... Object . ... data . channel . ... As mentioned above, the uvread routine can perform, at the programmers request, extra processing steps on the visibility data. ... If the original channels are numbers from 1 to , then, by using type='channel' , uvread will return massaged channels, where channel of the massaged channels is formed by averaging channels of the original data, starting at channel . ... If is specified as 0, then uvread will return as many channels as possible. object='reference' . ...

... The first of the equations defines the position of the spectral orders, m , in the raw image, while the second equation gives, for each order, the dispersion relation in one dimension. ... where the coefficients are computed using least squares techniques on a grid , i.e. sample number and line number of points located within the spectral orders of the image. These points in the grid are found automatically by an order--following algorithm, normally using the FLAT or STD image. ...

... Perform basic two-dimensional image reduction. Reject cosmic rays from CCD data. Process the contemporaneously obtained wavecal data to obtain the zeropoint shifts in the spectral and spatial directions. ... Subtract science image from wavecal . ... For each image in the science file, this task selects the wavecal in the wavecal file that is closest in time to the science image, and it copies the keyword values for the spectral shift from that wavecal header to the science header. calstis12 . ...

Comedi Documentation . ... I assume that your hardware device is in your computer, and that you know the relevant details about it, i.e., what kind of card it is, the I/O base, the IRQ, jumper settings related to input ranges, etc. To tell the comedi kernel module that you have a particular device, and some information about it, you will be running the comedi_config command. ... The overall info gives information about the device -- basically the same information as /proc/comedi. ...

You can also see this page in Russian with using KOI8 (X Windows) or CP1251 (MS Windows) Cyrillic coding. The Laboratory supports the space TV experiments, mainly in the planetary exploration missions. ... Image Co-registration . ... PHOBOS mission - Martian satellites investigations. Phobos on the Martian limb, the image from Phobos-2 probe from 02/28/89. ... Russian Space Bulletin. ... Last modified at June,26 1997 Alexey Kuzmin: akuzmin@mx.iki.rssi.ru . Back to IKI home page ...

... Stellar Evolution is driven entirely by the never ending battle between Pressure and Gravity . As imbalances are reached, the star is driven to find a new Energy source. ... Pressure and gravitational forces are equal, the star is stable and its core is sufficiently hot to fuse Hydrogen into Helium More about main sequence stars . ... The luminosity generated by the core fusion of Helium into Carbon is far greater than the shell luminosity associated with the fusion of Hydrogen into Helium. ...

... In the framework of a collaboration between ESO and OAT concerning the development of a data reduction pipeline and the related quality control subsystems software for UVES/VLT, a detailed feasibility study is being performed on the basis of data extracted from the EMMI/NTT archive. ... It is ESO policy to perform data reduction for VLT instruments in ``pipeline" mode, either at the observing premises or at headquarters. ... archive data were processed in pipeline mode; . ...

... Generate the list of ts les The rst thing to do is generate a le containing a list of the fits les you are interested in. ... You've de ned the in and out paths fitspath and mhpath, and the lename containing the list of ts les is called fitsfilelist. ... You generate all the lsfs les with lsfs_wrap, fitspath, mhpath, 'fitsfilelist', lsfspath Of course, if you're running IDL in a directory other than the one containing fitsfilelist, then you'll need to specify the path to fitsfilelist. ...

... Exposure Time Calculator (ETC) . Survey processing . ... VISTA is a 4-m class wide field survey telescope for the southern hemisphere, equipped with a near infrared camera (1.65 degree diameter field of view at VISTA's nominal pixel size) containing 67 million pixels of mean size 0.34 arcsec and available broad band filters at Z,Y,J,H,K s and a narrow band filter at 1.18 micron. A wide field visible camera, if constructed, could also be used on VISTA. ... Tile . ... ESO VISTA Public Surveys . ...