A high-resolving-power x-ray spectrometer for the OMEGA EP Laser (invited)

2016 ◽  
Vol 87 (11) ◽  
pp. 11D504 ◽  
Author(s):  
P. M. Nilson ◽  
F. Ehrne ◽  
C. Mileham ◽  
D. Mastrosimone ◽  
R. K. Jungquist ◽  
...  
Keyword(s):  
Resolving Power ◽  
X Ray

scholarly journals ESA’s X-Ray Astronomy Mission, XMM

1990 ◽  
Vol 123 ◽  
pp. 129-140
Author(s):  
B.G. Taylor ◽  
A. Peacock
Keyword(s):  
Resolving Power ◽  
Science Program ◽  
Eccentric Orbit ◽  
Ccd Cameras ◽  
Optical Telescope ◽  
X Ray ◽  
Medium Resolution ◽  
Reflection Gratings ◽  
Better Than

AbstractESA’s X-ray Astronomy Mission, XMM, scheduled for launch in 1998, is the second of four cornerstones of ESA’s long term science program Horizon 2000. Covering the range from about 0.1 to 10 keV, it will provide a high throughput of 5000 cm2 at 7 keV with three independant telescopes, and have a spatial resolution better than 30 arcsec. Broadband spectrophotometry is provided by CCD cameras while reflection gratings provide medium resolution spectroscopy (resolving power of about 400) in the range 0.3–3 keV. Long uninterrupted observations will be made from the 24 hr period, highly eccentric orbit, reaching a sensitivity approaching 10−15 erg cm−2 s−1 in one orbit. A 30 cm UV/optical telescope is bore-sighted with the x-ray telescopes to provide simultaneous optical counterparts to the numerous serendipitous X-ray sources which will be detected during every observation.

scholarly journals X-ray spectrometer having 12 000 resolving power at 8 keV energy

2017 ◽  
Vol 88 (10) ◽  
pp. 103107 ◽  
Author(s):  
John F. Seely ◽  
Lawrence T. Hudson ◽  
Albert Henins ◽  
Uri Feldman
Keyword(s):  
Resolving Power ◽  
X Ray

scholarly journals Disentangling AGN and starburst activities in NGC 6240 from an X-ray perspective

2014 ◽  
Vol 10 (S312) ◽  
pp. 36-38
Author(s):  
Junfeng Wang
Keyword(s):  
Active Galactic Nuclei ◽  
Large Scale ◽  
Imaging Spectroscopy ◽  
Galactic Nuclei ◽  
Resolving Power ◽  
High Excitation ◽  
X Ray ◽  
Supermassive Black Hole ◽  
X Ray Imaging ◽  
High Temperature Gas

AbstractThe circum-nuclear region in an active galaxy is often complex with presence of high excitation gas, collimated radio outflow, and star formation activities, besides the actively accreting supermassive black hole. The unique spatial resolving power of Chandra X-ray imaging spectroscopy enables more investigations to disentangle the active galactic nuclei and starburst activities. For galaxies in the throes of a violent merging event such as NGC6240, we were able to resolve the high temperature gas surrounding its binary active black holes and discovered a large scale soft X-ray halo.

scholarly journals Demonstration of resolving power λ/Δλ > 10,000 for a space-based x-ray transmission grating spectrometer

2019 ◽  
Vol 58 (5) ◽  
pp. 1223 ◽  
Author(s):  
Ralf K. Heilmann ◽  
Jeffery Kolodziejczak ◽  
Alexander R. Bruccoleri ◽  
Jessica A. Gaskin ◽  
Mark L. Schattenburg
Keyword(s):  
Resolving Power ◽  
X Ray ◽  
Transmission Grating ◽  
Grating Spectrometer

scholarly journals Innovative Techniques for X-ray Calorimetry

1990 ◽  
Vol 115 ◽  
pp. 357-360
Author(s):  
S. Labov ◽  
E. Silver ◽  
D. Landis ◽  
N. Madden ◽  
F. Goulding ◽  
...  
Keyword(s):  
Detection System ◽  
Light Emitting Diode ◽  
Thermal Response ◽  
Diagnostic Procedures ◽  
Resolving Power ◽  
Infrared Light ◽  
Temperature Control System ◽  
Thermal Detector ◽  
X Ray ◽  
Noise Characteristics

AbstractIn our x-ray calorimetry effort, we have developed several techniques which may be helpful to other groups working in this field. We are studying several different monolithic and composite calorimeter designs. In our readout configuration, the preamplifier circuit employs negative voltage feedback which allows us to accurately measure the temporal profile of the thermal pulse produced by an x-ray absorbed in a micro-calorimeter. Rise times of less than two microseconds have been observed in monolithic devices operating at .3 K. Furthermore, the feedback preamplifier can be configured for either positive or negative electro-thermal feedback. This preamplifier system is followed by an analog pulse shaping amplifier with a frequency response that can be adjusted to yield the maximum signal to noise ratio for a given thermal response of the calorimeter. In addition, we have developed several diagnostic procedures which have been useful in determining the operating and noise characteristics of our devices. These include an infrared light-emitting diode which flashes a discrete amount of energy on to the calorimeter, and a capacitively coupled test input to the preamplifier which allows us to directly determine the total noise in the thermal detection system. Finally, we are developing an adiabatic demagnetization refrigerator with a temperature control system that is designed to stabilize the 0.1 K cold stage to better than 8 μK. This is required for a resistive thermal detector with resolving power of 1000.

Recent Applications with the X-Ray Microscope

1957 ◽  
Vol 1 ◽  
pp. 483-494
Author(s):  
Selby E. Summers
Keyword(s):  
Resolving Power ◽  
Depth Of Field ◽  
Specimen Preparation ◽  
X Rays ◽  
Optical Instrument ◽  
X Ray ◽  
Technical Details ◽  
The Many ◽  
Preparation Techniques ◽  
Shadow Projection

AbstractThe X-ray microscope is an electrostatic optical instrument employing X-rays for shadow projection to magnify and reveal detailed internal structure of specimens opaque to light or electrons. Its many advantages — high resolving power, greater penetration, large depth of field, and stereographic presentation — make the X-ray Microscope a versatile instrument for industrial research and development. Because the instrument was recently introduced, little information is available on specimen preparation techniques, or types of specimens suitable for study. A few of the many possible applications will be discussed, as well as a brief review of the technical details of the instrument.

scholarly journals Multiwavelength campaign on Mrk 509

2019 ◽  
Vol 623 ◽  
pp. A82 ◽  
Author(s):  
G. A. Kriss ◽  
N. Arav ◽  
D. Edmonds ◽  
J. Ely ◽  
J. S. Kaastra ◽  
...  
Keyword(s):  
High Energy ◽  
Resolving Power ◽  
Host Galaxy ◽  
Active Nucleus ◽  
X Ray ◽  
Transmission Grating ◽  
Outflow Rate ◽  
Mass Outflow ◽  
Far Ultraviolet ◽  
The Impact

Aims. To elucidate the location, physical conditions, mass outflow rate, and kinetic luminosity of the outflow from the active nucleus of the Seyfert 1 galaxy Mrk 509, we used coordinated UV and X-ray spectral observations in 2012 to follow up our lengthier campaign conducted in 2009. Methods. We observed Mrk 509 with the Cosmic Origins Spectrograph (COS) on the Hubble Space Telescope (HST) on 2012-09-03 and 2012-10-11 coordinated with X-ray observations using the High Energy Transmission Grating on the Chandra X-ray Observatory. Our far-ultraviolet spectra used grating G140L on COS to cover wavelengths from 920–2000 Å at a resolving power of ∼2000, and gratings G130M and G160M to cover 1160–1750 Å at a resolving power of ∼15, 000. Results. We detect variability in the blueshifted UV absorption lines on timescales spanning 3–12 years. The inferred densities in the absorbing gas are greater than log n cm−3 ∼ 3. For ionization parameters ranging over log U = −1.5 to −0.2, we constrain the distances of the absorbers to be closer than 220 pc to the active nucleus. Conclusions. The impact on the host galaxy appears to be confined to the nuclear region.

Construction of the JAERI soft X-ray beamline for actinide material sciences

1998 ◽  
Vol 5 (3) ◽  
pp. 536-538 ◽  
Author(s):  
Takeshi Nakatani ◽  
Yuji Saitoh ◽  
Yuden Teraoka ◽  
Tetsuo Okane ◽  
Akinari Yokoya
Keyword(s):  
Photochemical Reactions ◽  
Resolving Power ◽  
Photoemission Spectroscopy ◽  
X Rays ◽  
Radioactive Materials ◽  
X Ray ◽  
Line Spacing ◽  
Material Sciences ◽  
Spectroscopy Studies ◽  
Under Construction

An undulator beamline for spectroscopy studies focusing on the electronic structure of actinide materials is under construction. Linearly or circularly polarized soft X-rays are provided by employing a variably polarizing undulator. Varied-line-spacing plane gratings and a sagittal-focusing system are used to monochromatize the undulator beam, whose energy ranges from 0.3 to 1.5 keV. A resolving power of 104 is expected in the whole energy region. These components are methodically operated by the SPring-8 beamline control system. There are three experimental stations in the beamline. In one of the stations the photoemission spectroscopy experiments are carried out at a radioisotope-controlled area where actinide compounds as well as unsealed radioactive materials are usable. Other experimental stations are planned in the beamline for surface photochemical reactions and biological applications.

scholarly journals Differences in the directions of ejection of x-ray photo-electrons from various atomic levels

1929 ◽  
Vol 126 (800) ◽  
pp. 138-143 ◽  
Keyword(s):  
Resolving Power ◽  
X Rays ◽  
Expansion Chamber ◽  
X Ray ◽  
Chamber Method ◽  
Heavy Atoms ◽  
Intensity Measurements ◽  
The Individual ◽  
Radio Corporation Of America ◽  
Slow Electrons

Very valuable studies of the directions in which photo-electrons are ejected by X-rays have been made recently by Williams, Auger, and Anderson. All of these observers, however, used the C. T. R. Wilson expansion-chamber method which, in spite of its power in working with the individual electron, suffers from the disadvantage that the particular energy level in the atom from which the electron is ejected in general cannot be determined. It is true that in the case of heavy atoms such as xenon and bromine, Auger and Anderson succeeded, through the use of X-rays of particular energies, in distinguishing the electrons thrown out of the K level from those thrown out of the L levels, but to go much further in this direction by the expansion-chamber method (and, for example, to distinguish the L I from the L II or L III electrons) seems hopeless. Consequently, the magnetic spectrograph developed by one of us for studying the velocity of the X-ray electrons as a function of the angle of emission was applied to the problem with the results which it is the purpose of this paper to describe. We, as yet, have not succeeded in determining the actual directions of ejection with the precision which has been attained in the expansion-chamber method, but the resolving power of the apparatus for velocities is so large that the particular level in which each electron group originates is in general quite unambiguous. A description of the apparatus used and the procedure followed has been given in the paper referred to above and need not be repeated here. Ballast lamps of the sort developed at the General Electric Company and sold by the Radio Corporation of America (radiotron UV-886) have proved very useful in holding the current through the solenoid which produces the magnetic field constant during the long exposures (100-200 hours) which are necessary. Eastman X-ray plates were used throughout, as they have been found to be the most sensitive of any so far tried (except Schumann plates which are much too irregular for intensity measurements). The work has been seriously handicapped by the lack of sensibility of the photographic plates for slow electrons and by their rapid falling off in sensibility for electrons of velocities below about 12,000 volts. X-ray tubes with silver, molybdenum and copper anticathodes were used. The characteristic radiation from copper is, however, in spite of its intrinsic intensity, too soft to eject electrons with sufficient velocity to give photographic results in a reasonable length of time with the apparatus used. All the results shown below consequently were obtained with the characteristic rays of either silver or molybdenum.

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