... 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 . ...

... SciSim release covered by this note . ... Data-Analysis-with-SAS in a simple and standardised way, and should allow calibration experts to re-assess the reliability of the different elements of XMM-Newton simulations. ... Also, a release of all calibration files to be used in the reduction, through the SAS, of SciSim generated data, is coordinated with this release. ... Furthermore, two SAS tasks (odffix and epicproc) had to be updated to make possible a proper SAS data reduction of simulated data. ...

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. ...

MAKING THE PROFILES . First of all you are expected to load a FITS file ("FILE"-"LOAD"). ... By pressing the middle button you copy the profile from the first profile window to the second one. ... An example: first integral can correspond to the profile of active region and second integral can correspond to the profile of quiet chromospheric region. ... The second profile (which is subtracted from the first one) you extract after clicking on "SUBTRACT"-"MARK QUIET PROFILE" and marking the region. ...

... Archives . ... X-ray summer school is on going. ... Recently I went to JSM 2007 and tried to attend talks about (bayesian) change point problems, which frequently appears in time series models, often found in economics. ... Tags: ARCH , Bayesian Block , challenges , change point problem , GARCH , light curves , summer school , X-ray . ... I received another type of changing point problem, defining a peak precisely, from a x-ray school student, who tried bayesian block but said it didn?t work. ...

... 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. ...

INTEGRAL AND RXTE OBSERVATIONS OF THE FAST X-RAY TRANSIENT XTEJ1901+014 D.I.Karasev, A.A.Lutovinov, and S.A.Grebenev Space Research Institute, Profsoyuznaya str. ... With the INTEGRAL/ISGRI the source was detected at a significance level of 20 with the persistent flux of 2.7 mCrab in a 17-100 keV energy band in 2003-2004 (during long observations of the Sagittarius arm region). ... Broadband (3-100 keV) energy spectrum of XTEJ1901+014 obtained by RXTE/PCA and INTEGRAL/ISGRI. ...

Next: Scattering properties Up: Polarization properties (transmitted radiation) Previous: Linear polarization: wavelength dependence . Traditionally, the main problem considered in connection with circular interstellar polarization is the meaning of the wavelength where changes the sign . ... This is also demonstrated by Fig. 19 (lower panel) which shows the wavelength dependence of the factors of linear and circular polarization for particles of magnetite as was done by Shapiro ([ 1975 ]). ...

... Next: 7 kslice_3d: slicing data Up: Karma User Manual Previous: 5 Volume Rendering a . The <kpvslice> programme allows you to use a two-dimensional image to define a slice through a three-dimensional data cube. ... The slice is drawn on the total column density or velocity field map, and the corresponding position-velocity diagram will appear in the other window. ... To load the cube, press the Cubes button in the left window and select a cube file. ... The image is displayed in the left window. ...

... The tension in members of the telescope changes as we move the dome, ch, azimuth, and tiedown tensions. The lifetime of a beam is counted in the number of times the change in tension goes through a cycle. ... Examples of telescope motion with corresponding unbalanced moment. ... The number of cycles were computed for : 5000, 10000, 15000, 20000 kipFeet momemnt change. ... The number of cycles on the telescope was computed using the change in the unbalanced moment (at a corner). ... cycles . ...

... F. A. Primini, and H. E. Payne, eds. See Spike Run.. ... It provides long range planning information to the scheduling team; it provides bright ob ject, timing, and orientation information to the observation planning team; and it provides graphical description of the observations and their constraints. ... Graphical User Interface (GUI) The GUI graphically displays the constraints that are computed by Spike and stored in the description files and in the database. ... See Spike Run.. ...