Next: Discussion Up: The Second EGRET Catalog Previous: First Catalog Sources . In the first EGRET catalog, upper limits were given for selected objects not detected during the Phase 1 all-sky survey. These upper limits are determined using the likelihood calculation and depend on the EGRET exposure to a given direction, the contribution of the diffuse gamma radiation, and the proximity and strength of detected sources. ...

The HyperNews Linux KHG Discussion Pages . Forum: The Linux Kernel Hackers' Guide . Re : resources hard limits . Keywords: getrlimit setrlimit limit ulimit hard resource limits . ... As for soft/hard limits, ulimit -S vs. ulimit -H ought to do that. Incidentally, if you specify neither, both should get changed at the same time. csh is an excemption; here you need to use limit -h for hard limits. ...

... Let us assume to begin with that there is no source at a given location, only background. Let us calculate the probability that the observed counts at that location are due solely to background. ... The routines described in the present section are designed to take as arguments the probability cutoff (actually a cutoff in likelihood is used) and the background, or expectation value for the counts, and use them to calculate the minimum value of source counts which is detectable at those levels. ...

... Next: The PROS Big Up: Software Systems Previous: Data Reduction Software . ... The srcinten task provides PROS users with a tool to compute count rates for point sources in the ROSAT High Resolution Imager (HRI). ... Corrected upper limits are cited at locations where the count rate falls below the source detection threshold. ... Srcinten is a new PROS task that computes and applies the above correction factors to the net counts in a user-specified aperture. ...

STIS Instrument Handbook for Cycle 24 . ... Space Telescope Imaging Spectrograph Instrument Handbook for Cycle 24 > Chapter 14: ImagingReference Material > 14.8 MAMA Imaging Bright Object Limits . ... In Table 14.40 , we present the complete set of bright object point source and integrated magnitude screening limits for the MAMA imaging modes. ... The imaging table also includes an integrated magnitude limit. ... Table 14.40: MAMA Bright-Object limits (V magnitudes and cgs units). ... FUV-MAMA . ...

... SELECT file, title, rank(ts_vec, to_tsquery('create schema')) FROM postgresql_manual WHERE ts_vec @@ to_tsquery('create schema') ORDER BY rank(ts_vec, to_tsquery('create schema')) DESC LIMIT 5; file | title | ... CREATE SCHEMA | ... SELECT file, title, rank('{0, 0, 0.01, 0.99}',ts_vec_tb, to_tsquery('create aggregate')) FROM postgresql_manual WHERE ts_vec_tb @@ to_tsquery('create aggregate') ORDER BY rank('{0, 0, 0.01, 0.99}', ts_vec_tb, to_tsquery('create aggregate')) DESC LIMIT 5; file | ...

lsst.tcc љ 1.2.2-3-g89ecb63 . ... Files . FileљList . ... include . ... cheby.h . ... 29 љ class ChebyshevPolynomial { . ... 37 љ std::vector<double> params , . ... 44 љ throw std::runtime_error( "ChebyshevPolynomial called with empty vector" ); . ... 98 љ double csh = (2 * xPrime * this-> params [order]) + this-> params [order-1]; . ... 112 љ std::vector<double> params ; . ... ChebyshevPolynomial(std::vector< double > params, double minX=-1, double maxX=1) . ... tcc::ChebyshevPolynomial::params . ...

... The VSOP Survey Continuum Source List . The radio sample for the VSOP continuum survey was defined to include all extragalactic radio sources with: . a total flux density at 5 GHz, S>=1.0 Jy . ... The sample also included all sources in the sky with a 5 GHz flux density S>5 Jy, regardless of spectral index and galactic latitude. ... The source would then be included in the VSOP sample (three of the sources were found with a flux density above 1 Jy and added to the sample). ...

This document explains some of the directives provided by the core server which are used to configure the basic operations of the server. ... Process Creation . Network Configuration . ... User . ... A single control process is responsible for launching child processes which listen for connections and serve them when they arrive. ... The User and Group directives are used to set the privileges of the Apache child processes. ... The child process creates multiple threads to serve requests. ...

Next: *upspecrdf, downspecrdf* - Transform Up: Spectral Analysis Previous: *grid_plot* - Plot Results . The conversion of count rate to flux depends on the intrinsic spectrum of the source, so xflux must be used in conjunction with fit . Fit generates a table of the best fit intrinsic spectrum ( _int.tab extension). xflux uses this table to calculate either the integrated flux between two energy limits or the flux density at a specific energy. ... This produces ``..._obs.tab'' file. ...

... 75 љ bool pointSourceVisible ( StelProjector * projector, const Vec3f & v, const float rcMag[2], . ... 108 љ void drawPointSource ( const Vec3f & win, const float rcMag[2], const Vec3f & bcolor); . ... 119 љ void postDrawSky3dModel ( StelProjectorP projector, const Vec3d & v, float illuminatedArea, float mag, const Vec3f & color = Vec3f (1.f,1.f,1.f)); . ... 272 љ float getMaxAdaptFov( void ) const { return maxAdaptFov;} . ... 280 љ float getMinAdaptFov( void ) const { return minAdaptFov;} . ...

In calculating the NIFS sensitivity, we adopt a read noise of 5 e - , a dark current of 0.01 e - s -1 pix -1 , and a maximum exposure time of 3600 s. Grating . ... e/pix) . ... OH Cont. (e/pix) . ... NIFS should achieve signal-to-noise ratios of ~ 10 per spectral pixel in a 0.1" 0.1" aperture for single 1800 s exposures on uniform, extended, continuum sources with surface brightnesses of J = 15.4, J = 15.0, H = 14.8, and K = 13.5 mag arcsec -2 using the Z , J , H , and K gratings, respectively. ...

On 1 February 2002 this Mirror was upgraded from NVSSlist v2.10 to NVSSlist v2.17 . ... This form searches the source catalog produced by the NRAO/VLA Sky Survey (NVSS). ... Object name [optional] : . ... Search radius and verification halfwidth in arcseconds [Optional] : . ... Enter a list of positions to search: . ... The contents of the NVSS source catalog and the techniques used by NVSSlist to derive error estimates and other parameters are described here. ...

The cumulative system performance is plotted for each receiver. ... When something occurs that may change the gain of the system (moving a horn, shimming the elevation rails) then a new epoch will be started. The old data is moved to the old system performance data page (the old data link points to this). ... Gain,Tsys,Sefd... (.ps) (.pdf) . ... Pointing errors (.ps) (.pdf) . ... Hour of day when sources measured (.ps). (.pdf) . list of sources with dates and filenames Old data . ...

... Start UT Source Start / Stop Early Tapes TPStart Stop UT LST EL AZ HA UP ParA Dwell (see above) SYNC ---------------------------------------------------------------------------------------- --- Sat 13 May 2006 Day 133 --- Next scan frequencies: 8417.00 8417.00 Next BBC frequencies: 617.00 617.00 Next scan bandwidths: 16.00 16.00 02 30 00 0537-441 03 49 16 65.0 128.6 -1.8 -68.5 0 1 1 52 02 30 00 02 40 00 --- 03 59 17 66.6 130.3 -1.7 ... Scan hours are for recording scans only. ...

... The results of long-term monitoring of Gigahertz-Peaked Spectrum sources were found the statistically significant differences (0.05 significance level) in the high-frequency spectral index distribution between subgroups of galaxies and quasars. ... This can mean that the electron energy distribution for GPS galaxies is steeper than for GPS quasars. ... The first area corresponds to GPS-quasars that have statistically larger value of redfhift, second area corresponds to GPS-galaxies. ...

... 172 ] Briefly, the count rate at the detector from a source at a redshift z is . ... Figure 55 shows the ``Green functions'' for the double compact binary merging rate   evolution assuming no collapse anisotropy. ... Another way that diverse peculiarities in the - distribution induced by the sources evolution could arise is connected with a possible non-monotonic character of the star formation rate in galaxies. ... 22 ] Figure  56 shows two-dimensional cuts through the parameter space. ...

... The actual cross-correlations were done as follows: north of WGACAT was correlated with the GB6 catalog with a correlation radius of one arc minute. ... We therefore cross-correlated WGACAT with the GB6 and PMN radio catalogs with a 1.5 arcmin radius. ... As a result of this experiment, we then added to the WGACAT/PMN candidate list the 29 unclassified sources obtained from the 1.5 arcmin correlation and having PSPC offsets arcmin, ratio between X-ray/radio offset and positional error , and . ...

... They are concerned with Attitude Control System of the spacecraft, satellite visibility from tracking stations, limits on the satellite autonomous operations during the orbit, and needs for auxiliary operations with the spacecraft. ... Among the operational constraints the most important one is the number of programmed slews per orbit, which determines the maximum number of radio sources to be observed during one orbit. ... System temperature (K) . ... Progress of the RadioAstron Project in Pictures...

... Diffraction-limited Bispectrum Speckle Interferometry and Speckle Polarimetry of the Young Bipolar Outflow Source S140 IRS1 . ... P06P We present bispectrum speckle interferometry and speckle polarimetry of the deeply embedded infrared bipolar outflow source S140 IRS1, a massive protostellar object in the L1204 molecular cloud. ... Our data suggest that the central source is marginally resolved with a FWHM diameter of approximately 20 mas (~ 20 AU). ...