... 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...

... This example uses an error array to determine the errors in the radial profile. task: imcnts . ... xs imcnts err=vigsnr_err expo=xdata$snr_exp.pl expthr=95.0 bkgdex=xdata$snr_exp bkgdth=95.0 bkgderr=vigsnr_err # Run the imcnts task with the appropriate parameters source image file : vigsnr # vigsnr.imh source region descriptor: a 300 300 0 50 n=5 # 5 annuli centered at 300 , 300 , 0 and 50 pixels min/max radius background image file or cts/pixel: cr # From the same ...

The visibility amplitude bias (there is also a closure phase bias, but this one is nominally corrected by the raw data averaging pipeline) is related to non-Poisson detector statistics due to after-pulsing, and to fixed pattern noise due to non-linearities in the modulation stroke. We determine the bias using so-called incoherent scans, which record data even though the delay lines are deliberately set away from the white light fringe. ... Averaging triple products.. ... Background data loaded. ...

T he Siding Spring Survey (SSS) is a Near-Earth Object search program that utilises the 0.5-m Uppsala Schmidt Telescope at Siding Spring Observatory, N.S.W., Australia. ... The mission of the Siding Spring Survey is to contribute to the inventory of near-earth objects (NEOs), or more specifically, the potentially hazardous asteroids (PHAs) and comets (PHOs) that may pose a threat of impact and thus harm to civilization. ... Based on the CSS Mission page . ... Siding Spring Survey Main Page . ...

. XMM-Newton Science Analysis System . omsource (omsource-1.15.5) [xmmsas_20070708_1801-7.1.0] . Meta Index / Home Page This window allows the user to select circular background regions which will be used to determine a value of the mean background-counts per pixel which may then be used in the photometry background determination. Subsections . Summary of Widgets . Table . Delete . Aperture . Background regions . update time . OK . XMM-Newton SOC/SSC -- 2007-07-09

Next: Imaging Polarimetry with NICMOS Up: NICMOS Data Calibration and Previous: The Photometric Performance of . ... NICMOSlook and Calnic C . ... Extracting spectra from a large number of NICMOS grism images requires a convenient interactive tool which allows a user to manipulate direct/grism image pairs. ... NICMOSlook and Calnic-C are two programs that were designed to take advantage of the fact that the NICMOS grism mode typically consists of taking both a direct and a grism image. ...

This layer is defined with a <LAYER> tag. You see that the background image is applied to the rectangular region occupied by the layer. The height of the filled-in area is determined by the height value. ... The style definition sets the background-image property. The height of the filled-in area is determined by the actual content. ... The style definition also includes a value for border-width and border color. ... The style definition includes a value for layer-background-image. ...

Next: Background Correction Up: Reduction using Standard Previous: Order definition: Method . The parameter WIDTH2 is the width of the calibration lines. ... Now we can execute CALIBRATE/ECHELLE . ... CALIBRATE/ECHELLE DONE ! ... The user is prompted for the identification of two calibration lines on the image display, repeated in overlapped regions of adjacent orders. ... The wavelength calibration is wrong and apparently no identification error was made: There are too many lines per order. ...

... This paper describes the main algorithms used by the Einstein Level One processing to create the exposure masks and the background maps for Einstein IPC images, and how these algorithms were recreated in the IRAF environment. Our goal was to recreate the algorithms used by the Level One Processing to create exposure masks and background maps for Einstein Image Proportional Counter (IPC) data (cf. sections 2.5 and 2.7 of Harnden et al. ...

... You are here: start €Ё lbaops €Ё lbanov2008 €Ё v255c . ... lbaops:lbanov2008:v255c . v255c Setup: . ... IFP#1-LO 6640 - 6656 MHz USB RCP . ... IFP#2-LO 6640 - 6656 MHz USB LCP . ... IFP#2-HI 6656 - 6672 MHz USB LCP . ... IFP#1-LO 6300 - 6316 MHz USB LCP . ... Ftp: ftp://ftp.atnf.csiro.au/pub/people/vlbi/v255/v255c . ... The 4 x 16 MHz bandpass setup will require feeding two separate LOs into IFP#1 and #2 on the DAS /frequency translator and splitting the LCP signal so that is feed into both sides. ...

... Primordial theory review : Dick Bond . Defects and the CMB review : Andy Albrecht . ... Gravitational wave contribution to CMB anisotropies : V.B. Lukash and E.V. Mikheeva . C_l from cosmic strings : Lloyd Knox . Some aspects of CMB anisotropies induced from topological defects : Mairi Sakellariadou . ... CMB anisotropies from scaling sources : Ruth Durrer . ... SZ observations I : Sarah Church . ... Holes in the microwave sky? ... Detecting cosmic strings in the CMB : James Robinson . ...

. Aristarchus was extremely clever and also figured out a way to determine the ratio of distances between the earth and the moon and the earth and the sun. While wrong, at least he reasoned that the sun was much farther from the earth than the moon. Just Try and Follow this! . Summary of Greek Science .

... Telescope concept . ... The Submillimetron Project is dedicated to astronomical studies at the submillimeter and far infrared wavelengths using a cryogenic telescope located on the Russian segment of the International Space Station (ISS). The Astro Space Center of the Lebedev Institute of the Russian Academy of Sciences is responsible for developing the Submillimetron Project. ... Currently, the Astro Space Center is carrying out a pre-Project study under contract with the Russian Space Agency. ...

... The Time shift for April, 17-18 20 April 1999 . ... The INTMINS April 1999 operations schedule was done on the base of the MIR ground track long-term prediction using the MIR's orbital elements status on 29/03/99 . ... The investigation of the time shift behaviour was began before 29/03/99 on the base of the different orbital elements determined (by KIAM RAN) 22/03/99, 25/03/99 and continued on the base of the orbital elements determined at 31/03/99, 5/04/99. ... Modified 20 April 1999  ...

Next: Extragalactic Gravitational Wave Background Previous: Transparency of the Stochastic . Let the sky be observed with a detector having a pencil beam diagram across. The number of stars per frequency decade that is swept by the detector is a function of celestial coordinates (say, galactic coordinates l , b ): . ... It is clear from the figure that for an all-sky detector the Galaxy becomes transparent above the frequency  Hz. ...

... The Race to Reveal Our Universe . ... Credit: BOOMERANG Project , NSF Explanation: A race is underway to understand our universe through background radiation produced during its infancy. Observationally, increasingly accurate balloon experiments are pressing to beat future space-faring satellites to definitive measurements of universe-determining spot characteristics of the cosmic microwave background (CMB) radiation. ... Publications with words: universe - cosmic microwave background radiation . ...

Full Stokes 327-MHz Continuum Observations of the GALFACTS Pilot Region Wasim Ra ja, Avinash Deshpande, Tapasi Ghosh, Chris Salter & Andrew R. Taylor Background and Scientific Justification Several existing surveys have mapped the polarized intensity of the extended Galactic emission at various frequencies using single dish as well as synthesis imaging. ... The underlying distribution of the polarized emission and the magneto-ionic medium would be apparent in the images resolved across Faraday depth. ...

... A consistent theory of turbulence has not been constructed as yet (this problem is linked with one of the one million dollar problems of the Clay Mathematics Institute), and therefore researchers all over the world rely on computer simulations to understand the underlying physics and processes in star forming environments. As computer power grows our simulations become more and more realistic, allowing us to include a lot of interesting and potentially vital physics into our models.  ...

... Some of them are demonstrated above, and I'll address the "how-to" aspects one by one. ... Save your image as transparent based on the average color of your background tile. ... It will appear to be all one color now, but it's still finely dithered. Use your eyedropper tool to select one of the colors, and fill the bottom layer of your working image with it. ... Either way you go, this method is the first step to for all the other ones, it's from this file that we get our transparency mask. ...

... 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. ...