... The exact directions of the offsets are parallel to the rows and columns of the CCD on which the aperture is specified. ... It is often useful to explicitly specify the desired rotation of the WFPC2 field-of-view on the sky. ... Figure 7.8 shows the CCD orientation and aperture locations relative to the U3 axis. ... Obtain the Position Angle (PA) of the source axis on the sky, measured in the standard way, North through East. ... desired source angle in field-of-view measured CW from +U3 axis) . ...

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• Fine Guidance Sensor Instrument Handbook
• Phase II Example: NICMOS Parallel Observations
• Mode = POSConfig = FGS

HI spectral-line observations of galaxies (Karen O'Neil) . Measuring the width, flux, etc. of the HI profile of two galaxies, using some combination of : dwarf emission line, HVC emission line, spiral emission line, and spiral absorption line. This project was designed to demonstrate the fundamentals of spectral line observing and position switching. ... The types of galaxies observed in this project are being kept open and will be determined when the project LST is known. ...

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• on,off position switching offsets
• Spectral Line Observations at AO
• Making Maps: Example + Animation

This layer is defined with a <LAYER> tag. You see that the background color is applied to the rectangular region occupied by the layer. The height of the colored area is determined by the height value. This layer is defined in CSS syntax. The style definition sets the position and background color, but doesn't set any values for border characteristics. ... The style definition includes a value for border-width. ... The style definition includes a value for layer-background-color. ...

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• Dynamic HTML in Communicator
• Long description for example illustrating positioning with respect to a
• Long description for example illustrating absolute positioning

... The processing of these associated images presents new challenges to the HST data processing pipelines, which heretofore operated only on single images. ... Stage 1 (CALNICA) calibrates individual exposures without information from other members of the association. ... Stage 2 of calibration (CALNICB) only operates on associated images that have previously gone through CALNICA processing, and creates combined images for each distinct (non-overlapping) pointing within the association. ...

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• GIRA - Two Channel Photometric Restoration
• Calculating the Position and Velocity Components of HST
• QPSIM: An IRAF/PROS Tool for Source Simulation

... Here follow some typical calls to epchain : epchain This processes the first IMAGING mode exposure (i.e. PNS010) and is equivalent to one of the calls epchain datamode = IMAGING odfaccess = odf exposure =010 schedule=S epchain datamode = IMAGING odfaccess =oal exposure =1 epchain datamode = IMAGING exposure =1 epchain odfaccess =name ... The call epchain datamode=ALL odfaccess=all will process all exposures of an ODF, independent of observing mode. ...

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• SourceListFile
• Example 3: Point source with explicit position

... Activity 3: Measuring the Position of the Sun in the Sky . Purpose: To give students the opportunity to measure the position of the Sun in the sky using simple tools and methods. ... Alternatively, you may have students devise their own methods of relative measurement and apply them to measuring the position of the Sun in the sky. ... Rangi is the sky, and when the Sun is near Rangi's head it is summer in New Zealand. ... Read the Maori story to students. ... back to Teachers' Newsletter Main Page ...

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• ASP: Indiana Jones and the Astronomers of Yore
• ASP: Making Your Own Astronomical Camera

... An OBJECT column gives the name of the object observed (usually a star name). ... In critical cases, it is common practice to measure sky on two or more positions around a target object, and these positions must be identified. ... A general treatment of this problem requires a column called OBJECT, bearing the usual name of the object (as in the star tables); a column labelled STARSKY, to distinguish between star+sky, star alone, or sky alone; and additional columns to identify the sky position. ...

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• Source Positions
• HTML Tag Reference
• Background Correction

... We received the SASS output for the HRI observation of 3C 120 (a highly variable radio galaxy with a prominent jet leaving the core at PA ) and smoothed the data with a Gaussian of FWHM = 3 '' ( Figure 13.1 ). ... The results are shown in Figure 13.2 . ... The FWHM of the original data ( Figure 13.1 ) is 11.8 (PA ); after dewobbling ( Figure 13.2 ) the width of the 50% contour is 7.6 . ... Figure 13.1 : The original data, smoothed with a Gaussian of FWHM = 3 . ...

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• QPOE Files
• Charged Particle Subtraction
• Determine a background subtracted radial profile

Pulkovo NEO Page . ... NEA Accuracy Estimation . ... The estimation of accuracy of the current CCD observations of asteroids and comets is constantly performed at Pulkovo Observatory. ... The (O-C) values, so called "Observed" minus "Calculated" positions, characterize numerically the observations of any observatory, both professional and amateur, during a short period (one or several close nights). ... So the (O-C) values for these objects nearly entirely define the errors of observations. ...

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• Pulkovo NEO Page: Estimation of Observational Accuracy
• Catalogue of double stars

Next: Head Positions and Track Up: OBSOLETE SECTIONS Previous: Mark III Observations Contents . ... Mark II recording systems have been removed from most active VLBI stations and the main Mark II correlators are no longer operating. ... Below is an example of a simple Mark II schedule. ... OBSMODE = '6cm Mark~II Standard Setup' ! ... SRCFILE = sources.obs ! ... EXAMPLE: Setup file for Mark~II observations (1 channel) at 6cm. -------------------------------------------------------------------- ! ...

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• PRECDATE
• casacore: casa::SolarPos Class Reference
• Tidbinbilla

The large magnetic cloud caused by coronal mass ejection at the Sun on January 6, 1997 came to the Earth at early morning on January 10 and continue to interact with Earth's magnetosphere till January 11 (see for example home page of this event prepeared by Dr. M.Peredo http://www-istp.gsfc.nasa.gov/istp/cloud_jan97/event.html ). ... During the days discussed here INTERBALL-1 satellite was in the magnetosphere (MS) near its dusk flunk - see the Fig. 1 for compearing. ...

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• Two points (INTERBALL-1 and MAGION-4) observations of magnetopause motion
• Shift
• The INTERBALL Auroral PROBE orbital elements

traxy -- Transform an X,Y position from input to output pixel position using the same conventions as drizzle traxy xin yin . xin = 400 [real] . ... The X dimension of the input image (this is used to determine the centre which is the origin of the transformations). (nyin = 800) [real] . ... So, if an object on an input image at a certain position is drizzled with a given set of parameters then the position of that object on the output can be predicted using traxy with the same parameter values. ...

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• TRANBACK (V0.2) --- Dec99 --- TRANBACK (V0.2)
• NICMOS Observes the Galactic Center
• POLIMPLOT (V1.00) --- April99 --- POLIMPLOT (V1.00)

New reduction of minor planets photographic plates obtained with Pulkovo Normal Astrograph A.A. Berezhnoy Pulkovo Observatory of RAS, Saint-Petersburg, Russia Minor Planet observations at Pulkovo Periodical observations of 14 bright asteroids named Selected Minor Planets (SMP) were performed at Pulkovo since 1948 within the international framework started by works of B.V. Numerov and D. Brouwer. ... 108 133 113 74 124 67 97 88 14 84 64 5 20 19 Epochs (YYYY.MM) 1200 Mean values of total obs. ...

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• http://www.puldb.ru/nikolaev_2011/PUB_NIKOLAEV_2011/damian.pdf
• http://www.puldb.ru/nikolaev_2011/PUB_NIKOLAEV_2011/mu.pdf
• Pulkovo Database of Observations of Visual Double Stars

... 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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• Discussion of MOC and "Face on Mars"
• IBIS - Installation
• Algorithm

... This appartus will drop a mass from different heights. When the mass strikes the ground, some percentage of its original energy will be absorbed by the ground. ... The percentage of the energy which is absorbed by the surface on each "bounce" (EAS) . ... The impact velocity of the object will also be given at each bounce. ... Start= Drop the ball after Energy, Mass and EAS have been set; resume after step or pause has been selected . ... Reset = Reset experiment to intial values . ...

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• THE HUBBLE LAW JAVA APPLET
• Astronomy HyperText Book
• The Galaxy Gallery Page VII: Infrared Imaging

Observation of the Sunyaev-Zel'dovich E ect toward CL0016+16 at 43 GHz M. Tsuboi et al. Ibaraki University, Japan We performed a mapping observation of the Sunyaev-Zel'dovich e ect toward a distant cluster of galaxies, CL0016+16, at 43 GHz using a newly developed 6-beam SIS receiver installed in the Nobeyama 45-m telescope. The temperature decrement of the cosmic microwave background radiation was measured to be
T  A = 0:490:05 mK at the central position of the cluster. ...

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• Determination of the relative orientation between radio and dynamical reference
• PPEUC Programme - Cosmic Microwave Background Workshop
• OptInt PmWiki : PmWiki / Wiki Style Examples

Beijing Ancient Observatory . ... Credit Copyright: Judy Tobin Explanation: Did observatories exist before telescopes ? One example that still stands today is the Beijing Ancient Observatory in China . ... It is interesting to compare the above picture to one taken in 1895 . ... NASA Web Site Statements, Warnings, and Disclaimers . NASA Official: Jay Norris. ... A service of: LHEA at NASA / GSFC . ... U. Based on Astronomy Picture Of the Day ...

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• XWare > APOD

... Time calculated from Fermi GBM Trigger Time = 14:12:08.67 ( Connaughton, GCN 9230 ). 1% coincident with our start zero image time. 3x3 degrees around Swift XRT position . ... SUBJECT: GRB 090424 : MASTER-Net prompt optical limit DATE: 09/04/25 20:29:42 GMT FROM: Vladimir Lipunov at Moscow State U/Krylov Obs E. Gorbovskoy, V. Lipunov, V.Kornilov, A.Belinski ... Our observations results: ---------------------------------------------------------------------- Fermi GRB Trigg.* ...

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• MASTER GRB101123A prompt observations

polimplot -- Plot a polarization vector map . ... inpol = "" [name] . Input linear polarization image (in %) to plot. inpopa = "" [name] . Input image for position angle of linear polarization vectors (degrees). poi_err = "" [boolean] . ... Name of corresponding polarization position angle error image (degrees). ... This task is a flexible tool for plotting a polarization vector map from two images of the polarization and the position angle of the polarization vector. ...

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• Astrometry
• OYSTER Lab
• Positions of the telescopes used in the 1.3 mm VLBI observations of the quasar

Astronomy Terms - To Help You Study The Universe . Articles | ... Learning about the universe, or the study of astronomy, can be fun for the individual or for the whole family. ... Learning a few simple terms will help you with this fascinating study. ... You will use a telescope or binoculars for your observation of the sky at night. ... Celestial Terms . ... Meteor or a shooting star – the light caused when a meteoroid burns up in Earth's . ... www.astronomy.net . About Astronomy Net | ...

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• Magnification (Power) And Using Eyepieces - an Astronomy Net Article
• U.S. Naval Observatory, AstroGuide Listing