As it is in Ephemerides task, O–C can be calculated with different accuracy. ... It presents three modes of accuracy. One can calculate position of a minor planet by the formulae of elliptic motion starting from the fundamental set of elements for given minor planet. ... Also there is possibility to calculate positions taking into account perturbations from different sets of perturbing bodies by numerical integration ( Integration mode). ... Accuracy of integration is equal to 10**(–10) AU. ...

... Format of the orbital elements | Estimation of the extrapolation errors | Version 1" of the orbital elements collection, determined by KIAM during flight and used for operations planning . Version 2" of the of the orbital elements collection, modified by IKI during flight and recommended for the orbital calculations during scientific data processing . ... Three kinds of the INTERBALL Auroral probe (IB_AUR) orbital elements' collections are presented here. ... IKI RAN | SSC IKI RAN | ...

... HST Phase II Proposal Instructions for Cycle 20 > Chapter 10: Fine Guidance Sensors (FGS) > 10.3 Mode = TRANSConfig = FGS . ... This observing strategy is discussed in the FGS Instrument Handbook . ... STEP-SIZE values of 0.6 or 1.0 are recommended (see the FGS Instrument Handbook ). ... Enter the ORIENT ation visit-level Special Requirement (see ORIENTation <angle1> TO <angle2> ) if the arrangement of the target or reference stars requires a particular orientation of the FGS field of view. ...

... The routine returns the offset (deltaX, deltaY) from the linear grid position for a specified detector location. ... the distortion (deltaX, deltaY) at the detector location (rawX, rawY) is derived from the distortion map stored in the extension FILTER-FilterId (e.g. FILTER-U, FILTER-V, FILTER-GRISM1 etc.) ... interpolate the extracted distortion points (RAWX_OFF ,RAWY_OFF ) and calculate the distortion (deltaX,deltaY) at the requested postion (rawX, rawY) . ... deltaX, deltaY . ...

... The HST uses an onboard model of its orbit to perform in real-time various control functions relating to spacecraft operations and observation support. ... New coefficients for the ephemeris are updated every other day, and are archived as FITS keywords for each HST observation data set. Using these coefficients,an observer can perform a variety of calibration and characterization calculations relating to the orbital position and velocity of the telescope. ...

... To access the measures do the following. ... Each of them can be either a scalar quantity with a scalar or vector for its actual value (see the following example):: from pyrap.quanta import quantity dm.epoch('utc','today') # note that your value will be different {'m0': {'unit': 'd', ' value ': 55147.912709756973}, 'refer': 'UTC', 'type': 'epoch'} dm.direction(' j2000 ','5h20m','-30.2deg') {'m0': {'unit': ' rad ', ' value ': 1.3962634015954634}, 'm1': {'unit': ' ...

... Does the time it takes different methods to create all the elements coincide with the universeт??s accepted age? ... Illinois Urbana-Champaign) Different kinds of stars create elements at different rates, all of which are consistent with the age of the universe. Get instant access to subscriber content on Astronomy.com! ... Registration is FREE and takes only a few seconds to complete. If you are already registered on Astronomy.com, please log in below. ...

lbw gain and turret position . ... A 2 deg turret step (2*.75= 1.5 arc minute on the sky) was used (about .5 beam widths). ... The green, blue, and dark red lines are all at about the same gain so the measured best position is at least .57 degrees above the surveyed position (it probably wouldn't hurt to redo this since we didn't go over the other side of the gain vs turret position curve). processing:x101/020401/doitsbh.pro The cband beam width at 5 Ghz is about 60 asecs. ... step Used . ...

The beam pattern and the polarization characteristics . of the radio telescope RATAN-600 . The Mueller matrix elements was computed via formulas [1]: . ... The BP were computed by the aperture method, proceeding from the fild distribution in the aperture of the primary mirror. The components of the main and cross-polarization components of the electric field in the vertical aperture of the primary mirror was computed in Frenel diffraction approximation. ...

... For given geographical longitude and time zone show the current data and time, Universal data and time, current local star time. ... Accept 10 different data formats (data&time, data with decimal day of month, data with decimal day of year, decimal year, some Julian dates), calculate from any formate to others, show day of week. Current data and time direct insertion function is exists. ... Calculate angular distance between two points at the sky by its equatorial coordinates. ...

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 . ...