Next: Calling Parameters Up: CAL_rawXY2mm Previous: CAL_rawXY2mm Contents . CCF LinCoord holds the positions of distinct reference points of the CCD's (at reference temperature) and the directions in which the counting of rawX and rawY increases. The size of each pixel is stored in CCF MiscData , and also a thermal expansion coefficient. Using these inputs, together with ( rawX,rawY ), the location of each pixel can be given in focal plane coordinates as a function of temperature. ...

Target Acquisition Reference Information . ... In almost all cases where an onboard acquisition will not work (because the object is in a crowded field, or is variable, or is a moving target), it is sufficient to use an early acquisition to get a WFPC2 or FOC image a few weeks in advance of the GHRS observation. ... Explicit BRIGHT and FAINT limits may be specified if you desire, although there is an increased risk of a failed acquisition unless you are confident of those fluxes. ... MAPs . ...

... The models provided are: . abs - absorption of x-rays by neutral gas with solar abundances. parameter 1 = . ... parameter 2 = . ... normalization - logarithmic value of the flux density at 1 keV in units of keV cm -2 s -1 keV -1 . ... normalization - logarithmic value of the normalization of the gaussian in units of keV cm -2 s -1 . ... absorption ( params )* model ( params ) . ... A single value for the normalization (i.e., fixed normalization) will force the program to use that value. ...

Next: Mass change Up: Evolutionary Scenarios of Binary Previous: Stellar Winds From Normal . As mentioned earlier, the duration of the binary evolutionary stage (say, I+I) is determined by the faster evolving component , where is the time each component spends at the corresponding evolutionary stage. ... Next, we should calculate the mass change for the slower evolving companion, the orbital semi-major axis and the eccentricity. Mass change . Semi-major axis change . ...

Finally, the radial velocity is also expressed in the reference frame of the Cosmic Background Radiation. This velocity is noted v3k . It is calculated from the heliocentric velocity v using the total solar motion of 360 km/s towards the direction defined by the B1950 equatorial coordinates B 11.25 H - 5.6 deg (Lubin Villela 1986). v3k = v + 360 cos(theta) Where theta is: cost(theta) = sin(de3k) sin (de1950) + cos (de3k) cos(de1950) cos(al3k - al1950) . ...

... CentralProcessor 0.11 documentation . ... It can be run with the following command, where ?config.in? is a file containing the configuration parameters described in the next section. ... Parset parameters understood by ccontsubtract are given in the following table (all parameters must have CContSubtract prefix, i.e. CContSubtract.dataset ). ... A number of other parameters allowing the user to narrow down the data selection are understood. ... Parameter . ... Data set file name to work with. ...

... Fitting the observed dependence includes calculations of the polarization cross-sections averaged over particles orientation and size distribution, their normalization and the comparison of obtained dependencies with Serkowski's curve representing observational data for a chosen star. ... Variations of the polarization factors with wavelength are shown in Fig. 16 for homogeneous spheroidal particles with PF orientation. ... The distinction between prolate and oblate spheroids is also clearly seen. ...

... Measurements Definition Sample Timestamp Definition : Time and date of measurement XML parameter : mtSampTime Windspeed Definition : 3 second rolling average of 250 millisecond samples XML parameter : mtWindspeed Units : MPH Raw Wind Direction Definition : 3 second rolling average of 250 millisecond samples XML parameter : mtRawWindDir Units : Degrees Adjusted Wind Direction ... XML parameter: mt60MinWindGustTime_2 Units: date and time ...

... We cannot use for this purpose equivalent widths and profiles of HI lines (well known criteria of atmospheric conditions for normal supergiants), since these lines are strongly distorted in the spectrum of IRAS04296 as seen in Fig. ... Figure: Upper: iron abundance FeI (circles) and FeII (crosses) calculated for IRAS04296+3429 with model parameters , and using lines with different excitation potentials EP of a low level; bottom: the same as a function of the equivalent width W . ...

THE PHOTOMETRIC RESEARCHS OF THE MERCURY'S SURFACE BY MEANS OF DIGITAL MODELS. ... The surface brightness of Mercury was measured Danjon (1933, 1949, 1953) and Harris (1961) in phase angle 3o-123o. The analysis of the various data of the integral photometric gives the results of determination of the main photometric constants for Mercury. ... THE PHOTOMETRIC RESEARCHS OF THE MERCURY'S SURFACE: S.G. Pugacheva The surface brightness of the Mercurian images was established on the geologic map Mercury. ...