... It is sometimes useful, as in image restoration where we want to evaluate the quality of the restoration, to compare images with an objective criterion. ... The correlation between the original image and the restored one gives a classical criterion. ... For each dyadic scale, we can compute the correlation coefficient and the quadratic error between the wavelet transforms of the original and the restored images. ... Figures and show the comparison of three images with a reference image. ...

Fair" UV Coverage for a Multi-resolution John Bunton, CSIRO Telecommunications and Industrial Physics, Australia Introduction If we wish to have a multi-resolution telescope with equal point source sensitivity at all resolutions then we must accept that the baseline distribution of the correlations is predetermined. ... This occurs for each added step in resolution. ... It is seen that for the combined telescope the total number of correlations is 5.17 times the number needed for a single resolution. ...

FGS Instrument Handbook for Cycle 24 . ... Fine Guidance Sensor Instrument Handbook for Cycle 24 > Appendix B: FGS1r PerformanceSummary > B.2 Angular Resolution Test . ... At the time of the test, the predicted angular separation of the components was 0.085" (Franz and Wasserman, private communication). ... By rolling the HST in 6 increments, the projected separation along the X axis varied from the predicted angular resolution limit of FGS1r (~6 mas) to the resolution limit of FGS3 (~20 mas). ...

makeflat -- makes flatfields corresponding to the output image of asncombine. makeflat association flatlist . ... ASCII file with list of flatfields as used by NICMOSlook. resolution . ... The ST-ECF tool NICMOSlook performs this task by determining the appropriate factor from narrow band flatfields. ... This task takes a list of flatfields in the same format as NICMOSlook, shifts and co-adds each of the flatfields in the list, and creates a new list which can be used as input for NICMOSlook. ...

... Дни открытых дверей к юбилею САО РАН (12-14 апреля 2016 г.) . Международная конференция "Dark Ages and White Nights (Spectroscopy of the CMB)" (20-24 июня 2016 г.) . ... Международная конференция MULTI-SPIN GALAXIES - 2016 (26-30 сентября 2016 г.) . Международная астрономическая конференция "Физика звезд: от коллапса до коллапса" (3-7 октября 2016 г.) Архив . ... Подробнее.. ... 10.02.16 . ... БТА в реальном времени . ... Цейсс-1000 в реальном времени . ... Последнее обновление: 22/03/2016 ...

... Values have been scaled arbitrarily. High ratios are shown in blue, corresponding to blue colors, and low ratios are shown in red, corresponding to red colors. ... Noise combined with background subtraction difficulties in the lower left quadrant of the WISP1 data (see Fig. \ref{Fig:wisp_snr_mskd}) make colors in this area very unreliable. ... The values shown here are typically a factor of ~3 less than those calculated for the Schmidt data, shown in Figure \ref{Fig:bj_alpha}. ...

... Empirical and theoretical modeling of 3-D structures in the solar corona is confronted by the tremendous amount of data needed to represent phenomena with a large dynamic range both in size and magnitude, and with a rapid temporal evolution. Octree representation of the 3-D coronal electron distribution offers the right compromise between resolution and size, allowing computation of synthetic images of the solar corona. ... The time interval between images is one day. ...

Colorful Moon Mosaic . ... Credit Copyright: Noel Carboni Explanation: No single exposure can easily capture faint stars along with the subtle colors of the Moon. ... The fascinating color differences along the lunar surface are real, though highly exaggerated, corresponding to regions with different chemical compositions . And while these color differences are not visible to the eye even with a telescope, moon watchers can still see a dramatic lunar presentation tonight. ...

... Imaging interferometry data presents us with two challenges: the aperture plane (i.e. the complex visibility function) is sparsely sampled, and the baseline phases are "totally corrupted" by the atmosphere while the closure phases, i.e. the sum of three closed loop baseline phases, is free of systematic errors. The two algorithms to take care of these challenges are deconvolution and phase self-calibration. The deconvolution algorithm we use is the CLEAN algorithm. ...

... OM grism data are obtained as image mode data. However the different nature of this type of data, spectra of the objects in the field of view instead of their "sky" image, makes that a special processing must be applied to the grism images. ... They are concatenated in a perl script, omgchain , which works in a similar way to the image and fast mode chains. ... All necessary corrections are applied to the grism data files. ... As we have pointed out OM grism data are image mode data. ...

... Let us first find out which way -- rise in spectral resolution with some loss in the S/N ratio or increase in the S/N ratio with a fixed spectral resolution -- is better for the purpose of reduction of equivalent width determination errors. ... N -- number of counts for 1 ? ... line equivalent width, . ... Thus if the spectral resolution is managed to be increased (i.e. to decrease )without loss in the number of counts falling at 1 ?, the equivalent width measurement error is then proportional to . ...

On April 27 the large sunspot in Active Region 8970 was observed using the Adaptive Optics system at the Swedish Vacuum Solar Telescope at La Palma. ... It showed to give a significant improvement of the image quality under less favorable conditions. Click on the image to get a high resolution version. ... The data cube is cut in three pieces to get manageable file sizes, you can glue them together to restore the whole 108 images cube. gband_ao.01_36.cube.fits 36.5 Mb: image 1 - 36 . ...

Magnetic Fields around Radio Galaxies Robert Laing (ESO) Laing et al. ... 2008) Negligible depolarization and 2 rotation Almost all Faraday effects must be due to foreground material How to fit depolarization caused by foreground Faraday rotation Complex polarization Rotation measure Integrate over a beam Observed RM for 0 2 rotation and depolarization Faraday rotation and depolarization 5.5 arcsec FWHM Faraday effects at high resolution FWHM = 1.5 ...

To appear in "Fourth Workshop on Robotic Autonomous Observatories (2015)"RevMexAA(SC) METEOR OBSERVATIONS WITH MINI-MEGATORTORA WIDE-FIELD MONITORING SYSTEM S. Karpov, 1, 3 N. Orekhova2 G. Beskin, 1, 3 A. Biryukov3,4 S. Bondar,2 E. Ivanov,2 E. Katkova,2 A. Perkov, and V. Sasyuk3 RESUMEN 2 Favor de prop orcionar un resumen en espanol. ... The faintest detected meteors has the peak brightness about 10 mag, while the ma jority - from 4 to 8 mag. ... 2010; Karpov et al. 2013; Beskin et al. ...

On the multifunctional orbital piloted complex Mir Russian Federation Government resolves: . To accept Russian Space Agency and Korolev Rocket- Space Corporation Energy's proposal to continue the exploitation of the multifunctional orbital piloted complex Mir (further - complex Mir) in 1999-2002. ... Russian Space Agency is to provide coordination and checking over carrying out the work determined by this Resolution. Russian Federation Government . ...

... Gives covariance Matrix for fitted track ­ Can calculate covariance Matrix without hits ­ simulate hits itself and use only detector geometry description (compact.xml file) · Hits smearing ­ First combine hits (SimTrackerHit) from the same particle in the detector layer (there may be few of them because Geant generates many hits along track) ­ Smear resulting TrackerHit and assign measurement matrix to it according to given detectors resolutions 10/26/ 2006 Nick Sinev , ...

Next: The Scenario Machine: Operational Up: Evolution of Magnetic Rotators Previous: Ejector-propeller hysteresis . ... The length of this segment is determined by the eccentricity. ... In this case no hysteresis occurs and transitions E -- P and the reverse take place in symmetrical points of the orbit. ... Here EP means a mixed state of the rotator at which it is in the ejector state during one part of the orbit, and in the propeller state during the rest of the orbital cycle. ...

One of the most innovative x-ray detector designs of the past decade is the microcalorimeter. ... In principle, energy resolutions as good as ~1 eV (FWHM) should be possible. ... In its most basic form a microcalorimeter consists of three parts: a thermal mass that absorbs the x-ray and converts the energy to heat, a thermometer to measure the temperature rise of the thermal mass, and a thermal link to a heat sink to allow the absorbed energy to escape from the thermal mass. ...

of SOHO `Waves, Oscillations Small­Scale Transient in Solar Atmosphere: A Joint SOHO TRACE', Palma Mallorca, Balearic Islands (Spain), 29 September -- October 2003 SP­547, January 2004) STUDY TRANSITION REGION AND CORONAL DOPPLER SHIFTS SOLAR CORONAL HOLE Popescu 1,2 Doyle 1 Armagh Observatory, College Armagh 9DG, Ireland 2 Astronomical Institute Romanian Academy, RO­75212 Bucharest ... 1997), Dammasch (1999), Hassler et al. ... chromospheric network boundaries: features . ...

... 8, ``Celestial Mechanics'', 2002 EPM2002 and EPM2002C -- two versions of high accuracy numerical planetary ephemerides constructed for TDB and TCB time scales E. V. Pitjeva Institute of Applied Astronomy, St. Petersburg, Russia To be consistent with IAU resolutions ICRS should be treated as four-- dimensional reference frame with TCB time scale in which planetary ephemerides should be constructed. ... 2001, 80, 249-- 271. ... Standish E. M. JPL Planetary and Lunar Ephemerides, DE405/LE405. ...