ppt 2.6 - NRAO: Socorro, New Mexico
... (Lucy & Solomon 1970; Feldmeier 1998). Shocks can form and produce observable emission – X-rays: soft, non-variable – NT radio? ...
... (Lucy & Solomon 1970; Feldmeier 1998). Shocks can form and produce observable emission – X-rays: soft, non-variable – NT radio? ...
The Astronomical Search for Origins
... NASA SMD Astrophysics: Discover the origin, structure, evolution, and destiny of the universe, and search for Earthlike planets ...
... NASA SMD Astrophysics: Discover the origin, structure, evolution, and destiny of the universe, and search for Earthlike planets ...
4242 MR304SC Spec.indd
... The system features simultaneous data acquisition from the two output ports (configured with a MCT and an InSb detector). One input port is used to fix a reference cancellation source. The other input port is designed to receive an input telescope and a viewing device. The MR304SC is equipped with sti ...
... The system features simultaneous data acquisition from the two output ports (configured with a MCT and an InSb detector). One input port is used to fix a reference cancellation source. The other input port is designed to receive an input telescope and a viewing device. The MR304SC is equipped with sti ...
Numerical solution of the radiative transfer equation: X
... Comptonization region is τ > ∼ 1. The regime of low temperature and high optical depth of the plasma indeed ensures that the spectrum is almost isotropized, so that it is possible to use ...
... Comptonization region is τ > ∼ 1. The regime of low temperature and high optical depth of the plasma indeed ensures that the spectrum is almost isotropized, so that it is possible to use ...
SOAR Spartan Infrared Camera E. Loh, MSU, July 2014
... The Spartan Infrared Camera operates in the 1–2.4μm wavelength range. It has two focal ratios, a wide-field (WF) configuration with 66 mas/pixel a high-res (HR) configuration with 40 mas/pixel, which has not proved to be useful. The detectors are four HAWAII-2 arrays, each with 2048×2048 pixels. Bes ...
... The Spartan Infrared Camera operates in the 1–2.4μm wavelength range. It has two focal ratios, a wide-field (WF) configuration with 66 mas/pixel a high-res (HR) configuration with 40 mas/pixel, which has not proved to be useful. The detectors are four HAWAII-2 arrays, each with 2048×2048 pixels. Bes ...
B - Astronomy
... A spectral line detected from the left limb of Venus is found to be of a longer wavelength than the same line detected on the right limb. Which side is approaching us? a. b. c. ...
... A spectral line detected from the left limb of Venus is found to be of a longer wavelength than the same line detected on the right limb. Which side is approaching us? a. b. c. ...
Can we determine the grain composition of the Interstellar Medium with
... empirical XAFS data taken at synchrotron beamlines to determine exact chemical state of the astrophysical dust Recent measurements of soft X-ray XAFS at ALS (Sept 04) FUTURE MISSIONS : area + spectral resolution ...
... empirical XAFS data taken at synchrotron beamlines to determine exact chemical state of the astrophysical dust Recent measurements of soft X-ray XAFS at ALS (Sept 04) FUTURE MISSIONS : area + spectral resolution ...
Lecture 3
... radiation, including stars, planets, and you. • An object’s thermal radiation spectrum depends on only one property: its temperature. • A blackbody is an ideal emitter that absorbs all incident energy and reradiates the energy. • We can use this to determine the temperatures of stars and planets. ...
... radiation, including stars, planets, and you. • An object’s thermal radiation spectrum depends on only one property: its temperature. • A blackbody is an ideal emitter that absorbs all incident energy and reradiates the energy. • We can use this to determine the temperatures of stars and planets. ...
Swift and NuSTAR observations of XTE J1859+083
... The topic of this thesis is to investigate the X-ray binary system XTE J1859+083 with performed observations by the NuSTAR and Swift telescopes. The X-ray source was discovered in 1999 (Marshall et al., 1999) with the Rossi X-ray Timing Explorer (RXTE). Since the detection the field around the sourc ...
... The topic of this thesis is to investigate the X-ray binary system XTE J1859+083 with performed observations by the NuSTAR and Swift telescopes. The X-ray source was discovered in 1999 (Marshall et al., 1999) with the Rossi X-ray Timing Explorer (RXTE). Since the detection the field around the sourc ...
3-0898-belz
... Introduction: HiRes • HiRes is a two-eyed nitrogen fluorescence experiment studying UHE cosmic rays. • Monocular: Wide energy range (1017.4 < E < 1020.5 eV), best statistics. • Stereo: best reconstruction, covers 1018.5 < E < 1020.5 eV. • Located at the army’s Dugway ...
... Introduction: HiRes • HiRes is a two-eyed nitrogen fluorescence experiment studying UHE cosmic rays. • Monocular: Wide energy range (1017.4 < E < 1020.5 eV), best statistics. • Stereo: best reconstruction, covers 1018.5 < E < 1020.5 eV. • Located at the army’s Dugway ...
1 Particle Interaction with Matter and Detectors
... Particle (nuclear) physics led the way in detector (and other e.g. WWW) developments which had major impact on other fields of science, technology, medicine and everyday’s life. ...
... Particle (nuclear) physics led the way in detector (and other e.g. WWW) developments which had major impact on other fields of science, technology, medicine and everyday’s life. ...
1.3 Accretion power in astrophysics
... The infalling matter have some angular momentum ( the secondary star is orbiting the compact object when the gas comes off the star, it, too will orbit the compact object) and conservation of angular momentum prevents matter from falling directly into the black hole) X-ray Binaries, Lewin, van Parad ...
... The infalling matter have some angular momentum ( the secondary star is orbiting the compact object when the gas comes off the star, it, too will orbit the compact object) and conservation of angular momentum prevents matter from falling directly into the black hole) X-ray Binaries, Lewin, van Parad ...
High-Energy Astrophysics
... However in high-energy astrophysical situations we find the inverse of this process often occurs. With relativistic, or extremely hot thermal electrons, scattering against radio-wavelength photons, the photons are scattered up to high energy at the expense of the electron energy. To calculate the ra ...
... However in high-energy astrophysical situations we find the inverse of this process often occurs. With relativistic, or extremely hot thermal electrons, scattering against radio-wavelength photons, the photons are scattered up to high energy at the expense of the electron energy. To calculate the ra ...
Shocking Truth about Massive Stars Lidia Oskinova Chandra’s First Decade of Discovery
... Our analysis indicates that star may be a FAST ROTATOR V rot sin i =4000 km/s. Current mass ~10 M ...
... Our analysis indicates that star may be a FAST ROTATOR V rot sin i =4000 km/s. Current mass ~10 M ...
PRESENTAZIONE WORKSHOP ASDC
... The Simbol-X project, and the collaboration with the French partners, unfortunately stopped, brought a lot of experience on this kind of mission, for both scientific and engineering issues. Feasibility of Exit-Sat and Simbol-X missions at the end of the projects phase A has been proved. By the w ...
... The Simbol-X project, and the collaboration with the French partners, unfortunately stopped, brought a lot of experience on this kind of mission, for both scientific and engineering issues. Feasibility of Exit-Sat and Simbol-X missions at the end of the projects phase A has been proved. By the w ...
A model of the X-ray response of the ACIS CCD
... edge in Si02 , which is different from the silicon absorption edge in the crystalline silicon. We have shown5 exists a 6 eV difference between the silicon absorption edge energies in Si and Si02 and the jump at 1846 eV is a clear indication to the Si02 origin of the peak. Our general scheme of model ...
... edge in Si02 , which is different from the silicon absorption edge in the crystalline silicon. We have shown5 exists a 6 eV difference between the silicon absorption edge energies in Si and Si02 and the jump at 1846 eV is a clear indication to the Si02 origin of the peak. Our general scheme of model ...
ML 5037-40
... the shape when 100V was applied to the center element, (b) , (c), (d) are the shapes when 100 V was applied to one element in the 1st, 2nd, and ...
... the shape when 100V was applied to the center element, (b) , (c), (d) are the shapes when 100 V was applied to one element in the 1st, 2nd, and ...
Lecture 4a - University of Rochester
... energy with its surrounding and a steady state is reached where there is no net energy flow. • To maintain a steady state the body must emit radiation at the same rate that it is absorbed. • A black body is an object that absorbs equally well radiation at all wavelengths. • A black body is described ...
... energy with its surrounding and a steady state is reached where there is no net energy flow. • To maintain a steady state the body must emit radiation at the same rate that it is absorbed. • A black body is an object that absorbs equally well radiation at all wavelengths. • A black body is described ...
arXiv 2011 Feroci
... steady progression of ever larger-area, hence more sensitive, X-ray timing instrumentation, from Uhuru (US, 0.08 m2 , [11]), via satellites such as EXOSAT (ESA, [21]) and Ginga (Japan, [29]) to, most recently, RXTE (US, 0.6 m2 , [27]). The latter instrument, thanks to it having the largest area so f ...
... steady progression of ever larger-area, hence more sensitive, X-ray timing instrumentation, from Uhuru (US, 0.08 m2 , [11]), via satellites such as EXOSAT (ESA, [21]) and Ginga (Japan, [29]) to, most recently, RXTE (US, 0.6 m2 , [27]). The latter instrument, thanks to it having the largest area so f ...
X-ray studies of star and planet formation Eric Feigelson
... 5. Establishing the stellar Initial Mass Function Near- and mid-infrared surveys can readily detect photospheres of the full IMF, including proto-brown dwarfs, out to 1-2 kpc. But, except in the closest star forming regions (e.g. Taurus, Orion), the fields are very badly (factors ~ few-100) contami ...
... 5. Establishing the stellar Initial Mass Function Near- and mid-infrared surveys can readily detect photospheres of the full IMF, including proto-brown dwarfs, out to 1-2 kpc. But, except in the closest star forming regions (e.g. Taurus, Orion), the fields are very badly (factors ~ few-100) contami ...
wdm_shanghai_Mayinzhe
... For m_X > 5keV, star formation efficiency is degenerated with WDM For low mass, the two are not degenerated. This is observable by the high-redshift measurement such as square kilometer array (2020). ...
... For m_X > 5keV, star formation efficiency is degenerated with WDM For low mass, the two are not degenerated. This is observable by the high-redshift measurement such as square kilometer array (2020). ...
Lecture 1, Overview and Basic Concepts (April 2)
... - FUSE (1999-2007), high-res spectroscopy, 90-120 nm - GALEX (2003-2011), UV surveys, imaging and spectroscopic observations in two bands: Far UV 1350-1780Å and Near UV 1770-2730Å ...
... - FUSE (1999-2007), high-res spectroscopy, 90-120 nm - GALEX (2003-2011), UV surveys, imaging and spectroscopic observations in two bands: Far UV 1350-1780Å and Near UV 1770-2730Å ...
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.