Next: Catalog Construction Up: Observations and Analysis Previous: Source Detections . ... It was assumed that the highest signal gives the most likely position of the source. ... Comparing the summed map with the maps from the individual energy ranges, the one which produced the smallest error box was chosen to represent the source position, as long as was greater than 4, a level chosen to reflect a reasonable degree of confidence in the detection. ...

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• Observations and Analysis
• Primary Catalog

... The HST uses an onboard model of its orbit to perform in real-time various control functions relating to spacecraft operations and observation support. ... New coefficients for the ephemeris are updated every other day, and are archived as FITS keywords for each HST observation data set. Using these coefficients,an observer can perform a variety of calibration and characterization calculations relating to the orbital position and velocity of the telescope. ...

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• Modern CCD Observations of Moving Celestial Objects: Algorithms and Software
• Robust Data Analysis Methods for Spectroscopy
• Identification and Analysis of Binary Star Systems using Probability Theory

The software package ERA (Ephemerides for Research in Astronomy) is a problem-oriented software system for solving heterogeneous calculating tasks of Ephemeris and Dynamical Astronomy. The package makes it possible to produce ephemeris calculations needed for both planning various observational programs and processing the resulting observations. ... The system includes packages of processing the position observations by both the Least Squares Method and by Kalman filtering. ...

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• (Untitled)
• Keywords_107

FGS Instrument Handbook for Cycle 24 . ... Fine Guidance Sensor Instrument Handbook for Cycle 24 > Chapter 5: FGS Calibration Program > 5.3 Linking Transfer and Position Mode Observations . ... Observations . ... As was mentioned in Section 3.4 , by using Transfer mode observations to determine a binary system?s true relative orbit, and using Position mode observations of nearby reference stars (and perhaps the binary as well) to determine the binary?s parallax, the system?s total mass can be derived. ...

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• WFPC2 Instrument Handbook Update
• Observing Faint Targets
• Using Multiple FP-POS positions with COS observations

... This task operates on event data in an event list. ... In the first two cases, the celestial coordinates of the reference point are taken respectively as the values of the RA_NOM , DEC_NOM or RA_OBJ , DEC_OBJ values in the input event file header. ... Although the OM attitude information may be more accurate, it will not be present throughout part of the observation, and as such, the default source for the attitude data should be "ahf". ...

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• Generation from In-Orbit Data

... Advises . Contact Advises . As an advise for amateurs we would like to underline: if it's possible, try to observe 3 asteroid positions per night and do not neglect to observe the Numbered Minor Planets in your telescope field of view as a "by product" of your observational programs. ... We think such estimations ought to be produced every morning after CCD observations of the moving celestial objects by observer himself. ...

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Position Switching Separation Tolerance with Arecibo in L-Band Travis McIntyre The University of New Mexico July 2010 Revised December 2013 Abstract The blocked telescope aperture at Arecibo creates standing waves in the bandpass around 1MHz. ... Test observations with Arecibo in L-Band show that position switching effectively removes standing waves for separations of one half FWHM or less. Standing waves remain for separations of one FWHM, increasing the rms of the baseline by 20%. ...

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• Reducing Mock DPS Observations in IDL
• Reducing Mock Pseudo-DPS Observations in IDL
• Spectral-Line Observing

Program: TRACE Purpose: TRACE plots image values at user given positions as function of distance to a plot centre (in 2-d (sub)sets). Category: ANALYSIS, PLOTTING File: trace.c Author: M.G.R. Vogelaar Keywords: INSET= Give set (, subset): Only one subset is allowed. ... XYBOX= Give size of box around one pixel: [3,3] The resulting value at a selected position is an average of the pixels in the defined box around that position. ... POSITION= Give position x, y: Physical values are allowed. ...

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• http://www.atnf.csiro.au/whats_on/workshops/synthesis2001/material/imanal.pdf
• http://www.atnf.csiro.au/whats_on/workshops/synthesis2003/talks/imanal.pdf
• Archive of VLBI Observations Majordomo List

Next: A Preliminary Investigation Up: Spatial Corrections of ROSAT Previous: Introduction . ... These tasks bin a time sorted photon event list based on an assigned phase that corresponds to the 402 second period of the wobble. ... The fundamental limitation of this method is how many source counts you have for centroiding each binned image section. ... Once the phase binned qpoes have been shifted in x,y so as to align the source centroid, they are restacked using 'qpappend_ftsi'. ...

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• The X-Ray Galactic SNR Catalog
• SAO RSDC Home Page - RRA - PSPC
• Chandra Images for SNR J0550.4-6823

Pulkovo NEO Page . ... EPOS Software Package . ... EPOS ( E phemeris P rogram for O bjects of the S olar system) is the Windows PC application for study and ephemeris support of observations of the Solar system objects. ... It controls the part of common data and transfers the control to one of the programs that solve the restricted set of tasks. ... So with the EPOS software package one can calculate the accurate ephemerides for many objects and get the quick illustration of their motion as well. ...

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• Pulkovo NEO Page: Estimation of Accuracy of the Observations
• Pulkovo NEO Page: Estimation of Observational Accuracy

Please enter the lightcurve file name and period search parameters: . Lightcurve file: . ... Apply the Heliocentric correction and convert all dates to Terrestrial Time (TT)? ... Also, the Heliocentric correction cannot be applied to such lightcurves. ... This period search service is also available at the mirror sites: Mirror 1 , Mirror 2 , Mirror 3 , Mirror 4 . You may download the latest source code distribution and install the period search service at your own web server. ...

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• The NMW survey homepage

... The J, H and K bands are characterized by a bright background, such a background is mainly due to the emission of atmospheric lines and of thermal radiation. ... If the source cover a large fraction of the slit, spectra off-source must be observed to adequately sample the sky background. ... The on chip integration time (time spent in each position of the slit) must not exceed 40 seconds in J and H bands and 60 seconds in K band. ... We suggest a sequence of 10 for each elementary integration time. ...

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• IBIS - Flat Fielding
• Arcetri H2O Ma