Next: Format of the Up: Auxiliary Data Previous: Description of the . For convenience in table handling only values for single lines or doublets (most of the observed cases) can be entered. If higher multiplicities are actually needed small changes have to be made in the table and program format. Possibility for 50 different atomic transitions. N.B. : in case of doublets, columns 3, 5, 7, 9, and 11 refer to the reddest component, and columns 4, 6, 8, 10 and 12 to the bluest. ...

Next: Star Formation Rate and Up: No Title Previous: Calculation of Evolutionary Tracks . To start calculations, we choose the distributions of the initial binary parameters: the mass of the primary ZAMS component, , binary mass ratio, , orbital separation a . ... whereas the mass ratio distribution is not. ... The zero assumption often made is that the mass ratio distribution has a flat shape, that is binaries with a high mass ratio occur as frequently as those with equal masses. ...

... A technique allowing automatic representation by a relatively small number of independent parameters based on the principal component analysis of data sequences is presented. ... In recent years the spectrum of observed astronomical data can be characterized as greatly varied. ... In this instance, the problem of initial description and classification of newly-observed data becomes most urgent, especially if there is a lack of preliminary observational material and theoretical expectations. ...

... Classes . ... casa::ComponentUpdate . ... ComponentUpdate (const ComponentList &model) . Construct an update machine for the sources in the given ComponentList , using the 'separate' type of solution, and ILM solve. ... makeEquations (const Array < DComplex > &deriv, const Vector < DComplex > &data) . ... enum casa::ComponentUpdate::Solve [private] . ... const Int casa::ComponentUpdate::N_unknown [N_Solve] [static, private] . ... ComponentUpdate::Solve casa::ComponentUpdate::solve_p [private] . ...

... arfgen (arfgen-1.70.4) [xmmsas_20060628_1801-7.0.0] . ... Generates an OGIP-compliant ([ 4 ]) ancillary response file (ARF). The ARF contains a table listing area values (the column SPECRESP ) for a number of different energy ranges (the columns ENERG_LO and ENERG_HI ). The ARF can be used in conjunction with the response matrix file (RMF, generated by rmfgen ) to allow fitting of particular spectral models against the observed spectral data. ... Implemented . ... Bad pixel correction . ...

... A file upload element on an HTML form. ... JavaScript 1.1: added type property . ... The HTML INPUT tag, with "file" as the value of the TYPE attribute. For a given form, the JavaScript runtime engine creates appropriate FileUpload objects and puts these objects in the elements array of the corresponding Form object. ... form . ... For all FileUpload objects, the value of the type property is "file" . ... Use the value property to obtain the file name that the user typed into a FileUpload object. ...

... The GHRS has the usual components of an astronomical spectrograph: entrance apertures, a collimator, dispersers, camera mirrors, and detectors. ... The collimator and camera mirrors are unexceptional and need no further description here (see ``The HST Focal Plane and the GHRS Apertures'' on page 73 for details). ... The first two first-order gratings, G140L and G140M, have their spectra imaged by mirror Cam-A onto detector D1, which is optimized for the shortest wavelengths. ...

CIMA is more than just the observing tool - in fact, the observing tool is just a part of a bigger package called the CIMA software package. ... There is also a another package called the CIMA WAPP software which contains the WAPP software, the special Tcl/Tk interpreter used by CIMA and support libraries. ... All CIMA software components recognize the following general options that are part of the CIMA version selection system: . ... The select_cima script can be used to set up a default version. ...

... 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: Stellar models Up: Introduction Previous: Photometry Contents . In a hierarchical stellar system, the separation between two neighboring stars is always much smaller than the separation of this pair from the next companion in the system, be it another pair or a single star. ... They are also numerically easier to handle than non-hierarchical systems, since each pair can be described with the standard orbital parameters, and each star with a small number of physical parameters. ... System . ...

... 18-Jan-2010 17:22 . ... Apache/2.2.3 (CentOS) Server at www.wdcb.ru Port 80 ...

... Co-ordinate systems description . Directories structure . The file names' construction . The file set description . ... The orbital information for each month is presented in the separate directory. The INTERBALL orbital data are located on the STDA server, for each month in the separate subdirectory, which name consists from the year (YYYY) and month (MM) numbers. The Parent Directory of the Tail Probe orbital data is http://www.iki.rssi.ru/da/interball/tail/orbit/ . ...

... Exposure Time Calculator (ETC) . ... ESO - Public Surveys . ... the recommended values to use for DIT, . ... Detector on-chip integration (DIT): seconds. to your chosen value - a separate page gives recommended values to use for DIT - for modes 1 and 2 below you may wish to start with the maximum recommended values as these will minimize the effect of read noise (a total object exposure of Y secs with DIT=X secs will produce Y/X lots of read noise) and give you a lower limit on the time needed. ...

True Color Image Gallery: Galactic SNR | Magellanic Cloud SNR . ... parameters were derived from bright shell at N . Abundance of O-like element was set to zero asumming Typ1 I SN( Hughes et al., 1995 ). source=(xswabs * xsvraymond) . reduce chi^2 = 7.41398 . ... DataSet 1: 153 data points -- 144 degrees of freedom. Statistic value = 1067.61 . ... DataSet 3: 90 data points -- 76 degrees of freedom. ... Back to SNR J0519.5-6902 Index . Chandra Supernova Remnant Catalog . ...

Irregular phenomena in the Earth Pole oscillation process and temporal variations of geopotential Valery Bondarenko, Vadim Perepelkin s The observed irregular phenomena in the Earth Pole oscillation process are very variety. ... These phenomena indicated in the IERS data are the "abnormal" fluctuation of the Earth Pole coordinates which owing to changing of the geodynamical parameters gives negative result in interpolation and forecast of the first approximation mathematical model. ... Fig. ...

Find Similar Abstracts (with default settings below ) . ... Also-Read Articles . ... Parameters of the 41 Dra system components . ... 00/2001 . ... Stars: Binaries, Binaries: Fundamental Parameters, Binaries: Individual . ... 61B Based on spectral and speckle-interferometric observations of the system 41 Dra, model atmosphere parameters of the system components have been derived: component Aa - T eff = 6500K, lg g = 3.99, R = 1.87 R solar , component Ab - T eff = 6500K, lg g = 4.11, R = 1.61 R solar . ...

... FTP access the basic models is here . ... Below, we put short descriptions of the used SED models for the photometric redshifts providing by the current server . ... The uniqueness of this model consists in expanding to the near IR (NIR) of Rocca-Volmerange and Guiderdoni's (1988) atlas of synthetic spectra with a revised stellar library, which includes parameters of cool stars. ... Homepage of the GISSEL model). ... Another model used earlier is the model of synthetic spectra of Poggianti (1997). ...

... Bojan Nikolic web pages (r. 329) . ... We present a Bayesian approach to calculating the coefficients that convert the outputs of ALMA 183 GHz water-vapour radiometers into estimates of path fluctuations that can be used to correct the observed interferometric visibilities. ... Inference of Coefficients for Use in Phase Correction . ... Simulating Atmospheric Phase Errors, Phase Correction and the Impact on ALMA Science . ... Copyright 2005 -- 2016, Bojan Nikolic feedback welcome ...

In this chapter we will consider an example of visual expert system written on the Actor Prolog language. ... There are a lot of methods of oil field bed stimulation that increase output of the oil production: thermal, physical-chemical, gas, microbiological, and others. ... Fig. ... The Top-Most diagram consists of three blocks: the "Describe parameters of hydrocarbon field" block, the "Check adaptability of existed methods of oil production" block, and the "Display solution" block. ... Gas methods. ...

Orbital data : INTERBALL AZ GSE and GSM cartesian coordinates, GSE cartesian velocity (once per 10 minutes). ... Magnetic field data from IMAP experiment. Magnetic fileld absolute value and magnetic field index (the difference between absolute value and model value), status flag. ... Counts of H+ and O+ ions are accumulated during one spin period by detectors D6 (antisunward looking), D8 (spin plane), D10 (sunward looking) of TRICS2 subsystem (1.0-30 keV). ... TRICS1, TRICS2, TRICS3 subsystems: . ...