![Cosmic Feedback from Supermassive Black Holes](http://s1.studyres.com/store/data/007747359_2-65211ceb3e639391267ab81166527403-300x300.png)
Cosmic Feedback from Supermassive Black Holes
... How did feedback from black holes influence the growth of structure? 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 hol ...
... How did feedback from black holes influence the growth of structure? 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 hol ...
eROSITA Mission Definition Document
... Most of the light created after the «dark ages» in the Universe comes from active centres of galaxies, emitted either by vigorous star formation processes or by prodigious supermassive black holes residing in the centre of almost every galaxy, swallowing stars and gas. It was only realized in recent ...
... Most of the light created after the «dark ages» in the Universe comes from active centres of galaxies, emitted either by vigorous star formation processes or by prodigious supermassive black holes residing in the centre of almost every galaxy, swallowing stars and gas. It was only realized in recent ...
blackbody
... and electrons in the material itself. Before this radiation reaches the surface and is emitted, it has been absorbed and reemitted many times within the material which “washes out” the original spectral information. Therefore the spectral emittance is sculpted into a smooth function of the wavelengt ...
... and electrons in the material itself. Before this radiation reaches the surface and is emitted, it has been absorbed and reemitted many times within the material which “washes out” the original spectral information. Therefore the spectral emittance is sculpted into a smooth function of the wavelengt ...
Superconducting Detectors: Sensitivity Over Ten Orders of Magnitude
... Below 40 GHz, the universe is classical (many photons per mode). The Universe has a temperature of about T=2.7 K (the afterglow of the Big Bang). The number of photons is determined by the temperature through Bose-Einstein statistics: ...
... Below 40 GHz, the universe is classical (many photons per mode). The Universe has a temperature of about T=2.7 K (the afterglow of the Big Bang). The number of photons is determined by the temperature through Bose-Einstein statistics: ...
Astronomy with mm-Mpc lenses - SLAC
... X-ray Detectors Band gap in silicon is a few eV One optical photon excites one electron in the CCD pixel No energy information X-ray photons deposit all their energy: charge proportional to energy. Dependent on frequent readout X-ray images are colour! Reflection grating spectrometers can be used t ...
... X-ray Detectors Band gap in silicon is a few eV One optical photon excites one electron in the CCD pixel No energy information X-ray photons deposit all their energy: charge proportional to energy. Dependent on frequent readout X-ray images are colour! Reflection grating spectrometers can be used t ...
Multiwavelength Imaging of Planetary Nebulae: Resolving Disentangling PN Structure
... Utilizing the CHANPLANS data for 14 PNe that exhibit diffuse X-ray emission, we constructed simple, spherically symmetric two-phase models using the astrophysical modeling tool, SHAPE. Our models consisted of a hot bubble and swept-up shell with the intent of investigating the X-ray morphology of th ...
... Utilizing the CHANPLANS data for 14 PNe that exhibit diffuse X-ray emission, we constructed simple, spherically symmetric two-phase models using the astrophysical modeling tool, SHAPE. Our models consisted of a hot bubble and swept-up shell with the intent of investigating the X-ray morphology of th ...
Mysterious transient objects - NCRA
... Flashes of gamma-rays from random directions in sky Few milliseconds to few seconds timescale Even 100 times more energetic than supernovae Brightest sources of cosmic gamma-ray photons in the universe In universe roughly 1 GRB is detected per day Short duration (< 2 sec) and long duration (> ...
... Flashes of gamma-rays from random directions in sky Few milliseconds to few seconds timescale Even 100 times more energetic than supernovae Brightest sources of cosmic gamma-ray photons in the universe In universe roughly 1 GRB is detected per day Short duration (< 2 sec) and long duration (> ...
W The X-Ray Universe X-ray images of the Universe are
... nuclei of galaxies, and hot gas in intergalactic space. The X rays detected by X-ray astronomers, like those put to use in industry, medicine, and laboratory research, must be produced by high-energy particles. It is not surprising, then, that an X-ray image of the sky can look markedly different fr ...
... nuclei of galaxies, and hot gas in intergalactic space. The X rays detected by X-ray astronomers, like those put to use in industry, medicine, and laboratory research, must be produced by high-energy particles. It is not surprising, then, that an X-ray image of the sky can look markedly different fr ...
Week_1
... Turbulence: Limit angular resolution to ~1 arc-second “Backgrounds”: flux from various sources limits sensitivity. Visual: ...
... Turbulence: Limit angular resolution to ~1 arc-second “Backgrounds”: flux from various sources limits sensitivity. Visual: ...
PHYSICAL PROPERTIES OF THE AXP 4U 0142+61 FROM X
... (92 ) higher than the value reported by Durant & van Kerkwijk (2006a) through a different and spectral model-independent analysis. Because it shows this large disagreement, we also tried a fit where the column density is fixed at the latter value. The resulting fit is unacceptable, with 2 ¼ 3:83 ...
... (92 ) higher than the value reported by Durant & van Kerkwijk (2006a) through a different and spectral model-independent analysis. Because it shows this large disagreement, we also tried a fit where the column density is fixed at the latter value. The resulting fit is unacceptable, with 2 ¼ 3:83 ...
end-of-summer report
... observation identifications that correspond to Chandra and XMM-Newton observations (see Tables 3 and 4 for a list of all IDs). Because the CDFS contains stellar sources that are faint compared to the background noise, we decided not to subtract the background. When subtracted, the total flux during ...
... observation identifications that correspond to Chandra and XMM-Newton observations (see Tables 3 and 4 for a list of all IDs). Because the CDFS contains stellar sources that are faint compared to the background noise, we decided not to subtract the background. When subtracted, the total flux during ...
Accreting magnetars: a new type of high-mass X-ray binaries? P. Reig,
... omits parts of the detector area like border pixels and columns with higher offset. Although the observation were made in the ‘partial window’ mode, the brightness of the source was so high that the EPIC instruments were affected by pile-up. Because the PN camera has a faster read-out time, it is le ...
... omits parts of the detector area like border pixels and columns with higher offset. Although the observation were made in the ‘partial window’ mode, the brightness of the source was so high that the EPIC instruments were affected by pile-up. Because the PN camera has a faster read-out time, it is le ...
SSS in young stellar populations: progenitors of the
... • Two sources appear to be slightly evolved massive stars • Third source, RX J0040.0+4100 too hot for models – could be due to presence of irradiated disk? ...
... • Two sources appear to be slightly evolved massive stars • Third source, RX J0040.0+4100 too hot for models – could be due to presence of irradiated disk? ...
Round table on medical applications
... micropattern gaseous detectors for high energy physics, astrophysics and medical applications In the last two decades very fast developments happened in the filed of gaseous detectors of photons and particles. Traditional gases detectors: wire–type and parallel plate-type (RPCs) -which are widely us ...
... micropattern gaseous detectors for high energy physics, astrophysics and medical applications In the last two decades very fast developments happened in the filed of gaseous detectors of photons and particles. Traditional gases detectors: wire–type and parallel plate-type (RPCs) -which are widely us ...
CHANDRA on ,
... fluorescence is always accompanied by the presence of a K edge in massive binaries. This edge is produced by those photons energetic enough to ionize the innermost K shell electrons of the atom. This hole is subsequently replenished by an electron from the upper level producing the observed fluoresc ...
... fluorescence is always accompanied by the presence of a K edge in massive binaries. This edge is produced by those photons energetic enough to ionize the innermost K shell electrons of the atom. This hole is subsequently replenished by an electron from the upper level producing the observed fluoresc ...
transparencies - Rencontres de Moriond
... us to observe the very early universe, violent astrophysical events or exciting areas of new physics • Current detectors are now beginning observations of the Galactic Centre at GHz and Optical Frequencies • A two element interferometer is being designed jointly by Birmingham and Jodrell Bank ...
... us to observe the very early universe, violent astrophysical events or exciting areas of new physics • Current detectors are now beginning observations of the Galactic Centre at GHz and Optical Frequencies • A two element interferometer is being designed jointly by Birmingham and Jodrell Bank ...
An Archive of Chandra Observations of Regions of Star Formation...
... forming clouds to levels rivaling near-IR telescopes. These features allow novel investigations of star formation which is more massive, more embedded and more distant than previously possible. Using the point source database, one could follow the progression of luminosity and variability for variou ...
... forming clouds to levels rivaling near-IR telescopes. These features allow novel investigations of star formation which is more massive, more embedded and more distant than previously possible. Using the point source database, one could follow the progression of luminosity and variability for variou ...
Astronomy Astrophysics − Orbital phase-resolved spectroscopy of 4U 1538
... We extracted the orbital phase-averaged spectrum of 4U 1538−52 with MAXI/GSC for the same observation duration using the MAXI on-demand processing2. For spectral analysis we used the xspec version 12.8.1 (Arnaud 1996) fitting package, released as a part of xanadu in the HEASoft tools. We used FTOOLg ...
... We extracted the orbital phase-averaged spectrum of 4U 1538−52 with MAXI/GSC for the same observation duration using the MAXI on-demand processing2. For spectral analysis we used the xspec version 12.8.1 (Arnaud 1996) fitting package, released as a part of xanadu in the HEASoft tools. We used FTOOLg ...
Supernovae
... Neutrinos carry energy out of the star and provide momentum through collisions to throw off material. Or they heat the material so that it expands. They have no mass (like photons) and can traverse large depths without being absorbed. ...
... Neutrinos carry energy out of the star and provide momentum through collisions to throw off material. Or they heat the material so that it expands. They have no mass (like photons) and can traverse large depths without being absorbed. ...
Handout
... Absorption and scatter will decrease energy reaching sensor, leading to underestimate of temperature Emission in atmosphere will increase energy reaching sensor, leading to overestimate of temperature Radiant/brightness temperature (measured by sensor) will be less than true (kinetic) temperature Tw ...
... Absorption and scatter will decrease energy reaching sensor, leading to underestimate of temperature Emission in atmosphere will increase energy reaching sensor, leading to overestimate of temperature Radiant/brightness temperature (measured by sensor) will be less than true (kinetic) temperature Tw ...
Svoboda, PPTX, 14 MB
... 3. We may not be able to take all events in a close SN. If the DAQ becomes saturated, we may have to either stop data taking at some point or pre-scale recording events. For example, we could record only 20% of all incoming data in order to get an unbiased snapshot of the whole burst. What is the be ...
... 3. We may not be able to take all events in a close SN. If the DAQ becomes saturated, we may have to either stop data taking at some point or pre-scale recording events. For example, we could record only 20% of all incoming data in order to get an unbiased snapshot of the whole burst. What is the be ...
Inverse Square Law, Blackbody Radiation y
... measured in watts. A source of light with a luminosity of 1 watt emits one joule of energy per ...
... measured in watts. A source of light with a luminosity of 1 watt emits one joule of energy per ...
ppt - Astronomy at Swarthmore College
... Some of the other hot stars observed with Chandra show broad, blueshifted, and asymmetric line profiles, similar to those seen in ζ Pup But…some hot stars have x-ray spectra with quite narrow lines, that are especially strong and high energy - not consistent with line-force instability wind shocks ...
... Some of the other hot stars observed with Chandra show broad, blueshifted, and asymmetric line profiles, similar to those seen in ζ Pup But…some hot stars have x-ray spectra with quite narrow lines, that are especially strong and high energy - not consistent with line-force instability wind shocks ...
Using the Electromagnetic Spectrum
... time. By giving us a snapshot of the temperature roughly every two years for the past decade. ...
... time. By giving us a snapshot of the temperature roughly every two years for the past decade. ...
X-ray astronomy detector
![](https://commons.wikimedia.org/wiki/Special:FilePath/Ill-2_O3.jpg?width=300)
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.