... The WFPC2 CCDs have a small b ut significant charge transfer efficiency (CTE) problem which causes some signal to be lost when charge is transferred down the chip during readout. This has the effect of making objects at higher row numbers (more charge transfers) appear fainter than they would if they were at low row numbers. The effect depends on the temperature of the CCDs. ... It is also possible that proportional losses for fainter stars, at least with no background, may be larger. ...

... 313 = 0.108 AOT= 0.036 - 0.749 12 14 (Path Radiance): 3 MODIS/Terra (=466 ); 28.07.2001, 05:50 GTM 15 : 31 MODIS/Te rra (=11 ); 28.07.2001, 05:50 GTM 16 ; 17 MODIS/Terra: , 2001 . 18 ' ' : MODIS/ Terra, , 200 1 . ... 65 MODIS /TE RRA 1 284 286 288 290 292 294 296 284 286 288 290 292 294 296 , , . ... 291 .2 = 2 .7 0 MODIS /TERRA 2 284 286 288 290 292 294 296 298 284 286 288 290 292 294 296 298 , , 26 , ETM+/Lansat-7 MODIS/Terra ! ...

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... The current MOS procedure envisages a less complicated correction mechanism than for the PN. ... The CTI correction applies a scalar correction to the event list set, on an event by event basis, in order to correct for loss of charge which has occurred in reading out the CCD array. ... We expect to correct for a fixed amount of charge loss, and a fractional amount of charge loss, which depends on the number of row and column transfers completed. ... http://xmm.vilspa.esa.es/ xmmdoc/MOS/mos_cti.html ...

The success of any ALMA phase-calibration strategy, which incorporates phase transfer, depends on a good understanding of how the atmospheric path delay changes with frequency (e.g. Holdaway Pardo 2001). ... We find the wet dispersive path delay becomes a significant fraction ( 5 per cent) of the non-dispersive delay for the high-frequency ALMA bands ( 160 GHz, Bands 5 to 10). ... The full text of the memo is available here . ... Dispersive path delay . 2009 Emily Curtis ...

... 1 available ; Nd:YAG based laser transmitter; 24 W average power (100 MW peak power ) at 532 nm; Additional output at 1064 nm fundamental (currently 355 nm is not available ); 6 ns pulse width; 40 Hz operation; 80 cm diameter Cassegrain telescope receiver; Fully pointable (but generally aircraft restricted to within 45 o of zenith; Electronic gated photomultiplier tube detection with low-altitude chopper; Data collection is ... F. Airglow Mirror Systems: . ...

... However, in some situations it is advantageous to use an image-preserving fiber optic bundle in place of conventional imaging optics. ... The Coherent Fiber Bundle . ... In order to successfully couple light from an imaging fiber bundle to the CCD, the CCD and fiber bundle must be in very close proximity. ... Besides the transmission losses through a large piece of glass, fiber-optic bundles have a transmission loss due to changes in the fiber diameter as light traverses the bundle. ...

... scattered light in flats less than 0.5% across 5' field of view . scattered light in flats less than 0.5% across entire field . ... no greater than 10% across field, and calibrateable to better than 1%. no greater than 5% across field, and calibrateable to better than 0.5%. ... provide unvignetted illumination across detector with new SDSS filter set . ... throughput stable to better than 0.5% over course of a night. throughput stable to better than 5% over thermal cycling and seasonal variation . ...

... Telescopes . ... Fig. ... Theoretical optical resolving power of the MSS, depending on the phases of the moon under typical weather conditions. ... The optical resolving power of the telescope with the MSS allows to observe stars of up to the 12 magnitude. ... Currently, more than 90% of observational time with the MSS spectrograph is used in the spectropolarimeter mode with a diffraction grating 24.7њ. ... wide spectral region with a reciprocal linear dispersion of 9 ?/mm (0.1215 ?/pix) at a time. ...

Dwarf novae are a subclass of cataclysmic variable stars in which a late-type secondary fills its Roche lobe and transfers mass to a white dwarf primary via an accretion disc. ... Those spiral structures are very similar to the spiral shocks discovered by Sawada, Matsuda & Hachisu (1986) in 2D finite difference numerical simulations in accretion discs. In this poster, we want to compare 2D numerical simulations of accretion disc with the observations of SH2 . ...

... To determine a lower limit to the sensitivity of current observations to measurements of NS surface temperatures, we have used data from the Einstein Slew Survey (Elvis et al. 1990) to establish temperature limits for 275 pulsars which received nonzero exposure during the survey. ... Filled squares correspond to pulsars actually detected in the survey data; the smaller symbols correspond to upper limits to the count rates. ... Click here for plot of x-ray data vs. cooling curves. ...

The Neutral Atmosphere H20 O 2 Water Vapour Radiometry Bob Sault O 2 H20 1 2 Microwave Radiometry Water Its dipolar structure means that its melting and boiling points are much higher than other simple molecules (e.g. CO2, O2, N2). ... Water vapour introduces 50-300cm of excess path. ... 5 6 Water vapour radiometry Continuum vs Line systems "Continuum" water vapour radiometers measure fluctuations far from water lines Line systems work near either of the two water lines: 22.3 GHz or 183 GHz. ...

If an object emits a total power (energy per unit time) L (L for luminosity), this radiation will spread outward into space, becoming more spread-out and diffuse as it goes. ... If an object receives more heat than it dissipates, then its temperature will rise. ... Any object at a temperature above absolute zero will radiate energy. ... A is the surface area of the black body, T is its temperature, and s = 5.67 « 10 -8 Wm -2 K -4 (the Stefan-Boltzmann constant). ...

... A1­RP­AD­98001 Issue : DRAFT Page 34 of 42 3.13 Power dissipation The nominal power dissipated through each coil is: RMS: 1 Watt PEAK: 9 Watt capacitive sensors air damping The nominal power dissipated by each crate is: RMS: 475 Watt PEAK: 570 Watt These figures are given by the following contributions: capsens boards ?? Watt control board ?? ... Watt 3.14 Mirror thermal control design The cooling system get input refrigerant some C below ambient temperature from the MMT plant. ...

Next: Roche lobe overflow (stage Up: Principal Evolutionary States of Previous: Main-sequence stars (stage I) . ... The duration of this stage for a binary component is no longer a function of the stellar mass alone (as in the case of single stars), but also depends on the initial binary type (A, B or C) (Iben and Tutukov, 1985, 1987[ 74 , 75 ]): . The radius of the post-MS star rapidly increases (on a thermal time-scale)   and reaches characteristic giant values. ...

Institute of Electronics and Computer Sciences Riga, LATVIA "Eventech" Ltd, Riga, LATVIA Y. Artyukh, V.Vedin, E. Boole, V. Bespalko, G. Ozolinsh Presentation is supported by: European Regional Structural Fund WPLTN-2012 TECHNICAL WORKSHOP St. Petersburg, Russia, 24-28 September 2012 OUR SPECIALIZATION As known, Satellite Laser Ranging (SLR) provides observation data sets to satisfy the objectives of a wide range of scientific, engineering, and operational applications. ...

. To transfer files use the command: hhcp source_file destination-file . The source_file is the file that you want to transfer. It can be a file on your local host or on the remote host. The transfer can be in either direction. The destination_file is the copy of the source_file. It too can be on your local host or a remote host, depending on where the source file is. Getting access authorisation . Sending a file to a remote host . Getting files from a remote host . Managing the file transfer queue .

... Because of the Earth 's gravity, atmosphere is horizontally stratified (see, e.g., Kelley, 1989). Its structure can be organized by using the neutral gas temperature, as shown in the figure from mid-latitudes (note the logarithmic altitude scale). When going upward from the ground within the lowermost atmospheric region, troposphere, the temperature decreases up to about 10 km altitude (tropopause). ... Here the radiation also ionizes the neutral atmosphere, creating the ionosphere . ... 1989. ...

What happens to a star heavier than five solar masses? ... Stars about ten solar masses probably behave like our five solar mass star until they reach the end of core-helium burning. ... The Crab nebula was formed after a massive explosion ripped a star apart in 1054. ... Today, the glowing outer layers of the star are still rushing away from a tiny star in the centre. ... An incredible explosion rips through the outer layers of the star, releasing colossal amounts of energy in a supernova explosion. ...

Microsymposium 34, MS058, 2001 ANOMALIES OF THE MOON'S THERMAL EMISSION IN THE IR SPECTRAL RANGE (10.5 - 12.5 micron). ... Sternberg State Astronomical Institute, Moscow, 119899, Russia, pugach@sai.msu.ru Summary: New satellite measurements of the lunar-surface radiation temperature were used to construct the spatial angular function of thermal radiation of the Moon in the infrared (10.5-12.5 micron) spectral range. ... These thermal anomalies are observed only in the limited range of phase angles. ...