. Next: Energy resolution Up: Charge Coupled Devices (CCDs) Previous: Contrasting optical and X-ray . Energy resolution . Detection Efficiency . Deep Depletion . Front Illumination . Back Illumination . Particle Background Rejection . Field of View . Dark current and cooling . Modes of Operation . Radiation Hardness . Dave Lumb . Fri Aug 30 07:43:04 MET DST 1996

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• Introduction
• Contrasting optical and X-ray applications
• Modes of Operation

... HST . ... Data . ... HST Overview . ... Phase I Proposing . ... STIS . ... Between launch on 14-Feb-1997 and failure of the "Side-1" electronics on 2001-May-16, CCD temperature was stabilized at -83 C. During the Side-1 era, the CCD median dark rate rose from 0.0013 to 0.0043 e-/sec/pix. CCD temperature cannot be stabilized with the "Side-2" electronics, so after 2001-May-16 thermal fluctuations perturb the dark rate. ... Please see HST Phase II Proposal Instructions for additional information. ...

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• Background
• A Brief Description of the Instrument and Its Operation
• COS Background Performance

... 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
• Object Detection Using Multi-Resolution Analysis
• A New PROS Task for Calculating HRI Source Intensities or Upper Limits

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

... 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
• CONICA: The high resolution near-infrared camera for the ESO VLT
• ST-ECF Grism Spectrum Software for NICMOS Grism Data

High resolution IR-spectrometer . ... Determination of concentration of atmospheric greenhouse gases (carbon dioxide and methane) from ground-based or spacecraft platforms. ... Compact eschelle spectrometer is built by autocollimation scheme with diffraction grating operating in high orders of diffraction, allowing thereby to reach the resolution up to ?/ 20 000. ... For observations at the ground-based platforms and aboard the ISS the instrument modification RUSALKA will be used. ...

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• Shift
• Folding Paper Model of Magnetosphere
• PhSRM

... 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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• Hardware sector, archive 2002
• Hardware sector, archive 2014

The overall efficiency (including atmospheric transmission, reflectivity of the telescope mirrors and overall efficiency of the optics and of the detector) for broad-band imaging should be about 25% in H and K, and about 15% in J. The main noise source for both broad- and narrow-band imaging should be the photon noise associated to the background+source flux. ... Flat fielding (and possibly background subtraction) might increase the noise by a factor 2 ? ...

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• Observing capabilities
• Arcetri Solar Physics Group: High Resolution Studies
• Optical System

... First of all, I should say that you cannot guarantee user-mode processes to have exact control of timing because of the multi-tasking nature of Linux. ... However, for most applications using I/O ports, this does not really matter. To minimise this, you may want to nice your process to a high-priority value (see the nice(2) manual page) or use real-time scheduling (see below). ... Linux 2.x kernels have soft real time support; see the manual page for sched_setscheduler(2) for details. ...

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• High resolution Zeeman spectrum of HD4778
• Optimization of spectroscopic observations
• DINACON

T he Siding Spring Survey (SSS) is a Near-Earth Object search program that utilises the 0.5-m Uppsala Schmidt Telescope at Siding Spring Observatory, N.S.W., Australia. ... The mission of the Siding Spring Survey is to contribute to the inventory of near-earth objects (NEOs), or more specifically, the potentially hazardous asteroids (PHAs) and comets (PHOs) that may pose a threat of impact and thus harm to civilization. ... Based on the CSS Mission page . ... Siding Spring Survey Main Page . ...

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... Instrument Status . Science Verification . ... CRIRES . ... SV observer shall submit their proposals using the Science Verification proposal template Proposers are asked to provide at least a short summary of the science goal, coordinates and magnitudes of GS and science target, a finding chart , the observing wavelength ID, as specified in appendix A of the UM and DIT, NDIT settings of science detectors as computed with the exposure time calculator (see below). ... with a 0.2 arcsec slit. ...

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• ESO - Paranal Science Operations: End of Missions Report
• ESO - Science Announcements
• ESO - Paranal Instrumentation

... Astrophysics Group . ... VSA . ... CAT . ... The Very Small Array is a custom-built radio telescope (operating between 26-36 GHz), designed expressly to make high resolution observations of the cosmic microwave background (CMB) radiation on angular scales around and below one degree. ... The VSA has been operated in ?compact array? and ?extended array? configurations (see the technical description below) and data collected to achieve high sensitivity in both regimes have been analysed. ... 1.75 GHz)...

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• Research David Buscher
• Astrophysics Group CAT
• VLSS Postage Stamp Server Documentation Help for VLSS Postage Stamp Server

... WISE is achieving 5sigma point source sensitivities better than 0.08, 0.11, 1, and 6 mJy in unconfused regions on the ecliptic in bands centered at wavelengths of 3.4, 4.6, 12, and 22 mum. ... The WISE All-Sky Release Source Catalog is available in compressed (gzip or bzip2) ascii form. ... Users should be aware that the Catalog table is extremely large. ... For complete documentation of the WISE All-Sky Release Source Catalog and the All-Sky Data Release, please see the Explanatory Supplement . ...

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• Electron bombarded sensors-resolution
• Explanatory Supplement to the 2MASS Second Incremental Data Release
• NASA EPSCoR Appendices B+C

... ARC 3.5m | Instrument Summary . ... ARCES (Echelle) : the ARC Echelle spectrograph, a high resolution (R~31,500) echelle spectrograph that observes the entire wavelength range from 3200 е to 10000 in a single image on a 2048x2048 CCD. This instrument is permanently mounted at the NA1 port. ... In addition to the facility instruments, several visitor instruments have been used at the 3.5m, and some of these are available to the ARC observing community by contacting the instrument PIs: . ...

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• MILT Description
• Performance of the SDSS cloud scanner I: the first movie
• APO Job Announcements

... Radio astronomy . ... This is impractical so, instead, we synthesise such a telescope by building an array of antennas. ... To obtain very high resolution, we use a technique known as Very Long Baseline Interferometry (VLBI) where we combine signals from the ATNF antennas together with other antennas in Australia, to form the Australian VLBI array, which can synthesise a telescope up to 3000 km in diameter. The resolution of this array exceeds even that of the Hubble Space Telescope. ...

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• MAPPIT 2: Second Generation High-Resolution Imaging at the AAT
• difx:highspecres [ATNF VLBI Wiki]
• Australia Telescope Compact Array Home Page

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

... 6.02.2002 . ... Credit: A. Kashlinsky ( SSAI ) S. Odenwald ( Raytheon ), 2MASS , NSF , NASA Explanation: What cosmic wallpaper is on the sky? ... Recently, however, the background in near infrared light was imaged at high resolution by the 2MASS telescope , and confirmed earlier estimates that it is over twice as bright as originally expected. ... Visible is light emitted from the very first stars and galaxies in the universe , emitted when the universe was less than half its current age. ...

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• A Year of Resolving Backgrounds
• Астронет > A Year of Resolving Backgrounds
• XWare > APOD

... 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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• Michael Juda - Home Page
• HEAD 2010: Chandra's Ultimate Angular Resolution
• Microcalorimeter Energy Resolution Example

... We will consider the rms, (K), for observations with a receiver of system temperature, T , frequency resolution, per polarization, and total integration time per observing cycle, . ... For ``in-band'' frequency switching, the line under investigation is always in the observing band. ... Position Switching or ``Out-of-Band'' Frequency Switching: Here the line is only observed for one half of the time, with noise being present all of the time. ...

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• Pulsar Instrumentation the Arecibo Observatory
• Getting the Best Performance from the API
• HF transmitter doc

... -NASA EXPERIENCE: Construction, Omaha, NE (1959) Aberdeen Proving Ground, MD (1959-1962) NASA EXPERIENCE: NASA Manned Spacecraft Center / Johnson Space Center , Houston, TX (1962-1995) · Mathematician, Operations Analysis Branch, Flight Operations Division (1962-1963) · Mathematician, Aerospace Technician, Trajectory Analysis Section, Flight Analysis Branch, Flight REFERENCES: "25 Years Plus," Space News Roundup (NASA Johnson Space Center), 3 February 1995, 4. ...

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• http://www.jsc.nasa.gov/history/oral_histories/ShelleyCB/ShelleyCB_Bio.pdf
• http://www.jsc.nasa.gov/history/oral_histories/WhittleDW/WhittleDW_Bio.pdf
• http://www.jsc.nasa.gov/history/oral_histories/DavisLD/DavisLD_Bio.pdf