Notes-EM
... Red has the longest wavelength of all the colors. Violet has the shortest wavelength of all the colors. ...
... Red has the longest wavelength of all the colors. Violet has the shortest wavelength of all the colors. ...
Chandra - Astronomy at Swarthmore College
... Soft-X-ray emission is ubiquitous in O stars LX ~ 10-7 LBol (LX ~ 1031 to 1033 ergs s-1) soft thermal spectrum, kT ~ few 0.1 keV minimal time variability ...
... Soft-X-ray emission is ubiquitous in O stars LX ~ 10-7 LBol (LX ~ 1031 to 1033 ergs s-1) soft thermal spectrum, kT ~ few 0.1 keV minimal time variability ...
Chandra, Spitzer & VLA Observations of Young Clusters Scott Wolk - CxC/CfA
... The X-Ray data indicate a distance of ~600pc. Using two independent methods we find a total cluster size of about 300 stars. There appear to be 9 transition disks - 5 seen in X-rays. ...
... The X-Ray data indicate a distance of ~600pc. Using two independent methods we find a total cluster size of about 300 stars. There appear to be 9 transition disks - 5 seen in X-rays. ...
X-ray sources in the starburst spiral galaxy M 83
... with an uncertainty of 0.00 5, their total photon counts and their counts in three separate energy bands (0.3–1.0 keV, 1.0–2.0 keV and 2.0–8.0 keV) are listed in Table A.1. The positions of the ROSAT sources given in Table 3 of Immler et al. (1999) have a systematic offset ∆(RA) ' −0.s 5 and ∆(Dec) ...
... with an uncertainty of 0.00 5, their total photon counts and their counts in three separate energy bands (0.3–1.0 keV, 1.0–2.0 keV and 2.0–8.0 keV) are listed in Table A.1. The positions of the ROSAT sources given in Table 3 of Immler et al. (1999) have a systematic offset ∆(RA) ' −0.s 5 and ∆(Dec) ...
The Science of Solar B Transient phenomena
... current (and future) theories in order to have a deeper understanding of this fundamental process. ...
... current (and future) theories in order to have a deeper understanding of this fundamental process. ...
Hoffmann_Photon_Science_Novosibirsk_1__2015
... Abrixas space mission spare telescope - 160 cm focal length ...
... Abrixas space mission spare telescope - 160 cm focal length ...
Cones
... imaging systems for trauma. The typical trauma system has a fixed source-toimage receptor distance (SID) and is equipped with diaphragms designed to accommodate film sizes of 13×18 cm, 20×25 cm, and 25×30 cm. Radiographic imaging systems for trauma can be positioned to image all parts of the body ...
... imaging systems for trauma. The typical trauma system has a fixed source-toimage receptor distance (SID) and is equipped with diaphragms designed to accommodate film sizes of 13×18 cm, 20×25 cm, and 25×30 cm. Radiographic imaging systems for trauma can be positioned to image all parts of the body ...
Light, radiation, telescopes
... With no atmosphere, seeing is about .01 arc seconds for 10 m telescope ...
... With no atmosphere, seeing is about .01 arc seconds for 10 m telescope ...
PPT - LSC
... comes from extra solar planets • Many extra solar planets are found using many absorption lines (～5000) of nearby G type stars since small orbital motion up to 10m/s can be measured • Loeb (1998) proposed to apply this techniques to many QSO absorption lines so that two observations between ten year ...
... comes from extra solar planets • Many extra solar planets are found using many absorption lines (～5000) of nearby G type stars since small orbital motion up to 10m/s can be measured • Loeb (1998) proposed to apply this techniques to many QSO absorption lines so that two observations between ten year ...
Gravitational Wave Astronomy using 0.1Hz space laser interferometer
... comes from extra solar planets • Many extra solar planets are found using many absorption lines (～5000) of nearby G type stars since small orbital motion up to 10m/s can be measured • Loeb (1998) proposed to apply this techniques to many QSO absorption lines so that two observations between ten year ...
... comes from extra solar planets • Many extra solar planets are found using many absorption lines (～5000) of nearby G type stars since small orbital motion up to 10m/s can be measured • Loeb (1998) proposed to apply this techniques to many QSO absorption lines so that two observations between ten year ...
Astronomy Today, Chapter 3 Radiation 3
... ii. It is boosted to a higher energy b. Emission i. An electron emits a specific wavelength ii. It drops to a lower energy 7. Compare the absorption and emission lines of an element. a. They match b. The element’s electrons absorb and give off matching wavelengths The Particle Nature of Radiation 8. ...
... ii. It is boosted to a higher energy b. Emission i. An electron emits a specific wavelength ii. It drops to a lower energy 7. Compare the absorption and emission lines of an element. a. They match b. The element’s electrons absorb and give off matching wavelengths The Particle Nature of Radiation 8. ...
HEA_Accretion_2003_04
... • Gas loses angular momentum through collisions, shocks, viscosity and magnetic fields: kinetic energy converted into heat and radiated. • Matter sinks deeper into gravity of compact object ...
... • Gas loses angular momentum through collisions, shocks, viscosity and magnetic fields: kinetic energy converted into heat and radiated. • Matter sinks deeper into gravity of compact object ...
Quiescent and flaring X-ray emission from the nearby M/T dwarf
... and O vii at 21.6–22.1 Å, the RGS spectra are not suitable for a quantitative analysis. Thus we considered only X-ray data taken with the EPIC (European Photon Imaging Camera), consisting of two MOS and one PN detector; all detectors operated in the “Full frame” mode with the medium filter. The PN i ...
... and O vii at 21.6–22.1 Å, the RGS spectra are not suitable for a quantitative analysis. Thus we considered only X-ray data taken with the EPIC (European Photon Imaging Camera), consisting of two MOS and one PN detector; all detectors operated in the “Full frame” mode with the medium filter. The PN i ...
X-Ray Telescopes
... identification of a remnant’s compact object. None of these types of studies is readily undertaken with nonimaging instruments. Other imaging approaches employing such devices as modulation collimators or scanned, tightly collimated detectors provide much poorer resolution (∼1 arcmin.) than that ava ...
... identification of a remnant’s compact object. None of these types of studies is readily undertaken with nonimaging instruments. Other imaging approaches employing such devices as modulation collimators or scanned, tightly collimated detectors provide much poorer resolution (∼1 arcmin.) than that ava ...
High Energy Emission in Extragalactic Nonblazar Sources
... (Requires low-redshift GRB to avoid attenuation by diffuse IR background) Delayed high-energy g-ray emission from superbowl burst Seven GRBs detected with EGRET either during prompt MeV burst emission or after MeV emission has decayed away (Dingus et al. 1998) Average spectrum of 4 GRBs detected ove ...
... (Requires low-redshift GRB to avoid attenuation by diffuse IR background) Delayed high-energy g-ray emission from superbowl burst Seven GRBs detected with EGRET either during prompt MeV burst emission or after MeV emission has decayed away (Dingus et al. 1998) Average spectrum of 4 GRBs detected ove ...
GEARS Workshop Monday - Georgia Southern University
... • What are some of the things you notice about places where we find young stars? ...
... • What are some of the things you notice about places where we find young stars? ...
Optical studies of an ultraluminous X-ray source: NGC1313 X-2 Jifeng Liu
... • emission lines from X-ray illuminated accretion disks are broad, >1200 km/s • radial velocity for a stellar mass black hole lower than 300 km/s • He II line from X-ray photoionized nebula/secondary • line shift severely affected by noise • need further observations • with higher signal-to-noise ra ...
... • emission lines from X-ray illuminated accretion disks are broad, >1200 km/s • radial velocity for a stellar mass black hole lower than 300 km/s • He II line from X-ray photoionized nebula/secondary • line shift severely affected by noise • need further observations • with higher signal-to-noise ra ...
Wide-Field Optical Spectrometer (WFOS)
... the positions of targets are achromatic over the 0.31-1.0μm wavelength range. The instrument will include a closed-loop flexure compensation system that removes any instrument-rotator-dependent flexure at the required level to maintain image quality and the effectiveness of calibrations. The MOBIE o ...
... the positions of targets are achromatic over the 0.31-1.0μm wavelength range. The instrument will include a closed-loop flexure compensation system that removes any instrument-rotator-dependent flexure at the required level to maintain image quality and the effectiveness of calibrations. The MOBIE o ...
Demonstration of multilayer reflective optics at photon energies
... for extreme ultraviolet lithography,” Appl. Opt. 46, 3736 (2007). ...
... for extreme ultraviolet lithography,” Appl. Opt. 46, 3736 (2007). ...
The Extreme Universe of Gamma-ray Astronomy
... particles and light? And, how do the particles in the jets accelerate to near light speed? ...
... particles and light? And, how do the particles in the jets accelerate to near light speed? ...
the gzipped ps-file - INFN-LNF
... gas target consisting of specially chosen structure materials to supress fluorescence X ray radiation as far as possible. CCDs (Marconi Applied Technologies, CCD5530) were used as X-ray detectors. Their advantages are large area, pixel analysis capability for background reduction and excellent energ ...
... gas target consisting of specially chosen structure materials to supress fluorescence X ray radiation as far as possible. CCDs (Marconi Applied Technologies, CCD5530) were used as X-ray detectors. Their advantages are large area, pixel analysis capability for background reduction and excellent energ ...
cohen_paris_v2_may2009 - Astronomy at Swarthmore College
... Conclusions, pt. 2 Magnetic massive stars have harder spectra with narrower lines and rotationally modulated variability, in general agreement with MHD simulations. Line ratio diagnostics are useful for localizing the hot plasma, and indicate that the MHD simulations predict a location that is too ...
... Conclusions, pt. 2 Magnetic massive stars have harder spectra with narrower lines and rotationally modulated variability, in general agreement with MHD simulations. Line ratio diagnostics are useful for localizing the hot plasma, and indicate that the MHD simulations predict a location that is too ...
ULX accretion states
... inner disk modified by scattering-thick region at T ~ a few keV L ~ 1 – a few LEdd , M ~ 30 – 100 Msun ...
... inner disk modified by scattering-thick region at T ~ a few keV L ~ 1 – a few LEdd , M ~ 30 – 100 Msun ...
An exceptionally bright flare from SGR 1806–20 and the origins of
... saturated the detectors within 1 ms. The detectors emerged from saturation on the falling edge 200 ms later and remained unsaturated after that. Photons with energies * 20 keV are unattenuated; thus the amplitude variations in the oscillatory phase are real, and are not caused by any known instrumen ...
... saturated the detectors within 1 ms. The detectors emerged from saturation on the falling edge 200 ms later and remained unsaturated after that. Photons with energies * 20 keV are unattenuated; thus the amplitude variations in the oscillatory phase are real, and are not caused by any known instrumen ...
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.