XMM-Newton Science Analysis System . bstools (ccftools-1.34) [xmmsas_20080701_1801-8.0.0] . Meta Index / Home Page The bstools package contains a small set of programs to support boresight misalignment calibration activities. The following tools are available: . ... strbs: Star Tracker BoreSight calculation . insbs: INStrument BoreSight calculation . srcinfov: compute position of SouRCe in Field Of View . ... XMM-Newton SOC/SSC -- 2008-07-02 ...

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FOS/BLUE Wavelength-Zeropoint Correction Procedure Summary: A significant time-dependent systematic shift of up to 7 quarter-stepped pixels (1.75 diodes) in the zero-point of the FOS/BL wavelength scale has been confirmed in FOS Instrument Science Report (ISR) CAL/FOS-149 (Rosa, Kerber, and Keyes). ... Figures 1 and 2 (PDF - 14 Kbytes) illustrate the magnitude of the observed shifts and the effectiveness of the quick-fix algorithm provided here. ... Obtain the FOS ISR: CAL/FOS-149 (PDF - 53 Kbytes) . ...

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• STIS Instrument Handbook
• Overall Instrument Description
• Chapter 2: Instrument Description

The VLTI Calibrator Selector Tool is a tool intended to assist in the selection of suitable interferometric calibrators for VLTI observations with MIDI and AMBER. It uses a model of the VLTI and its instruments to assess the fringe visibility, given the observed bandpass, the geometry, spectrum, and coordinates of the target and the time at which the observations are to be made. ... The tool offers an HTML/Java based interface and consists of two pages. ... The quality flag depends on LDD_chi2. ...

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• ESO - Paranal Instrumentation
• ESO - Processed Calibration Files for VLT instruments Now Available
• clMonitor

... Instruments are more complicated than star catalogs, but a MIDAS table file is still useful for holding the description of an instrument. ... The main sub-table contains information about the passbands used, and the second sub-table describes the detector(s). ... Basic data for an instrument file include the passbands used (and any coding that is used to represent them in the data); the detectors used, and their properties; and general information about temperature control and optical cleanliness. ...

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• Echelle Spectra
• Instrument Description: CASPEC
• mod_expires - Apache HTTP Server

... Description . Catalog . ... In the Catalog, we publish equatorial (ЮБ 2000 , ЮД 2000 ) and galactic (l,b) coordinates of cluster centers derived as the position of overdensity in 2MASS catalog (Koposov et al. ... Distances, color-excesses and ages are the mean-square values calculated using all available evaluations from different color-magnitude diagrams. ... There are individual pages for every cluster where all available plots and parameters are published. ... 2002). ...

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... CCD is a NICMOS 3 HgCdTe Focal Plane Array (FPS) 256x256 CCD . CCD pixel size = 40 m . CCD gain = 4.73 e - /ADU 0.2 (K.Gloria measured in 1994: 4.56 e - / ADU ( see plot here ) . CCD read noise = 110 e - / pixel 20 . ... Pixel scale = 0.48"/pixel @ f/5 (120 arcsec FOV), 0.24"/pixel @ f/10 (60 arcsec FOV), 0.11"/pixel @ f/20 (30 arcsec FOV) all binned 1x1 . ...

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• MILT Description
• APO 3.5-m Users Mail Servers
• Index of /arc35m/Instruments

... GSAOI Home . Instrument . ... The Gemini South Adaptive Optics Imager (GSAOI) is a near-infrared adaptive optics camera that will be used with the Multi-Conjugate Adaptive Optics (MCAO) system on the Gemini South 8-m telescope . ... Gemini's major instrumentation goal is to develop its Multi-Conjugate Adaptive Optics (MCAO) system for scientific use on Gemini South. ... Existing adaptive optics systems use a single natural guide star or artifical laser guide star to measure this image blur. ...

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• Gemini NIFS Brief Description.
• Gemini NIFS Manuals.
• Service and Calibration Manual

The following papers summarize the characterization and technical performance of IBIS : . ... Characterization of Fabry-Perot interferometers and multi-etalon transmission profiles. ... Righini, A., Cavallini, F., Reardon, K. P., 2010, Astronomy and Astrophysics , 515 , A85, . ... The filter wheel is located between the two interferometers. ... The interferometers can be rapidly tuned, simultaneously, so to allow sequential scanning of the spectral lines of interest (see movie in IBIS Intro ). ...

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• The Arcetri Spectral Code - E.Landi and M.Landini (2001)
• mod_auth_digest - Apache HTTP Server
• The LongSp Description

Orbital data : INTERBALL AZ GSE and GSM cartesian coordinates, GSE cartesian velocity (once per 10 minutes). ... Magnetic field data from IMAP experiment. Magnetic fileld absolute value and magnetic field index (the difference between absolute value and model value), status flag. ... Counts of H+ and O+ ions are accumulated during one spin period by detectors D6 (antisunward looking), D8 (spin plane), D10 (sunward looking) of TRICS2 subsystem (1.0-30 keV). ... TRICS1, TRICS2, TRICS3 subsystems: . ...

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• OMNIDIRECTIONAL PLASMA SENSOR VDP
• THE LOW ENERGY PLASMA COMPOSITION EXPERIMENT AMEI-2

... Instrument Description . Software: Version 4.0 . Version 3.0:Complete Documentation . ... ИОНОЗОНД ПАРУС, разработанный в ИЗМИРАН, предназначен для диагностики ионосферы и оперативного прогноза КВ связи. ... Общая структура ИОНОЗОНДА ПАРУС, Технические Характеристики , Конструктивные параметры на настоящий момент соответствуют модификации Комплекса: ВЕРСИЯ 3.0 . ... Там же находится полное описание Комплекса ИОНОЗОНД ПАРУС: ВЕРСИЯ 3.0 . ... 2004 IONOSONDE PARUS ...

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This diagram illustrates a frame-like layout with 'position: fixed'. The illustration shows a four-panel frameset. The top panel ("header") covers the entire width of the frameset and takes up 15% of the vertical space. ... To the right of the sidebar and below the header is the "main" area, whose dimensions are computed based on remaining available space. Finally, at the bottom, the "footer" area is 100px high and covers the entire width of the frameset. ...

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• Long description of example of cell background calculation
• Long description of example illustrating background calculation
• Long description of example illustrating table row height calculations and

... Exposure Time Calculator (ETC) . ... ESO - Public Surveys . ... the recommended values to use for DIT, . ... Detector on-chip integration (DIT): seconds. to your chosen value - a separate page gives recommended values to use for DIT - for modes 1 and 2 below you may wish to start with the maximum recommended values as these will minimize the effect of read noise (a total object exposure of Y secs with DIT=X secs will produce Y/X lots of read noise) and give you a lower limit on the time needed. ...

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• VISTA - Visible and Infrared Survey Telescope for Astronomy

... The properties of the currently available receivers are given in Table 3 . The columns of the table give the receiver name, frequency range, the typical System Temperature (T ), Gain, System Equivalent Flux Density (SEFD) and Half Power Beamwidth (HPBW) for zenith angles below 15 (as measured by Arecibo staff.) ... Full details of the ALFA observing system, its performance, how to join an ALFA Consortium, and the latest ALFA news is to be found via, http://www.naic.edu/alfa/ . ...

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• Arecibo Planetary Radar
• serverlList
• Arecibo Observatory L-Wide Band Receiver

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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• AI SPbU library of scattering codes

... It consists of two energy-angle analyzers EA-2 and EA-3 for low energy particles, and two identical oppositely directed time-of-flight (TOF) analyzers EM-1-1 and EM-1-2 for high energies. ... Analyzers of low energy charged particles (EA-2 and EA-3). ... The instruments allow to measure simultaneously in eight angular sectors evenly distributed in the angle 2 perpendicular to the satellite rotation axis, and sequentially in 7 energy intervals for each angular sector. ... Interval . ...

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• Cryogenic microwave load CryoLoad
• STDA files
• PhSRM

... Previous: The HERSCHEL/PACS Common Software System as Data Reduction System . ... The basic data reduction routines are coded in ANSI C. The high level scripting language Python is used to connect the C-routines allowing fast prototyping. Several Python scripts are written to produce the needed calibration data and to generate the final result, a wavelength calibrated data cube with the instrumental signatures removed. ... Figure 2: Mosaicked collapsed data cube of the galactic center . ...

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• Calibration and Performance Control for the VLT Instrumentation
• CIRSI Data Reduction System - CIRDR
• NASA's Instrument Control Markup Language (ICML)

Date: 11/24/2014 Time:05:26 Moon Age: 1.8 Available Observing Hours: 12.9 Observer: Instrument: Operator: Cage: Lebofsky, Bell 90PrimeOne Trueblood PF hours lost to: weather: 2.0 telescope: 0.0 instrument: 0.0 computer: 0.0 Time Temp Humidity Wind Vel. Wind Dir. Seeing Open 18:30 37.8F 50% 15 N 1.9 Close 05:20 37.1F 15% 15 NE 1.8 _________________ Description ______________________ Most of the night, seeing >2", which severely limited our available targets. ...

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• http://www.winer.org/Logs/NightLog-2014-10-25.txt
• http://www.winer.org/Logs/NightLog-2014-10-26.txt
• http://www.winer.org/Logs/NightLog-2014-10-27.txt

Program: CREATE Purpose: Creates a SET (and subsets) Category: UTILITY File: create.shl Author: K.G. Begeman Keywords: OUTSET= Name of set to create. ... N] This keyword is asked only when the set you want to create already exists. ... This item will be put in the header and will determine the coordinate system CTYPE1= Enter axis name of first axis [stop axis input] For the n_th axis the keyword will be CTYPEn=, like all the following keywords NAXIS1= Size of axis in grids. ...

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• The Parkes 21cm Multibeam Receiver
• casacore: Fitting_module
• casacore: casa::AppInfo Class Reference

... SFIT is a general-purpose code designed to optimize theoretical stellar spectra to an observed spectrum. ... While the programme expects input from "stdio", it is more natural to save commands in a file (eg "sfit_input") and run the code simply by . ... If the spectra to be fitted have a filename "star_spectrum", then the best fit spectrum will be written out, together with the renormalized input spectrum, to a file called "star_spectrum.fit". ... sets up model spectrum grid (and for 2nd star) . ...

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• Armagh Observatory
• Future Plans

... For the XRBs which are highly variable the concurrent presence of the RXTE/ASM that continuously measures their X-ray spectral states invites a new and innovative program to harness the available information to facilitate detailed studies of individual systems as well as comparative studies between classes of systems. ... This will enable them to quickly decide which data are worth putting in effort to extract and further analyze. ...

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• The AstroStat Slog Stat
• Topics in AstroStatistics
• The Chandra Multiwavelength Project (ChaMP)