Considerable effort has gone into the modeling of the HST point spread function (PSF), both in order to measure the optical aberrations in support of the WFPC2, COSTAR, and advanced scientific instruments, and to provide PSFs for image deconvolution in the aberrated telescope. ... As a consequence of the under-sampling in the WFPC2, the limiting magnitude attainable in the background limit varies by about 0.5 magnitude, depending on the position of the source within the CCD pixel. ... 0.9 . ...

... Armagh Observatory, College Hill, Armagh BT61 9DG, +44 (0)28 3752 2928 . ... Risks Comparable to NEOs . ... The Increasing Rate of Discovery of Asteroids . ... Comet and Asteroid Collision Probabilities . ... Extreme albedo comets and the impact hazard (PDF Format) . ... Asteroid Impact Animations . ... Workshop on Scientific Requirements for Mitigation of Hazardous Comets and Asteroids - 2002 . ... The Spaceguard Survey Report, 1992 (PDF) . Tsunami from Asteroid/Comet Impacts . ...

... The standard science quicklook processing produces over a dozen sky maps at each downlink, and these maps are automatically searched for potential transient point sources. ... We have found that a heuristic modification of a formula derived by Li & Ma (1983) provides reasonably accurate estimates of p -values for point source detections even for very low p -value detections. ... Case 1u. The most straightforward approach uses the signal , where . ... To get a p -value, use . ...

... Current APO Weather . ... Search Site . ... Information for New Users . ... Technical Staff pages . Night Logs and Mailing Lists (maintained by APO) . ... Technical Documents and Database Search . ... Observer's Documentation and Procedures . ... Problem Reporting and APO Technical Documents Database Search . ... APO Drawing/Document Management Procedures . ... APO Technical Documents Database Search . Home Astrophysical Research Consortium . ... Mail Lists (maintained by APO) . ...

Hide Zen home . ... Module knngist provides: . ... Find 10 most closest points to the Eiffel tower in Paris, which has 'mars' in their address. ... Champs de Mars, Paris 75007, France | ... 16, ave Rapp, Champ de Mars, Tour Eiffel, Paris, France | ... Champ de Mars Paris, France | ... 39 Rue Champ De Mars Paris, France | ... 12 rue du Champ de Mars Paris, France | ... Find 10 most closest points to the Eiffel tower from the 1st arrondissement of Paris (Paris 1), which addresses contains 'place'. ...

In this method the fields outside and inside a particle are represented by expansions in term of proper basis functions (practically always the vector spherical harmonics). Since the particle surface does not coincide with the coordinate surface, it is impossible to satisfy the boundary conditions exactly, and the expansions are limited by a finite number of terms, and the boundary conditions are considered in a finite set of points (matching points). ...

In calculating the NIFS sensitivity, we adopt a read noise of 5 e - , a dark current of 0.01 e - s -1 pix -1 , and a maximum exposure time of 3600 s. Grating . ... e/pix) . ... OH Cont. (e/pix) . ... NIFS should achieve signal-to-noise ratios of ~ 10 per spectral pixel in a 0.1" 0.1" aperture for single 1800 s exposures on uniform, extended, continuum sources with surface brightnesses of J = 15.4, J = 15.0, H = 14.8, and K = 13.5 mag arcsec -2 using the Z , J , H , and K gratings, respectively. ...

SINGULAR POINTS IN THE SOLAR CHROMOSPHERE . ... In the structure of the solar chromosphere, containing information on the configuration of the magnetic field, we have found and identified all the main types of the singular points ( see Fig. 1 ), which are known as inherent features of the 2-D vector field. ... The main types of the singular points are the node, the focus, the center, and the saddle. ... Singular point of the focus type in the solar chromosphere. ...

... Field size . Object name . ... Map size . ... Field size: the approximate size of the map in the Y direction. ... Galaxies: . ... Galaxies, which size exceeds some value depending on the field and map sizes, are displayed with their real positional angles and sizes by 25m isophote. ... In the "tools" fields there are links to the several famous AVO (Astrophysical Virtual Observatory) resources: NED and Simbad databases and DSS2 (Palomar Digitized Sky Survey) images of the corresponding sky area. ...

The cumulative system performance is plotted for each receiver. ... When something occurs that may change the gain of the system (moving a horn, shimming the elevation rails) then a new epoch will be started. The old data is moved to the old system performance data page (the old data link points to this). ... Gain,Tsys,Sefd... (.ps) (.pdf) . ... Pointing errors (.ps) (.pdf) . ... Hour of day when sources measured (.ps). (.pdf) . list of sources with dates and filenames Old data . ...

... Flux density at 1 GHz (/Jy): 8? ... X-ray: Pulsar wind nebula. Point sources: Pulsar near edge, with wind nebula. ... ADS . ... 1994, ApJ, 437, 781. VLA at 330 MHz (56''?111'': S=10.6 Jy) and 1.4 GHz (22''?27'') near pulsar. ... 1995, A&A, 298, 528. ROSAT of pulsar, and limit for remnant. ... VLA at 1.4, 4.9 and 8.5 GHz (25'') of pulsar wind nebula. ... 2002, ApJ, 567, L125. ... ATCA at 1.4 GHz (70''?47'') including polarisation, and Chandra observations of pulsar wind nebula. ...

... 739C As one part of a program to detect complete samples of active extragalactic objects, the 3.36x10^-3 sr field centered on alpha=12h04min, delta=+11deg30' (1950.0) was mapped with the Very Large Array at 1411MHz. Sixty-seven maps cover this field so that no point is more than 15arcmin from the nearest map center. ... The rms map noise is 0.030 + 0.001 mJy, and the resulting source list is complete to a map peak flux density S_p = 0.2 mJy within 25 arcmin of the field center. ...

... It plots visibilities (e.g. amplitude vs time), either one baseline at a time or all together, and allows discrepant points to be flagged with a cursor. ... No default. ... Key: axis Two character strings, giving the X and Y axes of the plot. Possible axis values are: time (the default for the X axis) lst Local apparent sidereal time. uvdistance sqrt(u**2+v**2) hangle (hour angle) channel (implies nofqav) amplitude (the default for the Y axis) phase real imaginary rms Theoretical rms noise. ...

... 2.3 Establishing the Extragalactic Distance Scale . ... 2.3.2 The Second Rung: Distances to stellar clusters . ... 2.3.4 Distances to Local Group Galaxies . ... The Luminosity Function of Planetary Nebulae . ... 3.2.2 Clusters of Galaxies . ... 4.2 Evidence for Dark Matter as a Function of Scale Size . ... 4.3 Other Dark Matter Indicators for Galaxies . ... What is the nature of the large-scale distribution of matter in the universe as traced by the three-dimensional galaxy distribution? ...

The beam pattern and the polarization characteristics . of the radio telescope RATAN-600 . The Mueller matrix elements was computed via formulas [1]: . ... The BP were computed by the aperture method, proceeding from the fild distribution in the aperture of the primary mirror. The components of the main and cross-polarization components of the electric field in the vertical aperture of the primary mirror was computed in Frenel diffraction approximation. ...

There are two modes to specify the time interval of ephemeris. ... This mode is applicable if the date of opposition belongs to the basic interval of 16 months from November of the year preceding to the title one to February of the subsequent one. In this case the ephemeris is centered at the nearest standard moment (its Julian day minus 0.5 is exactly divisible by 10) which precedes or coincides with the moment of opposition of minor planet in specified year. ...

XMM-Newton Science Analysis System Page: 1 esensmap July 1, 2008 Abstract Calculate EPIC sensitivity map 1 Instruments/Modes Instrument Mode EPIC MOS: IMAGING EPIC PN: IMAGING 2 Use pipeline processing yes interactive analysis yes 3 Description This task creates a sensitivity map giving point source detection upper limits (vignetting corrected source count rate corresponding to the likelihood of detection as speci ed in the parameter le) for each image pixel. ...

... Цвет: синий . ... Материал верха: натуральная кожа . ... Материал подошвы: резина . ... Пол: Мужской . Кроссовки Botticelli Limited. ... Материал: натуральная кожа. ... Пол: Унисекс . ... Игрушки максимально точно копируют оригинал и могут быть выполнены в натуральную величину. ... Материал верха: Натуральная кожа . Материал подкладки: Натуральная кожа . Материал стельки: Натуральная кожа . ... Маленькой ножке будет комфортно благодаря натуральным материалам и отверстиям для воздуха. ...

... Summary of reduced ISAAC fields . ... This data release includes eight fully reduced VLT/ISAAC fields in J,H,K s bands covering 50 arcmin 2 of the GOODS region in the Chandra Deep Field South (CDFS). ... 8 ISAAC fields) . ... The 8 ISAAC fields which are part of this data release are superimposed onto a SOFI image (J+K) (part of a previous EIS data release). ... In one case (GOODS field 11/J-band), for which not enough standard stars were available, the ZP was boostrapped from previous SOFI/EIS data...

STEP INTO THE BLUE - MEADE INSTRUMENTS PRODUCT GUIDE . ... Telescopes . ... Superb optical performance coupled with time proven computerized pointing and tracking has made the LX200 ACF series a best-seller in the high-performance telescope class. ... Meade's revolutionary LS LightSwitchтДв series of telescopes use advanced technologies to do what no other consumer telescopes have done before: take all the hassle out of using a telescope. ... ETX-80 Hard Carry Case . ... ETX-80 Hard Carry Case #07385. ...