Black holes in binary systems and galatic nuclei
... excellent agreement with Einstein General Relativity. Taking into account observational selection effects we can estimate the full number of stellar mass BHs in our Galaxy as ~107. For the mean mass MBH ≈ 9 – 10 M it is ~ 108 M or 0.1% of the baryonic mass in our Galaxy. ...
... excellent agreement with Einstein General Relativity. Taking into account observational selection effects we can estimate the full number of stellar mass BHs in our Galaxy as ~107. For the mean mass MBH ≈ 9 – 10 M it is ~ 108 M or 0.1% of the baryonic mass in our Galaxy. ...
NuSTAR SPECTROSCOPY OF GRS 1915+105: DISK
... We report on the results of spectral fits made to a NuSTAR observation of the black hole GRS 1915+105 in a “plateau” state. This state is of special interest because it is similar to the “low/hard” state seen in other black holes, especially in that compact, steady jets are launched in this phase. T ...
... We report on the results of spectral fits made to a NuSTAR observation of the black hole GRS 1915+105 in a “plateau” state. This state is of special interest because it is similar to the “low/hard” state seen in other black holes, especially in that compact, steady jets are launched in this phase. T ...
Search for Electronic Recoil Event Rate Modulation with 4 Years of
... The DAMA/LIBRA experiment has reported the observation of a periodic annual modulation of the low-energy (low-E), (2–6) keV, single-hit event rate in their NaI detectors [1], with a phase of ð144 7Þ day consistent with the standard dark matter halo [2,3]. The interpretation of this modulation as b ...
... The DAMA/LIBRA experiment has reported the observation of a periodic annual modulation of the low-energy (low-E), (2–6) keV, single-hit event rate in their NaI detectors [1], with a phase of ð144 7Þ day consistent with the standard dark matter halo [2,3]. The interpretation of this modulation as b ...
Document
... n-source: 13C(α,n)16O and/or 22Ne(α,n)25Mg quiescent scenarios: e.g. He burning (T8 ~ 1 – 4; E0 ~ 30 keV) ...
... n-source: 13C(α,n)16O and/or 22Ne(α,n)25Mg quiescent scenarios: e.g. He burning (T8 ~ 1 – 4; E0 ~ 30 keV) ...
Student Project - Ott Planetarium
... Spectroscopy is the study of how electromagnetic radiation, which we’ve just introduced, interacts with atoms. Atoms absorb and emit radiation across the entire spectrum; with each atom having a unique pattern. By analyzing the data that is collected by the the space telescopes, scientist use these ...
... Spectroscopy is the study of how electromagnetic radiation, which we’ve just introduced, interacts with atoms. Atoms absorb and emit radiation across the entire spectrum; with each atom having a unique pattern. By analyzing the data that is collected by the the space telescopes, scientist use these ...
dtu7ech03 pt 2 - Fort Thomas Independent Schools
... Light from cities scatters in our atmosphere reducing the visibility of celestial objects. This is called light pollution, and has been an increasing problem in recent years. The view from Kitt Peak National Observatory of the Tuscon, Arizona skyline in 1959 ...
... Light from cities scatters in our atmosphere reducing the visibility of celestial objects. This is called light pollution, and has been an increasing problem in recent years. The view from Kitt Peak National Observatory of the Tuscon, Arizona skyline in 1959 ...
Generation of highly energetic electrons at
... Context. During solar flares a large amount of energy is suddenly released and partly transfered into energetic electrons. They are of special interest since a substantial part of the energy released during a flare is deposited into the energetic electrons. RHESSI observations, e.g. of the solar eve ...
... Context. During solar flares a large amount of energy is suddenly released and partly transfered into energetic electrons. They are of special interest since a substantial part of the energy released during a flare is deposited into the energetic electrons. RHESSI observations, e.g. of the solar eve ...
An X-ray and Radio Study of the Varying Expansion Velocities in
... where a fuller description can be found. Other SNR works, such as Winkler et al. (2014) and Yamaguchi et al. (2016), have used this technique as well. We extract the 1D radial profiles from both epochs, with uncertainties on each data point, then shift epoch 1 relative to epoch 2, minimizing the val ...
... where a fuller description can be found. Other SNR works, such as Winkler et al. (2014) and Yamaguchi et al. (2016), have used this technique as well. We extract the 1D radial profiles from both epochs, with uncertainties on each data point, then shift epoch 1 relative to epoch 2, minimizing the val ...
Ay122a&Fall&2015+16& Background&subtrac9on,&calibra9on,& analysis& &
... to&transform&each&slit& into&a&rec9linear&grid&of& wavelength&(X&axis)&and& spa9al&posi9on&along&alit& (Y&axis).& ...
... to&transform&each&slit& into&a&rec9linear&grid&of& wavelength&(X&axis)&and& spa9al&posi9on&along&alit& (Y&axis).& ...
Determination of the astrophysical S factor of the 8B(p,γ)
... 9 Be target (1.2 g/cm2 ) and an aluminum achromatic wedge (mean thickness = 400 mg/cm2 ), the 8 B yield was roughly 104 s−1 at the energy of 14.4 MeV/u. The momentum acceptance was set using slits placed at the dispersive focal plane (F1) of RIPS, in order to obtain an energy spread of ±2%. Although ...
... 9 Be target (1.2 g/cm2 ) and an aluminum achromatic wedge (mean thickness = 400 mg/cm2 ), the 8 B yield was roughly 104 s−1 at the energy of 14.4 MeV/u. The momentum acceptance was set using slits placed at the dispersive focal plane (F1) of RIPS, in order to obtain an energy spread of ±2%. Although ...
a report on pulsars, written for PHAS1901
... dependence on frequency, v, given by L ∝ where ~0.75 . Since v > 1 and β < 1, as v increases, vβ will increase and v-β will decrease. this means that signal strength of pulses will be higher when observed at lower frequencies. Due to the fact that each pulse detected on the earth will correspond ...
... dependence on frequency, v, given by L ∝ where ~0.75 . Since v > 1 and β < 1, as v increases, vβ will increase and v-β will decrease. this means that signal strength of pulses will be higher when observed at lower frequencies. Due to the fact that each pulse detected on the earth will correspond ...
Gravitational Waves
... ✓ GWs propagate through matter with little interaction. Hard to detect, but they ...
... ✓ GWs propagate through matter with little interaction. Hard to detect, but they ...
Document
... equivalent isotropic luminosity 1049 erg/s. Collimation θ2/2 ~ 10-2 – 10-3. θ – jet opening angle. EGRET detected 66 (+27) sources of this type. New breakthrough is expected after the launch of GLAST. Several sources have been detected in the TeV range by ground-based gamma-ray telescopes. All of th ...
... equivalent isotropic luminosity 1049 erg/s. Collimation θ2/2 ~ 10-2 – 10-3. θ – jet opening angle. EGRET detected 66 (+27) sources of this type. New breakthrough is expected after the launch of GLAST. Several sources have been detected in the TeV range by ground-based gamma-ray telescopes. All of th ...
AGN jets
... equivalent isotropic luminosity 1049 erg/s. Collimation θ2/2 ~ 10-2 – 10-3. θ – jet opening angle. EGRET detected 66 (+27) sources of this type. New breakthrough is expected after the launch of GLAST. Several sources have been detected in the TeV range by ground-based gamma-ray telescopes. All of th ...
... equivalent isotropic luminosity 1049 erg/s. Collimation θ2/2 ~ 10-2 – 10-3. θ – jet opening angle. EGRET detected 66 (+27) sources of this type. New breakthrough is expected after the launch of GLAST. Several sources have been detected in the TeV range by ground-based gamma-ray telescopes. All of th ...
Radio Bubbles, Cooling X-ray Gas, Galaxy Interactions, and Star
... (Proposal ID 8301, PI Alastair Edge). The SOAR data were obtained as part of an Early Science run for the SOI. The pixels were binned 2 × 2, for a pixel scale of 0.15400 per pixel. The sky quality was excellent, with seeing below 100 and good transparency. The telescope focus needed to be optimized ...
... (Proposal ID 8301, PI Alastair Edge). The SOAR data were obtained as part of an Early Science run for the SOI. The pixels were binned 2 × 2, for a pixel scale of 0.15400 per pixel. The sky quality was excellent, with seeing below 100 and good transparency. The telescope focus needed to be optimized ...
HESS-II, an observatory for very high energies, proves its worth
... In the Universe, supermassive black holes, clusters of galaxies, supernove, binary sarsand pulsars act as natural accelerators of cosmic particles (electrons, ions, ...). These particules thus acquire very high energies, as witnessed by gamma ray emission. When these rays reach the upper atmosphere ...
... In the Universe, supermassive black holes, clusters of galaxies, supernove, binary sarsand pulsars act as natural accelerators of cosmic particles (electrons, ions, ...). These particules thus acquire very high energies, as witnessed by gamma ray emission. When these rays reach the upper atmosphere ...
Effective atomic numbers and electron densities of amino
... regarded as being built up of one kind of species with atomic number Zeff .In materials like biological molecules and other compounds, for photon interaction a single atomic number can not represent the atomic number uniquely across the entire energy region because of the effective atomic number bei ...
... regarded as being built up of one kind of species with atomic number Zeff .In materials like biological molecules and other compounds, for photon interaction a single atomic number can not represent the atomic number uniquely across the entire energy region because of the effective atomic number bei ...
Black Holes in Binary Systems and Galaxy Nuclei
... excellent agreement with Einstein General Relativity. Taking into account observational selection effects we can estimate the full number of stellar mass BHs in our Galaxy as ~107. For the mean mass MBH ≈ 9 – 10 MSun it is ~ 108 MSun or 0.1% of the baryonic mass in our Galaxy. ...
... excellent agreement with Einstein General Relativity. Taking into account observational selection effects we can estimate the full number of stellar mass BHs in our Galaxy as ~107. For the mean mass MBH ≈ 9 – 10 MSun it is ~ 108 MSun or 0.1% of the baryonic mass in our Galaxy. ...
this PDF file - University of Leicester
... 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 impossible to exist in nature, or at the least very highly unlikely. ...
... 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 impossible to exist in nature, or at the least very highly unlikely. ...
Detection of gamma-ray bursts in the 1 GeV–1 TeV energy range by
... detected in this mode of operation are in fact due to solitary particles from small showers generated by 10–100 GeV cosmic rays. Working in single particle mode, an air shower array could in principle detect a GRB in the energy range 1–10 3 GeV, if the secondary particles generated by the gamma-rays ...
... detected in this mode of operation are in fact due to solitary particles from small showers generated by 10–100 GeV cosmic rays. Working in single particle mode, an air shower array could in principle detect a GRB in the energy range 1–10 3 GeV, if the secondary particles generated by the gamma-rays ...
The Gaseous Halo of NGC 891 Edmund Hodges-Kluck Joel Bregman
... lines with an impact parameter of 5 kpc • We also developed a new method to constrain Z in an imaging sense using dust-scattered light • Halos are dusty (Menard+2010); dust visible in: • Emission (mid-IR; sky is bright; stars) ...
... lines with an impact parameter of 5 kpc • We also developed a new method to constrain Z in an imaging sense using dust-scattered light • Halos are dusty (Menard+2010); dust visible in: • Emission (mid-IR; sky is bright; stars) ...
How is Light Made?
... Now the particle nature of EM radiation. These little packets of light is known as photons. These photons carry a certain energy which is related to its frequency. This energy is equal to Planck’s constant (h) multiplied by the frequency of the photon. By substituting “nu” with the equation in the p ...
... Now the particle nature of EM radiation. These little packets of light is known as photons. These photons carry a certain energy which is related to its frequency. This energy is equal to Planck’s constant (h) multiplied by the frequency of the photon. By substituting “nu” with the equation in the p ...
1Ctauber.pdf
... The CMB is not exhausted We need an experiment which: • Has a sensitivity at least 10x better than WMAP • Has an angular resolution at least 2x better than WMAP • Can map the polarization of the CMB over the whole sky • Can cope with systematics and local signals Such an experiment is ~1000x more p ...
... The CMB is not exhausted We need an experiment which: • Has a sensitivity at least 10x better than WMAP • Has an angular resolution at least 2x better than WMAP • Can map the polarization of the CMB over the whole sky • Can cope with systematics and local signals Such an experiment is ~1000x more p ...
WFXT_Pareschi
... was to scan the sky and to detect distant clusters of galaxies through their X-ray emission. The idea was that it would be possible to equal or exceed the sensitivity of Chandra with an X-ray telescope of one tenth the area (and cost). This could be achieved by dedicating an entire mission of a smal ...
... was to scan the sky and to detect distant clusters of galaxies through their X-ray emission. The idea was that it would be possible to equal or exceed the sensitivity of Chandra with an X-ray telescope of one tenth the area (and cost). This could be achieved by dedicating an entire mission of a smal ...
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.