... Name of input EPIC pn or EPIC MOS events file (e.g., of a source or selected region) . ... whether to use background event set for background subtraction . ... Name of background EPIC pn or MOS event file . ... whether to use plotfile as output file name, otherwise construct name from input data set + `_pat.ps' . ... whether to create also QDP output file, construct name from input data set + `_pat.qdp' . ... whether to use the user-defined mode usermode instead of the SUBMODE model for comparison ....

... Classes . ... casa . casa::HyperPlaneParam< T > . Public Member Functions . ... HyperPlaneParam (const HyperPlaneParam &other) . Copy constructor (deep copy). template<class W > . ... Copy assignment (deep copy). virtual . ... virtual const String & . ... virtual casa::HyperPlaneParam < T >::~ HyperPlaneParam . ... virtual const String & casa::HyperPlaneParam < T >::name . ... virtual uInt casa::HyperPlaneParam < T >::ndim . ... Copy assignment (deep copy). template<class T> . ...

... we show that the comparison between the calculated and observed numbers of the most ``fragile'' (from the point of view of the binary evolution scenario )   galactic binary types (such as X-ray low-mass X-ray binaries (LMXB), cataclysmic variables (CV),   Be-stars   with compact companions, relative number of visible binary radiopulsars   with normal and compact secondary components) impose certain constraints on the feasible initial ... Phenomenological Kick Velocity . ...

... We demonstrate through numerical simulations that model parameters estimated with our technique are essentially bias-free, even when the average number of counts per bin is 1. ... The IW technique avoids such biases by estimating through successive iterations, where for each iteration, j, , and the best-fit parameters are determined by minimization of . ... In our sample, we find that the minimum values and best-fit parameters converge after about 6 iterations. ...

... Column 1 gives the object name from the Case or Markarian catalogs. ... For Markarian galaxies the errors of coordinates usually lie inside 2'' (Lipovetsky [ 1983 ]). Column 4 gives the eye-estimated apparent blue magnitudes according to the same sources. ... Other names of a galaxy we give in column 7. ... In column 3 we cite the original emission-line code of the galaxy for the strength of [O III ] doublet according to the Case catalog (s - strong, m - medium, w - weak). ...

Target Acquisition Reference Information . There are limits to the brightest and bluest stars that can be acquired with mirrors N1 and N2 because of the very high fluxes of these objects. Figure 7.3 on page 91 shows the limits for these two mirrors as set in the Constraints and Restrictions Document (CARD). ... Once you have predicted an acquisition count rate, you then determine the integration time per dwell point during the target acquisition: STEP-TIME. ... STEP-TIME Constraints . ...

main parameters . ... Small Detector   (SD) with thin polyethylene moderator and cadmium shield ; . Medium Detector (MD) with medium polyethylene moderator and cadmium shield ;   . Large Detector (LD) with thick polyethylene moderator and cadmium shield ; . ... Duty regime ; . ... Duty” frame with keeping data (92 bytes) in Duty r egime . Standard” frame with 6 spectra (212 bytes) in Mapping r egime . Profile” frame with 6 spectra and 2 profiles (512 bytes) in Burst r egime ...

Next: Program use Up: Description of program searchdup Previous: Description of program searchdup . Parameter input is done with a graphic user interface. ... Input file: Name of the input catalog file. It has to be formatted, one record per source/observation, according to the format used in the Arcetri observations and source archives. ... Minimum number of observations per source Source with less than this number of independent observations are not included in the output file . ...