Next: Individual data Up: Final results Previous: Residual plots . After the last residual plot, the final parameter values (and their errors) are printed, including the magnitudes and colors of the individual stars in the extinction solution. ... This is followed by a table of the individual residuals, which includes the symbols used to identify different stars in the residual plots. ... Tue Mar 28 16:52:29 MET DST 1995 ...

Next: Simulations Up: Maximum Likelihood Estimation of Previous: Introduction . The properties of an ensemble of faint galaxies can be defined by the distribution of the parameters of the models that best fit each individual object. ... The model also includes instrumental parameters, such as the sky background (estimated locally) and amplitude of the noise. ... The probability of the observed value is then computed for each pixel using the adopted error distribution. ...

Next: The Schedule File Up: THE SCHED USER MANUAL Version Previous: Satellite Tracking Contents . This chapter covers the main input files that SCHED reads. ... See the SCHED Input and Output Files section of this manual for brief descriptions of the files and pointers to the standard versions. ... Summary List of SCHED Parameters . ... List of Frequency File Parameters . Setup Files . Standard Setup Files . ... Summary List of Setup File Parameters . Details of Setup File Parameters . ...

... The main research task of the LRS was an investigation of interstellar medium of our Galaxy using its line emission in radio domain with the help of the gratest RATAN-600 Radio Telescope. ... The complex investigation of the Interstellar Clouds structure on the different scales and with the different radio lines for understanding of structure, dynamics and evolution of interstar gas and its interaction with other galactic constituents and the conditions for star formation. ...

... Default . ... The descriptions below focus on the meaning of each filename parameter, leaving the exact details of the inferred default value to be explained in the algorithm section. evlist . ... file . The response matrix file (OGIP-compliant format). ... If a spectrum file is not provided ( withspectrum =no) this parameter specifies the INDEX number of a source in the source description list (parameter srclist ), and thereby the incidence angle and selection regions for the response matrix. ...

ESO Phase 3 Data Release Description Please start from this template when preparing the documentation for your ESO Phase 3 data release. ... Finally, the release description will be published as submitted - without further editing by ESO - to support the user community in utilizing the data. ... Please indicate if this is a catalogue data release. ... Data Reduction and Calibration Please address the following questions for scientific catalogue data, particularly in case of source catalogues: . ...

The magnetic mapping is fulfilled by the magnetic field line tracing from the satellite position up to the Ionosphere (stop trace at the altitude 110 km). ... As a rule the Tsyganenko [1987] external magnetic field model and IOPT = 3 (Kp = 2) are used. ... The output file includes the following information: . ... For example the file with name aa9610d1.geo contains the information corresponding to the aposteriory magnetic mapping for INTERBALL Auroral Probe for the first decade of October 1996. ...

Arecibo World Day data description . ... The F-region program covers the altitude range of 140 - 660 km. ... The KINDAT code in the CEDAR database for these parameters is 2010. ... The KINDAT code in the CEDAR database is 2021 for this kind of data. The barker-code program allows the measurement of electron concentration at a height resolution of 0.6 km with a very high S/N. This program typically covers the altitude range of 60 - 500 km. The KINDAT code in the CEDAR database is 2015. ...

... Average resolution at altitude H=668 km . ... Swath width at H=668 km and inclination of beginning of swath 20.48 degrees . ... Resolution at H=668 км . ... Наименование параметра . ... 1 канале . ... Полоса обзора при H=668 км . ... 1-5 спектральной зоне, не более . ... 1 спектральной зоне . 0,48-0,52 мкм . ... 0,915-0,997 мкм . ... 1-4 канал . ... 1-4 каналов . ... Спектральные характеристики каналов (по уровню 0,5): . ... For more information send a mail to: info@sputnik.infospace.ru . ...

... SFIT is a general-purpose code designed to optimize theoretical stellar spectra to an observed spectrum. ... While the programme expects input from "stdio", it is more natural to save commands in a file (eg "sfit_input") and run the code simply by . ... If the spectra to be fitted have a filename "star_spectrum", then the best fit spectrum will be written out, together with the renormalized input spectrum, to a file called "star_spectrum.fit". ... sets up model spectrum grid (and for 2nd star) . ...

Next: *.imh and *.qp Extensions Up: IRAF/PROS Files Previous: IRAF Image Arrays . The x-ray data are stored in QPOE files (Quick Position-Ordered Events, *.qp ) rather than image arrays. ... Note that, unlike IRAF images, QPOE files have no associated header file, and are always stored in the current directory, unless explicitly specified otherwise. Non-PROS IRAF tasks can also access QPOE data files in place of image arrays. ... rp110590.qp[pi=2:30] . ... The ROSAT PSPC qp file images are . ...