... Osservatorio Astronomico, Bologna, Italy . ... Dipartimento di Astronomia, Universit? di Bologna, Bologna, Italy . Stellar photometry of simulated HST uncorrected and corrected images of a crowded star cluster has been carried out before and after deconvolution (with RMG, R-L, MEM, etc.) to optimize the reduction procedures and compare the degree of completeness and photometric accuracy actually achievable in the various cases. ... Surface Brightness Profiles . ...

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• Fusi Pecci et al.: Photometric Measurements of Simulated Restored Images
• Comparisons of Implementations
• Simulated Results with the HST

... Bad Astronomy . ... Bad Astronomy: The North Star, Polaris, is a very bright star. Good Astronomy: Polaris is a middling-bright star, easily missed. ... He said it was close to Polaris, the North Star, but he also said it was in the East. ... It's natural, I suppose, to think that such an important star should be bright, but really, that's a conceit, like thinking that the Earth is at the center of the Universe. If more people knew just why Polaris is the North Star, this Bad Idea would stop. ...

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• Phil Plait's Bad Astronomy: Mad Science
• Phil Plait's Bad Astronomy: Bitesize Astronomy
• Phil Plait's Bad Astronomy: Info

Next: Hierarchical adaptive filtering Up: Noise reduction from Previous: Hierarchical Wiener filtering . In the preceding algorithm we have assumed the properties of the signal and the noise to be stationary. The wavelet transform was first used to obtain an algorithm which is faster than classical Wiener Filtering. ... Knowing the noise distribution, we can determine the statistically significant level at each scale of the measured wavelet coefficients. ...

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• Multiresolution Analysis
• Combining Methods
• Regularization of Van Cittert's algorithm

... Each day a different image or photograph of our fascinating universe is featured, along with a brief explanation written by a professional astronomer. 2008 November 18 . Restored: First Image of the Earth from the Moon . Credit: NASA / LOIRP . Explanation: Pictured above is the first image ever taken of the Earth from the Moon. The image was taken in 1966 by Lunar Orbiter 1 and heralded by then-journalists as the Image of the Century. ... About APOD | ...

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• APOD: 2004 May 5 - NGC 6302: Big, Bright, Bug Nebula
• APOD: 2007 April 29 - NGC 6302: Big, Bright, Bug Nebula
• APOD: 2002 June 20 - Bright Galaxy M81

Next: Managing a calibrator catalog Up: How to work with Previous: How to work with Contents . At this time, STARBASE is used to perform two different tasks, namely reading primary and secondary catalogs, and computing astrophysical quantities from the collected information. ... Stars in the primary catalogs have unique ID numbers. ... They were derived from various astronomical catalogs by extracting the ID number (usually the HDN) and the desired data. ...

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• Observing list preparation
• Astronomical Image Retouching
• About AMOEBA

... Imaging of the core of the OMC-1 region using NICMOS camera 2 through the F212N and F215N filters shows a wide variety of interesting structure on scales of 0.2" at a very high dynamic range (Stolovy et al. ... The application of image restoration techniques, including multi-channel variants of the Richardson-Lucy technique, offers the chance to enhance structure on the finest scales and also to suppress the prominent and richly structured point-spread functions of the many bright stars in the...

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• stecf.cplucy - Enhanced Two-channel Photometric Restoration

XMM­Newton CCF Release Note XMM­CCF­REL­119 OM PSF Bing Chen June 13, 2002 1 CCF components Name of CCF VALDATE List of Blocks changed CAL VERSION XSCS flag OM PSF1DRB 0006 2000­01­01T00:00:00 PSF­U No PSF­B No PSF­V No PSF­UVW1 No PSF­UVM2 No PSF­UVW2 No 2 Changes This CCF file provides new measurement of OM PSF. ... 1 XMM­Newton CCF Release XMM­CCF­REL­119 Page: 2 Figure 1: Growth curves as a function of radius for V and UVW1 filters. ... Therefore, this new PSF is field position independent. ...

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• Description
• Analysis of very bright sources
• Introduction

In this gallery are many images of Low Surface Brightness Galaxies which have recently been discovered and analyzed. ... The central surface brightness of this galaxy is 24.28 . Malin 2 This galaxy is another huge disk galaxy with a scale length of 15 kpc and a redshift of 15000 km/a. The high surface brightness knot in one of its spiral arms actually has the same color, luminosity and H-alpha equivalent width as the entire Large Magellanic Cloud . ... Truly it is a Low Surface Brightness Galaxy. ...

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... During execution of attitude quality tests, the two tables of attitude coefficients were generated. This tables related to the same time interval on 18. 04. 1997, but have a different time resolution - 15 and 3 min. Using this tables, we have restored the magnetic field measurement. On this panels the measurement and the model(Tsyg96) magnetic field are plotted. 3 min resolution table turn out availiable to provide the better approach to the model magnetic field. ...

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• ENERGETIC PARTICLE EXPERIMENT DOK-2
• The Face on Mars
• The Acceleration of the Aurora

... Search . ATNF Home . About ATNF . ... About ATNF overview . ... Australia Telescope Steering Committee . ... Parkes radio telescope . ... Parkes | ... A Search for Bright Kuiper Belt Objects . ... Since 1992, 60 large Kuiper belt objects have been detected by ground-based telescopes. ... The detection of brighter objects would improve our ability to determine the Kuiper belt objects' surface composition and provide constraints on the population statistics of different formation mechanisms. ...

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• HIPASS Bright Galaxy Catalog
• Pulsar Group PmWiki/Backup and Restore
• Finding the Bivariate Brightness Distribution of galaxies from an HI selected

Next: Historical Background Up: R Coronae Borealis Stars Previous: R Coronae Borealis Stars . R Coronae Borealis stars, or RCB stars, are an important class of VARIABLE STAR . ... RCB stars, remarkably, do both. RCB stars are best known because of their irregular `fades'. ... The fades are caused by enormous clouds of dust which cover a large part of the star's surface. ... As well as irregular fades, the light output from RCBs goes up and down by a few per cent every 40 days or so. ...

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• INTRODUCTION
• annrep2004
• Multilevel backups

Next: Principles of organization Up: Further advance in the Previous: Further advance in the . ... An ability of using different catalogs makes this problem considerably simpler. Lately Different attempts have been made for combining many astronomical catalogs in unified databases NED, SIMBAD, ESIS, ADS, etc.(see reviews by Andernach et al.1994; Andernach 1995). ... We propose a new solution to this problem with a ``CATalogs supporting System'' (CATS) at Special Astrophysical Observatory (SAO). ...

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• Description of algorithm
• Experimetn COLD: Introduction
• Principles of organization

Atmospheric influence on the different radio-engineering system functioning . ESTIMATION OF ATMOSPHERIC OPTICAL CHARACTERISTICS AND REMOTELY SANSED IMAGE CORRECTION . ... Direct transmittance estimation results for 12 channels of the spectrometer CHRIS. ... We have managed to develop a direct method of estimating the discrete Normalized Atmospheric Point Spread Function (NAPSF) from available images alone, not using any external sources of information about the atmosphere. ... IRE RAS 1996-20 11 ...

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• Application of Chaotic Dynamical Systems to the Problems of Recognition and
• Experiment "Rain"

... Next: MEM Task for Up: Image Restoration and Previous: RegisteringPSF-Matching and . ... In gyro-hold tracking mode, HST is stabilized only with its gyros, and the Fine Guidance Sensors are not used to maintain pointing. ... Experiments have been done on WFPC 2 images of NGC 330 and NGC 422 (having exposure times of 80 and 100 s in gyro-hold mode) with complete success. ... An NGC 422 WFPC 2 WC2 image and an NGC 330 WFPC 2 PC1 image were taken in mode FSGLOCK = GYROS in 1994 January. ...

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• Clustering Analysis Algorithms and Their Applications to Digital POSS-II
• See Spike Run... Run, Spike, Run
• Determination of the Permissible Solutions Area by Image Reconstruction from a

. Please standby and you will be automatically connected to the new location of the unframed Supernova page. Or, click on the link above. If you have questions or problems, please email me at David Bishop dbishop@vhdl.org . Last modified: Mon Aug 27 12:40:15 EDT 2001

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• Nova in M31 2000 3
• Supernova 2006E in NGC 5338
• Bright Supernova - Archives

... Albireo: A Bright and Beautiful Double . ... Such is the case of the bright double star Albireo . Seen at even slight magnification, Albireo unfolds from a bright single point into a beautiful double star of strikingly different colors. ... The brighter yellow star is itself a binary star system, but too close together to be resolved even with a telescope. ... Публикации с ключевыми словами: star system - двойные звезды . Публикации со словами: star system - двойные звезды . ...

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• Albireo: A Bright and Beautiful Double
• XWare > APOD

Microsymposium 38, MS083, 2003 (A4 format) MERCURY: LOCAL VARIATIONS OF THE PHOTOMETRIC RELIEF. ... Because of trajectory and pointing angle constraints the planet could be observed from Mariner 10 only over a small range of phase angles between about 75o and 110o. Therefore the photometric investigations are restricted to measuring the distribution of brightness on the Mercurian disk. ... Raw versions of real-time processing pictures FDS 0000984 and FDS 0000986 were used (images 196 and 202). ...

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• http://selena.sai.msu.ru/Shev/Publications/ms38/ms082.pdf
• http://selena.sai.msu.ru/Pug/Publications/m44_70_pugacheva.pdf
• http://selena.sai.msu.ru/Pug/Publications/ms42/m42_60.pdf

Once students get the hang of it, they can find and measure the brightness of Delta Cephei in a few minutes. ... of Delta Cephei . ... Oct. ... The following table lists the measurements of Delta Cephei made by one amateur astronomer in autumn 1990. ... 4.0 . ... This activity is a simplified version of one that appeared in Hands-On Astrophysics, a series of activities prepared by the American Association of Variable Star Observers with support from the National Science Foundation. << previous page | ...

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• ASP: SETI?s Prospects Are Bright
• ASP: Accidental Astrophysics: The Devil's In the Magnitudes, Part II
• ASP: Black Holes to Blackboards: Seeing the Light

Next: Observational Zoo of Binaries Up: No Title Previous: Contents . In the early 1980s, our understanding of binary star evolution љ based on the pioneer work by Paczynski (1971)[ 150 ], Tutukov and Yungelson (1973)[ 195 ], van den Heuvel and Heise (1972)[ 201 ], allowed us to construct a general evolutionary scenario љ which successfully explained the genesis of well-studied normal stars and offered potential explanation for new X-ray sources discovered in space experiments. ...

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• Dependence on the Scenario Parameters and Initial Distributions
• Brightness constraint
• The Scenario Machine: Operational Guide

The xpamb program can act as a "classical" message bus interface between clients and servers. A client can send a data request to the message bus, which then interfaces with multiple servers and returns the data back to the client. ... For example, if the -info switch is used: xpaget xpamb -info foo then the info about that stored data buffer will be returned. If the -data is used with a specific name: xpaget xpamb -data foo then the stored data itself will be returned. ... data [name] . ...

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• Data Formats
• Everyday Classroom Tools: Introduction to the Threads of Inquiry
• QPOE Files