SAS home . SAS Watchout items . ... This thread contains a step-by-step recipe to extract a light curve of a point-like source for all the X-ray cameras, subtracting the background and correcting for exposure loses. ... The SAS task barycen performs this correction. ... If the following files are available: a) RGS event list; b) RGS source list, a call to the task performing light curve extraction, correction and background subtraction rgslccorr allows a user to create the light curve. ...

Top] [Prev] [Next] [Bottom] . Table 7.1 lists certain effects owing to the design of the FOC detector, optics, and electronics that afflict all FOC images and indicates whether the pipeline corrects for them. Characteristics Corrected in Standard Pipeline . ... The diagram below (Figure 7.1 ) describes where these various instrumental characteristics arise. ... The following sections describe the limitations of these calibrations and their effects on the uncorrected image characteristics. ...

Next: Bivariate polynomial interpolation Up: Echelle Spectra Previous: Removal of particle . The estimation of the background is one of the critical points in the reduction of echelle spectra for two reasons. ... diffuse light in the interorder space coming from adjacent orders. sky background spectrum . ... These locations are defined when performing the order definition (command DEFINE/ECHELLE or DEFINE/HOUGH ) and can be displayed by command LOAD/ECHELLE . ... Sky background definition . ...

Next: *imcalc* - Obtain a Up: Calibration Previous: Exposure Map . Background maps are provided by the standard processing for all ROSAT and Einstein instruments. For the PSPC and IPC these are in three standard bands: soft, hard, and broad (Table 6.2). ... N.B.: ROSAT PSPC background maps in SASS 5-6 or higher are generated by smoothing a source-subtracted, exposure corrected image (see the ROSAT Data Products Guide). ... imcalc* - Obtain a background subtracted image for ROSAT PSPC Data . ...

... Next: The PROS Big Up: Software Systems Previous: Data Reduction Software . ... The srcinten task provides PROS users with a tool to compute count rates for point sources in the ROSAT High Resolution Imager (HRI). ... Corrected upper limits are cited at locations where the count rate falls below the source detection threshold. ... Srcinten is a new PROS task that computes and applies the above correction factors to the net counts in a user-specified aperture. ...

ALMA | ... In this section, we explain why we need to correct phase fluctuations and ALMA's strategy to do this. Rapid fluctuations will be corrected with water vapour radiometers (WVRs). The Cavendish Astrophysics Group was also a leading contributor to the ALMA prototype WVRs, which were put through their paces in tests at the Submillimeter Array (SMA). ... The Cavendish Astrophysics Group in partnership with the Onsala Space Observatory built two prototype WVRs for the ALMA project. ...

... ATNF Home . ... About ATNF overview . ... Australia Telescope Steering Committee . ... Murchison Radio-astronomy Observatory . ... Parkes radio telescope . ... Parkes | ... Parkes projects/positions database . ... R.J. Sault, G.J. Carrad, P.J. Hall, J. Crofts, 2000, ``Radio path length correction using water vapourradiometry'' submitted to Proceedings of WARS 2000 . Bob Sault, Peter Hall, Graeme Carrad, 1999 "Atmospheric phase correction for the ATCA" , presented at URSI 1999 (Toronto, Canada). ...

The visibility amplitude bias (there is also a closure phase bias, but this one is nominally corrected by the raw data averaging pipeline) is related to non-Poisson detector statistics due to after-pulsing, and to fixed pattern noise due to non-linearities in the modulation stroke. We determine the bias using so-called incoherent scans, which record data even though the delay lines are deliberately set away from the white light fringe. ... Averaging triple products.. ... Background data loaded. ...

... 14.1 Foreground color: the 'color' property . ... 14.2.1 Background properties: 'background-color' , 'background-image' , 'background-repeat' , 'background-attachment' , 'background-position' , and 'background' . ... Background properties are not inherited, but the parent box's background will shine through by default because of the initial 'transparent' value on 'background-color' . ... BODY { background: white url("pendant.gif"); background-repeat: repeat-y; background-position: center; } . ...

... Step 1: The magnetic field line tracing from the satellite position up to magnetic equatorial plane using IGRF magnetic field model. Step 2: Tracing back from the point (produced on the Step 1) to the Ionosphere (by using only dipole magnetic field) . ... The magnetic field line tracing from the satellite position up to the Ionosphere (the stop trace altitude 110 km) using Main (dipole) + Extraterrestrial magnetic field model (for example, Tsyganenko [1987], or [1989], or [1990] ) . ...

T he Siding Spring Survey (SSS) is a Near-Earth Object search program that utilises the 0.5-m Uppsala Schmidt Telescope at Siding Spring Observatory, N.S.W., Australia. ... The mission of the Siding Spring Survey is to contribute to the inventory of near-earth objects (NEOs), or more specifically, the potentially hazardous asteroids (PHAs) and comets (PHOs) that may pose a threat of impact and thus harm to civilization. ... Based on the CSS Mission page . ... Siding Spring Survey Main Page . ...

Project P1979 (snezana and joel) were doing HI absorption on pulsars using 9 level sampling and folding mode with the wapps dumping acfs. ... If you are storing acf's, then the data is written to disc after step 4. ... Idl routines (written by me) are able to read pulsar wapp acf data and do the kulkarni/heiles 3 level correction and murray lewis's 9 level correction (actually the 9 level idl code was written to find this problem and is probably not in the production library yet.. ...

... 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. ...

... Step 1: The Footprint position calculation by the magnetic field line tracing from the satellite position up to the Ionosphere by using IGRF + Tsyganenko [1987] magnetic field model (the stop trace altitude 110 km). Step 2: Tracing back from the Footprint (produced on the Step 1) to the dipole equatorial plane (by using only IGRF magnetic field model up to the geocentric distance 8 RE and dipole field model after this distance). ... Back to the description . ...

Notes concerning the observations made by UKIRT for the YY Gem programme in March 1988. ... As spot modulation effects are relatively more prominent in V and flare effects in B, it was decided to monitor in K and V during eclipses and in K and B at out of eclipse phases. ... The data were corrected for extinction using the following extinction coefficients: B 0.27, V 0.10, K 0.07, J 0.10 . ... The following colour equations were derived for the UKIRT optical data using VISPHOT. ...

... The Near-Infrared Camera/Fabry-Perot Spectrometer (NIC-FPS) is a collaborative effort of the University of Colorado, the Astrophysical Research Consortium, Apache Point Observatory, and Ball Aerospace. It consists of a near-infrared imaging camera and a Fabry-Perot etalon which can be moved in and out of the beam, enabling full-field spectrometry with a selection of narrowband filters as blockers. ... CCD is a Rockwell Hawaii-1RG detector 1024 x1024 . CCD pixel size = 18 m . ...

Next: Gravitational Wave Background from Previous: Galactic Gravitational Wave Background . ... It is intuitively clear that at frequencies above the critical ones for our Galaxy, one will detect rare bright jerks produced by coalescing white dwarfs   (at a rate of 1 per 100 year) and NS (at a rate of 1 per - year) in our Galaxy, against a background of the extragalactic stochastic GW. ... Firstly we consider GWB from close individual galaxies, and then will discuss overall extragalactic GWB. ...

To run a process in the background as a job and carry on working add an (ampersand) at the end of the command line. ... The shell forks a child process to run the command and displays the job number ( [ n ] ) and the PID (Process IDentifier) number. ... If the command is likely to produce error messages you will need to redirect standard error. ... Do not run an interactive command that requires you to type something at the terminal as a background job. ... You will then have to kill its process . ...

... A Year of Resolving Backgrounds . ... In X-ray light the recently launched spacecraft Chandra and XMM resolved much of the seemingly uniform X-ray background into many discrete sources, many of which appear to be black holes at the centers of galaxies accreting matter. In microwave light , the BOOMERANG and MAXIMA-1 missions resolved with new clarity the seemingly uniform microwave background . ... Publications with keywords: cosmic microwave background radiation . ... Our Dusty Universe . ...

Family ASTRO Event Leaders can follow the links below to find a number of resources and more background reading to help them with their Astronomy Events and expand their knowledge on the topics covered in our series of Leader Kits for educators. ... Print and Web Resources on the Night Sky . ... If you have questions about Family ASTRO, see our Frequently Asked Questions for Educators and Astronomers page , or our Frequently Asked Questions for Families and Friends page. ...