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Table 1: Fitted Power Law Parameters
1997
"... In PAGE 4: ... We observe that the mean call probability to the rank r callee, Pr, can be modeled using a power or generalized Zipf apos;s law at all three reference time periods: Pr apos; A rp , where A is the scaling parameter and p is the exponent parameter. Table1 shows the tted parameters and mean square errors of the ts. Figure 3 and Figure 4 are linear and log-log plots of Pr versus callee rank for the three reference periods.... In PAGE 15: ...4% 46.3% count per sec Table1 0: Simulation Results and Percentage Di erence for Centralized Database Scheme... In PAGE 17: ...1 4,743.8 rate (per sec) Table1 1: Access Rate at Three Selected Simulation Times... In PAGE 19: ...ugust 1990. S.F. Bay area transportation measurements. [25] International air tra c between united states and other countries. National Transportation Statistics 1996: Table1 7,18. [26] C.... ..."
Cited by 48
Table 1: Power law exponents of simulation results
2002
"... In PAGE 8: ... Each simulation was carried out for 200,000 iterations, and for the purpose of regression we considered only the first 25 urns. The results of our simulations are presented in Table1 ; in all cases the correlation coefficient of the regression analysis was close to one. The discrepancy between the simulated values and the empirical... ..."
Cited by 10
TABLE I POWER-LAW PARAMETERS
Cited by 1
Table 23: Author Collaboration Network Power Law Measure ClairLib Power Law 3.15
2007
"... In PAGE 21: ... We start with some general statistics, centrality and clustering coefficients. Power law exponent results can be found in Table23 . Note that because this network is undirected, only the total degree power law measure has been included.... ..."
TABLE 2 POWER-LAW INDEX OF TOTAL POWER SPECTRUM
TABLE I. Power law exponent of the PDF of the normalized power shed.
2005
Table 1. Results for indegree and outdegree exp. coefficients for the power law equation.
"... In PAGE 5: ... Table1 shows the coefficient of the power law for indegree and outdegree. I1, I2 and I3 represents the iteration level of SUBDUE.... ..."
Table 3. Broken power{law ts with galactic and free absorption. For these datasets, the broken power-law model is statistically preferred with respect to a single power-law model (the F{tests in the last column are against the single power{law model with free absorption)
2001
"... In PAGE 4: ... 1989). The results from the single power-law ts are reported in Table 2, while Table3 reports the broken power-law ts parame- ters. Adopting a conservative approach, we assessed the presence of a spectral break when the broken power-law model was signi cantly better, according to the F{test, even with respect to the single power{law model with free absorption.... In PAGE 5: ...rrors at 68% conf. level for 3 and 4 parameters of interest ( 2 =3:52 and 4.72 respectively). adopting an absorption value greater than the galactic one. In most cases, however, the broken power{law models with galactic absorbing columns provided even better ts (according to the F{test, see Table3 ). For 1ES 0033+595 and PKS 0548{322, instead, there is evidence for a higher column density also using the broken power{law models.... In PAGE 5: ... The spectrum is characterized by a curved shape, which is better t- ted by a broken power-law than by a single power-law model (with both xed and free absorption). The best t, however, still requires a column density in excess of the galactic value (see Table3 ), with high signi cance (F{test gt; 99:8%). The spectral indices before and after the break Fig.... In PAGE 10: ....2.7. H 2356{309 The spectrum of this source is not compatible with a sin- gle power{law model: there is clear evidence for a convex spectral shape, that is best tted by a broken power{law with high signi cance ( gt;99.9%, see Table3 ). This locates the synchrotron peak around 1.... ..."
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