... Advanced Camera for Surveys Instrument Handbook for Cycle 24 > Chapter 3: ACS Capabilities, Design and Operations > 3.3 Instrument Design . ... The nonfunctioning HRC has a 1024 x 1024 SITe CCD, with 21 x 21 µm pixels that provided ~0.028 x 0.025 arcsecond/pixel spatial resolution with critical sampling at 6300 е. This gave the HRC a nominal 29 x 26 arcsecond field of view. ... The ACS design incorporates two main optical channels: one for the WFC, and one which is shared by the HRC and SBC. ...

HEXTE Phoswich Detector 6/19/2006 Calibration Workshop, Iceland 2006 1 HEXTE Features Aperture Modulator AGC Detector "Mu Metal" Housing 6/19/2006 Calibration Workshop, Iceland 2006 Particle Monitor 2 RXTE/HEXTE Design and Calibration · Calibration begins with instrument design. ... 6/19/2006 Calibration Workshop, Iceland 2006 7 HEXTE Calibration -- Energy Resolution All of the detectors could not be taken to the synchrotron beam for detailed calibration. ...

Next: The Transmission Gratings Up: The Instruments Previous: The Instruments . ... A conventional cross-grid charge detector reads out the photo-induced charge cloud and the electronics determine an arrival time to 16s, and the position with a resolution of about 18 m or 0.37 arcsec. ... The Massachusetts Institute of Technology's Center for Space Research, in collaboration with Lincoln Laboratories, developed the detector system and manufactured the CCDs; Lockheed-Martin integrated the instrument. ...

... 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. ...

Next: The ESO VLT CCD Detectors Software . ... Up: Instrument-Specific Software . ... The framework for data calibration and analysis of the VLT instrumentation is presented, based on the concepts of a calibration plan, pipeline calibration, quality control, and archiving of calibrated data for a ground-based observatory. ... Quality Control Pipeline provides quality assessment for instrument performance data and observing conditions, and tests the results of the Reduction Pipeline. ...

. Next: Using a Standard Up: Echelle Spectra Previous: Flat Field Correction . љ . Using a Standard Star . Fitting the Blaze Function . Pascal Ballester . Tue Mar 28 16:52:29 MET DST 1995

... 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: . ...

. Next: ROSAT and EINSTEIN Calibration Up: Point Response Functions Previous: Point Response Functions . Mathematical determinations of some PRFs can be found by typing: . xr> help prf . This in turn refers to several detailed help files for specific instruments. For an example of constructing an analytical model PRF for ROSAT . rsdc@cfa.harvard.edu . 1998-06-10

SHORT DESCRIPTIONS OF INSTRUMENTS . ... Particle detector RIEP-2802 was developed and built in Russia. ... The combined Soviet-French ONCH-TBF onboard instrument had in memory modes the data only from several filter-banks in the range from 10 Hz to 16 kHz (while in the real-time telemetry modes, the measurements included 5-component wave-form data in the range 10 Hz - 1.5 kHz for 3 magnetic and 2 electric field components, or a wide-band mode in the range 10 Hz - 15 kHz, and several filter banks). ...

The basic characteristics of the instrument are set by the aperture, focal length and resolution of the image forming lens, the dispersion of the spectrometer, and the sensitivity of the detector. ... The lens is internally focused, and maintains acceptable focus (2 pixels in the detector plane) over a typical spectral coverage of one grating setting. ... along the spatial dimension of a 25mm square detector in the final spectral image plane the 400mm lens is 3.2њ. ... Diffraction grating . ...

... NICS will be the only infrared instrument for the first light of the TNG; as a consequence, we decided to incorporate a sufficient degree of operation flexibility by providing the instrument with six different observing modes, three aimed at imaging and three at spectroscopy: . ... It will be possible to use the narrow band filters as order sorters; this will allow to perform high resolution long-slit spectroscopy in the wavelength ranges covered by the available narrow band filters. ...

... Status of the ELECTRON experiment . ... The objective of the ELECTRON experiment is to perform 3-D measurements of the plasma electrons in the energy range from 10 eV to 26000 eV, with good angular resolution, sensitivity and large dynamical range. ... Figure 1 presents the ELECTRON sensor. ... Click on the picture to view large one) . ... Figure 3 shows dynamical spectra with counting rate measurements performed by ELECTRON experiment during very multiple magnetopause crossings on February, 4, 1996...

Static Fourier spectrometers are often used for spectral measurements of the ionosphere emissions. There are two main advantages of Fourier spectrometers (FS) - large geometric factor and high spectral resolution; these parameters are two orders better than for grating spectral instruments. ... In scanning Fourier spectrometer optical and electric modulation of signal is used to avoid this problem, for static Fourier spectrometer there are no such ways. ...

Next: VLT First Light Up: Front Cover Previous: Participants . VLT First Light . ... Image Quality of the VLT . ... Near IR Astronomy with the ESO VLT . Introduction and Overview . Infrared instruments for the VLT . Instrument Summary . ... Performance . ... CONICA: The high resolution near-infrared camera for the ESO VLT . Introduction . Design of Imaging Optics . Analyzing Optics . Cryo-mechanical Design . ...

... 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 ...

ATM Forum Message . Forums: . ... Post . ... Indoor Resolution . ... Post Message | ... Then photographing a line pair chart which can be purchased at a printer supply stores and better photography supply stores would be one way. ... www.astronomy.net . ... Unless otherwise specified, web site content Copyright 1994-2016 John Huggins All Rights Reserved . Forum posts are Copyright their authors as specified in the heading above the post. "dbHTML," "AstroGuide," "ASTRONOMY.NET" & "VA.NET" . ...

... Meade Instruments Corporation . ... Refracting telescopes (Meade Models NG-60, NGC-60, DS-2070AT, ETX-70AT, LXD55-AR5, LX55-AR6 ) and mirror-lens telescopes ( ETX-90AT, 105AT, 125AT, LXD55-SC8, 8LX90, LX200 GPS Series ) are generally more versatile in a wide array of land and astronomical applications. ... The intermediate-level observer, or the non-casual telescope user who wishes to purchase one telescope for a lifetime, should consider a Meade Model LXD55 series, 8LX90, or LX200GPS. ... Meade 4M ...

... Dodson, Legge et al, ApJ, 2003 Spectral Line Sources · Requirement of high brightness temperatures means no thermal emission · Masers: Galactic Extragalactic · OH, H2O · OH, H2O, SiO, CH3OH · Galactic extra-galactic HI absorption VLBI arrays · VLBA (Very Long Baseline Array) Dedicated US array of ten 25m telescopes 330 MHz ­ 90 GHz · EVN (European VLBI Network) Formal collaboration of radio telescopes in Europe, Asia and South Africa ~15 telescopes 15m to 100m 330 MHz ­ 22/43 GHz ...

. english || русский . Main . Location . Telescope . Instruments . Program . Science . Publications . Images . Photos . Links . The following focal instruments are currently available at the telescope: . CCD-photometer . TFOSC -- medium and low resolution spectrometer . ( The page at TUG ) . High resolution echelle-spectrometer in coude focus . High Energy Astrophysics Department 2016 IKI RAN

... The top panel shows Stokes I (black solid line, in arbitrary units, and not corrected for the instrument response), P V (red solid line centred about 0), and the null profile (blue solid line, offset by -0.75 % for display purpose). ... The slope of the red interpolating lines in the bottom panels gives the mean longitudinal field from P V (left panel)and from the null profile (right panel, the latter being expected zero), both calculated using the H Balmer lines only. ...