Point Source SNR Plots . In this section we present plots which may be used to rapidly estimate signal-to-noise ratio (SNR) for point sources with stellar spectra observed through popular WFPC2 filters. ... There are separate lines for PC1 (light lines) and the WFC (heavy lines), as well as for ATD-GAIN=7 (default, solid lines), and ATD-GAIN=15 (dashed lines). Dotted lines across the top of each plot indicate the onset of saturation. ... We now give a sample SNR calculation using these plots. ...

... It lists the coefficients defining the colour transformations, the zero points for the different filters and the aperture radii used in the photometric calibration analysis. ... The AB system zero point of the filter FilterID is stored in the keyword ABM0 FilterID , e.g. the AB zero point of the the U-filter is stored in ABM0U. The flux conversion factor derived from White Dwarfs of the filter FilterID is stored in the keyword FCF FilterID . ... description . ... AB Flux conversion factor of U . ...

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... 05apr08- System Temperature/powerLevels (bsisk) . ... 05apr08- Fiber Span AC231, Fiber Optic Xmtr/Rcvr measurements by bsisk . Eddies down conversion box takes the output of the alfa filter bank, amplifies, downconverts, filters, amplifies, and then sends the IF signal down the fiber. ... GAIN . ... RF amp . ... The damage threshold for these devices is an input power of +20 dBm. ... 27Dbm at input to RF amp will cause 1 db compression at mixer output (assuming 20 db gain for misbiased RF amp). ...

Next: Star Formation Rate and Up: No Title Previous: Calculation of Evolutionary Tracks . To start calculations, we choose the distributions of the initial binary parameters: the mass of the primary ZAMS component, , binary mass ratio, , orbital separation a . ... whereas the mass ratio distribution is not. ... The zero assumption often made is that the mass ratio distribution has a flat shape, that is binaries with a high mass ratio occur as frequently as those with equal masses. ...

... Transforms a qpoe file according to the specified parameters. ... Any type of filtering can be applied to the input qpoe file, including region filtering. In addition, the size of the output event record can be different from the size of the input event record. Of course, usually one makes the output record equal to or smaller than the input. If the output record size is made greater than the input record, a warning is issued and the ``extra'' part of the record is undefined.) ...

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Next: Hierarchical Wiener filtering Up: Noise reduction from Previous: The convolution from . Let us consider a measured wavelet coefficient at the scale i . We assume that its value, at a given scale and a given position, results from a noisy process, with a Gaussian distribution with a mathematical expectation , and a standard deviation : . ... We get: . ... This is done from the study of the variation of the noise between two scales, with an hypothesis of a white gaussian noise; . ...

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... Обзор LPR фильтра. Впечатления от наблюдений с LPR фильтром. ... Характеристики цветных фильтров Baader-Planetarium . Мой перевод pdf- файла о фильтрах с сайта Baader-Planetarium (379 кб) . ...

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STEP INTO THE BLUE - MEADE INSTRUMENTS PRODUCT GUIDE . ... Products . Telescopes . LX850 Series . ... Coronado€о Solar . ... H-Alpha Filters . ... Blocking Filters . ... Coronado 5mm Blocking Filter . ... Blocking filter for Coronado primary filters . ... Coronado BF-5 right angle (1.25" diagonal) type secondary blocking filter. The blocking filter is the second element in any Coronado H-alpha system, it is just as crucial to your safety and the system's performance as the front element. ...

Laboratory work N7 Low-pass filtering. 1) Generate the signal with two periodic components and high-frequency noise. ... 2) Perform it's filtering with Panteleev filter 0 - h(t) = e 22 0 |t| 2 0 t 0 |t| cos + sin 2 2 , where 0 is a parameter. The frequency response of the Panteleev filter is ^ h( ) = 4 0 . 4 0 + 4 Select the cut-off frequency (by varying 0 ) for filtering out high-frequency periodic component and noise. 3) Plot the initial and filtered signal. ...

... FIELD | ... METHOD . ... java.lang.Object ij.plugin.filter.MaximumFinder . ... public class MaximumFinder . ... 32768 pixels in width or height version 01-Nov-2009 Bugfix: extra lines in segmented output eliminated; watershed is also faster now Maximum points encoded in long array for sorting instead of separete objects that need gc New output type 'List' . ... static int . ... The plugin is inferred from ImageJ by this method . ... int . ... Field Detail public static final int SINGLE_POINTS . ...

OptInt PmWiki : MROI Fast Tip Tilt / Tech Meet 9 . Nasmyth Optical Table . ... XS analysis: Attach:FTT_mount_analysis_05.pdf . DFB analysis: see below . ... How to locate and support optics . ... Assume that the table is supported by a vertical support (representing the side of the telescope) and a diagonal support running from the telescope to the end of the table furthest from the table. ... Printable View of http://www.mrao.cam.ac.uk/projects/OAS/pmwiki/pmwiki.php/MROIFastTipTilt/TechMeet9) ...

... The STECF IRAF layered package impol provides five tasks specifically aimed at reduction of HST imaging polarimetry data for ACS, FOC, NICMOS and WFPC2. ... Reduction of HST polarimetry data and simulation of raw polarimetry images, together with polarization vector plotting, are covered. ... hstpolsim -- Produce simulated polarization input data frames for HST instruments from images of the total signal, the linear polarization and the position angle of the polarization vectors. ...

... Big ellipse: the region of the photometric analysis Smaller ellipses: the adopted inner boundaries of the Main Body and the C component Small circles: diffuse background objects, manually selected and removed from the photometry Uncleaned CMDs [V-I, I] of I Zw 18, obtained using Aloisi et al. (left) and Izotov & Thuan (right) datasets. ... Where is the 'halo'? Blue compact dwarf galaxy SBS 1415+435 Hubble Space Telescope / Advanced Camera for Surveys NASA, ESA A. Aloisi (STScI, ESA) et al. ...

... This article describes the AXAF aspect determination pipeline and its components, and highlights a procedure for determining centroids-a crucial step in deriving the post-facto aspect solution. ... The Ground Aspect Determination System (GADS) pipeline is a collection of tools which process aspect telemetry and generate aspect data products. ... Using a subset of ACA pixel data from the Aspect Interval, we identify poorly-fitting PSFs and find spoiler stars in star and fiducial light images. ...

... Exposure Time Calculator (ETC) . Survey processing . ... VISTA is a 4-m class wide field survey telescope for the southern hemisphere, equipped with a near infrared camera (1.65 degree diameter field of view at VISTA's nominal pixel size) containing 67 million pixels of mean size 0.34 arcsec and available broad band filters at Z,Y,J,H,K s and a narrow band filter at 1.18 micron. A wide field visible camera, if constructed, could also be used on VISTA. ... Tile . ... ESO VISTA Public Surveys . ...

Classroom Activity: Making a Rainbow . ... When white light from the Sun or a light bulb passes through a prism, the light splits into its component wavelengths. ... Red, blue, green colored filters - if possible, cut 1x4-inch pieces of the filters for each student . ... Many students have the misconception that filters somehow dye the light a certain color. ... Younger students can draw the rainbow and make up a mnemonic for remembering the order of the colors (such as, ROY G. BIV). ...