XMM-Newton Science Analysis System . ... compute the background lightcurve of the problem event file applying the following selection expression CCDNR==9 AND (XDSP_CORR < -3.E-4 OR XDSP_CORR > 3.E-4) From the lightcurve, calculate the fraction of the total time for each of the pre-defined levels of background. Compute the background template spectra by weighting each of the template spectra by the corresponding factor calculated from the ligthcurve. XMM-Newton SOC/SSC -- 2006-06-28 ...

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• Description

... 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. ...

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• Non-parametric Algorithms in Data Reduction at RATAN-600
• A New Entropy Measure Based on Multiple Resolution and Noise Modeling
• Multiwave Continuum Data Reduction at RATAN-600

Taking into account the result by Watanabe P=2.5 days in outburst, I reconstruct old set of photographic observations being partly lost, and add some new observations. ... The periodogram calculated with the method by Lafler and Kinman is shown. ... The last periodogram indicates peaks corresponding following possible periods with the double-wave light curve: 0.4236, 0.4650, 0.5379, 0.6064, 0.7365, 0.871, 1.168, 1.5437, 2.8173, and 6.89 days. ...

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• Conditionals
• GRB follow-up team

The database contains references to the papers, data files and links to the Internet resources related to measurements and calculations of the optical constants in the wavelength interval from X-rays to radio domain. ... References to some useful books and reviews on the subject (e.g. the classical handbooks edited by E.D.Palik) and links to Internet collections of optical constants and personal WWW pages with related software were also placed in the database. You have arrived at our welcome page. ...

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• Database of Optical Properties -- Level: subpage
• The 2175? feature

... Chapter 12: Near Infrared Camera and Multi-Object Spectrometer(NICMOS) > 12.5 Tabular Data . ... Only exposures using the corresponding configuration ( NIC1 , NIC2 , NIC3 ) may use a given camera?s apertures. ... One aperture in each camera ( NIC1?FIX , NIC2?FIX , NIC3?FIX ) corresponds to a fixed pixel at or near the center of the detector array, which will not change on orbit. ... Only exposures using the corresponding configuration ( NIC1 , NIC2 , NIC3 ) may use a given camera?s spectral elements...

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• Notation and Model
• Algorithms
• Technique

The following tasks belong to the category CALCULATION: . Calculations with set data'' In parentheses the name of the source file is given. ... Apply a flat field correction to a map by fitting a 2-D polynomial to the background. ( flat.c ) . ... Program to calculate flux in user defined box. ( flux.c ) . ... RESWRI derives the kinematical parameters from the observed velocity field by fitting tilted-rings to the velocity field and fits harmonic terms after convergence of the ROTCUR part of code. ...

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• Sheltran - IF construct
• MNRF Program Management and Background
• selfcal

Displays the current status of Echelle spectrograph and allows you to change the configuration. ... Select TUI:Save Window Positions to remember the state of this checkbutton. ... The contextual menu on each control can return that control to the current setting of the instrument. ... Note that it saves the state of the controls, not the actual state of the instrument, so you can save any preset you like without commanding the instrument. ... Then change any controls you like and press Apply to apply. ...

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• TUI:Instruments:NICFPS:NICFPS window
• MCP Menu documentation
• TUI:Telescope:Offset Types

... The orbits as follows are considered: INTERBALL Tail Probe (IB_TAIL) & Auroral Probe (IB_AUR), GEOTAIL (NASA/ISAS), and POLAR (NASA). ... The situation investigation aim is to select the following favourable spatial positions (FSP) : . ... FSP3 : That part of the FSP1 & FSP2 time intervals, which corresponds to the magnetic conjugations of the any couple of the considered spacecraft. ... The polar diagram plot . ... The geocentric distance (GCD) of the 4 spacecraft as a function of the time. ...

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• About modification of the INTERBALL orbital elements
• Magnetic mapping
• Corrected Geomagnetic Coordinates

Next: Sky background definition Up: Background Definition Previous: Smoothing spline interpolation . The command BACKGROUND/SMOOTH enables to define the background without previous order definition. This feature is useful for example to correct for the background the image required for the order definition. ... All above methods are implemented in command BACKGROUND/ECHELLE and selected by the echelle keyword BKGMTD . ...

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• Emission-line galaxies
• Radio data
• Order Definition

My colleagues and I have recently completed a series of observations of SN1999an. ... The telescope is located at Martin Observatory in Blacksburg, VA, and is operated by the Physics Department of Virginia Tech. Our IAU Minor Planet Center Observatory Code is 841. ... Attached you will find a copy of one of our images (in .jpg format) with the supernova indicated. ... Virginia Tech Department of Physics . Back to Bright Supernovae . Back to Supernova 1999an . ...

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Patterns of calculated concentrations by pollutant for different receptor territories corresponding to stations (furthest down the picture) and POs (the remainder). While all patterns are qualitatively similar, there are marked quantitative differences between territories. The pollutants go along the abscissa in the following sequence from left to right: CO, NO, NO 2 , NOx, O 3 , PM10, SO 2 , benzene, toluene, formaldehyde, xylene, Cd, Ni (the last four are meteoparameters). ...

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• Corrected Geomagnetic Coordinates
• Submission of questions

... Imagine that for every pixel in the color image, you take its luminance value (that's how bright it appears). ... In the end, you will have a histogram which counts how many times each luminance value appears in the image (that histogram can be used to analyze the distribution of the luminance values in the im