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Table 2: The incidence n(z) of DLA and Lyman limit absorption for the = 1 CDM model, computed by our calibrated Press-Schechter procedure. Observational values are taken from Storrie- Lombardi et al. (1996) for DLA absorption and from Storrie-Lombardi et al. (1994) for Lyman limit absorption. Also listed is FC, the correction factor by which the KWHM results for n(z; 100 km s?1) must be multiplied to obtain the absorption n(z) produced by all halos.
"... In PAGE 8: ... We will compare them to observations in the next section. Table2 lists the values of n(z) determined by this procedure at z = 2, 3, and 4. It also lists the correction factors that must be applied to the quantities n(z; 100 km s?1) obtainable by the KWHM procedure in order to get the total abundance n(z) = n(z; 0).... In PAGE 8: ... (1994). The theoretical predictions and observed values are listed in Table2 . The resolution correction increases the predicted n(z) values relative to those of KWHM by about a factor of two, leading to quite good agreement with the observed abundance of DLA absorbers at z = 2 and 3.... ..."
Table 4: SNR pulse search limits
"... In PAGE 8: ...2. Flux Density Limits Table4 gives limits for average pulsar flux density, using the minimum detectable flux densities... In PAGE 9: ...for the inhomogeneity of the sky temperature of the objects, although some corrections were made when the beam filling factors were obviously small so that the net background sky temperature was much lower than that of the remnant. The observations at different frequencies and at different positions within the remnant are each given distinct limits in Table4 , and the fraction of the remnant solid angle that was covered by the observation is also indicated. The values for pulsar parameters used in determining the limits are: P = 30 ms; DM= 300 pc cm?3; duty cycle = 0:1.... In PAGE 9: ... 1. Limits for distinct observations of the same beam position have not been combined in Table4 , but are quoted separately. 4.... ..."
Table 1. Format codes used to limit searches
"... In PAGE 3: ... Originally, the pro- grammers established these two-letter indicators. Because other projects find this functionality desir- able, the codes are being modified to more closely match the lt;typeOfResource gt; terms in the Metadata Object Description Schema (MODS) ( Table1 ). The format codes will also be added to new non-MARC recordsets to allow combined searching of MARC, pseudo-MARC and non-MARC data.... ..."
Table 1: Damped Lyman alpha absorption systems and the radio ux densities of the background quasars. The background quasars are named according to B1950.0 (or in a few cases their more common name) with the J2000.0 optical positions quoted. zem is the emission redshift of the quasar and zabs and NHI [cm?2] are the redshift and the column density of the Lyman alpha absorber, respectively. The superscript on the column density gives the reference for the DLA (Section 2.1). Note that \* quot; denotes a candidate DLA which has yet to be con rmed using higher resolution spectroscopy. V is the visible magnitude and the nal ve columns give the radio ux densities at several frequencies. See Section 2 for further details.
"... In PAGE 3: ... In the nal sections we present the DLAs occulting radio-loud quasars along with any radio absorption features published and outline our future plans regarding the sample. 2 Explanatory comments and references In Table1 , for the column density we note that Corbelli, Salpeter amp; Bandiera (2001) argue that when NHI is estimated directly from the absorption line equivalent width, the value is systematically underestimated when compared to the estimate derived using Voigt pro le tting. This may be due to a biases associated with estimating the quasar continuum due the presence of Lyman forest absorption lines.... In PAGE 4: ...Omont et al. 2001)M. Finally, the results of White et al. (2000)W give new DLAs as well as the FIRST radio luminosities of the quasars illuminating these. Note that no radio information for the quasars in Table1 was found in the 5 GHz catalogue of Becker, White amp; Edwards (1991), the optically quiet quasar search of Kollgaard et al. (1995), the S5 radio source catalogue of Stickel amp; K uhr (1996), the 100 and 150 GHz observations of Southern at-spectrum sources (Beasley et al.... In PAGE 21: ...I. is the spectral index (both are estimated from the ux density values in Table1 ). In the last column, GPS designates a GHz peaked source with the approximate turnover frequency given in parenthesis.... ..."
Table 1: Statistics on point searches, varying bucket limits, times in [ s].
1999
"... In PAGE 8: ...Figure 4: Varying a) search times b) insert times. Table1 shows experiments of singe-point searches where the upper bucket size limit is varied between 50 up to 10,000 elements per bucket. 10 M records with 8 attributes were inserted using 320 MBytes of memory just for the record storage.... ..."
Table 1 - Effects of a Limited Search Interval in the GCC Function
2002
Cited by 2
TABLE 1 Results found by the clustering GA for different search volume limits
Table 3. Results with search limit of 2 rows divided by those with limit of 4.
Table 4. Results with search limit of 4 rows divided by those with limit of 10.
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