... srcinfov strra=<ra> strdec=<dec> apos=<apos> withsrccoord=true|false . ... srcinfov computes for each instrument the position of a given celestial source in the field of view (in TELCOORD coordinates). Input is the satellite attitude in terms of Right Ascension/Declination of the star tracker viewing direction and astronomical position angle [deg]. ...

... Next: 7 kslice_3d: slicing data Up: Karma User Manual Previous: 5 Volume Rendering a . The <kpvslice> programme allows you to use a two-dimensional image to define a slice through a three-dimensional data cube. ... The slice is drawn on the total column density or velocity field map, and the corresponding position-velocity diagram will appear in the other window. ... To load the cube, press the Cubes button in the left window and select a cube file. ... The image is displayed in the left window. ...

... connection points . ... The point P3 is the connection between the horizontal and vertical actuators and is the axis of rotation for the tail gunner motion. processing: survey/020204/reduc We can compute P3,P5 (the moveable points) in dome centerline coordinates if we have the actuator distances and we know the positions of the above connection points in dome centerline coordinates for a given position of the tertiary (say the nominal focus position).(see actuator distances to dome centerline ). ...

Computer Ephemeris for 2014 from DE200/LE200. ... Sidereal Time. ... Apparent equatorial positions. Ecliptical positions. ... Chebyshev polinomial approximation of positions. ... Position and velocity. ... Dynamical time. Sidereal time. ... Osculating elements of planetary orbits. Planetary configurations (by time). ... Fundamental ephemeris. ... Ephemeris for physical observations. ... Stars. ... All comments on Computer Ephemeris please direct to the author: charlie@mail.univ.kiev.ua ...

lsst.tcc љ 1.2.2-3-g89ecb63 . ... Files . ... python . ... axis . coordConvWithFP.py . ... 22 љ def coordConvWithFP (fromCoordSys, fromPVTPair, fromPxPMRadVel, fromDir, toCoordSys, obj, inst, zeroPM, useGSWavelen): . 23 љ """!Convert a coord from one coordinate system to another . ... 35 љ @param[in] obj object block computed at desired desired TAI date of conversion . ... 50 љ obj = tcc.base.Obj(obj) # make a copy so I can change obj.site if useGSWavelen . ... tcc.axis.rotFromObs.rotFromObs . ...

Weaving together Astronomy+Statistics+Computer Science+Engineering+Intrumentation, far beyond the growing borders . ... Posts tagged ?computer science? ... A postdoc job announcement from Prof. Joshua Bloom of UC Berkeley: . ... Jobs] postdoc position at UC Berkeley? Tags: AstroStat , computer science , job announcement , job market , time series , UC Berkeley . ... 1 Comment . ... Entries RSS . Comments RSS . ... vlk on [MADS] Parallel Coordinates . ... Entries (RSS) and Comments (RSS) . ...

... The exact directions of the offsets are parallel to the rows and columns of the CCD on which the aperture is specified. ... It is often useful to explicitly specify the desired rotation of the WFPC2 field-of-view on the sky. ... Figure 7.8 shows the CCD orientation and aperture locations relative to the U3 axis. ... Obtain the Position Angle (PA) of the source axis on the sky, measured in the standard way, North through East. ... desired source angle in field-of-view measured CW from +U3 axis) . ...

... To plot the data (and model, here xitau.model), I have read the model, computed the model values for the ASTROMETRY, and used Plot|ASTROMETRY to produce the ASTROMETRY plot widget. ... First, plot the data and with Util|Ellipse and the mouse buttons interactively define an apparent ellipse to fit your data as best as you can. ... Under Util|Orbit, there is a Thiele-Innes procedure to estimate the orbital elements using your apparent ellipse and Kepler's laws! ... Back to tour page . ...

The position of the objects on the sky were generally measured to a precision between 1 and 4 arcsec. ... For the stars, the position is always at epoch 2000, whatever J2000 or B1950 coordinates are printed. ... The celestial position is given as coordinates in 4 different systems: . ... B1950 . ... Galactic coordinates in the reference frame called "new" system, adopted by IAU in 1958. Galactic pole at B124900.0+272400, node at ra=282.25,l=33 deg (inclination 62.6 deg). ... 1 arcsec . ...

... Impact on source motion in Galactic coordinate system is given by Kovalevsky (2003), Malkin (2011) l cos b = -A sin l, b = -A cos l sin b, where A = R0 02 /c is the galactocentric acceleration called hereafter the GA constant. ... We just have to return to the traditional many-centuries-old astrometric practice of modelling the position of a celestial object as a linear trend with two parameters: the position at the initial (conventional) epoch and the apparent (proper) motion. ... 2011). ...

... There is an opportunity to perform O-C calculations for objects which are absent in the data base of the package. Such objects can be described by orbital elements or by initial coordinates and velocities. ... On pressing Edit file button user has a possibility to look through the list of object elements or their coordinates and velocities to add or to change it. ... For example, the designations of objects in the list can occupy the last position in each line. ...