Lexan coating to eliminate the UV sensitivity of soft X-ray proportional counters with a polypropylene window
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Fabricant, D. G.↗
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Results for “PROPORTIONAL COUNTER”
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Observations of SMC X-1 with the monitor proportional counter on the Einstein /HEAO 2/ X-ray Observatory - The pulse period and its history
The results of the sixth determination of the pulse period of the X-ray source SMC X-1 are presented. The observations were made in April 1979. The pulse period at this epoch was found to be (0.713683 + or - 0.000032) s referred to phase zero of the binary motion. This result together with all available historical data is utilized to quantify the observed trend toward spin-up. It is found that simple secular trends are not applicable. This finding is interpreted as evidence for additional variations in the pulse period. The obtained results are discussed in the context of present theoretical models for period variations in the binary pulsating X-ray sources. The apparent absence of spin-down episodes in the period history of SMC X-1 is also considered.
Darbro, W.↗
Penning gas mixtures for improving the energy resolution of proportional counters
An experimental investigation of the Penning effect in both argon and xenon has been carried out with a variety of quench gases of different ionization potentials. Acetylene with argon and trimethylamine with xenon show the strongest true Penning effect, returning very high gas gains for a given voltage and improved energy resolution over more conventional mixtures. Data for these mixtures, as well as others exhibiting weaker metastable effects, nonmetastable Penning effects, and charge transfer through photoionization, are presented.
Agrawal, P. C.↗
Imaging proportional counters for the stellar X-ray polarimeter
The xenon-filled IPCs being developed for the Stellar X-ray Polarimeter are described. The requirements placed on the IPCs by the design of the polarimeter are discussed and results on the performance of prototype counters are presented. The design of a prototype of the IPCs is described. Finally, the performance of the prototype is reported. Due to the extremely low count rates encountered in X-ray polarimetry, efficient background rejection is the most critical parameter of the IPCs. Using a background rejection scheme employing anticoincidence and pulse shape discrimination, a rejection efficiency of 99 percent has been achieved for Co-60-induced events over an energy range of 2 to 15 keV while retaining more than 80 percent of the X-ray efficiency.
Watkins, R. B., Jr.↗
The Effectiveness of the Proportional Counter With a Specially Designed Filter as a Solar X-Ray Monitor on the NEAR Mission
The X-ray instrument package on the Near Earth Asteroid Rendezvous (NEAR) spacecraft is designed to provide direct measurements of the major elemental abundances for the asteroid 433 Eros. These will be the first such measurements ever made for a 'primitive' body. For this task to be performed, simultaneous measurements must be provided of both the X-ray lines characteristic of major elements at the asteroid's surface as well as the solar flux, which is the source of these lines (1,2). The solar flux consists of a continuum which is generated by thermal bremstrahlung and radiative recombination, with superimposed major lines which result from emission due to transitions in H and He-like ions. The relative contribution of each component of the solar flux varies as the level of solar output changes, and thus solar output must be monitored to correct for varations in surface data caused by the changing levels of solar output.
Clark, P. E.↗
A Comprehensive Study of Pulse Profile Evolution in SGR 1806-20 and SGR 1900+14 with the Rossi X-ray Timing Explorer Proportional Counter Array
Soft gamma repeaters undergo pulse profile changes in connection with their burst activity. Here we present a comprehensive pulse profile history of SGR 1806-20 and SGR 1900+14 in three energy bands using Rossi X-Ray Timing Explorer/Proportiona1 Counter Array observations performed between 1996 and 2001. Using the Fourier harmonic powers of pulse profiles, we quantify the pulse shape evolution. Moreover, we determined the rms pulsed count rates (PCRs) of each profile. We show that the pulse profiles of SGR 1806-20 remain single pulsed, showing only modest changes for most of our observing span, while those of SGR 1900+14 change remarkably in all energy bands. Highly significant pulsations from SGR 1900+ 14 following the 1998 August 27 and 2001 April 18 bursts enabled us to study not only the decay of PCRs in different energy bands but also their correlations with each other.
Gogus, Ersin↗
The Soft Excess Emission in the Hercules Supercluster Observed with the ROSAT Position Sensitive Proportional Counter
Recent observations with the XMM-Newton satellite confirmed the existence of the soft excess phenomenon in galaxy clusters, earlier discovered in several EUVE, ROSAT and BeppoSAX observations. Excess of soft X-ray radiation in the spectra of several clusters -- above the contribution from the well-known hot intra-cluster gas -- is normally interpreted as emission from cooler gas (T~10^6 K) in the vicinity of galaxy clusters. In this paper we investigate the emission from three clusters in the Hercules concentration, MKW~S, A2052 and A2063. Available XMM observations for two of them (MKW~3s and A2052) indicate the presence of the excess emission, also associated with O VII emission lines. The clusters lie close to the North Polar Spur region, a portion of the sky which features strong soft X-ray emission. We analyze the ROSAT PSPC data of the three clusters and of eight other neighboring locations, in order to study the level of the local soft X-ray background and its influence on the determination of soft excess fluxes. Our analysis reveals that the North Polar Spur region has strong gradients in the soft X-ray emission, which render the background subtraction process quite cumbersome. Despite these complications, we are able to provide evidence for the presence of soft excess emission in the PSPC data of MKW~S, A2052 and A2063.
Bonamente, Massimiliana↗
An analysis of energy deposition in a tissue equivalent proportional counter onboard the space shuttle
An improved prediction for space radiations in the lower earth orbits measured by the shuttle TEPC is obtained when energy loss straggling and chord length distribution of the detector are considered. A generalized analytic model is used to describe the energy deposition of direct ion interaction events in a micron-size detector. The transport calculation accounting for the shuttle configuration is accomplished by using a new version of HZETRN that has been extensively verified with laboratory and flight data. The agreement of predicted and measured lineal energy spectra is within 70% for the region above 2 keV/micrometer but within a factor of 2.3 underpredicted for the region below this value. The inclusion of indirect delta ray events in the model is needed before possible causes for the underprediction below 2 keV/micrometer can be assessed.
Flight Experiment↗
Beamline and Flight Comparisons of the ARMAS Flight Module With the Tissue Equivalent Proportional Counter for Improving Atmospheric Radiation Monitoring Accuracy
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Brad “Buddy” Gersey↗
Calibration of the active radiation detector for Spacelab-One
The flight models of the active radiation detector (ARD) for the ENV-01 environmental monitor were calibrated using gamma radiation. Measured sensitivities of the ion chambers were 6.1 + or - 0.3 micron rad per count for ARD S/N1, and 10.4 + or - 0.5 micron rad per count for ARD S/N2. Both were linear over the measured range 0.10 to 500 m/rad hour. The particle counters (proportional counters) were set to respond to approximately 85% of minimum ionizing particles of unit charge passing through them. These counters were also calibrated in the gamma field.
Source record↗
The X-ray spectra of the BL Lacertae objects PKS 0548 - 322 and 3C 66A
Einstein Observatory simultaneous imaging proportional counter and monitor proportional counter data are combined in order to derive the energy spectra of the BL Lac objects PKS 0548-322 and 3C 66A between 0.2 and 10 keV. While the latter is found to be variable in both intensity and spectral shape, the former, although constant in the present data, is found to have experienced a spectrum variation in view of results from other experiments. Attention is given to the implications of flux and spectral variability in BL Lac objects for models of X-ray emission mechanisms. It is suggested that the wide spread of the spectral index distribution is due to the detection of the highly variable synchrotron-produced X-rays that are generally undetected in QSOs.
Maccacaro, T.↗
A broad band X-ray imaging spectrophotometer for astrophysical studies
A broadband X-ray imaging spectrophotometer (BBXRIS) has been built for astrophysical studies. The BBXRIS is based on a large-imaging gas scintillation proportional counter (LIGSPC), a combination of a gas scintillation proportional counter and a multiwire proportional counter, which achieves 8 percent (FWHM) energy resolution and 1.5-mm (FWHM) spatial resolution at 5.9 keV. The LIGSPC can be integrated with a grazing incidence mirror and a coded aperture mask to provide imaging over a broad range of X-ray energies. The results of tests involving the LIGSPC and a coded aperture mask are presented, and possible applications of the BBXRIS are discussed.
Lum, Kenneth S. K.↗
Chemical abundances of cosmic rays greater than 4.5 GV measured with a large area proportional counter-scintillation counter stack
A 6500 sq cm-ster cosmic-ray detector consisting of 12 gas counter trays sandwiched between two large-area circular scintillation counters was flown from Palestine, Texas in November 1972 to study the composition of primary particles greater than 1.5 GeV/nucleon in the charge range from 3 to 30. For each analyzed event, the particle trajectory was recorded, using four 20-wire proportional counter trays. Also recorded were the energy loss in each of the solid counters and the dE/dx losses in each of the 12 gas counters. The large dynamic range of the detector is established by operating six of the gas counters in the ionization mode. A description of the instrument and some preliminary results are given.
Lheureux, J.↗
Chemical abundances of cosmic rays greater than 4.5 GV measured with a large area proportional counter-scintillation counter stack
A 6500 sq cm-ster cosmic ray detector consisting of twelve gas counter trays sandwiched between two large area circular scintillation counters was flown from Palestine, Texas in November of 1972 to study the composition of primary particles 1.5 GeV/nucleon in the charge range 3 to 30. For each analyzed event, a recording was made of (1) the particle trajectory using four 20 wire proportional counter trays, (2) the energy loss in each of the solid counters, and (3) the dE/dx losses in each of the twelve gas counters. The large dynamic range of the detector is established by operating six of the gas counters in the ionization mode. A description of the instrument and some preliminary results are given.
Lheureux, J.↗
The nonstellar continuum of the Seyfert galaxy NGC 7213
The optical continuum of the nearby Seyfert galaxy NGC 7213 is decomposed into stellar and nonstellar components, and the spectrum at X-ray energies is derived from observations made with the Monitor Proportional Counter and the Imaging Proportional Counter aboard the Einstein Observatory. These results are used to obtain conclusions about the galaxy's column density and spectral index, covering fraction and visual extinction, and thermal emission. Ultraviolet, infrared, and radio observations published elsewhere are then combined with the new data to produce the overall continuum.
Halpern, J. P.↗
Binary phase correlated X-ray intensity variations and flaring activity in the RS CVn binary HR 1099
The monitor proportional counter and the imaging proportional counter of the Einstein Observatory were used to observe the X-ray variability of the RS CVn binary HR 1099. The X-ray intensity is found to vary with the 2.837-day period of the binary. An intense X-ray flare was noted on February 17, 1980. The present results are explained using a star spot model, and it is suggested that the flare heated plasma cools either mainly by radiation or equally by conduction and radiation.
Agrawal, P. C.↗
The x ray morphology of the relaxed cluster of galaxies A2256. 1: Evidence for a merger event
The rich cluster of galaxies A2256 was studied utilizing the imaging proportional counter (PSPC (Position Sensitive Proportional Counters)) on board the x-ray observatory ROSAT. A2256 is considered to be a relaxed, Comalike cluster which is dynamically well evolved. However, clear evidence for substructure in A2256 was found. The x-ray surface brightness distribution reveals two separate maxima in the center, one of which is coincident with the central cD galaxy while the morphology of the other shows indications that it is merging with the main cluster body. The x-ray temperatures of the two maxima are different; the probable merging object being about a factor of five cooler than the cluster. The previously measured broad velocity distribution supports the idea that a merger in this cluster is being observed.
Briel, U. G.↗
The Heavy Element Abundance in Groups of Galaxies
Over the past few years we have analyzed a sample of clusters observed by the Advanced Spacecraft for Cosmology Astrophysics (ASCA) X-ray satellite. We performed spatially resolved X-ray spectroscopy of a sample of 18 relaxed clusters of galaxies with gas temperatures below 4 keV. The spectral analysis was done using ASCA/SIS (Solid state Imaging Spectrometer) data combined with imaging data from ROSAT/PSPC (German acronym for X-ray satellite/Position Sensitive Proportional Counter) and Einstein/IPC (Imaging Proportional Counter) observations. We derived temperature profiles using single-temperature fits for all of the clusters in the sample, and also corrected for the presence of cold gas in the center of so-called 'cooling flow' clusters. For all of the clusters in the sample we derived Si and Fe abundance profiles. For a few of the clusters we also were able to derive Ne and S abundance profiles. We compared the elemental abundances derived at similar overdensities in all of the clusters in the sample. We also compared element mass-to-light ratios for the entire sample. We concluded that the preferential accretion of low entropy, low abundance gas into the potentials of groups and cold clusters can explain most of the observed trends in metallicity. In addition, we discussed the importance of preheating of the intracluster medium by Type II supernovae on the cluster scaling relations.
David, Laurence↗