... User Guide ] Task: uvgains Purpose: Create baseline-based channel gains from averaged uv-data Categories: uv analysis UVGAINS averages uv-data, and creates channel gains for each baseline for either spectral line or wideband channels. ... To apply the channel gains to another uv-data file, use COPYHD to copy the channel gains items (cgains, ncgains, ncbase) or wideband gains items (wgains, nwgains, nwbase) into the other uv-data file. ... Only un-averaged channel data can be used with options...

Next: Trouble Shooting at the Telescope Up: Spectral Line Appendices Previous: Basic Analyz Routines - For use with data taken AFTER March 6, 2000 . ... setvel : Uses the "optical" definition to convert frequencies to velocity, and then stores the velocities in register 41. ... Line 1 - The area, central velocity, and width at 50% of the mean flux. ... rcl 8;sto 501 To begin working on your data again, you must the restore both the data and frequecy info: rcl 500;sto 43;rcl 501;sto 8 . ... sto 43 . ...

Next: NPOI raw packet data Up: Introduction Previous: NAT data Contents . These procedures use more elementary functions to produce diagnostic plots. plot_fdldelay , baseline _int [, beam _int ][, /slide ] Plot the residual FDL delay in microns. If keyword slide is 1, then open a sliding plot widget. plot_fdlpower , baseline _int [, beam _int ][, /sf ] Plot a power spectrum (or structure function if sf=1 ) of the delay. ... If beam is not specified, use currently loaded data. ...

... The CDBS relations for the FOS reference files and reference tables are described below. ... There is one entry for each detector, disperser, aperture, and polarizer combination. cyccs7r: GIM correction scale factors used to scale the modeled shift of the spectrum due to the earth's magnetic field. cyccs8r: Predicted background count rates as a function of geomagnetic position used to scale the background reference file. cyccs9r : Un-illuminated diode ranges for each detector and grating combination...

... The very first step after correcting bias, dark, and overscan is to find the edges of the slitlets. This is done by the command LOCATE/MOS . This command takes the central trace of a flat-field and detects the edges of the slitlet by simple threshold comparison. ... The offsets in dispersion direction between the slitlets will be read from the header of the flat-field frame for FORS data and stored in :xoffset . ... The actual flat-correction is then performed with COMPUTE/IMAGE . ...

The main steps in the reduction of NIR spectroscopic data are flat-field correction, subtraction of sky emission, wavelength calibration, correction for telluric absorption and correction for optical system plus detector efficency. ... Sky subtracted frames are corrected computing analitically the tilt angle from the instrumental calibration parameters or directly measuring it from the data. ... The same procedures are applied to the reference stars frames to obtain the calibration spectra. ...

... Meta Index / Home Page This section documents warnings and errors generated by this task (if any). ... Refer to the index of all errors and warnings available in the HTML version of the SAS documentation. diffBin . ... Star catalogue not found- no astrometry correction done . warning . ... corrective action: < . Too few sources for astrometryNeed at least 10 stars to do a reliable correction . ... corrective action: No stars in catalogue- catalogue has not been used to correct positions . ...

... We start investigating the results from a non-magnetized (isotropic) plasma, before including the external magnetic field so important for space physics. ... propagating above the electron plasma frequency, w(pe) (reflection point for the waves) . note that, for very high frequencies, both phase and group velocities are equal to light velocity c, and we have electromagnetic wave in free space: even the electrons are unable to respond to the rapidly oscillating electric field! . ...

ALMA | ... In this section, we explain why we need to correct phase fluctuations and ALMA's strategy to do this. Rapid fluctuations will be corrected with water vapour radiometers (WVRs). The Cavendish Astrophysics Group was also a leading contributor to the ALMA prototype WVRs, which were put through their paces in tests at the Submillimeter Array (SMA). ... The Cavendish Astrophysics Group in partnership with the Onsala Space Observatory built two prototype WVRs for the ALMA project. ...

Integration and performance of the flight configuration SIR on TELIS P. Yagoubov1, G. de Lange1, A. de Lange, M. Romanini, R. Hoogeveen1, V. Koshelets2, G. Wagner3, M. Birk 1Nation 3 al Institute for ... Netherlands 2Institute of Radio Engineering and Electronics, IREE, Russia 3Institute for Remote Sensing Technology, DLR, Germany Abstract TELIS (Terahertz and submm Limb Sounder) is a cooperation between European institutes, DLR, RAL and SRON, to build a three- ... LO frequency 624.93 GHz. ...

... Left: A POSSM plot of the uncalibrated spectrum of DA 193 at 1.66 GHz on a baseline Bear Lakes to Noto. ... The phase slope as a function of frequency is clear evidence for a small delay error in the correlator model. Right: The same data as shown on the left, but corrected for a delay error and a residual fringe rate. ... Left: A VPLOT plot of the uncalibrated amplitude (upper frame) and uncalibrated phase (lower frame) as a function of time for the source DA 193 on a baseline HartRAO to Noto. ...

... comedi_dio_config -- change input/output properties of channel . ... int comedi_dio_config (comedi_t * device, unsigned int subdevice, unsigned int channel, unsigned int direction); . The function comedi_dio_config() configures individual channels in a digital I/O subdevice to be either input or output, depending on the value of parameter direction. ... Depending on the capabilities of the hardware device, multiple channels may be grouped together to determine direction. ...

Russian SHAREABLE DATA CENTER Institute of Solar-Terrestial Physics SB RAS . ... The algorithm and appropriate program for decametric radiosignal propagation conditions prediction for paths from 500 to 9000 km have been developed at ISTP SB on the basis of normal wave method (AltyntsevaB.I,Iliyin N.V., Kurkin V.I. and others //Decameters channel simulation on the base of normal wave method . ... Solar activity indices are chosen automatically from the prediction date from the database . ...

... IRAF View . This is the orientation of the image as viewed in an image display via IRAF (e.g. ximtool, saoimage). Note: This is different from the orientation of the image as viewed on a Macintosh, via Remark . ... A +X, +Y instrument offset will move a star in the direction indicated by the arrows. ... Note: The offset direction depends upon which interface the offset command was issued in! ... Note: This is different from the orientation of the image as viewed by IRAF. ...

Winer Observatory P.O. Box 797, Sonoita, Arizona 85637-0797, USA . ... 2/3-m Telescope . ... Irvin M. Winer . ... Science . ... Tom Kaye, an amateur astronomer from the Chicago, Illinois area, installed his Tau Boo campaign equipment at our facility in mid-February, 2000. ... The custom unit fed the starlight to an optical fiber that transmits the light to a bench spectrograph located in the Winer machine shop. ... The daily results from mid-February, 2000 to early March, 2000 are shown on the left. ...

grdgradient - Compute directional derivative or gradient from 2-D grd file representing z(x,y) grdgradient in _ grdfile -G out _ grdfile [ -A azim [/ azim2 ] ] [ -D [ c ][ o ][ n ] ] [ -L flag ] [ -M ] [ -N [ e ][ t ][ amp ][/ sigma [/ offset ]] ] [ -S slopefile ] [ -V ] grdgradient may be used to compute the directional derivative in a given direction ( -A ), or the direction ( -S ) [and the magnitude ( -D )] of the vector gradient of the data. ... If amp is not given, default amp = 1. ...

. Departement of Quantum Astrophysics . Head: Kurt V.G. , Prof. ultraviolet spectroscopy of planetary upper atmospheres and interplanetary/interstellar medium; . observations of gamma-bursts and optical identification of their sources; . long-base optical interferometry. Staff: .

Communications For Your Astronomy Event . ... For many years two-way radios had a feature called by many names including Motorola's Private Line, GE/Ericsson's "Channel Guard", E.F. Johnson's "Call Guard", RCA's "Quiet Channel." ... Some call it by the most correct name (probably) of Continuous Tone Coded Squelch System (CTCSS). ... Since most radios seem to have adopted a 1 - 38 sub-channel system we at last have a way to express what CTCSS tone we all wish to utilize with a simple number. ... Tone . ...

Next: Data and Image Processing . ... The EKH method is then a division in the Fourier plane by this sine function, which is equivalent to a convolution in the image plane by the Fourier transform of this cosec function (an infinite set of delta functions separated by the beam throw, positive on one side of the origin and negative on the other). ... Figure 1: EKH restoration of simulated data: image plane (left), Fourier plane (right) illustrating EKH sine-wave pattern of noise. ...

... Research . directions . ... By convention the scientific investigations conducted in the Laboratory can be subclassified into some groups: . 1. investigations of a real structure and phase transformations, determination of correlation between a structure and properties . ... in HTSC materials and oxide systems with a perovskite structure (V.Sh. ... Investigation of diffraction mechanisms of the diffraction image formation of defects in a crystal lattice . ... Copyright 2005 LSR ISSP RAS . ...