... Previous: Background Fluctuation Analysis from the Multiscale Entropy . ... A new measure of information is defined which is based on noise modeling and incorporates resolution scale. Properties of this measure are discussed. ... Additionally it allows for image noise modeling, and subsequent noise removal. ... Hence information- and entropy-based processing technologies will be necessary for the effective design and implementation of large, future generation, image databases. ...

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• Wavelength Calibration at Moderately High Resolution
• PICsIM - the INTEGRAL/IBIS/PICsIT Observation Simulation Tool for Prototype
• Background Fluctuation Analysis from the Multiscale Entropy

... Research . ... I use interferometric arrays of telescopes to yield images with an angular resolution more than one hundred times better than that of the Hubble Space Telescope. ... As a result, the MROI will be able to image targets 10 times fainter than those accessible with any other interferometer, and it will be able to make images on timescales of hours instead of days (Buscher et al 2013). ...

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• Astrophysics Group VSA

... 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 ...

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... 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 . ...

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Next: Galactic Gravitational Wave Background Previous: Structure of the Galaxy . We will call ``transparency'' of the background the ability of the observer to detect a gravitational wave signal other than that produced by binary systems, by means of adjusting variable parameters of an imaginary GW detector (namely, its angular resolution and frequency band), so that less than one occasional binary system falls into the detector's beam at a given frequency in a given direction. ...

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• Extragalactic Gravitational Wave Background
• Galactic Gravitational Wave Background
• Gravitational Wave Background from Individual Galaxies

... Meta Index / Home Page / Description / Soft flare rejection for . The EPIC-pn fast timing mode was designed so that a time resolution of 0.029 milliseconds can be achieved. ... Below this energy the data is affected by so-called soft flares which are caused by stack overflows generated by high energy particles. These so-called soft flares have sharp rise (from 0 counts/sec to several thousand counts/sec in 0.10-0.15 sec) then decaying back 0 counts/sec slightly slower in about 0.3-0.4 sec). ...

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• Energy resolution
• CCD Scientific Performance

... 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 . ...

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• On the problem of high spectral resolution observations of faint objects
• High resolution Zeeman spectrum of HD4778

Next: Optimal Combination Up: Optimal Combination of Sub-Stepped Previous: Optimal Combination of Sub-Stepped . The diodes of both GHRS detectors are spaced on 50 m centers. ... The spectrum projected on the 500 diodes is therefore not well sampled, with only one diode per resolution element. ... This procedure, which can also be accomplished together with sampling of the adjacent background, is fast and efficient in terms of observing time. ... where Dn refers to diode n and sn to substep n . ...

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• The Panchromatic Hubble Andromeda Treasury. VIII. A Wide-area, High-resolution
• Marshall Perrin's Research
• COS Spectroscopic Observing Strategies

... ST-ECF, ESO, STScI and the NICMOS IDT organized a workshop on near infrared imaging from space and ground was held in Pula on May 26-27, 1998. ... The meeting was held in May 1998, about one year after science observations started with NICMOS, and about half a year before the Infrared Spectrometer and Array Camera (ISAAC) starts to operate on the VLT. Currently, it is expected that NICMOS will operate until the end of 1998. ...

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• NICMOS Data Calibration and Analysis
• ASNCOMBINE (Nov98) --- nictools --- ASNCOMBINE (Nov98)
• No Title

New Opportunities 2010 and Beyond: The High-Energy/Radio Connection High Energy Missions Timeline XMM, Suzaku.. ... Hard X-ray Sky EXIST Wide-Field Hard X-ray Imaging: EXIST ·~20X more sensitive than Swift or INTEGRAL and cover full sky ·Detect ~104 sources, 10 positions, 3-600 keV spectra ·unique temporal survey: full sky imaging each orbit High Energy Telescope HET (10-600keV) (6 x 3 coded aperture telescopes; 131o x 65o FoV) Low Energy Telescope LET (3-30 ...

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• lbw_crosshead_rfi_may09
• high resolution decimation test
• HISA Poster for the 33rd Annual Meeting of CASCA, May, 2002

... Use the ROSAT broad band background which is a array file at 1/30 the *.qp file resolution, and contains data from PI bins 7-240. input files: xdata$rp110590.qp; xdata$rp110590_bk1.imh . ... xr> ximages xi> imcalc input file ('-' for STDIN) or imcalc commands: - # Interactive mode IMC) IMC) rp90_a.imh = xdata$rp110590.qp[bl=30,pi=7:240] - xdata$rp110590_bkl.imh # Select same size and channels as the background map # and subtract the background IMC) quit # To exit the interactive mode and imcalc . ...

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• The AstroStat Slog background
• To Resample Calibration Images
• Microcalorimeter Energy Resolution Example

... A Year of Resolving Backgrounds . ... In X-ray light the recently launched spacecraft Chandra and XMM resolved much of the seemingly uniform X-ray background into many discrete sources, many of which appear to be black holes at the centers of galaxies accreting matter. In microwave light , the BOOMERANG and MAXIMA-1 missions resolved with new clarity the seemingly uniform microwave background . ... Publications with keywords: cosmic microwave background radiation . ... Our Dusty Universe . ...

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• The Cosmic Infrared Background
• Астронет > A Year of Resolving Backgrounds
• Journal "Peremennye Zvezdy"

SiD Tracking using VXD Nick Sinev, University of Oregon Plan Motivation Track reconstruction algorithm Performance for single tracks Does it have any limits ? With backgrounds To do Motivation Tracking in SiD is a challenge, especially pattern recognition. ... Limitations caused by reconstruction speed consideration In the presence of high number of background hits, number of 3-point combinations used as track seed became enormous if we consider all combinations. ...

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• http://zebu.uoregon.edu/~uochep/talks/talks03/ecal.pdf
• http://zebu.uoregon.edu/~uochep/talks/talks02/LC-detectors-2.pdf
• http://zebu.uoregon.edu/~uochep/talks/talks01/Hopkins-det-01.PDF

Using DIFX with ASKAP Chris Phillips, eVLBI Project Scientist November 2011 Murchison Radio Observatory Murchison Radio Observatory gazetted towns: 0 population: up to 160 population: 16 million ASKAP Design Goals High-dynamic range, wide field-of-view imaging Number of dishes Dish diameter Max baseline Resolution Sensitivity Speed Observing frequency Field of View Processed Bandwidth Channels Integration time Focal Plane Phased Array 36 12 ...

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• http://www.atnf.csiro.au/research/WALLABY/Wallaby2010/RJurek-Wallaby2010.pdf
• Resolution of an interferometer
• An Imaging Survey of the Northern Galactic H Emission with Arcminute Resolution

Limiting Resolution . The terms MTF cutoff frequency, limiting resolution, and resolving power have all been used interchangeably to define the smallest target that can be resolved with an imaging system. Although the term 'limiting resolution' is often used to describe the smallest target length that can be imaged. ... For example, high frequency targets can be reproduced from their low frequency fundamentals and phase errors can produce 'phantom' images that resemble high frequencies. ...

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• Electron bombarded sensors-resolution
• Documentation: LEDA: parameter: bar
• Cosmic InfraRed Background Images

... Thus all regions of the 0.94-2.50 micron wavelength range accessible from Mauna Kea can be recorded using five fixed angle gratings. ... Grating Angle . ... Efficiencies for the NIFS gratings are shown above. The NIFS spectrograph uses a Bouwers collimator and a refractive camera. ... With these assumptions, the NIFS system efficiency including the Gemini telescope optics but excluding the transmission of the adaptive optics system is about 0.17 e - /photon at J , and 0.22 e - /photon at H and K . ...

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• Gemini Near-Infrared Integral-Field Spectrograph (NIFS) Detector.
• Gemini Near-Infrared Integral-Field Spectrograph (NIFS) Sensitivity.
• Siding Spring Survey

The 6th INTEGRAL Workshop . The Obscured Universe . ... The main goal of this workshop is to consider (via invited and contributed talks and posters) the scientific problems in the field of high energy astrophysics which are possible to solve using the International Gamma-Ray Astrophysics Laboratory INTEGRAL as well as to present and discuss the scientific results already obtained by this observatory and its coordinated observations with on-ground telescopes and other spacecrafts. ...

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• Andrey Kravtsov "High-Resolution Cosmological Simulations of Cluster Formation"
• z90-program

... Galaxies 99 Cosmic background with model of cloudy interstellar medium Yu. ... Figure 1: Averaged spectrum of the cosmic background I f in frequency range 0.25 200 MHz for the Galactic poles. ... First interpretation of the cosmic noise background spectrum at broad band frequency range 0.25 200 MHz with a model of the cloudy interstellar medium ISM is presented here. ... Synthesized background spectra I f for regions of the Galactic poles at the frequency range 0.25 200 MHz is presented in Fig. ...

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• http://www.gao.spb.ru/english/publ-s/viii-rfs/p011.pdf
• http://www.gao.spb.ru/english/publ-s/viii-rfs/p133.pdf

... Day-by-day lines contain complete set and intended for those who have been there (I mean, in Kyoto :) . ... Large format is mainly for 1600x1200 screens and fast link (pictures are up to 150K in size). Normal is for typical 1024x768 screen (i.e. 15" monitors). ... Photos look incredible on it. ... Large . ... Normal . ... Thumbnails . ... Contents with thumbnails: Large | ... Nara, one of the historical cities of Japan . ... August 17, Sunday. ... Nara. ... return to photo album contents | ...

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• The pyramidal (multi-resolution) CCT
• Album: Resolution
• Continuous wavelet transforms

... Apache HTTP Server Version 2.4 . ... This page could be summarized with the statement: don't configure Apache HTTP Server in such a way that it relies on DNS resolution for parsing of the configuration files. If httpd requires DNS resolution to parse the configuration files then your server may be subject to reliability problems (ie. it might not start up), or denial and theft of service attacks (including virtual hosts able to steal hits from other virtual hosts). ... The "main server" Address . ...

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• Fasti Web Site
• Arcetri Solar Physics Group: High Resolution Studies
• Performances of NICS