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Table 5: The areas, detection efficiencies, and background rates of 1yplcal hand- held and transportable neutron and gamma-ray detectors apos;

in Ph~pying pennitted by license only Reprints available directly ftom tile publisher C> 1990 Gordon and Breach Science Publishers S.A. Printed in tile United States of America Detecting Nuclear Warheads
by Steve Fetter, O Valery A. Frolov, B Marvin Miller, Robert Mozley, D Oleg F. Prilutsky, B Stanislav N. Rodionov, Roald Z. Sagdeevb
"... In PAGE 9: ... More massive detectors would be more sensitive, but their application to treaty verification will probably be limited to fixed portals through which objects to be inspected would pass.- Table5 summarizes the neutron- and gamma- ray-detector characteristics used here, together with typical background rates; table 6 gives the distance from the four weapon models at which the neutron or gamma-ray signal equals the background counting rate in the detector. As table 6 shows, the neutron signal from weapons containing plutonium * The helicopter-mounted detecwr that made the measurements reported in the paper by... ..."

Table 7: The maximum detection range for a given detection time for neutron and gamma-ray emissions from each weapon model If a signal of 5 standard deviations relative to background fluctuations is required

in Ph~pying pennitted by license only Reprints available directly ftom tile publisher C> 1990 Gordon and Breach Science Publishers S.A. Printed in tile United States of America Detecting Nuclear Warheads
by Steve Fetter, O Valery A. Frolov, B Marvin Miller, Robert Mozley, D Oleg F. Prilutsky, B Stanislav N. Rodionov, Roald Z. Sagdeevb

Table 1 | Flux Limits on Fast Gamma Ray Pulsars P energy

in SEARCH FOR FAST GALACTIC GAMMA RAY PULSARS P. Hertz
by Grove Kurfess, J. E. Grove, J. D. Kurfess, W. N. Johnson, M. S. Strickman, S. Matz, M. P. Ulmer
"... In PAGE 4: ... No pulsars, either isolated or in binary systems, have been detected to date. We give upper limits to a selection of our searches in Table1 and a typical power spectrum in Figure 1. A typical OSSE observation during the sky survey portion of the Compton Observatory mission last two weeks.... ..."

Table I: Event rates in AMANDA detector. For models accommodating the di use GeV background the rates are larger by 2 orders of magnitude. The rst column is the redshift of the burst, the second (third) column is the signal without (with) absorption of gamma rays in intergalactic backgrounds. In each columns the results is given for zenith angle = 60 and = 0. The fourth column gives the signal to square root of noise corresponding to column 3. The 5th column shows the time in days between bursts with z lower than the value shown in the rst column. The role of absorption for gamma ray detection is evident. Nearby bursts with z lt; 0:1 provide the best opportunity for detection. Their frequency is of the order of 1 burst every 2 3 years.

in Muon Detection of TeV Gamma Rays from Gamma Ray Bursts
by J. Alvarez-Muniz, F. Halzen

TABLE III GAMMA-RAY STRENGTH

in REPF3CNX4W’KMI C(3PY Applied Nuclear Data Research and Development
by United Stat 1977

Table 2: Elemental Contributions to Gamma-Ray Lines in Percent

in Gamma-Ray Measurements of Flare-to-Flare Variations in Ambient Solar Abundances
by Gerald Share And, Gerald H. Share, Ronald J. Murphy
"... In PAGE 8: ... (1990). Table2 lists eight of these features and estimates of the fractional contributions to each feature from speci c solar elements (Ramaty, Kozlovsky, and Lingenfelter, 1979; Ramaty and Kozlovsky 1994). Note that although the listed energies of the features are those of the primary de-excitation line, other lines not resolvable by the spectrometer and at slightly di erent energies may also contribute to the measured line strength.... In PAGE 10: ....1. FIP Abundance Variations As elemental abundances in various solar regions have been shown to be dependent on rst ionization potential (FIP), it makes sense to study the are-to- are line variability using this grouping. From Table2 we see that the lines at 0.... In PAGE 16: ...spallation products for harder spectra (see Table2 ).) A similar analysis reveals that the Ne/(C + N + O) ratio is also inversely correlated with spectral index at the 2:5 level.... ..."

Table 1. Shower and gamma-ray like event selection criteria.

in Observation of 3EG J1234-1318 with the CANGAROO-II Telescope
by T. Hattori

Table 1.1: classifications of gamma-ray astronomy [38].

in Abstract The CANGAROO (Collaboration of Australia and Nippon for A Gamma-Ray Observatory
by unknown authors

Table 1. Cumulative percentages of events passing gamma-ray

in TeV gamma-ray observations of Southern BL Lacs with the CANGAROO 3.8m Imaging Telescope
by M. D. Roberts, S. A. Dazeley, P. G. Edwards, T. Hara, Y. Hayami, J. Holder, F. Kakimoto, Kamei A. Kawachi, G. J. Thornton, S. Yanagita, T. Yoshida, T. Yoshikoshi 1998

Table 1. Gamma Ray Sources

in unknown title
by unknown authors
"... In PAGE 5: ... In some cases the numerical portions of these names di er slightly from those which have been used to identify these sources in previous publications because of more data and the improved di use model. Table1 contains information about the ux, position, and identi cation of the sources. The photon ux for energy gt; 100 MeV is presented, along with the value of pTs in this band.... ..."
Results 1 - 10 of 12,410