Next: Background Correction Up: Reduction using Standard Previous: Order definition: Method . The parameter WIDTH2 is the width of the calibration lines. ... Now we can execute CALIBRATE/ECHELLE . ... CALIBRATE/ECHELLE DONE ! ... The user is prompted for the identification of two calibration lines on the image display, repeated in overlapped regions of adjacent orders. ... The wavelength calibration is wrong and apparently no identification error was made: There are too many lines per order. ...

The bkg keyword is used to perform throughput and emission calculations pertaining to the background signal component of grism observations. In grism observations, a given detector pixel will receive source signal from only a small wavelength interval of the dispersed source spectrum, but it will receive background signal from the entire bandpass of the grism. ... The bkg keyword is only valid when grisms are specified as part of the obsmode. ...

Next: Imaging Polarimetry with NICMOS Up: NICMOS Data Calibration and Previous: The Photometric Performance of . ... NICMOSlook and Calnic C . ... Extracting spectra from a large number of NICMOS grism images requires a convenient interactive tool which allows a user to manipulate direct/grism image pairs. ... NICMOSlook and Calnic-C are two programs that were designed to take advantage of the fact that the NICMOS grism mode typically consists of taking both a direct and a grism image. ...

Computer Ephemeris. Ephemeris for physical observations of the planets. Explanations. Each row of the table contains for date specified at 0h of Time Terrestrial Dynamical: . ... position angle of axis of planetary rotation (degrees) - 'P', . ... illumanated part of the disk - k, . ... position angle of disk point with minimal illumination (degrees), . longitude of central meridian of the disk (degrees) - 'merid1' - system I and so... phase correction (degrees). ...

... About ATNF overview . ... Australia Telescope Steering Committee . ... Australia Telescope User Committee . ... Staff list | ... Murchison Radio-astronomy Observatory . ... Parkes radio telescope . Australia Telescope Compact Array . Mopra radio telescope . ... Australia Telescope Online Archive (ATOA) . ... VLBI . ... Australia Telescope 20GHz Survey . ... This message : [ Message body ] [ More options ( top , bottom ) ] . ... radio observations for the exploration of our Solar System and . ...

The beam pattern and the polarization characteristics . of the radio telescope RATAN-600 . The Mueller matrix elements was computed via formulas [1]: . ... The BP were computed by the aperture method, proceeding from the fild distribution in the aperture of the primary mirror. The components of the main and cross-polarization components of the electric field in the vertical aperture of the primary mirror was computed in Frenel diffraction approximation. ...

... Posts tagged ?X-ray? ... Posted by vlk . There is a lesson that statisticians, especially of the Bayesian persuasion, have been hammering into our skulls for ages: do not subtract background. ... 6 Comments . ... Algorithms arXiv Astro Bad AstroStat Bayesian CHASC Cross-Cultural Data Processing Fitting Frequentist Galaxies gamma-ray High-Energy Imaging Jargon Job Languages MC MCMC Meta Methods Misc News Nuggets Objects Optical Physics Quotes Spectral Stars Stat Timing Uncertainty X-ray . ...

... The J, H and K bands are characterized by a bright background, such a background is mainly due to the emission of atmospheric lines and of thermal radiation. ... If the source cover a large fraction of the slit, spectra off-source must be observed to adequately sample the sky background. ... The on chip integration time (time spent in each position of the slit) must not exceed 40 seconds in J and H bands and 60 seconds in K band. ... We suggest a sequence of 10 for each elementary integration time. ...

... 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. ...

... Next: The PROS Big Up: Software Systems Previous: Data Reduction Software . ... The srcinten task provides PROS users with a tool to compute count rates for point sources in the ROSAT High Resolution Imager (HRI). ... Corrected upper limits are cited at locations where the count rate falls below the source detection threshold. ... Srcinten is a new PROS task that computes and applies the above correction factors to the net counts in a user-specified aperture. ...

... Copyrightї1997 Bob Yen (byen@ix.netcom.com) (http://www.comet-track.com/hb/hb.html) . ... Information on Comet Hale-Bopp for the Non-Astronomer Hale-Bopp rotates about twice a day (3/14/97) . ... The Comet Observation Home Page was been selected to receive the Griffith Observatory Star Award for the week of February 2 - 8, 1997 for excellence in promoting astronomy to the public through the World Wide Web. ... Typically, about 1,000 individual users/computers access this page every day. ...

Notes concerning the observations made by UKIRT for the YY Gem programme in March 1988. ... As spot modulation effects are relatively more prominent in V and flare effects in B, it was decided to monitor in K and V during eclipses and in K and B at out of eclipse phases. ... The data were corrected for extinction using the following extinction coefficients: B 0.27, V 0.10, K 0.07, J 0.10 . ... The following colour equations were derived for the UKIRT optical data using VISPHOT. ...

The VLTI Calibrator Selector Tool is a tool intended to assist in the selection of suitable interferometric calibrators for VLTI observations with MIDI and AMBER. It uses a model of the VLTI and its instruments to assess the fringe visibility, given the observed bandpass, the geometry, spectrum, and coordinates of the target and the time at which the observations are to be made. ... The tool offers an HTML/Java based interface and consists of two pages. ... The quality flag depends on LDD_chi2. ...

... 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. ...

Twilight observations with MASS/DIMM B. Safonov Sternberg Astronomical Institute Moscow State University Comprehensive Characterization of Astronomical Sites, 2010 B. Safonov (Moscow State University) Twilight observations with MASS/DIMM SITE 2010 1 / 17 Why observe in twilight with MASS/DIMM? ... ASM includes 3 devices sensitive to background: guider, DIMM and MASS. B. Safonov (Moscow State University) Twilight observations with MASS/DIMM SITE 2010 2 / 17 Background in guider. ...

... Radio: Large shell, with flatter spectrum component (Vela X), and pulsar nebula. ... Distance: Vela pulsar parallax gives 0.3 kpc, optical spectra and H I studies suggest 0.25 kpc. ... Parkes 64-m at various frequencies, including 408 MHz (48': S=2300?300 Jy), 635 MHz (31': S=2360?300 Jy), 1410 MHz (14': S=1640?300 Jy) and 2650 MHz (7'.5: S=1400?250 Jy), plus discussion of the distance. ... VLA at 330 MHz (1'?1'.8) and comparison with ROSAT observations of Vela X. ADS . ... 2001, ApJ, 549, 416. ...

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... Информация Руководство и преподаватели Денисова Анна Юрьевна . ... Публикации . ... Денисова А.Ю. , Мясников В.В. Anomaly Detection Using Spectral Mismatch Between Anomaly Pattern and its Neighborhood // 23-rd International Conference on Computer Graphics, Visualization and Computer Vision (WSCG 2015), 8-12 июня 2015 г., Пльзень, Чехия, Vaclav Skala - UNION Agency , 2015 г., С. 41-47 . ... 2015. ... 2014. ... Sergeyev, V.V. , Денисова А.Ю. | ... Самара: Новая техника, 2015. 256 с. 1. ...

... This is possible at modest cost due to the low moments of inertia of the telescope and enclosure. ... This same performance will be achieved in higher winds when the telescope enclosure is facing away from the wind, or by using wind screens. ... The telescope system (MILT) will be remotely operable with an on-site operator's assistance by an astronomer located at one of the ARC member institutions. ... Mean Wind Speed . ... Offsets > 10 deg: 1 arc sec rms max . ... 5 sec max, tracking to tracking . ...

... During all period of our investigations Dr. N.Sumzina from the Institute of Applied Astronomy of RAS had prepared the Numbered Minor Planet positions from MPC Database for our processing with kind permission of the Director of Minor Planet Center Prof. Braian Marsden. ... Our extensive processing of the MPC data allows us to conclude that CCD observations of the Numbered and Unnumbered Minor Planets have the errors, sometimes very crude. ...