... To be read in conjunction with Section 4.11 of the WFPC2 Instrument Handbook , -Version 4.0. ... 1 The second study found evidence that CTE loss for faint stars has increased with time (Whitmore, 1998). The primary observational consequence of CTE loss is that a point source at the top of the chip appears to be fainter than if observed at the bottom of the chip, due to the loss of electrons as the star is read out down the chip (see Figure 1 ). ... Last updated: 06/16/98 10:38:00 . ...

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. ...

The Wind spacecraft. ... It was designed to observe the solar wind approaching Earth, from a position near the Lagrangian point L1, and it is part of the International Solar-Terrestrial Physics (ISTP) Initiative . ... The original plan called for "Wind" to approach its final station over two years, undergoing two close encounters with the Moon to boost its speed. ... For additional details and updates, see the home page of the "Wind" mission. Exploration" home page (index) Glossary . ...

... It was designed to observe the solar wind approaching Earth, from a position near the Lagrangian point L1, and it is part of the International Solar-Terrestrial Physics (ISTP) Initiative . ... The original plan called for "Wind" to approach its final station over two years, undergoing two close encounters with the Moon to boost its speed. ... If however the object is moving , the encounter is not symmetric, and in the end the spacecraft may have gained or lost speed, depending on its trajectory. ...

... 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. ...

Next: C.S. Jeffery, Research Astronomer Up: Research Previous: J.E. Chambers, Research Astronomer Contents . During 1998 Dr Gerry Doyle was involved with three PPARC PDRA research grants, and was also a co-organiser of two international conferences (the COSPAR Symposium `Activity Observed in the Sun and in Similar Stars', and the Armagh Cool Star Workshop `Solar and Stellar Activity: Similarities and Differences'). He was Associate Scientist with the CDS and SUMER instruments on SOHO. ...

GRANAT is the Russian x-ray sattelite launched to the high apogee orbit (200,000 km) and operated almost for 10 years (1989 -1999) , carrying out four major instruments: French SIGMA coded-mask hard x-ray telescope (30-1000 keV), Soviet ART-P coded-mask telescope (2??-60?? keV), all-sky monitor WATCH (6-150 keV), and a gamma-burst detector PHEBUS . ... Since September 1994, GRANAT is in the survey mode. ... Explore pages devoted to individual GRANAT instruments (including main scientific results): . ...

... the time of observation . ... Observing the Changing Position of the Sun To Establish Cardinal Directions . ... Observations of the Sun's apparent movement across the sky and its pattern of rising and setting in the east and west horizon helped to establish the cardinal directions. ... The final stage of the Sun's return was marked by the observation that the Sun had reached its highest altitude when the full width of your mitted hand could fill the gap between the Sun and the horizon. ...

... Data Analysis SAS News What is SAS? ... Calibration & Background Calibration Background Analysis . ... This document describes one of the projects assigned to me as part of my Young Graduate Trainee placement at ESAC, Spain. ... One project as part of placement involves the development of a new software task, which will form part of the general XMM-Newton scientific analysis package, SAS. ... The problem, however, lies in the way the data are binned in the original SAS process. ...

... 67Lawrence+ Of the 3118 sources in the Arecibo 611 MHz survey, 2911 have been observed using the NRAO 300 ft transit telescope at 6 cm. ... 4 Mean 1950 RA (see col.3.) ... 6 Mean 1950 Decl. (see col.3.). if A appears in col.1, the Arecibo dec. is listed. 7 Dec error in arc seconds (see col.3.) ... 16 Number of observations, in the form abc, where a is the number of observations averaged in RA, b is the number of observations averaged Dec, c is the number of observations averaged in flux. ...

Next: Radial velocity of the Up: Optical spectrum of IRAS04296 Previous: Observations and spectra reduction . ... However, molecular emission features are only very rarely observed in the optical spectra of PPNe. ... On the other hand, it is well known that cometary nuclei spectra show prominent Swan band emission. In both spectra of IRAS04296 we have discovered strong emission in the (0;0) and (0;1) bands of the Swan system of the molecule. ... Now consider the case of IRAS04296. ...

... About ATNF overview . ... Australia Telescope Steering Committee . ... Australia Telescope User Committee . ... Staff list | ... Murchison Radio-astronomy Observatory . ... Parkes radio telescope . Australia Telescope Compact Array . Mopra radio telescope . ... Australia Telescope Online Archive (ATOA) . ... VLBI . ... Australia Telescope 20GHz Survey . ... This message : [ Message body ] [ More options ( top , bottom ) ] . ... radio observations for the exploration of our Solar System and . ...

These observations are aimed at fully charactering FORS1 photometric system (UBVRI zero-points, color-terms and extinction coefficients) for the Tektronix 2048x2048 pixel CCD (24µm px) . To this aim, the two Landolt/Stetson photometric fields SA95 and SA101 will be observed on a number of epochs and at different airmasses during February and March 2007. ... SA101 . ... OBs for SA101 have to be observed during evenigh twilight (exceptions are expected for the second half of March) . ...

... Up: Data Analysis and Processing Techniques . ... Also, a method for quality control of CCD observations is suggested. ... Everyone who observes a celestial object using a CCD detects moving celestial objects as a ``by product''. ... We hope that our investigations may be useful for near-Earth space control and also for searches of the moving celestial objects through analysis of old and new CCD frames obtained at any amateur or professional astronomical observatory. ...

Next: Amorphous magnesium silicate Up: Examples of data contained Previous: Examples of data contained . ... We have used the infrared optical constants of forsterite contained in the database for calculating the absorption cross sections of spherical and non-spherical particles in the Rayleigh limit (see Fig. The spectra are obtained by averaging the cross sections calculated for the three different crystallographic directions. ...

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. ...

... Why does X-ray astronomy require satellite telescopes? ... That is why scientists use space based satellites to record and observe data from X-ray sources. ... It primarily observes X-ray sources and has a moderate imaging capabilities. ... X-rays (because of their short wavelengths) , as opposed to visual light, can penetrate through otherwise opaque objects e.g. bones X-rays can observe celestial objects that emit shorter wavelengths such as galaxies , quasars, and black holes. ... X-ray image . ...

... Polish scientists at the Space Research Centre, Polish Academy of Sciences, in Wroclaw, south-west Poland, have constructed an instrument called SphinX (short for Solar PHotometer In X-rays), which is an X-ray spectrophotometer, that will obtain spectra in the energy range 0.5--15 keV in 256 energy channels with frequency of up to 100 times a second. ... SphinX is part of a package of instruments known as TESIS (PI Prof. Sergei Kuzin, Lebedev Institute, Moscow). ... Space Research Centre, . ...

... Meade Instruments Corporation . ... Choosing the Right Microscope . ... On most microscopes the specimen glass remains fixed while the microscope's objective lens and eyepiece move as a unit up or down to focus the image. ... Eyepieces of varying powers work with objective lenses of varying powers to yield a range of microscope magnifications. ... Magnification: The effective magnification of a microscope is determined by multiplying the eyepiece power by the objective lens power . ... about meade |...

... It runs on unix, MacOS and possibly on Windows. ... On MacOS or Windows, double-click TUI. If MacOS complains that the application is unsigned then right-click TUI and select Open. ... If you have never run TUI before, set up your preferences before proceeding (for help on any item, right-click on the control and select Help from the menu that appears): . ... To save your window positions and remember which windows to open at startup, select Save Window Positions from the TUI menu. ...