... subroutine omlcbuild read parameters loop i=0, nSources get handle on source rates file get handle on source region file if (exposure IDs are different) issue warning get handle on background rates file get handle on background region file if (exposure IDs are different) issue warning if (exposure ID source != exposure ID background ) call fatal get source extraction radius = s_radius get ...

... Effects on signal to noise ratio! ... The Advanced Camera for Surveys (ACS) team at STScI has (Anderson & Bedin, 2010) that corrects for losses in charge how this algorithm changes the characteristics of the signal to eliminate unknown variables we use simulated images where explore a parameter space that includes background, object brightness, and position on the chip. ... Left shows an image with no CTE losses. ... Right is an image which has been corrected for CTE losses (FLC). ... PHOTOMETRY! ...

Next: Sky background definition Up: Background Definition Previous: Smoothing spline interpolation . The command BACKGROUND/SMOOTH enables to define the background without previous order definition. This feature is useful for example to correct for the background the image required for the order definition. ... All above methods are implemented in command BACKGROUND/ECHELLE and selected by the echelle keyword BKGMTD . ...

... This paper describes the main algorithms used by the Einstein Level One processing to create the exposure masks and the background maps for Einstein IPC images, and how these algorithms were recreated in the IRAF environment. Our goal was to recreate the algorithms used by the Level One Processing to create exposure masks and background maps for Einstein Image Proportional Counter (IPC) data (cf. sections 2.5 and 2.7 of Harnden et al. ...

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 . ...

... 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] ) . ...

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. ...

... 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 . ...

... Highlights . ... PPTA timeline . ... Data release 2 discussion . Editing this wiki . ... Detecting and limiting the gravitational-wave background: Yardley et al. (2011) used the PPTA data sets to attempt to detect a gravitational wave background. ... Jenet et al. (2006) provided the first stringent upper bound on the gravitational wave background using the PPTA data sets. ... 2012). ... We have used the PPTA observations to develop the first major pulsar-based timescale (Hobbs et al. ...

... The Cosmic X-Ray Background . ... Now, peering through a hole in the obscuring gas and dust of our own Milky Way Galaxy, the powerful orbiting XMM-Newton telescope has recorded this deep image of the x-ray sky , resolving some of the mysterious background into many faint individual sources. ... Do massive black holes reside in the hearts of all large galaxies? ... Publications with keywords: black hole - XMM-Newton - x-ray background - cosmic microwave background radiation - X-ray . ...

In 1995 Eugene set an annual rainfall record by recording, officially, 65.56 inches of rain. ... The mean annual rainfall for Eugene from the 25 year period 1970-1994 was 51.5 inches with a dispersion of 8 inches. ... Wettest Years: . ... Below are the official NWS corrected rain totals for the year 1996. Although these are now "official", I go on record here by saying there is no way I believe that Eugene, Oregon received 101 inches of rain in 1996. ... January: Old = 14.74; corrected = 14.48 . ...

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 . ...

This diagram shows the six superimposed "layers" of the CSS table model. This diagram illustrates the algorithm for calculating a cell's final background. ... The diagram shows how, looking down on the six rectangles, one may compute the background color of each cell. ... A cell without a background color in the top layer is depicted as a "window" onto the lower layers, which give its final background color. ...

... 2000 November 9 . The Cosmic X-Ray Background . ... Notably, the faint sources tend to be green and blue, showing x-ray characteristics of huge amounts of material falling into massive black holes in very distant galaxies. ... The XMM-Newton results add to the growing consensus that they do and that, from across the universe , x-rays produced as matter feeds these black holes account for the cosmic x-ray background. ... About APOD | ...

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.. ...

... Science Activities > PhD Thesis Topics offered by ESO Faculty Members > Thesis Topic: Foreground emission and Cosmic Microwave background intrinsic anisotropies . ... Since its discovery the Cosmic Microwave Radiation (CMB) has been one of the pillars of modern Cosmology. ... Further development of this work is the application of already tested algorithms to disentangle the foreground emission from the CMB maps and the determination of the CMB intrinsic emission. ... Return to list of thesis topics ...

... 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: 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 . ...

... We can help students grasp the significance of Hubble's extremely keen eye, and learn a bit about angles and math in the process, with the following in-class activity. ... Looking through binoculars or telescopes allows us to magnify a small section of the sky. To measure sizes or distances in that small section, astronomers divide a degree into 60 smaller pieces called arcminutes, and further subdivide minutes into 60 smaller sections called arcseconds. ... 30 feet = . ... 36 seconds . ...