are conducting near-IR and optical survey of archival Chandra fields in the Galactic Bulge, as part of the Chandra Multiwavelength Plane survey (ChaMPlane), which is an effort to measure the space density and luminosity function of all types of accreting binaries, particularly concentrating on th ...
Astronomy Basics
... Slide 6: Gallery picture from Keck Observatory Slide 2: Educational graphic from Imagine the Universe! Slide 3: Harvard's Field Guide to X-ray Astronomy. Slide 7: Educational graphic from Imagine the Universe! ...
... Slide 6: Gallery picture from Keck Observatory Slide 2: Educational graphic from Imagine the Universe! Slide 3: Harvard's Field Guide to X-ray Astronomy. Slide 7: Educational graphic from Imagine the Universe! ...
Paper (pdf)
... Astronomical observations at all wavelengths have revealed the existence of numerous types of objects where extremely energetic and exotic phenomena occur. These include X-ray binaries and active galactic nuclei (AGN) among others, where accretion onto a compact object (collapsed star or massive bla ...
... Astronomical observations at all wavelengths have revealed the existence of numerous types of objects where extremely energetic and exotic phenomena occur. These include X-ray binaries and active galactic nuclei (AGN) among others, where accretion onto a compact object (collapsed star or massive bla ...
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.